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Author name code: lin-haosheng
ADS astronomy entries on 2022-09-14
author:"Lin, Haosheng" AND aff:"Hawaii"
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Title: Dark Energy Survey year 3 results: Constraints on cosmological
parameters and galaxy-bias models from galaxy clustering and
galaxy-galaxy lensing using the redMaGiC sample
Authors: Pandey, S.; Krause, E.; DeRose, J.; MacCrann, N.;
Jain, B.; Crocce, M.; Blazek, J.; Choi, A.; Huang, H.; To, C.;
Fang, X.; Elvin-Poole, J.; Prat, J.; Porredon, A.; Secco, L. F.;
Rodriguez-Monroy, M.; Weaverdyck, N.; Park, Y.; Raveri, M.; Rozo, E.;
Rykoff, E. S.; Bernstein, G. M.; Sánchez, C.; Jarvis, M.; Troxel,
M. A.; Zacharegkas, G.; Chang, C.; Alarcon, A.; Alves, O.; Amon, A.;
Andrade-Oliveira, F.; Baxter, E.; Bechtol, K.; Becker, M. R.; Camacho,
H.; Campos, A.; Carnero Rosell, A.; Carrasco Kind, M.; Cawthon,
R.; Chen, R.; Chintalapati, P.; Davis, C.; Di Valentino, E.; Diehl,
H. T.; Dodelson, S.; Doux, C.; Drlica-Wagner, A.; Eckert, K.; Eifler,
T. F.; Elsner, F.; Everett, S.; Farahi, A.; Ferté, A.; Fosalba, P.;
Friedrich, O.; Gatti, M.; Giannini, G.; Gruen, D.; Gruendl, R. A.;
Harrison, I.; Hartley, W. G.; Huff, E. M.; Huterer, D.; Kovacs, A.;
Leget, P. F.; McCullough, J.; Muir, J.; Myles, J.; Navarro-Alsina, A.;
Omori, Y.; Rollins, R. P.; Roodman, A.; Rosenfeld, R.; Sevilla-Noarbe,
I.; Sheldon, E.; Shin, T.; Troja, A.; Tutusaus, I.; Varga, T. N.;
Wechsler, R. H.; Yanny, B.; Yin, B.; Zhang, Y.; Zuntz, J.; Abbott,
T. M. C.; Aguena, M.; Allam, S.; Annis, J.; Bacon, D.; Bertin, E.;
Brooks, D.; Burke, D. L.; Carretero, J.; Conselice, C.; Costanzi,
M.; da Costa, L. N.; Pereira, M. E. S.; De Vicente, J.; Dietrich,
J. P.; Doel, P.; Evrard, A. E.; Ferrero, I.; Flaugher, B.; Frieman,
J.; García-Bellido, J.; Gaztanaga, E.; Gerdes, D. W.; Giannantonio,
T.; Gschwend, J.; Gutierrez, G.; Hinton, S. R.; Hollowood, D. L.;
Honscheid, K.; James, D. J.; Jeltema, T.; Kuehn, K.; Kuropatkin,
N.; Lahav, O.; Lima, M.; Lin, H.; Maia, M. A. G.; Marshall, J. L.;
Melchior, P.; Menanteau, F.; Miller, C. J.; Miquel, R.; Mohr, J. J.;
Morgan, R.; Palmese, A.; Paz-Chinchón, F.; Petravick, D.; Pieres,
A.; Plazas Malagón, A. A.; Sanchez, E.; Scarpine, V.; Serrano, S.;
Smith, M.; Soares-Santos, M.; Suchyta, E.; Tarle, G.; Thomas, D.;
Weller, J.; DES Collaboration
2022PhRvD.106d3520P Altcode: 2021arXiv210513545P
We constrain cosmological parameters and galaxy-bias parameters
using the combination of galaxy clustering and galaxy-galaxy lensing
measurements from the Dark Energy Survey (DES) year-3 data. We describe
our modeling framework and choice of scales analyzed, validating their
robustness to theoretical uncertainties in small-scale clustering
by analyzing simulated data. Using a linear galaxy-bias model and
redMaGiC galaxy sample, we obtain 10% constraints on the matter
density of the Universe. We also implement a nonlinear galaxy-bias
model to probe smaller scales that includes parametrization based on
hybrid perturbation theory and find that it leads to a 17% gain in
cosmological constraining power. We perform robustness tests of our
methodology pipeline and demonstrate stability of the constraints
to changes in the theory model. Using the redMaGiC galaxy sample as
foreground lens galaxies and adopting the best-fitting cosmological
parameters from DES year-1 data, we find the galaxy clustering and
galaxy-galaxy lensing measurements to exhibit significant signals akin
to decorrelation between galaxies and mass on large scales, which is
not expected in any current models. This likely systematic measurement
error biases our constraints on galaxy bias and the S<SUB>8</SUB>
parameter. We find that a scale-, redshift- and sky-area-independent
phenomenological decorrelation parameter can effectively capture
this inconsistency between the galaxy clustering and galaxy-galaxy
lensing. We trace the source of this correlation to a color-dependent
photometric issue and minimize its impact on our result by changing
the selection criteria of redMaGiC galaxies. Using this new sample, our
constraints on the S<SUB>8</SUB> parameter are consistent with previous
studies and we find a small shift in the Ω<SUB>m</SUB> constraints
compared to the fiducial redMaGiC sample. We infer the constraints on
the mean host-halo mass of the redMaGiC galaxies in this new sample
from the large-scale bias constraints, finding the galaxies occupy
halos of mass approximately 1.6 ×10<SUP>13</SUP> M<SUB>⊙</SUB>/h .
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Title: Dark Energy Survey Year 3 results: Exploiting small-scale
information with lensing shear ratios
Authors: Sánchez, C.; Prat, J.; Zacharegkas, G.; Pandey, S.; Baxter,
E.; Bernstein, G. M.; Blazek, J.; Cawthon, R.; Chang, C.; Krause,
E.; Lemos, P.; Park, Y.; Raveri, M.; Sanchez, J.; Troxel, M. A.;
Amon, A.; Fang, X.; Friedrich, O.; Gruen, D.; Porredon, A.; Secco,
L. F.; Samuroff, S.; Alarcon, A.; Alves, O.; Andrade-Oliveira, F.;
Bechtol, K.; Becker, M. R.; Camacho, H.; Campos, A.; Carnero Rosell,
A.; Carrasco Kind, M.; Chen, R.; Choi, A.; Crocce, M.; Davis, C.;
De Vicente, J.; DeRose, J.; Di Valentino, E.; Diehl, H. T.; Dodelson,
S.; Doux, C.; Drlica-Wagner, A.; Eckert, K.; Eifler, T. F.; Elsner,
F.; Elvin-Poole, J.; Everett, S.; Ferté, A.; Fosalba, P.; Gatti, M.;
Giannini, G.; Gruendl, R. A.; Harrison, I.; Hartley, W. G.; Herner,
K.; Huff, E. M.; Huterer, D.; Jarvis, M.; Jain, B.; Kuropatkin, N.;
Leget, P. -F.; MacCrann, N.; McCullough, J.; Muir, J.; Myles, J.;
Navarro-Alsina, A.; Rollins, R. P.; Roodman, A.; Rosenfeld, R.;
Rykoff, E. S.; Sevilla-Noarbe, I.; Sheldon, E.; Shin, T.; Troja,
A.; Tutusaus, I.; Varga, T. N.; Wechsler, R. H.; Yanny, B.; Yin,
B.; Zhang, Y.; Zuntz, J.; Abbott, T. M. C.; Aguena, M.; Allam, S.;
Bacon, D.; Bertin, E.; Bhargava, S.; Brooks, D.; Buckley-Geer, E.;
Burke, D. L.; Carretero, J.; Costanzi, M.; da Costa, L. N.; Pereira,
M. E. S.; Desai, S.; Dietrich, J. P.; Doel, P.; Evrard, A. E.; Ferrero,
I.; Flaugher, B.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.;
Gerdes, D. W.; Giannantonio, T.; Gschwend, J.; Gutierrez, G.; Hinton,
S. R.; Hollowood, D. L.; Honscheid, K.; Hoyle, B.; James, D. J.; Kuehn,
K.; Lahav, O.; Lima, M.; Lin, H.; Maia, M. A. G.; Marshall, J. L.;
Martini, P.; Melchior, P.; Menanteau, F.; Miquel, R.; Mohr, J. J.;
Morgan, R.; Palmese, A.; Paz-Chinchón, F.; Petravick, D.; Pieres, A.;
Plazas Malagón, A. A.; Rodriguez-Monroy, M.; Sanchez, E.; Scarpine,
V.; Schubnell, M.; Serrano, S.; Smith, M.; Soares-Santos, M.; Suchyta,
E.; Swanson, M. E. C.; Tarle, G.; Thomas, D.; To, C.; DES Collaboration
2022PhRvD.105h3529S Altcode: 2021arXiv210513542S
Using the first three years of data from the Dark Energy Survey
(DES), we use ratios of small-scale galaxy-galaxy lensing measurements
around the same lens sample to constrain source redshift uncertainties,
intrinsic alignments and other systematics or nuisance parameters of our
model. Instead of using a simple geometric approach for the ratios as
has been done in the past, we use the full modeling of the galaxy-galaxy
lensing measurements, including the corresponding integration over the
power spectrum and the contributions from intrinsic alignments and
lens magnification. We perform extensive testing of the small-scale
shear-ratio (SR) modeling by studying the impact of different effects
such as the inclusion of baryonic physics, nonlinear biasing, halo
occupation distribution descriptions and lens magnification, among
others, and using realistic N -body simulations of the DES data. We
validate the robustness of our constraints in the data by using
two independent lens samples with different galaxy properties, and
by deriving constraints using the corresponding large-scale ratios
for which the modeling is simpler. The results applied to the DES
Y3 data demonstrate how the ratios provide significant improvements
in constraining power for several nuisance parameters in our model,
especially on source redshift calibration and intrinsic alignments. For
source redshifts, SR improves the constraints from the prior by up
to 38% in some redshift bins. Such improvements, and especially the
constraints it provides on intrinsic alignments, translate to tighter
cosmological constraints when shear ratios are combined with cosmic
shear and other 2pt functions. In particular, for the DES Y3 data,
SR improves S<SUB>8</SUB> constraints from cosmic shear by up to 31%,
and for the full combination of probes (3 ×2 pt ) by up to 10%. The
shear ratios presented in this work are used as an additional likelihood
for cosmic shear, 2 ×2 pt and the full 3 ×2 pt in the fiducial DES
Y3 cosmological analysis.
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Title: Dark energy survey year 3 results: High-precision measurement
and modeling of galaxy-galaxy lensing
Authors: Prat, J.; Blazek, J.; Sánchez, C.; Tutusaus, I.; Pandey,
S.; Elvin-Poole, J.; Krause, E.; Troxel, M. A.; Secco, L. F.; Amon,
A.; DeRose, J.; Zacharegkas, G.; Chang, C.; Jain, B.; MacCrann, N.;
Park, Y.; Sheldon, E.; Giannini, G.; Bocquet, S.; To, C.; Alarcon,
A.; Alves, O.; Andrade-Oliveira, F.; Baxter, E.; Bechtol, K.; Becker,
M. R.; Bernstein, G. M.; Camacho, H.; Campos, A.; Carnero Rosell,
A.; Carrasco Kind, M.; Cawthon, R.; Chen, R.; Choi, A.; Cordero, J.;
Crocce, M.; Davis, C.; De Vicente, J.; Diehl, H. T.; Dodelson, S.;
Doux, C.; Drlica-Wagner, A.; Eckert, K.; Eifler, T. F.; Elsner, F.;
Everett, S.; Fang, X.; Farahi, A.; Ferté, A.; Fosalba, P.; Friedrich,
O.; Gatti, M.; Gruen, D.; Gruendl, R. A.; Harrison, I.; Hartley,
W. G.; Herner, K.; Huang, H.; Huff, E. M.; Huterer, D.; Jarvis, M.;
Kuropatkin, N.; Leget, P. -F.; Lemos, P.; Liddle, A. R.; McCullough,
J.; Muir, J.; Myles, J.; Navarro-Alsina, A.; Porredon, A.; Raveri,
M.; Rodriguez-Monroy, M.; Rollins, R. P.; Roodman, A.; Rosenfeld, R.;
Ross, A. J.; Rykoff, E. S.; Sanchez, J.; Sevilla-Noarbe, I.; Shin, T.;
Troja, A.; Varga, T. N.; Weaverdyck, N.; Wechsler, R. H.; Yanny, B.;
Yin, B.; Zuntz, J.; Abbott, T. M. C.; Aguena, M.; Allam, S.; Annis,
J.; Bacon, D.; Brooks, D.; Burke, D. L.; Carretero, J.; Conselice, C.;
Costanzi, M.; da Costa, L. N.; Pereira, M. E. S.; Desai, S.; Dietrich,
J. P.; Doel, P.; Evrard, A. E.; Ferrero, I.; Flaugher, B.; Frieman,
J.; García-Bellido, J.; Gaztanaga, E.; Gerdes, D. W.; Giannantonio,
T.; Gschwend, J.; Gutierrez, G.; Hinton, S. R.; Hollowood, D. L.;
Honscheid, K.; James, D. J.; Kuehn, K.; Lahav, O.; Lin, H.; Maia,
M. A. G.; Marshall, J. L.; Martini, P.; Melchior, P.; Menanteau, F.;
Miller, C. J.; Miquel, R.; Mohr, J. J.; Morgan, R.; Ogando, R. L. C.;
Palmese, A.; Paz-Chinchón, F.; Petravick, D.; Plazas Malagón, A. A.;
Sanchez, E.; Serrano, S.; Smith, M.; Soares-Santos, M.; Suchyta, E.;
Tarle, G.; Thomas, D.; Weller, J.; DES Collaboration
2022PhRvD.105h3528P Altcode: 2021arXiv210513541P
We present and characterize the galaxy-galaxy lensing signal measured
using the first three years of data from the Dark Energy Survey (DES
Y3) covering 4132 deg<SUP>2</SUP> . These galaxy-galaxy measurements
are used in the DES Y3 3 ×2 pt cosmological analysis, which combines
weak lensing and galaxy clustering information. We use two lens
samples: a magnitude-limited sample and the redMaGiC sample, which
span the redshift range ∼0.2 - 1 with 10.7 and 2.6 M galaxies,
respectively. For the source catalog, we use the METACALIBRATION
shape sample, consisting of ≃100 M galaxies separated into four
tomographic bins. Our galaxy-galaxy lensing estimator is the mean
tangential shear, for which we obtain a total SNR of ∼148 for MagLim
(∼120 for redMaGiC), and ∼67 (∼55 ) after applying the scale
cuts of 6 Mpc /h . Thus we reach percent-level statistical precision,
which requires that our modeling and systematic-error control be of
comparable accuracy. The tangential shear model used in the 3 ×2 pt
cosmological analysis includes lens magnification, a five-parameter
intrinsic alignment model, marginalization over a point mass to
remove information from small scales and a linear galaxy bias model
validated with higher-order terms. We explore the impact of these
choices on the tangential shear observable and study the significance
of effects not included in our model, such as reduced shear, source
magnification, and source clustering. We also test the robustness of
our measurements to various observational and systematics effects,
such as the impact of observing conditions, lens-source clustering,
random-point subtraction, scale-dependent METACALIBRATION responses,
point spread function residuals, and B modes.
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Title: Dark Energy Survey Year 3 results: Cosmology from cosmic
shear and robustness to data calibration
Authors: Amon, A.; Gruen, D.; Troxel, M. A.; MacCrann, N.; Dodelson,
S.; Choi, A.; Doux, C.; Secco, L. F.; Samuroff, S.; Krause, E.;
Cordero, J.; Myles, J.; DeRose, J.; Wechsler, R. H.; Gatti, M.;
Navarro-Alsina, A.; Bernstein, G. M.; Jain, B.; Blazek, J.; Alarcon,
A.; Ferté, A.; Lemos, P.; Raveri, M.; Campos, A.; Prat, J.; Sánchez,
C.; Jarvis, M.; Alves, O.; Andrade-Oliveira, F.; Baxter, E.; Bechtol,
K.; Becker, M. R.; Bridle, S. L.; Camacho, H.; Carnero Rosell, A.;
Carrasco Kind, M.; Cawthon, R.; Chang, C.; Chen, R.; Chintalapati, P.;
Crocce, M.; Davis, C.; Diehl, H. T.; Drlica-Wagner, A.; Eckert, K.;
Eifler, T. F.; Elvin-Poole, J.; Everett, S.; Fang, X.; Fosalba, P.;
Friedrich, O.; Gaztanaga, E.; Giannini, G.; Gruendl, R. A.; Harrison,
I.; Hartley, W. G.; Herner, K.; Huang, H.; Huff, E. M.; Huterer, D.;
Kuropatkin, N.; Leget, P.; Liddle, A. R.; McCullough, J.; Muir, J.;
Pandey, S.; Park, Y.; Porredon, A.; Refregier, A.; Rollins, R. P.;
Roodman, A.; Rosenfeld, R.; Ross, A. J.; Rykoff, E. S.; Sanchez,
J.; Sevilla-Noarbe, I.; Sheldon, E.; Shin, T.; Troja, A.; Tutusaus,
I.; Tutusaus, I.; Varga, T. N.; Weaverdyck, N.; Yanny, B.; Yin, B.;
Zhang, Y.; Zuntz, J.; Aguena, M.; Allam, S.; Annis, J.; Bacon, D.;
Bertin, E.; Bhargava, S.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.;
Carretero, J.; Costanzi, M.; da Costa, L. N.; Pereira, M. E. S.;
De Vicente, J.; Desai, S.; Dietrich, J. P.; Doel, P.; Ferrero, I.;
Flaugher, B.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.; Gerdes,
D. W.; Giannantonio, T.; Gschwend, J.; Gutierrez, G.; Hinton, S. R.;
Hollowood, D. L.; Honscheid, K.; Hoyle, B.; James, D. J.; Kron, R.;
Kuehn, K.; Lahav, O.; Lima, M.; Lin, H.; Maia, M. A. G.; Marshall,
J. L.; Martini, P.; Melchior, P.; Menanteau, F.; Miquel, R.; Mohr,
J. J.; Morgan, R.; Ogando, R. L. C.; Palmese, A.; Paz-Chinchón, F.;
Petravick, D.; Pieres, A.; Romer, A. K.; Sanchez, E.; Scarpine, V.;
Schubnell, M.; Serrano, S.; Smith, M.; Soares-Santos, M.; Tarle, G.;
Thomas, D.; To, C.; Weller, J.; DES Collaboration
2022PhRvD.105b3514A Altcode: 2021arXiv210513543A
<related-article ext-link-type="doi" related-article-type="companion"
xlink:href="10.1103/PhysRevD.105.023515"/>This work, together with
its companion paper, Secco, Samuroff et al. [Phys. Rev. D 105, 023515
(2022), 10.1103/PhysRevD.105.023515], present the Dark Energy Survey
Year 3 cosmic-shear measurements and cosmological constraints based on
an analysis of over 100 million source galaxies. With the data spanning
4143 deg<SUP>2</SUP> on the sky, divided into four redshift bins,
we produce a measurement with a signal-to-noise of 40. We conduct
a blind analysis in the context of the Lambda-Cold Dark Matter (Λ
CDM ) model and find a 3% constraint of the clustering amplitude,
S<SUB>8</SUB>≡σ<SUB>8</SUB>(Ω<SUB>m</SUB>/0.3 )0.<SUP>5</SUP>=0.75
9<SUB>-0.023</SUB><SUP>+0.025</SUP>. A Λ CDM -Optimized analysis,
which safely includes smaller scale information, yields a 2% precision
measurement of S<SUB>8</SUB>=0.77 2<SUB>-0.017</SUB><SUP>+0.018</SUP>
that is consistent with the fiducial case. The two low-redshift
measurements are statistically consistent with the Planck Cosmic
Microwave Background result, however, both recovered S<SUB>8</SUB>
values are lower than the high-redshift prediction by 2.3 σ and
2.1 σ (p -values of 0.02 and 0.05), respectively. The measurements
are shown to be internally consistent across redshift bins, angular
scales and correlation functions. The analysis is demonstrated to be
robust to calibration systematics, with the S<SUB>8</SUB> posterior
consistent when varying the choice of redshift calibration sample,
the modeling of redshift uncertainty and methodology. Similarly,
we find that the corrections included to account for the blending
of galaxies shifts our best-fit S<SUB>8</SUB> by 0.5 σ without
incurring a substantial increase in uncertainty. We examine the
limiting factors for the precision of the cosmological constraints and
find observational systematics to be subdominant to the modeling of
astrophysics. Specifically, we identify the uncertainties in modeling
baryonic effects and intrinsic alignments as the limiting systematics.
---------------------------------------------------------
Title: Dark Energy Survey Year 3 results: Cosmology from cosmic
shear and robustness to modeling uncertainty
Authors: Secco, L. F.; Samuroff, S.; Krause, E.; Jain, B.; Blazek,
J.; Raveri, M.; Campos, A.; Amon, A.; Chen, A.; Doux, C.; Choi, A.;
Gruen, D.; Bernstein, G. M.; Chang, C.; DeRose, J.; Myles, J.; Ferté,
A.; Lemos, P.; Huterer, D.; Prat, J.; Troxel, M. A.; MacCrann, N.;
Liddle, A. R.; Kacprzak, T.; Fang, X.; Sánchez, C.; Pandey, S.;
Dodelson, S.; Chintalapati, P.; Hoffmann, K.; Alarcon, A.; Alves,
O.; Andrade-Oliveira, F.; Baxter, E. J.; Bechtol, K.; Becker, M. R.;
Brandao-Souza, A.; Camacho, H.; Carnero Rosell, A.; Carrasco Kind, M.;
Cawthon, R.; Cordero, J. P.; Crocce, M.; Davis, C.; Di Valentino, E.;
Drlica-Wagner, A.; Eckert, K.; Eifler, T. F.; Elidaiana, M.; Elsner,
F.; Elvin-Poole, J.; Everett, S.; Fosalba, P.; Friedrich, O.; Gatti,
M.; Giannini, G.; Gruendl, R. A.; Harrison, I.; Hartley, W. G.; Herner,
K.; Huang, H.; Huff, E. M.; Jarvis, M.; Jeffrey, N.; Kuropatkin, N.;
Leget, P. -F.; Muir, J.; Mccullough, J.; Navarro Alsina, A.; Omori,
Y.; Park, Y.; Porredon, A.; Rollins, R.; Roodman, A.; Rosenfeld,
R.; Ross, A. J.; Rykoff, E. S.; Sanchez, J.; Sevilla-Noarbe, I.;
Sheldon, E. S.; Shin, T.; Troja, A.; Tutusaus, I.; Varga, T. N.;
Weaverdyck, N.; Wechsler, R. H.; Yanny, B.; Yin, B.; Zhang, Y.; Zuntz,
J.; Abbott, T. M. C.; Aguena, M.; Allam, S.; Annis, J.; Bacon, D.;
Bertin, E.; Bhargava, S.; Bridle, S. L.; Brooks, D.; Buckley-Geer,
E.; Burke, D. L.; Carretero, J.; Costanzi, M.; da Costa, L. N.; De
Vicente, J.; Diehl, H. T.; Dietrich, J. P.; Doel, P.; Ferrero, I.;
Flaugher, B.; Frieman, J.; García-Bellido, J.; Gaztanaga, E.; Gerdes,
D. W.; Giannantonio, T.; Gschwend, J.; Gutierrez, G.; Hinton, S. R.;
Hollowood, D. L.; Honscheid, K.; Hoyle, B.; James, D. J.; Jeltema, T.;
Kuehn, K.; Lahav, O.; Lima, M.; Lin, H.; Maia, M. A. G.; Marshall,
J. L.; Martini, P.; Melchior, P.; Menanteau, F.; Miquel, R.; Mohr,
J. J.; Morgan, R.; Ogando, R. L. C.; Palmese, A.; Paz-Chinchón, F.;
Petravick, D.; Pieres, A.; Plazas Malagón, A. A.; Rodriguez-Monroy,
M.; Romer, A. K.; Sanchez, E.; Scarpine, V.; Schubnell, M.; Scolnic,
D.; Serrano, S.; Smith, M.; Soares-Santos, M.; Suchyta, E.; Swanson,
M. E. C.; Tarle, G.; Thomas, D.; To, C.; DES Collaboration
2022PhRvD.105b3515S Altcode: 2021arXiv210513544S
This work and its companion paper, Amon et al. [Phys. Rev. D
105, 023514 (2022), 10.1103/PhysRevD.105.023514], present
cosmic shear measurements and cosmological constraints from
over 100 million source galaxies in the Dark Energy Survey
(DES) Year 3 data. We constrain the lensing amplitude parameter
S<SUB>8</SUB>≡σ<SUB>8</SUB>√{Ω<SUB>m</SUB>/0.3 } at the 3% level
in Λ CDM : S<SUB>8</SUB>=0.75 9<SUB>-0.023</SUB><SUP>+0.025</SUP>
(68% CL). Our constraint is at the 2% level when using angular scale
cuts that are optimized for the Λ CDM analysis: S<SUB>8</SUB>=0.77
2<SUB>-0.017</SUB><SUP>+0.018</SUP> (68% CL). With cosmic shear alone,
we find no statistically significant constraint on the dark energy
equation-of-state parameter at our present statistical power. We carry
out our analysis blind, and compare our measurement with constraints
from two other contemporary weak lensing experiments: the Kilo-Degree
Survey (KiDS) and Hyper-Suprime Camera Subaru Strategic Program
(HSC). We additionally quantify the agreement between our data and
external constraints from the Cosmic Microwave Background (CMB). Our DES
Y3 result under the assumption of Λ CDM is found to be in statistical
agreement with Planck 2018, although favors a lower S<SUB>8</SUB>
than the CMB-inferred value by 2.3 σ (a p -value of 0.02). This paper
explores the robustness of these cosmic shear results to modeling
of intrinsic alignments, the matter power spectrum and baryonic
physics. We additionally explore the statistical preference of our data
for intrinsic alignment models of different complexity. The fiducial
cosmic shear model is tested using synthetic data, and we report no
biases greater than 0.3 σ in the plane of S<SUB>8</SUB>×Ω<SUB>m</SUB>
caused by uncertainties in the theoretical models.
---------------------------------------------------------
Title: Dark Energy Survey Year 3 results: Cosmological constraints
from galaxy clustering and weak lensing
Authors: Abbott, T. M. C.; Aguena, M.; Alarcon, A.; Allam, S.;
Alves, O.; Amon, A.; Andrade-Oliveira, F.; Annis, J.; Avila, S.;
Bacon, D.; Baxter, E.; Bechtol, K.; Becker, M. R.; Bernstein, G. M.;
Bhargava, S.; Birrer, S.; Blazek, J.; Brandao-Souza, A.; Bridle,
S. L.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Camacho, H.;
Campos, A.; Carnero Rosell, A.; Carrasco Kind, M.; Carretero, J.;
Castander, F. J.; Cawthon, R.; Chang, C.; Chen, A.; Chen, R.; Choi,
A.; Conselice, C.; Cordero, J.; Costanzi, M.; Crocce, M.; da Costa,
L. N.; da Silva Pereira, M. E.; Davis, C.; Davis, T. M.; De Vicente,
J.; DeRose, J.; Desai, S.; Di Valentino, E.; Diehl, H. T.; Dietrich,
J. P.; Dodelson, S.; Doel, P.; Doux, C.; Drlica-Wagner, A.; Eckert,
K.; Eifler, T. F.; Elsner, F.; Elvin-Poole, J.; Everett, S.; Evrard,
A. E.; Fang, X.; Farahi, A.; Fernandez, E.; Ferrero, I.; Ferté, A.;
Fosalba, P.; Friedrich, O.; Frieman, J.; García-Bellido, J.; Gatti,
M.; Gaztanaga, E.; Gerdes, D. W.; Giannantonio, T.; Giannini, G.;
Gruen, D.; Gruendl, R. A.; Gschwend, J.; Gutierrez, G.; Harrison,
I.; Hartley, W. G.; Herner, K.; Hinton, S. R.; Hollowood, D. L.;
Honscheid, K.; Hoyle, B.; Huff, E. M.; Huterer, D.; Jain, B.; James,
D. J.; Jarvis, M.; Jeffrey, N.; Jeltema, T.; Kovacs, A.; Krause, E.;
Kron, R.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Leget, P. -F.; Lemos,
P.; Liddle, A. R.; Lidman, C.; Lima, M.; Lin, H.; MacCrann, N.; Maia,
M. A. G.; Marshall, J. L.; Martini, P.; McCullough, J.; Melchior, P.;
Mena-Fernández, J.; Menanteau, F.; Miquel, R.; Mohr, J. J.; Morgan,
R.; Muir, J.; Myles, J.; Nadathur, S.; Navarro-Alsina, A.; Nichol,
R. C.; Ogando, R. L. C.; Omori, Y.; Palmese, A.; Pandey, S.; Park,
Y.; Paz-Chinchón, F.; Petravick, D.; Pieres, A.; Plazas Malagón,
A. A.; Porredon, A.; Prat, J.; Raveri, M.; Rodriguez-Monroy, M.;
Rollins, R. P.; Romer, A. K.; Roodman, A.; Rosenfeld, R.; Ross, A. J.;
Rykoff, E. S.; Samuroff, S.; Sánchez, C.; Sanchez, E.; Sanchez, J.;
Sanchez Cid, D.; Scarpine, V.; Schubnell, M.; Scolnic, D.; Secco,
L. F.; Serrano, S.; Sevilla-Noarbe, I.; Sheldon, E.; Shin, T.; Smith,
M.; Soares-Santos, M.; Suchyta, E.; Swanson, M. E. C.; Tabbutt, M.;
Tarle, G.; Thomas, D.; To, C.; Troja, A.; Troxel, M. A.; Tucker,
D. L.; Tutusaus, I.; Varga, T. N.; Walker, A. R.; Weaverdyck, N.;
Wechsler, R.; Weller, J.; Yanny, B.; Yin, B.; Zhang, Y.; Zuntz, J.;
DES Collaboration
2022PhRvD.105b3520A Altcode: 2021arXiv210513549D
We present the first cosmology results from large-scale structure using
the full 5000 deg<SUP>2</SUP> of imaging data from the Dark Energy
Survey (DES) Data Release 1. We perform an analysis of large-scale
structure combining three two-point correlation functions (3 ×2 pt
): (i) cosmic shear using 100 million source galaxies, (ii) galaxy
clustering, and (iii) the cross-correlation of source galaxy shear
with lens galaxy positions, galaxy-galaxy lensing. To achieve the
cosmological precision enabled by these measurements has required
updates to nearly every part of the analysis from DES Year 1, including
the use of two independent galaxy clustering samples, modeling advances,
and several novel improvements in the calibration of gravitational
shear and photometric redshift inference. The analysis was performed
under strict conditions to mitigate confirmation or observer bias;
we describe specific changes made to the lens galaxy sample following
unblinding of the results and tests of the robustness of our results
to this decision. We model the data within the flat Λ CDM and w CDM
cosmological models, marginalizing over 25 nuisance parameters. We
find consistent cosmological results between the three two-point
correlation functions; their combination yields clustering amplitude
S<SUB>8</SUB>=0.77 6<SUB>-0.017</SUB><SUP>+0.017</SUP> and matter
density Ω<SUB>m</SUB>=0.33 9<SUB>-0.031</SUB><SUP>+0.032</SUP>
in Λ CDM , mean with 68% confidence limits; S<SUB>8</SUB>=0.77
5<SUB>-0.024</SUB><SUP>+0.026</SUP>, Ω<SUB>m</SUB>=0.35
2<SUB>-0.041</SUB><SUP>+0.035</SUP>, and dark energy equation-of-state
parameter w =-0.9 8<SUB>-0.20</SUB><SUP>+0.32</SUP> in w CDM . These
constraints correspond to an improvement in signal-to-noise of
the DES Year 3 3 ×2 pt data relative to DES Year 1 by a factor of
2.1, about 20% more than expected from the increase in observing
area alone. This combination of DES data is consistent with the
prediction of the model favored by the Planck 2018 cosmic microwave
background (CMB) primary anisotropy data, which is quantified with a
probability-to-exceed p =0.13 -0.48. We find better agreement between
DES 3 ×2 pt and Planck than in DES Y1, despite the significantly
improved precision of both. When combining DES 3 ×2 pt data with
available baryon acoustic oscillation, redshift-space distortion,
and type Ia supernovae data, we find p =0.34 . Combining all of these
datasets with Planck CMB lensing yields joint parameter constraints
of S<SUB>8</SUB>=0.81 2<SUB>-0.008</SUB><SUP>+0.008</SUP>,
Ω<SUB>m</SUB>=0.30 6<SUB>-0.005</SUB><SUP>+0.004</SUP>,
h =0.68 0<SUB>-0.003</SUB><SUP>+0.004</SUP>, and
∑m<SUB>ν</SUB><0.13 eV (95% C.L.) in Λ CDM ;
S<SUB>8</SUB>=0.81 2<SUB>-0.008</SUB><SUP>+0.008</SUP>,
Ω<SUB>m</SUB>=0.30 2<SUB>-0.006</SUB><SUP>+0.006</SUP>,
h =0.68 7<SUB>-0.007</SUB><SUP>+0.006</SUP>, and w =-1.03
1<SUB>-0.027</SUB><SUP>+0.030</SUP> in w CDM .
---------------------------------------------------------
Title: Quantitative Validation of the Linear Polarization Tomographic
Inversion for the 3D Coronal Magnetic Field.
Authors: Kramar, Maxim; Lin, Haosheng
2021AGUFMSH12C..08K Altcode:
Due to the low optical density of the solar corona, direct inference
of the plasma properties of the corona is constrained by integration
over a line-of-sight (LOS) of coronal radiation signals. In order to
dis-entangle the LOS integrated observations to unveil the underlying
3D coronal plasma structures, tomographic inversion methods should be
applied. Information about the coronal magnetic field, electron density
and temperature are encoded in coronal emission lines through the normal
and saturated Hanle effect and the Zeeman effect observed in linear (LP)
and circular (CP) polarization components, respectively, of the Fe XIII
1074.7 nm forbidden line. We will present a quantitative study of the
accuracy of the LP regularized tomographic inversion for the coronal
magnetic field in expectation of the new synoptics Fe XIII 1074.7 nm LP
data that will become available from the Upgraded Coronal Multichannel
Polarimeter (UCoMP). Although the LP signal is stronger than CP, it
only contains information about the magnetic field orientation, but
not its strength. However, the photospheric magnetic field boundary
condition provides the constraint to the magnetic fields strength. We
use the divergence free property of the magnetic field as additional
constraint in the tomographic inversion. A magnetogydrodynamic (MHD)
model for the global solar coronal by Predictive Science Inc. was used
to synthesize spectropolarimetric observations of the Fe XIII line
during a half of the solar rotation period. The inversion result based
on that synthesized LP data showed that the standard deviation of the
relative error of the reconstructed magnetic field strength lies within
about 20% for regions with the field strength greater than 0.1 Gauss.
---------------------------------------------------------
Title: The National Science Foundation's Daniel K. Inouye Solar
Telescope — Status Update
Authors: Rimmele, T.; Woeger, F.; Tritschler, A.; Casini, R.; de Wijn,
A.; Fehlmann, A.; Harrington, D.; Jaeggli, S.; Anan, T.; Beck, C.;
Cauzzi, G.; Schad, T.; Criscuoli, S.; Davey, A.; Lin, H.; Kuhn, J.;
Rast, M.; Goode, P.; Knoelker, M.; Rosner, R.; von der Luehe, O.;
Mathioudakis, M.; Dkist Team
2021AAS...23810601R Altcode:
The National Science Foundation's 4m Daniel K. Inouye Solar Telescope
(DKIST) on Haleakala, Maui is now the largest solar telescope in the
world. DKIST's superb resolution and polarimetric sensitivity will
enable astronomers to unravel many of the mysteries the Sun presents,
including the origin of solar magnetism, the mechanisms of coronal
heating and drivers of flares and coronal mass ejections. Five
instruments, four of which provide highly sensitive measurements
of solar magnetic fields, including the illusive magnetic field of
the faint solar corona. The DKIST instruments will produce large and
complex data sets, which will be distributed through the NSO/DKIST Data
Center. DKIST has achieved first engineering solar light in December
of 2019. Due to COVID the start of the operations commissioning phase
is delayed and is now expected for fall of 2021. We present a status
update for the construction effort and progress with the operations
commissioning phase.
---------------------------------------------------------
Title: DKIST First-light Instrumentation
Authors: Woeger, F.; Rimmele, T.; Casini, R.; von der Luehe, O.; Lin,
H.; Kuhn, J.; Dkist Team
2021AAS...23810602W Altcode:
The NSF's Daniel K. Inouye Solar Telescope's (DKIST) four meter aperture
and state-of-the-art wavefront correction system and instrumentation
will facilitate new insights into the complexities of the solar
atmosphere. We will describe the details and status of the diverse
first light instruments, including the high order adaptive optics
system, that are being commissioned: The Visible Spectro-Polarimeter
(ViSP), the Visible Broadband Imager (VBI), the Visible Tunable Filter
(VTF), the Diffraction-Limited Spectro-Polarimeter (DL-NIRSP) and the
Cryogenic Spectro-Polarimeter (Cryo-NIRSP). We will present first data
demonstrating the telescope's instrument systems performance.
---------------------------------------------------------
Title: The Daniel K. Inouye Solar Telescope - Observatory Overview
Authors: Rimmele, Thomas R.; Warner, Mark; Keil, Stephen L.; Goode,
Philip R.; Knölker, Michael; Kuhn, Jeffrey R.; Rosner, Robert R.;
McMullin, Joseph P.; Casini, Roberto; Lin, Haosheng; Wöger, Friedrich;
von der Lühe, Oskar; Tritschler, Alexandra; Davey, Alisdair; de Wijn,
Alfred; Elmore, David F.; Fehlmann, André; Harrington, David M.;
Jaeggli, Sarah A.; Rast, Mark P.; Schad, Thomas A.; Schmidt, Wolfgang;
Mathioudakis, Mihalis; Mickey, Donald L.; Anan, Tetsu; Beck, Christian;
Marshall, Heather K.; Jeffers, Paul F.; Oschmann, Jacobus M.; Beard,
Andrew; Berst, David C.; Cowan, Bruce A.; Craig, Simon C.; Cross,
Eric; Cummings, Bryan K.; Donnelly, Colleen; de Vanssay, Jean-Benoit;
Eigenbrot, Arthur D.; Ferayorni, Andrew; Foster, Christopher; Galapon,
Chriselle Ann; Gedrites, Christopher; Gonzales, Kerry; Goodrich, Bret
D.; Gregory, Brian S.; Guzman, Stephanie S.; Guzzo, Stephen; Hegwer,
Steve; Hubbard, Robert P.; Hubbard, John R.; Johansson, Erik M.;
Johnson, Luke C.; Liang, Chen; Liang, Mary; McQuillen, Isaac; Mayer,
Christopher; Newman, Karl; Onodera, Brialyn; Phelps, LeEllen; Puentes,
Myles M.; Richards, Christopher; Rimmele, Lukas M.; Sekulic, Predrag;
Shimko, Stephan R.; Simison, Brett E.; Smith, Brett; Starman, Erik;
Sueoka, Stacey R.; Summers, Richard T.; Szabo, Aimee; Szabo, Louis;
Wampler, Stephen B.; Williams, Timothy R.; White, Charles
2020SoPh..295..172R Altcode:
We present an overview of the National Science Foundation's Daniel
K. Inouye Solar Telescope (DKIST), its instruments, and support
facilities. The 4 m aperture DKIST provides the highest-resolution
observations of the Sun ever achieved. The large aperture of
DKIST combined with state-of-the-art instrumentation provide the
sensitivity to measure the vector magnetic field in the chromosphere
and in the faint corona, i.e. for the first time with DKIST we will
be able to measure and study the most important free-energy source
in the outer solar atmosphere - the coronal magnetic field. Over its
operational lifetime DKIST will advance our knowledge of fundamental
astronomical processes, including highly dynamic solar eruptions
that are at the source of space-weather events that impact our
technological society. Design and construction of DKIST took over two
decades. DKIST implements a fast (f/2), off-axis Gregorian optical
design. The maximum available field-of-view is 5 arcmin. A complex
thermal-control system was implemented in order to remove at prime
focus the majority of the 13 kW collected by the primary mirror and
to keep optical surfaces and structures at ambient temperature, thus
avoiding self-induced local seeing. A high-order adaptive-optics
system with 1600 actuators corrects atmospheric seeing enabling
diffraction limited imaging and spectroscopy. Five instruments, four
of which are polarimeters, provide powerful diagnostic capability
over a broad wavelength range covering the visible, near-infrared,
and mid-infrared spectrum. New polarization-calibration strategies
were developed to achieve the stringent polarization accuracy
requirement of 5×10<SUP>−4</SUP>. Instruments can be combined and
operated simultaneously in order to obtain a maximum of observational
information. Observing time on DKIST is allocated through an open,
merit-based proposal process. DKIST will be operated primarily in
"service mode" and is expected to on average produce 3 PB of raw
data per year. A newly developed data center located at the NSO
Headquarters in Boulder will initially serve fully calibrated data to
the international users community. Higher-level data products, such as
physical parameters obtained from inversions of spectro-polarimetric
data will be added as resources allow.
---------------------------------------------------------
Title: Diverse Rock Types Detected in the Lunar South Pole-Aitken
Basin by Chang'E 4
Authors: Huang, J.; Xiao, Z.; Xiao, L.; Horgan, B. H. N.; Hu, X.;
Lucey, P. G.; Xiao, X.; Zhao, S.; Qian, Y.; Zhang, H.; Li, C.; Xu,
R.; He, Z.; Yang, J.; Xue, B.; He, Q.; Zhong, J.; Lin, H.; Huang,
C.; Xie, J.
2019AGUFM.P31C3471H Altcode:
South Pole-Aitken (SPA) basin is the largest confirmed lunar impact
structure between the South Pole and Aitken crater on the far side. The
pre-Nectarian SPA basin has a 2400-km-by-2050-km elliptical structure
centered at 53º S, 191º E, which should have exposed lower crust
and upper mantle. The Earth mantle dominant mineral olivine has only
been identified in small and localized exposures in the margins
of the SPA basin, within which the dominant mafic component is
pyroxene. The mineralogical characteristics could be explained by
the recent hypothesis that the lunar upper mantle is dominated by
low-calcium pyroxene (LCP), not olivine. Here we present observations
from imaging and spectral data of China Chang'E-4 (CE-4) mission in
the first 4 synodic days, especially the first in-situ visible/near
infrared spectrometer (VNIS) observation of an exposed boulder. We have
identified a variety of rock types, but not olivine-rich materials in
the landing region, which is consistent with orbital observations. The
obtained mineralogical information provides a better understanding of
the nature and origin of SPA materials.
---------------------------------------------------------
Title: Tomographic Measurements of Magnetic Free Energy in CME
Source Regions
Authors: Lin, H.; Kramar, M.; Tomczyk, S.
2019AGUFMSH53B3378L Altcode:
Magnetic free energies (MFEs) contained in highly non-potential coronal
magnetic field in active regions are believed to be the primary source
of energy of solar eruptions. Recent progresses in observational
capabilities and tomographic inversion techniques have allowed us
to directly determine the 3D structures of the temperature, density
and magnetic fields of the solar corona (Kramar et al., 2016) using
space EUV coronal emission line (CEL) data and ground-based synoptic
IR CELs polarization observations. The magnetic free energy of the
solar corona can now be directly derived from these observationally
determined coronal models. We will present measurements of the MFEs at
the source regions of coronal mass ejections (CMEs) and comparisons of
the MFEs with direct measurements of kinetic energies of the CMEs. These
studies will help us understand the energetics of the solar eruptions.
---------------------------------------------------------
Title: ngGONG: The Next Generation GONG - A New Solar Synoptic
Observational Network
Authors: Hill, Frank; Hammel, Heidi; Martinez-Pillet, Valentin; de
Wijn, A.; Gosain, S.; Burkepile, J.; Henney, C. J.; McAteer, J.; Bain,
H. M.; Manchester, W.; Lin, H.; Roth, M.; Ichimoto, K.; Suematsu, Y.
2019BAAS...51g..74H Altcode: 2019astro2020U..74H
The white paper describes a next-generation GONG, a ground-based
geographically distributed network of instrumentation to continually
observe the Sun. This would provide data for solar magnetic field
research and space weather forecasting, and would extend the time
coverage of helioseismology.
---------------------------------------------------------
Title: Investigating Coronal Magnetism with COSMO: Science on
the Critical Path To Understanding The “Weather” of Stars and
Stellarspheres
Authors: McIntosh, Scott; Tomczyk, Steven; Gibson, Sarah E.; Burkepile,
Joan; de Wijn, Alfred; Fan, Yuhong; deToma, Giuliana; Casini, Roberto;
Landi, Enrico; Zhang, Jie; DeLuca, Edward E.; Reeves, Katharine K.;
Golub, Leon; Raymond, John; Seaton, Daniel B.; Lin, Haosheng
2019BAAS...51g.165M Altcode: 2019astro2020U.165M
The Coronal Solar Magnetism Observatory (COSMO) is a unique ground-based
facility designed to address the shortfall in our capability to measure
magnetic fields in the solar corona.
---------------------------------------------------------
Title: TSMM - A Tomographic Solar Magnetism Mission
Authors: Lin, Haosheng; Kramar, Maxim
2019AAS...23412606L Altcode:
Detailed knowledges of the magnetic and thermal environment of the
solar atmosphere, including the photosphere, chromosphere, and the
corona, and how the plasma and the magnetic fields interact with
each other, are crucial for the understanding of the physics of solar
eruptions, which directly influences space weather in interplanetary
space. However, the inference of the 3D coronal vector magnetic fields
from observations is not straightforward due to the complex nature of
the emission process (resonance scattering through Hanle and Zeeman
effects) and line-of-sight (LOS) integration through the optically
thin corona. Recent progresses in spectropolarimetric measurements
of the polarized spectra of magnetically sensitive corona emission
lines and their interpretation, and the development of tomographic
inversion techniques now provides a viable path toward quantitative
characterization of the 3-dimensional coronal temperature, density,
and magnetic field structures. <P />Tomographic inversion relies on
observations of the object under study from multiple sight lines. For
earth-bound observers, tomographic inversion of the static temperature,
density, and magnetic fields structures can be realized using pseudo
tomographic observations due to the rotation of the sun. However, to
resolve the temporal evolution of the structures of the solar atmosphere
before, during, and after solar eruptions, a space mission consisting of
multiple spacecraft deployed in deep space circumsolar orbits is needed
to observe the sun from many sight lines simultaneously. This paper
describes recent progresses in tomographic inversion techniques, and an
instrument development effort to develop compact and high-performance
instrumentation that will enable the deployment of a deep-space
tomographic solar magnetism mission in the near future.
---------------------------------------------------------
Title: Optical Alignment of DL-NIRSP Spectrograph
Authors: Jaeggli, Sarah A.; Anan, Tetsu; Kramar, Maxim; Lin, Haosheng
2019AAS...23410612J Altcode:
The Diffraction-Limited Near-Infrared Spectropolarimeter (DL-NIRSP)
will be delivered as part of the first light instrumentation for the
Daniel K. Inouye Solar Telescope (DKIST) and is currently undergoing
lab integration at the University of Hawai'i Institute for Astronomy's
Advanced Technology Research Center on Maui. An off-axis hyperbolic
mirror, with a focal length of 1250 mm, is used as both collimator
and camera in the spectrograph, and makes this system particularly
difficult to align. The optical axis, or vertex, of the parent surface
is located approximately 260 mm from the center of the off-axis
section of the mirror, but there is no direct physical or optical
reference for the location and orientation of the optical axis. We
have made use of vendor data and a coordinate measuring machine (CMM)
arm to transfer coordinates from the back and perimeter surfaces of
the mirror to locate the optical axis focus and place the other optical
components in reference to this mechanical model. In coordination, we
have conducted tests of the optical quality at various points during
the alignment to ensure that the mechanical tolerances maintain the
optical quality of the system so that the instrument will be able to
achieve excellent spectral resolution limited by the spectrograph slit
width (λ/Δλ 250,000), and preserve the diffraction limited spatial
resolution provided by the telescope and feed optics (0.06" at 1 μm).
---------------------------------------------------------
Title: Retrieving 3D coronal magnetic field from ground and space
based spectropolarimetric observations
Authors: Kramar, Maxim; Lin, Haosheng
2019AAS...23430213K Altcode:
Solar coronal magnetic fields play a key role in the energetics and
dynamics of coronal heating, solar wind, solar flares, coronal mass
ejections (CME), filament eruptions, and determine space weather
processes. Therefore, precise knowledge of the 3D magnetic field
and thermodynamic structures of the corona is essential for the
heliophysics community's effort to understand the physics of the
solar wind and solar eruptive phenomena. With the recent advancement
of scalar and vector tomographic inversion techniques (Kramar et al.,
2016), it is now possible to directly derive the 3D coronal magnetic,
temperature, and electron density structures using synoptic Fe XIII
1075 nm coronal emission line (CEL) linear polarization data of the
Coronal Multichannel Polarimeter (CoMP, Tomczyk et al., 2008), and UV
coronal images from STEREO mission. This is a major milestone in our
effort to establish the capabilities to directly observe 3D magnetic
and thermodynamic structures of the corona. <P />Although the vector
tomography based on linear polarization (LP) data can be used to probe
certain coronal field configuration (Kramar et al. 2013), linear
polarization data alone does not allow us to uniquely reconstruct
all possible field configurations in general. In the near future,
the arrival of DKIST will provide the multi-CEL full-Stokes data more
accurate determination of the static corona using the rotation of
the Sun to emulate tomographic observations. <P />On the longer term,
observational determination of spatially and temporally resolved B(r;
t), T(r; t), and n(r; t) will require the deployment of a Space Coronal
Magnetometry Mission (SCMM) with a fleet of spacecraft observing the
Sun from many non-redundant circumsolar orbits simultaneously. <P
/>We will discuss how the use of full Stokes polarization data and
multiple observing geometry from and out of the ecliptic plane will
improve the accuracy of coronal magnetic field reconstruction.
---------------------------------------------------------
Title: COSMO Science
Authors: Gibson, Sarah; Tomczyk, Steven; Burkepile, Joan; Casini,
Roberto; Deluca, Ed; de Toma, Giuliana; deWijn, Alfred; Fan, Yuhong;
Golub, Leon; Judge, Philip; Landi, Enrico; Lin, Haosheng; McIntosh,
Scott; Reeves, Kathy; Seaton, Dan; Zhang, Jie
2019shin.confE..32G 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: Measuring the Magnetic Free Energy in pre-CME Corona by the
Vector Tomographic Reconstruction of 3D Coronal Magnetic Fields
Authors: Kramar, Maxim; Lin, Haosheng
2019shin.confE.198K Altcode:
The ejecta of Coronal Mass Ejections (CMEs) carry
approximately between 10**28 to 10**32 erg of kinetic energy
(https://cdaw.gsfc.nasa.gov/CME_list/). Magnetic free energy contained
in non-potential magnetic fields in solar active regions is believed
to be the energy source powering these energetic eruptions. This
hypothesis can be tested by direct measurement of the total energy
content, including thermodynamic and magnetic free energy, contained
in the pre- and post-CME active regions. Recent advancements of the
vector tomographic reconstruction technique (Kramar et al. 2016), and
capability for synoptic observation of global coronal emission lines
(CELs) linear polarization (CoMP instrument, Tomczyk et al. 2008)
have allowed, for the first time, direct observational inference of
the quasi-static 3D magnetic field structure of the solar corona. We
describe measurements of the magnetic free energy contained in pre-CME
corona derived from tomographically reconstructed coronal magnetic
field, and compare these measurements to the kinetic energy of CMEs
obtained by independent measurements of the mass and velocity of the
CMEs. <P />Rotational tomography with a single sight line from the
Earth limits the observational cadence of the coronal magnetic fields
to approximately two weeks (in some cases it can be reduced to about a
week). Future space mission idea that can provide information on how
the coronal magnetic fields evolve with temporal cadence appropriate
for the study of energetic solar eruptions will be presented also.
---------------------------------------------------------
Title: Photometric and Spectroscopic Properties of Type Ia Supernova
2018oh with Early Excess Emission from the Kepler 2 Observations
Authors: Li, W.; Wang, X.; Vinkó, J.; Mo, J.; Hosseinzadeh, G.; Sand,
D. J.; Zhang, J.; Lin, H.; PTSS/TNTS; Zhang, T.; Wang, L.; Zhang, J.;
Chen, Z.; Xiang, D.; Rui, L.; Huang, F.; Li, X.; Zhang, X.; Li, L.;
Baron, E.; Derkacy, J. M.; Zhao, X.; Sai, H.; Zhang, K.; Wang, L.; LCO;
Howell, D. A.; McCully, C.; Arcavi, I.; Valenti, S.; Hiramatsu, D.;
Burke, J.; KEGS; Rest, A.; Garnavich, P.; Tucker, B. E.; Narayan, G.;
Shaya, E.; Margheim, S.; Zenteno, A.; Villar, A.; UCSC; Dimitriadis,
G.; Foley, R. J.; Pan, Y. -C.; Coulter, D. A.; Fox, O. D.; Jha,
S. W.; Jones, D. O.; Kasen, D. N.; Kilpatrick, C. D.; Piro, A. L.;
Riess, A. G.; Rojas-Bravo, C.; ASAS-SN; Shappee, B. J.; Holoien,
T. W. -S.; Stanek, K. Z.; Drout, M. R.; Auchettl, K.; Kochanek,
C. S.; Brown, J. S.; Bose, S.; Bersier, D.; Brimacombe, J.; Chen,
P.; Dong, S.; Holmbo, S.; Muñoz, J. A.; Mutel, R. L.; Post, R. S.;
Prieto, J. L.; Shields, J.; Tallon, D.; Thompson, T. A.; Vallely,
P. J.; Villanueva, S., Jr.; Pan-STARRS; Smartt, S. J.; Smith, K. W.;
Chambers, K. C.; Flewelling, H. A.; Huber, M. E.; Magnier, E. A.;
Waters, C. Z.; Schultz, A. S. B.; Bulger, J.; Lowe, T. B.; Willman,
M.; Konkoly/Texas; Sárneczky, K.; Pál, A.; Wheeler, J. C.; Bódi,
A.; Bognár, Zs.; Csák, B.; Cseh, B.; Csörnyei, G.; Hanyecz, O.;
Ignácz, B.; Kalup, Cs.; Könyves-Tóth, R.; Kriskovics, L.; Ordasi,
A.; Rajmon, I.; Sódor, A.; Szabó, R.; Szakáts, R.; Zsidi, G.;
Arizona, University of; Milne, P.; Andrews, J. E.; Smith, N.; Bilinski,
C.; Swift; Brown, P. J.; ePESSTO; Nordin, J.; Williams, S. C.; Galbany,
L.; Palmerio, J.; Hook, I. M.; Inserra, C.; Maguire, K.; Cartier,
Régis; Razza, A.; Gutiérrez, C. P.; North Carolina, University of;
Hermes, J. J.; Reding, J. S.; Kaiser, B. C.; ATLAS; Tonry, J. L.;
Heinze, A. N.; Denneau, L.; Weiland, H.; Stalder, B.; K2 Mission Team;
Barentsen, G.; Dotson, J.; Barclay, T.; Gully-Santiago, M.; Hedges,
C.; Cody, A. M.; Howell, S.; Kepler Spacecraft Team; Coughlin, J.;
Van Cleve, J. E.; Cardoso, J. Vinícius de Miranda; Larson, K. A.;
McCalmont-Everton, K. M.; Peterson, C. A.; Ross, S. E.; Reedy, L. H.;
Osborne, D.; McGinn, C.; Kohnert, L.; Migliorini, L.; Wheaton, A.;
Spencer, B.; Labonde, C.; Castillo, G.; Beerman, G.; Steward, K.;
Hanley, M.; Larsen, R.; Gangopadhyay, R.; Kloetzel, R.; Weschler,
T.; Nystrom, V.; Moffatt, J.; Redick, M.; Griest, K.; Packard, M.;
Muszynski, M.; Kampmeier, J.; Bjella, R.; Flynn, S.; Elsaesser, B.
2019ApJ...870...12L Altcode: 2018arXiv181110056L
Supernova (SN) 2018oh (ASASSN-18bt) is the first spectroscopically
confirmed Type Ia supernova (SN Ia) observed in the Kepler
field. The Kepler data revealed an excess emission in its early
light curve, allowing us to place interesting constraints on its
progenitor system. Here we present extensive optical, ultraviolet,
and near-infrared photometry, as well as dense sampling of optical
spectra, for this object. SN 2018oh is relatively normal in its
photometric evolution, with a rise time of 18.3 ± 0.3 days and Δm
<SUB>15</SUB>(B) = 0.96 ± 0.03 mag, but it seems to have bluer B -
V colors. We construct the “UVOIR” bolometric light curve having
a peak luminosity of 1.49 × 10<SUP>43</SUP> erg s<SUP>-1</SUP>,
from which we derive a nickel mass as 0.55 ± 0.04 M <SUB>⊙</SUB>
by fitting radiation diffusion models powered by centrally located
<SUP>56</SUP>Ni. Note that the moment when nickel-powered luminosity
starts to emerge is +3.85 days after the first light in the Kepler
data, suggesting other origins of the early-time emission, e.g.,
mixing of <SUP>56</SUP>Ni to outer layers of the ejecta or interaction
between the ejecta and nearby circumstellar material or a nondegenerate
companion star. The spectral evolution of SN 2018oh is similar to that
of a normal SN Ia but is characterized by prominent and persistent
carbon absorption features. The C II features can be detected from the
early phases to about 3 weeks after the maximum light, representing the
latest detection of carbon ever recorded in an SN Ia. This indicates
that a considerable amount of unburned carbon exists in the ejecta of
SN 2018oh and may mix into deeper layers.
---------------------------------------------------------
Title: K2 Observations of SN 2018oh Reveal a Two-component Rising
Light Curve for a Type Ia Supernova
Authors: Dimitriadis, G.; Foley, R. J.; Rest, A.; Kasen, D.; Piro,
A. L.; Polin, A.; Jones, D. O.; Villar, A.; Narayan, G.; Coulter,
D. A.; Kilpatrick, C. D.; Pan, Y. -C.; Rojas-Bravo, C.; Fox, O. D.;
Jha, S. W.; Nugent, P. E.; Riess, A. G.; Scolnic, D.; Drout, M. R.;
K2 Mission Team; Barentsen, G.; Dotson, J.; Gully-Santiago, M.; Hedges,
C.; Cody, A. M.; Barclay, T.; Howell, S.; KEGS; Garnavich, P.; Tucker,
B. E.; Shaya, E.; Mushotzky, R.; Olling, R. P.; Margheim, S.; Zenteno,
A.; Kepler spacecraft Team; Coughlin, J.; Van Cleve, J. E.; Cardoso,
J. Vinícius de Miranda; Larson, K. A.; McCalmont-Everton, K. M.;
Peterson, C. A.; Ross, S. E.; Reedy, L. H.; Osborne, D.; McGinn,
C.; Kohnert, L.; Migliorini, L.; Wheaton, A.; Spencer, B.; Labonde,
C.; Castillo, G.; Beerman, G.; Steward, K.; Hanley, M.; Larsen, R.;
Gangopadhyay, R.; Kloetzel, R.; Weschler, T.; Nystrom, V.; Moffatt,
J.; Redick, M.; Griest, K.; Packard, M.; Muszynski, M.; Kampmeier,
J.; Bjella, R.; Flynn, S.; Elsaesser, B.; Pan-STARRS; Chambers,
K. C.; Flewelling, H. A.; Huber, M. E.; Magnier, E. A.; Waters,
C. Z.; Schultz, A. S. B.; Bulger, J.; Lowe, T. B.; Willman, M.;
Smartt, S. J.; Smith, K. W.; DECam; Points, S.; Strampelli, G. M.;
ASAS-SN; Brimacombe, J.; Chen, P.; Muñoz, J. A.; Mutel, R. L.;
Shields, J.; Vallely, P. J.; Villanueva, S., Jr.; PTSS/TNTS; Li,
W.; Wang, X.; Zhang, J.; Lin, H.; Mo, J.; Zhao, X.; Sai, H.; Zhang,
X.; Zhang, K.; Zhang, T.; Wang, L.; Zhang, J.; Baron, E.; DerKacy,
J. M.; Li, L.; Chen, Z.; Xiang, D.; Rui, L.; Wang, L.; Huang, F.;
Li, X.; Cumbres Observatory, Las; Hosseinzadeh, G.; Howell, D. A.;
Arcavi, I.; Hiramatsu, D.; Burke, J.; Valenti, S.; ATLAS; Tonry,
J. L.; Denneau, L.; Heinze, A. N.; Weiland, H.; Stalder, B.; Konkoly;
Vinkó, J.; Sárneczky, K.; Pál, A.; Bódi, A.; Bognár, Zs.; Csák,
B.; Cseh, B.; Csörnyei, G.; Hanyecz, O.; Ignácz, B.; Kalup, Cs.;
Könyves-Tóth, R.; Kriskovics, L.; Ordasi, A.; Rajmon, I.; Sódor,
A.; Szabó, R.; Szakáts, R.; Zsidi, G.; ePESSTO; Williams, S. C.;
Nordin, J.; Cartier, R.; Frohmaier, C.; Galbany, L.; Gutiérrez,
C. P.; Hook, I.; Inserra, C.; Smith, M.; Arizona, University of;
Sand, D. J.; Andrews, J. E.; Smith, N.; Bilinski, C.
2019ApJ...870L...1D Altcode: 2018arXiv181110061D
We present an exquisite 30 minute cadence Kepler (K2) light curve of
the Type Ia supernova (SN Ia) 2018oh (ASASSN-18bt), starting weeks
before explosion, covering the moment of explosion and the subsequent
rise, and continuing past peak brightness. These data are supplemented
by multi-color Panoramic Survey Telescope (Pan-STARRS1) and Rapid
Response System 1 and Cerro Tololo Inter-American Observatory 4 m
Dark Energy Camera (CTIO 4-m DECam) observations obtained within hours
of explosion. The K2 light curve has an unusual two-component shape,
where the flux rises with a steep linear gradient for the first few
days, followed by a quadratic rise as seen for typical supernovae
(SNe) Ia. This “flux excess” relative to canonical SN Ia behavior
is confirmed in our i-band light curve, and furthermore, SN 2018oh is
especially blue during the early epochs. The flux excess peaks 2.14 ±
0.04 days after explosion, has a FWHM of 3.12 ± 0.04 days, a blackbody
temperature of T=17,{500}<SUB>-9,000</SUB><SUP>+11,500</SUP> K, a peak
luminosity of 4.3+/- 0.2× {10}<SUP>37</SUP> {erg} {{{s}}}<SUP>-1</SUP>,
and a total integrated energy of 1.27+/- 0.01× {10}<SUP>43</SUP>
{erg}. We compare SN 2018oh to several models that may provide
additional heating at early times, including collision with a companion
and a shallow concentration of radioactive nickel. While all of these
models generally reproduce the early K2 light curve shape, we slightly
favor a companion interaction, at a distance of ∼2× {10}<SUP>12</SUP>
{cm} based on our early color measurements, although the exact distance
depends on the uncertain viewing angle. Additional confirmation of a
companion interaction in future modeling and observations of SN 2018oh
would provide strong support for a single-degenerate progenitor system.
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Title: Status of the Daniel K. Inouye Solar Telescope: unraveling
the mysteries the Sun.
Authors: Rimmele, Thomas R.; Martinez Pillet, Valentin; Goode, Philip
R.; Knoelker, Michael; Kuhn, Jeffrey Richard; Rosner, Robert; Casini,
Roberto; Lin, Haosheng; von der Luehe, Oskar; Woeger, Friedrich;
Tritschler, Alexandra; Fehlmann, Andre; Jaeggli, Sarah A.; Schmidt,
Wolfgang; De Wijn, Alfred; Rast, Mark; Harrington, David M.; Sueoka,
Stacey R.; Beck, Christian; Schad, Thomas A.; Warner, Mark; McMullin,
Joseph P.; Berukoff, Steven J.; Mathioudakis, Mihalis; DKIST Team
2018AAS...23231601R Altcode:
The 4m Daniel K. Inouye Solar Telescope (DKIST) currently under
construction on Haleakala, Maui will be the world’s largest solar
telescope. Designed to meet the needs of critical high resolution and
high sensitivity spectral and polarimetric observations of the sun,
this facility will perform key observations of our nearest star that
matters most to humankind. DKIST’s superb resolution and sensitivity
will enable astronomers to address many of the fundamental problems
in solar and stellar astrophysics, including the origin of stellar
magnetism, the mechanisms of coronal heating and drivers of the
solar wind, flares, coronal mass ejections and variability in solar
and stellar output. DKIST will also address basic research aspects of
Space Weather and help improve predictive capabilities. In combination
with synoptic observations and theoretical modeling DKIST will unravel
the many remaining mysteries of the Sun.The construction of DKIST is
progressing on schedule with 80% of the facility complete. Operations
are scheduled to begin early 2020. DKIST will replace the NSO
facilities on Kitt Peak and Sac Peak with a national facility with
worldwide unique capabilities. The design allows DKIST to operate as
a coronagraph. Taking advantage of its large aperture and infrared
polarimeters DKIST will be capable to routinely measure the currently
illusive coronal magnetic fields. The state-of-the-art adaptive optics
system provides diffraction limited imaging and the ability to resolve
features approximately 20 km on the Sun. Achieving this resolution
is critical for the ability to observe magnetic structures at their
intrinsic, fundamental scales. Five instruments will be available at
the start of operations, four of which will provide highly sensitive
measurements of solar magnetic fields throughout the solar atmosphere
- from the photosphere to the corona. The data from these instruments
will be distributed to the world wide community via the NSO/DKIST data
center located in Boulder. We present examples of science objectives
and provide an overview of the facility and project status, including
the ongoing efforts of the community to develop the critical science
plan for the first 2-3 years of operations.
---------------------------------------------------------
Title: Infrared Imaging Spectroscopy Using Massively Multiplexed
Slit-Based Techniques and Sub-Field Motion Correction
Authors: Schad, Thomas; Lin, Haosheng
2017SoPh..292..158S Altcode: 2018arXiv180905132S
Targeting dynamic spatially extended phenomena in the upper
solar atmosphere, a new instrument concept has been developed
and demonstrated at the Dunn Solar Telescope in New Mexico, USA,
which provides wide-field, rapid-scanning, high-resolution imaging
spectroscopy of the neutral helium λ 10830 spectral triplet. The
instrument combines a narrowband imaging channel with a novel
cospatial grating-based spectrograph with 17 parallel long slits
that are simultaneously imaged on a single HgCdTe detector. Over a
175<SUP>″</SUP>×125<SUP>″</SUP> field of view, a temporal cadence
of 8.5 s is achieved between successive maps that critically sample the
diffraction limit of the Dunn Solar Telescope at 1083 nm (1.22 λ /D
=0.36<SUP>″</SUP>) and provide a resolving power (R =λ /δ λ ) up
to ≈25 ,000 with a 1 nm bandwidth (i.e.275 kms−<SUP>1</SUP> Doppler
coverage). Capitalizing on the strict simultaneity of the narrowband
channel relative to each spectral image (acquired at a rate of 9.53
Hz), this work demonstrates that sub-field image motion introduced by
atmospheric seeing may be corrected post-facto in each mapped spectral
data cube. This instrument furnishes essential infrared spectral imaging
capabilities for current investigations while pioneering techniques
for high-resolution wide-field time-domain solar astronomy.
---------------------------------------------------------
Title: A gravitational-wave standard siren measurement of the
Hubble constant
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.; 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.;
Bustillo, J. Calderón; 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.; Diaz,
J. Casanueva; 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.; 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.; Datrier, L. E. H.;
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.; Eggenstein, H. -B.; 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.; Castro, J. M. Gonzalez; 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.; 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.; 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.; Liu, X.; 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.;
Hernandez, I. Magaña; Magaña-Sandoval, F.; Zertuche, L. Magaña;
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.; 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.; Meacher, D.; Meadors, G. D.; Mehmet, M.;
Meidam, J.; Mejuto-Villa, E.; Melatos, A.; Mendell, G.; Mercer, R. A.;
Merilh, E. L.; Merzougui, M.; Meshkov, S.; Messenger, C.; Messick, C.;
Metzdorff, R.; Meyers, P. M.; Miao, H.; Michel, C.; Middleton, H.;
Mikhailov, E. E.; Milano, L.; Miller, A. L.; Miller, B. B.; Miller,
J.; Millhouse, M.; Milovich-Goff, M. C.; Minazzoli, O.; Minenkov, Y.;
Ming, J.; Mishra, C.; Mitra, S.; Mitrofanov, V. P.; Mitselmakher,
G.; Mittleman, R.; Moffa, D.; Moggi, A.; Mogushi, K.; Mohan, M.;
Mohapatra, S. R. P.; Montani, M.; Moore, C. J.; Moraru, D.; Moreno,
G.; Morriss, S. R.; Mours, B.; Mow-Lowry, C. M.; Mueller, G.; Muir,
A. W.; Mukherjee, Arunava; Mukherjee, D.; Mukherjee, S.; Mukund, N.;
Mullavey, A.; Munch, J.; Muñiz, E. A.; Muratore, M.; Murray, P. G.;
Napier, K.; Nardecchia, I.; Naticchioni, L.; Nayak, R. K.; Neilson,
J.; Nelemans, G.; Nelson, T. J. N.; Nery, M.; Neunzert, A.; Nevin,
L.; Newport, J. M.; Newton, G.; Ng, K. K. Y.; Nguyen, T. T.; Nichols,
D.; Nielsen, A. B.; Nissanke, S.; Nitz, A.; Noack, A.; Nocera, F.;
Nolting, D.; North, C.; Nuttall, L. K.; Oberling, J.; O'Dea, G. D.;
Ogin, G. H.; Oh, J. J.; Oh, S. H.; Ohme, F.; Okada, M. A.; Oliver, M.;
Oppermann, P.; Oram, Richard J.; O'Reilly, B.; Ormiston, R.; Ortega,
L. F.; O'Shaughnessy, R.; Ossokine, S.; Ottaway, D. J.; Overmier, H.;
Owen, B. J.; Pace, A. E.; Page, J.; Page, M. A.; Pai, A.; Pai, S. A.;
Palamos, J. R.; Palashov, O.; Palomba, C.; Pal-Singh, A.; Pan, Howard;
Pan, Huang-Wei; Pang, B.; Pang, P. T. H.; Pankow, C.; Pannarale, F.;
Pant, B. C.; Paoletti, F.; Paoli, A.; Papa, M. A.; Parida, A.; Parker,
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E. J.; Sanchez, L. E.; Sanchis-Gual, N.; Sandberg, V.; Sanders,
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J.; Schmidt, J.; Schmidt, P.; Schnabel, R.; Schofield, R. M. S.;
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D. A.; Shaffer, T. J.; Shah, A. A.; Shahriar, M. S.; Shaner, M. B.;
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D.; Silva, A. D.; Singer, L. P.; Singh, A.; Singhal, A.; Sintes,
A. M.; Slagmolen, B. J. J.; Smith, B.; Smith, J. R.; Smith, R. J. E.;
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R. D.; Williamson, A. R.; Willis, J. L.; Willke, B.; Wimmer, M. H.;
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J.; Wong, K. W. K.; Worden, J.; Wright, J. L.; Wu, D. S.; Wysocki,
D. M.; Xiao, S.; Yamamoto, H.; Yancey, C. C.; Yang, L.; Yap, M. J.;
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M.; Zelenova, T.; Zendri, J. -P.; Zevin, M.; Zhang, L.; Zhang, M.;
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B. F.; Murguia-Berthier, A.; Pan, Y. -C.; Piro, A. L.; Prochaska,
J. X.; Ramirez-Ruiz, E.; Rest, A.; Rojas-Bravo, C.; Shappee, B. J.;
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2017Natur.551...85A Altcode: 2017arXiv171005835A
On 17 August 2017, the Advanced LIGO and Virgo detectors observed the
gravitational-wave event GW170817—a strong signal from the merger
of a binary neutron-star system. Less than two seconds after the
merger, a γ-ray burst (GRB 170817A) was detected within a region
of the sky consistent with the LIGO-Virgo-derived location of the
gravitational-wave source. This sky region was subsequently observed
by optical astronomy facilities, resulting in the identification of
an optical transient signal within about ten arcseconds of the galaxy
NGC 4993. This detection of GW170817 in both gravitational waves and
electromagnetic waves represents the first ‘multi-messenger’
astronomical observation. Such observations enable GW170817 to be
used as a ‘standard siren’ (meaning that the absolute distance
to the source can be determined directly from the gravitational-wave
measurements) to measure the Hubble constant. This quantity represents
the local expansion rate of the Universe, sets the overall scale of
the Universe and is of fundamental importance to cosmology. Here
we report a measurement of the Hubble constant that combines the
distance to the source inferred purely from the gravitational-wave
signal with the recession velocity inferred from measurements of
the redshift using the electromagnetic data. In contrast to previous
measurements, ours does not require the use of a cosmic ‘distance
ladder’: the gravitational-wave analysis can be used to estimate
the luminosity distance out to cosmological scales directly, without
the use of intermediate astronomical distance measurements. We
determine the Hubble constant to be about 70 kilometres per second
per megaparsec. This value is consistent with existing measurements,
while being completely independent of them. Additional standard siren
measurements from future gravitational-wave sources will enable the
Hubble constant to be constrained to high precision.
---------------------------------------------------------
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.;
Meacher, D.; Meadors, G. D.; Mehmet, M.; Meidam, J.; Mejuto-Villa, E.;
Melatos, A.; Mendell, G.; Mercer, R. A.; Merilh, E. L.; Merzougui, M.;
Meshkov, S.; Messenger, C.; Messick, C.; Metzdorff, R.; Meyers, P. M.;
Miao, H.; Michel, C.; Middleton, H.; Mikhailov, E. E.; Milano, L.;
Miller, A. L.; Miller, B. B.; Miller, J.; Millhouse, M.; Milovich-Goff,
M. C.; Minazzoli, O.; Minenkov, Y.; Ming, J.; Mishra, C.; Mitra, S.;
Mitrofanov, V. P.; Mitselmakher, G.; Mittleman, R.; Moffa, D.; Moggi,
A.; Mogushi, K.; Mohan, M.; Mohapatra, S. R. P.; Montani, M.; Moore,
C. J.; Moraru, D.; Moreno, G.; Morriss, S. R.; Mours, B.; Mow-Lowry,
C. M.; Mueller, G.; Muir, A. W.; Mukherjee, Arunava; Mukherjee, D.;
Mukherjee, S.; Mukund, N.; Mullavey, A.; Munch, J.; Muñiz, E. A.;
Muratore, M.; Murray, P. G.; Napier, K.; Nardecchia, I.; Naticchioni,
L.; Nayak, R. K.; Neilson, J.; Nelemans, G.; Nelson, T. J. N.; Nery,
M.; Neunzert, A.; Nevin, L.; Newport, J. M.; Newton, G.; Ng, K. K. Y.;
Nguyen, P.; Nguyen, T. T.; Nichols, D.; Nielsen, A. B.; Nissanke,
S.; Nitz, A.; Noack, A.; Nocera, F.; Nolting, D.; North, C.; Nuttall,
L. K.; Oberling, J.; O'Dea, G. D.; Ogin, G. H.; Oh, J. J.; Oh, S. H.;
Ohme, F.; Okada, M. A.; Oliver, M.; Oppermann, P.; Oram, Richard J.;
O'Reilly, B.; Ormiston, R.; Ortega, L. F.; O'Shaughnessy, R.; Ossokine,
S.; Ottaway, D. J.; Overmier, H.; Owen, B. J.; Pace, A. E.; Page,
J.; Page, M. A.; Pai, A.; Pai, S. A.; Palamos, J. R.; Palashov, O.;
Palomba, C.; Pal-Singh, A.; Pan, Howard; Pan, Huang-Wei; Pang, B.;
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Pasqualetti, A.; Passaquieti, R.; Passuello, D.; Patil, M.; Patricelli,
B.; Pearlstone, B. L.; Pedraza, M.; Pedurand, R.; Pekowsky, L.; Pele,
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Poe, M.; Poggiani, R.; Popolizio, P.; Porter, E. K.; Post, A.; Powell,
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M.; Qi, H.; Quetschke, V.; Quintero, E. A.; Quitzow-James, R.; Raab,
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J.; Steinlechner, S.; Steinmeyer, D.; Stevenson, S. P.; Stone, R.;
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Mase, K.; Maunu, R.; McNally, F.; Meagher, K.; Medici, M.; Meier,
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Momenté, G.; Montaruli, T.; Moore, R. W.; Moulai, M.; Nahnhauer,
R.; Nakarmi, P.; Naumann, U.; Neer, G.; Niederhausen, H.; Nowicki,
S. C.; Nygren, D. R.; Obertacke Pollmann, A.; Olivas, A.; O'Murchadha,
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Przybylski, G. T.; Raab, C.; Rädel, L.; Rameez, M.; Rawlins, K.; Rea,
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Usner, M.; Vandenbroucke, J.; Van Driessche, W.; van Eijndhoven, N.;
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Walck, C.; Wallace, A.; Wallraff, M.; Wandler, F. D.; Wandkowsky,
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Mate, S.; Bhalerao, V.; Bhattacharya, D.; Vibhute, A.; Dewangan,
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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Ph. P.; Tsvetkova, A. E.; Ulanov, M. V.; Cline, T.; IPN Collaboration;
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X. L.; Chang, Z.; Chen, G.; Chen, L.; Chen, T. X.; Chen, Y.; Chen,
Y. B.; Chen, Y. P.; Cui, W.; Cui, W. W.; Deng, J. K.; Dong, Y. W.; Du,
Y. Y.; Fu, M. X.; Gao, G. H.; Gao, H.; Gao, M.; Ge, M. Y.; Gu, Y. D.;
Guan, J.; Guo, C. C.; Han, D. W.; Hu, W.; Huang, Y.; Huo, J.; Jia,
S. M.; Jiang, L. H.; Jiang, W. C.; Jin, J.; Jin, Y. J.; Li, B.; Li,
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.;
Ou, G.; Qu, J. L.; Sai, N.; Sun, L.; Tan, Y.; Tao, L.; Tao, W. H.;
Tuo, Y. L.; Wang, G. F.; Wang, H. Y.; Wang, J.; Wang, W. S.; Wang,
Y. S.; Wen, X. Y.; Wu, B. B.; Wu, M.; Xiao, G. C.; Xu, H.; Xu, Y. P.;
Yan, L. L.; Yang, J. W.; Yang, S.; Yang, Y. J.; Zhang, A. M.; Zhang,
C. L.; Zhang, C. M.; Zhang, F.; Zhang, H. M.; Zhang, J.; Zhang, Q.;
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.;
Zhao, H. S.; Zhao, J. L.; Zhao, X. F.; Zheng, S. J.; Zhu, Y.; Zhu,
Y. X.; Zou, C. L.; Insight-HXMT Collaboration; Albert, A.; André,
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T.; Baret, B.; Barrios-Martí, J.; Basa, S.; Belhorma, B.; Bertin, V.;
Biagi, S.; Bormuth, R.; Bourret, S.; Bouwhuis, M. C.; Brânzaş, H.;
Bruijn, R.; Brunner, J.; Busto, J.; Capone, A.; Caramete, L.; Carr,
J.; Celli, S.; Cherkaoui El Moursli, R.; Chiarusi, T.; Circella,
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Coyle, P.; Creusot, A.; Díaz, A. F.; Deschamps, A.; De Bonis,
G.; Distefano, C.; Di Palma, I.; Domi, A.; Donzaud, C.; Dornic,
D.; Drouhin, D.; Eberl, T.; El Bojaddaini, I.; El Khayati, N.;
Elsässer, D.; Enzenhöfer, A.; Ettahiri, A.; Fassi, F.; Felis, I.;
Fusco, L. A.; Gay, P.; Giordano, V.; Glotin, H.; Grégoire, T.; Ruiz,
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Hello, Y.; Hernández-Rey, J. J.; Hössl, J.; Hofestädt, J.; Hugon,
C.; Illuminati, G.; James, C. W.; de Jong, M.; Jongen, M.; Kadler,
M.; Kalekin, O.; Katz, U.; Kiessling, D.; Kouchner, A.; Kreter, M.;
Kreykenbohm, I.; Kulikovskiy, V.; Lachaud, C.; Lahmann, R.; Lefèvre,
D.; Leonora, E.; Lotze, M.; Loucatos, S.; Marcelin, M.; Margiotta, A.;
Marinelli, A.; Martínez-Mora, J. A.; Mele, R.; Melis, K.; Michael,
T.; Migliozzi, P.; Moussa, A.; Navas, S.; Nezri, E.; Organokov, M.;
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V.; Pradier, T.; Quinn, L.; Racca, C.; Riccobene, G.; Sánchez-Losa,
A.; Saldaña, M.; Salvadori, I.; Samtleben, D. F. E.; Sanguineti,
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M.; Tayalati, Y.; Trovato, A.; Turpin, D.; Tönnis, C.; Vallage, B.;
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,
F. E.; Melandri, A.; Nousek, J. A.; Oates, S. R.; Osborne, J. P.;
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Sbarufatti, B.; Tagliaferri, G.; Tohuvavohu, A.; Swift Collaboration;
Tavani, M.; Verrecchia, F.; Bulgarelli, A.; Evangelista, Y.; Pacciani,
L.; Feroci, M.; Pittori, C.; Giuliani, A.; Del Monte, E.; Donnarumma,
I.; Argan, A.; Trois, A.; Ursi, A.; Cardillo, M.; Piano, G.; Longo,
F.; Lucarelli, F.; Munar-Adrover, P.; Fuschino, F.; Labanti, C.;
Marisaldi, M.; Minervini, G.; Fioretti, V.; Parmiggiani, N.; Gianotti,
F.; Trifoglio, M.; Di Persio, G.; Antonelli, L. A.; Barbiellini, G.;
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F.; Ferrari, A.; Morselli, A.; Paoletti, F.; Picozza, P.; Pilia,
M.; Rappoldi, A.; Soffitta, P.; Vercellone, S.; AGILE Team; Foley,
R. J.; Coulter, D. A.; Kilpatrick, C. D.; Drout, M. R.; Piro, A. L.;
Shappee, B. J.; Siebert, M. R.; Simon, J. D.; Ulloa, N.; Kasen, D.;
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Ramirez-Ruiz, E.; Rest, A.; Rojas-Bravo, C.; 1M2H Team; Berger, E.;
Soares-Santos, M.; Annis, J.; Alexander, K. D.; Allam, S.; Balbinot,
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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, <author; Chen, T. -W.; Krühler, T.; Schady,
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Nicuesa Guelbenzu, A.; GROND; Palliyaguru, N. T.; Tech University,
Texas; Shara, M. M.; Williams, T.; Vaisanen, P.; Potter, S. B.; Romero
Colmenero, E.; Crawford, S.; Buckley, D. A. H.; Mao, J.; SALT Group;
Díaz, M. C.; Macri, L. M.; García Lambas, D.; Mendes de Oliveira,
C.; Nilo Castellón, J. L.; Ribeiro, T.; Sánchez, B.; Schoenell,
W.; Abramo, L. R.; Akras, S.; Alcaniz, J. S.; Artola, R.; Beroiz,
M.; Bonoli, S.; Cabral, J.; Camuccio, R.; Chavushyan, V.; Coelho,
P.; Colazo, C.; Costa-Duarte, M. V.; Cuevas Larenas, H.; Domínguez
Romero, M.; Dultzin, D.; Fernández, D.; García, J.; Girardini, C.;
Gonçalves, D. R.; Gonçalves, T. S.; Gurovich, S.; Jiménez-Teja, Y.;
Kanaan, A.; Lares, M.; Lopes de Oliveira, R.; López-Cruz, O.; Melia,
R.; Molino, A.; Padilla, N.; Peñuela, T.; Placco, V. M.; Quiñones,
C.; Ramírez Rivera, A.; Renzi, V.; Riguccini, L.; Ríos-López, E.;
Rodriguez, H.; Sampedro, L.; Schneiter, M.; Sodré, L.; Starck, M.;
Torres-Flores, S.; Tornatore, M.; Zadrożny, A.; Castillo, M.; TOROS:
Transient Robotic Observatory of South Collaboration; Castro-Tirado,
A. J.; Tello, J. C.; Hu, Y. -D.; Zhang, B. -B.; Cunniffe, R.;
Castellón, A.; Hiriart, D.; Caballero-García, M. D.; Jelínek,
M.; Kubánek, P.; Pérez del Pulgar, C.; Park, I. H.; Jeong, S.;
Castro Cerón, J. M.; Pandey, S. B.; Yock, P. C.; Querel, R.; Fan,
Y.; Wang, C.; BOOTES Collaboration; Beardsley, A.; Brown, I. S.;
Crosse, B.; Emrich, D.; Franzen, T.; Gaensler, B. M.; Horsley,
L.; Johnston-Hollitt, M.; Kenney, D.; Morales, M. F.; Pallot, D.;
Sokolowski, M.; Steele, K.; Tingay, S. J.; Trott, C. M.; Walker, M.;
Wayth, R.; Williams, A.; Wu, C.; Murchison Widefield Array, MWA:;
Yoshida, A.; Sakamoto, T.; Kawakubo, Y.; Yamaoka, K.; Takahashi,
I.; Asaoka, Y.; Ozawa, S.; Torii, S.; Shimizu, Y.; Tamura, T.;
Ishizaki, W.; Cherry, M. L.; Ricciarini, S.; Penacchioni, A. V.;
Marrocchesi, P. S.; CALET Collaboration; Pozanenko, A. S.; Volnova,
A. A.; Mazaeva, E. D.; Minaev, P. Yu.; Krugov, M. A.; Kusakin, A. V.;
Reva, I. V.; Moskvitin, A. S.; Rumyantsev, V. V.; Inasaridze, R.;
Klunko, E. V.; Tungalag, N.; Schmalz, S. E.; Burhonov, O.; IKI-GW
Follow-up Collaboration; Abdalla, H.; Abramowski, A.; Aharonian, F.;
Ait Benkhali, F.; Angüner, E. O.; Arakawa, M.; Arrieta, M.; Aubert,
P.; Backes, M.; Balzer, A.; Barnard, M.; Becherini, Y.; Becker Tjus,
J.; Berge, D.; Bernhard, S.; Bernlöhr, K.; Blackwell, R.; Böttcher,
M.; Boisson, C.; Bolmont, J.; Bonnefoy, S.; Bordas, P.; Bregeon, J.;
Brun, F.; Brun, P.; Bryan, M.; Büchele, M.; Bulik, T.; Capasso, M.;
Caroff, S.; Carosi, A.; Casanova, S.; Cerruti, M.; Chakraborty, N.;
Chaves, R. C. G.; Chen, A.; Chevalier, J.; Colafrancesco, S.; Condon,
B.; Conrad, J.; Davids, I. D.; Decock, J.; Deil, C.; Devin, J.; deWilt,
P.; Dirson, L.; Djannati-Ataï, A.; Donath, A.; O'C. Drury, L.; Dutson,
K.; Dyks, J.; Edwards, T.; Egberts, K.; Emery, G.; Ernenwein, J. -P.;
Eschbach, S.; Farnier, C.; Fegan, S.; Fernandes, M. V.; Fiasson, A.;
Fontaine, G.; Funk, S.; Füssling, M.; Gabici, S.; Gallant, Y. A.;
Garrigoux, T.; Gaté, F.; Giavitto, G.; Giebels, B.; Glawion, D.;
Glicenstein, J. F.; Gottschall, D.; Grondin, M. -H.; Hahn, J.;
Haupt, M.; Hawkes, J.; Heinzelmann, G.; Henri, G.; Hermann, G.;
Hinton, J. A.; Hofmann, W.; Hoischen, C.; Holch, T. L.; Holler, M.;
Horns, D.; Ivascenko, A.; Iwasaki, H.; Jacholkowska, A.; Jamrozy, M.;
Jankowsky, D.; Jankowsky, F.; Jingo, M.; Jouvin, L.; Jung-Richardt,
I.; Kastendieck, M. A.; Katarzyński, K.; Katsuragawa, M.; Kerszberg,
D.; Khangulyan, D.; Khélifi, B.; King, J.; Klepser, S.; Klochkov,
D.; Kluźniak, W.; Komin, Nu.; Kosack, K.; Krakau, S.; Kraus, M.;
Krüger, P. P.; Laffon, H.; Lamanna, G.; Lau, J.; Lees, J. -P.;
Lefaucheur, J.; Lemière, A.; Lemoine-Goumard, M.; Lenain, J. -P.;
Leser, E.; Lohse, T.; Lorentz, M.; Liu, R.; Lypova, I.; Malyshev,
D.; Marandon, V.; Marcowith, A.; Mariaud, C.; Marx, R.; Maurin, G.;
Maxted, N.; Mayer, M.; Meintjes, P. J.; Meyer, M.; Mitchell, A. M. W.;
Moderski, R.; Mohamed, M.; Mohrmann, L.; Morå, K.; Moulin, E.; Murach,
T.; Nakashima, S.; de Naurois, M.; Ndiyavala, H.; Niederwanger, F.;
Niemiec, J.; Oakes, L.; O'Brien, P.; Odaka, H.; Ohm, S.; Ostrowski,
M.; Oya, I.; Padovani, M.; Panter, M.; Parsons, R. D.; Pekeur,
N. W.; Pelletier, G.; Perennes, C.; Petrucci, P. -O.; Peyaud, B.;
Piel, Q.; Pita, S.; Poireau, V.; Poon, H.; Prokhorov, D.; Prokoph,
H.; Pühlhofer, G.; Punch, M.; Quirrenbach, A.; Raab, S.; Rauth,
R.; Reimer, A.; Reimer, O.; Renaud, M.; de los Reyes, R.; Rieger,
F.; Rinchiuso, L.; Romoli, C.; Rowell, G.; Rudak, B.; Rulten, C. B.;
Sahakian, V.; Saito, S.; Sanchez, D. A.; Santangelo, A.; Sasaki, M.;
Schlickeiser, R.; Schüssler, F.; Schulz, A.; Schwanke, U.; Schwemmer,
S.; Seglar-Arroyo, M.; Settimo, M.; Seyffert, A. S.; Shafi, N.; Shilon,
I.; Shiningayamwe, K.; Simoni, R.; Sol, H.; Spanier, F.; Spir-Jacob,
M.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steppa, C.; Sushch,
I.; Takahashi, T.; Tavernet, J. -P.; Tavernier, T.; Taylor, A. M.;
Terrier, R.; Tibaldo, L.; Tiziani, D.; Tluczykont, M.; Trichard,
C.; Tsirou, M.; Tsuji, N.; Tuffs, R.; Uchiyama, Y.; van der Walt,
D. J.; van Eldik, C.; van Rensburg, C.; van Soelen, B.; Vasileiadis,
G.; Veh, J.; Venter, C.; Viana, A.; Vincent, P.; Vink, J.; Voisin,
F.; Völk, H. J.; Vuillaume, T.; Wadiasingh, Z.; Wagner, S. J.;
Wagner, P.; Wagner, R. M.; White, R.; Wierzcholska, A.; Willmann,
P.; Wörnlein, A.; Wouters, D.; Yang, R.; Zaborov, D.; Zacharias, M.;
Zanin, R.; Zdziarski, A. A.; Zech, A.; Zefi, F.; Ziegler, A.; Zorn,
J.; Żywucka, N.; H. E. S. S. Collaboration; Fender, R. P.; Broderick,
J. W.; Rowlinson, A.; Wijers, R. A. M. J.; Stewart, A. J.; ter Veen,
S.; Shulevski, A.; LOFAR Collaboration; Kavic, M.; Simonetti, J. H.;
League, C.; Tsai, J.; Obenberger, K. S.; Nathaniel, K.; Taylor,
G. B.; Dowell, J. D.; Liebling, S. L.; Estes, J. A.; Lippert, M.;
Sharma, I.; Vincent, P.; Farella, B.; Wavelength Array, LWA: Long;
Abeysekara, A. U.; Albert, A.; Alfaro, R.; Alvarez, C.; Arceo, R.;
Arteaga-Velázquez, J. C.; Avila Rojas, D.; Ayala Solares, H. A.;
Barber, A. S.; Becerra Gonzalez, J.; Becerril, A.; Belmont-Moreno,
E.; BenZvi, S. Y.; Berley, D.; Bernal, A.; Braun, J.; Brisbois, C.;
Caballero-Mora, K. S.; Capistrán, T.; Carramiñana, A.; Casanova,
S.; Castillo, M.; Cotti, U.; Cotzomi, J.; Coutiño de León, S.;
De León, C.; De la Fuente, E.; Diaz Hernandez, R.; Dichiara, S.;
Dingus, B. L.; DuVernois, M. A.; Díaz-Vélez, J. C.; Ellsworth,
R. W.; Engel, K.; Enríquez-Rivera, O.; Fiorino, D. W.; Fleischhack,
H.; Fraija, N.; García-González, J. A.; Garfias, F.; Gerhardt, M.;
Gonzõlez Muñoz, A.; González, M. M.; Goodman, J. A.; Hampel-Arias,
Z.; Harding, J. P.; Hernandez, S.; Hernandez-Almada, A.; Hona, B.;
Hüntemeyer, P.; Iriarte, A.; Jardin-Blicq, A.; Joshi, V.; Kaufmann,
S.; Kieda, D.; Lara, A.; Lauer, R. J.; Lennarz, D.; León Vargas, H.;
Linnemann, J. T.; Longinotti, A. L.; Raya, G. Luis; Luna-García,
R.; López-Coto, R.; Malone, K.; Marinelli, S. S.; Martinez, O.;
Martinez-Castellanos, I.; Martínez-Castro, J.; Martínez-Huerta, H.;
Matthews, J. A.; Miranda-Romagnoli, P.; Moreno, E.; Mostafá, M.;
Nellen, L.; Newbold, M.; Nisa, M. U.; Noriega-Papaqui, R.; Pelayo,
R.; Pretz, J.; Pérez-Pérez, E. G.; Ren, Z.; Rho, C. D.; Rivière,
C.; Rosa-González, D.; Rosenberg, M.; Ruiz-Velasco, E.; Salazar,
H.; Salesa Greus, F.; Sandoval, A.; Schneider, M.; Schoorlemmer, H.;
Sinnis, G.; Smith, A. J.; Springer, R. W.; Surajbali, P.; Tibolla, O.;
Tollefson, K.; Torres, I.; Ukwatta, T. N.; Weisgarber, T.; Westerhoff,
S.; Wisher, I. G.; Wood, J.; Yapici, T.; Yodh, G. B.; Younk, P. W.;
Zhou, H.; Álvarez, J. D.; HAWC Collaboration; Aab, A.; Abreu,
P.; Aglietta, M.; Albuquerque, I. F. M.; Albury, J. M.; Allekotte,
I.; Almela, A.; Alvarez Castillo, J.; Alvarez-Muñiz, J.; Anastasi,
G. A.; Anchordoqui, L.; Andrada, B.; Andringa, S.; Aramo, C.; Arsene,
N.; Asorey, H.; Assis, P.; Avila, G.; Badescu, A. M.; Balaceanu, A.;
Barbato, F.; Barreira Luz, R. J.; Becker, K. H.; Bellido, J. A.; Berat,
C.; Bertaina, M. E.; Bertou, X.; Biermann, P. L.; Biteau, J.; Blaess,
S. G.; Blanco, A.; Blazek, J.; Bleve, C.; Boháčová, M.; Bonifazi,
C.; Borodai, N.; Botti, A. M.; Brack, J.; Brancus, I.; Bretz, T.;
Bridgeman, A.; Briechle, F. L.; Buchholz, P.; Bueno, A.; Buitink,
S.; Buscemi, M.; Caballero-Mora, K. S.; Caccianiga, L.; Cancio,
A.; Canfora, F.; Caruso, R.; Castellina, A.; Catalani, F.; Cataldi,
G.; Cazon, L.; Chavez, A. G.; Chinellato, J. A.; Chudoba, J.; Clay,
R. W.; Cobos Cerutti, A. C.; Colalillo, R.; Coleman, A.; Collica,
L.; Coluccia, M. R.; Conceição, R.; Consolati, G.; Contreras, F.;
Cooper, M. J.; Coutu, S.; Covault, C. E.; Cronin, J.; D'Amico, S.;
Daniel, B.; Dasso, S.; Daumiller, K.; Dawson, B. R.; Day, J. A.; de
Almeida, R. M.; de Jong, S. J.; De Mauro, G.; de Mello Neto, J. R. T.;
De Mitri, I.; de Oliveira, J.; de Souza, V.; Debatin, J.; Deligny,
O.; Díaz Castro, M. L.; Diogo, F.; Dobrigkeit, C.; D'Olivo, J. C.;
Dorosti, Q.; Dos Anjos, R. C.; Dova, M. T.; Dundovic, A.; Ebr, J.;
Engel, R.; Erdmann, M.; Erfani, M.; Escobar, C. O.; Espadanal, J.;
Etchegoyen, A.; Falcke, H.; Farmer, J.; Farrar, G.; Fauth, A. C.;
Fazzini, N.; Feldbusch, F.; Fenu, F.; Fick, B.; Figueira, J. M.;
Filipčič, A.; Freire, M. M.; Fujii, T.; Fuster, A.; Gaïor, R.;
García, B.; Gaté, F.; Gemmeke, H.; Gherghel-Lascu, A.; Ghia, P. L.;
Giaccari, U.; Giammarchi, M.; Giller, M.; Głas, D.; Glaser, C.; Golup,
G.; Gómez Berisso, M.; Gómez Vitale, P. F.; González, N.; Gorgi,
A.; Gottowik, M.; Grillo, A. F.; Grubb, T. D.; Guarino, F.; Guedes,
G. P.; Halliday, R.; Hampel, M. R.; Hansen, P.; Harari, D.; Harrison,
T. A.; Harvey, V. M.; Haungs, A.; Hebbeker, T.; Heck, D.; Heimann,
P.; Herve, A. E.; Hill, G. C.; Hojvat, C.; Holt, E.; Homola, P.;
Hörandel, J. R.; Horvath, P.; Hrabovský, M.; Huege, T.; Hulsman, J.;
Insolia, A.; Isar, P. G.; Jandt, I.; Johnsen, J. A.; Josebachuili,
M.; Jurysek, J.; Kääpä, A.; Kampert, K. H.; Keilhauer,
B.; Kemmerich, N.; Kemp, J.; Kieckhafer, R. M.; Klages, H. O.;
Kleifges, M.; Kleinfeller, J.; Krause, R.; Krohm, N.; Kuempel, D.;
Kukec Mezek, G.; Kunka, N.; Kuotb Awad, A.; Lago, B. L.; LaHurd,
D.; Lang, R. G.; Lauscher, M.; Legumina, R.; Leigui de Oliveira,
M. A.; Letessier-Selvon, A.; Lhenry-Yvon, I.; Link, K.; Lo Presti,
D.; Lopes, L.; López, R.; López Casado, A.; Lorek, R.; Luce, Q.;
Lucero, A.; Malacari, M.; Mallamaci, M.; Mandat, D.; Mantsch, P.;
Mariazzi, A. G.; Maris, I. C.; Marsella, G.; Martello, D.; Martinez,
H.; Martínez Bravo, O.; Masías Meza, J. J.; Mathes, H. J.; Mathys,
S.; Matthews, J.; Matthiae, G.; Mayotte, E.; Mazur, P. O.; Medina, C.;
Medina-Tanco, G.; Melo, D.; Menshikov, A.; Merenda, K. -D.; Michal,
S.; Micheletti, M. I.; Middendorf, L.; Miramonti, L.; Mitrica, B.;
Mockler, D.; Mollerach, S.; Montanet, F.; Morello, C.; Morlino,
G.; Müller, A. L.; Müller, G.; Muller, M. A.; Müller, S.; Mussa,
R.; Naranjo, I.; Nguyen, P. H.; Niculescu-Oglinzanu, M.; Niechciol,
M.; Niemietz, L.; Niggemann, T.; Nitz, D.; Nosek, D.; Novotny, V.;
Nožka, L.; Núñez, L. A.; Oikonomou, F.; Olinto, A.; Palatka,
M.; Pallotta, J.; Papenbreer, P.; Parente, G.; Parra, A.; Paul, T.;
Pech, M.; Pedreira, F.; Pȩkala, J.; Peña-Rodriguez, J.; Pereira,
L. A. S.; Perlin, M.; Perrone, L.; Peters, C.; Petrera, S.; Phuntsok,
J.; Pierog, T.; Pimenta, M.; Pirronello, V.; Platino, M.; Plum, M.;
Poh, J.; Porowski, C.; Prado, R. R.; Privitera, P.; Prouza, M.; Quel,
E. J.; Querchfeld, S.; Quinn, S.; Ramos-Pollan, R.; Rautenberg, J.;
Ravignani, D.; Ridky, J.; Riehn, F.; Risse, M.; Ristori, P.; Rizi, V.;
Rodrigues de Carvalho, W.; Rodriguez Fernandez, G.; Rodriguez Rojo,
J.; Roncoroni, M. J.; Roth, M.; Roulet, E.; Rovero, A. C.; Ruehl,
P.; Saffi, S. J.; Saftoiu, A.; Salamida, F.; Salazar, H.; Saleh, A.;
Salina, G.; Sánchez, F.; Sanchez-Lucas, P.; Santos, E. M.; Santos,
E.; Sarazin, F.; Sarmento, R.; Sarmiento-Cano, C.; Sato, R.; Schauer,
M.; Scherini, V.; Schieler, H.; Schimp, M.; Schmidt, D.; Scholten,
O.; Schovánek, P.; Schröder, F. G.; Schröder, S.; Schulz, A.;
Schumacher, J.; Sciutto, S. J.; Segreto, A.; Shadkam, A.; Shellard,
R. C.; Sigl, G.; Silli, G.; Šmída, R.; Snow, G. R.; Sommers, P.;
Sonntag, S.; Soriano, J. F.; Squartini, R.; Stanca, D.; Stanič, S.;
Stasielak, J.; Stassi, P.; Stolpovskiy, M.; Strafella, F.; Streich,
A.; Suarez, F.; Suarez-Durán, M.; Sudholz, T.; Suomijärvi, T.;
Supanitsky, A. D.; Šupík, J.; Swain, J.; Szadkowski, Z.; Taboada, A.;
Taborda, O. A.; Timmermans, C.; Todero Peixoto, C. J.; Tomankova, L.;
Tomé, B.; Torralba Elipe, G.; Travnicek, P.; Trini, M.; Tueros, M.;
Ulrich, R.; Unger, M.; Urban, M.; Valdés Galicia, J. F.; Valiño,
I.; Valore, L.; van Aar, G.; van Bodegom, P.; van den Berg, A. M.;
van Vliet, A.; Varela, E.; Vargas Cárdenas, B.; Vázquez, R. A.;
Veberič, D.; Ventura, C.; Vergara Quispe, I. D.; Verzi, V.; Vicha,
J.; Villaseñor, L.; Vorobiov, S.; Wahlberg, H.; Wainberg, O.;
Walz, D.; Watson, A. A.; Weber, M.; Weindl, A.; Wiedeński, M.;
Wiencke, L.; Wilczyński, H.; Wirtz, M.; Wittkowski, D.; Wundheiler,
B.; Yang, L.; Yushkov, A.; Zas, E.; Zavrtanik, D.; Zavrtanik, M.;
Zepeda, A.; Zimmermann, B.; Ziolkowski, M.; Zong, Z.; Zuccarello,
F.; Pierre Auger Collaboration; Kim, S.; Schulze, S.; Bauer, F. E.;
Corral-Santana, J. M.; de Gregorio-Monsalvo, I.; González-López,
J.; Hartmann, D. H.; Ishwara-Chandra, C. H.; Martín, S.; Mehner,
A.; Misra, K.; Michałowski, M. J.; Resmi, L.; ALMA Collaboration;
Paragi, Z.; Agudo, I.; An, T.; Beswick, R.; Casadio, C.; Frey, S.;
Jonker, P.; Kettenis, M.; Marcote, B.; Moldon, J.; Szomoru, A.;
van Langevelde, H. J.; Yang, J.; Euro VLBI Team; Cwiek, A.; Cwiok,
M.; Czyrkowski, H.; Dabrowski, R.; Kasprowicz, G.; Mankiewicz, L.;
Nawrocki, K.; Opiela, R.; Piotrowski, L. W.; Wrochna, G.; Zaremba,
M.; Żarnecki, A. F.; Pi of Sky Collaboration; Haggard, D.; Nynka,
M.; Ruan, J. J.; Chandra Team at McGill University; Bland, P. A.;
Booler, T.; Devillepoix, H. A. R.; de Gois, J. S.; Hancock, P. J.;
Howie, R. M.; Paxman, J.; Sansom, E. K.; Towner, M. C.; Desert
Fireball Network, DFN:; Tonry, J.; Coughlin, M.; Stubbs, C. W.;
Denneau, L.; Heinze, A.; Stalder, B.; Weiland, H.; ATLAS; Eatough,
R. P.; Kramer, M.; Kraus, A.; Time Resolution Universe Survey, High;
Troja, E.; Piro, L.; Becerra González, J.; Butler, N. R.; Fox, O. D.;
Khandrika, H. G.; Kutyrev, A.; Lee, W. H.; Ricci, R.; Ryan, R. E.,
Jr.; Sánchez-Ramírez, R.; Veilleux, S.; Watson, A. M.; Wieringa,
M. H.; Burgess, J. M.; van Eerten, H.; Fontes, C. J.; Fryer, C. L.;
Korobkin, O.; Wollaeger, R. T.; RIMAS; RATIR; Camilo, F.; Foley,
A. R.; Goedhart, S.; Makhathini, S.; Oozeer, N.; Smirnov, O. M.;
Fender, R. P.; Woudt, P. A.; South Africa/MeerKAT, SKA
2017ApJ...848L..12A Altcode: 2017arXiv171005833L
On 2017 August 17 a binary neutron star coalescence candidate (later
designated GW170817) with merger time 12:41:04 UTC was observed
through gravitational waves by the Advanced LIGO and Advanced Virgo
detectors. The Fermi Gamma-ray Burst Monitor independently detected a
gamma-ray burst (GRB 170817A) with a time delay of ∼ 1.7 {{s}} with
respect to the merger time. From the gravitational-wave signal, the
source was initially localized to a sky region of 31 deg<SUP>2</SUP>
at a luminosity distance of {40}<SUB>-8</SUB><SUP>+8</SUP> 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}<SUB>⊙
</SUB>. 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. <P />Any correspondence should be
addressed to .
---------------------------------------------------------
Title: Critical Infrared Science with the Daniel K. Inouye Solar
Telescope
Authors: Schad, Thomas A.; Fehlmann, Andre; Jaeggli, Sarah A.; Kuhn,
Jeffrey Richard; Lin, Haosheng; Penn, Matthew J.; Rimmele, Thomas R.;
Woeger, Friedrich
2017SPD....4811703S Altcode:
Critical science planning for early operations of the Daniel K. Inouye
Solar Telescope is underway. With its large aperture, all-reflective
telescope design, and advanced instrumentation, DKIST provides
unprecedented access to the important infrared (IR) solar spectrum
between 1 and 5 microns. Breakthrough IR capabilities in coronal
polarimetry will sense the coronal magnetic field routinely for the
first time. The increased Zeeman resolution near the photospheric
opacity minimum will provide our deepest and most sensitive measurement
of quiet sun and active region magnetic fields to date. High-sensitivity
He I triplet polarimetry will dynamically probe the chromospheric
magnetic field in fibrils, spicules, and filaments, while observations
of molecular CO transitions will characterize the coolest regions
of the solar atmosphere. When combined with the longer timescales
of good atmospheric seeing compared with the visible, DKIST infrared
diagnostics are expected to be mainstays of solar physics in the DKIST
era. This paper will summarize the critical science areas addressed
by DKIST infrared instrumentation and invite the community to further
contribute to critical infrared science planning.
---------------------------------------------------------
Title: An Update on the Diffraction-Limited Near Infrared
Spectropolarimeter for the Daniel K. Inouye Solar Telescope
Authors: Jaeggli, Sarah A.; Lin, Haosheng; Onaka, Peter; McGregor,
Helen; Yamada, Hubert
2017SPD....4811704J Altcode:
DL-NIRSP is an integral field imaging spectropolarimeter for
photospheric, chromospheric, and coronal magnetic field studies
which is currently under development by the University of Hawaii’s
Institute for Astronomy as part of the first light instrument suite for
DKIST. DL-NIRSP pairs a multi-slit fiber-optic image slicer with narrow
bandpass isolation filters and large format detectors to achieve very
high cadence observations in three simultaneous wavelength channels
in the Visible-IR. Planned diagnostics at first light include Fe XI
789.2 nm, Ca II 854.2 nm, Fe XIII 1074.7 nm, Si I/He I 1083.0 nm, Si
X 1430.0 nm, and Fe I 1565.0 nm. More spectral lines will be added in
the future. As the last stop in the DKIST light distribution system,
DL-NIRSP will receive an AO corrected beam and will be able to operate
simultaneously with the other visible light instruments. We provide an
update on the current challenges and rewards yet to come with DL-NIRSP.
---------------------------------------------------------
Title: Vector Magnetic Field Measurements along a Cooled Stereo-imaged
Coronal Loop
Authors: Schad, T. A.; Penn, M. J.; Lin, H.; Judge, P. G.
2016ApJ...833....5S Altcode: 2016arXiv161005332S
The variation of the vector magnetic field along structures in
the solar corona remains unmeasured. Using a unique combination of
spectropolarimetry and stereoscopy, we infer and compare the vector
magnetic field structure and three-dimensional morphology of an
individuated coronal loop structure undergoing a thermal instability. We
analyze spectropolarimetric data of the He I λ10830 triplet
(1s2s{}<SUP>3</SUP>{S}<SUB>1</SUB>-1s2p{}<SUP>3</SUP>{P}<SUB>{2,1,0</SUB>})
obtained at the Dunn Solar Telescope with the Facility Infrared
Spectropolarimeter on 2011 September 19. Cool coronal loops are
identified by their prominent drainage signatures in the He I data
(redshifts up to 185 km s<SUP>-1</SUP>). Extinction of EUV background
radiation along these loops is observed by both the Atmospheric Imaging
Assembly on board the Solar Dynamics Observatory and the Extreme
Ultraviolet Imager on board spacecraft A of the Solar Terrestrial
Relations Observatory, and is used to stereoscopically triangulate
the loop geometry up to heights of 70 Mm (0.1R <SUB>Sun</SUB>) above
the solar surface. The He I polarized spectra along this loop exhibit
signatures indicative of atomic-level polarization, as well as magnetic
signatures through the Hanle and Zeeman effects. Spectropolarimetric
inversions indicate that the magnetic field is generally oriented
along the coronal loop axis, and provide the height dependence of the
magnetic field intensity. The technique we demonstrate is a powerful
one that may help better understand the thermodynamics of coronal
fine-structure magnetism.
---------------------------------------------------------
Title: Daniel K. Inouye Solar Telescope: High-resolution observing
of the dynamic Sun
Authors: Tritschler, A.; Rimmele, T. R.; Berukoff, S.; Casini, R.;
Kuhn, J. R.; Lin, H.; Rast, M. P.; McMullin, J. P.; Schmidt, W.;
Wöger, F.; DKIST Team
2016AN....337.1064T Altcode:
The 4-m aperture Daniel K. Inouye Solar Telescope (DKIST) formerly
known as the Advanced Technology Solar Telescope (ATST) is currently
under construction on Haleakalā (Maui, Hawai'i) projected to
start operations in 2019. At the time of completion, DKIST will be
the largest ground-based solar telescope providing unprecedented
resolution and photon collecting power. The DKIST will be equipped
with a set of first-light facility-class instruments offering unique
imaging, spectroscopic and spectropolarimetric observing opportunities
covering the visible to infrared wavelength range. This first-light
instrumentation suite will include: a Visible Broadband Imager (VBI) for
high-spatial and -temporal resolution imaging of the solar atmosphere; a
Visible Spectro-Polarimeter (ViSP) for sensitive and accurate multi-line
spectropolarimetry; a Fabry-Pérot based Visible Tunable Filter
(VTF) for high-spatial resolution spectropolarimetry; a fiber-fed
Diffraction-Limited Near Infra-Red Spectro-Polarimeter (DL-NIRSP)
for two-dimensional high-spatial resolution spectropolarimetry
(simultaneous spatial and spectral information); and a Cryogenic Near
Infra-Red Spectro-Polarimeter (Cryo-NIRSP) for coronal magnetic field
measurements and on-disk observations of, e.g., the CO lines at 4.7
μm. We will provide an overview of the DKIST's unique capabilities
with strong focus on the first-light instrumentation suite, highlight
some of the additional properties supporting observations of transient
and dynamic solar phenomena, and touch on some operational strategies
and the DKIST critical science plan.
---------------------------------------------------------
Title: Construction status of the Daniel K. Inouye solar telescope
Authors: McMullin, Joseph P.; Rimmele, Thomas R.; Warner, Mark;
Martinez Pillet, Valentin; Casini, Roberto; Berukoff, Steve; Craig,
Simon C.; Elmore, David; Ferayorni, Andrew; Goodrich, Bret D.;
Hubbard, Robert P.; Harrington, David; Hegwer, Steve; Jeffers, Paul;
Johansson, Erik M.; Kuhn, Jeff; Lin, Haosheng; Marshall, Heather;
Mathioudakis, Mihalis; McBride, William R.; McVeigh, William; Phelps,
LeEllen; Schmidt, Wolfgang; Shimko, Steve; Sueoka, Stacey; Tritschler,
Alexandra; Williams, Timothy R.; Wöger, Friedrich
2016SPIE.9906E..1BM Altcode:
We provide an update on the construction status of the Daniel
K. Inouye Solar Telescope. This 4-m diameter facility is designed to
enable detection and spatial/temporal resolution of the predicted,
fundamental astrophysical processes driving solar magnetism at
their intrinsic scales throughout the solar atmosphere. These data
will drive key research on solar magnetism and its influence on
solar winds, flares, coronal mass ejections and solar irradiance
variability. The facility is developed to support a broad wavelength
range (0.35 to 28 microns) and will employ state-of-the-art adaptive
optics systems to provide diffraction limited imaging, resolving
features approximately 20 km on the Sun. At the start of operations,
there will be five instruments initially deployed: Visible Broadband
Imager (VBI; National Solar Observatory), Visible SpectroPolarimeter
(ViSP; NCAR High Altitude Observatory), Visible Tunable Filter (VTF
(a Fabry-Perot tunable spectropolarimeter); Kiepenheuer Institute for
Solarphysics), Diffraction Limited NIR Spectropolarimeter (DL-NIRSP;
University of Hawaii, Institute for Astronomy) and the Cryogenic NIR
Spectropolarimeter (Cryo-NIRSP; University of Hawaii, Institute for
Astronomy). As of mid-2016, the project construction is in its 4th
year of site construction and 7th year overall. Major milestones in
the off-site development include the conclusion of the polishing of
the M1 mirror by University of Arizona, College of Optical Sciences,
the delivery of the Top End Optical Assembly (L3), the acceptance of
the Deformable Mirror System (Xinetics); all optical systems have been
contracted and are either accepted or in fabrication. The Enclosure
and Telescope Mount Assembly passed through their factory acceptance
in 2014 and 2015, respectively. The enclosure site construction
is currently concluding while the Telescope Mount Assembly site
erection is underway. The facility buildings (Utility and Support
and Operations) have been completed with ongoing work on the thermal
systems to support the challenging imaging requirements needed for the
solar research. Finally, we present the construction phase performance
(schedule, budget) with projections for the start of early operations.
---------------------------------------------------------
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.
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,
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V. B.; Branchesi, M.; Brau, J. E.; Briant, T.; Brillet, A.; Brinkmann,
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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,
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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.;
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T.; Evans, M.; Evans, T. M.; Everett, R.; Factourovich, M.; Fafone,
V.; Fair, H.; Fairhurst, S.; Fan, X.; Fang, Q.; Farinon, S.; Farr,
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Ferrante, I.; Ferreira, E. C.; Ferrini, F.; Fidecaro, F.; Fiori, I.;
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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,
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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.;
Meidam, J.; Melatos, A.; Mendell, G.; Mendoza-Gandara, D.; Mercer,
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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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Newton, G.; Nguyen, T. T.; Nielsen, A. B.; Nissanke, S.; Nitz, A.;
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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.;
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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,
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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.; 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
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: 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.;
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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.;
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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.;
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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.;
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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.;
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S. R. P.; Montani, M.; Moore, B. C.; Moore, C. J.; Moraru, D.;
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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,
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B.; Shawhan, P.; Sheperd, A.; Shoemaker, D. H.; Shoemaker, D. M.;
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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.;
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Thrane, E.; Tiwari, S.; Tiwari, V.; Tokmakov, K. V.; Tomlinson, C.;
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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
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: Construction Status and Early Science with the Daniel K. Inouye
Solar Telescope
Authors: McMullin, Joseph P.; Rimmele, Thomas R.; Warner, Mark;
Martinez Pillet, Valentin; Craig, Simon; Woeger, Friedrich; Tritschler,
Alexandra; Berukoff, Steven J.; Casini, Roberto; Goode, Philip R.;
Knoelker, Michael; Kuhn, Jeffrey Richard; Lin, Haosheng; Mathioudakis,
Mihalis; Reardon, Kevin P.; Rosner, Robert; Schmidt, Wolfgang
2016SPD....4720101M Altcode:
The 4-m Daniel K. Inouye Solar Telescope (DKIST) is in its seventh
year of overall development and its fourth year of site construction
on the summit of Haleakala, Maui. The Site Facilities (Utility
Building and Support & Operations Building) are in place with
ongoing construction of the Telescope Mount Assembly within. Off-site
the fabrication of the component systems is completing with early
integration testing and verification starting.Once complete this
facility will provide the highest sensitivity and resolution for study
of solar magnetism and the drivers of key processes impacting Earth
(solar wind, flares, coronal mass ejections, and variability in solar
output). The DKIST will be equipped initially with a battery of first
light instruments which cover a spectral range from the UV (380 nm)
to the near IR (5000 nm), and capable of providing both imaging and
spectro-polarimetric measurements throughout the solar atmosphere
(photosphere, chromosphere, and corona); these instruments are being
developed by the National Solar Observatory (Visible Broadband Imager),
High Altitude Observatory (Visible Spectro-Polarimeter), Kiepenheuer
Institute (Visible Tunable Filter) and the University of Hawaii
(Cryogenic Near-Infrared Spectro-Polarimeter and the Diffraction-Limited
Near-Infrared Spectro-Polarimeter). Further, a United Kingdom consortium
led by Queen's University Belfast is driving the development of high
speed cameras essential for capturing the highly dynamic processes
measured by these instruments. Finally, a state-of-the-art adaptive
optics system will support diffraction limited imaging capable of
resolving features approximately 20 km in scale on the Sun.We present
the overall status of the construction phase along with the current
challenges as well as a review of the planned science testing and the
transition into early science operations.
---------------------------------------------------------
Title: mxCSM: A 100-slit, 6-wavelength wide-field coronal
spectropolarimeter for the study of the dynamics and the magnetic
fields of the solar corona
Authors: Lin, Haosheng
2016FrASS...3....9L Altcode:
remendous progress has been made in the field of observational
coronal magnetometry in the first decade of the 21st century. With
the successful construction of the Coronal Multichannel Magnetometer
(CoMP) instrument, observations of the linear polarization of the
coronal emission lines (CELs), which carry information about the
azimuthal direction of the coronal magnetic fields, are now routinely
available. However, reliable and regular measurements of the circular
polarization signals of the CELs remain illusive. The CEL circular
polarization signals allow us to infer the magnetic field strength in
the corona, and is critically important of our understanding of the
solar corona. Current telescopes and instrument can only measure the
coronal magnetic field strength over a small field of view. Furthermore,
the observations require very long integration time that preclude
the study of dynamic events even when only a small field of view is
required. This paper describes a new instrument concept that employees
large-scale multiplexing technology to enhance the efficiency of current
coronal spectropolarimeter by more than two orders of magnitude. This
will allow for the instrument to increase of the integration time
at each spatial location by the same factor, while also achieving a
large field of view coverage. We will present the conceptual design
of a 100-slit coronal spectropolarimeter that can observe six coronal
emission lines simultaneously. Instruments based on this concept will
allow us to study the evolution of the coronal magnetic field even
with coronagraphs with modest aperture.
---------------------------------------------------------
Title: Direct Observation of Solar Coronal Magnetic Fields by Vector
Tomography of the Coronal Emission Line Polarizations
Authors: Kramar, M.; Lin, H.; Tomczyk, S.
2016ApJ...819L..36K Altcode: 2015arXiv150207200K
We present the first direct “observation” of the global-scale,
3D coronal magnetic fields of Carrington Rotation (CR) Cycle 2112
using vector tomographic inversion techniques. The vector tomographic
inversion uses measurements of the Fe xiii 10747 Å Hanle effect
polarization signals by the Coronal Multichannel Polarimeter (CoMP)
and 3D coronal density and temperature derived from scalar tomographic
inversion of Solar Terrestrial Relations Observatory (STEREO)/Extreme
Ultraviolet Imager (EUVI) coronal emission lines (CELs) intensity
images as inputs to derive a coronal magnetic field model that best
reproduces the observed polarization signals. While independent
verifications of the vector tomography results cannot be performed,
we compared the tomography inverted coronal magnetic fields with those
constructed by magnetohydrodynamic (MHD) simulations based on observed
photospheric magnetic fields of CR 2112 and 2113. We found that the
MHD model for CR 2112 is qualitatively consistent with the tomography
inverted result for most of the reconstruction domain except for several
regions. Particularly, for one of the most noticeable regions, we found
that the MHD simulation for CR 2113 predicted a model that more closely
resembles the vector tomography inverted magnetic fields. In another
case, our tomographic reconstruction predicted an open magnetic field at
a region where a coronal hole can be seen directly from a STEREO-B/EUVI
image. We discuss the utilities and limitations of the tomographic
inversion technique, and present ideas for future developments.
---------------------------------------------------------
Title: Constraints on the richness-mass relation and the optical-SZE
positional offset distribution for SZE-selected clusters
Authors: Saro, A.; Bocquet, S.; Rozo, E.; Benson, B. A.; Mohr,
J.; Rykoff, E. S.; Soares-Santos, M.; Bleem, L.; Dodelson, S.;
Melchior, P.; Sobreira, F.; Upadhyay, V.; Weller, J.; Abbott, T.;
Abdalla, F. B.; Allam, S.; Armstrong, R.; Banerji, M.; Bauer, A. H.;
Bayliss, M.; Benoit-Lévy, A.; Bernstein, G. M.; Bertin, E.; Brodwin,
M.; Brooks, D.; Buckley-Geer, E.; Burke, D. L.; Carlstrom, J. E.;
Capasso, R.; Capozzi, D.; Carnero Rosell, A.; Carrasco Kind, M.; Chiu,
I.; Covarrubias, R.; Crawford, T. M.; Crocce, M.; D'Andrea, C. B.;
da Costa, L. N.; DePoy, D. L.; Desai, S.; de Haan, T.; Diehl, H. T.;
Dietrich, J. P.; Doel, P.; Cunha, C. E.; Eifler, T. F.; Evrard, A. E.;
Fausti Neto, A.; Fernandez, E.; Flaugher, B.; Fosalba, P.; Frieman, J.;
Gangkofner, C.; Gaztanaga, E.; Gerdes, D.; Gruen, D.; Gruendl, R. A.;
Gupta, N.; Hennig, C.; Holzapfel, W. L.; Honscheid, K.; Jain, B.;
James, D.; Kuehn, K.; Kuropatkin, N.; Lahav, O.; Li, T. S.; Lin, H.;
Maia, M. A. G.; March, M.; Marshall, J. L.; Martini, Paul; McDonald,
M.; Miller, C. J.; Miquel, R.; Nord, B.; Ogando, R.; Plazas, A. A.;
Reichardt, C. L.; Romer, A. K.; Roodman, A.; Sako, M.; Sanchez, E.;
Schubnell, M.; Sevilla, I.; Smith, R. C.; Stalder, B.; Stark, A. A.;
Strazzullo, V.; Suchyta, E.; Swanson, M. E. C.; Tarle, G.; Thaler,
J.; Thomas, D.; Tucker, D.; Vikram, V.; von der Linden, A.; Walker,
A. R.; Wechsler, R. H.; Wester, W.; Zenteno, A.; Ziegler, K. E.
2015MNRAS.454.2305S Altcode: 2015arXiv150607814S
We cross-match galaxy cluster candidates selected via their
Sunyaev-Zel'dovich effect (SZE) signatures in 129.1 deg<SUP>2</SUP> of
the South Pole Telescope 2500d SPT-SZ survey with optically identified
clusters selected from the Dark Energy Survey science verification
data. We identify 25 clusters between 0.1 ≲ z ≲ 0.8 in the union of
the SPT-SZ and redMaPPer (RM) samples. RM is an optical cluster finding
algorithm that also returns a richness estimate for each cluster. We
model the richness λ-mass relation with the following function
<ln λ|M<SUB>500</SUB>> ∝ B<SUB>λ</SUB>ln M<SUB>500</SUB> +
C<SUB>λ</SUB>ln E(z) and use SPT-SZ cluster masses and RM richnesses
λ to constrain the parameters. We find B_λ = 1.14^{+0.21}_{-0.18}
and C_λ =0.73^{+0.77}_{-0.75}. The associated scatter in mass at fixed
richness is σ _{ln M|λ } = 0.18^{+0.08}_{-0.05} at a characteristic
richness λ = 70. We demonstrate that our model provides an adequate
description of the matched sample, showing that the fraction of
SPT-SZ-selected clusters with RM counterparts is consistent with
expectations and that the fraction of RM-selected clusters with
SPT-SZ counterparts is in mild tension with expectation. We model the
optical-SZE cluster positional offset distribution with the sum of two
Gaussians, showing that it is consistent with a dominant, centrally
peaked population and a subdominant population characterized by larger
offsets. We also cross-match the RM catalogue with SPT-SZ candidates
below the official catalogue threshold significance ξ = 4.5, using
the RM catalogue to provide optical confirmation and redshifts for 15
additional clusters with ξ ∈ [4, 4.5].
---------------------------------------------------------
Title: 3D Observation of the Global Coronal Magnetic Field by Vector
Tomography using the Coronal Emission Linear Polarization Data.
Authors: Kramar, Maxim; Lin, Haosheng; Tomczyk, Steven
2015IAUGA..2257404K Altcode:
Measurement of the coronal magnetic field is a crucial ingredient
in understanding the nature of solar coronal phenomena at all
scales. However, due to the low density and opacity of the solar
atmosphere, the coronal emission measurements are result of a
line-of-sight (LOS) integration through a nonuniform temperature,
density and magnetic field distribution. Therefore, except in a few
special cases, a direct inference of the 3D coronal magnetic field
structure from polarization data is in general not possible. Tomography
methods allow to resolve the LOS problem.We will present the
global-scale, 3D coronal vector magnetic fields obtained by a vector
tomographic inversion technique.The Vector tomographic inversion uses
measurements of the Fe XIII 10747 A Hanle effect linear polarization
signals by the Coronal Multichannel Polarimeter (CoMP) as inputs to
derive a coronal magnetic field model that best reproduces the observed
polarization signals. The 3D electron density and temperature, needed
as additional input, have been reconstructed by scalar field tomography
method based on STEREO/EUVI data. We will present the 3D coronal vector
magnetic field, electron density and temperature resulted from these
inversions.While independent verifications of the vector tomography
results cannot be performed, we compared the tomography inverted coronal
magnetic fields with those constructed by MagnetoHydroDynamic (MHD)
simulation based on observed photospheric magnetic fields and with 3D
coronal density structures obtained by scalar field tomography based
on coronal observations. We will discuss the utilities and limitations
of the inversion technique, and present ideas for future developments.
---------------------------------------------------------
Title: He I Vector Magnetic Field Maps of a Sunspot and Its
Superpenumbral Fine-Structure
Authors: Schad, T. A.; Penn, M. J.; Lin, H.; Tritschler, A.
2015SoPh..290.1607S Altcode: 2015arXiv150505567S; 2015SoPh..tmp...60S
Advanced inversions of high-resolution spectropolarimetric observations
of the He I triplet at 1083 nm are used to generate unique maps of
the chromospheric magnetic field vector across a sunspot and its
superpenumbral canopy. The observations were acquired by the Facility
Infrared Spectropolarimeter (FIRS) at the Dunn Solar Telescope (DST)
on 29 January 2012. Multiple atmospheric models are employed in the
inversions because superpenumbral Stokes profiles are dominated by
atomic-level polarization, while sunspot profiles are Zeeman-dominated,
but also exhibit signatures that might be induced by symmetry-breaking
effects of the radiation field incident on the chromospheric
material. We derive the equilibrium magnetic structure of a sunspot in
the chromosphere and furthermore show that the superpenumbral magnetic
field does not appear to be finely structured, unlike the observed
intensity structure. This suggests that fibrils are not concentrations
of magnetic flux, but are instead distinguished by individualized
thermalization. We also directly compare our inverted values with a
current-free extrapolation of the chromospheric field. With improved
measurements in the future, the average shear angle between the inferred
magnetic field and the potential field may offer a means to quantify
the non-potentiality of the chromospheric magnetic field to study the
onset of explosive solar phenomena.
---------------------------------------------------------
Title: DKIST: Observing the Sun at High Resolution
Authors: Tritschler, A.; Rimmele, T. R.; Berukoff, S.; Casini, R.;
Craig, S. C.; Elmore, D. F.; Hubbard, R. P.; Kuhn, J. R.; Lin, H.;
McMullin, J. P.; Reardon, K. P.; Schmidt, W.; Warner, M.; Woger, F.
2015csss...18..933T Altcode:
The 4-m aperture Daniel K. Inouye Solar Telescope (DKIST) formerly
known as the Advanced Technology Solar Telescope (ATST) and currently
under construction on Haleakalā (Maui, Hawai'i) will be the largest
solar ground-based telescope and leading resource for studying the
dynamic Sun and its phenomena at high spatial, spectral and temporal
resolution. Accurate and sensitive polarimetric observations at
high-spatial resolution throughout the solar atmosphere including the
corona is a high priority and a major science driver. As such the DKIST
will offer a combination of state-of-the-art instruments with imaging
and/or spectropolarimetric capabilities covering a broad wavelength
range. This first-light instrumentation suite will include: a Visible
Broadband Imager (VBI) for high-spatial and -temporal resolution
imaging of the solar atmosphere; a Visible Spectro-Polarimeter (ViSP)
for sensitive and accurate multi-line spectropolarimetry; a double
Fabry-Pérot based Visible Tunable Filter (VTF) for high-spatial
resolution spectropolarimetry; a fiber-fed 2D Diffraction-Limited Near
Infra-Red Spectro-Polarimeter (DL-NIRSP); and a Cryogenic Near Infra-Red
Spectro-Polarimeter (Cryo-NIRSP) for coronal magnetic field measurements
and on-disk observations of e.g. the CO lines at 4.7 microns. We
will provide a brief overview of the DKIST's unique capabilities to
perform spectroscopic and spectropolarimetric measurements of the solar
atmosphere using its first-light instrumentation suite, the status of
the construction project, and how facility and data access is provided
to the US and international community.
---------------------------------------------------------
Title: The Coronal Solar Magnetism Observatory (COSMO)
Authors: Tomczyk, S.; Landi, E.; Lin, H.; Zhang, J.
2014AGUFMSH53B4212T Altcode:
Measurements of coronal and chromospheric magnetic fields are arguably
the most important observables required in our understanding of the
emergence of magnetic flux into the solar atmosphere and the processes
responsible for the production of solar activity, coronal heating
and coronal dynamics. However, routine observations of the strength
and orientation of coronal and chromospheric magnetic fields are
not currently available. COSMO is a proposed ground-based suite of
instruments designed for routine study of coronal and chromospheric
magnetic fields and their environment. We will present an overview
of the COSMO and show recent progress in development of the COSMO
observatory.
---------------------------------------------------------
Title: Polarization properties of a birefringent fiber optic image
slicer for diffraction-limited dual-beam spectropolarimetry
Authors: Schad, Thomas; Lin, Haosheng; Ichimoto, Kiyoshi; Katsukawa,
Yukio
2014SPIE.9147E..6ES Altcode:
The birefringent fiber optic image slicer design, or BiFOIS,
adapts integral field spectroscopy methods to the special needs of
high-sensitivity, spatially-resolved spectropolarimetry. In solar
astronomy these methods are of particular importance, as dynamic
magnetism lies at the heart of various multi-scaled phenomena in the
solar atmosphere. While integral field units (IFU) based on fiber
optics have been in continual development for some time, standard
stock multimode fibers do not typically preserve polarization. The
importance of a birefringent fiber optic IFU design stems from the
need for dual-beam spatio-temporal polarimetric modulation to correct
for spurious polarization signals induced either by platform jitter or
atmospheric seeing. Here we characterize the polarization response of a
second generation BiFOIS IFU designed for solar spectropolarimetry. The
unit provides 60 × 64 spatial imaging pixels in a densely-packed,
high filling factor configuration. Particular attention is placed on
the spatial uniformity of the IFU polarization response. Calibrated
first-light solar observations are also presented to demonstrate the
performance of the device in a real application.
---------------------------------------------------------
Title: Construction status of the Daniel K. Inouye Solar Telescope
Authors: McMullin, Joseph P.; Rimmele, Thomas R.; Martínez Pillet,
Valentin; Berger, Thomas E.; Casini, Roberto; Craig, Simon C.; Elmore,
David F.; Goodrich, Bret D.; Hegwer, Steve L.; Hubbard, Robert P.;
Johansson, Erik M.; Kuhn, Jeffrey R.; Lin, Haosheng; McVeigh, William;
Schmidt, Wolfgang; Shimko, Steve; Tritschler, Alexandra; Warner,
Mark; Wöger, Friedrich
2014SPIE.9145E..25M Altcode:
The Daniel K. Inouye Solar Telescope (DKIST, renamed in December 2013
from the Advanced Technology Solar Telescope) will be the largest
solar facility built when it begins operations in 2019. Designed
and developed to meet the needs of critical high resolution and high
sensitivity spectral and polarimetric observations of the Sun, the
observatory will enable key research for the study of solar magnetism
and its influence on the solar wind, flares, coronal mass ejections
and solar irradiance variations. The 4-meter class facility will
operate over a broad wavelength range (0.38 to 28 microns, initially
0.38 to 5 microns), using a state-of-the-art adaptive optics system to
provide diffraction-limited imaging and the ability to resolve features
approximately 25 km on the Sun. Five first-light instruments will be
available at the start of operations: Visible Broadband Imager (VBI;
National Solar Observatory), Visible SpectroPolarimeter (ViSP; NCAR High
Altitude Observatory), Visible Tunable Filter (VTF; Kiepenheuer Institut
für Sonnenphysik), Diffraction Limited Near InfraRed SpectroPolarimeter
(DL-NIRSP; University of Hawai'i, Institute for Astronomy) and the
Cryogenic Near InfraRed SpectroPolarimeter (Cryo-NIRSP; University of
Hawai'i, Institute for Astronomy). As of mid-2014, the key subsystems
have been designed and fabrication is well underway, including the
site construction, which began in December 2012. We provide an update
on the development of the facilities both on site at the Haleakalā
Observatories on Maui and the development of components around the
world. We present the overall construction and integration schedule
leading to the handover to operations in mid 2019. In addition, we
outline the evolving challenges being met by the project, spanning the
full spectrum of issues covering technical, fiscal, and geographical,
that are specific to this project, though with clear counterparts to
other large astronomical construction projects.
---------------------------------------------------------
Title: mxSPEC: a massively multiplexed full-disk spectroheliograph
for solar physics research
Authors: Lin, Haosheng
2014SPIE.9147E..12L Altcode:
The Massively Multiplexed Spectrograph (mxSPEC) is a new instrument
concept that takes advantage of modern high-speed large-format focal
plane arrays (FPAs) and high efficiency bandpass isolation filters to
multiplex spectra from many slices of the telescope field simultaneously
onto the FPAs within a single grating spectrograph. This design greatly
reduces the time required to scan a large telescope field, and with
current technologies can achieve more than a factor of 50 or more
improvement of the system efficiency over a conventional long-slit
spectrograph. Furthermore, several spectral lines can be observed
at the same time with proper selection of the diffraction grating,
further improving the efficiency of this design to more than two
orders of magnitude over conventional single-slit, single-wavelength
instrument. This paper describes an experimental, proof-of-concept,
40-slit full-disk spectrograph that demonstrates the feasibility
of this new instrument concept and its potential for solar physics
research including helioseismology, dynamic solar events, and
global scale magnetic field observation of the solar disk and the
corona. We also present the preliminary design of a 4-line, 55-slit
spectroheliograph that can serve as the template for the instruments
of the next generation synoptic solar observatory.
---------------------------------------------------------
Title: The Daniel K. Inouye Solar Telescope first light instruments
and critical science plan
Authors: Elmore, David F.; Rimmele, Thomas; Casini, Roberto; Hegwer,
Steve; Kuhn, Jeff; Lin, Haosheng; McMullin, Joseph P.; Reardon, Kevin;
Schmidt, Wolfgang; Tritschler, Alexandra; Wöger, Friedrich
2014SPIE.9147E..07E Altcode:
The Daniel K. Inouye Solar Telescope is a 4-meter-class all-reflecting
telescope under construction on Haleakalā mountain on the island of
Maui, Hawai'i. When fully operational in 2019 it will be the world's
largest solar telescope with wavelength coverage of 380 nm to 28 microns
and advanced Adaptive Optics enabling the highest spatial resolution
measurements of the solar atmosphere yet achieved. We review the
first-generation DKIST instrument designs, select critical science
program topics, and the operations and data handling and processing
strategies to accomplish them.
---------------------------------------------------------
Title: Tools for 3D Spectropolarimetry - A Birefringent Fiber Optic
Image Slicer
Authors: Schad, Thomas A.; Lin, Haosheng
2014AAS...22412358S Altcode:
Image-slicing technology benefits astronomical spectropolarimetry by
transposing a three-dimensional informational set--two spatial and one
spectral dimension--into a format more amenable to simultaneous coverage
by conventional spectrographs. To probe, for example, the magnetism
of the fine-scaled, dynamic chromosphere, methods beyond slit-based
spectropolarimetry are essential. Fiber optic integral field units
(IFUs) present one promising solution. The importance of a birefringent
fiber-optic IFU design stems from the need of spatio-temporal modulation
to correct for spurious polarization signals induced either by platform
jitter or atmospheric seeing. Standard stock fibers do not typically
preserve polarization. Here we characterize the polarization response of
a close-packed IFU based on rectangular optical fibers, currently under
development for the Diffraction-Limited Near-IR Spectropolarimeter,
a facility instrument of the Advanced Technology Solar Telescope. Solar
observations utilizing this device will be presented.
---------------------------------------------------------
Title: 3D Coronal Magnetic Field Reconstruction based on infrared
polarimetric observations
Authors: Kramar, Maxim; Lin, Haosheng; Tomczyk, Steven
2014shin.confE.102K Altcode:
Measurement of the coronal magnetic field is a crucial ingredient in
understanding the nature of solar coronal phenomena at all scales. A
significant progress has been recently achieved here with deployment
of the Coronal Multichannel Polarimeter (CoMP) of the High Altitude
Observatory (HAO). The instrument provides polarization measurements of
Fe xiii 10747 A forbidden line emission. The observed polarization are
the result of a line-of-sight (LOS) integration through a nonuniform
temperature, density and magnetic field distribution. In order resolve
the LOS problem and utilize this type of data, the vector tomography
method has been developed for 3D reconstruction of the coronal magnetic
field. The 3D electron density and temperature, needed as additional
input, have been reconstructed by tomography method based on STEREO/EUVI
data. We will present the 3D coronal density, temperature and magnetic
field resulted from these inversions.
---------------------------------------------------------
Title: From static to dynamic mapping of chromospheric magnetism -
FIRS and SPIES
Authors: Schad, Thomas A.; Lin, Haosheng
2014AAS...22430204S Altcode:
Advancements in theoretical forward modeling and observational
techniques now allow the mapping of the chromospheric magnetic field
vector in some regions. We report on full maps of the chromospheric
magnetic field vector across a sunspot and its superpenumbra within
NOAA AR 11408. These maps are derived from full Stokes observations of
the He I triplet at 1083 nm, which show both Zeeman and atomic-level
polarization signatures. Yet, due to the long time to acquire these
observations with the slit-based Facility Infrared Spectropolarimeter
(FIRS), our measurements primarily probe long-lived chromospheric
structures, albeit at very high polarization sensitivity. The fast
temporal scales remain difficult to probe with conventional slit-based
spectropolarimeters. Alternatively, SPIES is an instrument based on a
birefringent fiber optic IFU, designed to multiplex a two-dimensional
spatial field with high spectral resolution spectropolarimetry, and is
an ideal tool for probing small-scale, dynamic magnetic features. We
will present movies of the dynamic chromosphere acquired from SPIES
across a sunspot and its fine-scaled superpenumbra.
---------------------------------------------------------
Title: Pan-STARRS 1 Observations of the Unusual Active Centaur
P/2011 S1(Gibbs)
Authors: Lin, H. W.; Chen, Y. T.; Lacerda, P.; Ip, W. H.; Holman,
M.; Protopapas, P.; Chen, W. P.; Burgett, W. S.; Chambers, K. C.;
Flewelling, H.; Huber, M. E.; Jedicke, R.; Kaiser, N.; Magnier, E. A.;
Metcalfe, N.; Price, P. A.
2014AJ....147..114L Altcode: 2014arXiv1402.6403L
P/2011 S1 (Gibbs) is an outer solar system comet or active Centaur
with a similar orbit to that of the famous 29P/Schwassmann-Wachmann
1. P/2011 S1 (Gibbs) has been observed by the Pan-STARRS 1 (PS1)
sky survey from 2010 to 2012. The resulting data allow us to perform
multi-color studies of the nucleus and coma of the comet. Analysis of
PS1 images reveals that P/2011 S1 (Gibbs) has a small nucleus <4
km radius, with colors g <SUB> P1</SUB> - r <SUB> P1</SUB> = 0.5 ±
0.02, r <SUB> P1</SUB> - i <SUB> P1</SUB> = 0.12 ± 0.02, and i <SUB>
P1</SUB> - z <SUB> P1</SUB> = 0.46 ± 0.03. The comet remained active
from 2010 to 2012, with a model-dependent mass-loss rate of ~100 kg
s<SUP>-1</SUP>. The mass-loss rate per unit surface area of P/2011
S1 (Gibbs) is as high as that of 29P/Schwassmann-Wachmann 1, making
it one of the most active Centaurs. The mass-loss rate also varies
with time from ~40 kg s<SUP>-1</SUP> to 150 kg s<SUP>-1</SUP>. Due
to its rather circular orbit, we propose that P/2011 S1 (Gibbs)
has 29P/Schwassmann-Wachmann 1-like outbursts that control the
outgassing rate. The results indicate that it may have a similar
surface composition to that of 29P/Schwassmann-Wachmann 1. Our numerical
simulations show that the future orbital evolution of P/2011 S1 (Gibbs)
is more similar to that of the main population of Centaurs than to
that of 29P/Schwassmann-Wachmann 1. The results also demonstrate that
P/2011 S1 (Gibbs) is dynamically unstable and can only remain near
its current orbit for roughly a thousand years.
---------------------------------------------------------
Title: Prominence Science with ATST Instrumentation
Authors: Rimmele, Thomas; Berger, Thomas; Casini, Roberto; Elmore,
David; Kuhn, Jeff; Lin, Haosheng; Schmidt, Wolfgang; Wöger, Friedrich
2014IAUS..300..362R Altcode:
The 4m Advance Technology Solar Telescope (ATST) is under construction
on Maui, HI. With its unprecedented resolution and photon collecting
power ATST will be an ideal tool for studying prominences and filaments
and their role in producing Coronal Mass Ejections that drive Space
Weather. The ATST facility will provide a set of first light instruments
that enable imaging and spectroscopy of the dynamic filament and
prominence structure at 8 times the resolution of Hinode. Polarimeters
allow high precision chromospheric and coronal magnetometry at visible
and infrared (IR) wavelengths. This paper summarizes the capabilities
of the ATST first-light instrumentation with focus on prominence and
filament science.
---------------------------------------------------------
Title: Vector Tomography for the Coronal Magnetic Field. II. Hanle
Effect Measurements
Authors: Kramar, M.; Inhester, B.; Lin, H.; Davila, J.
2013ApJ...775...25K Altcode:
In this paper, we investigate the feasibility of saturated coronal
Hanle effect vector tomography or the application of vector tomographic
inversion techniques to reconstruct the three-dimensional magnetic field
configuration of the solar corona using linear polarization measurements
of coronal emission lines. We applied Hanle effect vector tomographic
inversion to artificial data produced from analytical coronal magnetic
field models with equatorial and meridional currents and global coronal
magnetic field models constructed by extrapolation of real photospheric
magnetic field measurements. We tested tomographic inversion with
only Stokes Q, U, electron density, and temperature inputs to simulate
observations over large limb distances where the Stokes I parameters
are difficult to obtain with ground-based coronagraphs. We synthesized
the coronal linear polarization maps by inputting realistic noise
appropriate for ground-based observations over a period of two weeks
into the inversion algorithm. We found that our Hanle effect vector
tomographic inversion can partially recover the coronal field with a
poloidal field configuration, but that it is insensitive to a corona
with a toroidal field. This result demonstrates that Hanle effect
vector tomography is an effective tool for studying the solar corona
and that it is complementary to Zeeman effect vector tomography for
the reconstruction of the coronal magnetic field.
---------------------------------------------------------
Title: Coronal Magnetic Field Reconstruction based on HAO/CoMP
observations.
Authors: Kramar, Maxim; Lin, H.; Tomczyk, S.; Davila, J.
2013shin.confE..89K Altcode:
The magnetic field is the dominant force source in the solar coronal
plasma, the one that shapes its structure. Synoptic observations that
provide a direct information about the magnetic field have been recently
became available by High Altitude Observatory (HAO) Coronal Multichannel
Polarimeter (CoMP). The instrument provides linear polarization maps of
the Fe XIII 10747 A 'forbidden' line. The observed linear polarization
depends on magnetic field orientation through Hanle effect. These
observation, supplied with additional photospheric magnetic field
measurements and UV observations, are used for 3D reconstruction of
the coronal magnetic field by applying the vector tomography technique.
---------------------------------------------------------
Title: He I Vector Magnetometry of Field-aligned Superpenumbral
Fibrils
Authors: Schad, T. A.; Penn, M. J.; Lin, H.
2013ApJ...768..111S Altcode: 2013arXiv1303.4463S
Atomic-level polarization and Zeeman effect diagnostics in the neutral
helium triplet at 10830 Å in principle allow full vector magnetometry
of fine-scaled chromospheric fibrils. We present high-resolution
spectropolarimetric observations of superpenumbral fibrils in the
He I triplet with sufficient polarimetric sensitivity to infer
their full magnetic field geometry. He I observations from the
Facility Infrared Spectropolarimeter are paired with high-resolution
observations of the Hα 6563 Å and Ca II 8542 Å spectral lines from
the Interferometric Bidimensional Spectrometer from the Dunn Solar
Telescope in New Mexico. Linear and circular polarization signatures
in the He I triplet are measured and described, as well as analyzed
with the advanced inversion capability of the "Hanle and Zeeman Light"
modeling code. Our analysis provides direct evidence for the often
assumed field alignment of fibril structures. The projected angle of
the fibrils and the inferred magnetic field geometry align within an
error of ±10°. We describe changes in the inclination angle of these
features that reflect their connectivity with the photospheric magnetic
field. Evidence for an accelerated flow (~40 m s<SUP>-2</SUP>) along
an individual fibril anchored at its endpoints in the strong sunspot
and weaker plage in part supports the magnetic siphon flow mechanism's
role in the inverse Evershed effect. However, the connectivity of the
outer endpoint of many of the fibrils cannot be established.
---------------------------------------------------------
Title: The Advanced Technology Solar Telescope: Science Drivers and
Construction Status
Authors: Rimmele, Thomas; Berger, Thomas; McMullin, Joseph; Keil,
Stephen; Goode, Phil; Knoelker, Michael; Kuhn, Jeff; Rosner, Robert;
Casini, Roberto; Lin, Haosheng; Woeger, Friedrich; von der Luehe,
Oskar; Tritschler, Alexandra; Atst Team
2013EGUGA..15.6305R Altcode:
The 4-meter Advance Technology Solar Telescope (ATST) currently
under construction on the 3000 meter peak of Haleakala on Maui,
Hawaii will be the world's most powerful solar telescope and the
leading ground-based resource for studying solar magnetism. The
solar atmosphere is permeated by a 'magnetic carpet' that constantly
reweaves itself to control solar irradiance and its effects on Earth's
climate, the solar wind, and space weather phenomena such as flares and
coronal mass ejections. Precise measurement of solar magnetic fields
requires a large-aperture solar telescope capable of resolving a few
tens of kilometers on the solar surface. With its 4 meter aperture,
the ATST will for the first time resolve magnetic structure at the
intrinsic scales of plasma convection and turbulence. The ATST's
ability to perform accurate and precise spectroscopic and polarimetric
measurements of magnetic fields in all layers of the solar atmosphere,
including accurate mapping of the elusive coronal magnetic fields,
will be transformative in advancing our understanding of the magnetic
solar atmosphere. The ATST will utilize the Sun as an important astro-
and plasma-physics "laboratory" demonstrating key aspects of omnipresent
cosmic magnetic fields. The ATST construction effort is led by the US
National Solar Observatory. State-of-the-art instrumentation will be
constructed by US and international partner institutions. The technical
challenges the ATST is facing are numerous and include the design of the
off-axis main telescope, the development of a high order adaptive optics
system that delivers a corrected beam to the instrument laboratory,
effective handling of the solar heat load on optical and structural
elements, and minimizing scattered light to enable observations
of the faint corona. The ATST project has transitioned from design
and development to its construction phase. The project has awarded
design and fabrication contracts for major telescope subsystems. Site
construction has commenced following the successful conclusion of
the site permitting process. Science goals and construction status of
telescope and instrument systems will be discussed.
---------------------------------------------------------
Title: Reconstruction of the 3D Coronal Magnetic Field by Vector
Tomography with Infrared Spectropolarimetric Observations from CoMP
Authors: Kramar, M.; Lin, H.; Tomczyk, S.; Davila, J. M.; Inhester, B.
2012AGUFMSH42A..06K Altcode:
Magnetic fields determine the static and dynamic properties of the solar
corona. A significant progress has been achieved in direct measurement
of the magnetically sensitive coronal emission with deployment of
the HAO Coronal Multichannel Polarimeter (CoMP). The instrument
provides polarization measurements of Fe XIII 10747 A forbidden line
emission. The observed polarization depends on magnetic field through
the Hanle and Zeeman effects. However, because the coronal measurements
are integrated over line-of-site (LOS), it is impossible to derive the
configuration of the coronal magnetic field from a single observation
(from a single viewing direction). The vector tomography techniques
based on the infrared polarimetric measurements from several viewing
directions has been developed in order to resolve the 3D coronal
magnetic field structure over LOS. Because of the non-linear character
of the Hanle effect, the reconstruction result based on such data
is not straightforward and depends on the particular coronal field
configuration. For several possible cases of coronal magnetic field
configuration, it has been found that even just Stokes-Q and -U data
(supplied with 3D coronal density and temperature) can be used in the
vector tomography to provide a realistic 3D coronal magnetic field. The
3D coronal density and temperature needed as an supplemental input are
reconstructed by the scalar field tomography method using ultraviolet
observations from EUVI/STEREO. We will present the reconstructed 3D
coronal density, temperature and magnetic field in the range of ∼
1.3 R<SUB>⊙</SUB> obtained by the scalar and vector tomography.
---------------------------------------------------------
Title: SPIES: the spectropolarimetric imager for the energetic sun
Authors: Lin, Haosheng
2012SPIE.8446E..1DL Altcode:
The SpectroPolarimetric Imager for the Energetic Sun (SPIES) is a
project to develop a new class of spectropolarimetric instrument for
the study of highly dynamic solar phenomena. Understanding the physics
of dynamic solar phenomena requires detailed information about the
magnetic, thermal, and dynamic properties of the solar atmosphere
at every stage of their evolution. Although these properties can be
obtained with existing highperformance spectropolarimeters such as
the SpectroPolarimeter onboard the Hinode space solar observatory or
the Facility IR Spectropolarimeter of the Dunn Solar Telescope, these
instruments cannot observe the required field of view with temporal
resolution that can resolve the dynamic timescale of these energetic
events. SPIES-2K is an experimental true-imaging spectropolarimeter
developed under this program to address this deficiency in our
observing capability. It is based on a fiber-optic integral field
unit containing 2,048 standard multimode fused silica fibers, and is
capable of observing a 64 x 32 pixels field simultaneously with high
spatial and spectral resolution. Moreover, it can obtain the full
Stokes spectra of the field with a maximum temporal resolution of a
few seconds. This paper presents the design and characteristics of
the instrument, as well as preliminary results obtained at Fe I 1565
nm wavelength. Additionally, this paper also reports on recent studies
of the polarization maintenance optical fiber ribbon constructed from
rectangular element fibers for the Birefringence Fiber-Optic Image
Slicer, and discusses its application to future generation of SPIES
and other astronomical spectropolarimetry projects.
---------------------------------------------------------
Title: 3D Coronal Magnetic Field reconstructed by Vector Tomography
Method using CoMP data
Authors: Kramar, Maxim; Lin, H.; Tomczyk, S.; Inhester, B.; Davila, J.
2012shin.confE.141K Altcode:
Magnetic fields in the solar corona dominates the gas pressure
and therefore determine the static and dynamic properties of the
corona. Direct measurement of the coronal magnetic field is one of
the most challenging problems in observational solar astronomy and
recently a significant progress has been achieved here with deployment
of the HAO Coronal Multichannel Polarimeter (CoMP). The instrument
provides polarization measurements of Fe XIII 10747 A forbidden line
emission. The observed polarization depends on magnetic field through
the Hanle and Zeeman effects. However, because the coronal measurements
are integrated over line-of-site (LOS), it is impossible to derive the
configuration of the coronal magnetic field from a single observation
(from a single viewing direction). The vector tomography techniques
based on measurements from several viewing directions has the potential
to resolve the 3D coronal magnetic field structure over LOS. Because
of the non-linear character of the Hanle effect, the reconstruction
result based on such data is not straightforward and depends on the
particular coronal field configuration. Therefore, previously we also
studied what is the sensitivity of the vector tomographic inversion to
various coronal magnetic field models. For several possible cases of
coronal magnetic field configuration, it has been found that even just
Stokes-Q and -U data (supplied with 3D coronal density and temperature)
can be used in vector tomography to provide a realistic 3D coronal
magnetic field configuration. The 3D coronal density and temperature
needed as an supplemental input are reconstructed by the scalar field
tomography method using ultraviolet observations from EUVI/STEREO. We
will present the reconstructed 3D coronal magnetic field in the range
of ∼1.3 R_⊙ obtained by the vector tomographic technique that has
been applied to the CoMP data.
---------------------------------------------------------
Title: Multi-height Spectropolarimetry Of Sunspots With Firs And Ibis
Authors: Jaeggli, Sarah A.; Lin, H.; Tritschler, A.
2012AAS...22020606J Altcode:
The effects of radiative transfer prevent the characterization of
the magnetic field at a single geometric height in the photosphere
of a sunspot. Therefore, a full 3D characterization of the magnetic
field is necessary to understand many properties of sunspots, such as
the true state of hydrostatic equilibrium. Many current and proposed
solar spectropolarimeters are capable of taking near-simultaneous
observations at multiple wavelengths. Combining these rich datasets
provides a welcome problem to the community. We present the first joint
observations of the magnetically sensitive photospheric Fe I lines at
630 and 1565 nm taken with the Facility Infrared Spectropolarimeter
(FIRS); and the chromospheric Ca II line at 854 nm taken with the
Interferometric Bi-Dimensional Spectrometer (IBIS); both instruments
operated at the Dunn Solar Telescope. These wavelengths allow us to
probe the magnetic field over a broad range of heights, from the
bottom of the photosphere to the chromosphere. We investigate the
magnetic field topologies of several sunspots of different size and
magnetic complexity.
---------------------------------------------------------
Title: Spies - Spectral Polarimetric Imager For The Energetic Sun
Authors: Lin, Haosheng; Jaeggli, S.
2012AAS...22012306L Altcode:
Spectropolarimetric observation with uncompromised spatial, spectral,
and temporal resolution simulatneously over a substantial 2D field and
multiple spectral lines is the key to the resolution of many important
questions in modern solar physics. While 2D imaging spectroscopy
based on fiber optics integral field unit and image slicer has a long
history nighttime astronomy, adaptation for solar observation occured
only recently. This paper will present preliminary results of magnetic
field observation in the HeI 1083 nm and FeI 1565 nm lines obtained
with SPIES --- a true imaging spectropolarimeter based on a large format
(64 x 32 fibers input array) fiber-optic array optimized for the study
of evolution of magnetic and thermodynamic properties of energetic and
dynamic phenomena of the sun. We will also discuss considerations for
the use of fiber-optic array for solar spectropolarimetric applications,
as well as the design of SPIES.
---------------------------------------------------------
Title: On Molecular Hydrogen Formation and the Magnetohydrostatic
Equilibrium of Sunspots
Authors: Jaeggli, S. A.; Lin, H.; Uitenbroek, H.
2012ApJ...745..133J Altcode: 2011arXiv1110.0575J
We have investigated the problem of sunspot magnetohydrostatic
equilibrium with comprehensive IR sunspot magnetic field survey
observations of the highly sensitive Fe I lines at 15650 Å and nearby
OH lines. We have found that some sunspots show isothermal increases
in umbral magnetic field strength which cannot be explained by the
simplified sunspot model with a single-component ideal gas atmosphere
assumed in previous investigations. Large sunspots universally
display nonlinear increases in magnetic pressure over temperature,
while small sunspots and pores display linear behavior. The formation
of molecules provides a mechanism for isothermal concentration of
the umbral magnetic field, and we propose that this may explain the
observed rapid increase in umbral magnetic field strength relative to
temperature. Existing multi-component sunspot atmospheric models predict
that a significant amount of molecular hydrogen (H<SUB>2</SUB>) exists
in the sunspot umbra. The formation of H<SUB>2</SUB> can significantly
alter the thermodynamic properties of the sunspot atmosphere and
may play a significant role in sunspot evolution. In addition to the
survey observations, we have performed detailed chemical equilibrium
calculations with full consideration of radiative transfer effects
to establish OH as a proxy for H<SUB>2</SUB>, and demonstrate that a
significant population of H<SUB>2</SUB> exists in the coolest regions
of large sunspots.
---------------------------------------------------------
Title: SPIES: Spectropolarimetric Imager for Energetic Sun
Authors: Weis, Andrew; Lin, H.
2012AAS...21914409W Altcode:
Solar magnetic fields are responsible for the appearance of the
solar atmosphere. These magnetic fields are non-uniform, and are
strongest over sunspots. Magnetic fields are thought to cause energetic
phenomena such as solar flares and coronal mass ejections, which can
have damaging consequences in the near-Earth space environment and
high latitude regions, providing practical in addition to scientific
reasons to study them. Current instrumentation for observations
of solar magnetic fields use scanning slit spectrograph or tunable
filter, which allow us to resolve the time evolution of the fields to
the scale of minutes or longer. We are constructing a new instrument,
SPIES, based on a large-format (32 x 64) fiber-optic integral field
unit (IFU). The fiber-optic IFU allows us to observe over two spatial
dimensions and one spectral dimension simultaneously rather than in
steps, thus allowing for resolution of the time evolution to the level
of seconds. Due to fiber modal noise and small thermal drift of the
instrument over time, flat-fielding of the intensity spectra from the
discrete fiber-optic 'slits' becomes time dependent. An observing scheme
that records time-sensitive flat-fields was devised for SPIES. We will
present preliminary analysis of the full-Stokes polarization spectra
of a sunspot obtained with SPIES over a 90 minute time span. This work
was conducted through a Research Experience for Undergraduates (REU)
position at the University of Hawai'i's Institute for Astronomy and
was funded by the NSF.
---------------------------------------------------------
Title: Vector Tomography Inversion for the 3D Coronal Magnetic Field
Based on CoMP data
Authors: Kramar, M.; Lin, H.; Tomczyk, S.; Inhester, B.; Davila, J. M.
2011AGUFMSH43B1948K Altcode:
Magnetic fields in the solar corona dominates the gas pressure
and therefore determine the static and dynamic properties of the
corona. Direct measurement of the coronal magnetic field is one of
the most challenging problems in observational solar astronomy and
recently a significant progress has been achieved here with deployment
of the HAO Coronal Multichannel Polarimeter (CoMP). The instrument
provides polarization measurements of Fe XIII 10747 A forbidden line
emission. The observed polarization depends on magnetic field through
the Hanle and Zeeman effects. However, because the coronal measurements
are integrated over line-of-site (LOS), it is impossible to derive the
configuration of the coronal magnetic field from a single observation
(from a single viewing direction). The vector tomography techniques
based on measurements from several viewing directions has the potential
to resolve the 3D coronal magnetic field structure over LOS. Because
of the non-linear character of the Hanle effect, the reconstruction
result based on such data is not straightforward and depends on the
particular coronal field configuration. Therefore we study here what is
the sensitivity of the vector tomographic inversion to sophisticated
(MHD) coronal magnetic field models. For several important cases of
magnetic field configuration, it has been found that even just Stokes-Q
and -U data (supplied with 3D coronal density and temperature) can be
used in vector tomography to provide a realistic 3D coronal magnetic
field configuration. This vector tomograpic technique is applied to
CoMP data.
---------------------------------------------------------
Title: Vector Tomography for the 3D Coronal Magnetic Field with CoMP
Authors: Kramar, Maxim; Lin, Haosheng; Inhester, Bernd; Gibson, Sarah
2011shin.confE..29K Altcode:
Magnetic fields in the solar corona dominates the gas pressure
and therefore determine the static and dynamic properties of the
corona. Direct measurement of the coronal magnetic field is one of
the most challenging problems in observational solar astronomy and
recently a significant progress has been achieved here with deployment
of the HAO Coronal Multichannel Polarimeter (CoMP). The instrument
provides polarization measurements of Fe XIII 10747 A forbidden line
emission. The observed polarization depends on magnetic field through
the Hanle and Zeeman effects. However, because the coronal measurements
are integrated over line-of-site (LOS), it is impossible to derive the
configuration of the coronal magnetic field from a single observation
(from a single viewing direction). The vector tomography techniques
based on measurements from several viewing directions has the potential
to resolve the 3D coronal magnetic field structure over LOS. Because
of the non-linear character of the Hanle effect, the reconstruction
result based on such data is not straightforward and depends on the
particular coronal field configuration. Therefore we study here what
is the sensitivity of the vector tomographic inversion to sophisticated
(MHD) coronal magnetic field models. <P />For several important cases of
magnetic field configuration, it has been found that even just Stokes-Q
and -U data (supplied with 3D coronal density and temperature) can be
used in vector tomography to provide a realistic 3D coronal magnetic
field configuration. Effect of noise in the all input data has been
also studied. Inclusion of the Stokes-V data into the inversion will
significantly increase a number of of magnetic field configuration which
are possible to reconstruct. <P />Particularly, the reconstructions
may be used to analyze non-potential pre-CME magnetic configurations
or for improving a potential field model when the field is potential.
---------------------------------------------------------
Title: An Observational Study of the Formation and Evolution of
Sunspots
Authors: Jaeggli, Sarah A.; Lin, H.; Uitenbroek, H.
2011SPD....42.0302J Altcode: 2011BAAS..43S.0302J
It is well known that the thermal-magnetic relation in sunspots can
be non-linear. Previous investigations ascribe the non-linearity
of the relation to changing geometrical height of the measurement
due to radiative transfer effects (Wilson Depression) and the poorly
determined magnetic field curvature force. However, the very coolest
regions of some sunspots show a rapid increase in umbral magnetic
field strength relative to temperature which cannot be explained
by the simplified sunspot model with single-component ideal gas
atmosphere which has been previously assumed. This represents a
fundamental flaw in our understanding of the sunspot equilibrium
problem. Existing multiple-component sunspot atmospheric models
predict that a large amount of molecular hydrogen (H2) exists in
the sunspot umbra. The formation of molecules provides a mechanism
for isothermal concentration of the umbral magnetic field which may
explain the observed rapid increase in umbral magnetic field strength
relative to temperature. We have characterized the equilibrium forces
in sunspots using simultaneous visible and IR sunspot magnetic field
survey observations of the highly sensitive Fe I lines at 6302 and
15650 Angstroms and nearby OH lines which have been conducted with
the new Facility Infrared Spectropolarimeter (FIRS) at the Dunn Solar
Telescope. We have performed detailed chemical equilibrium calculations
with full consideration of radiative transfer effects to establish OH
as a proxy for H2, and demonstrate that a significant population of H2
exists in the coolest regions of large and more mature sunspots. We
further point out that the formation of H2 can significantly alter
the thermodynamic properties of the sunspot atmosphere and may play
a significant role in sunspot evolution.
---------------------------------------------------------
Title: Vector Tomography Based on Hanle and Zeeman Effects Observed
from Ecliptic Plane
Authors: Kramar, Maxim; Lin, H.; Gibson, S.
2011SPD....42.1830K Altcode: 2011BAAS..43S.1830K
The magnetically sensitive coronal emission lines provide
information about coronal magnetic field via Hanle and Zeeman
effects. As the measured emission are integrated over line-of-sight,
the vector tomography must be used for deriving 3D magnetic field
configuration. The unique solution for any field configuration exists
when observations are done from both ecliptic and out of ecliptic
plane and supplied by photospheric magnetic field measurements. When
observations are only from the ecliptic plane, the number of field
configurations which are possible to reconstruct are reduced. We
study here what types of coronal magnetic field configurations can be
reconstructed based on Hanle and Zeeman effects provided by CoMP and
SOLARC instruments. Effect of noise in the data and uncertainty in 3D
reconstruction of the coronal density and temperature are also studied.
---------------------------------------------------------
Title: Whole Earth Telescope observations of the subdwarf B star
KPD 1930+2752: a rich, short-period pulsator in a close binary
Authors: Reed, M. D.; Harms, S. L.; Poindexter, S.; Zhou, A. -Y.;
Eggen, J. R.; Morris, M. A.; Quint, A. C.; McDaniel, S.; Baran, A.;
Dolez, N.; Kawaler, S. D.; Kurtz, D. W.; Moskalik, P.; Riddle, R.;
Zola, S.; Østensen, R. H.; Solheim, J. -E.; Kepler, S. O.; Costa,
A. F. M.; Provencal, J. L.; Mullally, F.; Winget, D. W.; Vuckovic, M.;
Crowe, R.; Terry, D.; Avila, R.; Berkey, B.; Stewart, S.; Bodnarik,
J.; Bolton, D.; Binder, P. -M.; Sekiguchi, K.; Sullivan, D. J.; Kim,
S. -L.; Chen, W. -P.; Chen, C. -W.; Lin, H. -C.; Jian, X. -J.; Wu, H.;
Gou, J. -P.; Liu, Z.; Leibowitz, E.; Lipkin, Y.; Akan, C.; Cakirli,
O.; Janulis, R.; Pretorius, R.; Ogloza, W.; Stachowski, G.; Paparo,
M.; Szabo, R.; Csubry, Z.; Zsuffa, D.; Silvotti, R.; Marinoni, S.;
Bruni, I.; Vauclair, G.; Chevreton, M.; Matthews, J. M.; Cameron,
C.; Pablo, H.
2011MNRAS.412..371R Altcode: 2011MNRAS.tmp..184R; 2010arXiv1011.0387R
KPD 1930+2752 is a short-period pulsating subdwarf B (sdB) star. It is
also an ellipsoidal variable with a known binary period of 2.3 h. The
companion is most likely a white dwarf and the total mass of the
system is close to the Chandresekhar limit. In this paper, we report
the results of Whole Earth Telescope (WET) photometric observations
during 2003 and a smaller multisite campaign of 2002. From 355 h of WET
data, we detect 68 pulsation frequencies and suggest an additional 13
frequencies within a crowded and complex temporal spectrum between 3065
and 6343 μHz (periods between 326 and 157 s). We examine pulsation
properties including phase and amplitude stability in an attempt
to understand the nature of the pulsation mechanism. We examine a
stochastic mechanism by comparing amplitude variations with simulated
stochastic data. We also use the binary nature of KPD 1930+2752 for
identifying pulsation modes via multiplet structure and a tidally
induced pulsation geometry. Our results indicate a complicated pulsation
structure that includes short-period (≈16 h) amplitude variability,
rotationally split modes, tidally induced modes and some pulsations
which are geometrically limited on the sdB star.
---------------------------------------------------------
Title: Testing the vector tomography method for 3D reconstruction
of the coronal magnetic field for different coronal field models
Authors: Kramar, M.; Lin, H.; Inhester, B.
2010AGUFMSH31A1789K Altcode:
Magnetic fields in the solar corona dominates the gas pressure
and therefore determine the static and dynamic properties of the
corona. Direct measurement of the coronal magnetic field is one of the
most challenging problems in observational solar astronomy and recently
had significant progress (Lin et al. 2004; Tomczyk et al. 2008). The
polarization of infrared Fe XIII 10747 A forbidden line depends on
magnetic field through the Hanle and Zeeman effects. However, because
the coronal measurements are integrated over line-of-site (LOS),
it is impossible to derive the configuration of the coronal magnetic
field from a single observation (from a single viewing direction). The
vector tomography techniques based on measurements from several viewing
directions has the potential to resolve the 3D coronal magnetic
field structure over LOS. Previously, the potential of the method
was demonstrated for two basic model field configurations (Kramar et
al. 2006). Because of the non-linear character of the Hanle effect,
the reconstruction result based on such data is not straightforward
and depends on the particular coronal field configuration. Therefore we
study here what is the sensitivity of the vector tomographic inversion
to more sophisticated (MHD) coronal magnetic field models.
---------------------------------------------------------
Title: Magnetic Field Measurements at the Photosphere and Coronal Base
Authors: Judge, P. G.; Centeno, R.; Tritschler, A.; Uitenbroek, H.;
Jaeggli, S.; Lin, H.
2010AGUFMSH31A1783J Altcode:
We have obtained vector polarimetric measurements in lines of Fe I
(630nm), Ca II (854nm) and He I (1083nm) of several active regions
during 3-14 June 2010. The measurements were made at the Dunn Solar
Telescope at Sacramento Peak Observatory, using the FIRS and IBIS
instruments simultaneously. We discuss these and SDO data for NOAA
11076. The seeing was very good or excellent and the adaptive
optics system functioned well. In this preliminary analysis we
compare extrapolations of photospheric fields with the constraints
available from Stokes polarimetry, including the morphology and
kinematic properties of fibrils. Connections to the corona will also be
discussed. The implications for field extrapolations from photospheric
measurements will be discussed. We will make the reduced data freely
available on the web for interested researchers.
---------------------------------------------------------
Title: Utilization of redundant polarized solar spectra to infer
the polarization properties of the new generation of large aperture
solar telescopes
Authors: Elmore, David F.; Lin, Haosheng; Socas Navarro, Héctor;
Jaeggli, Sarah A.
2010SPIE.7735E..4EE Altcode: 2010SPIE.7735E.147E
Spectro-polarimetry plays an important role in the study of solar
magnetism and strongly influences the design of the new generation of
solar telescopes. Calibration of the polarization properties of the
telescope is a critical requirement needed to use these observations to
infer solar magnetic fields. However, the large apertures of these new
telescopes make direct calibration with polarization calibration optics
placed before all the telescope optical elements impractical. It is
therefore desirable to be able to infer the polarization properties
of the telescope optical elements utilizing solar observations
themselves. Taking advantage of the fact that the un-polarized,
linearly, and circularly polarized spectra originating from the Sun are
uncorrelated, we have developed techniques to utilize observations
of solar spectra with redundant combination of the polarization
states measured at several different telescope configurations to
infer the polarization properties of the telescope as a whole and of
its optical elements. We show results of these techniques applied to
spectro-plarimetric data obtained at the Dunn Solar Telescope.
---------------------------------------------------------
Title: Magnetic field measurements at the photosphere and coronal base
Authors: Judge, Philip; Centeno, R.; Tritschler, A.; Uitenbroek, H.;
Jaeggli, S.; Lin, H.
2010shin.confE..56J Altcode:
We have obtained vector polarimetric measurements in lines of Fe I
(630nm), Ca II (854nm) and He I (1083) of several active regions during
3-14 June 2010. The measurements were made at the Dunn Solar Telescope
at Sacramento Peak Observatory, using the FIRS and IBIS instruments
simultaneously. We discuss data for NOAA 11076 observed on 4 June
2010. The seeing was very good or excellent and the adaptive optics
system functioned well. In this preliminary analysis we compare linear
extrapolations of photospheric fields with the constraints available
from Stokes polarimetry, including the morphology and kinematic
properties of fibrils. The implications for field extrapolations from
photospheric measurements will be discussed. We will make the reduced
data freely available on the web for interested researchers.
---------------------------------------------------------
Title: On the Vector Tomographic Reconstruction for the pre-CME
Coronal Magnetic Field from Fe XIII 10747 A Emission Line Observations
Authors: Kramar, Maxim; Lin, H.; Inhester, B.; Davila, J.
2010AAS...21630203K Altcode:
Magnetic fields are the dominant fields that determine the static and
dynamic properties of the solar corona. The coronal mass ejections
(CMEs) involve the release of the magnetic energy stored in the
magnetic field. Therefore, analyzing the magnetic field could help
to understand the nature of CMEs. One of the more promising coronal
magnetic field measurement methods that have been successfully
demonstrated is the spectropolarimetric observations of the Fe XIII
10747 A forbidden emission line (Lin, Penn & Tomczyk 2000; Lin, Kuhn
& Coulter 2004; Tomczyk et al. 2007) formed due to Hanle and Zeeman
effects. However, these measurements are integrated over line-of-sight
(LOS). Therefore it is impossible to determine the configuration of
the coronal magnetic field from a single observation (single viewing
direction). <P />Vector tomography based on polarimetric observations
of the forbidden coronal emission lines can reconstruct the coronal
magnetic field when the observations are obtained from several viewing
directions. As the tomography method requires observations from many
directions, a rigid rotation of the coronal structures during a half of
solar rotation is assumed. However, many pre-CME magnetic configurations
evolve more rapidly causing significant reduce in the number of
available observing directions. Here we study the sensitivity of the
vector tomographic inversion to possible pre-CME coronal magnetic field
configurations and the number of available observing directions. We
show that the vector tomography techniques has the potential to resolve
the 3D coronal non-potential magnetic field structure.
---------------------------------------------------------
Title: Coronal magnetic fields from the inversion of linear
polarization measurements
Authors: Liu, Yu; Lin, Haosheng; Kuhn, Jeff
2010IAUS..264...96L Altcode:
Real 3-D coronal magnetic field reconstruction is expected to be made
based on the technologies of IR spectrometry and tomography, in which
the data from other wavelengths can be used as critical reference. Our
recent studies focused on this issue are briefly reviewed in this
paper. Liu & Lin (2008) first evaluated the validity of potential
field source surface model applied to one of five limb regions in
the corona by comparing the theoretical polarization maps with SOLARC
observations in the IR Fe XIII 10747 Å forbidden coronal emission line
(CEL). The five limb coronal regions were then studied together in
order to study the spatial relation between the bright EUV features
on the solar disk and the inferred IR emission sources, which were
obtained from the inversion of the SOLARC linear polarization (LP)
measurements (Liu 2009). The inversion for each fiber data in the field
of view was made by finding the best location where the difference
between the synthesized and the observed polarizations reaches the
minimum in the integration path along the line of sight. We found a
close relationship between the inferred IR emission source locations
and the EUV strong emission positions.
---------------------------------------------------------
Title: FIRS: a new instrument for photospheric and chromospheric
studies at the DST.
Authors: Jaeggli, S. A.; Lin, H.; Mickey, D. L.; Kuhn, J. R.; Hegwer,
S. L.; Rimmele, T. R.; Penn, M. J.
2010MmSAI..81..763J Altcode:
The simultaneous observation of select spectral lines at optical and
infrared wavelengths allows for the determination of the magnetic
field at several photospheric and chromospheric heights and thus
the 3D magnetic field gradient in the solar atmosphere. The Facility
Infrared Spectropolarimeter (FIRS) is a newly completed, multi-slit,
dual-beam spectropolarimeter installed at the Dunn Solar Telescope
(DST) at Sacramento Peak (NSO/SP). Separate optics and polarimeters
simultaneously observe two band-passes at visible and infrared
wavelengths with a choice of two modes: the Fe I 6302 Å and 15648 Å
lines in the photosphere; or the Fe I 6302 Å and He I 10830 Å line
in the photosphere and high chromosphere, respectively. FIRS can also
operate simultaneously with a white light camera, G-band imager, and
the Interferometric Bi-dimensional Spectrometer (IBIS) observing the
mid-chromospheric Ca II 8542 Å line. The instrument uses four parallel
slits to sample four slices of the solar surface simultaneously to
achieve fast, diffraction-limited precision imaging spectropolarimetry,
enabling the study of MHD phenomena with short dynamic time scales.
---------------------------------------------------------
Title: Vector tomographic reconstruction for the coronal magnetic
field from Fe XIII 10747 A emission line observations
Authors: Kramar, Maxim; Lin, Haosheng; Inhester, Bernd; Davila, Joseph
2010cosp...38.1862K Altcode: 2010cosp.meet.1862K
Magnetic fields in the solar corona are the dominant fields that
determine the static and dy-namic properties of this outermost region
of the solar atmosphere. It is within this tenuous region that the
magnetic force dominates the gas pressure. Direct measurement of
the coronal magnetic field is one of the most challenging problems
in observational solar astronomy. To date, one of the promising
measurement methods that have been successfully demonstrated is
the spectropolarimetric measurement of the Fe XIII 10747 A forbidden
emission line (Lin, Penn Tomczyk 2000; Lin, Kuhn Coulter 2004; Tomczyk
et al. 2007) formed due to Hanle and Zeeman effects. However, because
coronal measurements are integrated over line-of-site (LOS), it is
impossible to derive the configuration of the coronal magnetic field
from a single obser-vation (from a single viewing direction). In this
paper, we study the sensitivity of the vector tomographic inversion to
possible pre-CME coronal magnetic field configurations and number of
available observations. We show that the vector tomography techniques
based on Hanle and/or Zeeman effect observations has the potential to
resolve the 3D coronal non-potential magnetic field structure.
---------------------------------------------------------
Title: On the reconstructing the coronal magnetic field from Fe XIII
10747 A emission line observations
Authors: Kramar, M.; Lin, H.; Inhester, B.
2009AGUFMSH41B1662K Altcode:
Magnetic fields in the solar corona are the dominant fields that
determine the static and dynamic properties of this outermost region
of the solar atmosphere. It is within this tenuous region that the
magnetic force dominates the gas pressure. Direct measurement of
the coronal magnetic field is one of the most challenging problems
in observational solar astronomy. To date, one of the promising
measurement methods that have been successfully demonstrated is
the spectropolarimetric measurement of the Fe XIII 10747 A forbidden
emission line (CEL) (Lin, Penn, Tomczyk 2000; Lin, Kuhn, Coulter 2004;
Tomczyk et al. 2007) formed due to Hanle and Zeeman effects. However,
because coronal measurements are integrated over line-of-site (LOS), it
is impossible to derive the configuration of the coronal magnetic field
from a single observation (from a single viewing direction). Recent
development in vector tomography techniques based on IR forbidden
CEL polarization measurements from several viewing direction (Kramar,
Inhester, Solanki 2006; Kramar, Inhester 2007) has the potential to
resolve the 3D coronal magnetic field structure. In this paper, we
will present a study of the effects of instrumental characteristics on
the results of vector tomographic inversion using simulated data. We
also investigate the sensitivity of the vector tomographic inversion
to different coronal magnetic field configuration.
---------------------------------------------------------
Title: New Observation of Failed Filament Eruptions: The Influence
of Asymmetric Coronal Background Fields on Solar Eruptions
Authors: Liu, Y.; Su, J.; Xu, Z.; Lin, H.; Shibata, K.; Kurokawa, H.
2009ApJ...696L..70L Altcode:
Failed filament eruptions not associated with a coronal mass ejection
(CME) have been observed and reported as evidence for solar coronal
field confinement on erupting flux ropes. In those events, each
filament eventually returns to its origin on the solar surface. In
this Letter, a new observation of two failed filament eruptions is
reported which indicates that the mass of a confined filament can be
ejected to places far from the original filament channel. The jetlike
mass motions in the two failed filament eruptions are thought to be
due to the asymmetry of the background coronal magnetic fields with
respect to the locations of the filament channels. The asymmetry of the
coronal fields is confirmed by an extrapolation based on a potential
field model. The obvious imbalance between the positive and negative
magnetic flux (with a ratio of 1:3) in the bipolar active region is
thought to be the direct cause of the formation of the asymmetric
coronal fields. We think that the asymmetry of the background fields
can not only influence the trajectories of ejecta, but also provide
a relatively stronger confinement for flux rope eruptions than the
symmetric background fields do.
---------------------------------------------------------
Title: 2006 Whole Earth Telescope Observations of GD358: A New Look
at the Prototype DBV
Authors: Provencal, J. L.; Montgomery, M. H.; Kanaan, A.; Shipman,
H. L.; Childers, D.; Baran, A.; Kepler, S. O.; Reed, M.; Zhou, A.;
Eggen, J.; Watson, T. K.; Winget, D. E.; Thompson, S. E.; Riaz,
B.; Nitta, A.; Kleinman, S. J.; Crowe, R.; Slivkoff, J.; Sherard,
P.; Purves, N.; Binder, P.; Knight, R.; Kim, S. -L.; Chen, Wen-Ping;
Yang, M.; Lin, H. C.; Lin, C. C.; Chen, C. W.; Jiang, X. J.; Sergeev,
A. V.; Mkrtichian, D.; Andreev, M.; Janulis, R.; Siwak, M.; Zola,
S.; Koziel, D.; Stachowski, G.; Paparo, M.; Bognar, Zs.; Handler,
G.; Lorenz, D.; Steininger, B.; Beck, P.; Nagel, T.; Kusterer, D.;
Hoffman, A.; Reiff, E.; Kowalski, R.; Vauclair, G.; Charpinet, S.;
Chevreton, M.; Solheim, J. E.; Pakstiene, E.; Fraga, L.; Dalessio, J.
2009ApJ...693..564P Altcode: 2008arXiv0811.0768P
We report on the analysis of 436.1 hr of nearly continuous high-speed
photometry on the pulsating DB white dwarf GD358 acquired with the
Whole Earth Telescope (WET) during the 2006 international observing
run, designated XCOV25. The Fourier transform (FT) of the light curve
contains power between 1000 and 4000 μHz, with the dominant peak at
1234 μHz. We find 27 independent frequencies distributed in 10 modes,
as well as numerous combination frequencies. Our discussion focuses
on a new asteroseismological analysis of GD358, incorporating the 2006
data set and drawing on 24 years of archival observations. Our results
reveal that, while the general frequency locations of the identified
modes are consistent throughout the years, the multiplet structure
is complex and cannot be interpreted simply as l = 1 modes in the
limit of slow rotation. The high-k multiplets exhibit significant
variability in structure, amplitude and frequency. Any identification
of the m components for the high-k multiplets is highly suspect. The
k = 9 and 8 modes typically do show triplet structure more consistent
with theoretical expectations. The frequencies and amplitudes exhibit
some variability, but much less than the high-k modes. Analysis of the
k = 9 and 8 multiplet splittings from 1990 to 2008 reveal a long-term
change in multiplet splittings coinciding with the 1996 sforzando event,
where GD358 dramatically altered its pulsation characteristics on a
timescale of hours. We explore potential implications, including the
possible connections between convection and/or magnetic fields and
pulsations. We suggest future investigations, including theoretical
investigations of the relationship between magnetic fields, pulsation,
growth rates, and convection.
---------------------------------------------------------
Title: Pair Analysis of Field Galaxies from the Red-Sequence Cluster
Survey
Authors: Hsieh, B. C.; Yee, H. K. C.; Lin, H.; Gladders, M. D.;
Gilbank, D. G.
2008ApJ...683...33H Altcode: 2008arXiv0804.1604H
We study the evolution of the number of close companions of similar
luminosities per galaxy (N<SUB>c</SUB>) by choosing a volume-limited
subset of the photometric redshift catalog from the Red-Sequence Cluster
Survey (RCS-1). The sample contains over 157,000 objects with a moderate
redshift range of 0.25 <= z<= 0.8 and M<SUB>R<SUB>c</SUB></SUB>
<= - 20. This is the largest sample used for pair evolution analysis,
providing data over nine redshift bins with about 17,500 galaxies
in each. After applying incompleteness and projection corrections,
N<SUB>c</SUB> shows a clear evolution with redshift. The N<SUB>c</SUB>
value for the whole sample grows with redshift as (1 + z)<SUP>m</SUP>,
where m = 2.83 +/- 0.33 in good agreement with N-body simulations
in a ΛCDM cosmology. We also separate the sample into two different
absolute magnitude bins: -25 <= M<SUB>R<SUB>c</SUB></SUB> <= -
21 and -21 < M<SUB>R<SUB>c</SUB></SUB> <= - 20, and find that the
brighter the absolute magnitude, the smaller the m-value. Furthermore,
we study the evolution of the pair fraction for different projected
separation bins and different luminosities. We find that the m-value
becomes smaller for larger separation, and the pair fraction for the
fainter luminosity bin has stronger evolution. We derive the major
merger remnant fraction f<SUB>rem</SUB> = 0.06, which implies that
about 6% of galaxies with -25 <= M<SUB>R<SUB>c</SUB></SUB> <=
- 20 have undergone major mergers since z = 0.8.
---------------------------------------------------------
Title: Observational Test of Coronal Magnetic Field
Models. I. Comparison with Potential Field Model
Authors: Liu, Yu; Lin, Haosheng
2008ApJ...680.1496L Altcode: 2007arXiv0710.3223L
Recent advances have made it possible to obtain two-dimensional
line-of-sight magnetic field maps of the solar corona from
spectropolarimetric observations of the Fe XIII 1075 nm forbidden
coronal emission line. Together with the linear polarization
measurements that map the azimuthal direction of the coronal magnetic
field projected in the plane of the sky containing Sun center,
these coronal vector magnetograms allow for direct and quantitative
observational testing of theoretical coronal magnetic field models. This
paper presents a study testing the validity of potential-field
coronal magnetic field models. We constructed a theoretical coronal
magnetic field model of active region AR 10582 observed by the SOLARC
coronagraph in 2004 by using a global potential field extrapolation
of the synoptic map of Carrington Rotation 2014. Synthesized linear
and circular polarization maps from thin layers of the coronal magnetic
field model above the active region along the line of sight are compared
with the observed maps. We found that the observed linear and circular
polarization signals are consistent with the synthesized ones from
layers located just above the sunspot of AR 10582 near the plane of
the sky containing the Sun center.
---------------------------------------------------------
Title: The Facility IR Spectropolarimeter for the Dunn Solar Telescope
Authors: Jaeggli, S. A.; Lin, H.; Mickey, D. L.; Kuhn, J. R.; Hegwer,
S. L.; Rimmele, T. R.; Penn, M. J.
2008AGUSMSH31A..11J Altcode:
The Facility IR Spectropolarimeter(FIRS) is a multi-slit
spectropolarimeter designed for the Dunn Solar Telescope (DST) at the
National Solar Observatory on Sacramento Peak (NSO/SP) in New Mexico to
study magnetism on the solar surface. The instrument samples adjacent
slices of the solar surface using four parallel slits to achieve high
cadence, diffraction-limited, precision imaging-spectropolarimetry. Due
to the versatile, multi-armed design of the spectrograph, up to
four spectral lines at visible and infrared wavelengths, covering
four different heights in the solar atmosphere, can be observed
simultaneously. In this poster-paper we will describe the design,
capabilities, and performance of the instrument.
---------------------------------------------------------
Title: Developmental Aspects of a Multi-Slit Spectro-Polarimeter
Authors: George, K.; Sankarasubramanian, R.; Bayanna, R.; Lin, H.;
Venkatakrishnan, P.
2008eic..work..515G Altcode:
We report the development aspects of an integral field unit,
multi-slit spectro-polarimeter (MSSP) optimized for optical to near
infrared regime, which can be used to derive simultaneous spectral
and vector magnetic field information at high spatial, spectral and
temporal resolution of any extended astronomical object like the Sun,
with limited spectral coverage of few Angstrom. The instrument will be
first developed and tested in laboratory which in a later stage will
be used as a focal plane instrument for the Multi Application Solar
Telescope (MAST). The major technological challenges involved in setting
up and calibration of the instrument are discussed. The scientific
motivation for the system is highlighted, with special emphasis on
science limitations imposed by similar existing instruments elsewhere.
---------------------------------------------------------
Title: The COronal Solar Magnetism Observatory
Authors: Burkepile, J.; Tomczyk, S.; Lin, H.; Zurbuchen, T.; Judge,
P.; Casini, R.
2007AGUFMSH53A1070B Altcode:
Measurements of coronal and chromospheric magnetic fields are
arguably the most important observables required for advances in
our understanding of the emergence of magnetic flux into the solar
atmosphere and the processes responsible for the production of solar
activity, coronal heating and coronal dynamics. The COronal Solar
Magnetism Observatory (COSMO) is a proposed ground-based suite of
instruments designed for routine study of coronal and chromospheric
magnetic fields and their environment. The facility consists of 3
instruments: 1) a meter-class aperture coronal magnetometer devoted
to obtaining the highest quality polarimetric data of forbidden lines
of Fe XIII 1074.7 and 1079.8 nm.; 2) a chromosphere and prominence
magnetometer devoted primarily to measurements of lines of helium
(D3, 1083 nm) and perhaps Halpha, that will provide full disk vector
magnetic field observations; 3) a white-light polarized-brightness (pB)
coronagraph that will observe down to 1.05 solar radii at very high
time cadence (15 seconds) at high signal-to-noise. This new facility
will be operated by the High Altitude Observatory of the National
Center for Atmospheric Research (HAO/NCAR) in collaboration with the
University of Hawaii and the University of Michigan. COSMO will enhance
the value of existing and new observatories on the ground (SOLIS, ATST,
and FASR) and in space (SOHO, TRACE, GOES, SOLAR-B, STEREO, SDO) by
providing unique and crucial observations of the global coronal and
chromospheric magnetic field and its evolution.
---------------------------------------------------------
Title: Commissioning of the Dual-Beam Imaging Polarimeter for the
University of Hawaii 88 inch Telescope
Authors: Masiero, Joseph; Hodapp, Klaus; Harrington, Dave; Lin,
Haosheng
2007PASP..119.1126M Altcode: 2007arXiv0708.1335M
In this paper we present the design, calibration method, and initial
results of the Dual-Beam Imaging Polarimeter (DBIP). This new instrument
is designed to measure the optical polarization properties of point
sources, in particular, Main Belt asteroids. This instrument interfaces
between the Tek 2048×2048 camera and the University of Hawaii's 88
inch telescope and is available for facility use. Using DBIP we are
able to measure linear polarization with a 1 σ Poisson signal noise of
0.03% per measurement and a systematic error of order 0.06%+/-0.02%. In
addition, we discuss measurements of the polarization of the asteroid
16 Psyche that were taken as part of the instrument commissioning. We
confirm Psyche's negative polarization of -1.037%+/-0.006% but find
no significant modulation of the signal with rotation above the 0.05%
polarization level.
---------------------------------------------------------
Title: Mees Imaging Solar Spectrometer
Authors: Lin, Haosheng; Li, J.; Kuhn, J. R.; Mickey, D.; Habbal,
S. R.; Jaeggli, S. S.
2007AAS...210.9215L Altcode: 2007BAAS...39R.210L
We propose the construction of a new instrument, the Mees Imaging Solar
Spectrometer (MISS), optimized for spectroscopic study of energetic
solar events such as filament eruptions and solar flares, and their
relationship to coronal mass ejections. MISS is a fiber-optics-based
imaging spectrograph. It will be able to perform simultaneous
spectroscopic observations of selected spectral lines and continuum
over an extended field with high spatial and spectral resolution
and high cadence. It will operate nominally in a low-resolution (20"
per pixel), full-disk patrol mode, and can be rapidly switched to a
high-resolution (1" per pixel) region-of-interest mode of observation
when energetic events are detected. Several spectral lines, from CaII
H & K to HeI 1083 nm can be recorded in rapid succession. These
advanced imaging spectroscopic capabilities make it an ideal instrument
for the study of the rapid change of the physical conditions of the
solar atmosphere during these energetic events.
---------------------------------------------------------
Title: Coronal Magnetic Field
Authors: Lin, Haosheng
2007AAS...210.5201L Altcode: 2007BAAS...39..164L
Centuries after the birth of modern solar astronomy, the Sun's corona
still keeps many of its secrets: How is it heated to a million-degree
temperature? How does it harbor the cool and dense prominence gas
amid the tenuous and hot atmosphere? How does it drive the energetic
events that eject particles into interplanetary space with speed
exceeding 1% of the speed of light? We have greatly improved our
knowledge of the solar corona with decades of space X-ray and EUV
coronal observations, and many theories and models were put forward to
address these problems. In our current understanding, magnetic fields
are undoubtedly the most important fields in the corona, shaping its
structure and driving its dynamics. It is clear that the resolution
of these important questions all hinge on a better understanding of
the organization, evolution, and interaction of the coronal magnetic
field. However, as the direct measurement of coronal magnetic field
is a very challenging observational problem, most of our theories and
models were not experimentally verified. Nevertheless, we have finally
overcome the experimental difficulties and can now directly measure
the coronal magnetic field with great accuracy. This new capability
can now be used to study the static magnetic structure of the corona,
and offers hope that we will, in the near future, be able to directly
observe the evolution of the coronal magnetic field of energetic solar
events. More importantly, it finally allows us to conduct vigorous
observational tests of our theories and models. In this lecture, I
will review current research activities related to the observation,
interpretation, and modeling of the coronal magnetic field, and discuss
how they can help us resolve some of the long standing mysteries of
the solar corona.
---------------------------------------------------------
Title: The Coronal Magnetic Field Measurements On April 7, 2004
Authors: Liu, Yu; Lin, H.
2007AAS...210.9105L Altcode: 2007BAAS...39..204L
The magnetic field measurements in the corona above two quiet, close
active regions NOAA 10581 and 10582 at the solar west limb were taken by
the new coronagraph SOLARC installed on Haleakala. Spatially resolved
measurements of line-of-sight magnetic field strength and transverse
magnetic field direction of the solar corona were obtained at the
wavelength of IR 1074.7 nm. In the two-dimensional coronal magnetogram
made from the circular polarization, the observations showed a magnetic
neutral line at a height of about 0.16 solar radii above the solar
limb. Signatures of the the van Vleck effect were also shown from
the linear polarization measurements. These new coronal data, for
the first time, direct observational tests for theoretical coronal
magnetic field models. In this paper, we present a study comparing
the observed coronal magnetic field structures with the theoretical
results derived from the global potential field model. One important
conclusion in the study is that the SOLARC observations should reveal
the local coronal structures above strong photospheric field regions,
since both the observed linear and circular polarization signals are
found to have a best consistence with the calculated results for a
100 Mm-thick coronal region along the line of sight above the sunspot
in NOAA 10582. The usefulness and limitations of the potential field
extrapolation and various linear and non-linear force-free field
extrapolation methods, as well as directions for a more sophisticated
modelling effort involving MHD simulations and forward modeling of
the polarization signals that take full account of atomic polarization
and radiative transfer effects will be further studied and discussed.
---------------------------------------------------------
Title: COSMO: The Coronal Solar Magnetism Observatory
Authors: Burkepile, Joan; Tomczyk, S.; Lin, H.; Zurbuchen, T.;
Casini, R.
2007AAS...210.2519B Altcode: 2007BAAS...39..134B
The COronal Solar Magnetism Observatory (COSMO) is a proposed
ground-based suite of instruments designed to study coronal magnetic
fields and their environment using the polarization of forbidden
emission lines in the infrared. Supporting instruments focus on
prominence and chromospheric magnetometry and imaging and the evolution
of the electron scattered corona (K-corona). COSMO will address
one of the least understood problems in Sun-Earth connections: the
coronal magnetic field using breakthrough techonologies that have been
successfully demonstrated with proof-of-concept instrumentation. We will
present information about COSMO and science results from the prototype
instruments, including the detection of Alfven waves in the corona.
---------------------------------------------------------
Title: The Coronal Solar Magnetic Observatory (COSMO)
Authors: Tomczyk, S.; Zurbuchen, T.; Kuhn, J.; Lin, H.; Judge, P.;
Burkepile, J.; Casini, R.
2006AGUFMSM12A..03T Altcode:
Measurement of magnetic fields in the corona is arguably the most
important observable required for advances in our understanding of
the emergence of magnetic flux into the solar atmosphere and the
processes responsible for the production of solar activity, coronal
heating and coronal dynamics. We discuss plans for the COronal Solar
Magnetic Observatory (COSMO), which is a proposed ground-based suite
of instruments designed to routinely study coronal magnetic fields and
their environment. The core of the facility includes a meter-class
coronagraph with instrumentation dedicated to measuring the coronal
magnetic field using the polarization of forbidden emission lines in
the infrared. Supporting instruments focus on prominence magnetometry
and the dynamics of the electron-scattered corona (K-corona) and
chromosphere. In addition to acquiring routine synoptic observations
of coronal magnetic fields, the COSMO project will include the
establishment of a community-based user advisory panel to accept
observational campaigns submitted by members of the scientific community
at-large. COSMO will enhance the value of existing and new observatories
on the ground (SOLIS, ATST, FASR) and in space (SOHO, TRACE, GOES,
Solar-B, STEREO and SDO) by providing unique and crucial observations
of the global coronal magnetic field and its evolution and dynamics.
---------------------------------------------------------
Title: Coronal Magnetic Field Measurements and Comparison with
Theoretical Model
Authors: Liu, Y.; Lin, H.
2006AGUFMSH23B0363L Altcode:
Spatially resolved measurements of line-of-sight magnetic field
strength and transverse magnetic field direction of the solar corona
were obtained with the new SOLARC coronagraph and an optical fiber
imaging spectropolarimeter. Observations of the corona above active
regions NOAA 0581 and 0582 showed a reversal in the direction of the
line-of-sight component of the coronal magnetic field at a height of
0.16 solar radii above the solar limb. The linear polarization map
also showed signatures of the van Vleck effect. These new data allow,
for the first time, direct observational tests of theoretical coronal
magnetic field models. In this paper, we present a study comparing
the observed coronal magnetic field structures with the theoretical
model derived from potential field extrapolation. The usefulness and
limitations of potential field extrapolation, as well as directions
for a more sophisticated modeling effort involving MHD simulations and
forward modeling of the polarization signals that take full account
of atomic polarization and radiative transfer effects will be discussed.
---------------------------------------------------------
Title: VisIRIS: a visible/IR imaging spectropolarimeter based on a
birefringent fiber-optic image slicer
Authors: Lin, HaoSheng; Versteegh, Alex
2006SPIE.6269E..0KL Altcode: 2006SPIE.6269E..18L
High-resolution imaging spectropolarimetry in the visible and infrared
wavelengths is the most effective and accurate observational diagnostic
tool for many astrophysical problems, but many among them also require
a spatially resolved two-dimensional field of view. However, it is
difficult to achieve simultaneous three-dimensional (x, y, and λ)
coverage using instruments with a conventional design. A conventional
spectrograph achieves three-dimensional coverage either by scanning a
tunable filter through the spectral window of interest, or by scanning
a diffraction-grating-based long-slit spectrograph through the target
region. Scanning in either spectral or spatial direction unavoidably
degrades the quality of the data, and is time consuming. This
paper describes a new visible/IR imaging spectropolarimeter
design based on a novel birefringent fiber-optic image slicer and
multiple-slit spectrograph. With this design, simultaneous 3-D imaging
spectropolarimetry of astronomical objects with a large field of view
and high spatial and spectral resolution can be achieved.
---------------------------------------------------------
Title: Site testing for the Advanced Technology Solar Telescope
Authors: Hill, F.; Beckers, J.; Brandt, P.; Briggs, J.; Brown, T.;
Brown, W.; Collados, M.; Denker, C.; Fletcher, S.; Hegwer, S.; Horst,
T.; Komsa, M.; Kuhn, J.; Lecinski, A.; Lin, H.; Oncley, S.; Penn,
M.; Radick, R.; Rimmele, T.; Socas-Navarro, H.; Streander, K.
2006SPIE.6267E..1TH Altcode: 2006SPIE.6267E..59H
The Advanced Solar Technology Telescope (ATST) is a 4-m solar telescope
being designed for high spatial, spectral and temporal resolution,
as well as IR and low-scattered light observations. The overall
limit of performance of the telescope is strongly influenced by the
qualities of the site at which it is located. Six sites were tested
with a seeing monitor and a sky brightness instrument for 1.5 to 2
years. The sites were Big Bear (California), Haleakala (Hawaii), La
Palma (Canary Islands, Spain), Panguitch Lake (Utah), Sacramento Peak
(New Mexico), and San Pedro Martir (Baja California, Mexico). In this
paper we will describe the methods and results of the site survey,
which chose Haleakala as the location of the ATST.
---------------------------------------------------------
Title: Using Imaging Infrared Coronal Spectropolarimetry to Measure
the Near-Sun Plasma
Authors: Kuhn, J.; Lin, H.; Arnaud, J.; Jaeggli, S.
2005AGUFMSH44A..08K Altcode:
A moderate aperture ground-based coronagraph and an imaging infrared
spectropolarimeter have provided our first direct longitudinal coronal
magnetograms. This talk will describe the advantages and subtleties of
these techniques for direct coronal magnetometry. We also summarize
some of the diagnostic potential of current and likely future IR
spectropolarimetric instruments (like the Advanced Technology Solar
Telescope) for measuring the properties of the near-solar plasma.
---------------------------------------------------------
Title: Solar Site Survey for the Advanced Technology Solar
Telescope. I. Analysis of the Seeing Data
Authors: Socas-Navarro, H.; Beckers, J.; Brandt, P.; Briggs, J.;
Brown, T.; Brown, W.; Collados, M.; Denker, C.; Fletcher, S.; Hegwer,
S.; Hill, F.; Horst, T.; Komsa, M.; Kuhn, J.; Lecinski, A.; Lin, H.;
Oncley, S.; Penn, M.; Rimmele, T.; Streander, K.
2005PASP..117.1296S Altcode: 2005astro.ph..8690S
The site survey for the Advanced Technology Solar Telescope concluded
recently after more than 2 years of data gathering and analysis. Six
locations, including lake, island, and continental sites, were
thoroughly probed for image quality and sky brightness. The present
paper describes the analysis methodology employed to determine the
height stratification of the atmospheric turbulence. This information
is crucial, because daytime seeing is often very different between the
actual telescope aperture (~30 m) and the ground. Two independent
inversion codes have been developed to simultaneously analyze
data from a scintillometer array and a solar differential image
monitor. We show here the results of applying them to a sample subset
of data from 2003 May that was used for testing. Both codes retrieve a
similar seeing stratification through the height range of interest. A
quantitative comparison between our analysis procedure and actual in
situ measurements confirms the validity of the inversions. The sample
data presented in this paper reveal a qualitatively different behavior
for the lake sites (dominated by high-altitude seeing) and the rest
(dominated by near-ground turbulence).
---------------------------------------------------------
Title: A Photometric Redshift Galaxy Catalog from the Red-Sequence
Cluster Survey
Authors: Hsieh, B. C.; Yee, H. K. C.; Lin, H.; Gladders, M. D.
2005ApJS..158..161H Altcode: 2005astro.ph..2157H
The Red-Sequence Cluster Survey (RCS) provides a large and deep
photometric catalog of galaxies in the z<SUP>'</SUP> and R<SUB>c</SUB>
bands for 90 deg<SUP>2</SUP> of sky, and supplemental V and B data
have been obtained for 33.6 deg<SUP>2</SUP>. We compile a photometric
redshift catalog from these four-band data by utilizing the empirical
quadratic polynomial photometric redshift fitting technique in
combination with CNOC2 and GOODS/HDF-N redshift data. The training
set includes 4924 spectral redshifts. The resulting catalog contains
more than one million galaxies with photometric redshifts <1.5
and R<SUB>c</SUB><24, giving an rms scatter σ(Δz)<0.06 within
the redshift range 0.2<z<0.5 and σ(Δz)<0.11 for galaxies
at 0.0<z<1.5. We describe the empirical quadratic polynomial
photometric redshift fitting technique that we use to determine the
relation between redshift and photometry. A kd-tree algorithm is used
to divide up our sample to improve the accuracy of our catalog. We
also present a method for estimating the photometric redshift error
for individual galaxies. We show that the redshift distribution of
our sample is in excellent agreement with smaller and much deeper
photometric and spectroscopic redshift surveys.
---------------------------------------------------------
Title: The ATST Site Survey
Authors: Hill, F.; Beckers, J.; Brandt, P.; Briggs, J. W.; Brown, T.;
Brown, W.; Collados, M.; Denker, C.; Fletcher, S.; Hegwer, S.; Horst,
T.; Komsa, M.; Kuhn, J.; Lecinski, A.; Lin, H.; Oncley, S.; Penn, M.;
Radick, R.; Rimmele, T.; Socas-Navarro, H.; Soltau, D.; Streander, K.
2005AGUSMSP34A..04H Altcode:
The Advanced Technology Solar Telescope (ATST) will be the world's
largest aperture solar telescope, and is being designed for high
resolution, IR, and coronal research. It must be located at a site that
maximizes the scientific return of this substantial investment. We
present the instrumentation, analysis and results of the ATST site
survey. Two instrumentation sets were deployed at each of six sites to
measure seeing as a function of height, and sky brightness as a function
of wavelength and off-limb position. Analysis software was developed
to estimate the structure function Cn2 as a function of height near
the ground, and the results were verified by comparison with in-situ
measurements. Additional software was developed to estimate the sky
brightness. The statistics of the conditions at the sites were corrected
for observing habits and the annualized hours of specific observing
conditions were estimated. These results were used to identify three
excellent sites suitable to host the ATST: Haleakala, Big Bear and La
Palma. Among them, Haleakala is proposed as the optimal location of
the ATST, La Palma and Big Bear being viable alternative sites.
---------------------------------------------------------
Title: First-Light Instrumentation for the Advanced Technology
Solar Telescope
Authors: Rimmele, T.; Balasubramaniam, K.; Berger, T.; Elmore, D.;
Gary, A.; Keller, C.; Kuhn, J.; Lin, H.; Mickey, D.; Pevtsov, A.;
Robinson, B.; Sigwarth, M.; Soccas-Navarro, H.
2005AGUSMSP34A..03R Altcode:
The 4m Advanced Technology Solar Telescope (ATST) is the next
generation ground based solar telescope. In this paper we provide
an overview of the ATST post-focus instrumentation. The majority of
ATST instrumentation is located in an instrument Coude lab facility,
where a rotating platform provides image de-rotation. A high order
adaptive optics system delivers a corrected beam to the Coude lab
facility. Alternatively, instruments can be mounted at the Nasmyth
focus. For example, instruments for observing the faint corona
preferably will be mounted at Nasmyth where maximum throughput
is achieved. In addition, the Nasmyth focus has minimum telescope
polarization and minimum stray light. We give an overview of the
initial set of first generation instruments: the Visible-Light
Broadband Imager (VLBI), the Visible Spectro-Polarimeter (ViSP),
the Near-IR Spectro-Polarimeter (NIRSP), which includes a coronal
module, and the Visible Tunable Filter. We also discuss the unique and
efficient approach to the ATST instrumentation, which builds on the use
of common components such as detector systems, polarimetry packages
and various opto-mechanical components. For example, the science
requirement for polarimetric sensitivity (10-5 relative to intensity)
and accuracy (5'10-4 relative to intensity) place strong constraints
on the polarization analysis and calibration units. Consequently,
these systems are provided at the facility level, rather than making
it part of the requirement for each instrument.
---------------------------------------------------------
Title: Coronal Magnetic Field Measurements
Authors: Lin, H.; Kuhn, J. R.; Coulter, R.
2004ApJ...613L.177L Altcode:
A long-standing solar problem has been to measure the coronal magnetic
field. We believe it determines the coronal structure and dynamics from
the upper chromosphere out into the heliospheric environment. It is only
recently that Zeeman splitting observations of infrared coronal emission
lines have been successfully used to deduce the coronal magnetic flux
density. Here we extend this technique and report first results from a
novel coronal magnetometer that uses an off-axis reflecting coronagraph
and optical fiber-bundle imaging spectropolarimeter. We determine the
line-of-sight magnetic flux density and transverse field orientation
in a two-dimensional map with a sensitivity of about 1 G with 20"
spatial resolution after 70 minutes of integration. These full-Stokes
spectropolarimetric measurements of the forbidden Fe XIII 1075 nm
coronal emission line reveal the line-of-sight coronal magnetic field
100" above an active region to have a flux density of about 4 G.
---------------------------------------------------------
Title: Solar site testing for the Advanced Technology Solar Telescope
Authors: Hill, Frank; Beckers, Jacques; Brandt, Peter; Briggs, John;
Brown, Timothy; Brown, W.; Collados, Manuel; Denker, Carsten; Fletcher,
Steven; Hegwer, Steven; Horst, T.; Komsa, Mark; Kuhn, Jeff; Lecinski,
Alice; Lin, Haosheng; Oncley, Steve; Penn, Matthew; Rimmele, Thomas
R.; Socas-Navarro, Hector; Streander, Kim
2004SPIE.5489..122H Altcode:
The location of the Advanced Technology Solar Telescope (ATST) is a
critical factor in the overall performance of the telescope. We have
developed a set of instrumentation to measure daytime seeing, sky
brightness, cloud cover, water vapor, dust levels, and weather. The
instruments have been located at six sites for periods of one to two
years. Here we describe the sites and instrumentation, discuss the
data reduction, and present some preliminary results. We demonstrate
that it is possible to estimate seeing as a function of height near the
ground with an array of scintillometers, and that there is a distinct
qualitative difference in daytime seeing between sites with or without
a nearby lake.
---------------------------------------------------------
Title: Instrumentation for the Advanced Technology Solar Telescope
Authors: Rimmele, Thomas R.; Hubbard, Robert P.; Balasubramaniam,
K. S.; Berger, Tom; Elmore, David; Gary, G. Allen; Jennings, Don;
Keller, Christoph; Kuhn, Jeff; Lin, Haosheng; Mickey, Don; Moretto,
Gilberto; Socas-Navarro, Hector; Stenflo, Jan O.; Wang, Haimin
2004SPIE.5492..944R Altcode:
The 4-m aperture Advanced Technology Solar Telescope (ATST) is the
next generation ground based solar telescope. In this paper we provide
an overview of the ATST post-focus instrumentation. The majority of
ATST instrumentation is located in an instrument Coude lab facility,
where a rotating platform provides image de-rotation. A high order
adaptive optics system delivers a corrected beam to the Coude lab
facility. Alternatively, instruments can be mounted at Nasmyth or
a small Gregorian area. For example, instruments for observing the
faint corona preferably will be mounted at Nasmyth focus where maximum
throughput is achieved. In addition, the Nasmyth focus has minimum
telescope polarization and minimum stray light. We describe the set of
first generation instruments, which include a Visible-Light Broadband
Imager (VLBI), Visible and Near-Infrared (NIR) Spectropolarimeters,
Visible and NIR Tunable Filters, a Thermal-Infrared Polarimeter &
Spectrometer and a UV-Polarimeter. We also discuss unique and efficient
approaches to the ATST instrumentation, which builds on the use of
common components such as detector systems, polarimetry packages and
various opto-mechanical components.
---------------------------------------------------------
Title: The Advanced Technology Solar Telescope Site Survey Sky
Brightness Monitor
Authors: Lin, Haosheng; Penn, Matthew J.
2004PASP..116..652L Altcode:
The Advanced Technology Solar Telescope (ATST) will be a 4 m aperture
off-axis telescope with advanced high-resolution and low scattered
light capabilities for the observation of the solar photosphere and
corona. The site characteristics that are critical to the success of
the ATST coronal observations are the sky brightness, the precipitable
water vapor content, and the number and size distributions of the
dust particles. Therefore, part of the ATST site survey effort is
to obtain measurements of these atmospheric properties at all the
potential ATST sites. The ATST site survey Sky Brightness Monitor (SBM)
is a new instrument specifically developed for this task. The SBM is a
modified externally occulted coronagraph capable of imaging the solar
disk and sky simultaneously. The ability to image the Sun and the sky
simultaneously greatly simplifies the calibration of the sky-brightness
measurements. The SBM has a very simple optical configuration that makes
it a compact and low-maintenance instrument. The SBM is sensitive to sky
brightness below 1×10<SUP>-6</SUP> disk center intensity, with a field
of view extending from 4 to 8 R<SUB>solar</SUB>. It measures the solar
disk and sky brightness at three continuum bandpasses located at 450,
530, and 890 nm. A fourth bandpass is centered at the 940 nm water vapor
absorption band. With measurements of disk and sky brightness at these
four wavelengths, site characteristics such as extinctions, aerosol
content, and precipitable water vapor content can be derived. This
paper documents the design, specifications, calibration procedures,
and performance of the SBM.
---------------------------------------------------------
Title: Background-Induced Measurement Errors of the Coronal Intensity,
Density, Velocity, and Magnetic Field
Authors: Penn, M. J.; Lin, H.; Tomczyk, S.; Elmore, D.; Judge, P.
2004SoPh..222...61P Altcode:
The effect of a background signal on the signal-to-noise ratio is
discussed, with particular application to ground-based observations of
emission lines in the solar corona with the proposed Advanced Technology
Solar Telescope. The concepts of effective coronal aperture and
effective coronal integration time are introduced. Specific expressions
are developed for the 1σ measurement errors for coronal intensity,
coronal electron density, coronal velocity, and coronal magnetic field
measurements using emission lines and including a background.
---------------------------------------------------------
Title: Latest Results from the ATST Site Survey
Authors: Hill, F.; Collados, M.; Navarro, H.; Beckers, J.; Brandt,
P.; Briggs, J.; Brown, T.; Denker, C.; Hegwer, S.; Horst, T.; Komsa,
M.; Kuhn, J.; Lin, H.; Oncley, S.; Penn, M.; Rimmele, T.; Soltau,
D.; Streander, K.
2004AAS...204.6909H Altcode: 2004BAAS...36..795H
We present the latest results and current status of the site survey
portion of the Advanced Technology Solar Telescope (ATST) project. The
ATST will provide high resolution solar data in the visible and IR. The
site is a major factor determining the performance of the telescope. The
most critical site characteristics are the statistics of daytime seeing
quality and sky clarity. These conditions are being measured by a suite
of instruments at three sites (Big Bear, Haleakala, La Palma). These
sites were chosen from a set of six that have been tested starting in
November 2001. The instrumentation includes a solar differential image
motion monitor, an array of scintillometers, a miniature coronagraph,
a dust monitor, and a weather station. The analysis of the data provides
an estimate of the seeing as a function of height near the ground. We
will present the latest results of the analysis of the survey data set.
---------------------------------------------------------
Title: Title Requested
Authors: Lin, H.; Kuhn, J. R.; Coulter, R.
2004AAS...204.9807L Altcode: 2004BAAS...36Q.985L
A critical problem for understanding the solar corona has been
to measure its magnetic field that we believe determines its
structure and dynamics from the upper chromosphere out into the
heliospheric environment. The direct measurement of this field has
been a longstanding problem. Only recently have Zeeman splitting
observations of infrared coronal emission lines (Lin et al. 2000) been
used to deduce the coronal magnetic flux density. We have extended
this technique and report here our first results from a novel coronal
magnetometer that uses an off-axis reflecting coronagraph (SOLARC) and
optical fiber-bundle imaging spectropolarimeter (OFIS). Our results
reveal the line-of-sight magnetic flux density with a sensitivity of
a few gauss with 20 arcsec spatial resolution and approximately 60min
temporal resolution. These full Stokes spectropolarimetric data of
the forbidden FeXIII emission line at 1075nm imply a line-of-sight
coronal magnetic field above an active region with a flux density of
9G. Although these first results from SOLARC/OFIS have relatively coarse
resolution, they have potential for solving our coronal "dark energy"
problem with infrared magnetometry. This research has been supported by
the Multidisciplinary University Research Initiative (MURI) of the DOD,
NASA, and the National Science Foundation Atmospheric Research Program.
---------------------------------------------------------
Title: Extinction and Sky Brightness at Two Solar Observatories
Authors: Penn, M. J.; Lin, H.; Schmidt, A. M.; Gerke, J.; Hill, F.
2004SoPh..220..107P Altcode:
The Advanced Technology Solar Telescope site survey Sky Brightness
Monitor simultaneously images the solar disk and the sky to about
8 solar radii in four wavelengths at 450, 530, 890 and 940 nm. One
day of data from Mees Solar Observatory on Haleakala and from the
National Solar Observatory at Sacramento Peak (Sunspot, New Mexico)
are analyzed. Both sites show strong Rayleigh extinction, but while
Haleakala shows a larger aerosol component, Sunspot shows a large
variation in the aerosol component. Overall the Haleakala extinction
varies as λ<SUP>−2</SUP> whereas the Sunspot extinction changes
from about λ<SUP>−3.5</SUP> to about λ<SUP>−2</SUP>, suggesting
an increasing aerosol component during the day. Water vapor absorption
measurements from both sites are similar, though Sunspot shows larger
time variations than Haleakala. The instrument-corrected sky brightness
from both sites show comparable values, and again the Sunspot data show
more variations. The sky brightness values show a radial dependence
of sky brightness of r<SUP>−0.1</SUP> at Haleakala, but a dependence
of r<SUP>−1.0</SUP> at Sunspot. The wavelength variation of the sky
brightness at Haleakala is relatively constant at λ<SUP>−1.5</SUP>
but varies at Sunspot from λ<SUP>−1.5</SUP> to λ<SUP>−0.1</SUP>
again suggesting an increasing aerosol contribution during the day
at Sunspot. Finally, dust measurements near the ground are compared
with the extinction wavelength exponent for data taken at Haleakala
on 24 Feb. 2003. The measurements suggest more large dust particles
are present near the ground than averaged over the whole air column.
---------------------------------------------------------
Title: Measuring Coronal Magnetic Fields with Coronal Emission
Line Polarimetry
Authors: Lin, H.
2003AGUFMSH42D..02L Altcode:
Magnetic field is the dominating field in the solar corona, responsible
for the majestic coronal structures and dynamic events. However,
no direct measurements of the coronal magnetic fields are routinely
available and we can only infer the coronal magnetic field structures
from observed intensity images. Although several methods for the
diagnostics of coronal magnetic fields have been demonstrated,
measurement of the coronal magnetic fields remains a very challenging
observational task. This paper reports on a concerted effort at the
Institute for Astronomy (IfA) to establish routine vector coronal
magnetic field measurement capabilities using spectropolarimetric
observation of the near infrared Fe XIII 1074.7 nm coronal emission
line. The IfA effort includes observations of two-dimensional circular
polarization maps of the emission line which carry information about
the coronal magnetic field strength. High resolution observation
of the linear polarization maps which yield the projected direction
of the coronal magnetic field in the plane of the sky will also be
obtained. The latest results from these experiments will be presented.
---------------------------------------------------------
Title: ATST near-IR spectropolarimeter
Authors: Lin, Haosheng
2003SPIE.4853..215L Altcode:
The development of new solar IR instrumentation in the past decade
had opened new windows of opportunity for solar physics research
which were not accessible before. Many spectral lines in the near-IR
wavelength range from 1 to 2 microns offer powerful diagnostics for
the study of solar magnetism in the photosphere, the chromosphere,
and the corona. Significant progress and breakthroughs were made
in areas such as the generation of weak background magnetic fields
by small-scale surface dynamos, the physics of the sunspot, and the
direct measurement of magnetic fields in the corona. The combination of
these new IR diagnostics tools, and the unprecedented 4-meter aperture
and versatile photospheric and coronal capabilities of the Advanced
Technology Solar Telescope (ATST), will greatly enhance our capability
to study the Sun. It further promises breakthrough observations that
can help to resolve many of the long-standing mysteries of solar
physics. The instruments for the ATST will need to accommodate a
broad range of science subjects, each with its unique observational
requirements. This paper examine the near-IR instrumentation required
to achieve the ATST science goals, and present conceptual designs
of a near-IR SpectroPolarimeter (NIRSP) aimed at addressing the new
challenges of observational solar physics brought upon by the ATST.
---------------------------------------------------------
Title: Strategies for prime focus instrumentation in off-axis
Gregorian systems
Authors: Coulter, Roy; Kuhn, Jeff R.; Lin, Haosheng
2003SPIE.4853..558C Altcode:
A new generation of off-axis telescopes has been proposed to address
a number of high dynamic range problems in astrophysics. These
systems present unusual problems and opportunities for the instrument
designer. We will discuss some of the issues that must be resolved
when placing instrumentation at the prime focus. The heat stop and
occulter systems for the SOLARC off-axis coronagraph will be used to
illustrate strategies for solar telescope applications.
---------------------------------------------------------
Title: The SOLARC off-axis coronagraph
Authors: Kuhn, Jeff R.; Coulter, Roy; Lin, Haosheng; Mickey, Donald L.
2003SPIE.4853..318K Altcode:
A 0.5m aperture off-axis coronagraphic telescope is described. Its
fabrication, imaging, and scattered light performance is discussed in
the context of simple model expectations.
---------------------------------------------------------
Title: Near-infrared chromospheric observatory
Authors: Labonte, Barry; Rust, David M.; Bernasconi, Pietro N.;
Georgoulis, Manolis K.; Fox, Nicola J.; Kalkofen, Wolfgang; Lin,
Haosheng
2003SPIE.4853..140L Altcode:
NICO, the Near Infrared Chromosphere Observatory, is a platform for
determining the magnetic structure and fources of heating for the
solar chromosphere. NICO, a balloon-borne observatory, will use the
largest solar telescope flying to map the magnetic fields, velocities,
and heating events of the chromosphere and photosphere in detail. NICO
will introduce new technologies to solar flight missions, such as
wavefront sensing for monitoring telescope alignment, real-time
correlation tracking and high-speed image motion compensation, and
wide aperture Fabry-Perot etalons for extended spectral scanning.
---------------------------------------------------------
Title: The Near-Infrared Chromosphere Observatory (NICO)
Authors: Rust, D. M.; Bernasconi, P. N.; LaBonte, B. J.; Georgoulis,
M. K.; Kalkofen, W.; Fox, N. J.; Lin, H.
2002AAS...200.3902R Altcode: 2002BAAS...34..701R
NICO is a proposed cost-effective platform for determining the magnetic
structure and sources of heating for the solar chromosphere. It is a
balloon-borne observatory that will use the largest solar telescope
flying and very high data rates to map the magnetic fields, velocities,
and heating events of the chromosphere and photosphere in unprecedented
detail. NICO is based on the Flare Genesis Experiment (FGE), which
has pioneered in the application of technologies important to NASA's
flight program. NICO will also introduce new technologies, such
as wavefront sensing for monitoring telescope alignment; real-time
correlation tracking and high-speed image motion compensation for
smear-free imaging; and wide aperture Fabry-Perot filters for extended
spectral scanning. The telescope is a classic Cassegrain design with
an 80-cm diameter F/1.5 primary mirror made of Ultra-Low-Expansion
glass. The telescope structure is graphite-epoxy for lightweight,
temperature-insensitive support. The primary and secondary mirror
surfaces are coated with silver to reflect more than 97% of the incident
solar energy. The secondary is made of single-crystal silicon, which
provides excellent thermal conduction from the mirror surface to its
mount, with negligible thermal distortion. A third mirror acts as a
heat dump. It passes the light from a 15-mm diameter aperture in its
center, corresponding to a 322"-diameter circle on the solar surface,
while the rest of the solar radiation is reflected back out of the
front of the telescope. The telescope supplies the selected segment
of the solar image to a polarization and spectral analysis package
that operates with an image cadence 1 filtergram/sec. On-board data
storage is 3.2 Terabytes. Quick-look images will be sent in near real
time to the ground via the TDRSS communications link.
---------------------------------------------------------
Title: Near Infrared Magnetometry in the Photosphere and Corona
Authors: Lin, H.
2002AAS...200.3404L Altcode: 2002BAAS...34..690L
The interplay between the magnetic fields and the highly conductive
plasma in the atmosphere of the sun generates some of the most
fascinating and puzzling astronomical phenomena known to the
mankind. Because of its proximity to the earth, these solar activities
also have profound effect on life on earth. Therefore, understanding
solar magnetism is not only an intellectual inquiry of the curious
minds, it is also an endeavor to better the human life. The near
infrared wavelength regime between 1 to 2 microns contains many
spectral lines with powerful diagnostics capability for the study of
solar magnetic fields. These spectral lines offer enhanced magnetic
sensitivity in both the photosphere and corona, which not only allows
us to explore regions of the solar atmosphere not easily accessible by
other diagnostics, in many cases, it also provides critical measurements
to distinguish competing models, and therefore, advances our knowledge
of the sun. While the potential of the near-IR tools for the study
of solar magnetism was well recognized by the pioneers of the field
many decades ago, realization of some of their capabilities was
achieved only recently, due to the advance of the IR array detector
technology. In this talk, we will first review past achievements and
the current status of the near-IR solar physics research. Of course,
the excitement of the field is in the future challenges and progress
we are going to face and achieve with the Advanced Technology Solar
Telescope (ATST). Therefore, we will also discuss the scientific goals
of the ATST and present ideas on how to achieve these goals.
---------------------------------------------------------
Title: A Classical Model for the Damped, Magnetic Dipole Oscillator
Authors: Casini, Roberto; Lin, Haosheng
2002ApJ...571..540C Altcode:
We propose a simple classical model for the damped, magnetic dipole
oscillator based on a circuit analogy. The solution for the dynamical
equation of the associated magnetic moment is found to be similar
in form to the well-known solution for the damped, electric dipole
oscillator, but with the magnetic vector of the incident electromagnetic
wave as the forcing field, instead of the electric vector. This
model has been successfully applied to a classical derivation of the
polarization properties of the forbidden (M1) coronal emission lines.
---------------------------------------------------------
Title: Dynamically Close Galaxy Pairs and Merger Rate Evolution in
the CNOC2 Redshift Survey
Authors: Patton, D. R.; Pritchet, C. J.; Carlberg, R. G.; Marzke,
R. O.; Yee, H. K. C.; Hall, P. B.; Lin, H.; Morris, S. L.; Sawicki,
M.; Shepherd, C. W.; Wirth, G. D.
2002ApJ...565..208P Altcode: 2001astro.ph..9428P
We investigate redshift evolution in the galaxy merger and
accretion rates, using a well-defined sample of 4184 galaxies with
0.12<=z<=0.55 and R<SUB>C</SUB><=21.5. We identify 88 galaxies
in close (5<=r<SUB>p</SUB><=20 h<SUP>-1</SUP> kpc) dynamical
(Δv<=500 km s<SUP>-1</SUP>) pairs. These galaxies are used to
compute global pair statistics, after accounting for selection effects
resulting from the flux limit, k-corrections, luminosity evolution, and
spectroscopic incompleteness. We find that the number of companions
per galaxy (for -21<=M<SUP>k,e</SUP><SUB>B</SUB><=-18) is
N<SUB>c</SUB>=0.0321+/-0.0077 at z=0.3. The luminosity in companions,
per galaxy, is L<SUB>c</SUB>=0.0294+/-0.0084×10<SUP>10</SUP>
h<SUP>2</SUP> L<SUB>solar</SUB>. We assume that N<SUB>c</SUB>
is proportional to the galaxy merger rate, while L<SUB>c</SUB>
is directly related to the mass accretion rate. After increasing
the maximum pair separation to 50 h<SUP>-1</SUP> kpc and comparing
with the low-redshift SSRS2 pair sample, we infer evolution in the
galaxy merger and accretion rates of (1+z)<SUP>2.3+/-0.7</SUP> and
(1+z)<SUP>2.3+/-0.9</SUP>, respectively. These are the first such
estimates to be made using only confirmed dynamical pairs. When combined
with several additional assumptions, this implies that approximately
15% of present epoch galaxies with -21<=M<SUB>B</SUB><=-18 have
undergone a major merger since z=1.
---------------------------------------------------------
Title: Environment and Galaxy Evolution at Intermediate Redshift in
the CNOC2 Survey
Authors: Carlberg, R. G.; Yee, H. K. C.; Morris, S. L.; Lin, H.;
Hall, P. B.; Patton, D. R.; Sawicki, M.; Shepherd, C. W.
2001ApJ...563..736C Altcode: 2001astro.ph..6506C
The systematic variation of galaxy colors and types with clustering
environment could either be the result of local conditions at formation
or subsequent environmental effects as larger scale structures draw
together galaxies whose stellar mass is largely in place. Below redshift
0.7 galaxy luminosities (k-corrected and evolution compensated) are
relatively invariant, whereas galaxy star formation rates, as reflected
in their colors, are a “transient” property that have a wide range
for a given luminosity. The relations between these galaxy properties
and the clustering properties are key statistics for understanding the
forces driving late-time galaxy evolution. At z~0.4 the comoving galaxy
correlation length, r<SUB>0</SUB>, measured in the CNOC2 sample is
strongly color dependent, rising from 2 h<SUP>-1</SUP> Mpc to nearly
10 h<SUP>-1</SUP> Mpc as the volume-limited subsamples range from
blue to red. The luminosity dependence of r<SUB>0</SUB> at z~0.4 is
weak below L<SUB>*</SUB> in the R band, although there is an upturn at
high luminosity, where its interpretation depends on separating it from
the r<SUB>0</SUB>-color relation. In the B band there is a slow, smooth
increase of r<SUB>0</SUB> with luminosity, at least partially related to
the color dependence. Study of the evolution of galaxies within groups,
which create much of the strongly nonlinear correlation signal, allows
a physical investigation of the source of these relations. The dominant
effect of the group environment on star formation is seen in the radial
gradient of the mean galaxy colors, which on the average become redder
than the field toward the group centers. The color differentiation
begins around the dynamical radius of virialization of the groups. The
redder-than-field trend applies to groups with a line-of-sight velocity
dispersion, σ<SUB>1</SUB>>150 km s<SUP>-1</SUP>. There is an
indication, somewhat statistically insecure, that the high-luminosity
galaxies in groups with σ<SUB>1</SUB><125 km s<SUP>-1</SUP> become
bluer toward the group center. Monte Carlo orbit integrations initiated
at the measured positions and velocities show that the rate of galaxy
merging in the σ<SUB>1</SUB>>150 km s<SUP>-1</SUP> groups is very
low, whereas for σ<SUB>1</SUB><150 km s<SUP>-1</SUP> about 25%
of the galaxies will merge in 0.5 Gyr. We conclude that the higher
velocity dispersion groups largely act to suppress star formation
relative to the less clustered field, leading to “embalmed”
galaxies. On the other hand, the low velocity dispersion groups are
prime sites of both strong merging and enhanced star formation that
leads to the formation of some new massive galaxies at intermediate
redshifts. The tidal fields within the groups appear to be a strong
candidate for the physical source of the reduction of star formation
in group galaxies relative to field. Tides operate effectively at all
velocity dispersions to remove gas-rich companions and low-density gas
in galactic halos. We find a close resemblance of the color-dependent
galaxy luminosity function evolution in the field and groups, suggesting
that the clustering-dependent star formation reduction mechanism is
important for the evolution of field galaxies as a whole.
---------------------------------------------------------
Title: The Galaxy Correlation Function in the CNOC2 Redshift Survey:
Dependence on Color, Luminosity, and Redshift
Authors: Shepherd, C. W.; Carlberg, R. G.; Yee, H. K. C.; Morris,
S. L.; Lin, H.; Sawicki, M.; Hall, P. B.; Patton, D. R.
2001ApJ...560...72S Altcode: 2001astro.ph..6250S
We examine how the spatial correlation function of galaxies from the
Canadian Network for Observational Cosmology Field Galaxy Redshift
Survey (CNOC2) depends on galaxy color, luminosity, and redshift. The
projected correlation function w<SUB>p</SUB> is determined for
volume-limited samples of objects with 0.12<=z<0.51 and
evolution-compensated R<SUB>C</SUB>-band absolute magnitudes
M<SUP>0</SUP><SUB>R</SUB><-20, over the comoving projected
separation range 0.04 h<SUP>-1</SUP> Mpc<r<SUB>p</SUB><10
h<SUP>-1</SUP> Mpc. Our sample consists of 2937 galaxies that are
classified as being either early- or late-type objects according
to their spectral energy distribution (SED), as determined from
UBVR<SUB>C</SUB>I<SUB>C</SUB> photometry. For the sake of simplicity,
galaxy SEDs are classified independently of redshift: Our classification
scheme therefore does not take into account the color evolution of
galaxies. Objects with SEDs corresponding to early-type galaxies
are found to be more strongly clustered by a factor of ~3 and
to have a steeper correlation function than those with late-type
SEDs. Modeling the spatial correlation function, as a function of
comoving separation r, as ξ(r)=(r/r<SUB>0</SUB>)<SUP>-γ</SUP>, we
find r<SUB>0</SUB>=5.45+/-0.28 h<SUP>-1</SUP> Mpc and γ=1.91+/-0.06
for early-type objects, and r<SUB>0</SUB>=3.95+/-0.12 h<SUP>-1</SUP>
Mpc and γ=1.59+/-0.08 for late-type objects (for Ω<SUB>M</SUB>=0.2,
Ω<SUB>Λ</SUB>=0). While changing the cutoff between early-
and late-type SEDs does affect the correlation amplitudes of
the two samples, the ratio of the amplitudes remains constant to
within 10%. The redshift dependence of the correlation function
also depends on SED type. Modeling the redshift dependence of
the comoving correlation amplitude r<SUP>γ</SUP><SUB>0</SUB> as
r<SUP>γ</SUP><SUB>0</SUB>(z)~(1+z)<SUP>γ-3-ɛ</SUP>, we find that
early-type objects have ɛ=-3.9+/-1.0, and late-type objects have
ɛ=-7.7+/-1.3. Both classes of objects therefore have clustering
amplitudes, measured in comoving coordinates, which appear to decrease
rapidly with cosmic time. The excess clustering of galaxies with
early-type SEDs, relative to late-type objects, is present at all
redshifts in our sample. In contrast to the early- and late-type SED
samples, the combined sample undergoes little apparent evolution,
with ɛ=-2.1+/-1.3, which is consistent with earlier results. The
apparent increase with redshift of the clustering amplitude in
the early- and late-type samples is almost certainly caused by
evolution of the galaxies themselves rather than by evolution of
the correlation function. If galaxy SEDs have evolved significantly
since z~0.5, then our method of classifying SEDs may cause us to
overestimate the true evolution of the clustering amplitude for the
unevolved counterparts to our early- and late-type samples. However,
if color evolution is to explain the apparent clustering evolution,
the color evolution experienced by a galaxy must be correlated with
the galaxy correlation function. We also investigate the luminosity
dependence of the correlation function for volume-limited samples with
0.12<=z<0.40 and M<SUP>0</SUP><SUB>R</SUB><-19.25. We detect
a weak luminosity dependence of the correlation amplitude for galaxies
with early-type SEDs, dlogξ/dM<SUP>0</SUP><SUB>R</SUB>=-0.35+/-0.17,
but no significant dependence for late-type objects,
dlogξ/dM<SUP>0</SUP><SUB>R</SUB>=0.02+/-0.16.
---------------------------------------------------------
Title: Galaxy Groups at Intermediate Redshift
Authors: Carlberg, R. G.; Yee, H. K. C.; Morris, S. L.; Lin, H.;
Hall, P. B.; Patton, D. R.; Sawicki, M.; Shepherd, C. W.
2001ApJ...552..427C Altcode: 2000astro.ph..8201C
Galaxy groups likely to be virialized are identified within
the CNOC2 intermediate-redshift galaxy survey. The resulting
groups have a median velocity dispersion, σ<SUB>1</SUB>~=200 km
s<SUP>-1</SUP>. The virial mass-to-light ratios, using k-corrected
and evolution-compensated luminosities, have medians in the range of
150-250 h M<SUB>solar</SUB>/L<SUB>solar</SUB>, depending on group
definition details. The number-velocity dispersion relation at
σ<SUB>1</SUB>>~200 km s<SUP>-1</SUP> is in agreement with the
low-mass extrapolation of the cluster-normalized Press-Schechter
model. Lower velocity dispersion groups are deficient relative to
the Press-Schechter model. The two-point group-group autocorrelation
function has r<SUB>0</SUB>=6.8+/-0.3 h<SUP>-1</SUP> Mpc, which
is much larger than the correlations of individual galaxies, but
about as expected from biased clustering. The mean number density
of galaxies around group centers falls nearly as a power law with
r<SUP>-2.5</SUP> and has no well-defined core. The projected velocity
dispersion of galaxies around group centers is either flat or slowly
rising outward. The combination of a steeper than isothermal density
profile and the outward rising velocity dispersion implies that
the mass-to-light ratio of groups rises with radius if the velocity
ellipsoid is isotropic but could be nearly constant if the galaxy
orbits are nearly circular. Such strong tangential anisotropy is not
supported by other evidence. Although the implication of a rising M/L
must be viewed with caution, it could naturally arise through dynamical
friction acting on the galaxies in a background of “classical”
collisionless dark matter.
---------------------------------------------------------
Title: Weak-Lensing Study of Low-Mass Galaxy Groups: Implications
for Ω<SUB>m</SUB>
Authors: Hoekstra, H.; Franx, M.; Kuijken, K.; Carlberg, R. G.; Yee,
H. K. C.; Lin, H.; Morris, S. L.; Hall, P. B.; Patton, D. R.; Sawicki,
M.; Wirth, G. D.
2001ApJ...548L...5H Altcode: 2000astro.ph.12169H
We report on the first measurement of the average mass and mass-to-light
ratio of galaxy groups by analyzing the weak-lensing signal induced by
these systems. The groups, which have velocity dispersions of 50-400
km s<SUP>-1</SUP>, have been selected from the Canadian Network for
Observational Cosmology Field Galaxy Redshift Survey (CNOC2). This
survey allows the identification of a large number of groups with
redshifts ranging from z=0.12 to 0.55, ideal for a weak-lensing analysis
of their mass distribution. For our analysis we use a sample of 50
groups that are selected on the basis of a careful dynamical analysis of
group candidates. We detect a signal at the 99% confidence limit. The
best-fit singular isothermal sphere model yields an Einstein radius
r<SUB>E</SUB>=0.72"+/-0.29". This corresponds to a velocity dispersion
of <σ<SUP>2</SUP>><SUP>1/2</SUP>=274<SUP>+48</SUP><SUB>-
59</SUB> km s<SUP>-1</SUP> (using photometric redshift distributions
for the source galaxies), which is in good agreement with the
dynamical estimate. Under the assumption that the light traces
the mass, we find an average mass-to-light ratio of 191+/-83 h
M<SUB>solar</SUB>/L<SUB>Bsolar</SUB> in the rest-frame B band. Unlike
dynamical estimates, this result is insensitive to problems associated
with determining group membership. After correction of the observed
mass-to-light ratio for luminosity evolution to z=0, we find 254+/-110 h
M<SUB>solar</SUB>/L<SUB>Bsolar</SUB>, lower than what is found for rich
clusters. We use the observed mass-to-light ratio to estimate the matter
density of the universe, for which we find Ω<SUB>m</SUB>=0.19+/-0.10
(Ω<SUB>Λ</SUB>=0), in good agreement with other recent estimates. For
a closed universe (Ω<SUB>m</SUB>+Ω<SUB>Λ</SUB>=1), we obtain
Ω<SUB>m</SUB>=0.13+/-0.07. Based on observations made with the William
Herschel Telescope operated on the island of La Palma by the Isaac
Newton Group in the Spanish Observatorio del Roque de los Muchachos
of the Instituto de Astrofisica de Canarias.
---------------------------------------------------------
Title: The Evolution of Population Gradients in Galaxy Clusters:
The Butcher-Oemler Effect and Cluster Infall
Authors: Ellingson, E.; Lin, H.; Yee, H. K. C.; Carlberg, R. G.
2001ApJ...547..609E Altcode: 2000astro.ph.10141E
We present photometric and spectroscopic measurements of the galaxy
populations in clusters from the CNOC1 sample of rich, X-ray-luminous
clusters at 0.18<z<0.55. A classical measure of the galaxy
blue fraction for spectroscopically confirmed cluster members shows
a significant Butcher-Oemler effect for the sample, but only when
radii larger than 0.5r<SUB>200</SUB> are considered. We perform a
principal component analysis of galaxy spectra to divide the total
cluster light into contributions from stellar populations of different
ages. Composite radial distributions of different stellar populations
show strong gradients as a function of clustercentric radius. The
composite population is dominated by evolved populations in the core,
and gradually changes at radii greater than the virial radius to one
which is similar to coeval field galaxies. We do not see evidence at
any radius within the clusters for an excess of star formation over
that seen in the coeval field. Within this redshift range, significant
evolution in the fractional population gradient is seen. Both low-
and high-redshift clusters have similar populations in the cluster
cores, but higher redshift clusters have steeper gradients and more
star-forming galaxies at radii outside of the core region-in effect,
a restatement of the Butcher-Oemler effect. Luminosity density profiles
are consistent with a scenario where this phenomenon is due to a decline
over time in the infall rate of field galaxies into clusters. Depending
on how long galaxies reside in clusters before their star formation
rates are diminished, this suggests a decrease in the infall into
clusters of a factor of ~3 between z>0.8 and z~0.5. We also discuss
alternative scenarios for the evolution of cluster populations.
---------------------------------------------------------
Title: Data From the Precision Solar Photometric Telescope (Pspt)
in Hawaii From March 1998 to March 1999
Authors: White, Oran R.; Fox, Peter A.; Meisner, Randy; Rast, Mark
P.; Yasukawa, Eric; Koon, Darryl; Rice, Crystal; Lin, Haosheng; Kuhn,
Jeff; Coulter, Roy
2000SSRv...94...75W Altcode:
Two Precision Solar Photometric Telescopes (PSPT) designed and built at
the U.S. National Solar Observatory (NSO) are in operation in Rome and
Hawaii. A third PSPT is now in operation the NSO at Sunspot, NM. The
PSPT system records full disk solar images at three wavelengths:
K line at 393.3 nm and two continua at 409 nm and 607 nm throughout
the observing day. We currently study properties of limb darkening,
sunspots, and network in these images with particular emphasis on data
taken in July and September 1998. During this period, the number of
observations per month was high enough to show directional properties
of the radiation field surrounding sunspots. We show examples of our
PSPT images and describe our study of bright rings around sunspots.
---------------------------------------------------------
Title: Galaxy Clustering Evolution in the CNOC2 High-Luminosity Sample
Authors: Carlberg, R. G.; Yee, H. K. C.; Morris, S. L.; Lin, H.;
Hall, P. B.; Patton, D.; Sawicki, M.; Shepherd, C. W.
2000ApJ...542...57C Altcode: 1999astro.ph.10250C
The redshift evolution of the galaxy two-point correlation function
is a fundamental cosmological statistic. To identify similar galaxy
populations at different redshifts, we select a strict volume-limited
sample culled from the 6100 cataloged Canadian Network for Observational
Cosmology field galaxy redshift survey (CNOC2) galaxies. Our
high-luminosity subsample selects galaxies having k-corrected and
evolution-compensated R luminosities, M<SUP>k,e</SUP><SUB>R</SUB>,
above -20 mag (H<SUB>0</SUB>=100 km s<SUP>-1</SUP> Mpc<SUP>-1 </SUP>),
where M<SUP>k,e</SUP><SUB>*</SUB>(R)~=-20.3 mag. This subsample contains
about 2300 galaxies distributed between redshifts 0.1 and 0.65 spread
over a total of 1.55 deg<SUP>2</SUP> of sky. A similarly defined
low-redshift sample is drawn from the Las Campanas Redshift Survey. We
find that the comoving two-point correlation function can be described
as ξ(r|z)=(r<SUB>00</SUB>/r)<SUP>γ</SUP>(1+z)<SUP>-(3+ɛ- γ)</SUP>,
with r<SUB>00</SUB>=5.03+/-0.08 h<SUP>-1</SUP> Mpc, ɛ=-0.17+/-0.18,
and γ=1.87+/-0.07 over the z=0.03-0.65 redshift range, for
Ω<SUB>M</SUB>=0.2 and Λ=0. The measured clustering amplitude and its
evolution are dependent on the adopted cosmology. The measured evolution
rates for Ω<SUB>M</SUB>=1 and flat Ω<SUB>M</SUB>=0.2 background
cosmologies are ɛ=0.80+/-0.22 and ɛ=-0.81+/-0.19, respectively,
with r<SUB>00</SUB>=5.30+/-0.1 and 4.85+/-0.1 h<SUP>-1</SUP>
Mpc, respectively. The sensitivity of the derived correlations
to the evolution corrections and details of the measurements is
presented. The analytic prediction of biased clustering evolution for
only the low-density, ΛCDM cosmology is readily consistent with the
observations, with biased clustering in an open cosmology somewhat
marginally excluded and a biased Ω<SUB>M</SUB>=1 model predicting
clustering evolution that is more than 6 standard deviations from the
measured value.
---------------------------------------------------------
Title: The CNOC2 Field Galaxy Redshift Survey. I. The Survey and
the Catalog for the Patch CNOC 0223+00
Authors: Yee, H. K. C.; Morris, S. L.; Lin, H.; Carlberg, R. G.; Hall,
P. B.; Sawicki, Marcin; Patton, D. R.; Wirth, G. D.; Ellingson, E.;
Shepherd, C. W.
2000ApJS..129..475Y Altcode: 2000astro.ph..4026Y
The Canadian Network for Observational Cosmology (CNOC2) Field Galaxy
Redshift Survey is a spectroscopic/photometric survey of faint galaxies
over 1.5 deg<SUP>2</SUP> of sky with a nominal spectroscopic limit
of R<SUB>C</SUB>~21.5 mag. The primary goals of the survey are to
investigate the evolution of galaxy clustering and galaxy populations
over the redshift range of ~0.1-0.6. The survey area contains four
widely separated patches on the sky with a total sample of over 6000
redshifts, representing a sampling rate of about 45%. In addition,
five-color photometry (in I<SUB>C</SUB>, R<SUB>C</SUB>, V, B, and U) for
a complete sample of approximately 40,000 galaxies to R<SUB>C</SUB>~23.0
mag is also available. We describe the survey and observational
strategies, multiobject spectroscopy mask design procedure, and data
reduction techniques for creating the spectroscopic-photometric
catalogs. We also discuss the derivations of statistical weights,
including corrections for the effects of limited spectral bandwidth,
for the redshift sample, which allow it to be used as a complete
sample. As the initial release of the survey data, we present the full
data set and some statistics for the patch CNOC 0223+00.
---------------------------------------------------------
Title: Caltech Faint Galaxy Redshift Survey. XI. The Merger Rate to
Redshift 1 from Kinematic Pairs
Authors: Carlberg, R. G.; Cohen, Judith G.; Patton, D. R.; Blandford,
Roger; Hogg, David W.; Yee, H. K. C.; Morris, S. L.; Lin, H.; Hall,
Patrick B.; Sawicki, M.; Wirth, Gregory D.; Cowie, Lennox L.; Hu,
Esther; Songaila, Antoinette
2000ApJ...532L...1C Altcode: 2000astro.ph..2036C
The rate of mass accumulation due to galaxy merging depends on the mass,
density, and velocity distribution of galaxies in the near neighborhood
of a host galaxy. The fractional luminosity in kinematic pairs
combines all of these effects in a single estimator that is relatively
insensitive to population evolution. Here we use a k-corrected and
evolution-compensated volume-limited sample having an R-band absolute
magnitude of M<SUP>k,e</SUP><SUB>R</SUB><=-19.8+5logh mag drawing
about 300 redshifts from the Caltech Faint Galaxy Redshift Survey and
3000 from the Canadian Network for Observational Cosmology field galaxy
survey to measure the rate and redshift evolution of merging. The
combined sample has an approximately constant comoving number and
luminosity density from redshift 0.1 to 1.1 (Ω<SUB>M</SUB>=0.2,
Ω<SUB>Λ</SUB>=0.8) hence, any merger evolution will be dominated by
correlation and velocity evolution, not density evolution. We identify
kinematic pairs with projected separations less than either 50 or
100 h<SUP>-1</SUP> kpc and rest-frame velocity differences of less
than 1000 km s<SUP>-1</SUP>. The fractional luminosity in pairs is
modeled as f<SUB>L</SUB>(Δv,r<SUB>p</SUB>,M<SUP>k,e</SUP><SUB>r</SUB>)
(1+z)<SUP>m<SUB>L</SUB></SUP>, where [f<SUB>L</SUB>,m<SUB>L</SUB>]
are [0.14+/-0.07,0+/-1.4] and [0.37+/-0.7,0.1+/-0.5] for
r<SUB>p</SUB><=50 and 100 h<SUP>-1</SUP> kpc, respectively
(Ω<SUB>M</SUB>=0.2, Ω<SUB>Λ</SUB>=0.8). The value of m<SUB>L</SUB>
is about 0.6 larger if Λ=0. To convert these redshift-space
statistics to a merger rate, we use the data to derive a conversion
factor to a physical space pair density, a merger probability,
and a mean in-spiral time. The resulting mass accretion rate
per galaxy (M<SUB>1</SUB>,M<SUB>2</SUB>>=0.2M<SUB>*</SUB>)
is 0.02+/-0.01(1+z)<SUP>0.1+/-0.5</SUP>M<SUB>*</SUB>
Gyr<SUP>-1</SUP>. Present-day high-luminosity galaxies therefore
have accreted approximately 0.15M<SUB>*</SUB> of their mass over
the approximately 7 Gyr to redshift 1. Since merging is likely
only weakly dependent on the host mass, the fractional effect,
δM/M~=0.15M<SUB>*</SUB>/M, is dramatic for lower mass galaxies
but is, on the average, effectively perturbative for galaxies above
1M<SUB>*</SUB>.
---------------------------------------------------------
Title: Probable Detection of a Bright Infrared Coronal Emission Line
of Si IX near 3.93 Microns
Authors: Kuhn, J. R.; MacQueen, R. M.; Streete, J.; Tansey, G.; Mann,
I.; Hillebrand, P.; Coulter, R.; Lin, H.; Edmunds, D.; Judge, P.
1999ApJ...521..478K Altcode:
We report here the probable detection of an emission line of Si
IX that was observed from an open C130 aircraft over the Pacific
Ocean during the 1998 total solar eclipse. Although the IR data
themselves are inconclusive because of the uncertainty in the precise
central wavelengths of the narrowband filters during the eclipse,
the consistency of the measured IR limb excess with simultaneous EUV
emission measured by SOHO/Coronal Diagnostic Spectrometer and the EUV
Imager Telescope support our detection claim. This line appears to
be the brightest IR coronal line yet observed, and its existence may
significantly improve future prospects for obtaining optical coronal
magnetic field measurements.
---------------------------------------------------------
Title: The Ω<SUB>M</SUB>-Ω<SUB>Λ</SUB> Dependence of the Apparent
Cluster Ω
Authors: Carlberg, R. G.; Yee, H. K. C.; Morris, S. L.; Lin, H.;
Ellingson, E.; Patton, D.; Sawicki, M.; Shepherd, C. W.
1999ApJ...516..552C Altcode:
The Canadian Network for Observational Cosmology cluster data are used
to constrain the Ω<SUB>M</SUB>-Ω<SUB>Λ</SUB> pair to the region
Ω<SUB>M</SUB>~=0.24e<SUP>+/-0.3</SUP>(1-0.4Ω<SUB>Λ</SUB>) for
0<=Ω<SUB>Λ</SUB><=1. The constraint is based on estimating the
apparent mass density of the universe, Ω<SUB>e</SUB>(z), as the product
of cluster mass-to-light ratios, M/L, with the field luminosity density
at the same redshift. The luminosity density contains a volume element,
which for measurements at z>0 causes Ω<SUB>e</SUB>(z) to depend on
both the density parameter Ω<SUB>M</SUB> and the cosmological constant,
Ω<SUB>Λ</SUB>. The Ω<SUB>Λ</SUB>-dependence of the Ω<SUB>e</SUB>(z)
measurement is about 25% less than the volume-redshift relation but
about 50% greater than the luminosity-redshift relation. Most usefully
this constraint is approximately orthogonal to the luminosity-redshift
relation in the Ω<SUB>M</SUB>-Ω<SUB>Λ</SUB> plane. The practical
application to measuring cosmological parameters has the considerable
benefit that all quantities are used in a differential sense, so
that common selection effects and galaxy evolution effects will
cancel. The residual differential galaxy evolution between field,
and the clustered galaxies can be estimated from the sample data. The
inferred Ω<SUB>M</SUB> has an inverse correlation with Ω<SUB>Λ</SUB>,
giving a constraint complementary to both the cosmic microwave
background and the supernovae distances. Monte Carlo simulations,
calibrated with observational data, show that 100 clusters spread over
the 0-1 redshift range, each having M/L values of about 25% accuracy,
will measure Ω<SUB>Λ</SUB> to about 7% statistical error.
---------------------------------------------------------
Title: Evolution of Galaxy Correlations
Authors: Carlberg, R. G.; Yee, H. K. C.; Morris, S. L.; Lin, H.;
Sawicki, M.; Wirth, G.; Patton, D.; Shepherd, C. W.; Ellingson, E.;
Schade, D.; Pritchet, C. J.; Hartwick, F. D. A.
1998wfsc.conf..143C Altcode:
The CNOC field galaxy redshift survey, CNOC2, investigates the relations
between the dramatic evolution of field galaxies and their clustering
over the redshift range 0 to 0.7. We report preliminary results based
on two of the sky patches and within the redshift range of 0.12 to
0.55. The spatial two point correlation functions have a strong colour
dependence with scale, and a weaker, apparently scale free, luminosity
dependence. The population most likely to be conserved with redshift
is the high luminosity galaxies. In particular, we choose galaxies
with M_r^{k,e} <= -20 mag as our tracer population. We find that
the evolution of the clustered density in proper co-ordinates at r ls
10hmpc, rho<SUB>gg</SUB> propto r_0(z)^gamma(1+z)^3, where r_0(z) is
the proper correlation length, is best described as a "de-clustering",
propto (1+z)^{0.6 +- 0.4}. Or equivalently, there is a weak growth of
clustering in co-moving co-ordinates, x_0 propto (1+z)^{-0.3 +- 0.2}.
---------------------------------------------------------
Title: The Luminosity Function of Field Galaxies in the CNOC1
Redshift Survey
Authors: Lin, H.; Yee, H. K. C.; Carlberg, R. G.; Ellingson, E.
1997ApJ...475..494L Altcode: 1996astro.ph..8056L
We have computed the luminosity function for a sample of 389 field
galaxies from the Canadian Network for Observational Cosmology
cluster redshift survey (CNOC1) over the redshift range z =
0.2-0.6. We find Schechter parameters M<SUP>*</SUP><SUB>r</SUB>-5
log h = -20.8 +/- 0.4 and α = -1.3 +/- 0.2 in rest-frame Gunn r, and
M<SUP>*</SUP><SUB>B<SUB>AB</SUB></SUB>- 5 log h = -19.6 +/- 0.3 and
α = -0.9 +/- 0.2 in rest-frame B<SUB>AB</SUB>. We have also split
our sample at the color of a redshifted but nonevolving Sbc galaxy
and find distinctly different luminosity functions for red and blue
galaxies. Red galaxies have a shallow slope α ~ -0.4 and dominate
the bright end of the luminosity function, while blue galaxies have a
steep α ~ -1.4 and prevail at the faint end. Comparisons of the CNOC1
results to analogous intermediate-redshift luminosity functions from the
Canada-France (CFRS) and Autofib redshift surveys show broad agreement
among these independent samples, but there are also significant
differences which will require larger samples to resolve. Also, in
CNOC1 the red galaxy luminosity density stays about the same over the
range z = 0.2-0.6, while the blue galaxy luminosity density increases
steadily with redshift. These results are consistent with the trend
of the luminosity density versus redshift relations seen in the CFRS,
although the normalizations of the luminosity densities appear to
differ for blue galaxies. Comparison to the local luminosity function
from the Las Campanas redshift survey (LCRS) shows that the luminosity
density at z ~ 0.1 is only about half that seen at z ~ 0.4. A change in
the luminosity function shape, particularly at the faint end, appears
to be required to match the CNOC1 and LCRS luminosity functions, if
galaxy evolution is the sole cause of the differences seen. However,
it should be noted that the specific details of the construction of
different surveys may complicate the comparison of results and so may
need to be considered carefully.
