Author name code: fan
ADS astronomy entries on 2022-09-14
=author:"Fan, Y."
------------------------------------------------------------------------
Title: Synthetic Lyman-α emissions for the coronagraph aboard the
ASO-S mission. I. An eruptive prominence-cavity system
Authors: Zhao, J.; Zhang, P.; Gibson, S. E.; Fan, Y.; Feng, L.; Yu,
F.; Li, H.; Gan, W. Q.
Bibcode: 2022A&A...665A..39Z
Altcode:
Context. Strong ultraviolet (UV) emission from the sun will be observed
by the Lyman-α Solar Telescope (LST) on board the Advanced Space-based
Solar Observatory (ASO-S), scheduled for launch in 2022. It will
provide continuous observations from the solar disk to the corona
below a 2.5 solar radius with high resolution. To configure the
appropriate observing modes and also to better understand its upcoming
observations, a series of simulations and syntheses of different
structures and processes need to be done in advance.
Aims:
As prominence eruptions are the main drivers of space weather, the
need to monitor such phenomena has been set as a priority among the
objectives of ASO-S mission. In this work, we synthesize the evolution
of a modeled prominence-cavity system before and during its eruption
in the field of view (FOV) of LST.
Methods: We adopted the
input magnetohydrodynamic (MHD) model of a prominence-cavity system,
which is readily comparable to the Atmospheric Imaging Assembly (AIA)
observations. The Lyman-α emission of the prominence and its eruptive
counterparts are synthesized through the PRODOP code, which considers
non-local thermodynamic equilibrium (NLTE) radiative transfer processes,
while the other coronal part such as the cavity and surrounding
streamer, are synthesized with the FORWARD package, which deals with
optically thin structures.
Results: We present a discussion
of the evolution of the eruptive prominence-cavity system, analyzing
the synthetic emissions both on the disk near the limb and above the
limb as viewed by the coronagraph, as well as the three-dimensional
(3D) data of the MHD simulation.
Conclusions: The evolution of
the prominence-cavity system exhibits the condensation of cavity mass
onto the prominence and the evaporation of prominence plasma into the
central cavity. The synthetic emission in Lyman-α shows a similar
pattern as in the AIA extreme ultraviolet (EUV) wavelengths before
eruption, namely, the appearance of a "horn" substructure as a precursor
to the eruption. The emission of prominence with an optically thick
assumption is one to two orders of magnitude lower than the optically
thin one. Here, the dimming effect in Lyman-α is analyzed, for the
first time, for the eruptive prominence-cavity system. Accompanying the
prominence plasma motion during the eruption, the apparent dimming shows
a preferred location evolving from the top and bottom of the bright
core to the whole body above the bottom part, while the collisional
component progressively dominates the total emission of the flux rope
bright core at these locations. By analyzing the signal-to-noise ratio
(S/N) with a consideration of LST's optical design, we conclude that
the substructures in the cavity and the bright core of the CME can be
observed with sufficient S/N at different stages in the FOV of LST.
Title: Erratum: "Probing the Solar Meridional Circulation Using
Fourier Legendre Decomposition" (2021, ApJ, 911, 54)
Authors: Braun, D. C.; Birch, A. C.; Fan, Y.
Bibcode: 2022ApJ...924..140B
Altcode:
No abstract at ADS
Title: Search for the doubly charmed baryon
Ωcc+
Authors: LHCb Collaboration; Aaij, R.; Abellán Beteta, C.; Ackernley,
T.; Adeva, B.; Adinolfi, M.; Afsharnia, H.; Aidala, C. A.; Aiola, S.;
Ajaltouni, Z.; Akar, S.; Albrecht, J.; Alessio, F.; Alexander, M.;
Alfonso Albero, A.; Aliouche, Z.; Alkhazov, G.; Alvarez Cartelle, P.;
Amato, S.; Amhis, Y.; An, L.; Anderlini, L.; Andreianov, A.; Andreotti,
M.; Archilli, F.; Artamonov, A.; Artuso, M.; Arzymatov, K.; Aslanides,
E.; Atzeni, M.; Audurier, B.; Bachmann, S.; Bachmayer, M.; Back, J. J.;
Baladron Rodriguez, P.; Balagura, V.; Baldini, W.; Baptista Leite, J.;
Barlow, R. J.; Barsuk, S.; Barter, W.; Bartolini, M.; Baryshnikov, F.;
Basels, J. M.; Bassi, G.; Batsukh, B.; Battig, A.; Bay, A.; Becker, M.;
Bedeschi, F.; Bediaga, I.; Beiter, A.; Belavin, V.; Belin, S.; Bellee,
V.; Belous, K.; Belov, I.; Belyaev, I.; Bencivenni, G.; Ben-Haim, E.;
Berezhnoy, A.; Bernet, R.; Berninghoff, D.; Bernstein, H. C.; Bertella,
C.; Bertolin, A.; Betancourt, C.; Betti, F.; Bezshyiko, I.; Bhasin,
S.; Bhom, J.; Bian, L.; Bieker, M. S.; Bifani, S.; Billoir, P.; Birch,
M.; Bishop, F. C. R.; Bitadze, A.; Bizzeti, A.; Bjørn, M.; Blago,
M. P.; Blake, T.; Blanc, F.; Blusk, S.; Bobulska, D.; Boelhauve, J. A.;
Boente Garcia, O.; Boettcher, T.; Boldyrev, A.; Bondar, A.; Bondar,
N.; Borghi, S.; Borisyak, M.; Borsato, M.; Borsuk, J. T.; Bouchiba,
S. A.; Bowcock, T. J. V.; Boyer, A.; Bozzi, C.; Bradley, M. J.; Braun,
S.; Brea Rodriguez, A.; Brodski, M.; Brodzicka, J.; Brossa Gonzalo,
A.; Brundu, D.; Buonaura, A.; Burr, C.; Bursche, A.; Butkevich, A.;
Butter, J. S.; Buytaert, J.; Byczynski, W.; Cadeddu, S.; Cai, H.;
Calabrese, R.; Calefice, L.; Calero Diaz, L.; Cali, S.; Calladine,
R.; Calvi, M.; Calvo Gomez, M.; Camargo Magalhaes, P.; Campana,
P.; Campoverde Quezada, A. F.; Capelli, S.; Capriotti, L.; Carbone,
A.; Carboni, G.; Cardinale, R.; Cardini, A.; Carli, I.; Carniti, P.;
Carus, L.; Carvalho Akiba, K.; Casais Vidal, A.; Casse, G.; Cattaneo,
M.; Cavallero, G.; Celani, S.; Cerasoli, J.; Chadwick, A. J.; Chapman,
M. G.; Charles, M.; Charpentier, P.; Chatzikonstantinidis, G.; Chavez
Barajas, C. A.; Chefdeville, M.; Chen, C.; Chen, S.; Chernov, A.;
Chobanova, V.; Cholak, S.; Chrzaszcz, M.; Chubykin, A.; Chulikov, V.;
Ciambrone, P.; Cicala, M. F.; Cid Vidal, X.; Ciezarek, G.; Clarke,
P. E. L.; Clemencic, M.; Cliff, H. V.; Closier, J.; Cobbledick, J. L.;
Coco, V.; Coelho, J. A. B.; Cogan, J.; Cogneras, E.; Cojocariu,
L.; Collins, P.; Colombo, T.; Congedo, L.; Contu, A.; Cooke, N.;
Coombs, G.; Corti, G.; Costa Sobral, C. M.; Couturier, B.; Craik,
D. C.; Crkovská, J.; Cruz Torres, M.; Currie, R.; Da Silva, C. L.;
Dadabaev, S.; Dall'Occo, E.; Dalseno, J.; D'Ambrosio, C.; Danilina,
A.; d'Argent, P.; Davis, A.; De Aguiar Francisco, O.; De Bruyn,
K.; De Capua, S.; De Cian, M.; De Miranda, J. M.; De Paula, L.;
De Serio, M.; De Simone, D.; De Simone, P.; de Vries, J. A.; Dean,
C. T.; Decamp, D.; Del Buono, L.; Delaney, B.; Dembinski, H. -P.;
Dendek, A.; Denysenko, V.; Derkach, D.; Deschamps, O.; Desse, F.;
Dettori, F.; Dey, B.; Di Cicco, A.; Di Nezza, P.; Didenko, S.; Dieste
Maronas, L.; Dijkstra, H.; Dobishuk, V.; Donohoe, A. M.; Dordei, F.;
dos Reis, A. C.; Douglas, L.; Dovbnya, A.; Downes, A. G.; Dreimanis,
K.; Dudek, M. W.; Dufour, L.; Duk, V.; Durante, P.; Durham, J. M.;
Dutta, D.; Dziurda, A.; Dzyuba, A.; Easo, S.; Egede, U.; Egorychev,
V.; Eidelman, S.; Eisenhardt, S.; Ek-In, S.; Eklund, L.; Ely, S.;
Ene, A.; Epple, E.; Escher, S.; Eschle, J.; Esen, S.; Evans, T.;
Falabella, A.; Fan, J.; Fan, Y.; Fang, B.; Farry, S.; Fazzini, D.;
Féo, M.; Fernandez Prieto, A.; Fernandez-tenllado Arribas, J. M.;
Fernez, A. D.; Ferrari, F.; Ferreira Lopes, L.; Ferreira Rodrigues, F.;
Ferreres Sole, S.; Ferrillo, M.; Ferro-Luzzi, M.; Filippov, S.; Fini,
R. A.; Fiorini, M.; Firlej, M.; Fischer, K. M.; Fitzgerald, D. S.;
Fitzpatrick, C.; Fiutowski, T.; Fkiaras, A.; Fleuret, F.; Fontana,
M.; Fontanelli, F.; Forty, R.; Franco Lima, V.; Franco Sevilla, M.;
Frank, M.; Franzoso, E.; Frau, G.; Frei, C.; Friday, D. A.; Fu, J.;
Fuehring, Q.; Funk, W.; Gabriel, E.; Gaintseva, T.; Gallas Torreira,
A.; Galli, D.; Gambetta, S.; Gan, Y.; Gandelman, M.; Gandini, P.;
Gao, Y.; Garau, M.; Garcia Martin, L. M.; Garcia Moreno, P.; García
Pardiñas, J.; Garcia Plana, B.; Garcia Rosales, F. A.; Garrido, L.;
Gaspar, C.; Geertsema, R. E.; Gerick, D.; Gerken, L. L.; Gersabeck,
E.; Gersabeck, M.; Gershon, T.; Gerstel, D.; Ghez, P.; Gibson, V.;
Giemza, H. K.; Giovannetti, M.; Gioventù, A.; Gironella Gironell, P.;
Giubega, L.; Giugliano, C.; Gizdov, K.; Gkougkousis, E. L.; Gligorov,
V. V.; Göbel, C.; Golobardes, E.; Golubkov, D.; Golutvin, A.; Gomes,
A.; Gomez Fernandez, S.; Goncalves Abrantes, F.; Goncerz, M.; Gong,
G.; Gorbounov, P.; Gorelov, I. V.; Gotti, C.; Govorkova, E.; Grabowski,
J. P.; Grammatico, T.; Granado Cardoso, L. A.; Graugés, E.; Graverini,
E.; Graziani, G.; Grecu, A.; Greeven, L. M.; Griffith, P.; Grillo, L.;
Gromov, S.; Gruberg Cazon, B. R.; Gu, C.; Guarise, M.; Günther, P. A.;
Gushchin, E.; Guth, A.; Guz, Y.; Gys, T.; Hadavizadeh, T.; Haefeli,
G.; Haen, C.; Haimberger, J.; Halewood-leagas, T.; Hamilton, P. M.;
Hammerich, J. P.; Han, Q.; Han, X.; Hancock, T. H.; Hansmann-Menzemer,
S.; Harnew, N.; Harrison, T.; Hasse, C.; Hatch, M.; He, J.; Hecker,
M.; Heijhoff, K.; Heinicke, K.; Hennequin, A. M.; Hennessy, K.; Henry,
L.; Heuel, J.; Hicheur, A.; Hill, D.; Hilton, M.; Hollitt, S. E.; Hu,
J.; Hu, J.; Hu, W.; Hu, X.; Huang, W.; Huang, X.; Hulsbergen, W.;
Hunter, R. J.; Hushchyn, M.; Hutchcroft, D.; Hynds, D.; Ibis, P.;
Idzik, M.; Ilin, D.; Ilten, P.; Inglessi, A.; Ishteev, A.; Ivshin,
K.; Jacobsson, R.; Jakobsen, S.; Jans, E.; Jashal, B. K.; Jawahery,
A.; Jevtic, V.; Jezabek, M.; Jiang, F.; John, M.; Johnson, D.; Jones,
C. R.; Jones, T. P.; Jost, B.; Jurik, N.; Kandybei, S.; Kang, Y.;
Karacson, M.; Karpov, M.; Keizer, F.; Kenzie, M.; Ketel, T.; Khanji,
B.; Kharisova, A.; Kholodenko, S.; Kirn, T.; Kirsebom, V. S.; Kitouni,
O.; Klaver, S.; Klimaszewski, K.; Koliiev, S.; Kondybayeva, A.;
Konoplyannikov, A.; Kopciewicz, P.; Kopecna, R.; Koppenburg, P.;
Korolev, M.; Kostiuk, I.; Kot, O.; Kotriakhova, S.; Kravchenko, P.;
Kravchuk, L.; Krawczyk, R. D.; Kreps, M.; Kress, F.; Kretzschmar, S.;
Krokovny, P.; Krupa, W.; Krzemien, W.; Kucewicz, W.; Kucharczyk, M.;
Kudryavtsev, V.; Kuindersma, H. S.; Kunde, G. J.; Kvaratskheliya, T.;
Lacarrere, D.; Lafferty, G.; Lai, A.; Lampis, A.; Lancierini, D.; Lane,
J. J.; Lane, R.; Lanfranchi, G.; Langenbruch, C.; Langer, J.; Lantwin,
O.; Latham, T.; Lazzari, F.; Le Gac, R.; Lee, S. H.; Lefèvre, R.;
Leflat, A.; Legotin, S.; Leroy, O.; Lesiak, T.; Leverington, B.;
Li, H.; Li, L.; Li, P.; Li, S.; Li, Y.; Li, Y.; Li, Z.; Liang, X.;
Lin, T.; Lindner, R.; Lisovskyi, V.; Litvinov, R.; Liu, G.; Liu,
H.; Liu, S.; Loi, A.; Lomba Castro, J.; Longstaff, I.; Lopes, J. H.;
Lovell, G. H.; Lu, Y.; Lucchesi, D.; Luchuk, S.; Lucio Martinez, M.;
Lukashenko, V.; Luo, Y.; Lupato, A.; Luppi, E.; Lupton, O.; Lusiani,
A.; Lyu, X.; Ma, L.; Ma, R.; Maccolini, S.; Machefert, F.; Maciuc, F.;
Macko, V.; Mackowiak, P.; Maddrell-Mander, S.; Madejczyk, O.; Madhan
Mohan, L. R.; Maev, O.; Maevskiy, A.; Maisuzenko, D.; Majewski, M. W.;
Malczewski, J. J.; Malde, S.; Malecki, B.; Malinin, A.; Maltsev, T.;
Malygina, H.; Manca, G.; Mancinelli, G.; Manuzzi, D.; Marangotto, D.;
Maratas, J.; Marchand, J. F.; Marconi, U.; Mariani, S.; Marin Benito,
C.; Marinangeli, M.; Marks, J.; Marshall, A. M.; Marshall, P. J.;
Martellotti, G.; Martinazzoli, L.; Martinelli, M.; Martinez Santos, D.;
Martinez Vidal, F.; Massafferri, A.; Materok, M.; Matev, R.; Mathad,
A.; Mathe, Z.; Matiunin, V.; Matteuzzi, C.; Mattioli, K. R.; Mauri,
A.; Maurice, E.; Mauricio, J.; Mazurek, M.; McCann, M.; Mcconnell,
L.; Mcgrath, T. H.; McNab, A.; McNulty, R.; Mead, J. V.; Meadows, B.;
Meier, G.; Meinert, N.; Melnychuk, D.; Meloni, S.; Merk, M.; Merli,
A.; Meyer Garcia, L.; Mikhasenko, M.; Milanes, D. A.; Millard, E.;
Milovanovic, M.; Minard, M. -N.; Minotti, A.; Minzoni, L.; Mitchell,
S. E.; Mitreska, B.; Mitzel, D. S.; Mödden, A.; Mohammed, R. A.;
Moise, R. D.; Mombächer, T.; Monroy, I. A.; Monteil, S.; Morandin, M.;
Morello, G.; Morello, M. J.; Moron, J.; Morris, A. B.; Morris, A. G.;
Mountain, R.; Mu, H.; Muheim, F.; Mulder, M.; Müller, D.; Müller,
K.; Murphy, C. H.; Murray, D.; Muzzetto, P.; Naik, P.; Nakada, T.;
Nandakumar, R.; Nanut, T.; Nasteva, I.; Needham, M.; Neri, I.; Neri,
N.; Neubert, S.; Neufeld, N.; Newcombe, R.; Nguyen, T. D.; Nguyen-Mau,
C.; Niel, E. M.; Nieswand, S.; Nikitin, N.; Nolte, N. S.; Normand,
C.; Nunez, C.; Oblakowska-Mucha, A.; Obraztsov, V.; O'Hanlon, D. P.;
Oldeman, R.; Olivares, M. E.; Onderwater, C. J. G.; O'neil, R. H.;
Ossowska, A.; Otalora Goicochea, J. M.; Ovsiannikova, T.; Owen,
P.; Oyanguren, A.; Pagare, B.; Pais, P. R.; Pajero, T.; Palano,
A.; Palutan, M.; Pan, Y.; Panshin, G.; Papanestis, A.; Pappagallo,
M.; Pappalardo, L. L.; Pappenheimer, C.; Parker, W.; Parkes, C.;
Parkinson, C. J.; Passalacqua, B.; Passaleva, G.; Pastore, A.; Patel,
M.; Patrignani, C.; Pawley, C. J.; Pearce, A.; Pellegrino, A.; Pepe
Altarelli, M.; Perazzini, S.; Pereima, D.; Perret, P.; Petric, M.;
Petridis, K.; Petrolini, A.; Petrov, A.; Petrucci, S.; Petruzzo, M.;
Pham, T. T. H.; Philippov, A.; Pica, L.; Piccini, M.; Pietrzyk, B.;
Pietrzyk, G.; Pili, M.; Pinci, D.; Pisani, F.; Resmi, P. K.; Placinta,
V.; Plews, J.; Plo Casasus, M.; Polci, F.; Poli Lener, M.; Poliakova,
M.; Poluektov, A.; Polukhina, N.; Polyakov, I.; Polycarpo, E.; Pomery,
G. J.; Ponce, S.; Popov, D.; Popov, S.; Poslavskii, S.; Prasanth, K.;
Promberger, L.; Prouve, C.; Pugatch, V.; Pullen, H.; Punzi, G.; Qi,
H.; Qian, W.; Qin, J.; Qin, N.; Quagliani, R.; Quintana, B.; Raab,
N. V.; Rabadan Trejo, R. I.; Rachwal, B.; Rademacker, J. H.; Rama,
M.; Ramos Pernas, M.; Rangel, M. S.; Ratnikov, F.; Raven, G.; Reboud,
M.; Redi, F.; Reiss, F.; Remon Alepuz, C.; Ren, Z.; Renaudin, V.;
Ribatti, R.; Ricciardi, S.; Rinnert, K.; Robbe, P.; Robertson, G.;
Rodrigues, A. B.; Rodrigues, E.; Rodriguez Lopez, J. A.; Rollings,
A.; Roloff, P.; Romanovskiy, V.; Romero Lamas, M.; Romero Vidal, A.;
Roth, J. D.; Rotondo, M.; Rudolph, M. S.; Ruf, T.; Ruiz Vidal, J.;
Ryzhikov, A.; Ryzka, J.; Saborido Silva, J. J.; Sagidova, N.; Sahoo,
N.; Saitta, B.; Salomoni, M.; Sanchez Gonzalo, D.; Sanchez Gras, C.;
Santacesaria, R.; Santamarina Rios, C.; Santimaria, M.; Santovetti,
E.; Saranin, D.; Sarpis, G.; Sarpis, M.; Sarti, A.; Satriano, C.;
Satta, A.; Saur, M.; Savrina, D.; Sazak, H.; Scantlebury Smead,
L. G.; Scarabotto, A.; Schael, S.; Schiller, M.; Schindler, H.;
Schmelling, M.; Schmidt, B.; Schneider, O.; Schopper, A.; Schubiger,
M.; Schulte, S.; Schune, M. H.; Schwemmer, R.; Sciascia, B.; Sellam,
S.; Semennikov, A.; Senghi Soares, M.; Sergi, A.; Serra, N.; Sestini,
L.; Seuthe, A.; Seyfert, P.; Shang, Y.; Shangase, D. M.; Shapkin,
M.; Shchemerov, I.; Shchutska, L.; Shears, T.; Shekhtman, L.; Shen,
Z.; Shevchenko, V.; Shields, E. B.; Shmanin, E.; Shupperd, J. D.;
Siddi, B. G.; Silva Coutinho, R.; Simi, G.; Simone, S.; Skidmore, N.;
Skwarnicki, T.; Slater, M. W.; Slazyk, I.; Smallwood, J. C.; Smeaton,
J. G.; Smetkina, A.; Smith, E.; Smith, M.; Snoch, A.; Soares, M.;
Soares Lavra, L.; Sokoloff, M. D.; Soler, F. J. P.; Solovev, A.;
Solovyev, I.; Souza De Almeida, F. L.; Souza De Paula, B.; Spaan,
B.; Spadaro Norella, E.; Spradlin, P.; Stagni, F.; Stahl, M.; Stahl,
S.; Stefko, P.; Steinkamp, O.; Stenyakin, O.; Stevens, H.; Stone,
S.; Stramaglia, M. E.; Straticiuc, M.; Strekalina, D.; Suljik, F.;
Sun, J.; Sun, L.; Sun, Y.; Svihra, P.; Swallow, P. N.; Swientek, K.;
Szabelski, A.; Szumlak, T.; Szymanski, M.; Taneja, S.; Tanner, A. R.;
Terentev, A.; Teubert, F.; Thomas, E.; Thomson, K. A.; Tisserand,
V.; T'Jampens, S.; Tobin, M.; Tomassetti, L.; Torres Machado, D.;
Tou, D. Y.; Tran, M. T.; Trifonova, E.; Trippl, C.; Tuci, G.; Tully,
A.; Tuning, N.; Ukleja, A.; Unverzagt, D. J.; Ursov, E.; Usachov,
A.; Ustyuzhanin, A.; Uwer, U.; Vagner, A.; Vagnoni, V.; Valassi,
A.; Valenti, G.; Valls Canudas, N.; van Beuzekom, M.; Van Dijk, M.;
van Herwijnen, E.; Van Hulse, C. B.; van Veghel, M.; Vazquez Gomez,
R.; Vazquez Regueiro, P.; Vázquez Sierra, C.; Vecchi, S.; Velthuis,
J. J.; Veltri, M.; Venkateswaran, A.; Veronesi, M.; Vesterinen,
M.; Vieira, D.; Vieites Diaz, M.; Viemann, H.; Vilasis-Cardona,
X.; Vilella Figueras, E.; Villa, A.; Vincent, P.; Vom Bruch, D.;
Vorobyev, A.; Vorobyev, V.; Voropaev, N.; Vos, K.; Waldi, R.; Walsh,
J.; Wang, C.; Wang, J.; Wang, J.; Wang, J.; Wang, J.; Wang, M.; Wang,
R.; Wang, Y.; Wang, Z.; Wang, Z.; Wark, H. M.; Watson, N. K.; Weber,
S. G.; Websdale, D.; Weisser, C.; Westhenry, B. D. C.; White, D. J.;
Whitehead, M.; Wiedner, D.; Wilkinson, G.; Wilkinson, M.; Williams,
I.; Williams, M.; Williams, M. R. J.; Wilson, F. F.; Wislicki, W.;
Witek, M.; Witola, L.; Wormser, G.; Wotton, S. A.; Wu, H.; Wyllie,
K.; Xiang, Z.; Xiao, D.; Xie, Y.; Xu, A.; Xu, J.; Xu, L.; Xu, M.;
Xu, Q.; Xu, Z.; Xu, Z.; Yang, D.; Yang, S.; Yang, Y.; Yang, Z.; Yang,
Z.; Yao, Y.; Yeomans, L. E.; Yin, H.; Yu, J.; Yuan, X.; Yushchenko,
O.; Zaffaroni, E.; Zavertyaev, M.; Zdybal, M.; Zenaiev, O.; Zeng, M.;
Zhang, D.; Zhang, L.; Zhang, S.; Zhang, Y.; Zhang, Y.; Zharkova, A.;
Zhelezov, A.; Zheng, Y.; Zhou, X.; Zhou, Y.; Zhu, X.; Zhu, Z.; Zhukov,
V.; Zonneveld, J. B.; Zou, Q.; Zucchelli, S.; Zuliani, D.; Zunica, G.
Bibcode: 2021SCPMA..6401062L
Altcode: 2021arXiv210506841A
A search for the doubly charmed baryon Ωcc+
with the decay mode Ωcc+ →
Ξc+K−π+ is
performed using proton-proton collision data at a centre-of-mass
energy of 13 TeV collected by the LHCb experiment from 2016
to 2018, corresponding to an integrated luminosity of 5.4
fb−1. No significant signal is observed within the
invariant mass range of 3.6 to 4.0GeV/c2. Upper limits
are set on the ratio R of the production cross-section times
the total branching fraction of the Ωcc+
→ Ξc+K−π+
decay with respect to the Ξcc
++→Λc+K−π+π+
decay. Upper limits at 95% credibility level for R in the
range 0.005 to 0.11 are obtained for different hypotheses on the
Ωcc+ mass and lifetime in the rapidity range
from 2.0 to 4.5 and transverse momentum range from 4 to 15 GeV/c.
Title: The 4 m New Robotic Telescope Project: An Updated Report
Authors: Gutiérrez, C. M.; Torres, M.; Oria, A.; Fernández-Valdivia,
J. J.; Arnold, D.; Copley, D.; Copperwheat, C.; de Cos Juez, J.;
Franco, A.; Fan, Y.; García Piñero, A.; Harvey, E.; Jermak, H.;
Jiang, X.; Knapen, J. H.; McGrath, A.; Ranjbar, A.; Rebolo, R.;
Smith, R.; Steele, I. A.; Wang, Z.; Wu, X.; Xu, D.; Xue, S.; Yuan,
W.; Zheng, Y.
Bibcode: 2021RMxAC..53....8G
Altcode:
The New Robotic Telescope (NRT) is an international collaboration
to build and operate a 4m diameter fully robotic telescope. The
telescope will take advantage of the superb atmospheric conditions at
the Observatory of the Roque de los Muchachos (ORM). In conjunction
with a large aperture, entirely robotic operation, quick response,
and a set of versatile instrumentation in the optical and near-infrared
this guarantees a high scientific impact focused mainly in the area of
time domain astronomy. This paper presents the scientific motivation
and the status of the project, discussing possible technical solutions
under evaluation for the optics, mechanics and control system.
Title: The BOOTES Network in the Gravitational Wave Era
Authors: Hu, Y. D.; Li, X. Y.; Castro-Tirado, A. J.; Fernandez-García,
E. J.; Castellón, A.; Carrasco-García, I.; Perez del Pulgar, C.;
Caballero-García, M. D.; Querel, R.; Bai, J.; Fan, Y.; Guziy, S.;
Wang, C.; Xiong, D.; Xin, Y.; Zhao, X.; Hiriart, D.; Lee, W. H.;
Jeong, S.; Park, I. H.
Bibcode: 2021RMxAC..53...75H
Altcode:
The Burst Optical Observer and Transient Exploring System (BOOTES) is a
world-wide automatic telescope network which aims to repaid follow-up
of transient and astrophysical sources in the sky for which the first
station was installed in 1998. With the advent in 2015 of the LIGO/Virgo
interferometers, as part of the new generation of detectors designed
for the detection of the signal of gravitational waves, a new window
to explore the Universe has been opened. Here we present the status of
the BOOTES network, the related strategies regarding the follow-up of
gravitational wave events and the developments in the Gravitational
Wave Era. Some preliminary results regarding the BOOTES follow-up
observations are presented.
Title: GRB 140102A: insight into prompt spectral evolution and early
optical afterglow emission
Authors: Gupta, Rahul; Oates, S. R.; Pandey, S. B.; Castro-Tirado,
A. J.; Joshi, Jagdish C.; Hu, Y. -D.; Valeev, A. F.; Zhang, B. B.;
Zhang, Z.; Kumar, Amit; Aryan, A.; Lien, A.; Kumar, B.; Cui, Ch; Wang,
Ch; Dimple; Bhattacharya, D.; Sonbas, E.; Bai, J.; Tello, J. C.;
Gorosabel, J.; Castro Cerón, J. M.; Porto, J. R. F.; Misra, K.;
De Pasquale, M.; Caballero-García, M. D.; Jelínek, M.; Kubánek,
P.; Minaev, P. Yu; Cunniffe, R.; Sánchez-Ramírez, R.; Guziy, S.;
Jeong, S.; Tiwari, S. N.; Razzaque, S.; Bhalerao, V.; Pintado, V. C.;
Sokolov, V. V.; Zhao, X.; Fan, Y.; Xin, Y.
Bibcode: 2021MNRAS.505.4086G
Altcode: 2021MNRAS.505.4086.; 2021arXiv210513145G
We present and perform a detailed analysis of multiwavelength
observations of GRB 140102A, an optical bright GRB with an observed
reverse shock (RS) signature. Observations of this GRB were acquired
with the BOOTES-4 robotic telescope, the Fermi, and the Swift
missions. Time-resolved spectroscopy of the prompt emission shows
that changes to the peak energy (Ep) tracks intensity and
the low-energy spectral index seems to follow the intensity for the
first episode, whereas this tracking behaviour is less clear during
the second episode. The fit to the afterglow light curves shows that
the early optical afterglow can be described with RS emission and
is consistent with the thin shell scenario of the constant ambient
medium. The late time afterglow decay is also consistent with the
prediction of the external forward shock model. We determine the
properties of the shocks, Lorentz factor, magnetization parameters,
and ambient density of GRB 140102A, and compare these parameters with
another 12 GRBs, consistent with having RS produced by thin shells in
an interstellar medium like medium. The value of the magnetization
parameter (RB ≍ 18) indicates a moderately magnetized
baryonic dominant jet composition for GRB 140102A. We also report the
host galaxy photometric observations of GRB 140102A obtained with 10.4
m GTC, 3.5 m Calar Alto Astronomical Observatory, and 3.6 m Devasthal
optical telescope and find the host (photo z = $2.8^{+0.7}_{-0.9}$)
to be a high-mass, star-forming galaxy with a star formation rate of
$20 \pm 10 {\rm ~M_{\odot }}\, \rm yr^{-1}$.
Title: Boundary data-driven MHD simulations of the evolution of
AR 11158
Authors: Fan, Y.; Kazachenko, M.; Afanasev, A.; Fisher, G.
Bibcode: 2021AAS...23831320F
Altcode:
We have performed initial data-driven MHD simulations of the emergence
and evolution of Active Region (AR) 11158, using a lower boundary
driving electric field inferred from the time sequence of vector
magnetograms observed by the SDO/HMI with the PDFI-SS inversion method
(developed by Fisher et al. 2020), and an additional driving electric
field that represents sunspot rotation and shearing at the polarity
inversion line (PIL). We found that highly sheared, S-shaped sigmoid
loops form above the PIL of the central delta-sunspot, showing
morphology similar to that seen in the SDO/AIA observations. We
experiment with the additional electric field that drives the sunspot
rotation and shearing at the PIL and examine the conditions for the
development of the eruptive flares. Acknowledgement: This work
is supported in part by the NASA LWS grant 80NSSC19K0070 to NCAR.
Title: Formation of Coronal Flux Rope and Development of Blowout
Jet due to Magnetic Flux Emergence from the Solar Interior
Authors: Manek, B.; Fan, Y.; Fang, F.
Bibcode: 2021AAS...23821313M
Altcode:
We present 3D MHD simulations of a blowout jet formation from the
emergence of a twisted magnetic flux tube from the solar interior,
through the photosphere, into the corona. We explicitly incorporate the
solar corona's non-adiabatic effects, including simple empirical coronal
heating, optically thin radiative cooling, and field-aligned thermal
conduction. In the presence of an inclined ambient field in our study,
a coronal flux rope with an inverse configuration is formed. We find
that the coronal flux rope formed in our simulations is not due to the
subsurface flux tube's bodily emergence but due to the rotation of the
field lines above the PIL. This rotation arises from the shearing and
twisting motions at footpoints of the field lines, which transport twist
from the interior flux rope into the corona. A parameter survey
with varying lengths of the subsurface flux tube's buoyant segment
and different orientations of the inclined ambient field is carried
out in this work. We find that the formation of a rotating blowout
jet is a robust phenomenon in these cases. The coronal flux rope's
emerging core field erupts due to external magnetic reconnection with
the ambient field, thus transferring the twist from the flux tube to
the open field jet column. Interestingly, a subsurface flux tube with a
shorter buoyant section leads to a relatively earlier jet eruption due
to smaller anchoring at the photosphere. The jet eruption's energetics
also highlight the relative importance of shear Poynting flux than the
vertical Poynting flux in the relatively earlier jet eruption. This
work is supported in part by the NASA LWS grant 80NSSC19K0070 to NCAR.
Title: Probing the Solar Meridional Circulation Using Fourier
Legendre Decomposition
Authors: Braun, D. C.; Birch, A. C.; Fan, Y.
Bibcode: 2021ApJ...911...54B
Altcode: 2021arXiv210302499B
We apply the helioseismic methodology of Fourier Legendre decomposition
to 88 months of Dopplergrams obtained by the Helioseismic and Magnetic
Imager (HMI) as the basis of inferring the depth variation of the mean
meridional flow, as averaged between 20° and 60° latitude and in
time, in both the northern and southern hemispheres. We develop and
apply control procedures designed to assess and remove center-to-limb
artifacts using measurements obtained by performing the analysis with
respect to artificial poles at the east and west limbs. Forward modeling
is carried out using sensitivity functions proportional to the mode
kinetic energy density to evaluate the consistency of the corrected
frequency shifts with models of the depth variation of the meridional
circulation in the top half of the convection zone. The results, taken
at face value, imply substantial differences between the meridional
circulation in the northern and southern hemispheres. The inferred
presence of a return (equatorward propagating) flow at a depth of
approximately 40 Mm below the photosphere in the northern hemisphere is
surprising and appears to be inconsistent with many other helioseismic
analyses. This discrepancy may be the result of the inadequacy of our
methodology to remove systematic errors in HMI data. Our results appear
to be at least qualitatively similar to those by Gizon et al., which
point to an anomaly in HMI data that is not present in MDI or GONG data.
Title: Tracking CME substructure evolution through the solar wind
Authors: Gibson, S. E.; DeForest, C.; de Koning, C. A.; Fan, Y.;
Malanushenko, A. V.; Merkin, V. G.; Provornikova, E.; Thompson, B. J.;
Webb, D. F.
Bibcode: 2020AGUFMSH0280005G
Altcode:
Future coronagraphs and heliospheric imagers, in particular those
to be launched on the PUNCH mission, will have the capability to
track the evolution of CME substructures as the CME moves through and
interacts with the solar wind. We present analysis using polarization
data obtained from forward modeling simulations of CMEs in the corona
and inner heliosphere. We use these data to track the evolution
of substructures in three dimensions, and consider the diagnostic
potential of internal substructure vs structure at the front of the
CME. In particular, we develop methods for extracting information
about chirality of CME magnetic flux ropes from polarization data.
Title: GRB 201223A: BOOTES-4/MET early optical observation
Authors: Hu, Y. -D.; Fernandez-Garcia, E.; Castro, M. A.;
Castro-Tirado, A. J.; Perez del Pulgar, C.; Castellon, A.; Carrasco,
I.; Guziy, S.; Xiong, D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.
Bibcode: 2020GCN.29160....1H
Altcode:
Following the detection of GRB 201223A by Swift (Gropp et al. GCNC
29158), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical
Observatory (China) started to gather images in clear filter starting
at 18:01:22 UT (~176 s after trigger). The optical afterglow reported
by Swift/UVOT (Gropp et al. GCNC 29158), MASTER (Lipunov et al. GCNC
29157) and Nanshan/NEXT (Zhu et al. GCNC 29159) is detected with a
magnitude of 15.7+-0.15. Additional observations are ongoing. We thank
the staff at Lijiang observatory for their excellent support.
Title: Solar Prominence Bubbles and Associated Plasma Instabilities:
IRIS Observations and MHD Modeling
Authors: Liu, W.; Berger, T. E.; Fan, Y.
Bibcode: 2020AGUFMSH0010014L
Altcode:
Solar prominences are cool and dense plasma in the hot corona. The
so-called prominence bubbles are mysterious, dome-shaped, apparently
void structures residing in the lower portions of prominences. Such
bubbles are associated with various plasma instabilities, such as the
Rayleigh-Taylor (RT) and Kelvin-Helmholtz (KH) instabilities. The
former is manifested in plumes that are often produced at the top
boundary of a bubble and intrude upward into the dense prominence
material. The latter is found to be triggered by shear flows at the
bubble boundaries. We present recent observations of prominence
bubbles by IRIS, focusing on the diagnostic potential of RT and
KH instabilities on the physical conditions of the prominence and
its supporting magnetic field. We search for evidence of magnetic
flux emergence as the origin of prominence bubbles. We also present
preliminary 3D MHD simulations of the interaction of a bipole, as a
hypothetical bubble, emerging into an overlying prominence-carrying
flux-rope system. The simulations can provide further clues to the
origin and nature of prominence bubbles. We discuss their roll in mass
ad magnetic flux transport in the solar atmosphere.
Title: SunCET: A CubeSat Mission Dedicated to the Middle Corona
Authors: Mason, J. P.; Seaton, D. B.; Chamberlin, P. C.; Burkepile,
J.; Colaninno, R. C.; Dissauer, K.; Eparvier, F. G.; Fan, Y.; Gibson,
S. E.; Jones, A. R.; Kay, C.; Kirk, M. S.; Kohnert, R.; Thompson,
B. J.; Veronig, A.; West, M. J.; Woods, T. N.
Bibcode: 2020AGUFMSH0300006M
Altcode:
No abstract at ADS
Title: MHD Simulation of the 13 December 2006 Eruptive Flare of
AR10930
Authors: Fan, Y.
Bibcode: 2020AGUFMSH0440008F
Altcode:
We present an MHD simulation of the initiation of the coronal mass
ejection (CME) on 13 December 2006 in the emerging δ-sunspot active
region NOAA 10930. We have improved upon a previous simulation by Fan
(2016) in the following ways: (1) Incorporate an ambient solar wind
instead of using a static potential magnetic field extrapolation as
the initial state; (2) In addition to imposing the emergence of a
twisted flux rope at the lower boundary to build up the pre-eruption
field, also impose at the lower boundary a random electric field that
represents the effect of turbulent convection that drives field-line
braiding and the resultant resistive heating in the corona. With the
inclusion of this heating, which depends on the magnetic field topology,
we are able to model the synthetic soft X-ray emissions produced by
the coronal loops. We find that the simulated pre-eruption active
region magnetic field, where a twisted magnetic flux rope is built up
due to the flux emergence, produces synthetic soft X-ray emission that
shows qualitatively similar morphology as the observed X-ray image by
the Hinode/XRT, with the formation of an inverse-S shaped "sigmoid"
that sharpens at the onset of eruption. It is found that the rotation
and expansion of the erupting flux rope is significantly affected by
the two fast solar wind streams adjacent to the active region.
Title: Validation of the PDFI_SS Electric Field Inversion Method
Using MHD Simulations of Magnetic Flux Emergence
Authors: Afanasev, A.; Kazachenko, M.; Fan, Y.
Bibcode: 2020AGUFMSH046..02A
Altcode:
Knowledge of the vector electric field in the photosphere is useful
for calculations of the energy flux through the photosphere and for
boundary conditions for data-driven simulations of the evolving active
regions. Recently, the PDFI_SS method for estimating electric fields
from vector magnetic fields and Doppler velocities was improved to
incorporate the spherical geometry and a staggered-grid description
(Fisher et al. 2020). The method was previously validated using
synthetic input data from an anelastic magnetohydrodynamic simulation
(ANMHD). In this study, we further test the PDFI_SS method using
synthetic data from a more realistic flux emergence MHD simulation. We
use the output of the MHD simulations to perform the electric field
inversions at the photosphere and compare these to the known fields
in the simulation. We present results for different components of the
electric field vector and the Poynting flux. We discuss the similarities
and the differences, in particular, due to the complex structure of
horizontal plasma flows in the regions of high smooth magnetic fields.
Title: Major Scientific Challenges and Opportunities in Understanding
Magnetic Reconnection and Related Explosive Phenomena in Solar and
Heliospheric Plasmas
Authors: Ji, H.; Karpen, J.; Alt, A.; Antiochos, S.; Baalrud, S.;
Bale, S.; Bellan, P. M.; Begelman, M.; Beresnyak, A.; Bhattacharjee,
A.; Blackman, E. G.; Brennan, D.; Brown, M.; Buechner, J.; Burch, J.;
Cassak, P.; Chen, B.; Chen, L. -J.; Chen, Y.; Chien, A.; Comisso,
L.; Craig, D.; Dahlin, J.; Daughton, W.; DeLuca, E.; Dong, C. F.;
Dorfman, S.; Drake, J.; Ebrahimi, F.; Egedal, J.; Ergun, R.; Eyink,
G.; Fan, Y.; Fiksel, G.; Forest, C.; Fox, W.; Froula, D.; Fujimoto,
K.; Gao, L.; Genestreti, K.; Gibson, S.; Goldstein, M.; Guo, F.; Hare,
J.; Hesse, M.; Hoshino, M.; Hu, Q.; Huang, Y. -M.; Jara-Almonte, J.;
Karimabadi, H.; Klimchuk, J.; Kunz, M.; Kusano, K.; Lazarian, A.; Le,
A.; Lebedev, S.; Li, H.; Li, X.; Lin, Y.; Linton, M.; Liu, Y. -H.;
Liu, W.; Longcope, D.; Loureiro, N.; Lu, Q. -M.; Ma, Z-W.; Matthaeus,
W. H.; Meyerhofer, D.; Mozer, F.; Munsat, T.; Murphy, N. A.; Nilson,
P.; Ono, Y.; Opher, M.; Park, H.; Parker, S.; Petropoulou, M.; Phan,
T.; Prager, S.; Rempel, M.; Ren, C.; Ren, Y.; Rosner, R.; Roytershteyn,
V.; Sarff, J.; Savcheva, A.; Schaffner, D.; Schoeffier, K.; Scime, E.;
Shay, M.; Sironi, L.; Sitnov, M.; Stanier, A.; Swisdak, M.; TenBarge,
J.; Tharp, T.; Uzdensky, D.; Vaivads, A.; Velli, M.; Vishniac, E.;
Wang, H.; Werner, G.; Xiao, C.; Yamada, M.; Yokoyama, T.; Yoo, J.;
Zenitani, S.; Zweibel, E.
Bibcode: 2020arXiv200908779J
Altcode:
Magnetic reconnection underlies many explosive phenomena in the
heliosphere and in laboratory plasmas. The new research capabilities in
theory/simulations, observations, and laboratory experiments provide the
opportunity to solve the grand scientific challenges summarized in this
whitepaper. Success will require enhanced and sustained investments
from relevant funding agencies, increased interagency/international
partnerships, and close collaborations of the solar, heliospheric,
and laboratory plasma communities. These investments will deliver
transformative progress in understanding magnetic reconnection and
related explosive phenomena including space weather events.
Title: GRB 200608A: BOOTES-3 and BOOTES-4 optical upper limit
Authors: Hu, Y. -D.; Fernandez-Garcia, E.; Castro-Tirado, A. J.;
Carrasco, I.; Perez del Pulgar, C.; Caballero-Garcia, M. D.; Querel,
R.; Xiong, D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.
Bibcode: 2020GCN.27907....1H
Altcode:
The 60cm BOOTES-3/YA robotic telescope at NIWA Lauder in Otago (New
Zealand) responded to the Swift trigger of GRB 200608A (Moss et al. GCNC
27906). The first image (clear filter) was obtained at 19:18:40 UT
(~ 1.83 hr after trigger). In the co-added image (5 exposures 30s
each), no source is found at the region reported by Swift/BAT (Moss
et al. GCNC 27906) down to 17.4 mag. The 60cm BOOTES-4/MET robotic
telescope at Lijiang Astronomical Observatory (China) also gathered
images starting at 19:32:24 UT (~ 2.06 hr after trigger). No optical
afterglow is found down to 18.1 mag (unfiltered images) within the
Swift/BAT error box. Both observations were severely affected by the
presence of the moon about 13 degrees away. We thank the staff at NIWA
and YNO for their excellent support.
Title: The Mineralogy and Geochemistry of Shidian: A New Fall of CM
Chondrite in China
Authors: Fan, Y.; Li, S. J.; Liu, S.
Bibcode: 2020LPI....51.1234F
Altcode:
Shidian is a new falling meteorite in Yunnan, China which has
experienced serious aqueous alteration and was classified as CM2.2
subtype.
Title: SGR Swift J1818.0-1607: BOOTES-4/MET optical limit
Authors: Hu, Y. -D.; Fernandez-Garcia, E.; Castro-Tirado, A. J.;
Perez del Pulgar, C.; Castellon, A.; Carrasco, I.; Guziy, S.; Xiong,
D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.; et al.
Bibcode: 2020GCN.27378....1H
Altcode:
Following the detection of SGR Swift J1818.0-1607 by Swift (Evans et
al. GCNC 27373), the 0.6m BOOTES-4/MET robotic telescope at Lijiang
Astronomical Observatory (China) gathered images starting at 21:17:34
UT (47 s after trigger). No optical afterglow is found down to 19.3 mag
(in co-added 10x10 s unfiltered images) within the Swift/XRT error box,
consistent with the non-detection by Swift/UVOT (Evans et al. GCNC
27373). Further observations are ongoing. [GCN OPS NOTE(14mar20):
Per author's request, Y.Xin's affiliation was changed from "Yunnan
Nacional Astronomical Observatory" to "Yunnan Observatories of CAS".]
Title: Major Scientific Challenges and Opportunities in Understanding
Magnetic Reconnection and Related Explosive Phenomena throughout
the Universe
Authors: Ji, H.; Alt, A.; Antiochos, S.; Baalrud, S.; Bale, S.;
Bellan, P. M.; Begelman, M.; Beresnyak, A.; Blackman, E. G.; Brennan,
D.; Brown, M.; Buechner, J.; Burch, J.; Cassak, P.; Chen, L. -J.;
Chen, Y.; Chien, A.; Craig, D.; Dahlin, J.; Daughton, W.; DeLuca, E.;
Dong, C. F.; Dorfman, S.; Drake, J.; Ebrahimi, F.; Egedal, J.; Ergun,
R.; Eyink, G.; Fan, Y.; Fiksel, G.; Forest, C.; Fox, W.; Froula, D.;
Fujimoto, K.; Gao, L.; Genestreti, K.; Gibson, S.; Goldstein, M.; Guo,
F.; Hesse, M.; Hoshino, M.; Hu, Q.; Huang, Y. -M.; Jara-Almonte, J.;
Karimabadi, H.; Klimchuk, J.; Kunz, M.; Kusano, K.; Lazarian, A.;
Le, A.; Li, H.; Li, X.; Lin, Y.; Linton, M.; Liu, Y. -H.; Liu, W.;
Longcope, D.; Loureiro, N.; Lu, Q. -M.; Ma, Z-W.; Matthaeus, W. H.;
Meyerhofer, D.; Mozer, F.; Munsat, T.; Murphy, N. A.; Nilson, P.;
Ono, Y.; Opher, M.; Park, H.; Parker, S.; Petropoulou, M.; Phan, T.;
Prager, S.; Rempel, M.; Ren, C.; Ren, Y.; Rosner, R.; Roytershteyn,
V.; Sarff, J.; Savcheva, A.; Schaffner, D.; Schoeffier, K.; Scime, E.;
Shay, M.; Sitnov, M.; Stanier, A.; TenBarge, J.; Tharp, T.; Uzdensky,
D.; Vaivads, A.; Velli, M.; Vishniac, E.; Wang, H.; Werner, G.; Xiao,
C.; Yamada, M.; Yokoyama, T.; Yoo, J.; Zenitani, S.; Zweibel, E.
Bibcode: 2020arXiv200400079J
Altcode:
This white paper summarizes major scientific challenges and
opportunities in understanding magnetic reconnection and related
explosive phenomena as a fundamental plasma process.
Title: Probing the Variation with Depth of the Solar Meridional
Circulation Using Legendre Function Decomposition
Authors: Braun, D. C.; Birch, A.; Fan, Y.
Bibcode: 2020ASSP...57..125B
Altcode:
We apply the helioseismic methodology of Legendre Function Decomposition
to 7.5 years of Dopplergrams obtained by the Helioseismic and
Magnetic Imager (HMI) as the basis of inferring the depth variation
of the meridional flow between 20∘ and 60∘
latitude in both hemispheres. We assess and remove center-to-limb
artifacts using measurements obtained by applying the procedure to
pseudo poles at the east and west limbs. Forward modeling is carried
out to evaluate the consistency of the corrected frequency shifts
with models of the depth variation of the meridional circulation in
the top half of the convection zone. The observations are consistent
with a return flow in the northern hemisphere below about 40 Mm depth,
but no obvious return flow in the south.
Title: Testing Data-driven Simulations of Solar Eruptive Flares
Using Synthetic Magnetograms from Flux Emergence Simulations
Authors: Fan, Y.; Rempel, M.
Bibcode: 2019AGUFMSH33B3393F
Altcode:
To understand the feasibility of data-driven simulations of
solar eruptive events using the electric field inferred from the
observed time sequences of vector magnetograms, we have performed
synthetic data driven simulations using synthetic magnetograms and
electric fields extracted from interior-to-corona flux emergence
simulations. We have carried out coronal simulations of eruptive
flares with the MFE MHD code driven by the boundary data at the
base of the corona extracted from the flux emergence simulations
with the MURaM MHD code. We performed simulations driven with only
the horizontal v×B electric field and the vector B field extracted
from the MURaM simulation at the transition region height, but with
the thermodynamics self-determined from the MFE coronal simulation,
which includes the coronal heating due to numerical dissipation,
radiative cooling, and field aligned thermal conduction. The coronal
heating is due to dissipation of the Poynting flux from the lower
boundary electric field due to magneto-convection. We find that the
driven coronal simulations produce coronal emissions in AIA channels
that are qualitatively similar to those produced by MURaM, and most
importantly re-produce the main eruptive flares with sigmoid brightening
during the evolution. These experiments suggest that with only the VxB
electric field and the B field at the lower boundary (which would be
the situation using the observed vector magnetograms), it is possible
for coronal MHD simulations to reproduce the coronal magnetic field
evolution and onset of eruptions.
Title: Coronal Solar Magnetism Observatory Science Objectives
Authors: Gibson, S. E.; Tomczyk, S.; Burkepile, J.; Casini, R.;
DeLuca, E.; de Toma, G.; de Wijn, A.; Fan, Y.; Golub, L.; Judge,
P. G.; Landi, E.; McIntosh, S. W.; Reeves, K.; Seaton, D. B.; Zhang, J.
Bibcode: 2019AGUFMSH11C3395G
Altcode:
Space-weather forecast capability is held back by our current
lack of basic scientific understanding of CME magnetic evolution,
and the coronal magnetism that structures and drives the solar
wind. Comprehensive observations of the global magnetothermal
environment of the solar atmosphere are needed for progress. When fully
implemented, the COSMO suite of synoptic ground-based telescopes will
provide the community with comprehensive and simultaneous measurements
of magnetism, temperature, density and plasma flows and waves from the
photosphere through the chromosphere and out into the corona. We will
discuss how these observations will uniquely address a set of science
objectives that are central to the field of solar and space physics:
in particular, to understand the storage and release of magnetic energy,
to understand CME dynamics and consequences for shocks, to determine the
role of waves in solar atmospheric heating and solar wind acceleration,
to understand how the coronal magnetic field relates to the solar
dynamo, and to constrain and improve space-weather forecast models.
Title: GRB 191106A: BOOTES-4/MET optical limit
Authors: Hu, Y. -D.; Fernandez-Garcia, E.; Castro-Tirado, A. J.;
Perez del Pulgar, C.; Castellon, A.; Carrasco, I.; Guziy, S.; Xiong,
D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.
Bibcode: 2019GCN.26179....1H
Altcode:
Following the detection of GRB 191106A by Swift (Marshall et
al. GCNC 26177), the 0.6m BOOTES-4/MET robotic telescope at Lijiang
Astronomical Observatory (China) gathered images starting at 14:21 UT
(~5.7 min after trigger). No optical afterglow is found down to 20.7 mag
(unfiltered images) within the Swift/XRT error box, consistent with the
non-detections by Swift/UVOT (Marshall et al. GCNC 26177) and MASTER
(Lipunov et al. GCNC 26178). Observations are ongoing. We thank the
staff at Lijiang Astronomical Observatory for their excellent support.
Title: GRB 191122A: BOOTES-4/MET optical limit
Authors: Hu, Y. -D.; Fernandez-Garcia, E.; Castro-Tirado, A. J.;
Perez del Pulgar, C.; Castellon, A.; Carrasco, I.; Guziy, S.; Xiong,
D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.
Bibcode: 2019GCN.26273....1H
Altcode:
Following the detection of GRB 191122A by Swift (Sbarufatti et al. GCNC
26269), the 0.6m BOOTES-4/MET robotic telescope at Lijiang Astronomical
Observatory (China) started to gather images at 13:34 UT (~94s after
trigger). No optical afterglow is found down to 20.3 mag (unfiltered
images) at the enhaced Swift/XRT position (Evans et al. GCNC 26270),
consistent with the non-detections by Swift/UVOT (Sbarufatti et
al. GCNC 26269) and CHES (Sun et al. GCNC 26271). Observations are
ongoing." We thank the staff at Lijiang Astronomical Observatory for
their excellent support.
Title: GRB 191029A: BOOTES-4/MET optical limit
Authors: Hu, Y. -D.; Fernandez-Garcia, E.; Castro-Tirado, A. J.;
Perez del Pulgar, C.; Castellon, A.; Carrasco, I.; Reina, A.; Guziy,
S.; Xiong, D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.
Bibcode: 2019GCN.26092....1H
Altcode:
No abstract at ADS
Title: A multiwavelength analysis of a collection of short-duration
GRBs observed between 2012 and 2015
Authors: Pandey, S. B.; Hu, Y.; Castro-Tirado, Ao J.; Pozanenko,
A. S.; Sánchez-Ramírez, R.; Gorosabel, J.; Guziy, S.; Jelinek, M.;
Tello, J. C.; Jeong, S.; Oates, S. R.; Zhang, B. -B.; Mazaeva, E. D.;
Volnova, A. A.; Minaev, P. Yu; van Eerten, H. J.; Caballero-García,
M. D.; Pérez-Ramírez, D.; Bremer, M.; Winters, J. -M.; Park, I. H.;
Guelbenzu, A. Nicuesa; Klose, S.; Moskvitin, A.; Sokolov, V. V.;
Sonbas, E.; Ayala, A.; Cepa, J.; Butler, N.; Troja, E.; Chernenko,
A. M.; Molkov, S. V.; Volvach, A. E.; Inasaridze, R. Ya; Egamberdiyev,
Sh A.; Burkhonov, O.; Reva, I. V.; Polyakov, K. A.; Matkin, A. A.;
Ivanov, A. L.; Molotov, I.; Guver, T.; Watson, A. M.; Kutyrev, A.; Lee,
W. H.; Fox, O.; Littlejohns, O.; Cucchiara, A.; Gonzalez, J.; Richer,
M. G.; Román-Zúñiga, C. G.; Tanvir, N. R.; Bloom, J. S.; Prochaska,
J. X.; Gehrels, N.; Moseley, H.; de Diego, J. A.; Ramírez-Ruiz, E.;
Klunko, E. V.; Fan, Y.; Zhao, X.; Bai, J.; Wang, Ch; Xin, Y.; Cui,
Ch; Tungalag, N.; Peng, Z. -K.; Kumar, Amit; Gupta, Rahul; Aryan,
Amar; Kumar, Brajesh; Volvach, L. N.; Lamb, G. P.; Valeev, A. F.
Bibcode: 2019MNRAS.485.5294P
Altcode: 2019MNRAS.tmp..525P; 2019arXiv190207900P
We investigate the prompt emission and the afterglow properties of
short-duration gamma-ray burst (sGRB) 130603B and another eight sGRB
events during 2012-2015, observed by several multiwavelength facilities
including the Gran Canarias Telescope 10.4 m telescope. Prompt emission
high energy data of the events were obtained by INTEGRAL-SPI-ACS,
Swift-BAT, and Fermi-GBM satellites. The prompt emission data by
INTEGRAL in the energy range of 0.1-10 MeV for sGRB 130603B, sGRB
140606A, sGRB 140930B, sGRB 141212A, and sGRB 151228A do not show
any signature of the extended emission or precursor activity and
their spectral and temporal properties are similar to those seen
in case of other short bursts. For sGRB 130603B, our new afterglow
photometric data constrain the pre-jet-break temporal decay due to
denser temporal coverage. For sGRB 130603B, the afterglow light curve,
containing both our new and previously published photometric data is
broadly consistent with the ISM afterglow model. Modeling of the host
galaxies of sGRB 130603B and sGRB 141212A using the LePHARE software
supports a scenario in which the environment of the burst is undergoing
moderate star formation activity. From the inclusion of our late-time
data for eight other sGRBs we are able to: place tight constraints
on the non-detection of the afterglow, host galaxy, or any underlying
`kilonova' emission. Our late-time afterglow observations of the sGRB
170817A/GW170817 are also discussed and compared with the sub-set
of sGRBs.
Title: Data-optimized Coronal Field Model. I. Proof of Concept
Authors: Dalmasse, K.; Savcheva, A.; Gibson, S. E.; Fan, Y.; Nychka,
D. W.; Flyer, N.; Mathews, N.; DeLuca, E. E.
Bibcode: 2019ApJ...877..111D
Altcode: 2019arXiv190406308D
Deriving the strength and direction of the three-dimensional
(3D) magnetic field in the solar atmosphere is fundamental for
understanding its dynamics. Volume information on the magnetic field
mostly relies on coupling 3D reconstruction methods with photospheric
and/or chromospheric surface vector magnetic fields. Infrared
coronal polarimetry could provide additional information to better
constrain magnetic field reconstructions. However, combining such
data with reconstruction methods is challenging, e.g., because of the
optical thinness of the solar corona and the lack and limitations of
stereoscopic polarimetry. To address these issues, we introduce the
data-optimized coronal field model (DOCFM) framework, a model-data
fitting approach that combines a parameterized 3D generative model,
e.g., a magnetic field extrapolation or a magnetohydrodynamic model,
with forward modeling of coronal data. We test it with a parameterized
flux-rope insertion method and infrared coronal polarimetry where
synthetic observations are created from a known “ground-truth”
physical state. We show that this framework allows us to accurately
retrieve the ground-truth 3D magnetic field of a set of force-free
field solutions from the flux-rope insertion method. In observational
studies, the DOCFM will provide a means to force the solutions
derived with different reconstruction methods to satisfy additional
common coronal constraints. The DOCFM framework therefore opens new
perspectives for the exploitation of coronal polarimetry in magnetic
field reconstructions and for developing new techniques to more
reliably infer the 3D magnetic fields that trigger solar flares and
coronal mass ejections.
Title: Major Scientific Challenges and Opportunities in Understanding
Magnetic Reconnection and Related Explosive Phenomena throughout
the Universe
Authors: Ji, Hantao; Alt, A.; Antiochos, S.; Baalrud, S.; Bale, S.;
Bellan, P. M.; Begelman, M.; Beresnyak, A.; Blackman, E. G.; Brennan,
D.; Brown, M.; Buechner, J.; Burch, J.; Cassak, P.; Chen, L. -J.;
Chen, Y.; Chien, A.; Craig, D.; Dahlin, J.; Daughton, W.; DeLuca, E.;
Dong, C. F.; Dorfman, S.; Drake, J.; Ebrahimi, F.; Egedal, J.; Ergun,
R.; Eyink, G.; Fan, Y.; Fiksel, G.; Forest, C.; Fox, W.; Froula, D.;
Fujimoto, K.; Gao, L.; Genestreti, K.; Gibson, S.; Goldstein, M.;
Guo, F.; Hesse, M.; Hoshino, M.; Hu, Q.; Huang, Y. -M.; Jara-Almonte,
J.; Karimabadi, H.; Klimchuk, J.; Kunz, M.; Kusano, K.; Lazarian,
A.; Le, A.; Li, H.; Li, X.; Lin, Y.; Linton, M.; Liu, Y. -H.; Liu,
W.; Longcope, D.; Louriero, N.; Lu, Q. -M.; Ma, Z. -W.; Matthaeus,
W. H.; Meyerhofer, D.; Mozer, F.; Munsat, T.; Murphy, N. A.; Nilson,
P.; Ono, Y.; Opher, M.; Park, H.; Parker, S.; Petropoulou, M.; Phan,
T.; Prager, S.; Rempel, M.; Ren, C.; Ren, Y.; Rosner, R.; Roytershteyn,
V.; Sarff, J.; Savcheva, A.; Schaffner, D.; Schoeffier, K.; Scime, E.;
Shay, M.; Sitnov, M.; Stanier, A.; TenBarge, J.; Tharp, T.; Uzdensky,
D.; Vaivads, A.; Velli, M.; Vishniac, E.; Wang, H.; Werner, G.; Xiao,
C.; Yamada, M.; Yokoyama, T.; Yoo, J.; Zenitani, S.; Zweibel, E.
Bibcode: 2019BAAS...51c...5J
Altcode: 2019astro2020T...5J
This is a group white paper of 100 authors (each with explicit
permission via email) from 51 institutions on the topic of magnetic
reconnection which is relevant to 6 thematic areas. Grand challenges
and research opportunities are described in observations, numerical
modeling and laboratory experiments in the upcoming decade.
Title: GRB 190515B: BOOTES-4/MET and 2.2m CAHA optical limits.
Authors: Hu, Y. -D.; Li, X. -Y.; Fernandez-Garcia, E.; Ayala, A.;
Castro-Tirado, A. J.; Perez, C.; Castellon, A.; Carrasco, I.; Guziy,
S.; Xiong, D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.; Mao,
J.; Fernandez, A.; Hermelo, I.
Bibcode: 2019GCN.24567....1H
Altcode:
No abstract at ADS
Title: GRB 190211A: BOOTES-4/MET optical afterglow confirmation.
Authors: Hu, Y. -D.; Li, X. -Y.; Fernandez-Garcia, E.; Ayala, A.;
Castro-Tirado, A. J.; Perez, C.; Castellon, A.; Carrasco, I.; Guziy,
S.; Xiong, D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.
Bibcode: 2019GCN.23886....1H
Altcode:
No abstract at ADS
Title: GRB 190106A: BOOTES-4/MET optical observations.
Authors: Hu, Y. -D.; Li, X. -Y.; Fernandez-Garcia, E.; Ayala, A.;
Castro-Tirado, A. J.; Perez, C.; Castellon, A.; Carrasco, I.; Guziy,
S.; Xiong, D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.
Bibcode: 2019GCN.23627....1H
Altcode:
No abstract at ADS
Title: GRB 190114B: BOOTES-4/MET optical afterglow detection.
Authors: Fernandez-Garcia, E.; Hu, Y. -D.; Li, X. -Y.; Ayala, A.;
Castro-Tirado, A. J.; Perez, C.; Castellon, A.; Carrasco, I.; Xiong,
D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.
Bibcode: 2019GCN.23694....1F
Altcode:
No abstract at ADS
Title: GRB 190220B: BOOTES-4 optical observation.
Authors: Hu, Y. -D.; Li, X. -Y.; Fernandez-Garcia, E.; Ayala, A.;
Castro-Tirado, A. J.; Perez, C.; Castellon, A.; Carrasco, I.; Guziy,
S.; Xiong, D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.
Bibcode: 2019GCN.23916....1H
Altcode:
No abstract at ADS
Title: GRB 190123A: BOOTES-4/MET optical limit.
Authors: Hu, Y. -D.; Li, X. -Y.; Fernandez-Garcia, E.; Ayala, A.;
Castro-Tirado, A. J.; Perez, C.; Castellon, A.; Carrasco, I.; Guziy,
S.; Xiong, D.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.
Bibcode: 2019GCN.23772....1H
Altcode:
No abstract at ADS
Title: Modeling the Solar Convective Dynamo and Emerging Flux
Authors: Fan, Y.
Bibcode: 2017AGUFMSH12A..02F
Altcode:
Significant advances have been made in recent years in global-scale
fully dynamic three-dimensional convective dynamo simulations of the
solar/stellar convective envelopes to reproduce some of the basic
features of the Sun's large-scale cyclic magnetic field. It is found
that the presence of the dynamo-generated magnetic fields plays an
important role for the maintenance of the solar differential rotation,
without which the differential rotation tends to become anti-solar
(with a faster rotating pole instead of the observed faster rotation at
the equator). Convective dynamo simulations are also found to produce
emergence of coherent super-equipartition toroidal flux bundles with
a statistically significant mean tilt angle that is consistent with
the mean tilt of solar active regions. The emerging flux bundles are
sheared by the giant cell convection into a forward leaning loop shape
with its leading side (in the direction of rotation) pushed closer to
the strong downflow lanes. Such asymmetric emerging flux pattern may
lead to the observed asymmetric properties of solar active regions.
Title: Terminator 2020: Get Ready for the "Event" of The Next Decade
Authors: McIntosh, S. W.; Leamon, R. J.; Fan, Y.; Rempel, M.;
Dikpati, M.
Bibcode: 2017AGUFMSH22B..06M
Altcode:
The abrupt end of solar activity cycles 22 and 23 at the Sun's
equator are observed with instruments from the Solar and Heliospheric
Observatory (SOHO), Solar Terrestrial Relations Observatory (STEREO),
and Solar Dynamics Observatory (SDO). These events are remarkable in
that they rapidly trigger the onset of magnetic activity belonging
to the next solar cycle at mid-latitudes. The triggered onset of new
cycle flux emergence leads to blossoming of the new cycle shortly
thereafter. Using small-scale tracers of magnetic solar activity we
examine the timing of the cycle ``termination points'' in relation
to the excitation of new activity and find that the time taken
for the solar plasma to communicate this transition is less than
one solar rotation, and possibly as little as a eight days. This
very short transition time implies that the mean magnetic field
present in the Sun's convection zone is approximately 80 kG. This
value may be considerably larger than conventional explorations
estimate and therefore, have a significant dynamical impact on the
physical appearance of solar activity, and considerably impacting
our ability to perform first-principles numerical simulations of the
same. Should solar cycle 24 [and 25] continue in their progression
we anticipate that a termination event of this type should occur in
the 2020 timeframe. PSP will have a front row seat to observe this
systemic flip in solar magnetism and the induced changes in our star's
radiative and partiuculate output. Such observations may prove to be
critical in assessing the Sun's ability to force short term evolution
in the Earth's atmosphere.
Title: Update of the China-VO AstroCloud
Authors: Cui, C.; Yu, C.; Xiao, J.; He, B.; Li, C.; Fan, D.; Wang, C.;
Hong, Z.; Li, S.; Mi, L.; Wan, W.; Cao, Z.; Wang, J.; Yin, S.; Fan, Y.;
Wang, J.; Yang, S.; Ling, Y.; Zhang, H.; Chen, J.; Liu, L.; Chen, X.
Bibcode: 2017ASPC..512..553C
Altcode: 2018ASPC..512..553C; 2017adass..25..553C; 2016arXiv160103155C
As the cyber-infrastructure for Astronomical research from Chinese
Virtual Observatory (China-VO) project, AstroCloud has achieved
solid progress during the last year. The proposal management system
and data access system were redesigned. Several new sub-systems were
developed, including China-VO PaperData, AstroCloud Statics and Public
channel. More data sets and application environments are integrated into
the platform. LAMOST DR1, the largest astronomical spectrum archive,
was released to the public using the platform. The latest progress
will be introduced.
Title: Numerical MHD Coronal Simulations: Energy Statistics and
FORWARD Analysis.
Authors: Nimmo, K.; Rempel, M.; Chen, F.; Gibson, S. E.; Fan, Y.
Bibcode: 2017AGUFMSH43A2800N
Altcode:
We analyse a recent realistic radiative MHD simulation of the solar
corona that was computed with the extended version of the MURaM
code. The simulation covers the uppermost 8Mm of the solar convection
zone and reaches 115Mm into the solar corona. The simulation covers 48
hours of solar time and simulates the evolution of a complex active
region. The energy release in the corona is highly intermittent and
we identify a total of 118 individual events including flares and a
coronal mass ejection, which we analyse in further detail. From the
simulation we compute an X-ray flux mimicking observations by the GOES
(Geostationary Operational Environmental Satellite) satellite in the
wavelength range 1-8 Å. The power law index for the GOES X-ray flux
for flares of class C and above in this simulation is found to be
1.33452. We analyze the correlation between synthetic coronal emission
during flares and the magnetic energy release in the corona. The latter
is a quantity that cannot be directly determined in observations.The
FORWARD code is a tool used for the purpose of coronal magnetometry. It
can be used to compute synthetic observables from coronal models. We
focus on the interpretation of the High Altitude Observatory's CoMP
observations. The CoMP (COronal Multi-channel Polarimeter) instrument
measures the intensity and the linear and circular polarisation of
FeXIII at 1074.7nm.We discuss some important limitations of coronal
emission line polarimetry when simulating an extremely active solar
region, with emphasis on the influence of high velocities, temperatures
and densities on the FORWARD output.
Title: The Design and Application of Astronomy Data Lake in China-VO
Authors: Li, C.; Cui, C.; He, B.; Fan, D.; Wang, J.; Li, S.; Mi, L.;
Wan, W.; Chen, J.; Zhang, H.; Yu, C.; Xiao, J.; Wang, C.; Cao, Z.;
Fan, Y.; Hong, Z.; Wang, J.; Yin, S.; Liu, L.; Chen, X.
Bibcode: 2017ASPC..512..157L
Altcode: 2017adass..25..157L; 2018ASPC..512..157L
With the coming of many large astronomy observation facilities, such
as LAMOST, TMT, FAST, LSST, SKA, data storage for these facilities is
facing big challenges. Astronomy Data Lake, a distributed storage system
is designed to meet these requirements in the big data era. Astronomy
Data Lake, basing on a master-slave framework, integrates many
geographic distributed data storage resources into a single mount
point. It implements automatic data backup and disaster recovery,
with easy expansion capability. Based on this system, we developed
many data storage services, including database storage, private file
storage, computing data and paper data services for astronomers.
Title: Multi-messenger Observations of a Binary Neutron Star Merger
Authors: Abbott, B. P.; Abbott, R.; Abbott, T. D.; Acernese, F.;
Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari, R. X.; Adya,
V. B.; Affeldt, C.; Afrough, M.; Agarwal, B.; Agathos, M.; Agatsuma,
K.; Aggarwal, N.; Aguiar, O. D.; Aiello, L.; Ain, A.; Ajith, P.;
Allen, B.; Allen, G.; Allocca, A.; Altin, P. A.; Amato, A.; Ananyeva,
A.; Anderson, S. B.; Anderson, W. G.; Angelova, S. V.; Antier, S.;
Appert, S.; Arai, K.; Araya, M. C.; Areeda, J. S.; Arnaud, N.; Arun,
K. G.; Ascenzi, S.; Ashton, G.; Ast, M.; Aston, S. M.; Astone, P.;
Atallah, D. V.; Aufmuth, P.; Aulbert, C.; AultONeal, K.; Austin,
C.; Avila-Alvarez, A.; Babak, S.; Bacon, P.; Bader, M. K. M.; Bae,
S.; Baker, P. T.; Baldaccini, F.; Ballardin, G.; Ballmer, S. W.;
Banagiri, S.; Barayoga, J. C.; Barclay, S. E.; Barish, B. C.; Barker,
D.; Barkett, K.; Barone, F.; Barr, B.; Barsotti, L.; Barsuglia,
M.; Barta, D.; Barthelmy, S. D.; Bartlett, J.; Bartos, I.; Bassiri,
R.; Basti, A.; Batch, J. C.; Bawaj, M.; Bayley, J. C.; Bazzan, M.;
Bécsy, B.; Beer, C.; Bejger, M.; Belahcene, I.; Bell, A. S.; Berger,
B. K.; Bergmann, G.; Bero, J. J.; Berry, C. P. L.; Bersanetti, D.;
Bertolini, A.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko,
I. A.; Billingsley, G.; Billman, C. R.; Birch, J.; Birney, R.;
Birnholtz, O.; Biscans, S.; Biscoveanu, S.; Bisht, A.; Bitossi, M.;
Biwer, C.; Bizouard, M. A.; Blackburn, J. K.; Blackman, J.; Blair,
C. D.; Blair, D. G.; Blair, R. M.; Bloemen, S.; Bock, O.; Bode, N.;
Boer, M.; Bogaert, G.; Bohe, A.; Bondu, F.; Bonilla, E.; Bonnand, R.;
Boom, B. A.; Bork, R.; Boschi, V.; Bose, S.; Bossie, K.; Bouffanais,
Y.; Bozzi, A.; Bradaschia, C.; Brady, P. R.; Branchesi, M.; Brau,
J. E.; Briant, T.; Brillet, A.; Brinkmann, M.; Brisson, V.; Brockill,
P.; Broida, J. E.; Brooks, A. F.; Brown, D. A.; Brown, D. D.; Brunett,
S.; Buchanan, C. C.; Buikema, A.; Bulik, T.; Bulten, H. J.; Buonanno,
A.; Buskulic, D.; Buy, C.; Byer, R. L.; Cabero, M.; Cadonati, L.;
Cagnoli, G.; Cahillane, C.; Calderón Bustillo, J.; Callister, T. A.;
Calloni, E.; Camp, J. B.; Canepa, M.; Canizares, P.; Cannon, K. C.;
Cao, H.; Cao, J.; Capano, C. D.; Capocasa, E.; Carbognani, F.; Caride,
S.; Carney, M. F.; Casanueva Diaz, J.; Casentini, C.; Caudill, S.;
Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C. B.;
Cerdá-Durán, P.; Cerretani, G.; Cesarini, E.; Chamberlin, S. J.;
Chan, M.; Chao, S.; Charlton, P.; Chase, E.; Chassande-Mottin, E.;
Chatterjee, D.; Chatziioannou, K.; Cheeseboro, B. D.; Chen, H. Y.;
Chen, X.; Chen, Y.; Cheng, H. -P.; Chia, H.; Chincarini, A.; Chiummo,
A.; Chmiel, T.; Cho, H. S.; Cho, M.; Chow, J. H.; Christensen, N.;
Chu, Q.; Chua, A. J. K.; Chua, S.; Chung, A. K. W.; Chung, S.; Ciani,
G.; Ciolfi, R.; Cirelli, C. E.; Cirone, A.; Clara, F.; Clark, J. A.;
Clearwater, P.; Cleva, F.; Cocchieri, C.; Coccia, E.; Cohadon,
P. -F.; Cohen, D.; Colla, A.; Collette, C. G.; Cominsky, L. R.;
Constancio, M., Jr.; Conti, L.; Cooper, S. J.; Corban, P.; Corbitt,
T. R.; Cordero-Carrión, I.; Corley, K. R.; Cornish, N.; Corsi, A.;
Cortese, S.; Costa, C. A.; Coughlin, M. W.; Coughlin, S. B.; Coulon,
J. -P.; Countryman, S. T.; Couvares, P.; Covas, P. B.; Cowan, E. E.;
Coward, D. M.; Cowart, M. J.; Coyne, D. C.; Coyne, R.; Creighton,
J. D. E.; Creighton, T. D.; Cripe, J.; Crowder, S. G.; Cullen, T. J.;
Cumming, A.; Cunningham, L.; Cuoco, E.; Dal Canton, T.; Dálya,
G.; Danilishin, S. L.; D'Antonio, S.; Danzmann, K.; Dasgupta, A.;
Da Silva Costa, C. F.; Dattilo, V.; Dave, I.; Davier, M.; Davis, D.;
Daw, E. J.; Day, B.; De, S.; DeBra, D.; Degallaix, J.; De Laurentis,
M.; Deléglise, S.; Del Pozzo, W.; Demos, N.; Denker, T.; Dent, T.;
De Pietri, R.; Dergachev, V.; De Rosa, R.; DeRosa, R. T.; De Rossi,
C.; DeSalvo, R.; de Varona, O.; Devenson, J.; Dhurandhar, S.; Díaz,
M. C.; Di Fiore, L.; Di Giovanni, M.; Di Girolamo, T.; Di Lieto, A.;
Di Pace, S.; Di Palma, I.; Di Renzo, F.; Doctor, Z.; Dolique, V.;
Donovan, F.; Dooley, K. L.; Doravari, S.; Dorrington, I.; Douglas,
R.; Dovale Álvarez, M.; Downes, T. P.; Drago, M.; Dreissigacker,
C.; Driggers, J. C.; Du, Z.; Ducrot, M.; Dupej, P.; Dwyer, S. E.;
Edo, T. B.; Edwards, M. C.; Effler, A.; Ehrens, P.; Eichholz, J.;
Eikenberry, S. S.; Eisenstein, R. A.; Essick, R. C.; Estevez, D.;
Etienne, Z. B.; Etzel, T.; Evans, M.; Evans, T. M.; Factourovich,
M.; Fafone, V.; Fair, H.; Fairhurst, S.; Fan, X.; Farinon, S.; Farr,
B.; Farr, W. M.; Fauchon-Jones, E. J.; Favata, M.; Fays, M.; Fee,
C.; Fehrmann, H.; Feicht, J.; Fejer, M. M.; Fernandez-Galiana, A.;
Ferrante, I.; Ferreira, E. C.; Ferrini, F.; Fidecaro, F.; Finstad, D.;
Fiori, I.; Fiorucci, D.; Fishbach, M.; Fisher, R. P.; Fitz-Axen, M.;
Flaminio, R.; Fletcher, M.; Fong, H.; Font, J. A.; Forsyth, P. W. F.;
Forsyth, S. S.; Fournier, J. -D.; Frasca, S.; Frasconi, F.; Frei, Z.;
Freise, A.; Frey, R.; Frey, V.; Fries, E. M.; Fritschel, P.; Frolov,
V. V.; Fulda, P.; Fyffe, M.; Gabbard, H.; Gadre, B. U.; Gaebel,
S. M.; Gair, J. R.; Gammaitoni, L.; Ganija, M. R.; Gaonkar, S. G.;
Garcia-Quiros, C.; Garufi, F.; Gateley, B.; Gaudio, S.; Gaur, G.;
Gayathri, V.; Gehrels, N.; Gemme, G.; Genin, E.; Gennai, A.; George,
D.; George, J.; Gergely, L.; Germain, V.; Ghonge, S.; Ghosh, Abhirup;
Ghosh, Archisman; Ghosh, S.; Giaime, J. A.; Giardina, K. D.; Giazotto,
A.; Gill, K.; Glover, L.; Goetz, E.; Goetz, R.; Gomes, S.; Goncharov,
B.; González, G.; Gonzalez Castro, J. M.; Gopakumar, A.; Gorodetsky,
M. L.; Gossan, S. E.; Gosselin, M.; Gouaty, R.; Grado, A.; Graef, C.;
Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greco, G.; Green, A. C.;
Gretarsson, E. M.; Griswold, B.; Groot, P.; Grote, H.; Grunewald, S.;
Gruning, P.; Guidi, G. M.; Guo, X.; Gupta, A.; Gupta, M. K.; Gushwa,
K. E.; Gustafson, E. K.; Gustafson, R.; Halim, O.; Hall, B. R.; Hall,
E. D.; Hamilton, E. Z.; Hammond, G.; Haney, M.; Hanke, M. M.; Hanks,
J.; Hanna, C.; Hannam, M. D.; Hannuksela, O. A.; Hanson, J.; Hardwick,
T.; Harms, J.; Harry, G. M.; Harry, I. W.; Hart, M. J.; Haster, C. -J.;
Haughian, K.; Healy, J.; Heidmann, A.; Heintze, M. C.; Heitmann,
H.; Hello, P.; Hemming, G.; Hendry, M.; Heng, I. S.; Hennig, J.;
Heptonstall, A. W.; Heurs, M.; Hild, S.; Hinderer, T.; Hoak, D.;
Hofman, D.; Holt, K.; Holz, D. E.; Hopkins, P.; Horst, C.; Hough,
J.; Houston, E. A.; Howell, E. J.; Hreibi, A.; Hu, Y. M.; Huerta,
E. A.; Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh,
T.; Indik, N.; Inta, R.; Intini, G.; Isa, H. N.; Isac, J. -M.; Isi,
M.; Iyer, B. R.; Izumi, K.; Jacqmin, T.; Jani, K.; Jaranowski,
P.; Jawahar, S.; Jiménez-Forteza, F.; Johnson, W. W.; Jones,
D. I.; Jones, R.; Jonker, R. J. G.; Ju, L.; Junker, J.; Kalaghatgi,
C. V.; Kalogera, V.; Kamai, B.; Kandhasamy, S.; Kang, G.; Kanner,
J. B.; Kapadia, S. J.; Karki, S.; Karvinen, K. S.; Kasprzack, M.;
Katolik, M.; Katsavounidis, E.; Katzman, W.; Kaufer, S.; Kawabe, K.;
Kéfélian, F.; Keitel, D.; Kemball, A. J.; Kennedy, R.; Kent, C.;
Key, J. S.; Khalili, F. Y.; Khan, I.; Khan, S.; Khan, Z.; Khazanov,
E. A.; Kijbunchoo, N.; Kim, Chunglee; Kim, J. C.; Kim, K.; Kim, W.;
Kim, W. S.; Kim, Y. -M.; Kimbrell, S. J.; King, E. J.; King, P. J.;
Kinley-Hanlon, M.; Kirchhoff, R.; Kissel, J. S.; Kleybolte, L.;
Klimenko, S.; Knowles, T. D.; Koch, P.; Koehlenbeck, S. M.; Koley,
S.; Kondrashov, V.; Kontos, A.; Korobko, M.; Korth, W. Z.; Kowalska,
I.; Kozak, D. B.; Krämer, C.; Kringel, V.; Krishnan, B.; Królak,
A.; Kuehn, G.; Kumar, P.; Kumar, R.; Kumar, S.; Kuo, L.; Kutynia,
A.; Kwang, S.; Lackey, B. D.; Lai, K. H.; Landry, M.; Lang, R. N.;
Lange, J.; Lantz, B.; Lanza, R. K.; Larson, S. L.; Lartaux-Vollard,
A.; Lasky, P. D.; Laxen, M.; Lazzarini, A.; Lazzaro, C.; Leaci, P.;
Leavey, S.; Lee, C. H.; Lee, H. K.; Lee, H. M.; Lee, H. W.; Lee, K.;
Lehmann, J.; Lenon, A.; Leonardi, M.; Leroy, N.; Letendre, N.; Levin,
Y.; Li, T. G. F.; Linker, S. D.; Littenberg, T. B.; Liu, J.; Lo,
R. K. L.; Lockerbie, N. A.; London, L. T.; Lord, J. E.; Lorenzini,
M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lough, J. D.; Lousto,
C. O.; Lovelace, G.; Lück, H.; Lumaca, D.; Lundgren, A. P.; Lynch,
R.; Ma, Y.; Macas, R.; Macfoy, S.; Machenschalk, B.; MacInnis, M.;
Macleod, D. M.; Magaña Hernandez, I.; Magaña-Sandoval, F.; Magaña
Zertuche, L.; Magee, R. M.; Majorana, E.; Maksimovic, I.; Man, N.;
Mandic, V.; Mangano, V.; Mansell, G. L.; Manske, M.; Mantovani, M.;
Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markakis, C.;
Markosyan, A. S.; Markowitz, A.; Maros, E.; Marquina, A.; Marsh,
P.; Martelli, F.; Martellini, L.; Martin, I. W.; Martin, R. M.;
Martynov, D. V.; Mason, K.; Massera, E.; Masserot, A.; Massinger,
T. J.; Masso-Reid, M.; Mastrogiovanni, S.; Matas, A.; Matichard, F.;
Matone, L.; Mavalvala, N.; Mazumder, N.; McCarthy, R.; McClelland,
D. E.; McCormick, S.; McCuller, L.; McGuire, S. C.; McIntyre, G.;
McIver, J.; McManus, D. J.; McNeill, L.; McRae, T.; McWilliams, S. T.;
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Melatos, A.; Mendell, G.; Mercer, R. A.; Merilh, E. L.; Merzougui, M.;
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M.; Neunzert, A.; Nevin, L.; Newport, J. M.; Newton, G.; Ng, K. K. Y.;
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G. C.; Rao, A. R.; Vadawale, S. V.; AstroSat Cadmium Zinc Telluride
Imager Team; Svinkin, D. S.; Hurley, K.; Aptekar, R. L.; Frederiks,
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Y. B.; Chen, Y. P.; Cui, W.; Cui, W. W.; Deng, J. K.; Dong, Y. W.; Du,
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Guan, J.; Guo, C. C.; Han, D. W.; Hu, W.; Huang, Y.; Huo, J.; Jia,
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C. K.; Li, G.; Li, M. S.; Li, W.; Li, X.; Li, X. B.; Li, X. F.; Li,
Y. G.; Li, Z. J.; Li, Z. W.; Liang, X. H.; Liao, J. Y.; Liu, C. Z.;
Liu, G. Q.; Liu, H. W.; Liu, S. Z.; Liu, X. J.; Liu, Y.; Liu, Y. N.;
Lu, B.; Lu, X. F.; Luo, T.; Ma, X.; Meng, B.; Nang, Y.; Nie, J. Y.;
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Zhang, S.; Zhang, T.; Zhang, W.; Zhang, W. C.; Zhang, W. Z.; Zhang,
Y.; Zhang, Y.; Zhang, Y. F.; Zhang, Y. J.; Zhang, Z.; Zhang, Z. L.;
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C.; Illuminati, G.; James, C. W.; de Jong, M.; Jongen, M.; Kadler,
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Marinelli, A.; Martínez-Mora, J. A.; Mele, R.; Melis, K.; Michael,
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Van Elewyck, V.; Versari, F.; Vivolo, D.; Vizzoca, A.; Wilms, J.;
Zornoza, J. D.; Zúñiga, J.; ANTARES Collaboration; Beardmore, A. P.;
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de Pasquale, M.; Emery, S. W. K.; Evans, P. A.; Giommi, P.; Gronwall,
C.; Kennea, J. A.; Krimm, H. A.; Kuin, N. P. M.; Lien, A.; Marshall,
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M.; Rappoldi, A.; Soffitta, P.; Vercellone, S.; AGILE Team; Foley,
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Soares-Santos, M.; Annis, J.; Alexander, K. D.; Allam, S.; Balbinot,
E.; Blanchard, P.; Brout, D.; Butler, R. E.; Chornock, R.; Cook,
E. R.; Cowperthwaite, P.; Diehl, H. T.; Drlica-Wagner, A.; Drout,
M. R.; Durret, F.; Eftekhari, T.; Finley, D. A.; Fong, W.; Frieman,
J. A.; Fryer, C. L.; García-Bellido, J.; Gruendl, R. A.; Hartley,
W.; Herner, K.; Kessler, R.; Lin, H.; Lopes, P. A. A.; Lourenço,
A. C. C.; Margutti, R.; Marshall, J. L.; Matheson, T.; Medina, G. E.;
Metzger, B. D.; Muñoz, R. R.; Muir, J.; Nicholl, M.; Nugent, P.;
Palmese, A.; Paz-Chinchón, F.; Quataert, E.; Sako, M.; Sauseda, M.;
Schlegel, D. J.; Scolnic, D.; Secco, L. F.; Smith, N.; Sobreira, F.;
Villar, V. A.; Vivas, A. K.; Wester, W.; Williams, P. K. G.; Yanny,
B.; Zenteno, A.; Zhang, Y.; Abbott, T. M. C.; Banerji, M.; Bechtol,
K.; Benoit-Lévy, A.; Bertin, E.; Brooks, D.; Buckley-Geer, E.; Burke,
D. L.; Capozzi, D.; Carnero Rosell, A.; Carrasco Kind, M.; Castander,
F. J.; Crocce, M.; Cunha, C. E.; D'Andrea, C. B.; da Costa, L. N.;
Davis, C.; DePoy, D. L.; Desai, S.; Dietrich, J. P.; Eifler, T. F.;
Fernandez, E.; Flaugher, B.; Fosalba, P.; Gaztanaga, E.; Gerdes,
D. W.; Giannantonio, T.; Goldstein, D. A.; Gruen, D.; Gschwend, J.;
Gutierrez, G.; Honscheid, K.; James, D. J.; Jeltema, T.; Johnson,
M. W. G.; Johnson, M. D.; Kent, S.; Krause, E.; Kron, R.; Kuehn, K.;
Lahav, O.; Lima, M.; Maia, M. A. G.; March, M.; Martini, P.; McMahon,
R. G.; Menanteau, F.; Miller, C. J.; Miquel, R.; Mohr, J. J.; Nichol,
R. C.; Ogando, R. L. C.; Plazas, A. A.; Romer, A. K.; Roodman, A.;
Rykoff, E. S.; Sanchez, E.; Scarpine, V.; Schindler, R.; Schubnell,
M.; Sevilla-Noarbe, I.; Sheldon, E.; Smith, M.; Smith, R. C.; Stebbins,
A.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thomas, R. C.; Troxel,
M. A.; Tucker, D. L.; Vikram, V.; Walker, A. R.; Wechsler, R. H.;
Weller, J.; Carlin, J. L.; Gill, M. S. S.; Li, T. S.; Marriner, J.;
Neilsen, E.; Dark Energy Camera GW-EM Collaboration; DES Collaboration;
Haislip, J. B.; Kouprianov, V. V.; Reichart, D. E.; Sand, D. J.;
Tartaglia, L.; Valenti, S.; Yang, S.; DLT40 Collaboration; Benetti,
S.; Brocato, E.; Campana, S.; Cappellaro, E.; Covino, S.; D'Avanzo,
P.; D'Elia, V.; Getman, F.; Ghirlanda, G.; Ghisellini, G.; Limatola,
L.; Nicastro, L.; Palazzi, E.; Pian, E.; Piranomonte, S.; Possenti,
A.; Rossi, A.; Salafia, O. S.; Tomasella, L.; Amati, L.; Antonelli,
L. A.; Bernardini, M. G.; Bufano, F.; Capaccioli, M.; Casella, P.;
Dadina, M.; De Cesare, G.; Di Paola, A.; Giuffrida, G.; Giunta,
A.; Israel, G. L.; Lisi, M.; Maiorano, E.; Mapelli, M.; Masetti,
N.; Pescalli, A.; Pulone, L.; Salvaterra, R.; Schipani, P.; Spera,
M.; Stamerra, A.; Stella, L.; Testa, V.; Turatto, M.; Vergani, D.;
Aresu, G.; Bachetti, M.; Buffa, F.; Burgay, M.; Buttu, M.; Caria,
T.; Carretti, E.; Casasola, V.; Castangia, P.; Carboni, G.; Casu,
S.; Concu, R.; Corongiu, A.; Deiana, G. L.; Egron, E.; Fara, A.;
Gaudiomonte, F.; Gusai, V.; Ladu, A.; Loru, S.; Leurini, S.; Marongiu,
L.; Melis, A.; Melis, G.; Migoni, Carlo; Milia, Sabrina; Navarrini,
Alessandro; Orlati, A.; Ortu, P.; Palmas, S.; Pellizzoni, A.; Perrodin,
D.; Pisanu, T.; Poppi, S.; Righini, S.; Saba, A.; Serra, G.; Serrau,
M.; Stagni, M.; Surcis, G.; Vacca, V.; Vargiu, G. P.; Hunt, L. K.;
Jin, Z. P.; Klose, S.; Kouveliotou, C.; Mazzali, P. A.; Møller, P.;
Nava, L.; Piran, T.; Selsing, J.; Vergani, S. D.; Wiersema, K.; Toma,
K.; Higgins, A. B.; Mundell, C. G.; di Serego Alighieri, S.; Gótz,
D.; Gao, W.; Gomboc, A.; Kaper, L.; Kobayashi, S.; Kopac, D.; Mao,
J.; Starling, R. L. C.; Steele, I.; van der Horst, A. J.; GRAWITA:
GRAvitational Wave Inaf TeAm; Acero, F.; Atwood, W. B.; Baldini,
L.; Barbiellini, G.; Bastieri, D.; Berenji, B.; Bellazzini, R.;
Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonino, R.; Bottacini,
E.; Bregeon, J.; Buehler, R.; Buson, S.; Cameron, R. A.; Caputo, R.;
Caraveo, P. A.; Cavazzuti, E.; Chekhtman, A.; Cheung, C. C.; Chiang,
J.; Ciprini, S.; Cohen-Tanugi, J.; Cominsky, L. R.; Costantin, D.;
Cuoco, A.; D'Ammando, F.; de Palma, F.; Digel, S. W.; Di Lalla,
N.; Di Mauro, M.; Di Venere, L.; Dubois, R.; Fegan, S. J.; Focke,
W. B.; Franckowiak, A.; Fukazawa, Y.; Funk, S.; Fusco, P.; Gargano,
F.; Gasparrini, D.; Giglietto, N.; Giordano, F.; Giroletti, M.;
Glanzman, T.; Green, D.; Grondin, M. -H.; Guillemot, L.; Guiriec,
S.; Harding, A. K.; Horan, D.; Jóhannesson, G.; Kamae, T.; Kensei,
S.; Kuss, M.; La Mura, G.; Latronico, L.; Lemoine-Goumard, M.;
Longo, F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Magill,
J. D.; Maldera, S.; Manfreda, A.; Mazziotta, M. N.; McEnery, J. E.;
Meyer, M.; Michelson, P. F.; Mirabal, N.; Monzani, M. E.; Moretti,
E.; Morselli, A.; Moskalenko, I. V.; Negro, M.; Nuss, E.; Ojha, R.;
Omodei, N.; Orienti, M.; Orlando, E.; Palatiello, M.; Paliya, V. S.;
Paneque, D.; Pesce-Rollins, M.; Piron, F.; Porter, T. A.; Principe, G.;
Rainò, S.; Rando, R.; Razzano, M.; Razzaque, S.; Reimer, A.; Reimer,
O.; Reposeur, T.; Rochester, L. S.; Saz Parkinson, P. M.; Sgrò, C.;
Siskind, E. J.; Spada, F.; Spandre, G.; Suson, D. J.; Takahashi, M.;
Tanaka, Y.; Thayer, J. G.; Thayer, J. B.; Thompson, D. J.; Tibaldo,
L.; Torres, D. F.; Torresi, E.; Troja, E.; Venters, T. M.; Vianello,
G.; Zaharijas, G.; Fermi Large Area Telescope Collaboration; Allison,
J. R.; Bannister, K. W.; Dobie, D.; Kaplan, D. L.; Lenc, E.; Lynch,
C.; Murphy, T.; Sadler, E. M.; Australia Telescope Compact Array,
ATCA:; Hotan, A.; James, C. W.; Oslowski, S.; Raja, W.; Shannon,
R. M.; Whiting, M.; Australian SKA Pathfinder, ASKAP:; Arcavi,
I.; Howell, D. A.; McCully, C.; Hosseinzadeh, G.; Hiramatsu, D.;
Poznanski, D.; Barnes, J.; Zaltzman, M.; Vasylyev, S.; Maoz, D.; Las
Cumbres Observatory Group; Cooke, J.; Bailes, M.; Wolf, C.; Deller,
A. T.; Lidman, C.; Wang, L.; Gendre, B.; Andreoni, I.; Ackley, K.;
Pritchard, T. A.; Bessell, M. S.; Chang, S. -W.; Möller, A.; Onken,
C. A.; Scalzo, R. A.; Ridden-Harper, R.; Sharp, R. G.; Tucker, B. E.;
Farrell, T. J.; Elmer, E.; Johnston, S.; Venkatraman Krishnan, V.;
Keane, E. F.; Green, J. A.; Jameson, A.; Hu, L.; Ma, B.; Sun, T.;
Wu, X.; Wang, X.; Shang, Z.; Hu, Y.; Ashley, M. C. B.; Yuan, X.; Li,
X.; Tao, C.; Zhu, Z.; Zhang, H.; Suntzeff, N. B.; Zhou, J.; Yang, J.;
Orange, B.; Morris, D.; Cucchiara, A.; Giblin, T.; Klotz, A.; Staff,
J.; Thierry, P.; Schmidt, B. P.; OzGrav; (Deeper, DWF; Wider; program,
Faster; AST3; CAASTRO Collaborations; Tanvir, N. R.; Levan, A. J.;
Cano, Z.; de Ugarte-Postigo, A.; González-Fernández, C.; Greiner,
J.; Hjorth, J.; Irwin, M.; Krühler, T.; Mandel, I.; Milvang-Jensen,
B.; O'Brien, P.; Rol, E.; Rosetti, S.; Rosswog, S.; Rowlinson, A.;
Steeghs, D. T. H.; Thöne, C. C.; Ulaczyk, K.; Watson, D.; Bruun,
S. H.; Cutter, R.; Figuera Jaimes, R.; Fujii, Y. I.; Fruchter, A. S.;
Gompertz, B.; Jakobsson, P.; Hodosan, G.; Jèrgensen, U. G.; Kangas,
T.; Kann, D. A.; Rabus, M.; Schrøder, S. L.; Stanway, E. R.; Wijers,
R. A. M. J.; VINROUGE Collaboration; Lipunov, V. M.; Gorbovskoy, E. S.;
Kornilov, V. G.; Tyurina, N. V.; Balanutsa, P. V.; Kuznetsov, A. S.;
Vlasenko, D. M.; Podesta, R. C.; Lopez, C.; Podesta, F.; Levato,
H. O.; Saffe, C.; Mallamaci, C. C.; Budnev, N. M.; Gress, O. A.;
Kuvshinov, D. A.; Gorbunov, I. A.; Vladimirov, V. V.; Zimnukhov,
D. S.; Gabovich, A. V.; Yurkov, V. V.; Sergienko, Yu. P.; Rebolo,
R.; Serra-Ricart, M.; Tlatov, A. G.; Ishmuhametova, Yu. V.; MASTER
Collaboration; Abe, F.; Aoki, K.; Aoki, W.; Asakura, Y.; Baar, S.;
Barway, S.; Bond, I. A.; Doi, M.; Finet, F.; Fujiyoshi, T.; Furusawa,
H.; Honda, S.; Itoh, R.; Kanda, N.; Kawabata, K. S.; Kawabata, M.; Kim,
J. H.; Koshida, S.; Kuroda, D.; Lee, C. -H.; Liu, W.; Matsubayashi,
K.; Miyazaki, S.; Morihana, K.; Morokuma, T.; Motohara, K.; Murata,
K. L.; Nagai, H.; Nagashima, H.; Nagayama, T.; Nakaoka, T.; Nakata,
F.; Ohsawa, R.; Ohshima, T.; Ohta, K.; Okita, H.; Saito, T.; Saito,
Y.; Sako, S.; Sekiguchi, Y.; Sumi, T.; Tajitsu, A.; Takahashi,
J.; Takayama, M.; Tamura, Y.; Tanaka, I.; Tanaka, M.; Terai, T.;
Tominaga, N.; Tristram, P. J.; Uemura, M.; Utsumi, Y.; Yamaguchi,
M. S.; Yasuda, N.; Yoshida, M.; Zenko, T.; J-GEM; Adams, S. M.;
Anupama, G. C.; Bally, J.; Barway, S.; Bellm, E.; Blagorodnova, N.;
Cannella, C.; Chandra, P.; Chatterjee, D.; Clarke, T. E.; Cobb, B. E.;
Cook, D. O.; Copperwheat, C.; De, K.; Emery, S. W. K.; Feindt, U.;
Foster, K.; Fox, O. D.; Frail, D. A.; Fremling, C.; Frohmaier, C.;
Garcia, J. A.; Ghosh, S.; Giacintucci, S.; Goobar, A.; Gottlieb, O.;
Grefenstette, B. W.; Hallinan, G.; Harrison, F.; Heida, M.; Helou,
G.; Ho, A. Y. Q.; Horesh, A.; Hotokezaka, K.; Ip, W. -H.; Itoh, R.;
Jacobs, Bob; Jencson, J. E.; Kasen, D.; Kasliwal, M. M.; Kassim,
N. E.; Kim, H.; Kiran, B. S.; Kuin, N. P. M.; Kulkarni, S. R.;
Kupfer, T.; Lau, R. M.; Madsen, K.; Mazzali, P. A.; Miller, A. A.;
Miyasaka, H.; Mooley, K.; Myers, S. T.; Nakar, E.; Ngeow, C. -C.;
Nugent, P.; Ofek, E. O.; Palliyaguru, N.; Pavana, M.; Perley, D. A.;
Peters, W. M.; Pike, S.; Piran, T.; Qi, H.; Quimby, R. M.; Rana, J.;
Rosswog, S.; Rusu, F.; Sadler, E. M.; Van Sistine, A.; Sollerman, J.;
Xu, Y.; Yan, L.; Yatsu, Y.; Yu, P. -C.; Zhang, C.; Zhao, W.; GROWTH;
JAGWAR; Caltech-NRAO; TTU-NRAO; NuSTAR Collaborations; Chambers,
K. C.; Huber, M. E.; Schultz, A. S. B.; Bulger, J.; Flewelling, H.;
Magnier, E. A.; Lowe, T. B.; Wainscoat, R. J.; Waters, C.; Willman,
M.; Pan-STARRS; Ebisawa, K.; Hanyu, C.; Harita, S.; Hashimoto, T.;
Hidaka, K.; Hori, T.; Ishikawa, M.; Isobe, N.; Iwakiri, W.; Kawai,
H.; Kawai, N.; Kawamuro, T.; Kawase, T.; Kitaoka, Y.; Makishima,
K.; Matsuoka, M.; Mihara, T.; Morita, T.; Morita, K.; Nakahira, S.;
Nakajima, M.; Nakamura, Y.; Negoro, H.; Oda, S.; Sakamaki, A.; Sasaki,
R.; Serino, M.; Shidatsu, M.; Shimomukai, R.; Sugawara, Y.; Sugita,
S.; Sugizaki, M.; Tachibana, Y.; Takao, Y.; Tanimoto, A.; Tomida, H.;
Tsuboi, Y.; Tsunemi, H.; Ueda, Y.; Ueno, S.; Yamada, S.; Yamaoka,
K.; Yamauchi, M.; Yatabe, F.; Yoneyama, T.; Yoshii, T.; MAXI Team;
Coward, D. M.; Crisp, H.; Macpherson, D.; Andreoni, I.; Laugier,
R.; Noysena, K.; Klotz, A.; Gendre, B.; Thierry, P.; Turpin, D.;
Consortium, TZAC; Im, M.; Choi, C.; Kim, J.; Yoon, Y.; Lim, G.; Lee,
S. -K.; Lee, C. -U.; Kim, S. -L.; Ko, S. -W.; Joe, J.; Kwon, M. -K.;
Kim, P. -J.; Lim, S. -K.; Choi, J. -S.; KU Collaboration; Fynbo,
J. P. U.; Malesani, D.; Xu, D.; Optical Telescope, Nordic; Smartt,
S. J.; Jerkstrand, A.; Kankare, E.; Sim, S. A.; Fraser, M.; Inserra,
C.; Maguire, K.; Leloudas, G.; Magee, M.; Shingles, L. J.; Smith,
K. W.; Young, D. R.; Kotak, R.; Gal-Yam, A.; Lyman, J. D.; Homan,
D. S.; Agliozzo, C.; Anderson, J. P.; Angus, C. R.; Ashall, C.;
Barbarino, C.; Bauer, F. E.; Berton, M.; Botticella, M. T.; Bulla,
M.; Cannizzaro, G.; Cartier, R.; Cikota, A.; Clark, P.; De Cia,
A.; Della Valle, M.; Dennefeld, M.; Dessart, L.; Dimitriadis, G.;
Elias-Rosa, N.; Firth, R. E.; Flörs, A.; Frohmaier, C.; Galbany, L.;
González-Gaitán, S.; Gromadzki, M.; Gutiérrez, C. P.; Hamanowicz,
A.; Harmanen, J.; Heintz, K. E.; Hernandez, M. -S.; Hodgkin, S. T.;
Hook, I. M.; Izzo, L.; James, P. A.; Jonker, P. G.; Kerzendorf, W. E.;
Kostrzewa-Rutkowska, Z.; Kromer, M.; Kuncarayakti, H.; Lawrence,
A.; Manulis, I.; Mattila, S.; McBrien, O.; Müller, A.; Nordin, J.;
O'Neill, D.; Onori, F.; Palmerio, J. T.; Pastorello, A.; Patat, F.;
Pignata, G.; Podsiadlowski, P.; Razza, A.; Reynolds, T.; Roy, R.;
Ruiter, A. J.; Rybicki, K. A.; Salmon, L.; Pumo, M. L.; Prentice,
S. J.; Seitenzahl, I. R.; Smith, M.; Sollerman, J.; Sullivan, M.;
Szegedi, H.; Taddia, F.; Taubenberger, S.; Terreran, G.; Van Soelen,
B.; Vos, J.; Walton, N. A.; Wright, D. E.; Wyrzykowski, Ł.; Yaron,
O.; pre="(">ePESSTO, 2
at a luminosity distance of {40}-8+8 Mpc and
with component masses consistent with neutron stars. The component
masses were later measured to be in the range 0.86 to 2.26 {M}⊙
. An extensive observing campaign was launched across the
electromagnetic spectrum leading to the discovery of a bright optical
transient (SSS17a, now with the IAU identification of AT 2017gfo) in
NGC 4993 (at ∼ 40 {{Mpc}}) less than 11 hours after the merger by the
One-Meter, Two Hemisphere (1M2H) team using the 1 m Swope Telescope. The
optical transient was independently detected by multiple teams
within an hour. Subsequent observations targeted the object and its
environment. Early ultraviolet observations revealed a blue transient
that faded within 48 hours. Optical and infrared observations showed
a redward evolution over ∼10 days. Following early non-detections,
X-ray and radio emission were discovered at the transient's position ∼
9 and ∼ 16 days, respectively, after the merger. Both the X-ray and
radio emission likely arise from a physical process that is distinct
from the one that generates the UV/optical/near-infrared emission. No
ultra-high-energy gamma-rays and no neutrino candidates consistent with
the source were found in follow-up searches. These observations support
the hypothesis that GW170817 was produced by the merger of two neutron
stars in NGC 4993 followed by a short gamma-ray burst (GRB 170817A)
and a kilonova/macronova powered by the radioactive decay of r-process
nuclei synthesized in the ejecta. Any correspondence should be
addressed to .
Title: Introduction to the High Energy cosmic-Radiation Detection
(HERD) Facility onboard China's Future Space Station
Authors: Zhang, S. N.; Adriani, O.; Consortium, H.; Albergo, S.;
Ambrosi, G.; An, Q.; Azzarello, P.; Bai, Y.; Bao, T.; Bernardini, P.;
Bertucci, B.; Bi, X.; Bongi, M.; Bottai, S.; Cao, W.; Cao, Z.; Chai,
J.; Chang, J.; Chen, G.; Chen, Y.; Chen, Z.; Cui, X. H.; Dai, Z. G.;
D'Alessandro, R.; Santo, M. D.; Dong, Y.; Duranti, M.; Fan, Y.; Fang,
K.; Feng, C. Q.; Feng, H.; Formato, V.; Fusco, P.; Gao, J.; Gargano,
F.; Giglietto, N.; Gou, Q.; Guo, Y. Q.; He, H. H.; Hu, H.; Hu, P.;
Huang, G. S.; Huang, J.; Huang, Y. F.; Li, H.; Li, R.; Li, Y.; Li,
Z.; Liang, E. W.; Lin, S.; Liu, H.; Liu, H.; Liu, J. B.; Liu, S. B.;
Liu, S. M.; Liu, X.; Loparco, F.; Lyu, J.; Marsella, G.; Mazziottai,
M. N.; Mitri, I. D.; Mori, N.; Papini, P.; Pearce, M.; Peng, W.; Pohl,
M.; Quan, Z.; Ryde, F.; Shi, D.; Su, M.; Sun, X. L.; Sun, X.; Surdo,
A.; Tang, Z. C.; Vannuccini, E.; Walter, R.; Wang, B.; Wang, B.; Wang,
J. C.; Wang, J. M.; Wang, J.; Wang, L.; Wang, R.; Wang, X. L.; Wang,
X. Y.; Wang, Z.; Wei, D. M.; Wu, B.; Wu, J.; Wu, Q.; Wu, X.; Wu,
X. F.; Xu, M.; Xu, Z. Z.; Yan, H. R.; Yin, P. F.; Yu, Y. W.; Yuan,
Q.; Zha, M.; Zhang, L.; Zhang, L.; Yi, Z.; Zhang, Y. L.; Zhao, Z. G.
Bibcode: 2017ICRC...35.1077Z
Altcode: 2017PoS...301.1077Z
No abstract at ADS
Title: Tapping the Core - a study of Alfvénic energy flow in an
erupting flux-rope configuration
Authors: Fletcher, L.; Dalmasse, K.; Gibson, S. E.; Fan, Y.
Bibcode: 2016AGUFMSH31B2564F
Altcode:
We analyze the evolution of reconnecting magnetic field in a 3-D
numerical simulation of a partially-ejected solar flux rope, with a
focus on understanding how the flux rope dynamics is linked to the
flow of energy through the field and the solar atmosphere as Alfvénic
Poynting flux. The magnetic flux rope splits in two during its eruption,
with reconnection taking place between the erupting rope and surrounding
fields, and internally in the strong field of the rope. We track the
Poynting flux entering and leaving the simulation current sheets,
and by mapping this down to the solar surface we identify locations of
weak and strong energy deposition in the lower atmosphere. Our tracking
method enables us to link the lower atmosphere signatures to different
stages of the coronal reconnection. We find a predominantly two-ribbon
morphology in the locations of Poynting flux deposition in the lower
atmosphere, in which the transition from reconnection involving weaker
field external to the flux rope, to reconnection involving the flux rope
core field, is accompanied by rapid ribbon spreading. In the core-field
reconnection phase, ribbons move into strong field regions on the
solar surface, and locations of highly concentrated downward-directed
Poynting flux are found, which may be linked to the most energetic flare
`footpoints' seen in optical and hard X-ray emission.
Title: Scientific objectives and capabilities of the Coronal Solar
Magnetism Observatory
Authors: Tomczyk, S.; Landi, E.; Burkepile, J. T.; Casini, R.; DeLuca,
E. E.; Fan, Y.; Gibson, S. E.; Lin, H.; McIntosh, S. W.; Solomon,
S. C.; Toma, G.; Wijn, A. G.; Zhang, J.
Bibcode: 2016JGRA..121.7470T
Altcode:
Magnetic influences increase in importance in the solar atmosphere
from the photosphere out into the corona, yet our ability to routinely
measure magnetic fields in the outer solar atmosphere is lacking. We
describe the scientific objectives and capabilities of the COronal Solar
Magnetism Observatory (COSMO), a proposed synoptic facility designed
to measure magnetic fields and plasma properties in the large-scale
solar atmosphere. COSMO comprises a suite of three instruments chosen
to enable the study of the solar atmosphere as a coupled system: (1)
a coronagraph with a 1.5 m aperture to measure the magnetic field,
temperature, density, and dynamics of the corona; (2) an instrument
for diagnostics of chromospheric and prominence magnetic fields and
plasma properties; and (3) a white light K-coronagraph to measure
the density structure and dynamics of the corona and coronal mass
ejections. COSMO will provide a unique combination of magnetic field,
density, temperature, and velocity observations in the corona and
chromosphere that have the potential to transform our understanding
of fundamental physical processes in the solar atmosphere and their
role in the origins of solar variability and space weather.
Title: Supplement: “Localization and Broadband Follow-up of the
Gravitational-wave Transient GW150914” (2016, ApJL, 826, L13)
Authors: Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M. R.;
Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari,
R. X.; Adya, V. B.; Affeldt, C.; Agathos, M.; Agatsuma, K.; Aggarwal,
N.; Aguiar, O. D.; Aiello, L.; Ain, A.; Ajith, P.; Allen, B.; Allocca,
A.; Altin, P. A.; Anderson, S. B.; Anderson, W. G.; Arai, K.; Araya,
M. C.; Arceneaux, C. C.; Areeda, J. S.; Arnaud, N.; Arun, K. G.;
Ascenzi, S.; Ashton, G.; Ast, M.; Aston, S. M.; Astone, P.; Aufmuth,
P.; Aulbert, C.; Babak, S.; Bacon, P.; Bader, M. K. M.; Baker, P. T.;
Baldaccini, F.; Ballardin, G.; Ballmer, S. W.; Barayoga, J. C.;
Barclay, S. E.; Barish, B. C.; Barker, D.; Barone, F.; Barr, B.;
Barsotti, L.; Barsuglia, M.; Barta, D.; Barthelmy, S.; Bartlett, J.;
Bartos, I.; Bassiri, R.; Basti, A.; Batch, J. C.; Baune, C.; Bavigadda,
V.; Bazzan, M.; Behnke, B.; Bejger, M.; Bell, A. S.; Bell, C. J.;
Berger, B. K.; Bergman, J.; Bergmann, G.; Berry, C. P. L.; Bersanetti,
D.; Bertolini, A.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko,
I. A.; Billingsley, G.; Birch, J.; Birney, R.; Biscans, S.; Bisht,
A.; Bitossi, M.; Biwer, C.; Bizouard, M. A.; Blackburn, J. K.; Blair,
C. D.; Blair, D. G.; Blair, R. M.; Bloemen, S.; Bock, O.; Bodiya,
T. P.; Boer, M.; Bogaert, G.; Bogan, C.; Bohe, A.; Bojtos, P.; Bond,
C.; Bondu, F.; Bonnand, R.; Boom, B. A.; Bork, R.; Boschi, V.; Bose,
S.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.; Brady, P. R.; Braginsky,
V. B.; Branchesi, M.; Brau, J. E.; Briant, T.; Brillet, A.; Brinkmann,
M.; Brisson, V.; Brockill, P.; Brooks, A. F.; Brown, D. A.; Brown,
D. D.; Brown, N. M.; Buchanan, C. C.; Buikema, A.; Bulik, T.; Bulten,
H. J.; Buonanno, A.; Buskulic, D.; Buy, C.; Byer, R. L.; Cadonati, L.;
Cagnoli, G.; Cahillane, C.; Bustillo, J. C.; Callister, T.; Calloni,
E.; Camp, J. B.; Cannon, K. C.; Cao, J.; Capano, C. D.; Capocasa,
E.; Carbognani, F.; Caride, S.; Diaz, J. C.; Casentini, C.; Caudill,
S.; Cavagliá, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda,
C. B.; Baiardi, L. C.; Cerretani, G.; Cesarini, E.; Chakraborty, R.;
Chalermsongsak, T.; Chamberlin, S. J.; Chan, M.; Chao, S.; Charlton,
P.; Chassande-Mottin, E.; Chen, H. Y.; Chen, Y.; Cheng, C.; Chincarini,
A.; Chiummo, A.; Cho, H. S.; Cho, M.; Chow, J. H.; Christensen, N.;
Chu, Q.; Chua, S.; Chung, S.; Ciani, G.; Clara, F.; Clark, J. A.;
Cleva, F.; Coccia, E.; Cohadon, P. -F.; Colla, A.; Collette, C. G.;
Cominsky, L.; Constancio, M., Jr.; Conte, A.; Conti, L.; Cook, D.;
Corbitt, T. R.; Cornish, N.; Corsi, A.; Cortese, S.; Costa, C. A.;
Coughlin, M. W.; Coughlin, S. B.; Coulon, J. -P.; Countryman, S. T.;
Couvares, P.; Cowan, E. E.; Coward, D. M.; Cowart, M. J.; Coyne, D. C.;
Coyne, R.; Craig, K.; Creighton, J. D. E.; Cripe, J.; Crowder, S. G.;
Cumming, A.; Cunningham, L.; Cuoco, E.; Dal Canton, T.; Danilishin,
S. L.; D'Antonio, S.; Danzmann, K.; Darman, N. S.; Dattilo, V.; Dave,
I.; Daveloza, H. P.; Davier, M.; Davies, G. S.; Daw, E. J.; Day, R.;
DeBra, D.; Debreczeni, G.; Degallaix, J.; De Laurentis, M.; Deléglise,
S.; Del Pozzo, W.; Denker, T.; Dent, T.; Dereli, H.; Dergachev, V.;
DeRosa, R. T.; De Rosa, R.; DeSalvo, R.; Dhurandhar, S.; Díaz, M. C.;
Di Fiore, L.; Di Giovanni, M.; Di Lieto, A.; Di Pace, S.; Di Palma,
I.; Di Virgilio, A.; Dojcinoski, G.; Dolique, V.; Donovan, F.; Dooley,
K. L.; Doravari, S.; Douglas, R.; Downes, T. P.; Drago, M.; Drever,
R. W. P.; Driggers, J. C.; Du, Z.; Ducrot, M.; Dwyer, S. E.; Edo,
T. B.; Edwards, M. C.; Effler, A.; Eggenstein, H. -B.; Ehrens, P.;
Eichholz, J.; Eikenberry, S. S.; Engels, W.; Essick, R. C.; Etzel,
T.; Evans, M.; Evans, T. M.; Everett, R.; Factourovich, M.; Fafone,
V.; Fair, H.; Fairhurst, S.; Fan, X.; Fang, Q.; Farinon, S.; Farr,
B.; Farr, W. M.; Favata, M.; Fays, M.; Fehrmann, H.; Fejer, M. M.;
Ferrante, I.; Ferreira, E. C.; Ferrini, F.; Fidecaro, F.; Fiori, I.;
Fiorucci, D.; Fisher, R. P.; Flaminio, R.; Fletcher, M.; Fournier,
J. -D.; Franco, S.; Frasca, S.; Frasconi, F.; Frei, Z.; Freise, A.;
Frey, R.; Frey, V.; Fricke, T. T.; Fritschel, P.; Frolov, V. V.;
Fulda, P.; Fyffe, M.; Gabbard, H. A. G.; Gair, J. R.; Gammaitoni,
L.; Gaonkar, S. G.; Garufi, F.; Gatto, A.; Gaur, G.; Gehrels, N.;
Gemme, G.; Gendre, B.; Genin, E.; Gennai, A.; George, J.; Gergely, L.;
Germain, V.; Ghosh, A.; Ghosh, S.; Giaime, J. A.; Giardina, K. D.;
Giazotto, A.; Gill, K.; Glaefke, A.; Goetz, E.; Goetz, R.; Gondan,
L.; González, G.; Castro, J. M. G.; Gopakumar, A.; Gordon, N. A.;
Gorodetsky, M. L.; Gossan, S. E.; Gosselin, M.; Gouaty, R.; Graef,
C.; Graff, P. B.; Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greco,
G.; Green, A. C.; Groot, P.; Grote, H.; Grunewald, S.; Guidi, G. M.;
Guo, X.; Gupta, A.; Gupta, M. K.; Gushwa, K. E.; Gustafson, E. K.;
Gustafson, R.; Hacker, J. J.; Hall, B. R.; Hall, E. D.; Hammond, G.;
Haney, M.; Hanke, M. M.; Hanks, J.; Hanna, C.; Hannam, M. D.; Hanson,
J.; Hardwick, T.; Haris, K.; Harms, J.; Harry, G. M.; Harry, I. W.;
Hart, M. J.; Hartman, M. T.; Haster, C. -J.; Haughian, K.; Heidmann,
A.; Heintze, M. C.; Heitmann, H.; Hello, P.; Hemming, G.; Hendry,
M.; Heng, I. S.; Hennig, J.; Heptonstall, A. W.; Heurs, M.; Hild,
S.; Hoak, D.; Hodge, K. A.; Hofman, D.; Hollitt, S. E.; Holt, K.;
Holz, D. E.; Hopkins, P.; Hosken, D. J.; Hough, J.; Houston, E. A.;
Howell, E. J.; Hu, Y. M.; Huang, S.; Huerta, E. A.; Huet, D.; Hughey,
B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Idrisy, A.; Indik, N.;
Ingram, D. R.; Inta, R.; Isa, H. N.; Isac, J. -M.; Isi, M.; Islas,
G.; Isogai, T.; Iyer, B. R.; Izumi, K.; Jacqmin, T.; Jang, H.; Jani,
K.; Jaranowski, P.; Jawahar, S.; Jiménez-Forteza, F.; Johnson, W. W.;
Jones, D. I.; Jones, R.; Jonker, R. J. G.; Ju, L.; Kalaghatgi, C. V.;
Kalogera, V.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Karki, S.;
Kasprzack, M.; Katsavounidis, E.; Katzman, W.; Kaufer, S.; Kaur,
T.; Kawabe, K.; Kawazoe, F.; Kéfélian, F.; Kehl, M. S.; Keitel,
D.; Kelley, D. B.; Kells, W.; Kennedy, R.; Key, J. S.; Khalaidovski,
A.; Khalili, F. Y.; Khan, I.; Khan, S.; Khan, Z.; Khazanov, E. A.;
Kijbunchoo, N.; Kim, C.; Kim, J.; Kim, K.; Kim, N.; Kim, N.; Kim,
Y. -M.; King, E. J.; King, P. J.; Kinzel, D. L.; Kissel, J. S.;
Kleybolte, L.; Klimenko, S.; Koehlenbeck, S. M.; Kokeyama, K.; Koley,
S.; Kondrashov, V.; Kontos, A.; Korobko, M.; Korth, W. Z.; Kowalska,
I.; Kozak, D. B.; Kringel, V.; Królak, A.; Krueger, C.; Kuehn, G.;
Kumar, P.; Kuo, L.; Kutynia, A.; Lackey, B. D.; Landry, M.; Lange,
J.; Lantz, B.; Lasky, P. D.; Lazzarini, A.; Lazzaro, C.; Leaci,
P.; Leavey, S.; Lebigot, E. O.; Lee, C. H.; Lee, H. K.; Lee, H. M.;
Lee, K.; Lenon, A.; Leonardi, M.; Leong, J. R.; Leroy, N.; Letendre,
N.; Levin, Y.; Levine, B. M.; Li, T. G. F.; Libson, A.; Littenberg,
T. B.; Lockerbie, N. A.; Logue, J.; Lombardi, A. L.; Lord, J. E.;
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Matone, L.; Mavalvala, N.; Mazumder, N.; Mazzolo, G.; McCarthy, R.;
McClelland, D. E.; McCormick, S.; McGuire, S. C.; McIntyre, G.; McIver,
J.; McManus, D. J.; McWilliams, S. T.; Meacher, D.; Meadors, G. D.;
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C.; Meyers, P. M.; Mezzani, F.; Miao, H.; Michel, C.; Middleton, H.;
Mikhailov, E. E.; Milano, L.; Miller, J.; Millhouse, M.; Minenkov, Y.;
Ming, J.; Mirshekari, S.; Mishra, C.; Mitra, S.; Mitrofanov, V. P.;
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D.; Mukherjee, S.; Mukund, N.; Mullavey, A.; Munch, J.; Murphy, D. J.;
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E.; Brandt, T. J.; Bruel, P.; Buson, S.; Caliandro, G. A.; Cameron,
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Spandre, G.; Spinelli, P.; Suson, D. J.; Tajima, H.; Thayer, J. B.;
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B.; Perley, D.; Ferreti, R.; Prince, T.; Kendrick, R.; Horesh, A.;
Intermediate Palomar Transient Factory (iPTF Collaboration); Hurley,
K.; Golenetskii, S. V.; Aptekar, R. L.; Frederiks, D. D.; Svinkin,
D. S.; Rau, A.; von Kienlin, A.; Zhang, X.; Smith, D. M.; Cline,
T.; Krimm, H.; InterPlanetary Network; Abe, F.; Doi, M.; Fujisawa,
K.; Kawabata, K. S.; Morokuma, T.; Motohara, K.; Tanaka, M.; Ohta,
K.; Yanagisawa, K.; Yoshida, M.; J-GEM Collaboration; Baltay, C.;
Rabinowitz, D.; Ellman, N.; Rostami, S.; La Silla-QUEST Survey;
Bersier, D. F.; Bode, M. F.; Collins, C. A.; Copperwheat, C. M.;
Darnley, M. J.; Galloway, D. K.; Gomboc, A.; Kobayashi, S.; Mazzali,
P.; Mundell, C. G.; Piascik, A. S.; Pollacco, Don; Steele, I. A.;
Ulaczyk, K.; Liverpool Telescope Collaboration; Broderick, J. W.;
Fender, R. P.; Jonker, P. G.; Rowlinson, A.; Stappers, B. W.;
Wijers, R. A. M. J.; Low Frequency Array (LOFAR Collaboration);
Lipunov, V.; Gorbovskoy, E.; Tyurina, N.; Kornilov, V.; Balanutsa, P.;
Kuznetsov, A.; Buckley, D.; Rebolo, R.; Serra-Ricart, M.; Israelian,
G.; Budnev, N. M.; Gress, O.; Ivanov, K.; Poleshuk, V.; Tlatov, A.;
Yurkov, V.; MASTER Collaboration; Kawai, N.; Serino, M.; Negoro,
H.; Nakahira, S.; Mihara, T.; Tomida, H.; Ueno, S.; Tsunemi, H.;
Matsuoka, M.; MAXI Collaboration; Croft, S.; Feng, L.; Franzen,
T. M. O.; Gaensler, B. M.; Johnston-Hollitt, M.; Kaplan, D. L.;
Morales, M. F.; Tingay, S. J.; Wayth, R. B.; Williams, A.; Murchison
Wide-field Array (MWA Collaboration); Smartt, S. J.; Chambers, K. C.;
Smith, K. W.; Huber, M. E.; Young, D. R.; Wright, D. E.; Schultz, A.;
Denneau, L.; Flewelling, H.; Magnier, E. A.; Primak, N.; Rest, A.;
Sherstyuk, A.; Stalder, B.; Stubbs, C. W.; Tonry, J.; Waters, C.;
Willman, M.; Pan-STARRS Collaboration; Olivares E., F.; Campbell,
H.; Kotak, R.; Sollerman, J.; Smith, M.; Dennefeld, M.; Anderson,
J. P.; Botticella, M. T.; Chen, T. -W.; Della Valle, M.; Elias-Rosa,
N.; Fraser, M.; Inserra, C.; Kankare, E.; Kupfer, T.; Harmanen,
J.; Galbany, L.; Le Guillou, L.; Lyman, J. D.; Maguire, K.; Mitra,
A.; Nicholl, M.; Razza, A.; Terreran, G.; Valenti, S.; Gal-Yam, A.;
PESSTO Collaboration; Ćwiek, A.; Ćwiok, M.; Mankiewicz, L.; Opiela,
R.; Zaremba, M.; Żarnecki, A. F.; Pi of Sky Collaboration; Onken,
C. A.; Scalzo, R. A.; Schmidt, B. P.; Wolf, C.; Yuan, F.; SkyMapper
Collaboration; Evans, P. A.; Kennea, J. A.; Burrows, D. N.; Campana,
S.; Cenko, S. B.; Giommi, P.; Marshall, F. E.; Nousek, J.; O'Brien,
P.; Osborne, J. P.; Palmer, D.; Perri, M.; Siegel, M.; Tagliaferri,
G.; Swift Collaboration; Klotz, A.; Turpin, D.; Laugier, R.; TAROT
Collaboration; Zadko Collaboration; Algerian National Observatory,
Algerian Collaboration; C2PU Collaboration; Beroiz, M.; Peñuela,
T.; Macri, L. M.; Oelkers, R. J.; Lambas, D. G.; Vrech, R.; Cabral,
J.; Colazo, C.; Dominguez, M.; Sanchez, B.; Gurovich, S.; Lares,
M.; Marshall, J. L.; DePoy, D. L.; Padilla, N.; Pereyra, N. A.;
Benacquista, M.; TOROS Collaboration; Tanvir, N. R.; Wiersema, K.;
Levan, A. J.; Steeghs, D.; Hjorth, J.; Fynbo, J. P. U.; Malesani, D.;
Milvang-Jensen, B.; Watson, D.; Irwin, M.; Fernandez, C. G.; McMahon,
R. G.; Banerji, M.; Gonzalez-Solares, E.; Schulze, S.; de Ugarte
Postigo, A.; Thoene, C. C.; Cano, Z.; Rosswog, S.; VISTA Collaboration
Bibcode: 2016ApJS..225....8A
Altcode: 2016arXiv160407864A
This Supplement provides supporting material for Abbott et
al. (2016a). We briefly summarize past electromagnetic (EM) follow-up
efforts as well as the organization and policy of the current EM
follow-up program. We compare the four probability sky maps produced
for the gravitational-wave transient GW150914, and provide additional
details of the EM follow-up observations that were performed in the
different bands.
Title: XIPE: the x-ray imaging polarimetry explorer
Authors: Soffitta, P.; Bellazzini, R.; Bozzo, E.; Burwitz, V.;
Castro-Tirado, A.; Costa, E.; Courvoisier, T.; Feng, H.; Gburek,
S.; Goosmann, R.; Karas, V.; Matt, G.; Muleri, F.; Nandra, K.;
Pearce, M.; Poutanen, J.; Reglero, V.; Sabau Maria, D.; Santangelo,
A.; Tagliaferri, G.; Tenzer, C.; Vink, J.; Weisskopf, M. C.; Zane,
S.; Agudo, I.; Antonelli, A.; Attina, P.; Baldini, L.; Bykov, A.;
Carpentiero, R.; Cavazzuti, E.; Churazov, E.; Del Monte, E.; De
Martino, D.; Donnarumma, I.; Doroshenko, V.; Evangelista, Y.; Ferreira,
I.; Gallo, E.; Grosso, N.; Kaaret, P.; Kuulkers, E.; Laranaga, J.;
Latronico, L.; Lumb, D. H.; Macian, J.; Malzac, J.; Marin, F.; Massaro,
E.; Minuti, M.; Mundell, C.; Ness, J. U.; Oosterbroek, T.; Paltani, S.;
Pareschi, G.; Perna, R.; Petrucci, P. -O.; Pinazo, H. B.; Pinchera,
M.; Rodriguez, J. P.; Roncadelli, M.; Santovincenzo, A.; Sazonov,
S.; Sgro, C.; Spiga, D.; Svoboda, J.; Theobald, C.; Theodorou, T.;
Turolla, R.; Wilhelmi de Ona, E.; Winter, B.; Akbar, A. M.; Allan,
H.; Aloisio, R.; Altamirano, D.; Amati, L.; Amato, E.; Angelakis,
E.; Arezu, J.; Atteia, J. -L.; Axelsson, M.; Bachetti, M.; Ballo, L.;
Balman, S.; Bandiera, R.; Barcons, X.; Basso, S.; Baykal, A.; Becker,
W.; Behar, E.; Beheshtipour, B.; Belmont, R.; Berger, E.; Bernardini,
F.; Bianchi, S.; Bisnovatyi-Kogan, G.; Blasi, P.; Blay, P.; Bodaghee,
A.; Boer, M.; Boettcher, M.; Bogdanov, S.; Bombaci, I.; Bonino, R.;
Braga, J.; Brandt, W.; Brez, A.; Bucciantini, N.; Burderi, L.; Caiazzo,
I.; Campana, R.; Campana, S.; Capitanio, F.; Cappi, M.; Cardillo,
M.; Casella, P.; Catmabacak, O.; Cenko, B.; Cerda-Duran, P.; Cerruti,
C.; Chaty, S.; Chauvin, M.; Chen, Y.; Chenevez, J.; Chernyakova, M.;
Cheung, C. C. Teddy; Christodoulou, D.; Connell, P.; Corbet, R.; Coti
Zelati, F.; Covino, S.; Cui, W.; Cusumano, G.; D'Ai, A.; D'Ammando,
F.; Dadina, M.; Dai, Z.; De Rosa, A.; de Ruvo, L.; Degenaar, N.;
Del Santo, M.; Del Zanna, L.; Dewangan, G.; Di Cosimo, S.; Di Lalla,
N.; Di Persio, G.; Di Salvo, T.; Dias, T.; Done, C.; Dovciak, M.;
Doyle, G.; Ducci, L.; Elsner, R.; Enoto, T.; Escada, J.; Esposito,
P.; Eyles, C.; Fabiani, S.; Falanga, M.; Falocco, S.; Fan, Y.; Fender,
R.; Feroci, M.; Ferrigno, C.; Forman, W.; Foschini, L.; Fragile, C.;
Fuerst, F.; Fujita, Y.; Gasent-Blesa, J. L.; Gelfand, J.; Gendre, B.;
Ghirlanda, G.; Ghisellini, G.; Giroletti, M.; Goetz, D.; Gogus, E.;
Gomez, J. -L.; Gonzalez, D.; Gonzalez-Riestra, R.; Gotthelf, E.; Gou,
L.; Grandi, P.; Grinberg, V.; Grise, F.; Guidorzi, C.; Gurlebeck, N.;
Guver, T.; Haggard, D.; Hardcastle, M.; Hartmann, D.; Haswell, C.;
Heger, A.; Hernanz, M.; Heyl, J.; Ho, L.; Hoormann, J.; Horak, J.;
Huovelin, J.; Huppenkothen, D.; Iaria, R.; Inam Sitki, C.; Ingram,
A.; Israel, G.; Izzo, L.; Burgess, M.; Jackson, M.; Ji, L.; Jiang, J.;
Johannsen, T.; Jones, C.; Jorstad, S.; Kajava, J. J. E.; Kalamkar, M.;
Kalemci, E.; Kallman, T.; Kamble, A.; Kislat, F.; Kiss, M.; Klochkov,
D.; Koerding, E.; Kolehmainen, M.; Koljonen, K.; Komossa, S.; Kong,
A.; Korpela, S.; Kowalinski, M.; Krawczynski, H.; Kreykenbohm, I.;
Kuss, M.; Lai, D.; Lan, M.; Larsson, J.; Laycock, S.; Lazzati, D.;
Leahy, D.; Li, H.; Li, J.; Li, L. -X.; Li, T.; Li, Z.; Linares, M.;
Lister, M.; Liu, H.; Lodato, G.; Lohfink, A.; Longo, F.; Luna, G.;
Lutovinov, A.; Mahmoodifar, S.; Maia, J.; Mainieri, V.; Maitra, C.;
Maitra, D.; Majczyna, A.; Maldera, S.; Malyshev, D.; Manfreda, A.;
Manousakis, A.; Manuel, R.; Margutti, R.; Marinucci, A.; Markoff, S.;
Marscher, A.; Marshall, H.; Massaro, F.; McLaughlin, M.; Medina-Tanco,
G.; Mehdipour, M.; Middleton, M.; Mignani, R.; Mimica, P.; Mineo, T.;
Mingo, B.; Miniutti, G.; Mirac, S. M.; Morlino, G.; Motlagh, A. V.;
Motta, S.; Mushtukov, A.; Nagataki, S.; Nardini, F.; Nattila, J.;
Navarro, G. J.; Negri, B.; Negro, Matteo; Nenonen, S.; Neustroev,
V.; Nicastro, F.; Norton, A.; Nucita, A.; O'Brien, P.; O'Dell, S.
Bibcode: 2016SPIE.9905E..15S
Altcode:
XIPE, the X-ray Imaging Polarimetry Explorer, is a mission dedicated to
X-ray Astronomy. At the time of writing XIPE is in a competitive phase
A as fourth medium size mission of ESA (M4). It promises to reopen
the polarimetry window in high energy Astrophysics after more than 4
decades thanks to a detector that efficiently exploits the photoelectric
effect and to X-ray optics with large effective area. XIPE uniqueness is
time-spectrally-spatially- resolved X-ray polarimetry as a breakthrough
in high energy astrophysics and fundamental physics. Indeed the payload
consists of three Gas Pixel Detectors at the focus of three X-ray
optics with a total effective area larger than one XMM mirror but with
a low weight. The payload is compatible with the fairing of the Vega
launcher. XIPE is designed as an observatory for X-ray astronomers with
75 % of the time dedicated to a Guest Observer competitive program and
it is organized as a consortium across Europe with main contributions
from Italy, Germany, Spain, United Kingdom, Poland, Sweden.
Title: PANGU: a wide field gamma-ray imager and polarimeter
Authors: Wu, X.; Walter, R.; Su, M.; Ambrosi, G.; Azzarello, P.;
Böttcher, M.; Chang, J.; Chernyakova, M.; Fan, Y.; Farnier, C.;
Gargano, F.; Grenier, I.; Hajdas, W.; Mazziotta, M. N.; Pearce, M.;
Pohl, M.; Zdziarski, A.
Bibcode: 2016SPIE.9905E..6EW
Altcode:
PANGU (the PAir-productioN Gamma-ray Unit) is a gamma-ray telescope
with a wide field of view optimized for spectro-imaging, timing and
polarization studies. It will map the gamma-ray sky from 10 MeV to a few
GeV with unprecedented spatial resolution. This window on the Universe
is unique to detect photons produced directly by relativistic particles,
via the decay of neutral pions, or the annihilation or decay light from
anti-matter and the putative light dark matter candidates. A wealth
of questions can be probed among the most important themes of modern
physics and astrophysics. The PANGU instrument is a pair-conversion
gamma-ray telescope based on an innovative design of a silicon strip
tracker. It is light, compact and accurate. It consists of 100 layers
of silicon micro-strip detector of 80 x 80 cm2 in area,
stacked to height of about 90 cm, and covered by an anticoincidence
detector. PANGU relies on multiple scattering effects for energy
measurement, reaching an energy resolution between 30-50% for 10 MeV -
1 GeV. The novel tracker will allow the first polarization measurement
and provide the best angular resolution ever obtained in the soft
gamma ray and GeV band.
Title: Constraining coronal magnetic field models using coronal
polarimetry
Authors: Dalmasse, Kévin; Nychka, D. W.; Gibson, S. E.; Flyer, N.;
Fan, Y.
Bibcode: 2016shin.confE..42D
Altcode:
Knowing the 3D coronal magnetic field prior to the trigger of a
coronal mass ejection (CME) is one of the key features for predicting
their geomagnetic effect. Since the magnetic field is essentially
measured at the photosphere, one must rely on models to obtain the
3D magnetic field in the corona. Various coronal observables can then
be used to constrain the parameters, and hence the magnetic field, of
these models. One type of observable that is receiving an increasing
attention is coronal polarization of infrared lines such as the Fe
XIII 10747 A and 10798 A lines observed by the Coronal Multichannel
Polarimeter (CoMP), which are sensitive to the coronal magnetic
field. By combining forward modeling with a novel optimization method
applied to a synthetic test bed of a coronal magnetic flux rope, we
show that the polarimetric signal of coronal infrared lines contains
enough information to constrain the parameters, and hence the magnetic
structure, of coronal magnetic field models. We discuss future plans
for application of our method to solar observations.
Title: Localization and Broadband Follow-up of the Gravitational-wave
Transient GW150914
Authors: Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M. R.;
Acernese, F.; Ackley, K.; Adams, C.; Adams, T.; Addesso, P.; Adhikari,
R. X.; Adya, V. B.; Affeldt, C.; Agathos, M.; Agatsuma, K.; Aggarwal,
N.; Aguiar, O. D.; Aiello, L.; Ain, A.; Ajith, P.; Allen, B.; Allocca,
A.; Altin, P. A.; Anderson, S. B.; Anderson, W. G.; Arai, K.; Araya,
M. C.; Arceneaux, C. C.; Areeda, J. S.; Arnaud, N.; Arun, K. G.;
Ascenzi, S.; Ashton, G.; Ast, M.; Aston, S. M.; Astone, P.; Aufmuth,
P.; Aulbert, C.; Babak, S.; Bacon, P.; Bader, M. K. M.; Baker, P. T.;
Baldaccini, F.; Ballardin, G.; Ballmer, S. W.; Barayoga, J. C.;
Barclay, S. E.; Barish, B. C.; Barker, D.; Barone, F.; Barr, B.;
Barsotti, L.; Barsuglia, M.; Barta, D.; Barthelmy, S.; Bartlett, J.;
Bartos, I.; Bassiri, R.; Basti, A.; Batch, J. C.; Baune, C.; Bavigadda,
V.; Bazzan, M.; Behnke, B.; Bejger, M.; Bell, A. S.; Bell, C. J.;
Berger, B. K.; Bergman, J.; Bergmann, G.; Berry, C. P. L.; Bersanetti,
D.; Bertolini, A.; Betzwieser, J.; Bhagwat, S.; Bhandare, R.; Bilenko,
I. A.; Billingsley, G.; Birch, J.; Birney, R.; Biscans, S.; Bisht,
A.; Bitossi, M.; Biwer, C.; Bizouard, M. A.; Blackburn, J. K.; Blair,
C. D.; Blair, D. G.; Blair, R. M.; Bloemen, S.; Bock, O.; Bodiya,
T. P.; Boer, M.; Bogaert, G.; Bogan, C.; Bohe, A.; Bojtos, P.; Bond,
C.; Bondu, F.; Bonnand, R.; Boom, B. A.; Bork, R.; Boschi, V.; Bose,
S.; Bouffanais, Y.; Bozzi, A.; Bradaschia, C.; Brady, P. R.; Braginsky,
V. B.; Branchesi, M.; Brau, J. E.; Briant, T.; Brillet, A.; Brinkmann,
M.; Brisson, V.; Brockill, P.; Brooks, A. F.; Brown, D. A.; Brown,
D. D.; Brown, N. M.; Buchanan, C. C.; Buikema, A.; Bulik, T.; Bulten,
H. J.; Buonanno, A.; Buskulic, D.; Buy, C.; Byer, R. L.; Cadonati, L.;
Cagnoli, G.; Cahillane, C.; Bustillo, J. C.; Callister, T.; Calloni,
E.; Camp, J. B.; Cannon, K. C.; Cao, J.; Capano, C. D.; Capocasa,
E.; Carbognani, F.; Caride, S.; Diaz, J. C.; Casentini, C.; Caudill,
S.; Cavagliá, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda,
C. B.; Baiardi, L. C.; Cerretani, G.; Cesarini, E.; Chakraborty, R.;
Chalermsongsak, T.; Chamberlin, S. J.; Chan, M.; Chao, S.; Charlton,
P.; Chassande-Mottin, E.; Chen, H. Y.; Chen, Y.; Cheng, C.; Chincarini,
A.; Chiummo, A.; Cho, H. S.; Cho, M.; Chow, J. H.; Christensen, N.;
Chu, Q.; Chua, S.; Chung, S.; Ciani, G.; Clara, F.; Clark, J. A.;
Cleva, F.; Coccia, E.; Cohadon, P. -F.; Colla, A.; Collette, C. G.;
Cominsky, L.; Constancio, M., Jr.; Conte, A.; Conti, L.; Cook, D.;
Corbitt, T. R.; Cornish, N.; Corsi, A.; Cortese, S.; Costa, C. A.;
Coughlin, M. W.; Coughlin, S. B.; Coulon, J. -P.; Countryman, S. T.;
Couvares, P.; Cowan, E. E.; Coward, D. M.; Cowart, M. J.; Coyne, D. C.;
Coyne, R.; Craig, K.; Creighton, J. D. E.; Cripe, J.; Crowder, S. G.;
Cumming, A.; Cunningham, L.; Cuoco, E.; Dal Canton, T.; Danilishin,
S. L.; D'Antonio, S.; Danzmann, K.; Darman, N. S.; Dattilo, V.; Dave,
I.; Daveloza, H. P.; Davier, M.; Davies, G. S.; Daw, E. J.; Day, R.;
Debra, D.; Debreczeni, G.; Degallaix, J.; de Laurentis, M.; Deléglise,
S.; Del Pozzo, W.; Denker, T.; Dent, T.; Dereli, H.; Dergachev, V.;
Derosa, R. T.; De Rosa, R.; Desalvo, R.; Dhurandhar, S.; Díaz, M. C.;
di Fiore, L.; di Giovanni, M.; di Lieto, A.; di Pace, S.; di Palma,
I.; di Virgilio, A.; Dojcinoski, G.; Dolique, V.; Donovan, F.; Dooley,
K. L.; Doravari, S.; Douglas, R.; Downes, T. P.; Drago, M.; Drever,
R. W. P.; Driggers, J. C.; Du, Z.; Ducrot, M.; Dwyer, S. E.; Edo,
T. B.; Edwards, M. C.; Effler, A.; Eggenstein, H. -B.; Ehrens, P.;
Eichholz, J.; Eikenberry, S. S.; Engels, W.; Essick, R. C.; Etzel,
T.; Evans, M.; Evans, T. M.; Everett, R.; Factourovich, M.; Fafone,
V.; Fair, H.; Fairhurst, S.; Fan, X.; Fang, Q.; Farinon, S.; Farr,
B.; Farr, W. M.; Favata, M.; Fays, M.; Fehrmann, H.; Fejer, M. M.;
Ferrante, I.; Ferreira, E. C.; Ferrini, F.; Fidecaro, F.; Fiori, I.;
Fiorucci, D.; Fisher, R. P.; Flaminio, R.; Fletcher, M.; Fournier,
J. -D.; Franco, S.; Frasca, S.; Frasconi, F.; Frei, Z.; Freise, A.;
Frey, R.; Frey, V.; Fricke, T. T.; Fritschel, P.; Frolov, V. V.;
Fulda, P.; Fyffe, M.; Gabbard, H. A. G.; Gair, J. R.; Gammaitoni,
L.; Gaonkar, S. G.; Garufi, F.; Gatto, A.; Gaur, G.; Gehrels, N.;
Gemme, G.; Gendre, B.; Genin, E.; Gennai, A.; George, J.; Gergely, L.;
Germain, V.; Ghosh, A.; Ghosh, S.; Giaime, J. A.; Giardina, K. D.;
Giazotto, A.; Gill, K.; Glaefke, A.; Goetz, E.; Goetz, R.; Gondan,
L.; González, G.; Castro, J. M. G.; Gopakumar, A.; Gordon, N. A.;
Gorodetsky, M. L.; Gossan, S. E.; Gosselin, M.; Gouaty, R.; Graef,
C.; Graff, P. B.; Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greco,
G.; Green, A. C.; Groot, P.; Grote, H.; Grunewald, S.; Guidi, G. M.;
Guo, X.; Gupta, A.; Gupta, M. K.; Gushwa, K. E.; Gustafson, E. K.;
Gustafson, R.; Hacker, J. J.; Hall, B. R.; Hall, E. D.; Hammond, G.;
Haney, M.; Hanke, M. M.; Hanks, J.; Hanna, C.; Hannam, M. D.; Hanson,
J.; Hardwick, T.; Haris, K.; Harms, J.; Harry, G. M.; Harry, I. W.;
Hart, M. J.; Hartman, M. T.; Haster, C. -J.; Haughian, K.; Heidmann,
A.; Heintze, M. C.; Heitmann, H.; Hello, P.; Hemming, G.; Hendry,
M.; Heng, I. S.; Hennig, J.; Heptonstall, A. W.; Heurs, M.; Hild,
S.; Hoak, D.; Hodge, K. A.; Hofman, D.; Hollitt, S. E.; Holt, K.;
Holz, D. E.; Hopkins, P.; Hosken, D. J.; Hough, J.; Houston, E. A.;
Howell, E. J.; Hu, Y. M.; Huang, S.; Huerta, E. A.; Huet, D.; Hughey,
B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Idrisy, A.; Indik, N.;
Ingram, D. R.; Inta, R.; Isa, H. N.; Isac, J. -M.; Isi, M.; Islas,
G.; Isogai, T.; Iyer, B. R.; Izumi, K.; Jacqmin, T.; Jang, H.; Jani,
K.; Jaranowski, P.; Jawahar, S.; Jiménez-Forteza, F.; Johnson, W. W.;
Jones, D. I.; Jones, R.; Jonker, R. J. G.; Ju, L.; Kalaghatgi, C. V.;
Kalogera, V.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Karki, S.;
Kasprzack, M.; Katsavounidis, E.; Katzman, W.; Kaufer, S.; Kaur,
T.; Kawabe, K.; Kawazoe, F.; Kéfélian, F.; Kehl, M. S.; Keitel,
D.; Kelley, D. B.; Kells, W.; Kennedy, R.; Key, J. S.; Khalaidovski,
A.; Khalili, F. Y.; Khan, I.; Khan, S.; Khan, Z.; Khazanov, E. A.;
Kijbunchoo, N.; Kim, C.; Kim, J.; Kim, K.; Kim, N.; Kim, N.; Kim,
Y. -M.; King, E. J.; King, P. J.; Kinzel, D. L.; Kissel, J. S.;
Kleybolte, L.; Klimenko, S.; Koehlenbeck, S. M.; Kokeyama, K.; Koley,
S.; Kondrashov, V.; Kontos, A.; Korobko, M.; Korth, W. Z.; Kowalska,
I.; Kozak, D. B.; Kringel, V.; Królak, A.; Krueger, C.; Kuehn, G.;
Kumar, P.; Kuo, L.; Kutynia, A.; Lackey, B. D.; Landry, M.; Lange,
J.; Lantz, B.; Lasky, P. D.; Lazzarini, A.; Lazzaro, C.; Leaci,
P.; Leavey, S.; Lebigot, E. O.; Lee, C. H.; Lee, H. K.; Lee, H. M.;
Lee, K.; Lenon, A.; Leonardi, M.; Leong, J. R.; Leroy, N.; Letendre,
N.; Levin, Y.; Levine, B. M.; Li, T. G. F.; Libson, A.; Littenberg,
T. B.; Lockerbie, N. A.; Logue, J.; Lombardi, A. L.; Lord, J. E.;
Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lough, J. D.;
Lück, H.; Lundgren, A. P.; Luo, J.; Lynch, R.; Ma, Y.; MacDonald, T.;
Machenschalk, B.; Macinnis, M.; MacLeod, D. M.; Magaña-Sandoval, F.;
Magee, R. M.; Mageswaran, M.; Majorana, E.; Maksimovic, I.; Malvezzi,
V.; Man, N.; Mandel, I.; Mandic, V.; Mangano, V.; Mansell, G. L.;
Manske, M.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka, S.;
Márka, Z.; Markosyan, A. S.; Maros, E.; Martelli, F.; Martellini, L.;
Martin, I. W.; Martin, R. M.; Martynov, D. V.; Marx, J. N.; Mason,
K.; Masserot, A.; Massinger, T. J.; Masso-Reid, M.; Matichard, F.;
Matone, L.; Mavalvala, N.; Mazumder, N.; Mazzolo, G.; McCarthy, R.;
McClelland, D. E.; McCormick, S.; McGuire, S. C.; McIntyre, G.; McIver,
J.; McManus, D. J.; McWilliams, S. T.; Meacher, D.; Meadors, G. D.;
Meidam, J.; Melatos, A.; Mendell, G.; Mendoza-Gandara, D.; Mercer,
R. A.; Merilh, E.; Merzougui, M.; Meshkov, S.; Messenger, C.; Messick,
C.; Meyers, P. M.; Mezzani, F.; Miao, H.; Michel, C.; Middleton, H.;
Mikhailov, E. E.; Milano, L.; Miller, J.; Millhouse, M.; Minenkov, Y.;
Ming, J.; Mirshekari, S.; Mishra, C.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Moggi, A.; Mohan, M.; Mohapatra,
S. R. P.; Montani, M.; Moore, B. C.; Moore, C. J.; Moraru, D.;
Moreno, G.; Morriss, S. R.; Mossavi, K.; Mours, B.; Mow-Lowry, C. M.;
Mueller, C. L.; Mueller, G.; Muir, A. W.; Mukherjee, A.; Mukherjee,
D.; Mukherjee, S.; Mukund, N.; Mullavey, A.; Munch, J.; Murphy, D. J.;
Murray, P. G.; Mytidis, A.; Nardecchia, I.; Naticchioni, L.; Nayak,
R. K.; Necula, V.; Nedkova, K.; Nelemans, G.; Neri, M.; Neunzert, A.;
Newton, G.; Nguyen, T. T.; Nielsen, A. B.; Nissanke, S.; Nitz, A.;
Nocera, F.; Nolting, D.; Normandin, M. E. N.; Nuttall, L. K.; Oberling,
J.; Ochsner, E.; O'Dell, J.; Oelker, E.; Ogin, G. H.; Oh, J. J.; Oh,
S. H.; Ohme, F.; Oliver, M.; Oppermann, P.; Oram, R. J.; O'Reilly,
B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens, R. S.; Overmier,
H.; Owen, B. J.; Pai, A.; Pai, S. A.; Palamos, J. R.; Palashov, O.;
Palliyaguru, N.; Palomba, C.; Pal-Singh, A.; Pan, H.; Pankow, C.;
Pannarale, F.; Pant, B. C.; Paoletti, F.; Paoli, A.; Papa, M. A.;
Paris, H. R.; Parker, W.; Pascucci, D.; Pasqualetti, A.; Passaquieti,
R.; Passuello, D.; Patricelli, B.; Patrick, Z.; Pearlstone, B. L.;
Pedraza, M.; Pedurand, R.; Pekowsky, L.; Pele, A.; Penn, S.; Perreca,
A.; Phelps, M.; Piccinni, O.; Pichot, M.; Piergiovanni, F.; Pierro,
V.; Pillant, G.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Poggiani,
R.; Popolizio, P.; Post, A.; Powell, J.; Prasad, J.; Predoi, V.;
Premachandra, S. S.; Prestegard, T.; Price, L. R.; Prijatelj, M.;
Principe, M.; Privitera, S.; Prodi, G. A.; Prokhorov, L.; Puncken,
O.; Punturo, M.; Puppo, P.; Pürrer, M.; Qi, H.; Qin, J.; Quetschke,
V.; Quintero, E. A.; Quitzow-James, R.; Raab, F. J.; Rabeling, D. S.;
Radkins, H.; Raffai, P.; Raja, S.; Rakhmanov, M.; Rapagnani, P.;
Raymond, V.; Razzano, M.; Re, V.; Read, J.; Reed, C. M.; Regimbau,
T.; Rei, L.; Reid, S.; Reitze, D. H.; Rew, H.; Reyes, S. D.; Ricci,
F.; Riles, K.; Robertson, N. A.; Robie, R.; Robinet, F.; Rocchi, A.;
Rolland, L.; Rollins, J. G.; Roma, V. J.; Romano, R.; Romanov, G.;
Romie, J. H.; Rosińska, D.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan,
K.; Sachdev, S.; Sadecki, T.; Sadeghian, L.; Salconi, L.; Saleem,
M.; Salemi, F.; Samajdar, A.; Sammut, L.; Sanchez, E. J.; Sandberg,
V.; Sandeen, B.; Sanders, J. R.; Sassolas, B.; Sathyaprakash, B. S.;
Saulson, P. R.; Sauter, O.; Savage, R. L.; Sawadsky, A.; Schale, P.;
Schilling, R.; Schmidt, J.; Schmidt, P.; Schnabel, R.; Schofield,
R. M. S.; Schönbeck, A.; Schreiber, E.; Schuette, D.; Schutz,
B. F.; Scott, J.; Scott, S. M.; Sellers, D.; Sentenac, D.; Sequino,
V.; Sergeev, A.; Serna, G.; Setyawati, Y.; Sevigny, A.; Shaddock,
D. A.; Shah, S.; Shahriar, M. S.; Shaltev, M.; Shao, Z.; Shapiro,
B.; Shawhan, P.; Sheperd, A.; Shoemaker, D. H.; Shoemaker, D. M.;
Siellez, K.; Siemens, X.; Sigg, D.; Silva, A. D.; Simakov, D.; Singer,
A.; Singh, A.; Singh, R.; Singhal, A.; Sintes, A. M.; Slagmolen,
B. J. J.; Smith, J. R.; Smith, N. D.; Smith, R. J. E.; Son, E. J.;
Sorazu, B.; Sorrentino, F.; Souradeep, T.; Srivastava, A. K.; Staley,
A.; Steinke, M.; Steinlechner, J.; Steinlechner, S.; Steinmeyer, D.;
Stephens, B. C.; Stone, R.; Strain, K. A.; Straniero, N.; Stratta, G.;
Strauss, N. A.; Strigin, S.; Sturani, R.; Stuver, A. L.; Summerscales,
T. Z.; Sun, L.; Sutton, P. J.; Swinkels, B. L.; Szczepańczyk, M. J.;
Tacca, M.; Talukder, D.; Tanner, D. B.; Tápai, M.; Tarabrin, S. P.;
Taracchini, A.; Taylor, R.; Theeg, T.; Thirugnanasambandam, M. P.;
Thomas, E. G.; Thomas, M.; Thomas, P.; Thorne, K. A.; Thorne, K. S.;
Thrane, E.; Tiwari, S.; Tiwari, V.; Tokmakov, K. V.; Tomlinson, C.;
Tonelli, M.; Torres, C. V.; Torrie, C. I.; Töyrä, D.; Travasso,
F.; Traylor, G.; Trifirò, D.; Tringali, M. C.; Trozzo, L.; Tse, M.;
Turconi, M.; Tuyenbayev, D.; Ugolini, D.; Unnikrishnan, C. S.; Urban,
A. L.; Usman, S. A.; Vahlbruch, H.; Vajente, G.; Valdes, G.; van
Bakel, N.; van Beuzekom, M.; van den Brand, J. F. J.; van den Broeck,
C.; Vander-Hyde, D. C.; van der Schaaf, L.; van Heijningen, J. V.;
van Veggel, A. A.; Vardaro, M.; Vass, S.; Vasúth, M.; Vaulin, R.;
Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Venkateswara, K.;
Verkindt, D.; Vetrano, F.; Viceré, A.; Vinciguerra, S.; Vine, D. J.;
Vinet, J. -Y.; Vitale, S.; Vo, T.; Vocca, H.; Vorvick, C.; Voss, D.;
Vousden, W. D.; Vyatchanin, S. P.; Wade, A. R.; Wade, L. E.; Wade,
M.; Walker, M.; Wallace, L.; Walsh, S.; Wang, G.; Wang, H.; Wang,
M.; Wang, X.; Wang, Y.; Ward, R. L.; Warner, J.; Was, M.; Weaver,
B.; Wei, L. -W.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Welborn,
T.; Wen, L.; Weßels, P.; Westphal, T.; Wette, K.; Whelan, J. T.;
White, D. J.; Whiting, B. F.; Williams, R. D.; Williamson, A. R.;
Willis, J. L.; Willke, B.; Wimmer, M. H.; Winkler, W.; Wipf, C. C.;
Wittel, H.; Woan, G.; Worden, J.; Wright, J. L.; Wu, G.; Yablon, J.;
Yam, W.; Yamamoto, H.; Yancey, C. C.; Yap, M. J.; Yu, H.; Yvert, M.;
Zadrożny, A.; Zangrando, L.; Zanolin, M.; Zendri, J. -P.; Zevin,
M.; Zhang, F.; Zhang, L.; Zhang, M.; Zhang, Y.; Zhao, C.; Zhou, M.;
Zhou, Z.; Zhu, X. J.; Zucker, M. E.; Zuraw, S. E.; Zweizig, J.; Ligo
Scientific Collaboration; VIRGO Collaboration; Allison, J.; Bannister,
K.; Bell, M. E.; Chatterjee, S.; Chippendale, A. P.; Edwards, P. G.;
Harvey-Smith, L.; Heywood, Ian; Hotan, A.; Indermuehle, B.; Marvil, J.;
McConnell, D.; Murphy, T.; Popping, A.; Reynolds, J.; Sault, R. J.;
Voronkov, M. A.; Whiting, M. T.; Australian Square Kilometer Array
Pathfinder (Askap Collaboration); Castro-Tirado, A. J.; Cunniffe, R.;
Jelínek, M.; Tello, J. C.; Oates, S. R.; Hu, Y. -D.; Kubánek, P.;
Guziy, S.; Castellón, A.; García-Cerezo, A.; Muñoz, V. F.; Pérez
Del Pulgar, C.; Castillo-Carrión, S.; Castro Cerón, J. M.; Hudec,
R.; Caballero-García, M. D.; Páta, P.; Vitek, S.; Adame, J. A.;
Konig, S.; Rendón, F.; Mateo Sanguino, T. De J.; Fernández-Muñoz,
R.; Yock, P. C.; Rattenbury, N.; Allen, W. H.; Querel, R.; Jeong,
S.; Park, I. H.; Bai, J.; Cui, Ch.; Fan, Y.; Wang, Ch.; Hiriart,
D.; Lee, W. H.; Claret, A.; Sánchez-Ramírez, R.; Pandey, S. B.;
Mediavilla, T.; Sabau-Graziati, L.; Bootes Collaboration; Abbott,
T. M. C.; Abdalla, F. B.; Allam, S.; Annis, J.; Armstrong, R.;
Benoit-Lévy, A.; Berger, E.; Bernstein, R. A.; Bertin, E.; Brout, D.;
Buckley-Geer, E.; Burke, D. L.; Capozzi, D.; Carretero, J.; Castander,
F. J.; Chornock, R.; Cowperthwaite, P. S.; Crocce, M.; Cunha, C. E.;
D'Andrea, C. B.; da Costa, L. N.; Desai, S.; Diehl, H. T.; Dietrich,
J. P.; Doctor, Z.; Drlica-Wagner, A.; Drout, M. R.; Eifler, T. F.;
Estrada, J.; Evrard, A. E.; Fernandez, E.; Finley, D. A.; Flaugher,
B.; Foley, R. J.; Fong, W. -F.; Fosalba, P.; Fox, D. B.; Frieman, J.;
Fryer, C. L.; Gaztanaga, E.; Gerdes, D. W.; Goldstein, D. A.; Gruen,
D.; Gruendl, R. A.; Gutierrez, G.; Herner, K.; Honscheid, K.; James,
D. J.; Johnson, M. D.; Johnson, M. W. G.; Karliner, I.; Kasen, D.;
Kent, S.; Kessler, R.; Kim, A. G.; Kind, M. C.; Kuehn, K.; Kuropatkin,
N.; Lahav, O.; Li, T. S.; Lima, M.; Lin, H.; Maia, M. A. G.; Margutti,
R.; Marriner, J.; Martini, P.; Matheson, T.; Melchior, P.; Metzger,
B. D.; Miller, C. J.; Miquel, R.; Neilsen, E.; Nichol, R. C.; Nord,
B.; Nugent, P.; Ogando, R.; Petravick, D.; Plazas, A. A.; Quataert,
E.; Roe, N.; Romer, A. K.; Roodman, A.; Rosell, A. C.; Rykoff, E. S.;
Sako, M.; Sanchez, E.; Scarpine, V.; Schindler, R.; Schubnell, M.;
Scolnic, D.; Sevilla-Noarbe, I.; Sheldon, E.; Smith, N.; Smith, R. C.;
Soares-Santos, M.; Sobreira, F.; Stebbins, A.; Suchyta, E.; Swanson,
M. E. C.; Tarle, G.; Thaler, J.; Thomas, D.; Thomas, R. C.; Tucker,
D. L.; Vikram, V.; Walker, A. R.; Wechsler, R. H.; Wester, W.; Yanny,
B.; Zhang, Y.; Zuntz, J.; Dark Energy Survey Collaboration; Dark Energy
Camera Gw-Em Collaboration; Connaughton, V.; Burns, E.; Goldstein, A.;
Briggs, M. S.; Zhang, B. -B.; Hui, C. M.; Jenke, P.; Wilson-Hodge,
C. A.; Bhat, P. N.; Bissaldi, E.; Cleveland, W.; Fitzpatrick, G.;
Giles, M. M.; Gibby, M. H.; Greiner, J.; von Kienlin, A.; Kippen,
R. M.; McBreen, S.; Mailyan, B.; Meegan, C. A.; Paciesas, W. S.;
Preece, R. D.; Roberts, O.; Sparke, L.; Stanbro, M.; Toelge, K.; Veres,
P.; Yu, H. -F.; Blackburn, L.; Fermi Gbm Collaboration; Ackermann,
M.; Ajello, M.; Albert, A.; Anderson, B.; Atwood, W. B.; Axelsson,
M.; Baldini, L.; Barbiellini, G.; Bastieri, D.; Bellazzini, R.;
Bissaldi, E.; Blandford, R. D.; Bloom, E. D.; Bonino, R.; Bottacini,
E.; Brandt, T. J.; Bruel, P.; Buson, S.; Caliandro, G. A.; Cameron,
R. A.; Caragiulo, M.; Caraveo, P. A.; Cavazzuti, E.; Charles, E.;
Chekhtman, A.; Chiang, J.; Chiaro, G.; Ciprini, S.; Cohen-Tanugi,
J.; Cominsky, L. R.; Costanza, F.; Cuoco, A.; D'Ammando, F.; de
Palma, F.; Desiante, R.; Digel, S. W.; di Lalla, N.; di Mauro, M.;
di Venere, L.; Domínguez, A.; Drell, P. S.; Dubois, R.; Favuzzi, C.;
Ferrara, E. C.; Franckowiak, A.; Fukazawa, Y.; Funk, S.; Fusco, P.;
Gargano, F.; Gasparrini, D.; Giglietto, N.; Giommi, P.; Giordano, F.;
Giroletti, M.; Glanzman, T.; Godfrey, G.; Gomez-Vargas, G. A.; Green,
D.; Grenier, I. A.; Grove, J. E.; Guiriec, S.; Hadasch, D.; Harding,
A. K.; Hays, E.; Hewitt, J. W.; Hill, A. B.; Horan, D.; Jogler, T.;
Jóhannesson, G.; Johnson, A. S.; Kensei, S.; Kocevski, D.; Kuss,
M.; La Mura, G.; Larsson, S.; Latronico, L.; Li, J.; Li, L.; Longo,
F.; Loparco, F.; Lovellette, M. N.; Lubrano, P.; Magill, J.; Maldera,
S.; Manfreda, A.; Marelli, M.; Mayer, M.; Mazziotta, M. N.; McEnery,
J. E.; Meyer, M.; Michelson, P. F.; Mirabal, N.; Mizuno, T.; Moiseev,
A. A.; Monzani, M. E.; Moretti, E.; Morselli, A.; Moskalenko, I. V.;
Negro, M.; Nuss, E.; Ohsugi, T.; Omodei, N.; Orienti, M.; Orlando,
E.; Ormes, J. F.; Paneque, D.; Perkins, J. S.; Pesce-Rollins, M.;
Piron, F.; Pivato, G.; Porter, T. A.; Racusin, J. L.; Rainò, S.;
Rando, R.; Razzaque, S.; Reimer, A.; Reimer, O.; Salvetti, D.; Saz
Parkinson, P. M.; Sgrò, C.; Simone, D.; Siskind, E. J.; Spada, F.;
Spandre, G.; Spinelli, P.; Suson, D. J.; Tajima, H.; Thayer, J. B.;
Thompson, D. J.; Tibaldo, L.; Torres, D. F.; Troja, E.; Uchiyama,
Y.; Venters, T. M.; Vianello, G.; Wood, K. S.; Wood, M.; Zhu, S.;
Zimmer, S.; Fermi Lat Collaboration; Brocato, E.; Cappellaro, E.;
Covino, S.; Grado, A.; Nicastro, L.; Palazzi, E.; Pian, E.; Amati, L.;
Antonelli, L. A.; Capaccioli, M.; D'Avanzo, P.; D'Elia, V.; Getman,
F.; Giuffrida, G.; Iannicola, G.; Limatola, L.; Lisi, M.; Marinoni,
S.; Marrese, P.; Melandri, A.; Piranomonte, S.; Possenti, A.; Pulone,
L.; Rossi, A.; Stamerra, A.; Stella, L.; Testa, V.; Tomasella, L.;
Yang, S.; Gravitational Wave Inaf Team (Grawita); Bazzano, A.; Bozzo,
E.; Brandt, S.; Courvoisier, T. J. -L.; Ferrigno, C.; Hanlon, L.;
Kuulkers, E.; Laurent, P.; Mereghetti, S.; Roques, J. P.; Savchenko,
V.; Ubertini, P.; INTEGRAL Collaboration; Kasliwal, M. M.; Singer,
L. P.; Cao, Y.; Duggan, G.; Kulkarni, S. R.; Bhalerao, V.; Miller,
A. A.; Barlow, T.; Bellm, E.; Manulis, I.; Rana, J.; Laher, R.; Masci,
F.; Surace, J.; Rebbapragada, U.; Cook, D.; van Sistine, A.; Sesar,
B.; Perley, D.; Ferreti, R.; Prince, T.; Kendrick, R.; Horesh, A.;
Intermediate Palomar Transient Factory (Iptf Collaboration); Hurley,
K.; Golenetskii, S. V.; Aptekar, R. L.; Frederiks, D. D.; Svinkin,
D. S.; Rau, A.; von Kienlin, A.; Zhang, X.; Smith, D. M.; Cline,
T.; Krimm, H.; Network, Interplanetary; Abe, F.; Doi, M.; Fujisawa,
K.; Kawabata, K. S.; Morokuma, T.; Motohara, K.; Tanaka, M.; Ohta,
K.; Yanagisawa, K.; Yoshida, M.; J-Gem Collaboration; Baltay, C.;
Rabinowitz, D.; Ellman, N.; Rostami, S.; La Silla-Quest Survey;
Bersier, D. F.; Bode, M. F.; Collins, C. A.; Copperwheat, C. M.;
Darnley, M. J.; Galloway, D. K.; Gomboc, A.; Kobayashi, S.; Mazzali,
P.; Mundell, C. G.; Piascik, A. S.; Pollacco, Don; Steele, I. A.;
Ulaczyk, K.; Liverpool Telescope Collaboration; Broderick, J. W.;
Fender, R. P.; Jonker, P. G.; Rowlinson, A.; Stappers, B. W.;
Wijers, R. A. M. J.; Low Frequency Array (Lofar Collaboration);
Lipunov, V.; Gorbovskoy, E.; Tyurina, N.; Kornilov, V.; Balanutsa, P.;
Kuznetsov, A.; Buckley, D.; Rebolo, R.; Serra-Ricart, M.; Israelian,
G.; Budnev, N. M.; Gress, O.; Ivanov, K.; Poleshuk, V.; Tlatov, A.;
Yurkov, V.; Master Collaboration; Kawai, N.; Serino, M.; Negoro,
H.; Nakahira, S.; Mihara, T.; Tomida, H.; Ueno, S.; Tsunemi, H.;
Matsuoka, M.; Maxi Collaboration; Croft, S.; Feng, L.; Franzen,
T. M. O.; Gaensler, B. M.; Johnston-Hollitt, M.; Kaplan, D. L.;
Morales, M. F.; Tingay, S. J.; Wayth, R. B.; Williams, A.; Murchison
Wide-Field Array (Mwa Collaboration); Smartt, S. J.; Chambers, K. C.;
Smith, K. W.; Huber, M. E.; Young, D. R.; Wright, D. E.; Schultz, A.;
Denneau, L.; Flewelling, H.; Magnier, E. A.; Primak, N.; Rest, A.;
Sherstyuk, A.; Stalder, B.; Stubbs, C. W.; Tonry, J.; Waters, C.;
Willman, M.; Pan-Starrs Collaboration; Olivares E., F.; Campbell,
H.; Kotak, R.; Sollerman, J.; Smith, M.; Dennefeld, M.; Anderson,
J. P.; Botticella, M. T.; Chen, T. -W.; Della Valle, M.; Elias-Rosa,
N.; Fraser, M.; Inserra, C.; Kankare, E.; Kupfer, T.; Harmanen,
J.; Galbany, L.; Le Guillou, L.; Lyman, J. D.; Maguire, K.; Mitra,
A.; Nicholl, M.; Razza, A.; Terreran, G.; Valenti, S.; Gal-Yam, A.;
Pessto Collaboration; Ćwiek, A.; Ćwiok, M.; Mankiewicz, L.; Opiela,
R.; Zaremba, M.; Żarnecki, A. F.; Pi Of Sky Collaboration; Onken,
C. A.; Scalzo, R. A.; Schmidt, B. P.; Wolf, C.; Yuan, F.; Skymapper
Collaboration; Evans, P. A.; Kennea, J. A.; Burrows, D. N.; Campana,
S.; Cenko, S. B.; Giommi, P.; Marshall, F. E.; Nousek, J.; O'Brien,
P.; Osborne, J. P.; Palmer, D.; Perri, M.; Siegel, M.; Tagliaferri,
G.; Swift Collaboration; Klotz, A.; Turpin, D.; Laugier, R.; Tarot,
Zadko, Algerian National Observatory C2PU Collaboration; Beroiz, M.;
Peñuela, T.; Macri, L. M.; Oelkers, R. J.; Lambas, D. G.; Vrech,
R.; Cabral, J.; Colazo, C.; Dominguez, M.; Sanchez, B.; Gurovich, S.;
Lares, M.; Marshall, J. L.; Depoy, D. L.; Padilla, N.; Pereyra, N. A.;
Benacquista, M.; Toros Collaboration; Tanvir, N. R.; Wiersema, K.;
Levan, A. J.; Steeghs, D.; Hjorth, J.; Fynbo, J. P. U.; Malesani, D.;
Milvang-Jensen, B.; Watson, D.; Irwin, M.; Fernandez, C. G.; McMahon,
R. G.; Banerji, M.; Gonzalez-Solares, E.; Schulze, S.; de Ugarte
Postigo, A.; Thoene, C. C.; Cano, Z.; Rosswog, S.; Vista Collaboration
Bibcode: 2016ApJ...826L..13A
Altcode: 2016arXiv160208492A
A gravitational-wave (GW) transient was identified in data recorded
by the Advanced Laser Interferometer Gravitational-wave Observatory
(LIGO) detectors on 2015 September 14. The event, initially designated
G184098 and later given the name GW150914, is described in detail
elsewhere. By prior arrangement, preliminary estimates of the time,
significance, and sky location of the event were shared with 63 teams of
observers covering radio, optical, near-infrared, X-ray, and gamma-ray
wavelengths with ground- and space-based facilities. In this Letter we
describe the low-latency analysis of the GW data and present the sky
localization of the first observed compact binary merger. We summarize
the follow-up observations reported by 25 teams via private Gamma-ray
Coordinates Network circulars, giving an overview of the participating
facilities, the GW sky localization coverage, the timeline, and depth
of the observations. As this event turned out to be a binary black hole
merger, there is little expectation of a detectable electromagnetic
(EM) signature. Nevertheless, this first broadband campaign to search
for a counterpart of an Advanced LIGO source represents a milestone and
highlights the broad capabilities of the transient astronomy community
and the observing strategies that have been developed to pursue neutron
star binary merger events. Detailed investigations of the EM data and
results of the EM follow-up campaign are being disseminated in papers
by the individual teams.
Title: Transient Classification Report for 2016-02-19
Authors: Zhang, J.; Fan, Y.; Wang, X.
Bibcode: 2016TNSCR.136....1Z
Altcode:
No abstract at ADS
Title: Towards a Data-Optimized Coronal Magnetic Field Model (DOC-FM):
Synthetic Test Beds and Multiwavelength Forward Modeling
Authors: Gibson, S. E.; Dalmasse, K.; Fan, Y.; Fineschi, S.; MacKay,
D.; Rempel, M.; White, S. M.
Bibcode: 2015AGUFMSH54B..04G
Altcode:
Understanding the physical state of the solar corona is key to
deciphering the origins of space weather as well as to realistically
representing the environment to be navigated by missions such as
Solar Orbiter and Solar Probe Plus. However, inverting solar coronal
observations to reconstruct this physical state -- and in particular
the three-dimensional coronal magnetic field - is complicated by
limited lines of sight and by projection effects. On the other hand,
the sensitivity of multiwavelength observations to different physical
mechanisms implies a potential for simultaneous probing of different
parts of the coronal plasma. In order to study this complementarity, and
to ultimately establish an optimal set of observations for constraining
the three-dimensional coronal magnetic field, we are developing a suite
of representative simulations to act as diagnostic test beds. We will
present three such test beds: a coronal active region, a quiescent
prominence, and a global corona. Each fully define the physical state
of density, temperature, and vector magnetic field in three dimensions
throughout the simulation domain. From these test beds, and using the
FORWARD SolarSoft IDL codes, we will create a broad range of synthetic
data. Radio observables will include intensity and circular polarization
(including gyroresonance effects) and Faraday rotation for a range of
frequencies. Infrared and visible forbidden line diagnostics of Zeeman
and saturated Hanle effects will yield full Stokes vector (I, Q, U,
V) synthetic data, and UV permitted line Hanle diagnostics will yield
intensity and linear polarization. In addition, we will synthesize
UV and SXR imager data, UV/EUV spectrometric data, and white light
brightness and polarized brightness. All of these synthetic data,
along with the "ground truth" physical state of the simulations from
which they are derived, will be made available to the community for
the purpose of testing coronal inversion techniques.
Title: On the Observation and Simulation of Solar Coronal Twin Jets
Authors: Liu, J.; Fang, F.; Wang, Y.; Mcintosh, S. W.; Fan, Y.;
Zhang, Q.
Bibcode: 2015AGUFMSH31B2405L
Altcode:
We present the first observation, analysis and modeling on solar coronal
twin jets, which occurred after a preceding jet. Detailed analysis
on the kinetics of the preceding jet reveals its blowout-jet nature,
which resembles the study by Liu et al. 2014. However the erupting
process and kinetics of the twin jets appear to be different from
the preceding one. To address the triggering mechanism of the twins,
we continue the 3D MHD numerical simulation work in Fang et al. 2014
after the eruption of a blowout jet. Numerical simulation shows that
the resulting sigmoidal magnetic fields after the blowout jet keep
reconnecting with the ambient fields, producing the observed twin
jets. Combining our observation and simulation, we suggest that with
the continuous energy transport from the subsurface convection zone into
the corona, solar coronal twin jets could be generated by reconnection
between a sigmoidal magnetic structure and the open ambient fields.
Title: Towards a Data-Optimized Coronal Magnetic Field Model (DOC-FM):
Simulating Flux Ropes with the Flux Rope Insertion Method
Authors: Dalmasse, K.; DeLuca, E. E.; Savcheva, A. S.; Gibson, S. E.;
Fan, Y.
Bibcode: 2015AGUFMSH51B2444D
Altcode:
Knowledge of the 3D magnetic filed structure at the time of major solar
eruptions is vital or understanding of the space weather effects of
these eruptions. Multiple data-constrained techniques that reconstruct
the 3D coronal field based on photospheric magnetograms have been
used to achieve this goal. In particular, we have used the flux rope
insertion method to obtain the coronal magnetic field of multiple
regions containing flux ropes or sheared arcades based on line-of-sight
magnetograms and X-ray and EUV observations of coronal loops. For the
purpose of developing statistical measures of the goodness of fit of
these models to the observations, here we present our modeling of flux
ropes based on synthetic magnetograms obtained from Fan & Gibson
emerging flux rope simulation. The goal is to reproduce the flux rope
structure from a given time step of the MHD simulations based only
on the photospheric magnetogram and synthetic forward modeled coronal
emission obtained from the same step of the MHD simulation. For this
purpose we create a large grid of models with the flux rope insertion
method with different combinations of axial and poloidal flux, which
give us different morphology of the flux rope. Then we compare the
synthetic coronal emission with the shape of the current distribution
and field lines from the models to come up with a best fit. This fit
is then tested using the statistical methods developed by our team.
Title: Towards a Data-Optimized Coronal Magnetic Field Model (DOC-FM):
Statistical Method for Diagnosing the Coronal Magnetic Field
Authors: Dalmasse, K.; Nychka, D. W.; Gibson, S. E.; Fan, Y.
Bibcode: 2015AGUFMSH21B2395D
Altcode:
Solar coronal mass ejections (CMEs) and solar flares are the
main drivers of space weather. Their potential impact on Earth is
determined by the morphology and orientation of the magnetic structure
associated with these events and its evolution as it propagates into the
interplanetary magnetic field. Knowing the 3D coronal magnetic field
prior to the trigger of a CME is therefore one of the key features
for predicting their geomagnetic effect. Since the magnetic field is
essentially measured at the photosphere, one must rely on reconstruction
models to obtain the 3D magnetic field in the corona. Hence, obtaining
an accurate model of the real 3D coronal magnetic field is one of
the cornerstones for precise Space Weather Forecasting. In this work,
we propose a new method for data-constrained reconstruction of the 3D
coronal magnetic field. Model-data fitting is achieved by optimizing
a user-specified metric, M, quantifying the difference between a
dataset (including e.g. polarization, extreme-ultraviolet emission,
X-ray emission) and its synthetic analogue. The synthetic data is
produced by forward calculations applied to a 3D magnetic model that
depends upon a finite set of parameters. After introducing the method,
we present its validation on a synthetic test bed consisting of a
coronal magnetic flux rope assumed to depend on four parameters,
i.e. height in the corona, latitude, longitude, and tilt angle. A
specific value of each parameter is used to generate a ground truth
and the corresponding synthetic data. We show that, when M does not
possess any degenerate minimum, our method performs well and the
best-fit parameters provide a good approximation of the ground-truth
parameters. We then show how using additional observations can help
in removing any existing degeneracy. Finally, we discuss future plans
for validation and application of our method to solar observations.
Title: Early optical follow-up of the nearby active star DG CVn
during its 2014 superflare
Authors: Caballero-García, M. D.; Šimon, V.; Jelínek, M.;
Castro-Tirado, A. J.; Cwiek, A.; Claret, A.; Opiela, R.; Żarnecki,
A. F.; Gorosabel, J.; Oates, S. R.; Cunniffe, R.; Jeong, S.; Hudec, R.;
Sokolov, V. V.; Makarov, D. I.; Tello, J. C.; Lara-Gil, O.; Kubánek,
P.; Guziy, S.; Bai, J.; Fan, Y.; Wang, C.; Park, I. H.
Bibcode: 2015MNRAS.452.4195C
Altcode: 2015arXiv150703143C
DG Canum Venaticorum (DG CVn) is a binary system in which one of the
components is an M-type dwarf ultrafast rotator, only three of which are
known in the solar neighbourhood. Observations of DG CVn by the Swift
satellite and several ground-based observatories during its superflare
event on 2014 allowed us to perform a complete hard X-ray-optical
follow-up of a superflare from the red-dwarf star. The observations
support the fact that the superflare can be explained by the presence of
(a) large active region(s) on the surface of the star. Such activity is
similar to the most extreme solar flaring events. This points towards
a plausible extrapolation between the behaviour from the most active
red-dwarf stars and the processes occurring in the Sun.
Title: AstroCloud, a Cyber-Infrastructure for Astronomy Research:
Cloud Computing Environments
Authors: Li, C.; Wang, J.; Cui, C.; He, B.; Fan, D.; Yang, Y.; Chen,
J.; Zhang, H.; Yu, C.; Xiao, J.; Wang, C.; Cao, Z.; Fan, Y.; Hong,
Z.; Li, S.; Mi, L.; Wan, W.; Wang, J.; Yin, S.
Bibcode: 2015ASPC..495..487L
Altcode: 2015adass..24..487L
AstroCloud is a cyber-Infrastructure for Astronomy Research initiated
by Chinese Virtual Observatory (China-VO) under funding support from
NDRC (National Development and Reform commission) and CAS (Chinese
Academy of Sciences). Based on CloudStack, an open source software,
we set up the cloud computing environment for AstroCloud Project. It
consists of five distributed nodes across the mainland of China. Users
can use and analysis data in this cloud computing environment. Based
on GlusterFS, we built a scalable cloud storage system. Each user has
a private space, which can be shared among different virtual machines
and desktop systems. With this environments, astronomer can access to
astronomical data collected by different telescopes and data centers
easily, and data producers can archive their datasets safely.
Title: AstroCloud, a Cyber-Infrastructure for Astronomy Research:
Data Access and Interoperability
Authors: Fan, D.; He, B.; Xiao, J.; Li, S.; Li, C.; Cui, C.; Yu,
C.; Hong, Z.; Yin, S.; Wang, C.; Cao, Z.; Fan, Y.; Mi, L.; Wan, W.;
Wang, J.
Bibcode: 2015ASPC..495..477F
Altcode: 2014arXiv1411.5072F; 2015adass..24..477F
Data access and interoperability module connects the observation
proposals, data, virtual machines and software. According to the
unique identifier of PI (principal investigator), an email address
or an internal ID, data can be collected by PI's proposals, or by the
search interfaces, e.g. conesearch. Files associated with the searched
results could be easily transported to cloud storages, including
the storage with virtual machines, or several commercial platforms
like Dropbox. Benefitted from the standards of IVOA (International
Observatories Alliance), VOTable formatted searching result could be
sent to kinds of VO software. Latter endeavor will try to integrate
more data and connect archives and some other astronomical resources.
Title: AstroCloud, a Cyber-Infrastructure for Astronomy Research:
Overview
Authors: Cui, C.; Yu, C.; Xiao, J.; He, B.; Li, C.; Fan, D.; Wang,
C.; Hong, Z.; Li, S.; Mi, L.; Wan, W.; Cao, Z.; Wang, J.; Yin, S.;
Fan, Y.; Wang, J.
Bibcode: 2015ASPC..495..469C
Altcode: 2015adass..24..469C
AstroCloud is a cyber-Infrastructure for Astronomy Research initiated by
Chinese Virtual Observatory (China-VO) under funding support from NDRC
(National Development and Reform commission) and CAS (Chinese Academy
of Sciences). Tasks such as proposal submission, proposal peer-review,
data archiving, data quality control, data release and open access,
Cloud based data processing and analyzing, will be all supported on
the platform. It will act as a full lifecycle management system for
astronomical data and telescopes. Achievements from international
Virtual Observatories and Cloud Computing are adopted heavily. In
this paper, backgrounds of the project, key features of the system,
and latest progresses are introduced.
Title: AstroCloud, a Cyber-Infrastructure for Astronomy Research:
Architecture
Authors: Xiao, J.; Yu, C.; Cui, C.; He, B.; Li, C.; Fan, D.; Hong,
Z.; Yin, S.; Wang, C.; Cao, Z.; Fan, Y.; Li, S.; Mi, L.; Wan, W.;
Wang, J.; Zhang, H.
Bibcode: 2015ASPC..495..473X
Altcode: 2014arXiv1411.5070X; 2015adass..24..473X
AstroCloud is a cyber-Infrastructure for Astronomy Research initiated
by Chinese Virtual Observatory (China-VO) under funding support from
NDRC (National Development and Reform commission) and CAS (Chinese
Academy of Sciences). The ultimate goal of this project is to provide a
comprehensive end-to-end astronomy research environment where several
independent systems seamlessly collaborate to support the full lifecycle
of the modern observational astronomy based on big data, from proposal
submission, to data archiving, data release, and to in-situ data
analysis and processing. In this paper, the architecture and key
designs of the AstroCloud platform are introduced, including data
access middleware, access control and security framework, extendible
proposal workflow, and system integration mechanism.
Title: PANGU: A High Resolution Gamma-Ray Space Telescope
Authors: Wu, X.; Chang, J.; Walter, R.; Su, M.; Ambrosi, G.; Böttcher,
M.; Chernyakova, M.; Fan, Y.; Farnier, C.; Gargano, F.; Grenier, I.;
Hajdas, W.; Mazziotta, M. N.; Morselli, A.; Pearce, M.; Pohl, M.;
von Ballmoos, P.; Zdziarski, A.; Pangu Collaboration
Bibcode: 2015ICRC...34..964W
Altcode: 2015PoS...236..964W
No abstract at ADS
Title: Effects of Radiative Diffusion on Thin Flux Tubes in Turbulent
Solar-like Convection
Authors: Weber, M. A.; Fan, Y.
Bibcode: 2015SoPh..290.1295W
Altcode: 2015arXiv150308034W; 2015SoPh..tmp...33W
We study the combined effects of convection and radiative
diffusion on the evolution of thin magnetic flux tubes in the solar
interior. Radiative diffusion is the primary supplier of heat to
convective motions in the lower convection zone, and it results in
a heat input per unit volume of magnetic flux tubes that has been
ignored by many previous thin flux tube studies. We use a thin flux tube
model subject to convection taken from a rotating spherical shell of
turbulent, solar-like convection as described by Weber, Fan, and Miesch
(Astrophys. J.741, 11, 2011; Solar Phys.287, 239, 2013), now taking
into account the influence of radiative heating on 1022 Mx
flux tubes, corresponding to flux tubes of large active regions. Our
simulations show that flux tubes of ≤ 60 kG that are subject to
solar-like convective flows do not anchor in the overshoot region,
but rather drift upward because of the increased buoyancy of the flux
tube earlier in its evolution, which results from including radiative
diffusion. Flux tubes of magnetic field strengths ranging from 15 kG
to 100 kG have rise times of ≤ 0.2 years and exhibit a Joy's Law
tilt-angle trend. Our results suggest that radiative heating is an
effective mechanism by which flux tubes can escape from the stably
stratified overshoot region. Moreover, flux tubes do not necessarily
need to be anchored in the overshoot region to produce emergence
properties similar to those of active regions on the Sun.
Title: PANGU (PAir-productioN Gamma-ray Unit): A High Resolution
Gamma-ray Space Telescope
Authors: Wu, X.; Chang, J.; Walter, R.; Su, M.; Ambrosi, G.; Böttcher,
M.; Chernyakova, M.; Fan, Y.; Farnier, C.; Gargano, F.; Grenier, I.;
Hajdas, W.; Mazziotta, M. N.; Morselli, A.; Pearce, M.; Pohl, M.;
von Ballmoos, P.; Zdziarski, A.; Pangu Collaboration
Bibcode: 2015mbhe.confE..69W
Altcode: 2015PoS...246E..69W
No abstract at ADS
Title: GRB 150423A: GMG observation limit.
Authors: Mao, J.; Fan, Y.; Bai, J. -M.
Bibcode: 2015GCN.17803....1M
Altcode: 2015GCN..17803...1M
No abstract at ADS
Title: Coronal Eruptions in Simulations of Magnetic Flux Emergence
from the Convection Zone
Authors: Fang, F.; Fan, Y.; Mcintosh, S. W.
Bibcode: 2014AGUFMSH44A..06F
Altcode:
Solar magnetic fields permeate various layers of the Sun from the
interior to the corona and interact with the local plasma. The physical
properties of the plasma vary drastically from the convection zone
to the corona, with a density drop of 14 orders of magnitude. The
interaction between the plasma and magnetic fields strongly distort
the field structure during the emergence. The emerged fields dominate
the dynamics in the corona and may drive magnetic eruptions, with
significant release of magnetic energy into thermal and kinetic energy
of the plasma. Here we present numerical simulations of flux emergence
into pre-existing fields in a coupled convection-zone-corona system,
and study the resulting eruption of the magnetic fields in the corona,
e.g. blowout jets. Analysis of the simulation results illustrates
how the mass and energy is transferred from the interior into outer
atmosphere during the eruptions. Comparison with modern observations
provides us a physical understanding of the observed coronal eruptions
in flux emerging regions.
Title: The dark nature of GRB 130528A and its host galaxy
Authors: Jeong, S.; Castro-Tirado, A. J.; Bremer, M.; Winters,
J. M.; Gorosabel, J.; Guziy, S.; Pandey, S. B.; Jelínek, M.;
Sánchez-Ramírez, R.; Sokolov, Ilya V.; Orekhova, N. V.; Moskvitin,
A. S.; Tello, J. C.; Cunniffe, R.; Lara-Gil, O.; Oates, S. R.;
Pérez-Ramírez, D.; Bai, J.; Fan, Y.; Wang, C.; Park, I. H.
Bibcode: 2014A&A...569A..93J
Altcode: 2014arXiv1404.0939J
Aims: We study the dark nature of GRB 130528A through
multi-wavelength observations and conclude that the main reason
for the optical darkness is local extinction inside of the host
galaxy.
Methods: Automatic observations were performed at the
Burst Optical Observer and Transient Exploring System (BOOTES)-4/MET
robotic telescope. We also triggered target of opportunity (ToO)
observations at Observatorio de Sierra Nevada (OSN), IRAM Plateau
de Bure Interferometer (PdBI) and Gran Telescopio Canarias (GTC
+ OSIRIS). The host galaxy photometric observations in optical
to near-infrared (nIR) wavelengths were achieved through large
ground-based aperture telescopes, such as 10.4 m Gran Telescopio
Canarias (GTC), 4.2 m William Herschel Telescope (WHT), 6 m Bolshoi
Teleskop Alt-azimutalnyi (BTA) telescope, and 2 m Liverpool Telescope
(LT). Based on these observations, spectral energy distributions (SED)
for the host galaxy and afterglow were constructed.
Results:
Thanks to millimetre (mm) observations at PdBI, we confirm the presence
of a mm source within the XRT error circle that faded over the course of
our observations and identify the host galaxy. However, we do not find
any credible optical source within early observations with BOOTES-4/MET
and 1.5 m OSN telescopes. Spectroscopic observation of this galaxy by
GTC showed a single faint emission line that likely corresponds to [OII]
3727 Å at a redshift of 1.250 ± 0.001, implying a star formation rate
(M⊙/yr) > 6.18 M⊙/yr without correcting
for dust extinction. The probable line-of-sight extinction towards GRB
130528A is revealed through analysis of the afterglow SED, resulting
in a value of A^GRBV≥ 0.9 at the rest frame; this is
comparable to extinction levels found among other dark GRBs. The SED
of the host galaxy is explained well (χ2/d.o.f. = 0.564)
by a luminous (MB = -21.16), low-extinction (AV =
0, rest frame), and aged (2.6 Gyr) stellar population. We can explain
this apparent contradiction in global and line-of-sight extinction if
the GRB birth place happened to lie in a local dense environment. In
light of having relatively small specific star formation rate ~5.3
M⊙/yr (L/L⋆)-1, this also could
explain the age of the old stellar population of host galaxy.
Title: Circular polarization in the optical afterglow of GRB 121024A
Authors: Wiersema, K.; Covino, S.; Toma, K.; van der Horst, A. J.;
Varela, K.; Min, M.; Greiner, J.; Starling, R. L. C.; Tanvir,
N. R.; Wijers, R. A. M. J.; Campana, S.; Curran, P. A.; Fan, Y.;
Fynbo, J. P. U.; Gorosabel, J.; Gomboc, A.; Götz, D.; Hjorth, J.;
Jin, Z. P.; Kobayashi, S.; Kouveliotou, C.; Mundell, C.; O'Brien,
P. T.; Pian, E.; Rowlinson, A.; Russell, D. M.; Salvaterra, R.; di
Serego Alighieri, S.; Tagliaferri, G.; Vergani, S. D.; Elliott, J.;
Fariña, C.; Hartoog, O. E.; Karjalainen, R.; Klose, S.; Knust, F.;
Levan, A. J.; Schady, P.; Sudilovsky, V.; Willingale, R.
Bibcode: 2014Natur.509..201W
Altcode: 2014arXiv1410.0489W
Gamma-ray bursts (GRBs) are most probably powered by collimated
relativistic outflows (jets) from accreting black holes at cosmological
distances. Bright afterglows are produced when the outflow collides
with the ambient medium. Afterglow polarization directly probes the
magnetic properties of the jet when measured minutes after the burst,
and it probes the geometric properties of the jet and the ambient medium
when measured hours to days after the burst. High values of optical
polarization detected minutes after the burst of GRB 120308A indicate
the presence of large-scale ordered magnetic fields originating from the
central engine (the power source of the GRB). Theoretical models predict
low degrees of linear polarization and no circular polarization at late
times, when the energy in the original ejecta is quickly transferred to
the ambient medium and propagates farther into the medium as a blast
wave. Here we report the detection of circularly polarized light in
the afterglow of GRB 121024A, measured 0.15 days after the burst. We
show that the circular polarization is intrinsic to the afterglow
and unlikely to be produced by dust scattering or plasma propagation
effects. A possible explanation is to invoke anisotropic (rather than
the commonly assumed isotropic) electron pitch-angle distributions,
and we suggest that new models are required to produce the complex
microphysics of realistic shocks in relativistic jets.
Title: GRB 141109B: BOOTES-4 and TERSKOL optical upper limit.
Authors: Sokolov, I. V.; Moskvitin, A.; Sokolov, V. V.; Guziy, S.;
Castro-Tirado, A. J.; Tello, J. C.; Fan, Y.; Zhao, X.; Bai, J.; Wang,
Ch.; Xin, Y.
Bibcode: 2014GCN.17047....1S
Altcode: 2014GCN..17047...1S
No abstract at ADS
Title: GRB 140102A: BOOTES-4 early optical observations.
Authors: Guziy, S.; Gorosabel, J.; Castro-Tirado, A. J.; Cunniffe,
R.; Jelinek, M.; Jeong, S.; Lara-Gil, O.; Sanchez-Ramirez, R.; Tello,
J. C.; Kubanek, P.; Pandey, S. B.; Fan, Y.; Zhao, X.; Bai, J.; Wang,
Ch.; Xin, Y.; Cui, Ch.
Bibcode: 2014GCN.15685....1G
Altcode: 2014GCN..15685...1G
No abstract at ADS
Title: Coronal Cavity Survey: Morphological Clues to Eruptive
Magnetic Topologies
Authors: Forland, B. C.; Gibson, S. E.; Dove, J. B.; Rachmeler, L. A.;
Fan, Y.
Bibcode: 2013SoPh..288..603F
Altcode:
We present a survey on coronal prominence cavities conducted using 19
months of data from the Atmospheric Imaging Assembly (AIA) instrument
aboard the Solar Dynamics Observatory (SDO) satellite. Coronal
cavities are elliptical regions of rarefied density lying above and
around prominences. They can be long-lived (weeks to months) but are
often observed to eventually erupt as part of a coronal mass ejection
(CME). We determine morphological properties of the cavities both
by qualitatively assessing their shape, and quantitatively fitting
them with ellipses. We demonstrate consistency between these two
approaches, and find that fitted ellipses are taller than they are wide
for almost all cavities studied, in agreement with an earlier analysis
of white-light cavities. We examine correlations between cavity shape,
aspect ratio, and propensity for eruption. We find that cavities with
a teardrop-shaped morphology are more likely to erupt, and we discuss
the implications of this morphology for magnetic topologies associated
with CME models. We provide the full details of the survey for broad
scientific use as supplemental material.
Title: Polarimetric Properties of Flux Ropes and Sheared Arcades in
Coronal Prominence Cavities
Authors: Rachmeler, L. A.; Gibson, S. E.; Dove, J. B.; DeVore, C. R.;
Fan, Y.
Bibcode: 2013SoPh..288..617R
Altcode: 2013arXiv1304.7594R
The coronal magnetic field is the primary driver of solar dynamic
events. Linear and circular polarization signals of certain infrared
coronal emission lines contain information about the magnetic field,
and to access this information either a forward or an inversion method
must be used. We study three coronal magnetic configurations that
are applicable to polar-crown filament cavities by doing forward
calculations to produce synthetic polarization data. We analyze
these forward data to determine the distinguishing characteristics of
each model. We conclude that it is possible to distinguish between
cylindrical flux ropes, spheromak flux ropes, and sheared arcades
using coronal polarization measurements. If one of these models is
found to be consistent with observational measurements, it will mean
positive identification of the magnetic morphology that surrounds
certain quiescent filaments, which will lead to a better understanding
of how they form and why they erupt.
Title: Comparing Simulations of Rising Flux Tubes Through the
Solar Convection Zone with Observations of Solar Active Regions:
Constraining the Dynamo Field Strength
Authors: Weber, M. A.; Fan, Y.; Miesch, M. S.
Bibcode: 2013SoPh..287..239W
Altcode: 2012arXiv1208.1292W; 2012SoPh..tmp..208W
We study how active-region-scale flux tubes rise buoyantly from the
base of the convection zone to near the solar surface by embedding
a thin flux tube model in a rotating spherical shell of solar-like
turbulent convection. These toroidal flux tubes that we simulate range
in magnetic field strength from 15 kG to 100 kG at initial latitudes
of 1∘ to 40∘ in both hemispheres. This
article expands upon Weber, Fan, and Miesch (Astrophys. J.741, 11,
2011) (Article 1) with the inclusion of tubes with magnetic flux
of 1020 Mx and 1021 Mx, and more simulations
of the previously investigated case of 1022 Mx, sampling
more convective flows than the previous article, greatly improving
statistics. Observed properties of active regions are compared to
properties of the simulated emerging flux tubes, including: the tilt
of active regions in accordance with Joy's Law as in Article 1, and
in addition the scatter of tilt angles about the Joy's Law trend, the
most commonly occurring tilt angle, the rotation rate of the emerging
loops with respect to the surrounding plasma, and the nature of the
magnetic field at the flux tube apex. We discuss how these diagnostic
properties constrain the initial field strength of the active-region
flux tubes at the bottom of the solar convection zone, and suggest
that flux tubes of initial magnetic field strengths of ≥ 40 kG are
good candidates for the progenitors of large (1021 Mx to
1022 Mx) solar active regions, which agrees with the results
from Article 1 for flux tubes of 1022 Mx. With the addition
of more magnetic flux values and more simulations, we find that for all
magnetic field strengths, the emerging tubes show a positive Joy's Law
trend, and that this trend does not show a statistically significant
dependence on the magnetic flux.
Title: The Active Longitude Phenomenon and its Possible Convective
Origin
Authors: Weber, Maria A.; Fan, Y.; Miesch, M. S.
Bibcode: 2013SPD....4420403W
Altcode:
Using a thin flux tube model in a rotating spherical shell of
turbulent, solar-like convection, we find that the distribution of
emerging flux tubes in our simulation is inhomogeneous in longitude,
with properties similar to those of active longitudes on the Sun and
other solar-like stars. The large-scale pattern of flux emergence our
simulations produce exhibit preferred longitudinal modes of low order,
drift with respect to a fixed reference system, and show alignment
at low latitudes within 15 degrees on either side of the equator. We
suggest that these active-longitude-like emergence patterns are the
result of columnar, rotationally aligned giant cells present in our
convection simulation at low latitudes. If giant convecting cells exist
in the bulk of the solar convection zone, this phenomenon, along with
differential rotation, could in part provide an explanation for the
existence and behavior of active longitudes.
Title: Formation of Magnetic Structures during Emergence of Untwisted
Flux Rope
Authors: Fang, Fang; Fan, Y.; Rempel, M.
Bibcode: 2013SPD....44..102F
Altcode:
Ideal MHD simulations have shown that the twist of the magnetic flux
rope before emergence plays an important role in the coherency of the
emerged magnetic structures. Recently, with more realistic simulations
with turbulent convection, it is found that magnetic structures can
form at the photosphere from emergence of uniform magnetic fields. The
discrepancy therefore leads to a controversial question that whether the
twist exists before the emergence or is formed afterwards by surface
flows. In light of this, we carry out simulations on the emergence of
untwisted flux rope from the convection zone into the corona, using
more realistic treatment of the thermodynamic processes in the solar
interior and the outer atmosphere. In our coupled simulations, we
study the interaction between the convective motion and the magnetic
fields and also the formation of coronal structures in comparison
with observations.
Title: GRBS Followed-up by the bootes network
Authors: Guziy, S.; Castro-Tirado, A.; Jelínek, M.; Gorosabel,
J.; Kubánek, P.; Cunniffe, R.; Lara-Gil, O.; Rabaza-Castillo, O.;
de Ugarte Postigo, A.; Sánchez-Ramírez, R.; Tello, J.; Pérez del
Pulgar, C.; Castillo-Carrión, S.; Castro Cerón, J.; Mateo Sanguino,
T. de J.; Hudec, R.; Vitek, S.; de la Morena Carretero, B.; Díaz
Andreu, J.; Fernández-Muñoz, R.; Pérez-Ramírez, D.; Yock, P.;
Allen, W.; Bond, I.; Kheyfets, I.; Christie, G.; Sabau-Graziati, L.;
Cui, C.; Fan, Y.; Park, I. H.
Bibcode: 2013EAS....61..251G
Altcode:
The Burst Observer and Optical Transient Exploring System (BOOTES),
is a global robotic observatory network, which started in 1998 with
Spanish leadership devoted to study optical emissions from gamma ray
bursts (GRBs) that occur in the Universe. We present shot history and
current status of BOOTES network. The Network philosophy, science and
some details of 117 GRBs followed-up are discussed.
Title: A Theory on the Possible Convective Origins of Active
Longitudes on Solar-like Stars
Authors: Weber, Maria A.; Fan, Y.; Miesch, M. S.
Bibcode: 2013AAS...22230403W
Altcode:
Using a thin flux tube model in a rotating spherical shell of turbulent,
solar- like convective flows, we find that the distribution of
emerging flux tubes in our simulation is inhomogeneous in longitude,
with properties similar to those of active longitudes on the Sun and
other solar-like stars. The large-scale pattern of flux emergence our
simulations produce exhibits preferred longitudinal modes of low order,
drift with respect to a fixed reference system, and alignment across the
Equator at low latitudes between ±15 degrees. We suggest that these
active-longitude- like emergence patterns are the result of columnar,
rotationally aligned giant cells present in our convection simulation
at low latitudes. If giant convecting cells exist in the bulk of
the solar convection zone, this phenomenon, along with differential
rotation, could in part provide an explanation for the behavior of
active longitudes.
Title: Approach to Integrate Global-Sun Models of Magnetic Flux
Emergence and Transport for Space Weather Studies
Authors: Mansour, Nagi Nicolas; Wray, A.; Mehrotra, P.; Henney, C.;
arge, N.; Manchester, C.; Godinez, H.; Koller, J.; Kosovichev, A.;
Scherrer, P.; Zhao, J.; Stein, R.; Duvall, T.; Fan, Y.
Bibcode: 2013enss.confE.125M
Altcode:
The Sun lies at the center of space weather and is the source of its
variability. The primary input to coronal and solar wind models is
the activity of the magnetic field in the solar photosphere. Recent
advancements in solar observations and numerical simulations provide
a basis for developing physics-based models for the dynamics of
the magnetic field from the deep convection zone of the Sun to the
corona with the goal of providing robust near real-time boundary
conditions at the base of space weather forecast models. The goal is
to develop new strategic capabilities that enable characterization
and prediction of the magnetic field structure and flow dynamics of
the Sun by assimilating data from helioseismology and magnetic field
observations into physics-based realistic magnetohydrodynamics (MHD)
simulations. The integration of first-principle modeling of solar
magnetism and flow dynamics with real-time observational data via
advanced data assimilation methods is a new, transformative step in
space weather research and prediction. This approach will substantially
enhance an existing model of magnetic flux distribution and transport
developed by the Air Force Research Lab. The development plan is to use
the Space Weather Modeling Framework (SWMF) to develop Coupled Models
for Emerging flux Simulations (CMES) that couples three existing models:
(1) an MHD formulation with the anelastic approximation to simulate
the deep convection zone (FSAM code), (2) an MHD formulation with
full compressible Navier-Stokes equations and a detailed description
of radiative transfer and thermodynamics to simulate near-surface
convection and the photosphere (Stagger code), and (3) an MHD
formulation with full, compressible Navier-Stokes equations and an
approximate description of radiative transfer and heating to simulate
the corona (Module in BATS-R-US). CMES will enable simulations of the
emergence of magnetic structures from the deep convection zone to the
corona. Finally, a plan will be summarized on the development of a
Flux Emergence Prediction Tool (FEPT) in which helioseismology-derived
data and vector magnetic maps are assimilated into CMES that couples
the dynamics of magnetic flux from the deep interior to the corona.
Title: GRB 130313A: simultaneous and follow-up optical observations
at BOOTES-3 and BOOTES-4.
Authors: Tello, J. C.; Guziy, S.; Lara-Gil, O.; Cunniffe, R.; Jelinek,
M.; Gorosabel, J.; Kubanek, P.; Cr, I. A.; Fan, Y.; Zhao, X.; Bai, J.;
Wang, C.; Xin, Y.; Cui, Ch.; Allen, W.; Yock, Ph.; Castro-Tirado, A. J.
Bibcode: 2013GCN.14299....1T
Altcode: 2013GCN..14299...1T
No abstract at ADS
Title: Solar Active Longitudes and North/South Flux Emergence
Asymmetries Resulting from Thin Flux Tube Simulations in a Solar-like
Convective Envelope
Authors: Weber, M. A.; Fan, Y.; Miesch, M. S.
Bibcode: 2012AGUFMSH41D2126W
Altcode:
Solar observations show that the emergence of active features
is distributed inhomogeneously in longitude according to sunspot
activity, solar x-ray flares, and coronal streamers. In addition,
an asymmetry exists between active region associated phenomena in the
Northern and Southern hemispheres. Using a thin flux tube model in a
rotating spherical shell of solar-like convective flows, we find that
these simulated flux tubes tend to emerge asymmetrically in number
in the Northern and Southern hemispheres, and emerge at preferred
longitudes. The active longitudes our simulations produce often span
across the equator between low latitudes of 15° to -15°, and persist
and propagate prograde for multiple solar rotation periods. We suggest
that the active longitudes in our simulation are the result of columnar,
rotationally aligned giant cells present in the convection simulation at
low latitudes. If giant convecting cells exist in the bulk of the solar
convection zone, this phenomenon could in part provide an explanation
for the North/South asymmetry of active region emergence as well as
active longitudes.
Title: Search for Gravitational Waves Associated with Gamma-Ray
Bursts during LIGO Science Run 6 and Virgo Science Runs 2 and 3
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.;
Abernathy, M.; Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R. X.;
Affeldt, C.; Agathos, M.; Agatsuma, K.; Ajith, P.; Allen, B.; Amador
Ceron, E.; Amariutei, D.; Anderson, S. B.; Anderson, W. G.; Arai,
K.; Arain, M. A.; Araya, M. C.; Aston, S. M.; Astone, P.; Atkinson,
D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker, P.;
Ballardin, G.; Ballmer, S.; Barayoga, J. C. B.; Barker, D.; Barone,
F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos,
I.; Bassiri, R.; Bastarrika, M.; Basti, A.; Batch, J.; Bauchrowitz,
J.; Bauer, Th. S.; Bebronne, M.; Beck, D.; Behnke, B.; Bejger, M.;
Beker, M. G.; Bell, A. S.; Belopolski, I.; Benacquista, M.; Berliner,
J. M.; Bertolini, A.; Betzwieser, J.; Beveridge, N.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas, R.; Bitossi, M.;
Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.;
Bland, B.; Blom, M.; Bock, O.; Bodiya, T. P.; Bogan, C.; Bondarescu,
R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Boschi,
V.; Bose, S.; Bosi, L.; Bouhou, B.; Braccini, S.; Bradaschia, C.;
Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brau, J. E.; Breyer,
J.; Briant, T.; Bridges, D. O.; Brillet, A.; Brinkmann, M.; Brisson,
V.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Bulik, T.; Bulten,
H. J.; Buonanno, A.; Burguet-Castell, J.; Buskulic, D.; Buy, C.; Byer,
R. L.; Cadonati, L.; Calloni, E.; Camp, J. B.; Campsie, P.; Cannizzo,
J.; Cannon, K.; Canuel, B.; Cao, J.; Capano, C. D.; Carbognani,
F.; Carbone, L.; Caride, S.; Caudill, S.; Cavaglià, M.; Cavalier,
F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.; Chaibi, O.;
Chalermsongsak, T.; Charlton, P.; Chassande-Mottin, E.; Chelkowski,
S.; Chen, W.; Chen, X.; Chen, Y.; Chincarini, A.; Chiummo, A.; Cho,
H. S.; Chow, J.; Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.;
Chung, S.; Ciani, G.; Clara, F.; Clark, D. E.; Clark, J.; Clayton,
J. H.; Cleva, F.; Coccia, E.; Cohadon, P. -F.; Colacino, C. N.; Colas,
J.; Colla, A.; Colombini, M.; Conte, A.; Conte, R.; Cook, D.; Corbitt,
T. R.; Cordier, M.; Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin,
M.; Coulon, J. -P.; Couvares, P.; Coward, D. M.; Cowart, M.; Coyne,
D. C.; Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Cumming,
A.; Cunningham, L.; Cuoco, E.; Cutler, R. M.; Dahl, K.; Danilishin,
S. L.; Dannenberg, R.; D'Antonio, S.; Danzmann, K.; Dattilo, V.;
Daudert, B.; Daveloza, H.; Davier, M.; Daw, E. J.; Day, R.; Dayanga,
T.; De Rosa, R.; DeBra, D.; Debreczeni, G.; Degallaix, J.; Del Pozzo,
W.; del Prete, M.; Dent, T.; Dergachev, V.; DeRosa, R.; DeSalvo, R.;
Dhurandhar, S.; Di Fiore, L.; Di Lieto, A.; Di Palma, I.; Emilio,
M. Di Paolo; Di Virgilio, A.; Díaz, M.; Dietz, A.; Donovan, F.;
Dooley, K. L.; Drago, M.; Drever, R. W. P.; Driggers, J. C.; Du, Z.;
Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar, M.; Edwards, M.; Effler,
A.; Ehrens, P.; Endrőczi, G.; Engel, R.; Etzel, T.; Evans, K.; Evans,
M.; Evans, T.; Factourovich, M.; Fafone, V.; Fairhurst, S.; Fan, Y.;
Farr, B. F.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Feroz, F.; Ferrante,
I.; Fidecaro, F.; Finn, L. S.; Fiori, I.; Fisher, R. P.; Flaminio,
R.; Flanigan, M.; Foley, S.; Forsi, E.; Forte, L. A.; Fotopoulos, N.;
Fournier, J. -D.; Franc, J.; Franco, S.; Frasca, S.; Frasconi, F.;
Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.;
Friedrich, D.; Fritschel, P.; Frolov, V. V.; Fujimoto, M. -K.; Fulda,
P. J.; Fyffe, M.; Gair, J.; Galimberti, M.; Gammaitoni, L.; Garcia,
J.; Garufi, F.; Gáspár, M. E.; Gehrels, N.; Gemme, G.; Geng, R.;
Genin, E.; Gennai, A.; Gergely, L. Á.; Ghosh, S.; Giaime, J. A.;
Giampanis, S.; Giardina, K. D.; Giazotto, A.; Gil-Casanova, S.; Gill,
C.; Gleason, J.; Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky,
M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Graff, P. B.; Granata,
M.; Grant, A.; Gras, S.; Gray, C.; Gray, N.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald,
S.; Guidi, G. M.; Guido, C.; Gupta, R.; Gustafson, E. K.; Gustafson,
R.; Ha, T.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna,
C.; Hanson, J.; Hardt, A.; Harms, J.; Harry, G. M.; Harry, I. W.;
Harstad, E. D.; Hartman, M. T.; Haughian, K.; Hayama, K.; Hayau,
J. -F.; Heefner, J.; Heidmann, A.; Heintze, M. C.; Heitmann, H.;
Hello, P.; Hendry, M. A.; Heng, I. S.; Heptonstall, A. W.; Herrera,
V.; Hewitson, M.; Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Holtrop,
M.; Hong, T.; Hooper, S.; Hosken, D. J.; Hough, J.; Howell, E. J.;
Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.;
Inta, R.; Isogai, T.; Ivanov, A.; Izumi, K.; Jacobson, M.; James,
E.; Jang, Y. J.; Jaranowski, P.; Jesse, E.; Johnson, W. W.; Jones,
D. I.; Jones, G.; Jones, R.; Jonker, R. J. G.; Ju, L.; Kalmus, P.;
Kalogera, V.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Kasturi, R.;
Katsavounidis, E.; Katzman, W.; Kaufer, H.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kelley, D.; Kells, W.; Keppel, D. G.; Keresztes, Z.;
Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.; Kim, B. K.; Kim,
C.; Kim, H.; Kim, K.; Kim, N.; Kim, Y. M.; King, P. J.; Kinzel, D. L.;
Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Koranda,
S.; Korth, W. Z.; Kowalska, I.; Kozak, D.; Kranz, O.; Kringel, V.;
Krishnamurthy, S.; Krishnan, B.; Królak, A.; Kuehn, G.; Kumar, P.;
Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.; Lastzka, N.;
Lawrie, C.; Lazzarini, A.; Leaci, P.; Lee, C. H.; Lee, H. K.; Lee,
H. M.; Leong, J. R.; Leonor, I.; Leroy, N.; Letendre, N.; Li, J.; Li,
T. G. F.; Liguori, N.; Lindquist, P. E.; Liu, Y.; Liu, Z.; Lockerbie,
N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo,
G.; Lough, J.; Luan, J.; Lubinski, M.; Lück, H.; Lundgren, A. P.;
Macdonald, E.; Machenschalk, B.; MacInnis, M.; Macleod, D. M.;
Mageswaran, M.; Mailand, K.; Majorana, E.; Maksimovic, I.; Malvezzi,
V.; Man, N.; Mandel, I.; Mandic, V.; Mantovani, M.; Marandi, A.;
Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markosyan, A.;
Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.; Martin, R. M.;
Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.; Matone, L.;
Matzner, R. A.; Mavalvala, N.; Mazzolo, G.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIver, J.; McKechan, D. J. A.;
McWilliams, S.; Meadors, G. D.; Mehmet, M.; Meier, T.; Melatos,
A.; Melissinos, A. C.; Mendell, G.; Mercer, R. A.; Meshkov, S.;
Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.; Miller,
J.; Minenkov, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman,
R.; Miyakawa, O.; Moe, B.; Mohan, M.; Mohanty, S. D.; Mohapatra,
S. R. P.; Moraru, D.; Moreno, G.; Morgado, N.; Morgia, A.; Mori,
T.; Morriss, S. R.; Mosca, S.; Mossavi, K.; Mours, B.; Mow-Lowry,
C. M.; Mueller, C. L.; Mueller, G.; Mukherjee, S.; Mullavey, A.;
Müller-Ebhardt, H.; Munch, J.; Murphy, D.; Murray, P. G.; Mytidis, A.;
Nash, T.; Naticchioni, L.; Necula, V.; Nelson, J.; Neri, I.; Newton,
G.; Nguyen, T.; Nishizawa, A.; Nitz, A.; Nocera, F.; Nolting, D.;
Normandin, M. E.; Nuttall, L.; Ochsner, E.; O'Dell, J.; Oelker, E.;
Ogin, G. H.; Oh, J. J.; Oh, S. H.; O'Reilly, B.; O'Shaughnessy, R.;
Osthelder, C.; Ott, C. D.; Ottaway, D. J.; Ottens, R. S.; Overmier,
H.; Owen, B. J.; Page, A.; Palladino, L.; Palomba, C.; Pan, Y.;
Pankow, C.; Paoletti, F.; Paoletti, R.; Papa, M. A.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pedraza,
M.; Peiris, P.; Pekowsky, L.; Penn, S.; Perreca, A.; Persichetti,
G.; Phelps, M.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.;
Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Poggiani, R.; Pöld, J.; Postiglione, F.; Prato, M.;
Predoi, V.; Prestegard, T.; Price, L. R.; Prijatelj, M.; Principe, M.;
Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov, L. G.; Puncken, O.;
Punturo, M.; Puppo, P.; Quetschke, V.; Quitzow-James, R.; Raab, F. J.;
Rabeling, D. S.; Rácz, I.; Radkins, H.; Raffai, P.; Rakhmanov, M.;
Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Redwine, K.; Reed,
C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.;
Riesen, R.; Riles, K.; Robertson, N. A.; Robinet, F.; Robinson, C.;
Robinson, E. L.; Rocchi, A.; Roddy, S.; Rodriguez, C.; Rodruck, M.;
Rolland, L.; Rollins, J. G.; Romano, J. D.; Romano, R.; Romie, J. H.;
Rosińska, D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan,
K.; Sainathan, P.; Salemi, F.; Sammut, L.; Sandberg, V.; Sannibale,
V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.; Sassolas,
B.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.;
Schilling, R.; Schnabel, R.; Schofield, R. M. S.; Schreiber, E.;
Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.;
Seifert, F.; Sellers, D.; Sentenac, D.; Sergeev, A.; Shaddock, D. A.;
Shaltev, M.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.;
Siemens, X.; Sigg, D.; Singer, A.; Singer, L.; Sintes, A. M.; Skelton,
G. R.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.;
Smith, R. J. E.; Smith-Lefebvre, N. D.; Somiya, K.; Sorazu, B.; Soto,
J.; Speirits, F. C.; Sperandio, L.; Stefszky, M.; Stein, A. J.; Stein,
L. C.; Steinert, E.; Steinlechner, J.; Steinlechner, S.; Steplewski,
S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S. E.; Stroeer,
A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sung, M.;
Susmithan, S.; Sutton, P. J.; Swinkels, B.; Tacca, M.; Taffarello, L.;
Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor,
R.; ter Braack, A. P. M.; Thomas, P.; Thorne, K. A.; Thorne, K. S.;
Thrane, E.; Thüring, A.; Tokmakov, K. V.; Tomlinson, C.; Toncelli,
A.; Tonelli, M.; Torre, O.; Torres, C.; Torrie, C. I.; Tournefier,
E.; Tucker, E.; Travasso, F.; Traylor, G.; Tseng, K.; Ugolini, D.;
Vahlbruch, H.; Vajente, G.; van den Brand, J. F. J.; Van Den Broeck,
C.; van der Putten, S.; van Veggel, A. A.; Vass, S.; Vasuth, M.;
Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.; Veitch, J.;
Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.; Viceré, A.;
Villar, A. E.; Vinet, J. -Y.; Vitale, S.; Vocca, H.; Vorvick, C.;
Vyatchanin, S. P.; Wade, A.; Wade, L.; Wade, M.; Waldman, S. J.;
Wallace, L.; Wan, Y.; Wang, M.; Wang, X.; Wang, Z.; Wanner, A.;
Ward, R. L.; Was, M.; Weinert, M.; Weinstein, A. J.; Weiss, R.;
Wen, L.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan,
J. T.; Whitcomb, S. E.; White, D. J.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, L.; Williams, R.; Willke, B.; Winkelmann,
L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Wittel, H.; Woan, G.;
Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto, K.;
Yancey, C. C.; Yang, H.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.;
Yvert, M.; Zadrożny, A.; Zanolin, M.; Zendri, J. -P.; Zhang, F.;
Zhang, L.; Zhang, W.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.;
LIGO Scientific Collaboration; Virgo Collaboration; Briggs, M. S.;
Connaughton, V.; Hurley, K. C.; Jenke, P. A.; von Kienlin, A.; Rau,
A.; Zhang, X. -L.
Bibcode: 2012ApJ...760...12A
Altcode: 2012arXiv1205.2216T; 2012arXiv1205.2216B
We present the results of a search for gravitational waves associated
with 154 gamma-ray bursts (GRBs) that were detected by satellite-based
gamma-ray experiments in 2009-2010, during the sixth LIGO science run
and the second and third Virgo science runs. We perform two distinct
searches: a modeled search for coalescences of either two neutron stars
or a neutron star and black hole, and a search for generic, unmodeled
gravitational-wave bursts. We find no evidence for gravitational-wave
counterparts, either with any individual GRB in this sample or with
the population as a whole. For all GRBs we place lower bounds on
the distance to the progenitor, under the optimistic assumption of a
gravitational-wave emission energy of 10-2 M ⊙ c
2 at 150 Hz, with a median limit of 17 Mpc. For short-hard
GRBs we place exclusion distances on binary neutron star and
neutron-star-black-hole progenitors, using astrophysically motivated
priors on the source parameters, with median values of 16 Mpc and 28
Mpc, respectively. These distance limits, while significantly larger
than for a search that is not aided by GRB satellite observations,
are not large enough to expect a coincidence with a GRB. However,
projecting these exclusions to the sensitivities of Advanced LIGO and
Virgo, which should begin operation in 2015, we find that the detection
of gravitational waves associated with GRBs will become quite possible.
Title: Thermal Signatures of Tether-cutting Reconnections in
Pre-eruption Coronal Flux Ropes: Hot Central Voids in Coronal Cavities
Authors: Fan, Y.
Bibcode: 2012ApJ...758...60F
Altcode: 2012arXiv1205.1028F
Using a three-dimensional MHD simulation, we model the quasi-static
evolution and the onset of eruption of a coronal flux rope. The
simulation begins with a twisted flux rope emerging at the lower
boundary and pushing into a pre-existing coronal potential arcade
field. At a chosen time the emergence is stopped with the lower
boundary taken to be rigid. Then the coronal flux rope settles
into a quasi-static rise phase during which an underlying, central
sigmoid-shaped current layer forms along the so-called hyperbolic flux
tube (HFT), a generalization of the X-line configuration. Reconnections
in the dissipating current layer effectively add twisted flux to the
flux rope and thus allow it to rise quasi-statically, even though
the magnetic energy is decreasing as the system relaxes. We examine
the thermal features produced by the current layer formation and the
associated "tether-cutting" reconnections as a result of heating and
field aligned thermal conduction. It is found that a central hot,
low-density channel containing reconnected, twisted flux threading
under the flux rope axis forms on top of the central current layer. When
viewed in the line of sight roughly aligned with the hot channel (which
is roughly along the neutral line), the central current layer appears as
a high-density vertical column with upward extensions as a "U"-shaped
dense shell enclosing a central hot, low-density void. Such thermal
features have been observed within coronal prominence cavities. Our MHD
simulation suggests that they are the signatures of the development
of the HFT topology and the associated tether-cutting reconnections,
and that the central void grows and rises with the reconnections,
until the flux rope reaches the critical height for the onset of the
torus instability and dynamic eruption ensues.
Title: Erratum: Search for gravitational waves from binary black
hole inspiral, merger, and ringdown [Phys. Rev. D 83, 122005 (2011)]
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.;
Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.; Ajith, P.; Allen,
B.; Allen, G. S.; Amador Ceron, E.; Amin, R. S.; Anderson, S. B.;
Anderson, W. G.; Antonucci, F.; Arain, M. A.; Araya, M. C.; Aronsson,
M.; Aso, Y.; Aston, S. M.; Astone, P.; Atkinson, D.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.; Ballinger, T.;
Ballmer, S.; Barker, D.; Barnum, S.; Barone, F.; Barr, B.; Barriga,
P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri,
R.; Bastarrika, M.; Bauchrowitz, J.; Bauer, Th. S.; Behnke, B.; Beker,
M. G.; Belletoile, A.; Benacquista, M.; Bertolini, A.; Betzwieser,
J.; Beveridge, N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Birch, J.; Birindelli, S.; Biswas, R.; Bitossi, M.; Bizouard,
M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland,
B.; Blom, M.; Boccara, C.; Bock, O.; Bodiya, T. P.; Bondarescu, R.;
Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Boschi, V.;
Bose, S.; Bosi, L.; Bouhou, B.; Boyle, M.; Braccini, S.; Bradaschia,
C.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges,
D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks,
A. F.; Brown, D. A.; Budzyński, R.; Bulik, T.; Bulten, H. J.;
Buonanno, A.; Burguet–Castell, J.; Burmeister, O.; Buskulic, D.;
Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Cain, J.; Calloni,
E.; Camp, J. B.; Campagna, E.; Campsie, P.; Cannizzo, J.; Cannon, K.;
Canuel, B.; Cao, J.; Capano, C.; Carbognani, F.; Caride, S.; Caudill,
S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.;
Cesarini, E.; Chaibi, O.; Chalermsongsak, T.; Chalkley, E.; Charlton,
P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, Y.; Chincarini, A.;
Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.; Clark, D.; Clark,
J.; Clayton, J. H.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas,
J.; Colla, A.; Colombini, M.; Conte, R.; Cook, D.; Corbitt, T. R.;
Cornish, N.; Corsi, A.; Costa, C. A.; Coulon, J. -P.; Coward, D. M.;
Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.;
Culter, R. M.; Cumming, A.; Cunningham, L.; Cuoco, E.; Dahl, K.;
Danilishin, S. L.; Dannenberg, R.; D'Antonio, S.; Danzmann, K.; Das,
K.; Dattilo, V.; Daudert, B.; Davier, M.; Davies, G.; Davis, A.; Daw,
E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra, D.; Debreczeni, G.;
Degallaix, J.; del Prete, M.; Dent, T.; Dergachev, V.; DeRosa, R.;
DeSalvo, R.; Devanka, P.; Dhurandhar, S.; Di Fiore, L.; Di Lieto,
A.; Di Palma, I.; Di Paolo Emilio, M.; Di Virgilio, A.; Díaz, M.;
Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes, E. E.; Dorsher, S.;
Douglas, E. S. D.; Drago, M.; Drever, R. W. P.; Driggers, J. C.;
Dueck, J.; Dumas, J. -C.; Eberle, T.; Edgar, M.; Edwards, M.; Effler,
A.; Ehrens, P.; Ely, G.; Engel, R.; Etzel, T.; Evans, M.; Evans, T.;
Fafone, V.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Fazi, D.; Fehrmann,
H.; Feldbaum, D.; Ferrante, I.; Fidecaro, F.; Finn, L. S.; Fiori,
I.; Flaminio, R.; Flanigan, M.; Flasch, K.; Foley, S.; Forrest,
C.; Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.;
Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.;
Freise, A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.;
Frolov, V. V.; Fulda, P.; Fyffe, M.; Galimberti, M.; Gammaitoni, L.;
Garofoli, J. A.; Garufi, F.; Gáspár, M. E.; Gemme, G.; Genin, E.;
Gennai, A.; Gholami, I.; Ghosh, S.; Giaime, J. A.; Giampanis, S.;
Giardina, K. D.; Giazotto, A.; Gill, C.; Goetz, E.; Goggin, L. M.;
González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.;
Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald,
S.; Guidi, G. M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hall,
P.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Haughian, K.; Hayama, K.; Hayau, J. -F.; Hayler, T.; Heefner, J.;
Heitmann, H.; Hello, P.; Heng, I. S.; Heptonstall, A. W.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken,
D. J.; Hough, J.; Howell, E. J.; Hoyland, D.; Huet, D.; Hughey, B.;
Husa, S.; Huttner, S. H.; Huynh–Dinh, T.; Ingram, D. R.; Inta, R.;
Isogai, T.; Ivanov, A.; Jaranowski, P.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kanner, J. B.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.;
Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khazanov, E. A.; Kim, H.; King, P. J.; Kinzel, D. L.; Kissel,
J. S.; Klimenko, S.; Kondrashov, V.; Kopparapu, R.; Koranda, S.;
Kowalska, I.; Kozak, D.; Krause, T.; Kringel, V.; Krishnamurthy,
S.; Krishnan, B.; Królak, A.; Kuehn, G.; Kullman, J.; Kumar, R.;
Kwee, P.; Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lazzarini,
A.; Leaci, P.; Leong, J.; Leonor, I.; Leroy, N.; Letendre, N.; Li,
J.; Li, T. G. F.; Liguori, N.; Lin, H.; Lindquist, P. E.; Lockerbie,
N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo,
G.; Lu, P.; Luan, J.; Lubinski, M.; Lucianetti, A.; Lück, H.;
Lundgren, A. D.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Mak, C.; Maksimovic, I.; Man, N.; Mandel,
I.; Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.;
Meadors, G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.;
Miller, J.; Minenkov, Y.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Moe, B.; Mohan, M.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moraru, D.; Moreau, J.; Moreno, G.; Morgado,
N.; Morgia, A.; Morioka, T.; Mors, K.; Mosca, S.; Moscatelli, V.;
Mossavi, K.; Mours, B.; Mow–Lowry, C. M.; Mueller, G.; Mukherjee,
S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murray, P. G.;
Nash, T.; Nawrodt, R.; Nelson, J.; Neri, I.; Newton, G.; Nishizawa,
A.; Nocera, F.; Nolting, D.; Ochsner, E.; O'Dell, J.; Ogin, G. H.;
Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.;
Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page,
A.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow,
C.; Paoletti, F.; Papa, M. A.; Pardi, S.; Pareja, M.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pathak,
D.; Pedraza, M.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca,
A.; Persichetti, G.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.;
Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Poggiani, R.; Postiglione, F.; Prato, M.; Predoi,
V.; Price, L. R.; Prijatelj, M.; Principe, M.; Privitera, S.; Prix,
R.; Prodi, G. A.; Prokhorov, L.; Puncken, O.; Punturo, M.; Puppo,
P.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Rácz, I.; Radke,
T.; Radkins, H.; Raffai, P.; Rakhmanov, M.; Rankins, B.; Rapagnani,
P.; Raymond, V.; Re, V.; Reed, C. M.; Reed, T.; Regimbau, T.; Reid,
S.; Reitze, D. H.; Ricci, F.; Riesen, R.; Riles, K.; Roberts, P.;
Robertson, N. A.; Robinet, F.; Robinson, C.; Robinson, E. L.; Rocchi,
A.; Roddy, S.; Rolland, L.; Rollins, J.; Romano, J. D.; Romano, R.;
Romie, J. H.; Rosińska, D.; Röver, C.; Rowan, S.; Rüdiger, A.;
Ruggi, P.; Ryan, K.; Sakata, S.; Sakosky, M.; Salemi, F.; Sammut, L.;
Sancho de la Jordana, L.; Sandberg, V.; Sannibale, V.; Santamaría,
L.; Santostasi, G.; Saraf, S.; Sassolas, B.; Sathyaprakash, B. S.;
Sato, S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.; Schilling,
R.; Schnabel, R.; Schofield, R. M. S.; Schulz, B.; Schutz, B. F.;
Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Seifert, F.;
Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sergeev, A.; Shaddock,
D. A.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.;
Siemens, X.; Sigg, D.; Singer, A.; Sintes, A. M.; Skelton, G.;
Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Smith,
N. D.; Somiya, K.; Sorazu, B.; Speirits, F. C.; Sperandio, L.; Stein,
A. J.; Stein, L. C.; Steinlechner, S.; Steplewski, S.; Stochino, A.;
Stone, R.; Strain, K. A.; Strigin, S.; Stroeer, A. S.; Sturani, R.;
Stuver, A. L.; Summerscales, T. Z.; Sung, M.; Susmithan, S.; Sutton,
P. J.; Swinkels, B.; Szokoly, G. P.; Tacca, M.; Talukder, D.; Tanner,
D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.; Thomas, P.; Thorne,
K. A.; Thorne, K. S.; Thrane, E.; Thüring, A.; Titsler, C.; Tokmakov,
K. V.; Toncelli, A.; Tonelli, M.; Torre, O.; Torres, C.; Torrie,
C. I.; Tournefier, E.; Travasso, F.; Traylor, G.; Trias, M.; Tseng,
K.; Turner, L.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vaishnav,
B.; Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.; Van Den
Broeck, C.; van der Putten, S.; van der Sluys, M. V.; van Veggel,
A. A.; Vass, S.; Vasuth, M.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.;
Vedovato, G.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.;
Vetrano, F.; Viceré, A.; Villar, A. E.; Vinet, J. -Y.; Vocca, H.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Wanner,
A.; Ward, R. L.; Was, M.; Wei, P.; Weinert, M.; Weinstein, A. J.;
Weiss, R.; Wen, L.; Wen, S.; Wessels, P.; West, M.; Westphal, T.;
Wette, K.; Whelan, J. T.; Whitcomb, S. E.; White, D.; Whiting, B. F.;
Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Winkelmann,
L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.;
Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto, K.; Yeaton-Massey,
D.; Yoshida, S.; Yu, P.; Yvert, M.; Zanolin, M.; Zhang, L.; Zhang,
Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2012PhRvD..86f9903A
Altcode:
No abstract at ADS
Title: Implications for the Origin of GRB 051103 from LIGO
Observations
Authors: Abadie, J.; Abbott, B. P.; Abbott, T. D.; Abbott, R.;
Abernathy, M.; Adams, C.; Adhikari, R.; Affeldt, C.; Ajith, P.;
Allen, B.; Allen, G. S.; Amador Ceron, E.; Amariutei, D.; Amin, R. S.;
Anderson, S. B.; Anderson, W. G.; Arai, K.; Arain, M. A.; Araya, M. C.;
Aston, S. M.; Atkinson, D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.;
Babak, S.; Baker, P.; Ballmer, S.; Barker, D.; Barnum, S.; Barr, B.;
Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.; Bassiri, R.;
Bastarrika, M.; Bauchrowitz, J.; Behnke, B.; Bell, A. S.; Belopolski,
I.; Benacquista, M.; Bertolini, A.; Betzwieser, J.; Beveridge, N.;
Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas,
R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland,
B.; Bock, O.; Bodiya, T. P.; Bogan, C.; Bondarescu, R.; Bork, R.;
Born, M.; Bose, S.; Boyle, M.; Brady, P. R.; Braginsky, V. B.; Brau,
J. E.; Breyer, J.; Bridges, D. O.; Brinkmann, M.; Britzger, M.; Brooks,
A. F.; Brown, D. A.; Brummitt, A.; Buonanno, A.; Burguet-Castell, J.;
Burmeister, O.; Byer, R. L.; Cadonati, L.; Camp, J. B.; Campsie, P.;
Cannizzo, J.; Cannon, K.; Cao, J.; Capano, C.; Caride, S.; Caudill, S.;
Cavaglia, M.; Cepeda, C.; Chalermsongsak, T.; Chalkley, E.; Charlton,
P.; Chelkowski, S.; Chen, Y.; Christensen, N.; Chua, S. S. Y.; Chung,
S.; Chung, C. T. Y.; Clara, F.; Clark, D.; Clark, J.; Clayton, J. H.;
Conte, R.; Cook, D.; Corbitt, T. R. C.; Cornish, N.; Costa, C. A.;
Coughlin, M.; Coward, D. M.; Coyne, D. C.; Creighton, J. D. E.;
Creighton, T. D.; Cruise, A. M.; Cumming, A.; Cunningham, L.; Culter,
R. M.; Dahl, K.; Danilishin, S. L.; Dannenberg, R.; Danzmann, K.;
Das, K.; Daudert, B.; Daveloza, H.; Davies, G.; Daw, E. J.; Dayanga,
T.; DeBra, D.; Degallaix, J.; Dent, T.; Dergachev, V.; DeRosa, R.;
DeSalvo, R.; Dhurandhar, S.; Di Palma, I.; Díaz, M.; Donovan, F.;
Dooley, K. L.; Dorsher, S.; Douglas, E. S. D.; Drever, R. W. P.;
Driggers, J. C.; Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar, M.;
Edwards, M.; Effler, A.; Ehrens, P.; Engel, R.; Etzel, T.; Evans, M.;
Evans, T.; Factourovich, M.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Fazi,
D.; Fehrmann, H.; Feldbaum, D.; Finn, L. S.; Flanigan, M.; Foley, S.;
Forsi, E.; Fotopoulos, N.; Frede, M.; Frei, M.; Frei, Z.; Freise,
A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov,
V. V.; Fulda, P.; Fyffe, M.; Garcia, J.; Garofoli, J. A.; Gholami, I.;
Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Gill, C.;
Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler,
S.; Graef, C.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Grosso, R.; Grote, H.; Grunewald, S.; Guido, C.;
Gupta, R.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.;
Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.; Hanson, J.; Harms, J.;
Harry, G. M.; Harry, I. W.; Harstad, E. D.; Hartman, M. T.; Haughian,
K.; Hayama, K.; Heefner, J.; Hendry, M. A.; Heng, I. S.; Heptonstall,
A. W.; Herrera, V.; Hewitson, M.; Hild, S.; Hoak, D.; Hodge, K. A.;
Holt, K.; Hong, T.; Hooper, S.; Hosken, D. J.; Hough, J.; Howell,
E. J.; Hughey, B.; Husa, S.; Huttner, S. H.; Ingram, D. R.; Inta,
R.; Isogai, T.; Ivanov, A.; Johnson, W. W.; Jones, D. I.; Jones,
G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy, S.;
Kanner, J. B.; Katsavounidis, E.; Katzman, W.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kells, W.; Kelner, M.; Keppel, D. G.; Khalaidovski,
A.; Khalili, F. Y.; Khazanov, E. A.; Kim, N.; Kim, H.; King, P. J.;
Kinzel, D. L.; Kissel, J. S.; Klimenko, S.; Kondrashov, V.; Kopparapu,
R.; Koranda, S.; Korth, W. Z.; Kozak, D.; Kringel, V.; Krishnamurthy,
S.; Krishnan, B.; Kuehn, G.; Kumar, R.; Kwee, P.; Landry, M.; Lantz,
B.; Lastzka, N.; Lazzarini, A.; Leaci, P.; Leong, J.; Leonor, I.; Li,
J.; Lindquist, P. E.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu,
P.; Luan, J.; Lubinski, M.; Lück, H.; Lundgren, A. P.; Macdonald, E.;
Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Mandel,
I.; Mandic, V.; Marandi, A.; Márka, S.; Márka, Z.; Maros, E.; Martin,
I. W.; Martin, R. M.; Marx, J. N.; Mason, K.; Matichard, F.; Matone,
L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.;
McGuire, S. C.; McIntyre, G.; McIver, J.; McKechan, D. J. A.; Meadors,
G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.; Mendell,
G.; Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Miao, H.;
Miller, J.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman,
R.; Miyakawa, O.; Moe, B.; Moesta, P.; Mohanty, S. D.; Moraru, D.;
Moreno, G.; Mossavi, K.; Mow-Lowry, C. M.; Mueller, G.; Mukherjee,
S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murphy, D.; Murray,
P. G.; Nash, T.; Nawrodt, R.; Nelson, J.; Newton, G.; Nishizawa, A.;
Nolting, D.; Nuttall, L.; O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.;
O'Dell, J.; Ogin, G. H.; Oldenburg, R. G.; Osthelder, C.; Ott, C. D.;
Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page, A.;
Pan, Y.; Pankow, C.; Papa, M. A.; Patel, P.; Pedraza, M.; Pekowsky,
L.; Penn, S.; Peralta, C.; Perreca, A.; Phelps, M.; Pickenpack, M.;
Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Podkaminer,
J.; Pöld, J.; Postiglione, F.; Predoi, V.; Price, L. R.; Prijatelj,
M.; Principe, M.; Privitera, S.; Prix, R.; Prokhorov, L.; Puncken,
O.; Quetschke, V.; Raab, F. J.; Radkins, H.; Raffai, P.; Rakhmanov,
M.; Ramet, C. R.; Rankins, B.; Mohapatra, S. R. P.; Raymond, V.;
Redwine, K.; Reed, C. M.; Reed, T.; Reid, S.; Reitze, D. H.; Riesen,
R.; Riles, K.; Roberts, P.; Robertson, N. A.; Robinson, C.; Robinson,
E. L.; Roddy, S.; Rollins, J.; Romano, J. D.; Romie, J. H.; Röver, C.;
Rowan, S.; Rüdiger, A.; Ryan, K.; Sakata, S.; Sakosky, M.; Salemi,
F.; Salit, M.; Sammut, L.; Sancho de la Jordana, L.; Sandberg, V.;
Sannibale, V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.;
Saraf, S.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R.;
Schilling, R.; Schlamminger, S.; Schnabel, R.; Schofield, R. M. S.;
Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.;
Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev,
A.; Shaddock, D. A.; Shaltev, M.; Shapiro, B.; Shawhan, P.; Shihan
Weerathunga, T.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg,
D.; Singer, A.; Singer, L.; Sintes, A. M.; Skelton, G.; Slagmolen,
B. J. J.; Slutsky, J.; Smith, R.; Smith, J. R.; Smith, M. R.; Smith,
N. D.; Somiya, K.; Sorazu, B.; Soto, J.; Speirits, F. C.; Stein, A. J.;
Steinlechner, J.; Steinlechner, S.; Steplewski, S.; Stefszky, M.;
Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S.; Stroeer, A. S.;
Stuver, A. L.; Summerscales, T. Z.; Sung, M.; Susmithan, S.; Sutton,
P. J.; Szokoly, G. P.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.;
Taylor, J. R.; Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.;
Thrane, E.; Thüring, A.; Tokmakov, K. V.; Torres, C.; Torrie, C. I.;
Traylor, G.; Trias, M.; Tseng, K.; Ugolini, D.; Urbanek, K.; Vahlbruch,
H.; Vaishnav, B.; Vallisneri, M.; Van Den Broeck, C.; van der Sluys,
M. V.; van Veggel, A. A.; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch,
J.; Veitch, P. J.; Veltkamp, C.; Villar, A. E.; Vorvick, C.; Vyachanin,
S. P.; Waldman, S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Wei, P.;
Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels,
P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.;
White, D.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams,
H. R.; Williams, L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf,
C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Yablon, J.;
Yakushin, I.; Yamamoto, K.; Yamamoto, H.; Yang, H.; Yeaton-Massey,
D.; Yoshida, S.; Yu, P.; Zanolin, M.; Zhang, L.; Zhang, Z.; Zhao, C.;
Zotov, N.; Zucker, M. E.; Zweizig, J.; LIGO Collaboration; Bizouard,
M. A.; Dietz, A.; Guidi, G. M.; Was, M.
Bibcode: 2012ApJ...755....2A
Altcode: 2012arXiv1201.4413T
We present the results of a LIGO search for gravitational waves
(GWs) associated with GRB 051103, a short-duration hard-spectrum
gamma-ray burst (GRB) whose electromagnetically determined sky
position is coincident with the spiral galaxy M81, which is 3.6 Mpc
from Earth. Possible progenitors for short-hard GRBs include compact
object mergers and soft gamma repeater (SGR) giant flares. A merger
progenitor would produce a characteristic GW signal that should be
detectable at a distance of M81, while GW emission from an SGR is not
expected to be detectable at that distance. We found no evidence of a
GW signal associated with GRB 051103. Assuming weakly beamed γ-ray
emission with a jet semi-angle of 30°, we exclude a binary neutron
star merger in M81 as the progenitor with a confidence of 98%. Neutron
star-black hole mergers are excluded with >99% confidence. If the
event occurred in M81, then our findings support the hypothesis that
GRB 051103 was due to an SGR giant flare, making it one of the most
distant extragalactic magnetars observed to date.
Title: Upper limits on a stochastic gravitational-wave background
using LIGO and Virgo interferometers at 600-1000 Hz
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.;
Abernathy, M.; Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.;
Affeldt, C.; Agathos, M.; Agatsuma, K.; Ajith, P.; Allen, B.; Amador
Ceron, E.; Amariutei, D.; Anderson, S. B.; Anderson, W. G.; Arai,
K.; Arain, M. A.; Araya, M. C.; Aston, S. M.; Astone, P.; Atkinson,
D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker, P.;
Ballardin, G.; Ballmer, S.; Barayoga, J. C. B.; Barker, D.; Barone,
F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Basti, A.; Batch, J.; Bauchrowitz, J.;
Bauer, Th. S.; Bebronne, M.; Beck, D.; Behnke, B.; Bejger, M.; Beker,
M. G.; Bell, A. S.; Belletoile, A.; Belopolski, I.; Benacquista,
M.; Berliner, J. M.; Bertolini, A.; Betzwieser, J.; Beveridge,
N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Birch, J.;
Biswas, R.; Bitossi, M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.;
Blackburn, L.; Blair, D.; Bland, B.; Blom, M.; Bock, O.; Bodiya, T. P.;
Bogan, C.; Bondarescu, R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork,
R.; Born, M.; Boschi, V.; Bose, S.; Bosi, L.; Bouhou, B.; Braccini, S.;
Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brau,
J. E.; Breyer, J.; Briant, T.; Bridges, D. O.; Brillet, A.; Brinkmann,
M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Bulik,
T.; Bulten, H. J.; Buonanno, A.; Burguet–Castell, J.; Buskulic,
D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Calloni, E.;
Camp, J. B.; Campsie, P.; Cannizzo, J.; Cannon, K.; Canuel, B.;
Cao, J.; Capano, C. D.; Carbognani, F.; Carbone, L.; Caride, S.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chaibi, O.; Chalermsongsak, T.; Charlton,
P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, W.; Chen, X.; Chen,
Y.; Chincarini, A.; Chiummo, A.; Cho, H. S.; Chow, J.; Christensen,
N.; Chua, S. S. Y.; Chung, C. T. Y.; Chung, S.; Ciani, G.; Clara,
F.; Clark, D. E.; Clark, J.; Clayton, J. H.; Cleva, F.; Coccia, E.;
Cohadon, P. -F.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini,
M.; Conte, A.; Conte, R.; Cook, D.; Corbitt, T. R.; Cordier, M.;
Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin, M.; Coulon, J. -P.;
Couvares, P.; Coward, D. M.; Cowart, M.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Cumming, A.; Cunningham,
L.; Cuoco, E.; Cutler, R. M.; Dahl, K.; Danilishin, S. L.; Dannenberg,
R.; D'Antonio, S.; Danzmann, K.; Dattilo, V.; Daudert, B.; Daveloza,
H.; Davier, M.; Daw, E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra,
D.; Debreczeni, G.; Del Pozzo, W.; del Prete, M.; Dent, T.; Dergachev,
V.; DeRosa, R.; DeSalvo, R.; Dhurandhar, S.; Di Fiore, L.; Di Lieto,
A.; Di Palma, I.; Di Paolo Emilio, M.; Di Virgilio, A.; Díaz, M.;
Dietz, A.; Donovan, F.; Dooley, K. L.; Drago, M.; Drever, R. W. P.;
Driggers, J. C.; Du, Z.; Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar,
M.; Edwards, M.; Effler, A.; Ehrens, P.; Endrőczi, G.; Engel, R.;
Etzel, T.; Evans, K.; Evans, M.; Evans, T.; Factourovich, M.; Fafone,
V.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Fazi, D.; Fehrmann, H.;
Feldbaum, D.; Feroz, F.; Ferrante, I.; Fidecaro, F.; Finn, L. S.;
Fiori, I.; Fisher, R. P.; Flaminio, R.; Flanigan, M.; Foley, S.;
Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.; Franc, J.;
Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.;
Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov, V. V.;
Fujimoto, M. -K.; Fulda, P. J.; Fyffe, M.; Gair, J.; Galimberti, M.;
Gammaitoni, L.; Garcia, J.; Garufi, F.; Gáspár, M. E.; Gemme, G.;
Geng, R.; Genin, E.; Gennai, A.; Gergely, L. Á.; Ghosh, S.; Giaime,
J. A.; Giampanis, S.; Giardina, K. D.; Giazotto, A.; Gil-Casanova,
S.; Gill, C.; Gleason, J.; Goetz, E.; Goggin, L. M.; González, G.;
Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Graff, P. B.;
Granata, M.; Grant, A.; Gras, S.; Gray, C.; Gray, N.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.;
Grunewald, S.; Guidi, G. M.; Guido, C. .; Gupta, R.; Gustafson, E. K.;
Gustafson, R.; Ha, T.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks,
J.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.;
Harstad, E. D.; Hartman, M. T.; Haughian, K.; Hayama, K.; Hayau,
J. -F.; Heefner, J.; Heidmann, A.; Heintze, M. C.; Heitmann, H.;
Hello, P.; Hendry, M. A.; Heng, I. S.; Heptonstall, A. W.; Herrera,
V.; Hewitson, M.; Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Holtrop,
M.; Hong, T.; Hooper, S.; Hosken, D. J.; Hough, J.; Howell, E. J.;
Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.;
Inta, R.; Isogai, T.; Ivanov, A.; Izumi, K.; Jacobson, M.; James, E.;
Jang, Y. J.; Jaranowski, P.; Jesse, E.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kang, G.; Kanner, J. B.; Kasturi, R.; Katsavounidis, E.; Katzman,
W.; Kaufer, H.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kelley, D.;
Kells, W.; Keppel, D. G.; Keresztes, Z.; Khalaidovski, A.; Khalili,
F. Y.; Khazanov, E. A.; Kim, B. K.; Kim, C.; Kim, H.; Kim, K.; Kim,
N.; Kim, Y. M.; King, P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko,
S.; Kokeyama, K.; Kondrashov, V.; Koranda, S.; Korth, W. Z.; Kowalska,
I.; Kozak, D.; Kranz, O.; Kringel, V.; Krishnamurthy, S.; Krishnan,
B.; Królak, A.; Kuehn, G.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry,
M.; Lantz, B.; Lastzka, N.; Lawrie, C.; Lazzarini, A.; Leaci, P.; Lee,
C. H.; Lee, H. K.; Lee, H. M.; Leong, J. R.; Leonor, I.; Leroy, N.;
Letendre, N.; Li, J.; Li, T. G. F.; Liguori, N.; Lindquist, P. E.; Liu,
Y.; Liu, Z.; Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.;
Lormand, M.; Losurdo, G.; Lough, J.; Luan, J.; Lubinski, M.; Lück,
H.; Lundgren, A. P.; Macdonald, E.; Machenschalk, B.; MacInnis, M.;
Macleod, D. M.; Mageswaran, M.; Mailand, K.; Majorana, E.; Maksimovic,
I.; Man, N.; Mandel, I.; Mandic, V.; Mantovani, M.; Marandi, A.;
Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markosyan, A.;
Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.; Martin, R. M.;
Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.; Matone, L.;
Matzner, R. A.; Mavalvala, N.; Mazzolo, G.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIver, J.; McKechan, D. J. A.;
McWilliams, S.; Meadors, G. D.; Mehmet, M.; Meier, T.; Melatos,
A.; Melissinos, A. C.; Mendell, G.; Mercer, R. A.; Meshkov, S.;
Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.; Miller,
J.; Minenkov, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman,
R.; Miyakawa, O.; Moe, B.; Mohan, M.; Mohanty, S. D.; Mohapatra,
S. R. P.; Moraru, D.; Moreno, G.; Morgado, N.; Morgia, A.; Mori,
T.; Morriss, S. R.; Mosca, S.; Mossavi, K.; Mours, B.; Mow–Lowry,
C. M.; Mueller, C. L.; Mueller, G.; Mukherjee, S.; Mullavey, A.;
Müller-Ebhardt, H.; Munch, J.; Murphy, D.; Murray, P. G.; Mytidis, A.;
Nash, T.; Naticchioni, L.; Necula, V.; Nelson, J.; Neri, I.; Newton,
G.; Nguyen, T.; Nishizawa, A.; Nitz, A.; Nocera, F.; Nolting, D.;
Normandin, M. E.; Nuttall, L.; Ochsner, E.; O'Dell, J.; Oelker, E.;
Ogin, G. H.; Oh, J. J.; Oh, S. H.; O'Reilly, B.; O'Shaughnessy, R.;
Osthelder, C.; Ott, C. D.; Ottaway, D. J.; Ottens, R. S.; Overmier,
H.; Owen, B. J.; Page, A.; Pagliaroli, G.; Palladino, L.; Palomba,
C.; Pan, Y.; Pankow, C.; Paoletti, F.; Papa, M. A.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pedraza,
M.; Peiris, P.; Pekowsky, L.; Penn, S.; Perreca, A.; Persichetti,
G.; Phelps, M.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.;
Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Poggiani, R.; Pöld, J.; Postiglione, F.; Prato, M.;
Predoi, V.; Prestegard, T.; Price, L. R.; Prijatelj, M.; Principe, M.;
Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov, L. G.; Puncken, O.;
Punturo, M.; Puppo, P.; Quetschke, V.; Quitzow-James, R.; Raab, F. J.;
Rabeling, D. S.; Rácz, I.; Radkins, H.; Raffai, P.; Rakhmanov, M.;
Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Redwine, K.; Reed,
C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.;
Riesen, R.; Riles, K.; Robertson, N. A.; Robinet, F.; Robinson, C.;
Robinson, E. L.; Rocchi, A.; Roddy, S.; Rodriguez, C.; Rodruck, M.;
Rolland, L.; Rollins, J. G.; Romano, J. D.; Romano, R.; Romie, J. H.;
Rosińska, D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan,
K.; Sainathan, P.; Salemi, F.; Sammut, L.; Sandberg, V.; Sannibale,
V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.; Sassolas,
B.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.;
Schilling, R.; Schnabel, R.; Schofield, R. M. S.; Schreiber, E.;
Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.;
Seifert, F.; Sellers, D.; Sentenac, D.; Sergeev, A.; Shaddock, D. A.;
Shaltev, M.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.;
Siemens, X.; Sigg, D.; Singer, A.; Singer, L.; Sintes, A. M.; Skelton,
G. R.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.;
Smith, R. J. E.; Smith-Lefebvre, N. D.; Somiya, K.; Sorazu, B.; Soto,
J.; Speirits, F. C.; Sperandio, L.; Stefszky, M.; Stein, A. J.; Stein,
L. C.; Steinert, E.; Steinlechner, J.; Steinlechner, S.; Steplewski,
S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S. E.; Stroeer,
A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sung, M.;
Susmithan, S.; Sutton, P. J.; Swinkels, B.; Tacca, M.; Taffarello, L.;
Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor,
R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.; Thüring,
A.; Tokmakov, K. V.; Tomlinson, C.; Toncelli, A.; Tonelli, M.; Torre,
O.; Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso, F.; Traylor,
G.; Tseng, K.; Ugolini, D.; Vahlbruch, H.; Vajente, G.; van den
Brand, J. F. J.; Van Den Broeck, C.; van der Putten, S.; van Veggel,
A. A.; Vass, S.; Vasuth, M.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.;
Vedovato, G.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.;
Vetrano, F.; Viceré, A.; Villar, A. E.; Vinet, J. -Y.; Vitale, S.;
Vocca, H.; Vorvick, C.; Vyatchanin, S. P.; Wade, A.; Wade, L.; Wade,
M.; Waldman, S. J.; Wallace, L.; Wan, Y.; Wang, M.; Wang, X.; Wang, Z.;
Wanner, A.; Ward, R. L.; Was, M.; Weinert, M.; Weinstein, A. J.; Weiss,
R.; Wen, L.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan,
J. T.; Whitcomb, S. E.; White, D. J.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, L.; Williams, R.; Willke, B.; Winkelmann,
L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Wittel, H.; Woan, G.;
Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto, K.;
Yancey, C. C.; Yang, H.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.;
Yvert, M.; Zadroźny, A.; Zanolin, M.; Zendri, J. -P.; Zhang, F.;
Zhang, L.; Zhang, W.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2012PhRvD..85l2001A
Altcode: 2011arXiv1112.5004A
A stochastic background of gravitational waves is expected to arise
from a superposition of many incoherent sources of gravitational waves,
of either cosmological or astrophysical origin. This background is
a target for the current generation of ground-based detectors. In
this article we present the first joint search for a stochastic
background using data from the LIGO and Virgo interferometers. In a
frequency band of 600-1000 Hz, we obtained a 95% upper limit on the
amplitude of ΩGW(f)=Ω3(f/900Hz)3,
of Ω3<0.32, assuming a value of the Hubble parameter
of h100=0.71. These new limits are a factor of seven better
than the previous best in this frequency band.
Title: All-sky search for gravitational-wave bursts in the second
joint LIGO-Virgo run
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.;
Abernathy, M.; Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.;
Affeldt, C.; Agathos, M.; Agatsuma, K.; Ajith, P.; Allen, B.; Amador
Ceron, E.; Amariutei, D.; Anderson, S. B.; Anderson, W. G.; Arai,
K.; Arain, M. A.; Araya, M. C.; Aston, S. M.; Astone, P.; Atkinson,
D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker, P.;
Ballardin, G.; Ballmer, S.; Barayoga, J. C. B.; Barker, D.; Barone,
F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Basti, A.; Batch, J.; Bauchrowitz, J.;
Bauer, Th. S.; Bebronne, M.; Beck, D.; Behnke, B.; Bejger, M.; Beker,
M. G.; Bell, A. S.; Belletoile, A.; Belopolski, I.; Benacquista,
M.; Berliner, J. M.; Bertolini, A.; Betzwieser, J.; Beveridge,
N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Birch, J.;
Biswas, R.; Bitossi, M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.;
Blackburn, L.; Blair, D.; Bland, B.; Blom, M.; Bock, O.; Bodiya, T. P.;
Bogan, C.; Bondarescu, R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork,
R.; Born, M.; Boschi, V.; Bose, S.; Bosi, L.; Bouhou, B.; Braccini, S.;
Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brau,
J. E.; Breyer, J.; Briant, T.; Bridges, D. O.; Brillet, A.; Brinkmann,
M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Bulik,
T.; Bulten, H. J.; Buonanno, A.; Burguet–Castell, J.; Buskulic,
D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Calloni, E.;
Camp, J. B.; Campsie, P.; Cannizzo, J.; Cannon, K.; Canuel, B.;
Cao, J.; Capano, C. D.; Carbognani, F.; Carbone, L.; Caride, S.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chaibi, O.; Chalermsongsak, T.; Charlton,
P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, W.; Chen, X.; Chen,
Y.; Chincarini, A.; Chiummo, A.; Cho, H. S.; Chow, J.; Christensen,
N.; Chua, S. S. Y.; Chung, C. T. Y.; Chung, S.; Ciani, G.; Clara,
F.; Clark, D. E.; Clark, J.; Clayton, J. H.; Cleva, F.; Coccia, E.;
Cohadon, P. -F.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini,
M.; Conte, A.; Conte, R.; Cook, D.; Corbitt, T. R.; Cordier, M.;
Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin, M.; Coulon, J. -P.;
Couvares, P.; Coward, D. M.; Cowart, M.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Cumming, A.; Cunningham,
L.; Cuoco, E.; Cutler, R. M.; Dahl, K.; Danilishin, S. L.; Dannenberg,
R.; D'Antonio, S.; Danzmann, K.; Dattilo, V.; Daudert, B.; Daveloza,
H.; Davier, M.; Daw, E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra,
D.; Debreczeni, G.; Del Pozzo, W.; del Prete, M.; Dent, T.; Dergachev,
V.; DeRosa, R.; DeSalvo, R.; Dhurandhar, S.; Di Fiore, L.; Di Lieto,
A.; Di Palma, I.; Di Paolo Emilio, M.; Di Virgilio, A.; Díaz, M.;
Dietz, A.; Donovan, F.; Dooley, K. L.; Drago, M.; Drever, R. W. P.;
Driggers, J. C.; Du, Z.; Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar,
M.; Edwards, M.; Effler, A.; Ehrens, P.; Endrőczi, G.; Engel, R.;
Etzel, T.; Evans, K.; Evans, M.; Evans, T.; Factourovich, M.; Fafone,
V.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Fazi, D.; Fehrmann, H.;
Feldbaum, D.; Feroz, F.; Ferrante, I.; Fidecaro, F.; Finn, L. S.;
Fiori, I.; Fisher, R. P.; Flaminio, R.; Flanigan, M.; Foley, S.;
Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.; Franc, J.;
Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.;
Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov, V. V.;
Fujimoto, M. -K.; Fulda, P. J.; Fyffe, M.; Gair, J.; Galimberti, M.;
Gammaitoni, L.; Garcia, J.; Garufi, F.; Gáspár, M. E.; Gemme, G.;
Geng, R.; Genin, E.; Gennai, A.; Gergely, L. Á.; Ghosh, S.; Giaime,
J. A.; Giampanis, S.; Giardina, K. D.; Giazotto, A.; Gil-Casanova,
S.; Gill, C.; Gleason, J.; Goetz, E.; Goggin, L. M.; González, G.;
Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Graff, P. B.;
Granata, M.; Grant, A.; Gras, S.; Gray, C.; Gray, N.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote,
H.; Grunewald, S.; Guidi, G. M.; Guido, C.; Gupta, R.; Gustafson,
E. K.; Gustafson, R.; Ha, T.; Hallam, J. M.; Hammer, D.; Hammond,
G.; Hanks, J.; Hanna, C.; Hanson, J.; Harms, J.; Hardt, A.; Harry,
G. M.; Harry, I. W.; Harstad, E. D.; Hartman, M. T.; Haughian, K.;
Hayama, K.; Hayau, J. -F.; Heefner, J.; Heidmann, A.; Heintze, M. C.;
Heitmann, H.; Hello, P.; Hendry, M. A.; Heng, I. S.; Heptonstall,
A. W.; Herrera, V.; Hewitson, M.; Hild, S.; Hoak, D.; Hodge, K. A.;
Holt, K.; Holtrop, M.; Hong, T.; Hooper, S.; Hosken, D. J.; Hough, J.;
Howell, E. J.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.;
Ingram, D. R.; Inta, R.; Isogai, T.; Ivanov, A.; Izumi, K.; Jacobson,
M.; James, E.; Jang, Y. J.; Jaranowski, P.; Jesse, E.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kandhasamy, S.; Kang, G.; Kanner, J. B.; Kasturi, R.; Katsavounidis,
E.; Katzman, W.; Kaufer, H.; Kawabe, K.; Kawamura, S.; Kawazoe, F.;
Kelley, D.; Kells, W.; Keppel, D. G.; Keresztes, Z.; Khalaidovski,
A.; Khalili, F. Y.; Khazanov, E. A.; Kim, B. K.; Kim, C.; Kim, H.;
Kim, K.; Kim, N.; Kim, Y. M.; King, P. J.; Kinzel, D. L.; Kissel,
J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Koranda, S.; Korth,
W. Z.; Kowalska, I.; Kozak, D.; Kranz, O.; Kringel, V.; Krishnamurthy,
S.; Krishnan, B.; Królak, A.; Kuehn, G.; Kumar, R.; Kwee, P.; Lam,
P. K.; Landry, M.; Lantz, B.; Lastzka, N.; Lawrie, C.; Lazzarini,
A.; Leaci, P.; Lee, C. H.; Lee, H. K.; Lee, H. M.; Leong, J. R.;
Leonor, I.; Leroy, N.; Letendre, N.; Li, J.; Li, T. G. F.; Liguori,
N.; Lindquist, P. E.; Liu, Y.; Liu, Z.; Lockerbie, N. A.; Lodhia,
D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lough,
J.; Luan, J.; Lubinski, M.; Lück, H.; Lundgren, A. P.; Macdonald,
E.; Machenschalk, B.; MacInnis, M.; Macleod, D. M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Maksimovic, I.; Man, N.; Mandel, I.; Mandic,
V.; Mantovani, M.; Marandi, A.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Markosyan, A.; Maros, E.; Marque, J.; Martelli, F.;
Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.;
Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala, N.; Mazzolo,
G.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McIntyre, G.;
McIver, J.; McKechan, D. J. A.; McWilliams, S.; Meadors, G. D.;
Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.; Mendell, G.;
Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Miao, H.;
Michel, C.; Milano, L.; Miller, J.; Minenkov, Y.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohan, M.;
Mohanty, S. D.; Mohapatra, S. R. P.; Moraru, D.; Moreno, G.; Morgado,
N.; Morgia, A.; Mori, T.; Morriss, S. R.; Mosca, S.; Mossavi, K.;
Mours, B.; Mow–Lowry, C. M.; Mueller, C. L.; Mueller, G.; Mukherjee,
S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murphy, D.; Murray,
P. G.; Mytidis, A.; Nash, T.; Naticchioni, L.; Necula, V.; Nelson,
J.; Neri, I.; Newton, G.; Nguyen, T.; Nishizawa, A.; Nitz, A.; Nocera,
F.; Nolting, D.; Normandin, M. E.; Nuttall, L.; Ochsner, E.; O'Dell,
J.; Oelker, E.; Ogin, G. H.; Oh, J. J.; Oh, S. H.; O'Reilly, B.;
O'Shaughnessy, R.; Osthelder, C.; Ott, C. D.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Page, A.; Pagliaroli, G.; Palladino,
L.; Palomba, C.; Pan, Y.; Pankow, C.; Paoletti, F.; Papa, M. A.;
Parisi, M.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel,
P.; Pedraza, M.; Peiris, P.; Pekowsky, L.; Penn, S.; Perreca, A.;
Persichetti, G.; Phelps, M.; Pichot, M.; Pickenpack, M.; Piergiovanni,
F.; Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Poggiani, R.; Pöld, J.; Postiglione, F.; Prato, M.;
Predoi, V.; Prestegard, T.; Price, L. R.; Prijatelj, M.; Principe, M.;
Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov, L. G.; Puncken, O.;
Punturo, M.; Puppo, P.; Quetschke, V.; Quitzow-James, R.; Raab, F. J.;
Rabeling, D. S.; Rácz, I.; Radkins, H.; Raffai, P.; Rakhmanov, M.;
Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Redwine, K.; Reed,
C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.;
Riesen, R.; Riles, K.; Robertson, N. A.; Robinet, F.; Robinson, C.;
Robinson, E. L.; Rocchi, A.; Roddy, S.; Rodriguez, C.; Rodruck, M.;
Rolland, L.; Rollins, J. G.; Romano, J. D.; Romano, R.; Romie, J. H.;
Rosińska, D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan,
K.; Sainathan, P.; Salemi, F.; Sammut, L.; Sandberg, V.; Sannibale,
V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.; Sassolas,
B.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.;
Schilling, R.; Schnabel, R.; Schofield, R. M. S.; Schreiber, E.;
Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.;
Seifert, F.; Sellers, D.; Sentenac, D.; Sergeev, A.; Shaddock, D. A.;
Shaltev, M.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.;
Siemens, X.; Sigg, D.; Singer, A.; Singer, L.; Sintes, A. M.; Skelton,
G. R.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.;
Smith, R. J. E.; Smith-Lefebvre, N. D.; Somiya, K.; Sorazu, B.; Soto,
J.; Speirits, F. C.; Sperandio, L.; Stefszky, M.; Stein, A. J.; Stein,
L. C.; Steinert, E.; Steinlechner, J.; Steinlechner, S.; Steplewski,
S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S. E.; Stroeer,
A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sung, M.;
Susmithan, S.; Sutton, P. J.; Swinkels, B.; Tacca, M.; Taffarello, L.;
Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor,
R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.; Thüring, A.;
Tokmakov, K. V.; Tomlinson, C.; Toncelli, A.; Tonelli, M.; Torre, O.;
Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso, F.; Traylor, G.;
Tseng, K.; Tucker, E.; Ugolini, D.; Vahlbruch, H.; Vajente, G.; van den
Brand, J. F. J.; Van Den Broeck, C.; van der Putten, S.; van Veggel,
A. A.; Vass, S.; Vasuth, M.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.;
Vedovato, G.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.;
Vetrano, F.; Viceré, A.; Villar, A. E.; Vinet, J. -Y.; Vitale, S.;
Vocca, H.; Vorvick, C.; Vyatchanin, S. P.; Wade, A.; Wade, L.; Wade,
M.; Waldman, S. J.; Wallace, L.; Wan, Y.; Wang, M.; Wang, X.; Wang, Z.;
Wanner, A.; Ward, R. L.; Was, M.; Weinert, M.; Weinstein, A. J.; Weiss,
R.; Wen, L.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan,
J. T.; Whitcomb, S. E.; White, D. J.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, L.; Williams, R.; Willke, B.; Winkelmann,
L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Wittel, H.; Woan, G.;
Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto, K.;
Yancey, C. C.; Yang, H.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.;
Yvert, M.; Zadrożny, A.; Zanolin, M.; Zendri, J. -P.; Zhang, F.;
Zhang, L.; Zhang, W.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2012PhRvD..85l2007A
Altcode: 2012arXiv1202.2788T
We present results from a search for gravitational-wave bursts in
the data collected by the LIGO and Virgo detectors between July 7,
2009 and October 20, 2010: data are analyzed when at least two
of the three LIGO-Virgo detectors are in coincident operation,
with a total observation time of 207 days. The analysis searches
for transients of duration ≲1s over the frequency band 64-5000
Hz, without other assumptions on the signal waveform, polarization,
direction or occurrence time. All identified events are consistent with
the expected accidental background. We set frequentist upper limits
on the rate of gravitational-wave bursts by combining this search
with the previous LIGO-Virgo search on the data collected between
November 2005 and October 2007. The upper limit on the rate of strong
gravitational-wave bursts at the Earth is 1.3 events per year at 90%
confidence. We also present upper limits on source rate density per
year and Mpc3 for sample populations of standard-candle
sources. As in the previous joint run, typical sensitivities of the
search in terms of the root-sum-squared strain amplitude for these
waveforms lie in the range ∼5×10-22Hz-1/2
to ∼1×10-20Hz-1/2. The combination of the
two joint runs entails the most sensitive all-sky search for generic
gravitational-wave bursts and synthesizes the results achieved by the
initial generation of interferometric detectors.
Title: Dynamic Evolution of Active Region Flux Tubes in the Turbulent
Convective Envelope of a Young Sun: Solar-like Fast Rotators
Authors: Weber, Maria A.; Brown, B. P.; Fan, Y.
Bibcode: 2012AAS...22020109W
Altcode:
Our Sun rotated much more rapidly when it was younger, as is suggested
by observations of rapidly rotating solar-like stars and the influence
of the solar wind, which removes angular momentum from the Sun. By
studying how flux emergence may have occurred on the young Sun,
we are likely to learn more about the nature of the solar dynamo
early in the Sun's history, as well as other solar-like stars. To
investigate this, we embed a toroidal flux tube near the base of the
convection zone of a rotating spherical shell of turbulent convection
performed for solar-like stars that rotate 3, 5, and 10 times the
current solar rate. Our objective is to understand how the convective
flows of these fast rotators can influence the emergent properties of
flux tubes which would rise to create active regions, or starspots,
of a variety of magnetic flux strengths, magnetic fields, and initial
latitudes. Flux tube properties we will discuss include rise times,
latitude of emergence, and tilt angles of the emerging flux tube limbs
with respect to the east-west direction. Also of interest is identifying
the regimes where dynamics of the flux tube are convection dominated
or magnetic buoyancy dominated, as well as attempting to identify
active longitudes.
Title: First low-latency LIGO+Virgo search for binary inspirals and
their electromagnetic counterparts
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.;
Abernathy, M.; Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.;
Affeldt, C.; Agathos, M.; Agatsuma, K.; Ajith, P.; Allen, B.; Amador
Ceron, E.; Amariutei, D.; Anderson, S. B.; Anderson, W. G.; Arai,
K.; Arain, M. A.; Araya, M. C.; Aston, S. M.; Astone, P.; Atkinson,
D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker, P.;
Ballardin, G.; Ballmer, S.; Barayoga, J. C. B.; Barker, D.; Barone,
F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Basti, A.; Batch, J.; Bauchrowitz, J.;
Bauer, Th. S.; Bebronne, M.; Beck, D.; Behnke, B.; Bejger, M.; Beker,
M. G.; Bell, A. S.; Belletoile, A.; Belopolski, I.; Benacquista,
M.; Berliner, J. M.; Bertolini, A.; Betzwieser, J.; Beveridge,
N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Birch, J.;
Biswas, R.; Bitossi, M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.;
Blackburn, L.; Blair, D.; Bland, B.; Blom, M.; Bock, O.; Bodiya, T. P.;
Bogan, C.; Bondarescu, R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork,
R.; Born, M.; Boschi, V.; Bose, S.; Bosi, L.; Bouhou, B.; Braccini,
S.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Branchesi, M.;
Brau, J. E.; Breyer, J.; Briant, T.; Bridges, D. O.; Brillet, A.;
Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown, D. A.;
Bulik, T.; Bulten, H. J.; Buonanno, A.; Burguet-Castell, J.; Buskulic,
D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Calloni, E.;
Camp, J. B.; Campsie, P.; Cannizzo, J.; Cannon, K.; Canuel, B.;
Cao, J.; Capano, C. D.; Carbognani, F.; Carbone, L.; Caride, S.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chaibi, O.; Chalermsongsak, T.; Charlton,
P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, W.; Chen, X.; Chen,
Y.; Chincarini, A.; Chiummo, A.; Cho, H. S.; Chow, J.; Christensen,
N.; Chua, S. S. Y.; Chung, C. T. Y.; Chung, S.; Ciani, G.; Clara,
F.; Clark, D. E.; Clark, J.; Clayton, J. H.; Cleva, F.; Coccia, E.;
Cohadon, P. -F.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini,
M.; Conte, A.; Conte, R.; Cook, D.; Corbitt, T. R.; Cordier, M.;
Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin, M.; Coulon, J. -P.;
Couvares, P.; Coward, D. M.; Cowart, M.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Cumming, A.; Cunningham,
L.; Cuoco, E.; Cutler, R. M.; Dahl, K.; Danilishin, S. L.; Dannenberg,
R.; D'Antonio, S.; Danzmann, K.; Dattilo, V.; Daudert, B.; Daveloza,
H.; Davier, M.; Daw, E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra,
D.; Debreczeni, G.; Del Pozzo, W.; del Prete, M.; Dent, T.; Dergachev,
V.; DeRosa, R.; DeSalvo, R.; Dhurandhar, S.; Di Fiore, L.; Di Lieto,
A.; Di Palma, I.; Emilio, M. Di Paolo; Di Virgilio, A.; Díaz, M.;
Dietz, A.; Donovan, F.; Dooley, K. L.; Drago, M.; Drever, R. W. P.;
Driggers, J. C.; Du, Z.; Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar,
M.; Edwards, M.; Effler, A.; Ehrens, P.; Endrőczi, G.; Engel, R.;
Etzel, T.; Evans, K.; Evans, M.; Evans, T.; Factourovich, M.; Fafone,
V.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Fazi, D.; Fehrmann, H.;
Feldbaum, D.; Feroz, F.; Ferrante, I.; Fidecaro, F.; Finn, L. S.;
Fiori, I.; Fisher, R. P.; Flaminio, R.; Flanigan, M.; Foley, S.;
Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.; Franc, J.;
Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.;
Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov, V. V.;
Fujimoto, M. -K.; Fulda, P. J.; Fyffe, M.; Gair, J.; Galimberti, M.;
Gammaitoni, L.; Garcia, J.; Garufi, F.; Gáspár, M. E.; Gemme, G.;
Geng, R.; Genin, E.; Gennai, A.; Gergely, L. Á.; Ghosh, S.; Giaime,
J. A.; Giampanis, S.; Giardina, K. D.; Giazotto, A.; Gil-Casanova,
S.; Gill, C.; Gleason, J.; Goetz, E.; Goggin, L. M.; González, G.;
Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Graff, P. B.;
Granata, M.; Grant, A.; Gras, S.; Gray, C.; Gray, N.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.;
Grunewald, S.; Guidi, G. M.; Guido, C.; Gupta, R.; Gustafson, E. K.;
Gustafson, R.; Ha, T.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks,
J.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.;
Harstad, E. D.; Hartman, M. T.; Haughian, K.; Hayama, K.; Hayau,
J. -F.; Heefner, J.; Heidmann, A.; Heintze, M. C.; Heitmann, H.;
Hello, P.; Hendry, M. A.; Heng, I. S.; Heptonstall, A. W.; Herrera,
V.; Hewitson, M.; Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Holtrop,
M.; Hong, T.; Hooper, S.; Hosken, D. J.; Hough, J.; Howell, E. J.;
Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.;
Inta, R.; Isogai, T.; Ivanov, A.; Izumi, K.; Jacobson, M.; James, E.;
Jang, Y. J.; Jaranowski, P.; Jesse, E.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kang, G.; Kanner, J. B.; Kasturi, R.; Katsavounidis, E.; Katzman,
W.; Kaufer, H.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kelley, D.;
Kells, W.; Keppel, D. G.; Keresztes, Z.; Khalaidovski, A.; Khalili,
F. Y.; Khazanov, E. A.; Kim, B. K.; Kim, C.; Kim, H.; Kim, K.; Kim,
N.; Kim, Y. M.; King, P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko,
S.; Kokeyama, K.; Kondrashov, V.; Koranda, S.; Korth, W. Z.; Kowalska,
I.; Kozak, D.; Kranz, O.; Kringel, V.; Krishnamurthy, S.; Krishnan,
B.; Królak, A.; Kuehn, G.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry,
M.; Lantz, B.; Lastzka, N.; Lawrie, C.; Lazzarini, A.; Leaci, P.; Lee,
C. H.; Lee, H. K.; Lee, H. M.; Leong, J. R.; Leonor, I.; Leroy, N.;
Letendre, N.; Li, J.; Li, T. G. F.; Liguori, N.; Lindquist, P. E.; Liu,
Y.; Liu, Z.; Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.;
Lormand, M.; Losurdo, G.; Lough, J.; Luan, J.; Lubinski, M.; Lück,
H.; Lundgren, A. P.; Macdonald, E.; Machenschalk, B.; MacInnis, M.;
Macleod, D. M.; Mageswaran, M.; Mailand, K.; Majorana, E.; Maksimovic,
I.; Man, N.; Mandel, I.; Mandic, V.; Mantovani, M.; Marandi, A.;
Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markosyan, A.;
Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.; Martin, R. M.;
Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.; Matone, L.;
Matzner, R. A.; Mavalvala, N.; Mazzolo, G.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIver, J.; McKechan, D. J. A.;
McWilliams, S.; Meadors, G. D.; Mehmet, M.; Meier, T.; Melatos,
A.; Melissinos, A. C.; Mendell, G.; Mercer, R. A.; Meshkov, S.;
Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.; Miller,
J.; Minenkov, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman,
R.; Miyakawa, O.; Moe, B.; Mohan, M.; Mohanty, S. D.; Mohapatra,
S. R. P.; Moraru, D.; Moreno, G.; Morgado, N.; Morgia, A.; Mori,
T.; Morriss, S. R.; Mosca, S.; Mossavi, K.; Mours, B.; Mow-Lowry,
C. M.; Mueller, C. L.; Mueller, G.; Mukherjee, S.; Mullavey, A.;
Müller-Ebhardt, H.; Munch, J.; Murphy, D.; Murray, P. G.; Mytidis, A.;
Nash, T.; Naticchioni, L.; Necula, V.; Nelson, J.; Neri, I.; Newton,
G.; Nguyen, T.; Nishizawa, A.; Nitz, A.; Nocera, F.; Nolting, D.;
Normandin, M. E.; Nuttall, L.; Ochsner, E.; O'Dell, J.; Oelker, E.;
Ogin, G. H.; Oh, J. J.; Oh, S. H.; O'Reilly, B.; O'Shaughnessy, R.;
Osthelder, C.; Ott, C. D.; Ottaway, D. J.; Ottens, R. S.; Overmier,
H.; Owen, B. J.; Page, A.; Pagliaroli, G.; Palladino, L.; Palomba,
C.; Pan, Y.; Pankow, C.; Paoletti, F.; Papa, M. A.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pedraza,
M.; Peiris, P.; Pekowsky, L.; Penn, S.; Perreca, A.; Persichetti,
G.; Phelps, M.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.;
Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Poggiani, R.; Pöld, J.; Postiglione, F.; Prato, M.;
Predoi, V.; Prestegard, T.; Price, L. R.; Prijatelj, M.; Principe, M.;
Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov, L. G.; Puncken, O.;
Punturo, M.; Puppo, P.; Quetschke, V.; Quitzow-James, R.; Raab, F. J.;
Rabeling, D. S.; Rácz, I.; Radkins, H.; Raffai, P.; Rakhmanov, M.;
Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Redwine, K.; Reed,
C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.;
Riesen, R.; Riles, K.; Robertson, N. A.; Robinet, F.; Robinson, C.;
Robinson, E. L.; Rocchi, A.; Roddy, S.; Rodriguez, C.; Rodruck, M.;
Rolland, L.; Rollins, J. G.; Romano, J. D.; Romano, R.; Romie, J. H.;
Rosińska, D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan,
K.; Sainathan, P.; Salemi, F.; Sammut, L.; Sandberg, V.; Sannibale,
V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.; Sassolas,
B.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.;
Schilling, R.; Schnabel, R.; Schofield, R. M. S.; Schreiber, E.;
Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.;
Seifert, F.; Sellers, D.; Sentenac, D.; Sergeev, A.; Shaddock, D. A.;
Shaltev, M.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.;
Siemens, X.; Sigg, D.; Singer, A.; Singer, L.; Sintes, A. M.; Skelton,
G. R.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.;
Smith, R. J. E.; Smith-Lefebvre, N. D.; Somiya, K.; Sorazu, B.; Soto,
J.; Speirits, F. C.; Sperandio, L.; Stefszky, M.; Stein, A. J.; Stein,
L. C.; Steinert, E.; Steinlechner, J.; Steinlechner, S.; Steplewski,
S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S. E.; Stroeer,
A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sung, M.;
Susmithan, S.; Sutton, P. J.; Swinkels, B.; Tacca, M.; Taffarello, L.;
Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor,
R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.; Thüring,
A.; Tokmakov, K. V.; Tomlinson, C.; Toncelli, A.; Tonelli, M.; Torre,
O.; Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso, F.; Traylor,
G.; Tseng, K.; Ugolini, D.; Vahlbruch, H.; Vajente, G.; van den
Brand, J. F. J.; Van Den Broeck, C.; van der Putten, S.; van Veggel,
A. A.; Vass, S.; Vasuth, M.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.;
Vedovato, G.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.;
Vetrano, F.; Viceré, A.; Villar, A. E.; Vinet, J. -Y.; Vitale, S.;
Vocca, H.; Vorvick, C.; Vyatchanin, S. P.; Wade, A.; Wade, L.; Wade,
M.; Waldman, S. J.; Wallace, L.; Wan, Y.; Wang, M.; Wang, X.; Wang, Z.;
Wanner, A.; Ward, R. L.; Was, M.; Weinert, M.; Weinstein, A. J.; Weiss,
R.; Wen, L.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan,
J. T.; Whitcomb, S. E.; White, D. J.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, L.; Williams, R.; Willke, B.; Winkelmann,
L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Wittel, H.; Woan, G.;
Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto, K.;
Yancey, C. C.; Yang, H.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.;
Yvert, M.; Zadrożny, A.; Zanolin, M.; Zendri, J. -P.; Zhang, F.;
Zhang, L.; Zhang, W.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2012A&A...541A.155A
Altcode: 2011arXiv1112.6005T
Aims: The detection and measurement of gravitational-waves
from coalescing neutron-star binary systems is an important science
goal for ground-based gravitational-wave detectors. In addition
to emitting gravitational-waves at frequencies that span the most
sensitive bands of the LIGO and Virgo detectors, these sources
are also amongst the most likely to produce an electromagnetic
counterpart to the gravitational-wave emission. A joint detection of
the gravitational-wave and electromagnetic signals would provide a
powerful new probe for astronomy.
Methods: During the period
between September 19 and October 20, 2010, the first low-latency search
for gravitational-waves from binary inspirals in LIGO and Virgo data
was conducted. The resulting triggers were sent to electromagnetic
observatories for followup. We describe the generation and processing
of the low-latency gravitational-wave triggers. The results of the
electromagnetic image analysis will be described elsewhere.
Results: Over the course of the science run, three gravitational-wave
triggers passed all of the low-latency selection cuts. Of these, one
was followed up by several of our observational partners. Analysis of
the gravitational-wave data leads to an estimated false alarm rate
of once every 6.4 days, falling far short of the requirement for a
detection based solely on gravitational-wave data.
Title: Search for gravitational waves from intermediate mass binary
black holes
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.;
Abernathy, M.; Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.;
Affeldt, C.; Agathos, M.; Agatsuma, K.; Ajith, P.; Allen, B.; Amador
Ceron, E.; Amariutei, D.; Anderson, S. B.; Anderson, W. G.; Arai,
K.; Arain, M. A.; Araya, M. C.; Aston, S. M.; Astone, P.; Atkinson,
D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker, P.;
Ballardin, G.; Ballmer, S.; Barayoga, J. C. B.; Barker, D.; Barone,
F.; Barr, B.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Basti, A.; Batch, J.; Bauchrowitz, J.;
Bauer, Th. S.; Bebronne, M.; Beck, D.; Behnke, B.; Bejger, M.; Beker,
M. G.; Bell, A. S.; Belletoile, A.; Belopolski, I.; Benacquista,
M.; Berliner, J. M.; Bertolini, A.; Betzwieser, J.; Beveridge,
N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Birch, J.;
Biswas, R.; Bitossi, M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.;
Blackburn, L.; Blair, D.; Bland, B.; Blom, M.; Bock, O.; Bodiya, T. P.;
Bogan, C.; Bondarescu, R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork,
R.; Born, M.; Boschi, V.; Bose, S.; Bosi, L.; Bouhou, B.; Braccini,
S.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Branchesi, M.;
Brau, J. E.; Breyer, J.; Briant, T.; Bridges, D. O.; Brillet, A.;
Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown, D. A.;
Bulik, T.; Bulten, H. J.; Buonanno, A.; Burguet-Castell, J.; Buskulic,
D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Calloni, E.;
Camp, J. B.; Campsie, P.; Cannizzo, J.; Cannon, K.; Canuel, B.;
Cao, J.; Capano, C. D.; Carbognani, F.; Carbone, L.; Caride, S.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chaibi, O.; Chalermsongsak, T.; Charlton,
P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, W.; Chen, X.; Chen,
Y.; Chincarini, A.; Chiummo, A.; Cho, H.; Chow, J.; Christensen,
N.; Chua, S. S. Y.; Chung, C. T. Y.; Chung, S.; Ciani, G.; Clara,
F.; Clark, D. E.; Clark, J.; Clayton, J. H.; Cleva, F.; Coccia, E.;
Cohadon, P. -F.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini,
M.; Conte, A.; Conte, R.; Cook, D.; Corbitt, T. R.; Cordier, M.;
Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin, M.; Coulon, J. -P.;
Couvares, P.; Coward, D. M.; Cowart, M.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Cumming, A.; Cunningham,
L.; Cuoco, E.; Cutler, R. M.; Dahl, K.; Danilishin, S. L.; Dannenberg,
R.; D'Antonio, S.; Danzmann, K.; Dattilo, V.; Daudert, B.; Daveloza,
H.; Davier, M.; Daw, E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra,
D.; Debreczeni, G.; Del Pozzo, W.; del Prete, M.; Dent, T.; Dergachev,
V.; DeRosa, R.; DeSalvo, R.; Dhurandhar, S.; Di Fiore, L.; Di Lieto,
A.; Di Palma, I.; Di Paolo Emilio, M.; Di Virgilio, A.; Díaz, M.;
Dietz, A.; Donovan, F.; Dooley, K. L.; Drago, M.; Drever, R. W. P.;
Driggers, J. C.; Du, Z.; Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar,
M.; Edwards, M.; Effler, A.; Ehrens, P.; Endrőczi, G.; Engel, R.;
Etzel, T.; Evans, K.; Evans, M.; Evans, T.; Factourovich, M.; Fafone,
V.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Fazi, D.; Fehrmann, H.;
Feldbaum, D.; Feroz, F.; Ferrante, I.; Fidecaro, F.; Finn, L. S.;
Fiori, I.; Fisher, R. P.; Flaminio, R.; Flanigan, M.; Foley, S.;
Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.; Franc, J.;
Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.;
Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov, V. V.;
Fujimoto, M. -K.; Fulda, P. J.; Fyffe, M.; Gair, J.; Galimberti, M.;
Gammaitoni, L.; Garcia, J.; Garufi, F.; Gáspár, M. E.; Gemme, G.;
Geng, R.; Genin, E.; Gennai, A.; Gergely, L. Á.; Ghosh, S.; Giaime,
J. A.; Giampanis, S.; Giardina, K. D.; Giazotto, A.; Gil, S.; Gill,
C.; Gleason, J.; Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky,
M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Graff, P. B.; Granata,
M.; Grant, A.; Gras, S.; Gray, C.; Gray, N.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald, S.;
Guidi, G. M.; Guido, C.; Gupta, R.; Gustafson, E. K.; Gustafson, R.;
Ha, T.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Hartman, M. T.; Haughian, K.; Hayama, K.; Hayau, J. -F.; Heefner,
J.; Heidmann, A.; Heintze, M. C.; Heitmann, H.; Hello, P.; Hendry,
M. A.; Heng, I. S.; Heptonstall, A. W.; Herrera, V.; Hewitson, M.;
Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Holtrop, M.; Hong, T.;
Hooper, S.; Hosken, D. J.; Hough, J.; Howell, E. J.; Hughey, B.; Husa,
S.; Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.; Inta, R.; Isogai,
T.; Ivanov, A.; Izumi, K.; Jacobson, M.; James, E.; Jang, Y. J.;
Jaranowski, P.; Jesse, E.; Johnson, W. W.; Jones, D. I.; Jones, G.;
Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy, S.; Kang, G.;
Kanner, J. B.; Kasturi, R.; Katsavounidis, E.; Katzman, W.; Kaufer, H.;
Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kelley, D.; Kells, W.; Keppel,
D. G.; Keresztes, Z.; Khalaidovski, A.; Khalili, F. Y.; Khazanov,
E. A.; Kim, B.; Kim, C.; Kim, H.; Kim, K.; Kim, N.; Kim, Y. -M.;
King, P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.; Kokeyama,
K.; Kondrashov, V.; Koranda, S.; Korth, W. Z.; Kowalska, I.; Kozak,
D.; Kranz, O.; Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Królak,
A.; Kuehn, G.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.;
Lastzka, N.; Lawrie, C.; Lazzarini, A.; Leaci, P.; Lee, C. H.; Lee,
H. K.; Lee, H. M.; Leong, J. R.; Leonor, I.; Leroy, N.; Letendre,
N.; Li, J.; Li, T. G. F.; Liguori, N.; Lindquist, P. E.; Liu, Y.;
Liu, Z.; Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.;
Lormand, M.; Losurdo, G.; Lough, J.; Luan, J.; Lubinski, M.; Lück,
H.; Lundgren, A. P.; Macdonald, E.; Machenschalk, B.; MacInnis, M.;
Macleod, D. M.; Mageswaran, M.; Mailand, K.; Majorana, E.; Maksimovic,
I.; Man, N.; Mandel, I.; Mandic, V.; Mantovani, M.; Marandi, A.;
Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markosyan, A.;
Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.; Martin, R. M.;
Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.; Matone, L.;
Matzner, R. A.; Mavalvala, N.; Mazzolo, G.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIver, J.; McKechan, D. J. A.;
McWilliams, S.; Meadors, G. D.; Mehmet, M.; Meier, T.; Melatos,
A.; Melissinos, A. C.; Mendell, G.; Mercer, R. A.; Meshkov, S.;
Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.; Miller,
J.; Minenkov, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Moe, B.; Mohan, M.; Mohanty, S. D.; Mohapatra, S. R. P.;
Moraru, D.; Moreno, G.; Morgado, N.; Morgia, A.; Mori, T.; Morriss,
S. R.; Mosca, S.; Mossavi, K.; Mours, B.; Mow-Lowry, C. M.; Mueller,
C. L.; Mueller, G.; Mukherjee, S.; Mullavey, A.; Müller-Ebhardt,
H.; Munch, J.; Murphy, D.; Murray, P. G.; Mytidis, A.; Nash, T.;
Naticchioni, L.; Necula, V.; Nelson, J.; Newton, G.; Nguyen, T.;
Nishizawa, A.; Nitz, A.; Nocera, F.; Nolting, D.; Normandin, M. E.;
Nuttall, L.; Ochsner, E.; O'Dell, J.; Oelker, E.; Ogin, G. H.; Oh,
J. J.; Oh, S. H.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.; Ott,
C. D.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page,
A.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow, C.;
Paoletti, F.; Papa, M. A.; Parisi, M.; Pasqualetti, A.; Passaquieti,
R.; Passuello, D.; Patel, P.; Pedraza, M.; Peiris, P.; Pekowsky, L.;
Penn, S.; Perreca, A.; Persichetti, G.; Phelps, M.; Pickenpack, M.;
Piergiovanni, F.; Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin, M.;
Pletsch, H. J.; Plissi, M. V.; Poggiani, R.; Pöld, J.; Postiglione,
F.; Prato, M.; Predoi, V.; Prestegard, T.; Price, L. R.; Prijatelj, M.;
Principe, M.; Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov, L. G.;
Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Quitzow-James,
R.; Raab, F. J.; Rabeling, D. S.; Rácz, I.; Radkins, H.; Raffai,
P.; Rakhmanov, M.; Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.;
Redwine, K.; Reed, C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze,
D. H.; Ricci, F.; Riesen, R.; Riles, K.; Robertson, N. A.; Robinet,
F.; Robinson, C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Rodriguez,
C.; Rodruck, M.; Rolland, L.; Rollins, J. G.; Romano, J. D.; Romano,
R.; Romie, J. H.; Rosińska, D.; Röver, C.; Rowan, S.; Rüdiger, A.;
Ruggi, P.; Ryan, K.; Sainathan, P.; Salemi, F.; Sammut, L.; Sandberg,
V.; Sannibale, V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi,
G.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.;
Savage, R. L.; Schilling, R.; Schnabel, R.; Schofield, R. M. S.;
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D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.; Singer, L.;
Sintes, A. M.; Skelton, G. R.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, R. J. E.; Smith-Lefebvre, N. D.; Somiya,
K.; Sorazu, B.; Soto, J.; Speirits, F. C.; Sperandio, L.; Stefszky,
M.; Stein, A. J.; Stein, L. C.; Steinert, E.; Steinlechner, J.;
Steinlechner, S.; Steplewski, S.; Stochino, A.; Stone, R.; Strain,
K. A.; Strigin, S. E.; Stroeer, A. S.; Sturani, R.; Stuver, A. L.;
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B.; Tacca, M.; Taffarello, L.; Talukder, D.; Tanner, D. B.; Tarabrin,
S. P.; Taylor, J. R.; Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne,
K. S.; Thrane, E.; Thüring, A.; Tokmakov, K. V.; Tomlinson, C.;
Toncelli, A.; Tonelli, M.; Torre, O.; Torres, C.; Torrie, C. I.;
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Vahlbruch, H.; Vajente, G.; van den Brand, J. F. J.; Van Den Broeck,
C.; van der Putten, S.; van Veggel, A. A.; Vass, S.; Vasuth, M.;
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A.; Villar, A. E.; Vinet, J. -Y.; Vitale, S.; Vitale, S.; Vocca, H.;
Vorvick, C.; Vyatchanin, S. P.; Wade, A.; Wade, L.; Wade, M.; Waldman,
S. J.; Wallace, L.; Wan, Y.; Wang, M.; Wang, X.; Wang, Z.; Wanner,
A.; Ward, R. L.; Was, M.; Weinert, M.; Weinstein, A. J.; Weiss, R.;
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J. T.; Whitcomb, S. E.; White, D. J.; Whiting, B. F.; Wilkinson, C.;
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L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Wittel, H.; Woan, G.;
Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto, K.;
Yancey, C. C.; Yang, H.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.;
Yvert, M.; Zadroźny, A.; Zanolin, M.; Zendri, J. -P.; Zhang, F.;
Zhang, L.; Zhang, W.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2012PhRvD..85j2004A
Altcode: 2012arXiv1201.5999T
We present the results of a weakly modeled burst search for
gravitational waves from mergers of nonspinning intermediate mass
black holes in the total mass range 100-450M⊙ and with the
component mass ratios between 1∶1 and 4∶1. The search was conducted
on data collected by the LIGO and Virgo detectors between November of
2005 and October of 2007. No plausible signals were observed by the
search which constrains the astrophysical rates of the intermediate
mass black holes mergers as a function of the component masses. In
the most efficiently detected bin centered on 88+88M⊙,
for nonspinning sources, the rate density upper limit is 0.13 per
Mpc3 per Myr at the 90% confidence level.
Title: Implementation and testing of the first prompt search for
gravitational wave transients with electromagnetic counterparts
Authors: LIGO Scientific Collaboration; Virgo Collaboration; Abadie,
J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.; Abernathy, M.; Accadia,
T.; Acernese, F.; Adams, C.; Adhikari, R.; Affeldt, C.; Ajith, P.;
Allen, B.; Allen, G. S.; Amador Ceron, E.; Amariutei, D.; Amin, R. S.;
Anderson, S. B.; Anderson, W. G.; Arai, K.; Arain, M. A.; Araya,
M. C.; Aston, S. M.; Astone, P.; Atkinson, D.; Aufmuth, P.; Aulbert,
C.; Aylott, B. E.; Babak, S.; Baker, P.; Ballardin, G.; Ballmer,
S.; Barker, D.; Barone, F.; Barr, B.; Barriga, P.; Barsotti, L.;
Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri, R.; Bastarrika, M.;
Basti, A.; Batch, J.; Bauchrowitz, J.; Bauer, Th. S.; Bebronne, M.;
Behnke, B.; Beker, M. G.; Bell, A. S.; Belletoile, A.; Belopolski,
I.; Benacquista, M.; Berliner, J. M.; Bertolini, A.; Betzwieser,
J.; Beveridge, N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Birch, J.; Biswas, R.; Bitossi, M.; Bizouard, M. A.; Black, E.;
Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.; Blom, M.; Bock,
O.; Bodiya, T. P.; Bogan, C.; Bondarescu, R.; Bondu, F.; Bonelli,
L.; Bonnand, R.; Bork, R.; Born, M.; Boschi, V.; Bose, S.; Bosi, L.;
Bouhou, B.; Braccini, S.; Bradaschia, C.; Brady, P. R.; Braginsky,
V. B.; Branchesi, M.; Brau, J. E.; Breyer, J.; Briant, T.; Bridges,
D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks,
A. F.; Brown, D. A.; Brummit, A.; Bulik, T.; Bulten, H. J.; Buonanno,
A.; Burguet-Castell, J.; Burmeister, O.; Buskulic, D.; Buy, C.; Byer,
R. L.; Cadonati, L.; Cagnoli, G.; Calloni, E.; Camp, J. B.; Campsie,
P.; Cannizzo, J.; Cannon, K.; Canuel, B.; Cao, J.; Capano, C. D.;
Carbognani, F.; Caride, S.; Caudill, S.; Cavaglià, M.; Cavalier,
F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarin, E.; Chaibi, O.;
Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chassande-Mottin,
E.; Chelkowski, S.; Chen, Y.; Chincarini, A.; Chiummo, A.; Cho, H.;
Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.; Chung, S.; Ciani,
G.; Clara, F.; Clark, D. E.; Clark, J.; Clayton, J. H.; Cleva, F.;
Coccia, E.; Cohadon, P. -F.; Colacino, C. N.; Colas, J.; Colla,
A.; Colombini, M.; Conte, A.; Conte, R.; Cook, D.; Corbitt, T. R.;
Cordier, M.; Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin, M.;
Coulon, J. -P.; Couvares, P.; Coward, D. M.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Cumming, A.; Cunningham, L.;
Cuoco, E.; Cutler, R. M.; Dahl, K.; Danilishin, S. L.; Dannenberg, R.;
D'Antonio, S.; Danzmann, K.; Dattilo, V.; Daudert, B.; Daveloza, H.;
Davier, M.; Davies, G.; Daw, E. J.; Day, R.; Dayanga, T.; DeRosa, R.;
Debra, D.; Debreczeni, G.; Degallaix, J.; Del Pozzo, W.; Del Prete,
M.; Dent, T.; Dergachev, V.; Derosa, R.; Desalvo, R.; Dhillon, V.;
Dhurandhar, S.; Di Fiore, L.; Di Lieto, A.; Di Palma, I.; De Paolo
Emilio, M.; Di Virgilio, A.; Díaz, M.; Dietz, A.; Diguglielmo, J.;
Donovan, F.; Dooley, K. L.; Dorsher, S.; Drago, M.; Drever, R. W. P.;
Driggers, J. C.; Du, Z.; Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar,
M.; Edwards, M.; Effler, A.; Ehrens, P.; Endröczi, G.; Engel, R.;
Etzel, T.; Evans, K.; Evans, M.; Evans, T.; Factourovich, M.; Fafone,
V.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Farr, W.; Fazi, D.; Fehrmann,
H.; Feldbaum, D.; Ferrante, I.; Fidecaro, F.; Finn, L. S.; Fiori,
I.; Fisher, R. P.; Flaminio, R.; Flanigan, M.; Foley, S.; Forsi, E.;
Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.; Franc, J.; Frasca,
S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey,
R.; Fricke, T. T.; Fridriksson, J. K.; Friedrich, D.; Fritschel, P.;
Frolov, V. V.; Fulda, P. J.; Fyffe, M.; Galimberti, M.; Gammaitoni,
L.; Ganija, M. R.; Garcia, J.; Garofoli, J. A.; Garufi, F.; Gáspár,
M. E.; Gemme, G.; Geng, R.; Genin, E.; Gennai, A.; Gergely, L. Á.;
Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Giazotto,
A.; Gill, C.; Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky,
M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Granata, M.; Grant, A.;
Gras, S.; Gray, C.; Gray, N.; Greenhalgh, R. J. S.; Gretarsson, A. M.;
Greverie, C.; Grosso, R.; Grote, H.; Grunewald, S.; Guidi, G. M.;
Guido, C.; Gupta, R.; Gustafson, E. K.; Gustafson, R.; Ha, T.; Hage,
B.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Hartman, M. T.; Haughian, K.; Hayama, K.; Hayau, J. -F.; Hayler,
T.; Heefner, J.; Heidmann, A.; Heintze, M. C.; Heitmann, H.; Hello,
P.; Hendry, M. A.; Heng, I. S.; Heptonstall, A. W.; Herrera, V.;
Hewitson, M.; Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Homan,
J.; Hong, T.; Hooper, S.; Hosken, D. J.; Hough, J.; Howell, E. J.;
Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.;
Inta, R.; Isogai, T.; Ivanov, A.; Izumi, K.; Jacobson, M.; Jang,
H.; Jaranowski, P.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones,
R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kamaretsos, I.; Kandhasamy,
S.; Kang, G.; Kanner, J. B.; Katsavounidis, E.; Katzman, W.; Kaufer,
H.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Keresztes, Z.; Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.;
Kim, B.; Kim, C.; Kim, D.; Kim, H.; Kim, K.; Kim, N.; Kim, Y. -M.;
King, P. J.; Kinsey, M.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.;
Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Korth, W. Z.;
Kowalska, I.; Kozak, D.; Kringel, V.; Krishnamurthy, S.; Krishnan,
B.; Krâ´Olak, A.; Kuehn, G.; Kumar, R.; Kwee, P.; Laas-Bourez, M.;
Lam, P. K.; Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lawrie,
C.; Lazzarini, A.; Leaci, P.; Lee, C. H.; Lee, H. M.; Leindecker,
N.; Leong, J. R.; Leonor, I.; Leroy, N.; Letendre, N.; Li, J.; Li,
T. G. F.; Liguori, N.; Lindquist, P. E.; Lockerbie, N. A.; Lodhia,
D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Luan, J.;
Lubinski, M.; Lück, H.; Lundgren, A. P.; MacDonald, E.; Machenschalk,
B.; Macinnis, M.; MacLeod, D. M.; Mageswaran, M.; Mailand, K.;
Majorana, E.; Maksimovic, I.; Man, N.; Mandel, I.; Mandic, V.;
Mantovani, M.; Marandi, A.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Markosyan, A.; Maros, E.; Marque, J.; Martelli, F.;
Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.;
Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala, N.; Mazzolo,
G.; McCarthy, R.; McClelland, D. E.; McDaniel, P.; McGuire, S. C.;
McIntyre, G.; McIver, J.; McKechan, D. J. A.; Meadors, G. D.; Mehmet,
M.; Meier, T.; Melatos, A.; Melissinos, A. C.; Mendell, G.; Menendez,
D.; Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Miao, H.;
Michel, C.; Milano, L.; Miller, J.; Minenkov, Y.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Moesta, P.;
Mohan, M.; Mohanty, S. D.; Mohapatra, S. R. P.; Moraru, D.; Moreno,
G.; Morgado, N.; Morgia, A.; Mori, T.; Mosca, S.; Mossavi, K.; Mours,
B.; Mow-Lowry, C. M.; Mueller, C. L.; Mueller, G.; Mukherjee, S.;
Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murphy, D.; Murray,
P. G.; Mytidis, A.; Nash, T.; Naticchioni, L.; Nawrodt, R.; Necula,
V.; Nelson, J.; Newton, G.; Nishizawa, A.; Nocera, F.; Nolting, D.;
Nuttall, L.; Ochsner, E.; O'Dell, J.; Oelker, E.; Ogin, G. H.; Oh,
J. J.; Oh, S. H.; Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.;
Osthelder, C.; Ott, C. D.; Ottaway, D. J.; Ottens, R. S.; Overmier,
H.; Owen, B. J.; Page, A.; Pagliaroli, G.; Palladino, L.; Palomba,
C.; Pan, Y.; Pankow, C.; Paoletti, F.; Papa, M. A.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pedraza,
M.; Peiris, P.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.;
Persichetti, G.; Phelps, M.; Pickenpack, M.; Piergiovanni, F.; Pietka,
M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi,
M. V.; Poggiani, R.; Pöld, J.; Postiglione, F.; Prato, M.; Predoi,
V.; Price, L. R.; Prijatelj, M.; Principe, M.; Privitera, S.; Prix,
R.; Prodi, G. A.; Prokhorov, L.; Puncken, O.; Punturo, M.; Puppo, P.;
Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Rácz, I.; Radkins, H.;
Raffai, P.; Rakhmanov, M.; Ramet, C. R.; Rankins, B.; Rapagnani, P.;
Rapoport, S.; Raymond, V.; Re, V.; Redwine, K.; Reed, C. M.; Reed,
T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.; Riesen, R.;
Riles, K.; Robertson, N. A.; Robinet, F.; Robinson, C.; Robinson,
E. L.; Rocchi, A.; Roddy, S.; Rodriguez, C.; Rodruck, M.; Rolland,
L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.; Rosińska,
D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Ryll,
H.; Sainathan, P.; Sakosky, M.; Salemi, F.; Samblowski, A.; Sammut,
L.; Sancho de La Jordana, L.; Sandberg, V.; Sankar, S.; Sannibale,
V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.; Sassolas,
B.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.;
Schilling, R.; Schlamminger, S.; Schnabel, R.; Schofield, R. M. S.;
Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.;
Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sentenac,
D.; Sergeev, A.; Shaddock, D. A.; Shaltev, M.; Shapiro, B.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.;
Singer, L.; Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Smith, R. J. E.; Somiya,
K.; Sorazu, B.; Soto, J.; Speirits, F. C.; Sperandio, L.; Stefszky,
M.; Stein, A. J.; Steinert, E.; Steinlechner, J.; Steinlechner, S.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S.;
Stroeer, A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.;
Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Tacca, M.;
Taffarello, L.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor,
J. R.; Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane,
E.; Thüring, A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.; Tonelli,
M.; Torre, O.; Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso,
F.; Traylor, G.; Trias, M.; Tseng, K.; Ugolini, D.; Urbanek, K.;
Vahlbruch, H.; Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.;
van den Broeck, C.; van der Putten, S.; van Veggel, A. A.; Vass, S.;
Vasuth, M.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.;
Veitch, J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.;
Viceré, A.; Villar, A. E.; Vinet, J. -Y.; Vitale, S.; Vitale, S.;
Vocca, H.; Vorvick, C.; Vyatchanin, S. P.; Wade, A.; Waldman, S. J.;
Wallace, L.; Wan, Y.; Wang, X.; Wang, Z.; Wanner, A.; Ward, R. L.; Was,
M.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen,
S.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.;
Whitcomb, S. E.; White, D.; Whiting, B. F.; Wilkinson, C.; Willems,
P. A.; Williams, H. R.; Williams, L.; Willke, B.; Winkelmann, L.;
Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Wittel, H.; Woan, G.;
Wooley, R.; Worden, J.; Yablon, J.; Yakushin, I.; Yamamoto, H.;
Yamamoto, K.; Yang, H.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.;
Yvert, M.; Zadroźny, A.; Zanolin, M.; Zendri, J. -P.; Zhang, F.;
Zhang, L.; Zhang, W.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker, M. E.;
Zweizig, J.; Akerlof, C.; Boer, M.; Fender, R.; Gehrels, N.; Klotz,
A.; Ofek, E. O.; Smith, M.; Sokolowski, M.; Stappers, B. W.; Steele,
I.; Swinbank, J.; Wijeres, R. A. M. J.
Bibcode: 2012A&A...539A.124L
Altcode: 2011arXiv1109.3498T; 2012A&A...539A.124A
Aims: A transient astrophysical event observed in both
gravitational wave (GW) and electromagnetic (EM) channels would yield
rich scientific rewards. A first program initiating EM follow-ups to
possible transient GW events has been developed and exercised by the
LIGO and Virgo community in association with several partners. In this
paper, we describe and evaluate the methods used to promptly identify
and localize GW event candidates and to request images of targeted sky
locations.
Methods: During two observing periods (Dec. 17, 2009
to Jan. 8, 2010 and Sep. 2 to Oct. 20, 2010), a low-latency analysis
pipeline was used to identify GW event candidates and to reconstruct
maps of possible sky locations. A catalog of nearby galaxies and
Milky Way globular clusters was used to select the most promising sky
positions to be imaged, and this directional information was delivered
to EM observatories with time lags of about thirty minutes. A Monte
Carlo simulation has been used to evaluate the low-latency GW pipeline's
ability to reconstruct source positions correctly.
Results:
For signals near the detection threshold, our low-latency algorithms
often localized simulated GW burst signals to tens of square degrees,
while neutron star/neutron star inspirals and neutron star/black hole
inspirals were localized to a few hundred square degrees. Localization
precision improves for moderately stronger signals. The correct sky
location of signals well above threshold and originating from nearby
galaxies may be observed with ~50% or better probability with a few
pointings of wide-field telescopes.
Title: Publisher's Note: Search for gravitational waves associated
with the August 2006 timing glitch of the Vela pulsar [Phys. Rev. D
83, 042001 (2011)]
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith,
P.; Allen, B.; Allen, G.; Amador Ceron, E.; Amin, R. S.; Anderson,
S. B.; Anderson, W. G.; Arain, M. A.; Araya, M.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker,
D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista, M.; Bennett,
M. F.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.;
Bland, B.; Bock, O.; Bodiya, T. P.; Bondarescu, R.; Bork, R.; Born,
M.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer,
J.; Bridges, D. O.; Brinkmann, M.; Britzger, M.; Brooks, A. F.;
Brown, D. A.; Bullington, A.; Buonanno, A.; Burmeister, O.; Byer,
R. L.; Cadonati, L.; Cain, J.; Camp, J. B.; Cannizzo, J.; Cannon,
K. C.; Cao, J.; Capano, C.; Cardenas, L.; Caudill, S.; Cavaglià, M.;
Cepeda, C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chatterji,
S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Chua, S. S. Y.; Chung,
C. T. Y.; Clark, D.; Clark, J.; Clayton, J. H.; Conte, R.; Cook, D.;
Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Dahl, K.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; Dayanga, T.; DeBra, D.; Degallaix, J.;
Dergachev, V.; DeSalvo, R.; Dhurandhar, S.; Díaz, M.; Donovan, F.;
Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Driggers, J.; Dueck,
J.; Duke, I.; Dumas, J. -C.; Dwyer, S.; Edgar, M.; Edwards, M.; Effler,
A.; Ehrens, P.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Faltas,
Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Finn, L. S.; Flasch, K.; Foley,
S.; Forrest, C.; Fotopoulos, N.; Frede, M.; Frei, M.; Frei, Z.; Freise,
A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov,
V. V.; Fulda, P.; Fyffe, M.; Garofoli, J. A.; Ghosh, S.; Giaime, J. A.;
Giampanis, S.; Giardina, K. D.; Goetz, E.; Goggin, L. M.; González,
G.; Goßler, S.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Grosso, R.; Grote, H.; Grunewald, S.; Gustafson,
E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer, D.; Hammond,
G. D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.;
Harstad, E. D.; Haughian, K.; Hayama, K.; Hayler, T.; Heefner, J.;
Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose, E.;
Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough, J.; Howell,
E.; Hoyland, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Ingram, D. R.;
Isogai, T.; Ivanov, A.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones,
R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy, S.; Kanner, J.;
Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.;
Keppel, D. G.; Khalaidovski, A.; Khalili, F. Y.; Khan, R.; Khazanov,
E.; Kim, H.; King, P. J.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.;
Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.; Kringel, V.;
Krishnan, B.; Kuehn, G.; Kullman, J.; Kumar, R.; Kwee, P.; Lam, P. K.;
Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lazzarini, A.; Leaci,
P.; Lei, M.; Leindecker, N.; Leonor, I.; Lin, H.; Lindquist, P. E.;
Littenberg, T. B.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu, P.;
Lubinski, M.; Lucianetti, A.; Lück, H.; Lundgren, A.; Machenschalk,
B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Mak, C.; Mandel,
I.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.; Markowitz,
J.; Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.;
Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.;
McClelland, D. E.; McGuire, S. C.; McIntyre, G.; McKechan, D. J. A.;
Mehmet, M.; Melatos, A.; Melissinos, A. C.; Mendell, G.; Menéndez,
D. F.; Mercer, R. A.; Merrill, L.; Meshkov, S.; Messenger, C.; Meyer,
M. S.; Miao, H.; Miller, J.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moreno, G.; Mors, K.; Mossavi, K.; MowLowry, C.;
Mueller, G.; Müller-Ebhardt, H.; Mukherjee, S.; Mullavey, A.; Munch,
J.; Murray, P. G.; Nash, T.; Nawrodt, R.; Nelson, J.; Newton, G.;
Nishida, E.; Nishizawa, A.; O'Dell, J.; O'Reilly, B.; O'Shaughnessy,
R.; Ochsner, E.; Ogin, G. H.; Oldenburg, R.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Page, A.; Pan, Y.; Pankow, C.; Papa,
M. A.; Patel, P.; Pathak, D.; Pedraza, M.; Pekowsky, L.; Penn, S.;
Peralta, C.; Perreca, A.; Pickenpack, M.; Pinto, I. M.; Pitkin, M.;
Pletsch, H. J.; Plissi, M. V.; Postiglione, F.; Principe, M.; Prix,
R.; Prokhorov, L.; Puncken, O.; Quetschke, V.; Raab, F. J.; Rabeling,
D. S.; Radkins, H.; Raffai, P.; Raics, Z.; Rakhmanov, M.; Raymond,
V.; Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.;
Riesen, R.; Riles, K.; Roberts, P.; Robertson, N. A.; Robinson, C.;
Robinson, E. L.; Roddy, S.; Röver, C.; Rollins, J.; Romano, J. D.;
Romie, J. H.; Rowan, S.; Rüdiger, A.; Ryan, K.; Sakata, S.; Sammut,
L.; Sancho de la Jordana, L.; Sandberg, V.; Sannibale, V.; Santamaría,
L.; Santostasi, G.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato,
S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schulz, B.; Schutz, B. F.; Schwinberg,
P.; Scott, J.; Scott, S. M.; Searle, A. C.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Sergeev, A.; Shapiro, B.; Shawhan, P.; Shoemaker,
D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sintes, A. M.; Skelton,
G.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.;
Smith, N. D.; Somiya, K.; Sorazu, B.; Speirits, F.; Stein, A. J.;
Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.;
Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.; Sung,
M.; Susmithan, S.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.;
Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.; Thorne,
K. A.; Thorne, K. S.; Thüring, A.; Titsler, C.; Tokmakov, K. V.;
Torres, C.; Torrie, C. I.; Traylor, G.; Trias, M.; Turner, L.; Ugolini,
D.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; Van Den Broeck,
C.; van der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin, R.;
Vecchio, A.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Villar, A.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Wanner,
A.; Ward, R. L.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss,
R.; Wen, L.; Wen, S.; Wessels, P.; West, M.; Westphal, T.; Wette,
K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut,
I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan,
G.; Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto,
K.; Yeaton-Massey, D.; Yoshida, S.; Zanolin, M.; Zhang, L.; Zhang,
Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.; Buchner, S.
Bibcode: 2012PhRvD..85h9902A
Altcode:
No abstract at ADS
Title: Search for gravitational waves from low mass compact binary
coalescence in LIGO's sixth science run and Virgo's science runs 2
and 3
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.;
Abernathy, M.; Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.;
Affeldt, C.; Agathos, M.; Ajith, P.; Allen, B.; Allen, G. S.; Amador
Ceron, E.; Amariutei, D.; Amin, R. S.; Anderson, S. B.; Anderson,
W. G.; Arai, K.; Arain, M. A.; Araya, M. C.; Aston, S. M.; Astone,
P.; Atkinson, D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.;
Baker, P.; Ballardin, G.; Ballmer, S.; Barker, D.; Barone, F.; Barr,
B.; Barriga, P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos,
I.; Bassiri, R.; Bastarrika, M.; Basti, A.; Batch, J.; Bauchrowitz, J.;
Bauer, Th. S.; Bebronne, M.; Behnke, B.; Beker, M. G.; Bell, A. S.;
Belletoile, A.; Belopolski, I.; Benacquista, M.; Berliner, J. M.;
Bertolini, A.; Betzwieser, J.; Beveridge, N.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas, R.; Bitossi,
M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.;
Blair, D.; Bland, B.; Blom, M.; Bock, O.; Bodiya, T. P.; Bogan,
C.; Bondarescu, R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.;
Born, M.; Boschi, V.; Bose, S.; Bosi, L.; Bouhou, B.; Braccini, S.;
Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brau,
J. E.; Breyer, J.; Briant, T.; Bridges, D. O.; Brillet, A.; Brinkmann,
M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Brummit,
A.; Bulik, T.; Bulten, H. J.; Buonanno, A.; Burguet–Castell, J.;
Burmeister, O.; Buskulic, D.; Buy, C.; Byer, R. L.; Cadonati, L.;
Cagnoli, G.; Calloni, E.; Camp, J. B.; Campsie, P.; Cannizzo, J.;
Cannon, K.; Canuel, B.; Cao, J.; Capano, C. D.; Carbognani, F.;
Caride, S.; Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri,
R.; Cella, G.; Cepeda, C.; Cesarini, E.; Chaibi, O.; Chalermsongsak,
T.; Chalkley, E.; Charlton, P.; Chassande-Mottin, E.; Chelkowski, S.;
Chen, Y.; Chincarini, A.; Chiummo, A.; Cho, H.; Christensen, N.; Chua,
S. S. Y.; Chung, C. T. Y.; Chung, S.; Ciani, G.; Clara, F.; Clark,
D. E.; Clark, J.; Clayton, J. H.; Cleva, F.; Coccia, E.; Cohadon,
P. -F.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini, M.; Conte,
A.; Conte, R.; Cook, D.; Corbitt, T. R.; Cordier, M.; Cornish, N.;
Corsi, A.; Costa, C. A.; Coughlin, M.; Coulon, J. -P.; Couvares, P.;
Coward, D. M.; Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.;
Cruise, A. M.; Cumming, A.; Cunningham, L.; Cuoco, E.; Cutler, R. M.;
Dahl, K.; Danilishin, S. L.; Dannenberg, R.; D'Antonio, S.; Danzmann,
K.; Dattilo, V.; Daudert, B.; Daveloza, H.; Davier, M.; Davies, G.;
Daw, E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra, D.; Debreczeni,
G.; Degallaix, J.; Del Pozzo, W.; del Prete, M.; Dent, T.; Dergachev,
V.; DeRosa, R.; DeSalvo, R.; Dhurandhar, S.; Di Fiore, L.; Di Lieto,
A.; Di Palma, I.; Di Paolo Emilio, M.; Di Virgilio, A.; Díaz, M.;
Dietz, A.; DiGuglielmo, J.; Donovan, F.; Dooley, K. L.; Dorsher, S.;
Drago, M.; Drever, R. W. P.; Driggers, J. C.; Du, Z.; Dumas, J. -C.;
Dwyer, S.; Eberle, T.; Edgar, M.; Edwards, M.; Effler, A.; Ehrens,
P.; Endrőczi, G.; Engel, R.; Etzel, T.; Evans, K.; Evans, M.; Evans,
T.; Factourovich, M.; Fafone, V.; Fairhurst, S.; Fan, Y.; Farr, B. F.;
Farr, W.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Ferrante, I.; Fidecaro,
F.; Finn, L. S.; Fiori, I.; Fisher, R. P.; Flaminio, R.; Flanigan, M.;
Foley, S.; Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.;
Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.;
Freise, A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.;
Frolov, V. V.; Fulda, P. J.; Fyffe, M.; Galimberti, M.; Gammaitoni,
L.; Ganija, M. R.; Garcia, J.; Garofoli, J. A.; Garufi, F.; Gáspár,
M. E.; Gemme, G.; Geng, R.; Genin, E.; Gennai, A.; Gergely, L. Á.;
Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Giazotto,
A.; Gill, C.; Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky,
M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Granata, M.; Grant, A.;
Gras, S.; Gray, C.; Gray, N.; Greenhalgh, R. J. S.; Gretarsson,
A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald, S.; Guidi,
G. M.; Guido, C.; Gupta, R.; Gustafson, E. K.; Gustafson, R.; Ha, T.;
Hage, B.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna,
C.; Hanson, J.; Hardt, A.; Harms, J.; Harry, G. M.; Harry, I. W.;
Harstad, E. D.; Hartman, M. T.; Haughian, K.; Hayama, K.; Hayau,
J. -F.; Heefner, J.; Heidmann, A.; Heintze, M. C.; Heitmann, H.;
Hello, P.; Hendry, M. A.; Heng, I. S.; Heptonstall, A. W.; Herrera,
V.; Hewitson, M.; Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Hong, T.;
Hooper, S.; Hosken, D. J.; Hough, J.; Howell, E. J.; Hughey, B.; Husa,
S.; Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.; Inta, R.; Isogai,
T.; Ivanov, A.; Izumi, K.; Jacobson, M.; Jang, H.; Jaranowski, P.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.;
Kalogera, V.; Kamaretsos, I.; Kandhasamy, S.; Kang, G.; Kanner, J. B.;
Katsavounidis, E.; Katzman, W.; Kaufer, H.; Kawabe, K.; Kawamura, S.;
Kawazoe, F.; Kells, W.; Keppel, D. G.; Keresztes, Z.; Khalaidovski,
A.; Khalili, F. Y.; Khazanov, E. A.; Kim, B.; Kim, C.; Kim, D.; Kim,
H.; Kim, K.; Kim, N.; Kim, Y. -M.; King, P. J.; Kinsey, M.; Kinzel,
D. L.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.;
Kopparapu, R.; Koranda, S.; Korth, W. Z.; Kowalska, I.; Kozak, D.;
Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Królak, A.; Kuehn,
G.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lang, M.; Lantz, B.;
Lastzka, N.; Lawrie, C.; Lazzarini, A.; Leaci, P.; Lee, C. H.; Lee,
H. M.; Leindecker, N.; Leong, J. R.; Leonor, I.; Leroy, N.; Letendre,
N.; Li, J.; Li, T. G. F.; Liguori, N.; Lindquist, P. E.; Lockerbie,
N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo,
G.; Luan, J.; Lubinski, M.; Lück, H.; Lundgren, A. P.; Macdonald,
E.; Machenschalk, B.; MacInnis, M.; Macleod, D. M.; Mageswaran,
M.; Mailand, K.; Majorana, E.; Maksimovic, I.; Man, N.; Mandel, I.;
Mandic, V.; Mantovani, M.; Marandi, A.; Marchesoni, F.; Marion,
F.; Márka, S.; Márka, Z.; Markosyan, A.; Maros, E.; Marque, J.;
Martelli, F.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.;
Masserot, A.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala,
N.; Mazzolo, G.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.;
McIntyre, G.; McIver, J.; McKechan, D. J. A.; Meadors, G. D.; Mehmet,
M.; Meier, T.; Melatos, A.; Melissinos, A. C.; Mendell, G.; Menendez,
D.; Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Miao, H.;
Michel, C.; Milano, L.; Miller, J.; Minenkov, Y.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Moesta, P.;
Mohan, M.; Mohanty, S. D.; Mohapatra, S. R. P.; Moraru, D.; Moreno,
G.; Morgado, N.; Morgia, A.; Mori, T.; Mosca, S.; Mossavi, K.; Mours,
B.; Mow-Lowry, C. M.; Mueller, C. L.; Mueller, G.; Mukherjee, S.;
Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murphy, D.; Murray,
P. G.; Mytidis, A.; Nash, T.; Naticchioni, L.; Nawrodt, R.; Necula,
V.; Nelson, J.; Newton, G.; Nishizawa, A.; Nocera, F.; Nolting, D.;
Nuttall, L.; Ochsner, E.; O'Dell, J.; Oelker, E.; Ogin, G. H.; Oh,
J. J.; Oh, S. H.; Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.;
Osthelder, C.; Ott, C. D.; Ottaway, D. J.; Ottens, R. S.; Overmier,
H.; Owen, B. J.; Page, A.; Pagliaroli, G.; Palladino, L.; Palomba,
C.; Pan, Y.; Pankow, C.; Paoletti, F.; Papa, M. A.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pedraza,
M.; Peiris, P.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.;
Persichetti, G.; Phelps, M.; Pickenpack, M.; Piergiovanni, F.;
Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Poggiani, R.; Pöld, J.; Postiglione, F.; Prato, M.;
Predoi, V.; Price, L. R.; Prijatelj, M.; Principe, M.; Privitera,
S.; Prix, R.; Prodi, G. A.; Prokhorov, L.; Puncken, O.; Punturo, M.;
Puppo, P.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Rácz, I.;
Radkins, H.; Raffai, P.; Rakhmanov, M.; Ramet, C. R.; Rankins, B.;
Rapagnani, P.; Raymond, V.; Re, V.; Redwine, K.; Reed, C. M.; Reed,
T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.; Riesen, R.;
Riles, K.; Robertson, N. A.; Robinet, F.; Robinson, C.; Robinson,
E. L.; Rocchi, A.; Roddy, S.; Rodriguez, C.; Rodruck, M.; Rolland,
L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.; Rosińska,
D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Ryll,
H.; Sainathan, P.; Sakosky, M.; Salemi, F.; Samblowski, A.; Sammut,
L.; Sancho de la Jordana, L.; Sandberg, V.; Sankar, S.; Sannibale,
V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.; Sassolas,
B.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.;
Schilling, R.; Schlamminger, S.; Schnabel, R.; Schofield, R. M. S.;
Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.;
Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sentenac,
D.; Sergeev, A.; Shaddock, D. A.; Shaltev, M.; Shapiro, B.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.;
Singer, L.; Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Smith, R. J. E.; Somiya,
K.; Sorazu, B.; Soto, J.; Speirits, F. C.; Sperandio, L.; Stefszky,
M.; Stein, A. J.; Steinert, E.; Steinlechner, J.; Steinlechner, S.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin,
S.; Stroeer, A. S.; Sturani, R.; Stuver, A. L.; Summerscales,
T. Z.; Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Tacca,
M.; Taffarello, L.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.;
Taylor, J. R.; Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.;
Thrane, E.; Thüring, A.; Titsler, C.; Tokmakov, K. V.; Toncelli,
A.; Tonelli, M.; Torre, O.; Torres, C.; Torrie, C. I.; Tournefier,
E.; Travasso, F.; Traylor, G.; Trias, M.; Tseng, K.; Tucker, E.;
Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vajente, G.; Vallisneri,
M.; van den Brand, J. F. J.; Van Den Broeck, C.; van der Putten, S.;
van Veggel, A. A.; Vass, S.; Vasuth, M.; Vaulin, R.; Vavoulidis, M.;
Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Veltkamp, C.;
Verkindt, D.; Vetrano, F.; Viceré, A.; Villar, A. E.; Vinet, J. -Y.;
Vitale, S.; Vitale, S.; Vocca, H.; Vorvick, C.; Vyatchanin, S. P.;
Wade, A.; Waldman, S. J.; Wallace, L.; Wan, Y.; Wang, X.; Wang, Z.;
Wanner, A.; Ward, R. L.; Was, M.; Wei, P.; Weinert, M.; Weinstein,
A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels, P.; West, M.; Westphal,
T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; White, D.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.;
Wittel, H.; Woan, G.; Wooley, R.; Worden, J.; Yablon, J.; Yakushin,
I.; Yamamoto, H.; Yamamoto, K.; Yang, H.; Yeaton-Massey, D.; Yoshida,
S.; Yu, P.; Yvert, M.; Zadroźny, A.; Zanolin, M.; Zendri, J. -P.;
Zhang, F.; Zhang, L.; Zhang, W.; Zhang, Z.; Zhao, C.; Zotov, N.;
Zucker, M. E.; Zweizig, J.
Bibcode: 2012PhRvD..85h2002A
Altcode: 2011arXiv1111.7314T; 2011arXiv1111.7314S
We report on a search for gravitational waves from coalescing compact
binaries using LIGO and Virgo observations between July 7, 2009, and
October 20, 2010. We searched for signals from binaries with total mass
between 2 and 25M⊙; this includes binary neutron stars,
binary black holes, and binaries consisting of a black hole and neutron
star. The detectors were sensitive to systems up to 40 Mpc distant
for binary neutron stars, and further for higher mass systems. No
gravitational-wave signals were detected. We report upper limits on
the rate of compact binary coalescence as a function of total mass,
including the results from previous LIGO and Virgo observations. The
cumulative 90% confidence rate upper limits of the binary coalescence
of binary neutron star, neutron star-black hole, and binary black
hole systems are 1.3×10-4, 3.1×10-5, and
6.4×10-6Mpc-3yr-1, respectively. These
upper limits are up to a factor 1.4 lower than previously derived
limits. We also report on results from a blind injection challenge.
Title: Publisher's Note: Search for gravitational waves from
compact binary coalescence in LIGO and Virgo data from S5 and VSR1
[Phys. Rev. D 82, 102001 (2010)]
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.; Accadia,
T.; Acernese, F.; Adams, C.; Adhikari, R.; Ajith, P.; Allen, B.;
Allen, G.; Amador Ceron, E.; Amin, R. S.; Anderson, S. B.; Anderson,
W. G.; Antonucci, F.; Arain, M. A.; Araya, M.; Aronsson, M.; Arun,
K. G.; Aso, Y.; Aston, S.; Astone, P.; Atkinson, D. E.; Aufmuth,
P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.; Ballinger, T.;
Ballmer, S.; Barker, D.; Barnum, S.; Barone, F.; Barr, B.; Barriga,
P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri,
R.; Bastarrika, M.; Bauchrowitz, J.; Bauer, Th. S.; Behnke, B.; Beker,
M. G.; Belletoile, A.; Benacquista, M.; Bertolini, A.; Betzwieser,
J.; Beveridge, N.; Beyersdorf, P. T.; Bigotta, S.; Bilenko, I. A.;
Billingsley, G.; Birch, J.; Birindelli, S.; Biswas, R.; Bitossi,
M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.;
Blair, D.; Bland, B.; Blom, M.; Boccara, C.; Bock, O.; Bodiya,
T. P.; Bondarescu, R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork,
R.; Born, M.; Bose, S.; Bosi, L.; Bouhou, B.; Boyle, M.; Braccini,
S.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Breyer, J.; Bridges, D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.;
Britzger, M.; Brooks, A. F.; Brown, D. A.; Budzyński, R.; Bulik,
T.; Bulten, H. J.; Buonanno, A.; Burguet-Castell, J.; Burmeister, O.;
Buskulic, D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Cain,
J.; Calloni, E.; Camp, J. B.; Campagna, E.; Campsie, P.; Cannizzo,
J.; Cannon, K. C.; Canuel, B.; Cao, J.; Capano, C.; Carbognani, F.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chalermsongsak, T.; Chalkley, E.; Charlton,
P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, Y.; Chincarini, A.;
Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.; Clark, D.; Clark,
J.; Clayton, J. H.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas, J.;
Colla, A.; Colombini, M.; Conte, R.; Cook, D.; Corbitt, T. R.; Cornish,
N.; Corsi, A.; Costa, C. A.; Coulon, J. -P.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Cuoco, E.; Dahl, K.; Danilishin, S. L.;
Dannenberg, R.; D'Antonio, S.; Danzmann, K.; Das, K.; Dattilo, V.;
Daudert, B.; Davier, M.; Davies, G.; Davis, A.; Daw, E. J.; Day,
R.; Dayanga, T.; De Rosa, R.; DeBra, D.; Degallaix, J.; del Prete,
M.; Dergachev, V.; DeRosa, R.; DeSalvo, R.; Devanka, P.; Dhurandhar,
S.; Di Fiore, L.; Di Lieto, A.; Di Palma, I.; Di Paolo Emilio, M.;
Di Virgilio, A.; Díaz, M.; Dietz, A.; Donovan, F.; Dooley, K. L.;
Doomes, E. E.; Dorsher, S.; Douglas, E. S. D.; Drago, M.; Drever,
R. W. P.; Driggers, J. C.; Dueck, J.; Dumas, J. -C.; Dwyer, S.; Eberle,
T.; Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.; Ely, G.; Engel,
R.; Etzel, T.; Evans, M.; Evans, T.; Fafone, V.; Fairhurst, S.; Fan,
Y.; Farr, B. F.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Ferrante,
I.; Fidecaro, F.; Finn, L. S.; Fiori, I.; Flaminio, R.; Flanigan,
M.; Flasch, K.; Foley, S.; Forrest, C.; Forsi, E.; Fotopoulos, N.;
Fournier, J. -D.; Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich,
D.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Galimberti,
M.; Gammaitoni, L.; Garofoli, J. A.; Garufi, F.; Gemme, G.; Genin,
E.; Gennai, A.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina,
K. D.; Giazotto, A.; Gill, C.; Goetz, E.; Goggin, L. M.; González,
G.; Goßler, S.; Gouaty, R.; Graef, C.; Granata, M.; Grant, A.; Gras,
S.; Gray, C.; Greenhalgh, R. J. S.; Gretarsson, A. M.; Greverie,
C.; Grosso, R.; Grote, H.; Grunewald, S.; Guidi, G. M.; Gustafson,
E. K.; Gustafson, R.; Hage, B.; Hall, P.; Hallam, J. M.; Hammer,
D.; Hammond, G.; Hanks, J.; Hanna, C.; Hanson, J.; Harms, J.; Harry,
G. M.; Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.; Hayau,
J. -F.; Hayler, T.; Heefner, J.; Heitmann, H.; Hello, P.; Heng, I. S.;
Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge,
K. A.; Holt, K.; Hosken, D. J.; Hough, J.; Howell, E.; Hoyland, D.;
Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.;
Ingram, D. R.; Inta, R.; Isogai, T.; Ivanov, A.; Jaranowski, P.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kandhasamy, S.; Kanner, J.; Katsavounidis, E.;
Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.; Kim, H.; King,
P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.; Kondrashov, V.;
Kopparapu, R.; Koranda, S.; Kowalska, I.; Kozak, D.; Krause, T.;
Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Królak, A.; Kuehn, G.;
Kullman, J.; Kumar, R.; Kwee, P.; Landry, M.; Lang, M.; Lantz, B.;
Lastzka, N.; Lazzarini, A.; Leaci, P.; Leong, J.; Leonor, I.; Leroy,
N.; Letendre, N.; Li, J.; Li, T. G. F.; Lin, H.; Lindquist, P. E.;
Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.;
Losurdo, G.; Lu, P.; Luan, J.; Lubinski, M.; Lucianetti, A.; Lück,
H.; Lundgren, A.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Mak, C.; Maksimovic, I.; Man, N.; Mandel,
I.; Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.;
Meadors, G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.;
Miller, J.; Minenkov, Y.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Moe, B.; Mohan, M.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moraru, D.; Moreau, J.; Moreno, G.; Morgado,
N.; Morgia, A.; Mors, K.; Mosca, S.; Moscatelli, V.; Mossavi, K.;
Mours, B.; MowLowry, C.; Mueller, G.; Mukherjee, S.; Mullavey, A.;
Müller-Ebhardt, H.; Munch, J.; Murray, P. G.; Nash, T.; Nawrodt,
R.; Nelson, J.; Neri, I.; Newton, G.; Nishida, E.; Nishizawa, A.;
Nocera, F.; Nolting, D.; Ochsner, E.; O'Dell, J.; Ogin, G. H.;
Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.;
Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page,
A.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow,
C.; Paoletti, F.; Papa, M. A.; Pardi, S.; Pareja, M.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pathak,
D.; Pedraza, M.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.;
Persichetti, G.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.; Pietka,
M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi,
M. V.; Poggiani, R.; Postiglione, F.; Prato, M.; Predoi, V.; Price,
L. R.; Prijatelj, M.; Principe, M.; Prix, R.; Prodi, G. A.; Prokhorov,
L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Raab, F. J.;
Rabeling, D. S.; Radke, T.; Radkins, H.; Raffai, P.; Rakhmanov, M.;
Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Reed, C. M.; Reed,
T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.; Riesen, R.;
Riles, K.; Roberts, P.; Robertson, N. A.; Robinet, F.; Robinson,
C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Röver, C.; Rolland, L.;
Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.; Rosińska, D.;
Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sakata, S.; Sakosky,
M.; Salemi, F.; Sammut, L.; Sancho de la Jordana, L.; Sandberg, V.;
Sannibale, V.; Santamaría, L.; Santostasi, G.; Saraf, S.; Sassolas,
B.; Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.; Saulson, P. R.;
Savage, R.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz, B.;
Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.;
Seifert, F.; Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sergeev, A.;
Shaddock, D.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley,
A.; Siemens, X.; Sigg, D.; Singer, A.; Sintes, A. M.; Skelton, G.;
Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Smith,
N. D.; Somiya, K.; Sorazu, B.; Speirits, F. C.; Sperandio, L.; Stein,
A. J.; Stein, L. C.; Steinlechner, S.; Steplewski, S.; Stochino,
A.; Stone, R.; Strain, K. A.; Strigin, S.; Stroeer, A.; Sturani, R.;
Stuver, A. L.; Summerscales, T. Z.; Sung, M.; Susmithan, S.; Sutton,
P. J.; Swinkels, B.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.;
Taylor, J. R.; Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.;
Thrane, E.; Thüring, A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.;
Tonelli, M.; Torre, O.; Torres, C.; Torrie, C. I.; Tournefier, E.;
Travasso, F.; Traylor, G.; Trias, M.; Trummer, J.; Tseng, K.; Turner,
L.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vaishnav, B.; Vajente,
G.; Vallisneri, M.; van den Brand, J. F. J.; Van Den Broeck, C.;
van der Putten, S.; van der Sluys, M. V.; van Veggel, A. A.; Vass,
S.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.; Veitch,
J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.; Viceré,
A.; Villar, A.; Vinet, J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin,
S. P.; Waldman, S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Was,
M.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen,
S.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.;
Whitcomb, S. E.; White, D. J.; Whiting, B. F.; Wilkinson, C.; Willems,
P. A.; Williams, L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf,
C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Yakushin,
I.; Yamamoto, H.; Yamamoto, K.; Yeaton-Massey, D.; Yoshida, S.; Yu,
P. P.; Yvert, M.; Zanolin, M.; Zhang, L.; Zhang, Z.; Zhao, C.; Zotov,
N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2012PhRvD..85h9903A
Altcode:
No abstract at ADS
Title: Publisher's Note: Search for gravitational waves from binary
black hole inspiral, merger, and ringdown [Phys. Rev. D 83, 122005
(2011)]
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.;
Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.; Ajith, P.; Allen,
B.; Allen, G. S.; Amador Ceron, E.; Amin, R. S.; Anderson, S. B.;
Anderson, W. G.; Antonucci, F.; Arain, M. A.; Araya, M. C.; Aronsson,
M.; Aso, Y.; Aston, S. M.; Astone, P.; Atkinson, D.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.; Ballinger, T.;
Ballmer, S.; Barker, D.; Barnum, S.; Barone, F.; Barr, B.; Barriga,
P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri,
R.; Bastarrika, M.; Bauchrowitz, J.; Bauer, Th. S.; Behnke, B.; Beker,
M. G.; Belletoile, A.; Benacquista, M.; Bertolini, A.; Betzwieser,
J.; Beveridge, N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Birch, J.; Birindelli, S.; Biswas, R.; Bitossi, M.; Bizouard,
M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland,
B.; Blom, M.; Boccara, C.; Bock, O.; Bodiya, T. P.; Bondarescu, R.;
Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Boschi, V.;
Bose, S.; Bosi, L.; Bouhou, B.; Boyle, M.; Braccini, S.; Bradaschia,
C.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges,
D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks,
A. F.; Brown, D. A.; Budzyński, R.; Bulik, T.; Bulten, H. J.;
Buonanno, A.; Burguet–Castell, J.; Burmeister, O.; Buskulic, D.;
Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Cain, J.; Calloni,
E.; Camp, J. B.; Campagna, E.; Campsie, P.; Cannizzo, J.; Cannon, K.;
Canuel, B.; Cao, J.; Capano, C.; Carbognani, F.; Caride, S.; Caudill,
S.; Cavagliá, M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.;
Cesarini, E.; Chaibi, O.; Chalermsongsak, T.; Chalkley, E.; Charlton,
P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, Y.; Chincarini, A.;
Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.; Clark, D.; Clark,
J.; Clayton, J. H.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas,
J.; Colla, A.; Colombini, M.; Conte, R.; Cook, D.; Corbitt, T. R.;
Cornish, N.; Corsi, A.; Costa, C. A.; Coulon, J. -P.; Coward, D. M.;
Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.;
Culter, R. M.; Cumming, A.; Cunningham, L.; Cuoco, E.; Dahl, K.;
Danilishin, S. L.; Dannenberg, R.; D'Antonio, S.; Danzmann, K.; Das,
K.; Dattilo, V.; Daudert, B.; Davier, M.; Davies, G.; Davis, A.; Daw,
E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra, D.; Debreczeni, G.;
Degallaix, J.; del Prete, M.; Dergachev, V.; DeRosa, R.; DeSalvo, R.;
Devanka, P.; Dhurandhar, S.; Di Fiore, L.; Di Lieto, A.; Di Palma,
I.; Di Paolo Emilio, M.; Di Virgilio, A.; Díaz, M.; Dietz, A.;
Donovan, F.; Dooley, K. L.; Doomes, E. E.; Dorsher, S.; Douglas,
E. S. D.; Drago, M.; Drever, R. W. P.; Driggers, J. C.; Dueck, J.;
Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar, M.; Edwards, M.; Effler,
A.; Ehrens, P.; Ely, G.; Engel, R.; Etzel, T.; Evans, M.; Evans, T.;
Fafone, V.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Fazi, D.; Fehrmann,
H.; Feldbaum, D.; Ferrante, I.; Fidecaro, F.; Finn, L. S.; Fiori,
I.; Flaminio, R.; Flanigan, M.; Flasch, K.; Foley, S.; Forrest,
C.; Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.;
Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.;
Freise, A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.;
Frolov, V. V.; Fulda, P.; Fyffe, M.; Galimberti, M.; Gammaitoni, L.;
Garofoli, J. A.; Garufi, F.; Gáspár, M. E.; Gemme, G.; Genin, E.;
Gennai, A.; Gholami, I.; Ghosh, S.; Giaime, J. A.; Giampanis, S.;
Giardina, K. D.; Giazotto, A.; Gill, C.; Goetz, E.; Goggin, L. M.;
González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.;
Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald,
S.; Guidi, G. M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hall,
P.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Haughian, K.; Hayama, K.; Hayau, J. -F.; Hayler, T.; Heefner, J.;
Heitmann, H.; Hello, P.; Heng, I. S.; Heptonstall, A. W.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken,
D. J.; Hough, J.; Howell, E. J.; Hoyland, D.; Huet, D.; Hughey, B.;
Husa, S.; Huttner, S. H.; Huynh–Dinh, T.; Ingram, D. R.; Inta, R.;
Isogai, T.; Ivanov, A.; Jaranowski, P.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kanner, J. B.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.;
Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khazanov, E. A.; Kim, H.; King, P. J.; Kinzel, D. L.; Kissel,
J. S.; Klimenko, S.; Kondrashov, V.; Kopparapu, R.; Koranda, S.;
Kowalska, I.; Kozak, D.; Krause, T.; Kringel, V.; Krishnamurthy,
S.; Krishnan, B.; Królak, A.; Kuehn, G.; Kullman, J.; Kumar, R.;
Kwee, P.; Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lazzarini,
A.; Leaci, P.; Leong, J.; Leonor, I.; Leroy, N.; Letendre, N.; Li,
J.; Li, T. G. F.; Liguori, N.; Lin, H.; Lindquist, P. E.; Lockerbie,
N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo,
G.; Lu, P.; Luan, J.; Lubinski, M.; Lucianetti, A.; Lück, H.;
Lundgren, A. D.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Mak, C.; Maksimovic, I.; Man, N.; Mandel,
I.; Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.;
Meadors, G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.;
Miller, J.; Minenkov, Y.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Moe, B.; Mohan, M.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moraru, D.; Moreau, J.; Moreno, G.; Morgado,
N.; Morgia, A.; Morioka, T.; Mors, K.; Mosca, S.; Moscatelli, V.;
Mossavi, K.; Mours, B.; Mow–Lowry, C. M.; Mueller, G.; Mukherjee,
S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murray, P. G.;
Nash, T.; Nawrodt, R.; Nelson, J.; Neri, I.; Newton, G.; Nishizawa,
A.; Nocera, F.; Nolting, D.; Ochsner, E.; O'Dell, J.; Ogin, G. H.;
Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.;
Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page,
A.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow,
C.; Paoletti, F.; Papa, M. A.; Pardi, S.; Pareja, M.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pathak,
D.; Pedraza, M.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.;
Persichetti, G.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.; Pietka,
M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi,
M. V.; Poggiani, R.; Postiglione, F.; Prato, M.; Predoi, V.; Price,
L. R.; Prijatelj, M.; Principe, M.; Prix, R.; Prodi, G. A.; Prokhorov,
L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Raab,
F. J.; Rabeling, D. S.; Rácz, I.; Radke, T.; Radkins, H.; Raffai,
P.; Rakhmanov, M.; Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.;
Reed, C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci,
F.; Riesen, R.; Riles, K.; Roberts, P.; Robertson, N. A.; Robinet,
F.; Robinson, C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Rolland,
L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.; Rosińska,
D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sakata,
S.; Sakosky, M.; Salemi, F.; Sammut, L.; Sancho de la Jordana, L.;
Sandberg, V.; Sannibale, V.; Santamaría, L.; Santostasi, G.; Saraf,
S.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.;
Saulson, P. R.; Savage, R.; Schilling, R.; Schnabel, R.; Schofield,
R. M. S.; Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott,
S. M.; Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.;
Sentenac, D.; Sergeev, A.; Shaddock, D. A.; Shapiro, B.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.;
Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Speirits,
F. C.; Sperandio, L.; Stein, A. J.; Stein, L. C.; Steinlechner, S.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S.;
Stroeer, A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sung,
M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Szokoly, G. P.; Tacca,
M.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.;
Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.;
Thüring, A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.;
Torre, O.; Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso, F.;
Traylor, G.; Trias, M.; Tseng, K.; Turner, L.; Ugolini, D.; Urbanek,
K.; Vahlbruch, H.; Vaishnav, B.; Vajente, G.; Vallisneri, M.; van den
Brand, J. F. J.; Van Den Broeck, C.; van der Putten, S.; van der Sluys,
M. V.; van Veggel, A. A.; Vass, S.; Vasuth, M.; Vaulin, R.; Vavoulidis,
M.; Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Veltkamp,
C.; Verkindt, D.; Vetrano, F.; Viceré, A.; Villar, A. E.; Vinet,
J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.;
Wallace, L.; Wanner, A.; Ward, R. L.; Was, M.; Wei, P.; Weinert, M.;
Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels, P.; West, M.;
Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; White, D.;
Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke,
B.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan,
G.; Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto,
K.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.; Yvert, M.; Zanolin, M.;
Zhang, L.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2012PhRvD..85h9904A
Altcode:
No abstract at ADS
Title: Publisher's Note: All-sky search for gravitational-wave bursts
in the first joint LIGO-GEO-Virgo run [Phys. Rev. D 81, 102001 (2010)]
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Accadia, T.; Acernese,
F.; Adhikari, R.; Ajith, P.; Allen, B.; Allen, G.; Amador Ceron,
E.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Antonucci, F.;
Arain, M. A.; Araya, M.; Arun, K. G.; Aso, Y.; Aston, S.; Astone,
P.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin,
G.; Ballmer, S.; Barker, D.; Barone, F.; Barr, B.; Barriga, P.;
Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri, R.;
Bastarrika, M.; Bauer, Th. S.; Behnke, B.; Beker, M. G.; Belletoile,
A.; Benacquista, M.; Betzwieser, J.; Beyersdorf, P. T.; Bigotta, S.;
Bilenko, I. A.; Billingsley, G.; Birindelli, S.; Biswas, R.; Bizouard,
M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland,
B.; Blom, M.; Boccara, C.; Bock, O.; Bodiya, T. P.; Bondarescu, R.;
Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Bose, S.;
Bosi, L.; Bouhou, B.; Braccini, S.; Bradaschia, C.; Brady, P. R.;
Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges, D. O.; Brillet,
A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown,
D. A.; Budzyński, R.; Bulik, T.; Bullington, A.; Bulten, H. J.;
Buonanno, A.; Burmeister, O.; Buskulic, D.; Buy, C.; Byer, R. L.;
Cadonati, L.; Cagnoli, G.; Cain, J.; Calloni, E.; Camp, J. B.;
Campagna, E.; Cannizzo, J.; Cannon, K. C.; Canuel, B.; Cao, J.;
Capano, C. D.; Carbognani, F.; Cardenas, L.; Caudill, S.; Cavaglià,
M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.;
Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chassande-Mottin, E.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Chincarini, A.; Christensen,
N.; Chua, S. S. Y.; Chung, C. T. Y.; Clark, D.; Clark, J.; Clayton,
J. H.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas, J.; Colla,
A.; Colombini, M.; Conte, R.; Cook, D.; Corbitt, T. R. C.; Cornish,
N.; Corsi, A.; Coulon, J. -P.; Coward, D.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Cuoco, E.; Dahl, K.; Danilishin, S. L.; D'Antonio, S.;
Danzmann, K.; Dattilo, V.; Daudert, B.; Davier, M.; Davies, G.; Daw,
E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra, D.; Degallaix, J.;
del Prete, M.; Dergachev, V.; DeSalvo, R.; Dhurandhar, S.; Di Fiore,
L.; Di Lieto, A.; Di Paolo Emilio, M.; Di Virgilio, A.; Díaz, M.;
Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes, E. E.; Drago, M.;
Drever, R. W. P.; Driggers, J.; Dueck, J.; Duke, I.; Dumas, J. -C.;
Dwyer, S.; Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.; Etzel,
T.; Evans, M.; Evans, T.; Fafone, V.; Fairhurst, S.; Faltas, Y.;
Fan, Y.; Fazi, D.; Fehrmann, H.; Ferrante, I.; Fidecaro, F.; Finn,
L. S.; Fiori, I.; Flaminio, R.; Flasch, K.; Foley, S.; Forrest, C.;
Fotopoulos, N.; Fournier, J. -D.; Franc, J.; Frasca, S.; Frasconi, F.;
Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.;
Friedrich, D.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.;
Galimberti, M.; Gammaitoni, L.; Garofoli, J. A.; Garufi, F.; Gemme,
G.; Genin, E.; Gennai, A.; Ghosh, S.; Giaime, J. A.; Giampanis, S.;
Giardina, K. D.; Giazotto, A.; Goetz, E.; Goggin, L. M.; González,
G.; Goßler, S.; Gouaty, R.; Granata, M.; Grant, A.; Gras, S.; Gray,
C.; Greenhalgh, R. J. S.; Gretarsson, A. M.; Greverie, C.; Grosso, R.;
Grote, H.; Grunewald, S.; Guidi, G. M.; Gustafson, E. K.; Gustafson,
R.; Hage, B.; Hallam, J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Haughian, K.; Hayama, K.; Hayau, J. -F.; Hayler, T.; Heefner, J.;
Heitmann, H.; Hello, P.; Heng, I. S.; Heptonstall, A.; Hewitson, M.;
Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.;
Hough, J.; Howell, E.; Hoyland, D.; Huet, D.; Hughey, B.; Husa, S.;
Huttner, S. H.; Ingram, D. R.; Isogai, T.; Ivanov, A.; Jaranowski,
P.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.;
Kalmus, P.; Kalogera, V.; Kandhasamy, S.; Kanner, J.; Katsavounidis,
E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalaidovski, A.; Khalili, F. Y.; Khan, R.; Khazanov, E.; Kim, H.;
King, P. J.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov,
V.; Kopparapu, R.; Koranda, S.; Kowalska, I.; Kozak, D.; Kringel,
V.; Krishnan, B.; Królak, A.; Kuehn, G.; Kullman, J.; Kumar, R.;
Kwee, P.; Lam, P. K.; Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.;
Lazzarini, A.; Leaci, P.; Lei, M.; Leindecker, N.; Leonor, I.; Leroy,
N.; Letendre, N.; Li, T. G. F.; Lin, H.; Lindquist, P. E.; Littenberg,
T. B.; Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.;
Lormand, M.; Losurdo, G.; Lu, P.; Lubinski, M.; Lucianetti, A.; Lück,
H.; Lundgren, A.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Mak, C.; Maksimovic, I.; Man, N.; Mandel,
I.; Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Markosyan, A.; Markowitz, J.; Maros, E.; Marque, J.;
Martelli, F.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.;
Masserot, A.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala,
N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McIntyre, G.;
McKechan, D. J. A.; Mehmet, M.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.;
Miller, J.; Minenkov, Y.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohan, M.;
Mohanty, S. D.; Mohapatra, S. R. P.; Moreau, J.; Moreno, G.; Morgado,
N.; Morgia, A.; Mors, K.; Mosca, S.; Moscatelli, V.; Mossavi, K.;
Mours, B.; MowLowry, C.; Mueller, G.; Mukherjee, S.; Mullavey, A.;
Müller-Ebhardt, H.; Munch, J.; Murray, P. G.; Nash, T.; Nawrodt, R.;
Nelson, J.; Neri, I.; Newton, G.; Nishida, E.; Nishizawa, A.; Nocera,
F.; Ochsner, E.; O'Dell, J.; Ogin, G. H.; Oldenburg, R.; O'Reilly,
B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.;
Owen, B. J.; Page, A.; Pagliaroli, G.; Palladino, L.; Palomba, C.;
Pan, Y.; Pankow, C.; Paoletti, F.; Papa, M. A.; Pardi, S.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pathak,
D.; Pedraza, M.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.;
Persichetti, G.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.; Pietka,
M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi,
M. V.; Poggiani, R.; Postiglione, F.; Prato, M.; Principe, M.; Prix,
R.; Prodi, G. A.; Prokhorov, L.; Puncken, O.; Punturo, M.; Puppo, P.;
Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Rabeling, D. S.; Radkins,
H.; Raffai, P.; Raics, Z.; Rakhmanov, M.; Rapagnani, P.; Raymond,
V.; Re, V.; Reed, C. M.; Reed, T.; Regimbau, T.; Rehbein, H.; Reid,
S.; Reitze, D. H.; Ricci, F.; Riesen, R.; Riles, K.; Roberts, P.;
Robertson, N. A.; Robinet, F.; Robinson, C.; Robinson, E. L.; Rocchi,
A.; Roddy, S.; Röver, C.; Rolland, L.; Rollins, J.; Romano, J. D.;
Romano, R.; Romie, J. H.; Rosińska, D.; Rowan, S.; Rüdiger, A.;
Ruggi, P.; Ryan, K.; Sakata, S.; Salemi, F.; Sammut, L.; Sancho de la
Jordana, L.; Sandberg, V.; Sannibale, V.; Santamaría, L.; Santostasi,
G.; Saraf, S.; Sarin, P.; Sassolas, B.; Sathyaprakash, B. S.; Sato,
S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schulz, B.; Schutz, B. F.; Schwinberg,
P.; Scott, J.; Scott, S. M.; Searle, A. C.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Sentenac, D.; Sergeev, A.; Shapiro, B.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sintes,
A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.;
Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Sperandio, L.;
Stein, A. J.; Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.;
Strain, K. A.; Strigin, S.; Stroeer, A.; Sturani, R.; Stuver, A. L.;
Summerscales, T. Z.; Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels,
B.; Szokoly, G. P.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.;
Taylor, J. R.; Taylor, R.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.; Torres,
C.; Torrie, C. I.; Tournefier, E.; Travasso, F.; Traylor, G.; Trias,
M.; Trummer, J.; Turner, L.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.;
Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.; Van Den Broeck,
C.; van der Putten, S.; van der Sluys, M. V.; Vass, S.; Vaulin, R.;
Vavoulidis, M.; Vecchio, A.; Vedovato, G.; van Veggel, A. A.; Veitch,
J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.; Viceré,
A.; Villar, A.; Vinet, J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin,
S. P.; Waldman, S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Was,
M.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen,
S.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.;
Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.;
Williams, H. R.; Williams, L.; Willke, B.; Wilmut, I.; Winkelmann,
L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.;
Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto, K.; Yeaton-Massey,
D.; Yoshida, S.; Yvert, M.; Zanolin, M.; Zhang, L.; Zhang, Z.; Zhao,
C.; Zotov, N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2012PhRvD..85h9905A
Altcode:
No abstract at ADS
Title: Numerical calculation of convection with reduced speed of
sound technique
Authors: Hotta, H.; Rempel, M.; Yokoyama, T.; Iida, Y.; Fan, Y.
Bibcode: 2012A&A...539A..30H
Altcode: 2012arXiv1201.1061H
Context. The anelastic approximation is often adopted in numerical
calculations with low Mach numbers, such as those including stellar
internal convection. This approximation requires so-called frequent
global communication, because of an elliptic partial differential
equation. Frequent global communication is, however, negative factor for
the parallel computing performed with a large number of CPUs.
Aims: We test the validity of a method that artificially reduces the
speed of sound for the compressible fluid equations in the context of
stellar internal convection. This reduction in the speed of sound leads
to longer time steps despite the low Mach number, while the numerical
scheme remains fully explicit and the mathematical system is hyperbolic,
thus does not require frequent global communication.
Methods:
Two- and three-dimensional compressible hydrodynamic equations are
solved numerically. Some statistical quantities of solutions computed
with different effective Mach numbers (owing to the reduction in the
speed of sound) are compared to test the validity of our approach.
Results: Numerical simulations with artificially reduced speed
of sound are a valid approach as long as the effective Mach number
(based on the lower speed of sound) remains less than 0.7.
Title: Building the BOOTES world-wide Network of Robotic telescopes
Authors: Castro-Tirado, A. J.; Jelínek, M.; Gorosabel, J.; Kubánek,
P.; Cunniffe, R.; Guziy, S.; Lara-Gil, O.; Rabaza-Castillo,
O.; de Ugarte Postigo, A.; Sánchez-Ramírez, R.; Tello, J. C.;
Muñoz-Martínez, V.; Pérez del Pulgar, C.; Castillo-Carrión, S.;
Castro Cerón, J. M.; Mateo Sanguino, T. de J.; Hudec, R.; Vitek, S.;
de la Morena Carretero, B. A.; Díaz Andreu, J. A.; Fernández-Muñoz,
R.; Pérez-Ramírez, D.; Yock, P. A.; Allen, W. H.; Bond, I.; Christie,
G.; Sabau-Graziati, L.; Castro, A.; Pozanenko, A.; Bai, J.; Fan, Y.;
Cui, C.
Bibcode: 2012ASInC...7..313C
Altcode:
We show the status of the BOOTES Network, which is expanding worldwide
with four autonomous robotic observatories already deployed in Spain,
New Zealand and China. We briefly discuss the technical as well as
the scientific aspects we have already achieved and the goals we are
aiming at.
Title: All-sky search for periodic gravitational waves in the full
S5 LIGO data
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abbott, T. D.;
Abernathy, M.; Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.;
Affeldt, C.; Ajith, P.; Allen, B.; Allen, G. S.; Amador Ceron, E.;
Amariutei, D.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arai,
K.; Arain, M. A.; Araya, M. C.; Aston, S. M.; Astone, P.; Atkinson,
D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker,
P.; Ballardin, G.; Ballmer, S.; Barker, D.; Barone, F.; Barr, B.;
Barriga, P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Basti, A.; Batch, J.; Bauchrowitz, J.;
Bauer, Th. S.; Bebronne, M.; Behnke, B.; Beker, M. G.; Bell, A. S.;
Belletoile, A.; Belopolski, I.; Benacquista, M.; Berliner, J. M.;
Bertolini, A.; Betzwieser, J.; Beveridge, N.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas, R.; Bitossi, M.;
Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.;
Bland, B.; Blom, M.; Bock, O.; Bodiya, T. P.; Bogan, C.; Bondarescu,
R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Boschi,
V.; Bose, S.; Bosi, L.; Bouhou, B.; Braccini, S.; Bradaschia, C.;
Brady, P. R.; Braginsky, V. B.; Branchesi, M.; Brau, J. E.; Breyer,
J.; Briant, T.; Bridges, D. O.; Brillet, A.; Brinkmann, M.; Brisson,
V.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Brummit, A.; Bulik,
T.; Bulten, H. J.; Buonanno, A.; Burguet–Castell, J.; Burmeister,
O.; Buskulic, D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.;
Calloni, E.; Camp, J. B.; Campsie, P.; Cannizzo, J.; Cannon, K.;
Canuel, B.; Cao, J.; Capano, C. D.; Carbognani, F.; Caride, S.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chaibi, O.; Chalermsongsak, T.; Chalkley,
E.; Charlton, P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, Y.;
Chincarini, A.; Chiummo, A.; Cho, H.; Christensen, N.; Chua, S. S. Y.;
Chung, C. T. Y.; Chung, S.; Ciani, G.; Clara, F.; Clark, D. E.;
Clark, J.; Clayton, J. H.; Cleva, F.; Coccia, E.; Cohadon, P. -F.;
Colacino, C. N.; Colas, J.; Colla, A.; Colombini, M.; Conte, A.;
Conte, R.; Cook, D.; Corbitt, T. R.; Cordier, M.; Cornish, N.; Corsi,
A.; Costa, C. A.; Coughlin, M.; Coulon, J. -P.; Couvares, P.; Coward,
D. M.; Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Cruise,
A. M.; Cumming, A.; Cunningham, L.; Cuoco, E.; Cutler, R. M.; Dahl,
K.; Danilishin, S. L.; Dannenberg, R.; D'Antonio, S.; Danzmann, K.;
Dattilo, V.; Daudert, B.; Daveloza, H.; Davier, M.; Davies, G.; Daw,
E. J.; Day, R.; Dayanga, T.; de Rosa, R.; Debra, D.; Debreczeni, G.;
Degallaix, J.; Del Pozzo, W.; Del Prete, M.; Dent, T.; Dergachev, V.;
Derosa, R.; Desalvo, R.; Dhurandhar, S.; di Fiore, L.; Diguglielmo,
J.; di Lieto, A.; di Palma, I.; di Paolo Emilio, M.; di Virgilio,
A.; Díaz, M.; Dietz, A.; Donovan, F.; Dooley, K. L.; Dorsher, S.;
Drago, M.; Drever, R. W. P.; Driggers, J. C.; Du, Z.; Dumas, J. -C.;
Dwyer, S.; Eberle, T.; Edgar, M.; Edwards, M.; Effler, A.; Ehrens,
P.; Endrőczi, G.; Engel, R.; Etzel, T.; Evans, K.; Evans, M.; Evans,
T.; Factourovich, M.; Fafone, V.; Fairhurst, S.; Fan, Y.; Farr, B. F.;
Farr, W.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Ferrante, I.; Fidecaro,
F.; Finn, L. S.; Fiori, I.; Fisher, R. P.; Flaminio, R.; Flanigan, M.;
Foley, S.; Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.;
Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.;
Freise, A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.;
Frolov, V. V.; Fulda, P. J.; Fyffe, M.; Galimberti, M.; Gammaitoni,
L.; Ganija, M. R.; Garcia, J.; Garofoli, J. A.; Garufi, F.; Gáspár,
M. E.; Gemme, G.; Geng, R.; Genin, E.; Gennai, A.; Gergely, L. Á.;
Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Giazotto,
A.; Gill, C.; Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky,
M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Granata, M.; Grant, A.;
Gras, S.; Gray, C.; Gray, N.; Greenhalgh, R. J. S.; Gretarsson, A. M.;
Greverie, C.; Grosso, R.; Grote, H.; Grunewald, S.; Guidi, G. M.;
Guido, C.; Gupta, R.; Gustafson, E. K.; Gustafson, R.; Ha, T.; Hage,
B.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Hartman, M. T.; Haughian, K.; Hayama, K.; Hayau, J. -F.; Hayler, T.;
Heefner, J.; Heidmann, A.; Heintze, M. C.; Heitmann, H.; Hello, P.;
Hendry, M. A.; Heng, I. S.; Heptonstall, A. W.; Herrera, V.; Hewitson,
M.; Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Hong, T.; Hooper,
S.; Hosken, D. J.; Hough, J.; Howell, E. J.; Hughey, B.; Husa, S.;
Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.; Inta, R.; Isogai,
T.; Ivanov, A.; Izumi, K.; Jacobson, M.; Jang, H.; Jaranowski, P.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.;
Kalogera, V.; Kamaretsos, I.; Kandhasamy, S.; Kang, G.; Kanner, J. B.;
Katsavounidis, E.; Katzman, W.; Kaufer, H.; Kawabe, K.; Kawamura, S.;
Kawazoe, F.; Kells, W.; Keppel, D. G.; Keresztes, Z.; Khalaidovski,
A.; Khalili, F. Y.; Khazanov, E. A.; Kim, B.; Kim, C.; Kim, D.; Kim,
H.; Kim, K.; Kim, N.; Kim, Y. -M.; King, P. J.; Kinsey, M.; Kinzel,
D. L.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.;
Kopparapu, R.; Koranda, S.; Korth, W. Z.; Kowalska, I.; Kozak, D.;
Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Królak, A.; Kuehn,
G.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lang, M.; Lantz, B.;
Lastzka, N.; Lawrie, C.; Lazzarini, A.; Leaci, P.; Lee, C. H.; Lee,
H. M.; Leindecker, N.; Leong, J. R.; Leonor, I.; Leroy, N.; Letendre,
N.; Li, J.; Li, T. G. F.; Liguori, N.; Lindquist, P. E.; Lockerbie,
N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo,
G.; Luan, J.; Lubinski, M.; Lück, H.; Lundgren, A. P.; MacDonald,
E.; Machenschalk, B.; Macinnis, M.; MacLeod, D. M.; Mageswaran,
M.; Mailand, K.; Majorana, E.; Maksimovic, I.; Man, N.; Mandel, I.;
Mandic, V.; Mantovani, M.; Marandi, A.; Marchesoni, F.; Marion,
F.; Márka, S.; Márka, Z.; Markosyan, A.; Maros, E.; Marque, J.;
Martelli, F.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.;
Masserot, A.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala,
N.; Mazzolo, G.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.;
McIntyre, G.; McIver, J.; McKechan, D. J. A.; Meadors, G. D.; Mehmet,
M.; Meier, T.; Melatos, A.; Melissinos, A. C.; Mendell, G.; Menendez,
D.; Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Miao, H.;
Michel, C.; Milano, L.; Miller, J.; Minenkov, Y.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Moesta, P.;
Mohan, M.; Mohanty, S. D.; Mohapatra, S. R. P.; Moraru, D.; Moreno,
G.; Morgado, N.; Morgia, A.; Mori, T.; Mosca, S.; Mossavi, K.; Mours,
B.; Mow-Lowry, C. M.; Mueller, C. L.; Mueller, G.; Mukherjee, S.;
Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murphy, D.; Murray,
P. G.; Mytidis, A.; Nash, T.; Naticchioni, L.; Nawrodt, R.; Necula,
V.; Nelson, J.; Newton, G.; Nishizawa, A.; Nocera, F.; Nolting, D.;
Nuttall, L.; Ochsner, E.; O'Dell, J.; Oelker, E.; Ogin, G. H.; Oh,
J. J.; Oh, S. H.; Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.;
Osthelder, C.; Ott, C. D.; Ottaway, D. J.; Ottens, R. S.; Overmier,
H.; Owen, B. J.; Page, A.; Pagliaroli, G.; Palladino, L.; Palomba,
C.; Pan, Y.; Pankow, C.; Paoletti, F.; Papa, M. A.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pedraza,
M.; Peiris, P.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.;
Persichetti, G.; Phelps, M.; Pickenpack, M.; Piergiovanni, F.;
Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Poggiani, R.; Pöld, J.; Postiglione, F.; Prato, M.;
Predoi, V.; Price, L. R.; Prijatelj, M.; Principe, M.; Privitera,
S.; Prix, R.; Prodi, G. A.; Prokhorov, L.; Puncken, O.; Punturo, M.;
Puppo, P.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Rácz, I.;
Radkins, H.; Raffai, P.; Rakhmanov, M.; Ramet, C. R.; Rankins, B.;
Rapagnani, P.; Raymond, V.; Re, V.; Redwine, K.; Reed, C. M.; Reed,
T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.; Riesen, R.;
Riles, K.; Robertson, N. A.; Robinet, F.; Robinson, C.; Robinson,
E. L.; Rocchi, A.; Roddy, S.; Rodriguez, C.; Rodruck, M.; Rolland,
L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.; Rosińska,
D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Ryll,
H.; Sainathan, P.; Sakosky, M.; Salemi, F.; Samblowski, A.; Sammut,
L.; Sancho de La Jordana, L.; Sandberg, V.; Sankar, S.; Sannibale,
V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.; Sassolas,
B.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.;
Schilling, R.; Schlamminger, S.; Schnabel, R.; Schofield, R. M. S.;
Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.;
Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sentenac,
D.; Sergeev, A.; Shaddock, D. A.; Shaltev, M.; Shapiro, B.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.;
Singer, L.; Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Smith, R. J. E.; Somiya,
K.; Sorazu, B.; Soto, J.; Speirits, F. C.; Sperandio, L.; Stefszky,
M.; Stein, A. J.; Steinert, E.; Steinlechner, J.; Steinlechner, S.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S.;
Stroeer, A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.;
Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Tacca, M.;
Taffarello, L.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor,
J. R.; Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane,
E.; Thüring, A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.; Tonelli,
M.; Torre, O.; Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso,
F.; Traylor, G.; Trias, M.; Tseng, K.; Ugolini, D.; Urbanek, K.;
Vahlbruch, H.; Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.;
van den Broeck, C.; van der Putten, S.; van Veggel, A. A.; Vass, S.;
Vasuth, M.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.;
Veitch, J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.;
Viceré, A.; Villar, A. E.; Vinet, J. -Y.; Vitale, S.; Vitale, S.;
Vocca, H.; Vorvick, C.; Vyatchanin, S. P.; Wade, A.; Waldman, S. J.;
Wallace, L.; Wan, Y.; Wang, X.; Wang, Z.; Wanner, A.; Ward, R. L.; Was,
M.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen,
S.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.;
Whitcomb, S. E.; White, D.; Whiting, B. F.; Wilkinson, C.; Willems,
P. A.; Williams, H. R.; Williams, L.; Willke, B.; Winkelmann, L.;
Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Wittel, H.; Woan, G.; Wooley,
R.; Worden, J.; Yablon, J.; Yakushin, I.; Yamamoto, H.; Yamamoto,
K.; Yang, H.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.; Yvert, M.;
Zadroźny, A.; Zanolin, M.; Zendri, J. -P.; Zhang, F.; Zhang, L.;
Zhang, W.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2012PhRvD..85b2001A
Altcode: 2011arXiv1110.0208A
We report on an all-sky search for periodic gravitational waves in the
frequency band 50-800 Hz and with the frequency time derivative in the
range of 0 through -6×10-9Hz/s. Such a signal could be
produced by a nearby spinning and slightly nonaxisymmetric isolated
neutron star in our Galaxy. After recent improvements in the search
program that yielded a 10× increase in computational efficiency,
we have searched in two years of data collected during LIGO’s
fifth science run and have obtained the most sensitive all-sky upper
limits on gravitational-wave strain to date. Near 150 Hz our upper
limit on worst-case linearly polarized strain amplitude h0
is 1×10-24, while at the high end of our frequency range
we achieve a worst-case upper limit of 3.8×10-24 for all
polarizations and sky locations. These results constitute a factor
of 2 improvement upon previously published data. A new detection
pipeline utilizing a loosely coherent algorithm was able to follow up
weaker outliers, increasing the volume of space where signals can be
detected by a factor of 10, but has not revealed any gravitational-wave
signals. The pipeline has been tested for robustness with respect to
deviations from the model of an isolated neutron star, such as caused
by a low-mass or long-period binary companion.
Title: GRB 121123A: BOOTES-4 and IAC80 optical observations.
Authors: Guziy, S.; Sanchez-Ramirez, R.; Monteagudo Narvion, L.; Lara,
O.; Jelinek, M.; Kubanek, P.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.;
Xin, Y.; Cui, C.; Cunniffe, R.; Castro-Tirado, A. J.; Tello, J. C.;
Gorosabel, J.
Bibcode: 2012GCN.13987....1G
Altcode: 2012GCN..13987...1G
No abstract at ADS
Title: GRB 121226A: BOOTES-4/MET optical observations.
Authors: Guziy, S.; Lara, O.; Cunniffe, R.; Gorosabel, J.; Jelinek,
M.; Kubanek, P.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.; Xin, Y.; Cui,
Ch.; Castro-Tirado, A. J.
Bibcode: 2012GCN.14106....1G
Altcode: 2012GCN..14106...1G
No abstract at ADS
Title: GRB 121123A: BOOTES-4 optical observations.
Authors: Guziy, S.; Sanchez-Ramirez, R.; Monteagudo Narvion, L.; Lara,
O.; Jelinek, M.; Kubanek, P.; Fan, Y.; Zhao, X.; Bai, J.; Wang, C.;
Xin, Y.; Cui, C.; Cunniffe, R.; Castro-Tirado, A. J.; Tello, J. C.;
Gorosabel, J.
Bibcode: 2012GCN.14026....1G
Altcode: 2012GCN..14026...1G
No abstract at ADS
Title: GRB 120320A: BOOTES-4 optical upper limit.
Authors: Tello, J. C.; Kubanek, P.; Gorosabel, J.; Castro-Tirado,
A. J.; Guziy, S.; Fan, Y.; Zhao, X.; Bai, J.; Cui, C.
Bibcode: 2012GCN.13080....1T
Altcode: 2012GCN..13080...1T
No abstract at ADS
Title: Fermi trigger 358364818: BOOTES-4 observations.
Authors: Guziy, S.; Kubanek, P.; Fan, Y.; Castro-Tirado, A. J.
Bibcode: 2012GCN.13286....1G
Altcode: 2012GCN..13286...1G
No abstract at ADS
Title: Directional Limits on Persistent Gravitational Waves Using
LIGO S5 Science Data
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.;
Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.; Ajith, P.;
Allen, B.; Allen, G. S.; Amador Ceron, E.; Amin, R. S.; Anderson,
S. B.; Anderson, W. G.; Antonucci, F.; Arain, M. A.; Araya, M. C.;
Aronsson, M.; Arun, K. G.; Aso, Y.; Aston, S. M.; Astone, P.; Atkinson,
D.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.;
Ballmer, S.; Barker, D.; Barnum, S.; Barone, F.; Barr, B.; Barriga,
P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri,
R.; Bastarrika, M.; Bauchrowitz, J.; Bauer, Th. S.; Behnke, B.; Beker,
M. G.; Belletoile, A.; Benacquista, M.; Bertolini, A.; Betzwieser,
J.; Beveridge, N.; Beyersdorf, P. T.; Bigotta, S.; Bilenko, I. A.;
Billingsley, G.; Birch, J.; Birindelli, S.; Biswas, R.; Bitossi, M.;
Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.;
Bland, B.; Blom, M.; Boccara, C.; Bock, O.; Bodiya, T. P.; Bondarescu,
R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Bose,
S.; Bosi, L.; Bouhou, B.; Boyle, M.; Braccini, S.; Bradaschia, C.;
Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges,
D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks,
A. F.; Brown, D. A.; Budzyński, R.; Bulik, T.; Bulten, H. J.;
Buonanno, A.; Burguet-Castell, J.; Burmeister, O.; Buskulic, D.;
Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Cain, J.; Calloni,
E.; Camp, J. B.; Campagna, E.; Campsie, P.; Cannizzo, J.; Cannon,
K.; Canuel, B.; Cao, J.; Capano, C.; Carbognani, F.; Caride, S.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chalermsongsak, T.; Chalkley, E.; Charlton,
P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, Y.; Chincarini, A.;
Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.; Clark, D.; Clark,
J.; Clayton, J. H.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas,
J.; Colla, A.; Colombini, M.; Conte, R.; Cook, D.; Corbitt, T. R.;
Cornish, N.; Corsi, A.; Costa, C. A.; Coulon, J. -P.; Coward, D. M.;
Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.;
Culter, R. M.; Cumming, A.; Cunningham, L.; Cuoco, E.; Dahl, K.;
Danilishin, S. L.; Dannenberg, R.; D'Antonio, S.; Danzmann, K.; Das,
K.; Dattilo, V.; Daudert, B.; Davier, M.; Davies, G.; Davis, A.; Daw,
E. J.; Day, R.; Dayanga, T.; de Rosa, R.; Debra, D.; Degallaix, J.;
Del Prete, M.; Dergachev, V.; Derosa, R.; Desalvo, R.; Devanka, P.;
Dhurandhar, S.; di Fiore, L.; di Lieto, A.; di Palma, I.; di Paolo
Emilio, M.; di Virgilio, A.; Díaz, M.; Dietz, A.; Donovan, F.;
Dooley, K. L.; Doomes, E. E.; Dorsher, S.; Douglas, E. S. D.; Drago,
M.; Drever, R. W. P.; Driggers, J. C.; Dueck, J.; Dumas, J. -C.;
Eberle, T.; Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.; Engel,
R.; Etzel, T.; Evans, M.; Evans, T.; Fafone, V.; Fairhurst, S.; Fan,
Y.; Farr, B. F.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Ferrante,
I.; Fidecaro, F.; Finn, L. S.; Fiori, I.; Flaminio, R.; Flanigan,
M.; Flasch, K.; Foley, S.; Forrest, C.; Forsi, E.; Fotopoulos, N.;
Fournier, J. -D.; Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich,
D.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Galimberti,
M.; Gammaitoni, L.; Garofoli, J. A.; Garufi, F.; Gemme, G.; Genin,
E.; Gennai, A.; Gholami, I.; Ghosh, S.; Giaime, J. A.; Giampanis, S.;
Giardina, K. D.; Giazotto, A.; Gill, C.; Goetz, E.; Goggin, L. M.;
González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.;
Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald,
S.; Guidi, G. M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hall,
P.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Haughian, K.; Hayama, K.; Hayau, J. -F.; Hayler, T.; Heefner, J.;
Heitmann, H.; Hello, P.; Heng, I. S.; Heptonstall, A. W.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken,
D. J.; Hough, J.; Howell, E. J.; Hoyland, D.; Huet, D.; Hughey, B.;
Husa, S.; Huttner, S. H.; Huynh–Dinh, T.; Ingram, D. R.; Inta, R.;
Isogai, T.; Ivanov, A.; Jaranowski, P.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kanner, J. B.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.;
Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khazanov, E. A.; Kim, H.; King, P. J.; Kinzel, D. L.; Kissel,
J. S.; Klimenko, S.; Kondrashov, V.; Kopparapu, R.; Koranda, S.;
Kowalska, I.; Kozak, D.; Krause, T.; Kringel, V.; Krishnamurthy,
S.; Krishnan, B.; Królak, A.; Kuehn, G.; Kullman, J.; Kumar, R.;
Kwee, P.; Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lazzarini,
A.; Leaci, P.; Leong, J.; Leonor, I.; Leroy, N.; Letendre, N.; Li,
J.; Li, T. G. F.; Liguori, N.; Lin, H.; Lindquist, P. E.; Lockerbie,
N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo,
G.; Lu, P.; Luan, J.; Lubinski, M.; Lucianetti, A.; Lück, H.;
Lundgren, A. D.; Machenschalk, B.; Macinnis, M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Mak, C.; Maksimovic, I.; Man, N.; Mandel,
I.; Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.;
Meadors, G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.;
Miller, J.; Minenkov, Y.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Moe, B.; Mohan, M.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moraru, D.; Moreau, J.; Moreno, G.; Morgado,
N.; Morgia, A.; Morioka, T.; Mors, K.; Mosca, S.; Moscatelli, V.;
Mossavi, K.; Mours, B.; Mow–Lowry, C. M.; Mueller, G.; Mukherjee,
S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murray, P. G.;
Nash, T.; Nawrodt, R.; Nelson, J.; Neri, I.; Newton, G.; Nishizawa,
A.; Nocera, F.; Nolting, D.; Ochsner, E.; O'Dell, J.; Ogin, G. H.;
Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.;
Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page,
A.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow,
C.; Paoletti, F.; Papa, M. A.; Pardi, S.; Pareja, M.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pathak,
D.; Pedraza, M.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca,
A.; Persichetti, G.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.;
Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Poggiani, R.; Postiglione, F.; Prato, M.; Predoi, V.;
Price, L. R.; Prijatelj, M.; Principe, M.; Prix, R.; Prodi, G. A.;
Prokhorov, L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.;
Raab, F. J.; Rabeling, D. S.; Radke, T.; Radkins, H.; Raffai, P.;
Rakhmanov, M.; Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Reed,
C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.;
Riesen, R.; Riles, K.; Roberts, P.; Robertson, N. A.; Robinet, F.;
Robinson, C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Röver, C.;
Rolland, L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.;
Rosińska, D.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sakata,
S.; Sakosky, M.; Salemi, F.; Sammut, L.; Sancho de La Jordana, L.;
Sandberg, V.; Sannibale, V.; Santamaría, L.; Santostasi, G.; Saraf,
S.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.;
Saulson, P. R.; Savage, R.; Schilling, R.; Schnabel, R.; Schofield,
R. M. S.; Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott,
S. M.; Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.;
Sentenac, D.; Sergeev, A.; Shaddock, D. A.; Shapiro, B.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.;
Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Speirits,
F. C.; Sperandio, L.; Stein, A. J.; Stein, L. C.; Steinlechner, S.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin,
S.; Stroeer, A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.;
Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Szokoly, G. P.;
Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor,
R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.; Thüring,
A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.; Torre, O.;
Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso, F.; Traylor, G.;
Trias, M.; Trummer, J.; Tseng, K.; Turner, L.; Ugolini, D.; Urbanek,
K.; Vahlbruch, H.; Vaishnav, B.; Vajente, G.; Vallisneri, M.; van
den Brand, J. F. J.; van den Broeck, C.; van der Putten, S.; van der
Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin, R.; Vavoulidis,
M.; Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Veltkamp,
C.; Verkindt, D.; Vetrano, F.; Viceré, A.; Villar, A. E.; Vinet,
J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.;
Wallace, L.; Wanner, A.; Ward, R. L.; Was, M.; Wei, P.; Weinert, M.;
Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels, P.; West, M.;
Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; White, D.;
Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke,
B.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan,
G.; Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto,
K.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.; Yvert, M.; Zanolin, M.;
Zhang, L.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2011PhRvL.107A1102A
Altcode: 2011arXiv1109.1809A
The gravitational-wave (GW) sky may include nearby pointlike sources as
well as stochastic backgrounds. We perform two directional searches for
persistent GWs using data from the LIGO S5 science run: one optimized
for pointlike sources and one for arbitrary extended sources. Finding
no evidence to support the detection of GWs, we present 90% confidence
level (C.L.) upper-limit maps of GW strain power with typical values
between 2-20×10-50strain2Hz-1 and
5-35×10-49strain2Hz-1sr-1
for pointlike and extended sources, respectively. The latter result is
the first of its kind. We also set 90% C.L. limits on the narrow-band
root-mean-square GW strain from interesting targets including Sco X-1,
SN 1987A and the Galactic center as low as ≈7×10-25
in the most sensitive frequency range near 160 Hz.
Title: A gravitational wave observatory operating beyond the quantum
shot-noise limit
Authors: Ligo Scientific Collaboration; Abadie, J.; Abbott, B. P.;
Abbott, R.; Abbott, T. D.; Abernathy, M.; Adams, C.; Adhikari, R.;
Affeldt, C.; Allen, B.; Allen, G. S.; Amador Ceron, E.; Amariutei,
D.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arai, K.; Arain,
M. A.; Araya, M. C.; Aston, S. M.; Atkinson, D.; Aufmuth, P.; Aulbert,
C.; Aylott, B. E.; Babak, S.; Baker, P.; Ballmer, S.; Barker, D.;
Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Batch, J.; Bauchrowitz, J.; Behnke,
B.; Bell, A. S.; Belopolski, I.; Benacquista, M.; Berliner, J. M.;
Bertolini, A.; Betzwieser, J.; Beveridge, N.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas, R.; Black,
E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.; Bock,
O.; Bodiya, T. P.; Bogan, C.; Bondarescu, R.; Bork, R.; Born, M.;
Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer, J.;
Bridges, D. O.; Brinkmann, M.; Britzger, M.; Brooks, A. F.; Brown,
D. A.; Brummitt, A.; Buonanno, A.; Burguet-Castell, J.; Burmeister,
O.; Byer, R. L.; Cadonati, L.; Camp, J. B.; Campsie, P.; Cannizzo,
J.; Cannon, K.; Cao, J.; Capano, C. D.; Caride, S.; Caudill, S.;
Cavagliá, M.; Cepeda, C.; Chalermsongsak, T.; Chalkley, E.; Charlton,
P.; Chelkowski, S.; Chen, Y.; Christensen, N.; Cho, H.; Chua, S. S. Y.;
Chung, S.; Chung, C. T. Y.; Ciani, G.; Clara, F.; Clark, D. E.; Clark,
J.; Clayton, J. H.; Conte, R.; Cook, D.; Corbitt, T. R.; Cordier,
M.; Cornish, N.; Corsi, A.; Costa, C. A.; Coughlin, M.; Couvares,
P.; Coward, D. M.; Coyne, D. C.; Creighton, J. D. E.; Creighton,
T. D.; Cruise, A. M.; Cumming, A.; Cunningham, L.; Cutler, R. M.;
Dahl, K.; Danilishin, S. L.; Dannenberg, R.; Danzmann, K.; Daudert,
B.; Daveloza, H.; Davies, G.; Daw, E. J.; Dayanga, T.; Debra, D.;
Degallaix, J.; Dent, T.; Dergachev, V.; Derosa, R.; Desalvo, R.;
Dhurandhar, S.; Diguglielmo, J.; di Palma, I.; Díaz, M.; Donovan,
F.; Dooley, K. L.; Dorsher, S.; Drever, R. W. P.; Driggers, J. C.;
Du, Z.; Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar, M.; Edwards,
M.; Effler, A.; Ehrens, P.; Engel, R.; Etzel, T.; Evans, K.; Evans,
M.; Evans, T.; Factourovich, M.; Fairhurst, S.; Fan, Y.; Farr, B. F.;
Farr, W.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Finn, L. S.; Fisher,
R. P.; Flanigan, M.; Foley, S.; Forsi, E.; Fotopoulos, N.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich, D.;
Fritschel, P.; Frolov, V. V.; Fulda, P. J.; Fyffe, M.; Ganija, M. R.;
Garcia, J.; Garofoli, J. A.; Geng, R.; Gergely, L. Á.; Gholami, I.;
Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Gill, C.;
Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler,
S.; Graef, C.; Grant, A.; Gras, S.; Gray, C.; Gray, N.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Grosso, R.; Grote, H.; Grunewald, S.;
Guido, C.; Gupta, R.; Gustafson, E. K.; Gustafson, R.; Ha, T.; Hage,
B.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Hartman, M. T.; Haughian, K.; Hayama, K.; Heefner, J.; Heintze, M. C.;
Hendry, M. A.; Heng, I. S.; Heptonstall, A. W.; Herrera, V.; Hewitson,
M.; Hild, S.; Hoak, D.; Hodge, K. A.; Holt, K.; Hong, T.; Hooper, S.;
Hosken, D. J.; Hough, J.; Howell, E. J.; Hughey, B.; Huynh-Dinh, T.;
Husa, S.; Huttner, S. H.; Ingram, D. R.; Inta, R.; Isogai, T.; Ivanov,
A.; Izumi, K.; Jacobson, M.; Jang, H.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kamaretsos,
I.; Kandhasamy, S.; Kang, G.; Kanner, J. B.; Katsavounidis, E.;
Katzman, W.; Kaufer, H.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells,
W.; Keppel, D. G.; Keresztes, Z.; Khalaidovski, A.; Khalili, F. Y.;
Khazanov, E. A.; Kim, B.; Kim, C.; Kim, D.; Kim, H.; Kim, K.; Kim, N.;
Kim, Y. -M.; King, P. J.; Kinsey, M.; Kinzel, D. L.; Kissel, J. S.;
Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda,
S.; Korth, W. Z.; Kozak, D.; Kringel, V.; Krishnamurthy, S.; Krishnan,
B.; Kuehn, G.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lang, M.;
Lantz, B.; Lastzka, N.; Lawrie, C.; Lazzarini, A.; Leaci, P.; Lee,
C. H.; Lee, H. M.; Leindecker, N.; Leong, J. R.; Leonor, I.; Li, J.;
Lindquist, P. E.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Luan, J.;
Lubinski, M.; Lück, H.; Lundgren, A. P.; MacDonald, E.; Machenschalk,
B.; Macinnis, M.; MacLeod, D. M.; Mageswaran, M.; Mailand, K.; Mandel,
I.; Mandic, V.; Marandi, A.; Márka, S.; Márka, Z.; Markosyan, A.;
Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.;
Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala, N.; Mazzolo,
G.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McIntyre, G.;
McIver, J.; McKechan, D. J. A.; Meadors, G. D.; Mehmet, M.; Meier, T.;
Melatos, A.; Melissinos, A. C.; Mendell, G.; Menendez, D.; Mercer,
R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Miao, H.; Miller,
J.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa,
O.; Moe, B.; Moesta, P.; Mohanty, S. D.; Moraru, D.; Moreno, G.;
Mori, T.; Mossavi, K.; Mow-Lowry, C. M.; Mueller, C. L.; Mueller, G.;
Mukherjee, S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murphy,
D.; Murray, P. G.; Mytidis, A.; Nash, T.; Nawrodt, R.; Necula, V.;
Nelson, J.; Newton, G.; Nishizawa, A.; Nolting, D.; Nuttall, L.;
O'Dell, J.; O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.; Oelker,
E.; Oh, J. J.; Oh, S. H.; Ogin, G. H.; Oldenburg, R. G.; Osthelder,
C.; Ott, C. D.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen,
B. J.; Page, A.; Pan, Y.; Pankow, C.; Papa, M. A.; Ajith, P.; Patel,
P.; Pedraza, M.; Peiris, P.; Pekowsky, L.; Penn, S.; Peralta, C.;
Perreca, A.; Phelps, M.; Pickenpack, M.; Pinto, I. M.; Pitkin, M.;
Pletsch, H. J.; Plissi, M. V.; Pöld, J.; Postiglione, F.; Predoi,
V.; Price, L. R.; Prijatelj, M.; Principe, M.; Privitera, S.; Prix,
R.; Prokhorov, L.; Puncken, O.; Quetschke, V.; Raab, F. J.; Radkins,
H.; Raffai, P.; Rakhmanov, M.; Ramet, C. R.; Rankins, B.; Mohapatra,
S. R. P.; Raymond, V.; Redwine, K.; Reed, C. M.; Reed, T.; Reid, S.;
Reitze, D. H.; Riesen, R.; Riles, K.; Robertson, N. A.; Robinson,
C.; Robinson, E. L.; Roddy, S.; Rodriguez, C.; Rodruck, M.; Rollins,
J.; Romano, J. D.; Romie, J. H.; Röver, C.; Rowan, S.; Rüdiger, A.;
Ryan, K.; Ryll, H.; Sainathan, P.; Sakosky, M.; Salemi, F.; Samblowski,
A.; Sammut, L.; Sancho de La Jordana, L.; Sandberg, V.; Sankar, S.;
Sannibale, V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi,
G.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R. L.;
Schilling, R.; Schlamminger, S.; Schnabel, R.; Schofield, R. M. S.;
Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.;
Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.;
Shaddock, D. A.; Shaltev, M.; Shapiro, B.; Shawhan, P.; Shoemaker,
D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.; Singer, L.;
Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
R. J. E.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.;
Sorazu, B.; Soto, J.; Speirits, F. C.; Stein, A. J.; Steinert, E.;
Steinlechner, J.; Steinlechner, S.; Steplewski, S.; Stefszky, M.;
Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S.; Stroeer, A. S.;
Stuver, A. L.; Summerscales, T. Z.; Sung, M.; Susmithan, S.; Sutton,
P. J.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.;
Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.;
Thüring, A.; Titsler, C.; Tokmakov, K. V.; Torres, C.; Torrie, C. I.;
Traylor, G.; Trias, M.; Tseng, K.; Ugolini, D.; Urbanek, K.; Vahlbruch,
H.; Vallisneri, M.; van Veggel, A. A.; Vass, S.; Vaulin, R.; Vecchio,
A.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Villar, A. E.; Vitale,
S.; Vorvick, C.; Vyatchanin, S. P.; Wade, A.; Waldman, S. J.; Wallace,
L.; Wan, Y.; Wanner, A.; Wang, X.; Wang, Z.; Ward, R. L.; Wei, P.;
Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels,
P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.;
White, D.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams,
H. R.; Williams, L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf,
C. C.; Wittel, H.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden,
J.; Yablon, J.; Yakushin, I.; Yamamoto, K.; Yamamoto, H.; Yang, H.;
Yeaton-Massey, D.; Yoshida, S.; Yu, P.; Zanolin, M.; Zhang, L.; Zhang,
W.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2011NatPh...7..962L
Altcode: 2011arXiv1109.2295T
Around the globe several observatories are seeking the first direct
detection of gravitational waves (GWs). These waves are predicted by
Einstein's general theory of relativity and are generated, for example,
by black-hole binary systems. Present GW detectors are Michelson-type
kilometre-scale laser interferometers measuring the distance changes
between mirrors suspended in vacuum. The sensitivity of these detectors
at frequencies above several hundred hertz is limited by the vacuum
(zero-point) fluctuations of the electromagnetic field. A quantum
technology--the injection of squeezed light--offers a solution to
this problem. Here we demonstrate the squeezed-light enhancement of
GEO600, which will be the GW observatory operated by the LIGO Scientific
Collaboration in its search for GWs for the next 3-4 years. GEO600 now
operates with its best ever sensitivity, which proves the usefulness
of quantum entanglement and the qualification of squeezed light as a
key technology for future GW astronomy.
Title: Comparing Simulations of Rising Flux Tubes Through the Solar
Convection Zone with Observations of Active Region Properties:
Constraining the Dynamo Field Strength
Authors: Weber, M. A.; Fan, Y.; Miesch, M.
Bibcode: 2011AGUFMSH41B..05W
Altcode:
We use a thin flux tube model in a rotating spherical shell of turbulent
convective flows to study how active region scale flux tubes rise
buoyantly from the bottom of the convection zone to near the solar
surface. We investigate toroidal flux tubes originating at the base
of the convection zone with field strengths ranging from 15 kG to 100
kG at initial latitudes ranging from 1° to 40° with a total flux
of 1020 Mx to 1022 Mx. With the influence of
a convective velocity field, the dynamic evolution of the flux tube
changes from convection dominated to magnetic buoyancy dominated as the
initial field strength increases from 15 kG to 100 kG. With convection,
rise times are reduced (from years to months) for all fluxes, and loops
are able to emerge at low latitudes even for a large flux. We examine
phase velocities of the emerging loop apices, geometric and magnetic
field asymmetries between the leading and following legs of the emerging
loops, and the tilt angle of the emerging flux tube as a function of the
latitude in order to identify a Joy's Law trend. Also, we investigate
whether there is a larger spread in tilt angles at lower latitudes. By
comparing our flux tube simulation results with observations of solar
active regions, we attempt to constrain the magnetic field generated
by the solar dynamo at the base of the convection zone.
Title: A Magnetohydrodynamic Model of the 2006 December 13 Eruptive
Flare
Authors: Fan, Y.
Bibcode: 2011ApJ...740...68F
Altcode: 2011arXiv1109.3734F
We present a three-dimensional magnetohydrodynamic simulation
that qualitatively models the coronal magnetic field evolution
associated with the eruptive flare that occurred on 2006 December 13
in the emerging δ-sunspot region NOAA 10930 observed by the Hinode
satellite. The simulation is set up to drive the emergence of an
east-west-oriented magnetic flux rope at the lower boundary into a
preexisting coronal field constructed from the Solar and Heliospheric
Observatory/Michelson Doppler Imager full-disk magnetogram at 20:51:01
UT on 2006 December 12. The resulting coronal flux rope embedded in
the ambient coronal magnetic field first settles into a stage of
quasi-static rise and then undergoes a dynamic eruption, with the
leading edge of the flux rope cavity accelerating to a steady speed of
about 830 km s-1. The pre-eruption coronal magnetic field
shows morphology that is in qualitative agreement with that seen in
the Hinode soft X-ray observation in both the magnetic connectivity
as well as the development of an inverse-S-shaped X-ray sigmoid. We
examine the properties of the erupting flux rope and the morphology
of the post-reconnection loops, and compare them with the observations.
Title: Dynamic Evolution of Emerging Magnetic Flux Tubes in the
Solar Convective Envelope
Authors: Fan, Y.
Bibcode: 2011sdmi.confE..35F
Altcode:
I present recent results on modeling the buoyant rise of active region
scale flux tubes in the solar convective envelope based on both a thin
flux tube model incorporating the effects of giant-cell convection as
well as 3D spherical-shell anelastic MHD simulations. It is found that
the dynamic evolution of the flux tube changes from magnetic buoyancy
dominated to convection dominated as the initial field strength of
the flux tube varies from about 100 kG to 15 kG. Overall, the effect
of the convective flow is found to allow mid to weak field strength
range flux tubes (∼ 15 kG - 50 kG) to develop emerging loops with
properties that are more consistent with the observed properties of
solar active regions. For these flux tubes, the convective flow is
found to reduce the rise time, reduce the latitude of emergence through
anchoring by downdrafts, and promote tilt angles that are consistent
with the observed mean tilt of solar active regions because of the mean
kinetic helicity in the flow. The initial twist of the tube cannot be
too high in order for the tilt of the emerging loops to be dominated
by the effect of the Coriolis force and be consistent with the mean
tilt of solar active regions. I will also discuss the properties of the
emerging flux tube as it approaches the top layers of solar convective
envelope based on these models.
Title: Beating the Spin-down Limit on Gravitational Wave Emission
from the Vela Pulsar
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.;
Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.; Affeldt, C.;
Allen, B.; Allen, G. S.; Amador Ceron, E.; Amariutei, D.; Amin,
R. S.; Anderson, S. B.; Anderson, W. G.; Antonucci, F.; Arai, K.;
Arain, M. A.; Araya, M. C.; Aston, S. M.; Astone, P.; Atkinson,
D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker, P.;
Ballardin, G.; Ballmer, S.; Barker, D.; Barnum, S.; Barone, F.; Barr,
B.; Barriga, P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos,
I.; Bassiri, R.; Bastarrika, M.; Basti, A.; Bauchrowitz, J.; Bauer,
Th. S.; Behnke, B.; Bejger, M.; Beker, M. G.; Bell, A. S.; Belletoile,
A.; Belopolski, I.; Benacquista, M.; Bertolini, A.; Betzwieser, J.;
Beveridge, N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.;
Birch, J.; Birindelli, S.; Biswas, R.; Bitossi, M.; Bizouard, M. A.;
Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.;
Blom, M.; Bock, O.; Bodiya, T. P.; Bogan, C.; Bondarescu, R.; Bondu,
F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Boschi, V.; Bose,
S.; Bosi, L.; Bouhou, B.; Boyle, M.; Braccini, S.; Bradaschia, C.;
Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges,
D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks,
A. F.; Brown, D. A.; Brummit, A.; Budzyński, R.; Bulik, T.; Bulten,
H. J.; Buonanno, A.; Burguet-Castell, J.; Burmeister, O.; Buskulic, D.;
Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Cain, J.; Calloni,
E.; Camp, J. B.; Campagna, E.; Campsie, P.; Cannizzo, J.; Cannon,
K.; Canuel, B.; Cao, J.; Capano, C.; Carbognani, F.; Caride, S.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chaibi, O.; Chalermsongsak, T.; Chalkley,
E.; Charlton, P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, Y.;
Chincarini, A.; Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.;
Chung, S.; Clara, F.; Clark, D.; Clark, J.; Clayton, J. H.; Cleva,
F.; Coccia, E.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini, M.;
Conte, R.; Cook, D.; Corbitt, T. R.; Cornish, N.; Corsi, A.; Costa,
C. A.; Coughlin, M.; Coulon, J. -P.; Coward, D. M.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Cuoco, E.; Dahl, K.; Danilishin, S. L.;
Dannenberg, R.; D'Antonio, S.; Danzmann, K.; Das, K.; Dattilo, V.;
Daudert, B.; Daveloza, H.; Davier, M.; Davies, G.; Daw, E. J.; Day,
R.; Dayanga, T.; De Rosa, R.; DeBra, D.; Debreczeni, G.; Degallaix,
J.; del Prete, M.; Dent, T.; Dergachev, V.; DeRosa, R.; DeSalvo, R.;
Dhurandhar, S.; Di Fiore, L.; Di Lieto, A.; Di Palma, I.; Emilio, M. Di
Paolo; Di Virgilio, A.; Díaz, M.; Dietz, A.; Donovan, F.; Dooley,
K. L.; Dorsher, S.; Douglas, E. S. D.; Drago, M.; Drever, R. W. P.;
Driggers, J. C.; Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar, M.;
Edwards, M.; Effler, A.; Ehrens, P.; Engel, R.; Etzel, T.; Evans, M.;
Evans, T.; Factourovich, M.; Fafone, V.; Fairhurst, S.; Fan, Y.; Farr,
B. F.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Ferrante, I.; Fidecaro,
F.; Finn, L. S.; Fiori, I.; Flaminio, R.; Flanigan, M.; Foley, S.;
Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.; Franc,
J.; Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise,
A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov,
V. V.; Fulda, P.; Fyffe, M.; Galimberti, M.; Gammaitoni, L.; Garcia,
J.; Garofoli, J. A.; Garufi, F.; Gáspár, M. E.; Gemme, G.; Genin,
E.; Gennai, A.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina,
K. D.; Giazotto, A.; Gill, C.; Goetz, E.; Goggin, L. M.; González,
G.; Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Granata,
M.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.; Gretarsson,
A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald, S.; Guidi,
G. M.; Guido, C.; Gupta, R.; Gustafson, E. K.; Gustafson, R.; Hage,
B.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Hartman, M. T.; Haughian, K.; Hayama, K.; Hayau, J. -F.; Hayler, T.;
Heefner, J.; Heitmann, H.; Hello, P.; Hendry, M. A.; Heng, I. S.;
Heptonstall, A. W.; Herrera, V.; Hewitson, M.; Hild, S.; Hoak, D.;
Hodge, K. A.; Holt, K.; Hong, T.; Hooper, S.; Hosken, D. J.; Hough,
J.; Howell, E. J.; Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.;
Ingram, D. R.; Inta, R.; Isogai, T.; Ivanov, A.; Jaranowski, P.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kandhasamy, S.; Kanner, J. B.; Katsavounidis, E.;
Katzman, W.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Kelner,
M.; Keppel, D. G.; Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.;
Kim, H.; Kim, N.; King, P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko,
S.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Korth, W. Z.; Kowalska,
I.; Kozak, D.; Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Królak,
A.; Kuehn, G.; Kumar, R.; Kwee, P.; Landry, M.; Lantz, B.; Lastzka,
N.; Lazzarini, A.; Leaci, P.; Leong, J.; Leonor, I.; Leroy, N.;
Letendre, N.; Li, J.; Li, T. G. F.; Liguori, N.; Lindquist, P. E.;
Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand,
M.; Losurdo, G.; Lu, P.; Luan, J.; Lubinski, M.; Lück, H.; Lundgren,
A. P.; Macdonald, E.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Maksimovic, I.; Man, N.; Mandel, I.; Mandic,
V.; Mantovani, M.; Marandi, A.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McKechan, D. J. A.; Meadors,
G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.; Mendell,
G.; Mercer, R. A.; Merill, L.; Meshkov, S.; Messenger, C.; Meyer,
M. S.; Miao, H.; Michel, C.; Milano, L.; Miller, J.; Minenkov, Y.;
Mino, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa,
O.; Moe, B.; Moesta, P.; Mohan, M.; Mohanty, S. D.; Mohapatra,
S. R. P.; Moraru, D.; Moreno, G.; Morgado, N.; Morgia, A.; Mosca, S.;
Moscatelli, V.; Mossavi, K.; Mours, B.; Mow-Lowry, C. M.; Mueller,
G.; Mukherjee, S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.;
Murray, P. G.; Nash, T.; Nawrodt, R.; Nelson, J.; Neri, I.; Newton,
G.; Nishida, E.; Nishizawa, A.; Nocera, F.; Nolting, D.; Ochsner, E.;
O'Dell, J.; Ogin, G. H.; Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy,
R.; Osthelder, C.; Ott, C. D.; Ottaway, D. J.; Ottens, R. S.; Overmier,
H.; Owen, B. J.; Page, A.; Pagliaroli, G.; Palladino, L.; Palomba,
C.; Pan, Y.; Pankow, C.; Paoletti, F.; Papa, M. A.; Parameswaran, A.;
Pardi, S.; Parisi, M.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.;
Patel, P.; Pathak, D.; Pedraza, M.; Pekowsky, L.; Penn, S.; Peralta,
C.; Perreca, A.; Persichetti, G.; Phelps, M.; Pichot, M.; Pickenpack,
M.; Piergiovanni, F.; Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin,
M.; Pletsch, H. J.; Plissi, M. V.; Podkaminer, J.; Poggiani, R.;
Pöld, J.; Postiglione, F.; Prato, M.; Predoi, V.; Price, L. R.;
Prijatelj, M.; Principe, M.; Privitera, S.; Prix, R.; Prodi, G. A.;
Prokhorov, L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.;
Raab, F. J.; Rabeling, D. S.; Rácz, I.; Radkins, H.; Raffai, P.;
Rakhmanov, M.; Ramet, C. R.; Rankins, B.; Rapagnani, P.; Raymond,
V.; Re, V.; Redwine, K.; Reed, C. M.; Reed, T.; Regimbau, T.; Reid,
S.; Reitze, D. H.; Ricci, F.; Riesen, R.; Riles, K.; Roberts, P.;
Robertson, N. A.; Robinet, F.; Robinson, C.; Robinson, E. L.; Rocchi,
A.; Roddy, S.; Rolland, L.; Rollins, J.; Romano, J. D.; Romano, R.;
Romie, J. H.; Rosińska, D.; Röver, C.; Rowan, S.; Rüdiger, A.;
Ruggi, P.; Ryan, K.; Sakata, S.; Sakosky, M.; Salemi, F.; Salit,
M.; Sammut, L.; Sancho de la Jordana, L.; Sandberg, V.; Sannibale,
V.; Santamaría, L.; Santiago-Prieto, I.; Santostasi, G.; Saraf,
S.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.;
Saulson, P. R.; Savage, R.; Schilling, R.; Schlamminger, S.; Schnabel,
R.; Schofield, R. M. S.; Schulz, B.; Schutz, B. F.; Schwinberg, P.;
Scott, J.; Scott, S. M.; Searle, A. C.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Sentenac, D.; Sergeev, A.; Shaddock, D. A.; Shaltev,
M.; Shapiro, B.; Shawhan, P.; Shihan Weerathunga, T.; Shoemaker,
D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.; Singer, L.;
Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Smith, R.; Somiya, K.; Sorazu,
B.; Soto, J.; Speirits, F. C.; Sperandio, L.; Stefszky, M.; Stein,
A. J.; Steinlechner, J.; Steinlechner, S.; Steplewski, S.; Stochino,
A.; Stone, R.; Strain, K. A.; Strigin, S.; Stroeer, A. S.; Sturani,
R.; Stuver, A. L.; Summerscales, T. Z.; Sung, M.; Susmithan, S.;
Sutton, P. J.; Swinkels, B.; Szokoly, G. P.; Tacca, M.; Talukder, D.;
Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.; Thomas,
P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.; Thüring, A.; Titsler,
C.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.; Torre, O.; Torres,
C.; Torrie, C. I.; Tournefier, E.; Travasso, F.; Traylor, G.; Trias,
M.; Tseng, K.; Turner, L.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.;
Vaishnav, B.; Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.;
Van Den Broeck, C.; van der Putten, S.; van der Sluys, M. V.; van
Veggel, A. A.; Vass, S.; Vasuth, M.; Vaulin, R.; Vavoulidis, M.;
Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Veltkamp, C.;
Verkindt, D.; Vetrano, F.; Viceré, A.; Villar, A. E.; Vinet, J. -Y.;
Vocca, H.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace,
L.; Wanner, A.; Ward, R. L.; Was, M.; Wei, P.; Weinert, M.; Weinstein,
A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels, P.; West, M.; Westphal,
T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; White, D.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams,
L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman,
A. G.; Woan, G.; Wooley, R.; Worden, J.; Yablon, J.; Yakushin, I.;
Yamamoto, H.; Yamamoto, K.; Yang, H.; Yeaton-Massey, D.; Yoshida,
S.; Yu, P.; Yvert, M.; Zanolin, M.; Zhang, L.; Zhang, Z.; Zhao, C.;
Zotov, N.; Zucker, M. E.; Zweizig, J.; LIGO Scientific Collaboration;
Virgo Collaboration; Buchner, S.; Hotan, A.; Palfreyman, J.
Bibcode: 2011ApJ...737...93A
Altcode: 2011arXiv1104.2712T
We present direct upper limits on continuous gravitational wave
emission from the Vela pulsar using data from the Virgo detector's
second science run. These upper limits have been obtained using three
independent methods that assume the gravitational wave emission follows
the radio timing. Two of the methods produce frequentist upper limits
for an assumed known orientation of the star's spin axis and value of
the wave polarization angle of, respectively, 1.9 × 10-24
and 2.2 × 10-24, with 95% confidence. The third method,
under the same hypothesis, produces a Bayesian upper limit of 2.1 ×
10-24, with 95% degree of belief. These limits are below the
indirect spin-down limit of 3.3 × 10-24 for the Vela pulsar,
defined by the energy loss rate inferred from observed decrease in
Vela's spin frequency, and correspond to a limit on the star ellipticity
of ~10-3. Slightly less stringent results, but still well
below the spin-down limit, are obtained assuming the star's spin axis
inclination and the wave polarization angles are unknown.
Title: Solar Prominence Eruptions and CMEs at the Start of Cycle 24
Authors: de Toma, Giuliana; Gibson, S.; Burkepile, J.; Fan, Y.;
Reinard, A.
Bibcode: 2011shin.confE.147D
Altcode:
We present the analysis of prominence eruptions and CMEs during the
rising phase of cycle 24. We combine data from the two STEREO and
SDO spacecraft (that are near quadrature) to observe simultaneously
the region where a CME originates and the CME moving outward in the
plane-of-the-sky. This allows us to compute trajectories for the
CME and the associated eruptive prominence and, at the same time, to
study the on-disk CME manifestations such as flares, dimming regions,
and coronal waves with high spatial and temporal resolution.
Title: Search for gravitational waves from binary black hole inspiral,
merger, and ringdown
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.;
Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.; Ajith, P.;
Allen, B.; Allen, G. S.; Amador Ceron, E.; Amin, R. S.; Anderson,
S. B.; Anderson, W. G.; Antonucci, F.; Arain, M. A.; Araya, M. C.;
Aronsson, M.; Aso, Y.; Aston, S. M.; Astone, P.; Atkinson, D.; Aufmuth,
P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.; Ballinger,
T.; Ballmer, S.; Barker, D.; Barnum, S.; Barone, F.; Barr, B.;
Barriga, P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Bauchrowitz, J.; Bauer, Th. S.; Behnke,
B.; Beker, M. G.; Belletoile, A.; Benacquista, M.; Bertolini, A.;
Betzwieser, J.; Beveridge, N.; Beyersdorf, P. T.; Bilenko, I. A.;
Billingsley, G.; Birch, J.; Birindelli, S.; Biswas, R.; Bitossi,
M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.;
Blair, D.; Bland, B.; Blom, M.; Boccara, C.; Bock, O.; Bodiya, T. P.;
Bondarescu, R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born,
M.; Boschi, V.; Bose, S.; Bosi, L.; Bouhou, B.; Boyle, M.; Braccini,
S.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Breyer, J.; Bridges, D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.;
Britzger, M.; Brooks, A. F.; Brown, D. A.; Budzyński, R.; Bulik,
T.; Bulten, H. J.; Buonanno, A.; Burguet-Castell, J.; Burmeister, O.;
Buskulic, D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Cain,
J.; Calloni, E.; Camp, J. B.; Campagna, E.; Campsie, P.; Cannizzo,
J.; Cannon, K.; Canuel, B.; Cao, J.; Capano, C.; Carbognani, F.;
Caride, S.; Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.;
Cella, G.; Cepeda, C.; Cesarini, E.; Chaibi, O.; Chalermsongsak, T.;
Chalkley, E.; Charlton, P.; Chassande-Mottin, E.; Chelkowski, S.;
Chen, Y.; Chincarini, A.; Christensen, N.; Chua, S. S. Y.; Chung,
C. T. Y.; Clark, D.; Clark, J.; Clayton, J. H.; Cleva, F.; Coccia,
E.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini, M.; Conte, R.;
Cook, D.; Corbitt, T. R.; Cornish, N.; Corsi, A.; Costa, C. A.; Coulon,
J. -P.; Coward, D. M.; Coyne, D. C.; Creighton, J. D. E.; Creighton,
T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.; Cunningham, L.;
Cuoco, E.; Dahl, K.; Danilishin, S. L.; Dannenberg, R.; D'Antonio,
S.; Danzmann, K.; Das, K.; Dattilo, V.; Daudert, B.; Davier, M.;
Davies, G.; Davis, A.; Daw, E. J.; Day, R.; Dayanga, T.; Derosa, R.;
Debra, D.; Debreczeni, G.; Degallaix, J.; Del Prete, M.; Dergachev,
V.; de Rosa, R.; Desalvo, R.; Devanka, P.; Dhurandhar, S.; di Fiore,
L.; di Lieto, A.; di Palma, I.; di Paolo Emilio, M.; di Virgilio,
A.; Díaz, M.; Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes, E. E.;
Dorsher, S.; Douglas, E. S. D.; Drago, M.; Drever, R. W. P.; Driggers,
J. C.; Dueck, J.; Dumas, J. -C.; Eberle, T.; Edgar, M.; Edwards, M.;
Effler, A.; Ehrens, P.; Ely, G.; Engel, R.; Etzel, T.; Evans, M.;
Evans, T.; Fafone, V.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Fazi,
D.; Fehrmann, H.; Feldbaum, D.; Ferrante, I.; Fidecaro, F.; Finn,
L. S.; Fiori, I.; Flaminio, R.; Flanigan, M.; Flasch, K.; Foley, S.;
Forrest, C.; Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.;
Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.;
Freise, A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.;
Frolov, V. V.; Fulda, P.; Fyffe, M.; Galimberti, M.; Gammaitoni, L.;
Garofoli, J. A.; Garufi, F.; Gáspár, M. E.; Gemme, G.; Genin, E.;
Gennai, A.; Gholami, I.; Ghosh, S.; Giaime, J. A.; Giampanis, S.;
Giardina, K. D.; Giazotto, A.; Gill, C.; Goetz, E.; Goggin, L. M.;
González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.;
Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald,
S.; Guidi, G. M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hall,
P.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Haughian, K.; Hayama, K.; Hayau, J. -F.; Hayler, T.; Heefner, J.;
Heitmann, H.; Hello, P.; Heng, I. S.; Heptonstall, A. W.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken,
D. J.; Hough, J.; Howell, E. J.; Hoyland, D.; Huet, D.; Hughey, B.;
Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.; Inta, R.;
Isogai, T.; Ivanov, A.; Jaranowski, P.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kanner, J. B.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.;
Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khazanov, E. A.; Kim, H.; King, P. J.; Kinzel, D. L.; Kissel,
J. S.; Klimenko, S.; Kondrashov, V.; Kopparapu, R.; Koranda, S.;
Kowalska, I.; Kozak, D.; Krause, T.; Kringel, V.; Krishnamurthy,
S.; Krishnan, B.; Królak, A.; Kuehn, G.; Kullman, J.; Kumar, R.;
Kwee, P.; Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lazzarini,
A.; Leaci, P.; Leong, J.; Leonor, I.; Leroy, N.; Letendre, N.; Li,
J.; Li, T. G. F.; Liguori, N.; Lin, H.; Lindquist, P. E.; Lockerbie,
N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo,
G.; Lu, P.; Luan, J.; Lubiński, M.; Lucianetti, A.; Lück, H.;
Lundgren, A. D.; Machenschalk, B.; Macinnis, M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Mak, C.; Maksimovic, I.; Man, N.; Mandel,
I.; Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.;
Meadors, G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.;
Miller, J.; Minenkov, Y.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Moe, B.; Mohan, M.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moraru, D.; Moreau, J.; Moreno, G.; Morgado,
N.; Morgia, A.; Morioka, T.; Mors, K.; Mosca, S.; Moscatelli, V.;
Mossavi, K.; Mours, B.; Mow-Lowry, C. M.; Mueller, G.; Mukherjee,
S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murray, P. G.;
Nash, T.; Nawrodt, R.; Nelson, J.; Neri, I.; Newton, G.; Nishizawa,
A.; Nocera, F.; Nolting, D.; Ochsner, E.; O'Dell, J.; Ogin, G. H.;
Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.;
Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page,
A.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow,
C.; Paoletti, F.; Papa, M. A.; Pardi, S.; Pareja, M.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pathak,
D.; Pedraza, M.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.;
Persichetti, G.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.; Pietka,
M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi,
M. V.; Poggiani, R.; Postiglione, F.; Prato, M.; Predoi, V.; Price,
L. R.; Prijatelj, M.; Principe, M.; Prix, R.; Prodi, G. A.; Prokhorov,
L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Raab,
F. J.; Rabeling, D. S.; Rácz, I.; Radke, T.; Radkins, H.; Raffai,
P.; Rakhmanov, M.; Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.;
Reed, C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci,
F.; Riesen, R.; Riles, K.; Roberts, P.; Robertson, N. A.; Robinet,
F.; Robinson, C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Rolland,
L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.; Rosińska,
D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sakata,
S.; Sakosky, M.; Salemi, F.; Sammut, L.; Sancho de La Jordana, L.;
Sandberg, V.; Sannibale, V.; Santamaría, L.; Santostasi, G.; Saraf,
S.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.;
Saulson, P. R.; Savage, R.; Schilling, R.; Schnabel, R.; Schofield,
R. M. S.; Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott,
S. M.; Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.;
Sentenac, D.; Sergeev, A.; Shaddock, D. A.; Shapiro, B.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.;
Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Speirits,
F. C.; Sperandio, L.; Stein, A. J.; Stein, L. C.; Steinlechner, S.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin,
S.; Stroeer, A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.;
Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Szokoly, G. P.;
Tacca, M.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor,
J. R.; Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane,
E.; Thüring, A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.; Tonelli,
M.; Torre, O.; Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso, F.;
Traylor, G.; Trias, M.; Tseng, K.; Turner, L.; Ugolini, D.; Urbanek,
K.; Vahlbruch, H.; Vaishnav, B.; Vajente, G.; Vallisneri, M.; van den
Brand, J. F. J.; van den Broeck, C.; van der Putten, S.; van der Sluys,
M. V.; van Veggel, A. A.; Vass, S.; Vasuth, M.; Vaulin, R.; Vavoulidis,
M.; Vecchio, A.; Vedovato, G.; Veitch, J.; Veitch, P. J.; Veltkamp,
C.; Verkindt, D.; Vetrano, F.; Viceré, A.; Villar, A. E.; Vinet,
J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.;
Wallace, L.; Wanner, A.; Ward, R. L.; Was, M.; Wei, P.; Weinert, M.;
Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels, P.; West, M.;
Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; White, D.;
Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke,
B.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan,
G.; Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto,
K.; Yeaton-Massey, D.; Yoshida, S.; Yu, P.; Yvert, M.; Zanolin, M.;
Zhang, L.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig,
J.; LIGO Scientific Collaboration; Virgo Collaboration
Bibcode: 2011PhRvD..83l2005A
Altcode: 2011arXiv1102.3781T
We present the first modeled search for gravitational waves using
the complete binary black-hole gravitational waveform from inspiral
through the merger and ringdown for binaries with negligible component
spin. We searched approximately 2 years of LIGO data, taken between
November 2005 and September 2007, for systems with component masses of
1-99M⊙ and total masses of 25-100M⊙. We did
not detect any plausible gravitational-wave signals but we do place
upper limits on the merger rate of binary black holes as a function of
the component masses in this range. We constrain the rate of mergers for
19M⊙≤m1, m2≤28M⊙
binary black-hole systems with negligible spin to be no more than
2.0Mpc-3Myr-1 at 90% confidence.
Title: Search for Gravitational Wave Bursts from Six Magnetars
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.;
Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.; Affeldt, C.;
Allen, B.; Allen, G. S.; Amador Ceron, E.; Amariutei, D.; Amin,
R. S.; Anderson, S. B.; Anderson, W. G.; Antonucci, F.; Arai, K.;
Arain, M. A.; Araya, M. C.; Aston, S. M.; Astone, P.; Atkinson,
D.; Aufmuth, P.; Aulbert, C.; Aylott, B. E.; Babak, S.; Baker, P.;
Ballardin, G.; Ballmer, S.; Barker, D.; Barnum, S.; Barone, F.;
Barr, B.; Barriga, P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.;
Bartos, I.; Bassiri, R.; Bastarrika, M.; Basti, A.; Bauchrowitz, J.;
Bauer, Th. S.; Behnke, B.; Beker, M. G.; Bell, A. S.; Belletoile,
A.; Belopolski, I.; Benacquista, M.; Bertolini, A.; Betzwieser, J.;
Beveridge, N.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.;
Birch, J.; Birindelli, S.; Biswas, R.; Bitossi, M.; Bizouard, M. A.;
Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.;
Blom, M.; Bock, O.; Bodiya, T. P.; Bogan, C.; Bondarescu, R.; Bondu,
F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Boschi, V.; Bose,
S.; Bosi, L.; Bouhou, B.; Boyle, M.; Braccini, S.; Bradaschia, C.;
Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges,
D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks,
A. F.; Brown, D. A.; Brummit, A.; Budzyński, R.; Bulik, T.; Bulten,
H. J.; Buonanno, A.; Burguet-Castell, J.; Burmeister, O.; Buskulic, D.;
Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Cain, J.; Calloni,
E.; Camp, J. B.; Campagna, E.; Campsie, P.; Cannizzo, J.; Cannon,
K.; Canuel, B.; Cao, J.; Capano, C.; Carbognani, F.; Caride, S.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chaibi, O.; Chalermsongsak, T.; Chalkley,
E.; Charlton, P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, Y.;
Chincarini, A.; Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.;
Chung, S.; Clara, F.; Clark, D.; Clark, J.; Clayton, J. H.; Cleva,
F.; Coccia, E.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini, M.;
Conte, R.; Cook, D.; Corbitt, T. R.; Cornish, N.; Corsi, A.; Costa,
C. A.; Coughlin, M.; Coulon, J. -P.; Coward, D. M.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Cuoco, E.; Dahl, K.; Danilishin, S. L.;
Dannenberg, R.; D'Antonio, S.; Danzmann, K.; Das, K.; Dattilo, V.;
Daudert, B.; Daveloza, H.; Davier, M.; Davies, G.; Daw, E. J.; Day,
R.; Dayanga, T.; De Rosa, R.; DeBra, D.; Debreczeni, G.; Degallaix,
J.; del Prete, M.; Dent, T.; Dergachev, V.; DeRosa, R.; DeSalvo, R.;
Dhurandhar, S.; Di Fiore, L.; Di Lieto, A.; Di Palma, I.; Emilio, M. Di
Paolo; Di Virgilio, A.; Díaz, M.; Dietz, A.; Donovan, F.; Dooley,
K. L.; Dorsher, S.; Douglas, E. S. D.; Drago, M.; Drever, R. W. P.;
Driggers, J. C.; Dumas, J. -C.; Dwyer, S.; Eberle, T.; Edgar, M.;
Edwards, M.; Effler, A.; Ehrens, P.; Engel, R.; Etzel, T.; Evans, M.;
Evans, T.; Factourovich, M.; Fafone, V.; Fairhurst, S.; Fan, Y.; Farr,
B. F.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Ferrante, I.; Fidecaro,
F.; Finn, L. S.; Fiori, I.; Flaminio, R.; Flanigan, M.; Foley, S.;
Forsi, E.; Forte, L. A.; Fotopoulos, N.; Fournier, J. -D.; Franc,
J.; Frasca, S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise,
A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov,
V. V.; Fulda, P.; Fyffe, M.; Galimberti, M.; Gammaitoni, L.; Garcia,
J.; Garofoli, J. A.; Garufi, F.; Gáspár, M. E.; Gemme, G.; Genin,
E.; Gennai, A.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina,
K. D.; Giazotto, A.; Gill, C.; Goetz, E.; Goggin, L. M.; González,
G.; Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Granata,
M.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.; Gretarsson,
A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald, S.; Guidi,
G. M.; Guido, C.; Gupta, R.; Gustafson, E. K.; Gustafson, R.; Hage,
B.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Hartman, M. T.; Haughian, K.; Hayama, K.; Hayau, J. -F.; Hayler, T.;
Heefner, J.; Heitmann, H.; Hello, P.; Hendry, M. A.; Heng, I. S.;
Heptonstall, A. W.; Herrera, V.; Hewitson, M.; Hild, S.; Hoak, D.;
Hodge, K. A.; Holt, K.; Hong, T.; Hooper, S.; Hosken, D. J.; Hough,
J.; Howell, E. J.; Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.;
Ingram, D. R.; Inta, R.; Isogai, T.; Ivanov, A.; Jaranowski, P.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kandhasamy, S.; Kanner, J. B.; Katsavounidis, E.;
Katzman, W.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Kelner,
M.; Keppel, D. G.; Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.;
Kim, H.; Kim, N.; King, P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko,
S.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Korth, W. Z.; Kowalska,
I.; Kozak, D.; Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Królak,
A.; Kuehn, G.; Kumar, R.; Kwee, P.; Landry, M.; Lantz, B.; Lastzka,
N.; Lazzarini, A.; Leaci, P.; Leong, J.; Leonor, I.; Leroy, N.;
Letendre, N.; Li, J.; Li, T. G. F.; Liguori, N.; Lindquist, P. E.;
Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand,
M.; Losurdo, G.; Lu, P.; Luan, J.; Lubiński, M.; Lück, H.; Lundgren,
A. P.; Macdonald, E.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Maksimovic, I.; Man, N.; Mandel, I.; Mandic,
V.; Mantovani, M.; Marandi, A.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McKechan, D. J. A.; Meadors,
G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.; Mendell,
G.; Mercer, R. A.; Merill, L.; Meshkov, S.; Messenger, C.; Meyer,
M. S.; Miao, H.; Michel, C.; Milano, L.; Miller, J.; Minenkov, Y.;
Mino, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Moe, B.; Moesta, P.; Mohan, M.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moraru, D.; Moreno, G.; Morgado, N.; Morgia,
A.; Mosca, S.; Moscatelli, V.; Mossavi, K.; Mours, B.; Mow-Lowry,
C. M.; Mueller, G.; Mukherjee, S.; Mullavey, A.; Müller-Ebhardt, H.;
Munch, J.; Murray, P. G.; Nash, T.; Nawrodt, R.; Nelson, J.; Neri,
I.; Newton, G.; Nishida, E.; Nishizawa, A.; Nocera, F.; Nolting, D.;
Ochsner, E.; O'Dell, J.; Ogin, G. H.; Oldenburg, R. G.; O'Reilly,
B.; O'Shaughnessy, R.; Osthelder, C.; Ott, C. D.; Ottaway, D. J.;
Ottens, R. S.; Overmier, H.; Owen, B. J.; Page, A.; Pagliaroli, G.;
Palladino, L.; Palomba, C.; Pan, Y.; Pankow, C.; Paoletti, F.; Papa,
M. A.; Parameswaran, A.; Pardi, S.; Parisi, M.; Pasqualetti, A.;
Passaquieti, R.; Passuello, D.; Patel, P.; Pathak, D.; Pedraza, M.;
Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.; Persichetti, G.;
Phelps, M.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.; Pietka,
M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi,
M. V.; Podkaminer, J.; Poggiani, R.; Pöld, J.; Postiglione, F.;
Prato, M.; Predoi, V.; Price, L. R.; Prijatelj, M.; Principe, M.;
Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov, L.; Puncken, O.;
Punturo, M.; Puppo, P.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.;
Rácz, I.; Radkins, H.; Raffai, P.; Rakhmanov, M.; Ramet, C. R.;
Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Redwine, K.; Reed,
C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.;
Riesen, R.; Riles, K.; Roberts, P.; Robertson, N. A.; Robinet, F.;
Robinson, C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Rolland, L.;
Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.; Rosińska, D.;
Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sakata, S.;
Sakosky, M.; Salemi, F.; Salit, M.; Sammut, L.; Sancho de la Jordana,
L.; Sandberg, V.; Sannibale, V.; Santamaría, L.; Santiago-Prieto,
I.; Santostasi, G.; Saraf, S.; Sassolas, B.; Sathyaprakash, B. S.;
Sato, S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.; Schilling,
R.; Schlamminger, S.; Schnabel, R.; Schofield, R. M. S.; Schulz, B.;
Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.;
Seifert, F.; Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sergeev,
A.; Shaddock, D. A.; Shaltev, M.; Shapiro, B.; Shawhan, P.; Shihan
Weerathunga, T.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg,
D.; Singer, A.; Singer, L.; Sintes, A. M.; Skelton, G.; Slagmolen,
B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Smith,
R.; Somiya, K.; Sorazu, B.; Soto, J.; Speirits, F. C.; Sperandio,
L.; Stefszky, M.; Stein, A. J.; Steinlechner, J.; Steinlechner, S.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S.;
Stroeer, A. S.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sung,
M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Szokoly, G. P.; Tacca,
M.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.;
Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.;
Thüring, A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.; Tonelli,
M.; Torre, O.; Torres, C.; Torrie, C. I.; Tournefier, E.; Travasso,
F.; Traylor, G.; Trias, M.; Tseng, K.; Turner, L.; Ugolini, D.;
Urbanek, K.; Vahlbruch, H.; Vaishnav, B.; Vajente, G.; Vallisneri,
M.; van den Brand, J. F. J.; Van Den Broeck, C.; van der Putten,
S.; van der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vasuth, M.;
Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.; Veitch, J.;
Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.; Viceré, A.;
Villar, A. E.; Vinet, J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin, S. P.;
Waldman, S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Was, M.; Wei, P.;
Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels,
P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.;
White, D.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams,
H. R.; Williams, L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf,
C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Yablon, J.;
Yakushin, I.; Yamamoto, H.; Yamamoto, K.; Yang, H.; Yeaton-Massey,
D.; Yoshida, S.; Yu, P.; Yvert, M.; Zanolin, M.; Zhang, L.; Zhang,
Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.; LIGO Scientific
Collaboration; Virgo Collaboration; Aptekar, R. L.; Boynton, W. V.;
Briggs, M. S.; Cline, T. L.; Connaughton, V.; Frederiks, D. D.;
Gehrels, N.; Goldsten, J. O.; Golovin, D.; van der Horst, A. J.;
Hurley, K. C.; Kaneko, Y.; von Kienlin, A.; Kouveliotou, C.; Krimm,
H. A.; Lin, L.; Mitrofanov, I.; Ohno, M.; Pal'shin, V. D.; Rau, A.;
Sanin, A.; Tashiro, M. S.; Terada, Y.; Yamaoka, K.
Bibcode: 2011ApJ...734L..35A
Altcode: 2010arXiv1011.4079L; 2010arXiv1011.4079A
Soft gamma repeaters (SGRs) and anomalous X-ray pulsars (AXPs) are
thought to be magnetars: neutron stars powered by extreme magnetic
fields. These rare objects are characterized by repeated and sometimes
spectacular gamma-ray bursts. The burst mechanism might involve
crustal fractures and excitation of non-radial modes which would emit
gravitational waves (GWs). We present the results of a search for GW
bursts from six galactic magnetars that is sensitive to neutron star
f-modes, thought to be the most efficient GW emitting oscillatory
modes in compact stars. One of them, SGR 0501+4516, is likely ~1
kpc from Earth, an order of magnitude closer than magnetars targeted
in previous GW searches. A second, AXP 1E 1547.0-5408, gave a burst
with an estimated isotropic energy >1044 erg which is
comparable to the giant flares. We find no evidence of GWs associated
with a sample of 1279 electromagnetic triggers from six magnetars
occurring between 2006 November and 2009 June, in GW data from the LIGO,
Virgo, and GEO600 detectors. Our lowest model-dependent GW emission
energy upper limits for band- and time-limited white noise bursts in
the detector sensitive band, and for f-mode ringdowns (at 1090 Hz),
are 3.0 × 1044 d 2 1 erg and 1.4
× 1047 d 2 1 erg, respectively,
where d_{1} = \frac{d_{{0501}}}{1\,{kpc}} and d 0501 is the
distance to SGR 0501+4516. These limits on GW emission from f-modes are
an order of magnitude lower than any previous, and approach the range
of electromagnetic energies seen in SGR giant flares for the first time.
Title: Comparison Between Observation and Simulation of Magnetic
Field Changes Associated with Flares
Authors: Li, Yixuan; Jing, J.; Fan, Y.; Wang, H.
Bibcode: 2011SPD....42.2220L
Altcode: 2011BAAS..43S.2220L
It has been a long-standing question in solar physics how magnetic
field structure changes with eruptive events (e.g., flares and coronal
mass ejections). In an effort to understand the physics behind the
phenomena, we present the eruption-associated changes in magnetic
inclination angle, the horizontal component of magnetic field vectors,
the Lorentz force, the magnetic shear angle and the footpoint motion
of the flare. The study is mainly based on the three-dimensional MHD
simulation of the evolution of the magnetic field in the corona by
Yuhong Fan, and compared with some observational data. The results
suggest that the field lines at the flaring magnetic polarity inversion
line become more horizontal near the surface, that is in agreement
with the prediction of Hudson et al. In addition, the footpoints show
the de-shearing and diverging motion following the converging motion
during the flare.
Title: The Rise of Active Region Flux Tubes in the Turbulent Solar
Convective Envelope
Authors: Weber, Maria A.; Fan, Y.; Miesch, M.
Bibcode: 2011SPD....42.0206W
Altcode: 2011BAAS..43S.0206W
We use a thin flux tube model in a rotating spherical shell of
turbulent convective flows to study how active region scale flux
tubes rise buoyantly from the bottom of the convection zone to near
the solar surface. We investigate toroidal flux tubes at the base
of the convection zone with field strengths ranging from 15 kG to
100 kG at initial latitudes ranging from 1 to 40 degrees. We find
that the dynamic evolution of the flux tube changes from convection
dominated to magnetic buoyancy dominated as the initial field strength
increases from 15 kG to 100 kG. At 100 kG, the development of rising
loops are mainly controlled by the growth of the magnetic buoyancy
instability. Mean properties of the emerging loops are in agreement
with previous thin flux tube models in the absence of convection. At
a low field strength of 15 kG, the development of the rising loops
are largely controlled by convective flows, and the properties of the
emerging loops are significantly changed compared to previous results
in the absence of convection. With convection, the rise times are
drastically reduced (from years to months), and the loops are able to
emerge at low latitudes. However the tilt angles of these emerging
loops show large scatters and are not consistent with Joy's law of
active region tilts. In order for the mean tilts of emerging loops to
be consistent with Joy's Law, the initial field strength at the base
of the convection zone needs to be greater than or equal to 40 kG. We
also examine other asymmetries that develop between the leading and
following sides of the emerging loops. Including all results, we find
that field strengths of 40 - 50 kG produce emerging loops that best
match the observed properties of solar active regions.
Title: Publisher's Note: Search for gravitational waves associated
with the August 2006 timing glitch of the Vela pulsar [Phys. Rev. D
83, 042001 (2011)]
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith,
P.; Allen, B.; Allen, G.; Amador Ceron, E.; Amin, R. S.; Anderson,
S. B.; Anderson, W. G.; Arain, M. A.; Araya, M.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker,
D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista, M.; Bennett,
M. F.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.;
Bland, B.; Bock, O.; Bodiya, T. P.; Bondarescu, R.; Bork, R.; Born,
M.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer,
J.; Bridges, D. O.; Brinkmann, M.; Britzger, M.; Brooks, A. F.;
Brown, D. A.; Bullington, A.; Buonanno, A.; Burmeister, O.; Byer,
R. L.; Cadonati, L.; Cain, J.; Camp, J. B.; Cannizzo, J.; Cannon,
K. C.; Cao, J.; Capano, C.; Cardenas, L.; Caudill, S.; Cavaglià, M.;
Cepeda, C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chatterji,
S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Chua, S. S. Y.; Chung,
C. T. Y.; Clark, D.; Clark, J.; Clayton, J. H.; Conte, R.; Cook, D.;
Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Dahl, K.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; Dayanga, T.; Debra, D.; Degallaix, J.;
Dergachev, V.; Desalvo, R.; Dhurandhar, S.; Díaz, M.; Donovan, F.;
Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Driggers, J.; Dueck,
J.; Duke, I.; Dumas, J. -C.; Edgar, M.; Edwards, M.; Effler, A.;
Ehrens, P.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Faltas, Y.;
Fan, Y.; Fazi, D.; Fehrmann, H.; Finn, L. S.; Flasch, K.; Foley, S.;
Forrest, C.; Fotopoulos, N.; Frede, M.; Frei, M.; Frei, Z.; Freise,
A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov,
V. V.; Fulda, P.; Fyffe, M.; Garofoli, J. A.; Ghosh, S.; Giaime, J. A.;
Giampanis, S.; Giardina, K. D.; Goetz, E.; Goggin, L. M.; González,
G.; Goßler, S.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Grosso, R.; Grote, H.; Grunewald, S.; Gustafson,
E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer, D.; Hammond,
G. D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.;
Harstad, E. D.; Haughian, K.; Hayama, K.; Hayler, T.; Heefner, J.;
Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose, E.;
Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough, J.; Howell,
E.; Hoyland, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Ingram, D. R.;
Isogai, T.; Ivanov, A.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones,
R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy, S.; Kanner, J.;
Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.;
Keppel, D. G.; Khalaidovski, A.; Khalili, F. Y.; Khan, R.; Khazanov,
E.; Kim, H.; King, P. J.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.;
Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.; Kringel, V.;
Krishnan, B.; Kuehn, G.; Kullman, J.; Kumar, R.; Kwee, P.; Lam, P. K.;
Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lazzarini, A.; Leaci,
P.; Lei, M.; Leindecker, N.; Leonor, I.; Lin, H.; Lindquist, P. E.;
Littenberg, T. B.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu, P.;
Lubiński, M.; Lucianetti, A.; Lück, H.; Lundgren, A.; Machenschalk,
B.; Macinnis, M.; Mageswaran, M.; Mailand, K.; Mak, C.; Mandel,
I.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.; Markowitz,
J.; Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.;
Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.;
McClelland, D. E.; McGuire, S. C.; McIntyre, G.; McKechan, D. J. A.;
Mehmet, M.; Melatos, A.; Melissinos, A. C.; Mendell, G.; Menéndez,
D. F.; Mercer, R. A.; Merrill, L.; Meshkov, S.; Messenger, C.; Meyer,
M. S.; Miao, H.; Miller, J.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moreno, G.; Mors, K.; Mossavi, K.; Mowlowry, C.;
Mueller, G.; Müller-Ebhardt, H.; Mukherjee, S.; Mullavey, A.; Munch,
J.; Murray, P. G.; Nash, T.; Nawrodt, R.; Nelson, J.; Newton, G.;
Nishida, E.; Nishizawa, A.; O'Dell, J.; O'Reilly, B.; O'Shaughnessy,
R.; Ochsner, E.; Ogin, G. H.; Oldenburg, R.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Page, A.; Pan, Y.; Pankow, C.; Papa,
M. A.; Patel, P.; Pathak, D.; Pedraza, M.; Pekowsky, L.; Penn, S.;
Peralta, C.; Perreca, A.; Pickenpack, M.; Pinto, I. M.; Pitkin, M.;
Pletsch, H. J.; Plissi, M. V.; Postiglione, F.; Principe, M.; Prix,
R.; Prokhorov, L.; Puncken, O.; Quetschke, V.; Raab, F. J.; Rabeling,
D. S.; Radkins, H.; Raffai, P.; Raics, Z.; Rakhmanov, M.; Raymond,
V.; Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.;
Riesen, R.; Riles, K.; Roberts, P.; Robertson, N. A.; Robinson, C.;
Robinson, E. L.; Roddy, S.; Röver, C.; Rollins, J.; Romano, J. D.;
Romie, J. H.; Rowan, S.; Rüdiger, A.; Ryan, K.; Sakata, S.; Sammut,
L.; Sancho de La Jordana, L.; Sandberg, V.; Sannibale, V.; Santamaría,
L.; Santostasi, G.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato,
S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schulz, B.; Schutz, B. F.; Schwinberg,
P.; Scott, J.; Scott, S. M.; Searle, A. C.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Sergeev, A.; Shapiro, B.; Shawhan, P.; Shoemaker,
D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sintes, A. M.; Skelton,
G.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.;
Smith, N. D.; Somiya, K.; Sorazu, B.; Speirits, F.; Stein, A. J.;
Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.;
Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.; Sung,
M.; Susmithan, S.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.;
Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.; Thorne,
K. A.; Thorne, K. S.; Thüring, A.; Titsler, C.; Tokmakov, K. V.;
Torres, C.; Torrie, C. I.; Traylor, G.; Trias, M.; Turner, L.; Ugolini,
D.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; van den Broeck,
C.; van der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin, R.;
Vecchio, A.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Villar, A.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Wanner,
A.; Ward, R. L.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss,
R.; Wen, L.; Wen, S.; Wessels, P.; West, M.; Westphal, T.; Wette,
K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut,
I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan,
G.; Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto,
K.; Yeaton-Massey, D.; Yoshida, S.; Zanolin, M.; Zhang, L.; Zhang,
Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.; Buchner, S.
Bibcode: 2011PhRvD..83f9902A
Altcode:
No abstract at ADS
Title: Search for gravitational waves associated with the August
2006 timing glitch of the Vela pulsar
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith,
P.; Allen, B.; Allen, G.; Amador Ceron, E.; Amin, R. S.; Anderson,
S. B.; Anderson, W. G.; Arain, M. A.; Araya, M.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker,
D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista, M.; Bennett,
M. F.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.;
Bland, B.; Bock, O.; Bodiya, T. P.; Bondarescu, R.; Bork, R.; Born,
M.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer,
J.; Bridges, D. O.; Brinkmann, M.; Britzger, M.; Brooks, A. F.;
Brown, D. A.; Bullington, A.; Buonanno, A.; Burmeister, O.; Byer,
R. L.; Cadonati, L.; Cain, J.; Camp, J. B.; Cannizzo, J.; Cannon,
K. C.; Cao, J.; Capano, C.; Cardenas, L.; Caudill, S.; Cavaglià, M.;
Cepeda, C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chatterji,
S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Chua, S. S. Y.; Chung,
C. T. Y.; Clark, D.; Clark, J.; Clayton, J. H.; Conte, R.; Cook, D.;
Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Dahl, K.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; Dayanga, T.; Debra, D.; Degallaix, J.;
Dergachev, V.; Desalvo, R.; Dhurandhar, S.; Díaz, M.; Donovan, F.;
Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Driggers, J.; Dueck,
J.; Duke, I.; Dumas, J. -C.; Edgar, M.; Edwards, M.; Effler, A.;
Ehrens, P.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Faltas, Y.;
Fan, Y.; Fazi, D.; Fehrmann, H.; Finn, L. S.; Flasch, K.; Foley, S.;
Forrest, C.; Fotopoulos, N.; Frede, M.; Frei, M.; Frei, Z.; Freise,
A.; Frey, R.; Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov,
V. V.; Fulda, P.; Fyffe, M.; Garofoli, J. A.; Ghosh, S.; Giaime, J. A.;
Giampanis, S.; Giardina, K. D.; Goetz, E.; Goggin, L. M.; González,
G.; Goßler, S.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Grosso, R.; Grote, H.; Grunewald, S.; Gustafson,
E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer, D.; Hammond,
G. D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.;
Harstad, E. D.; Haughian, K.; Hayama, K.; Hayler, T.; Heefner, J.;
Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose, E.;
Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough, J.; Howell,
E.; Hoyland, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Ingram, D. R.;
Isogai, T.; Ivanov, A.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones,
R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy, S.; Kanner, J.;
Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.;
Keppel, D. G.; Khalaidovski, A.; Khalili, F. Y.; Khan, R.; Khazanov,
E.; Kim, H.; King, P. J.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.;
Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.; Kringel, V.;
Krishnan, B.; Kuehn, G.; Kullman, J.; Kumar, R.; Kwee, P.; Lam, P. K.;
Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lazzarini, A.; Leaci,
P.; Lei, M.; Leindecker, N.; Leonor, I.; Lin, H.; Lindquist, P. E.;
Littenberg, T. B.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu, P.;
Lubiński, M.; Lucianetti, A.; Lück, H.; Lundgren, A.; Machenschalk,
B.; Macinnis, M.; Mageswaran, M.; Mailand, K.; Mak, C.; Mandel,
I.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.; Markowitz,
J.; Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.;
Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.;
McClelland, D. E.; McGuire, S. C.; McIntyre, G.; McKechan, D. J. A.;
Mehmet, M.; Melatos, A.; Melissinos, A. C.; Mendell, G.; Menéndez,
D. F.; Mercer, R. A.; Merrill, L.; Meshkov, S.; Messenger, C.; Meyer,
M. S.; Miao, H.; Miller, J.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moreno, G.; Mors, K.; Mossavi, K.; Mowlowry, C.;
Mueller, G.; Müller-Ebhardt, H.; Mukherjee, S.; Mullavey, A.; Munch,
J.; Murray, P. G.; Nash, T.; Nawrodt, R.; Nelson, J.; Newton, G.;
Nishida, E.; Nishizawa, A.; O'Dell, J.; O'Reilly, B.; O'Shaughnessy,
R.; Ochsner, E.; Ogin, G. H.; Oldenburg, R.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Page, A.; Pan, Y.; Pankow, C.; Papa,
M. A.; Patel, P.; Pathak, D.; Pedraza, M.; Pekowsky, L.; Penn, S.;
Peralta, C.; Perreca, A.; Pickenpack, M.; Pinto, I. M.; Pitkin, M.;
Pletsch, H. J.; Plissi, M. V.; Postiglione, F.; Principe, M.; Prix,
R.; Prokhorov, L.; Puncken, O.; Quetschke, V.; Raab, F. J.; Rabeling,
D. S.; Radkins, H.; Raffai, P.; Raics, Z.; Rakhmanov, M.; Raymond,
V.; Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.;
Riesen, R.; Riles, K.; Roberts, P.; Robertson, N. A.; Robinson, C.;
Robinson, E. L.; Roddy, S.; Röver, C.; Rollins, J.; Romano, J. D.;
Romie, J. H.; Rowan, S.; Rüdiger, A.; Ryan, K.; Sakata, S.; Sammut,
L.; Sancho de La Jordana, L.; Sandberg, V.; Sannibale, V.; Santamaría,
L.; Santostasi, G.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato,
S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schulz, B.; Schutz, B. F.; Schwinberg,
P.; Scott, J.; Scott, S. M.; Searle, A. C.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Sergeev, A.; Shapiro, B.; Shawhan, P.; Shoemaker,
D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sintes, A. M.; Skelton,
G.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.;
Smith, N. D.; Somiya, K.; Sorazu, B.; Speirits, F.; Stein, A. J.;
Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.;
Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.; Sung,
M.; Susmithan, S.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.;
Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.; Thorne,
K. A.; Thorne, K. S.; Thüring, A.; Titsler, C.; Tokmakov, K. V.;
Torres, C.; Torrie, C. I.; Traylor, G.; Trias, M.; Turner, L.; Ugolini,
D.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; van den Broeck,
C.; van der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin, R.;
Vecchio, A.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Villar, A.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Wanner,
A.; Ward, R. L.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss,
R.; Wen, L.; Wen, S.; Wessels, P.; West, M.; Westphal, T.; Wette,
K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut,
I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan,
G.; Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto,
K.; Yeaton-Massey, D.; Yoshida, S.; Zanolin, M.; Zhang, L.; Zhang,
Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.; Buchner, S.
Bibcode: 2011PhRvD..83d2001A
Altcode: 2010arXiv1011.1357T
The physical mechanisms responsible for pulsar timing glitches are
thought to excite quasinormal mode oscillations in their parent neutron
star that couple to gravitational-wave emission. In August 2006, a
timing glitch was observed in the radio emission of PSR B0833-45,
the Vela pulsar. At the time of the glitch, the two colocated
Hanford gravitational-wave detectors of the Laser Interferometer
Gravitational-wave observatory (LIGO) were operational and taking
data as part of the fifth LIGO science run (S5). We present the first
direct search for the gravitational-wave emission associated with
oscillations of the fundamental quadrupole mode excited by a pulsar
timing glitch. No gravitational-wave detection candidate was found. We
place Bayesian 90% confidence upper limits of 6.3×10-21
to 1.4×10-20 on the peak intrinsic strain amplitude of
gravitational-wave ring-down signals, depending on which spherical
harmonic mode is excited. The corresponding range of energy upper
limits is 5.0×1044 to 1.3×1045erg.
Title: Dynamics of active region flux tubes in the solar convection
zone
Authors: Fan, Y.
Bibcode: 2011ASInC...2...81F
Altcode:
I review recent results on modeling the buoyant rise of active region
scale flux tubes in the solar convective envelope based on both a thin
flux tube model incorporating the effects of giant-cell convection
as well as direct 3D spherical-shell anelastic MHD simulations. It is
found that the dynamic evolution of the flux tube changes from magnetic
buoyancy dominated to convection dominated as the initial field strength
of the flux tube varies from about 100 kG to 15 kG. Mid-range field
strengths of about 40 - 50 kG seem to produce emerging loops that best
match the observed properties of solar active regions. The initial
twist of the tube cannot be too high in order for the tilt of the
emerging loops to be dominated by the effect of the Coriolis force and
be consistent with the mean tilt of solar active regions. Future high
resolution (low diffusivity) global-scale MHD simulations in a rotating,
fully convecting spherical shell representative of the solar convective
envelope are needed to self-consistently study the formation and dynamic
rise of active region scale flux tubes in the solar convection zone.
Title: 3D Study of Solar Eruptions Using SDO and STEREO Observations
Authors: de Toma, G.; Reinard, A. A.; Gibson, S. E.; Burkepile, J.;
Fan, Y.; Torok, T.
Bibcode: 2010AGUFMSH23A1834D
Altcode:
Combination of data from the recently launched SDO and the two STEREO
spacecraft -that are now at about 80deg from the Sun-Earth direction-
offers the unprecedented opportunity to observe simultaneously the
region where a CME originates and the CME moving outward in the
plane-of-the-sky. This allows us to compute trajectories for the
CME and the associated eruptive prominence and, at the same time, to
study the on-disk CME manifestations such as flares, dimming regions,
and coronal waves with very high spatial and temporal resolution. We
present examples of Earth-directed CMEs, when the CME can be traced
from the Sun to the Earth, that take advantage of this unique satellite
configuration.
Title: The Rise of Active Region Flux Tubes in the Turbulent Solar
Convective Envelope
Authors: Weber, M. A.; Fan, Y.; Miesch, M.
Bibcode: 2010AGUFMSH42A..03W
Altcode:
We use a thin flux tube model in a rotating spherical shell of
turbulent convective flows computed separately from an existing 3D
global simulation to study how active region scale flux tubes rise
buoyantly from the bottom of the convection zone to near the solar
surface. We investigate initial toroidal flux tubes at the base of
the convection zone with field strengths ranging from 15 kG to 100 kG
at initial latitudes ranging from 2 to 40 degrees. We find that the
dynamic evolution of the flux tube changes from magnetic buoyancy
dominated to convection dominated as we decrease the initial field
strength from 100 kG to 15 kG. At 100 kG, the strong tension of the
flux tube is able to resist the bending due to the convective flows and
the development of Omega-shaped rising loops are mainly controlled by
the growth of the magnetic buoyancy instability, with the strongest
convective down drafts producing some moderate perturbations to the
final emerging loops. The mean properties of the final emerging loops
are in agreement with previous thin flux tube models in the absence
of convection. On the other hand, at a low field strength of 15 kG, we
find that the development of the rising Omega-shaped loops are largely
controlled by the convective flows and the properties of the emerging
loops are significantly changed compared to the results from previous
thin flux tube models in the absence of convection. With convection,
the rise times are drastically reduced (from years to 1-2 months),
the loops are able to emerge at low latitudes, and the majority of the
emerging loops show tilt angles of the proper sign (consistent with
the active region tilts), and also show a field strength asymmetry
that would be consistent with the observed morphological asymmetry
of active regions. We discuss the implications of these results with
regard to the field strength of the dynamo generated large-scale
toroidal magnetic field at the base of the solar convection zone.
Title: On the Eruption of Coronal Flux Ropes
Authors: Fan, Y.
Bibcode: 2010AGUFMSH23B1842F
Altcode:
We present 3D MHD simulations of the evolution of the magnetic field in
the corona where the emergence of a twisted magnetic flux tube is driven
at the lower boundary into a pre-existing coronal potential arcade
field. In all the simulations, a quasi-equilibrium of a coronal flux
rope with an underlying sigmoid-shaped current sheet is formed after
the emergence is stopped, and subsequently the flux rope under-goes
a quasi-static rise due to reconnections in the current sheet. It is
found that the onset of eruption of the coronal flux rope takes place
when the flux rope reaches a critical height at which the corresponding
potential field declines with height at a sufficiently steep rate,
consistent with the onset of the torus instability of the flux rope. We
find that the modeled magnetic field evolution in the corona during
both the earlier quasi-static rise and the subsequent eruptive phase
can explain several basic observed features associated with eruptive
flares and CMEs originating from regions with pre-existing X-ray
sigmoids. We also report progress on simulations of improved realism
where the pre-existing coronal magnetic field and the lower boundary
driving conditions are specified based on the observed magnetic field
evolution on the solar surface.
Title: Calibration of the LIGO gravitational wave detectors in the
fifth science run
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.; Adams,
C.; Adhikari, R.; Ajith, P.; Allen, B.; Allen, G.; Amador Ceron, E.;
Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.; Araya,
M.; Aronsson, M.; Aso, Y.; Aston, S.; Atkinson, D. E.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker, D.; Barnum,
S.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Bauchrowitz, J.; Behnke, B.; Benacquista,
M.; Bertolini, A.; Betzwieser, J.; Beveridge, N.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas, R.; Black,
E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.; Bock,
O.; Bodiya, T. P.; Bondarescu, R.; Bork, R.; Born, M.; Bose, S.;
Boyle, M.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Breyer, J.;
Bridges, D. O.; Brinkmann, M.; Britzger, M.; Brooks, A. F.; Brown,
D. A.; Buonanno, A.; Burguet-Castell, J.; Burmeister, O.; Byer, R. L.;
Cadonati, L.; Cain, J.; Camp, J. B.; Campsie, P.; Cannizzo, J.; Cannon,
K. C.; Cao, J.; Capano, C.; Caride, S.; Caudill, S.; Cavaglià, M.;
Cepeda, C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chelkowski,
S.; Chen, Y.; Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.; Clark,
D.; Clark, J.; Clayton, J. H.; Conte, R.; Cook, D.; Corbitt, T. R.;
Cornish, N.; Costa, C. A.; Coward, D. M.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Dahl, K.; Danilishin, S. L.; Dannenberg, R.; Danzmann,
K.; Das, K.; Daudert, B.; Davies, G.; Davis, A.; Daw, E. J.; Dayanga,
T.; Debra, D.; Degallaix, J.; Dergachev, V.; Derosa, R.; Desalvo,
R.; Devanka, P.; Dhurandhar, S.; di Palma, I.; Díaz, M.; Donovan,
F.; Dooley, K. L.; Doomes, E. E.; Dorsher, S.; Douglas, E. S. D.;
Drever, R. W. P.; Driggers, J. C.; Dueck, J.; Dumas, J. -C.; Eberle,
T.; Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.; Engel, R.; Etzel,
T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Fazi,
D.; Fehrmann, H.; Feldbaum, D.; Finn, L. S.; Flanigan, M.; Flasch, K.;
Foley, S.; Forrest, C.; Forsi, E.; Fotopoulos, N.; Frede, M.; Frei,
M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich, D.;
Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Garofoli, J. A.;
Gholami, I.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.;
Gill, C.; Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky, M. L.;
Goßler, S.; Graef, C.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Grosso, R.; Grote, H.; Grunewald, S.;
Gustafson, E. K.; Gustafson, R.; Hage, B.; Hall, P.; Hallam, J. M.;
Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.; Hanson, J.; Harms, J.;
Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.;
Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall, A. W.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken,
D. J.; Hough, J.; Howell, E. J.; Hoyland, D.; Hughey, B.; Husa, S.;
Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.; Inta, R.; Isogai,
T.; Ivanov, A.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.;
Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy, S.; Kanner, J. B.;
Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.;
Keppel, D. G.; Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.;
Kim, H.; King, P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.;
Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.; Krause, T.;
Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Kuehn, G.; Kullman,
J.; Kumar, R.; Kwee, P.; Landry, M.; Lang, M.; Lantz, B.; Lastzka,
N.; Lazzarini, A.; Leaci, P.; Leong, J.; Leonor, I.; Li, J.; Lin,
H.; Lindquist, P. E.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu,
P.; Luan, J.; Lubinski, M.; Lucianetti, A.; Lück, H.; Lundgren,
A.; Machenschalk, B.; Macinnis, M.; Mageswaran, M.; Mailand, K.;
Mak, C.; Mandel, I.; Mandic, V.; Márka, S.; Márka, Z.; Maros, E.;
Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.;
Meadors, G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Miller, J.; Mino, Y.;
Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Moe,
B.; Mohanty, S. D.; Mohapatra, S. R. P.; Moraru, D.; Moreno, G.;
Morioka, T.; Mors, K.; Mossavi, K.; Mowlowry, C. M.; Mueller, G.;
Mukherjee, S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murray,
P. G.; Nash, T.; Nawrodt, R.; Nelson, J.; Newton, G.; Nishizawa,
A.; Nolting, D.; Ochsner, E.; O'Dell, J.; Ogin, G. H.; Oldenburg,
R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.; Ottaway,
D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page, A.; Pan, Y.;
Pankow, C.; Papa, M. A.; Pareja, M.; Patel, P.; Pathak, D.; Pedraza,
M.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.; Pickenpack, M.;
Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Postiglione,
F.; Predoi, V.; Price, L. R.; Prijatelj, M.; Principe, M.; Prix, R.;
Prokhorov, L.; Puncken, O.; Quetschke, V.; Raab, F. J.; Radke, T.;
Radkins, H.; Raffai, P.; Rakhmanov, M.; Rankins, B.; Raymond, V.;
Reed, C. M.; Reed, T.; Reid, S.; Reitze, D. H.; Riesen, R.; Riles,
K.; Roberts, P.; Robertson, N. A.; Robinson, C.; Robinson, E. L.;
Roddy, S.; Röver, C.; Rollins, J.; Romano, J. D.; Romie, J. H.;
Rowan, S.; Rüdiger, A.; Ryan, K.; Sakata, S.; Sakosky, M.; Salemi,
F.; Sammut, L.; Sancho de La Jordana, L.; Sandberg, V.; Sannibale,
V.; Santamaría, L.; Santostasi, G.; Saraf, S.; Sathyaprakash, B. S.;
Sato, S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.; Schilling,
R.; Schnabel, R.; Schofield, R. M. S.; Schulz, B.; Schutz, B. F.;
Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Seifert, F.;
Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shaddock, D. A.; Shapiro,
B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.;
Singer, A.; Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu,
B.; Speirits, F. C.; Stein, A. J.; Stein, L. C.; Steinlechner, S.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin,
S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.; Sung, M.;
Susmithan, S.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.; Tanner,
D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.; Thomas, P.; Thorne,
K. A.; Thorne, K. S.; Thrane, E.; Thüring, A.; Titsler, C.; Tokmakov,
K. V.; Torres, C.; Torrie, C. I.; Traylor, G.; Trias, M.; Tseng, K.;
Turner, L.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vaishnav, B.;
Vallisneri, M.; van den Broeck, C.; van der Sluys, M. V.; van Veggel,
A. A.; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P. J.;
Veltkamp, C.; Villar, A. E.; Vorvick, C.; Vyachanin, S. P.; Waldman,
S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Wei, P.; Weinert, M.;
Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels, P.; West, M.;
Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; White, D. J.;
Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke,
B.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan,
G.; Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto,
K.; Yeaton-Massey, D.; Yoshida, S.; Yu, P. P.; Zanolin, M.; Zhang,
L.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.;
LIGO Scientific Collaboration
Bibcode: 2010NIMPA.624..223A
Altcode: 2010arXiv1007.3973L
The Laser Interferometer Gravitational Wave Observatory (LIGO) is a
network of three detectors built to detect local perturbations in the
space-time metric from astrophysical sources. These detectors, two in
Hanford, WA and one in Livingston, LA, are power-recycled Fabry-Perot
Michelson interferometers. In their fifth science run (S5), between
November 2005 and October 2007, these detectors accumulated one year of
triple coincident data while operating at their designed sensitivity. In
this paper, we describe the calibration of the instruments in the S5
data set, including measurement techniques and uncertainty estimation.
Title: An Estimate of the Detectability of Rising Flux Tubes
Authors: Birch, A. C.; Braun, D. C.; Fan, Y.
Bibcode: 2010ApJ...723L.190B
Altcode:
The physics of the formation of magnetic active regions (ARs) is one
of the most important problems in solar physics. One main class of
theories suggests that ARs are the result of magnetic flux that rises
from the tachocline. Time-distance helioseismology, which is based on
measurements of wave propagation, promises to allow the study of the
subsurface behavior of this magnetic flux. Here, we use a model for a
buoyant magnetic flux concentration together with the ray approximation
to show that the dominant effect on the wave propagation is expected
to be from the roughly 100 m s-1 retrograde flow associated
with the rising flux. Using a B-spline-based method for carrying out
inversions of wave travel times for flows in spherical geometry, we
show that at 3 days before emergence the detection of this retrograde
flow at a depth of 30 Mm should be possible with a signal-to-noise
level of about 8 with a sample of 150 emerging ARs.
Title: Search for gravitational waves from compact binary coalescence
in LIGO and Virgo data from S5 and VSR1
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.; Accadia,
T.; Acernese, F.; Adams, C.; Adhikari, R.; Ajith, P.; Allen, B.;
Allen, G.; Amador Ceron, E.; Amin, R. S.; Anderson, S. B.; Anderson,
W. G.; Antonucci, F.; Arain, M. A.; Araya, M.; Aronsson, M.; Arun,
K. G.; Aso, Y.; Aston, S.; Astone, P.; Atkinson, D. E.; Aufmuth,
P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.; Ballinger, T.;
Ballmer, S.; Barker, D.; Barnum, S.; Barone, F.; Barr, B.; Barriga,
P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri,
R.; Bastarrika, M.; Bauchrowitz, J.; Bauer, Th. S.; Behnke, B.; Beker,
M. G.; Belletoile, A.; Benacquista, M.; Bertolini, A.; Betzwieser,
J.; Beveridge, N.; Beyersdorf, P. T.; Bigotta, S.; Bilenko, I. A.;
Billingsley, G.; Birch, J.; Birindelli, S.; Biswas, R.; Bitossi,
M.; Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.;
Blair, D.; Bland, B.; Blom, M.; Boccara, C.; Bock, O.; Bodiya,
T. P.; Bondarescu, R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork,
R.; Born, M.; Bose, S.; Bosi, L.; Bouhou, B.; Boyle, M.; Braccini,
S.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Breyer, J.; Bridges, D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.;
Britzger, M.; Brooks, A. F.; Brown, D. A.; Budzyński, R.; Bulik, T.;
Bulten, H. J.; Buonanno, A.; Burguet–Castell, J.; Burmeister, O.;
Buskulic, D.; Buy, C.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Cain,
J.; Calloni, E.; Camp, J. B.; Campagna, E.; Campsie, P.; Cannizzo,
J.; Cannon, K. C.; Canuel, B.; Cao, J.; Capano, C.; Carbognani, F.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chalermsongsak, T.; Chalkley, E.; Charlton,
P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, Y.; Chincarini, A.;
Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.; Clark, D.; Clark,
J.; Clayton, J. H.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas, J.;
Colla, A.; Colombini, M.; Conte, R.; Cook, D.; Corbitt, T. R.; Cornish,
N.; Corsi, A.; Costa, C. A.; Coulon, J. -P.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Cuoco, E.; Dahl, K.; Danilishin, S. L.;
Dannenberg, R.; D'Antonio, S.; Danzmann, K.; Das, K.; Dattilo, V.;
Daudert, B.; Davier, M.; Davies, G.; Davis, A.; Daw, E. J.; Day,
R.; Dayanga, T.; de Rosa, R.; Debra, D.; Degallaix, J.; Del Prete,
M.; Dergachev, V.; Derosa, R.; Desalvo, R.; Devanka, P.; Dhurandhar,
S.; di Fiore, L.; di Lieto, A.; di Palma, I.; di Paolo Emilio, M.;
di Virgilio, A.; Díaz, M.; Dietz, A.; Donovan, F.; Dooley, K. L.;
Doomes, E. E.; Dorsher, S.; Douglas, E. S. D.; Drago, M.; Drever,
R. W. P.; Driggers, J. C.; Dueck, J.; Dumas, J. -C.; Eberle, T.;
Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.; Ely, G.; Engel, R.;
Etzel, T.; Evans, M.; Evans, T.; Fafone, V.; Fairhurst, S.; Fan,
Y.; Farr, B. F.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Ferrante,
I.; Fidecaro, F.; Finn, L. S.; Fiori, I.; Flaminio, R.; Flanigan,
M.; Flasch, K.; Foley, S.; Forrest, C.; Forsi, E.; Fotopoulos, N.;
Fournier, J. -D.; Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich,
D.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Galimberti,
M.; Gammaitoni, L.; Garofoli, J. A.; Garufi, F.; Gemme, G.; Genin,
E.; Gennai, A.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina,
K. D.; Giazotto, A.; Gill, C.; Goetz, E.; Goggin, L. M.; González,
G.; Goßler, S.; Gouaty, R.; Graef, C.; Granata, M.; Grant, A.; Gras,
S.; Gray, C.; Greenhalgh, R. J. S.; Gretarsson, A. M.; Greverie,
C.; Grosso, R.; Grote, H.; Grunewald, S.; Guidi, G. M.; Gustafson,
E. K.; Gustafson, R.; Hage, B.; Hall, P.; Hallam, J. M.; Hammer,
D.; Hammond, G.; Hanks, J.; Hanna, C.; Hanson, J.; Harms, J.; Harry,
G. M.; Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.; Hayau,
J. -F.; Hayler, T.; Heefner, J.; Heitmann, H.; Hello, P.; Heng, I. S.;
Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge,
K. A.; Holt, K.; Hosken, D. J.; Hough, J.; Howell, E.; Hoyland, D.;
Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh–Dinh, T.;
Ingram, D. R.; Inta, R.; Isogai, T.; Ivanov, A.; Jaranowski, P.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kandhasamy, S.; Kanner, J.; Katsavounidis, E.;
Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.; Kim, H.; King,
P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.; Kondrashov, V.;
Kopparapu, R.; Koranda, S.; Kowalska, I.; Kozak, D.; Krause, T.;
Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Królak, A.; Kuehn, G.;
Kullman, J.; Kumar, R.; Kwee, P.; Landry, M.; Lang, M.; Lantz, B.;
Lastzka, N.; Lazzarini, A.; Leaci, P.; Leong, J.; Leonor, I.; Leroy,
N.; Letendre, N.; Li, J.; Li, T. G. F.; Lin, H.; Lindquist, P. E.;
Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.;
Losurdo, G.; Lu, P.; Luan, J.; Lubiński, M.; Lucianetti, A.; Lück,
H.; Lundgren, A.; Machenschalk, B.; Macinnis, M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Mak, C.; Maksimovic, I.; Man, N.; Mandel,
I.; Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.;
Meadors, G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.;
Miller, J.; Minenkov, Y.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Moe, B.; Mohan, M.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moraru, D.; Moreau, J.; Moreno, G.; Morgado,
N.; Morgia, A.; Mors, K.; Mosca, S.; Moscatelli, V.; Mossavi, K.;
Mours, B.; Mowlowry, C.; Mueller, G.; Mukherjee, S.; Mullavey, A.;
Müller-Ebhardt, H.; Munch, J.; Murray, P. G.; Nash, T.; Nawrodt,
R.; Nelson, J.; Neri, I.; Newton, G.; Nishida, E.; Nishizawa, A.;
Nocera, F.; Nolting, D.; Ochsner, E.; O'Dell, J.; Ogin, G. H.;
Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.;
Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page,
A.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow,
C.; Paoletti, F.; Papa, M. A.; Pardi, S.; Pareja, M.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pathak,
D.; Pedraza, M.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.;
Persichetti, G.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.; Pietka,
M.; Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi,
M. V.; Poggiani, R.; Postiglione, F.; Prato, M.; Predoi, V.; Price,
L. R.; Prijatelj, M.; Principe, M.; Prix, R.; Prodi, G. A.; Prokhorov,
L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Raab, F. J.;
Rabeling, D. S.; Radke, T.; Radkins, H.; Raffai, P.; Rakhmanov, M.;
Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Reed, C. M.; Reed,
T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.; Riesen, R.;
Riles, K.; Roberts, P.; Robertson, N. A.; Robinet, F.; Robinson,
C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Röver, C.; Rolland, L.;
Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.; Rosińska, D.;
Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sakata, S.; Sakosky,
M.; Salemi, F.; Sammut, L.; Sancho de La Jordana, L.; Sandberg, V.;
Sannibale, V.; Santamaría, L.; Santostasi, G.; Saraf, S.; Sassolas,
B.; Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.; Saulson, P. R.;
Savage, R.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz, B.;
Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.;
Seifert, F.; Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sergeev, A.;
Shaddock, D.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley,
A.; Siemens, X.; Sigg, D.; Singer, A.; Sintes, A. M.; Skelton, G.;
Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Smith,
N. D.; Somiya, K.; Sorazu, B.; Speirits, F. C.; Sperandio, L.; Stein,
A. J.; Stein, L. C.; Steinlechner, S.; Steplewski, S.; Stochino,
A.; Stone, R.; Strain, K. A.; Strigin, S.; Stroeer, A.; Sturani, R.;
Stuver, A. L.; Summerscales, T. Z.; Sung, M.; Susmithan, S.; Sutton,
P. J.; Swinkels, B.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.;
Taylor, J. R.; Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.;
Thrane, E.; Thüring, A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.;
Tonelli, M.; Torre, O.; Torres, C.; Torrie, C. I.; Tournefier, E.;
Travasso, F.; Traylor, G.; Trias, M.; Trummer, J.; Tseng, K.; Turner,
L.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vaishnav, B.; Vajente,
G.; Vallisneri, M.; van den Brand, J. F. J.; van den Broeck, C.;
van der Putten, S.; van der Sluys, M. V.; van Veggel, A. A.; Vass,
S.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.; Veitch,
J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.; Viceré,
A.; Villar, A.; Vinet, J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin,
S. P.; Waldman, S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Was,
M.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen,
S.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.;
Whitcomb, S. E.; White, D. J.; Whiting, B. F.; Wilkinson, C.; Willems,
P. A.; Williams, L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf,
C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Yakushin,
I.; Yamamoto, H.; Yamamoto, K.; Yeaton-Massey, D.; Yoshida, S.; Yu,
P. P.; Yvert, M.; Zanolin, M.; Zhang, L.; Zhang, Z.; Zhao, C.; Zotov,
N.; Zucker, M. E.; Zweizig, J.
Bibcode: 2010PhRvD..82j2001A
Altcode: 2010arXiv1005.4655T
We report the results of the first search for gravitational waves from
compact binary coalescence using data from the Laser Interferometer
Gravitational-Wave Observatory and Virgo detectors. Five months of data
were collected during the Laser Interferometer Gravitational-Wave
Observatory’s S5 and Virgo’s VSR1 science runs. The search
focused on signals from binary mergers with a total mass between 2
and 35M⊙. No gravitational waves are identified. The
cumulative 90%-confidence upper limits on the rate of compact
binary coalescence are calculated for nonspinning binary neutron
stars, black hole-neutron star systems, and binary black holes to
be 8.7×10-3yr-1L10-1,
2.2×10-3yr-1L10-1,
and 4.4×10-4yr-1L10-1,
respectively, where L10 is 1010 times the blue
solar luminosity. These upper limits are compared with astrophysical
expectations.
Title: First Search for Gravitational Waves from the Youngest Known
Neutron Star
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.; Adams,
C.; Adhikari, R.; Ajith, P.; Allen, B.; Allen, G.; Amador Ceron, E.;
Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.; Araya,
M.; Aronsson, M.; Aso, Y.; Aston, S.; Atkinson, D. E.; Aufmuth,
P.; Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker, D.;
Barnum, S.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.;
Bartos, I.; Bassiri, R.; Bastarrika, M.; Bauchrowitz, J.; Behnke,
B.; Benacquista, M.; Bertolini, A.; Betzwieser, J.; Beveridge, N.;
Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Birch, J.; Biswas,
R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland,
B.; Bock, O.; Bodiya, T. P.; Bondarescu, R.; Bork, R.; Born, M.;
Bose, S.; Boyle, M.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Breyer, J.; Bridges, D. O.; Brinkmann, M.; Britzger, M.; Brooks,
A. F.; Brown, D. A.; Buonanno, A.; Burguet-Castell, J.; Burmeister,
O.; Byer, R. L.; Cadonati, L.; Camp, J. B.; Campsie, P.; Cannizzo,
J.; Cannon, K. C.; Cao, J.; Capano, C.; Caride, S.; Caudill, S.;
Cavaglià, M.; Cepeda, C.; Chalermsongsak, T.; Chalkley, E.; Charlton,
P.; Chelkowski, S.; Chen, Y.; Christensen, N.; Chua, S. S. Y.; Chung,
C. T. Y.; Clark, D.; Clark, J.; Clayton, J. H.; Conte, R.; Cook, D.;
Corbitt, T. R.; Cornish, N.; Costa, C. A.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Dahl, K.; Danilishin, S. L.; Dannenberg,
R.; Danzmann, K.; Das, K.; Daudert, B.; Davies, G.; Davis, A.; Daw,
E. J.; Dayanga, T.; DeBra, D.; Degallaix, J.; Dergachev, V.; DeRosa,
R.; DeSalvo, R.; Devanka, P.; Dhurandhar, S.; Di Palma, I.; Díaz,
M.; Donovan, F.; Dooley, K. L.; Doomes, E. E.; Dorsher, S.; Douglas,
E. S. D.; Drever, R. W. P.; Driggers, J. C.; Dueck, J.; Dumas, J. -C.;
Eberle, T.; Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.; Engel,
R.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan, Y.; Farr,
B. F.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Finn, L. S.; Flanigan,
M.; Flasch, K.; Foley, S.; Forrest, C.; Forsi, E.; Fotopoulos, N.;
Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.;
Friedrich, D.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.;
Garofoli, J. A.; Gholami, I.; Ghosh, S.; Giaime, J. A.; Giampanis,
S.; Giardina, K. D.; Gill, C.; Goetz, E.; Goggin, L. M.; González,
G.; Gorodetsky, M. L.; Goßler, S.; Graef, C.; Grant, A.; Gras, S.;
Gray, C.; Greenhalgh, R. J. S.; Gretarsson, A. M.; Grosso, R.; Grote,
H.; Grunewald, S.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hall,
P.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Haughian, K.; Hayama, K.; Heefner, J.; Heng, I. S.; Heptonstall, A.;
Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt,
K.; Hosken, D. J.; Hough, J.; Howell, E.; Hoyland, D.; Hughey, B.;
Husa, S.; Huttner, S. H.; Huynh-Dinh, T.; Ingram, D. R.; Inta, R.;
Isogai, T.; Ivanov, A.; Johnson, W. W.; Jones, D. I.; Jones, G.;
Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy, S.; Kanner,
J.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells,
W.; Keppel, D. G.; Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.;
Kim, H.; King, P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.;
Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.; Krause, T.;
Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Kuehn, G.; Kullman,
J.; Kumar, R.; Kwee, P.; Landry, M.; Lang, M.; Lantz, B.; Lastzka,
N.; Lazzarini, A.; Leaci, P.; Leong, J.; Leonor, I.; Li, J.; Lin,
H.; Lindquist, P. E.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu,
P.; Luan, J.; Lubiński, M.; Lucianetti, A.; Lück, H.; Lundgren,
A.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand, K.;
Mak, C.; Mandel, I.; Mandic, V.; Márka, S.; Márka, Z.; Maros, E.;
Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.;
Meadors, G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Miller, J.; Mino, Y.;
Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Moe, B.; Mohanty, S. D.; Mohapatra, S. R. P.; Moraru, D.; Moreno,
G.; Morioka, T.; Mors, K.; Mossavi, K.; MowLowry, C.; Mueller, G.;
Mukherjee, S.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murray,
P. G.; Nash, T.; Nawrodt, R.; Nelson, J.; Newton, G.; Nishizawa,
A.; Nolting, D.; Ochsner, E.; O'Dell, J.; Ogin, G. H.; Oldenburg,
R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.; Ottaway,
D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page, A.; Pan,
Y.; Pankow, C.; Papa, M. A.; Pareja, M.; Patel, P.; Pedraza, M.;
Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.; Pickenpack, M.;
Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Postiglione,
F.; Predoi, V.; Price, L. R.; Prijatelj, M.; Principe, M.; Prix, R.;
Prokhorov, L.; Puncken, O.; Quetschke, V.; Raab, F. J.; Radke, T.;
Radkins, H.; Raffai, P.; Rakhmanov, M.; Rankins, B.; Raymond, V.;
Reed, C. M.; Reed, T.; Reid, S.; Reitze, D. H.; Riesen, R.; Riles,
K.; Roberts, P.; Robertson, N. A.; Robinson, C.; Robinson, E. L.;
Roddy, S.; Röver, C.; Rollins, J.; Romano, J. D.; Romie, J. H.;
Rowan, S.; Rüdiger, A.; Ryan, K.; Sakata, S.; Sakosky, M.; Salemi,
F.; Sammut, L.; Sancho de la Jordana, L.; Sandberg, V.; Sannibale,
V.; Santamaría, L.; Santostasi, G.; Saraf, S.; Sathyaprakash, B. S.;
Sato, S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schulz, B.; Schutz, B. F.; Schwinberg,
P.; Scott, J.; Scott, S. M.; Searle, A. C.; Seifert, F.; Sellers,
D.; Sengupta, A. S.; Sergeev, A.; Shaddock, D.; Shapiro, B.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer, A.;
Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Speirits,
F. C.; Stein, A. J.; Stein, L. C.; Steinlechner, S.; Steplewski,
S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S.; Stroeer,
A.; Stuver, A. L.; Summerscales, T. Z.; Sung, M.; Susmithan, S.;
Sutton, P. J.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor,
J. R.; Taylor, R.; Thomas, P.; Thorne, K. A.; Thorne, K. S.; Thrane,
E.; Thüring, A.; Titsler, C.; Tokmakov, K. V.; Torres, C.; Torrie,
C. I.; Traylor, G.; Trias, M.; Tseng, K.; Ugolini, D.; Urbanek, K.;
Vahlbruch, H.; Vaishnav, B.; Vallisneri, M.; Van Den Broeck, C.; van
der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin, R.; Vecchio,
A.; Veitch, J.; Veitch, P. J.; Veltkamp, C.; Villar, A.; Vorvick,
C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Wanner, A.; Ward,
R. L.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.;
Wen, S.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan,
J. T.; Whitcomb, S. E.; White, D. J.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, L.; Willke, B.; Winkelmann, L.; Winkler,
W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.;
Yakushin, I.; Yamamoto, H.; Yamamoto, K.; Yeaton-Massey, D.; Yoshida,
S.; Yu, P. P.; Zanolin, M.; Zhang, L.; Zhang, Z.; Zhao, C.; Zotov,
N.; Zucker, M. E.; Zweizig, J.; LIGO Scientific Collaboration
Bibcode: 2010ApJ...722.1504A
Altcode: 2010arXiv1006.2535L
We present a search for periodic gravitational waves from the neutron
star in the supernova remnant Cassiopeia A. The search coherently
analyzes data in a 12 day interval taken from the fifth science run of
the Laser Interferometer Gravitational-Wave Observatory. It searches
gravitational-wave frequencies from 100 to 300 Hz and covers a wide
range of first and second frequency derivatives appropriate for
the age of the remnant and for different spin-down mechanisms. No
gravitational-wave signal was detected. Within the range of search
frequencies, we set 95% confidence upper limits of (0.7-1.2) ×
10-24 on the intrinsic gravitational-wave strain, (0.4-4)
× 10-4 on the equatorial ellipticity of the neutron star,
and 0.005-0.14 on the amplitude of r-mode oscillations of the neutron
star. These direct upper limits beat indirect limits derived from
energy conservation and enter the range of theoretical predictions
involving crystalline exotic matter or runaway r-modes. This paper is
also the first gravitational-wave search to present upper limits on
the r-mode amplitude.
Title: TOPICAL REVIEW: Predictions for the rates of compact binary
coalescences observable by ground-based gravitational-wave detectors
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M.;
Accadia, T.; Acernese, F.; Adams, C.; Adhikari, R.; Ajith, P.;
Allen, B.; Allen, G.; Amador Ceron, E.; Amin, R. S.; Anderson, S. B.;
Anderson, W. G.; Antonucci, F.; Aoudia, S.; Arain, M. A.; Araya, M.;
Aronsson, M.; Arun, K. G.; Aso, Y.; Aston, S.; Astone, P.; Atkinson,
D. E.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.;
Ballmer, S.; Barker, D.; Barnum, S.; Barone, F.; Barr, B.; Barriga,
P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri,
R.; Bastarrika, M.; Bauchrowitz, J.; Bauer, Th S.; Behnke, B.; Beker,
M. G.; Belczynski, K.; Benacquista, M.; Bertolini, A.; Betzwieser,
J.; Beveridge, N.; Beyersdorf, P. T.; Bigotta, S.; Bilenko, I. A.;
Billingsley, G.; Birch, J.; Birindelli, S.; Biswas, R.; Bitossi, M.;
Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair,
D.; Bland, B.; Blom, M.; Blomberg, A.; Boccara, C.; Bock, O.; Bodiya,
T. P.; Bondarescu, R.; Bondu, F.; Bonelli, L.; Bork, R.; Born, M.;
Bose, S.; Bosi, L.; Boyle, M.; Braccini, S.; Bradaschia, C.; Brady,
P. R.; Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges, D. O.;
Brillet, A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks, A. F.;
Brown, D. A.; Budzyński, R.; Bulik, T.; Bulten, H. J.; Buonanno,
A.; Burguet-Castell, J.; Burmeister, O.; Buskulic, D.; Byer, R. L.;
Cadonati, L.; Cagnoli, G.; Calloni, E.; Camp, J. B.; Campagna,
E.; Campsie, P.; Cannizzo, J.; Cannon, K. C.; Canuel, B.; Cao, J.;
Capano, C.; Carbognani, F.; Caride, S.; Caudill, S.; Cavaglià, M.;
Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.;
Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chassande Mottin,
E.; Chelkowski, S.; Chen, Y.; Chincarini, A.; Christensen, N.; Chua,
S. S. Y.; Chung, C. T. Y.; Clark, D.; Clark, J.; Clayton, J. H.; Cleva,
F.; Coccia, E.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini, M.;
Conte, R.; Cook, D.; Corbitt, T. R.; Corda, C.; Cornish, N.; Corsi,
A.; Costa, C. A.; Coulon, J. P.; Coward, D.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Cuoco, E.; Dahl, K.; Danilishin, S. L.; Dannenberg, R.;
D'Antonio, S.; Danzmann, K.; Dari, A.; Das, K.; Dattilo, V.; Daudert,
B.; Davier, M.; Davies, G.; Davis, A.; Daw, E. J.; Day, R.; Dayanga,
T.; De Rosa, R.; DeBra, D.; Degallaix, J.; del Prete, M.; Dergachev,
V.; DeRosa, R.; DeSalvo, R.; Devanka, P.; Dhurandhar, S.; Di Fiore,
L.; Di Lieto, A.; Di Palma, I.; Emilio, M. Di Paolo; Di Virgilio,
A.; Díaz, M.; Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes, E. E.;
Dorsher, S.; Douglas, E. S. D.; Drago, M.; Drever, R. W. P.; Driggers,
J. C.; Dueck, J.; Dumas, J. C.; Eberle, T.; Edgar, M.; Edwards, M.;
Effler, A.; Ehrens, P.; Engel, R.; Etzel, T.; Evans, M.; Evans, T.;
Fafone, V.; Fairhurst, S.; Fan, Y.; Farr, B. F.; Fazi, D.; Fehrmann,
H.; Feldbaum, D.; Ferrante, I.; Fidecaro, F.; Finn, L. S.; Fiori,
I.; Flaminio, R.; Flanigan, M.; Flasch, K.; Foley, S.; Forrest, C.;
Forsi, E.; Fotopoulos, N.; Fournier, J. D.; Franc, J.; Frasca, S.;
Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.;
Fricke, T. T.; Friedrich, D.; Fritschel, P.; Frolov, V. V.; Fulda,
P.; Fyffe, M.; Gammaitoni, L.; Garofoli, J. A.; Garufi, F.; Gemme,
G.; Genin, E.; Gennai, A.; Gholami, I.; Ghosh, S.; Giaime, J. A.;
Giampanis, S.; Giardina, K. D.; Giazotto, A.; Gill, C.; Goetz, E.;
Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty,
R.; Graef, C.; Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.;
Grunewald, S.; Guidi, G. M.; Gustafson, E. K.; Gustafson, R.; Hage,
B.; Hall, P.; Hallam, J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna,
C.; Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Haughian, K.; Hayama, K.; Heefner, J.; Heitmann, H.; Hello, P.; Heng,
I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.;
Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough, J.; Howell, E.; Hoyland,
D.; Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh-Dinh, T.;
Ingram, D. R.; Inta, R.; Isogai, T.; Ivanov, A.; Jaranowski, P.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kandhasamy, S.; Kanner, J.; Katsavounidis, E.;
Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.; Kim, C.; Kim, H.;
King, P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.; Kondrashov,
V.; Kopparapu, R.; Koranda, S.; Kowalska, I.; Kozak, D.; Krause, T.;
Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Królak, A.; Kuehn, G.;
Kullman, J.; Kumar, R.; Kwee, P.; Landry, M.; Lang, M.; Lantz, B.;
Lastzka, N.; Lazzarini, A.; Leaci, P.; Leong, J.; Leonor, I.; Leroy,
N.; Letendre, N.; Li, J.; Li, T. G. F.; Lin, H.; Lindquist, P. E.;
Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.;
Losurdo, G.; Lu, P.; Luan, J.; Lubiński, M.; Lucianetti, A.; Lück,
H.; Lundgren, A.; Machenschalk, B.; MacInnis, M.; Mackowski, J. M.;
Mageswaran, M.; Mailand, K.; Majorana, E.; Mak, C.; Man, N.; Mandel,
I.; Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.;
Meadors, G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.;
Miller, J.; Minenkov, Y.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Moe, B.; Mohan, M.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moraru, D.; Moreau, J.; Moreno, G.; Morgado,
N.; Morgia, A.; Morioka, T.; Mors, K.; Mosca, S.; Moscatelli, V.;
Mossavi, K.; Mours, B.; MowLowry, C.; Mueller, G.; Mukherjee, S.;
Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murray, P. G.; Nash, T.;
Nawrodt, R.; Nelson, J.; Neri, I.; Newton, G.; Nishizawa, A.; Nocera,
F.; Nolting, D.; Ochsner, E.; O'Dell, J.; Ogin, G. H.; Oldenburg,
R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.; Ottaway, D. J.;
Ottens, R. S.; Overmier, H.; Owen, B. J.; Page, A.; Pagliaroli, G.;
Palladino, L.; Palomba, C.; Pan, Y.; Pankow, C.; Paoletti, F.; Papa,
M. A.; Pardi, S.; Pareja, M.; Parisi, M.; Pasqualetti, A.; Passaquieti,
R.; Passuello, D.; Patel, P.; Pedraza, M.; Pekowsky, L.; Penn, S.;
Peralta, C.; Perreca, A.; Persichetti, G.; Pichot, M.; Pickenpack,
M.; Piergiovanni, F.; Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin,
M.; Pletsch, H. J.; Plissi, M. V.; Poggiani, R.; Postiglione, F.;
Prato, M.; Predoi, V.; Price, L. R.; Prijatelj, M.; Principe, M.;
Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov, L.; Puncken, O.;
Punturo, M.; Puppo, P.; Quetschke, V.; Raab, F. J.; Rabaste, O.;
Rabeling, D. S.; Radke, T.; Radkins, H.; Raffai, P.; Rakhmanov, M.;
Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Reed, C. M.; Reed,
T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.; Riesen, R.;
Riles, K.; Roberts, P.; Robertson, N. A.; Robinet, F.; Robinson,
C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Röver, C.; Rogstad, S.;
Rolland, L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.;
Rosińska, D.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sakata,
S.; Sakosky, M.; Salemi, F.; Sammut, L.; Sancho de la Jordana, L.;
Sandberg, V.; Sannibale, V.; Santamaría, L.; Santostasi, G.; Saraf,
S.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.;
Saulson, P. R.; Savage, R.; Schilling, R.; Schnabel, R.; Schofield,
R.; Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott,
S. M.; Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.;
Sentenac, D.; Sergeev, A.; Shaddock, D. A.; Shapiro, B.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer,
A.; Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.;
Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.;
Speirits, F. C.; Stein, A. J.; Stein, L. C.; Steinlechner, S.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin,
S.; Stroeer, A.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.;
Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Talukder, D.;
Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.; Thomas,
P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.; Thüring, A.; Titsler,
C.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.; Torres, C.; Torrie,
C. I.; Tournefier, E.; Travasso, F.; Traylor, G.; Trias, M.; Trummer,
J.; Tseng, K.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vaishnav, B.;
Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.; Van Den Broeck,
C.; van der Putten, S.; van der Sluys, M. V.; van Veggel, A. A.; Vass,
S.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.; Veitch, J.;
Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.; Viceré, A.;
Villar, A.; Vinet, J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin, S. P.;
Waldman, S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Was, M.; Wei, P.;
Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels,
P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.;
White, D. J.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams,
L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman,
A. G.; Woan, G.; Wooley, R.; Worden, J.; Yakushin, I.; Yamamoto,
H.; Yamamoto, K.; Yeaton-Massey, D.; Yoshida, S.; Yu, P. P.; Yvert,
M.; Zanolin, M.; Zhang, L.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker,
M. E.; Zweizig, J.; LIGO Scientific Collaboration; Virgo Collaboration
Bibcode: 2010CQGra..27q3001A
Altcode: 2010arXiv1003.2480L
We present an up-to-date, comprehensive summary of the rates for all
types of compact binary coalescence sources detectable by the initial
and advanced versions of the ground-based gravitational-wave detectors
LIGO and Virgo. Astrophysical estimates for compact-binary coalescence
rates depend on a number of assumptions and unknown model parameters and
are still uncertain. The most confident among these estimates are the
rate predictions for coalescing binary neutron stars which are based
on extrapolations from observed binary pulsars in our galaxy. These
yield a likely coalescence rate of 100 Myr-1 per Milky Way
Equivalent Galaxy (MWEG), although the rate could plausibly range
from 1 Myr-1 MWEG-1 to 1000 Myr-1
MWEG-1 (Kalogera et al 2004 Astrophys. J. 601 L179;
Kalogera et al 2004 Astrophys. J. 614 L137 (erratum)). We convert
coalescence rates into detection rates based on data from the LIGO S5
and Virgo VSR2 science runs and projected sensitivities for our advanced
detectors. Using the detector sensitivities derived from these data,
we find a likely detection rate of 0.02 per year for Initial LIGO-Virgo
interferometers, with a plausible range between 2 × 10-4
and 0.2 per year. The likely binary neutron-star detection rate for
the Advanced LIGO-Virgo network increases to 40 events per year,
with a range between 0.4 and 400 per year.
Title: On the Eruption of Coronal Flux Ropes
Authors: Fan, Y.
Bibcode: 2010ApJ...719..728F
Altcode:
We present three-dimensional MHD simulations of the evolution of
the magnetic field in the corona where the emergence of a twisted
magnetic flux tube is driven at the lower boundary into a pre-existing
coronal potential arcade field. Through a sequence of simulations in
which we vary the amount of twisted flux transported into the corona
before the emergence is stopped, we investigate the conditions that
lead to a dynamic eruption of the resulting coronal flux rope. It is
found that the critical condition for the onset of eruption is for
the center of the flux rope to reach a critical height at which the
corresponding potential field declines with height at a sufficiently
steep rate, consistent with the onset of the torus instability of the
flux rope. In some cases, immediately after the emergence is stopped,
the coronal flux rope first settles into a quasi-static rise with an
underlying sigmoid-shaped current layer developing. Preferential heating
of field lines going through this current layer may give rise to the
observed quiescent X-ray sigmoid loops before eruption. Reconnections
in the current layer during the initial quasi-static stage is found
to add detached flux to the coronal flux rope, allowing it to rise
quasi-statically to the critical height and dynamic eruption of the
flux rope then ensues. By identifying field lines whose tops are
in the most intense part of the current layer during the eruption,
we deduce the evolution and morphology of the post-flare X-ray loops
and the flare ribbons at their footpoints.
Title: Synthetic aperture controlled source electromagnetics
Authors: Fan, Y.; Snieder, R.; Slob, E.; Hunziker, J.; Singer, J.;
Sheiman, J.; Rosenquist, M.
Bibcode: 2010GeoRL..3713305F
Altcode:
Controlled-source electromagnetics (CSEM) has been used as a de-risking
tool in the hydrocarbon exploration industry. Although there have been
successful applications of CSEM, this technique is still not widely used
in the industry because the limited types of hydrocarbon reservoirs
CSEM can detect. In this paper, we apply the concept of synthetic
aperture to CSEM data. Synthetic aperture allows us to design sources
with specific radiation patterns for different purposes. The ability to
detect reservoirs is dramatically increased after forming an appropriate
synthetic aperture antenna. Consequently, the types of hydrocarbon
reservoirs that CSEM can detect are significantly extended. Because
synthetic apertures are constructed as a data processing step, there
is no additional cost for the CSEM acquisition. Synthetic aperture has
potential for simplifying and reducing the cost of CSEM acquisition. We
show a data example that illustrates the increased sensitivity obtained
by applying synthetic aperture CSEM source.
Title: Search for Gravitational-wave Inspiral Signals Associated
with Short Gamma-ray Bursts During LIGO's Fifth and Virgo's First
Science Run
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Accadia, T.; Acernese,
F.; Adhikari, R.; Ajith, P.; Allen, B.; Allen, G.; Amador Ceron,
E.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Antonucci,
F.; Aoudia, S.; Arain, M. A.; Araya, M.; Arun, K. G.; Aso, Y.;
Aston, S.; Astone, P.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker,
P.; Ballardin, G.; Ballmer, S.; Barker, D.; Barone, F.; Barr, B.;
Barriga, P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Bauer, Th. S.; Behnke, B.; Beker, M. G.;
Belletoile, A.; Benacquista, M.; Betzwieser, J.; Beyersdorf, P. T.;
Bigotta, S.; Bilenko, I. A.; Billingsley, G.; Birindelli, S.; Biswas,
R.; Bizouard, M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.;
Blair, D.; Bland, B.; Blom, M.; Boccara, C.; Bock, O.; Bodiya, T. P.;
Bondarescu, R.; Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born,
M.; Bose, S.; Bosi, L.; Braccini, S.; Bradaschia, C.; Brady, P. R.;
Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges, D. O.; Brillet, A.;
Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown, D. A.;
Budzyński, R.; Bulik, T.; Bullington, A.; Bulten, H. J.; Buonanno,
A.; Burguet-Castell, J.; Burmeister, O.; Buskulic, D.; Buy, C.;
Byer, R. L.; Cadonati, L.; Cagnoli, G.; Cain, J.; Calloni, E.; Camp,
J. B.; Campagna, E.; Cannizzo, J.; Cannon, K. C.; Canuel, B.; Cao, J.;
Capano, C. D.; Carbognani, F.; Cardenas, L.; Caudill, S.; Cavaglià,
M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.;
Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chassande-Mottin, E.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Chincarini, A.; Christensen,
N.; Chua, S. S. Y.; Chung, C. T. Y.; Clark, D.; Clark, J.; Clayton,
J. H.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas, J.; Colla,
A.; Colombini, M.; Conte, R.; Cook, D.; Corbitt, T. R. C.; Cornish,
N.; Corsi, A.; Coulon, J. -P.; Coward, D.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Cuoco, E.; Dahl, K.; Danilishin, S. L.; D'Antonio, S.;
Danzmann, K.; Dattilo, V.; Daudert, B.; Davier, M.; Davies, G.; Daw,
E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra, D.; Degallaix, J.;
del Prete, M.; Dergachev, V.; DeSalvo, R.; Dhurandhar, S.; Di Fiore,
L.; Di Lieto, A.; Emilio, M. Di Paolo; Di Virgilio, A.; Díaz, M.;
Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes, E. E.; Drago, M.;
Drever, R. W. P.; Driggers, J.; Dueck, J.; Duke, I.; Dumas, J. -C.;
Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.; Etzel, T.; Evans, M.;
Evans, T.; Fafone, V.; Fairhurst, S.; Faltas, Y.; Fan, Y.; Fazi, D.;
Fehrmann, H.; Ferrante, I.; Fidecaro, F.; Finn, L. S.; Fiori, I.;
Flaminio, R.; Flasch, K.; Foley, S.; Forrest, C.; Fotopoulos, N.;
Fournier, J. -D.; Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich,
D.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Galimberti,
M.; Gammaitoni, L.; Garofoli, J. A.; Garufi, F.; Gemme, G.; Genin, E.;
Gennai, A.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.;
Giazotto, A.; Goetz, E.; Goggin, L. M.; González, G.; Goßler, S.;
Gouaty, R.; Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.;
Grunewald, S.; Guidi, G. M.; Gustafson, E. K.; Gustafson, R.; Hage,
B.; Hallam, J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson,
J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian,
K.; Hayama, K.; Hayler, T.; Heefner, J.; Heitmann, H.; Hello, P.;
Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose, E.;
Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough, J.; Howell,
E.; Hoyland, D.; Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.;
Ingram, D. R.; Isogai, T.; Ivanov, A.; Jaranowski, P.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kandhasamy, S.; Kanner, J.; Katsavounidis, E.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khan, R.; Khazanov, E.; Kim, H.; King, P. J.; Kissel, J. S.;
Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda,
S.; Kowalska, I.; Kozak, D.; Kringel, V.; Krishnan, B.; Królak, A.;
Kuehn, G.; Kullman, J.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.;
Lang, M.; Lantz, B.; Lastzka, N.; Lazzarini, A.; Leaci, P.; Lei, M.;
Leindecker, N.; Leonor, I.; Leroy, N.; Letendre, N.; Li, T. G. F.; Lin,
H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie, N. A.; Lodhia,
D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo, G.; Lu, P.;
Lubiński, M.; Lucianetti, A.; Lück, H.; Lundgren, A.; Machenschalk,
B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Majorana, E.; Mak,
C.; Maksimovic, I.; Man, N.; Mandel, I.; Mandic, V.; Mantovani, M.;
Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McKechan, D. J. A.; Mehmet,
M.; Melatos, A.; Melissinos, A. C.; Mendell, G.; Menéndez, D. F.;
Mercer, R. A.; Merill, L.; Meshkov, S.; Messenger, C.; Meyer, M. S.;
Miao, H.; Michel, C.; Milano, L.; Miller, J.; Minenkov, Y.; Mino,
Y.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman,
R.; Miyakawa, O.; Moe, B.; Mohan, M.; Mohanty, S. D.; Mohapatra,
S. R. P.; Moreau, J.; Moreno, G.; Morgado, N.; Morgia, A.; Mors,
K.; Mosca, S.; Moscatelli, V.; Mossavi, K.; Mours, B.; MowLowry,
C.; Mueller, G.; Mukherjee, S.; Mullavey, A.; Müller-Ebhardt, H.;
Munch, J.; Murray, P. G.; Nash, T.; Nawrodt, R.; Nelson, J.; Neri,
I.; Newton, G.; Nishida, E.; Nishizawa, A.; Nocera, F.; Ochsner, E.;
O'Dell, J.; Ogin, G. H.; Oldenburg, R.; O'Reilly, B.; O'Shaughnessy,
R.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page,
A.; Pagliaroli, G.; Palomba, C.; Pan, Y.; Pankow, C.; Paoletti, F.;
Papa, M. A.; Pardi, S.; Parisi, M.; Pasqualetti, A.; Passaquieti, R.;
Passuello, D.; Patel, P.; Pathak, D.; Pedraza, M.; Pekowsky, L.; Penn,
S.; Peralta, C.; Perreca, A.; Persichetti, G.; Pichot, M.; Pickenpack,
M.; Piergiovanni, F.; Pietka, M.; Pinard, L.; Pinto, I. M.; Pitkin,
M.; Pletsch, H. J.; Plissi, M. V.; Poggiani, R.; Postiglione, F.;
Prato, M.; Predoi, V.; Principe, M.; Prix, R.; Prodi, G. A.; Prokhorov,
L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Raab, F. J.;
Rabeling, D. S.; Radkins, H.; Raffai, P.; Raics, Z.; Rakhmanov, M.;
Rapagnani, P.; Raymond, V.; Re, V.; Reed, C. M.; Reed, T.; Regimbau,
T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Ricci, F.; Riesen, R.;
Riles, K.; Roberts, P.; Robertson, N. A.; Robinet, F.; Robinson,
C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Röver, C.; Rolland, L.;
Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.; Rosińska, D.;
Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sakata, S.; Salemi, F.;
Sammut, L.; Sancho de la Jordana, L.; Sandberg, V.; Sannibale, V.;
Santamaría, L.; Santostasi, G.; Saraf, S.; Sarin, P.; Sassolas, B.;
Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.; Saulson, P. R.;
Savage, R.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz, B.;
Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.;
Seifert, F.; Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sergeev, A.;
Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.;
Sigg, D.; Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.;
Stein, A. J.; Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.;
Strain, K. A.; Strigin, S.; Stroeer, A.; Sturani, R.; Stuver, A. L.;
Summerscales, T. Z.; Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels,
B.; Szokoly, G. P.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.;
Taylor, J. R.; Taylor, R.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Titsler, C.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.; Torres,
C.; Torrie, C. I.; Tournefier, E.; Travasso, F.; Traylor, G.; Trias,
M.; Trummer, J.; Turner, L.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.;
Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.; Van Den Broeck,
C.; van der Putten, S.; van der Sluys, M. V.; Vass, S.; Vaulin, R.;
Vavoulidis, M.; Vecchio, A.; Vedovato, G.; van Veggel, A. A.; Veitch,
J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.; Viceré,
A.; Villar, A.; Vinet, J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin,
S. P.; Waldman, S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Was,
M.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen,
S.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.;
Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.;
Williams, H. R.; Williams, L.; Willke, B.; Wilmut, I.; Winkelmann,
L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.;
Worden, J.; Yakushin, I.; Yamamoto, H.; Yamamoto, K.; Yeaton-Massey,
D.; Yoshida, S.; Yu, P. P.; Yvert, M.; Zanolin, M.; Zhang, L.; Zhang,
Z.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.; LIGO Scientific
Collaboration; Virgo Collaboration
Bibcode: 2010ApJ...715.1453A
Altcode: 2010arXiv1001.0165T; 2010arXiv1001.0165L
Progenitor scenarios for short gamma-ray bursts (short GRBs)
include coalescenses of two neutron stars or a neutron star and
black hole, which would necessarily be accompanied by the emission
of strong gravitational waves. We present a search for these known
gravitational-wave signatures in temporal and directional coincidence
with 22 GRBs that had sufficient gravitational-wave data available
in multiple instruments during LIGO's fifth science run, S5, and
Virgo's first science run, VSR1. We find no statistically significant
gravitational-wave candidates within a [ - 5, + 1) s window around
the trigger time of any GRB. Using the Wilcoxon-Mann-Whitney U-test,
we find no evidence for an excess of weak gravitational-wave signals
in our sample of GRBs. We exclude neutron star-black hole progenitors
to a median 90% confidence exclusion distance of 6.7 Mpc.
Title: Search For Gravitational-wave Bursts Associated with Gamma-ray
Bursts using Data from LIGO Science Run 5 and Virgo Science Run 1
Authors: Abbott, B. P.; Abbott, R.; Acernese, F.; Adhikari, R.; Ajith,
P.; Allen, B.; Allen, G.; Alshourbagy, M.; Amin, R. S.; Anderson,
S. B.; Anderson, W. G.; Antonucci, F.; Aoudia, S.; Arain, M. A.; Araya,
M.; Armandula, H.; Armor, P.; Arun, K. G.; Aso, Y.; Aston, S.; Astone,
P.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.;
Ballmer, S.; Barker, C.; Barker, D.; Barone, F.; Barr, B.; Barriga,
P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri,
R.; Bastarrika, M.; Bauer, Th. S.; Behnke, B.; Beker, M.; Benacquista,
M.; Betzwieser, J.; Beyersdorf, P. T.; Bigotta, S.; Bilenko, I. A.;
Billingsley, G.; Birindelli, S.; Biswas, R.; Bizouard, M. A.; Black,
E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.; Boccara,
C.; Bodiya, T. P.; Bogue, L.; Bondu, F.; Bonelli, L.; Bork, R.;
Boschi, V.; Bose, S.; Bosi, L.; Braccini, S.; Bradaschia, C.; Brady,
P. R.; Braginsky, V. B.; Brau, J. E.; Bridges, D. O.; Brillet, A.;
Brinkmann, M.; Brisson, V.; Brooks, A. F.; Brown, D. A.; Brummit, A.;
Brunet, G.; Budzyński, R.; Bulik, T.; Bullington, A.; Bulten, H. J.;
Buonanno, A.; Burmeister, O.; Buskulic, D.; Byer, R. L.; Cadonati,
L.; Cagnoli, G.; Calloni, E.; Camp, J. B.; Campagna, E.; Cannizzo,
J.; Cannon, K. C.; Canuel, B.; Cao, J.; Carbognani, F.; Cardenas, L.;
Caride, S.; Castaldi, G.; Caudill, S.; Cavaglià, M.; Cavalier, F.;
Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.; Chalermsongsak,
T.; Chalkley, E.; Charlton, P.; Chassande-Mottin, E.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Chincarini, A.; Christensen, N.; Chung,
C. T. Y.; Clark, D.; Clark, J.; Clayton, J. H.; Cleva, F.; Coccia,
E.; Cokelaer, T.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini,
M.; Conte, R.; Cook, D.; Corbitt, T. R. C.; Corda, C.; Cornish,
N.; Corsi, A.; Coulon, J. -P.; Coward, D.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Cuoco, E.; Danilishin, S. L.; D'Antonio, S.; Danzmann,
K.; Dari, A.; Dattilo, V.; Daudert, B.; Davier, M.; Davies, G.; Daw,
E. J.; Day, R.; De Rosa, R.; DeBra, D.; Degallaix, J.; del Prete, M.;
Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandhar, S.; Di Fiore, L.;
Di Lieto, A.; Emilio, M. Di Paolo; Di Virgilio, A.; Díaz, M.; Dietz,
A.; Donovan, F.; Dooley, K. L.; Doomes, E. E.; Drago, M.; Drever,
R. W. P.; Dueck, J.; Duke, I.; Dumas, J. -C.; Dwyer, J. G.; Echols,
C.; Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.; Espinoza, E.;
Etzel, T.; Evans, M.; Evans, T.; Fafone, V.; Fairhurst, S.; Faltas,
Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Ferrante, I.; Fidecaro, F.; Finn,
L. S.; Fiori, I.; Flaminio, R.; Flasch, K.; Foley, S.; Forrest, C.;
Fotopoulos, N.; Fournier, J. -D.; Franc, J.; Franzen, A.; Frasca,
S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey,
R.; Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi,
V.; Gammaitoni, L.; Garofoli, J. A.; Garufi, F.; Gemme, G.; Genin,
E.; Gennai, A.; Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina,
K. D.; Giazotto, A.; Goda, K.; Goetz, E.; Goggin, L. M.; González, G.;
Gorodetsky, M. L.; Goeßzetler, S.; Goßler, S.; Gouaty, R.; Granata,
M.; Granata, V.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Greverie, C.; Grimaldi, F.; Grosso, R.;
Grote, H.; Grunewald, S.; Guenther, M.; Guidi, G.; Gustafson, E. K.;
Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer, D.; Hammond, G. D.;
Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad,
E. D.; Haughian, K.; Hayama, K.; Heefner, J.; Heitmann, H.; Hello,
P.; Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose, E.;
Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough, J.; Hoyland,
D.; Huet, D.; Hughey, B.; Huttner, S. H.; Ingram, D. R.; Isogai, T.;
Ito, M.; Ivanov, A.; Jaranowski, P.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kandhasamy, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski,
A.; Khalili, F. Y.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.;
Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda,
S.; Kowalska, I.; Kozak, D.; Krishnan, B.; Królak, A.; Kumar, R.;
Kwee, P.; La Penna, P.; Lam, P. K.; Landry, M.; Lantz, B.; Lazzarini,
A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor, I.; Leroy, N.; Letendre,
N.; Li, C.; Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie,
N. A.; Lodhia, D.; Longo, M.; Lorenzini, M.; Loriette, V.; Lormand,
M.; Losurdo, G.; Lu, P.; Lubiński, M.; Lucianetti, A.; Lück, H.;
Machenschalk, B.; MacInnis, M.; Mackowski, J. -M.; Mageswaran, M.;
Mailand, K.; Majorana, E.; Man, N.; Mandel, I.; Mandic, V.; Mantovani,
M.; Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McHugh, M.; McIntyre, G.; McKechan, D. J. A.;
McKenzie, K.; Mehmet, M.; Melatos, A.; Melissinos, A. C.; Mendell,
G.; Menéndez, D. F.; Menzinger, F.; Mercer, R. A.; Meshkov, S.;
Messenger, C.; Meyer, M. S.; Michel, C.; Milano, L.; Miller, J.;
Minelli, J.; Minenkov, Y.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohan, M.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moreau, J.; Moreno, G.; Morgado, N.; Morgia,
A.; Morioka, T.; Mors, K.; Mosca, S.; Moscatelli, V.; Mossavi, K.;
Mours, B.; MowLowry, C.; Mueller, G.; Muhammad, D.; Mukherjee, S.;
Mukhopadhyay, H.; Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murray,
P. G.; Myers, E.; Myers, J.; Nash, T.; Nelson, J.; Neri, I.; Newton,
G.; Nishizawa, A.; Nocera, F.; Numata, K.; Ochsner, E.; O'Dell, J.;
Ogin, G. H.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Pagliaroli, G.; Palomba, C.; Pan,
Y.; Pankow, C.; Paoletti, F.; Papa, M. A.; Parameshwaraiah, V.;
Pardi, S.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel,
P.; Pedraza, M.; Penn, S.; Perreca, A.; Persichetti, G.; Pichot, M.;
Piergiovanni, F.; Pierro, V.; Pietka, M.; Pinard, L.; Pinto, I. M.;
Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Poggiani, R.; Postiglione,
F.; Prato, M.; Principe, M.; Prix, R.; Prodi, G. A.; Prokhorov, L.;
Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Raab, F. J.;
Rabaste, O.; Rabeling, D. S.; Radkins, H.; Raffai, P.; Raics, Z.;
Rainer, N.; Rakhmanov, M.; Rapagnani, P.; Raymond, V.; Re, V.; Reed,
C. M.; Reed, T.; Regimbau, T.; Rehbein, H.; Reid, S.; Reitze, D. H.;
Ricci, F.; Riesen, R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson,
N. A.; Robinet, F.; Robinson, C.; Robinson, E. L.; Rocchi, A.; Roddy,
S.; Rolland, L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie,
J. H.; Rosińska, D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.;
Russell, P.; Ryan, K.; Sakata, S.; Salemi, F.; Sancho de la Jordana,
L.; Sandberg, V.; Sannibale, V.; Santamaría, L.; Saraf, S.; Sarin,
P.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.;
Saulson, P. R.; Savage, R.; Savov, P.; Scanlan, M.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schulz, B.; Schutz, B. F.; Schwinberg,
P.; Scott, J.; Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.;
Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sergeev, A.; Shapiro, B.;
Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.;
Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein, A.;
Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.;
Strigin, S.; Stroeer, A.; Sturani, R.; Stuver, A. L.; Summerscales,
T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.; Swinkels, B.; Szokoly,
G. P.; Talukder, D.; Tang, L.; Tanner, D. B.; Tarabrin, S. P.;
Taylor, J. R.; Taylor, R.; Terenzi, R.; Thacker, J.; Thorne, K. A.;
Thorne, K. S.; Thüring, A.; Tokmakov, K. V.; Toncelli, A.; Tonelli,
M.; Torres, C.; Torrie, C.; Tournefier, E.; Travasso, F.; Traylor,
G.; Trias, M.; Trummer, J.; Ugolini, D.; Ulmen, J.; Urbanek, K.;
Vahlbruch, H.; Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.;
Van Den Broeck, C.; van der Putten, S.; van der Sluys, M. V.; van
Veggel, A. A.; Vass, S.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.;
Vedovato, G.; Veitch, J.; Veitch, P.; Veltkamp, C.; Verkindt, D.;
Vetrano, F.; Viceré, A.; Villar, A.; Vinet, J. -Y.; Vocca, H.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward,
R. L.; Was, M.; Weidner, A.; Weinert, M.; Weinstein, A. J.; Weiss, R.;
Wen, L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Wilmut, I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.;
Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin,
I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Yvert, M.; Zanolin, M.; Zhang,
J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M. E.; zur Mühlen, H.;
Zweizig, J.; LIGO Scientific Collaboration; Virgo Collaboration
Bibcode: 2010ApJ...715.1438A
Altcode: 2009arXiv0908.3824L
We present the results of a search for gravitational-wave bursts
(GWBs) associated with 137 gamma-ray bursts (GRBs) that were
detected by satellite-based gamma-ray experiments during the fifth
LIGO science run and first Virgo science run. The data used in this
analysis were collected from 2005 November 4 to 2007 October 1, and
most of the GRB triggers were from the Swift satellite. The search
uses a coherent network analysis method that takes into account the
different locations and orientations of the interferometers at the
three LIGO-Virgo sites. We find no evidence for GWB signals associated
with this sample of GRBs. Using simulated short-duration (<1 s)
waveforms, we set upper limits on the amplitude of gravitational
waves associated with each GRB. We also place lower bounds on the
distance to each GRB under the assumption of a fixed energy emission in
gravitational waves, with a median limit of D ~ 12 Mpc(E iso
GW/0.01 M sun c 2)1/2 for
emission at frequencies around 150 Hz, where the LIGO-Virgo detector
network has best sensitivity. We present astrophysical interpretations
and implications of these results, and prospects for corresponding
searches during future LIGO-Virgo runs.
Title: Developing Physics-Based Procedures for Local Helioseismic
Probing of Sunspots and Magnetic Regions
Authors: Birch, Aaron; Braun, D. C.; Crouch, A.; Rempel, M.; Fan,
Y.; Centeno, R.; Toomre, J.; Haber, D.; Hindman, B.; Featherstone,
N.; Duvall, T., Jr.; Jackiewicz, J.; Thompson, M.; Stein, R.; Gizon,
L.; Cameron, R.; Saidi, Y.; Hanasoge, S.; Burston, R.; Schunker, H.;
Moradi, H.
Bibcode: 2010AAS...21630805B
Altcode:
We have initiated a project to test and improve the local helioseismic
techniques of time-distance and ring-diagram analysis. Our goals are
to develop and implement physics-based methods that will (1) enable the
reliable determinations of subsurface flow, magnetic field, and thermal
structure in regions of strong magnetic fields and (2) be quantitatively
tested with realistic solar magnetoconvection simulations in the
presence of sunspot-like magnetic fields. We are proceeding through a
combination of improvements in local helioseismic measurements, forward
modeling of the helioseismic wavefield, kernel computations, inversions,
and validation through numerical simulations. As improvements over
existing techniques are made they will be applied to the SDO/HMI
observations. This work is funded through the the NASA Heliophysics
Science Division through the Solar Dynamics Observatory (SDO) Science
Center program.
Title: All-sky search for gravitational-wave bursts in the first
joint LIGO-GEO-Virgo run
Authors: Abadie, J.; Abbott, B. P.; Abbott, R.; Accadia, T.; Acernese,
F.; Adhikari, R.; Ajith, P.; Allen, B.; Allen, G.; Amador Ceron,
E.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Antonucci, F.;
Arain, M. A.; Araya, M.; Arun, K. G.; Aso, Y.; Aston, S.; Astone,
P.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin,
G.; Ballmer, S.; Barker, D.; Barone, F.; Barr, B.; Barriga, P.;
Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri, R.;
Bastarrika, M.; Bauer, Th. S.; Behnke, B.; Beker, M. G.; Belletoile,
A.; Benacquista, M.; Betzwieser, J.; Beyersdorf, P. T.; Bigotta, S.;
Bilenko, I. A.; Billingsley, G.; Birindelli, S.; Biswas, R.; Bizouard,
M. A.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland,
B.; Blom, M.; Boccara, C.; Bock, O.; Bodiya, T. P.; Bondarescu, R.;
Bondu, F.; Bonelli, L.; Bonnand, R.; Bork, R.; Born, M.; Bose, S.;
Bosi, L.; Bouhou, B.; Braccini, S.; Bradaschia, C.; Brady, P. R.;
Braginsky, V. B.; Brau, J. E.; Breyer, J.; Bridges, D. O.; Brillet,
A.; Brinkmann, M.; Brisson, V.; Britzger, M.; Brooks, A. F.; Brown,
D. A.; Budzyński, R.; Bulik, T.; Bullington, A.; Bulten, H. J.;
Buonanno, A.; Burmeister, O.; Buskulic, D.; Buy, C.; Byer, R. L.;
Cadonati, L.; Cagnoli, G.; Cain, J.; Calloni, E.; Camp, J. B.;
Campagna, E.; Cannizzo, J.; Cannon, K. C.; Canuel, B.; Cao, J.;
Capano, C. D.; Carbognani, F.; Cardenas, L.; Caudill, S.; Cavaglià,
M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.;
Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chassande-Mottin, E.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Chincarini, A.; Christensen,
N.; Chua, S. S. Y.; Chung, C. T. Y.; Clark, D.; Clark, J.; Clayton,
J. H.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas, J.; Colla,
A.; Colombini, M.; Conte, R.; Cook, D.; Corbitt, T. R. C.; Cornish,
N.; Corsi, A.; Coulon, J. -P.; Coward, D.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Cuoco, E.; Dahl, K.; Danilishin, S. L.; D'Antonio, S.;
Danzmann, K.; Dattilo, V.; Daudert, B.; Davier, M.; Davies, G.; Daw,
E. J.; Day, R.; Dayanga, T.; de Rosa, R.; Debra, D.; Degallaix, J.;
Del Prete, M.; Dergachev, V.; Desalvo, R.; Dhurandhar, S.; di Fiore,
L.; di Lieto, A.; di Paolo Emilio, M.; di Virgilio, A.; Díaz, M.;
Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes, E. E.; Drago, M.;
Drever, R. W. P.; Driggers, J.; Dueck, J.; Duke, I.; Dumas, J. -C.;
Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.; Etzel, T.; Evans, M.;
Evans, T.; Fafone, V.; Fairhurst, S.; Faltas, Y.; Fan, Y.; Fazi, D.;
Fehrmann, H.; Ferrante, I.; Fidecaro, F.; Finn, L. S.; Fiori, I.;
Flaminio, R.; Flasch, K.; Foley, S.; Forrest, C.; Fotopoulos, N.;
Fournier, J. -D.; Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich,
D.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Galimberti,
M.; Gammaitoni, L.; Garofoli, J. A.; Garufi, F.; Gemme, G.; Genin, E.;
Gennai, A.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.;
Giazotto, A.; Goetz, E.; Goggin, L. M.; González, G.; Goßler, S.;
Gouaty, R.; Granata, M.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Greverie, C.; Grosso, R.; Grote, H.;
Grunewald, S.; Guidi, G. M.; Gustafson, E. K.; Gustafson, R.; Hage,
B.; Hallam, J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson,
J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian,
K.; Hayama, K.; Hayau, J. -F.; Hayler, T.; Heefner, J.; Heitmann,
H.; Hello, P.; Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild,
S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.;
Hough, J.; Howell, E.; Hoyland, D.; Huet, D.; Hughey, B.; Husa, S.;
Huttner, S. H.; Ingram, D. R.; Isogai, T.; Ivanov, A.; Jaranowski, P.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.;
Kalogera, V.; Kandhasamy, S.; Kanner, J.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski,
A.; Khalili, F. Y.; Khan, R.; Khazanov, E.; Kim, H.; King, P. J.;
Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu,
R.; Koranda, S.; Kowalska, I.; Kozak, D.; Kringel, V.; Krishnan, B.;
Królak, A.; Kuehn, G.; Kullman, J.; Kumar, R.; Kwee, P.; Lam, P. K.;
Landry, M.; Lang, M.; Lantz, B.; Lastzka, N.; Lazzarini, A.; Leaci,
P.; Lei, M.; Leindecker, N.; Leonor, I.; Leroy, N.; Letendre, N.; Li,
T. G. F.; Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie,
N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.; Losurdo,
G.; Lu, P.; Lubiński, M.; Lucianetti, A.; Lück, H.; Lundgren,
A.; Machenschalk, B.; Macinnis, M.; Mageswaran, M.; Mailand, K.;
Majorana, E.; Mak, C.; Maksimovic, I.; Man, N.; Mandel, I.; Mandic,
V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka, S.; Márka, Z.;
Markosyan, A.; Markowitz, J.; Maros, E.; Marque, J.; Martelli, F.;
Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.;
Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.;
McClelland, D. E.; McGuire, S. C.; McIntyre, G.; McKechan, D. J. A.;
Mehmet, M.; Melatos, A.; Melissinos, A. C.; Mendell, G.; Menéndez,
D. F.; Mercer, R. A.; Merill, L.; Meshkov, S.; Messenger, C.; Meyer,
M. S.; Miao, H.; Michel, C.; Milano, L.; Miller, J.; Minenkov, Y.;
Mino, Y.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman,
R.; Miyakawa, O.; Moe, B.; Mohan, M.; Mohanty, S. D.; Mohapatra,
S. R. P.; Moreau, J.; Moreno, G.; Morgado, N.; Morgia, A.; Mors,
K.; Mosca, S.; Moscatelli, V.; Mossavi, K.; Mours, B.; Mowlowry,
C.; Mueller, G.; Mukherjee, S.; Mullavey, A.; Müller-Ebhardt, H.;
Munch, J.; Murray, P. G.; Nash, T.; Nawrodt, R.; Nelson, J.; Neri,
I.; Newton, G.; Nishida, E.; Nishizawa, A.; Nocera, F.; Ochsner, E.;
O'Dell, J.; Ogin, G. H.; Oldenburg, R.; O'Reilly, B.; O'Shaughnessy,
R.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page,
A.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow, C.;
Paoletti, F.; Papa, M. A.; Pardi, S.; Parisi, M.; Pasqualetti, A.;
Passaquieti, R.; Passuello, D.; Patel, P.; Pathak, D.; Pedraza, M.;
Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.; Persichetti, G.;
Pichot, M.; Pickenpack, M.; Piergiovanni, F.; Pietka, M.; Pinard, L.;
Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Poggiani,
R.; Postiglione, F.; Prato, M.; Principe, M.; Prix, R.; Prodi, G. A.;
Prokhorov, L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.;
Raab, F. J.; Rabeling, D. S.; Rabeling, D. S.; Radkins, H.; Raffai, P.;
Raics, Z.; Rakhmanov, M.; Rapagnani, P.; Raymond, V.; Re, V.; Reed,
C. M.; Reed, T.; Regimbau, T.; Rehbein, H.; Reid, S.; Reitze, D. H.;
Ricci, F.; Riesen, R.; Riles, K.; Roberts, P.; Robertson, N. A.;
Robinet, F.; Robinson, C.; Robinson, E. L.; Rocchi, A.; Roddy, S.;
Röver, C.; Rolland, L.; Rollins, J.; Romano, J. D.; Romano, R.;
Romie, J. H.; Rosińska, D.; Rowan, S.; Rüdiger, A.; Ruggi, P.;
Ryan, K.; Sakata, S.; Salemi, F.; Sammut, L.; Sancho de La Jordana,
L.; Sandberg, V.; Sannibale, V.; Santamaría, L.; Santostasi, G.;
Saraf, S.; Sarin, P.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.;
Satterthwaite, M.; Saulson, P. R.; Savage, R.; Schilling, R.; Schnabel,
R.; Schofield, R.; Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott,
J.; Scott, S. M.; Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Sentenac, D.; Sergeev, A.; Shapiro, B.; Shawhan, P.; Shoemaker,
D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sintes, A. M.; Skelton,
G.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.;
Smith, N. D.; Somiya, K.; Sorazu, B.; Sperandio, L.; Stein, A. J.;
Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.;
Strigin, S.; Stroeer, A.; Sturani, R.; Stuver, A. L.; Summerscales,
T. Z.; Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Szokoly,
G. P.; Talukder, D.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.;
Taylor, R.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Titsler,
C.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.; Torres, C.; Torrie,
C. I.; Tournefier, E.; Travasso, F.; Traylor, G.; Trias, M.; Trummer,
J.; Turner, L.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vajente, G.;
Vallisneri, M.; van den Brand, J. F. J.; van den Broeck, C.; van der
Putten, S.; van der Sluys, M. V.; Vass, S.; Vaulin, R.; Vavoulidis,
M.; Vecchio, A.; Vedovato, G.; van Veggel, A. A.; Veitch, J.; Veitch,
P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.; Viceré, A.; Villar,
A.; Vinet, J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin, S. P.; Waldman,
S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Was, M.; Wei, P.; Weinert,
M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wessels, P.; West,
M.; Westphal, T.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Wilmut, I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.;
Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Yakushin, I.;
Yamamoto, H.; Yamamoto, K.; Yeaton-Massey, D.; Yoshida, S.; Yvert,
M.; Zanolin, M.; Zhang, L.; Zhang, Z.; Zhao, C.; Zotov, N.; Zucker,
M. E.; Zweizig, J.; LIGO Scientific Collaboration; Virgo Collaboration
Bibcode: 2010PhRvD..81j2001A
Altcode: 2010arXiv1002.1036T
We present results from an all-sky search for unmodeled
gravitational-wave bursts in the data collected by the LIGO, GEO
600 and Virgo detectors between November 2006 and October 2007. The
search is performed by three different analysis algorithms over
the frequency band 50-6000 Hz. Data are analyzed for times with at
least two of the four LIGO-Virgo detectors in coincident operation,
with a total live time of 266 days. No events produced by the search
algorithms survive the selection cuts. We set a frequentist upper limit
on the rate of gravitational-wave bursts impinging on our network of
detectors. When combined with the previous LIGO search of the data
collected between November 2005 and November 2006, the upper limit on
the rate of detectable gravitational-wave bursts in the 64-2048 Hz band
is 2.0 events per year at 90% confidence. We also present event rate
versus strength exclusion plots for several types of plausible burst
waveforms. The sensitivity of the combined search is expressed in terms
of the root-sum-squared strain amplitude for a variety of simulated
waveforms and lies in the range 6×10-22Hz-1/2
to 2×10-20Hz-1/2. This is the first untriggered
burst search to use data from the LIGO and Virgo detectors together,
and the most sensitive untriggered burst search performed so far.
Title: Searches for Gravitational Waves from Known Pulsars with
Science Run 5 LIGO Data
Authors: Abbott, B. P.; Abbott, R.; Acernese, F.; Adhikari, R.; Ajith,
P.; Allen, B.; Allen, G.; Alshourbagy, M.; Amin, R. S.; Anderson,
S. B.; Anderson, W. G.; Antonucci, F.; Aoudia, S.; Arain, M. A.; Araya,
M.; Armandula, H.; Armor, P.; Arun, K. G.; Aso, Y.; Aston, S.; Astone,
P.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.;
Ballmer, S.; Barker, C.; Barker, D.; Barone, F.; Barr, B.; Barriga,
P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri,
R.; Bastarrika, M.; Bauer, Th. S.; Behnke, B.; Beker, M.; Benacquista,
M.; Betzwieser, J.; Beyersdorf, P. T.; Bigotta, S.; Bilenko, I. A.;
Billingsley, G.; Birindelli, S.; Biswas, R.; Bizouard, M. A.; Black,
E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.; Boccara,
C.; Bodiya, T. P.; Bogue, L.; Bondu, F.; Bonelli, L.; Bork, R.;
Boschi, V.; Bose, S.; Bosi, L.; Braccini, S.; Bradaschia, C.; Brady,
P. R.; Braginsky, V. B.; Brau, J. E.; Bridges, D. O.; Brillet, A.;
Brinkmann, M.; Brisson, V.; Van Den Broeck, C.; Brooks, A. F.; Brown,
D. A.; Brummit, A.; Brunet, G.; Budzyński, R.; Bulik, T.; Bullington,
A.; Bulten, H. J.; Buonanno, A.; Burmeister, O.; Buskulic, D.; Byer,
R. L.; Cadonati, L.; Cagnoli, G.; Calloni, E.; Camp, J. B.; Campagna,
E.; Cannizzo, J.; Cannon, K. C.; Canuel, B.; Cao, J.; Carbognani,
F.; Cardenas, L.; Caride, S.; Castaldi, G.; Caudill, S.; Cavaglià,
M.; Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.;
Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chassande-Mottin, E.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Chincarini, A.; Christensen,
N.; Chung, C. T. Y.; Clark, D.; Clark, J.; Clayton, J. H.; Cleva,
F.; Coccia, E.; Cokelaer, T.; Colacino, C. N.; Colas, J.; Colla, A.;
Colombini, M.; Conte, R.; Cook, D.; Corbitt, T. R. C.; Corda, C.;
Cornish, N.; Corsi, A.; Coulon, J. -P.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Cuoco, E.; Danilishin, S. L.; D'Antonio,
S.; Danzmann, K.; Dari, A.; Dattilo, V.; Daudert, B.; Davier, M.;
Davies, G.; Daw, E. J.; Day, R.; De Rosa, R.; DeBra, D.; Degallaix,
J.; del Prete, M.; Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandhar,
S.; Di Fiore, L.; Di Lieto, A.; Emilio, M. Di Paolo; Di Virgilio,
A.; Díaz, M.; Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes, E. E.;
Drago, M.; Drever, R. W. P.; Dueck, J.; Duke, I.; Dumas, J. -C.; Dwyer,
J. G.; Echols, C.; Edgar, M.; Effler, A.; Ehrens, P.; Espinoza, E.;
Etzel, T.; Evans, M.; Evans, T.; Fafone, V.; Fairhurst, S.; Faltas,
Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Ferrante, I.; Fidecaro, F.; Finn,
L. S.; Fiori, I.; Flaminio, R.; Flasch, K.; Foley, S.; Forrest, C.;
Fotopoulos, N.; Fournier, J. -D.; Franc, J.; Franzen, A.; Frasca,
S.; Frasconi, F.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey,
R.; Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.;
Gammaitoni, L.; Garofoli, J. A.; Garufi, F.; Gemme, G.; Genin, E.;
Gennai, A.; Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina,
K. D.; Giazotto, A.; Goda, K.; Goetz, E.; Goggin, L. M.; González,
G.; Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Granata, M.; Granata,
V.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Greverie, C.; Grimaldi, F.; Grosso, R.; Grote, H.;
Grunewald, S.; Guenther, M.; Guidi, G.; Gustafson, E. K.; Gustafson,
R.; Hage, B.; Hallam, J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.;
Haughian, K.; Hayama, K.; Heefner, J.; Heitmann, H.; Hello, P.; Heng,
I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.;
Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough, J.; Hoyland, D.; Huet,
D.; Hughey, B.; Huttner, S. H.; Ingram, D. R.; Isogai, T.; Ito, M.;
Ivanov, A.; Jaranowski, P.; Johnson, B.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Sancho de la Jordana, L.; Ju, L.; Kalmus, P.;
Kalogera, V.; Kandhasamy, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis,
E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalaidovski, A.; Khalili, F. Y.; Khan, R.; Khazanov, E.; King, P.;
Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu,
R.; Koranda, S.; Kowalska, I.; Kozak, D.; Krishnan, B.; Królak, A.;
Kumar, R.; Kwee, P.; La Penna, P.; Lam, P. K.; Landry, M.; Lantz, B.;
Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor, I.; Leroy, N.;
Letendre, N.; Li, C.; Lin, H.; Lindquist, P. E.; Littenberg, T. B.;
Lockerbie, N. A.; Lodhia, D.; Longo, M.; Lorenzini, M.; Loriette,
V.; Lormand, M.; Losurdo, G.; Lu, P.; Lubiński, M.; Lucianetti,
A.; Lück, H.; Machenschalk, B.; MacInnis, M.; Mackowski, J. -M.;
Mageswaran, M.; Mailand, K.; Majorana, E.; Man, N.; Mandel, I.;
Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka, S.;
Márka, Z.; Markosyan, A.; Markowitz, J.; Maros, E.; Marque, J.;
Martelli, F.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.;
Masserot, A.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala,
N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.;
McIntyre, G.; McKechan, D. J. A.; McKenzie, K.; Mehmet, M.; Melatos,
A.; Melissinos, A. C.; Mendell, G.; Menéndez, D. F.; Menzinger, F.;
Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Michel,
C.; Milano, L.; Miller, J.; Minelli, J.; Minenkov, Y.; Mino, Y.;
Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa, O.;
Moe, B.; Mohan, M.; Mohanty, S. D.; Mohapatra, S. R. P.; Moreau, J.;
Moreno, G.; Morgado, N.; Morgia, A.; Morioka, T.; Mors, K.; Mosca,
S.; Moscatelli, V.; Mossavi, K.; Mours, B.; MowLowry, C.; Mueller,
G.; Muhammad, D.; zur Mühlen, H.; Mukherjee, S.; Mukhopadhyay, H.;
Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murray, P. G.; Myers,
E.; Myers, J.; Nash, T.; Nelson, J.; Neri, I.; Newton, G.; Nishizawa,
A.; Nocera, F.; Numata, K.; Ochsner, E.; O'Dell, J.; Ogin, G. H.;
O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens, R. S.;
Overmier, H.; Owen, B. J.; Pagliaroli, G.; Palomba, C.; Pan, Y.;
Pankow, C.; Paoletti, F.; Papa, M. A.; Parameshwaraiah, V.; Pardi,
S.; Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.;
Pedraza, M.; Penn, S.; Perreca, A.; Persichetti, G.; Pichot, M.;
Piergiovanni, F.; Pierro, V.; Pietka, M.; Pinard, L.; Pinto, I. M.;
Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Poggiani, R.; Postiglione,
F.; Prato, M.; Principe, M.; Prix, R.; Prodi, G. A.; Prokhorov, L.;
Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Raab, F. J.;
Rabaste, O.; Rabeling, D. S.; Radkins, H.; Raffai, P.; Raics, Z.;
Rainer, N.; Rakhmanov, M.; Rapagnani, P.; Raymond, V.; Re, V.; Reed,
C. M.; Reed, T.; Regimbau, T.; Rehbein, H.; Reid, S.; Reitze, D. H.;
Ricci, F.; Riesen, R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson,
N. A.; Robinet, F.; Robinson, C.; Robinson, E. L.; Rocchi, A.; Roddy,
S.; Rolland, L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.;
Rosińska, D.; Röver, C.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Russell,
P.; Ryan, K.; Sakata, S.; Salemi, F.; Sandberg, V.; Sannibale, V.;
Santamaría, L.; Saraf, S.; Sarin, P.; Sassolas, B.; Sathyaprakash,
B. S.; Sato, S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.; Savov,
P.; Scanlan, M.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz,
B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle,
A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sentenac,
D.; Sergeev, A.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley,
A.; Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen,
B. J. J.; Slutsky, J.; van der Sluys, M. V.; Smith, J. R.; Smith,
M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein, A.; Stein, L. C.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin,
S.; Stroeer, A.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.;
Sun, K. -X.; Sung, M.; Sutton, P. J.; Swinkels, B.; Szokoly, G. P.;
Talukder, D.; Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.;
Taylor, R.; Terenzi, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.;
Thüring, A.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.; Torres,
C.; Torrie, C.; Tournefier, E.; Travasso, F.; Traylor, G.; Trias,
M.; Trummer, J.; Ugolini, D.; Ulmen, J.; Urbanek, K.; Vahlbruch, H.;
Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.; van der Putten,
S.; Vass, S.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.;
van Veggel, A. A.; Veitch, J.; Veitch, P.; Veltkamp, C.; Verkindt,
D.; Vetrano, F.; Viceré, A.; Villar, A.; Vinet, J. -Y.; Vocca, H.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward,
R. L.; Was, M.; Weidner, A.; Weinert, M.; Weinstein, A. J.; Weiss, R.;
Wen, L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams,
L.; Willke, B.; Wilmut, I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.;
Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.;
Yamamoto, H.; Yan, Z.; Yoshida, S.; Yvert, M.; Zanolin, M.; Zhang, J.;
Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zweizig, J.; Bégin,
S.; Corongiu, A.; D'Amico, N.; Freire, P. C. C.; Hessels, J. W. T.;
Hobbs, G. B.; Kramer, M.; Lyne, A. G.; Manchester, R. N.; Marshall,
F. E.; Middleditch, J.; Possenti, A.; Ransom, S. M.; Stairs, I. H.;
Stappers, B.; LIGO Scientific Collaboration; Virgo Collaboration
Bibcode: 2010ApJ...713..671A
Altcode: 2009arXiv0909.3583T
We present a search for gravitational waves from 116 known millisecond
and young pulsars using data from the fifth science run of the LIGO
detectors. For this search, ephemerides overlapping the run period
were obtained for all pulsars using radio and X-ray observations. We
demonstrate an updated search method that allows for small uncertainties
in the pulsar phase parameters to be included in the search. We report
no signal detection from any of the targets and therefore interpret our
results as upper limits on the gravitational wave signal strength. The
most interesting limits are those for young pulsars. We present updated
limits on gravitational radiation from the Crab pulsar, where the
measured limit is now a factor of 7 below the spin-down limit. This
limits the power radiated via gravitational waves to be less than ~2%
of the available spin-down power. For the X-ray pulsar J0537 - 6910 we
reach the spin-down limit under the assumption that any gravitational
wave signal from it stays phase locked to the X-ray pulses over timing
glitches, and for pulsars J1913+1011 and J1952+3252 we are only a
factor of a few above the spin-down limit. Of the recycled millisecond
pulsars, several of the measured upper limits are only about an order
of magnitude above their spin-down limits. For these our best (lowest)
upper limit on gravitational wave amplitude is 2.3 × 10-26
for J1603 - 7202 and our best (lowest) limit on the inferred pulsar
ellipticity is 7.0 × 10-8 for J2124 - 3358.
Title: Sensitivity to Gravitational Waves from Compact Binary
Coalescences Achieved during LIGO's Fifth and Virgo's First Science
Run
Authors: The LIGO Scientific Collaboration; the Virgo Collaboration;
Abadie, J.; Abbott, B. P.; Abbott, R.; Abernathy, M; Accadia, T.;
Acernese, F.; Adams, C.; Adhikari, R.; Ajith, P.; Allen, B.; Allen,
G.; Amador Ceron, E.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.;
Antonucci, F.; Aoudia, S.; Arain, M. A.; Araya, M.; Aronsson, M.;
Arun, K. G.; Aso, Y.; Aston, S.; Astone, P.; Atkinson, D. E.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.;
Ballmer, S.; Barker, D.; Barnum, S.; Barone, F.; Barr, B.; Barriga,
P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri,
R.; Bastarrika, M.; Bauchrowitz, J.; Bauer, Th. S.; Behnke, B.; Beker,
M. G.; Benacquista, M.; Bertolini, A.; Betzwieser, J.; Beveridge,
N.; Beyersdorf, P. T.; Bigotta, S.; Bilenko, I. A.; Billingsley, G.;
Birch, J.; Birindelli, S.; Biswas, R.; Bitossi, M.; Bizouard, M. A.;
Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.;
Blom, M.; Boccara, C.; Bock, O.; Bodiya, T. P.; Bondarescu, R.; Bondu,
F.; Bonelli, L.; Bork, R.; Born, M.; Bose, S.; Bosi, L.; Boyle, M.;
Braccini, S.; Bradaschia, C.; Brady, P. R.; Braginsky, V. B.; Brau,
J. E.; Breyer, J.; Bridges, D. O.; Brillet, A.; Brinkmann, M.; Brisson,
V.; Britzger, M.; Brooks, A. F.; Brown, D. A.; Budzyński, R.; Bulik,
T.; Bulten, H. J.; Buonanno, A.; Burguet--Castell, J.; Burmeister,
O.; Buskulic, D.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Calloni,
E.; Camp, J. B.; Campagna, E.; Campsie, P.; Cannizzo, J.; Cannon,
K. C.; Canuel, B.; Cao, J.; Capano, C.; Carbognani, F.; Caride, S.;
Caudill, S.; Cavaglià, M.; Cavalier, F.; Cavalieri, R.; Cella, G.;
Cepeda, C.; Cesarini, E.; Chalermsongsak, T.; Chalkley, E.; Charlton,
P.; Chassande-Mottin, E.; Chelkowski, S.; Chen, Y.; Chincarini, A.;
Christensen, N.; Chua, S. S. Y.; Chung, C. T. Y.; Clark, D.; Clark,
J.; Clayton, J. H.; Cleva, F.; Coccia, E.; Colacino, C. N.; Colas, J.;
Colla, A.; Colombini, M.; Conte, R.; Cook, D.; Corbitt, T. R.; Corda,
C.; Cornish, N.; Corsi, A.; Costa, C. A.; Coulon, J. -P.; Coward,
D.; Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Cruise,
A. M.; Culter, R. M.; Cumming, A.; Cunningham, L.; Cuoco, E.; Dahl,
K.; Danilishin, S. L.; Dannenberg, R.; D'Antonio, S.; Danzmann, K.;
Dari, A.; Das, K.; Dattilo, V.; Daudert, B.; Davier, M.; Davies, G.;
Davis, A.; Daw, E. J.; Day, R.; Dayanga, T.; De Rosa, R.; DeBra, D.;
Degallaix, J.; del Prete, M.; Dergachev, V.; DeRosa, R.; DeSalvo, R.;
Devanka, P.; Dhurandhar, S.; Di Fiore, L.; Di Lieto, A.; Di Palma, I.;
Emilio, M. Di Paolo; Di Virgilio, A.; Díaz, M.; Dietz, A.; Donovan,
F.; Dooley, K. L.; Doomes, E. E.; Dorsher, S.; Douglas, E. S. D.;
Drago, M.; Drever, R. W. P.; Driggers, J. C.; Dueck, J.; Dumas,
J. -C.; Eberle, T.; Edgar, M.; Edwards, M.; Effler, A.; Ehrens, P.;
Engel, R.; Etzel, T.; Evans, M.; Evans, T.; Fafone, V.; Fairhurst, S.;
Fan, Y.; Farr, B. F.; Fazi, D.; Fehrmann, H.; Feldbaum, D.; Ferrante,
I.; Fidecaro, F.; Finn, L. S.; Fiori, I.; Flaminio, R.; Flanigan,
M.; Flasch, K.; Foley, S.; Forrest, C.; Forsi, E.; Fotopoulos, N.;
Fournier, J. -D.; Franc, J.; Frasca, S.; Frasconi, F.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Friedrich,
D.; Fritschel, P.; Frolov, V. V.; Fulda, P.; Fyffe, M.; Gammaitoni,
L.; Garofoli, J. A.; Garufi, F.; Gemme, G.; Genin, E.; Gennai, A.;
Gholami, I.; Ghosh, S.; Giaime, J. A.; Giampanis, S.; Giardina,
K. D.; Giazotto, A.; Gill, C.; Goetz, E.; Goggin, L. M.; González,
G.; Gorodetsky, M. L.; Goßler, S.; Gouaty, R.; Graef, C.; Granata,
M.; Grant, A.; Gras, S.; Gray, C.; Greenhalgh, R. J. S.; Gretarsson,
A. M.; Greverie, C.; Grosso, R.; Grote, H.; Grunewald, S.; Guidi,
G. M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hall, P.; Hallam,
J. M.; Hammer, D.; Hammond, G.; Hanks, J.; Hanna, C.; Hanson, J.;
Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian,
K.; Hayama, K.; Heefner, J.; Heitmann, H.; Hello, P.; Heng, I. S.;
Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge,
K. A.; Holt, K.; Hosken, D. J.; Hough, J.; Howell, E.; Hoyland, D.;
Huet, D.; Hughey, B.; Husa, S.; Huttner, S. H.; Huynh--Dinh, T.;
Ingram, D. R.; Inta, R.; Isogai, T.; Ivanov, A.; Jaranowski, P.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kandhasamy, S.; Kanner, J.; Katsavounidis, E.;
Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalaidovski, A.; Khalili, F. Y.; Khazanov, E. A.; Kim, C.; Kim, H.;
King, P. J.; Kinzel, D. L.; Kissel, J. S.; Klimenko, S.; Kondrashov,
V.; Kopparapu, R.; Koranda, S.; Kowalska, I.; Kozak, D.; Krause, T.;
Kringel, V.; Krishnamurthy, S.; Krishnan, B.; Królak, A.; Kuehn, G.;
Kullman, J.; Kumar, R.; Kwee, P.; Landry, M.; Lang, M.; Lantz, B.;
Lastzka, N.; Lazzarini, A.; Leaci, P.; Leong, J.; Leonor, I.; Leroy,
N.; Letendre, N.; Li, J.; Li, T. G. F.; Lin, H.; Lindquist, P. E.;
Lockerbie, N. A.; Lodhia, D.; Lorenzini, M.; Loriette, V.; Lormand, M.;
Losurdo, G.; Lu, P.; Luan, J.; Lubinski, M.; Lucianetti, A.; Lück,
H.; Lundgren, A.; Machenschalk, B.; MacInnis, M.; Mackowski, J. M.;
Mageswaran, M.; Mailand, K.; Majorana, E.; Mak, C.; Man, N.; Mandel,
I.; Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka,
S.; Márka, Z.; Maros, E.; Marque, J.; Martelli, F.; Martin, I. W.;
Martin, R. M.; Marx, J. N.; Mason, K.; Masserot, A.; Matichard, F.;
Matone, L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McIntyre, G.; McIvor, G.; McKechan, D. J. A.;
Meadors, G.; Mehmet, M.; Meier, T.; Melatos, A.; Melissinos, A. C.;
Mendell, G.; Menéndez, D. F.; Mercer, R. A.; Merill, L.; Meshkov,
S.; Messenger, C.; Meyer, M. S.; Miao, H.; Michel, C.; Milano, L.;
Miller, J.; Minenkov, Y.; Mino, Y.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Moe, B.; Mohan, M.; Mohanty, S. D.;
Mohapatra, S. R. P.; Moraru, D.; Moreau, J.; Moreno, G.; Morgado,
N.; Morgia, A.; Morioka, T.; Mors, K.; Mosca, S.; Moscatelli, V.;
Mossavi, K.; Mours, B.; MowLowry, C.; Mueller, G.; Mukherjee, S.;
Mullavey, A.; Müller-Ebhardt, H.; Munch, J.; Murray, P. G.; Nash,
T.; Nawrodt, R.; Nelson, J.; Neri, I.; Newton, G.; Nishizawa, A.;
Nocera, F.; Nolting, D.; Ochsner, E.; O'Dell, J.; Ogin, G. H.;
Oldenburg, R. G.; O'Reilly, B.; O'Shaughnessy, R.; Osthelder, C.;
Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Page,
A.; Pagliaroli, G.; Palladino, L.; Palomba, C.; Pan, Y.; Pankow,
C.; Paoletti, F.; Papa, M. A.; Pardi, S.; Pareja, M.; Parisi, M.;
Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patel, P.; Pedraza,
M.; Pekowsky, L.; Penn, S.; Peralta, C.; Perreca, A.; Persichetti,
G.; Pichot, M.; Pickenpack, M.; Piergiovanni, F.; Pietka, M.; Pinard,
L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Poggiani,
R.; Postiglione, F.; Prato, M.; Predoi, V.; Price, L. R.; Prijatelj,
M.; Principe, M.; Privitera, S.; Prix, R.; Prodi, G. A.; Prokhorov,
L.; Puncken, O.; Punturo, M.; Puppo, P.; Quetschke, V.; Raab, F. J.;
Rabaste, O.; Rabeling, D. S.; Radke, T.; Radkins, H.; Raffai, P.;
Rakhmanov, M.; Rankins, B.; Rapagnani, P.; Raymond, V.; Re, V.; Reed,
C. M.; Reed, T.; Regimbau, T.; Reid, S.; Reitze, D. H.; Ricci, F.;
Riesen, R.; Riles, K.; Roberts, P.; Robertson, N. A.; Robinet, F.;
Robinson, C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Röver, C.;
Rolland, L.; Rollins, J.; Romano, J. D.; Romano, R.; Romie, J. H.;
Rosińska, D.; Rowan, S.; Rüdiger, A.; Ruggi, P.; Ryan, K.; Sakata,
S.; Sakosky, M.; Salemi, F.; Sammut, L.; Sancho de la Jordana, L.;
Sandberg, V.; Sannibale, V.; Santamaría, L.; Santostasi, G.; Saraf,
S.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.;
Saulson, P. R.; Savage, R.; Schilling, R.; Schnabel, R.; Schofield,
R.; Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott,
S. M.; Searle, A. C.; Seifert, F.; Sellers, D.; Sengupta, A. S.;
Sentenac, D.; Sergeev, A.; Shaddock, D.; Shapiro, B.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Singer,
A.; Sintes, A. M.; Skelton, G.; Slagmolen, B. J. J.; Slutsky, J.;
Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.;
Speirits, F. C.; Stein, A. J.; Stein, L. C.; Steinlechner, S.;
Steplewski, S.; Stochino, A.; Stone, R.; Strain, K. A.; Strigin,
S.; Stroeer, A.; Sturani, R.; Stuver, A. L.; Summerscales, T. Z.;
Sung, M.; Susmithan, S.; Sutton, P. J.; Swinkels, B.; Talukder, D.;
Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.; Thomas,
P.; Thorne, K. A.; Thorne, K. S.; Thrane, E.; Thüring, A.; Titsler,
C.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.; Torres, C.; Torrie,
C. I.; Tournefier, E.; Travasso, F.; Traylor, G.; Trias, M.; Trummer,
J.; Tseng, K.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vaishnav, B.;
Vajente, G.; Vallisneri, M.; van den Brand, J. F. J.; Van Den Broeck,
C.; van der Putten, S.; van der Sluys, M. V.; van Veggel, A. A.; Vass,
S.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.; Vedovato, G.; Veitch,
J.; Veitch, P. J.; Veltkamp, C.; Verkindt, D.; Vetrano, F.; Viceré,
A.; Villar, A.; Vinet, J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin,
S. P.; Waldman, S. J.; Wallace, L.; Wanner, A.; Ward, R. L.; Was,
M.; Wei, P.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen,
S.; Wessels, P.; West, M.; Westphal, T.; Wette, K.; Whelan, J. T.;
Whitcomb, S. E.; White, D. J.; Whiting, B. F.; Wilkinson, C.; Willems,
P. A.; Williams, L.; Willke, B.; Winkelmann, L.; Winkler, W.; Wipf,
C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Yakushin,
I.; Yamamoto, H.; Yamamoto, K.; Yeaton-Massey, D.; Yoshida, S.; Yu,
P. P.; Yvert, M.; Zanolin, M.; Zhang, L.; Zhang, Z.; Zhao, C.; Zotov,
N.; Zucker, M. E.; Zweizig, J.; Belczynski, K.
Bibcode: 2010arXiv1003.2481T
Altcode: 2010arXiv1003.2481L
We summarize the sensitivity achieved by the LIGO and Virgo
gravitational wave detectors for compact binary coalescence (CBC)
searches during LIGO's fifth science run and Virgo's first science
run. We present noise spectral density curves for each of the
four detectors that operated during these science runs which are
representative of the typical performance achieved by the detectors
for CBC searches. These spectra are intended for release to the public
as a summary of detector performance for CBC searches during these
science runs.
Title: On the Origin of the Asymmetric Helicity Injection in Emerging
Active Regions
Authors: Fan, Y.; Alexander, D.; Tian, L.
Bibcode: 2009ApJ...707..604F
Altcode:
To explore the possible causes of the observed asymmetric helicity flux
in emerging active regions between the leading and following polarities
reported in a recent study by Tian & Alexander, we examine the
subsurface evolution of buoyantly rising Ω-shaped flux tubes using
three-dimensional, spherical-shell anelastic MHD simulations. We find
that due to the asymmetric stretching of the Ω-shaped tube by the
Coriolis force, the leading side of the emerging tube has a greater
field strength, is more buoyant, and remains more cohesive compared
to the following side. As a result, the magnetic field lines in the
leading leg show more coherent values of local twist α ≡ (∇ × B)
· B/B 2, whereas the values in the following leg show large
fluctuations and are of mixed sign. On average, however, the field
lines in the leading leg do not show a systematically greater mean
twist compared to the following leg. Due to the higher rise velocity
of the leading leg, the upward helicity flux through a horizontal
cross section at each depth in the upper half of the convection zone
is significantly greater in the leading polarity region than that in
the following leg. This may contribute to the observed asymmetric
helicity flux in emerging active regions. Furthermore, based on a
simplified model of active region flux emergence into the corona by
Longcope & Welsch, we show that a stronger field strength in the
leading tube can result in a faster rotation of the leading polarity
sunspot driven by torsional Alfvén waves during flux emergence into
the corona, contributing to a greater helicity injection rate in the
leading polarity of an emerging active region.
Title: Modeling the Subsurface Evolution of Active-Region Flux Tubes
Authors: Fan, Y.
Bibcode: 2009ASPC..416..489F
Altcode: 2009arXiv0901.1822F
I present results from a set of 3-D spherical-shell MHD simulations
of the buoyant rise of active region flux tubes in the solar interior
that put new constraints on the initial twist of the subsurface tubes
in order for them to emerge with tilt angles consistent with the
observed Joy's law for the mean tilt of solar active regions. Due to
asymmetric stretching of the Ω-shaped tube by the Coriolis force, a
field strength asymmetry develops with the leading side having a greater
field strength and thus being more cohesive compared to the following
side. Furthermore, the magnetic flux in the leading leg shows more
coherent values of local twist α ≡ <STRONG>J</STRONG>
ṡ <STRONG>B</STRONG> / B2, whereas the values
in the following leg show large fluctuations and are of mixed signs.
Title: Erratum: All-sky search for periodic gravitational waves in
LIGO S4 data [Phys. Rev. D 77, 022001 (2008)]
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.;
Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue, L.; Bork,
R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington, A.; Bunkowski,
A.; Buonanno, A.; Burmeister, O.; Busby, D.; Byer, R. L.; Cadonati,
L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.;
Cao, J.; Cardenas, L.; Casey, M. M.; Castaldi, G.; Cepeda, C.; Chalkey,
E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini,
F.; Chin, D.; Chin, E.; Chow, J.; Christensen, N.; Clark, J.; Cochrane,
P.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.; Conte, R.; Cook, D.;
Corbitt, T.; Coward, D.; Coyne, D.; Creighton, J. D. E.; Creighton,
T. D.; Croce, R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.;
Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; Debra, D.;
Degallaix, J.; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.;
Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dickson, J.; di Credico,
A.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.;
Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza,
E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan, Y.; Fazi,
D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos, N.; Franzen,
A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.; Fritschel,
P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L. M.; González, G.; Gossler, S.; Grant, A.; Gras, S.; Gray,
C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote,
H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler,
T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell,
E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito,
M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.;
Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim, C.; King, P.; Kissel,
J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R. K.;
Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.;
Lazzarini, A.; Lee, B.; Lei, M.; Leiner, J.; Leonhardt, V.; Leonor, I.;
Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.; Longo, M.; Lormand, M.;
Lubiński, M.; Lück, H.; Machenschalk, B.; Macinnis, M.; Mageswaran,
M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.; Márka, S.;
Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason, K.; Matone,
L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire,
S. C.; McHugh, M.; McKenzie, K.; McNabb, J. W. C.; McWilliams, S.;
Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.; Meshkov, S.;
Messaritaki, E.; Messenger, C. J.; Meyers, D.; Mikhailov, E.; Mitra,
S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa,
O.; Mohanty, S.; Moreno, G.; Mossavi, K.; Mowlowry, C.; Moylan, A.;
Mudge, D.; Mueller, G.; Mukherjee, S.; Müller-Ebhardt, H.; Munch, J.;
Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton, G.; Nishizawa, A.;
Numata, K.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier,
H.; Owen, B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.;
Pedraza, M.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch,
H.; Plissi, M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab,
F.; Rabeling, D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov,
M.; Ramsunder, M.; Rawlins, K.; Ray-Majumder, S.; Re, V.; Rehbein,
H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; Sancho de La Jordana, L.; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.;
Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.;
Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.;
Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung,
M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor,
R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; van den Broeck, C.; Varvella, M.; Vass, S.; Vecchio,
A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.;
Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Webber, D.;
Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.;
Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.;
Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods,
D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan,
Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao,
C.; Zotov, N.; Zucker, M.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2009PhRvD..80l9904A
Altcode:
No abstract at ADS
Title: ERRATUM: "Beating the Spin-Down Limit on
Gravitational Wave Emission from the Crab Pulsar" (2008, ApJ, 683, L45)
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen,
B.; Allen, G.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M. A.; Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.;
Barish, B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton,
M. A.; Bastarrika, M.; Bayer, K.; Betzwieser, J.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.;
Blackburn, L.; Blair, D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork,
R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Brinkmann, M.; Brooks, A.; Brown, D. A.; Brunet, G.; Bullington, A.;
Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati, L.; Cagnoli,
G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cao, J.; Cardenas, L.;
Casebolt, T.; Castaldi, G.; Cepeda, C.; Chalkley, E.; Charlton, P.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Clark, D.;
Clark, J.; Cokelaer, T.; Conte, R.; Cook, D.; Corbitt, T.; Coyne,
D.; Creighton, J. D. E.; Cumming, A.; Cunningham, L.; Cutler, R. M.;
Dalrymple, J.; Danzmann, K.; Davies, G.; De Bra, D.; Degallaix, J.;
Degree, M.; Dergachev, V.; Desai, S.; De Salvo, R.; Dhurandhar, S.;
Díaz, M.; Dickson, J.; Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes,
E. E.; Drever, R. W. P.; Duke, I.; Dumas, J. -C.; Dupuis, R. J.; Dwyer,
J. G.; Echols, C.; Effler, A.; Ehrens, P.; Espinoza, E.; Etzel, T.;
Evans, T.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fehrmann, H.; Fejer,
M. M.; Finn, L. S.; Flasch, K.; Fotopoulos, N.; Freise, A.; Frey, R.;
Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Garofoli, J.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L.; González, G.; Gossler, S.; Gouaty, R.; Grant,
A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.; Gretarsson,
A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grunewald, S.; Guenther,
M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayama,
K.; Hayler, T.; Heefner, J.; Heng, I. S.; Hennessy, M.; Heptonstall,
A.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough,
J.; Huttner, S. H.; Ingram, D.; Ito, M.; Ivanov, A.; Johnson, B.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kamat, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis,
E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalili, F. Ya.; Khan, R.; Khazanov, E.; Kim, C.; King, P.; Kissel,
J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R. K.;
Kozak, D.; Kozhevatov, I.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry,
M.; Lang, M. M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leindecker, N.;
Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lin, H.; Lindquist, P.;
Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu, P.; Lubiński, M.;
Lucianetti, A.; Lück, H.; Machenschalk, B.; Mac Innis, M.; Mageswaran,
M.; Mailand, K.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Martin, I.; Martin, R. M.; Marx, J. N.;
Mason, K.; Matichard, F.; Matone, L.; Matzner, R.; Mavalvala, N.;
McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McIntyre,
G.; McIvor, G.; McKechan, D.; McKenzie, K.; Meier, T.; Melissinos, A.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger, C. J.; Meyers, D.;
Miller, J.; Minelli, J.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S.; Moreno, G.;
Mossavi, K.; Lowry, C. Mow; Mueller, G.; Mukherjee, S.; Mukhopadhyay,
H.; Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.;
Nash, T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell,
J.; Ogin, G.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.; Papa, M. A.;
Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Perreca, A.;
Petrie, T.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.;
Postiglione, F.; Principe, M.; Prix, R.; Quetschke, V.; Raab, F.;
Rabeling, D. S.; Radkins, H.; Rainer, N.; Rakhmanov, M.; Ramsunder,
M.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; Sancho de la Jordana, L.; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S. W.; Schilling,
R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.;
Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens,
X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.;
Stein, L. C.; Stochino, A.; Stone, R.; Strain, K. A.; Strom, D. M.;
Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.;
Takahashi, H.; Tanner, D. B.; Taylor, R.; Taylor, R.; Thacker, J.;
Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov, K. V.; Torres,
C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.; Ugolini, D.; Ulmen,
J.; Urbanek, K.; Vahlbruch, H.; Van Den Broeck, C.; van der Sluys,
M.; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar,
A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward,
H.; Ward, R.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut,
I.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.;
Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida,
S.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker,
M.; Zweizig, J.; LIGO Scientific Collaboration; Santostasi, G.
Bibcode: 2009ApJ...706L.203A
Altcode:
A processing error in the signal template used in this search led to
upper limits about 30% lower than we now know is warranted by the early
S5 data. We have re-analyzed that data and find new upper limits on
the strain parameter h 0 of 4.9 × 10-25/3.9 ×
10-25 for uniform/restricted prior assumptions concerning
the Crab inclination and polarization angles. These results have now
been superseded by upper limits of 2.6 × 10-25/2.0 ×
10-25 based on the full S5 data and presented in Abbott et
al. (2009). The multitemplate search was not affected by the error.
Title: Search for high frequency gravitational-wave bursts in the
first calendar year of LIGO's fifth science run
Authors: Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen, B.;
Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.;
Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker, C.; Barker,
D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista, M.; Betzwieser,
J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Biswas, R.;
Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.;
Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose, S.; Brady,
P. R.; Braginsky, V. B.; Brau, J. E.; Bridges, D. O.; Brinkmann, M.;
Brooks, A. F.; Brown, D. A.; Brummit, A.; Brunet, G.; Bullington,
A.; Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati, L.; Camp,
J. B.; Cannizzo, J.; Cannon, K. C.; Cao, J.; Cardenas, L.; Caride, S.;
Castaldi, G.; Caudill, S.; Cavaglià, M.; Cepeda, C.; Chalermsongsak,
T.; Chalkley, E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen,
Y.; Christensen, N.; Chung, C. T. Y.; Clark, D.; Clark, J.; Clayton,
J. H.; Cokelaer, T.; Colacino, C. N.; Conte, R.; Cook, D.; Corbitt,
T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.; di Credico, A.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; Debra, D.; Degallaix, J.; Dergachev, V.;
Desai, S.; Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dietz, A.; Donovan,
F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Dueck, J.; Duke,
I.; Dumas, J. -C.; Dwyer, J. G.; Echols, C.; Edgar, M.; Effler, A.;
Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst,
S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Finn, L. S.; Flasch,
K.; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen, A.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.;
Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J. A.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty,
R.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grunewald,
S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam,
J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson, J.; Harms, J.;
Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.;
Heefner, J.; Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.;
Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough,
J.; Hoyland, D.; Hughey, B.; Huttner, S. H.; Ingram, D. R.; Isogai,
T.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.; Klimenko, S.;
Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.;
Krishnan, B.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.;
Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor, I.; Li, C.;
Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie, N. A.; Lodhia,
D.; Longo, M.; Lormand, M.; Lu, P.; Lubiński, M.; Lucianetti, A.;
Lück, H.; Machenschalk, B.; Macinnis, M.; Mageswaran, M.; Mailand,
K.; Mandel, I.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.;
Mason, K.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala,
N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.;
McIntyre, G.; McKechan, D. J. A.; McKenzie, K.; Mehmet, M.; Melatos,
A.; Melissinos, A. C.; Menéndez, D. F.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messenger, C.; Meyer, M. S.; Miller, J.; Minelli,
J.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Moe, B.; Mohanty, S. D.; Mohapatra, S. R. P.; Moreno,
G.; Morioka, T.; Mors, K.; Mossavi, K.; Mowlowry, C.; Mueller, G.;
Müller-Ebhardt, H.; Muhammad, D.; Mukherjee, S.; Mukhopadhyay, H.;
Mullavey, A.; Munch, J.; Murray, P. G.; Myers, E.; Myers, J.; Nash,
T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell, J.;
O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.; Ogin, G. H.; Ottaway,
D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.;
Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.;
Perraca, A.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Postiglione, F.; Principe, M.; Prix, R.; Prokhorov, L.;
Puncken, O.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins,
H.; Raffai, P.; Raics, Z.; Rainer, N.; Rakhmanov, M.; Raymond, V.;
Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen,
R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson, N. A.; Robinson,
C.; Robinson, E. L.; Roddy, S.; Röver, C.; Rollins, J.; Romano,
J. D.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Russell, P.; Ryan, K.;
Sakata, S.; de La Jordana, L. Sancho; Sandberg, V.; Sannibale, V.;
Santamaría, L.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Satterthwaite, M.; Saulson, P. R.; Savage, R.; Savov, P.; Scanlan,
M.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz, B.; Schutz,
B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Sears,
B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shapiro,
B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.;
Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein,
A.; Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain,
K. A.; Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.;
Sun, K. -X.; Sung, M.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.;
Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov,
K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Ugolini, D.;
Ulmen, J.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; van den Broeck,
C.; van der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin, R.;
Vecchio, A.; Veitch, J.; Veitch, P.; Veltkamp, C.; Villadsen, J.;
Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace,
L.; Ward, R. L.; Weidner, A.; Weinert, M.; Weinstein, A. J.; Weiss, R.;
Wen, L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Wilmut, I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.;
Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin,
I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang,
L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2009PhRvD..80j2002A
Altcode: 2009arXiv0904.4910L
We present an all-sky search for gravitational waves in the frequency
range 1 to 6 kHz during the first calendar year of LIGO’s fifth
science run. This is the first untriggered LIGO burst analysis
to be conducted above 3 kHz. We discuss the unique properties of
interferometric data in this regime. 161.3 days of triple-coincident
data were analyzed. No gravitational events above threshold were
observed and a frequentist upper limit of 5.4year-1 on
the rate of strong gravitational-wave bursts was placed at a 90%
confidence level. Implications for specific theoretical models of
gravitational-wave emission are also discussed.
Title: Search for gravitational-wave bursts in the first year of
the fifth LIGO science run
Authors: Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen,
B.; Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain,
M. A.; Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker,
C.; Barker, D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.;
Bartos, I.; Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista,
M.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair,
D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose,
S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Bridges, D. O.;
Brinkmann, M.; Brooks, A. F.; Brown, D. A.; Brummit, A.; Brunet, G.;
Bullington, A.; Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati,
L.; Camp, J. B.; Cannizzo, J.; Cannon, K. C.; Cao, J.; Cardenas,
L.; Caride, S.; Castaldi, G.; Caudill, S.; Cavaglià, M.; Cepeda,
C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Christensen, N.; Chung, C. T. Y.; Clark, D.;
Clark, J.; Clayton, J. H.; Cokelaer, T.; Colacino, C. N.; Conte, R.;
Cook, D.; Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; Debra, D.; Degallaix, J.; Dergachev, V.;
Desai, S.; Desalvo, R.; Dhurandhar, S.; Díaz, M.; di Credico, A.;
Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.;
Dueck, J.; Duke, I.; Dumas, J. -C.; Dwyer, J. G.; Echols, C.; Edgar,
M.; Effler, A.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans,
T.; Fairhurst, S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Finn,
L. S.; Flasch, K.; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen,
A.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T.;
Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J. A.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler,
S.; Gouaty, R.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.;
Grunewald, S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage,
B.; Hallam, J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson,
J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian,
K.; Hayama, K.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken,
D. J.; Hough, J.; Hoyland, D.; Hughey, B.; Huttner, S. H.; Ingram,
D. R.; Isogai, T.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kandhasamy, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski,
A.; Khalili, F. Y.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.;
Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.;
Kozak, D.; Krishnan, B.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.;
Lantz, B.; Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor,
I.; Li, C.; Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie,
N. A.; Lodhia, D.; Longo, M.; Lormand, M.; Lu, P.; Lubiński, M.;
Lucianetti, A.; Lück, H.; Machenschalk, B.; Macinnis, M.; Mageswaran,
M.; Mailand, K.; Mandel, I.; Mandic, V.; Márka, S.; Márka, Z.;
Markosyan, A.; Markowitz, J.; Maros, E.; Martin, I. W.; Martin,
R. M.; Marx, J. N.; Mason, K.; Matichard, F.; Matone, L.; Matzner,
R. A.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.;
McHugh, M.; McIntyre, G.; McKechan, D. J. A.; McKenzie, K.; Mehmet,
M.; Melatos, A.; Melissinos, A. C.; Menéndez, D. F.; Mendell, G.;
Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Miller, J.;
Minelli, J.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman,
R.; Miyakawa, O.; Moe, B.; Mohanty, S. D.; Mohapatra, S. R. P.; Moreno,
G.; Morioka, T.; Mors, K.; Mossavi, K.; Mowlowry, C.; Mueller, G.;
Müller-Ebhardt, H.; Muhammad, D.; Mukherjee, S.; Mukhopadhyay, H.;
Mullavey, A.; Munch, J.; Murray, P. G.; Myers, E.; Myers, J.; Nash,
T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell, J.;
O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.; Ogin, G. H.; Ottaway,
D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.;
Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.;
Perraca, A.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Postiglione, F.; Principe, M.; Prix, R.; Prokhorov, L.;
Puncken, O.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins,
H.; Raffai, P.; Raics, Z.; Rainer, N.; Rakhmanov, M.; Raymond, V.;
Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen,
R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson, N. A.; Robinson,
C.; Robinson, E. L.; Roddy, S.; Röver, C.; Rollins, J.; Romano,
J. D.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Russell, P.; Ryan, K.;
Sakata, S.; Sancho de La Jordana, L.; Sandberg, V.; Sannibale, V.;
Santamaría, L.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Satterthwaite, M.; Saulson, P. R.; Savage, R.; Savov, P.; Scanlan,
M.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz, B.; Schutz,
B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Sears,
B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shapiro,
B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.;
Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein,
A.; Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain,
K. A.; Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.;
Sun, K. -X.; Sung, M.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.;
Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thüring, A.; Tokmakov, K. V.; Torres,
C.; Torrie, C.; Traylor, G.; Trias, M.; Ugolini, D.; Ulmen, J.;
Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; van den Broeck, C.; van
der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin, R.; Vecchio,
A.; Veitch, J.; Veitch, P.; Veltkamp, C.; Villar, A.; Vorvick, C.;
Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, R. L.; Weidner,
A.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut,
I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan,
G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan,
Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov,
N.; Zucker, M. E.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2009PhRvD..80j2001A
Altcode: 2009arXiv0905.0020L
We present the results obtained from an all-sky search for
gravitational-wave (GW) bursts in the 64-2000 Hz frequency range
in data collected by the LIGO detectors during the first year
(November 2005—November 2006) of their fifth science run. The
total analyzed live time was 268.6 days. Multiple hierarchical
data analysis methods were invoked in this search. The overall
sensitivity expressed in terms of the root-sum-square (rss) strain
amplitude hrss for gravitational-wave bursts with various
morphologies was in the range of 6×10-22Hz-1/2 to
a few×10-21Hz-1/2. No GW signals were observed
and a frequentist upper limit of 3.75 events per year on the rate of
strong GW bursts was placed at the 90% confidence level. As in our
previous searches, we also combined this rate limit with the detection
efficiency for selected waveform morphologies to obtain event rate
versus strength exclusion curves. In sensitivity, these exclusion
curves are the most stringent to date.
Title: A Model of Coronal Streamers with Underlying Flux Ropes
Authors: Cottaar, M.; Fan, Y.
Bibcode: 2009ApJ...704..576C
Altcode:
We present global two-dimensional axisymmetric isothermal MHD
simulations of the dynamic evolution of a coronal helmet streamer,
driven at the lower boundary by the emergence of a twisted flux rope. By
varying both the detached toroidal and poloidal fluxes emerged into
the corona, but fixing the normal flux distribution at the surface at
the end of the emergence, we obtain solutions that either settle to a
new steady state of a stable helmet streamer containing a flux rope,
or result in a disruption of the helmet with the underlying flux rope
being expelled in a coronal mass ejection (CME)-like eruption. In all
of the cases studied, we find that the transition from a stable to an
eruptive state takes place at a magnetic energy that is very close to
the Aly open field energy. Furthermore, we find that the transition
from a stable to an eruptive end state does not occur at a single
critical value of the total relative magnetic helicity, but depends
on the profile of the underlying flux rope. Cases where the detached
flux rope contains a higher amount of self-helicity, i.e., higher
internal twist or detached poloidal flux, are found to become eruptive
at a significantly lower total helicity. For the eruptive cases, the
detached flux rope after emergence first rises quasi-statically due
to a gradual opening of the field lines at the edge of the streamer
and a slow reconnection below the flux rope, which continues to
slowly increase the amount of the detached flux. This decreases the
downward magnetic tension on the flux rope. The dynamic eruption is
initiated when the magnetic pressure gradient no longer decreases fast
enough to balance the decrease in the magnetic tension. Later rapid
reconnections below the flux rope are important for accelerating the
flux rope. For the stable helmets, we find that no cavities are formed
due to the simplifying assumption of isothermal energetics and the
uniform density lower boundary condition. However during the eruption
we see the development of the 3-part structure of a CME.
Title: Search for gravitational wave ringdowns from perturbed black
holes in LIGO S4 data
Authors: Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen, B.;
Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.;
Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker, C.; Barker,
D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista, M.; Betzwieser,
J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Biswas, R.;
Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.;
Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose, S.; Brady,
P. R.; Braginsky, V. B.; Brau, J. E.; Bridges, D. O.; Brinkmann, M.;
Brooks, A. F.; Brown, D. A.; Brummit, A.; Brunet, G.; Bullington,
A.; Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati, L.; Camp,
J. B.; Cannizzo, J.; Cannon, K. C.; Cao, J.; Cardenas, L.; Cardoso,
V.; Caride, S.; Castaldi, G.; Caudill, S.; Cavaglià, M.; Cepeda,
C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Christensen, N.; Chung, C. T. Y.; Clark, D.;
Clark, J.; Clayton, J. H.; Cokelaer, T.; Colacino, C. N.; Conte, R.;
Cook, D.; Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; Debra, D.; Degallaix, J.; Dergachev, V.;
Desai, S.; Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dietz, A.; Donovan,
F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Dueck, J.; Duke,
I.; Dumas, J. -C.; Dwyer, J. G.; Echols, C.; Edgar, M.; Effler, A.;
Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst,
S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Finn, L. S.; Flasch,
K.; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen, A.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.;
Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J. A.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty,
R.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grunewald,
S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam,
J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson, J.; Harms, J.;
Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.;
Heefner, J.; Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.;
Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough,
J.; Hoyland, D.; Hughey, B.; Huttner, S. H.; Ingram, D. R.; Isogai,
T.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.; Klimenko, S.;
Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.;
Krishnan, B.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.;
Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor, I.; Li, C.;
Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie, N. A.; Lodhia,
D.; Longo, M.; Lormand, M.; Lu, P.; Lubiński, M.; Lucianetti, A.;
Lück, H.; Machenschalk, B.; Macinnis, M.; Mageswaran, M.; Mailand,
K.; Mandel, I.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.;
Mason, K.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala,
N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.;
McIntyre, G.; McKechan, D. J. A.; McKenzie, K.; Mehmet, M.; Melatos,
A.; Melissinos, A. C.; Menéndez, D. F.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messenger, C.; Meyer, M. S.; Miller, J.; Minelli,
J.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Moe, B.; Mohanty, S. D.; Mohapatra, S. R. P.; Moreno,
G.; Morioka, T.; Mors, K.; Mossavi, K.; Mowlowry, C.; Mueller, G.;
Müller-Ebhardt, H.; Muhammad, D.; Mukherjee, S.; Mukhopadhyay, H.;
Mullavey, A.; Munch, J.; Murray, P. G.; Myers, E.; Myers, J.; Nash,
T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell, J.;
O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.; Ogin, G. H.; Ottaway,
D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.;
Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.;
Perraca, A.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Postiglione, F.; Principe, M.; Prix, R.; Prokhorov,
L.; Punken, O.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins,
H.; Raffai, P.; Raics, Z.; Rainer, N.; Rakhmanov, M.; Raymond, V.;
Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen,
R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson, N. A.; Robinson,
C.; Robinson, E. L.; Roddy, S.; Röver, C.; Rollins, J.; Romano,
J. D.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Russell, P.; Ryan, K.;
Sakata, S.; de La Jordana, L. Sancho; Sandberg, V.; Sannibale, V.;
Santamaría, L.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Satterthwaite, M.; Saulson, P. R.; Savage, R.; Savov, P.; Scanlan,
M.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz, B.; Schutz,
B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Sears,
B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shapiro,
B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.;
Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein,
A.; Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain,
K. A.; Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.;
Sun, K. -X.; Sung, M.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.;
Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov,
K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Ugolini,
D.; Ulmen, J.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; van den
Broeck, C.; van der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin,
R.; Vecchio, A.; Veitch, J.; Veitch, P.; Veltkamp, C.; Villar, A.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward,
R. L.; Weidner, A.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen,
L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Wilmut, I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.;
Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin,
I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang,
L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2009PhRvD..80f2001A
Altcode: 2009arXiv0905.1654T
According to general relativity a perturbed black hole will settle
to a stationary configuration by the emission of gravitational
radiation. Such a perturbation will occur, for example, in the
coalescence of a black hole binary, following their inspiral and
subsequent merger. At late times the waveform is a superposition of
quasinormal modes, which we refer to as the ringdown. The dominant
mode is expected to be the fundamental mode, l=m=2. Since this is a
well-known waveform, matched filtering can be implemented to search for
this signal using LIGO data. We present a search for gravitational waves
from black hole ringdowns in the fourth LIGO science run S4, during
which LIGO was sensitive to the dominant mode of perturbed black holes
with masses in the range of 10M⊙ to 500M⊙, the
regime of intermediate-mass black holes, to distances up to 300 Mpc. We
present a search for gravitational waves from black hole ringdowns
using data from S4. No gravitational wave candidates were found;
we place a 90%-confidence upper limit on the rate of ringdowns from
black holes with mass between 85M⊙ and 390M⊙
in the local universe, assuming a uniform distribution of sources, of
3.2×10-5yr-1Mpc-3=1.6×10-3yr-1L10-1,where
L10 is 1010 times the solar blue-light luminosity.
Title: First LIGO search for gravitational wave bursts from cosmic
(super)strings
Authors: Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen,
B.; Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain,
M. A.; Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker,
C.; Barker, D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.;
Bartos, I.; Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista,
M.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair,
D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose,
S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Bridges, D. O.;
Brinkmann, M.; Brooks, A. F.; Brown, D. A.; Brummit, A.; Brunet, G.;
Bullington, A.; Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati,
L.; Camp, J. B.; Cannizzo, J.; Cannon, K. C.; Cao, J.; Cardenas,
L.; Caride, S.; Castaldi, G.; Caudill, S.; Cavaglià, M.; Cepeda,
C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Christensen, N.; Chung, C. T. Y.; Clark, D.;
Clark, J.; Clayton, J. H.; Cokelaer, T.; Colacino, C. N.; Conte, R.;
Cook, D.; Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; Debra, D.; Degallaix, J.; Dergachev, V.;
Desai, S.; Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dietz, A.; Donovan,
F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Dueck, J.; Duke,
I.; Dumas, J. -C.; Dwyer, J. G.; Echols, C.; Edgar, M.; Effler, A.;
Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst,
S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Finn, L. S.; Flasch,
K.; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen, A.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.;
Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J. A.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty,
R.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grunewald,
S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam,
J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson, J.; Harms, J.;
Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.;
Heefner, J.; Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.;
Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough,
J.; Hoyland, D.; Hughey, B.; Huttner, S. H.; Ingram, D. R.; Isogai,
T.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.; Klimenko, S.;
Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.;
Krishnan, B.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.;
Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor, I.; Li, C.;
Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie, N. A.; Lodhia,
D.; Longo, M.; Lormand, M.; Lu, P.; Lubiński, M.; Lucianetti, A.;
Lück, H.; Machenschalk, B.; Macinnis, M.; Mageswaran, M.; Mailand,
K.; Mandel, I.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.;
Mason, K.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala,
N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.;
McIntyre, G.; McKechan, D. J. A.; McKenzie, K.; Mehmet, M.; Melatos,
A.; Melissinos, A. C.; Menéndez, D. F.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messenger, C.; Meyer, M. S.; Miller, J.; Minelli,
J.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Moe, B.; Mohanty, S. D.; Mohapatra, S. R. P.; Moreno,
G.; Morioka, T.; Mors, K.; Mossavi, K.; Mowlowry, C.; Mueller, G.;
Müller-Ebhardt, H.; Muhammad, D.; Mukherjee, S.; Mukhopadhyay, H.;
Mullavey, A.; Munch, J.; Murray, P. G.; Myers, E.; Myers, J.; Nash,
T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell, J.;
O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.; Ogin, G. H.; Ottaway,
D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.;
Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.;
Perreca, A.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Postiglione, F.; Principe, M.; Prix, R.; Prokhorov,
L.; Punken, O.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins,
H.; Raffai, P.; Raics, Z.; Rainer, N.; Rakhmanov, M.; Raymond, V.;
Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen,
R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson, N. A.; Robinson,
C.; Robinson, E. L.; Roddy, S.; Röver, C.; Rollins, J.; Romano,
J. D.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Russell, P.; Ryan, K.;
Sakata, S.; Sancho de La Jordana, L.; Sandberg, V.; Sannibale, V.;
Santamaría, L.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Satterthwaite, M.; Saulson, P. R.; Savage, R.; Savov, P.; Scanlan,
M.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz, B.; Schutz,
B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Sears,
B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shapiro,
B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.;
Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein,
A.; Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain,
K. A.; Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.;
Sun, K. -X.; Sung, M.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.;
Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov,
K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Ugolini,
D.; Ulmen, J.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; van den
Broeck, C.; van der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin,
R.; Vecchio, A.; Veitch, J.; Veitch, P.; Veltkamp, C.; Villar, A.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward,
R. L.; Weidner, A.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen,
L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Wilmut, I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.;
Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin,
I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang,
L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zur Mühlen, H.; Zweizig,
J.; Robinet, F.
Bibcode: 2009PhRvD..80f2002A
Altcode: 2009arXiv0904.4718L
We report on a matched-filter search for gravitational wave bursts
from cosmic string cusps using LIGO data from the fourth science run
(S4) which took place in February and March 2005. No gravitational
waves were detected in 14.9 days of data from times when all three
LIGO detectors were operating. We interpret the result in terms of a
frequentist upper limit on the rate of gravitational wave bursts and
use the limits on the rate to constrain the parameter space (string
tension, reconnection probability, and loop sizes) of cosmic string
models. Many grand unified theory-scale models (with string tension
Gμ/c2≈10-6) can be ruled out at 90% confidence
for reconnection probabilities p≤10-3 if loop sizes are
set by gravitational back reaction.
Title: Additive Self-helicity as a Kink Mode Threshold
Authors: Malanushenko, A.; Longcope, D. W.; Fan, Y.; Gibson, S. E.
Bibcode: 2009ApJ...702..580M
Altcode: 2009arXiv0909.4959M
In this paper, we propose that additive self-helicity, introduced
by Longcope and Malanushenko, plays a role in the kink instability
for complex equilibria, similar to twist helicity for thin flux
tubes. We support this hypothesis by a calculation of additive
self-helicity of a twisted flux tube from the simulation of Fan and
Gibson. As more twist gets introduced, the additive self-helicity
increases, and the kink instability of the tube coincides with the
drop of additive self-helicity, after the latter reaches the value
of HA /Φ2 ≈ 1.5 (where Φ is the flux of the
tube and HA is the additive self-helicity). We compare the
additive self-helicity to twist for a thin subportion of the tube
to illustrate that HA /Φ2 is equal to the
twist number, studied by Berger and Field, when the thin flux tube
approximation is applicable. We suggest that the quantity HA
/Φ2 could be treated as a generalization of a twist number,
when the thin flux tube approximation is not applicable. A threshold on
a generalized twist number might prove extremely useful studying complex
equilibria, just as the twist number itself has proven useful studying
idealized thin flux tubes. We explicitly describe a numerical method
for calculating additive self-helicity, which includes an algorithm
for identifying a domain occupied by a flux bundle and a method of
calculating potential magnetic field confined to this domain. We also
describe a numerical method to calculate twist of a thin flux tube,
using a frame parallelly transported along the axis of the tube.
Title: Einstein@Home search for periodic gravitational waves in
early S5 LIGO data
Authors: Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen,
B.; Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain,
M. A.; Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker,
C.; Barker, D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.;
Bartos, I.; Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista,
M.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair,
D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose,
S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Bridges, D. O.;
Brinkmann, M.; Brooks, A. F.; Brown, D. A.; Brummit, A.; Brunet, G.;
Bullington, A.; Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati,
L.; Camp, J. B.; Cannizzo, J.; Cannon, K. C.; Cao, J.; Cardenas,
L.; Caride, S.; Castaldi, G.; Caudill, S.; Cavaglià, M.; Cepeda,
C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Christensen, N.; Chung, C. T. Y.; Clark, D.;
Clark, J.; Clayton, J. H.; Cokelaer, T.; Colacino, C. N.; Conte, R.;
Cook, D.; Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; Debra, D.; Degallaix, J.; Dergachev, V.;
Desai, S.; Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dietz, A.; Donovan,
F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Dueck, J.; Duke,
I.; Dumas, J. -C.; Dwyer, J. G.; Echols, C.; Edgar, M.; Effler, A.;
Ehrens, P.; Ely, G.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.;
Fairhurst, S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Finn,
L. S.; Flasch, K.; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen,
A.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T.;
Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J. A.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler,
S.; Gouaty, R.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.;
Grunewald, S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage,
B.; Hallam, J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson,
J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian,
K.; Hayama, K.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken,
D. J.; Hough, J.; Hoyland, D.; Hughey, B.; Huttner, S. H.; Ingram,
D. R.; Isogai, T.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kandhasamy, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski,
A.; Khalili, F. Y.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.;
Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.;
Kozak, D.; Krishnan, B.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.;
Lantz, B.; Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor,
I.; Li, C.; Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie,
N. A.; Lodhia, D.; Longo, M.; Lormand, M.; Lu, P.; Lubiński, M.;
Lucianetti, A.; Lück, H.; Machenschalk, B.; Macinnis, M.; Mageswaran,
M.; Mailand, K.; Mandel, I.; Mandic, V.; Márka, S.; Márka, Z.;
Markosyan, A.; Markowitz, J.; Maros, E.; Martin, I. W.; Martin,
R. M.; Marx, J. N.; Mason, K.; Matichard, F.; Matone, L.; Matzner,
R. A.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.;
McHugh, M.; McIntyre, G.; McKechan, D. J. A.; McKenzie, K.; Mehmet,
M.; Melatos, A.; Melissinos, A. C.; Menéndez, D. F.; Mendell, G.;
Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Miller, J.;
Minelli, J.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman,
R.; Miyakawa, O.; Moe, B.; Mohanty, S. D.; Mohapatra, S. R. P.; Moreno,
G.; Morioka, T.; Mors, K.; Mossavi, K.; Mowlowry, C.; Mueller, G.;
Müller-Ebhardt, H.; Muhammad, D.; Mukherjee, S.; Mukhopadhyay, H.;
Mullavey, A.; Munch, J.; Murray, P. G.; Myers, E.; Myers, J.; Nash,
T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell, J.;
O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.; Ogin, G. H.; Ottaway,
D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.;
Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.;
Perreca, A.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Postiglione, F.; Principe, M.; Prix, R.; Prokhorov,
L.; Punken, O.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins,
H.; Raffai, P.; Raics, Z.; Rainer, N.; Rakhmanov, M.; Raymond, V.;
Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen,
R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson, N. A.; Robinson,
C.; Robinson, E. L.; Roddy, S.; Röver, C.; Rollins, J.; Romano,
J. D.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Russell, P.; Ryan, K.;
Sakata, S.; Sancho de La Jordana, L.; Sandberg, V.; Sannibale, V.;
Santamaría, L.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Satterthwaite, M.; Saulson, P. R.; Savage, R.; Savov, P.; Scanlan,
M.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz, B.; Schutz,
B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Sears,
B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shapiro,
B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.;
Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein,
A.; Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain,
K. A.; Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.;
Sun, K. -X.; Sung, M.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.;
Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov,
K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Ugolini,
D.; Ulmen, J.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; van den
Broeck, C.; van der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin,
R.; Vecchio, A.; Veitch, J.; Veitch, P.; Veltkamp, C.; Villar, A.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward,
R. L.; Weidner, A.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen,
L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Wilmut, I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.;
Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin,
I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang,
L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zur Mühlen, H.; Zweizig,
J.; Anderson, D. P.
Bibcode: 2009PhRvD..80d2003A
Altcode: 2009arXiv0905.1705L
This paper reports on an all-sky search for periodic gravitational
waves from sources such as deformed isolated rapidly spinning neutron
stars. The analysis uses 840 hours of data from 66 days of the fifth
LIGO science run (S5). The data were searched for quasimonochromatic
waves with frequencies f in the range from 50 to 1500 Hz, with a linear
frequency drift f˙ (measured at the solar system barycenter) in the
range -f/τ<f˙<0.1f/τ, for a minimum spin-down age τ of 1000
years for signals below 400 Hz and 8000 years above 400 Hz. The main
computational work of the search was distributed over approximately 100
000 computers volunteered by the general public. This large computing
power allowed the use of a relatively long coherent integration time
of 30 hours while searching a large parameter space. This search
extends Einstein@Home’s previous search in LIGO S4 data to about
3 times better sensitivity. No statistically significant signals
were found. In the 125-225 Hz band, more than 90% of sources with
dimensionless gravitational-wave strain tensor amplitude greater than
3×10-24 would have been detected.
Title: An upper limit on the stochastic gravitational-wave background
of cosmological origin
Authors: Abbott, B. P.; Abbott, R.; Acernese, F.; Adhikari, R.; Ajith,
P.; Allen, B.; Allen, G.; Alshourbagy, M.; Amin, R. S.; Anderson,
S. B.; Anderson, W. G.; Antonucci, F.; Aoudia, S.; Arain, M. A.; Araya,
M.; Armandula, H.; Armor, P.; Arun, K. G.; Aso, Y.; Aston, S.; Astone,
P.; Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballardin, G.;
Ballmer, S.; Barker, C.; Barker, D.; Barone, F.; Barr, B.; Barriga,
P.; Barsotti, L.; Barsuglia, M.; Barton, M. A.; Bartos, I.; Bassiri,
R.; Bastarrika, M.; Bauer, Th. S.; Behnke, B.; Beker, M.; Benacquista,
M.; Betzwieser, J.; Beyersdorf, P. T.; Bigotta, S.; Bilenko, I. A.;
Billingsley, G.; Birindelli, S.; Biswas, R.; Bizouard, M. A.; Black,
E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.; Boccara, C.;
Bodiya, T. P.; Bogue, L.; Bondu, F.; Bonelli, L.; Bork, R.; Boschi,
V.; Bose, S.; Bosi, L.; Braccini, S.; Bradaschia, C.; Brady, P. R.;
Braginsky, V. B.; Van Den Brand, J. F. J.; Brau, J. E.; Bridges,
D. O.; Brillet, A.; Brinkmann, M.; Brisson, V.; van den Broeck, C.;
Brooks, A. F.; Brown, D. A.; Brummit, A.; Brunet, G.; Bullington,
A.; Bulten, H. J.; Buonanno, A.; Burmeister, O.; Buskulic, D.; Byer,
R. L.; Cadonati, L.; Cagnoli, G.; Calloni, E.; Camp, J. B.; Campagna,
E.; Cannizzo, J.; Cannon, K. C.; Canuel, B.; Cao, J.; Carbognani, F.;
Cardenas, L.; Caride, S.; Castaldi, G.; Caudill, S.; Cavaglià, M.;
Cavalier, F.; Cavalieri, R.; Cella, G.; Cepeda, C.; Cesarini, E.;
Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chassande-Mottin,
E.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Chung,
C. T. Y.; Clark, D.; Clark, J.; Clayton, J. H.; Cleva, F.; Coccia,
E.; Cokelaer, T.; Colacino, C. N.; Colas, J.; Colla, A.; Colombini,
M.; Conte, R.; Cook, D.; Corbitt, T. R. C.; Corda, C.; Cornish,
N.; Corsi, A.; Coulon, J. -P.; Coward, D.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Cuoco, E.; Danilishin, S. L.; D'Antonio, S.; Danzmann,
K.; Dari, A.; Dattilo, V.; Daudert, B.; Davier, M.; Davies, G.; Daw,
E. J.; Day, R.; de Rosa, R.; Debra, D.; Degallaix, J.; Del Prete, M.;
Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar, S.; di Fiore, L.; di
Lieto, A.; di Paolo Emilio, M.; di Virgilio, A.; Díaz, M.; Dietz, A.;
Donovan, F.; Dooley, K. L.; Doomes, E. E.; Drago, M.; Drever, R. W. P.;
Dueck, J.; Duke, I.; Dumas, J. -C.; Dwyer, J. G.; Echols, C.; Edgar,
M.; Effler, A.; Ehrens, P.; Ely, G.; Espinoza, E.; Etzel, T.; Evans,
M.; Evans, T.; Fafone, V.; Fairhurst, S.; Faltas, Y.; Fan, Y.; Fazi,
D.; Fehrmann, H.; Ferrante, I.; Fidecaro, F.; Finn, L. S.; Fiori,
I.; Flaminio, R.; Flasch, K.; Foley, S.; Forrest, C.; Fotopoulos,
N.; Fournier, J. -D.; Franc, J.; Franzen, A.; Frasca, S.; Frasconi,
F.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T.;
Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Gammaitoni, L.;
Garofoli, J. A.; Gennai, A.; Gholami, I.; Giaime, J. A.; Giampanis,
S.; Giardina, K. D.; Giazotto, A.; Goda, K.; Goetz, E.; Goggin,
L. M.; González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty, R.;
Granata, M.; Granata, V.; Grant, A.; Gras, S.; Gray, C.; Gray, M.;
Greenhalgh, R. J. S.; Gretarsson, A. M.; Greverie, C.; Grimaldi,
F.; Grosso, R.; Grote, H.; Grunewald, S.; Guenther, M.; Guidi, G.;
Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer,
D.; Hammond, G. D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G. M.;
Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.; Heefner, J.;
Heitmann, H.; Hello, P.; Heng, I. S.; Heptonstall, A.; Hewitson, M.;
Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.;
Hough, J.; Hoyland, D.; Huet, D.; Hughey, B.; Huttner, S. H.; Ingram,
D. R.; Isogai, T.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Sancho de La Jordana, L.; Ju, L.;
Kalmus, P.; Kalogera, V.; Kandhasamy, S.; Kanner, J.; Kasprzyk, D.;
Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.;
Keppel, D. G.; Khalaidovski, A.; Khalili, F. Y.; Khan, R.; Khazanov,
E.; King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov,
V.; Kopparapu, R.; Koranda, S.; Kozak, D.; Krishnan, B.; Kumar, R.;
Kwee, P.; La Penna, P.; Lam, P. K.; Landry, M.; Lantz, B.; Laval, M.;
Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor, I.; Leroy, N.;
Letendre, N.; Li, C.; Lin, H.; Lindquist, P. E.; Littenberg, T. B.;
Lockerbie, N. A.; Lodhia, D.; Longo, M.; Lorenzini, M.; Loriette,
V.; Lormand, M.; Losurdo, G.; Lu, P.; Lubiński, M.; Lucianetti,
A.; Lück, H.; Machenschalk, B.; Macinnis, M.; Mackowski, J. -M.;
Mageswaran, M.; Mailand, K.; Majorana, E.; Man, N.; Mandel, I.;
Mandic, V.; Mantovani, M.; Marchesoni, F.; Marion, F.; Márka, S.;
Márka, Z.; Markosyan, A.; Markowitz, J.; Maros, E.; Marque, J.;
Martelli, F.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.;
Masserot, A.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala,
N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.;
McIntyre, G.; McKechan, D. J. A.; McKenzie, K.; Mehmet, M.; Melatos,
A.; Melissinos, A. C.; Mendell, G.; Menéndez, D. F.; Menzinger, F.;
Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.; Michel,
C.; Milano, L.; Miller, J.; Minelli, J.; Minenkov, Y.; Mino, Y.;
Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa, O.;
Moe, B.; Mohan, M.; Mohanty, S. D.; Mohapatra, S. R. P.; Moreau, J.;
Moreno, G.; Morgado, N.; Morgia, A.; Morioka, T.; Mors, K.; Mosca,
S.; Mossavi, K.; Mours, B.; Mowlowry, C.; Mueller, G.; Muhammad,
D.; Mühlen, H. Zur; Mukherjee, S.; Mukhopadhyay, H.; Mullavey, A.;
Müller-Ebhardt, H.; Munch, J.; Murray, P. G.; Myers, E.; Myers, J.;
Nash, T.; Nelson, J.; Neri, I.; Newton, G.; Nishizawa, A.; Nocera,
F.; Numata, K.; Ochsner, E.; O'Dell, J.; Ogin, G. H.; O'Reilly, B.;
O'Shaughnessy, R.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen,
B. J.; Pagliaroli, G.; Palomba, C.; Pan, Y.; Pankow, C.; Paoletti,
F.; Papa, M. A.; Parameshwaraiah, V.; Pardi, S.; Pasqualetti, A.;
Passaquieti, R.; Passuello, D.; Patel, P.; Pedraza, M.; Penn, S.;
Perreca, A.; Persichetti, G.; Pichot, M.; Piergiovanni, F.; Pierro, V.;
Pinard, L.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.;
Poggiani, R.; Postiglione, F.; Principe, M.; Prix, R.; Prodi, G. A.;
Prokhorov, L.; Punken, O.; Punturo, M.; Puppo, P.; Van Der Putten,
S.; Quetschke, V.; Raab, F. J.; Rabaste, O.; Rabeling, D. S.; Radkins,
H.; Raffai, P.; Raics, Z.; Rainer, N.; Rakhmanov, M.; Rapagnani, P.;
Raymond, V.; Re, V.; Reed, C. M.; Reed, T.; Regimbau, T.; Rehbein,
H.; Reid, S.; Reitze, D. H.; Ricci, F.; Riesen, R.; Riles, K.;
Rivera, B.; Roberts, P.; Robertson, N. A.; Robinet, F.; Robinson,
C.; Robinson, E. L.; Rocchi, A.; Roddy, S.; Rolland, L.; Rollins,
J.; Romano, J. D.; Romano, R.; Romie, J. H.; Röver, C.; Rowan, S.;
Rüdiger, A.; Ruggi, P.; Russell, P.; Ryan, K.; Sakata, S.; Salemi,
F.; Sandberg, V.; Sannibale, V.; Santamaría, L.; Saraf, S.; Sarin,
P.; Sassolas, B.; Sathyaprakash, B. S.; Sato, S.; Satterthwaite, M.;
Saulson, P. R.; Savage, R.; Savov, P.; Scanlan, M.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schulz, B.; Schutz, B. F.; Schwinberg,
P.; Scott, J.; Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.;
Sellers, D.; Sengupta, A. S.; Sentenac, D.; Sergeev, A.; Shapiro,
B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg,
D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.;
van der Sluys, M. V.; Smith, J. R.; Smith, M. R.; Smith, N. D.;
Somiya, K.; Sorazu, B.; Stein, A.; Stein, L. C.; Steplewski, S.;
Stochino, A.; Stone, R.; Strain, K. A.; Strigin, S.; Stroeer, A.;
Sturani, R.; Stuver, A. L.; Summerscales, T. Z.; Sun, K. -X.; Sung,
M.; Sutton, P. J.; Swinkels, B. L.; Szokoly, G. P.; Talukder, D.;
Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.;
Terenzi, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Tokmakov, K. V.; Toncelli, A.; Tonelli, M.; Torres, C.; Torrie,
C.; Tournefier, E.; Travasso, F.; Traylor, G.; Trias, M.; Trummer,
J.; Ugolini, D.; Ulmen, J.; Urbanek, K.; Vahlbruch, H.; Vajente, G.;
Vallisneri, M.; Vass, S.; Vaulin, R.; Vavoulidis, M.; Vecchio, A.;
Vedovato, G.; van Veggel, A. A.; Veitch, J.; Veitch, P.; Veltkamp,
C.; Verkindt, D.; Vetrano, F.; Viceré, A.; Villar, A.; Vinet,
J. -Y.; Vocca, H.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.;
Wallace, L.; Ward, H.; Ward, R. L.; Was, M.; Weidner, A.; Weinert,
M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wette, K.; Whelan,
J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.;
Williams, H. R.; Williams, L.; Willke, B.; Wilmut, I.; Winkelmann,
L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.;
Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida,
S.; Yvert, M.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov,
N.; Zucker, M. E.; Zweizig, J.; LIGO Collaboration; Virgo Collaboration
Bibcode: 2009Natur.460..990A
Altcode: 2009arXiv0910.5772T
A stochastic background of gravitational waves is expected to arise
from a superposition of a large number of unresolved gravitational-wave
sources of astrophysical and cosmological origin. It should carry unique
signatures from the earliest epochs in the evolution of the Universe,
inaccessible to standard astrophysical observations. Direct measurements
of the amplitude of this background are therefore of fundamental
importance for understanding the evolution of the Universe when it
was younger than one minute. Here we report limits on the amplitude
of the stochastic gravitational-wave background using the data from a
two-year science run of the Laser Interferometer Gravitational-wave
Observatory (LIGO). Our result constrains the energy density of the
stochastic gravitational-wave background normalized by the critical
energy density of the Universe, in the frequency band around 100Hz, to
be <6.9×10-6 at 95% confidence. The data rule out models
of early Universe evolution with relatively large equation-of-state
parameter, as well as cosmic (super)string models with relatively small
string tension that are favoured in some string theory models. This
search for the stochastic background improves on the indirect limits
from Big Bang nucleosynthesis and cosmic microwave background at 100Hz.
Title: Stacked Search for Gravitational Waves from the 2006 SGR
1900+14 Storm
Authors: Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen,
B.; Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain,
M. A.; Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker,
C.; Barker, D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.;
Bartos, I.; Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista,
M.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair,
D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose,
S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Bridges, D. O.;
Brinkmann, M.; Brooks, A. F.; Brown, D. A.; Brummit, A.; Brunet, G.;
Bullington, A.; Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati,
L.; Camp, J. B.; Cannizzo, J.; Cannon, K. C.; Cao, J.; Cardenas,
L.; Caride, S.; Castaldi, G.; Caudill, S.; Cavaglià, M.; Cepeda,
C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Christensen, N.; Chung, C. T. Y.; Clark, D.;
Clark, J.; Clayton, J. H.; Cokelaer, T.; Colacino, C. N.; Conte, R.;
Cook, D.; Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; DeBra, D.; Degallaix, J.; Dergachev, V.;
Desai, S.; DeSalvo, R.; Dhurandhar, S.; Díaz, M.; Dietz, A.; Donovan,
F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Dueck, J.; Duke,
I.; Dumas, J. -C.; Dwyer, J. G.; Echols, C.; Edgar, M.; Effler, A.;
Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst,
S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Finn, L. S.; Flasch,
K.; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen, A.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.;
Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J. A.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty,
R.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grunewald,
S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam,
J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson, J.; Harms, J.;
Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.;
Heefner, J.; Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.;
Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough,
J.; Hoyland, D.; Hughey, B.; Huttner, S. H.; Ingram, D. R.; Isogai,
T.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.; Klimenko, S.;
Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.;
Krishnan, B.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.;
Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor, I.; Li, C.;
Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie, N. A.; Lodhia,
D.; Longo, M.; Lormand, M.; Lu, P.; Lubiński, M.; Lucianetti, A.;
Lück, H.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand,
K.; Mandel, I.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.;
Mason, K.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala,
N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.;
McIntyre, G.; McKechan, D. J. A.; McKenzie, K.; Mehmet, M.; Melatos,
A.; Melissinos, A. C.; Menéndez, D. F.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messenger, C.; Meyer, M. S.; Miller, J.; Minelli,
J.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Moe, B.; Mohanty, S. D.; Mohapatra, S. R. P.; Moreno,
G.; Morioka, T.; Mors, K.; Mossavi, K.; Mow Lowry, C.; Mueller, G.;
Müller-Ebhardt, H.; Muhammad, D.; Mukherjee, S.; Mukhopadhyay, H.;
Mullavey, A.; Munch, J.; Murray, P. G.; Myers, E.; Myers, J.; Nash,
T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell, J.;
O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.; Ogin, G. H.; Ottaway,
D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.;
Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.;
Perreca, A.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Postiglione, F.; Principe, M.; Prix, R.; Prokhorov,
L.; Punken, O.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins,
H.; Raffai, P.; Raics, Z.; Rainer, N.; Rakhmanov, M.; Raymond, V.;
Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen,
R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson, N. A.; Robinson,
C.; Robinson, E. L.; Roddy, S.; Röver, C.; Rollins, J.; Romano,
J. D.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Russell, P.; Ryan, K.;
Sakata, S.; Sancho de la Jordana, L.; Sandberg, V.; Sannibale, V.;
Santamaría, L.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Satterthwaite, M.; Saulson, P. R.; Savage, R.; Savov, P.; Scanlan,
M.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz, B.; Schutz,
B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Sears,
B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shapiro,
B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.;
Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein,
A.; Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain,
K. A.; Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.;
Sun, K. -X.; Sung, M.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.;
Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov,
K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Ugolini,
D.; Ulmen, J.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; van den
Broeck, C.; van der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin,
R.; Vecchio, A.; Veitch, J.; Veitch, P.; Veltkamp, C.; Villar, A.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward,
R. L.; Weidner, A.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen,
L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Wilmut, I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.;
Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin,
I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang,
L.; Zhao, C.; Zotov, N.; Zucker, M. E.; zur Mühlen, H.; Zweizig;
J.; LIGO Scientific Collaboration
Bibcode: 2009ApJ...701L..68A
Altcode: 2009arXiv0905.0005L
We present the results of a LIGO search for short-duration gravitational
waves (GWs) associated with the 2006 March 29 SGR 1900+14 storm. A
new search method is used, "stacking" the GW data around the
times of individual soft-gamma bursts in the storm to enhance
sensitivity for models in which multiple bursts are accompanied by
GW emission. We assume that variation in the time difference between
burst electromagnetic emission and potential burst GW emission is
small relative to the GW signal duration, and we time-align GW excess
power time-frequency tilings containing individual burst triggers to
their corresponding electromagnetic emissions. We use two GW emission
models in our search: a fluence-weighted model and a flat (unweighted)
model for the most electromagnetically energetic bursts. We find
no evidence of GWs associated with either model. Model-dependent
GW strain, isotropic GW emission energy E GW, and γ ≡
E GW/E EM upper limits are estimated using a
variety of assumed waveforms. The stacking method allows us to set
the most stringent model-dependent limits on transient GW strain
published to date. We find E GW upper limit estimates (at
a nominal distance of 10 kpc) of between 2 × 1045 erg and
6 × 1050 erg depending on the waveform type. These limits
are an order of magnitude lower than upper limits published previously
for this storm and overlap with the range of electromagnetic energies
emitted in soft gamma repeater (SGR) giant flares.
Title: Search for gravitational waves from low mass compact binary
coalescence in 186 days of LIGO's fifth science run
Authors: Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen, B.;
Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.;
Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker, C.; Barker,
D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista, M.; Betzwieser,
J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Biswas, R.;
Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.;
Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose, S.; Brady,
P. R.; Braginsky, V. B.; Brau, J. E.; Bridges, D. O.; Brinkmann, M.;
Brooks, A. F.; Brown, D. A.; Brummit, A.; Brunet, G.; Bullington,
A.; Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati, L.; Camp,
J. B.; Cannizzo, J.; Cannon, K. C.; Cao, J.; Capano, C. D.; Cardenas,
L.; Caride, S.; Castaldi, G.; Caudill, S.; Cavaglià, M.; Cepeda,
C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Christensen, N.; Chung, C. T. Y.; Clark, D.;
Clark, J.; Clayton, J. H.; Cokelaer, T.; Colacino, C. N.; Conte, R.;
Cook, D.; Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; Debra, D.; Degallaix, J.; Dergachev, V.;
Desai, S.; Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dietz, A.; Donovan,
F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Dueck, J.; Duke,
I.; Dumas, J. -C.; Dwyer, J. G.; Echols, C.; Edgar, M.; Effler, A.;
Ehrens, P.; Ely, G.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.;
Fairhurst, S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Finn,
L. S.; Flasch, K.; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen,
A.; Frede, M.; Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T.;
Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J. A.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler,
S.; Gouaty, R.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh,
R. J. S.; Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.;
Grunewald, S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage,
B.; Hallam, J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson,
J.; Harms, J.; Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian,
K.; Hayama, K.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken,
D. J.; Hough, J.; Hoyland, D.; Hughey, B.; Huttner, S. H.; Ingram,
D. R.; Isogai, T.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kandhasamy, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski,
A.; Khalili, F. Y.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.;
Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.;
Kozak, D.; Krishnan, B.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.;
Lantz, B.; Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor,
I.; Li, C.; Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie,
N. A.; Lodhia, D.; Longo, M.; Lormand, M.; Lu, P.; Lubiński, M.;
Lucianetti, A.; Lück, H.; Lundgren, A. P.; Machenschalk, B.; Macinnis,
M.; Mageswaran, M.; Mailand, K.; Mandel, I.; Mandic, V.; Márka,
S.; Márka, Z.; Markosyan, A.; Markowitz, J.; Maros, E.; Martin,
I. W.; Martin, R. M.; Marx, J. N.; Mason, K.; Matichard, F.; Matone,
L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.;
McGuire, S. C.; McHugh, M.; McIntyre, G.; McKechan, D. J. A.; McKenzie,
K.; Mehmet, M.; Melatos, A.; Melissinos, A. C.; Menéndez, D. F.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.;
Miller, J.; Minelli, J.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S. D.; Mohapatra,
S. R. P.; Moreno, G.; Morioka, T.; Mors, K.; Mossavi, K.; Mowlowry,
C.; Mueller, G.; Müller-Ebhardt, H.; Muhammad, D.; Mukherjee, S.;
Mukhopadhyay, H.; Mullavey, A.; Munch, J.; Murray, P. G.; Myers, E.;
Myers, J.; Nash, T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata,
K.; O'Dell, J.; O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.; Ogin,
G. H.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan,
Y.; Pankow, C.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza,
M.; Penn, S.; Perraca, A.; Pierro, V.; Pinto, I. M.; Pitkin, M.;
Pletsch, H. J.; Plissi, M. V.; Postiglione, F.; Principe, M.; Prix,
R.; Prokhorov, L.; Punken, O.; Quetschke, V.; Raab, F. J.; Rabeling,
D. S.; Radkins, H.; Raffai, P.; Raics, Z.; Rainer, N.; Rakhmanov, M.;
Raymond, V.; Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze,
D. H.; Riesen, R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson,
N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Röver, C.; Rollins,
J.; Romano, J. D.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Russell,
P.; Ryan, K.; Sakata, S.; Sancho de La Jordana, L.; Sandberg, V.;
Sannibale, V.; Santamaría, L.; Saraf, S.; Sarin, P.; Sathyaprakash,
B. S.; Sato, S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.;
Savov, P.; Scanlan, M.; Schilling, R.; Schnabel, R.; Schofield, R.;
Schulz, B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.;
Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.;
Sergeev, A.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.;
Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.;
Slutsky, J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.;
Sorazu, B.; Stein, A.; Stein, L. C.; Steplewski, S.; Stochino, A.;
Stone, R.; Strain, K. A.; Strigin, S.; Stroeer, A.; Stuver, A. L.;
Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.; Szokoly,
G. P.; Talukder, D.; Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor,
J. R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Ugolini, D.; Ulmen, J.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.;
van den Broeck, C.; van der Sluys, M. V.; van Veggel, A. A.; Vass,
S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P.; Veltkamp, C.;
Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace,
L.; Ward, R. L.; Weidner, A.; Weinert, M.; Weinstein, A. J.; Weiss, R.;
Wen, L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Wilmut, I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.;
Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin,
I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang,
L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2009PhRvD..80d7101A
Altcode: 2009arXiv0905.3710T; 2009arXiv0905.3710L
We report on a search for gravitational waves from coalescing
compact binaries, of total mass between 2 and 35M⊙,
using LIGO observations between November 14, 2006 and May 18,
2007. No gravitational-wave signals were detected. We report upper
limits on the rate of compact binary coalescence as a function of
total mass. The LIGO cumulative 90%-confidence rate upper limits
of the binary coalescence of neutron stars, black holes and black
hole-neutron star systems are 1.4×10-2, 7.3×10-4
and 3.6×10-3yr-1L10-1,
respectively, where L10 is 1010 times the blue
solar luminosity.
Title: LIGO: the Laser Interferometer Gravitational-Wave Observatory
Authors: Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen,
B.; Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain,
M. A.; Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker,
C.; Barker, D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.;
Bartos, I.; Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista,
M.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley,
G.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn, L.; Blair,
D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose,
S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Bridges, D. O.;
Brinkmann, M.; Brooks, A. F.; Brown, D. A.; Brummit, A.; Brunet, G.;
Bullington, A.; Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati,
L.; Camp, J. B.; Cannizzo, J.; Cannon, K. C.; Cao, J.; Cardenas,
L.; Caride, S.; Castaldi, G.; Caudill, S.; Cavaglià, M.; Cepeda,
C.; Chalermsongsak, T.; Chalkley, E.; Charlton, P.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Christensen, N.; Chung, C. T. Y.; Clark, D.;
Clark, J.; Clayton, J. H.; Cokelaer, T.; Colacino, C. N.; Conte, R.;
Cook, D.; Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.;
Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.;
Cumming, A.; Cunningham, L.; Danilishin, S. L.; Danzmann, K.; Daudert,
B.; Davies, G.; Daw, E. J.; DeBra, D.; Degallaix, J.; Dergachev, V.;
Desai, S.; DeSalvo, R.; Dhurandhar, S.; Díaz, M.; Dietz, A.; Donovan,
F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Dueck, J.; Duke,
I.; Dumas, J. -C.; Dwyer, J. G.; Echols, C.; Edgar, M.; Effler, A.;
Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst,
S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fehrmenn, H.; Finn, L. S.; Flasch,
K.; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen, A.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.;
Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J. A.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty,
R.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grunewald,
S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam,
J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson, J.; Harms, J.;
Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.;
Heefner, J.; Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.;
Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough,
J.; Hoyland, D.; Hughey, B.; Huttner, S. H.; Ingram, D. R.; Isogai,
T.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.; Klimenko, S.;
Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.;
Krishnan, B.; Kumar, R.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.;
Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor, I.; Li, C.;
Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie, N. A.; Lodhia,
D.; Longo, M.; Lormand, M.; Lu, P.; Lubiński, M.; Lucianetti, A.;
Lück, H.; Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand,
K.; Mandel, I.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.;
Mason, K.; Matichard, F.; Matone, L.; Matzner, R. A.; Mavalvala,
N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.;
McIntyre, G.; McKechan, D. J. A.; McKenzie, K.; Mehmet, M.; Melatos,
A.; Melissinos, A. C.; Menéndez, D. F.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messenger, C.; Meyer, M. S.; Miller, J.; Minelli,
J.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Moe, B.; Mohanty, S. D.; Mohapatra, S. R. P.; Moreno,
G.; Morioka, T.; Mors, K.; Mossavi, K.; Mow Lowry, C.; Mueller, G.;
Müller-Ebhardt, H.; Muhammad, D.; Mukherjee, S.; Mukhopadhyay, H.;
Mullavey, A.; Munch, J.; Murray, P. G.; Myers, E.; Myers, J.; Nash,
T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell, J.;
O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.; Ogin, G. H.; Ottaway,
D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.;
Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.;
Perraca, A.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.;
Plissi, M. V.; Postiglione, F.; Principe, M.; Prix, R.; Prokhorov,
L.; Punken, O.; Quetschke, V.; Raab, F. J.; Rabeling, D. S.; Radkins,
H.; Raffai, P.; Raics, Z.; Rainer, N.; Rakhmanov, M.; Raymond, V.;
Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen,
R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson, N. A.; Robinson,
C.; Robinson, E. L.; Roddy, S.; Röver, C.; Rollins, J.; Romano,
J. D.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Russell, P.; Ryan, K.;
Sakata, S.; de la Jordana, L. Sancho; Sandberg, V.; Sannibale, V.;
Santamaría, L.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Satterthwaite, M.; Saulson, P. R.; Savage, R.; Savov, P.; Scanlan,
M.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz, B.; Schutz,
B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Sears,
B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shapiro,
B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.;
Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein,
A.; Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.; Strain,
K. A.; Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales, T. Z.;
Sun, K. -X.; Sung, M.; Sutton, P. J.; Szokoly, G. P.; Talukder, D.;
Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thüring, A.; Tokmakov, K. V.; Torres,
C.; Torrie, C.; Traylor, G.; Trias, M.; Ugolini, D.; Ulmen, J.;
Urbanek, K.; Vahlbruch, H.; Vallisneri, M.; van den Broeck, C.; van
der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin, R.; Vecchio,
A.; Veitch, J.; Veitch, P.; Veltkamp, C.; Villar, A.; Vorvick, C.;
Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, R. L.; Weidner,
A.; Weinert, M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut,
I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan,
G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan,
Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov,
N.; Zucker, M. E.; Mühlen, H. zur; Zweizig, J.
Bibcode: 2009RPPh...72g6901A
Altcode: 2007arXiv0711.3041T
The goal of the Laser Interferometric Gravitational-Wave Observatory
(LIGO) is to detect and study gravitational waves (GWs) of
astrophysical origin. Direct detection of GWs holds the promise of
testing general relativity in the strong-field regime, of providing
a new probe of exotic objects such as black holes and neutron stars
and of uncovering unanticipated new astrophysics. LIGO, a joint
Caltech-MIT project supported by the National Science Foundation,
operates three multi-kilometer interferometers at two widely
separated sites in the United States. These detectors are the result
of decades of worldwide technology development, design, construction
and commissioning. They are now operating at their design sensitivity,
and are sensitive to gravitational wave strains smaller than one part
in 1021. With this unprecedented sensitivity, the data
are being analyzed to detect or place limits on GWs from a variety of
potential astrophysical sources.
Title: The H, O isotopic characteristics and mineralization age of
the Baishan molybdenum deposit in Eastern Tianshan
Authors: Zhang, D. Y.; Zhou, T. F.; Yuan, F.; Fan, Y.
Bibcode: 2009GeCAS..73R1503Z
Altcode:
No abstract at ADS
Title: Search for gravitational waves from low mass binary
coalescences in the first year of LIGO's S5 data
Authors: Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen, B.;
Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.;
Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Barker, C.; Barker,
D.; Barr, B.; Barriga, P.; Barsotti, L.; Barton, M. A.; Bartos, I.;
Bassiri, R.; Bastarrika, M.; Behnke, B.; Benacquista, M.; Betzwieser,
J.; Beyersdorf, P. T.; Bilenko, I. A.; Billingsley, G.; Biswas, R.;
Black, E.; Blackburn, J. K.; Blackburn, L.; Blair, D.; Bland, B.;
Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.;
Braginsky, V. B.; Brau, J. E.; Bridges, D. O.; Brinkmann, M.; Brooks,
A. F.; Brown, D. A.; Brummit, A.; Brunet, G.; Bullington, A.; Buonanno,
A.; Burmeister, O.; Byer, R. L.; Cadonati, L.; Camp, J. B.; Cannizzo,
J.; Cannon, K. C.; Cao, J.; Capano, C. D.; Cardenas, L.; Caride, S.;
Castaldi, G.; Caudill, S.; Cavaglià, M.; Cepeda, C.; Chalermsongsak,
T.; Chalkley, E.; Charlton, P.; Chatterji, S.; Chelkowski, S.;
Chen, Y.; Christensen, N.; Chung, C. T. Y.; Clark, D.; Clark, J.;
Clayton, J. H.; Cokelaer, T.; Colacino, C. N.; Conte, R.; Cook, D.;
Corbitt, T. R. C.; Cornish, N.; Coward, D.; Coyne, D. C.; Creighton,
J. D. E.; Creighton, T. D.; Cruise, A. M.; Culter, R. M.; Cumming, A.;
Cunningham, L.; Danilishin, S. L.; Danzmann, K.; Daudert, B.; Davies,
G.; Daw, E. J.; Debra, D.; Degallaix, J.; Dergachev, V.; Desai, S.;
Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dietz, A.; Donovan, F.; Dooley,
K. L.; Doomes, E. E.; Drever, R. W. P.; Dueck, J.; Duke, I.; Dumas,
J. -C.; Dwyer, J. G.; Echols, C.; Edgar, M.; Effler, A.; Ehrens, P.;
Ely, G.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst,
S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fehrmann, H.; Finn, L. S.; Flasch,
K.; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen, A.; Frede, M.;
Frei, M.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.;
Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J. A.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L. M.; González, G.; Gorodetsky, M. L.; Goßler, S.; Gouaty,
R.; Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.;
Gretarsson, A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grunewald,
S.; Guenther, M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam,
J. M.; Hammer, D.; Hammond, G. D.; Hanna, C.; Hanson, J.; Harms, J.;
Harry, G. M.; Harry, I. W.; Harstad, E. D.; Haughian, K.; Hayama, K.;
Heefner, J.; Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild, S.;
Hirose, E.; Hoak, D.; Hodge, K. A.; Holt, K.; Hosken, D. J.; Hough,
J.; Hoyland, D.; Hughey, B.; Huttner, S. H.; Ingram, D. R.; Isogai,
T.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.; Jones, D. I.;
Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kandhasamy,
S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski, A.; Khalili,
F. Y.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.; Klimenko, S.;
Kokeyama, K.; Kondrashov, V.; Kopparapu, R.; Koranda, S.; Kozak, D.;
Krishnan, B.; Kumar, R.; Kwee, P.; Laljani, V.; Lam, P. K.; Landry, M.;
Lantz, B.; Lazzarini, A.; Lei, H.; Lei, M.; Leindecker, N.; Leonor,
I.; Li, C.; Lin, H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie,
N. A.; Lodhia, D.; Longo, M.; Lormand, M.; Lu, P.; Lubiński, M.;
Lucianetti, A.; Lück, H.; Lundgren, A.; Machenschalk, B.; Macinnis,
M.; Mageswaran, M.; Mailand, K.; Mandel, I.; Mandic, V.; Márka,
S.; Márka, Z.; Markosyan, A.; Markowitz, J.; Maros, E.; Martin,
I. W.; Martin, R. M.; Marx, J. N.; Mason, K.; Matichard, F.; Matone,
L.; Matzner, R. A.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.;
McGuire, S. C.; McHugh, M.; McIntyre, G.; McKechan, D. J. A.; McKenzie,
K.; Mehmet, M.; Melatos, A.; Melissinos, A. C.; Menéndez, D. F.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger, C.; Meyer, M. S.;
Miller, J.; Minelli, J.; Mino, Y.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S. D.; Mohapatra,
S. R. P.; Moreno, G.; Morioka, T.; Mors, K.; Mossavi, K.; Mowlowry,
C.; Mueller, G.; Müller-Ebhardt, H.; Muhammad, D.; Mukherjee, S.;
Mukhopadhyay, H.; Mullavey, A.; Munch, J.; Murray, P. G.; Myers, E.;
Myers, J.; Nash, T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata,
K.; O'Dell, J.; O'Reilly, B.; O'Shaughnessy, R.; Ochsner, E.; Ogin,
G. H.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.; Owen, B. J.; Pan,
Y.; Pankow, C.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza,
M.; Penn, S.; Perraca, A.; Pierro, V.; Pinto, I. M.; Pitkin, M.;
Pletsch, H. J.; Plissi, M. V.; Postiglione, F.; Principe, M.; Prix,
R.; Prokhorov, L.; Punken, O.; Quetschke, V.; Raab, F. J.; Rabeling,
D. S.; Radkins, H.; Raffai, P.; Raics, Z.; Rainer, N.; Rakhmanov, M.;
Raymond, V.; Reed, C. M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze,
D. H.; Riesen, R.; Riles, K.; Rivera, B.; Roberts, P.; Robertson,
N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Röver, C.; Rollins,
J.; Romano, J. D.; Romie, J. H.; Rowan, S.; Rüdiger, A.; Russell,
P.; Ryan, K.; Sakata, S.; de La Jordana, L. Sancho; Sandberg, V.;
Sannibale, V.; Santamaría, L.; Saraf, S.; Sarin, P.; Sathyaprakash,
B. S.; Sato, S.; Satterthwaite, M.; Saulson, P. R.; Savage, R.; Savov,
P.; Scanlan, M.; Schilling, R.; Schnabel, R.; Schofield, R.; Schulz,
B.; Schutz, B. F.; Schwinberg, P.; Scott, J.; Scott, S. M.; Searle,
A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev,
A.; Shapiro, B.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens,
X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu,
B.; Stein, A.; Stein, L. C.; Steplewski, S.; Stochino, A.; Stone, R.;
Strain, K. A.; Strigin, S.; Stroeer, A.; Stuver, A. L.; Summerscales,
T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.; Szokoly, G. P.; Talukder,
D.; Tang, L.; Tanner, D. B.; Tarabrin, S. P.; Taylor, J. R.;
Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Ugolini, D.; Ulmen, J.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.;
van den Broeck, C.; van der Sluys, M. V.; van Veggel, A. A.; Vass,
S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P.; Veltkamp, C.;
Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace,
L.; Ward, R. L.; Weidner, A.; Weinert, M.; Weinstein, A. J.; Weiss, R.;
Wen, L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Wilmut, I.; Winkelmann, L.; Winkler, W.; Wipf, C. C.;
Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin,
I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang,
L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2009PhRvD..79l2001A
Altcode: 2009arXiv0901.0302L
We have searched for gravitational waves from coalescing low mass
compact binary systems with a total mass between 2M⊙
and 35M⊙ and a minimum component mass of 1M⊙
using data from the first year of the fifth science run of the three
LIGO detectors, operating at design sensitivity. Depending on the
mass, we are sensitive to coalescences as far as 150 Mpc from the
Earth. No gravitational-wave signals were observed above the expected
background. Assuming a population of compact binary objects with a
Gaussian mass distribution representing binary neutron star systems,
black hole-neutron star binary systems, and binary black hole systems,
we calculate the 90% confidence upper limit on the rate of coalescences
to be 3.9×10-2yr-1L10-1,
1.1×10-2yr-1L10-1,
and 2.5×10-3yr-1L10-1,
respectively, where L10 is 1010 times the blue
solar luminosity. We also set improved upper limits on the rate of
compact binary coalescences per unit blue-light luminosity, as a
function of mass.
Title: Characteristics of hydrothermal alteration in the Shaxi
Porphyry Cu-Au deposit, Anhui Province, China: Paragenesis and
geochemical
Authors: Zhang, L. J.; Zhou, T. F.; Fan, Y.; Yuan, F.
Bibcode: 2009GeCAS..73R1506Z
Altcode:
No abstract at ADS
Title: The Emergence of a Twisted Flux Tube into the Solar Atmosphere:
Sunspot Rotations and the Formation of a Coronal Flux Rope
Authors: Fan, Y.
Bibcode: 2009ApJ...697.1529F
Altcode: 2009arXiv0903.1288F
We present a three-dimensional simulation of the dynamic emergence of a
twisted magnetic flux tube from the top layer of the solar convection
zone into the solar atmosphere and corona. It is found that after a
brief initial stage of flux emergence during which the two polarities
of the bipolar region become separated and the tubes intersecting
the photosphere become vertical, significant rotational motion sets
in within each polarity. The rotational motions of the two polarities
are found to twist up the inner field lines of the emerged fields such
that they change their orientation into an inverse configuration (i.e.,
pointing from the negative polarity to the positive polarity over the
neutral line). As a result, a flux rope with sigmoid-shaped, dipped
core fields forms in the corona, and the center of the flux rope rises
in the corona with increasing velocity as the twisting of the flux rope
footpoints continues. The rotational motion in the two polarities is
a result of propagation of nonlinear torsional Alfvén waves along the
flux tube, which transports significant twist from the tube's interior
portion toward its expanded coronal portion. This is a basic process
whereby twisted flux ropes are developed in the corona with increasing
twist and magnetic energy, leading up to solar eruptions.
Title: The discovery of an independent thallium mineral (TlI) in
the Xiangquan thallium deposit in He county, Anhui Province, China
Authors: Fan, Y.; Zhou, T. F.; Yuan, F.
Bibcode: 2009GeCAS..73Q.352F
Altcode:
No abstract at ADS
Title: A Model of Coronal Streamers with Underlying Flux Ropes
Authors: Cottaar, Michiel; Fan, Y.
Bibcode: 2009SPD....40.3705C
Altcode:
We present global two-dimensional axisymmetric isothermal MHD
simulations of the dynamic evolution of a coronal helmet streamer,
driven at the lower boundary by the emergence of a twisted flux
rope. By varying both the amount of the toroidal magnetic flux as well
as the amount of the detached poloidal flux in the emerged flux rope,
we obtain solutions that either settle to a new steady state of a
stable helmet streamer containing a flux rope, or result in a loss of
equilibrium of the helmet with the underlying flux rope being expelled
in a CME-like eruption. We find that the transition from a stable to
an eruptive end state does not occur at a single critical value of the
total relative magnetic helicity, but depends on the profile of the
underlying flux rope. Cases where the detached flux rope contains a
higher amount of self helicity, i.e. higher internal twist, are found
to become eruptive at a significantly lower total helicity. However,
in all of the cases studied, we find that the transition from a stable
to eruptive end state takes place at a magnetic energy that is very
close to the Aly open field energy. For the eruptive cases, we find
that the eruption is not driven by magnetic reconnections behind the
flux rope, but is a result of a lack of equilibrium between the upwards
directed magnetic pressure and the downwards directed magnetic tension
and the gravitational force. For the stable helmets we do not find
the formation of significant cavities due to the isothermality and
the imposed constant pressure at the lower boundary. However during
the eruptions we clearly see the 3-part structure of a CME.
Title: All-Sky LIGO Search for Periodic Gravitational Waves in the
Early Fifth-Science-Run Data
Authors: Abbott, B. P.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen, B.;
Allen, G.; Amin, R. S.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.;
Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Baker, P.; Ballmer, S.; Bantilan, H.; Barish,
B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barsotti, L.;
Barton, M. A.; Bartos, I.; Bassiri, R.; Bastarrika, M.; Behnke, B.;
Benacquista, M.; Betzwieser, J.; Beyersdorf, P. T.; Bilenko, I. A.;
Billingsley, G.; Biswas, R.; Black, E.; Blackburn, J. K.; Blackburn,
L.; Blair, D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork, R.; Boschi,
V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Brinkmann,
M.; Brooks, A. F.; Brown, D. A.; Brunet, G.; Bullington, A.; Buonanno,
A.; Burmeister, O.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp,
J. B.; Cannizzo, J.; Cannon, K. C.; Cao, J.; Cardenas, L.; Cardoso,
V.; Caride, S.; Casebolt, T.; Castaldi, G.; Caudill, S.; Cavaglià,
M.; Cepeda, C.; Chalkley, E.; Charlton, P.; Chatterji, S.; Chelkowski,
S.; Chen, Y.; Christensen, N.; Clark, D.; Clark, J.; Clayton, J. H.;
Cokelaer, T.; Conte, R.; Cook, D.; Corbitt, T. R. C.; Cornish, N.;
Coyne, D. C.; Creighton, J. D. E.; Creighton, T. D.; Cruise, A. M.;
Cumming, A.; Cunningham, L.; Cutler, R. M.; Danzmann, K.; Daudert,
B.; Davies, G.; Debra, D.; Degallaix, J.; Dergachev, V.; Desai,
S.; Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dickson, J.; Dietz, A.;
Donovan, F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Duke,
I.; Dumas, J. -C.; Dwyer, J.; Echols, C.; Edgar, M.; Effler, A.;
Ehrens, P.; Ely, G.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.;
Fairhurst, S.; Faltas, Y.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn,
L. S.; Flasch, K.; Foley, S.; Forrest, C.; Fotopoulos, N.; Franzen,
A.; Frei, Z.; Freise, A.; Frey, R.; Fricke, T. T.; Fritschel, P.;
Frolov, V. V.; Fyffe, M.; Garofoli, J. A.; Gholami, I.; Giaime, J. A.;
Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.; Goggin, L. M.;
González, G.; Gossler, S.; Gouaty, R.; Grant, A.; Gras, S.; Gray,
C.; Gray, M.; Greenhalgh, R. J. S.; Gretarsson, A. M.; Grimaldi, F.;
Grosso, R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, E. K.;
Gustafson, R.; Hage, B.; Hallam, J. M.; Hanna, C.; Hanson, J.; Harms,
J.; Harry, G. M.; Harstad, E. D.; Haughian, E.; Hayama, K.; Hayler,
T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Hewitson, M.; Hild,
S.; Hirose, E.; Hoak, D.; Holt, K.; Hosken, D.; Hough, J.; Huttner,
S. H.; Ingram, D.; Ito, M.; Ivanov, A.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kamat, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.;
Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalaidovski,
A.; Khalili, F. Ya.; Khan, R.; Khazanov, E.; King, P.; Kissel, J. S.;
Klimenko, S.; Kocsis, B.; Kokeyama, K.; Kondrashov, V.; Kopparapu,
R.; Koranda, S.; Kozak, D.; Kozhevatov, I.; Krishnan, B.; Kwee, P.;
Landry, M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leonor, I.; Li, C.; Lin,
H.; Lindquist, P. E.; Littenberg, T. B.; Lockerbie, N. A.; Lodhia,
D.; Lormand, M.; Lu, P.; Lubiński, M.; Lucianetti, A.; Lück, H.;
Machenschalk, B.; Macinnis, M.; Mageswaran, M.; Mailand, K.; Mandel,
I.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.; Markowitz,
J.; Maros, E.; Martin, I. W.; Martin, R. M.; Marx, J. N.; Mason, K.;
Matichard, F.; Matone, L.; Matzner, R.; Mavalvala, N.; McCarthy,
R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McIntyre, G.;
McKechan, D.; McKenzie, K.; Mehmet, M.; Melissinos, A.; Mendell, G.;
Mercer, R. A.; Meshkov, S.; Messenger, C. J.; Meyers, D.; Miller, A.;
Miller, J.; Minelli, J.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S. D.; Moreno,
G.; Mors, K.; Mossavi, K.; Mowlowry, C.; Mueller, G.; Muhammad, D.;
Mukherjee, S.; Mukhopadhyay, H.; Mullavey, A.; Müller-Ebhardt, H.;
Munch, J.; Murray, P. G.; Myers, E.; Myers, J.; Nash, T.; Nelson,
J.; Newton, G.; Nishizawa, A.; Numata, K.; Ochsner, E.; O'Dell, J.;
Ogin, G.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.; Papa, M. A.;
Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Perraca, A.;
Petrie, T.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.;
Postiglione, F.; Principe, M.; Prix, R.; Quetschke, V.; Raab, F. J.;
Rabeling, D. S.; Radkins, H.; Raffai, P.; Rainer, N.; Rakhmanov, M.;
Ramsunder, M.; Reed, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen,
R.; Riles, K.; Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson,
E. L.; Roddy, S.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J. H.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.;
Sakata, S.; Sancho de La Jordana, L.; Sandberg, V.; Sannibale, V.;
Santamaria, L.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato,
S.; Saulson, P. R.; Savage, R.; Savov, P.; Scanlan, M.; Schediwy,
S. W.; Schilling, R.; Schnabel, R.; Schofield, R.; Schutz, B. F.;
Schwinberg, P.; Scott, J.; Scott, S. M.; Searle, A. C.; Sears, B.;
Seifert, F.; Sellers, D.; Sengupta, A. S.; Sergeev, A.; Shapiro, B.;
Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg, D.;
Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith,
J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.; Stein,
L. C.; Strain, K. A.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.;
Sung, M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Taylor, R.;
Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias,
M.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; van den Broeck, C.; van
der Sluys, M. V.; van Veggel, A. A.; Vass, S.; Vaulin, R.; Vecchio,
A.; Veitch, J. D.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin,
S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R. L.; Weinert,
M.; Weinstein, A. J.; Weiss, R.; Wen, L.; Wen, S.; Wette, K.; Whelan,
J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.;
Williams, H. R.; Williams, L.; Willke, B.; Wilmut, I.; Winkler, W.;
Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.; Wu, W.;
Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Zanolin, M.; Zhang,
J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M. E.; Zur Mühlen, H.;
Zweizig, J.
Bibcode: 2009PhRvL.102k1102A
Altcode: 2008arXiv0810.0283L
We report on an all-sky search with the LIGO detectors for
periodic gravitational waves in the frequency range 50-1100
Hz and with the frequency’s time derivative in the range
-5×10-9-0Hzs-1. Data from the first eight months
of the fifth LIGO science run (S5) have been used in this search,
which is based on a semicoherent method (PowerFlux) of summing strain
power. Observing no evidence of periodic gravitational radiation, we
report 95% confidence-level upper limits on radiation emitted by any
unknown isolated rotating neutron stars within the search range. Strain
limits below 10-24 are obtained over a 200-Hz band, and the
sensitivity improvement over previous searches increases the spatial
volume sampled by an average factor of about 100 over the entire
search band. For a neutron star with nominal equatorial ellipticity
of 10-6, the search is sensitive to distances as great as
500 pc.
Title: Strategies for the control of parametric instability in
advanced gravitational wave detectors
Authors: Ju, L.; Blair, D. G.; Zhao, C.; Gras, S.; Zhang, Z.; Barriga,
P.; Miao, H.; Fan, Y.; Merrill, L.
Bibcode: 2009CQGra..26a5002J
Altcode:
Parametric instabilities have been predicted to occur in all advanced
high optical power gravitational wave detectors. In this paper we
review the problem of parametric instabilities, summarize the latest
findings and assess various schemes proposed for their control. We show
that non-resonant passive damping of test masses reduces parametric
instability but has a noise penalty, and fails to suppress the Q-factor
of many modes. Resonant passive damping is shown to have significant
advantages but requires detailed modeling. An optical feedback mode
suppression interferometer is proposed which is capable of suppressing
all instabilities but requires experimental development.
Title: Einstein@Home search for periodic gravitational waves in LIGO
S4 data
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen, B.;
Allen, G.; Amin, R.; Anderson, D. P.; Anderson, S. B.; Anderson, W. G.;
Arain, M. A.; Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston,
S.; Aufmuth, P.; Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.;
Barish, B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton,
M. A.; Bastarrika, M.; Bayer, K.; Betzwieser, J.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.;
Blackburn, L.; Blair, D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork,
R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Brinkmann, M.; Brooks, A.; Brown, D. A.; Brunet, G.; Bullington, A.;
Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati, L.; Cagnoli, G.;
Camp, J. B.; Cannizzo, J.; Cannon, K.; Cao, J.; Cardenas, L.; Casebolt,
T.; Castaldi, G.; Cepeda, C.; Chalkley, E.; Charlton, P.; Chatterji,
S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Clark, D.; Clark, J.;
Cokelaer, T.; Conte, R.; Cook, D.; Corbitt, T.; Coyne, D.; Creighton,
J. D. E.; Creighton, T. D.; Cumming, A.; Cunningham, L.; Cutler,
R. M.; Dalrymple, J.; Danzmann, K.; Davies, G.; Debra, D.; Degallaix,
J.; Degree, M.; Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar,
S.; Díaz, M.; Dickson, J.; Dietz, A.; Donovan, F.; Dooley, K. L.;
Doomes, E. E.; Drever, R. W. P.; Duke, I.; Dumas, J. -C.; Dupuis,
R. J.; Dwyer, J. G.; Echols, C.; Effler, A.; Ehrens, P.; Ely, G.;
Espinoza, E.; Etzel, T.; Evans, T.; Fairhurst, S.; Fan, Y.; Fazi,
D.; Fehrmann, H.; Fejer, M. M.; Finn, L. S.; Flasch, K.; Fotopoulos,
N.; Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.; Frolov, V. V.;
Fyffe, M.; Garofoli, J.; Gholami, I.; Giaime, J. A.; Giampanis, S.;
Giardina, K. D.; Goda, K.; Goetz, E.; Goggin, L.; González, G.;
Gossler, S.; Gouaty, R.; Grant, A.; Gras, S.; Gray, C.; Gray, M.;
Greenhalgh, R. J. S.; Gretarsson, A. M.; Grimaldi, F.; Grosso, R.;
Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, E. K.; Gustafson,
R.; Hage, B.; Hallam, J. M.; Hammer, D.; Hanna, C.; Hanson, J.; Harms,
J.; Harry, G.; Harstad, E.; Hayama, K.; Hayler, T.; Heefner, J.; Heng,
I. S.; Hennessy, M.; Heptonstall, A.; Hewitson, M.; Hild, S.; Hirose,
E.; Hoak, D.; Hosken, D.; Hough, J.; Huttner, S. H.; Ingram, D.; Ito,
M.; Ivanov, A.; Johnson, B.; Johnson, W. W.; Jones, D. I.; Jones, G.;
Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.; Kamat, S.; Kanner, J.;
Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.;
Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Khan, R.; Khazanov, E.; Kim,
C.; King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov,
V.; Kopparapu, R. K.; Kozak, D.; Kozhevatov, I.; Krishnan, B.; Kwee,
P.; Lam, P. K.; Landry, M.; Lang, M. M.; Lantz, B.; Lazzarini, A.;
Lei, M.; Leindecker, N.; Leonhardt, V.; Leonor, I.; Libbrecht, K.;
Lin, H.; Lindquist, P.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.;
Lu, P.; Lubiński, M.; Lucianetti, A.; Lück, H.; Machenschalk, B.;
Macinnis, M.; Mageswaran, M.; Mailand, K.; Mandic, V.; Márka, S.;
Márka, Z.; Markosyan, A.; Markowitz, J.; Maros, E.; Martin, I.;
Martin, R. M.; Marx, J. N.; Mason, K.; Matichard, F.; Matone, L.;
Matzner, R.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire,
S. C.; McHugh, M.; McIntyre, G.; McIvor, G.; McKechan, D.; McKenzie,
K.; Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.; Meshkov,
S.; Messenger, C. J.; Meyers, D.; Miller, J.; Minelli, J.; Mitra,
S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa,
O.; Moe, B.; Mohanty, S.; Moreno, G.; Mossavi, K.; Mowlowry, C.;
Mueller, G.; Mukherjee, S.; Mukhopadhyay, H.; Müller-Ebhardt, H.;
Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash, T.; Nelson, J.;
Newton, G.; Nishizawa, A.; Numata, K.; O'Dell, J.; Ogin, G.; O'Reilly,
B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens, R. S.; Overmier, H.;
Owen, B. J.; Pan, Y.; Pankow, C.; Papa, M. A.; Parameshwaraiah, V.;
Patel, P.; Pedraza, M.; Penn, S.; Perreca, A.; Petrie, T.; Pinto,
I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.; Postiglione, F.;
Principe, M.; Prix, R.; Quetschke, V.; Raab, F.; Rabeling, D. S.;
Radkins, H.; Rainer, N.; Rakhmanov, M.; Ramsunder, M.; Rehbein, H.;
Reid, S.; Reitze, D. H.; Riesen, R.; Riles, K.; Rivera, B.; Robertson,
N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan,
A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.; Rowan, S.;
Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi,
M.; de La Jordana, L. Sancho; Sandberg, V.; Sannibale, V.; Saraf, S.;
Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R.;
Savov, P.; Schediwy, S. W.; Schilling, R.; Schnabel, R.; Schofield,
R.; Schutz, B. F.; Schwinberg, P.; Scott, S. M.; Searle, A. C.; Sears,
B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Shawhan, P.; Shoemaker,
D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.;
Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Smith,
N. D.; Somiya, K.; Sorazu, B.; Stein, L. C.; Stochino, A.; Stone, R.;
Strain, K. A.; Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun,
K. -X.; Sung, M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Taylor,
R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias,
M.; Tyler, W.; Ugolini, D.; Ulmen, J.; Urbanek, K.; Vahlbruch, H.;
van den Broeck, C.; van der Sluys, M.; Vass, S.; Vaulin, R.; Vecchio,
A.; Veitch, J.; Veitch, P.; Vigeland, S.; Villar, A.; Vorvick, C.;
Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R.;
Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette, K.; Whelan,
J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson,
C.; Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut,
I.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.;
Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida,
S.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker,
M.; Zweizig, J.
Bibcode: 2009PhRvD..79b2001A
Altcode: 2008arXiv0804.1747L
A search for periodic gravitational waves, from sources such as
isolated rapidly spinning neutron stars, was carried out using
510 h of data from the fourth LIGO science run (S4). The search
was for quasimonochromatic waves in the frequency range from 50 to
1500 Hz, with a linear frequency drift f˙ (measured at the solar
system barycenter) in the range -f/τ<f˙<0.1f/τ, where the
minimum spin-down age τ was 1000 yr for signals below 300 Hz and
10 000 yr above 300 Hz. The main computational work of the search
was distributed over approximately 100 000 computers volunteered by
the general public. This large computing power allowed the use of a
relatively long coherent integration time of 30 h, despite the large
parameter space searched. No statistically significant signals were
found. The sensitivity of the search is estimated, along with the
fraction of parameter space that was vetoed because of contamination
by instrumental artifacts. In the 100 to 200 Hz band, more than 90%
of sources with dimensionless gravitational-wave strain amplitude
greater than 10-23 would have been detected.
Title: First joint search for gravitational-wave bursts in LIGO and
GEO 600 data
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen, B.;
Allen, G.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.;
Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.; Aufmuth,
P.; Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bartos,
I.; Bastarrika, M.; Bayer, K.; Betzwieser, J.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn,
K.; Blackburn, L.; Blair, D.; Bland, B.; Bodiya, T. P.; Bogue, L.;
Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.;
Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown, D. A.; Brunet, G.;
Bullington, A.; Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati,
L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cao, J.;
Cardenas, L.; Casebolt, T.; Castaldi, G.; Cepeda, C.; Chalkley, E.;
Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Christensen,
N.; Clark, D.; Clark, J.; Cokelaer, T.; Conte, R.; Cook, D.; Corbitt,
T.; Coyne, D.; Creighton, J. D. E.; Cumming, A.; Cunningham, L.;
Cutler, R. M.; Dalrymple, J.; Danzmann, K.; Davies, G.; DeBra, D.;
Degallaix, J.; Degree, M.; Dergachev, V.; Desai, S.; DeSalvo, R.;
Dhurandhar, S.; Díaz, M.; Dickson, J.; Di Credico, A.; Dietz, A.;
Donovan, F.; Dooley, K. L.; Doomes, E. E.; Drever, R. W. P.; Duke,
I.; Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Echols, C.; Effler,
A.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, T.; Fairhurst, S.;
Fan, Y.; Fazi, D.; Fehrmann, H.; Fejer, M. M.; Finn, L. S.; Flasch,
K.; Fotopoulos, N.; Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.;
Frolov, V. V.; Fyffe, M.; Garofoli, J.; Gholami, I.; Giaime, J. A.;
Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.; Goggin, L.;
González, G.; Gossler, S.; Gouaty, R.; Grant, A.; Gras, S.; Gray,
C.; Gray, M.; Greenhalgh, R. J. S.; Gretarsson, A. M.; Grimaldi,
F.; Grosso, R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson,
E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer, D.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayama, K.; Hayler, T.;
Heefner, J.; Heng, I. S.; Hennessy, M.; Heptonstall, A.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Hughey,
B.; Huttner, S. H.; Ingram, D.; Ito, M.; Ivanov, A.; Johnson, B.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kamat, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis,
E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalili, F. Ya; Khan, R.; Khazanov, E.; Kim, C.; King, P.; Kissel,
J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R. K.;
Kozak, D.; Kozhevatov, I.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry,
M.; Lang, M. M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leindecker, N.;
Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lin, H.; Lindquist, P.;
Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu, P.; Lubiński, M.;
Lucianetti, A.; Lück, H.; Machenschalk, B.; MacInnis, M.; Mageswaran,
M.; Mailand, K.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Martin, I.; Martin, R. M.; Marx, J. N.;
Mason, K.; Matichard, F.; Matone, L.; Matzner, R.; Mavalvala, N.;
McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McIntyre,
G.; McIvor, G.; McKechan, D.; McKenzie, K.; Meier, T.; Melissinos, A.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger, C. J.; Meyers, D.;
Miller, J.; Minelli, J.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S.; Moreno, G.;
Mossavi, K.; Lowry, C. Mow; Mueller, G.; Mukherjee, S.; Mukhopadhyay,
H.; Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.;
Nash, T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell,
J.; Ogin, G.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.; Papa, M. A.;
Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Perreca, A.;
Petrie, T.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.;
Postiglione, F.; Principe, M.; Prix, R.; Quetschke, V.; Raab, F.;
Rabeling, D. S.; Radkins, H.; Rainer, N.; Rakhmanov, M.; Ramsunder,
M.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; Sancho de la Jordana, L.; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S. W.; Schilling,
R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.;
Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens,
X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.;
Stein, L. C.; Stochino, A.; Stone, R.; Strain, K. A.; Strom, D. M.;
Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.;
Takahashi, H.; Tanner, D. B.; Taylor, R.; Taylor, R.; Thacker, J.;
Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tinto, M.; Tokmakov,
K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.;
Ugolini, D.; Ulmen, J.; Urbanek, K.; Vahlbruch, H.; Van Den Broeck,
C.; van der Sluys, M.; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch,
J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman,
S. J.; Wallace, L.; Ward, H.; Ward, R.; Weinert, M.; Weinstein, A.;
Weiss, R.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting,
B. F.; Wilkinson, C.; Willems, P. A.; Williams, H. R.; Williams, L.;
Willke, B.; Wilmut, I.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.;
Woan, G.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto,
H.; Yan, Z.; Yoshida, S.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao,
C.; Zotov, N.; Zucker, M.; Zweizig, J.; LIGO Scientific Collaboration
Bibcode: 2008CQGra..25x5008A
Altcode: 2008arXiv0807.2834L
We present the results of the first joint search for gravitational-wave
bursts by the LIGO and GEO 600 detectors. We search for bursts with
characteristic central frequencies in the band 768 2048 Hz in the
data acquired between 22 February and 23 March, 2005 (fourth LSC
Science Run S4). We discuss the inclusion of the GEO 600 data in the
Waveburst CorrPower pipeline that first searches for coincident excess
power events without taking into account differences in the antenna
responses or strain sensitivities of the various detectors. We compare
the performance of this pipeline to that of the coherent Waveburst
pipeline based on the maximum likelihood statistic. This likelihood
statistic is derived from a coherent sum of the detector data streams
that takes into account the antenna patterns and sensitivities of the
different detectors in the network. We find that the coherent Waveburst
pipeline is sensitive to signals of amplitude 30 50% smaller than the
Waveburst CorrPower pipeline. We perform a search for gravitational-wave
bursts using both pipelines and find no detection candidates in the
S4 data set when all four instruments were operating stably.
Title: Search for Gravitational-Wave Bursts from Soft Gamma Repeaters
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen, B.;
Allen, G.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain, M. A.;
Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.; Aufmuth,
P.; Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bartos,
I.; Bastarrika, M.; Bayer, K.; Betzwieser, J.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.;
Blackburn, L.; Blair, D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork,
R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Brinkmann, M.; Brooks, A.; Brown, D. A.; Brunet, G.; Bullington, A.;
Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati, L.; Cagnoli,
G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cao, J.; Cardenas, L.;
Casebolt, T.; Castaldi, G.; Cepeda, C.; Chalkley, E.; Charlton, P.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Clark, D.;
Clark, J.; Cokelaer, T.; Conte, R.; Cook, D.; Corbitt, T.; Coyne,
D.; Creighton, J. D. E.; Cumming, A.; Cunningham, L.; Cutler, R. M.;
Dalrymple, J.; Danzmann, K.; Davies, G.; Debra, D.; Degallaix, J.;
Degree, M.; Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar, S.;
Díaz, M.; Dickson, J.; Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes,
E. E.; Drever, R. W. P.; Duke, I.; Dumas, J. -C.; Dupuis, R. J.; Dwyer,
J. G.; Echols, C.; Effler, A.; Ehrens, P.; Espinoza, E.; Etzel, T.;
Evans, T.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fehrmann, H.; Fejer,
M. M.; Finn, L. S.; Flasch, K.; Fotopoulos, N.; Freise, A.; Frey, R.;
Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Garofoli, J.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L.; González, G.; Gossler, S.; Gouaty, R.; Grant,
A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.; Gretarsson,
A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grunewald, S.; Guenther,
M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayama,
K.; Hayler, T.; Heefner, J.; Heng, I. S.; Hennessy, M.; Heptonstall,
A.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough,
J.; Huttner, S. H.; Ingram, D.; Ito, M.; Ivanov, A.; Johnson, B.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kamat, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis,
E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalili, F. Ya.; Khan, R.; Khazanov, E.; Kim, C.; King, P.; Kissel,
J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R. K.;
Kozak, D.; Kozhevatov, I.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry,
M.; Lang, M. M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leindecker, N.;
Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lin, H.; Lindquist, P.;
Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu, P.; Lubiński, M.;
Lucianetti, A.; Lück, H.; Machenschalk, B.; Macinnis, M.; Mageswaran,
M.; Mailand, K.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Martin, I.; Martin, R. M.; Marx, J. N.;
Mason, K.; Matichard, F.; Matone, L.; Matzner, R.; Mavalvala, N.;
McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McIntyre,
G.; McIvor, G.; McKechan, D.; McKenzie, K.; Meier, T.; Melissinos, A.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger, C. J.; Meyers, D.;
Miller, J.; Minelli, J.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S.; Moreno, G.;
Mossavi, K.; Mowlowry, C.; Mueller, G.; Mukherjee, S.; Mukhopadhyay,
H.; Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.;
Nash, T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell,
J.; Ogin, G.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.; Papa, M. A.;
Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Perreca, A.;
Petrie, T.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.;
Postiglione, F.; Principe, M.; Prix, R.; Quetschke, V.; Raab, F.;
Rabeling, D. S.; Radkins, H.; Rainer, N.; Rakhmanov, M.; Ramsunder,
M.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; de La Jordana, L. Sancho; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S. W.; Schilling,
R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.;
Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens,
X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.;
Stein, L. C.; Stochino, A.; Stone, R.; Strain, K. A.; Strom, D. M.;
Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.;
Takahashi, H.; Tanner, D. B.; Taylor, R.; Taylor, R.; Thacker, J.;
Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov, K. V.; Torres,
C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.; Ugolini, D.; Ulmen,
J.; Urbanek, K.; Vahlbruch, H.; van den Broeck, C.; van der Sluys,
M.; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar,
A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward,
H.; Ward, R.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut,
I.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.;
Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida,
S.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker,
M.; Zweizig, J.; Barthelmy, S.; Gehrels, N.; Hurley, K. C.; Palmer, D.
Bibcode: 2008PhRvL.101u1102A
Altcode: 2008arXiv0808.2050L
We present a LIGO search for short-duration gravitational waves (GWs)
associated with soft gamma ray repeater (SGR) bursts. This is the first
search sensitive to neutron star f modes, usually considered the most
efficient GW emitting modes. We find no evidence of GWs associated
with any SGR burst in a sample consisting of the 27 Dec. 2004 giant
flare from SGR 1806-20 and 190 lesser events from SGR 1806-20 and SGR
1900+14. The unprecedented sensitivity of the detectors allows us to
set the most stringent limits on transient GW amplitudes published to
date. We find upper limit estimates on the model-dependent isotropic
GW emission energies (at a nominal distance of 10 kpc) between
3×1045 and 9×1052 erg depending on waveform
type, detector antenna factors and noise characteristics at the time
of the burst. These upper limits are within the theoretically predicted
range of some SGR models.
Title: Partially ejected flux ropes: Implications for interplanetary
coronal mass ejections
Authors: Gibson, S. E.; Fan, Y.
Bibcode: 2008JGRA..113.9103G
Altcode:
Connecting interplanetary coronal mass ejections (ICMEs) to their
solar pre-eruption source requires a clear understanding of how that
source may have evolved during eruption. Gibson and Fan (2006a) have
presented a three-dimensional numerical magnetohydrodynamic simulation
of a CME, which showed how, in the course of eruption, a coronal flux
rope may writhe and reconnect both internally and with surrounding
fields in a manner that leads to a partial ejection of only part of
the rope as a CME. In this paper, we will explicitly describe how the
evolution during eruption found in that simulation leads to alterations
of the magnetic connectivity, helicity, orientation, and topology of
the ejected portion of the rope so that it differs significantly from
that of the pre-eruption rope. Moreover, because a significant part of
the magnetic helicity remains behind in the lower portion of the rope
that survives the eruption, the region is likely to experience further
eruptions. These changes would complicate how ICMEs embedded in the
solar wind relate to their solar source. In particular, the location
and evolution of transient coronal holes, topology of magnetic clouds
("tethered spheromak"), and likelihood of interacting ICMEs would
differ significantly from what would be predicted for a CME which did
not undergo writhing and partial ejection during eruption.
Title: Observation of three-mode parametric interactions in long
optical cavities
Authors: Zhao, C.; Ju, L.; Fan, Y.; Gras, S.; Slagmolen, B. J. J.;
Miao, H.; Barriga, P.; Blair, D. G.; Hosken, D. J.; Brooks, A. F.;
Veitch, P. J.; Mudge, D.; Munch, J.
Bibcode: 2008PhRvA..78b3807Z
Altcode: 2008arXiv0801.1150Z
We report the observation of three-mode optoacoustic parametric
interactions of the type predicted to cause parametric instabilities
in a 77-m -long, high-optical-power cavity that uses suspended sapphire
mirrors. Resonant interaction occurs between two distinct optical modes
and an acoustic mode of one mirror when the difference in frequency
between the two optical cavity modes is close to the frequency of the
acoustic mode. Experimental results validate the theory of parametric
instability in high-power optical cavities, and demonstrate tunable
parametric gain ∼10-2 and more than 20dB amplification of
a high-order optical mode power generated by an applied acoustic signal.
Title: Beating the Spin-Down Limit on Gravitational Wave Emission
from the Crab Pulsar
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen,
B.; Allen, G.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M. A.; Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.;
Barish, B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton,
M. A.; Bastarrika, M.; Bayer, K.; Betzwieser, J.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.;
Blackburn, L.; Blair, D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork,
R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Brinkmann, M.; Brooks, A.; Brown, D. A.; Brunet, G.; Bullington, A.;
Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati, L.; Cagnoli,
G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cao, J.; Cardenas, L.;
Casebolt, T.; Castaldi, G.; Cepeda, C.; Chalkley, E.; Charlton, P.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Clark, D.;
Clark, J.; Cokelaer, T.; Conte, R.; Cook, D.; Corbitt, T.; Coyne,
D.; Creighton, J. D. E.; Cumming, A.; Cunningham, L.; Cutler, R. M.;
Dalrymple, J.; Danzmann, K.; Davies, G.; DeBra, D.; Degallaix, J.;
Degree, M.; Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandhar, S.;
Díaz, M.; Dickson, J.; Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes,
E. E.; Drever, R. W. P.; Duke, I.; Dumas, J. -C.; Dupuis, R. J.; Dwyer,
J. G.; Echols, C.; Effler, A.; Ehrens, P.; Espinoza, E.; Etzel, T.;
Evans, T.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fehrmann, H.; Fejer,
M. M.; Finn, L. S.; Flasch, K.; Fotopoulos, N.; Freise, A.; Frey, R.;
Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Garofoli, J.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L.; González, G.; Gossler, S.; Gouaty, R.; Grant,
A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.; Gretarsson,
A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grunewald, S.; Guenther,
M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayama,
K.; Hayler, T.; Heefner, J.; Heng, I. S.; Hennessy, M.; Heptonstall,
A.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough,
J.; Huttner, S. H.; Ingram, D.; Ito, M.; Ivanov, A.; Johnson, B.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kamat, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis,
E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalili, F. Ya.; Khan, R.; Khazanov, E.; Kim, C.; King, P.; Kissel,
J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R. K.;
Kozak, D.; Kozhevatov, I.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry,
M.; Lang, M. M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leindecker,
N.; Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lin, H.; Lindquist,
P.; Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu, P.; Lubinski, M.;
Lucianetti, A.; Lück, H.; Machenschalk, B.; MacInnis, M.; Mageswaran,
M.; Mailand, K.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Martin, I.; Martin, R. M.; Marx, J. N.;
Mason, K.; Matichard, F.; Matone, L.; Matzner, R.; Mavalvala, N.;
McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McIntyre,
G.; McIvor, G.; McKechan, D.; McKenzie, K.; Meier, T.; Melissinos, A.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger, C. J.; Meyers, D.;
Miller, J.; Minelli, J.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S.; Moreno, G.;
Mossavi, K.; MowLowry, C.; Mueller, G.; Mukherjee, S.; Mukhopadhyay,
H.; Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.;
Nash, T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell,
J.; Ogin, G.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.; Papa, M. A.;
Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Perreca, A.;
Petrie, T.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.;
Postiglione, F.; Principe, M.; Prix, R.; Quetschke, V.; Raab, F.;
Rabeling, D. S.; Radkins, H.; Rainer, N.; Rakhmanov, M.; Ramsunder,
M.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; Sancho de la Jordana, L.; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S. W.; Schilling,
R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.;
Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens,
X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.;
Stein, L. C.; Stochino, A.; Stone, R.; Strain, K. A.; Strom, D. M.;
Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.;
Takahashi, H.; Tanner, D. B.; Taylor, R.; Taylor, R.; Thacker, J.;
Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov, K. V.; Torres,
C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.; Ugolini, D.; Ulmen,
J.; Urbanek, K.; Vahlbruch, H.; Van Den Broeck, C.; van der Sluys,
M.; Vass, S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar,
A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward,
H.; Ward, R.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.;
Willems, P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut,
I.; Winkler, W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.;
Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida,
S.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker,
M.; Zweizig, J.; LIGO Scientific Collaboration; Santostasi, G.
Bibcode: 2008ApJ...683L..45A
Altcode: 2008arXiv0805.4758T
We present direct upper limits on gravitational wave emission from the
Crab pulsar using data from the first 9 months of the fifth science run
of the Laser Interferometer Gravitational-wave Observatory (LIGO). These
limits are based on two searches. In the first we assume that the
gravitational wave emission follows the observed radio timing, giving
an upper limit on gravitational wave emission that beats indirect
limits inferred from the spin-down and braking index of the pulsar
and the energetics of the nebula. In the second we allow for a small
mismatch between the gravitational and radio signal frequencies and
interpret our results in the context of two possible gravitational
wave emission mechanisms.
Title: Search of S3 LIGO data for gravitational wave signals from
spinning black hole and neutron star binary inspirals
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.; Bilenko, I. A.;
Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.; Blackburn, L.;
Blair, D.; Bland, B.; Bogenstahl, J.; Bogue, L.; Bork, R.; Boschi, V.;
Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Brinkmann, M.;
Brooks, A.; Brown, D. A.; Bullington, A.; Bunkowski, A.; Buonanno,
A.; Burmeister, O.; Busby, D.; Byer, R. L.; Cadonati, L.; Cagnoli,
G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.; Cao, J.;
Cardenas, L.; Castaldi, G.; Cepeda, C.; Chalkley, E.; Charlton, P.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini, F.; Christensen, N.;
Clark, J.; Cochrane, P.; Cokelaer, T.; Coldwell, R.; Conte, R.; Cook,
D.; Corbitt, T.; Coyne, D.; Creighton, J. D. E.; Croce, R. P.; Crooks,
D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple, J.; D'Ambrosio,
E.; Danzmann, K.; Davies, G.; Debra, D.; Degallaix, J.; Degree, M.;
Demma, T.; Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar, S.;
Díaz, M.; Dickson, J.; di Credico, A.; Diederichs, G.; Dietz, A.;
Doomes, E. E.; Drever, R. W. P.; Dumas, J. -C.; Dupuis, R. J.; Dwyer,
J. G.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.;
Fairhurst, S.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.; Fiumara,
V.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.; Freise, A.; Frey,
R.; Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.;
Garofoli, J.; Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina,
K. D.; Goda, K.; Goetz, E.; Goggin, L. M.; González, G.; Gossler, S.;
Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson,
A. M.; Grosso, R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson,
R.; Hage, B.; Hammer, D.; Hanna, C.; Hanson, J.; Harms, J.; Harry,
G.; Harstad, E.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall,
A.; Heurs, M.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken,
D.; Hough, J.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer,
E.; Ito, M.; Itoh, Y.; Ivanov, A.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera,
V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.;
Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim, C.;
King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov,
V.; Kopparapu, R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.;
Landry, M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leiner, J.; Leonhardt,
V.; Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.; Longo,
M.; Lormand, M.; Lubiński, M.; Lück, H.; Machenschalk, B.; Macinnis,
M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.;
Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason,
K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McWilliams, S.;
Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.; Meshkov, S.;
Messaritaki, E.; Messenger, C. J.; Meyers, D.; Mikhailov, E.; Mitra,
S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa,
O.; Mohanty, S.; Moreno, G.; Mossavi, K.; Mowlowry, C.; Moylan, A.;
Mudge, D.; Mueller, G.; Mukherjee, S.; Müller-Ebhardt, H.; Munch, J.;
Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton, G.; Nishizawa, A.;
Numata, K.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier,
H.; Owen, B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.;
Pedraza, M.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch,
H.; Plissi, M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab,
F.; Rabeling, D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.;
Ramsunder, M.; Ray-Majumder, S.; Re, V.; Rehbein, H.; Reid, S.; Reitze,
D. H.; Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.; Robertson,
N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan,
A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.; Rowan, S.;
Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi,
M.; Sancho de La Jordana, L.; Sandberg, V.; Sannibale, V.; Saraf, S.;
Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage, R.;
Savov, P.; Schediwy, S.; Schilling, R.; Schnabel, R.; Schofield, R.;
Schutz, B. F.; Schwinberg, P.; Scott, S. M.; Searle, A. C.; Sears, B.;
Seifert, F.; Sellers, D.; Sengupta, A. S.; Shawhan, P.; Shoemaker,
D. H.; Sibley, A.; Sidles, J. A.; Siemens, X.; Sigg, D.; Sinha,
S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.;
Smith, M. R.; Somiya, K.; Strain, K. A.; Strom, D. M.; Stuver, A.;
Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.; Takahashi,
H.; Tanner, D. B.; Taylor, R.; Taylor, R.; Thacker, J.; Thorne,
K. A.; Thorne, K. S.; Thüring, A.; Tokmakov, K. V.; Torres, C.;
Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.; Ugolini, D.; Urbanek,
K.; Vahlbruch, H.; Vallisneri, M.; van den Broeck, C.; Varvella, M.;
Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick,
C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward,
R.; Watts, K.; Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.;
Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.;
Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.;
Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods,
D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan,
Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao,
C.; Zotov, N.; Zucker, M.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2008PhRvD..78d2002A
Altcode: 2007arXiv0712.2050T
We report on the methods and results of the first dedicated search
for gravitational waves emitted during the inspiral of compact
binaries with spinning component bodies. We analyze 788 hours
of data collected during the third science run (S3) of the LIGO
detectors. We searched for binary systems using a detection template
family specially designed to capture the effects of the spin-induced
precession of the orbital plane. We present details of the techniques
developed to enable this search for spin-modulated gravitational
waves, highlighting the differences between this and other recent
searches for binaries with nonspinning components. The template bank
we employed was found to yield high matches with our spin-modulated
target waveform for binaries with masses in the asymmetric range
1.0M⊙<m1<3.0M⊙ and
12.0M⊙<m2<20.0M⊙
which is where we would expect the spin of the binary’s
components to have a significant effect. We find that our
search of S3 LIGO data has good sensitivity to binaries in the
Milky Way and to a small fraction of binaries in M31 and M33
with masses in the range 1.0M⊙<m1,
m2<20.0M⊙. No gravitational wave
signals were identified during this search. Assuming a binary
population with spinning components and Gaussian distribution
of masses representing a prototypical neutron star black
hole system with m1≃1.35M⊙ and
m2≃5M⊙, we calculate the 90%-confidence
upper limit on the rate of coalescence of these systems to be
15.9yr-1L10-1, where L10
is 1010 times the blue light luminosity of the Sun.
Title: The Science benefits and preliminary design of the southern
hemisphere gravitational wave detector AIGO
Authors: Blair, D. G.; Barriga, P.; Brooks, A. F.; Charlton, P.;
Coward, D.; Dumas, J. -C.; Fan, Y.; Galloway, D.; Gras, S.; Hosken,
D. J.; Howell, E.; Hughes, S.; Ju, L.; McClelland, D. E.; Melatos,
A.; Miao, H.; Munch, J.; Scott, S. M.; Slagmolen, B. J. J.; Veitch,
P. J.; Wen, L.; Webb, J. K.; Wolley, A.; Yan, Z.; Zhao, C.
Bibcode: 2008JPhCS.122a2001B
Altcode:
The proposed southern hemisphere gravitational wave detector AIGO
increases the projected average baseline of the global array of ground
based gravitational wave detectors by a factor ~4. This allows the
world array to be substantially improved. The orientation of AIGO allows
much better resolution of both wave polarisations. This enables better
distance estimates for inspiral events, allowing unambiguous optical
identification of host galaxies for about 25% of neutron star binary
inspiral events. This can allow Hubble Law estimation without optical
identification of an outburst, and can also allow deep exposure imaging
with electromagnetic telescopes to search for weak afterglows. This
allows independent estimates of cosmological acceleration and dark
energy as well as improved understanding of the physics of neutron
star and black hole coalescences. This paper reviews and summarises the
science benefits of AIGO and presents a preliminary conceptual design.
Title: Implications for the Origin of GRB 070201 from LIGO
Observations
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.; Bilenko, I. A.;
Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.; Blackburn, L.;
Blair, D.; Bland, B.; Bogenstahl, J.; Bogue, L.; Bork, R.; Boschi, V.;
Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Brinkmann, M.;
Brooks, A.; Brown, D. A.; Bullington, A.; Bunkowski, A.; Buonanno,
A.; Burmeister, O.; Busby, D.; Byer, R. L.; Cadonati, L.; Cagnoli,
G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.; Cao, J.;
Cardenas, L.; Castaldi, G.; Cepeda, C.; Chalkley, E.; Charlton, P.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini, F.; Christensen, N.;
Clark, J.; Cochrane, P.; Cokelaer, T.; Coldwell, R.; Conte, R.; Cook,
D.; Corbitt, T.; Coyne, D.; Creighton, J. D. E.; Croce, R. P.; Crooks,
D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple, J.; D'Ambrosio,
E.; Danzmann, K.; Davies, G.; DeBra, D.; Degallaix, J.; Degree, M.;
Demma, T.; Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandhar, S.;
Díaz, M.; Dickson, J.; Di Credico, A.; Diederichs, G.; Dietz, A.;
Doomes, E. E.; Drever, R. W. P.; Dumas, J. -C.; Dupuis, R. J.; Dwyer,
J. G.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.;
Fairhurst, S.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.; Fiumara,
V.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.; Freise, A.; Frey,
R.; Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.;
Garofoli, J.; Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina,
K. D.; Goda, K.; Goetz, E.; Goggin, L. M.; González, G.; Gossler, S.;
Grant, A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson,
A. M.; Grosso, R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson,
R.; Hage, B.; Hammer, D.; Hanna, C.; Hanson, J.; Harms, J.; Harry,
G.; Harstad, E.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall,
A.; Heurs, M.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken,
D.; Hough, J.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer,
E.; Ito, M.; Itoh, Y.; Ivanov, A.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera,
V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.;
Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim, C.;
King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov,
V.; Kopparapu, R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.;
Landry, M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leiner, J.; Leonhardt,
V.; Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.; Longo,
M.; Lormand, M.; Lubinski, M.; Lück, H.; Machenschalk, B.; MacInnis,
M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.;
Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason,
K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McWilliams, S.; Meier,
T.; Melissinos, A.; Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger,
C. J.; Meyers, D.; Mikhailov, E.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Mohanty, S.; Moreno,
G.; Mossavi, K.; MowLowry, C.; Moylan, A.; Mudge, D.; Mueller, G.;
Mukherjee, S.; Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.;
Myers, J.; Nash, T.; Newton, G.; Nishizawa, A.; Numata, K.; O'Reilly,
B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.;
Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.;
Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi,
M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab, F.; Rabeling,
D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Ramsunder,
M.; Ray-Majumder, S.; Re, V.; Rehbein, H.; Reid, S.; Reitze, D. H.;
Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.; Robertson, N. A.;
Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan,
A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.; Rowan, S.;
Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi,
M.; Sancho de la Jordana, L.; Sandberg, V.; Sannibale, V.; Saraf, S.;
Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.; Savage,
R.; Savov, P.; Schediwy, S.; Schilling, R.; Schnabel, R.; Schofield,
R.; Schutz, B. F.; Schwinberg, P.; Scott, S. M.; Searle, A. C.; Sears,
B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Shawhan, P.; Shoemaker,
D. H.; Sibley, A.; Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.;
Slagmolen, B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya,
K.; Strain, K. A.; Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun,
K. -X.; Sung, M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Taylor,
R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Tyler, W.; Ugolini, D.; Urbanek, K.; Vahlbruch, H.; Vallisneri, M.;
Van Den Broeck, C.; Varvella, M.; Vass, S.; Vecchio, A.; Veitch, J.;
Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.;
Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Weidner, A.; Weinert, M.;
Weinstein, A.; Weiss, R.; Wen, S.; Wette, K.; Whelan, J. T.; Whitcomb,
S. E.; Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.;
Willke, B.; Wilmut, I.; Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman,
A. G.; Woan, G.; Woods, D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin,
I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes, N.; Zanolin, M.;
Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M.; zur Mühlen,
H.; Zweizig, J.; LIGO Scientific Collaboration; Hurley, K. C.
Bibcode: 2008ApJ...681.1419A
Altcode: 2007arXiv0711.1163A; 2007arXiv0711.1163L
We analyzed the available LIGO data coincident with GRB
070201, a short-duration, hard-spectrum γ-ray burst (GRB) whose
electromagnetically determined sky position is coincident with the
spiral arms of the Andromeda galaxy (M31). Possible progenitors of
such short, hard GRBs include mergers of neutron stars or a neutron
star and a black hole, or soft γ-ray repeater (SGR) flares. These
events can be accompanied by gravitational-wave emission. No plausible
gravitational-wave candidates were found within a 180 s long window
around the time of GRB 070201. This result implies that a compact binary
progenitor of GRB 070201, with masses in the range 1 M⊙
< m1 < 3 M⊙ and 1 M⊙ <
m2 < 40 M⊙, located in M31 is excluded at
>99% confidence. If the GRB 070201 progenitor was not in M31, then
we can exclude a binary neutron star merger progenitor with distance
D < 3.5 Mpc, assuming random inclination, at 90% confidence. The
result also implies that an unmodeled gravitational-wave burst from
GRB 070201 most probably emitted less than 4.4 × 10-4
M⊙c2 (7.9 × 1050 ergs) in any 100
ms long period within the signal region if the source was in M31 and
radiated isotropically at the same frequency as LIGO's peak sensitivity
(f ≈ 150 Hz). This upper limit does not exclude current models of
SGRs at the M31 distance.
Title: Genesis of the native copper mineralisation in Eastern Tianshan
Authors: Yuan, F.; Zhou, T. F.; Zhang, D. Y.; Fan, Y.
Bibcode: 2008GeCAS..72Q1066Y
Altcode:
No abstract at ADS
Title: Multitypes of ore-forming fluid systems in the Mesozoic
polymetallic middle and lower reaches of the Yangtze River area
mineralization belt, china
Authors: Zhou, T. F.; Yuan, F.; Fan, Y.; Cooke, D.; Zhao, G.
Bibcode: 2008GeCAS..72R1100Z
Altcode:
No abstract at ADS
Title: Geochemical characteristics of Longqiao iron deposit, Anhui,
China
Authors: Zhang, Le Jun; Zhou, T. F.; Yuan, F.; Fan, Y.; Duan, C.
Bibcode: 2008GeCAS..72R1085Z
Altcode:
No abstract at ADS
Title: Characteristics and zircon La-ICP MS U-Pb ages of the A-type
intrusive rocks in Zongyang county, Anhui Province, East China
Authors: Fan, Y.; Zhou, T. F.; Yuan, F.; Cooke, D.
Bibcode: 2008GeCAS..72R.253F
Altcode:
No abstract at ADS
Title: Astrophysically triggered searches for gravitational waves:
status and prospects
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Ajith, P.; Allen,
B.; Allen, G.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M. A.; Araya, M.; Armandula, H.; Armor, P.; Aso, Y.; Aston, S.;
Aufmuth, P.; Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.;
Barish, B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton,
M. A.; Bastarrika, M.; Bayer, K.; Betzwieser, J.; Beyersdorf, P. T.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.;
Blackburn, L.; Blair, D.; Bland, B.; Bodiya, T. P.; Bogue, L.; Bork,
R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Brinkmann, M.; Brooks, A.; Brown, D. A.; Brunet, G.; Bullington, A.;
Buonanno, A.; Burmeister, O.; Byer, R. L.; Cadonati, L.; Cagnoli,
G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cao, J.; Cardenas, L.;
Casebolt, T.; Castaldi, G.; Cepeda, C.; Chalkley, E.; Charlton, P.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Christensen, N.; Clark, D.;
Clark, J.; Cokelaer, T.; Conte, R.; Cook, D.; Corbitt, T.; Coyne,
D.; Creighton, J. D. E.; Cumming, A.; Cunningham, L.; Cutler, R. M.;
Dalrymple, J.; Danzmann, K.; Davies, G.; DeBra, D.; Degallaix, J.;
Degree, M.; Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandhar, S.;
Díaz, M.; Dickson, J.; Dietz, A.; Donovan, F.; Dooley, K. L.; Doomes,
E. E.; Drever, R. W. P.; Duke, I.; Dumas, J. -C.; Dupuis, R. J.; Dwyer,
J. G.; Echols, C.; Effler, A.; Ehrens, P.; Espinoza, E.; Etzel, T.;
Evans, T.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fehrmann, H.; Fejer,
M. M.; Finn, L. S.; Flasch, K.; Fotopoulos, N.; Freise, A.; Frey, R.;
Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.; Garofoli, J.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L.; González, G.; Gossler, S.; Gouaty, R.; Grant,
A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, R. J. S.; Gretarsson,
A. M.; Grimaldi, F.; Grosso, R.; Grote, H.; Grunewald, S.; Guenther,
M.; Gustafson, E. K.; Gustafson, R.; Hage, B.; Hallam, J. M.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayama,
K.; Hayler, T.; Heefner, J.; Heng, I. S.; Hennessy, M.; Heptonstall,
A.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough,
J.; Huttner, S. H.; Ingram, D.; Ito, M.; Ivanov, A.; Johnson, B.;
Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus,
P.; Kalogera, V.; Kamat, S.; Kanner, J.; Kasprzyk, D.; Katsavounidis,
E.; Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.;
Khalili, F. Ya; Khan, R.; Khazanov, E.; Kim, C.; King, P.; Kissel,
J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu, R. K.;
Kozak, D.; Kozhevatov, I.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry,
M.; Lang, M. M.; Lantz, B.; Lazzarini, A.; Lei, M.; Leindecker, N.;
Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lin, H.; Lindquist, P.;
Lockerbie, N. A.; Lodhia, D.; Lormand, M.; Lu, P.; Lubiński, M.;
Lucianetti, A.; Lück, H.; Machenschalk, B.; MacInnis, M.; Mageswaran,
M.; Mailand, K.; Mandic, V.; Márka, S.; Márka, Z.; Markosyan, A.;
Markowitz, J.; Maros, E.; Martin, I.; Martin, R. M.; Marx, J. N.;
Mason, K.; Matichard, F.; Matone, L.; Matzner, R.; Mavalvala, N.;
McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McIntyre,
G.; McIvor, G.; McKechan, D.; McKenzie, K.; Meier, T.; Melissinos, A.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messenger, C. J.; Meyers, D.;
Miller, J.; Minelli, J.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Miyakawa, O.; Moe, B.; Mohanty, S.; Moreno, G.;
Mossavi, K.; Lowry, C. Mow; Mueller, G.; Mukherjee, S.; Mukhopadhyay,
H.; Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.;
Nash, T.; Nelson, J.; Newton, G.; Nishizawa, A.; Numata, K.; O'Dell,
J.; Ogin, G.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Ottens,
R. S.; Overmier, H.; Owen, B. J.; Pan, Y.; Pankow, C.; Papa, M. A.;
Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Perreca, A.;
Petrie, T.; Pinto, I. M.; Pitkin, M.; Pletsch, H. J.; Plissi, M. V.;
Postiglione, F.; Principe, M.; Prix, R.; Quetschke, V.; Raab, F.;
Rabeling, D. S.; Radkins, H.; Rainer, N.; Rakhmanov, M.; Ramsunder,
M.; Rehbein, H.; Reid, S.; Reitze, D. H.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; Sancho de la Jordana, L.; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S. W.; Schilling,
R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.;
Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens,
X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Smith, N. D.; Somiya, K.; Sorazu, B.;
Stein, L. C.; Stochino, A.; Stone, R.; Strain, K. A.; Strom, D. M.;
Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.;
Takahashi, H.; Tanner, D. B.; Taylor, R.; Taylor, R.; Thacker, J.;
Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov, K. V.; Torres,
C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.; Ugolini, D.; Ulmen,
J.; Urbanek, K.; Vahlbruch, H.; Van Den Broeck, C.; van der Sluys, M.;
Vass, S.; Vaulin, R.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar, A.;
Vorvick, C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.;
Ward, R.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette, K.;
Whelan, J. T.; Whitcomb, S. E.; Whiting, B. F.; Wilkinson, C.; Willems,
P. A.; Williams, H. R.; Williams, L.; Willke, B.; Wilmut, I.; Winkler,
W.; Wipf, C. C.; Wiseman, A. G.; Woan, G.; Wooley, R.; Worden, J.;
Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Zanolin,
M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker, M.; Zweizig,
J.; LIGO Scientific Collaboration; Acernese, F.; Alshourbagy, M.;
Amico, P.; Antonucci, F.; Aoudia, S.; Astone, P.; Avino, S.; Baggio,
L.; Ballardin, G.; Barone, F.; Barsotti, L.; Barsuglia, M.; Bauer, Th
S.; Bigotta, S.; Birindelli, S.; Bizouard, M. A.; Boccara, C.; Bondu,
F.; Bosi, L.; Braccini, S.; Bradaschia, C.; Brillet, A.; Brisson, V.;
Buskulic, D.; Cagnoli, G.; Calloni, E.; Campagna, E.; Carbognani, F.;
Cavalier, F.; Cavalieri, R.; Cella, G.; Cesarini, E.; Chassande-Mottin,
E.; Clapson, A. -C.; Cleva, F.; Coccia, E.; Corda, C.; Corsi, A.;
Cottone, F.; Coulon, J. -P.; Cuoco, E.; D'Antonio, S.; Dari, A.;
Dattilo, V.; Davier, M.; De Rosa, R.; DelPrete, M.; Di Fiore, L.; Di
Lieto, A.; Emilio, M. Di Paolo; Di Virgilio, A.; Evans, M.; Fafone,
V.; Ferrante, I.; Fidecaro, F.; Fiori, I.; Flaminio, R.; Fournier,
J. -D.; Frasca, S.; Frasconi, F.; Gammaitoni, L.; Garufi, F.; Genin,
E.; Gennai, A.; Giazotto, A.; Giordano, L.; Granata, V.; Greverie,
C.; Grosjean, D.; Guidi, G.; Hamdani, S.; Hebri, S.; Heitmann, H.;
Hello, P.; Huet, D.; Kreckelbergh, S.; La Penna, P.; Laval, M.;
Leroy, N.; Letendre, N.; Lopez, B.; Lorenzini, M.; Loriette, V.;
Losurdo, G.; Mackowski, J. -M.; Majorana, E.; Man, C. N.; Mantovani,
M.; Marchesoni, F.; Marion, F.; Marque, J.; Martelli, F.; Masserot,
A.; Menzinger, F.; Milano, L.; Minenkov, Y.; Moins, C.; Moreau, J.;
Morgado, N.; Mosca, S.; Mours, B.; Neri, I.; Nocera, F.; Pagliaroli,
G.; Palomba, C.; Paoletti, F.; Pardi, S.; Pasqualetti, A.; Passaquieti,
R.; Passuello, D.; Piergiovanni, F.; Pinard, L.; Poggiani, R.; Punturo,
M.; Puppo, P.; Rapagnani, P.; Regimbau, T.; Remillieux, A.; Ricci,
F.; Ricciardi, I.; Rocchi, A.; Rolland, L.; Romano, R.; Ruggi, P.;
Russo, G.; Solimeno, S.; Spallicci, A.; Swinkels, B. L.; Tarallo, M.;
Terenzi, R.; Toncelli, A.; Tonelli, M.; Tournefier, E.; Travasso, F.;
Vajente, G.; van den Brand, J. F. J.; van der Putten, S.; Verkindt,
D.; Vetrano, F.; Viceré, A.; Vinet, J. -Y.; Vocca, H.; Yvert, M.;
Virgo Collaboration
Bibcode: 2008CQGra..25k4051A
Altcode: 2008arXiv0802.4320T
In gravitational-wave detection, special emphasis is put onto searches
that focus on cosmic events detected by other types of astrophysical
observatories. The astrophysical triggers, e.g. from γ-ray and x-ray
satellites, optical telescopes and neutrino observatories, provide a
trigger time for analyzing gravitational-wave data coincident with the
event. In certain cases the expected frequency range, source energetics,
directional and progenitor information are also available. Beyond
allowing the recognition of gravitational waveforms with amplitudes
closer to the noise floor of the detector, these triggered searches
should also lead to rich science results even before the onset of
Advanced LIGO. In this paper we provide a broad review of LIGO's
astrophysically triggered searches and the sources they target.
Title: Forming tori: Implications and possible origins of a "tethered
spheromak" topology for magnetic clouds
Authors: Gibson, S. E.; Fan, Y.
Bibcode: 2008AGUSMSH31C..06G
Altcode:
We present a "tethered spheromak" model for magnetic clouds. The
proposed topology differs from previous magnetic cloud models invoking
spheromaks in that large portions of the field remain connected to
the sun. This magnetic configuration may explain observed departures
from the standard magnetic cloud model of a cylindrically-symmetric
magnetic flux rope, such as magnetic fields which rotate more than 180
degrees. It is also topologically complex enough to include intermingled
detached, doubly attached, and apparently open fields in a manner
consistent with observations of sporadic heat flux dropouts within
otherwise bidirectional or unidirectional streaming electrons. We use
a numerical simulation to demonstrate how, for solar eruptions where
the kink instability drives significant rotation of an erupting flux
rope, such a tethered spheromak may form during that rope's partial
ejection. It does so because writhing motions and reconnections create
twist about two distinct axes of rotation: the first associated with
the rotated portion of the original rope axis, and the second formed
in situ via reconnections between the erupting rope and surrounding
coronal arcade fields.
Title: A joint search for gravitational wave bursts with AURIGA
and LIGO
Authors: Baggio, L.; Bignotto, M.; Bonaldi, M.; Cerdonio, M.; De Rosa,
M.; Falferi, P.; Fattori, S.; Fortini, P.; Giusfredi, G.; Inguscio, M.;
Liguori, N.; Longo, S.; Marin, F.; Mezzena, R.; Mion, A.; Ortolan, A.;
Poggi, S.; Prodi, G. A.; Re, V.; Salemi, F.; Soranzo, G.; Taffarello,
L.; Vedovato, G.; Vinante, A.; Vitale, S.; Zendri, J. P.; Abbott, B.;
Abbott, R.; Adhikari, R.; Agresti, J.; Ajith, P.; Allen, B.; Amin, R.;
Anderson, S. B.; Anderson, W. G.; Arain, M.; Araya, M.; Armandula, H.;
Ashley, M.; Aston, S.; Aufmuth, P.; Aulbert, C.; Babak, S.; Ballmer,
S.; Bantilan, H.; Barish, B. C.; Barker, C.; Barker, D.; Barr, B.;
Barriga, P.; Barton, M. A.; Bayer, K.; Belczynski, K.; Betzwieser,
J.; Beyersdorf, P. T.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.;
Biswas, R.; Black, E.; Blackburn, K.; Blackburn, L.; Blair, D.; Bland,
B.; Bogenstahl, J.; Bogue, L.; Bork, R.; Boschi, V.; Bose, S.; Brady,
P. R.; Braginsky, V. B.; Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown,
D. A.; Bullington, A.; Bunkowski, A.; Buonanno, A.; Burmeister, O.;
Busby, D.; Butler, W. E.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp,
J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas,
L.; Carter, K.; Casey, M. M.; Castaldi, G.; Cepeda, C.; Chalkley, E.;
Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini, F.;
Chin, D.; Chin, E.; Chow, J.; Christensen, N.; Clark, J.; Cochrane,
P.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.; Conte, R.; Cook, D.;
Corbitt, T.; Coward, D.; Coyne, D.; Creighton, J. D. E.; Creighton,
T. D.; Croce, R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.;
Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; DeBra, D.;
Degallaix, J.; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.;
DeSalvo, R.; Dhurandhar, S.; Díaz, M.; Dickson, J.; Di Credico,
A.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.;
Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza,
E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan, Y.; Fazi,
D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos, N.; Franzen,
A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.;
Frolov, V. V.; Fyffe, M.; Galdi, V.; Ganezer, K. S.; Garofoli, J.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L. M.; González, G.; Gossler, S.; Grant, A.; Gras,
S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso,
R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.;
Hammer, D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad,
E.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.;
Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.;
Howell, E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.;
Ito, M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson,
W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.;
Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya; Kim, C.;
King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov,
V.; Kopparapu, R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.;
Landry, M.; Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leiner, J.;
Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie,
N. A.; Longo, M.; Lormand, M.; Lubiński, M.; Lück, H.; Machenschalk,
B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.;
Marano, S.; Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx,
J. N.; Mason, K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.;
McClelland, D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McNabb,
J. W. C.; McWilliams, S.; Meier, T.; Melissinos, A.; Mendell, G.;
Mercer, R. A.; Meshkov, S.; Messenger, C. J.; Meyers, D.; Mikhailov,
E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi, K.; Lowry, C. Mow;
Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.; Müller-Ebhardt,
H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton, G.;
Nishizawa, A.; Nocera, F.; Numata, K.; O'Reilly, B.; O'Shaughnessy,
R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.;
Parameshwaraiah, V.; Parameswariah, C.; Patel, P.; Pedraza, M.;
Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi,
M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab, F.; Rabeling,
D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Ramsunder,
M.; Rawlins, K.; Ray-Majumder, S.; Regimbau, T.; Rehbein, H.; Reid,
S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.;
Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez,
A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.;
Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.;
Samidi, M.; Sancho de la Jordana, L.; Sandberg, V.; Sanders, G. H.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Sazonov, A.; Schediwy, S.;
Schilling, R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg,
P.; Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens,
X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky,
J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.; Strom,
D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton,
P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor, R.; Taylor,
R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tinto,
M.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; Van Den Broeck, C.; van Putten, M.; Varvella, M.;
Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick,
C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward,
R.; Watts, K.; Webber, D.; Weidner, A.; Weinert, M.; Weinstein, A.;
Weiss, R.; Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck, D. M.;
Whitcomb, S. E.; Whiting, B. F.; Wiley, S.; Wilkinson, C.; Willems,
P. A.; Williams, L.; Willke, B.; Wilmut, I.; Winkler, W.; Wipf, C. C.;
Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.; Wooley, R.; Worden,
J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes,
N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker,
M.; zur Mühlen, H.; Zweizig, J.
Bibcode: 2008CQGra..25i5004B
Altcode: 2007arXiv0710.0497A
The first simultaneous operation of the AURIGA detectorhttp://www.auriga.lnl.infn.it
and the LIGO observatoryhttp://www.ligo.org was an opportunity
to explore real data, joint analysis methods between two very
different types of gravitational wave detectors: resonant bars and
interferometers. This paper describes a coincident gravitational
wave burst search, where data from the LIGO interferometers are
cross-correlated at the time of AURIGA candidate events to identify
coincident transients. The analysis pipeline is tuned with two
thresholds, on the signal-to-noise ratio of AURIGA candidate events and
on the significance of the cross-correlation test in LIGO. The false
alarm rate is estimated by introducing time shifts between data sets
and the network detection efficiency is measured by adding simulated
gravitational wave signals to the detector output. The simulated
waveforms have a significant fraction of power in the narrower AURIGA
band. In the absence of a detection, we discuss how to set an upper
limit on the rate of gravitational waves and to interpret it according
to different source models. Due to the short amount of analyzed data
and to the high rate of non-Gaussian transients in the detectors' noise
at the time, the relevance of this study is methodological: this was
the first joint search for gravitational wave bursts among detectors
with such different spectral sensitivity and the first opportunity
for the resonant and interferometric communities to unify languages
and techniques in the pursuit of their common goal.
Title: Observing the unobservable? Modeling coronal cavity densities
Authors: Fuller, J.; Gibson, S. E.; Detoma, G.; Fan, Y.
Bibcode: 2008AGUSMSP51A..04F
Altcode:
Prominence cavities in coronal helmet streamers are readily detectable
in white light coronagraph images, yet their interpretation may be
complicated by projection effects. In order to determine a cavity's
density structure, it is essential to quantify the contribution of
non-cavity features along the line of sight. We model the coronal cavity
as an axisymmetric torus that encircles the Sun at constant latitude,
and fit it to observations of a white light cavity observed by the
Mauna Loa Solar Observatory (MLSO) MK4 coronagraph from January 25-30,
2006. We demonstrate that spurious non-cavity contributions (including
departures from axisymmetry) are minimal enough to be incorporated in
a density analysis as conservatively estimated uncertainties in the
data. We calculate a radial density profile for cavity material and for
the surrounding helmet streamer (which we refer to as the "cavity rim"),
and find that the cavity density is depleted by a maximum of 40 percent
compared to the surrounding helmet streamer at low altitudes (1.18 solar
radii), but is consistently higher (double or more) than in coronal
holes. We also find that the relative density depletion between cavity
and surrounding helmet decreases as a function of height. We show that
both increased temperature in the cavity relative to the surrounding
helmet streamer and a magnetic flux rope configuration might lead to
such a flattened density profile. Finally, our model provides general
observational guidelines that can be used to determine when a cavity is
sufficiently unobstructed to be a good candidate for plasma diagnostics.
Title: Observing the Unobservable? Modeling Coronal Cavity Densities
Authors: Fuller, J.; Gibson, S. E.; de Toma, G.; Fan, Y.
Bibcode: 2008ApJ...678..515F
Altcode:
Prominence cavities in coronal helmet streamers are readily detectable
in white-light coronagraph images, yet their interpretation may be
complicated by projection effects. In order to determine a cavity's
density structure, it is essential to quantify the contribution of
noncavity features along the line of sight. We model the coronal cavity
as an axisymmetric torus that encircles the Sun at constant latitude and
fit it to observations of a white-light cavity observed by the Mauna
Loa Solar Observatory (MLSO) MK4 coronagraph from 2006 January 25 to
30. We demonstrate that spurious noncavity contributions (including
departures from axisymmetry) are minimal enough to be incorporated in
a density analysis as conservatively estimated uncertainties in the
data. We calculate a radial density profile for cavity material and
for the surrounding helmet streamer (which we refer to as the "cavity
rim") and find that the cavity density is depleted by a maximum of 40%
compared to the surrounding helmet streamer at low altitudes (1.18
R⊙) but is consistently higher (double or more) than in
coronal holes. We also find that the relative density depletion between
cavity and surrounding helmet decreases as a function of height. We
show that both increased temperature in the cavity relative to the
surrounding helmet streamer and a magnetic flux rope configuration
might lead to such a flattened density profile. Finally, our model
provides general observational guidelines that can be used to determine
when a cavity is sufficiently unobstructed to be a good candidate for
plasma diagnostics.
Title: Publisher's Note: First cross-correlation analysis of
interferometric and resonant-bar gravitational-wave data for
stochastic backgrounds [Phys. Rev. D 76, 022001 (2007)]
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn,
K.; Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue,
L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.;
Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington,
A.; Bunkowski, A.; Buonanno, A.; Burgamy, M.; Burmeister, O.; Busby,
D.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo,
J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas, L.; Casey, M. M.;
Castaldi, G.; Cepeda, C.; Chalkey, E.; Charlton, P.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Chiadini, F.; Chin, D.; Chin, E.; Chow, J.;
Christensen, N.; Clark, J.; Cochrane, P.; Cokelaer, T.; Colacino,
C. N.; Coldwell, R.; Conte, R.; Cook, D.; Corbitt, T.; Coward, D.;
Coyne, D.; Creighton, J. D. E.; Creighton, T. D.; Croce, R. P.; Crooks,
D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple, J.; D'Ambrosio, E.;
Danzmann, K.; Davies, G.; Debra, D.; Degallaix, J.; Degree, M.; Demma,
T.; Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar, S.; Diaz, M.;
Dickson, J.; di Credico, A.; Diederichs, G.; Dietz, A.; Doomes, E. E.;
Drever, R. W. P.; Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens,
P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan,
Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos,
N.; Franzen, A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.;
Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L.; Gonzalez, G.; Gossler, S.; Grant, A.; Gras,
S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso,
R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.;
Hamilton, W. O.; Hammer, D.; Hanna, C.; Hanson, J.; Harms, J.; Harry,
G.; Harstad, E.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall,
A.; Heurs, M.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken,
D.; Hough, J.; Howell, E.; Hoyland, D.; Huttner, S. H.; Ingram, D.;
Innerhofer, E.; Ito, M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson,
B.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.;
Kalmus, P.; Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili,
F. Ya.; Kim, C.; King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.;
Kondrashov, V.; Kopparapu, R. K.; Kozak, D.; Krishnan, B.; Kwee, P.;
Lam, P. K.; Landry, M.; Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.;
Leiner, J.; Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lindquist, P.;
Lockerbie, N. A.; Longo, M.; Lormand, M.; Lubiński, M.; Luck, H.;
Machenschalk, B.; Macinnis, M.; Mageswaran, M.; Mailand, K.; Malec,
M.; Mandic, V.; Marano, S.; Marka, S.; Markowitz, J.; Maros, E.;
Martin, I.; Marx, J. N.; Mason, K.; Matone, L.; Matta, V.; Mavalvala,
N.; McCarthy, R.; McCaulley, B. J.; McClelland, D. E.; McGuire, S. C.;
McHugh, M.; McKenzie, K.; McNabb, J. W. C.; McWilliams, S.; Meier, T.;
Melissinos, A.; Mendell, G.; Mercer, R. A.; Meshkov, S.; Messaritaki,
E.; Messenger, C. J.; Meyers, D.; Mikhailov, E.; Miller, P.; Mitra,
S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa,
O.; Mohanty, S.; Moody, V.; Moreno, G.; Mossavi, K.; Mowlowry, C.;
Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.; Muller-Ebhardt,
H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton,
G.; Nishizawa, A.; Numata, K.; O'Reilly, B.; O'Shaughnessy, R.;
Ottaway, D. J.; Overmier, H.; Owen, B. J.; Paik, H. -J.; Pan, Y.;
Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.;
Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi, M. V.;
Postiglione, F.; Prix, R.; Quetschke, V.; Raab, F.; Rabeling, D.;
Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Ramsuder, M.;
Rawlins, K.; Ray-Majumder, S.; Re, V.; Rehbein, H.; Reid, S.; Reitze,
D. H.; Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.; Robertson,
N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan,
A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.; Rowan, S.;
Rudiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi,
M.; Sancho de La Jordana, L.; Sandberg, V.; Sannibale, V.; Saraf,
S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.;
Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.; Schnabel, R.;
Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott, S. M.; Searle,
A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.; Siemens, X.; Sigg,
D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.;
Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.; Strom, D. M.;
Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.;
Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor, R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thuring, A.; Tokmakov,
K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.;
Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.; Vallisneri,
M.; van den Broeck, C.; Varvella, M.; Vass, S.; Vecchio, A.; Veitch,
J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman,
S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Weaver, J.; Webber,
D.; Weber, A.; Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.;
Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.;
Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke,
B.; Wilmut, I.; Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.;
Woan, G.; Woods, D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.;
Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang,
J.; Zhang, L.; Zhang, P.; Zhao, C.; Zotov, N.; Zucker, M.; Zur Muhlen,
H.; Zweizig, J.
Bibcode: 2008PhRvD..77f9904A
Altcode:
No abstract at ADS
Title: Publisher's Note: All-sky search for periodic gravitational
waves in LIGO S4 data [Phys. Rev. D 77, 022001 (2008)]
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.;
Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue, L.; Bork,
R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington, A.; Bunkowski,
A.; Buonanno, A.; Burmeister, O.; Busby, D.; Byer, R. L.; Cadonati,
L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.;
Cao, J.; Cardenas, L.; Casey, M. M.; Castaldi, G.; Cepeda, C.; Chalkey,
E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini,
F.; Chin, D.; Chin, E.; Chow, J.; Christensen, N.; Clark, J.; Cochrane,
P.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.; Conte, R.; Cook, D.;
Corbitt, T.; Coward, D.; Coyne, D.; Creighton, J. D. E.; Creighton,
T. D.; Croce, R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.;
Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; Debra, D.;
Degallaix, J.; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.;
Desalvo, R.; Dhurandhar, S.; Diaz, M.; Dickson, J.; di Credico,
A.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.;
Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza,
E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan, Y.; Fazi,
D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos, N.; Franzen,
A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.; Fritschel,
P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L. M.; Gonzalez, G.; Gossler, S.; Grant, A.; Gras, S.; Gray,
C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote,
H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler,
T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell,
E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito,
M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe,
F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim, C.; King, P.;
Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu,
R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry, M.;
Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leiner, J.; Leonhardt, V.;
Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.; Longo, M.;
Lormand, M.; Lubiński, M.; Luck, H.; Machenschalk, B.; Macinnis, M.;
Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.; Marka,
S.; Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason, K.;
Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.;
McGuire, S. C.; McHugh, M.; McKenzie, K.; McNabb, J. W. C.; McWilliams,
S.; Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.; Meshkov, S.;
Messaritaki, E.; Messenger, C. J.; Meyers, D.; Mikhailov, E.; Mitra,
S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa,
O.; Mohanty, S.; Moreno, G.; Mossavi, K.; Mowlowry, C.; Moylan, A.;
Mudge, D.; Mueller, G.; Mukherjee, S.; Muller-Ebhardt, H.; Munch, J.;
Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton, G.; Nishizawa, A.;
Numata, K.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier,
H.; Owen, B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.;
Pedraza, M.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch,
H.; Plissi, M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab,
F.; Rabeling, D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov,
M.; Ramsunder, M.; Rawlins, K.; Ray-Majumder, S.; Re, V.; Rehbein,
H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rudiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; Sancho de La Jordana, L.; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.;
Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.;
Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.;
Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung,
M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor,
R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thuring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; van den Broeck, C.; Varvella, M.; Vass, S.; Vecchio,
A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.;
Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Webber, D.;
Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.;
Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.;
Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods,
D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan,
Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao,
C.; Zotov, N.; Zucker, M.; Zur Muhlen, H.; Zweizig, J.
Bibcode: 2008PhRvD..77f9902A
Altcode:
No abstract at ADS
Title: Search for gravitational waves from binary inspirals in S3
and S4 LIGO data
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn,
K.; Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue,
L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.;
Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington,
A.; Bunkowski, A.; Buonanno, A.; Burmeister, O.; Busby, D.; Butler,
W. E.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo,
J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas, L.; Carter, K.;
Casey, M. M.; Castaldi, G.; Cepeda, C.; Chalkey, E.; Charlton, P.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini, F.; Chin, D.; Chin,
E.; Chow, J.; Christensen, N.; Clark, J.; Cochrane, P.; Cokelaer,
T.; Colacino, C. N.; Coldwell, R.; Conte, R.; Cook, D.; Corbitt, T.;
Coward, D.; Coyne, D.; Creighton, J. D. E.; Creighton, T. D.; Croce,
R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple,
J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; Debra, D.; Degallaix,
J.; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.; Desalvo, R.;
Dhurandhar, S.; Díaz, M.; Dickson, J.; di Credico, A.; Diederichs,
G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.; Dumas, J. -C.; Dupuis,
R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.;
Evans, T.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn,
L. S.; Fiumara, V.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.;
Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.; Frolov, V. V.;
Fyffe, M.; Galdi, V.; Ganezer, K. S.; Garofoli, J.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L.; González, G.; Gossler, S.; Grant, A.; Gras, S.; Gray,
C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote,
H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler,
T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell,
E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito,
M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe,
F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim, C.; King, P.;
Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu,
R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry, M.;
Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leiner, J.; Leonhardt, V.;
Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.; Longo, M.;
Lormand, M.; Lubiński, M.; Lück, H.; Machenschalk, B.; Macinnis,
M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.;
Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason,
K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McNabb, J. W. C.;
McWilliams, S.; Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messaritaki, E.; Messenger, C. J.; Meyers, D.; Mikhailov,
E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi, K.; Mowlowry, C.;
Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.; Müller-Ebhardt,
H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton, G.;
Nishizawa, A.; Nocera, F.; Numata, K.; O'Reilly, B.; O'Shaughnessy,
R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.;
Parameshwaraiah, V.; Parameswariah, C.; Patel, P.; Pedraza, M.;
Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi,
M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab, F.; Rabeling,
D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Rawlins, K.;
Ray-Majumder, S.; Re, V.; Regimbau, T.; Rehbein, H.; Reid, S.; Reitze,
D. H.; Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.; Robertson,
N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan,
A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.; Rowan, S.;
Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi, M.;
de La Jordana, L. Sancho; Sandberg, V.; Sanders, G. H.; Sannibale,
V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson,
P. R.; Savage, R.; Savov, P.; Sazonov, A.; Schediwy, S.; Schilling,
R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.;
Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.;
Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.;
Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung,
M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor,
R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; van den Broeck, C.; van Putten, M.; Varvella, M.;
Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick,
C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward,
R.; Watts, K.; Webber, D.; Weidner, A.; Weinert, M.; Weinstein,
A.; Weiss, R.; Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck, D. M.;
Whitcomb, S. E.; Whiting, B. F.; Wiley, S.; Wilkinson, C.; Willems,
P. A.; Williams, L.; Willke, B.; Wilmut, I.; Winkler, W.; Wipf, C. C.;
Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.; Wooley, R.; Worden,
J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes,
N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker,
M.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2008PhRvD..77f2002A
Altcode: 2007arXiv0704.3368L
We report on a search for gravitational waves from the
coalescence of compact binaries during the third and fourth
LIGO science runs. The search focused on gravitational waves
generated during the inspiral phase of the binary evolution. In
our analysis, we considered three categories of compact binary
systems, ordered by mass: (i) primordial black hole binaries
with masses in the range 0.35M⊙<m1,
m2<1.0M⊙, (ii) binary neutron stars
with masses in the range 1.0M⊙<m1,
m2<3.0M⊙, and (iii) binary black holes
with masses in the range 3.0M⊙<m1,
m2<mmax with the additional
constraint m1+m2<mmax,
where mmax was set to 40.0M⊙
and 80.0M⊙ in the third and fourth science runs,
respectively. Although the detectors could probe to distances as far as
tens of Mpc, no gravitational-wave signals were identified in the 1364
hours of data we analyzed. Assuming a binary population with a Gaussian
distribution around 0.75-0.75M⊙, 1.4-1.4M⊙,
and 5.0-5.0M⊙, we derived 90%-confidence upper limit rates
of 4.9yr-1L10-1 for primordial black
hole binaries, 1.2yr-1L10-1 for binary
neutron stars, and 0.5yr-1L10-1 for
stellar mass binary black holes, where L10 is 1010
times the blue-light luminosity of the Sun.
Title: Search for gravitational waves associated with 39 gamma-ray
bursts using data from the second, third, and fourth LIGO runs
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Berukoff, S. J.; Betzwieser, J.; Beyersdorf,
P. T.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.; Biswas, R.;
Black, E.; Blackburn, K.; Blackburn, L.; Blair, D.; Bland, B.;
Bogenstahl, J.; Bogue, L.; Bork, R.; Boschi, V.; Bose, S.; Brady,
P. R.; Braginsky, V. B.; Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown,
D. A.; Bullington, A.; Bunkowski, A.; Buonanno, A.; Burmeister, O.;
Busby, D.; Butler, W. E.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp,
J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas,
L.; Carter, K.; Casey, M. M.; Castaldi, G.; Cepeda, C.; Chalkley, E.;
Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini, F.;
Chin, D.; Chin, E.; Chow, J.; Christensen, N.; Clark, J.; Cochrane,
P.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.; Coles, M.; Conte, R.;
Cook, D.; Corbitt, T.; Coward, D.; Coyne, D.; Creighton, J. D. E.;
Creighton, T. D.; Croce, R. P.; Crooks, D. R. M.; Cruise, A. M.;
Csatorday, P.; Cumming, A.; Dalrymple, J.; D'Ambrosio, E.; Danzmann,
K.; Davies, G.; Daw, E.; Debra, D.; Degallaix, J.; Degree, M.; Delker,
T.; Demma, T.; Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar,
S.; Díaz, M.; Dickson, J.; di Credico, A.; Diederichs, G.; Dietz,
A.; Ding, H.; Doomes, E. E.; Drever, R. W. P.; Dumas, J. -C.; Dupuis,
R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.;
Evans, T.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.;
Fiumara, V.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.; Freise,
A.; Frey, R.; Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.;
Galdi, V.; Ganezer, K. S.; Garofoli, J.; Gholami, I.; Giaime, J. A.;
Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.; Goggin, L.;
González, G.; Gossler, S.; Grant, A.; Gras, S.; Gray, C.; Gray, M.;
Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote, H.; Grunewald,
S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer, D.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler, T.; Heefner,
J.; Heinzel, G.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell,
E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito, M.;
Itoh, Y.; Ivanov, A.; Jackrel, D.; Jennrich, O.; Johnson, B.; Johnson,
W. W.; Johnston, W. R.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.;
Kalmus, P.; Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili,
F. Ya.; Killow, C. J.; Kim, C.; King, P.; Kissel, J. S.; Klimenko, S.;
Kokeyama, K.; Kondrashov, V.; Kopparapu, R. K.; Kozak, D.; Krishnan,
B.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.; Lazzarini, A.; Lee,
B.; Lei, M.; Leiner, J.; Leonhardt, V.; Leonor, I.; Libbrecht, K.;
Libson, A.; Lindquist, P.; Lockerbie, N. A.; Logan, J.; Longo, M.;
Lormand, M.; Lubiński, M.; Lück, H.; Machenschalk, B.; Macinnis,
M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.;
Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason,
K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McNabb, J. W. C.;
McWilliams, S.; Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messaritaki, E.; Messenger, C. J.; Meyers, D.; Mikhailov,
E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi, K.; Mowlowry, C.;
Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.; Müller-Ebhardt,
H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nagano, S.; Nash,
T.; Newton, G.; Nishizawa, A.; Nocera, F.; Numata, K.; Nutzman, P.;
O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen,
B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Parameswariah, C.;
Patel, P.; Pedraza, M.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin,
M.; Pletsch, H.; Plissi, M. V.; Postiglione, F.; Prix, R.; Quetschke,
V.; Raab, F.; Rabeling, D.; Radkins, H.; Rahkola, R.; Rainer, N.;
Rakhmanov, M.; Ramsunder, M.; Rawlins, K.; Ray-Majumder, S.; Re,
V.; Regimbau, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Ribichini,
L.; Richman, S.; Riesen, R.; Riles, K.; Rivera, B.; Robertson, N. A.;
Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan, A. M.;
Rollins, J.; Romano, J. D.; Romie, J.; Rong, H.; Route, R.; Rowan, S.;
Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi, M.;
Sancho de La Jordana, L.; Sandberg, V.; Sanders, G. H.; Sannibale,
V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson,
P. R.; Savage, R.; Savov, P.; Sazonov, A.; Schediwy, S.; Schilling,
R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.;
Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles,
J. A.; Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen,
B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain,
K. A.; Strand, N. E.; Strom, D. M.; Stuver, A.; Summerscales, T. Z.;
Sun, K. -X.; Sung, M.; Sutton, P. J.; Sylvestre, J.; Takahashi, H.;
Takamori, A.; Tanner, D. B.; Tarallo, M.; Taylor, R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tinto, M.;
Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; van den Broeck, C.; van Putten, M.; Varvella, M.;
Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick,
C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward,
R.; Watts, K.; Webber, D.; Weidner, A.; Weinert, M.; Weinstein, A.;
Weiss, R.; Wen, L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck,
D. M.; Whitcomb, S. E.; Whiting, B. F.; Wiley, S.; Wilkinson, C.;
Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.; Winkler, W.;
Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.; Wooley,
R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida,
S.; Yunes, N.; Zaleski, K. D.; Zanolin, M.; Zhang, J.; Zhang, L.;
Zhao, C.; Zotov, N.; Zucker, M.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2008PhRvD..77f2004A
Altcode: 2007arXiv0709.0766L
We present the results of a search for short-duration gravitational-wave
bursts associated with 39 gamma-ray bursts (GRBs) detected by
gamma-ray satellite experiments during LIGO’s S2, S3, and S4 science
runs. The search involves calculating the crosscorrelation between
two interferometer data streams surrounding the GRB trigger time. We
search for associated gravitational radiation from single GRBs, and also
apply statistical tests to search for a gravitational-wave signature
associated with the whole sample. For the sample examined, we find no
evidence for the association of gravitational radiation with GRBs,
either on a single-GRB basis or on a statistical basis. Simulating
gravitational-wave bursts with sine-Gaussian waveforms, we set
upper limits on the root-sum-square of the gravitational-wave strain
amplitude of such waveforms at the times of the GRB triggers. We also
demonstrate how a sample of several GRBs can be used collectively to
set constraints on population models. The small number of GRBs and the
significant change in sensitivity of the detectors over the three runs,
however, limits the usefulness of a population study for the S2, S3,
and S4 runs. Finally, we discuss prospects for the search sensitivity
for the ongoing S5 run, and beyond for the next generation of detectors.
Title: The Three-dimensional Evolution of Buoyant Magnetic Flux
Tubes in a Model Solar Convective Envelope
Authors: Fan, Y.
Bibcode: 2008ApJ...676..680F
Altcode:
We present a set of three-dimensional spherical shell anelastic MHD
simulations of the buoyant rise of magnetic flux tubes from the base
of the convection zone to a depth of 16 Mm below the photosphere. It
is found that when a twisted flux tube arches upward due to buoyancy,
it rotates out of the plane and thus produces a tilt at the apex. Our
simulations show that for tubes with the twist rate that is necessary
for a cohesive rise, the twist-induced tilt dominates that caused by
the Coriolis force, and furthermore, the twist-induced tilt is of the
wrong direction (opposite to the observational Joy's law) if the twist
is left-handed (right-handed) in the northern (southern) hemisphere,
following the observed hemispheric preference of the sign of the active
region twist. It is found that in order for the emerging tube to show
the correct tilt direction (consistent with observations), the initial
twist rate of the flux tube needs to be less than half of that needed
for a cohesive rise. Under such conditions, severe flux loss is found
during the rise. We also found that due to the asymmetric stretching
of the rising tube by the Coriolis force, a field strength asymmetry
develops, with the field in the leading leg (leading in the direction
of rotation) of the Ω-shaped emerging tube being stronger than the
field in the following leg, which results in a more compact morphology
in the leading polarity of the emerging active region.
Title: Publisher's Note: Upper limits on gravitational wave emission
from 78 radio pulsars [Phys. Rev. D 76, 042001 (2007)]
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn,
K.; Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue,
L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.;
Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington,
A.; Bunkowski, A.; Buonanno, A.; Burmeister, O.; Busby, D.; Butler,
W. E.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo,
J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas, L.; Carter, K.;
Casey, M. M.; Castaldi, G.; Cepeda, C.; Chalkey, E.; Charlton, P.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini, F.; Chin, D.; Chin,
E.; Chow, J.; Christensen, N.; Clark, J.; Cochrane, P.; Cokelaer,
T.; Colacino, C. N.; Coldwell, R.; Conte, R.; Cook, D.; Corbitt, T.;
Coward, D.; Coyne, D.; Creighton, J. D. E.; Creighton, T. D.; Croce,
R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple,
J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; Debra, D.; Degallaix,
J.; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.; Desalvo, R.;
Dhurandhar, S.; Diaz, M.; Dickson, J.; di Credico, A.; Diederichs,
G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.; Dumas, J. -C.; Dupuis,
R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.;
Evans, T.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn,
L. S.; Fiumara, V.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.;
Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.; Frolov, V. V.;
Fyffe, M.; Galdi, V.; Ganezer, K. S.; Garofoli, J.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L.; Gonzalez, G.; Gossler, S.; Grant, A.; Gras, S.; Gray, C.;
Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote, H.;
Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer, D.;
Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler,
T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell,
E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito,
M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe,
F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim, C.; King, P.;
Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu,
R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry, M.;
Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leiner, J.; Leonhardt,
V.; Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.; Longo,
M.; Lormand, M.; Lubiński, M.; Luck, H.; Machenschalk, B.; Macinnis,
M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.;
Marka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason,
K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McNabb, J. W. C.;
McWilliams, S.; Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messaritaki, E.; Messenger, C. J.; Meyers, D.; Mikhailov,
E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi, K.; Mowlowry, C.;
Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.; Muller-Ebhardt, H.;
Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton, G.;
Nishizawa, A.; Nocera, F.; Numata, K.; O'Reilly, B.; O'Shaughnessy,
R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.;
Parameshwaraiah, V.; Parameshwaraiah, C.; Patel, P.; Pedraza, M.;
Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi,
M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab, F.; Rabeling,
D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Rawlins, K.;
Ray-Majumder, S.; Re, V.; Regimbau, T.; Rehbein, H.; Reid, S.; Reitze,
D. H.; Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.; Robertson,
N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan,
A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.; Rowan, S.;
Rudiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi, M.;
Sancho de La Jordana, L.; Sandberg, V.; Sanders, G. H.; Sannibale,
V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson,
P. R.; Savage, R.; Savov, P.; Sazonov, A.; Schediwy, S.; Schilling,
R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.;
Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.;
Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.;
Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung,
M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor,
R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thuring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; van den Broeck, C.; van Putten, M.; Varvella, M.;
Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick,
C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward,
R.; Watts, K.; Webber, D.; Weidner, A.; Weinert, M.; Weinstein,
A.; Weiss, R.; Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck, D. M.;
Whitcomb, S. E.; Whiting, B. F.; Wiley, S.; Wilkinson, C.; Willems,
P. A.; Williams, L.; Willke, B.; Wilmut, I.; Winkler, W.; Wipf, C. C.;
Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.; Wooley, R.; Worden,
J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes,
N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker,
M.; Zur Muhlen, H.; Zweizig, J.; Kramer, M.; Lyne, A. G.
Bibcode: 2008PhRvD..77f9905A
Altcode:
No abstract at ADS
Title: ERRATUM: Search for gravitational-wave bursts in LIGO data
from the fourth science run
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn,
K.; Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue,
L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.;
Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington, A.;
Bunkowski, A.; Buonanno, A.; Burmeister, O.; Busby, D.; Byer, R. L.;
Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.;
Cantley, C. A.; Cao, J.; Cardenas, L.; Casey, M. M.; Castaldi, G.;
Cepeda, C.; Chalkey, E.; Charlton, P.; Chatterji, S.; Chelkowski, S.;
Chen, Y.; Chiadini, F.; Chin, D.; Chin, E.; Chow, J.; Christensen, N.;
Clark, J.; Cochrane, P.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.;
Conte, R.; Cook, D.; Corbitt, T.; Coward, D.; Coyne, D.; Creighton,
J. D. E.; Creighton, T. D.; Croce, R. P.; Crooks, D. R. M.; Cruise,
A. M.; Cumming, A.; Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.;
Davies, G.; DeBra, D.; Degallaix, J.; Degree, M.; Demma, T.; Dergachev,
V.; Desai, S.; DeSalvo, R.; Dhurandhar, S.; Díaz, M.; Dickson, J.;
Di Credico, A.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever,
R. W. P.; Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.;
Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan,
Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos,
N.; Franzen, A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.;
Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda,
K.; Goetz, E.; Goggin, L. M.; González, G.; Gossler, S.; Grant,
A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.;
Grosso, R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, R.;
Hage, B.; Hammer, D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.;
Harstad, E.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall, A.;
Heurs, M.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken,
D.; Hough, J.; Howell, E.; Hoyland, D.; Huttner, S. H.; Ingram, D.;
Innerhofer, E.; Ito, M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson,
B.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.;
Kalmus, P.; Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili,
F. Ya; Kim, C.; King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.;
Kondrashov, V.; Kopparapu, R. K.; Kozak, D.; Krishnan, B.; Kwee, P.;
Lam, P. K.; Landry, M.; Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.;
Leiner, J.; Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lindquist, P.;
Lockerbie, N. A.; Longo, M.; Lormand, M.; Lubiński, M.; Lück, H.;
Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Malec, M.;
Mandic, V.; Marano, S.; Márka, S.; Markowitz, J.; Maros, E.; Martin,
I.; Marx, J. N.; Mason, K.; Matone, L.; Matta, V.; Mavalvala, N.;
McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McKenzie,
K.; McNabb, J. W. C.; McWilliams, S.; Meier, T.; Melissinos, A.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messaritaki, E.; Messenger,
C. J.; Meyers, D.; Mikhailov, E.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Mohanty, S.; Moreno,
G.; Mossavi, K.; Lowry, C. Mow; Moylan, A.; Mudge, D.; Mueller, G.;
Mukherjee, S.; Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.;
Myers, J.; Nash, T.; Newton, G.; Nishizawa, A.; Numata, K.; O'Reilly,
B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.;
Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.;
Pelc, J.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch,
H.; Plissi, M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab,
F.; Rabeling, D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov,
M.; Ramsunder, M.; Rawlins, K.; Ray-Majumder, S.; Re, V.; Rehbein,
H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; Sancho de la Jordana, L.; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.;
Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.;
Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.;
Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.;
Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor, R.;
Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.;
Tinto, M.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias,
M.; Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; Van Den Broeck, C.; Varvella, M.; Vass, S.; Vecchio,
A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.;
Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Webber, D.;
Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.;
Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.;
Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods,
D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan,
Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao,
C.; Zotov, N.; Zucker, M.; zur Mühlen, H.; Zweizig, J.; LIGO
Scientific Collaboration
Bibcode: 2008CQGra..25c9801A
Altcode: 2008CQGra..25c9801B
The full text of this article is available in the PDF provided.
Title: All-sky search for periodic gravitational waves in LIGO S4 data
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.;
Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue, L.; Bork,
R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington, A.; Bunkowski,
A.; Buonanno, A.; Burmeister, O.; Busby, D.; Byer, R. L.; Cadonati,
L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley,
C. A.; Cao, J.; Cardenas, L.; Casey, M. M.; Castaldi, G.; Cepeda, C.;
Chalkley, E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.;
Chiadini, F.; Chin, D.; Chin, E.; Chow, J.; Christensen, N.; Clark, J.;
Cochrane, P.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.; Conte, R.;
Cook, D.; Corbitt, T.; Coward, D.; Coyne, D.; Creighton, J. D. E.;
Creighton, T. D.; Croce, R. P.; Crooks, D. R. M.; Cruise, A. M.;
Cumming, A.; Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.;
Debra, D.; Degallaix, J.; Degree, M.; Demma, T.; Dergachev, V.; Desai,
S.; Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dickson, J.; di Credico,
A.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.;
Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza,
E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan, Y.; Fazi,
D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos, N.; Franzen,
A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.; Fritschel,
P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L. M.; González, G.; Gossler, S.; Grant, A.; Gras, S.; Gray,
C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote,
H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler,
T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell,
E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito,
M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe,
F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim, C.; King, P.;
Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu,
R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry, M.;
Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leiner, J.; Leonhardt, V.;
Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.; Longo, M.;
Lormand, M.; Lubiński, M.; Lück, H.; Machenschalk, B.; Macinnis,
M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.;
Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason,
K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McNabb, J. W. C.;
McWilliams, S.; Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messenger, C. J.; Meyers, D.; Mikhailov, E.; Mitra,
S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa,
O.; Mohanty, S.; Moreno, G.; Mossavi, K.; Mowlowry, C.; Moylan, A.;
Mudge, D.; Mueller, G.; Mukherjee, S.; Müller-Ebhardt, H.; Munch, J.;
Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton, G.; Nishizawa, A.;
Numata, K.; O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier,
H.; Owen, B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.;
Pedraza, M.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch,
H.; Plissi, M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab,
F.; Rabeling, D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov,
M.; Ramsunder, M.; Rawlins, K.; Ray-Majumder, S.; Re, V.; Rehbein,
H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; Sancho de La Jordana, L.; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Siemens, X.; Sigg,
D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.;
Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.; Strom, D. M.;
Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.;
Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor, R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov,
K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.;
Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.; Vallisneri,
M.; van den Broeck, C.; Varvella, M.; Vass, S.; Vecchio, A.; Veitch,
J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman,
S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Webber, D.;
Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.;
Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.;
Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods,
D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan,
Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao,
C.; Zotov, N.; Zucker, M.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2008PhRvD..77b2001A
Altcode: 2007arXiv0708.3818L
We report on an all-sky search with the LIGO detectors for
periodic gravitational waves in the frequency range 50 1000
Hz and with the frequency’s time derivative in the range
-1×10-8Hzs-1 to zero. Data from the fourth
LIGO science run (S4) have been used in this search. Three different
semicoherent methods of transforming and summing strain power from
short Fourier transforms (SFTs) of the calibrated data have been
used. The first, known as StackSlide, averages normalized power from
each SFT. A “weighted Hough” scheme is also developed and used,
which also allows for a multi-interferometer search. The third
method, known as PowerFlux, is a variant of the StackSlide method
in which the power is weighted before summing. In both the weighted
Hough and PowerFlux methods, the weights are chosen according to the
noise and detector antenna-pattern to maximize the signal-to-noise
ratio. The respective advantages and disadvantages of these methods are
discussed. Observing no evidence of periodic gravitational radiation,
we report upper limits; we interpret these as limits on this radiation
from isolated rotating neutron stars. The best population-based upper
limit with 95% confidence on the gravitational-wave strain amplitude,
found for simulated sources distributed isotropically across the sky
and with isotropically distributed spin axes, is 4.28×10-24
(near 140 Hz). Strict upper limits are also obtained for small patches
on the sky for best-case and worst-case inclinations of the spin axes.
Title: Onset of coronal mass ejections due to loss of confinement
of coronal flux ropes
Authors: Fan, Y.; Gibson, S.
Bibcode: 2007AGUFMSH51C..04F
Altcode:
Using MHD numerical simulations in a three-dimensional spherical
geometry, we model the loss of confinement and eruption of a flux
rope emerging quasistatically into a pre-existing coronal arcade
field. Our numerical experiments have investigated two distinct
triggering mechanisms that led to the eruption of the flux rope. In
one case, the overlying arcade field declines with height more slowly
such that the emerging flux rope remains confined until a high amount
of internal twist is built up, with the rope self-helicity normalized
by the square of the rope flux reaching about -1.4, and the flux rope
becomes significantly kinked. The kinking motion causes rotation of
the tube to an orientation that makes it easier for it to rupture
through the arcade field, leading to an eruption. In the second case,
the overlying field is made to decline more rapidly with height and the
emerging flux rope is found to lose equilibrium and erupt via the torus
instability when the flux rope self-helicity normalized by the square
of the rope flux is only -0.63, before it becomes kinked. The values of
the total relative magnetic helicity normalized by the square of the
total anchored flux are, on the other hand, quite close for the two
cases when the eruption takes place. We study the eruptive properties
resulting from the two mechansisms and compare them with observations.
Title: Search for gravitational-wave bursts in LIGO data from the
fourth science run
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn,
K.; Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue,
L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.;
Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington, A.;
Bunkowski, A.; Buonanno, A.; Burmeister, O.; Busby, D.; Byer, R. L.;
Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.;
Cantley, C. A.; Cao, J.; Cardenas, L.; Casey, M. M.; Castaldi, G.;
Cepeda, C.; Chalkey, E.; Charlton, P.; Chatterji, S.; Chelkowski, S.;
Chen, Y.; Chiadini, F.; Chin, D.; Chin, E.; Chow, J.; Christensen, N.;
Clark, J.; Cochrane, P.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.;
Conte, R.; Cook, D.; Corbitt, T.; Coward, D.; Coyne, D.; Creighton,
J. D. E.; Creighton, T. D.; Croce, R. P.; Crooks, D. R. M.; Cruise,
A. M.; Cumming, A.; Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.;
Davies, G.; DeBra, D.; Degallaix, J.; Degree, M.; Demma, T.; Dergachev,
V.; Desai, S.; DeSalvo, R.; Dhurandhar, S.; Díaz, M.; Dickson, J.;
Di Credico, A.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever,
R. W. P.; Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.;
Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan,
Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos,
N.; Franzen, A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.;
Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda,
K.; Goetz, E.; Goggin, L. M.; González, G.; Gossler, S.; Grant,
A.; Gras, S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.;
Grosso, R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, R.;
Hage, B.; Hammer, D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.;
Harstad, E.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall, A.;
Heurs, M.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken,
D.; Hough, J.; Howell, E.; Hoyland, D.; Huttner, S. H.; Ingram, D.;
Innerhofer, E.; Ito, M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson,
B.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.;
Kalmus, P.; Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili,
F. Ya; Kim, C.; King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.;
Kondrashov, V.; Kopparapu, R. K.; Kozak, D.; Krishnan, B.; Kwee, P.;
Lam, P. K.; Landry, M.; Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.;
Leiner, J.; Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lindquist, P.;
Lockerbie, N. A.; Longo, M.; Lormand, M.; Lubiński, M.; Lück, H.;
Machenschalk, B.; MacInnis, M.; Mageswaran, M.; Mailand, K.; Malec, M.;
Mandic, V.; Marano, S.; Márka, S.; Markowitz, J.; Maros, E.; Martin,
I.; Marx, J. N.; Mason, K.; Matone, L.; Matta, V.; Mavalvala, N.;
McCarthy, R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McKenzie,
K.; McNabb, J. W. C.; McWilliams, S.; Meier, T.; Melissinos, A.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messaritaki, E.; Messenger,
C. J.; Meyers, D.; Mikhailov, E.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Mohanty, S.; Moreno,
G.; Mossavi, K.; Lowry, C. Mow; Moylan, A.; Mudge, D.; Mueller, G.;
Mukherjee, S.; Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.;
Myers, J.; Nash, T.; Newton, G.; Nishizawa, A.; Numata, K.; O'Reilly,
B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.;
Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.;
Pelc, J.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch,
H.; Plissi, M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab,
F.; Rabeling, D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov,
M.; Ramsunder, M.; Rawlins, K.; Ray-Majumder, S.; Re, V.; Rehbein,
H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; Sancho de la Jordana, L.; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.;
Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.;
Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.;
Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.;
Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor, R.;
Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.;
Tinto, M.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias,
M.; Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; Van Den Broeck, C.; Varvella, M.; Vass, S.; Vecchio,
A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.;
Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Webber, D.;
Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.;
Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.;
Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods,
D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan,
Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao,
C.; Zotov, N.; Zucker, M.; zur Mühlen, H.; Zweizig, J.; LIGO
Scientific Collaboration
Bibcode: 2007CQGra..24.5343A
Altcode: 2007arXiv0704.0943L
The fourth science run of the LIGO and GEO 600 gravitational-wave
detectors, carried out in early 2005, collected data with significantly
lower noise than previous science runs. We report on a search for
short-duration gravitational-wave bursts with arbitrary waveform
in the 64 1600 Hz frequency range appearing in all three LIGO
interferometers. Signal consistency tests, data quality cuts and
auxiliary-channel vetoes are applied to reduce the rate of spurious
triggers. No gravitational-wave signals are detected in 15.5 days
of live observation time; we set a frequentist upper limit of 0.15
day-1 (at 90% confidence level) on the rate of bursts
with large enough amplitudes to be detected reliably. The amplitude
sensitivity of the search, characterized using Monte Carlo simulations,
is several times better than that of previous searches. We also provide
rough estimates of the distances at which representative supernova and
binary black hole merger signals could be detected with 50% efficiency
by this analysis.
Title: Searches for periodic gravitational waves from unknown isolated
sources and Scorpius X-1: Results from the second LIGO science run
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Berukoff, S. J.; Betzwieser, J.; Beyersdorf,
P. T.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.; Biswas, R.;
Black, E.; Blackburn, K.; Blackburn, L.; Blair, B.; Bland, B.;
Bogenstahl, J.; Bogue, L.; Bork, R.; Boschi, V.; Bose, S.; Brady,
P. R.; Braginsky, V. B.; Brau, J. E.; Brinkmann, M.; Brooks, A.;
Brown, D. A.; Bullington, A.; Bunkowski, A.; Buonanno, A.; Burmeister,
O.; Busby, D.; Butler, W. E.; Byer, R. L.; Cadonati, L.; Cagnoli,
G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.; Cao, J.;
Cardenas, L.; Carter, K.; Casey, M. M.; Castaldi, G.; Cepeda, C.;
Chalkey, E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.;
Chiadini, F.; Chin, D.; Chin, E.; Chow, J.; Christensen, N.; Clark,
J.; Cochrane, . P.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.;
Coles, M.; Conte, R.; Cook, D.; Corbitt, T.; Coward, D.; Coyne,
D.; Creighton, J. D. E.; Creighton, T. D.; Croce, R. P.; Crooks,
D. R. M.; Cruise, A. M.; Csatorday, P.; Cumming, A.; Cutler, C.;
Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; Daw,
E.; Debra, D.; Degallaix, J.; Degree, M.; Delker, T.; Demma, T.;
Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar, S.; Díaz,
M.; Dickson, J.; di Credico, A.; Diederichs, G.; Dietz, A.; Ding,
H.; Doomes, E. E.; Drever, R. W. P.; Dumas, J. -C.; Dupuis, R. J.;
Dwyer, J. G.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans,
T.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.;
Fiumara, V.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.; Freise,
A.; Frey, R.; Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.;
Galdi, V.; Ganezer, K. S.; Garofoli, J.; Gholami, I.; Giaime, J. A.;
Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.; Goggin, L. M.;
González, G.; Gossler, S.; Grant, A.; Gras, S.; Gray, C.; Gray, M.;
Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote, H.; Grunewald,
S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer, D.; Hanna, C.;
Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler, T.; Heefner,
J.; Heinzel, G.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell,
E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito, M.;
Itoh, Y.; Ivanov, A.; Jackrel, D.; Jennrich, O.; Johnson, B.; Johnson,
W. W.; Johnston, W. R.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.;
Kalmus, P.; Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili,
F. Ya.; Killow, C. J.; Kim, C.; King, P.; Kissell, J. S.; Klimenko, S.;
Kokeyama, K.; Kondrashov, V.; Kopparapu, R. K.; Kozak, D.; Krishnan,
B.; Kwee, P.; Lam, P. K.; Landry, M.; Lantz, B.; Lazzarini, A.; Lee,
B.; Lei, M.; Leiner, J.; Leonhardt, V.; Leonor, I.; Libbrecht, K.;
Libson, A.; Lindquist, P.; Lockerbie, N. A.; Logan, J.; Longo, M.;
Lormand, M.; Lubiński, M.; Lück, H.; Machenschalk, B.; Macinnis,
M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.;
Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason,
K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McNabb, J. W. C.;
McWilliams, S.; Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messaritaki, E.; Messenger, C. J.; Meyers, D.; Mikhailov,
E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi, K.; Mowlowry, C.;
Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.; Müller-Ebhardt,
H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nagano, S.; Nash,
T.; Newton, G.; Nishizawa, A.; Nocera, F.; Numata, K.; Nutzman, P.;
O'Reilly, B.; O'Shaughnessy, R.; Ottaway, D. J.; Overmier, H.; Owen,
B. J.; Pan, Y.; Papa, M. A.; Parameshwaraiah, V.; Parameswariah, C.;
Patel, P.; Pedraza, M.; Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin,
M.; Pletsch, H.; Plissi, M. V.; Postiglione, F.; Prix, R.; Quetschke,
V.; Raab, F.; Rabeling, D.; Radkins, H.; Rahkola, R.; Rainer, N.;
Rakhmanov, M.; Ramsunder, M.; Rawlins, K.; Ray-Majumder, S.; Re, V.;
Regimbau, T.; Rehbein, H.; Reid, S.; Reitze, D. H.; Ribichini, L.;
Richman, S.; Riesen, R.; Riles, K.; Rivera, B.; Robertson, N. A.;
Robinson, C.; Robison, E. L.; Roddy, S.; Rodriguez, A.; Rogan,
A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Rong, H.; Route, R.;
Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata,
S.; Samidi, M.; Sancho de La Jordana, L.; Sandberg, V.; Sanders,
G. H.; Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B.; Sato,
S.; Saulson, P. R.; Savage, R.; Savov, P.; Sazonov, A.; Schediwy, S.;
Schilling, R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg,
P.; Scott, S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles,
J. A.; Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen,
B. J. J.; Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain,
K. A.; Strand, N. E.; Strom, D. M.; Stuver, A.; Summerscales, T. Z.;
Sun, K. -X.; Sung, M.; Sutton, P. J.; Sylvestre, J.; Takahashi, H.;
Takamori, A.; Tanner, D. B.; Tarallo, M.; Taylor, R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tinto, M.;
Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; van den Broeck, C.; van Putten, M.; Varvella, M.;
Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick,
C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward,
R.; Watts, K.; Webber, D.; Weidner, A.; Weinert, M.; Weinstein, A.;
Weiss, R.; Wen, L.; Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck,
D. . M.; Whitcomb, S. E.; Whiting, B. F.; Wiley, S.; Wilkinson, C.;
Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.; Winkler, W.;
Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.; Wooley,
R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida,
S.; Yunes, N.; Zaleski, K. D.; Zanolin, M.; Zhang, J.; Zhang, L.;
Zhao, C.; Zotov, N.; Zucker, M.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2007PhRvD..76h2001A
Altcode: 2006gr.qc.....5028T
We carry out two searches for periodic gravitational waves using the
most sensitive few hours of data from the second LIGO science run. Both
searches exploit fully coherent matched filtering and cover wide areas
of parameter space, an innovation over previous analyses which requires
considerable algorithm development and computational power. The first
search is targeted at isolated, previously unknown neutron stars,
covers the entire sky in the frequency band 160 728.8 Hz, and assumes
a frequency derivative of less than 4×10-10Hz/s. The second
search targets the accreting neutron star in the low-mass x-ray binary
Scorpius X-1 and covers the frequency bands 464 484 Hz and 604 624 Hz
as well as the two relevant binary orbit parameters. Because of the
high computational cost of these searches we limit the analyses to
the most sensitive 10 hours and 6 hours of data, respectively. Given
the limited sensitivity and duration of the analyzed data set,
we do not attempt deep follow-up studies. Rather we concentrate
on demonstrating the data analysis method on a real data set and
present our results as upper limits over large volumes of the parameter
space. In order to achieve this, we look for coincidences in parameter
space between the Livingston and Hanford 4-km interferometers. For
isolated neutron stars our 95% confidence level upper limits on the
gravitational wave strain amplitude range from 6.6×10-23
to 1×10-21 across the frequency band; for Scorpius
X-1 they range from 1.7×10-22 to 1.3×10-21
across the two 20-Hz frequency bands. The upper limits presented in
this paper are the first broadband wide parameter space upper limits
on periodic gravitational waves from coherent search techniques. The
methods developed here lay the foundations for upcoming hierarchical
searches of more sensitive data which may detect astrophysical signals.
Title: Upper limit map of a background of gravitational waves
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.;
Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue, L.; Bork,
R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington, A.; Bunkowski,
A.; Buonanno, A.; Burmeister, O.; Busby, D.; Byer, R. L.; Cadonati,
L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.;
Cao, J.; Cardenas, L.; Casey, M. M.; Castaldi, G.; Cepeda, C.; Chalkey,
E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini,
F.; Chin, D.; Chin, E.; Chow, J.; Christensen, N.; Clark, J.; Cochrane,
P.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.; Conte, R.; Cook, D.;
Corbitt, T.; Coward, D.; Coyne, D.; Creighton, J. D. E.; Creighton,
T. D.; Croce, R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.;
Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; Debra, D.;
Degallaix, J.; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.;
Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dickson, J.; di Credico,
A.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.;
Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza,
E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan, Y.; Fazi,
D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos, N.; Franzen,
A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.; Fritschel,
P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L. M.; González, G.; Gossler, S.; Grant, A.; Gras, S.; Gray,
C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote,
H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler,
T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell,
E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito,
M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe,
F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim, C.; King, P.;
Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu,
R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry, M.;
Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leiner, J.; Leonhardt,
V.; Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.;
Longo, M.; Lormand, M.; Lubiński, M.; Lück, H.; Machenschalk, B.;
Macinnis, M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.;
Marano, S.; Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx,
J. N.; Mason, K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.;
McClelland, D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McNabb,
J. W. C.; McWilliams, S.; Meier, T.; Melissinos, A.; Mendell, G.;
Mercer, R. A.; Meshkov, S.; Messaritaki, E.; Messenger, C. J.; Meyers,
D.; Mikhailov, E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.;
Mittleman, R.; Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi, K.;
Mowlowry, C.; Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.;
Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.;
Newton, G.; Nishizawa, A.; Numata, K.; O'Reilly, B.; O'Shaughnessy,
R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.;
Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Pierro, V.;
Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi, M. V.; Postiglione, F.;
Prix, R.; Quetschke, V.; Raab, F.; Rabeling, D.; Radkins, H.; Rahkola,
R.; Rainer, N.; Rakhmanov, M.; Rawlins, K.; Ray-Majumder, S.; Re, V.;
Rehbein, H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles,
K.; Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; Sancho de La Jordana, L.; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.;
Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.;
Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.;
Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung,
M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor,
R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; van den Broeck, C.; Varvella, M.; Vass, S.; Vecchio,
A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.;
Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Webber, D.;
Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.;
Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.;
Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods,
D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan,
Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao,
C.; Zotov, N.; Zucker, M.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2007PhRvD..76h2003A
Altcode: 2007astro.ph..3234T
We searched for an anisotropic background of gravitational waves
using data from the LIGO S4 science run and a method that is
optimized for point sources. This is appropriate if, for example,
the gravitational wave background is dominated by a small number
of distinct astrophysical sources. No signal was seen. Upper limit
maps were produced assuming two different power laws for the source
strain power spectrum. For an f-3 power law and using
the 50 Hz to 1.8 kHz band the upper limits on the source strain
power spectrum vary between 1.2×10-48Hz-1
(100Hz/f)3 and 1.2×10-47Hz-1
(100Hz/f)3, depending on the position in the
sky. Similarly, in the case of constant strain power spectrum, the
upper limits vary between 8.5×10-49Hz-1 and
6.1×10-48Hz-1. As a side product a limit on an
isotropic background of gravitational waves was also obtained. All
limits are at the 90% confidence level. Finally, as an application,
we focused on the direction of Sco-X1, the brightest low-mass x-ray
binary. We compare the upper limit on strain amplitude obtained by
this method to expectations based on the x-ray flux from Sco-X1.
Title: Onset of Coronal Mass Ejections Due to Loss of Confinement
of Coronal Flux Ropes
Authors: Fan, Y.; Gibson, S. E.
Bibcode: 2007ApJ...668.1232F
Altcode:
Using MHD numerical simulations in a three-dimensional spherical
geometry, we model the loss of confinement and eruption of a flux rope
emerging quasi-statically into a preexisting coronal arcade field. Our
numerical experiments investigated two distinct mechanisms that led
to the eruption of the flux rope. In one case, the overlying arcade
field declines with height slowly such that the emerging flux rope
remains confined until its self-relative magnetic helicity normalized
by the square of the rope's flux reaches -1.4 and the flux rope becomes
significantly kinked. The kinking motion causes rotation of the tube
to an orientation that makes it easier for it to rupture through the
arcade field, leading to an eruption. In the second case, the overlying
field declines more rapidly with height, and the emerging flux rope is
found to lose equilibrium and erupt via the torus instability when its
self-relative magnetic helicity normalized by the square of its flux
is only approximately -0.63, before it becomes kinked. The values of
the total relative magnetic helicity of the entire coronal magnetic
field (including both the flux rope and the arcade field) normalized
by the square of the total magnetic flux are, on the other hand, of
similar magnitudes for the two cases when the eruption takes place. We
compare and contrast the eruptive properties and the posteruption
states resulting from the two cases.
Title: Search for gravitational wave radiation associated with the
pulsating tail of the SGR 1806-20 hyperflare of 27 December 2004
using LIGO
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn, K.;
Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue, L.; Bork,
R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.;
Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington, A.; Bunkowski,
A.; Buonanno, A.; Burmeister, O.; Busby, D.; Byer, R. L.; Cadonati,
L.; Cagnoli, G.; Camp, J. B.; Cannizzo, J.; Cannon, K.; Cantley, C. A.;
Cao, J.; Cardenas, L.; Casey, M. M.; Castaldi, G.; Cepeda, C.; Chalkey,
E.; Charlton, P.; Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini,
F.; Chin, D.; Chin, E.; Chow, J.; Christensen, N.; Clark, J.; Cochrane,
P.; Cokelaer, T.; Colacino, C. N.; Coldwell, R.; Conte, R.; Cook, D.;
Corbitt, T.; Coward, D.; Coyne, D.; Creighton, J. D. E.; Creighton,
T. D.; Croce, R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.;
Dalrymple, J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; Debra, D.;
Degallaix, J.; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.;
Desalvo, R.; Dhurandhar, S.; Díaz, M.; Dickson, J.; di Credico,
A.; Diederichs, G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.;
Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza,
E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan, Y.; Fazi,
D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos, N.; Franzen,
A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.; Fritschel,
P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L.; González, G.; Gossler, S.; Grant, A.; Gras, S.; Gray,
C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote,
H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler,
T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell,
E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito,
M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kamat, S.; Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura,
S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim,
C.; King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov,
V.; Kopparapu, R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.;
Landry, M.; Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leiner, J.;
Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie,
N. A.; Longo, M.; Lormand, M.; Lubiński, M.; Lück, H.; Machenschalk,
B.; Macinnis, M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.;
Marano, S.; Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx,
J. N.; Mason, K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy,
R.; McClelland, D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.;
McNabb, J. W. C.; McWilliams, S.; Meier, T.; Melissinos, A.; Mendell,
G.; Mercer, R. A.; Meshkov, S.; Messaritaki, E.; Messenger, C. J.;
Meyers, D.; Mikhailov, E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi,
K.; Mowlowry, C.; Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.;
Müller-Ebhardt, H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash,
T.; Newton, G.; Nishizawa, A.; Numata, K.; O'Reilly, B.; O'Shaughnessy,
R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.;
Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.; Pierro, V.;
Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi, M. V.; Postiglione, F.;
Prix, R.; Quetschke, V.; Raab, F.; Rabeling, D.; Radkins, H.; Rahkola,
R.; Rainer, N.; Rakhmanov, M.; Rawlins, K.; Ray-Majumder, S.; Re, V.;
Rehbein, H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles,
K.; Rivera, B.; Robertson, N. A.; Robinson, C.; Robinson, E. L.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; de La Jordana, L. Sancho; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.;
Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.;
Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.;
Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.;
Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.;
Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor, R.;
Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.;
Tinto, M.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias,
M.; Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; van den Broeck, C.; Varvella, M.; Vass, S.; Vecchio,
A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.;
Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Webber, D.;
Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.;
Wilkinson, C.; Willems, P. A.; Williams, L.; Willke, B.; Wilmut, I.;
Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods,
D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan,
Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao,
C.; Zotov, N.; Zucker, M.; Zur Mühlen, H.; Zweizig, J.
Bibcode: 2007PhRvD..76f2003A
Altcode: 2007astro.ph..3419T
We have searched for gravitational waves (GWs) associated with the
SGR 1806-20 hyperflare of 27 December 2004. This event, originating
from a Galactic neutron star, displayed exceptional energetics. Recent
investigations of the x-ray light curve’s pulsating tail revealed
the presence of quasiperiodic oscillations (QPOs) in the 30 2000 Hz
frequency range, most of which coincides with the bandwidth of the
LIGO detectors. These QPOs, with well-characterized frequencies, can
plausibly be attributed to seismic modes of the neutron star which
could emit GWs. Our search targeted potential quasimonochromatic GWs
lasting for tens of seconds and emitted at the QPO frequencies. We
have observed no candidate signals above a predetermined threshold,
and our lowest upper limit was set by the 92.5 Hz QPO observed in
the interval from 150 s to 260 s after the start of the flare. This
bound corresponds to a (90% confidence) root-sum-squared amplitude
hrss-det90%=4.5×10-22strainHz-1/2
on the GW waveform strength in the detectable polarization
state reaching our Hanford (WA) 4 km detector. We illustrate
the astrophysical significance of the result via an estimated
characteristic energy in GW emission that we would expect to be able
to detect. The above result corresponds to 7.7×1046erg
(=4.3×10-8M⊙c2), which is
of the same order as the total (isotropic) energy emitted in the
electromagnetic spectrum. This result provides a means to probe
the energy reservoir of the source with the best upper limit on the
GW waveform strength published and represents the first broadband
asteroseismology measurement using a GW detector.
Title: Upper limits on gravitational wave emission from 78 radio
pulsars
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn,
K.; Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue,
L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.;
Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington,
A.; Bunkowski, A.; Buonanno, A.; Burmeister, O.; Busby, D.; Butler,
W. E.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo,
J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas, L.; Carter, K.;
Casey, M. M.; Castaldi, G.; Cepeda, C.; Chalkey, E.; Charlton, P.;
Chatterji, S.; Chelkowski, S.; Chen, Y.; Chiadini, F.; Chin, D.; Chin,
E.; Chow, J.; Christensen, N.; Clark, J.; Cochrane, P.; Cokelaer,
T.; Colacino, C. N.; Coldwell, R.; Conte, R.; Cook, D.; Corbitt, T.;
Coward, D.; Coyne, D.; Creighton, J. D. E.; Creighton, T. D.; Croce,
R. P.; Crooks, D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple,
J.; D'Ambrosio, E.; Danzmann, K.; Davies, G.; Debra, D.; Degallaix,
J.; Degree, M.; Demma, T.; Dergachev, V.; Desai, S.; Desalvo, R.;
Dhurandhar, S.; Díaz, M.; Dickson, J.; di Credico, A.; Diederichs,
G.; Dietz, A.; Doomes, E. E.; Drever, R. W. P.; Dumas, J. -C.; Dupuis,
R. J.; Dwyer, J. G.; Ehrens, P.; Espinoza, E.; Etzel, T.; Evans, M.;
Evans, T.; Fairhurst, S.; Fan, Y.; Fazi, D.; Fejer, M. M.; Finn,
L. S.; Fiumara, V.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.;
Freise, A.; Frey, R.; Fricke, T.; Fritschel, P.; Frolov, V. V.;
Fyffe, M.; Galdi, V.; Ganezer, K. S.; Garofoli, J.; Gholami, I.;
Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.; Goetz, E.;
Goggin, L.; González, G.; Gossler, S.; Grant, A.; Gras, S.; Gray,
C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso, R.; Grote,
H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.; Hammer,
D.; Hanna, C.; Hanson, J.; Harms, J.; Harry, G.; Harstad, E.; Hayler,
T.; Heefner, J.; Heng, I. S.; Heptonstall, A.; Heurs, M.; Hewitson,
M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken, D.; Hough, J.; Howell,
E.; Hoyland, D.; Huttner, S. H.; Ingram, D.; Innerhofer, E.; Ito,
M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson, B.; Johnson, W. W.;
Jones, D. I.; Jones, G.; Jones, R.; Ju, L.; Kalmus, P.; Kalogera, V.;
Kasprzyk, D.; Katsavounidis, E.; Kawabe, K.; Kawamura, S.; Kawazoe,
F.; Kells, W.; Keppel, D. G.; Khalili, F. Ya.; Kim, C.; King, P.;
Kissel, J. S.; Klimenko, S.; Kokeyama, K.; Kondrashov, V.; Kopparapu,
R. K.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.; Landry, M.;
Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leiner, J.; Leonhardt, V.;
Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.; Longo, M.;
Lormand, M.; Lubiński, M.; Lück, H.; Machenschalk, B.; Macinnis,
M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Marano, S.;
Márka, S.; Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason,
K.; Matone, L.; Matta, V.; Mavalvala, N.; McCarthy, R.; McClelland,
D. E.; McGuire, S. C.; McHugh, M.; McKenzie, K.; McNabb, J. W. C.;
McWilliams, S.; Meier, T.; Melissinos, A.; Mendell, G.; Mercer, R. A.;
Meshkov, S.; Messaritaki, E.; Messenger, C. J.; Meyers, D.; Mikhailov,
E.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.;
Miyakawa, O.; Mohanty, S.; Moreno, G.; Mossavi, K.; Mowlowry, C.;
Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.; Müller-Ebhardt,
H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton, G.;
Nishizawa, A.; Nocera, F.; Numata, K.; O'Reilly, B.; O'Shaughnessy,
R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.;
Parameshwaraiah, V.; Parameswariah, C.; Patel, P.; Pedraza, M.;
Penn, S.; Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi,
M. V.; Postiglione, F.; Prix, R.; Quetschke, V.; Raab, F.; Rabeling,
D.; Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Rawlins, K.;
Ray-Majumder, S.; Re, V.; Regimbau, T.; Rehbein, H.; Reid, S.; Reitze,
D. H.; Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.; Robertson,
N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan,
A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.; Rowan, S.;
Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi, M.;
de La Jordana, L. Sancho; Sandberg, V.; Sanders, G. H.; Sannibale,
V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson,
P. R.; Savage, R.; Savov, P.; Sazonov, A.; Schediwy, S.; Schilling,
R.; Schnabel, R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott,
S. M.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta,
A. S.; Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.;
Siemens, X.; Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.;
Slutsky, J.; Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.;
Strom, D. M.; Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung,
M.; Sutton, P. J.; Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor,
R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring,
A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.;
Tyler, W.; Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.;
Vallisneri, M.; van den Broeck, C.; van Putten, M.; Varvella, M.;
Vass, S.; Vecchio, A.; Veitch, J.; Veitch, P.; Villar, A.; Vorvick,
C.; Vyachanin, S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward,
R.; Watts, K.; Webber, D.; Weidner, A.; Weinert, M.; Weinstein,
A.; Weiss, R.; Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck, D. M.;
Whitcomb, S. E.; Whiting, B. F.; Wiley, S.; Wilkinson, C.; Willems,
P. A.; Williams, L.; Willke, B.; Wilmut, I.; Winkler, W.; Wipf, C. C.;
Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.; Wooley, R.; Worden,
J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes,
N.; Zanolin, M.; Zhang, J.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker,
M.; Zur Mühlen, H.; Zweizig, J.; Kramer, M.; Lyne, A. G.
Bibcode: 2007PhRvD..76d2001A
Altcode: 2007gr.qc.....2039T
We present upper limits on the gravitational wave emission from 78
radio pulsars based on data from the third and fourth science runs
of the LIGO and GEO 600 gravitational wave detectors. The data from
both runs have been combined coherently to maximize sensitivity. For
the first time, pulsars within binary (or multiple) systems have been
included in the search by taking into account the signal modulation
due to their orbits. Our upper limits are therefore the first measured
for 56 of these pulsars. For the remaining 22, our results improve on
previous upper limits by up to a factor of 10. For example, our tightest
upper limit on the gravitational strain is 2.6×10-25 for
PSR J1603-7202, and the equatorial ellipticity of PSR J2124 3358 is
less than 10-6. Furthermore, our strain upper limit for the
Crab pulsar is only 2.2 times greater than the fiducial spin-down limit.
Title: Publisher's Note: First cross-correlation analysis of
interferometric and resonant-bar gravitational-wave data for
stochastic backgrounds [Phys. Rev. DPRVDAQ0556-2821 76, 022001 (2007)]
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn,
K.; Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue,
L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.;
Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington,
A.; Bunkowski, A.; Buonanno, A.; Burgamy, M.; Burmeister, O.; Busby,
D.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo,
J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas, L.; Casey, M. M.;
Castaldi, G.; Cepeda, C.; Chalkey, E.; Charlton, P.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Chiadini, F.; Chin, D.; Chin, E.; Chow, J.;
Christensen, N.; Clark, J.; Cochrane, P.; Cokelaer, T.; Colacino,
C. N.; Coldwell, R.; Conte, R.; Cook, D.; Corbitt, T.; Coward, D.;
Coyne, D.; Creighton, J. D. E.; Creighton, T. D.; Croce, R. P.; Crooks,
D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple, J.; D'Ambrosio, E.;
Danzmann, K.; Davies, G.; Debra, D.; Degallaix, J.; Degree, M.; Demma,
T.; Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar, S.; Diaz, M.;
Dickson, J.; di Credico, A.; Diederichs, G.; Dietz, A.; Doomes, E. E.;
Drever, R. W. P.; Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens,
P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan,
Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos,
N.; Franzen, A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.;
Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L.; Gonzalez, G.; Gossler, S.; Grant, A.; Gras,
S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso,
R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.;
Hamilton, W. O.; Hammer, D.; Hanna, C.; Hanson, J.; Harms, J.; Harry,
G.; Harstad, E.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall,
A.; Heurs, M.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken,
D.; Hough, J.; Howell, E.; Hoyland, D.; Huttner, S. H.; Ingram, D.;
Innerhofer, E.; Ito, M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson,
B.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.;
Kalmus, P.; Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili,
F. Ya.; Kim, C.; King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.;
Kondrashov, V.; Kopparapu, R. K.; Kozak, D.; Krishnan, B.; Kwee, P.;
Lam, P. K.; Landry, M.; Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.;
Leiner, J.; Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lindquist, P.;
Lockerbie, N. A.; Longo, M.; Lormand, M.; Lubiński, M.; Luck, H.;
Machenschalk, B.; Macinnis, M.; Mageswaran, M.; Mailand, K.; Malec,
M.; Mandic, V.; Marano, S.; Marka, S.; Markowitz, J.; Maros, E.;
Martin, I.; Marx, J. N.; Mason, K.; Matone, L.; Matta, V.; Mavalvala,
N.; McCarthy, R.; McCaulley, B. J.; McClelland, D. E.; McGuire, S. C.;
McHugh, M.; McKenzie, K.; McNabb, J. W. C.; McWilliams, S.; Meier, T.;
Melissinos, A.; Mendell, G.; Mercer, R. A.; Meshkov, S.; Messaritaki,
E.; Messenger, C. J.; Meyers, D.; Mikhailov, E.; Miller, P.; Mitra,
S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa,
O.; Mohanty, S.; Moody, V.; Moreno, G.; Mossavi, K.; Mowlowry, C.;
Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.; Muller-Ebhardt,
H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash, T.; Newton,
G.; Nishizawa, A.; Numata, K.; O'Reilly, B.; O'Shaughnessy, R.;
Ottaway, D. J.; Overmier, H.; Owen, B. J.; Paik, H. -J.; Pan, Y.;
Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.;
Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi, M. V.;
Postiglione, F.; Prix, R.; Quetschke, V.; Raab, F.; Rabeling, D.;
Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Ramsuder, M.;
Rawlins, K.; Ray-Majumder, S.; Re, V.; Rehbein, H.; Reid, S.; Reitze,
D. H.; Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.; Robertson,
N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.; Rogan,
A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.; Rowan, S.;
Rudiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata, S.; Samidi,
M.; de La Jordana, L. Sancho; Sandberg, V.; Sannibale, V.; Saraf,
S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson, P. R.;
Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.; Schnabel, R.;
Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott, S. M.; Searle,
A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.; Shawhan,
P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.; Siemens, X.; Sigg,
D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.;
Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.; Strom, D. M.;
Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.;
Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor, R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thuring, A.; Tokmakov,
K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.;
Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.; Vallisneri,
M.; van den Broeck, C.; Varvella, M.; Vass, S.; Vecchio, A.; Veitch,
J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman,
S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Weaver, J.; Webber,
D.; Weber, A.; Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.;
Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.;
Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke,
B.; Wilmut, I.; Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.;
Woan, G.; Woods, D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.;
Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang,
J.; Zhang, L.; Zhang, P.; Zhao, C.; Zotov, N.; Zucker, M.; Zur Muhlen,
H.; Zweizig, J.
Bibcode: 2007PhRvD..76b9905A
Altcode:
No abstract at ADS
Title: First cross-correlation analysis of interferometric and
resonant-bar gravitational-wave data for stochastic backgrounds
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Arain,
M.; Araya, M.; Armandula, H.; Ashley, M.; Aston, S.; Aufmuth, P.;
Aulbert, C.; Babak, S.; Ballmer, S.; Bantilan, H.; Barish, B. C.;
Barker, C.; Barker, D.; Barr, B.; Barriga, P.; Barton, M. A.; Bayer,
K.; Belczynski, K.; Betzwieser, J.; Beyersdorf, P. T.; Bhawal, B.;
Bilenko, I. A.; Billingsley, G.; Biswas, R.; Black, E.; Blackburn,
K.; Blackburn, L.; Blair, D.; Bland, B.; Bogenstahl, J.; Bogue,
L.; Bork, R.; Boschi, V.; Bose, S.; Brady, P. R.; Braginsky, V. B.;
Brau, J. E.; Brinkmann, M.; Brooks, A.; Brown, D. A.; Bullington,
A.; Bunkowski, A.; Buonanno, A.; Burgamy, M.; Burmeister, O.; Busby,
D.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.; Cannizzo,
J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas, L.; Casey, M. M.;
Castaldi, G.; Cepeda, C.; Chalkey, E.; Charlton, P.; Chatterji, S.;
Chelkowski, S.; Chen, Y.; Chiadini, F.; Chin, D.; Chin, E.; Chow, J.;
Christensen, N.; Clark, J.; Cochrane, P.; Cokelaer, T.; Colacino,
C. N.; Coldwell, R.; Conte, R.; Cook, D.; Corbitt, T.; Coward, D.;
Coyne, D.; Creighton, J. D. E.; Creighton, T. D.; Croce, R. P.; Crooks,
D. R. M.; Cruise, A. M.; Cumming, A.; Dalrymple, J.; D'Ambrosio, E.;
Danzmann, K.; Davies, G.; Debra, D.; Degallaix, J.; Degree, M.; Demma,
T.; Dergachev, V.; Desai, S.; Desalvo, R.; Dhurandhar, S.; Díaz, M.;
Dickson, J.; di Credico, A.; Diederichs, G.; Dietz, A.; Doomes, E. E.;
Drever, R. W. P.; Dumas, J. -C.; Dupuis, R. J.; Dwyer, J. G.; Ehrens,
P.; Espinoza, E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan,
Y.; Fazi, D.; Fejer, M. M.; Finn, L. S.; Fiumara, V.; Fotopoulos,
N.; Franzen, A.; Franzen, K. Y.; Freise, A.; Frey, R.; Fricke, T.;
Fritschel, P.; Frolov, V. V.; Fyffe, M.; Galdi, V.; Garofoli, J.;
Gholami, I.; Giaime, J. A.; Giampanis, S.; Giardina, K. D.; Goda, K.;
Goetz, E.; Goggin, L.; González, G.; Gossler, S.; Grant, A.; Gras,
S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grosso,
R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson, R.; Hage, B.;
Hamilton, W. O.; Hammer, D.; Hanna, C.; Hanson, J.; Harms, J.; Harry,
G.; Harstad, E.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall,
A.; Heurs, M.; Hewitson, M.; Hild, S.; Hirose, E.; Hoak, D.; Hosken,
D.; Hough, J.; Howell, E.; Hoyland, D.; Huttner, S. H.; Ingram, D.;
Innerhofer, E.; Ito, M.; Itoh, Y.; Ivanov, A.; Jackrel, D.; Johnson,
B.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.; Ju, L.;
Kalmus, P.; Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.; Kawabe,
K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Keppel, D. G.; Khalili,
F. Ya.; Kim, C.; King, P.; Kissel, J. S.; Klimenko, S.; Kokeyama, K.;
Kondrashov, V.; Kopparapu, R. K.; Kozak, D.; Krishnan, B.; Kwee, P.;
Lam, P. K.; Landry, M.; Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.;
Leiner, J.; Leonhardt, V.; Leonor, I.; Libbrecht, K.; Lindquist, P.;
Lockerbie, N. A.; Longo, M.; Lormand, M.; Lubiński, M.; Lück, H.;
Machenschalk, B.; Macinnis, M.; Mageswaran, M.; Mailand, K.; Malec,
M.; Mandic, V.; Marano, S.; Márka, S.; Markowitz, J.; Maros, E.;
Martin, I.; Marx, J. N.; Mason, K.; Matone, L.; Matta, V.; Mavalvala,
N.; McCarthy, R.; McCaulley, B. J.; McClelland, D. E.; McGuire, S. C.;
McHugh, M.; McKenzie, K.; McNabb, J. W. C.; McWilliams, S.; Meier, T.;
Melissinos, A.; Mendell, G.; Mercer, R. A.; Meshkov, S.; Messaritaki,
E.; Messenger, C. J.; Meyers, D.; Mikhailov, E.; Miller, P.; Mitra,
S.; Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Miyakawa,
O.; Mohanty, S.; Moody, V.; Moreno, G.; Mossavi, K.; Mowlowry, C.;
Moylan, A.; Mudge, D.; Mueller, G.; Mukherjee, S.; Müller-Ebhardt,
H.; Munch, J.; Murray, P.; Myers, E.; Myers, J.; Nash, T.; Nettles,
D.; Newton, G.; Nishizawa, A.; Numata, K.; O'Reilly, B.; O'Shaughnessy,
R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Paik, H. -J.; Pan, Y.;
Papa, M. A.; Parameshwaraiah, V.; Patel, P.; Pedraza, M.; Penn, S.;
Pierro, V.; Pinto, I. M.; Pitkin, M.; Pletsch, H.; Plissi, M. V.;
Postiglione, F.; Prix, R.; Quetschke, V.; Raab, F.; Rabeling, D.;
Radkins, H.; Rahkola, R.; Rainer, N.; Rakhmanov, M.; Ramsunder, M.;
Rawlins, K.; Ray-Majumder, S.; Re, V.; Rehbein, H.; Reid, S.; Reitze,
D. H.; Ribichini, L.; Riesen, R.; Riles, K.; Rivera, B.; Robertson,
N. A.; Robinson, C.; Robinson, E. L.; Roddy, S.; Rodriguez, A.;
Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie, J.; Route, R.;
Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan, K.; Sakata,
S.; Samidi, M.; Sancho de La Jordana, L.; Sandberg, V.; Sannibale,
V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.; Saulson,
P. R.; Savage, R.; Savov, P.; Schediwy, S.; Schilling, R.; Schnabel,
R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott, S. M.;
Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.; Sengupta, A. S.;
Shawhan, P.; Shoemaker, D. H.; Sibley, A.; Sidles, J. A.; Siemens, X.;
Sigg, D.; Sinha, S.; Sintes, A. M.; Slagmolen, B. J. J.; Slutsky, J.;
Smith, J. R.; Smith, M. R.; Somiya, K.; Strain, K. A.; Strom, D. M.;
Stuver, A.; Summerscales, T. Z.; Sun, K. -X.; Sung, M.; Sutton, P. J.;
Takahashi, H.; Tanner, D. B.; Tarallo, M.; Taylor, R.; Taylor, R.;
Thacker, J.; Thorne, K. A.; Thorne, K. S.; Thüring, A.; Tokmakov,
K. V.; Torres, C.; Torrie, C.; Traylor, G.; Trias, M.; Tyler, W.;
Ugolini, D.; Ungarelli, C.; Urbanek, K.; Vahlbruch, H.; Vallisneri,
M.; van den Broeck, C.; Varvella, M.; Vass, S.; Vecchio, A.; Veitch,
J.; Veitch, P.; Villar, A.; Vorvick, C.; Vyachanin, S. P.; Waldman,
S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.; Weaver, J.; Webber,
D.; Weber, A.; Weidner, A.; Weinert, M.; Weinstein, A.; Weiss, R.;
Wen, S.; Wette, K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.;
Whiting, B. F.; Wilkinson, C.; Willems, P. A.; Williams, L.; Willke,
B.; Wilmut, I.; Winkler, W.; Wipf, C. C.; Wise, S.; Wiseman, A. G.;
Woan, G.; Woods, D.; Wooley, R.; Worden, J.; Wu, W.; Yakushin, I.;
Yamamoto, H.; Yan, Z.; Yoshida, S.; Yunes, N.; Zanolin, M.; Zhang, J.;
Zhang, L.; Zhang, P.; Zhao, C.; Zotov, N.; Zucker, M.; Zur Mühlen,
H.; Zweizig, J.
Bibcode: 2007PhRvD..76b2001A
Altcode: 2007gr.qc.....3068L
Data from the LIGO Livingston interferometer and the ALLEGRO
resonant-bar detector, taken during LIGO’s fourth science run,
were examined for cross correlations indicative of a stochastic
gravitational-wave background in the frequency range 850 950 Hz,
with most of the sensitivity arising between 905 and 925 Hz. ALLEGRO
was operated in three different orientations during the experiment
to modulate the relative sign of gravitational-wave and environmental
correlations. No statistically significant correlations were seen in
any of the orientations, and the results were used to set a Bayesian
90% confidence level upper limit of Ωgw(f)≤1.02,
which corresponds to a gravitational-wave strain at 915 Hz of
1.5×10-23Hz-1/2. In the traditional units of
h1002Ωgw(f), this is a limit of 0.53,
2 orders of magnitude better than the previous direct limit at these
frequencies. The method was also validated with successful extraction
of simulated signals injected in hardware and software.
Title: λ Boo stars among the γ Dor-type pulsators: the cases of
HD 218427 and HD 239276
Authors: Rodríguez, E.; Suárez, J. C.; Moya, A.; Dupret, M. A.;
Grigahcène, A.; Costa, V.; López-González, M. J.; Zhou, A. -Y.;
Amado, P. J.; Poretti, E.; Wei, J. -Y.; Fan, Y.
Bibcode: 2007CoAst.150..131R
Altcode:
No abstract at ADS
Title: Splitting Flux Ropes: Modeling The Eruption Of Magnetic
Structures On The Sun
Authors: Gibson, Sarah; Fan, Y.
Bibcode: 2007AAS...210.5806G
Altcode: 2007BAAS...39..168G
Coronal mass ejections (CMEs) and their associated space weather
manifestations are routinely interpreted as possessing a helical
magnetic flux rope structure. An ongoing controversy remains, however,
as to whether a precursor flux rope exists as a coronal equilibrium
state prior to eruption, or whether it is formed during eruption. This
is an important question to resolve, since CME initiation models and
space weather predictions depend upon a clear understanding of the
configuration of pre-CME magnetic fields and their evolution during
eruption. We will describe an alternative which lies between the
two extremes of a totally erupting, pre-existing rope, and a rope
that forms completely in situ during eruption, i.e., a precursor flux
rope that splits in two and reconnects with surrounding fields during
eruption. We consider the implications of such a "partially-expelled
flux rope" model for a range of CME-related observations, including
partially-erupting filaments, the evolution of post-flare loops and
flare ribbon morphologies, and transient coronal holes.
Title: Summertime European heat and drought waves induced by
wintertime Mediterranean rainfall deficit
Authors: Vautard, R.; Yiou, P.; D'Andrea, F.; de Noblet, N.; Viovy,
N.; Cassou, C.; Polcher, J.; Ciais, P.; Kageyama, M.; Fan, Y.
Bibcode: 2007GeoRL..34.7711V
Altcode:
The risk of extreme heat waves in Europe like the unprecedented one of
summer 2003 is likely to increase in the future, calling for increased
understanding of these phenomena. From an analysis of meteorological
records over 58 years, we show that hot summers are preceded by
winter rainfall deficits over Southern Europe. Subsequent drought
and heat spreads northward throughout Europe in early summer, due to
atmospheric transport of anomalously warm and dry air from Southern
Europe in southerly wind episodes. This is shown by the observations
and supported by mesoscale meteorological sensitivity simulations
for Summer 1994. Moreover previous winter and early spring rainfall
frequency in the Mediterranean regions is correlated with summer
temperature in central continental Europe. These results emphasize
the critical role of the water reservoir in the soil of continental
Mediterranean areas for the maintenance of European climate.
Title: Searching for a Stochastic Background of Gravitational Waves
with the Laser Interferometer Gravitational-Wave Observatory
Authors: Abbott, B.; Abbott, R.; Adhikari, R.; Agresti, J.; Ajith,
P.; Allen, B.; Amin, R.; Anderson, S. B.; Anderson, W. G.; Araya, M.;
Armandula, H.; Ashley, M.; Aston, S.; Aulbert, C.; Babak, S.; Ballmer,
S.; Barish, B. C.; Barker, C.; Barker, D.; Barr, B.; Barriga, P.;
Barton, M. A.; Bayer, K.; Belczynski, K.; Betzwieser, J.; Beyersdorf,
P.; Bhawal, B.; Bilenko, I. A.; Billingsley, G.; Black, E.; Blackburn,
K.; Blackburn, L.; Blair, D.; Bland, B.; Bogue, L.; Bork, R.; Bose,
S.; Brady, P. R.; Braginsky, V. B.; Brau, J. E.; Brooks, A.; Brown,
D. A.; Bullington, A.; Bunkowski, A.; Buonanno, A.; Burman, R.;
Busby, D.; Byer, R. L.; Cadonati, L.; Cagnoli, G.; Camp, J. B.;
Cannizzo, J.; Cannon, K.; Cantley, C. A.; Cao, J.; Cardenas, L.;
Casey, M. M.; Cepeda, C.; Charlton, P.; Chatterji, S.; Chelkowski,
S.; Chen, Y.; Chin, D.; Chin, E.; Chow, J.; Christensen, N.; Cokelaer,
T.; Colacino, C. N.; Coldwell, R.; Cook, D.; Corbitt, T.; Coward, D.;
Coyne, D.; Creighton, J. D. E.; Creighton, T. D.; Crooks, D. R. M.;
Cruise, A. M.; Cumming, A.; Cutler, C.; Dalrymple, J.; D'Ambrosio,
E.; Danzmann, K.; Davies, G.; de Vine, G.; DeBra, D.; Degallaix, J.;
Dergachev, V.; Desai, S.; DeSalvo, R.; Dhurandar, S.; Di Credico,
A.; Díaz, M.; Dickson, J.; Diederichs, G.; Dietz, A.; Doomes, E. E.;
Drever, R. W. P.; Dumas, J. -C.; Dupuis, R. J.; Ehrens, P.; Elliffe,
E.; Etzel, T.; Evans, M.; Evans, T.; Fairhurst, S.; Fan, Y.; Fejer,
M. M.; Finn, L. S.; Fotopoulos, N.; Franzen, A.; Franzen, K. Y.;
Frey, R. E.; Fricke, T.; Fritschel, P.; Frolov, V. V.; Fyffe, M.;
Garofoli, J.; Gholami, I.; Giaime, J. A.; Giampanis, S.; Goda, K.;
Goetz, E.; Goggin, L.; González, G.; Gossler, S.; Grant, A.; Gras,
S.; Gray, C.; Gray, M.; Greenhalgh, J.; Gretarsson, A. M.; Grimmett,
D.; Grosso, R.; Grote, H.; Grunewald, S.; Guenther, M.; Gustafson,
R.; Hage, B.; Hanna, C.; Hanson, J.; Hardham, C.; Harms, J.; Harry,
G.; Harstad, E.; Hayler, T.; Heefner, J.; Heng, I. S.; Heptonstall,
A.; Heurs, M.; Hewitson, M.; Hild, S.; Hindman, N.; Hirose, E.; Hoak,
D.; Hoang, P.; Hosken, D.; Hough, J.; Howell, E.; Hoyland, D.; Hua,
W.; Huttner, S.; Ingram, D.; Ito, M.; Itoh, Y.; Ivanov, A.; Jackrel,
D.; Johnson, B.; Johnson, W. W.; Jones, D. I.; Jones, G.; Jones, R.;
Ju, L.; Kalmus, P.; Kalogera, V.; Kasprzyk, D.; Katsavounidis, E.;
Kawabe, K.; Kawamura, S.; Kawazoe, F.; Kells, W.; Khalili, F. Ya.;
Khan, A.; Kim, C.; King, P.; Klimenko, S.; Kokeyama, K.; Kondrashov,
V.; Koranda, S.; Kozak, D.; Krishnan, B.; Kwee, P.; Lam, P. K.;
Landry, M.; Lantz, B.; Lazzarini, A.; Lee, B.; Lei, M.; Leonhardt,
V.; Leonor, I.; Libbrecht, K.; Lindquist, P.; Lockerbie, N. A.;
Lormand, M.; Lubiński, M.; Lück, H.; Machenschalk, B.; MacInnis,
M.; Mageswaran, M.; Mailand, K.; Malec, M.; Mandic, V.; Márka, S.;
Markowitz, J.; Maros, E.; Martin, I.; Marx, J. N.; Mason, K.; Matone,
L.; Mavalvala, N.; McCarthy, R.; McClelland, D. E.; McGuire, S. C.;
McHugh, M.; McKenzie, K.; McNabb, J. W. C.; Meier, T.; Melissinos, A.;
Mendell, G.; Mercer, R. A.; Meshkov, S.; Messaritaki, E.; Messenger,
C. J.; Meyers, D.; Mikhailov, E.; Mitra, S.; Mitrofanov, V. P.;
Mitselmakher, G.; Mittleman, R.; Miyakawa, O.; Mohanty, S.; Moreno,
G.; Mossavi, K.; MowLowry, C.; Moylan, A.; Mudge, D.; Mueller, G.;
Müller-Ebhardt, H.; Mukherjee, S.; Munch, J.; Murray, P.; Myers,
E.; Myers, J.; Newton, G.; Numata, K.; O'Reilly, B.; O'Shaughnessy,
R.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pan, Y.; Papa, M. A.;
Parameshwaraiah, V.; Pedraza, M.; Penn, S.; Pitkin, M.; Plissi, M. V.;
Prix, R.; Quetschke, V.; Raab, F.; Rabeling, D.; Radkins, H.; Rahkola,
R.; Rakhmanov, M.; Rawlins, K.; Ray-Majumder, S.; Re, V.; Rehbein,
H.; Reid, S.; Reitze, D. H.; Ribichini, L.; Riesen, R.; Riles, K.;
Rivera, B.; Robertson, D. I.; Robertson, N. A.; Robinson, C.; Roddy,
S.; Rodriguez, A.; Rogan, A. M.; Rollins, J.; Romano, J. D.; Romie,
J.; Route, R.; Rowan, S.; Rüdiger, A.; Ruet, L.; Russell, P.; Ryan,
K.; Sakata, S.; Samidi, M.; de la Jordana, L. Sancho; Sandberg, V.;
Sannibale, V.; Saraf, S.; Sarin, P.; Sathyaprakash, B. S.; Sato, S.;
Saulson, P. R.; Savage, R.; Schediwy, S.; Schilling, R.; Schnabel,
R.; Schofield, R.; Schutz, B. F.; Schwinberg, P.; Scott, S. M.;
Seader, S. E.; Searle, A. C.; Sears, B.; Seifert, F.; Sellers, D.;
Sengupta, A. S.; Shawhan, P.; Sheard, B.; Shoemaker, D. H.; Sibley,
A.; Siemens, X.; Sigg, D.; Sintes, A. M.; Slagmolen, B.; Slutsky,
J.; Smith, J.; Smith, M. R.; Sneddon, P.; Somiya, K.; Speake, C.;
Spjeld, O.; Strain, K. A.; Strom, D. M.; Stuver, A.; Summerscales,
T.; Sun, K.; Sung, M.; Sutton, P. J.; Tanner, D. B.; Tarallo, M.;
Taylor, R.; Taylor, R.; Thacker, J.; Thorne, K. A.; Thorne, K. S.;
Thüring, A.; Tokmakov, K. V.; Torres, C.; Torrie, C.; Traylor,
G.; Trias, M.; Tyler, W.; Ugolini, D.; Ungarelli, C.; Vahlbruch,
H.; Vallisneri, M.; Varvella, M.; Vass, S.; Vecchio, A.; Veitch,
J.; Veitch, P.; Vigeland, S.; Villar, A.; Vorvick, C.; Vyachanin,
S. P.; Waldman, S. J.; Wallace, L.; Ward, H.; Ward, R.; Watts, K.;
Webber, D.; Weidner, A.; Weinstein, A.; Weiss, R.; Wen, S.; Wette,
K.; Whelan, J. T.; Whitbeck, D. M.; Whitcomb, S. E.; Whiting, B. F.;
Wilkinson, C.; Willems, P. A.; Willke, B.; Wilmut, I.; Winkler, W.;
Wipf, C. C.; Wise, S.; Wiseman, A. G.; Woan, G.; Woods, D.; Wooley,
R.; Worden, J.; Wu, W.; Yakushin, I.; Yamamoto, H.; Yan, Z.; Yoshida,
S.; Yunes, N.; Zanolin, M.; Zhang, L.; Zhao, C.; Zotov, N.; Zucker,
M.; zur Mühlen, H.; Zweizig, J.; LIGO Scientific Collaboration
Bibcode: 2007ApJ...659..918A
Altcode: 2006astro.ph..8606L
The Laser Interferometer Gravitational-Wave Observatory (LIGO) has
performed the fourth science run, S4, with significantly improved
interferometer sensitivities with respect to previous runs. Using
data acquired during this science run, we place a limit on the
amplitude of a stochastic background of gravitational waves. For
a frequency independent spectrum, the new Bayesian 90% upper
limit is ΩGW×[H0/(72 km s-1
Mpc-1)2<6.5×10-5. This is
currently the most sensitive result in the frequency range 51-150 Hz,
with a factor of 13 improvement over the previous LIGO result. We
discuss the complementarity of the new result with other constraints
on a stochastic background of gravitational waves, and we investigate
implications of the new result for different models of this background.
Title: The Evolving Sigmoid: Evidence for Magnetic Flux Ropes in
the Corona Before, During, and after CMES
Authors: Gibson, S. E.; Fan, Y.; Török, T.; Kliem, B.
Bibcode: 2007sdeh.book..131G
Altcode:
No abstract at ADS
Title: Coronal prominence structure and dynamics: A magnetic flux
rope interpretation
Authors: Gibson, S. E.; Fan, Y.
Bibcode: 2006JGRA..11112103G
Altcode:
The solar prominence is an example of a space physics phenomenon
that can be modeled as a twisted magnetic flux tube or magnetic flux
"rope." In such models the prominence is one observable part of
a larger magnetic structure capable of storing magnetic energy to
drive eruptions. We show how a flux rope model explains a range of
observations of prominences and associated structures such as cavities
and soft X-ray sigmoids and discuss in particular the observational
and dynamic consequences of three-dimensional reconnections in and
around the evolving magnetic flux rope. We demonstrate that the
flux rope model can describe the prominence's preeruption structure
and dynamics, loss of equilibrium, and behavior during and after an
eruption in which part of the flux rope is expelled from the corona.
Title: Asteroseismology of the new multiperiodic γ Dor variable
HD 239276
Authors: Rodríguez, E.; Costa, V.; Zhou, A. -Y.; Grigahcène, A.;
Dupret, M. A.; Suárez, J. C.; Moya, A.; López-González, M. J.;
Wei, J. -Y.; Fan, Y.
Bibcode: 2006A&A...456..261R
Altcode:
The variability of HD 239276 was suspected photometrically nearly
twenty years ago, but was confirmed with new observations obtained in
2001 during a two-site photometric campaign carried out from Spain,
in uvbyβ Strömgren-Crawford photometry, and China, using the Johnson
V filter. Two low-dispersion spectra were also collected. The results
establish this star as a new multiperiodic γ Dor-type pulsator with
deficiency in metallicity. Its possible λ Boo nature is discussed. The
frequency analysis shows three pulsational frequencies as significant,
but some more are probably present among the residuals. The method
based on phase shifts and amplitude ratios in multicolour photometry is
used to identify the excited modes with non-adiabatic time-dependent
convection models. A very good agreement between the theoretical
and observed amplitude ratios is obtained and the two main modes are
identified as l=1 modes. Nevertheless, our results do not allow us to
discriminate between a solar abundance and a metal deficient nature
for this star. The frequency ratio method is further used for the
identification of the modes. The results suggest low metallicity for
this star, but a λ Boo nature may be not ruled out.
Title: The Evolving Sigmoid: Evidence for Magnetic Flux Ropes in
the Corona Before, During, and After CMES
Authors: Gibson, S. E.; Fan, Y.; Török, T.; Kliem, B.
Bibcode: 2006SSRv..124..131G
Altcode: 2007SSRv..tmp...52G
It is generally accepted that the energy that drives coronal mass
ejections (CMEs) is magnetic in origin. Sheared and twisted coronal
fields can store free magnetic energy which ultimately is released
in the CME. We explore the possibility of the specific magnetic
configuration of a magnetic flux rope of field lines that twist
about an axial field line. The flux rope model predicts coronal
observables, including heating along forward or inverse S-shaped,
or sigmoid, topological surfaces. Therefore, studying the observed
evolution of such sigmoids prior to, during, and after the CME gives
us crucial insight into the physics of coronal storage and release of
magnetic energy. In particular, we consider (1) soft-X-ray sigmoids,
both transient and persistent; (2) The formation of a current sheet
and cusp-shaped post-flare loops below the CME; (3) Reappearance of
sigmoids after CMEs; (4) Partially erupting filaments; (5) Magnetic
cloud observations of filament material.
Title: Compensation of Strong Thermal Lensing in High-Optical-Power
Cavities
Authors: Zhao, C.; Degallaix, J.; Ju, L.; Fan, Y.; Blair, D. G.;
Slagmolen, B. J. J.; Gray, M. B.; Lowry, C. M. Mow; McClelland,
D. E.; Hosken, D. J.; Mudge, D.; Brooks, A.; Munch, J.; Veitch, P. J.;
Barton, M. A.; Billingsley, G.
Bibcode: 2006PhRvL..96w1101Z
Altcode: 2006gr.qc.....2096Z
In an experiment to simulate the conditions in high optical power
advanced gravitational wave detectors, we show for the first time
that the time evolution of strong thermal lenses follows the predicted
infinite sum of exponentials (approximated by a double exponential), and
that such lenses can be compensated using an intracavity compensation
plate heated on its cylindrical surface. We show that high finesse
∼1400 can be achieved in cavities with internal compensation plates,
and that mode matching can be maintained. The experiment achieves
a wave front distortion similar to that expected for the input test
mass substrate in the Advanced Laser Interferometer Gravitational Wave
Observatory, and shows that thermal compensation schemes are viable. It
is also shown that the measurements allow a direct measurement of
substrate optical absorption in the test mass and the compensation
plate.
Title: VizieR Online Data Catalog: Differential uvby photometry of
HD 239276 (Rodriguez+, 2006)
Authors: Rodriguez, E.; Costa, V.; Zhou, A. -Y.; Grigahcene, A.;
Dupret, M. A.; Suárez, J. C.; Moya, A.; Lopez-Gonzalez, M. J.; Wei,
J. -Y.; Fan, Y.
Bibcode: 2006yCat..34560261R
Altcode:
Table 2 contents 139 simultaneous measurements collected during in each
of the four uvby colours of the Stromgren photometric system for the
Gamma Doradus variable HD 239276. The observations were carried out
by the authors through the years 1986-1987 using the 0.90m telescope
at Sierra Nevada Observatory, Spain and the six-channel uvby-Hbeta
spectrograph photometer for simultaneous measurements in uvby or in
the narrow and wide Hbeta channels, respectively. Table 3 contents
101 measurements collected in the V filter of the Johnson photometric
system for the Gamma Doradus variable HD 239276. The observations were
carried out by the authors through the year 2001 using the three-channel
high-speed photoelectric photometer P45-A mounted on the 0.85m telescope
at Xinglong Station of the Beijing Astronomical Observatory, China. Table 4 contents 582 simultaneous measurements collected during in
each of the four uvby colours of the Stromgren photometric system for
the Gamma Doradus variable HD 239276. The observations were carried
out by the authors through the year 2001 using the 0.90m telescope
at Sierra Nevada Observatory, Spain and the six-channel uvby-Hbeta
spectrograph photometer for simultaneous measurements in uvby or in
the narrow and wide Hbeta channels, respectively. (3 data files).
Title: Is Reconnection Necessary for Kinked CME Onset?
Authors: Rachmeler, Laurel; DeForest, C. E.; Gibson, S. E.; Fan, Y.
Bibcode: 2006SPD....37.0902R
Altcode: 2006BAAS...38..236R
We present initial results from a controlled numerical experiment to
determine whether CME onset requires reconnection or can be driven
primarily by loss of plasma equilibrium. The early onset of the kink
instability proceeds with little reconnection in traditional MHD
simulations, but still at a nonzero rate. After the initial onset
of the instability, reconnection proceeds rapidly across the newly
formed current sheet, contributing to the ejection of the kink. We
have simulated the kink instability driven purely by loss of plasma
equilibrium - in the absence of numerical reconnection - as an early
step to understanding the role of reconnection in CME evolution.
Title: On the Nature of the X-Ray Bright Core in a Stable Filament
Channel
Authors: Fan, Y.; Gibson, S. E.
Bibcode: 2006ApJ...641L.149F
Altcode:
In a search for the cause of the intense heating revealed by X-ray
emission in filament channels, we have simulated the evolution of
a twisted toroidal flux rope emerging quasi-statically into the
corona. Initially, the simulated flux rope remains confined in
equilibrium as the stored magnetic energy increases. With enough
twist buildup, there is a sudden catastrophic loss of equilibrium
and total expulsion of the flux rope. We focused on the quasi-static
phase in which a current sheet forms within the flux rope cavity,
along the so-called bald-patch separatrix surface (BPSS). This
comprises an envelope of field lines that graze the anchoring lower
boundary, enclosing the detached helical field that supports the
prominence. Significant magnetic energy dissipation and heating are
expected to center around such current sheets. The heating that should
result provides a plausible explanation for the hot X-ray sources,
although they appear to be colocated with cool material. If our
physical picture is correct, then the development of X-ray ``bright
cores'' or ``sigmoids'' in a filament channel suggests the presence of
a BPSS separating the helical field of a twisted flux rope in stable
confinement from the surrounding untwisted fields.
Title: Status of the Australian Consortium for Interferometric
Gravitational Astronomy
Authors: McClelland, D. E.; Scott, S. M.; Gray, M. B.; Searle,
A. C.; Goßler, S.; Slagmolen, B. J. J.; Dickson, J.; Chow, J. H.;
de Vine, G.; McKenzie, K.; Mow-Lowry, C. M.; Moylan, A.; Rabeling,
D. S.; Sheard, B. S.; Cumpston, J.; Wette, K.; Blair, D. G.; Ju, L.;
Burman, R.; Coward, D.; Zhao, C.; Barrigo, P.; Chin, E.; Degallaix,
J.; Fan, Y.; Gras, S.; Howell, E.; Lee, B.; Schediwy, S.; Yan, Z.;
Munch, J.; Veitch, P. J.; Mudge, D.; Brooks, A.; Hosken, D.
Bibcode: 2006CQGra..23S..41M
Altcode:
We report the status of research and development being undertaken
by the members of the Australian Consortium for Interferometric
Gravitational Astronomy.
Title: Gingin High Optical Power Test Facility
Authors: Zhao, C.; Blair, D. G.; Barrigo, P.; Degallaix, J.; Dumas,
J. -C.; Fan, Y.; Gras, S.; Ju, L.; Lee, B.; Schediwy, S.; Yan, Z.;
McClelland, D. E.; Scott, S. M.; Gray, M. B.; Searle, A. C.; Gossler,
S.; Slagmolen, B. J. J.; Dickson, J.; McKenzie, K.; Mow-Lowry, C.;
Moylan, A.; Rabeling, D.; Cumpston, J.; Wette, K.; Munch, J.; Veitch,
P. J.; Mudge, D.; Brooks, A.; Hosken, D.
Bibcode: 2006JPhCS..32..368Z
Altcode:
The Australian Consortium for Gravitational Wave Astronomy (ACIGA) in
collaboration with LIGO is developing a high optical power research
facility at the AIGO site, Gingin, Western Australia. Research at
the facility will provide solutions to the problems that advanced
gravitational wave detectors will encounter with extremely high
optical power. The problems include thermal lensing and parametric
instabilities. This article will present the status of the facility
and the plan for the future experiments.
Title: The Partial Expulsion of a Magnetic Flux Rope
Authors: Gibson, S. E.; Fan, Y.
Bibcode: 2006ApJ...637L..65G
Altcode:
We demonstrate the partial expulsion of a three-dimensional magnetic
flux rope, in which an upper, escaping rope is separated from a lower,
surviving rope by cusped, reconnecting loop field lines. We use the
three-dimensional magnetohydrodynamic model recently presented by Fan,
extended to examine the erupting rope's end state. As in that work, the
modeled flux rope in spherical coordinates erupts when enough twist has
emerged to induce a loss of equilibrium. After multiple reconnections at
current sheets that form during the eruption, the rope breaks in two,
so that only a part of it escapes. We consider the details of how this
separation occurs and discuss the observational significance of such
a partially expelled flux rope for partially erupting filaments and
re-forming X-ray sigmoids.
Title: The emergence and evolution of twisted coronal magnetic fields:
comparing models and observations
Authors: Gibson, S.; Fan, Y.
Bibcode: 2006cosp...36.1839G
Altcode: 2006cosp.meet.1839G
We will present new results comparing coronal plasma observations to
observables predicted by MHD models of twisted magnetic structures in
the corona We will focus on their emergence through the photosphere
their subsequent equilibrium states and their eruptive properties We
will show that observations of coronal filaments before during and
after eruptions can be explained In particular we will demonstrate
that the observed relationship between filament filament cavity and
hot X-ray sources such as sigmoids are reproduced for a variety of
twisted magnetic structures in equilibrium We will also demonstrate that
modeled loss of equilibrium and eruption of such magnetic structures
can explain a range of observed behaviors of filaments their cavities
and X-ray sigmoids during and after eruptions These include observations
of partially-erupting filaments and the immediate reformation of X-ray
sigmoids after an eruption
Title: Tolerance of yeast to ethanol decreased after space flight
Authors: Xia, B.; Sun, Y.; Yi, Z.; He, J.; Jiang, X.; Fan, Y.;
Zhuang, F.
Bibcode: 2006cosp...36.1911X
Altcode: 2006cosp.meet.1911X
Background Saccharomyces cerevisiae is an important industry
microorganism and the tolerance to ethanol is one of the main
characteristics to decide its yield potential USA researchers reported
that E coli cells growing in simulated microgravity environment were
much more resistant to the growth-inhibitory and production-inhibitory
effects of ethanol than cells growing in shaken flasks In this
research we will investigate the tolerance of yeast to ethanol in real
microgravity environment Method S cerevisiae cells were cultured for
18 d in YPD medium containing various concentrations of ethanol 0 6
8 and 10 V V during the China s 22 th recoverable satellite mission
Optical density living cells counts metabolism and morphology in
each culture were measured S cerevisiae cells were exposed to 20 V V
ethanol to investigate the tolerance to ethanol Result The biomass
of cells culture at 0 times g is 40 lower than that of the ground
control in medium of YPD With the increase of concentration of ethanol
in medium the rate of living cells decreased steeply especially in 0
times g culture The living cell of 0 times g is 65 5 lower than the
control cells The viability of 0 times g cells and ground control
cells exposed to 20 ethanol for 6h is 1 7 and 10 5 respectively No
remarkable differences were found in the cell morphology and glucose
consumption Conclusion These results suggest that under
Title: The Emergence and Evolution of Twisted Magnetic Flux Ropes
in the Solar Corona
Authors: Fan, Y.; Gibson, S. E.; Manchester, W.
Bibcode: 2005ESASP.596E..26F
Altcode: 2005ccmf.confE..26F
No abstract at ADS
Title: Coronal Mass Ejections as Loss of Confinement of Kinked
Magnetic Flux Ropes
Authors: Fan, Y.
Bibcode: 2005ApJ...630..543F
Altcode:
We perform MHD simulations in a spherical geometry of the evolution
of the three-dimensional coronal magnetic field as a twisted magnetic
flux tube emerges slowly into the low-β corona previously occupied
by a potential arcade. We study the evolution of the emerged flux
rope in the corona as its twist and magnetic energy increases due to
flux emergence. We find two distinct stages of the evolution. The
earlier evolution is nearly quasi-static, with the flux rope being
able to settle into an neighboring equilibrium when the emergence is
stopped. When the twist in the emerged flux rope reaches some critical
level, the flux rope is found to undergo kink motion and erupt through
the arcade field at a localized region, with most of the arcade field
remaining closed. The nonlinear evolution of the kink instability
facilitates the loss of confinement of the flux rope by changing its
orientation at the apex such that it becomes easier for the flux rope
to part and erupt through the arcade. The eruption of the writhing
flux rope produces prominence field with Λ-shaped and cross-legged
morphologies that have been seen in the cores of some CMEs.
Title: Evolution of Twisted Magnetic Flux Robes Emerging into the
Solar Corona (Invited)
Authors: Fan, Y.; Gibson, S. E.
Bibcode: 2005ESASP.592..241F
Altcode: 2005ESASP.592E..36F; 2005soho...16E..36F
No abstract at ADS
Title: On the Availability of Sufficient Twist in Solar Active
Regions to Trigger the Kink Instability
Authors: Leka, K. D.; Fan, Y.; Barnes, G.
Bibcode: 2005ApJ...626.1091L
Altcode:
The question of whether there is sufficient magnetic twist in solar
active regions for the onset of the kink instability is examined
using a ``blind test'' of analysis methods commonly used to interpret
observational data. ``Photospheric magnetograms'' are constructed from
a recently developed numerical simulation of a kink-unstable emerging
flux rope with nearly constant (negative) wind. The calculation of the
best-fit linear force-free parameter αbest is applied,
with the goal of recovering the model input helicity. It is shown
that for this simple magnetic structure, three effects combine to
produce an underestimation of the known helicity: (1) the influence of
horizontal fields with lower local α values within the flux rope; (2)
an assumed simple relation between αbest and the winding
rate q does not apply to nonaxis fields in a flux rope that is not
thin; and (3) the difficulty in interpreting the force-free twist
parameter measured for a field that is forced. A different method to
evaluate the magnetic twist in active region flux ropes is presented,
which is based on evaluating the peak α value at the flux rope
axis. When applied to data from the numerical simulation, the twist
component of the magnetic helicity is essentially recovered. Both
the αbest and the new αpeak methods are then
applied to observational photospheric vector magnetic field data of
NOAA AR 7201. The αbest approach is then confounded further
in NOAA AR 7201 by a distribution of α that contains both signs, as
is generally observed in active regions. The result from the proposed
αpeak approach suggests that a larger magnetic twist is
present in this active region's δ-spot than would have been inferred
from αbest, by at least a factor of 3. It is argued that
the magnetic fields in localized active region flux ropes may indeed
carry greater than 2π winds, and thus the kink instability is a
possible trigger mechanism for solar flares and coronal mass ejections.
Title: CME Onset Due to Loss of Confinement of Twisted Magnetic
Flux Ropes
Authors: Fan, Y.; Gibson, S.
Bibcode: 2005AGUSMSP23A..08F
Altcode:
We present MHD simulations in both 2D axisymmetric and 3D spherical
geometries of the evolution of a twisted magnetic flux rope emerging
into the low-β corona previously occupied by a potential arcade
field. We describe both the initial quasi-static evolution whereby
stable equilibrium structures can form with stored free magnetic
energy, and the eventual loss of confinement or equilibrium of the
twisted magnetic flux rope as sufficient twist is being transported
into the corona, resulting in the onset of a CME. We investigate how
the evolution and the loss of equilibrium for a 3D line-tied flux rope
differ compared to the case of a 2D axisymmetric flux rope.
Title: The Source of Magnetic Shear in CME Source Regions
Authors: Manchester, W. B.; Fan, Y.; Gombosi, T. I.
Bibcode: 2005AGUSMSH53B..03M
Altcode:
We present a two and three-dimensional numerical magnetohydrodynamic
simulations of magnetic flux emergence in three geometries including
horizontal layers, arcades and flux ropes. In all cases, the magnetic
structures are initially embedded in gravitationally stratified plasma
in non-force-free states in which plasma pressure confines the magnetic
fields. As the magnetic fields buoyantly rise, they greatly expand in
the reduced pressure of the upper atmosphere. In all cases, we find
that the legs of ascending bipole loop structures move in opposite
horizontal directions drawing the magnetic field parallel to the
neutral line. The shearing motions naturally occur as the magnetic
field expands in the stratified atmosphere which produces a gradient in
the axial field. This gradient results in a horizontal Lorentz force
that drives the legs of the bipole loop in opposite directions. The
shearing motions transport axial flux and energy from the submerged
portion of the field to the expanding portion, which may cause it to
violently erupt. This shearing process is very robust and explains the
highly sheared state of the magnetic field associated with prominences,
flares and coronal mass ejections.
Title: Dynamics of Emerging Flux Tubes
Authors: Fan, Y.
Bibcode: 2004ASPC..325...47F
Altcode:
Bipolar magnetic regions on the solar surface are believed to correspond
to the topmost portions of Ω-shaped arching flux tubes that have risen
buoyantly from the base of the solar convection zone, where strong
toroidal magnetic fields are being generated by the dynamo process. The
dynamic evolution of such rising flux tubes in the solar convection zone
has been studied extensively using a simplified 1D thin flux tube model,
and more recently with direct multi-dimensional MHD simulations. In
this paper we review some recent results of MHD simulations of the
formation and dynamic rise of buoyant Ω-loops in the solar convection
zone. We discuss results with regard to the following topics:
(1) the formation of buoyant flux tubes from a horizontal magnetic
layer at the base of the solar convection zone due to the growth of
the buoyancy instabilities, (2) the necessary twist for maintaining
cohesion of the rising flux tubes, (3) the kink evolution of highly
twisted emerging tubes, (4) the influence of 3D stratified convection
on the rise and the structure of buoyant flux tubes, and finally (5)
the emergence of twisted magnetic flux tubes into the solar atmosphere.
Title: Observational Consequences of a Magnetic Flux Rope Emerging
into the Corona
Authors: Gibson, S. E.; Fan, Y.; Mandrini, C.; Fisher, G.; Demoulin, P.
Bibcode: 2004ApJ...617..600G
Altcode:
We show that a numerical simulation of a magnetic flux rope emerging
into a coronal magnetic field predicts solar structures and dynamics
consistent with observations. We first consider the structure,
evolution, and relative location and orientation of S-shaped, or
sigmoid, active regions and filaments. The basic assumptions are that
(1) X-ray sigmoids appear at the regions of the flux rope known as
``bald-patch-associated separatrix surfaces (BPSSs), where, under
dynamic forcing, current sheets can form, leading to reconnection
and localized heating, and that (2) filaments are regions of enhanced
density contained within dips in the magnetic flux rope. We demonstrate
that the shapes and relative orientations and locations of the BPSS
and dipped field are consistent with observations of X-ray sigmoids and
their associated filaments. Moreover, we show that current layers indeed
form along the sigmoidal BPSS as the flux rope is driven by the kink
instability. Finally, we consider how apparent horizontal motions of
magnetic elements at the photosphere caused by the emerging flux rope
might be interpreted. In particular, we show that local correlation
tracking analysis of a time series of magnetograms for our simulation
leads to an underestimate of the amount of magnetic helicity transported
into the corona by the flux rope, largely because of undetectable
twisting motions along the magnetic flux surfaces. Observations of
rotating sunspots may provide better information about such rotational
motions, and we show that if we consider the separated flux rope legs as
proxies for fully formed sunspots, the amount of rotation that would
be observed before the region becomes kink unstable would be in the
range 40°-200° per leg/sunspot, consistent with observations.
Title: The Dynamic Evolution of Twisted Magnetic Flux Tubes in a
Three-dimensional Convecting Flow. II. Turbulent Pumping and the
Cohesion of Ω-Loops
Authors: Abbett, W. P.; Fisher, G. H.; Fan, Y.; Bercik, D. J.
Bibcode: 2004ApJ...612..557A
Altcode:
We present a set of three-dimensional MHD simulations using the
anelastic approximation of active region-scale flux ropes embedded
in a turbulent, stratified model convection zone. We simulate the
evolution of Ω-loops and other magnetic structures of varying field
strengths, helicities, and morphologies in both rotating and nonrotating
background states. We show that if the magnetic energy of a flux tube
is weak relative to the kinetic energy density of strong downdrafts,
convective flows dominate the evolution, flux tubes of any shape
rapidly lose cohesion, and the magnetic field redistributes itself
throughout the domain over timescales characteristic of convective
turnover. We determine the conditions under which magnetic tension
resulting from field line twist can provide the force necessary to
prevent a relatively weak flux tube from losing cohesion during its
ascent through the turbulent convection zone. Our simulations show
that there is no initial tendency for a horizontal magnetic flux tube
or layer to be preferentially transported in one vertical direction
over the other solely as a result of the presence of an asymmetric
vertical flow field. However, as the simulations progress, there is
a transient net transport of magnetic flux into the lower half of the
computational domain as the distribution of the magnetic field changes
and flux is expelled from cell centers into converging downflows and
intergranular lanes. This pumping mechanism is weak and uncorrelated
with the degree of vertical flow asymmetry. We find that the strong
turbulent pumping evident in simulations of penetrative convection-the
efficient transport of magnetic flux to the base of the convection
zone over several local turnover times-does not manifest itself in a
closed domain in the absence of a convective overshoot layer. Thus,
we suggest that this rapid redistribution of flux is primarily due to
the penetration of magnetic flux into the stable layer where it remains
over a timescale that far exceeds that of convective turnover. We also
find that different treatments of the viscosity of a Newtonian fluid-in
which the coefficient of either kinematic or dynamic viscosity is
held constant throughout the domain-do not affect the global average
evolution of embedded magnetic structures, although the details of
the evolution may differ between models.
Title: Eruption of a Buoyantly Emerging Magnetic Flux Rope
Authors: Manchester, W., IV; Gombosi, T.; DeZeeuw, D.; Fan, Y.
Bibcode: 2004ApJ...610..588M
Altcode:
We present a three-dimensional numerical magnetohydrodynamic simulation
designed to model the emergence of a magnetic flux rope passing
from below the photosphere into the corona. For the initial state,
we prescribe a plane-parallel atmosphere that comprises a polytropic
convection zone, photosphere, transition region, and corona. Embedded
in this system is an isolated horizontal magnetic flux rope located
10 photospheric pressure scale heights below the photosphere. The
flux rope is uniformly twisted, with the plasma temperature inside
the rope reduced to compensate for the magnetic pressure. Density
is reduced in the middle of the rope, so that this section buoyantly
rises. The early evolution proceeds with the middle of the rope rising
to the photosphere and expanding into the corona. Just as it seems the
system might approach equilibrium, the upper part of the flux rope
begins to separate from the lower, mass-laden part. The separation
occurs through stretching of the field, which forms a current sheet,
where reconnection severs the field lines to form a new system of
closed flux. This flux then erupts into the corona. Essential to the
eruption process are shearing motions driven by the Lorentz force,
which naturally occur as the rope expands in the pressure-stratified
atmosphere. The shearing motions transport axial flux and energy to
the expanding portion of the magnetic field, driving the eruption.
Title: Numerical Simulations of Three-dimensional Coronal Magnetic
Fields Resulting from the Emergence of Twisted Magnetic Flux Tubes
Authors: Fan, Y.; Gibson, S. E.
Bibcode: 2004ApJ...609.1123F
Altcode:
We present the results of MHD simulations in the low-β regime of the
evolution of the three-dimensional coronal magnetic field as an arched,
twisted magnetic flux tube emerges into a preexisting coronal potential
magnetic arcade. We find that the line-tied emerging flux tube becomes
kink-unstable when a sufficient amount of twist is transported into
the corona. For an emerging flux tube with a left-handed twist (which
is the preferred sense of twist for active region flux tubes in the
northern hemisphere), the kink motion of the tube and its interaction
with the ambient coronal magnetic field lead to the formation of an
intense current layer that displays an inverse-S shape, consistent
with the X-ray sigmoid morphology preferentially seen in the northern
hemisphere. The position of the current layer in relation to the
lower boundary magnetic field of the emerging flux tube is also
in good agreement with the observed spatial relations between the
X-ray sigmoids and their associated photospheric bipolar magnetic
regions. We argue that the inverse-S-shaped current layer formed is
consistent with being a magnetic tangential discontinuity limited by
numerical resolution and thus may result in the magnetic reconnection
and significant heating that causes X-ray sigmoid brightenings.
Title: A new asteroid-associated meteor shower and notes on
comet-asteroid connection
Authors: Meng, H.; Zhu, J.; Gong, X.; Li, Y.; Yang, B.; Gao, J.;
Guan, M.; Fan, Y.; Xia, D.
Bibcode: 2004Icar..169..385M
Altcode:
The calculation of the orbit of the potentially hazardous Asteroid 2001
YB 5 suggests a possible meteor shower around January 7.5,
2002 UT. Video observations revealed an unidentified radiant around the
predicted maximum time, at RA=121.5°, Dec=+11.5°(for solar longitude
287.30°). Visual observers also reported unusually high rates from
that region on the same night, indicating that 2001 YB 5
did produce a weak meteor shower. Furthermore, it is noticed that 2001
YB 5 is a rare B-type asteroid in same spectral class with
Asteroid (3200) Phaethon, the parent body of the only previously known
asteroid-associate meteor shower, Geminids.
Title: Numerical Simulations of 3D Coronal Magnetic Fields Resulting
from the Emergence of Twisted Magnetic Flux Tubes
Authors: Fan, Y.; Gibson, S. E.
Bibcode: 2004AAS...204.1803F
Altcode: 2004BAAS...36..682F
We present MHD simulations in the low-β regime of the evolution of
the 3D coronal magnetic field as an arched, twisted magnetic flux
tube is transported into a pre-existing coronal potential magnetic
arcade. It is found that the line-tied emerging flux tube becomes
kink unstable when a sufficient amount of twist is transported into
the corona. For an emerging flux tube with a left-handed twist (which
is the preferred sense of twist for active region flux tubes in the
northern hemisphere), the kink motion of the tube and its interaction
with the ambient coronal magnetic field lead to the formation of an
intense current layer which displays an inverse-S shape, consistent
with the X-ray sigmoid morphology preferentially seen in the northern
hemisphere. Our simulation results may explain the X-ray sigmoid
brightenings that are observed during eruptive flares and confirm the
prediction by previous topological studies that magnetic tangential
discontinuities (or current sheets) should form along the so called
``bald-patch'' separatrix surface, across which the connectivity of
the coronal magnetic field with the dense photosphere undergoes a sharp
transition. Finally, we will also present simulations in a 3D spherical
geometry of a CME-like eruption of the coronal magnetic field due to
the kink instability of a twisted magnetic flux rope emerging into
the corona.
Title: Eruption of a Buoyantly Emerging Magnetic Flux Rope
Authors: Manchester, W. B.; Fan, Y.; Gombosi, T.; de Zeeuw, D.;
Sokolov, I.; Toth, G.
Bibcode: 2003AGUFMSH22A0178M
Altcode:
We present a three-dimensional numerical ideal magnetohydrodynamic
simulation designed to model the emergence of magnetic flux passing
from below the photosphere into the corona. For the initial state, we
prescribe a plane parallel atmosphere that comprises the convection
zone, isothermal photosphere and chromosphere, and isothermal
corona. Embedded in this system is a isolated horizontal magnetic
flux rope located 10 photospheric pressure scale heights below the
photosphere. The flux rope is uniformly twisted with plasma temperature
inside the tube reduced to compensate for the magnetic pressure. Density
is reduced in the middle of the rope so that this section buoyantly
rises. The early evolution of precedes with the middle of the rope
rising to the photosphere and expanding into the corona. Just as it
seems the system might approach equilibrium, the upper part of the
flux rope begins to separate from the lower, mass ladened part. The
separation occurs by stretching of the field to form a current sheet
where reconnection severs the field lines to form a new system of closed
flux. This flux then erupts into the corona. Essential to the eruption
process are shearing motions driven by the Lorentz force which naturally
occurs as the rope expands in the pressure stratified atmosphere. The
shearing motions transport axial flux and energy to the expanding
portion of the magnetic field which contributes to the eruption. Once
the axial flux is largely transported from the submerged field, the
expansion of the magnetic field in the corona begins to decelerate.
Title: Observational consequences of a magnetic flux rope topology
Authors: Gibson, S.; Barnes, G.; Demoulin, P.; Fan, Y.; Fisher, G.;
Leka, K.; Longcope, D.; Mandrini, C.; Metcalf, T.
Bibcode: 2003AGUFMSH42B0516G
Altcode:
We consider the implications of a magnetic flux rope topology for
the interpretation of observations of sigmoidal active regions. A
region of tangential magnetic discontinuities can be identified
using techniques that determine a bald patch (BP) and corresponding
separatrices or a quasi-separatrix layer (QSL) -- for a flux rope this
region can be S-shaped, or sigmoidal. If such a region is physically
driven, current sheets can form yielding conditions appropriate for
reconnective heating. Using a numerical simulation of an emerging
flux rope driven by the kink instability, Fan and Gibson (ApJL, 2003)
showed that current sheets indeed formed a sigmoidal surface. In this
poster we will demonstrate that the current sheets formed on the BP and
BP separatrices. Moreover, we will use the results of the numerical
simulation as proxies for observations: specifically the simulated
field at the photosphere as proxy for the magnetic boundary condition,
the sigmoidal current sheets as proxy for the X-ray active region
emission, and the location of dipped magnetic field lines as proxy
for a filament. We will then consider to what extent such observations
might be used to understand and constrain the basic properties of the
coronal field.
Title: Turbulent Magnetic Field Generation in Rotating Stars
Authors: Bercik, D. J.; Abbett, W. P.; Fisher, G. H.; Fan, Y.
Bibcode: 2003AGUFMSH42B0536B
Altcode:
Observationally, it has been found that magnetic activity is a
strong function of rotation rate. The connection between rotation and
dynamo-generated fields is not well understood, however. The typical
interface dynamo theory applied to the Sun to describe its activity
cycle assumes the existence of a velocity shear layer. Such a model
is inappropriate for fully convective stars that are nevertheless
active, such as late-type M and L stars and pre-main sequence T Tauri
stars; in these stars a turbulent dynamo is generally believed to
be the mechanism of magnetic field generation. We investigate the
connection between observed activity behavior and magnetic field
generation in fully convective stars through a series of simulations
of the turbulent dynamo. The simulations were performed in a Cartesian
domain using ANMHD, a 3D MHD anelastic code. We compare the resulting
magnetic topologies for a series of Rossby numbers and comment on the
implications for the sizes of coronal loops and activity levels.
Title: The Mass of a Solar Quiescent Prominence
Authors: Low, B. C.; Fong, B.; Fan, Y.
Bibcode: 2003ApJ...594.1060L
Altcode:
This paper follows up on our recent paper on the role of prominence mass
in the storage of magnetic energy for driving a coronal mass ejection
(CME). The previous paper erroneously rejected a set of sheet-prominence
solutions, the recovery of which allows for a simple theoretical
estimate of the mass of a quiescent prominence. For coronal fields
of 5-10 G, these hydromagnetic solutions suggest that a prominence
mass of (1-26)×1016 g is needed to hold detached magnetic
fields of intensity comparable to the coronal fields in an unbounded
atmosphere such that the global magnetic field is energetically able to
spontaneously open up and still have enough energy to account for the
kinetic and gravitational potential energies carried away in a CME. This
simple result is discussed in relation to observed prominence magnetic
field intensities, densities, and masses, pointing to the relevance
of such observations to the question of magnetic energy storage in
the solar corona.
Title: The Emergence of a Twisted Magnetic Flux Tube into a
Preexisting Coronal Arcade
Authors: Fan, Y.; Gibson, S. E.
Bibcode: 2003ApJ...589L.105F
Altcode:
To investigate the dynamic evolution of a coronal magnetic field in
response to the emergence of significantly twisted magnetic structures,
we perform MHD simulations in the low-β regime of the emergence of
a twisted magnetic flux tube into a preexisting coronal potential
magnetic arcade. Our simulation of a twisted flux tube, which when
fully emerged contains a twist of 1.875×2π field-line rotation
about the axis between the anchored footpoints, leads to a magnetic
structure with substantial writhing of the tube axis (with an apex
rotation >90°) as a result of the nonlinear evolution of the kink
instability. For an emerging tube with a left-handed twist (which is the
preferred sense of twist for active regions in the northern hemisphere),
the writhing of the tube is also left-handed, producing a forward-S
shape for the tube axis as viewed from the top, which is opposite to
the inverse-S-shaped X-ray sigmoid structures preferentially seen in
the northern hemisphere. However, we find that the writhing motion of
the tube and its interaction with the ambient coronal magnetic field
also drive the formation of an intense current layer that displays an
inverse-S shape, consistent with the shape of X-ray sigmoids.
Title: SAO 32177: a New Multiperiodic Dor Variable
Authors: Rodríguez, E.; Costa, V.; López-González, M. J.; Zhou,
A. Y.; García, J. M.; Wei, J. Y.; Fan, Y.
Bibcode: 2003aahd.conf..391R
Altcode:
No abstract at ADS
Title: Can Simulations of Active Region Magnetic Fields Lead to a
Simplified Model of Turbulent Pumping?
Authors: Abbett, W. P.; Fisher, G. H.; Fan, Y.; Bercik, D. J.
Bibcode: 2003SPD....34.1905A
Altcode: 2003BAAS...35..842A
We present a series of 3-D MHD simulations in the anelastic
approximation of active region scale magnetic flux ropes embedded in
a highly stratified, turbulent model convection zone. The numerical
calculations are carried out over long time scales (of order a solar
rotation time) at high magnetic Reynolds numbers and suggest that
the process of ``turbulent pumping'' --- the tendency for magnetic
flux to be efficiently transported from surface layers to the base of
the convection zone --- does not manifest itself in the absence of
a convective overshoot layer. If the overshoot layer is present, we
suggest a simple, statistical model (similar to a 1-D, depth-dependent
eddy-diffusivity treatment with a characteristic time-scale of
supergranulation) that describes the average properties of the flux
storage process.
Title: The Emergence of a Twisted Magnetic Flux Tube into a
Pre-existing Coronal Arcade
Authors: Fan, Y.; Gibson, S. E.
Bibcode: 2003SPD....34.0416F
Altcode: 2003BAAS...35..813F
To investigate the dynamic evolution of coronal magnetic field in
response to the emergence of significantly twisted magnetic structures,
we perform MHD simulations in the low-β regime of the emergence of
a twisted magnetic flux tube into a pre-existing coronal potential
magnetic arcade. Our simulation of a twisted flux tube, which when
fully emerged, contains a twist of 1.875 x 2 π field-line rotation
about the axis between the anchored footpoints, leads to a magnetic
structure with substantial writhing of the tube axis (apex rotation
> 90o) as a result of the non-linear evolution of the
kink instability. For an emerging tube with a left-handed twist
(which is the preferred sense of twist for active regions in the
northern hemisphere), the writhing of the tube is also left-handed,
producing a forward S-shape for the tube axis as viewed from the top,
which is opposite to the inverse S-shaped X-ray sigmoid structures
preferentially seen in the northern hemisphere. However we find that
the writhing motion of the tube and its interaction with the ambient
coronal magnetic field also drives the formation of an intense current
layer which displays an inverse S-shape, consistent with the shape
of X-ray sigmoids. We compare the resulting current layer from the
dynamic simulation with an analysis of the separatrix surface between
winding and non-winding fields at various states of emergence. The National Center for Atmospheric Research is sponsored by the
National Science Foundation. This work is supported in part by AFOSR
grant F49620-02-0191.
Title: Dynamics of CME Driven by a Buoyant Prominence Flux Tube
Authors: Fan, Y.; Low, B. C.
Bibcode: 2003ASPC..286..347F
Altcode: 2003ctmf.conf..347F
No abstract at ADS
Title: The Dynamic Evolution of Twisted Magnetic Flux Tubes in a
Three-dimensional Convecting Flow. I. Uniformly Buoyant Horizontal
Tubes
Authors: Fan, Y.; Abbett, W. P.; Fisher, G. H.
Bibcode: 2003ApJ...582.1206F
Altcode:
We present three-dimensional numerical simulations of the dynamic
evolution of uniformly buoyant, twisted horizontal magnetic flux
tubes in a three-dimensional stratified convective velocity field. Our
calculations are relevant to understanding how stratified convection in
the deep solar convection zone may affect the rise and the structure
of buoyant flux tubes that are responsible for the emergence of solar
active regions. We find that in order for the magnetic buoyancy force
of the tube to dominate the hydrodynamic force due to the convective
downflows, the field strength B of the flux tube needs to be greater
than (Hp/a)1/2Beq~3Beq,
where Hp is the pressure scale height, a is the tube
radius, and Beq is the field strength in equipartition
with the kinetic energy density of the strong downdrafts. For tubes
of equipartition field strength (B=Beq), the dynamic
evolution depends sensitively on the local condition of the convective
flow. Sections of the tube in the paths of strong downdrafts are
pinned down to the bottom despite their buoyancy, while the rise
speed of sections within upflow regions is significantly boosted;
Ω-shaped emerging tubes can form between downdrafts. Although flux
tubes with B=Beq are found to be severely distorted by
convection, the degree of distortion obtained from our simulations
is not severe enough to clearly rule out the Ω-tubes that are able
to emerge between downdrafts as possible progenitors of solar active
regions. As the initial field strength of the tube becomes higher than
the critical value of ~(Hp/a)1/2Beq
given above, the dynamic evolution converges toward the results of
previous simulations of the buoyant rise of magnetic flux tubes in a
static, adiabatically stratified model solar convection zone. Tubes
with 10 times the equipartition field strength are found to rise
unimpeded by the downdrafts and are not significantly distorted by
the three-dimensional convective flow.
Title: Numerical Simulations of Magnetic Fields in Astrophysical
Turbulence
Authors: Zweibel, E. G.; Heitsch, F.; Fan, Y.
Bibcode: 2003LNP...614..101Z
Altcode: 2003tmfa.conf..101Z; 2002astro.ph..2525Z
The generation and evolution of astrophysical magnetic fields occurs
largely through the action of turbulence. In many situations, the
magnetic field is strong enough to influence many important properties
of turbulence itself. Numerical simulation of magnetized turbulence
is especially challenging in the astrophysical regime because of the
high magnetic Reynolds numbers involved, but some aspects of this
difficulty can be avoided in weakly ionized systems.
Title: Indications and implications of twisted magnetic flux in
the corona
Authors: Gibson, S. E.; Fan, Y.; Jain, R.; Low, B.
Bibcode: 2002AGUFMSH52A0446G
Altcode:
The question of whether magnetic flux ropes are fundamental to CMEs and
their precursors will be addressed using a combination of analytic and
numerical models, along with coronal observations. We have developed
computational tools for evaluating observable properties of modeled
magnetic flux ropes suspended in the corona, such as separatrix surfaces
and dipped magnetic fields. We have also developed numerical models to
demonstrate how a flux rope emerging into an overlying coronal magnetic
arcade will relax to a force-free configuration, with associated
formation of current sheets. Using the results of these two parallel
studies, we will directly compare separatrix surfaces determined from
an analytic (non-force-free) equilibrium model to the current sheets
formed during numerical force-free relaxation of the same initial field
configuration. We will then consider these in the context of observed
X-ray sigmoid structures. We have also developed mathematical methods
for determining the magnetic free energy in analytic models of both
magnetic flux ropes, as well as sheared field configurations that
contain no rope. We will compare the free energies thus determined
for both sheared and twisted fields, as functions of spatial size,
magnetic field strength, and degree of shear or twist. We will consider
the implications of these results for the energetics of coronal mass
ejections.
Title: The Dynamic Evolution of Twisted Omega-loops in a 3-D
Convecting Flow
Authors: Abbett, W. P.; Fan, Y.; Fisher, G. H.
Bibcode: 2002AGUFMSH52A0474A
Altcode:
We present the latest results from 3D MHD simulations (in the anelastic
approximation) of buoyant magnetic flux tubes interacting with turbulent
convection in the solar interior. We focus our study on active region
scale flux ropes and Omega-loops, and perform a large parameter space
study of the effects of not only initial field strength, but twist and
loop geometry on the morphology and dynamics of sub-surface magnetic
structures. We also investigate the effects of different numerical
treatments of viscosity, and quantify the amount of magnetic field in
each simulation that succumbs to the effects of turbulent pumping.
Title: Magnetic flux ropes: Would we know one if we saw one?
Authors: Gibson, S. E.; Low, B. C.; Leka, K. D.; Fan, Y.; Fletcher, L.
Bibcode: 2002ESASP.505..265G
Altcode: 2002IAUCo.188..265G; 2002solm.conf..265G
There has been much debate lately about whether twisted magnetic flux
ropes exist in the corona. When asked for observational evidence
of them, the temptation is to show images of apparently twisted
structures. However, we must be very careful of projection effects in
interpreting these observations. Two critical aspects of understanding
how we might observe flux ropes are 1) the 3D nature of the flux rope,
and 2) physically, which bits are visible and for what reasons? In
this paper we will use a simple but physically reasonable 3D analytic
model to address these two issues, and develop techniques that can in
future be used on more general models, both analytic and numerical.
Title: Quiescent Solar Prominences and Magnetic-Energy Storage
Authors: Fong, B.; Low, B. C.; Fan, Y.
Bibcode: 2002ApJ...571..987F
Altcode:
Analytical solutions are presented to describe the hydromagnetic support
of quiescent solar prominences treated as cold plasma sheets in the
characteristic normal and inverse configurations. The solar corona is
modeled to be axisymmetric outside a unit sphere, with the prominence
sheet lying in the equatorial plane extending from the sphere out
to a finite radial distance subject to an inverse-square Newtonian
gravity. The relationship between prominence support and the global
topology of the surrounding poloidal magnetic field is discussed, with
a particular interest in the role of magnetic flux ropes in the support
of inverse prominences. A novel solution is also studied describing
a rope of purely azimuthal magnetic flux held in equilibrium by the
weight of an internal distribution of cold mass and by an external
poloidal magnetic field rigidly anchored to the base of the model
corona. This solution illustrates the role that prominence weight may
play in storing magnetic energy for driving coronal mass ejections.
Title: The Rise of Twisted Horizontal Flux Tubes in a 3D Convecting
Flow
Authors: Fan, Y.; Abbett, W. P.; Fisher, G. H.
Bibcode: 2002AAS...200.0306F
Altcode: 2002BAAS...34..642F
We present 3D numerical simulations of the dynamic evolution of twisted
horizontal magnetic flux tubes in a stratified convecting convection
zone. We investigate how the trajectory, rise velocity, and cohesion of
the buoyant flux tubes are affected by the 3D stratified convection. It
is found that the field strength of the magnetic flux tube needs to
be significantly above the value of equipartition with the kinetic
energy of convection in order for the flux tube to rise cohesively
to the top of the stratified domain. These simulations add further
support to the strong toroidal field strength ( ~ 5 x 104 G
to 105 G) at the base of the solar convection zone, suggested
by previous thin flux tube calculations of emerging flux tubes through
the solar convective envelope. NCAR is sponsored by the National Science
Foundation. Part of this work was carried out while the authors were
participating in the solar magnetic field program held at ITP, UCSB.
Title: Emergence of twisted magnetic flux into the corona
Authors: Gibson, S.; Low, B. C.; Fan, Y.; Fletcher, L.
Bibcode: 2002AAS...200.3603G
Altcode: 2002BAAS...34..693G
The interaction between emerging magnetic structures and preexisting
overlying coronal structures will be addressed using a combination of
observations and physical models that incorporate a range of twisted
magnetic topologies. Solar explosive events such as coronal mass
ejections (CMEs) and flares are commonly considered to be driven by
the free magnetic energy stored in twisted (current carrying) coronal
magnetic fields. Understanding the origin and the three-dimensional
nature of these twisted coronal magnetic structures is a crucial step
towards explaining and predicting CMEs and flares. One possible and
appealing picture is that the twisted coronal magnetic structures
form as a result of the emergence of twisted magnetic flux tubes
from the solar interior. We might imagine a scenario where a flux
rope forms sub-photospherically, emerges through the photosphere,
exists in the corona until it loses its stability and erupts in a
CME which moves out through interplanetary space until ultimately
impacting on the Earth's magnetosphere. Attractively simple as this
picture is, reality is likely to be more complicated since the various
regimes are physically very different and pre-existing structures
would get in the way of our traveling flux rope. We will concentrate
on joining up two of these regimes, by considering how a flux rope
could rise from beneath the photosphere and emerge into the corona,
interacting with pre-existing coronal structures. We will approach this
problem by using a combination of numerical models of the flux rope
emergence from beneath the photosphere, analytic models of coronal
dynamic and equilibrium magnetic structures, and photospheric and
coronal observations of the 3-d structure and evolution of a so-called
"sigmoidal", or S-shaped active region. In so doing we hope to gain
essential insight into how twisted magnetic fields are formed and how
they could be ultimately removed from the solar corona.
Title: The Emergence of a Twisted Ω-Tube into the Solar Atmosphere
Authors: Fan, Y.
Bibcode: 2001ApJ...554L.111F
Altcode:
We report the results of a three-dimensional MHD simulation of the
dynamic emergence of a twisted, Ω-shaped tube from the top layer of
the solar convection zone into the atmosphere and the corona. It is
found that the tube segment at the apex of the Ω-tube expands into
the stably stratified atmosphere as a result of the magnetic buoyancy
instability (or the Parker instability). Our simulation of the emergence
of a left-hand-twisted Ω-tube reproduces several major observed
features of a newly developing active region described by Strous and
coworkers, including the orientation of the arch-filament system,
the distribution of the vertical magnetic field on the photosphere,
the locations of sunspot formation, and the organized shear flow
pattern in the photospheric horizontal velocity field.
Title: Emergence of a Twisted Ω -loop Into the Solar Atmosphere
Authors: Fan, Y.
Bibcode: 2001AGUSM..SP51B09F
Altcode:
We report the results of a 3D MHD simulation of the dynamic emergence of
a twisted Ω -loop from the top layer of the convection zone (where the
plasma β is high) into the solar atmosphere and the corona. Compared
to previous 2D simulations of the emergence of an infinitely long
horizontal flux tube by Magara (2001), our calculations include the 3D
effect of bending the flux tube so that only a segment of the Ω -loop
intersects the photosphere. Similar to the 2D results, we find that
as the tube segment at the apex of the Ω -loop enters the photosphere
boundary, the tube first decelerates because the flux tube encounters
the stable stratification of the isothermal atmosphere. Subsequently,
the magnetic flux entering the photosphere boundary develops a magnetic
buoyancy instability (or the Parker instability) which causes the upper
part of the apex tube segment to rapidly expand into the atmosphere. The
growth of the Parker instability is characterized by an exponential
increase with time of the rise velocity of the front boundary of the
flux tube expanding into the atmosphere, and by downflows of plasma
along the emerged field lines. At the beginning of the emergence, the
emerged field lines are nearly north-south oriented. Subsequently, a
shear motion develops where the field-line footpoints on the two sides
of the polarity inversion line are sheared in the east-west direction,
with the footpoints of the leading (following) polarity moving westward
(eastward). We find that with time an intensification of vertical
magnetic field of the leading and following polarities takes place
respectively at the west and east corners of the emerged magnetic region
on the photosphere, in agreement with the Hale polarity rule. The line
connecting the two major intensification spots of the two polarities
is tilted slightly away from the east-west direction in the sense that
is anti-Joy's law if the emerging tube has left-handed twist in the
northern hemisphere. We find that our simulation of the emergence of
a left-hand-twisted Ω -loop can explain the major observed features
in a newly emerged active region studied by Strous et al. (1996,1999),
including the orientation of the arch-filament system, the distribution
and horizontal motion of flux on the photosphere, and the location of
formation of sunspot pores.
Title: Supernova 2001X in NGC 5921
Authors: Li, W.; Fan, Y.; Qiu, Y. L.; Hu, J. Y.; Schwartz, M.
Bibcode: 2001IAUC.7591....1L
Altcode: 2001IAUC.7591A...1L
W. Li, University of California at Berkeley, communicates that Y. Fan,
Y. L. Qiu, and J. Y. Hu, on behalf of Beijing Astronomical Observatory
(BAO) Supernova Survey, report the discovery of an apparent supernova
(mag about 17.0) found on an unfiltered image taken with the BAO 0.6-m
telescope on Feb. 27.8 UT. SN 2001X is located at R.A. = 15h21m55s.45,
Decl. = +5 03'42".1 (equinox 2000.0), which is 15".5 west and 32".4
south of the nucleus of NGC 5921. SN 2001X was confirmed on an
unfiltered image taken by M. Schwartz on Mar. 2.5 with the Tenagra
Observatory 0.5-m automatic telescope, from which Li measured the
position end figures to be 55s.46 +/- 0s.03, 43".1 +/- 0".2, and the
magnitude of the supernova to be 15.2. Images of the same field taken
with the BAO 0.6-m telescope on Feb. 6.9 (limiting mag about 17.5)
and with the Tenagra 0.5-m telescope on Feb. 17.5 (limiting mag about
18.0) showed nothing at this position. Li remarks that a normal type-Ia
supernova in this galaxy might reach mag about 13.
Title: The Emergence of Magnetic Flux in Active Regions
Authors: Abbett, W. P.; Fisher, G. H.; Fan, Y.
Bibcode: 2001IAUS..203..225A
Altcode:
Over the past decade, ``thin flux tube'' models have proven successful
in explaining many properties of active regions in terms of magnetic
flux tube dynamics in the solar interior. Unfortunately, recent,
more sophisticated two-dimensional MHD simulations of the emergence
of magnetic flux have shown that many of the assumptions adopted in
the thin flux tube approximation are invalid. For example, unless
the flux tubes exhibit a large amount of initial field line twist ---
and observations of emerging active regions suggest they do not ---
they will fragment (break apart) before they are able to emerge through
the surface. We attempt to resolve this paradox using a number of 3-D
MHD simulations (in the anelastic approximation) that describe the
rise and fragmentation of twisted magnetic flux tubes. We find that
the degree of fragmentation of an evolving Omega-loop depends strongly
on the three-dimensional geometry of the tube --- the greater the apex
curvature, the lesser the degree of fragmentation for a fixed amount of
initial twist. We also find that the Coriolis force plays a dynamically
important role in the evolution and emergence of magnetic flux. We are
able to infer general observational characteristics of the emerging
flux, and compare our theoretical data with recent observations.
Title: Formation of Arching Flux Tubes at the Base of the Solar
Convection Zone
Authors: Fan, Y.
Bibcode: 2001IAUS..203..273F
Altcode:
Bipolar magnetic regions on the solar surface are believed to correspond
to the topmost portions of Ω-shaped arching flux tubes that have risen
buoyantly from the base of the solar convection zone, where strong
toroidal magnetic fields are generated by the dynamo process. The
undular Parker instability is one of the likely mechanisms by which
buoyant, arching flux tubes can develop from the toroidal magnetic
field. In this talk, I present our recent 3-D simulations of the growth
of the undular Parker instability in a horizontal magnetic layer with
uni-directional field lines, embedded in an adiabatically-stratified
polytropic atmosphere. We consider the limit of very high plasma
β, representing the condition at the base of the solar convection
zone. The simulations show that distinct arching flux tubes form, and
that buoyancy grows exponentially at the apexes of the tubes as a result
of the diverging flow of mass from the apexes to the troughs. Even
though the initial magnetic field is untwisted, the difference in motion
between the apexes and the troughs causes bending and braiding of the
longitudinal field lines, whose restoring tension force improves the
cohesion of the rising flux tubes in comparison to previous results
from 2-D simulations of the rise of horizontal flux tubes.
Title: Nonlinear Growth of the Three-dimensional Undular Instability
of a Horizontal Magnetic Layer and the Formation of Arching Flux Tubes
Authors: Fan, Y.
Bibcode: 2001ApJ...546..509F
Altcode:
We use an anelastic MHD code to simulate the nonlinear evolution of
the three-dimensional undular instability of a horizontal magnetic
layer with a fixed field line direction, embedded in an adiabatically
stratified atmosphere. We consider the limit of very high plasma
β, representing the condition at the base of the solar convection
zone. We show that, in the limit of high plasma β and nearly
adiabatic stratification, the anelastic formulation gives an accurate
description of the magnetic buoyancy instabilities. We specify the
thermodynamic conditions of the magnetic layer such that it is stable
against pure interchange modes (with zero wavenumber in the direction
of the magnetic field) and is unstable only to three-dimensional
undular modes (with nonzero wavenumbers in both horizontal directions
parallel and perpendicular to the field). Our simulations show that
distinct arching flux tubes form as a result of the growth of the
three-dimensional undular instability. The apices of the arching tubes
become increasingly buoyant because of the diverging mass flow from the
apices to the troughs. The field strength at each loop apex decreases
with height at a significantly smaller rate in comparison with that for
the rise of a horizontal flux tube, because of the stretching of the
loop field lines. Even though the initial magnetic field is untwisted,
it is found that the upward moving tube cross sections of the arching
tubes maintain their cohesion as they rise through the distance of
about 1 density scale height included in the simulation domain. The
difference in motion between the apices and the troughs causes bending
and braiding of the longitudinal field lines, whose restoring tension
force improves the cohesion of the rising flux tubes in comparison with
previous two-dimensional simulations of the buoyant rise of horizontal
flux tubes with no initial twist. In addition, the fact that both the
buoyancy and the tension forces grow self-consistently from zero as
the tubes arch is also a crucial factor for the cohesion of the rising
tubes. The result of our simulations suggests that the minimum value
for the ratio of poloidal field strength over toroidal field strength
(i.e., twist) at the base of the solar convection zone, necessary to
ensure a cohesive rise of magnetic flux through the solar convection
zone, may be far less than that suggested by the two-dimensional
calculations of the buoyant rise of infinitely long horizontal tubes.
Title: Multi-mode kink instability as a mechanism for δ-spot
formation
Authors: Linton, M. G.; Fisher, G. H.; Dahlburg, R. B.; Fan, Y.;
Longcope, D. W.
Bibcode: 2001AdSpR..26.1781L
Altcode:
We investigate the current driven kink instability of twisted magnetic
flux tubes in the solar convection zone. The possibility that kinking
flux tubes are responsible for the formation of some δ-spot active
regions provides the motivation for this work. We simulate the evolution
of a twisted flux tube with a highly parallelized three dimensional
MHD spectral code run on a 128 cubed grid. We find that highly twisted
flux tubes, when perturbed with a single wavenumber mode, develop large
kinks which lead to δ-spot tilt angles as large as 60°. We find that
when tubes are perturbed with multiple wavenumber modes, the modes can
interact to create a localized kink tilted by as much as 80° with
respect to the unkinked portion of the tube. We show that this kind
of kinked flux tube can create a δ-spot configuration with opposite
polarity spots emerging and remaining in close proximity to each other,
with shear developing along the neutral line as the region develops, and
with the opposite polarity regions rapidly rotating about each other.
Title: The Effects of Rotation on the Evolution of Rising Omega
Loops in a Stratified Model Convection Zone
Authors: Abbett, W. P.; Fisher, G. H.; Fan, Y.
Bibcode: 2001ApJ...546.1194A
Altcode: 2000astro.ph..8501A
We present three-dimensional MHD simulations of buoyant magnetic flux
tubes that rise through a stratified model convection zone in the
presence of solar rotation. The equations of MHD are solved in the
anelastic approximation, and the results are used to determine the
effects of solar rotation on the dynamic evolution of an Ω-loop. We
find that the Coriolis force significantly suppresses the degree
of fragmentation at the apex of the loop during its ascent toward
the photosphere. If the initial axial field strength of the tube is
reduced, then, in the absence of forces due to convective motions,
the degree of apex fragmentation is also reduced. Our simulations
confirm the results of thin flux-tube calculations that show the
leading polarity of an emerging active region positioned closer to
the equator than the trailing polarity and the trailing leg of the
loop oriented more vertically than the leading leg. We show that the
Coriolis force slows the rise of the tube and induces a retrograde
flow in both the magnetized and unmagnetized plasma of an emerging
active region. Observationally, we predict that this flow will appear
to originate at the leading polarity and will terminate at the trailing
polarity.
Title: Erratum: The Three-dimensional Evolution of Rising, Twisted
Magnetic Flux Tubes in a Gravitationally Stratified Model Convection
Zone
Authors: Abbett, W. P.; Fisher, G. H.; Fan, Y.
Bibcode: 2000ApJ...542.1119A
Altcode:
In the article ``The Three-dimensional Evolution of Rising, Twisted
Magnetic Flux Tubes in a Gravitationally Stratified Model Convection
Zone'' by W. P. Abbett, G. H. Fisher, and Y. Fan (ApJ, 540, 548
[2000]), an error was introduced into one of the equations during
the production process. A cross product symbol was mistakenly
removed from equation (2). The corrected equation is as follows:
ρ0(∂v/∂t+v˙∇v)= -∇p1+ρ1g +
1/4π (∇XB)XB+∇˙Π. The Press sincerely apologizes for this error.
Title: The Three-dimensional Evolution of Rising, Twisted Magnetic
Flux Tubes in a Gravitationally Stratified Model Convection Zone
Authors: Abbett, W. P.; Fisher, G. H.; Fan, Y.
Bibcode: 2000ApJ...540..548A
Altcode: 2000astro.ph..4031A
We present three-dimensional numerical simulations of the rise and
fragmentation of twisted, initially horizontal magnetic flux tubes that
evolve into emerging Ω-loops. The flux tubes rise buoyantly through an
adiabatically stratified plasma that represents the solar convection
zone. The MHD equations are solved in the anelastic approximation,
and the results are compared with studies of flux-tube fragmentation
in two dimensions. We find that if the initial amount of field line
twist is below a critical value, the degree of fragmentation at the
apex of a rising Ω-loop depends on its three-dimensional geometry: the
greater the apex curvature of a given Ω-loop, the lesser the degree
of fragmentation of the loop as it approaches the photosphere. Thus,
the amount of initial twist necessary for the loop to retain its
cohesion can be reduced substantially from the two-dimensional
limit. The simulations also suggest that, as a fragmented flux
tube emerges through a relatively quiet portion of the solar disk,
extended crescent-shaped magnetic features of opposite polarity should
form and steadily recede from one another. These features eventually
coalesce after the fragmented portion of the Ω-loop emerges through
the photosphere.
Title: VizieR Online Data Catalog: Purple Mountain H2O
maser atlas (Han+
Authors: Han, F.; Mao, R. Q.; Lei, C. M.; Wu, Y. -F.; Sun, J.; Wang,
J. S.; Pei, C. C.; Xiang, D. -L.; Fan, Y.; Tang, G. S.; Ji, H. R.
Bibcode: 2000yCatp050001401H
Altcode:
Observations of H2O maser sources on the 13.7m radio telesc
Purple Mountain observatory from Aug 1990 to Jan 1994 are briefly
summarized. The results of observations are presented in Table 1 and
Figure 1. The total number of objects observed is 435. 195 objects are
detected among them 108 are new detections. A brief description of the
instrumentation and data processing are also given. (1 data file).
Title: 3D MHD Simulation of Flux Tube Dynamics: Comparison with Thin
Flux Tube Models
Authors: Fisher, G. H.; Abbett, W. P.; Fan, Y.
Bibcode: 2000SPD....31.0135F
Altcode: 2000BAAS...32..807F
We have used the anelastic 3D MHD code ``ANMHD'' to perform simulations
of emerging magnetic flux tubes moving in a gravitationally stratified
background model representing the solar convection zone. The MHD
model is computed within a local Cartesian geometry, with Coriolis
forces included, using the f-plane approximation. The evolution of
flux tubes computed with the code will be compared and contrasted with
results computed with the thin flux tube approximation. This work was
supported by NASA and NSF.
Title: The Subphotospheric Structure of Emerging Flux
Authors: Fan, Y.
Bibcode: 2000SPD....31.0305F
Altcode: 2000BAAS...32..834F
Bipolar magnetic regions on the solar surface are believed to correspond
to the topmost portions of Ω -shaped arching flux tubes that have
risen buoyantly from the base of the solar convection zone, where strong
toroidal magnetic fields are being generated by the dynamo process. The
dynamic evolution of such rising flux tube structures in the solar
convection zone has been studied extensively using a simplified thin
flux tube model, and more recently with direct multi-dimensional
MHD simulations. In this talk I will give an overview of some recent
results of 3-dimensional MHD simulations of the formation and dynamic
rise of buoyant Ω loops in the solar interior: (1) I will present
direct numerical simulations of the formation of coherent, 3-D Ω -loop
structures as a result of the growth of the undular Parker instability
of a neutrally buoyant horizontal flux tube or flux sheet initially
in hydrostatic equilibrium. (2) The question of the critical twist
necessary for maintaining cohesion of the rising flux tubes will be
discussed in light of recent 3-D simulations of fragmenting Ω -loops by
Abbett et al. (3) I will describe simulations of the non-linear growth
of the current driven kink instability along rising flux tubes that
are highly twisted, and show that kinked Ω -loops reproduce several
observed features of the so-called δ -sunspots. Finally, the issue
of the connectivity of the emerged flux with its source at the base
of the convection zone will be discussed by examining the conditions
of hydrostatic equilibrium along a vertical flux tube extending across
the solar convection zone. The National Center for Atmospheric Research
(NCAR) is sponsored by the National Science Foundation
Title: The Cohesion of 3-D Magnetic Flux Tubes in a Rotating,
Stratified Model Convection Zone
Authors: Abbett, W. P.; Fisher, G.; Fan, Y.
Bibcode: 2000SPD....31.0136A
Altcode: 2000BAAS...32..807A
We present the latest results from a series of 3-D MHD simulations in
the anelastic approximation that describe the rise of magnetic flux
tubes through an adiabatically stratified model convection zone. The
effects of solar rotation and the Coriolis force are included in
the models. The simulations begin with initially horizontal magnetic
flux tubes which subsequently evolve into Omega-loops. We find that
the degree of ``fragmentation'' at the apex of a rising Omega-loop
depends strongly on both the three-dimensional geometry of the loop,
and on the field strength along the axis of the initial tube. Loops
with a relatively high degree of apex curvature, and of moderate to low
initial axial field strength retain their cohesion throughout their
rise toward the photosphere --- even in the absence of initial field
line twist. We are able to infer general observational characteristics
of the emerging flux, and compare our theoretical data with recent
observations of active regions. This work was funded by NSF grants
AST 98-19727 and ATM 98-96316, and by NASA grant NAGS-8468. The
computations were partially supported by the National Center for
Atmospheric Research, and the National Computational Science Alliance.
Title: Magnetic flux tubes inside the sun
Authors: Fisher, G. H.; Fan, Y.; Longcope, D. W.; Linton, M. G.;
Abbett, W. P.
Bibcode: 2000PhPl....7.2173F
Altcode:
Bipolar magnetic active regions are the largest concentrations of
magnetic flux on the Sun. In this paper, the properties of active
regions are investigated in terms of the dynamics of magnetic flux
tubes which emerge from the base of the solar convection zone, where
the solar cycle dynamo is believed to operate, to the photosphere. Flux
tube dynamics are computed with the ``thin flux tube'' approximation,
and by using magnetohydrodynamics simulation. Simulations of active
region emergence and evolution, when compared with the known observed
properties of active regions, have yielded the following results: (1)
The magnetic field at the base of the convection zone is confined to
an approximately toroidal geometry with a field strength in the range
3-10×104 G. The latitude distribution of the toroidal
field at the base of the convection zone is more or less mirrored by
the observed active latitudes; there is not a large poleward drift of
active regions as they emerge. The time scale for emergence of an active
region from the base of the convection zone to the surface is typically
2-4 months. (2) The tilt of active regions is due primarily to the
Coriolis force acting to twist the diverging flows of the rising flux
loops. The dispersion in tilts is caused primarily by the buffeting of
flux tubes by convective motions as they rise through the interior. (3)
Coriolis forces also bend active region flux tube shapes toward the
following (i.e., antirotational) direction, resulting in a steeper
leg on the following side as compared to the leading side of an active
region. When the active region emerges through the photosphere, this
results in a more rapid separation of the leading spots away from the
magnetic neutral line as compared to the following spots. This bending
motion also results in the neutral line being closer to the following
magnetic polarity. (4) The properties of the strongly sheared, flare
productive δ-spot active regions can be accounted for by the dynamics
of highly twisted Ω loops that succumb to the helical kink instability
as they emerge through the solar interior.
Title: The Solar Dynamo and Emerging Flux - (Invited Review)
Authors: Fisher, G. H.; Fan, Y.; Longcope, D. W.; Linton, M. G.;
Pevtsov, A. A.
Bibcode: 2000SoPh..192..119F
Altcode:
The largest concentrations of magnetic flux on the Sun occur in
active regions. In this paper, the properties of active regions are
investigated in terms of the dynamics of magnetic flux tubes which
emerge from the base of the solar convection zone, where the solar cycle
dynamo is believed to operate, to the photosphere. Flux tube dynamics
are computed using the `thin flux tube' approximation, and by using
MHD simulation. Simulations of active region emergence and evolution,
when compared with the known observed properties of active regions,
have yielded the following results: (1) The magnetic field at the
base of the convection zone is confined to an approximately toroidal
geometry with a field strength in the range (3-10)×104
G. The latitude distribution of the toroidal field at the base of
the convection zone is more or less mirrored by the observed active
latitudes; there is not a large poleward drift of active regions as
they emerge. The time scale for emergence of an active region from the
base of the convection zone to the surface is typically 2-4 months. The
equatorial gap in the distribution of active regions has two possible
origins; if the toroidal field strength is close to 105 G,
it is due to the lack of equilibrium solutions at low latitude; if it
is closer to 3×104 G, it may be due to modest poleward drift
during emergence. (2) The tilt of active regions is due primarily to the
Coriolis force acting to twist the diverging flows of the rising flux
loops. The dispersion in tilts is caused primarily by the buffeting of
flux tubes by convective motions as they rise through the interior. (3)
The Coriolis force also bends the active region flux tube shape toward
the following (i.e., anti-rotational) direction, resulting in a steeper
leg on the following side as compared to the leading side of an active
region. When the active region emerges through the photosphere, this
results in a more rapid separation of the leading spots away from the
magnetic neutral line as compared to the following spots. This bending
motion also results in the neutral line being closer to the following
magnetic polarity. (4) Active regions behave kinematically after they
emerge because of `dynamic disconnection', which occurs because of the
lack of a solution to the hydrostatic equilibrium equation once the flux
loop has emerged. This could explain why active regions decay once they
have emerged, and why the advection-diffusion description of active
regions works well after emergence. Smaller flux tubes may undergo
`flux tube explosion', a similar process, and provide a source for the
constant emergence of small-scale magnetic fields. (5) The slight trend
of most active regions to have a negative magnetic twist in the northern
hemisphere and positive twist in the south can be accounted for by the
action of Coriolis forces on convective eddies, which ultimately writhes
active region flux tubes to produce a magnetic twist of the correct
sign and amplitude to explain the observations. (6) The properties of
the strongly sheared, flare productive δ-spot active regions can be
accounted for by the dynamics of highly twisted Ω loops that succumb to
the helical kink instability as they emerge through the solar interior.
Title: On the twist of emerging flux loops in the solar convection
zone
Authors: Fan, Y.; Gong, Donglai
Bibcode: 2000SoPh..192..141F
Altcode:
We perform numerical simulations of emerging flux loops in the solar
convective envelope based on a weakly twisted thin flux tube model
recently derived by Longcope and Klapper, generalizing the original
formulation for the dynamics of untwisted thin flux tubes by Spruit. The
generalized formulation includes the description of torsional Alfvén
waves and takes into account the coupling of the writhing motion
of the tube axis to the change in the flux tube twist based on the
requirement of global helicity conservation of the closed thin flux
tube. In this model, the twist of the thin flux tube is described by
a quantity q defined as the angular rate of field-line rotation about
the tube axis per unit length of the tube. We examine the evolution of
twist along Ω-shaped emerging flux loops which are formed as a result
of the non-linear growth of the Parker instability of toroidal magnetic
flux tubes at the base of the solar convection zone. We find that: (1)
In the northern hemisphere, a left-handed twist is generated in the flux
tubes as a result of the right-handed tilt or writhe of the emerging
loops induced by the Coriolis force. The generated twist increases
with the latitude of emergence over the range from 0° to about 38°
latitude, but then decreases when the emerging latitude exceeds 38°,
because of a change in the preferred eruption pattern. The magnitude
of the generated twist q is very small, ≲2×10−4
rad Mm−1, more than an order of magnitude smaller than
the observed amplitude of twist (∼0.01 rad Mm−1) in
solar active regions. (2) For a toroidal flux ring with a uniform
initial twist q0 along the ring, the twist amplitude |q|
at the apex of the emerging loop decrease by a factor of about 0.67
because of the stretching of the loop, as it rises from the base of the
convection zone to about 20 Mm below the photosphere, at which depth
the flux tube can no longer be considered thin. However, because of the
more rapid increase of the tube cross-sectional radius a with height,
|qa|, which corresponds to the ratio between the azimuthal field to
the axial field Bθ/Bl of the tube, increases
by a factor of about 2.5 at the apex of the loop, as it rises over
the same distance. (3) Because of the effect of the Coriolis force,
the distribution of twist along the emerging loop is asymmetric between
the leading (in the direction of rotation) and the following sides of
the loop. Both |q| and |qa| are greater at the following side than the
leading at any depth. Based on the evolution of twist along emerging
flux loops, we discuss possible constraints on the twist q0
of initial toroidal flux tubes at the base of the convection zone.
Title: The Effect of the Helical Kink Instability on the Morphology
of Emerging Active Regions
Authors: Linton, M. G.; Fisher, G. H.; Dahlburg, R. B.; Fan, Y.
Bibcode: 1999ESASP.448..609L
Altcode: 1999mfsp.conf..609L; 1999ESPM....9..609L
No abstract at ADS
Title: Relationship of the Multimode Kink Instability to δ-Spot
Formation
Authors: Linton, M. G.; Fisher, G. H.; Dahlburg, R. B.; Fan, Y.
Bibcode: 1999ApJ...522.1190L
Altcode:
We study the current-driven kink instability with a three-dimensional
MHD spectral code, under conditions appropriate for the convection
zone of the Sun. Our goal is to determine whether the kink instability
can explain the unusual morphology of certain ``δ-spot'' active
regions. The characteristics of these δ-spots are unusually large
tilt upon emergence, subsequent rotation, compactness during their
lifetime, magnetic shear that develops along the neutral line of their
vertical magnetic field, and unusually high flare activity. We find
that highly twisted tubes perturbed with a single unstable kink mode
evolve to a new helical equilibrium with finite amplitude. This kink
would produce an active region that emerged tilted and then rotated and
so is suggestive of δ-spot behavior. It would not, however, produce
other characteristics of δ-spots such as compactness and shear. We
then investigate the kink instability in tubes perturbed simultaneously
with several unstable modes at different wavelengths. These tubes
develop a concentrated kink at the point at which the modes interact
constructively. We show that such a concentrated kink would first emerge
highly tilted, rotate during its subsequent emergence while remaining
compact, and develop strong shear along its magnetic neutral line,
in agreement with δ-spot observations. In addition we find that very
strong concentrated kinks develop a current sheet at which the magnetic
field reconnects, causing field lines near the center of the tube to
become knotted. This reconnection could be related to the high flare
activity of δ-spots.
Title: The Rise of Kink-unstable Magnetic Flux Tubes and the Origin
of δ-Configuration Sunspots
Authors: Fan, Y.; Zweibel, E. G.; Linton, M. G.; Fisher, G. H.
Bibcode: 1999ApJ...521..460F
Altcode:
We perform three-dimensional simulations of the rise of twisted magnetic
flux tubes in an adiabatically stratified model solar convection
zone. The initial flux tube in our simulations is a uniformly twisted,
buoyant, horizontal tube located near the bottom of the stratified
layer. The twist of the initial flux tube is described by a parameter
α, which is defined as the angular rate of field-line rotation about
the tube axis per unit length of the tube. We study the nonlinear
evolution of the helical kink instability of the flux tube as it rises
through the stratified layer. We find from our simulations that in order
for the tube to develop significant kinking during its rise, the initial
twist of the tube needs to be close to or greater than the critical
limit (αc) for the onset of the kink instability. If the
initial twist is significantly below the critical limit (α below about
50% of αc), we find essentially no kink development and
the evolution is similar to the results from previous two-dimensional
simulations of the rise of twisted, horizontal flux tubes. On the other
hand, if the initial twist is sufficiently greater than the critical
limit such that the e-folding period of the fastest growing kink mode
is small compared to the rise time of the tube, we find sharp bending
and distortion of the tube as a result of the nonlinear evolution of
the kink instability. In this case, we find that due to the effect of
gravitational stratification, the kinked flux tube arches upward and
evolves into a buckled loop with a local change of tube orientation
at the loop apex that exceeds 90° from the original direction of the
tube. The emergence of this buckled loop can give rise to a compact
magnetic bipole with polarity order inverted from the Hale polarity
law, similar to the configuration often seen in δ spots. Furthermore,
our simulations show that the writhing of the tube axis as a result
of the kink instability stretches the flux tube and increases its
buoyancy. Hence, the development of the kink instability can speed up
the overall rise of the flux tube.
Title: The Emergence of Kink-Unstable Magnetic Flux Tubes and the
Origin of delta -Configuration Sunspots
Authors: Fan, Y.; Zweibel, E. G.; Linton, M. G.; Fisher, G. H.
Bibcode: 1999AAS...194.5903F
Altcode: 1999BAAS...31Q.918F
The so-called delta -configuration sunspots are an unusual class of
compact sunspots in which umbrae of opposite polarities are gathered
closely in a common penumbra, and the polarity order is often inverted
from Hale's polarity law. One appealing suggestion for the origin of
the delta -spots, is that they are formed through the emergence of
flux tubes that have become kinked (or knotted) due to the onset of the
current driven kink instability. In this talk I present 3D simulations
of the non-linear evolution of the helical kink instability of twisted
magnetic flux tubes rising buoyantly through an adiabatically stratified
layer. We study the kink evolution of buoyant flux tubes with a range
of different initial twist. We find that in order for the tube to
develop significant kinking during its rise, the initial twist of the
tube needs to be close to or greater than the critical limit for the
onset of the kink instability. If the initial twist is sufficiently
super-critical such that the e-folding period of the fastest growing
kink mode is small compared to the rise time of the tube, we find that
sharp bending and distortion of the tube develop. Due to the effect of
gravitational stratification, the kinked flux tube arches upward and
evolves into a buckled loop with a local change of tube orientation
at the loop apex that exceeds 90(deg) from the original direction of
the tube. I will discuss the similarities and differences between the
structure of the buckled emerging flux loop and the magnetic field
morphology of several delta -spots.
Title: The Current Driven Kink Instability and Its Relationship to
delta - SPOT Active Regions
Authors: Linton, M. G.; Fisher, G. H.; Longcope, D. W.; Dahlburg,
R. B.; Fan, Y.
Bibcode: 1999AAS...194.5902L
Altcode: 1999BAAS...31..918L
The current driven kink instability may be the cause of both the unusual
morphology of solar delta -spot active regions and the tendency of
these regions to be significantly more flare active than most active
regions. We investigate the current driven kink instability of flux
tubes in the solar interior both with a linear stability analysis and
with nonlinear MHD simulations. The linear analysis shows that there is
a critical twist, which depends on the axial magnetic field profile,
that a flux tube needs to become kink unstable. This critical twist
decreases as the tube expands, so twisted flux tubes will become
increasingly unstable as they rise through the convection zone. The
nonlinear simulations show that a twisted tube excited by a single
unstable kink mode will evolve to a helical equilibrium state. The
emergence through the photosphere of such a kinked tube would create
an active region which was tilted with respect to Hale's law and
which would rotate as it evolved, as delta -spots are observed to
do. We then find that, when excited by multiple unstable kink modes,
highly twisted flux tubes develop concentrated kinks. These concentrated
kinks would produce more of the observed characteristics of delta -spot
active regions. They would create active regions which, in addition to
emerging tilted and then rotating, would remain compact as they evolved,
and develop strong shear along their magnetic neutral line. Finally,
we find that a strong concentrated kink develops a current sheet at
which the magnetic field reconnects, which may be the cause of the
high flare activity of delta -spots.
Title: Anelastic Magnetohydrodynamic Equations for Modeling Solar
and Stellar Convection Zones
Authors: Lantz, S. R.; Fan, Y.
Bibcode: 1999ApJS..121..247L
Altcode:
The anelastic approximation has strong advantages for numerical
simulations of stellar and solar convection zones. The chief and
generally known one is that it suppresses acoustic modes, permitting
larger simulated time steps to be taken than would be possible in a
fully compressible model. This paper clarifies and extends previous work
on the anelastic approximation by presenting a new vorticity-based
formulation that can be used for two- and three-dimensional MHD
simulations. In the new formulation, all fluctuating thermodynamic
variables except the entropy are eliminated from the equations. This
shows in the plainest way how the anelastic approximation generalizes
the Boussinesq approximation, which appears as a special limit. The
roots of both models are traced to the mixing-length theory of
convection, which establishes the scaling parameters for ``deep''
(weakly superadiabatic) convection at low Mach numbers. The Ogura &
Phillips and the Glatzmaier derivations of the anelastic model are
broadened to include a possible depth dependence in the thermodynamic
properties of constituent gases. This permits a variable state of gas
ionization, for example, which is important for stars like the Sun,
in which the convecting regions coincide with the ionization zones
of hydrogen and helium. Tests with the new model are presented, in
which it is shown that the new model is capable of reproducing earlier
results in the linear and nonlinear stages of convection.
Title: The Origin and Role of Twist in Active Regions
Authors: Fisher, G. H.; Longcope, D. W.; Linton, M. G.; Fan, Y.;
Pevtsov, A. A.
Bibcode: 1999soho....9E..56F
Altcode:
The implications of twist in active region magnetic fields is considered
in this paper. The latitudinal distribution of twist that has been
derived from recent vector magnetogram observations may be explained by
the effects of convective turbulence with a non-zero kinetic helicity
acting on active region scale magnetic flux tubes as they rise through
the convection zone. Highly twisted, kink unstable flux tubes are then
discussed as a possible explanation for many of the observed properties
of flare productive, "d-spot'' active regions.
Title: Erratum: Helioseismic Measurements of the Subsurface
Meridional Flow
Authors: Braun, D. C.; Fan, Y.
Bibcode: 1999ApJ...510L..81B
Altcode:
In the Letter ``Helioseismic Measurements of the Subsurface Meridional
Flow'' by D. C. Braun and Y. Fan (ApJ,
508, L105 [1998]), equation (4) was misprinted and should appear as
follows:<Uθ>≡-(θmax-θmin)-1θminθmaxU\b.dot
θ̂dθ. (4)
Title: The Origin and Role of Twist in Active Regions
Authors: Fisher, G. H.; Longcope, D. W.; Linton, M. G.; Fan, Y.;
Pevtsov, A. A.
Bibcode: 1999ASPC..178...35F
Altcode: 1999sdnc.conf...35F
No abstract at ADS
Title: The Solar Dynamo and Emerging Flux
Authors: Fisher, G. H.; Fan, Y.; Longcope, D. W.; Linton, M. G.;
Pevtsov, A. A.
Bibcode: 1999soho....9E..18F
Altcode:
Much has been learned about the dynamics of magnetic flux tubes in the
solar interior over the past decade. By using theoretical models for
the dynamics of active region flux ropes, it is possible to estimate
observable properties of active regions, such as their orientation,
position on the disk, and morphology, and then compare these properties
with active region observations. By varying conditions of the magnetic
flux ropes as the base of the convection zone until observed properties
are matched, one can deduce properties of the magnetic field in the
dynamo layer, such as the magnetic field strength. Observed properties
such as the active region tilt angle, the dispersion of the tilt angle,
and magnetic helicity in active regions will be discussed in terms
of the dynamics of flux tubes rising through the convection zone and
their interaction with convective motions. Properties of Delta spot
active regions will be discussed in terms of the kink instability of
magnetic flux ropes.
Title: Formation of Kinked Emerging Loops in the Solar Convection Zone
Authors: Fan, Y.
Bibcode: 1999soho....9E..55F
Altcode:
Through 3D numerical simulations, we investigate the formation of kinked
emerging magnetic flux loops as a result of the non-linear growth of the
current driven kink instability of highly twisted magnetic flux tubes
in the solar convection zone. The effect of the Coriolis force due to
solar rotation is included. The initial flux tubes in our simulations
are east-west oriented, horizontal tubes in mechanical equilibrium
with a degree of twist that is significantly above the critical limit
for the onset of the kink instability. The growth of the helical kink
instability makes the flux tube buoyant and causes it to rise. Due to
the effect of gravitational stratification, the kinked flux tube arches
upward and evolves into a kinked emerging loop with a local change
of tube orientation at the loop apex that exceeds 90 degrees from
the original direction of the tube. As was discussed in our previous
works, the emergence of the kinked loop can give rise to a compact
magnetic bipolar region with inverted polarity order, similar to the
structure often seen in delta-spots. Inclusion of the Coriolis force
due to solar rotation is found to cause propagation of the kinks along
the tube in the direction opposite to the direction of rotation. The
Coriolis force can either enhance or reduce the amount of tilt of the
apex of the kinked loop depending on which hemisphere the flux tube
is in and the sense of the twist of the tube. The National Center for
Atmospheric Research is sponsored by the National Science Foundation.
Title: Helioseismic Measurements of the Subsurface Meridional Flow
Authors: Braun, D. C.; Fan, Y.
Bibcode: 1998ApJ...508L.105B
Altcode:
We measure the mean frequencies of acoustic (p-mode) waves propagating
toward and away from the poles of the Sun from observations made with
the Solar Oscillations Investigation-Michelson Doppler Imager on board
the Solar and Heliospheric Observatory and the ground-based Global
Oscillations Network Group. We demonstrate that there is a significant
frequency shift between poleward- and equatorward-traveling waves
measured over solar latitudes 20°-60°, which is consistent with
the Doppler effect of a poleward meridional flow on the order of 10 m
s-1. From the variation of the frequency shifts of p-modes
with degree l between 72 and 882 as a function of the lower turning
point depth, we infer the speed of the meridional flow, averaged over
these latitudes, over a range in depth extending over the top half
of the solar convection zone. We find no evidence for a significant
equatorward return flow within this depth range.
Title: The Rise of Kink-Unstable Magnetic Flux Tubes in the Solar
Convection Zone
Authors: Fan, Y.; Zweibel, E. G.; Linton, M. G.; Fisher, G. H.
Bibcode: 1998ApJ...505L..59F
Altcode:
We report preliminary results of a three-dimensional simulation of the
buoyant rise of a strongly twisted, kink-unstable magnetic flux tube
through a gravitationally stratified layer representing the solar
convection zone. The numerical calculations employ the well-known
anelastic approximation, which is suitable for studying slow, subsonic
dynamical processes in the pressure-dominated, high-β plasma of the
solar interior. This Letter investigates the case in which the initial
twist of the buoyant flux tube is sufficiently high that the e-folding
growth times of the unstable kink modes are short in comparison to
the rise time of the flux tube. Our simulation shows that the flux
tube becomes kinked and that the top portion of the flux tube evolves
into a buckled shape with the tube axis being deflected by more than
90° from its original orientation. We suggest that the emergence
of this buckled flux tube can give rise to a compact magnetic bipole
with polarity order inverted from Hale's polarity law, similar to the
configuration often seen in δ spots.
Title: Seismic Holography of Solar Activity
Authors: Braun, D. C.; Lindsey, C.; Fan, Y.; Fagan, M.
Bibcode: 1998ApJ...502..968B
Altcode:
Helioseismic images of sunspots show a remarkable acoustic anomaly
surrounding the sunspot. We applied the computational formalism of
``helioseismic holography'' to SOHO-MDI observations to render
acoustic images of NOAA AR 7973, an active region containing a
moderately large sunspot. The results of this study are based on
simple ``acoustic power holography,'' to image the absorption of
p-mode waves by the sunspot. These images clearly show a strong,
compact acoustic deficit representing the sunspot, as well as plages
in the neighborhood of the sunspot, consistent with earlier results of
``Hankel analysis.'' However, they also show surrounding the sunspot
a conspicuous acoustic halo extending out to a radius of approximately
35,000 km. We propose that this ``acoustic moat'' is the helioseismic
manifestation of a single convection eddy that is driven by the thermal
disturbance resulting from the local blockage of convective transport
in the sunspot subphotosphere. Depth diagnostics based on acoustic
focus show a rapidly defocusing sunspot image as the focal plane is
submerged. Acoustic noise models in which absorption by the sunspot
is entirely superficial yield images that defocus significantly more
slowly with increasing focal-plane depth than the SOHO-MDI images of
NOAA AR 7973. Extending the absorption significantly beneath the model
photosphere enhances the discrepancy. More recent tests tentatively
suggest that this ``focus anomaly'' is the result of neglect of image
smearing introduced into the MDI instrument to suppress aliasing,
and that a proper account of the instrumental MTF will render
defocus profiles roughly consistent with superficial absorption. Our
holographic images roughly indicate that the sunspot in NOAA AR 7973
absorbs low-l waves with approximately the same efficiency as it does
high-l waves. Contrary to widely held opinion, this result is entirely
consistent with that of the Hankel analysis, given that the absorption
of waves by magnetic regions is indeed superficial. We expect that the
efficient absorption of low-l waves will make it possible to image large
active regions on the far side of the Sun by the acoustic-absorption
signatures they render at their antipodes.
Title: Two-dimensional Simulations of Buoyantly Rising, Interacting
Magnetic Flux Tubes
Authors: Fan, Y.; Zweibel, E. G.; Lantz, S. R.
Bibcode: 1998ApJ...493..480F
Altcode:
We perform two-dimensional simulations of the buoyant rise of twisted
horizontal magnetic flux tubes through an adiabatically stratified
layer representing the solar convection zone or other marginally
stable atmosphere. The numerical calculations employ the anelastic
approximation to the basic MHD equations. We confirm the results
of recent compressible simulations by Moreno-Insertis & Emonet
that the azimuthal component of the tube magnetic field can prevent
the splitting of the tube into a vortex pair, and that most of the
flux in the initial tube cross section rises in the form of a rigid
body that reaches a terminal speed similar to the prediction of the
often-employed thin-flux-tube model. We also study the interaction
between a pair of buoyant flux tubes as they rise in proximity. In the
case of two identical flux tubes that start from the same level, we find
that the wake behind each tube interacts with the wake of the other,
prompting mirror-symmetric vortex shedding in each wake. As a result,
each tube gains around it a net circulation of the opposite sign of
the most recently shed eddy; this causes a periodic, horizontal lift
force that makes the tubes oscillate horizontally as they rise. The
tube interactions in this case differ substantially from the inviscid
limit studied previously. For two identical flux tubes that start at
different levels, the resulting interactions depend upon the details of
the initial configuration of the two tubes and can be very different
from the interactions seen in the symmetrical case. In the asymmetric
case, it becomes possible for one flux tube to be drawn into the wake
of the other, leading eventually to a merger of the tubes.
Title: New detections of H_2O maser sources on the 13.7 M radio
telescope of Purple Mountain Observatory
Authors: Han, F.; Mao, R. Q.; Lu, J.; Wu, Y. F.; Sun, J.; Wang, J. S.;
Pei, C. C.; Fan, Y.; Tang, G. S.; Ji, H. R.
Bibcode: 1998A&AS..127..181H
Altcode:
Observations of H_2O maser sources on the 13.7 m radio telescope
of Purple Mountain Observatory from 1990 Aug. to 1994 Jan. are
summarized. For searching new water masers, the total number of search
candidates is about 360, with 110 objects detected. Among them are 96
new detections. A list of the new detections and their spectra are
presented. Table 1 and Fig. 1 are only available in electronic form
at the CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5)
or via http: //cdsweb.u-strasbg.fr/Abstract.html
Title: VizieR Online Data Catalog: H2O maser sources new detections
(Han+ 1998)
Authors: Han, F.; Mao, R. Q.; Lu, J.; Wu, Y. F.; Sun, J.; Wang, J. S.;
Pei, C. C.; Fan, Y.; Tang, G. S.; Ji, H. R.
Bibcode: 1997yCat..41270181H
Altcode:
Observations of H2O maser sources on the 13.7m radio
telesc Purple Mountain Observatory from 1990 Aug. to 1994 Jan. are
summarized. For searching new water masers, the total number of search
candidates is about 360, with 110 objects detected. Among them are
96 new detections. A list of the new detections and their spectra are
presented. (1 data file).
Title: Two-dimensional Anelastic MHD Simulations of the Buoyant Rise
of Magnetic Flux Tubes in the Solar Convection Zone
Authors: Fan, Y.; Zweibel, E. G.; Lantz, S. R.
Bibcode: 1997SPD....28.1704F
Altcode: 1997BAAS...29..921F
We perform two-dimensional simulations of the buoyant rise of
twisted horizontal magnetic flux tubes through an adiabatically
stratified layer representing the solar convection zone. The numerical
calculations employ the anelastic approximation of the basic MHD
equations. We confirm the results of recent compressible simulations
by Moreno-Insertis and Emonet that the transverse component of the tube
magnetic field can prevent the splitting of the tube into a vortex pair,
and that most of the flux in the initial tube cross-section rises in
the form of a rigid body and reaches a terminal speed similar to the
prediction of the thin flux tube model. Furthermore, we studied the
interaction between a pair of buoyant flux tubes as they rise side by
side. Our simulations show that the vortices in the wakes of the two
tubes interact and are continuously shed by the tubes. As a result
each tube gains around it a net circulation of the opposite sign of
the shed eddy and experiences a periodic lift force which causes the
tubes to show an oscillatory horizontal motion as they rise.
Title: Doppler Acoustic Diagnostics of Subsurface Solar Magnetic
Structure
Authors: Lindsey, C.; Braun, D. C.; Jefferies, S. M.; Woodard, M. F.;
Fan, Y.; Gu, Y.; Redfield, S.
Bibcode: 1996ApJ...470..636L
Altcode:
We used the Bartol-NSO-NASA South Pole helioseismic observations of 1991
January to probe the subsurface structure of active regions to depths
of ∼15,000 km. The helioseismic signature we particularly examine is
intended to register acoustic Doppler effects caused by horizontal flows
associated with the active region. We propose to show that the Doppler
acoustic signature of horizontal flows is particularly well suited
for deep subsurface diagnostics in terms of vertical discrimination
of the structure. This study is based primarily on observations of
NOAA Active Regions 6431, 6432, 6440, and 6442 between 1991 January
1 and January 8. We interpret the acoustic signatures we find in
terms of a general outflow of the solar medium surrounding the active
region. The acoustic signatures are strongly dependent on wavenumber,
which suggests an outflow that is quite weak near the surface, the upper
4000 km of the subphotosphere, but which increases strongly with depth
to velocities of several hundred meters per second at 15,000 km. This
depth profile evolves rapidly as the active region matures. Young
active regions show a strong outflow signature for waves that explore
depths between 4000 and 8000 km. As the active region matures, the
outflow vacates these intermediate layers and submerges to depths
mostly below 8000 km. We examine the location of AR 6442 for a
possible preemergence signature. We also show evidence for extended,
relatively superficial flows in the quiet Sun between the active region
bands directed roughly into the active region bands.
Title: Radiative Heating and the Buoyant Rise of Magnetic Flux Tubes
in the Solar interior
Authors: Fan, Y.; Fisher, G. H.
Bibcode: 1996SoPh..166...17F
Altcode:
We study the effect of radiative heating on the evolution of thin
magnetic flux tubes in the solar interior and on the eruption of
magnetic flux loops to the surface. Magnetic flux tubes experience
radiative heating because (1) the mean temperature gradient in the
lower convection zone and the overshoot region deviates substantially
from that of radiative equilibrium, and hence there is a non-zero
divergence of radiative heat flux; and (2) the magnetic pressure of the
flux tube causes a small change of the thermodynamic properties within
the tube relative to the surrounding field-free fluid, resulting in an
additional divergence of radiative heat flux. Our calculations show
that the former constitutes the dominant source of radiative heating
experienced by the flux tube.
Title: Helioseismic Measurements of Subsurface Outflows From Sunspots
Authors: Braun, D. C.; Fan, Y.; Lindsey, C.; Jefferies, S. M.
Bibcode: 1996AAS...188.6911B
Altcode: 1996BAAS...28Q.937B
We measure the mean frequencies of acoustic waves propagating toward
and away from sunspots employing a spot-centered Fourier-Hankel
decomposition of p-mode amplitudes as measured from observations made at
the South Pole in 1988 and 1991. There is a significant frequency shift
between the inward and outward traveling waves which is consistent with
the Doppler effect of a radial outflow from the sunspots. For p-modes
of temporal frequencies of 3 mHz it is observed that the frequency
shift decreases slightly with spatial frequency, for modes with degree
l between 160 to 600. From the l dependence of the frequency shift, we
infer that the mean radial outflow within the observed annular region
(which extends between 30 and 137 Mm from the spots) increases nearly
linearly with depth, reaching a magnitude of about 200 m/s at a depth
of 20 Mm. This outflow exhibits properties similar to flows recently
reported by Lindsey, et al. (1996 ApJ submitted) using spatially
sensitive local helioseismic techniques. This work is supported by
NSF Grant AST 9496171 and NASA Grant NAGW-4143.
Title: Doppler Acoustic Diagnostics of Subsurface Solar Magnetic
Structure
Authors: Lindsey, C.; Braun, D.; Jefferies, S.; Fan, Y.; Gu, Y.;
Redfield, S.
Bibcode: 1996AAS...188.7903L
Altcode: 1996BAAS...28R.955L
We used the Bartol-NSO-NASA South Pole helioseismic observations of 1991
January to study the subsurface structure of active regions to depths of
~ 15,000 km. The helioseismic signature we particularly examine is based
on acoustic Doppler effects caused by horizontal flows associated with
the active region. We demonstrate that the Doppler-acoustic signature
of horizontal flows is particularly well suited for deep subsurface
diagnostics in terms of vertical discrimination of the structure. This
study is based primarily on observations of NOAA active regions 6431,
6432, 6440 and 6442 between 1991 January 1 and January 8. We interpret
the Doppler signatures we find in terms of a general outflow of the
solar medium surrounding the active region. The existence of deep
subsurface structure is indicated by the strong dependence of the
Doppler signature on horizontal wavelength. The outflows in surface
layers, the upper 4,000 km of the subphotosphere, are quite weak but
increase strongly with depth to velocities of several hundred m/s at
15,000 km. This depth profile evolves rapidly as the active region
matures. Young active regions show strong outflows at depths between
4,000 and 8,000 km. As the active region matures, the outflow vacates
these intermediate layers and submerges to depths mostly below 8,000
km. We examine the location of Region 6442 for a possible pre-emergence
signature. We also show strong evidence for extended, relatively
superficial flows in the quiet Sun between the active-region bands
directed roughly into the active region bands.
Title: Radiative Heating and the Buoyant Rise of Magnetic Flux Tubes
in the Solar Interior
Authors: Fan, Y.; Fisher, G. H.
Bibcode: 1996AAS...188.3510F
Altcode: 1996BAAS...28..872F
We study the effect of radiative heating on the evolution of thin
magnetic flux tubes in the solar interior and on the eruption of
magnetic flux loops to the surface. Magnetic flux tubes experience
radiative heating because (1) the mean temperature gradient in the
lower convection zone and the overshoot region deviates substantially
from that of radiative equilibrium, and hence there is a non-zero
divergence of radiative heat flux; and (2) The magnetic pressure of
the flux tube causes a small change of the thermodynamic properties
within the tube relative to the surrounding field free fluid, resulting
in an additional divergence of radiative heat flux. We find that the
former constitutes the dominant source of radiative heating experienced
by the flux tube. In the overshoot region, the radiative heating is
found to cause a quasi-static rising of the toroidal flux tubes with
an upward drift velocity ~ 10(-3) | delta |^ {-1} cm s(-1) , where
delta equiv bigtriangledown - bigtriangledown _ad < 0 describes the
subadiabaticity in the overshoot layer. Using numerical simulations we
study the formation of ``Omega '' shaped emerging loops from toroidal
flux tubes in the overshoot region as a result of radiative heating. The
initial toroidal tube is assumed to be non-uniform in its thermodynamic
properties along the tube and lies at varying depths beneath the base
of the convection zone. The tube is initially in a state of neutral
buoyancy with the internal density of the tube plasma equal to the local
external density. We find from our numerical simulations that such a
toroidal tube rises quasi-statically due to radiative heating. The top
portion of the non-uniform tube first enters the convection zone and
may be brought to an unstable configuration which eventually leads to
the eruption of an anchored flux loop to the surface.
Title: Diagnostics of a Subsurface Radial Outflow From a Sunspot
Authors: Braun, D. C.; Fan, Y.; Lindsey, C.; Jefferies, S. M.
Bibcode: 1996astro.ph..3078B
Altcode:
We measure the mean frequencies of acoustic waves propagating toward
and away from a sunspot employing a spot-centered Fourier-Hankel
decomposition of p-mode amplitudes as measured from a set of
observations made at the South Pole in 1991. We demonstrate that
there is a significant frequency shift between the inward and outward
traveling waves which is consistent with the Doppler effect of a radial
outflow from the sunspot. For p-modes of temporal frequencies of 3
mHz it is observed that the frequency shift decreases slightly with
spatial frequency, for modes with degree l between 160 to 600. From
the l dependence of the frequency shift, we infer that the mean radial
outflow within the observed annular region (which extends between 30 and
137 Mm from the spot) increases nearly linearly with depth, reaching a
magnitude of about 200 m/s at a depth of 20 Mm. This outflow exhibits
properties similar to flows recently reported by Lindsey, et al. (1996)
using spatially sensitive local helioseismic techniques.
Title: The Dynamics of Magnetic Flux Tubes in the Solar Convection
Zone
Authors: Fisher, G. H.; Fan, Y.; Longcope, D. W.; Linton, M. C.
Bibcode: 1996mpsa.conf..329F
Altcode: 1996IAUCo.153..329F
No abstract at ADS
Title: Scattering of p-Modes by Sunspots. II. Calculations of Phase
Shifts from a Phenomenological Model
Authors: Fan, Y.; Braun, D. C.; Chou, D. -Y.
Bibcode: 1995ApJ...451..877F
Altcode:
We model the scattering of p-mode waves in a polytropic atmosphere
by localized inhomogeneities in wave speed, pressure, and density
of the medium. The effect of the inhomogeneities is attributed to
a source term in the pressure wave equation. The inhomogeneous wave
equation for the scattered waves is solved under the simplification
of the Born approximation. From the solution for the scattered waves,
we compute the phase shifts between the incoming and outgoing waves of
individual modes. We find that the variations of the computed
phase shifts with degree l and radial order n of the modes show
different behavior for inhomogeneities with different characteristic
depths. Depths significantly shallower than the depth of the modes
seem to show a phase shift dependence on l and n that is similar to
the qualitative behavior of the observed phase shifts produced by
sunspots. Direct quantitative comparison of the computed phase shifts
with observations is limited to modes with lower degree (l < 200)
in which the observed phase shifts are reasonably small so that the
Born approximation is applicable. We find that for inhomogeneities
with a wave speed contrast reasonable for sunspots, occupying a volume
described by a characteristic depth D 108 cm and horizontal radius R ≍
2.5 × 109 cm, the computed phase shifts at lower l range
are in agreement with the observed phase shifts from sunspots in both
their magnitudes as well as their variation with l and frequency (or n).
Title: An atlas of H2O maser observations on the 13.7 m
radio telescope of Purple Mountain Observatory.
Authors: Han, F.; Mao, R. Q.; Lu, J.; Lei, C. M.; Wu, Y. F.; Sun, J.;
Wang, J. S.; Pei, C. C.; Xiang, D. L.; Fan, Y.; Tang, G. S.; Ji, H. R.
Bibcode: 1995PPMtO..14..184H
Altcode:
Observations of H2O maser sources with the 13.7 m radio
telescope of Purple Mountain Observatory from August 1990 to January
1994 are briefly described and the results are presented. A total number
of 435 objects were observed. Of these, 195 objects were detected,
with 108 new detections.
Title: An atlas of H2O maser observations on the 13.7m radio telescope
of Purple Mountain Observatory.
Authors: Han, F.; Mao, R. Q.; Lei, C. M.; Wu, Y. F.; Sun, J.; Wang,
J. S.; Pei, C. C.; Xiang, D. L.; Fan, Y.; Tang, G. S.; Ji, H. R.
Bibcode: 1995PPMtO..14..185H
Altcode:
No abstract at ADS
Title: Ephemeral Regions and the Diffusion of Photospheric Magnetic
Fields
Authors: Harvey, K. L.; Fan, Y.
Bibcode: 1995SPD....26.1009H
Altcode: 1995BAAS...27..978H
No abstract at ADS
Title: Observations and Models of p-Mode Scattering by Sunspots
Authors: Braun, D. C.; Fan, Y.
Bibcode: 1995SPD....26..403B
Altcode: 1995BAAS...27..954B
No abstract at ADS
Title: On the Post-Emergence Evolutions of Active Region Flux Tubes
in the Solar Convection Zone
Authors: Fan, Y.; Fisher, G. H.
Bibcode: 1995SPD....26.1004F
Altcode: 1995BAAS...27..977F
No abstract at ADS
Title: Comparisons between Theory and Observation of Active Region
Tilts
Authors: Fisher, G. H.; Fan, Y.; Howard, R. F.
Bibcode: 1995ApJ...438..463F
Altcode:
Active regions in the Sun are generally tilted relative to the azimuthal
direction, with the leading side being closer to the equator than the
following side. This tilts is known to increase with latitude. Recently,
theoretical calculations of the dynamics of emerging, initially toroidal
active-region flux tubes have been done, showing that the observed
tilts can be explained by the Coriolis force acting on a diverging
flow field in emerging flux loops. The calculations of Fan, Fisher,
& McClymont predict that alpha proportional to Phi1/4
B0 exp -5/4 sin theta, where alpha is the tilt angle of
the active region, B0 is the magnetic field strength of the
active-region flux tube near the base of the convection zone, and phi is
the amount of magnetic flux in the tube. We compare these theoretical
predictions with the behavior of a sample of 24,701 sunspot groups
observed at Mount Wilson over a period of 68 yr, using the polarity
separation distance d as a proxy for phi. Our major findings are given.
Title: Dynamics of Emerging Active Region Flux Loops
Authors: Fan, Y.; Fisher, G. H.; McClymont, A. N.
Bibcode: 1994ApJ...436..907F
Altcode:
The buoyant rise of a magnetic flux loop arising from a single perturbed
segment of a toroidal flux ring lying slightly beneath the base of the
convection zone is studied by way of numerical simulations. We have
considered flux loop evolution assuming both solid-body rotation,
and differential rotation consistent with recent results from
helioseismology. Our major results are presented, and we offer some
speculations on the decay of active regions, based on the results of our
studies. We speculate that as plasma in the tube attempts to establish
hydrostatic equilibrium along the field lines after the flux emergence
has taken place, the tube field strength at some intermediate depths
below the surface becomes sufficiently small at the surface portions
of the tube (which have cooled and undergone convective collapse)
become dynamically disconnected from those portions near the base
of the convection zone. The surface proportions of the emerged flux
tubes are then transported by motions near the photosphere, such as
supergranular convection and meridional flow.
Title: A Model of P-mode Scattering by Sunspots
Authors: Fan, Y.; Braun, D. C.
Bibcode: 1994AAS...185.4406F
Altcode: 1994BAAS...26.1377F
It has recently been discovered that sunspots scatter intermediate and
high-degree p-modes. The scattering may be characterized by a shift
in phase between modes travelling toward and away from the spot. These
observations offer the hope that suitable models of the scattering may
yield important clues about the subsurface evolution and structure
of magnetic regions. We model the scattering of p-mode waves in a
polytropic atmosphere by localized inhomogeneities in compressibility
(the wave speed), density and pressure of the media. The effect of the
inhomogeneities is to introduce a source term in the pressure wave
equation. We solve this inhomogeneous equation for the scattered
wave amplitudes using standard Green's function techniques under
the simplification of the Born approximation. We found that with
reasonable strength (or contrast) of the inhomogeneities we can
obtain phase shifts between the outgoing and the in-going waves
similar to observations of p-modes in both the magnitude and degree
(l) dependence. We discuss how the strength of the scattered waves may
depend on the depth distribution of the inhomogeneities. This work is
supported by a NSF grant AST-9496171 and NASA grant NAGW-4143 awarded
to DCB. YF is supported by ONR grant N00014-91-J-1040.
Title: Twisting Motions in Emerging Active Region Flux Tubes
Authors: Fisher, G. H.; Fan, Y.
Bibcode: 1993BAAS...25R1206F
Altcode:
No abstract at ADS
Title: The Origin of Morphological Asymmetries in Bipolar Active
Regions
Authors: Fan, Y.; Fisher, G. H.; Deluca, E. E.
Bibcode: 1993ApJ...405..390F
Altcode:
A series of 3D numerical simulations was carried out to examine the
dynamical evolution of emerging flux loops in the solar convective
envelope. The innermost portions of the loops are anchored beneath the
base of the convective zone by the subadiabatic temperature gradient
of the underlying overshoot region. It is found that, as the emerging
loops approach the photosphere, the magnetic field strength of the
leading side of each rising loop is about twice as large as that of the
following side at the same depth. The evacuation of plasma out of the
leading side of the rising loop results in an enhanced magnetic field
strength there compared with the following side. It is argued that this
result provides a natural explanation for the fact that the preceding
(leading) polarity tends to have a less organized and more fragmented
appearance, and that the preceding spots tend to be larger in area and
fewer in number, and have a longer lifetime than the following spots.
Title: The Evolution of Anchored Magnetic Flux Loops in the Convective
Envelope of the Sun
Authors: Fan, Y.; Fisher, G. H.; Deluca, E. E.
Bibcode: 1993ASPC...42...89F
Altcode: 1993gong.conf...89F
No abstract at ADS
Title: Local Acoustic Diagnostics of the Solar Interior
Authors: Braun, D. C.; Lindsey, C.; Fan, Y.; Jefferies, S. M.
Bibcode: 1992ApJ...392..739B
Altcode:
Two diagnostic utilities, acoustic power maps, and surface acoustic
flux maps are used to explore the local diagnostics of magnetic field
structure in the solar interior. The acoustic power maps, constructed
from 50 hr of continuous K-line intensity images, show three general
features: acoustic power deficits at 3 mHz corresponding to surface
magnetic flux, acoustic power enhancements at 6 mHz surrounding the
exterior of magnetic regions, and occasional power deficits at 3 mHz
which extend beyond magnetic regions visible on the surface to regions
of quiet-sun. Surface acoustic flux vector maps of two active regions
were constructed for two 6-hr time-series of Dopplergrams. Both maps
show the divergence of 3-mHz acoustic flux into surface magnetic
structures and also sources and sinks of wave energy which are not
associated with surface features.
Title: Prospects in Acoustic Holography of the Solar Interior
Authors: Lindsey, C.; Braun, D. C.; Fan, Y.; Jefferies, S. M.
Bibcode: 1992AAS...180.1703L
Altcode: 1992BAAS...24..753L
Acoustic power maps of the solar surface show strong evidence
of magnetic structure crossing the solar equator not far beneath
the photosphere to connect the active latitude bands. These maps,
generated using the Bartol-NSO-NASA South Pole Observations show long
finger-like acoustic shadows we think are caused by absorption of
acoustic energy by the submerged magnetic structure. These features
suggest a solar interior magnetic structure quite different from any
previously expected. These new results open the prospect of a new and
powerful solar interior diagnostic based on acoustic holography.
Title: On the Dynamics of Emerging Toroidal Magnetic Flux Tubes
Authors: Fan, Y.; Fisher, G. H.; Deluca, E. E.
Bibcode: 1992AAS...180.0502F
Altcode: 1992BAAS...24..733F
We study the dynamic evolution of emerging toroidal magnetic flux
rings in the solar convective envelope by carrying out 3D numerical
simulations based on the thin flux tube approximation of Spruit. We
find: 1)For an axisymmetric flux ring, the aerodynamic drag force
experienced by the ring when moving with respect to the ambient
fluid transfers no angular momentum to the ring. Therefore in
both cases, with or without the drag force, the ring moves nearly
parallel to the rotational axis of the sun and emerges at a latitude
significantly poleward of sunspot zones, as pointed out by Choudhuri
and Gilman. However, for a non-axisymmetric flux ring (i.e. with
wave-like undulations along its circumference), the aerodynamic drag
force can transfer angular momentum to the flux ring, and therefore
reduces the latitude of flux emergence to within the observed sunspot
latitudes. 2)As each apex of a flux loop rises due to the magnetic
buoyancy force, gas inside the flux tube tends to diverge from the
apex. In the meantime, however, the Coriolis force drives a flow
within the flux tube opposite to the direction of rotation. Thus the
point of maximum divergence in the flow within the tube is shifted
from the apex into the leading side (in the direction of rotation)
of the emerging loop. The evacuation of plasma from the leading side
of the loop results in a much lower internal gas pressure there as
compared to that in the following side at the same depth. Therefore,
the magnetic field strength is stronger on the leading side. The
numerical simulations show that the field strength in the leading side
of the loop can be twice as large as that of the following side at the
same depth. This result offers a simple explanation for the observed
fact that the leading polarity of an active region is more compact,
forms sunspots more easily, and has a longer life time than does the
following polarity.
Title: Fine Structures in the Solar Radio Burst at 2-CENTIMETER
Waveband
Authors: Gao, Z. M.; Li, Z. Y.; Huo, C. P.; Fan, Y.
Bibcode: 1992AcApS..12..167G
Altcode:
No abstract at ADS
Title: Temporal Fine Structure of Solar Radio Burst at 2-CENTIMETER
Waveband
Authors: Gao, Z. M.; Li, Z. Y.; Huo, C. P.; Fan, Y.
Bibcode: 1991AcApS..11..288G
Altcode:
No abstract at ADS
Title: The Role of Slow Mode Waves in p-mode Absorption by Sunspots
Authors: Fan, Y.; Fisher, G. H.; McClymont, A. N.
Bibcode: 1991BAAS...23Q1049F
Altcode:
No abstract at ADS
Title: AR:5395 - Preliminary Analysis of the Double Peak Structures
of Microwave Bursts
Authors: Gao, Z. M.; Li, W. D.; Li, Z. Y.; Huo, C. P.; Fan, Y.; Fu,
Q. J.
Bibcode: 1990PYunO...4..106G
Altcode:
No abstract at ADS
Title: Vertical Currents in a Flare-Productive Active Region
Authors: Fan, Y.; Canfield, R. C.; McClymont, A. N.
Bibcode: 1990BAAS...22..827F
Altcode:
No abstract at ADS
Title: The Magnetic Morphology of Chromospheric Particle Precipitation
in Three October 1989 (AR 5747) Flares
Authors: Leka, K. D.; Canfield, R. C.; Wülser, J. -P.; Fan, Y.
Bibcode: 1990BAAS...22..824L
Altcode:
No abstract at ADS
Title: A New Concept of Constructing an Accurate Coordinate System
from Groundbased Optical Observations
Authors: Mao, W.; Hu, X. C.; Guo, X. J.; Fan, Y.
Bibcode: 1990IAUS..141..129M
Altcode:
No abstract at ADS
Title: Significance of Groundbased Fundamental Astrometry during
Spacetime
Authors: Fan, Y.; Mao, W.
Bibcode: 1990PrA.....8..214F
Altcode:
No abstract at ADS
Title: Result of Solar 2-CENTIMETER Waveband in the Joint Observation
1989JAN12-19
Authors: Gao, Z. M.; Li, Z. Y.; Huo, C. P.; Zhai, P. J.; Fan, Y.
Bibcode: 1989PYunO.155....1G
Altcode:
No abstract at ADS
Title: Astronomical Review of High Time Resolution Radio Observational
Techniques
Authors: Fan, Y.; Gao, Z. M.; Huo, C. P.
Bibcode: 1988PYunO...4...33F
Altcode:
No abstract at ADS
Title: The quasi-absolute determination of the refraction correction
by means of middle and lower latitude meridian circle.
Authors: Mao, W.; Li, Z. -M.; Fan, Y.; Hu, X. -C.; Du, M. -H.
Bibcode: 1987POBeo..35..315M
Altcode:
A method is proposed in this paper to determine the values of
atmospheric refraction by observing a star in the direction of the
prime vertical with a Middle and Lower Latitude Meridian Circle. It is
expected to compile with these observations an atmospheric refraction
table much closer to the actual situation.
Title: Grating form of the micrometer of a low-latitude meridian
circle. II.
Authors: Wang, L. -K.; Fan, Y.; Mao, W.
Bibcode: 1987PYunO...2....1W
Altcode:
No abstract at ADS
Title: Determination of the irregularity of the pivot of the
horizontal axisof a meridian circle by means of an axis collimator.
Authors: Fan, Y.; Wang, L. -K.; Mao, W.
Bibcode: 1987PYunO...2....7F
Altcode:
No abstract at ADS
Title: A New Method of Determining Absolute Azimuth and Latitude
and Suggestion for a New Type of Meridian Circle
Authors: Mao, W.; Li, Z. M.; Fan, Y.; Hu, S. S.; Du, M. H.
Bibcode: 1986IAUS..109..551M
Altcode:
This article describes a new method by which azimuth and the
instantaneous latitude of a meridian-prime vertical-transit instrument
can be determined absolutely in mid- and low-latitude areas, and
discusses some experimental observations obtained on a remodeled Zeiss
transit instrument. Requirements for the development of a new type of
transit circle along the lines of this new method are also presented.
Title: Analysis of the Effects of Errors on the Reading of the
Graduated Circle
Authors: Fan, Y.; Mao, W.
Bibcode: 1986PYunO...1...41F
Altcode:
The authors propose a "one-shot determination method" for fixing
the angular distance of the reading microscope. The effects of
the eccentricity error of the circle, the tilt of the circle and
the reading microscopes and the flexure of the circle on the circle
reading are discussed. It is proved that the arbitrary distribution
of microscopes by means of the method for fixing the angular distance
will not affect the final accuracy of the circle reading.
Title: The Comparison of Two Methods for the Absolute Determination
of the Azimuth of a Meridian Circle
Authors: Fan, Y.; Mao, W.
Bibcode: 1986PYunO...1...36F
Altcode:
The conventional circumpolar star - azimuth mark observation method
is compared to the newly proposed first vertical meridian circle
observation method. The results show that much more accurate determined
values can be obtained if the new method is used.
Title: The Observation of a Star by Making a 180DEG Rotation of the
Horizontal Axis of a Lower-Latitude Meridian Circle
Authors: Fan, Y.; Li, Z. M.; Mao, W.
Bibcode: 1985PYunO...1...21F
Altcode:
No abstract at ADS
Title: The Grating Form of the Micrometer of a Low-Latitude Meridian
Circle
Authors: Mao, W.; Fan, Y.
Bibcode: 1985PYunO...2...34M
Altcode:
No abstract at ADS
Title: The Absolute Determination the Refraction Correction with a
Lower-Latitude Meridian Circle
Authors: Mao, W.; Li, Z. M.; Fan, Y.; Hu, X. C.; Du, M. H.
Bibcode: 1985PYunO...1...29M
Altcode:
No abstract at ADS
Title: A new method of absolute determination of a transit
instrument's azimuth and latitude.
Authors: Mao, W.; Li, Z.; Fan, Y.; Hu, X.; Du, M.; Li, H.
Bibcode: 1984SSSMP..27.1183M
Altcode:
This article deals with a new method of the absolute determination
for the meridian observations in mid and low latitude areas and
raises a limitation that the traditional method cannot be used at low
latitudes. The new method will play an important role in improving
the reference system of the fundamental celestial sphere. Experimental
observations with a reconstructed Zeiss transit instrument show that
the principle of the new method is right.
Title: Determination of the azimuth error of the transit instrument
by means of prime vertical observations
Authors: Mao, W.; Li, Z. -M.; Fan, Y.; Hu, X. -S.; Li, H.
Bibcode: 1983AcASn..24..169M
Altcode: 1984AcASn..24..169M
The principle and some test results of determining the instrumental
azimuth by measuring the times of passage of the same stars through the
meridian and the prime vertical are presented. The test measurements
were made on a reconstructed Zeiss transit instrument equipped with
four supporting pillars. The results of the test show that the method
is successful. Applied to the meridian circle, this method replaces
the traditional method of determining the absolute azimuth by observing
circumpolar stars and thereby bypases the difficulties inherent therein
and the errors involved in the method of transfer via the azimuth mark.
Title: SiO isotopic maser emission from VY Canis Majoris.
Authors: Deguchi, S.; Good, J.; Fan, Y.; Mao, X.; Wang, D.; Ukita, N.
Bibcode: 1983ApJ...264L..65D
Altcode:
To investigate the peculiar line shape of the ground-state SiO emission
from VY CMa, the (Si-28)O, (Si-29)O, and (Si-30)O emission profiles were
observed. Strong narrow emission in the (Si-29)O spectrum was detected,
twice the strength of the (Si-28)O narrow emission. No (Si-30)O emission
was detected at the limit of the noise. The observations are difficult
to interpret in terms of a spherically symmetric, expanding shell,
but they can be explained by a model in which the inner envelope
is not a shell but rather forms a rotating edge-on disk. The maser
amplification would occur mainly in a radial direction since there
is no radial velocity gradient. The center of the maser emission thus
coincides with the velocity of the central star. The pumping radiation
comes from the central star. The inversion is produced by the same
eight-micron absorption mechanism as in the Robinson and Van Blerkom
(1981) model, but here the reradiated photons escape in a direction
perpendicular to the disk.
Title: A Circuit Controlled Installation for Refitting a Transit
Authors: Li, Z. M.; Hu, X. C.; Fan, Y.; Du, M. H.; Mao, W.
Bibcode: 1983PYunO...1...29L
Altcode:
No abstract at ADS
Title: A further discussion on the mass loss of Mira stars
Authors: Sun, J.; Wu, S. -M.; Fan, Y.
Bibcode: 1982AcApS...2...49S
Altcode:
Mass-loss rates for 42 Mira-type variables with a known period, spectral
type, and associated double-peak OH maser spectrum are calculated
on the assumption of mass loss via a stellar wind driven by radiation
pressure. The relations between mass-loss rate and luminosity, pulsation
period, maser-shell expansion velocity, and effective temperature are
determined. The results show that the mass-loss rate of a Mira-type
variable is proportional to the first power of luminosity, is linearly
correlated with both pulsation period and maser-shell expansion
velocity, but is not correlated with effective temperature. It is
concluded that pulsation period and maser-shell expansion velocity
are linearly correlated for Mira stars.
Title: The Test Results of the Azimuth Equations Absolutely Determined
with a Refitted Transit Instrument
Authors: Li, Z. M.; Fan, Y.; Hu, X. C.; Mao, W.
Bibcode: 1982PYunO...2...27L
Altcode:
No abstract at ADS
Title: Determining the Absolute Parameters of the Meridian Circle
by Observing the Prime Vertical - Part Three - the Overall Effects
of Several Errors and Corrected Values on the Determination of
Azimuth Equations
Authors: Fan, Y.; Hu, X. C.; Li, Z. M.; Mao, W.
Bibcode: 1982PYunO...2...13F
Altcode:
No abstract at ADS
Title: Statistics of correlation between the velocity separation
of double peaks of maser source and associated variable's period,
and a mass loss from variables
Authors: Fan, Y.; Sun, J.
Bibcode: 1980AcASn..21..379F
Altcode:
No abstract at ADS