Author name code: brown-tim
ADS astronomy entries on 2022-09-14
=author:"Brown, T.M." OR =author:"Brown, Timothy M." OR =author:"Brown, Timothy" OR =author:"Brown, Tim" 
------------------------------------------------------------------------  

Title: VizieR Online Data Catalog: HST stellar photometry of Eridanus
    II (Simon+, 2021)
Authors: Simon, J. D.; Brown, T. M.; Drlica-Wagner, A.; Li, T. S.;
   Avila, R. J.; Bechtol, K.; Clementini, G.; Crnojevic, D.; Garofalo,
   A.; Geha, M.; Sand, D. J.; Strader, J.; Willman, B.
Bibcode: 2022yCat..19080018S
Altcode:
  We observed EriII with the Wide Field Channel of the Advanced Camera for
  Surveys (ACS) on Hubble Space Telescope (HST) through program GO-14234
  (PI:Simon). The observations were scheduled over seven visits between
  2016 January 16 and 2016 February 8. We devoted four visits (8 orbits)
  to imaging in the F814W filter, totaling 20680s. The remaining three
  visits (two visits of two orbits each and one single-orbit visit)
  were used to image EriII in the F606W filter, totaling 12830s. <P />(1
  data file).

Title: VizieR Online Data Catalog: AMIGA: The Circumgalactic Medium
    of Andromeda (Lehner+, 2020)
Authors: Lehner, N.; Berek, S. C.; Howk, J. C.; Wakker, B. P.;
   Tumlinson, J.; Jenkins, E. B.; Prochaska, J. X.; Augustin, R.; Ji,
   S.; Faucher-Giguere, C. -A.; Hafen, Z.; Peeples, M. S.; Barger, K. A.;
   Berg, M. A.; Bordoloi, R.; Brown, T. M.; Fox, A. J.; Gilbert, K. M.;
   Guhathakurta, P.; Kalirai, J. S.; Lockman, F. J.; O'Meara, J. M.;
   Pisano, D. J.; Ribaudo, J.; Werk, J. K.
Bibcode: 2021yCat..19000009L
Altcode:
  With Project Absorption Maps In the Gas of Andromeda (AMIGA), we have
  surveyed the circumgalactic medium (CGM) of a single galaxy (M31) with
  an unprecedented number of background targets (43). The 43 QSOs were
  all observed with Hubble Space Telescope/Cosmic Origins Spectrograph
  (HST/COS) G130M/G160M or G130M (providing in particular OI, CII, CIV,
  SiII, SiIII, and SiIV), and 11 were also observed with Far Ultraviolet
  Spectroscopic Explorer (FUSE) (providing OVI). The resolution of the
  COS G130M/G160M and the S/Ns have been key for the success of this
  program. <P />(6 data files).

Title: GF-GMD/gmtb-scm: GF-GMD/SCM & forcing data
Authors: Grantfirl; Heinzeller, Dom; DomHeinzeller; Pegion, Phil;
   Carson, Laurie; Brown, Timothy; Tanyasmirnova
Bibcode: 2021zndo...5292370G
Altcode:
  GMTB Single Column Model

Title: Brightness Fluctuation Spectra of Sun-like Stars. I. The
    Mid-frequency Continuum
Authors: Brown, Timothy M.; García, Rafael A.; Mathur, Savita;
   Metcalfe, Travis S.; Santos, Ângela R. G.
Bibcode: 2021ApJ...916...66B
Altcode: 2021arXiv210512231B
  We analyze space-based time-series photometry of Sun-like stars, mostly
  in the Pleiades, but also field stars and the Sun itself. We focus
  on timescales between roughly 1 hr and 1 day. In the corresponding
  frequency band these stars display brightness fluctuations with a
  decreasing power-law continuous spectrum. K2 and Kepler observations
  show that the rms flicker due to this mid-frequency continuum (MFC)
  can reach almost 1%, approaching the modulation amplitude from active
  regions. The MFC amplitude varies by a factor up to 40 among Pleiades
  members with similar T<SUB>eff</SUB>, depending mainly on the stellar
  Rossby number Ro. For Ro ≤ 0.04, the mean amplitude is roughly
  constant at about 0.4%; at larger Ro the amplitude decreases rapidly,
  shrinking by about two orders of magnitude for Ro ≃ 1. Among stars,
  the MFC amplitude correlates poorly with that of modulation from
  rotating active regions. Among field stars observed for 3 yr by Kepler,
  the quarterly average modulation amplitudes from active regions are
  much more time variable than the quarterly MFC amplitudes. We argue
  that the process causing the MFC is largely magnetic in nature and
  that its power-law spectrum comes from magnetic processes distinct
  from the star's global dynamo, with shorter timescales. By analogy with
  solar phenomena, we hypothesize that the MFC arises from a (sometimes
  energetic) variant of the solar magnetic network, perhaps combined
  with rotation-related changes in the morphology of supergranules.

Title: TOI-1830 and TOI-1312: Two EBs hosting very low-mass stellar
    companions in eccentric orbits
Authors: Rabus, Markus; Carmichael, Theron W.; Shporer, Avi; Johnson,
   Marshall; Latham, David W.; Brown, Tim; Gan, Tianjun; Collins, Karen
   A.; Barkaoui, Khalid; Bieryla, Allyson; Kielkopf, John F.; Gonzalez,
   Erica J.; Addison, Brett C.; Henriksen, Andreea I.; Buchhave, Lars;
   Rasmussen, René Tronsgaard; Astudillo-Defru, Nicola; Fulton, Benjamin;
   Howell, Steve B.; Ciardi, David; Hellier, Coel; Ghachoui, Mourad;
   Timmermans, Mathilde
Bibcode: 2021tsc2.confE.179R
Altcode:
  &lt;strong&gt;We describe in the underlying investigation the
  discovery of two eclipsing binary systems. In both cases, the
  companions are most likely fully convective low-mass stars. The TESS
  team initially alerted the systems as TOI-1830 (TIC20182165, HD133725)
  and TOI-1312 (TIC405904232), and we subsequently observed them with
  spectroscopy. The TESS light curves and spectroscopic observations were
  analyzed in a combined data-driven framework to estimate the systems'
  parameters. Radial velocity (RV) measurements with LCO/NRES, NOT/FIES,
  SONG, and TRES indicated for the TOI-1830 system a companion mass of
  0.11 M⊙ in a 9.781-day eccentric orbit and a 0.10 M⊙ companion in an
  11.080-day eccentric orbit for the TOI-1312 system. At the same time,
  the spectroscopic observations were used to estimate the spectral
  type of the main stars for TOI-1830 and TOI-1312. We measured the
  radii ratio from the TESS light curves and estimated the companions'
  radii, assuming the main stars' radii as measured from spectroscopy and
  isochrones. Given the youth of TOI-1830 and the evolved age of TOI-1312,
  both systems will provide valuable insights into the stellar evolution
  of close binary systems.&lt;/strong&gt;

Title: LCO Key Project: Standing on the shoulders of the network -
    Follow-up of TESS planet candidates with LCO
Authors: Shporer, Avi; Collins, Karen; Johnson, Marshall; Armstrong,
   James; Brown, Tim; Conti, Dennis; Fulton, Ben; Gan, Tianjun; Keith,
   Horne; Jensen, Eric; Jontof-Hutter, Daniel; Kielkopf, John; Latham,
   Dave; Mao, Shude; Massey, Bob; Mazeh, Tsevi; Murgas, Felipe; Narita,
   Norio; Palle, Enric; Rabus, Markus; Schwarz, Richard; Sefako,
   Ramatholo; Shahaf, Sahar; Siverd, Rob; Srdoc, Gregor; Stockdale, Chris
Bibcode: 2021tsc2.confE.136S
Altcode:
  Accomplishing the exoplanet science enabled by TESS requires follow-up
  of many transiting planet candidates throughout the entire sky, to
  identify false positives (FPs) and confirm real planets. An efficient
  follow-up requires a global facility and a large amount of telescope
  time. This Las Cumbres Observatory (LCO) Key Project is designed to do
  just that, with about 2,500 hours of telescope time per semester for 6
  semesters, 2020B - 2023A. LCO telescopes are fully automated, including
  10 x 0.4m, 11 x 1.0m, and 2 x 2.0m telescopes in 7 sites. We are using
  all LCO telescopes, equipped with imagers, and we also have time on
  the high resolution NRES spectrographs, installed in 4 sites. Imagers
  are used to observe the TESS candidates during transit and check if
  the transit signal seen in TESS data originates from the target or
  from a nearby star blended with the target in the TESS wide pixels and
  wide PSF. The NRES spectrographs are used for measuring the stellar
  parameters of bright TESS candidate host stars down to 10th magnitude,
  identifying obvious FPs (SB1, SB2), and measuring the orbits of massive
  planets. This Key Project is part of most TESS planet discoveries. We
  present our methodologies and some of our discoveries.

Title: VizieR Online Data Catalog: Internal kinematics of 9 globular
    clusters with HST (Cohen+, 2021)
Authors: Cohen, R. E.; Bellini, A.; Libralato, M.; Correnti, M.;
   Brown, T. M.; Kalirai, J. S.
Bibcode: 2021yCat..51610041C
Altcode:
  We have obtained second-epoch photometry of all nine of these clusters,
  between 2003 July and 2019 August, with the Advanced Camera for
  Surveys/Wide Field Camera (ACS/WFC) onboard Hubble Space Telescope (HST)
  in the F606W and F814W filters (GO-15065, PI:Cohen). <P />(1 data file).

Title: VulcanClimateModeling/fv3gfs-fortran: GMD release
Authors: Heinzeller, Dom; Underwood, Seth; DomHeinzeller; Grantfirl;
   Wang, Jun; Liang, Zhi; Menzel-Gfdl; Robinson, Tom; Brown, Timothy;
   Bensonr; Hartnett, Ed; JulieSchramm; Uramirez8707; Gbw-Gfdl; Carson,
   Laurie; McGibbon, Jeremy; Fuhrer, Oliver; Jess; Clark, Spencer;
   Tanyasmirnova; Hallberg, Robert; Ligiabernardet; Potts, Mark; Zadeh,
   Niki; Olson, Joseph; Jovic, Dusan; Rheacangeo; Fabienpaulot; Goldy;
   Haiqinli
Bibcode: 2021zndo...4470023H
Altcode:
  Code used in preparation of submission of manuscript on fv3gfs-wrapper
  to GMD.

Title: VizieR Online Data Catalog: Optical photometry and RVs of
    TOI-481b and TOI-892b (Brahm+, 2020)
Authors: Brahm, R.; Nielsen, L. D.; Wittenmyer, R. A.; Wang, S.;
   Rodriguez, J. E.; Espinoza, N.; Jones, M. I.; Jordan, A.; Henning,
   T.; Hobson, M.; Kossakowski, D.; Rojas, F.; Sarkis, P.; Schlecker, M.;
   Trifonov, T.; Shahaf, S.; Ricker, G.; Vanderspek, R.; Latham, D. W.;
   Seager, S.; Winn, J. N.; Jenkins, J. M.; Addison, B. C.; Bakos, G. A.;
   Bhatti, W.; Bayliss, D.; Berlind, P.; Bieryla, A.; Bouchy, F.; Bowler,
   B. P.; Briceno, C.; Brown, T. M.; Bryant, E. M.; Caldwell, D. A.;
   Charbonneau, D.; Collins, K. A.; Davis, A. B.; Esquerdo, G. A.; Fulton,
   B. J.; Guerrero, N. M.; Henze, C. E.; Hogan, A.; Horner, J.; Huang,
   C. X.; Irwin, J.; Kane, S. R.; Kielkopf, J.; Mann, A. W.; Mazeh, T.;
   McCormac, J.; McCully, C.; Mengel, M. W.; Mireles, I.; Okumura, J.;
   Plavchan, P.; Quinn, S. N.; Rabus, M.; Saesen, S.; Schlieder, J. E.;
   Segransan, D.; Shiao, B.; Shporer, A.; Siverd, R. J.; Stassun, K. G.;
   Suc, V.; Tan, T. -G.; Torres, P.; Tinney, C. G.; Udry, S.; Vanzi,
   L.; Vezie, M.; Vines, J. I.; Vuckovic, M.; Wright, D. J.; Yahalomi,
   D. A.; Zapata, A.; Zhang, H.; Ziegler, C.
Bibcode: 2021yCat..51600235B
Altcode:
  TOI-481 and TOI-892 were monitored by Transiting Exoplanet Survey
  Satellite (TESS) during its first year of operation. TOI-481 was
  observed in short-cadence (2minutes) mode in Sectors 6, 7, 9, 10,
  and 13, and in long-cadence (30minutes) mode in Sector 3. On the
  other hand, TOI-892 was only observed in Sector 6, in long-cadence
  mode. <P />TOI-481 and TOI-892 were monitored with seven different
  spectrographs with the goal of measuring radial velocity variations
  to confirm the planetary nature of the transiting candidates
  and constrain their orbital parameters and masses. The Fiber-fed
  Extended Range Optical Spectrograph (FEROS) has a resolving power of
  R=48000 and is installed on the Max Planck Gesellschaft (MPG) 2.2 m
  telescope at La Silla Observatory in Chile. The CHIRON instrument is
  a high-resolution (R=80000) and fiber-fed spectrograph mounted on the
  1.5m Smarts telescope at the Cerro Tololo Inter-American Observatory
  (CTIO), Chile. The Tillinghast Reflector Echelle Spectrograph (TRES)
  is a R=44000 fiber-fed instrument mounted on the 1.5m Tillinghast
  Reflector at the Fred L. Whipple Observatory (FLWO) on Mt. Hopkins,
  Arizona. CORALIE is a high-resolution (R=60000) fiber-fed spectrograph
  mounted on the 1.2m Swiss Euler telescope at La Silla Observatory,
  Chile. Minerva-Australis is an array of four PlaneWave CDK700
  telescopes which can be simultaneously fiber-fed to a single KiwiSpec
  R4-100 high-resolution (R=80000) spectrograph. TOI-481 was monitored
  by Minerva-Australis using one and/or two telescopes in the array
  Minerva3 and Minerva4. Las Cumbres Observatory's Network of Robotic
  Echelle Spectrographs (NRES) is a global array of echelle spectrographs
  mounted on 1 m telescopes, with a resolving power of R~53000. <P />(2
  data files).

Title: TOI-481 b and TOI-892 b: Two Long-period Hot Jupiters from
    the Transiting Exoplanet Survey Satellite
Authors: Brahm, Rafael; Nielsen, Louise D.; Wittenmyer, Robert A.;
   Wang, Songhu; Rodriguez, Joseph E.; Espinoza, Néstor; Jones, Matías
   I.; Jordán, Andrés; Henning, Thomas; Hobson, Melissa; Kossakowski,
   Diana; Rojas, Felipe; Sarkis, Paula; Schlecker, Martin; Trifonov,
   Trifon; Shahaf, Sahar; Ricker, George; Vanderspek, Roland; Latham,
   David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Addison,
   Brett C.; Bakos, Gáspár Á.; Bhatti, Waqas; Bayliss, Daniel;
   Berlind, Perry; Bieryla, Allyson; Bouchy, Francois; Bowler, Brendan
   P.; Briceño, César; Brown, Timothy M.; Bryant, Edward M.; Caldwell,
   Douglas A.; Charbonneau, David; Collins, Karen A.; Davis, Allen B.;
   Esquerdo, Gilbert A.; Fulton, Benjamin J.; Guerrero, Natalia M.; Henze,
   Christopher E.; Hogan, Aleisha; Horner, Jonathan; Huang, Chelsea X.;
   Irwin, Jonathan; Kane, Stephen R.; Kielkopf, John; Mann, Andrew W.;
   Mazeh, Tsevi; McCormac, James; McCully, Curtis; Mengel, Matthew W.;
   Mireles, Ismael; Okumura, Jack; Plavchan, Peter; Quinn, Samuel N.;
   Rabus, Markus; Saesen, Sophie; Schlieder, Joshua E.; Segransan, Damien;
   Shiao, Bernie; Shporer, Avi; Siverd, Robert J.; Stassun, Keivan G.;
   Suc, Vincent; Tan, Thiam-Guan; Torres, Pascal; Tinney, Chris G.; Udry,
   Stephane; Vanzi, Leonardo; Vezie, Michael; Vines, Jose I.; Vuckovic,
   Maja; Wright, Duncan J.; Yahalomi, Daniel A.; Zapata, Abner; Zhang,
   Hui; Ziegler, Carl
Bibcode: 2020AJ....160..235B
Altcode: 2020arXiv200908881B
  We present the discovery of two new 10 day period giant planets from
  the Transiting Exoplanet Survey Satellite mission, whose masses
  were precisely determined using a wide diversity of ground-based
  facilities. TOI-481 b and TOI-892 b have similar radii (0.99 ± 0.01
  ${R}_{{\rm{J}}}$ and 1.07 ± 0.02 ${R}_{{\rm{J}}}$ , respectively),
  and orbital periods (10.3311 days and 10.6266 days, respectively),
  but significantly different masses (1.53 ± 0.03 ${M}_{{\rm{J}}}$
  versus 0.95 ± 0.07 ${M}_{{\rm{J}}}$ , respectively). Both planets
  orbit metal-rich stars ( $[\mathrm{Fe}/{\rm{H}}]$ = $+0.26\pm 0.05$
  dex and $[\mathrm{Fe}/{\rm{H}}]$ = $+0.24\pm 0.05$ for TOI-481 and
  TOI-892, respectively) but at different evolutionary stages. TOI-481
  is a ${M}_{\star }$ = 1.14 ± 0.02 ${M}_{\odot }$ , ${R}_{\star }$
  = 1.66 ± 0.02 ${R}_{\odot }$ G-type star ( ${T}_{\mathrm{eff}}$
  = $5735\pm 72$ K), that with an age of 6.7 Gyr, is in the turn-off
  point of the main sequence. TOI-892 on the other hand, is a F-type
  dwarf star ( ${T}_{\mathrm{eff}}$ = $6261\pm 80$ K), which has a
  mass of ${M}_{\star }$ = 1.28 ± 0.03 ${M}_{\odot }$ and a radius of
  ${R}_{\star }$ = 1.39 ± 0.02 ${R}_{\odot }$ . TOI-481 b and TOI-892
  b join the scarcely populated region of transiting gas giants with
  orbital periods longer than 10 days, which is important to constrain
  theories of the formation and structure of hot Jupiters.

Title: Very regular high-frequency pulsation modes in young
    intermediate-mass stars
Authors: Bedding, Timothy R.; Murphy, Simon J.; Hey, Daniel R.; Huber,
   Daniel; Li, Tanda; Smalley, Barry; Stello, Dennis; White, Timothy R.;
   Ball, Warrick H.; Chaplin, William J.; Colman, Isabel L.; Fuller,
   Jim; Gaidos, Eric; Harbeck, Daniel R.; Hermes, J. J.; Holdsworth,
   Daniel L.; Li, Gang; Li, Yaguang; Mann, Andrew W.; Reese, Daniel R.;
   Sekaran, Sanjay; Yu, Jie; Antoci, Victoria; Bergmann, Christoph;
   Brown, Timothy M.; Howard, Andrew W.; Ireland, Michael J.; Isaacson,
   Howard; Jenkins, Jon M.; Kjeldsen, Hans; McCully, Curtis; Rabus,
   Markus; Rains, Adam D.; Ricker, George R.; Tinney, Christopher G.;
   Vanderspek, Roland K.
Bibcode: 2020Natur.581..147B
Altcode: 2020arXiv200506157B
  Asteroseismology probes the internal structures of stars by using
  their natural pulsation frequencies<SUP>1</SUP>. It relies on
  identifying sequences of pulsation modes that can be compared with
  theoretical models, which has been done successfully for many classes
  of pulsators, including low-mass solar-type stars<SUP>2</SUP>,
  red giants<SUP>3</SUP>, high-mass stars<SUP>4</SUP> and white
  dwarfs<SUP>5</SUP>. However, a large group of pulsating stars of
  intermediate mass—the so-called δ Scuti stars—have rich pulsation
  spectra for which systematic mode identification has not hitherto been
  possible<SUP>6,7</SUP>. This arises because only a seemingly random
  subset of possible modes are excited and because rapid rotation tends
  to spoil regular patterns<SUP>8-10</SUP>. Here we report the detection
  of remarkably regular sequences of high-frequency pulsation modes in
  60 intermediate-mass main-sequence stars, which enables definitive mode
  identification. The space motions of some of these stars indicate that
  they are members of known associations of young stars, as confirmed
  by modelling of their pulsation spectra.

Title: A new absorption component in the H-alpha line profile of
    eta Carinae
Authors: Damineli, Augusto; Navarete, Felipe; Heathcote, Bernard;
   Di Scala, Giorgio; Harrison, Ken; Di Scala, Giorigo; Johnston,
   Mark; McGee, Padric; Cacella, Paulo; Bohlsen, Terry; Rabus, Markus;
   Brown, Tim
Bibcode: 2020ATel13639....1D
Altcode:
  Based on a high signal-to-noise and high plus intermediate resolution
  (R=100,000 and R &gt; 6,000) ground-based monitoring of eta Carinae
  periastron (ATEL #13508, ATEL #13600), we report the following results:
  The narrow absorption at -138 km/s (FWHM=25 km/s), believed to be
  formed in the Little Homunculus, reached zero intensity already during
  the past orbital cycle.

Title: Ground-based spectroscopic monitoring of the 2020 periastron
    in eta Carinae
Authors: Navarete, Felipe; Damineli, Augusto; Richardson, Noel;
   Ibrahim, Nour; Heathcote, Bernard; Di Scala, Giorgio; Harrison,
   Ken; Di Scala, Lidia; Johnston, Mark; McGee, Padric; Cacella, Paulo;
   Bohlsen, Terry; Rabus, Markus; Brown, Tim
Bibcode: 2020ATel13600....1N
Altcode:
  Based on a high signal-to-noise and high plus intermediate
  resolution (R=100,000 and R &gt; 6,000) ground-based monitoring of
  eta Carinae periastron (ATEL #13508), we report the following results:
  Representative lines of the extended primary's photosphere, (H- &amp;
  delta; and SiII &amp; lambda;6347A) indicate no significant changes
  as compared to the 2014.5 (Teodoro et al. 2016, ApJ 819, 131).

Title: The Hubble Space Telescope UV Legacy Survey of Galactic
    Globular Clusters. XX. Ages of Single and Multiple Stellar Populations
    in Seven Bulge Globular Clusters
Authors: Oliveira, R. A. P.; Souza, S. O.; Kerber, L. O.; Barbuy,
   B.; Ortolani, S.; Piotto, G.; Nardiello, D.; Pérez-Villegas, A.;
   Maia, F. F. S.; Bica, E.; Cassisi, S.; D'Antona, F.; Lagioia, E. P.;
   Libralato, M.; Milone, A. P.; Anderson, J.; Aparicio, A.; Bedin,
   L. R.; Brown, T. M.; King, I. R.; Marino, A. F.; Pietrinferni, A.;
   Renzini, A.; Sarajedini, A.; van der Marel, R.; Vesperini, E.
Bibcode: 2020ApJ...891...37O
Altcode: 2020arXiv200108611O
  In the present work we analyzed seven globular clusters (GCs) selected
  from their location in the Galactic bulge and with metallicity values
  in the range -1.30 ≲ [Fe/H] ≲ -0.50. The aim of this work is first
  to derive cluster ages assuming single stellar populations and second
  to identify the stars from first (1G) and second generations (2G) from
  the main sequence, subgiant, and red giant branches, and to derive their
  age differences. Based on a combination of UV and optical filters used
  in this project, we apply the Gaussian mixture models to distinguish
  the multiple stellar populations. Applying statistical isochrone
  fitting, we derive self-consistent ages, distances, metallicities,
  and reddening values for the sample clusters. An average age of 12.3
  ± 0.4 Gyr was obtained both using DSED and BaSTI (accounting atomic
  diffusion effects) isochrones, without a clear distinction between the
  moderately metal-poor and the more metal-rich bulge clusters, except
  for NGC 6717 and the inner halo NGC 6362 with ∼13.5 Gyr. We derived
  a weighted mean age difference between the multiple populations hosted
  by each GC of 41 ± 170 Myr adopting canonical He abundances; whereas
  for higher He in 2G stars, this difference reduces to 17 ± 170 Myr,
  but with individual uncertainties of 500 Myr.

Title: Erratum: DQWD
Authors: Milone, A. P.; Vesperini, E.; Marino, A. F.; Hong, J.; van
   der Marel, R.; Anderson, J.; Renzini, A.; Cordoni, G.; Bedin, L. R.;
   Bellini, A.; Brown, T. M.; Antona, F. D.; Lagioia, E. P.; Libralato,
   M.; Nardiello, D.; Piotto, G.; Tailo, M.; Cool, A.; Salaris, M.;
   Sarajedini, A.
Bibcode: 2020MNRAS.492.4589M
Altcode: 2020MNRAS.tmp..150M
  No abstract at ADS

Title: The Hubble Space Telescope UV Legacy Survey of Galactic
    globular clusters - XXI. Binaries among multiple stellar populations
Authors: Milone, A. P.; Vesperini, E.; Marino, A. F.; Hong, J.; van
   der Marel, R.; Anderson, J.; Renzini, A.; Cordoni, G.; Bedin, L. R.;
   Bellini, A.; Brown, T. M.; D'Antona, F.; Lagioia, E. P.; Libralato,
   M.; Nardiello, D.; Piotto, G.; Tailo, M.; Cool, A.; Salaris, M.;
   Sarajedini, A.
Bibcode: 2020MNRAS.492.5457M
Altcode: 2019MNRAS.tmp.3249M; 2020arXiv200206479M; 2019MNRAS.tmp..199M
  A number of scenarios for the formation of multiple populations in
  globular clusters (GCs) predict that second generation (2G) stars
  form in a compact and dense subsystem embedded in a more extended
  first-generation (1G) system. If these scenarios are accurate,
  a consequence of the denser 2G formation environment is that 2G
  binaries should be more significantly affected by stellar interactions
  and disrupted at a larger rate than 1G binaries. The fractions and
  properties of binary stars can thus provide a dynamical fingerprint
  of the formation epoch of multiple-population GCs and their subsequent
  dynamical evolution. We investigate the connection between binaries and
  multiple populations in five GCs, NGC 288, NGC 6121 (M 4), NGC 6352,
  NGC 6362, and NGC 6838 (M 71). To do this, we introduce a new method
  based on the comparison of Hubble Space Telescope observations of
  binaries in the F275W, F336W, F438W, F606W, and F814W filters with a
  large number of simulated binaries. In the inner regions probed by our
  data, we do not find large differences between the local 1G and the 2G
  binary incidences in four of the studied clusters, the only exception
  being M 4 where the 1G binary incidence is about three times larger
  than the 2G incidence. The results found are in general agreement with
  the results of simulations predicting significant differences in the
  global 1G and 2G incidences and in the local values in the clusters'
  outer regions but similar incidences in the inner regions. The
  significant difference found in M 4 is consistent with simulations
  with a larger fraction of wider binaries. Our analysis also provides
  the first evidence of mixed (1G-2G) binaries, a population predicted
  by numerical simulations to form in a cluster's inner regions as a
  result of stellar encounters during which one component of a binary
  is replaced by a star of a different population.

Title: The 2020 periastron passage of eta Carine seen in He I and
    He II lines
Authors: Navarete, Felipe; Damineli, Augusto; Jablonski, Francisco;
   Brown, Tim; Rabus, Markus
Bibcode: 2020ATel13508....1N
Altcode:
  In the framework of a monitoring campaign of the low excitation event
  (Damineli et a. 1998, A &amp; A Supp. 133, 299) in eta Carinae, we
  report results on the periastron passage expected to occur on 2020
  February 17 (Teodoro et al. 2016, ApJ 819:131).

Title: TESS Spots a Compact System of Super-Earths around the
    Naked-eye Star HR 858
Authors: Vanderburg, Andrew; Huang, Chelsea X.; Rodriguez, Joseph E.;
   Becker, Juliette C.; Ricker, George R.; Vanderspek, Roland K.; Latham,
   David W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Addison,
   Brett; Bieryla, Allyson; Briceño, Cesar; Bowler, Brendan P.; Brown,
   Timothy M.; Burke, Christopher J.; Burt, Jennifer A.; Caldwell,
   Douglas A.; Clark, Jake T.; Crossfield, Ian; Dittmann, Jason A.;
   Dynes, Scott; Fulton, Benjamin J.; Guerrero, Natalia; Harbeck, Daniel;
   Horner, Jonathan; Kane, Stephen R.; Kielkopf, John; Kraus, Adam L.;
   Kreidberg, Laura; Law, Nicolas; Mann, Andrew W.; Mengel, Matthew W.;
   Morton, Timothy D.; Okumura, Jack; Pearce, Logan A.; Plavchan, Peter;
   Quinn, Samuel N.; Rabus, Markus; Rose, Mark E.; Rowden, Pam; Shporer,
   Avi; Siverd, Robert J.; Smith, Jeffrey C.; Stassun, Keivan; Tinney,
   C. G.; Wittenmyer, Rob; Wright, Duncan J.; Zhang, Hui; Zhou, George;
   Ziegler, Carl A.
Bibcode: 2019ApJ...881L..19V
Altcode: 2019arXiv190505193V
  Transiting Exoplanet Survey Satellite (TESS) observations have revealed
  a compact multiplanet system around the sixth-magnitude star HR 858
  (TIC 178155732, TOI 396), located 32 pc away. Three planets, each about
  twice the size of Earth, transit this slightly evolved, late F-type
  star, which is also a member of a visual binary. Two of the planets
  may be in mean motion resonance. We analyze the TESS observations,
  using novel methods to model and remove instrumental systematic errors,
  and combine these data with follow-up observations taken from a suite
  of ground-based telescopes to characterize the planetary system. The
  HR 858 planets are enticing targets for precise radial velocity
  observations, secondary eclipse spectroscopy, and measurements of the
  Rossiter-McLaughlin effect.

Title: Do Sun-like stars experience a magnetic mid-life
    crisis? Investigation from a new Ca HK activity survey using LCO NRES
Authors: Goga, Adam; Metcalfe, Travis S.; Egeland, Ricky; Brown,
   Timothy M.
Bibcode: 2019shin.confE.111G
Altcode:
  The dynamo effect, which modulates the magnetic field of stars,
  is a topic of active research. While there are many dynamo models,
  most only work for a small subgroup of stars and may be specifically
  designed for the Sun. We have monitored the S-Index, a magnetic proxy,
  for a sample of bright stars with known rotation rates (Prot &lt;
  22 days), to discover short magnetic activity cycles (Pcyc &lt; 5
  years) that are precursors of the 11-year solar cycle. This study adds
  additional constraints to current and future dynamo models by producing
  data for stars whose cycles are unknown. Las Cumbres Observatory's
  Network of Robotic Echelle Spectrographs (NRES) has a large archive
  of data for many stars. NRES is a global telescope system with six
  sites whose main purpose is to study exoplanets. We have developed an
  automated pipeline in Python to pull the intensity of the Ca II H and
  K emission features from the NRES spectra which are used to find the
  S-Index. With our pipeline, we have seen evidence of magnetic cycles
  in stars whose activity is known through previous studies. Our study
  demonstrates that the NRES system is sensitive enough to discover
  magnetic activity in stars. We can now probe these stars deeper for
  unknown underlying activity which may help understand their dynamo
  process. The pipeline is highly extendable and allows users to add
  features to find additional information from NRES data.

Title: Star cluster catalogues for the LEGUS dwarf galaxies
Authors: Cook, D. O.; Lee, J. C.; Adamo, A.; Kim, H.; Chandar, R.;
   Whitmore, B. C.; Mok, A.; Ryon, J. E.; Dale, D. A.; Calzetti, D.;
   Andrews, J. E.; Aloisi, A.; Ashworth, G.; Bright, S. N.; Brown, T. M.;
   Christian, C.; Cignoni, M.; Clayton, G. C.; da Silva, R.; de Mink,
   S. E.; Dobbs, C. L.; Elmegreen, B. G.; Elmegreen, D. M.; Evans, A. S.;
   Fumagalli, M.; Gallagher, J. S.; Gouliermis, D. A.; Grasha, K.; Grebel,
   E. K.; Herrero, A.; Hunter, D. A.; Jensen, E. I.; Johnson, K. E.;
   Kahre, L.; Kennicutt, R. C.; Krumholz, M. R.; Lee, N. J.; Lennon, D.;
   Linden, S.; Martin, C.; Messa, M.; Nair, P.; Nota, A.; Östlin, G.;
   Parziale, R. C.; Pellerin, A.; Regan, M. W.; Sabbi, E.; Sacchi, E.;
   Schaerer, D.; Schiminovich, D.; Shabani, F.; Slane, F. A.; Small, J.;
   Smith, C. L.; Smith, L. J.; Taibi, S.; Thilker, D. A.; de la Torre,
   I. C.; Tosi, M.; Turner, J. A.; Ubeda, L.; Van Dyk, S. D.; Walterbos,
   R. AM; Wofford, A.
Bibcode: 2019MNRAS.484.4897C
Altcode: 2019arXiv190200082C; 2019MNRAS.tmp..337C
  We present the star cluster catalogues for 17 dwarf and irregular
  galaxies in the HST Treasury Program `Legacy ExtraGalactic UV Survey'
  (LEGUS). Cluster identification and photometry in this sub-sample are
  similar to that of the entire LEGUS sample, but special methods were
  developed to provide robust catalogues with accurate fluxes due to low
  cluster statistics. The colours and ages are largely consistent for
  two widely used aperture corrections, but a significant fraction of the
  clusters are more compact than the average training cluster. However,
  the ensemble luminosity, mass, and age distributions are consistent
  suggesting that the systematics between the two methods are less than
  the random errors. When compared with the clusters from previous dwarf
  galaxy samples, we find that the LEGUS catalogues are more complete
  and provide more accurate total fluxes. Combining all clusters
  into a composite dwarf galaxy, we find that the luminosity and mass
  functions can be described by a power law with the canonical index
  of -2 independent of age and global SFR binning. The age distribution
  declines as a power law, with an index of ≈- 0.80 ± 0.15, independent
  of cluster mass and global SFR binning. This decline of clusters is
  dominated by cluster disruption since the combined star formation
  histories and integrated-light SFRs are both approximately constant
  over the last few hundred Myr. Finally, we find little evidence for an
  upper-mass cut-off (&lt;2σ) in the composite cluster mass function, and
  can rule out a truncation mass below ≈10<SUP>4.5</SUP>M<SUB>⊙</SUB>
  but cannot rule out the existence of a truncation at higher masses.

Title: TESS Delivers Its First Earth-sized Planet and a Warm
    Sub-Neptune
Authors: Dragomir, Diana; Teske, Johanna; Günther, Maximilian N.;
   Ségransan, Damien; Burt, Jennifer A.; Huang, Chelsea X.; Vanderburg,
   Andrew; Matthews, Elisabeth; Dumusque, Xavier; Stassun, Keivan G.;
   Pepper, Joshua; Ricker, George R.; Vanderspek, Roland; Latham, David
   W.; Seager, Sara; Winn, Joshua N.; Jenkins, Jon M.; Beatty, Thomas;
   Bouchy, François; Brown, Timothy M.; Butler, R. Paul; Ciardi, David
   R.; Crane, Jeffrey D.; Eastman, Jason D.; Fossati, Luca; Francis, Jim;
   Fulton, Benjamin J.; Gaudi, B. Scott; Goeke, Robert F.; James, David;
   Klaus, Todd C.; Kuhn, Rudolf B.; Lovis, Christophe; Lund, Michael
   B.; McDermott, Scott; Paegert, Martin; Pepe, Francesco; Rodriguez,
   Joseph E.; Sha, Lizhou; Shectman, Stephen A.; Shporer, Avi; Siverd,
   Robert J.; Garcia Soto, Aylin; Stevens, Daniel J.; Twicken, Joseph D.;
   Udry, Stéphane; Villanueva, Steven, Jr.; Wang, Sharon X.; Wohler,
   Bill; Yao, Xinyu; Zhan, Zhuchang
Bibcode: 2019ApJ...875L...7D
Altcode: 2019arXiv190100051D
  The future of exoplanet science is bright, as Transiting Exoplanet
  Survey Satellite (TESS) once again demonstrates with the discovery
  of its longest-period confirmed planet to date. We hereby present
  HD 21749b (TOI 186.01), a sub-Neptune in a 36 day orbit around a
  bright (V = 8.1) nearby (16 pc) K4.5 dwarf. TESS measures HD 21749b
  to be {2.61}<SUB>-0.16</SUB><SUP>+0.17</SUP> R <SUB>⊕</SUB>,
  and combined archival and follow-up precision radial velocity data
  put the mass of the planet at {22.7}<SUB>-1.9</SUB><SUP>+2.2</SUP>
  M <SUB>⊕</SUB>. HD 21749b contributes to the TESS Level 1 Science
  Requirement of providing 50 transiting planets smaller than 4
  R <SUB>⊕</SUB> with measured masses. Furthermore, we report
  the discovery of HD 21749c (TOI 186.02), the first Earth-sized
  ({R}<SUB>p</SUB>={0.892}<SUB>-0.058</SUB><SUP>+0.064</SUP>{R}<SUB>\oplus
  </SUB>) planet from TESS. The HD 21749 system is a prime target
  for comparative studies of planetary composition and architecture in
  multi-planet systems. <P />This Letter includes data gathered with the
  6.5 m Magellan Telescopes located at Las Campanas Observatory, Chile.

Title: HD 202772A b: A Transiting Hot Jupiter around a Bright,
    Mildly Evolved Star in a Visual Binary Discovered by TESS
Authors: Wang, Songhu; Jones, Matias; Shporer, Avi; Fulton,
   Benjamin J.; Paredes, Leonardo A.; Trifonov, Trifon; Kossakowski,
   Diana; Eastman, Jason; Redfield, Seth; Günther, Maximilian N.;
   Kreidberg, Laura; Huang, Chelsea X.; Millholland, Sarah; Seligman,
   Darryl; Fischer, Debra; Brahm, Rafael; Wang, Xian-Yu; Cruz, Bryndis;
   Henry, Todd; James, Hodari-Sadiki; Addison, Brett; Liang, En-Si;
   Davis, Allen B.; Tronsgaard, René; Worku, Keduse; Brewer, John M.;
   Kürster, Martin; Zhang, Hui; Beichman, Charles A.; Bieryla, Allyson;
   Brown, Timothy M.; Christiansen, Jessie L.; Ciardi, David R.; Collins,
   Karen A.; Esquerdo, Gilbert A.; Howard, Andrew W.; Isaacson, Howard;
   Latham, David W.; Mazeh, Tsevi; Petigura, Erik A.; Quinn, Samuel N.;
   Shahaf, Sahar; Siverd, Robert J.; Rodler, Florian; Reffert, Sabine;
   Zakhozhay, Olga; Ricker, George R.; Vanderspek, Roland; Seager, Sara;
   Winn, Joshua N.; Jenkins, Jon M.; Boyd, Patricia T.; Fűrész, Gábor;
   Henze, Christopher; Levine, Alen M.; Morris, Robert; Paegert, Martin;
   Stassun, Keivan G.; Ting, Eric B.; Vezie, Michael; Laughlin, Gregory
Bibcode: 2019AJ....157...51W
Altcode: 2018arXiv181002341W
  We report the first confirmation of a hot Jupiter discovered by the
  Transiting Exoplanet Survey Satellite (TESS) mission: HD 202772A
  b. The transit signal was detected in the data from TESS Sector 1,
  and was confirmed to be of planetary origin through radial velocity
  (RV) measurements. HD 202772A b is orbiting a mildly evolved star with
  a period of 3.3 days. With an apparent magnitude of V = 8.3, the star is
  among the brightest and most massive known to host a hot Jupiter. Based
  on the 27 days of TESS photometry and RV data from the CHIRON, HARPS,
  and Tillinghast Reflector Echelle Spectrograph, the planet has a mass
  of {1.017}<SUB>-0.068</SUB><SUP>+0.070</SUP> {M}<SUB>{{J</SUB>}} and
  radius of {1.545}<SUB>-0.060</SUB><SUP>+0.052</SUP> {R}<SUB>{{J</SUB>}},
  making it an inflated gas giant. HD 202772A b is a rare example of a
  transiting hot Jupiter around a quickly evolving star. It is also one
  of the most strongly irradiated hot Jupiters currently known.

Title: The Las Cumbres Observatory's Network of Robotic Echelle
Spectrographs in 2019: Current status and next steps
Authors: Harbeck, Daniel R.; Brown, Tim; Siverd, Robert; McCully,
   Curtis; Foale, Steve; Nation, Jon; Henderson, Todd; Taylor, Brook;
   de Vera, Jon; Smith, Cary; Kirby, Annie
Bibcode: 2019AAS...23314603H
Altcode:
  Over the last two years, the Las Cumbres Observatory (LCOGT) has
  deployed the Network of Robotic Echelle Spectrographs (NRES), which
  consists of optical high-precision spectrographs that are fed by 1-meter
  telescopes at four sites: In Chile (CTIO), USA (McDonald Observatory),
  South Africa (SAAO), and Israel (Wise Observatory). These spectrographs
  are identically designed and built, and they cover a wavelength range
  from 390nm to 860nm at a resolution of ~45000. After ~1.5 years of
  installation and commissioning efforts, fully robotic science operations
  are now regularly underway with the NRES system. Although significant
  telescope time is currently assigned in support of NASA's TESS mission,
  NRES is a valuable resource for the entire astronomical community
  via open access through the NSF / NOAO. In this report we describe
  the current performance of the spectrographs for both radial velocity
  measurement and stellar classification and also discuss opportunities
  and plans for further improvement.

Title: Developing the infrastructure of bright-star exoplanet hunting:
    the Kilodegree Extremely Little Telescope (KELT) and the Network of
    Robotic Echelle Spectrographs (NRES)
Authors: Siverd, Robert; Stassun, Keivan G.; Lund, Michael B.; Stevens,
   Daniel J.; Brown, Tim; Harbeck, Daniel R.
Bibcode: 2019AAS...23342202S
Altcode:
  The Kilodegree Extremely Little Telescope (KELT) is an ongoing,
  wide-field (26x26 deg) photometric survey for transiting exoplanets
  using small-aperture telescopes in Arizona, USA and Sutherland, SA
  to monitor ~70% of the sky at ~30-minute cadence. KELT was built to
  find high-value transiting exoplanets around bright host stars. Using
  off-the-shelf hardware, the KELT telescopes achieve better-than-1%
  precision for 7.5 Reaching the needed photometric precision is
  complicated by source blending (23"/pix) and PSF variability. Careful
  use of existing and modified difference imaging tools brought success
  but with significant compromises. Our new Catalog-Driven Extraction
  (CDE) is a set of key changes to both our reduction pipelines and data
  handling that markedly improve photometric accuracy and simplify the
  candidate identification process. Further, CDE-generated light curves
  are suited to a wider range of science tasks and will become a valuable
  community resource. Confirming a transiting exoplanet involves other
  hurdles beyond photometry. Chief among these is obtaining a radial
  velocity (RV) orbit. The scarcity of spectroscopic resources is a
  genuine bottleneck for exoplanet confirmation. To fill this void,
  Las Cumbres Observatory (LCO) has designed, built, and deployed the
  Network of Robotic Echelle Spectrographs (NRES) to its worldwide
  network of robotic 1-meter telescopes. NRES consists of four,
  optical, fiber-fed, R~45000 spectrographs designed for RV and stellar
  classification. Now operational, NRES is poised to become an important
  resource for exoplanet discovery and stellar astrophysics. The KELT and
  NRES presented very different development challenges despite related
  science goals. In this report I discuss the significant and different
  infrastructural challenges involved in these two projects and share
  important lessons learned. Finally, I discuss some of the exciting
  prospects for future work in bright-star time-domain science.

Title: The Hubble Space Telescope UV legacy survey of galactic
    globular clusters - XVI. The helium abundance of multiple populations
Authors: Milone, A. P.; Marino, A. F.; Renzini, A.; D'Antona, F.;
   Anderson, J.; Barbuy, B.; Bedin, L. R.; Bellini, A.; Brown, T. M.;
   Cassisi, S.; Cordoni, G.; Lagioia, E. P.; Nardiello, D.; Ortolani,
   S.; Piotto, G.; Sarajedini, A.; Tailo, M.; van der Marel, R. P.;
   Vesperini, E.
Bibcode: 2018MNRAS.481.5098M
Altcode: 2018MNRAS.tmp.2453M; 2018arXiv180905006M
  Recent work, based on data from the Hubble Space Telescope (HST )
  UV Legacy Survey of Galactic Globular Clusters (GCs), has revealed
  that all the analysed clusters host two groups of first- (1G) and
  second-generation (2G) stars. In most GCs, both 1G and 2G stars
  host substellar populations with different chemical composition. We
  compare multiwavelength HST photometry with synthetic spectra to
  determine for the first time the average helium difference between
  the 2G and 1G stars in a large sample of 57 GCs and the maximum helium
  variation within each of them. We find that in all clusters 2G stars
  are consistent with being enhanced in helium with respect to 1G. The
  maximum helium variation ranges from less than 0.01 to more than 0.10
  in helium mass fraction and correlates with both the cluster mass and
  the colour extension of the horizontal branch (HB). These findings
  demonstrate that the internal helium variation is one of the main
  (second) parameters governing the HB morphology.

Title: VizieR Online Data Catalog: LEGUS galaxies1 observations
    (Sabbi+, 2018)
Authors: Sabbi, E.; Calzetti, D.; Ubeda, L.; Adamo, A.; Cignoni,
   M.; Thilker, D.; Aloisi, A.; Elmegreen, B. G.; Elmegreen, D. M.;
   Gouliermis, D. A.; Grebel, E. K.; Messa, M.; Smith, L. J.; Tosi, M.;
   Dolphin, A.; Andrews, J. E.; Ashworth, G.; Bright, S. N.; Brown, T. M.;
   Chandar, R.; Christian, C.; Clayton, G. C.; Cook, D. O.; Dale, D. A.;
   de Mink, S. E.; Dobbs, C.; Evans, A. S.; Fumagalli, M.; Gallagher,
   J. S.; Grasha, K.; Herrero, A.; Hunter, D. A.; Johnson, K. E.; Kahre,
   L.; Kennicutt, R. C.; Kim, H.; Krumholz, M. R.; Lee, J. C.; Lennon, D.;
   Martin, C.; Nair, P.; Nota, A.; Ostlin, G.; Pellerin, A.; Prieto, J.;
   Regan, M. W.; Ryon, J. E.; Sacchi, E.; Schaerer, D.; Schiminovich,
   D.; Shabani, F.; van Dyk, S. D.; Walterbos, R.; Whitmore, B. C.;
   Wofford, A.
Bibcode: 2018yCat..22350023S
Altcode:
  The Legacy ExtraGalactic UV Survey (LEGUS) is a multiwavelength Cycle 21
  Treasury program on the Hubble Space Telescope (HST). LEGUS was awarded
  154 orbits in Cycle 21 to observe 50 star-forming galaxies with the
  UVIS channel of the Wide Field Camera 3 (WFC3) in the filters F275W,
  F336W, and when not already available in the Mikulski Archive for
  the Space Telescope (MAST) archive, also in the filters F438W, F555W,
  and F814W. For simplicity, from now on, in the text we will refer to
  these filters as NUV, U, B, V, and I, respectively. <P />To increase
  the legacy value of the project, ACS archival data in the filters B,
  V, and/or I have been aligned to the LEGUS data. <P />See the log
  of the observations in Table 1 (spanning November 2002 to September
  2014). <P />(4 data files).

Title: UV and Optical Variability of the Young Star T Cha Produced
    by Inner Disk Obscuration
Authors: Brown, Alexander; France, Kevin; Walter, Frederick; Schneider,
   Christian P.; Brown, Timothy; Andrews, Sean; Wilner, David
Bibcode: 2018csss.confE..28B
Altcode:
  The young (7 Myr) 1.5 M⊙ T Tauri star T Cha shows dramatic
  variability. The optical extinction varies by at least 3 magnitudes on
  few hour time-scales. The obscuration is produced by material at the
  inner edge of the circumstellar disk and therefore characterizing
  the absorbing material can reveal important clues regarding the
  transport of gas and dust within such disks. The inner disk of T Cha is
  particularly interesting, because T Cha has a transitional disk with a
  large gap at 0.2- 15 AU in the dust disk and allows study of the gas
  and dust structure in the terrestrial planet formation zone during
  this important rapid phase of protoplanetary disk evolution. For this
  reason we have conducted a comprehensive, multi-spectral- region,
  observing campaign to study the UV/X-ray/optical variability of T
  Cha. During 2018 February/March we monitored the optical photometric
  and spectral variability using LCOGT and the SMARTS telescopes. These
  optical data provide a broad context within which to interpret
  our shorter UV and X-ray observations. We observed T Cha during 3
  coordinated observations (each 5 HST orbits + 25 ksec XMM; on 2018
  Feb 22, Feb 26, Mar 2) using HST COS/STIS to measure the UV-optical
  spectra and XMM-Newton to measure the X-ray energy distribution. The
  observed spectral changes are well correlated and demonstrate the
  influence of the same absorbing material in the different spectral
  regions. In this poster we examine which spectral features in the
  different spectral regions (FUV/NUV/optical/X-ray) change and by how
  much, and thereby determine the location of different emitting regions
  within the complex stellar/inner disk system relative to the absorbers
  along the line-of-sight to the stellar photosphere. Understanding these
  contributions is vital for estimating the properties of the absorbing
  gas and dust. (This work is supported by grant HST-GO-15128 and time
  awarded by HST, XMM-Newton, LCOGT, and SMARTS.)

Title: NRES: the network of robotic echelle spectrographs
Authors: Siverd, Robert J.; Brown, Timothy M.; Barnes, Stuart; Bowman,
   Mark K.; De Vera, Jon; Foale, Stephen; Harbeck, Daniel-Rolf; Henderson,
   Todd; Hygelund, John; Kirby, Annie; McCully, Curtis; Nation, Jon S.;
   Smith, Cary; Taylor, Brook; Tufts, Joseph R.
Bibcode: 2018SPIE10702E..6CS
Altcode:
  Las Cumbres Observatory Global Telescope Network (LCOGT) has built
  the Network of Robotic Echelle Spectrographs (NRES), consisting of
  four identical, high-resolution optical spectrographs, each fiber-fed
  simultaneously by up to two 1-meter telescopes and a calibration
  source. Two units have been installed and are currently executing
  scientific observations. A third unit has been installed and is
  presently in commissioning. A fourth unit has been shipped to site and
  will be installed in mid 2018. Operating on four separate continents
  in both the Northern and Southern hemispheres, these instruments
  comprise a globally-distributed, autonomous spectrograph facility
  for stellar classification and high-precision radial velocity of
  bright stars. Simulations suggest we will achieve long-term radial
  velocity precision of 3 m/s in less than an hour for stars with V &lt;
  12. Radial velocity precision of 75 m/s has already been demonstrated
  with our automatic data-processing pipeline across multiple sites. Work
  is ongoing to improve several NRES system components including
  telescope control (robotic source acquisition in particular) and the
  data-processing pipeline. In this document we briefly overview the NRES
  design, its purpose and goals, results achieved to date in the field,
  and the ongoing development effort to improve instrument performance.

Title: UV, X-ray, and Optical Variability of the Young Star T Cha
Produced by Inner Disk Obscuration: Results from a Coordinated HST,
    XMM-Newton, LCOGT, and SMARTS Observing Campaign
Authors: Brown, Alexander; France, Kevin; Walter, Frederick M.;
   Schneider, P. Christian; Brown, Timothy M.; Andrews, Sean M.; Wilner,
   David J.
Bibcode: 2018AAS...23221909B
Altcode:
  The young (7 Myr) 1.5 solar mass T Tauri star T Chamaeleontis shows
  dramatic variability. The optical extinction varies by at least 3
  magnitudes on few hour time-scales with no obvious periodicity. The
  obscuration is produced by material at the inner edge of the
  circumstellar disk and therefore characterizing the absorbing material
  can reveal important clues regarding the transport of gas and dust
  within such disks. The inner disk of T Cha is particularly interesting,
  because T Cha has a transitional disk with a large gap at 0.2-15 AU
  in the dust disk and allows study of the gas and dust structure in the
  terrestrial planet formation zone during this important rapid phase of
  protoplanetary disk evolution. For this reason we have conducted a major
  multi-spectral-region observing campaign to study the UV/X-ray/optical
  variability of T Cha. During 2018 February/March we monitored the
  optical photometric and spectral variability using LCOGT (Chile/South
  Africa/Australia) and the SMARTS telescopes in Chile. These optical data
  provide a broad context within which to interpret our shorter UV and
  X-ray observations. We observed T Cha during 3 coordinated observations
  (each 5 HST orbits + 25 ksec XMM; on 2018 Feb 22, Feb 26, Mar 2)
  using the HST COS/STIS spectrographs to measure the FUV/NUV spectra and
  XMM-Newton to measure the corresponding X-ray energy distribution. The
  observed spectral changes are well correlated and demonstrate the
  influence of the same absorbing material in all the spectral regions
  observed. By examining which spectral features change and by how much
  we can determine the location of different emitting regions relative to
  the absorbers along the line-of-sight to the star. In this poster we
  provide an overview of the variability seen in the different spectral
  regions and quantify the dust and gas content of T Cha's inner disk
  edge.(This work is supported by grant HST-GO-15128 and time awarded
  by HST, XMM-Newton, LCOGT, and SMARTS. We acknowledge the assistance
  provided by Dr. Todd Henry in conducting this observing campaign.)

Title: The Hubble Space Telescope UV Legacy Survey of Galactic
    globular clusters - XIII. ACS/WFC parallel-field catalogues
Authors: Simioni, M.; Bedin, L. R.; Aparicio, A.; Piotto, G.; Milone,
   A. P.; Nardiello, D.; Anderson, J.; Bellini, A.; Brown, T. M.;
   Cassisi, S.; Cunial, A.; Granata, V.; Ortolani, S.; van der Marel,
   R. P.; Vesperini, E.
Bibcode: 2018MNRAS.476..271S
Altcode: 2018MNRAS.tmp..176S; 2018arXiv180107445S
  As part of the Hubble Space Telescope UV Legacy Survey of Galactic
  globular clusters, 110 parallel fields were observed with the Wide
  Field Channel of the Advanced Camera for Surveys, in the outskirts of
  48 globular clusters, plus the open cluster NGC 6791. Totalling about
  0.3 deg<SUP>2</SUP> of observed sky, this is the largest homogeneous
  Hubble Space Telescope photometric survey of Galalctic globular
  clusters outskirts to date. In particular, two distinct pointings have
  been obtained for each target on average, all centred at about 6.5
  arcmin from the cluster centre, thus covering a mean area of about 23
  arcmin<SUP>2</SUP> for each globular cluster. For each field, at least
  one exposure in both F475W and F814W filters was collected. In this
  work, we publicly release the astrometric and photometric catalogues
  and the astrometrized atlases for each of these fields.

Title: The K2 M67 Study: A Curiously Young Star in an Eclipsing
    Binary in an Old Open Cluster
Authors: Sandquist, Eric L.; Mathieu, Robert D.; Quinn, Samuel N.;
   Pollack, Maxwell L.; Latham, David W.; Brown, Timothy M.; Esselstein,
   Rebecca; Aigrain, Suzanne; Parviainen, Hannu; Vanderburg, Andrew;
   Stello, Dennis; Somers, Garrett; Pinsonneault, Marc H.; Tayar, Jamie;
   Orosz, Jerome A.; Bedin, Luigi R.; Libralato, Mattia; Malavolta,
   Luca; Nardiello, Domenico
Bibcode: 2018AJ....155..152S
Altcode: 2018arXiv180205854S
  We present an analysis of a slightly eccentric (e = 0.05), partially
  eclipsing, long-period (P = 69.73 days) main-sequence binary system
  (WOCS 12009, Sanders 1247) in the benchmark old open cluster M67. Using
  Kepler K2 and ground-based photometry, along with a large set of
  new and reanalyzed spectra, we derived highly precise masses (1.111
  ± 0.015 and 0.748 ± 0.005 M <SUB>⊙</SUB>) and radii (1.071 ±
  0.008 ± 0.003 and 0.713 ± 0.019 ± 0.026 R <SUB>⊙</SUB>, with
  statistical and systematic error estimates) for the stars. The radius
  of the secondary star is in agreement with theory. The primary, however,
  is approximately 15% smaller than reasonable isochrones for the cluster
  predict. Our best explanation is that the primary star was produced from
  the merger of two stars, as this can also account for the nondetection
  of photospheric lithium and its higher temperature relative to other
  cluster main-sequence stars at the same V magnitude. To understand the
  dynamical characteristics (low measured rotational line broadening of
  the primary star and low eccentricity of the current binary orbit),
  we believe that the most probable (but not the only) explanation
  is the tidal evolution of a close binary within a primordial triple
  system (possibly after a period of Kozai-Lidov oscillations), leading
  to merger approximately 1 Gyr ago. This star appears to be a future
  blue straggler that is being revealed as the cluster ages and the most
  massive main-sequence stars die out. <P />Based on observations made at
  Kitt Peak National Observatory, National Optical Astronomy Observatory,
  which is operated by the Association of Universities for Research
  in Astronomy (AURA) under a cooperative agreement with the National
  Science Foundation; with the Tillinghast Reflector Echelle Spectrograph
  (TRES) on the 1.5 m Tillinghast telescope, located at the Smithsonian
  Astrophysical Observatory’s Fred L. Whipple Observatory on Mt. Hopkins
  in Arizona; the HARPS-N spectrograph on the Italian Telescopio Nazionale
  Galileo (TNG), operated on the island of La Palma by the INAF Fundacion
  Galileo Galilei (Spanish Observatory of Roque de los Muchachos of the
  IAC); and the Las Cumbres Observatory Global Telescope network.

Title: Extinction Maps and Dust-to-gas Ratios in Nearby Galaxies
    with LEGUS
Authors: Kahre, L.; Walterbos, R. A.; Kim, H.; Thilker, D.; Calzetti,
   D.; Lee, J. C.; Sabbi, E.; Ubeda, L.; Aloisi, A.; Cignoni, M.; Cook,
   D. O.; Dale, D. A.; Elmegreen, B. G.; Elmegreen, D. M.; Fumagalli,
   M.; Gallagher, J. S., III; Gouliermis, D. A.; Grasha, K.; Grebel,
   E. K.; Hunter, D. A.; Sacchi, E.; Smith, L. J.; Tosi, M.; Adamo, A.;
   Andrews, J. E.; Ashworth, G.; Bright, S. N.; Brown, T. M.; Chandar,
   R.; Christian, C.; de Mink, S. E.; Dobbs, C.; Evans, A. S.; Herrero,
   A.; Johnson, K. E.; Kennicutt, R. C.; Krumholz, M. R.; Messa, M.;
   Nair, P.; Nota, A.; Pellerin, A.; Ryon, J. E.; Schaerer, D.; Shabani,
   F.; Van Dyk, S. D.; Whitmore, B. C.; Wofford, A.
Bibcode: 2018ApJ...855..133K
Altcode: 2018arXiv180206915K
  We present a study of the dust-to-gas ratios in five nearby
  galaxies: NGC 628 (M74), NGC 6503, NGC 7793, UGC 5139 (Holmberg I),
  and UGC 4305 (Holmberg II). Using Hubble Space Telescope broadband
  WFC3/UVIS UV and optical images from the Treasury program Legacy
  ExtraGalactic UV Survey (LEGUS) combined with archival HST/Advanced
  Camera for Surveys data, we correct thousands of individual stars
  for extinction across these five galaxies using an isochrone-matching
  (reddening-free Q) method. We generate extinction maps for each galaxy
  from the individual stellar extinctions using both adaptive and fixed
  resolution techniques and correlate these maps with neutral H I and CO
  gas maps from the literature, including the H I Nearby Galaxy Survey
  and the HERA CO-Line Extragalactic Survey. We calculate dust-to-gas
  ratios and investigate variations in the dust-to-gas ratio with galaxy
  metallicity. We find a power-law relationship between dust-to-gas
  ratio and metallicity, consistent with other studies of dust-to-gas
  ratio compared to metallicity. We find a change in the relation when
  H<SUB>2</SUB> is not included. This implies that underestimation of
  {N}<SUB>{{{H</SUB>}}<SUB>2</SUB>} in low-metallicity dwarfs from a
  too-low CO-to-H<SUB>2</SUB> conversion factor X <SUB>CO</SUB> could have
  produced too low a slope in the derived relationship between dust-to-gas
  ratio and metallicity. We also compare our extinctions to those derived
  from fitting the spectral energy distribution (SED) using the Bayesian
  Extinction and Stellar Tool for NGC 7793 and find systematically lower
  extinctions from SED fitting as compared to isochrone matching.

Title: The Resolved Stellar Populations in the LEGUS Galaxies1
Authors: Sabbi, E.; Calzetti, D.; Ubeda, L.; Adamo, A.; Cignoni,
   M.; Thilker, D.; Aloisi, A.; Elmegreen, B. G.; Elmegreen, D. M.;
   Gouliermis, D. A.; Grebel, E. K.; Messa, M.; Smith, L. J.; Tosi, M.;
   Dolphin, A.; Andrews, J. E.; Ashworth, G.; Bright, S. N.; Brown, T. M.;
   Chandar, R.; Christian, C.; Clayton, G. C.; Cook, D. O.; Dale, D. A.;
   de Mink, S. E.; Dobbs, C.; Evans, A. S.; Fumagalli, M.; Gallagher,
   J. S., III; Grasha, K.; Herrero, A.; Hunter, D. A.; Johnson, K. E.;
   Kahre, L.; Kennicutt, R. C.; Kim, H.; Krumholz, M. R.; Lee, J. C.;
   Lennon, D.; Martin, C.; Nair, P.; Nota, A.; Östlin, G.; Pellerin,
   A.; Prieto, J.; Regan, M. W.; Ryon, J. E.; Sacchi, E.; Schaerer,
   D.; Schiminovich, D.; Shabani, F.; Van Dyk, S. D.; Walterbos, R.;
   Whitmore, B. C.; Wofford, A.
Bibcode: 2018ApJS..235...23S
Altcode: 2018arXiv180105467S
  The Legacy ExtraGalactic UV Survey (LEGUS) is a multiwavelength Cycle 21
  Treasury program on the Hubble Space Telescope. It studied 50 nearby
  star-forming galaxies in 5 bands from the near-UV to the I-band,
  combining new Wide Field Camera 3 observations with archival Advanced
  Camera for Surveys data. LEGUS was designed to investigate how star
  formation occurs and develops on both small and large scales, and how
  it relates to the galactic environments. In this paper we present the
  photometric catalogs for all the apparently single stars identified
  in the 50 LEGUS galaxies. Photometric catalogs and mosaicked images
  for all filters are available for download. We present optical and
  near-UV color-magnitude diagrams for all the galaxies. For each galaxy
  we derived the distance from the tip of the red giant branch. We then
  used the NUV color-magnitude diagrams to identify stars more massive
  than 14 M <SUB>⊙</SUB>, and compared their number with the number of
  massive stars expected from the GALEX FUV luminosity. Our analysis shows
  that the fraction of massive stars forming in star clusters and stellar
  associations is about constant with the star formation rate. This lack
  of a relation suggests that the timescale for evaporation of unbound
  structures is comparable or longer than 10 Myr. At low star formation
  rates this translates to an excess of mass in clustered environments
  as compared to model predictions of cluster evolution, suggesting that
  a significant fraction of stars form in unbound systems. <P />Based
  on observations with the NASA/ESA Hubble Space Telescope, obtained at
  the Space Telescope Science Institute, which is operated by AURA Inc.,
  under NASA contract NAS 5-26555.

Title: A High-precision Trigonometric Parallax to an Ancient
    Metal-poor Globular Cluster
Authors: Brown, T. M.; Casertano, S.; Strader, J.; Riess, A.;
   VandenBerg, D. A.; Soderblom, D. R.; Kalirai, J.; Salinas, R.
Bibcode: 2018ApJ...856L...6B
Altcode: 2018arXiv180302927B
  Using the Wide Field Camera 3 (WFC3) on the Hubble Space Telescope
  (HST), we have obtained a direct trigonometric parallax for the
  nearest metal-poor globular cluster, NGC 6397. Although trigonometric
  parallaxes have been previously measured for many nearby open clusters,
  this is the first parallax for an ancient metal-poor population—one
  that is used as a fundamental template in many stellar population
  studies. This high-precision measurement was enabled by the HST/WFC3
  spatial-scanning mode, providing hundreds of astrometric measurements
  for dozens of stars in the cluster and also for Galactic field stars
  along the same sightline. We find a parallax of 0.418 ± 0.013 ±
  0.018 mas (statistical, systematic), corresponding to a true distance
  modulus of 11.89 ± 0.07 ± 0.09 mag (2.39 ± 0.07 ± 0.10 kpc). The
  V luminosity at the stellar main-sequence turnoff implies an absolute
  cluster age of 13.4 ± 0.7 ± 1.2 Gyr. <P />Based on observations
  made with the NASA/ESA Hubble Space Telescope, obtained at the Space
  Telescope Science Institute, which is operated by the Association of
  Universities for Research in Astronomy, Inc., under NASA contract NAS
  5-26555. These observations are associated with programs GO-13817,
  GO-14336, and GO-14773.

Title: The crucial role of ground-based, Doppler measurements for
    the future of exoplanet science
Authors: Steffen, Jason H.; Plavchan, Peter; Brown, Timothy; Ford,
   Eric B.; Howard, Andrew W.; Jang-Condell, Hannah; Latham, David W.;
   Lissauer, Jack J.; Nelson, Benjamin E.; Newman, Patrick; Ragozzine,
   Darin
Bibcode: 2018arXiv180306057S
Altcode:
  We outline the important role that ground-based, Doppler monitoring
  of exoplanetary systems will play in advancing our theories of planet
  formation and dynamical evolution. A census of planetary systems
  requires a well designed survey to be executed over the course of a
  decade or longer. A coordinated survey to monitor several thousand
  targets each at ~1000 epochs (~3-5 million new observations) will
  require roughly 40 dedicated spectrographs. We advocate for improvements
  in data management, data sharing, analysis techniques, and software
  testing, as well as possible changes to the funding structures for
  exoplanet science.

Title: NRES: The Network of Robotic Echelle Spectrographs
Authors: Siverd, Robert; Brown, Tim; Henderson, Todd; Hygelund, John;
   Barnes, Stuart; de Vera, Jon; Eastman, Jason; Kirby, Annie; Smith,
   Cary; Taylor, Brook; Tufts, Joseph; van Eyken, Julian
Bibcode: 2018AAS...23115224S
Altcode:
  Las Cumbres Observatory (LCO) is building the Network of Robotic Echelle
  Spectrographs (NRES), which will consist of four (up to six in the
  future) identical, optical (390 - 860 nm) high-precision spectrographs,
  each fiber-fed simultaneously by up to two 1-meter telescopes and a
  Thorium-Argon calibration source. We plan to install one at up to 6
  observatory sites in the Northern and Southern hemispheres, creating
  a single, globally-distributed, autonomous spectrograph facility
  using up to ten 1-m telescopes. Simulations suggest we will achieve
  long-term radial velocity precision of 3 m/s in less than an hour
  for stars brighter than V = 11 or 12 once the system reaches full
  capability. Acting in concert, these four spectrographs will provide
  a new, unique facility for stellar characterization and precise radial
  velocities.Following a few months of on-sky evaluation at our BPL test
  facility, the first spectrograph unit was shipped to CTIO in late 2016
  and installed in March 2017. After several more months of additional
  testing and commissioning, regular science operations began with this
  node in September 2017. The second NRES spectrograph was installed at
  McDonald Observatory in September 2017 and released to the network after
  its own brief commissioning period, extending spectroscopic capability
  to the Northern hemisphere. The third NRES spectrograph was installed at
  SAAO in November 2017 and released to our science community just before
  year's end. The fourth NRES unit shipped in October and is currently
  en route to Wise Observatory in Israel with an expected release to
  the science community in early 2018.We will briefly overview the LCO
  telescope network, the NRES spectrograph design, the advantages it
  provides, and development challenges we encountered along the way. We
  will further discuss real-world performance from our first three units,
  initial science results, and the ongoing software development effort
  needed to automate such a facility for a wide array of science cases.

Title: A Universal Transition in Atmospheric Diffusion for Hot
    Subdwarfs Near 18,000 K
Authors: Brown, T. M.; Taylor, J. M.; Cassisi, S.; Sweigart, A. V.;
   Bellini, A.; Bedin, L. R.; Salaris, M.; Renzini, A.; Dalessandro, E.
Bibcode: 2017ApJ...851..118B
Altcode: 2017arXiv171108036B
  In the color-magnitude diagrams of globular clusters, when the
  locus of stars on the horizontal branch extends to hot temperatures,
  discontinuities are observed at colors corresponding to ∼12,000 and
  ∼18,000 K. The former is the “Grundahl jump” that is associated
  with the onset of radiative levitation in the atmospheres of hot
  subdwarfs. The latter is the “Momany jump” that has remained
  unexplained. Using the Space Telescope Imaging Spectrograph on
  the Hubble Space Telescope, we have obtained ultraviolet and blue
  spectroscopy of six hot subdwarfs straddling the Momany jump in the
  massive globular cluster ω Cen. By comparison to model atmospheres
  and synthetic spectra, we find that the feature is due primarily to a
  decrease in atmospheric Fe for stars hotter than the feature, amplified
  by the temperature dependence of the Fe absorption at these effective
  temperatures. <P />Based on observations made with the NASA/ESA Hubble
  Space Telescope, obtained at the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in
  Astronomy, Inc., under NASA contract NAS 5-26555. These observations
  are associated with program GO-14759.

Title: Christopherwharrop/Rocoto: Rocoto 1.2.4
Authors: Harrop, Christopher; samtrahan; christinaholt; Brown, Timothy
Bibcode: 2017zndo....890939H
Altcode:
  This release contains a number of bug fixes and some new features. See
  RELEASE_NOTES.md for details.

Title: The Hubble Space Telescope "Program of Last Resort"
Authors: Bellini, A.; Grogin, N. A.; Hathi, N.; Brown, T. M.
Bibcode: 2017acs..rept...12B
Altcode:
  Every year, the Space Telescope Science Institute allocates over
  3000 orbits of Hubble time to approved Guest Observer, Snapshot, and
  Director's Discretionary programs. The many targets among all these
  programs are not distributed uniformly around the celestial sphere,
  and most targets have observational constraints that limit their
  schedulability to something less than the entire year. Despite the best
  efforts of the Hubble schedulers to allocate every last orbit, a small
  but persistent fraction ( 2 - 3%) of the orbits go unused. Salvaging
  this unused observing time presents an opportunity for the Institute to
  benefit the astronomy community. The Institute's Hubble Mission Office
  has initiated a pilot, ultra-low priority SNAP program (14840, PI:
  Bellini) in Cycle 24, with the goal of taking useful data in Hubble
  orbits that absolutely no other program is able to use. The initial
  target list comprises 500 moderately large, bright NGC/IC galaxies that
  were not previously imaged by HST in V -like filters. As of September
  2017, over 100 galaxies have been observed as part of this program
  (≥ 2 galaxies per week). This document focuses on the data quality
  of the first 10 months of observations. All data taken through the
  SNAP-14840 program are intended for legacy science only, and STScI
  strongly encourage the astronomical community to use these data for
  science purposes.

Title: NRES: The Network of Robotic Echelle Spectrographs
Authors: Siverd, Robert; Brown, Timothy M.; Henderson, Todd; Hygelund,
   John; Barnes, Stuart; Bowman, Mark; De Vera, Jon; Eastman, Jason D.;
   Kirby, Annie; Norbury, Martin; Smith, Cary; Taylor, Brook; Tufts,
   Joseph; Van Eyken, Julian C.
Bibcode: 2017AAS...23010207S
Altcode:
  Las Cumbres Observatory (LCO) is building the Network of Robotic Echelle
  Spectrographs (NRES), which will consist of four to six identical,
  optical (390 - 860 nm) high-precision spectrographs, each fiber-fed
  simultaneously by up to two 1-meter telescopes and a Thorium-Argon
  calibration source. We plan to install one at up to 6 observatory
  sites in the Northern and Southern hemispheres, creating a single,
  globally-distributed, autonomous spectrograph facility using up to ten
  1-m telescopes. Simulations suggest we will achieve long-term radial
  velocity precision of 3 m/s in less than an hour for stars brighter
  than V = 11 or 12. Following a few months of on-sky evaluation at our
  BPL test facility, the first spectrograph unit was shipped to CTIO in
  late 2016 and installed in March 2017. Barring serious complications, we
  expect regular scheduled science observing to begin in mid-2017. Three
  additional units are in building or testing phases and slated for
  deployment in late 2017. Acting in concert, these four spectrographs
  will provide a new, unique facility for stellar characterization and
  precise radial velocities. We will briefly overview the LCO telescope
  network, the NRES spectrograph design, the advantages it provides,
  and development challenges we encountered along the way. We will
  further discuss real-world performance from our first unit, initial
  science results, and the ongoing software development effort needed
  to automate such a facility for a wide array of science cases.

Title: Legacy ExtraGalactic UV Survey with The Hubble Space Telescope:
    Stellar Cluster Catalogs and First Insights Into Cluster Formation
    and Evolution in NGC 628
Authors: Adamo, A.; Ryon, J. E.; Messa, M.; Kim, H.; Grasha, K.; Cook,
   D. O.; Calzetti, D.; Lee, J. C.; Whitmore, B. C.; Elmegreen, B. G.;
   Ubeda, L.; Smith, L. J.; Bright, S. N.; Runnholm, A.; Andrews, J. E.;
   Fumagalli, M.; Gouliermis, D. A.; Kahre, L.; Nair, P.; Thilker, D.;
   Walterbos, R.; Wofford, A.; Aloisi, A.; Ashworth, G.; Brown, T. M.;
   Chandar, R.; Christian, C.; Cignoni, M.; Clayton, G. C.; Dale, D. A.;
   de Mink, S. E.; Dobbs, C.; Elmegreen, D. M.; Evans, A. S.; Gallagher,
   J. S., III; Grebel, E. K.; Herrero, A.; Hunter, D. A.; Johnson, K. E.;
   Kennicutt, R. C.; Krumholz, M. R.; Lennon, D.; Levay, K.; Martin,
   C.; Nota, A.; Östlin, G.; Pellerin, A.; Prieto, J.; Regan, M. W.;
   Sabbi, E.; Sacchi, E.; Schaerer, D.; Schiminovich, D.; Shabani, F.;
   Tosi, M.; Van Dyk, S. D.; Zackrisson, E.
Bibcode: 2017ApJ...841..131A
Altcode: 2017arXiv170501588A
  We report the large effort that is producing comprehensive high-level
  young star cluster (YSC) catalogs for a significant fraction of galaxies
  observed with the Legacy ExtraGalactic UV Survey (LEGUS) Hubble treasury
  program. We present the methodology developed to extract cluster
  positions, verify their genuine nature, produce multiband photometry
  (from NUV to NIR), and derive their physical properties via spectral
  energy distribution fitting analyses. We use the nearby spiral galaxy
  NGC 628 as a test case for demonstrating the impact that LEGUS will
  have on our understanding of the formation and evolution of YSCs and
  compact stellar associations within their host galaxy. Our analysis
  of the cluster luminosity function from the UV to the NIR finds a
  steepening at the bright end and at all wavelengths suggesting a dearth
  of luminous clusters. The cluster mass function of NGC 628 is consistent
  with a power-law distribution of slopes ∼ -2 and a truncation of a
  few times 10<SUP>5</SUP> {M}<SUB>⊙ </SUB>. After their formation,
  YSCs and compact associations follow different evolutionary paths. YSCs
  survive for a longer time frame, confirming their being potentially
  bound systems. Associations disappear on timescales comparable to
  hierarchically organized star-forming regions, suggesting that they are
  expanding systems. We find mass-independent cluster disruption in the
  inner region of NGC 628, while in the outer part of the galaxy there
  is little or no disruption. We observe faster disruption rates for
  low mass (≤10<SUP>4</SUP> {M}<SUB>⊙ </SUB>) clusters, suggesting
  that a mass-dependent component is necessary to fully describe the YSC
  disruption process in NGC 628. <P />Based on observations obtained with
  the NASA/ESA Hubble Space Telescope, at the Space Telescope Science
  Institute, which is operated by the Association of Universities for
  Research in Astronomy, Inc., under NASA contract NAS 5-26555.

Title: Just how hot are the ω Centauri extreme horizontal branch
    pulsators?
Authors: Latour, M.; Randall, S. K.; Chayer, P.; Fontaine, G.;
   Calamida, A.; Ely, J.; Brown, T. M.; Landsman, W.
Bibcode: 2017A&A...600A.130L
Altcode: 2017arXiv170207609L
  Context. Past studies based on optical spectroscopy suggest that the
  five <ASTROBJ>ω Cen</ASTROBJ> pulsators form a rather homogeneous group
  of hydrogen-rich subdwarf O stars with effective temperatures of around
  50 000 K. This places the stars below the red edge of the theoretical
  instability strip in the log g-T<SUB>eff</SUB> diagram, where no
  pulsation modes are predicted to be excited. <BR /> Aims: Our goal is
  to determine whether this temperature discrepancy is real, or whether
  the stars' effective temperatures were simply underestimated. <BR />
  Methods: We present a spectral analysis of two rapidly pulsating extreme
  horizontal branch (EHB) stars found in <ASTROBJ>ω Cen</ASTROBJ>. We
  obtained Hubble Space Telescope/COS UV spectra of two ω Cen pulsators,
  V1 and V5, and used the ionisation equilibrium of UV metallic lines
  to better constrain their effective temperatures. As a by-product we
  also obtained FUV lightcurves of the two pulsators. <BR /> Results:
  Using the relative strength of the N iv and N v lines as a temperature
  indicator yields T<SUB>eff</SUB> values close to 60 000 K, significantly
  hotter than the temperatures previously derived. From the FUV light
  curves we were able to confirm the main pulsation periods known from
  optical data. <BR /> Conclusions: With the UV spectra indicating
  higher effective temperatures than previously assumed, the sdO stars
  would now be found within the predicted instability strip. Such higher
  temperatures also provide consistent spectroscopic masses for both the
  cool and hot EHB stars of our previously studied sample. <P />Based
  on observations (proposal GO-13707) with the NASA/ESA Hubble Space
  Telescope, obtained at the Space Telescope Science Institute, which is
  operated by the Association of Universities for Research in Astronomy,
  Inc., under NASA contract NAS5-26666.

Title: The Hubble Space Telescope UV Legacy Survey of Galactic
    globular clusters - XI. The horizontal branch in NGC 6388 and NGC 6441
Authors: Tailo, M.; D'Antona, F.; Milone, A. P.; Bellini, A.; Ventura,
   P.; Di Criscienzo, M.; Cassisi, S.; Piotto, G.; Salaris, M.; Brown,
   T. M.; Vesperini, E.; Bedin, L. R.; Marino, A. F.; Nardiello, D.;
   Anderson, J.
Bibcode: 2017MNRAS.465.1046T
Altcode: 2016arXiv161008264T
  The Hubble Space Telescope UV Legacy survey of Galactic globular
  clusters (GC) is characterizing many different aspects of their multiple
  stellar populations. The `Grundahl-jump' (G-jump) is a discontinuity in
  ultraviolet brightness of blue horizontal branch (HB) stars, signalling
  the onset of radiative metal levitation. The HB Legacy data confirmed
  that the G-jump is located at the same T<SUB>eff</SUB> (≃11 500 K) in
  nearly all clusters. The only exceptions are the metal-rich clusters NGC
  6388 and NGC 6441, where the G-jump occurs at T<SUB>eff</SUB> ≃ 13-14
  000 K. We compute synthetic HB models based on new evolutionary tracks
  including the effect of helium diffusion, and approximately accounting
  for the effect of metal levitation in a stable atmosphere. Our models
  show that the G-jump location depends on the interplay between the
  time-scale of diffusion and the time-scale of the evolution in the
  T<SUB>eff</SUB> range 11 500 K≲T<SUB>eff</SUB>≲14 000 K. The
  G-jump becomes hotter than 11 500 K only for stars that have, in this
  T<SUB>eff</SUB> range, a helium mass fraction Y ≳ 0.35. Similarly
  high Y values are also consistent with the modelling of the HB in NGC
  6388 and NGC 6441. In these clusters, we predict that a significant
  fraction of HB stars show helium in their spectra above 11 500 K,
  and full helium settling should only be found beyond the hotter G-jump.

Title: The Hubble Space Telescope UV Legacy Survey of Galactic
    globular clusters - IX. The Atlas of multiple stellar populations
Authors: Milone, A. P.; Piotto, G.; Renzini, A.; Marino, A. F.; Bedin,
   L. R.; Vesperini, E.; D'Antona, F.; Nardiello, D.; Anderson, J.; King,
   I. R.; Yong, D.; Bellini, A.; Aparicio, A.; Barbuy, B.; Brown, T. M.;
   Cassisi, S.; Ortolani, S.; Salaris, M.; Sarajedini, A.; van der Marel,
   R. P.
Bibcode: 2017MNRAS.464.3636M
Altcode: 2016MNRAS.tmp.1516M; 2016arXiv161000451M
  We use high-precision photometry of red-giant-branch (RGB) stars in
  57 Galactic globular clusters (GCs), mostly from the `Hubble Space
  Telescope (HST) UV Legacy Survey of Galactic GCs', to identify and
  characterize their multiple stellar populations. For each cluster the
  pseudo-two-colour diagram (or `chromosome map') is presented, built
  with a suitable combination of stellar magnitudes in the F275W, F336W,
  F438W, and F814W filters that maximizes the separation between multiple
  populations. In the chromosome map of most GCs (type-I clusters),
  stars separate in two distinct groups that we identify with the first
  (1G) and the second generation (2G). This identification is further
  supported by noticing that 1G stars have primordial (oxygen-rich,
  sodium-poor) chemical composition, whereas 2G stars are enhanced in
  sodium and depleted in oxygen. This 1G-2G separation is not possible
  for a few GCs where the two sequences have apparently merged into an
  extended, continuous sequence. In some GCs (type-II clusters) the 1G
  and/or the 2G sequences appear to be split, hence displaying more
  complex chromosome maps. These clusters exhibit multiple subgiant
  branches (SGBs) also in purely optical colour-magnitude diagrams,
  with the fainter SGB joining into a red RGB which is populated by
  stars with enhanced heavy-element abundance. We measure the RGB width
  by using appropriate colours and pseudo-colours. When the metallicity
  dependence is removed, the RGB width correlates with the cluster
  mass. The fraction of 1G stars ranges from ∼8 per cent to ∼67
  per cent and anticorrelates with the cluster mass, indicating that
  incidence and complexity of the multiple population phenomenon both
  increase with cluster mass.

Title: The Hubble Space Telescope UV Legacy Survey of Galactic
    Globular Clusters. VIII. Preliminary Public Catalog Release
Authors: Soto, M.; Bellini, A.; Anderson, J.; Piotto, G.; Bedin,
   L. R.; van der Marel, R. P.; Milone, A. P.; Brown, T. M.; Cool, A. M.;
   King, I. R.; Sarajedini, A.; Granata, V.; Cassisi, S.; Aparicio, A.;
   Hidalgo, S.; Ortolani, S.; Nardiello, D.
Bibcode: 2017AJ....153...19S
Altcode: 2016arXiv161200714S
  The Hubble Space Telescope (HST) UV Legacy Survey of Galactic
  Globular Clusters (GO-13297) has been specifically designed
  to complement the existing F606W and F814W observations of the
  Advanced Camera for Surveys (ACS) Globular Cluster Survey (GO-10775)
  by observing the most accessible 47 of the previous survey’s 65
  clusters in three WFC3/UVIS filters F275W, F336W, and F438W. The
  new survey also adds super-solar metallicity open cluster NGC 6791
  to increase the metallicity diversity. The combined survey provides
  a homogeneous 5-band data set that can be used to pursue a broad
  range of scientific investigations. In particular, the chosen UV
  filters allow the identification of multiple stellar populations by
  targeting the regions of the spectrum that are sensitive to abundance
  variations in C, N, and O. In order to provide the community with
  uniform preliminary catalogs, we have devised an automated procedure
  that performs high-quality photometry on the new UV observations (along
  with similar observations of seven other programs in the archive). This
  procedure finds and measures the potential sources on each individual
  exposure using library point-spread functions and cross-correlates
  these observations with the original ACS-Survey catalog. The catalog
  of 57 clusters we publish here will be useful to identify stars in
  the different stellar populations, in particular for spectroscopic
  follow-up. Eventually, we will construct a more sophisticated catalog
  and artificial-star tests based on an optimal reduction of the UV
  survey data, but the catalogs presented here give the community the
  chance to make early use of this HST Treasury survey.

Title: NRES: the network of robotic Echelle spectrographs
Authors: Siverd, Robert J.; Brown, Timothy M.; Hygelund, John;
   Henderson, Todd; Tufts, Joseph R.; Eastman, Jason D.; van Eyken,
   Julian; Barnes, Stuart
Bibcode: 2016SPIE.9908E..6XS
Altcode:
  Las Cumbres Observatory Global Network (LCOGT) is building the Network
  of Robotic Echelle Spectrographs (NRES), which will consist of six
  identical, optical (390 - 860 nm) high-precision spectrographs,
  each fiber-fed simultaneously by up to two 1-meter telescopes and a
  thorium argon calibration source. We plan to install one at up to 6
  observatory sites in the Northern and Southern hemispheres, creating a
  single, globally-distributed, autonomous spectrograph facility using
  up to twelve 1-meter telescopes. Simulations suggest we will achieve
  long-term radial velocity precision of 3 m/s in less than an hour for
  stars brighter than V = 12. We have been funded with NSF MRI and ATI
  grants, and expect our first spectrograph to be deployed in fall 2016,
  with the full network operation of 5 or 6 units beginning in 2017. We
  will briefly overview the NRES design, goals, robotic operation,
  and status. In addition, we will discuss early results from our
  prototype spectrograph, the laboratory and on-sky performance of our
  first production unit, and the ongoing software development effort to
  bring this resource online.

Title: Discovery of a Long-Period Eclipsing Binary in M67
Authors: Sandquist, Eric L.; Latham, David W.; Mathieu, Robert D.;
   Vanderburg, Andrew; Brown, Timothy M.; M67 K2 Team
Bibcode: 2016AAS...22811701S
Altcode:
  We announce the detection of an eclipsing binary (WOCS 12009 / Sanders
  1247) near the turnoff of the heavily-studied old open cluster M67
  using K2 Campaign 5 data. The object was previously known to be
  a double-lined spectroscopic binary, and the orbit period (69.75 d)
  agrees with the photometric period. We present a preliminary analysis of
  the K2 photometry, multi-band ground-based photometry of the eclipses,
  and extensive radial velocity observations of the two stars. Precise
  measurements of the pair will begin to provide mass and radius scales
  for cluster stars, and will constrain the age of this iconic open
  cluster.We gratefully acknowledge support from NASA through grant
  NNX15AW24A to R.D.M.

Title: NRES: The Network of Robotic Echelle Spectrographs
Authors: Siverd, Robert; Brown, Timothy M.; Henderson, Todd; Hygelund,
   John; Tufts, Joseph; Eastman, Jason; Barnes, Stuart; Van Eyken,
   Julian C.
Bibcode: 2016AAS...22840101S
Altcode:
  Las Cumbres Observatory Global Network (LCOGT) is building the Network
  of Robotic Echelle Spectrographs (NRES), which will consist of six
  identical, optical (390 - 860 nm) high-precision spectrographs, each
  fiber-fed simultaneously by up to two 1-meter telescopes and a thorium
  argon calibration source. We plan to install one at up to 6 observatory
  sites in the Northern and Southern hemispheres, creating a single,
  globally-distributed, autonomous spectrograph facility using up to
  twelve 1-m telescopes. Simulations suggest we will achieve long-term
  radial velocity precision of 3 m/s in less than an hour for stars
  brighter than V = 12. We have been funded with NSF MRI and ATI grants,
  and expect to deploy the first spectrograph in fall 2016, with the full
  network operation of 5 or 6 units beginning in 2017. We will briefly
  overview the NRES design, goals, robotic operation, and status. In
  addition, we will discuss early results from our prototype spectrograph,
  the laboratory and on-sky performance of our first production unit,
  initial science results, and the ongoing software development effort
  to bring this resource online.

Title: The Hubble Space Telescope UV Legacy Survey of Galactic
    Globular Clusters. VII. Implications from the Nearly Universal Nature
    of Horizontal Branch Discontinuities
Authors: Brown, T. M.; Cassisi, S.; D'Antona, F.; Salaris, M.; Milone,
   A. P.; Dalessandro, E.; Piotto, G.; Renzini, A.; Sweigart, A. V.;
   Bellini, A.; Ortolani, S.; Sarajedini, A.; Aparicio, A.; Bedin, L. R.;
   Anderson, J.; Pietrinferni, A.; Nardiello, D.
Bibcode: 2016ApJ...822...44B
Altcode: 2016arXiv160307651B
  The UV-initiative Hubble Space Telescope Treasury survey of Galactic
  globular clusters provides a new window into the phenomena that shape
  the morphological features of the horizontal branch (HB). Using this
  large and homogeneous catalog of UV and blue photometry, we demonstrate
  that the HB exhibits discontinuities that are remarkably consistent
  in color (effective temperature). This consistency is apparent even
  among some of the most massive clusters hosting multiple distinct
  sub-populations (such as NGC 2808, ω Cen, and NGC 6715), demonstrating
  that these phenomena are primarily driven by atmospheric physics
  that is independent of the underlying population properties. However,
  inconsistencies arise in the metal-rich clusters NGC 6388 and NGC 6441,
  where the discontinuity within the blue HB (BHB) distribution shifts
  ∼1000-2000 K hotter. We demonstrate that this shift is likely due to
  a large helium enhancement in the BHB stars of these clusters, which in
  turn affects the surface convection and evolution of such stars. Our
  survey also increases the number of Galactic globular clusters known
  to host blue-hook stars (also known as late hot flashers) from 6
  to 23 clusters. These clusters are biased toward the bright end of
  the globular cluster luminosity function, confirming that blue-hook
  stars tend to form in the most massive clusters with significant
  self-enrichment. <P />Based on observations made with the NASA/ESA
  Hubble Space Telescope, obtained at the Space Telescope Science
  Institute, which is operated by the Association of Universities for
  Research in Astronomy, Inc., under NASA contract NAS 5-26555. These
  observations are associated with program GO-13297.

Title: VizieR Online Data Catalog: Photometry and redshifts of
    galaxies in the UDF (Rafelski+, 2015)
Authors: Rafelski, M.; Teplitz, H. I.; Gardner, J. P.; Coe, D.; Bond,
   N. A.; Koekemoer, A. M.; Grogin, N.; Kurczynski, P.; McGrath, E. J.;
   Bourque, M.; Atek, H.; Brown, T. M.; Colbert, J. W.; Codoreanu,
   A.; Ferguson, H. C.; Finkelstein, S. L.; Gawiser, E.; Giavalisco,
   M.; Gronwall, C.; Hanish, D. J.; Lee, K. -S.; Mehta, V.; de Mello,
   D. F.; Ravindranath, S.; Ryan, R. E.; Scarlata, C.; Siana, B.; Soto,
   E.; Voyer, E. N.
Bibcode: 2016yCat..51500031R
Altcode:
  We present photometry and derived redshifts from up to eleven bandpasses
  for 9927 galaxies in the Hubble Ultra Deep field (UDF), covering
  an observed wavelength range from the near-ultraviolet (NUV) to the
  near-infrared (NIR) with Hubble Space Telescope (HST) observations. <P
  />The NUV coverage of the UDF (UVUDF) is comprised of three WFC3-UVIS
  filters: F225W, F275W, and F336W. The UVUDF observations were obtained
  in 2012. The optical data are covered by the four original Advanced
  Camera for Surveys (ACS) optical filters: F435W, F606W, F775W, and
  F850LP. The deep NIR coverage includes four WFC3-IR filters: F105W,
  F125W, F140W, and F160W obtained in the UDF09 and UDF12 programs
  (Oesch et al. 2010ApJ...709L..21O, 2010ApJ...709L..16O; Bouwens et
  al. 2011ApJ...737...90B; Ellis et al. 2013ApJ...763L...7E; Koekemoer
  et al. 2013ApJS..209....3K). The entire field is also covered by three
  of the four WFC3-IR filters (F105W, F125W, and F160W) in the CANDELS
  GOODS-S observations (Grogin et al. 2011ApJS..197...35G; Koekemoer et
  al. 2011ApJS..197...36K). <P />(2 data files).

Title: NRES: The Network of Robotic Echelle Spectrographs
Authors: Siverd, Robert; Brown, Timothy M.; Hygelund, John; Henderson,
   Todd; Tufts, Joseph; Eastman, Jason; Van Eyken, Julian C.; Barnes,
   Stuart
Bibcode: 2016AAS...22711307S
Altcode:
  Las Cumbres Observatory Global Network (LCOGT) is building the Network
  of Robotic Echelle Spectrographs (NRES), which will consist of six
  identical, optical (390 - 860 nm) high-precision spectrographs, each
  fiber-fed simultaneously by up to two 1-meter telescopes and a thorium
  argon calibration source. We plan to install one at up to 6 observatory
  sites in the Northern and Southern hemispheres, creating a single,
  globally-distributed, autonomous spectrograph facility using up to
  twelve 1-m telescopes. Simulations suggest we will achieve long-term
  radial velocity precision of 3 m/s in less than an hour for stars
  brighter than V = 12. We have been funded with NSF MRI and ATI grants,
  and expect our first spectrograph to be deployed in early 2016, with
  the full network operation of 5 or 6 units beginning in 2017. We
  will briefly overview the NRES design, goals, robotic operation,
  and status. In addition, we will discuss early results from our
  prototype spectrograph, the laboratory and on-sky performance of our
  first production unit, and the ongoing software development effort to
  bring this resource online.

Title: Follow-up of K2 planet candiates with the LCOGT network
Authors: Dragomir, Diana; Bayliss, Daniel; Colón, Knicole; Cochran,
   William; Zhou, George; Brown, Timothy; Shporer, Avi; Espinoza, Nestor;
   Fulton, Benjamin
Bibcode: 2015ESS.....310303D
Altcode:
  K2 has proven to be an outstanding successor to the Kepler mission. It
  has already revealed dozens of new planet candidates, and unlike those
  found by the primary mission, many of these systems’ host stars are
  sufficiently bright to allow extensive follow-up observations. This is
  especially important since each of the K2 observing campaigns are only
  ~80 days long, leaving the community with the discovery of exciting
  new systems but often not enough time coverage to enable a thorough
  characterization of these systems.We are leading a large effort
  to observe K2 transiting planet candidates with the LCOGT telescope
  network. LCOGT’s longitudinal coverage, multiple identical telescopes
  per site and automated queue observing make it an ideal facility for
  fast, high-precision and multi-color follow-up. Our program focuses on
  specific aspects of K2 follow-up for which the network is especially
  powerful: period determination for candidates with fewer than three
  K2 transits; transit timing variation monitoring to measure planetary
  masses, orbital parameters and to search for additional planets in
  multiple systems; and multi-color photometry to vet planet candidates
  and carry-out preliminary atmospheric spectroscopy.We will present
  new results for a selection of systems observed so far through this
  program. These include K2-19, a multi-planet system extremely close
  to 3:2 resonance and experiencing transit timing variations with
  amplitudes as large as one hour; EPIC201702477, a long-period planet
  with only two K2 transits; WASP-47, a system hosting a hot Jupiter and
  two K2-discovered small planets; and EPIC201637175b, a disintegrating
  rocky planet.Our program demonstrates that LCOGT is uniquely positioned
  to be the primary ground-based photometric follow-up resource for K2
  exoplanet discoveries, but also for the numerous bright systems that
  will result from the TESS mission. LCOGT photometry complements ongoing
  radial velocity and atmospheric spectroscopy efforts to reveal a more
  complete picture of the bright, nearby exoplanet systems discovered
  by these missions.

Title: The Hubble Space Telescope UV Legacy Survey of Galactic
    Globular Clusters - V. Constraints on formation scenarios
Authors: Renzini, A.; D'Antona, F.; Cassisi, S.; King, I. R.; Milone,
   A. P.; Ventura, P.; Anderson, J.; Bedin, L. R.; Bellini, A.; Brown,
   T. M.; Piotto, G.; van der Marel, R. P.; Barbuy, B.; Dalessandro, E.;
   Hidalgo, S.; Marino, A. F.; Ortolani, S.; Salaris, M.; Sarajedini, A.
Bibcode: 2015MNRAS.454.4197R
Altcode: 2015arXiv151001468R
  We build on the evidence provided by our Legacy Survey of Galactic
  globular clusters (GC) to submit to a crucial test four scenarios
  currently entertained for the formation of multiple stellar generations
  in GCs. The observational constraints on multiple generations to be
  fulfilled are manifold, including GC specificity, ubiquity, variety,
  predominance, discreteness, supernova avoidance, p-capture processing,
  helium enrichment and mass budget. We argue that scenarios appealing to
  supermassive stars, fast rotating massive stars and massive interactive
  binaries violate in an irreparable fashion two or more among such
  constraints. Also the scenario appealing to asymptotic giant branch
  (AGB) stars as producers of the material for next generation stars
  encounters severe difficulties, specifically concerning the mass budget
  problem and the detailed chemical composition of second-generation
  stars. We qualitatively explore ways possibly allowing one to save
  the AGB scenario, specifically appealing to a possible revision of
  the cross-section of a critical reaction rate destroying sodium,
  or alternatively by a more extensive exploration of the vast
  parameter space controlling the evolutionary behaviour of AGB stellar
  models. Still, we cannot ensure success for these efforts and totally
  new scenarios may have to be invented to understand how GCs formed in
  the early Universe.

Title: The GIRAFFE Inner Bulge Survey (GIBS). II. Metallicity
    distributions and alpha element abundances at fixed Galactic latitude
Authors: Gonzalez, O. A.; Zoccali, M.; Vasquez, S.; Hill, V.; Rejkuba,
   M.; Valenti, E.; Rojas-Arriagada, A.; Renzini, A.; Babusiaux, C.;
   Minniti, D.; Brown, T. M.
Bibcode: 2015A&A...584A..46G
Altcode: 2015arXiv150802576G
  <BR /> Aims: We investigate metallicity and α-element abundance
  gradients along a Galactic longitude strip, at latitude b ~ -4°, with
  the aim of providing observational constraints for the structure and
  origin of the Milky Way bulge. <BR /> Methods: High-resolution (R ~
  22 500) spectra for 400 K giants, in four fields within -4.8° ≲ b
  ≲ -3.4° and -10° ≲ l ≲ +10°, were obtained within the GIRAFFE
  Inner Bulge Survey (GIBS) project. To this sample we added another
  ~400 stars in Baade's Window at (l,b) = (1°,-4°), observed with the
  identical instrumental configuration: FLAMES GIRAFFE in Medusa mode
  with HR13 setup. All target stars lie within the red clump of the bulge
  colour-magnitude diagram, thus minimising contamination from the disc or
  halo stars. The spectroscopic stellar surface parameters were derived
  with an automatic method based on the GALA code, while the [Ca/Fe]
  and [Mg/Fe] abundances as a function of [Fe/H] were derived through a
  comparison with the synthetic spectra using MOOG. We constructed the
  metallicity distributions for the entire sample, and for each field
  individually, in order to investigate the presence of gradients or
  field-to-field variations in the shape of the distributions. <BR />
  Results: The metallicity distributions in the five fields are consistent
  with being drawn from a single parent population, indicating the
  absence of a gradient along the major axis of the Galactic bar. The
  global metallicity distribution is nicely fitted by two Gaussians. The
  metal-poor component is rather broad, with a mean at ⟨ [Fe/H] ⟩ =
  -0.31 dex and σ = 0.31 dex. The metal-rich component is narrower, with
  mean ⟨ [Fe/H] ⟩ = + 0.26 and σ = 0.2 dex. The [Mg/Fe] ratio follows
  a tight trend with [Fe/H], with enhancement with respect to solar in
  the metal-poor regime similar to the value observed for giant stars in
  the local thick disc. [Ca/Fe] abundances follow a similar trend, but
  with a considerably larger scatter than [Mg/Fe]. A decrease in [Mg/Fe]
  is observed at [Fe/H] = -0.44 dex. This knee is in agreement with our
  previous bulge study of K-giants along the minor axis, but is 0.1 dex
  lower in metallicity than the value reported for the microlensed dwarf
  and subgiant stars in the bulge. We found no variation in α-element
  abundance distributions between different fields. <P />Based on
  observations taken with ESO telescopes at the La Silla Paranal
  Observatory under programme IDs 187.B-909(A) and 71.B-0196.Full
  Table 3 is only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/584/A46">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/584/A46</A>

Title: The Brightest Young Star Clusters in NGC 5253.
Authors: Calzetti, D.; Johnson, K. E.; Adamo, A.; Gallagher, J. S.,
   III; Andrews, J. E.; Smith, L. J.; Clayton, G. C.; Lee, J. C.;
   Sabbi, E.; Ubeda, L.; Kim, H.; Ryon, J. E.; Thilker, D.; Bright,
   S. N.; Zackrisson, E.; Kennicutt, R. C.; de Mink, S. E.; Whitmore,
   B. C.; Aloisi, A.; Chandar, R.; Cignoni, M.; Cook, D.; Dale, D. A.;
   Elmegreen, B. G.; Elmegreen, D. M.; Evans, A. S.; Fumagalli, M.;
   Gouliermis, D. A.; Grasha, K.; Grebel, E. K.; Krumholz, M. R.;
   Walterbos, R.; Wofford, A.; Brown, T. M.; Christian, C.; Dobbs, C.;
   Herrero, A.; Kahre, L.; Messa, M.; Nair, P.; Nota, A.; Östlin, G.;
   Pellerin, A.; Sacchi, E.; Schaerer, D.; Tosi, M.
Bibcode: 2015ApJ...811...75C
Altcode: 2015arXiv150804476C
  The nearby dwarf starburst galaxy NGC 5253 hosts a number of young,
  massive star clusters, the two youngest of which are centrally
  concentrated and surrounded by thermal radio emission (the “radio
  nebula”). To investigate the role of these clusters in the starburst
  energetics, we combine new and archival Hubble Space Telescope images
  of NGC 5253 with wavelength coverage from 1500 Å to 1.9 μm in 13
  filters. These include Hα, Pβ, and Pα, and the imaging from the
  Hubble Treasury Program LEGUS (Legacy Extragalactic UV Survey). The
  extraordinarily well-sampled spectral energy distributions enable
  modeling with unprecedented accuracy the ages, masses, and extinctions
  of the nine optically brightest clusters (M<SUB>V</SUB> &lt; -8.8)
  and the two young radio nebula clusters. The clusters have ages
  ∼1-15 Myr and masses ∼1 × 10<SUP>4</SUP>-2.5 × 10<SUP>5</SUP>
  M<SUB>⊙</SUB>. The clusters’ spatial location and ages indicate that
  star formation has become more concentrated toward the radio nebula
  over the last ∼15 Myr. The most massive cluster is in the radio
  nebula; with a mass ∼2.5 × 10<SUP>5</SUP> M<SUB>⊙</SUB> and an
  age ∼1 Myr, it is 2-4 times less massive and younger than previously
  estimated. It is within a dust cloud with A<SUB>V</SUB> ∼ 50 mag, and
  shows a clear near-IR excess, likely from hot dust. The second radio
  nebula cluster is also ∼1 Myr old, confirming the extreme youth of
  the starburst region. These two clusters account for about half of the
  ionizing photon rate in the radio nebula, and will eventually supply
  about 2/3 of the mechanical energy in present-day shocks. Additional
  sources are required to supply the remaining ionizing radiation, and may
  include very massive stars. <P />Based on observations obtained with
  the NASA/ESA Hubble Space Telescope, at the Space Telescope Science
  Institute, which is operated by the Association of Universities for
  Research in Astronomy, Inc., under NASA contract NAS 5-26555.

Title: New Insights on the Galactic Bulge Initial Mass Function
Authors: Calamida, A.; Sahu, K. C.; Casertano, S.; Anderson, J.;
   Cassisi, S.; Gennaro, M.; Cignoni, M.; Brown, T. M.; Kains, N.;
   Ferguson, H.; Livio, M.; Bond, H. E.; Buonanno, R.; Clarkson, W.;
   Ferraro, I.; Pietrinferni, A.; Salaris, M.; Valenti, J.
Bibcode: 2015ApJ...810....8C
Altcode: 2015arXiv150507128C
  We have derived the Galactic bulge initial mass function (IMF) of the
  Sagittarius Window Eclipsing Extrasolar Planet Search field in the
  mass range 0.15 \lt M/{M}<SUB>⊙ </SUB> 1.0, using deep photometry
  collected with the Advanced Camera for Surveys on the Hubble Space
  Telescope. Observations at several epochs, spread over 9 years, allowed
  us to separate the disk and bulge stars down to very faint magnitudes,
  F814W ≈ 26 mag, with a proper-motion accuracy better than 0.5 mas
  yr<SUP>-1</SUP> (20 km s<SUP>-1</SUP>). This allowed us to determine the
  IMF of the pure bulge component uncontaminated by disk stars for this
  low-reddening field in the Sagittarius window. In deriving the mass
  function, we took into account the presence of unresolved binaries,
  errors in photometry, distance modulus and reddening, as well as
  the metallicity dispersion and the uncertainties caused by adopting
  different theoretical color-temperature relations. We found that the
  Galactic bulge IMF can be fitted with two power laws with a break at
  M∼ 0.56 {M}<SUB>⊙ </SUB>, the slope being steeper (α =-2.41+/-
  0.50) for the higher masses, and shallower (α =-1.25+/- 0.20) for
  the lower masses. In the high-mass range, our derived mass function
  agrees well with the mass function derived for other regions of the
  bulge. In the low-mass range however, our mass function is slightly
  shallower, which suggests that separating the disk and bulge components
  is particularly important in the low-mass range. The slope of the
  bulge mass function is also similar to the slope of the mass function
  derived for the disk in the high-mass regime, but the bulge mass
  function is slightly steeper in the low-mass regime. We used our new
  mass function to derive stellar mass-to-light values for the Galactic
  bulge and we obtained 2.1 \lt M/{L}<SUB>F814W</SUB> \lt 2.4 and 3.1
  \lt M/{L}<SUB>F606W</SUB> \lt 3.6 according to different assumptions
  on the slope of the IMF for masses larger than 1{M}<SUB>⊙ </SUB>. <P
  />Based on observations made with the NASA/ESA Hubble Space Telescope,
  obtained by the Space Telescope Science Institute. STScI is operated
  by the Association of Universities for Research in Astronomy, Inc.,
  under NASA contract NAS 5-26555.

Title: Is there a relation between stellar wind braking and the
    spatial structure of surface magnetic fields?
Authors: Brown, Timothy M.
Bibcode: 2015IAUGA..2257429B
Altcode:
  For open cluster ages between about 100 Myr and 500 Myr, plots of
  rotational period vs. color (or equivalently, stellar mass) are almost
  bimodal, with distinct groups fast and slow rotators at all masses
  between roughly 0.5 and 1.3 M_sun. One cannot explain these diagrams
  without invoking some process with a lifetime of a few hundred Myr,
  that for some but not all stars isolates most of the stellar angular
  momentum from the torque caused by a magnetized stellar wind. The
  prevailing theory [e.g. Epstein &amp; Pinsonneault 2014 (ApJ 780,
  159) and references therein] locates this process at the base of the
  stellar convection zone, allowing the wind to spin down the convection
  zone without much affecting the core. In Brown 2014 (ApJ 789,101) I
  suggested rather that the break occurs above the stellar photosphere,
  with different spatial structures of the stellar dynamos accounting
  for drastically different degrees of magnetic coupling to the stellar
  wind. In this talk I will describe preliminary results from two
  observing programs that aim to test the latter hypothesis.One program
  uses photometry from the LCOGT (ground-based, world-wide) telescope
  network to measure rotational periods of stars in fairly young
  open clusters, to improve comparisons between modeled and observed
  period-color diagrams by increasing sample sizes. The LCOGT network
  proves nearly ideal for this kind of work, having already provided good
  data sets for the clusters NGC 6281 and NGC 3532. These clusters are
  both about 300 Myr old, filling a gap in the current age distribution
  of observed clusters. The second program uses K2 photometry combined
  with multicolor photometry (from LCOGT) and spectroscopy (from the ARC
  3.5m telescope) to search for rotation-dependent differences in possible
  proxies for the typical spatial scale of surface magnetic fields. These
  include the spot/photosphere temperature contrast, and short-timescale
  variations in various diagnostics of projected starspot area.

Title: A New Method for Deriving the Stellar Birth Function of
    Resolved Stellar Populations.
Authors: Gennaro, M.; Tchernyshyov, K.; Brown, T. M.; Gordon, K. D.
Bibcode: 2015ApJ...808...45G
Altcode: 2015arXiv150404865G
  We present a new method for deriving the stellar birth function (SBF) of
  resolved stellar populations. The SBF (stars born per unit mass, time,
  and metallicity) is the combination of the initial mass function (IMF),
  the star formation history (SFH), and the metallicity distribution
  function (MDF). The framework of our analysis is that of Poisson Point
  Processes (PPPs), a class of statistical models suitable when dealing
  with points (stars) in a multidimensional space (the measurement
  space of multiple photometric bands). The theory of PPPs easily
  accommodates the modeling of measurement errors as well as that of
  incompleteness. Our method avoids binning stars in the color-magnitude
  diagram and uses the whole likelihood function for each data point;
  combining the individual likelihoods allows the computation of the
  posterior probability for the population's SBF. Within the proposed
  framework it is possible to include nuisance parameters, such as
  distance and extinction, by specifying their prior distributions and
  marginalizing over them. The aim of this paper is to assess the validity
  of this new approach under a range of assumptions, using only simulated
  data. Forthcoming work will show applications to real data. Although
  it has a broad scope of possible applications, we have developed
  this method to study multi-band Hubble Space Telescope observations
  of the Milky Way Bulge. Therefore we will focus on simulations with
  characteristics similar to those of the Galactic Bulge. <P />Based on
  observations made with the NASA/ESA Hubble Space Telescope, obtained at
  STScI, which is operated by AURA, Inc., under NASA contract NAS 5-26555.

Title: UV Insights into the Complex Populations of M87 Globular
    Clusters
Authors: Bellini, A.; Renzini, A.; Anderson, J.; Bedin, L. R.; Piotto,
   G.; Soto, M.; Brown, T. M.; Milone, A. P.; Sohn, S. T.; Sweigart, A. V.
Bibcode: 2015ApJ...805..178B
Altcode: 2015arXiv150401742B
  We have imaged with Hubble Space Telescope WFC3/UVIS the central
  2\buildrel{ \prime}\over{.} 7× 2\buildrel{ \prime}\over{.} 7 region
  of the giant elliptical galaxy M87, using the ultraviolet filter
  F275W. In combination with archival ACS/WFC data taken through the
  F606W and F814W filters, covering the same field, we have constructed
  integrated-light UV-optical colors and magnitudes for 1460 objects,
  most of which are believed to be globular clusters (GCs) belonging to
  M87. The purpose was to ascertain whether the multiple-populations
  syndrome, ubiquitous among Galactic GCs, also exists among the M87
  family of clusters. To achieve this goal, we sought those GCs with
  exceptionally blue UV-to-optical colors because helium-enriched
  sub-populations produce a horizontal-branch morphology that is well
  populated at high effective temperature. For comparison, integrated,
  synthetic UV-optical and purely optical colors and magnitudes have
  been constructed for 45 Galactic GCs, starting from individual-star
  photometry obtained with the same instruments and the same filters. We
  identify a small group of M87 clusters exhibiting a radial UV-optical
  color gradient, representing our best candidate GCs hosting multiple
  populations with extreme helium content. We also find that the central
  spatial distribution of the bluer GCs is flattened in a direction
  parallel to the jet, while the distribution of redder GCs is more
  spherical. We release to the astronomical community our photometric
  catalog in F275W, F606W, and F814W bands and the high-quality image
  stacks in the same bands. <P />Based on proprietary and archival
  observations with the NASA/ESA Hubble Space Telescope, obtained at the
  Space Telescope Science Institute, which is operated by AURA, Inc.,
  under NASA contract NAS 5-26555.

Title: Low False Positive Rate of Kepler Candidates Estimated From
    A Combination Of Spitzer And Follow-Up Observations
Authors: Désert, Jean-Michel; Charbonneau, David; Torres, Guillermo;
   Fressin, François; Ballard, Sarah; Bryson, Stephen T.; Knutson,
   Heather A.; Batalha, Natalie M.; Borucki, William J.; Brown, Timothy
   M.; Deming, Drake; Ford, Eric B.; Fortney, Jonathan J.; Gilliland,
   Ronald L.; Latham, David W.; Seager, Sara
Bibcode: 2015ApJ...804...59D
Altcode: 2015arXiv150303173D
  NASA’s Kepler mission has provided several thousand transiting
  planet candidates during the 4 yr of its nominal mission, yet only
  a small subset of these candidates have been confirmed as true
  planets. Therefore, the most fundamental question about these
  candidates is the fraction of bona fide planets. Estimating the
  rate of false positives of the overall Kepler sample is necessary to
  derive the planet occurrence rate. We present the results from two
  large observational campaigns that were conducted with the Spitzer
  Space Telescope during the the Kepler mission. These observations
  are dedicated to estimating the false positive rate (FPR) among
  the Kepler candidates. We select a sub-sample of 51 candidates,
  spanning wide ranges in stellar, orbital, and planetary parameter
  space, and we observe their transits with Spitzer at 4.5 μm. We use
  these observations to measures the candidate’s transit depths and
  infrared magnitudes. An authentic planet produces an achromatic transit
  depth (neglecting the modest effect of limb darkening). Conversely
  a bandpass-dependent depth alerts us to the potential presence of
  a blending star that could be the source of the observed eclipse:
  a false positive scenario. For most of the candidates (85%), the
  transit depths measured with Kepler are consistent with the transit
  depths measured with Spitzer as expected for planetary objects, while
  we find that the most discrepant measurements are due to the presence of
  unresolved stars that dilute the photometry. The Spitzer constraints on
  their own yield FPRs between 5% and depending on the Kepler Objects of
  Interest. By considering the population of the Kepler field stars, and
  by combining follow-up observations (imaging) when available, we find
  that the overall FPR of our sample is low. The measured upper limit
  on the FPR of our sample is 8.8% at a confidence level of 3σ. This
  observational result, which uses the achromatic property of planetary
  transit signals that is not investigated by the Kepler observations,
  provides an independent indication that Kepler’s FPR is low.

Title: The Hubble Space Telescope UV Legacy Survey of Galactic
    Globular Clusters. I. Overview of the Project and Detection of
    Multiple Stellar Populations
Authors: Piotto, G.; Milone, A. P.; Bedin, L. R.; Anderson, J.;
   King, I. R.; Marino, A. F.; Nardiello, D.; Aparicio, A.; Barbuy,
   B.; Bellini, A.; Brown, T. M.; Cassisi, S.; Cool, A. M.; Cunial, A.;
   Dalessandro, E.; D'Antona, F.; Ferraro, F. R.; Hidalgo, S.; Lanzoni,
   B.; Monelli, M.; Ortolani, S.; Renzini, A.; Salaris, M.; Sarajedini,
   A.; van der Marel, R. P.; Vesperini, E.; Zoccali, M.
Bibcode: 2015AJ....149...91P
Altcode: 2014arXiv1410.4564P
  In this paper we describe a new UV-initiative Hubble Space Telescope
  project (GO-13297) that will complement the existing F606W and F814W
  database of the Advanced Camera for Surveys Globular Cluster (GC)
  Treasury by imaging most of its clusters through UV/blue WFC3/UVIS
  filters F275W, F336W, and F438W. This “magic trio” of filters
  has shown an uncanny ability to disentangle and characterize multiple
  population (MP) patterns in GCs in a way that is exquisitely sensitive
  to C, N, and O abundance variations. Combination of these passbands
  with those in the optical also gives the best leverage for measuring
  helium enrichment. The dozen clusters that had previously been observed
  in these bands exhibit a bewildering variety of MP patterns, and the
  new survey will map the full variance of the phenomenon. The ubiquity
  of multiple stellar generations in GCs has made the formation of these
  cornerstone objects more intriguing than ever; GC formation and the
  origin of their MPs have now become one and the same problem. In this
  paper we will describe the database and our data reduction strategy, as
  well as the uses we intend to make of the final photometry, astrometry,
  and PMs. We will also present preliminary color-magnitude diagrams
  from the data so far collected. These diagrams also draw on data
  from GO-12605 and GO-12311, which served as a pilot project for the
  present GO-13297. <P />Based on observations with the NASA/ESA Hubble
  Space Telescope, obtained at the Space Telescope Science Institute,
  which is operated by AURA, Inc., under NASA contract NAS 5-26555.

Title: Legacy Extragalactic UV Survey (LEGUS) With the Hubble Space
    Telescope. I. Survey Description
Authors: Calzetti, D.; Lee, J. C.; Sabbi, E.; Adamo, A.; Smith, L. J.;
   Andrews, J. E.; Ubeda, L.; Bright, S. N.; Thilker, D.; Aloisi, A.;
   Brown, T. M.; Chandar, R.; Christian, C.; Cignoni, M.; Clayton, G. C.;
   da Silva, R.; de Mink, S. E.; Dobbs, C.; Elmegreen, B. G.; Elmegreen,
   D. M.; Evans, A. S.; Fumagalli, M.; Gallagher, J. S., III; Gouliermis,
   D. A.; Grebel, E. K.; Herrero, A.; Hunter, D. A.; Johnson, K. E.;
   Kennicutt, R. C.; Kim, H.; Krumholz, M. R.; Lennon, D.; Levay, K.;
   Martin, C.; Nair, P.; Nota, A.; Östlin, G.; Pellerin, A.; Prieto,
   J.; Regan, M. W.; Ryon, J. E.; Schaerer, D.; Schiminovich, D.; Tosi,
   M.; Van Dyk, S. D.; Walterbos, R.; Whitmore, B. C.; Wofford, A.
Bibcode: 2015AJ....149...51C
Altcode: 2014arXiv1410.7456C
  The Legacy ExtraGalactic UV Survey (LEGUS) is a Cycle 21 Treasury
  program on the Hubble Space Telescope aimed at the investigation of star
  formation and its relation with galactic environment in nearby galaxies,
  from the scales of individual stars to those of ∼kiloparsec-size
  clustered structures. Five-band imaging from the near-ultraviolet to
  the I band with the Wide-Field Camera 3 (WFC3), plus parallel optical
  imaging with the Advanced Camera for Surveys (ACS), is being collected
  for selected pointings of 50 galaxies within the local 12 Mpc. The
  filters used for the observations with the WFC3 are F275W(λ2704 Å),
  F336W(λ3355 Å), F438W(λ4325 Å), F555W(λ5308 Å), and F814W(λ8024
  Å) the parallel observations with the ACS use the filters F435W(λ4328
  Å), F606W(λ5921 Å), and F814W(λ8057 Å). The multiband images are
  yielding accurate recent (≲50 Myr) star formation histories from
  resolved massive stars and the extinction-corrected ages and masses of
  star clusters and associations. The extensive inventories of massive
  stars and clustered systems will be used to investigate the spatial
  and temporal evolution of star formation within galaxies. This will, in
  turn, inform theories of galaxy evolution and improve the understanding
  of the physical underpinning of the gas-star formation relation and
  the nature of star formation at high redshift. This paper describes
  the survey, its goals and observational strategy, and the initial
  scientific results. Because LEGUS will provide a reference survey
  and a foundation for future observations with the James Webb Space
  Telescope and with ALMA, a large number of data products are planned
  for delivery to the community. <P />Based on observations obtained with
  the NASA/ESA Hubble Space Telescope at the Space Telescope Science
  Institute, which is operated by the Association of Universities for
  Research in Astronomy under NASA Contract NAS 5-26555.

Title: The Hubble Space Telescope UV Legacy Survey of galactic
    globular clusters - II. The seven stellar populations of NGC 7089
    (M2)<SUP>⋆</SUP>
Authors: Milone, A. P.; Marino, A. F.; Piotto, G.; Bedin, L. R.;
   Anderson, J.; Renzini, A.; King, I. R.; Bellini, A.; Brown, T. M.;
   Cassisi, S.; D'Antona, F.; Jerjen, H.; Nardiello, D.; Salaris,
   M.; Marel, R. P. van der; Vesperini, E.; Yong, D.; Aparicio, A.;
   Sarajedini, A.; Zoccali, M.
Bibcode: 2015MNRAS.447..927M
Altcode: 2014arXiv1411.5043M; 2015MNRAS.447..931M
  We present high-precision multiband photometry for the globular cluster
  (GC) M2. We combine the analysis of the photometric data obtained from
  the Hubble Space Telescope UV Legacy Survey of Galactic GCs GO-13297,
  with chemical abundances by Yong et al., and compare the photometry with
  models in order to analyse the multiple stellar sequences we identified
  in the colour-magnitude diagram. We find three main stellar components,
  composed of metal-poor, metal-intermediate, and metal-rich stars
  (hereafter referred to as population A, B, and C, respectively). The
  components A and B include stars with different s-process element
  abundances. They host six sub-populations with different light-element
  abundances, and exhibit an internal variation in helium up to ΔY
  ∼ 0.07 dex. In contrast with M22, another cluster characterized
  by the presence of populations with different metallicities, M2
  contains a third stellar component, C, which shows neither evidence for
  sub-populations nor an internal spread in light-elements. Population C
  does not exhibit the typical photometric signatures that are associated
  with abundance variations of light elements produced by hydrogen burning
  at hot temperatures. We compare M2 with other GCs with intrinsic
  heavy-element variations and conclude that M2 resembles M22, but it
  includes an additional stellar component that makes it more similar to
  the central region of the Sagittarius galaxy, which hosts a GC (M54)
  and the nucleus of the Sagittarius galaxy itself.

Title: NRES: The Network of Robotic Echelle Spectrographs
Authors: Siverd, Robert; Eastman, Jason D.; Brown, Timothy M.;
   Hygelund, John; Henderson, Todd; Tufts, Joseph; Van Eyken, Julian C.;
   Barnes, Stuart
Bibcode: 2015AAS...22540904S
Altcode:
  Las Cumbres Observatory Global Network (LCOGT) is building the Network
  of Robotic Echelle Spectrographs (NRES), which will consist of six
  identical, optical (390 - 860 nm) high-precision spectrographs, each
  fiber-fed simultaneously by two 1 meter telescopes and a thorium
  argon calibration source, one at each of our observatory sites in
  the Northern and Southern hemispheres. Thus, NRES will be a single,
  globally-distributed, autonomous observing facility using twelve 1-m
  telescopes. Simulations suggest we will achieve long-term radial
  velocity precision of better than 3 m/s in less than an hour for
  stars brighter than V = 12. We have been funded with NSF MRI and ATI
  grants, and expect our first spectrograph to be deployed in mid 2015,
  with the full network operation of all 6 units beginning in 2016. We
  will discuss the NRES design, goals, robotic operation, and status,
  as well as the early results from our prototype spectrograph.

Title: Transiting Exoplanet Survey Satellite (TESS)
Authors: Ricker, George R.; Winn, Joshua N.; Vanderspek, Roland;
   Latham, David W.; Bakos, Gáspár Á.; Bean, Jacob L.; Berta-Thompson,
   Zachory K.; Brown, Timothy M.; Buchhave, Lars; Butler, Nathaniel
   R.; Butler, R. Paul; Chaplin, William J.; Charbonneau, David;
   Christensen-Dalsgaard, Jørgen; Clampin, Mark; Deming, Drake; Doty,
   John; De Lee, Nathan; Dressing, Courtney; Dunham, Edward W.; Endl,
   Michael; Fressin, Francois; Ge, Jian; Henning, Thomas; Holman, Matthew
   J.; Howard, Andrew W.; Ida, Shigeru; Jenkins, Jon M.; Jernigan,
   Garrett; Johnson, John Asher; Kaltenegger, Lisa; Kawai, Nobuyuki;
   Kjeldsen, Hans; Laughlin, Gregory; Levine, Alan M.; Lin, Douglas;
   Lissauer, Jack J.; MacQueen, Phillip; Marcy, Geoffrey; McCullough,
   Peter R.; Morton, Timothy D.; Narita, Norio; Paegert, Martin; Palle,
   Enric; Pepe, Francesco; Pepper, Joshua; Quirrenbach, Andreas; Rinehart,
   Stephen A.; Sasselov, Dimitar; Sato, Bun'ei; Seager, Sara; Sozzetti,
   Alessandro; Stassun, Keivan G.; Sullivan, Peter; Szentgyorgyi, Andrew;
   Torres, Guillermo; Udry, Stephane; Villasenor, Joel
Bibcode: 2015JATIS...1a4003R
Altcode:
  The Transiting Exoplanet Survey Satellite (TESS) will search for
  planets transiting bright and nearby stars. TESS has been selected
  by NASA for launch in 2017 as an Astrophysics Explorer mission. The
  spacecraft will be placed into a highly elliptical 13.7-day orbit
  around the Earth. During its 2-year mission, TESS will employ four
  wide-field optical charge-coupled device cameras to monitor at least
  200,000 main-sequence dwarf stars with I<SUB>C</SUB>≈4-13 for
  temporary drops in brightness caused by planetary transits. Each
  star will be observed for an interval ranging from 1 month to 1
  year, depending mainly on the star's ecliptic latitude. The longest
  observing intervals will be for stars near the ecliptic poles, which
  are the optimal locations for follow-up observations with the James
  Webb Space Telescope. Brightness measurements of preselected target
  stars will be recorded every 2 min, and full frame images will be
  recorded every 30 min. TESS stars will be 10 to 100 times brighter
  than those surveyed by the pioneering Kepler mission. This will make
  TESS planets easier to characterize with follow-up observations. TESS
  is expected to find more than a thousand planets smaller than Neptune,
  including dozens that are comparable in size to the Earth. Public data
  releases will occur every 4 months, inviting immediate community-wide
  efforts to study the new planets. The TESS legacy will be a catalog
  of the nearest and brightest stars hosting transiting planets, which
  will endure as highly favorable targets for detailed investigations.

Title: Transiting Exoplanet Survey Satellite (TESS)
Authors: Ricker, George R.; Winn, Joshua N.; Vanderspek, Roland;
   Latham, David W.; Bakos, Gáspár. Á.; Bean, Jacob L.; Berta-Thompson,
   Zachory K.; Brown, Timothy M.; Buchhave, Lars; Butler, Nathaniel
   R.; Butler, R. Paul; Chaplin, William J.; Charbonneau, David;
   Christensen-Dalsgaard, Jørgen; Clampin, Mark; Deming, Drake; Doty,
   John; De Lee, Nathan; Dressing, Courtney; Dunham, E. W.; Endl, Michael;
   Fressin, Francois; Ge, Jian; Henning, Thomas; Holman, Matthew J.;
   Howard, Andrew W.; Ida, Shigeru; Jenkins, Jon; Jernigan, Garrett;
   Johnson, John A.; Kaltenegger, Lisa; Kawai, Nobuyuki; Kjeldsen, Hans;
   Laughlin, Gregory; Levine, Alan M.; Lin, Douglas; Lissauer, Jack J.;
   MacQueen, Phillip; Marcy, Geoffrey; McCullough, P. R.; Morton, Timothy
   D.; Narita, Norio; Paegert, Martin; Palle, Enric; Pepe, Francesco;
   Pepper, Joshua; Quirrenbach, Andreas; Rinehart, S. A.; Sasselov,
   Dimitar; Sato, Bun'ei; Seager, Sara; Sozzetti, Alessandro; Stassun,
   Keivan G.; Sullivan, Peter; Szentgyorgyi, Andrew; Torres, Guillermo;
   Udry, Stephane; Villasenor, Joel
Bibcode: 2014SPIE.9143E..20R
Altcode: 2014arXiv1406.0151R
  The Transiting Exoplanet Survey Satellite (TESS ) will search for
  planets transiting bright and nearby stars. TESS has been selected
  by NASA for launch in 2017 as an Astrophysics Explorer mission. The
  spacecraft will be placed into a highly elliptical 13.7-day orbit
  around the Earth. During its two-year mission, TESS will employ
  four wide-field optical CCD cameras to monitor at least 200,000
  main-sequence dwarf stars with I<SUB>C</SUB> (approximately less than)
  13 for temporary drops in brightness caused by planetary transits. Each
  star will be observed for an interval ranging from one month to one
  year, depending mainly on the star's ecliptic latitude. The longest
  observing intervals will be for stars near the ecliptic poles, which
  are the optimal locations for follow-up observations with the James
  Webb Space Telescope. Brightness measurements of preselected target
  stars will be recorded every 2 min, and full frame images will be
  recorded every 30 min. TESS stars will be 10-100 times brighter than
  those surveyed by the pioneering Kepler mission. This will make TESS
  planets easier to characterize with follow-up observations. TESS is
  expected to find more than a thousand planets smaller than Neptune,
  including dozens that are comparable in size to the Earth. Public data
  releases will occur every four months, inviting immediate community-wide
  efforts to study the new planets. The TESS legacy will be a catalog
  of the nearest and brightest stars hosting transiting planets, which
  will endure as highly favorable targets for detailed investigations.

Title: The Metastable Dynamo Model of Stellar Rotational Evolution
Authors: Brown, Timothy M.
Bibcode: 2014ApJ...789..101B
Altcode: 2014arXiv1403.4525B
  This paper introduces a new empirical model for the rotational
  evolution of Sun-like stars—those with surface convection zones
  and non-convective interior regions. Previous models do not match the
  morphology of observed (rotation period)-color diagrams, notably the
  existence of a relatively long-lived "C-sequence" of fast rotators first
  identified by Barnes. This failure motivates the Metastable Dynamo Model
  (MDM) described here. The MDM posits that stars are born with their
  magnetic dynamos operating in a mode that couples very weakly to the
  stellar wind, so their (initially very short) rotation periods at first
  change little with time. At some point, this mode spontaneously and
  randomly changes to a strongly coupled mode, the transition occurring
  with a mass-dependent lifetime that is of the order of 100 Myr. I show
  that with this assumption, one can obtain good fits to observations of
  young clusters, particularly for ages of 150-200 Myr. Previous models
  and the MDM both give qualitative agreement with the morphology of
  the slower-rotating "I-sequence" stars, but none of them have been
  shown to accurately reproduce the stellar-mass-dependent evolution
  of the I-sequence stars, especially for clusters older than a few
  hundred million years. I discuss observational experiments that can
  test aspects of the MDM, and speculate that the physics underlying the
  MDM may be related to other situations described in the literature,
  in which stellar dynamos may have a multi-modal character.

Title: NRES: the network of robotic Echelle spectrographs
Authors: Eastman, Jason D.; Brown, Timothy M.; Hygelund, John; van
   Eyken, Julian; Tufts, Joseph R.; Barnes, Stuart
Bibcode: 2014SPIE.9147E..16E
Altcode:
  Las Cumbres Observatory Global Network (LCOGT) is building the Network
  of Robotic Echelle Spectrographs (NRES), which will consist of six
  identical, optical (390 - 860 nm) high-precision spectrographs, each
  fiber-fed simultaneously by two 1 meter telescopes and a thorium
  argon calibration source, one at each of our observatory sites in
  the Northern and Southern hemispheres. Thus, NRES will be a single,
  globally-distributed, autonomous observing facility using twelve 1-m
  telescopes. Simulations suggest we will achieve long-term precision
  of better than 3 m/s in less than an hour for stars brighter than V =
  12. We have been fully funded with an NSF MRI grant, and expect our
  first spectrograph to be deployed in Spring of 2015, with the full
  network operation of all 6 units beginning in Spring of 2016. We
  discuss the NRES design, goals, and robotic operation, as well as the
  early results from our prototype spectrograph.

Title: VizieR Online Data Catalog: Small Kepler planets radial
    velocities (Marcy+, 2014)
Authors: Marcy, G. W.; Isaacson, H.; Howard, A. W.; Rowe, J. F.;
   Jenkins, J. M.; Bryson, S. T.; Latham, D. W.; Howell, S. B.;
   Gautier, T. N., III; Batalha, N. M.; Rogers, L.; Ciardi, D.; Fischer,
   D. A.; Gilliland, R. L.; Kjeldsen, H.; Christensen-Dalsgaard, J.;
   Huber, D.; Chaplin, W. J.; Basu, S.; Buchhave, L. A.; Quinn, S. N.;
   Borucki, W. J.; Koch, D. G.; Hunter, R.; Caldwell, D. A.; van Cleve,
   J.; Kolbl, R.; Weiss, L. M.; Petigura, E.; Seager, S.; Morton, T.;
   Johnson, J. A.; Ballard, S.; Burke, C.; Cochran, W. D.; Endl, M.;
   MacQueen, P.; Everett, M. E.; Lissauer, J. J.; Ford, E. B.; Torres,
   G.; Fressin, F.; Brown, T. M.; Steffen, J. H.; Charbonneau, D.; Basri,
   G. S.; Sasselov, D. D.; Winn, J.; Sanchis-Ojeda, R.; Christiansen,
   J.; Adams, E.; Henze, C.; Dupree, A.; Fabrycky, D. C.; Fortney, J. J.;
   Tarter, J.; Holman, M. J.; Tenenbaum, P.; Shporer, A.; Lucas, P. W.;
   Welsh, W. F.; Orosz, J. A.; Bedding, T. R.; Campante, T. L.; Davies,
   G. R.; Elsworth, Y.; Handberg, R.; Hekker, S.; Karoff, C.; Kawaler,
   S. D.; Lund, M. N.; Lundkvist, M.; Metcalfe, T. S.; Miglio, A.; Silva
   Aguirre, V.; Stello, D.; White, T. R.; Boss, A.; Devore, E.; Gould,
   A.; Prsa, A.; Agol, E.; Barclay, T.; Coughlin, J.; Brugamyer, E.;
   Mullally, F.; Quintana, E. V.; Still, M.; Thompson, S. E.; Morrison,
   D.; Twicken, J. D.; Desert, J. -M.; Carter, J.; Crepp, J. R.; Hebrard,
   G.; Santerne, A.; Moutou, C.; Sobeck, C.; Hudgins, D.; Haas, M. R.;
   Robertson, P.; Lillo-Box, J.; Barrado, D.
Bibcode: 2014yCat..22100020M
Altcode:
  Here we report measured masses, radii, and densities (or upper limits
  on those values) for 42 transiting planet candidates contained within
  22 bright Kepler Objects of Interest (KOIs) from Batalha et al. (2013,
  Cat. J/ApJS/204/24). We carried out multiple Doppler-shift measurements
  of the host stars using the Keck 1 telescope. From the spectroscopy
  and Doppler measurements, we compute self-consistent measurements of
  stellar and planet radii, employing either stellar structure models
  or asteroseismology measurements from the Kepler photometry. We also
  search for (and report) 7 additional non-transiting planets revealed
  by the precise radial velocities (RVs), for a total of 49 planets. <P
  />We carried out "reconnaissance" high-resolution spectroscopy on ~1000
  KOIs with spectral resolution, R~50000, and S/N=20-100 per pixel. The
  dual goals were searching for false positives and refining the stellar
  parameters. We obtained one or two such reconnaissance spectra using
  one of four facilities: the McDonald Observatory 2.7m, the Tillinghast
  1.5m on Mt. Hopkins, the Lick Observatory 3m, and the 2.6m Nordic
  Optical Telescope. <P />Speckle imaging of each of the selected 22
  KOIs was obtained using the two-color DSSI speckle camera at the WIYN
  3.5m telescope on Kitt Peak. <P />All 22 KOIs were observed with the
  Keck NIRC2-AO system. <P />(3 data files).

Title: PTFO 8-8695b: An Extremely Young T-Tauri-Transiting Planet
Authors: van Eyken, J. C.; Ciardi, D. R.; Barnes, J. W.; Brown,
   T. M.; Dragomir, D.; Eastman, J.; Beichman, C. A.; Belle, G. v.;
   Braun, K. v.; Carey, S.; Crockett, C.; Fortney, J. J.; Howell, S. B.;
   Jackson, B. K.; Johns-Krull, C.; Kane, S. R.; Lister, T.; Mazin, B.;
   McLane, J.; Plavchan, P.; Prato, L.; Shporer, A.; Stauffer, J. R.;
   PTF Collaboration
Bibcode: 2014ebi..confP3.57V
Altcode:
  Estimated at only ~3Myr old, PTFO 8-8695b is a candidate for the
  youngest transiting planet yet found, and presents a potentially
  valuable snapshot of a close-in pre-main-sequence planet still in its
  infancy. Ongoing investigation is painting an unusual but increasingly
  compelling picture: orbiting a rapidly-rotating T-Tauri star at just
  under a half-day period, it appears the planet's orbit may be inclined
  and precessing on timescales as short as ~hundreds of days - a timescale
  easily accessible to observation. The star shows substantial flaring
  activity, and the planet's measured radius suggests that it may be
  actively be losing mass. The unusual properties of this object make
  it particularly interesting for continued investigation. We present
  some of our current observations and our interpretation of the data.

Title: Masses, Radii, and Orbits of Small Kepler Planets: The
    Transition from Gaseous to Rocky Planets
Authors: Marcy, Geoffrey W.; Isaacson, Howard; Howard, Andrew W.;
   Rowe, Jason F.; Jenkins, Jon M.; Bryson, Stephen T.; Latham, David
   W.; Howell, Steve B.; Gautier, Thomas N., III; Batalha, Natalie M.;
   Rogers, Leslie; Ciardi, David; Fischer, Debra A.; Gilliland, Ronald
   L.; Kjeldsen, Hans; Christensen-Dalsgaard, Jørgen; Huber, Daniel;
   Chaplin, William J.; Basu, Sarbani; Buchhave, Lars A.; Quinn, Samuel
   N.; Borucki, William J.; Koch, David G.; Hunter, Roger; Caldwell,
   Douglas A.; Van Cleve, Jeffrey; Kolbl, Rea; Weiss, Lauren M.;
   Petigura, Erik; Seager, Sara; Morton, Timothy; Johnson, John Asher;
   Ballard, Sarah; Burke, Chris; Cochran, William D.; Endl, Michael;
   MacQueen, Phillip; Everett, Mark E.; Lissauer, Jack J.; Ford, Eric
   B.; Torres, Guillermo; Fressin, Francois; Brown, Timothy M.; Steffen,
   Jason H.; Charbonneau, David; Basri, Gibor S.; Sasselov, Dimitar D.;
   Winn, Joshua; Sanchis-Ojeda, Roberto; Christiansen, Jessie; Adams,
   Elisabeth; Henze, Christopher; Dupree, Andrea; Fabrycky, Daniel C.;
   Fortney, Jonathan J.; Tarter, Jill; Holman, Matthew J.; Tenenbaum,
   Peter; Shporer, Avi; Lucas, Philip W.; Welsh, William F.; Orosz,
   Jerome A.; Bedding, T. R.; Campante, T. L.; Davies, G. R.; Elsworth,
   Y.; Handberg, R.; Hekker, S.; Karoff, C.; Kawaler, S. D.; Lund,
   M. N.; Lundkvist, M.; Metcalfe, T. S.; Miglio, A.; Silva Aguirre, V.;
   Stello, D.; White, T. R.; Boss, Alan; Devore, Edna; Gould, Alan; Prsa,
   Andrej; Agol, Eric; Barclay, Thomas; Coughlin, Jeff; Brugamyer, Erik;
   Mullally, Fergal; Quintana, Elisa V.; Still, Martin; Thompson, Susan
   E.; Morrison, David; Twicken, Joseph D.; Désert, Jean-Michel; Carter,
   Josh; Crepp, Justin R.; Hébrard, Guillaume; Santerne, Alexandre;
   Moutou, Claire; Sobeck, Charlie; Hudgins, Douglas; Haas, Michael R.;
   Robertson, Paul; Lillo-Box, Jorge; Barrado, David
Bibcode: 2014ApJS..210...20M
Altcode: 2014arXiv1401.4195M
  We report on the masses, sizes, and orbits of the planets orbiting
  22 Kepler stars. There are 49 planet candidates around these stars,
  including 42 detected through transits and 7 revealed by precise
  Doppler measurements of the host stars. Based on an analysis of the
  Kepler brightness measurements, along with high-resolution imaging and
  spectroscopy, Doppler spectroscopy, and (for 11 stars) asteroseismology,
  we establish low false-positive probabilities (FPPs) for all of the
  transiting planets (41 of 42 have an FPP under 1%), and we constrain
  their sizes and masses. Most of the transiting planets are smaller
  than three times the size of Earth. For 16 planets, the Doppler
  signal was securely detected, providing a direct measurement of the
  planet's mass. For the other 26 planets we provide either marginal mass
  measurements or upper limits to their masses and densities; in many
  cases we can rule out a rocky composition. We identify six planets
  with densities above 5 g cm<SUP>-3</SUP>, suggesting a mostly rocky
  interior for them. Indeed, the only planets that are compatible with a
  purely rocky composition are smaller than ~2 R <SUB>⊕</SUB>. Larger
  planets evidently contain a larger fraction of low-density material (H,
  He, and H<SUB>2</SUB>O). <P />Based in part on observations obtained
  at the W. M. Keck Observatory, which is operated by the University of
  California and the California Institute of Technology.

Title: Adapting Low-Tech Gear to Exoplanet Discovery
Authors: Brown, Timothy M.
Bibcode: 2014AAS...223.9106B
Altcode:
  The discovery of 51 Peg b by Mayor and Queloz revealed (among other
  things) that discovering extrasolar planets, though certainly difficult,
  was not as hard as professional astronomers had previously thought. At
  the same time, the astronomical equipment available to amateurs --
  including optics, mountings, and CCD detectors -- had become quite
  capable. This combination of factors led to successful exoplanet
  programs that leaned heavily on amateur-grade hardware, seeking faster
  development times and lower costs than were possible for traditional
  no-compromises astronomical instrument programs. I will describe two of
  these in which I played a role: the AFOE (Advanced Fiber Optic Echelle)
  spectrograph, and the STellar Astrophysics and Research on Exoplanets
  (STARE) transit-search wide-field imager.

Title: Legacy ExtraGalactic UV Survey (LEGUS): The HST View of Star
    Formation in Nearby Galaxies
Authors: Calzetti, Daniela; Lee, J. C.; Adamo, A.; Aloisi, A.; Andrews,
   J. E.; Brown, T. M.; Chandar, R.; Christian, C. A.; Cignoni, M.;
   Clayton, G. C.; Da Silva, R. L.; de Mink, S. E.; Dobbs, C.; Elmegreen,
   B.; Elmegreen, D. M.; Evans, A. S.; Fumagalli, M.; Gallagher, J. S.;
   Gouliermis, D.; Grebel, E.; Herrero-Davo`, A.; Hilbert, B.; Hunter,
   D. A.; Johnson, K. E.; Kennicutt, R.; Kim, H.; Krumholz, M. R.; Lennon,
   D. J.; Martin, C. D.; Nair, P.; Nota, A.; Pellerin, A.; Prieto, J.;
   Regan, M. W.; Sabbi, E.; Schaerer, D.; Schiminovich, D.; Smith, L. J.;
   Thilker, D. A.; Tosi, M.; Van Dyk, S. D.; Walterbos, R. A.; Whitmore,
   B. C.; Wofford, A.
Bibcode: 2014AAS...22325408C
Altcode:
  The Treasury program LEGUS (HST/GO-13364) is the first HST UV Atlas
  of nearby galaxies, and is aimed at the thorough investigation of star
  formation and its relation with galaxy environment, from the scales of
  individual stars to those of ~kpc clustered structures. The 154-orbits
  program is obtaining NUV,U,B,V,I images of 50 star-forming galaxies
  in the distance range 4-12 Mpc, covering the full range of morphology,
  star formation rate (SFR), mass, metallicity, internal structure, and
  interaction state found in the local Universe. The imaging survey will
  yield accurate recent (&lt;50 Myr) star formation histories (SFHs)
  from resolved massive stars, and the extinction-corrected ages and
  masses of star clusters and associations. These extensive inventories
  of massive stars, clustered systems, and SFHs will be used to: (1)
  quantify how the clustering of star formation evolves both in space and
  in time; (2) discriminate among models of star cluster evolution; (3)
  investigate the effects of SFH on the UV SFR calibrations; (4) explore
  the impact of environment on star formation and cluster evolution across
  the full range of galactic and ISM properties. LEGUS observations
  will inform theories of star formation and galaxy evolution, and
  improve the understanding of the physical underpinning of the gas-star
  formation relation and the nature of the clumpy star formation at high
  redshift. LEGUS will generate the most homogeneous high-resolution,
  wide-field UV dataset to date, building and expanding on the GALEX
  legacy. Data products that will be delivered to the community include:
  catalogs of massive stars and star clusters, catalogs of star cluster
  properties (ages, masses, extinction), and a one-stop shop for all the
  ancillary data available for this well-studied galaxy sample. LEGUS will
  provide the reference survey and the foundation for future observations
  with JWST and with ALMA. This abstract accompanies another one from the
  same project, and presents the status of the project, its structure,
  and the data products that will be delivered to the community; the
  other abstract presents the science goals of LEGUS and how these will
  be addressed by the HST observations.

Title: The white dwarf cooling sequence of the Galactic bulge
Authors: Calamida, Annalisa; Sahu, K. C.; Anderson, J.; Casertano,
   S.; Brown, T. M.; Cassisi, S.; Sokol, J.; Bond, H. E.; Ferguson,
   H. C.; Livio, M.; Salaris, M.; Ferraro, I.; Valenti, J. A.
Bibcode: 2014AAS...22331508C
Altcode:
  We present F606W,F814W (V,I)-band time-series data of ~1 million stars
  in the low-reddening Sagittarius window in the Galactic bulge. Images
  were collected with the Advanced Camera far Surveys (ACS) and the Wide
  Field Camera 3 mounted on the Hubble Space Telescope. The total field
  of view is ~ 17x18 arcminutes, which was observed approximately every
  two weeks for two consecutive years, with the principal aim to detect
  a hidden population of isolated black holes and neutron stars in the
  Galactic disk through astrometric microlensing. Here we present some
  results based on the combined deep images of the four ACS fields. The
  final photometric catalog of ~ 1 million stars reaches down to V ~ 31
  mag. Proper motions were also measured, with an accuracy of better than
  ~ 0.15 mas/yr at V ~ 26 mag in both coordinates. We were then able to
  separate disk and bulge stars and obtain a clean bulge color-magnitude
  diagram. Together with several candidate extreme horizontal branch
  (EHB) stars we were able to identify for the first time a clearly
  defined white dwarf (WD) cooling sequence in the bulge. The comparison
  between theory and observations shows that a fraction of the WDs is
  systematically redder than the canonical cooling tracks for CO-core DA
  WDs. This evidence would suggest the presence of He-core WDs in the
  bulge, formed in close binaries, as has been found in some Galactic
  globular and open clusters. The presence of close binaries in the EHB
  and WD bulge population is further supported by the finding of two
  EHB ellipsoidal variables and a candidate dwarf nova in outburst in
  one of the ACS fields.

Title: Noise characteristics of LCOGT time series photometry
Authors: Dragomir, Diana; Brown, T. M.
Bibcode: 2014AAS...22330202D
Altcode:
  The Las Cumbres Observatory Global Telescope (LCOGT) facility consists
  of a network of robotic telescopes located at multiple sites in both the
  northern and southern hemispheres. We have deployed and commissioned
  nine 1.0m telescopes. Eight of these are distributed longitudinally
  at three sites to provide continuous night-time coverage in the
  south. LCOGT's unique capabilities can contribute to a wide range of
  research in the field of time-domain astronomy. To ensure optimal data
  quality for individual as well as combined multi-telescope time series,
  it is essential that we understand and correct - whenever possible - the
  instrument systematics affecting LCOGT network observations. We identify
  physical sources of noise present in LCOGT 1.0m photometry, and we use
  singular value decomposition (SVD) to filter correlated noise patterns
  common to an ensemble of stars in a given time series data set. We
  quantify and compare the levels of uncorrelated and correlated noise
  before and after SVD filtering using power spectral analysis. Finally,
  we discuss the properties of and methods to reduce any remaining
  post-SVD red noise that is due to instrumental systematics.

Title: The formation history of the Ultra-Faint Dwarf galaxies
Authors: Brown, T. M.; Tumlinson, J.; Geha, M.; Kirby, E.; VandenBerg,
   D. A.; Kalirai, J. S.; Simon, J. D.; Avila, R. J.; Munoz, R. R.;
   Guhathakurta, P.; Renzini, A.; Ferguson, H. C.; Vargas, L. C.;
   Gennaro, M.
Bibcode: 2014MmSAI..85..493B
Altcode: 2013arXiv1310.0824B
  We present early results from a Hubble Space Telescope survey of the
  ultra-faint dwarf galaxies. These Milky Way satellites were discovered
  in the Sloan Digital Sky Survey, and appear to be an extension of the
  classical dwarf spheroidals to low luminosities, offering a new front
  in the efforts to understand the missing satellite problem. Because they
  are the least luminous, most dark matter dominated, and least chemically
  evolved galaxies known, the ultra-faint dwarfs are the best candidate
  fossils from the early universe. The primary goal of the survey is
  to measure the star-formation histories of these galaxies and discern
  any synchronization due to the reionization of the universe. We find
  that the six galaxies of our survey have very similar star-formation
  histories, and that each is dominated by stars older than 12 Gyr.

Title: The LCOGT Science Collaboration
Authors: Brown, Timothy M.; Boroson, T. A.; Howell, D. A.; Street,
   R.; Lister, T.
Bibcode: 2014AAS...22325443B
Altcode:
  Las Cumbres Observatory Global Telescope (LCOGT) has deployed a
  global network of 1-m and 2m optical telescopes, optimized for work
  in time-domain astronomy. Since our scientific staff is rather small,
  and since network operation necessarily involves close collaborations
  with other astronomical institutions, we aim to extend the scientific
  depth and scope of the Observatory by creating a formal Science
  Collaboration. This poster explains the structure and membership
  of the Collaboration, with emphasis on the notion of Key Projects
  that we intend as vehicles to perform scientific programs for which
  LCOGT's facilities are uniquely suited, and which will have the
  greatest scientific impact. The general subjects of these projects
  are already defined (Supernovae, Extrasolar Planets, Solar System,
  AGN, and Stellar Astrophysics). A Collaboration-wide proposal process
  to be carried out in early 2014 will determine which problems within
  these categories will be addressed in the first round of Key Projects.

Title: NRES: The Network of Robotic Echelle Spectrographs
Authors: Eastman, Jason; Brown, T. M.; Hygelund, J.; Van Eyken, J. C.
Bibcode: 2014AAS...22313605E
Altcode:
  Las Cumbres Observatory Global Network (LCOGT) is building the Network
  of Robotic Echelle Spectrographs (NRES), which will consist of six
  identical, optical (390 - 860 nm) high-precision spectrographs, each
  fiber-fed simultaneously by two 1 meter telescopes and a thorium
  argon calibration source, one at each of our observatory sites in
  the Northern and Southern hemispheres. Thus, NRES will be a single,
  globally-distributed, autonomous observing facility using twelve 1-m
  telescopes. Simulations suggest we will achieve long-term precision
  of better than 3 m/s in less than an hour for stars brighter than V =
  12. We have been fully funded with an NSF MRI grant, and expect our
  first spectrograph to be deployed in Spring of 2015, with the full
  network operation of all 6 units beginning in Spring of 2015. We will
  discuss the NRES design, goals, and robotic operation, as well as the
  early results from our prototype spectrograph.

Title: The IMF and SFH of the Galactic Bulge from HST
Authors: Gennaro, M.; Brown, T. M.; Anderson, J.; Avila, R.; van den
   Berg, D. A.; Sahu, K.; Bond, H. E.; Casertano, S.; Ferguson, H. C.;
   Livio, M.; Minniti, D.; Panagia, N.; Renzini, A.; Tumlinson, J.;
   Valenti, E.; Valenti, J. A.; Zoccali, M.
Bibcode: 2014fegb.confE..23G
Altcode:
  No abstract at ADS

Title: LEGUS: A Legacy ExtraGalactic UV Survey of Nearby Galaxies
    with HST
Authors: Lee, Janice C.; Calzetti, D.; Adamo, A.; Aloisi, A.; Andrews,
   J. E.; Brown, T. M.; Chandar, R.; Christian, C. A.; Cignoni, M.;
   Clayton, G. C.; Da Silva, R. L.; de Mink, S. E.; Dobbs, C.; Elmegreen,
   B.; Elmegreen, D. M.; Evans, A. S.; Fumagalli, M.; Gallagher, J. S.;
   Gouliermis, D.; Grebel, E.; Herrero-Davo`, A.; Hilbert, B.; Hunter,
   D. A.; Johnson, K. E.; Kennicutt, R.; Kim, H.; Krumholz, M. R.; Lennon,
   D. J.; Martin, C. D.; Nair, P.; Nota, A.; Pellerin, A.; Prieto, J.;
   Regan, M. W.; Sabbi, E.; Schaerer, D.; Schiminovich, D.; Smith, L. J.;
   Thilker, D. A.; Tosi, M.; Van Dyk, S. D.; Walterbos, R. A.; Whitmore,
   B. C.; Wofford, A.
Bibcode: 2014AAS...22321701L
Altcode:
  We introduce LEGUS, a Hubble Space Telescope program which will
  provide a critical missing piece in our efforts to solve the star
  formation puzzle: a robust characterization of the links between star
  formation on two fundamental scales, those of individual young stars,
  stellar clusters and associations over parsec scales, and of galaxy
  disks over kiloparsec scales. As a 154-orbit Treasury survey, LEGUS
  has begun obtaining NUV,U,B,V,I imaging of 50 star-forming galaxies,
  at distances of 4-12 Mpc. The dataset is guaranteed to have exceptional
  legacy value, as the targets have been carefully selected to uniformly
  sample a full range of global galaxy properties, as well as have
  the largest suites of multi-wavelength ancillary data available. The
  high-resolution HST NUV and U imaging are key for deriving accurate
  recent (&lt;50 Myr) star formation histories from resolved massive
  stars, along with the ages and masses for complete samples of star
  clusters and associations in each galaxy. We present an overview of
  the sample, the observations, and provide a first look at the science
  that the LEGUS team is pursuing. A companion poster presents the status
  of the program, and a more detailed description of the extensive data
  products being developed which will seed community science, and provide
  a foundation for studies of star formation with ALMA and JWST.

Title: The History of the Fourier Tachometer
Authors: Beckers, J. M.; Brown, T. M.
Bibcode: 2013ASPC..478...93B
Altcode:
  Following a suggestion by one of us (T. Brown) we developed in 1978
  at the Sacramento Peak Observatory the first version of what we
  called a Fourier Tachometer which measured the phase of a single
  frequency component of the Fourier transform of the solar spectrum
  associated with a specific solar spectrum line (Beckers &amp; Brown
  1978). This phase is a direct measure of the wavelength of that
  Line, its Doppler shift and by using polarization optics, its Zeeman
  splitting. This first version based on a Michelson interferometer
  (FT I) was later (Evans 1081) greatly improved by J.W. Evans by using
  a Solid Polarizing Interferometer (version FT II). The latest version
  stands out by its ability to: (i) get wavelength measurements over a
  large 2D field-of-view without the cumbersome use of a high-resolution
  spectrograph, (ii) have a wide angular field-of-view and étendue, (iii)
  be mechanically stable and use much real-time digital processing. The
  FT II was selected for use in Global Oscillation Network Group (GONG)
  in about 1985 and has since then also been used in the space based
  helioseismometers — Micheson Doppler Imager (MDI) onboard Solar
  and Heliospheric Observatory (Scherrer et al. 1995) and Helioseismic
  Magnetic Imager (HMI) onboard Solar Dynamics Observatory (Scherrer et
  al. 2012). The FT II performance has increased over the years with the
  current HMI version having 4096 × 4096 pixels, or 0.5 × 0.5 arcsec
  for the HMI full disk facility, and a cadence of 45 seconds. However,
  except for some early observations at the Sacramento Peak, the Fourier
  Tachometer has not appeared to have been applied to non-helioseismology
  ground-based observations. In ground-based telescopes science full
  precise line profiles are generally desired making the FT II undesirable
  since it only measures something close to their center-of-gravity. For
  future very large diameter (1.5 - 8 m) ground-based solar telescopes
  that will also be the case. But complimentary FT II observations,
  for example from the spectrograph reflecting slit-jaws, would
  provide valuable, high time and spatial resolution complimentary
  observations. The HMI version would have pixel sizes of about 0.03
  × 0.03 arcsec, closely matching the telescope resolution over a 2
  × 2 arcmin field-of-view provided by its Multi-Conjugate Adaptive
  Optics system.

Title: Observations and Orbits of Comets
Authors: Bacci, P.; Tesi, L.; Fagioli, G.; Cernis, K.; Foglia, S.;
   Galli, G.; Buzzi, L.; Snodgrass, C.; Sarneczky, K.; Bill, H.; Arnold,
   L.; Wainscoat, R. J.; Micheli, M.; Forshay, P.; Scotti, J. V.; Hill,
   R. E.; Kowalski, R. A.; Boattini, A.; Christensen, E. J.; Gibbs,
   A. R.; Grauer, A. D.; Johnson, J. A.; Larson, S. M.; Shelly, F. C.;
   Durig, D. T.; Wilkinson, I. J.; Brown, T. M.; Hergenrother, C. W.;
   Schwartz, M.; Holvorcem, P. R.; Castellano, J.; Vidal, J. R.; Dupouy,
   P.; de Vanssay, J. B.; Storey, D.; Salto, J. L.; Naves, R.; Kocher, P.;
   Cozzi, E.; Klotz, A.; Kugel, F.; Nicolas, J.; Aymami, J. M.; Montoro,
   L.; Bosch, J. M.; Olivera, R.; Audejean, M.; Bryssinck, E.; Soulier,
   J. -F.; Diepvens, A.; Gerke, V.; Plaksa, S.; Prystavski, T.; Hegedus,
   T.; Borkovits, T.; Biro, I. B.; Szing, A.; Csorgei, T.; Dangl, G.;
   Tercu, O.; Dumitriu, A.; Mantero, A.; Zhao, H. B.; Li, B.; Xia, Y.;
   Zhaori, G.; Hong, R. Q.; Hu, L. F.; Lu, H.; Takahashi, T.; Herald, D.;
   Primak, N.; Schultz, A.; Goggia, T.; Willman, M.; Veres, P.; Owens,
   R. P.; Angelone, C. G.; Christou, A. A.; Dymock, R.; Guido, E.; Howes,
   N.; Nicolini, M.; Thaluang, T.; Sato, H.; Hug, G.; Sherrod, P. C.;
   Bell, C.; Transient Factory, P.; Waszczak, A.; Masek, M.; Cerny, J.;
   Ebr, J.; Prouza, M.; Kubanek, P.; Jelinek, M.; Honkova, K.; Jurysek,
   J.; Lozano, J.; Martin, J. L.; Luis Martin Velasco, J.; Buczynski,
   D.; Limon, F.; Gonzalez, J.; Carreno, A.; Piqueras, J.; Hernandez,
   J. F.; Garcia, F.; Benishek, V.; Hudin, L.; Vintdevara, C.; Lake,
   P. B.; Maury, A.; F Soulier, J.; G Bosch, J.; Tremosa, L.; Soldan A.,
   F. C.; Williams, G. V.
Bibcode: 2013MPEC....V...07B
Altcode:
  No abstract at ADS

Title: Stellar ages through the corners of the boxy bulge
Authors: Valenti, E.; Zoccali, M.; Renzini, A.; Brown, T. M.; Gonzalez,
   O. A.; Minniti, D.; Debattista, V. P.; Mayer, L.
Bibcode: 2013A&A...559A..98V
Altcode: 2013arXiv1309.4570V
  <BR /> Aims: In some scenarios for the formation of the Milky Way bulge,
  the stellar population at the edges of the boxy bulge may be younger
  than those on the minor axis or close to the Galactic center. So far
  the only bulge region where deep color-magnitude diagrams have been
  obtained is indeed along the minor axis. To overcome this limitation,
  we aim to age-date the bulge stellar populations far away from
  the bulge minor axis. <BR /> Methods: Color-magnitude diagrams and
  luminosity functions have been obtained from deep near-IR VLT/HAWK-I
  images taken at the two Southern corners of the boxy bulge, i.e.,
  near the opposite edges of the Galactic bar. The foreground disk
  contamination has been statistically removed using a pure disk field
  observed with the same instrument and located approximately at similar
  Galactic latitudes of the two bulge fields and ~30° in longitude
  away from the Galactic center. For each bulge field, mean reddening
  and distance are determined using the position of red clump stars,
  and the metallicity distribution is derived photometrically using
  the color distribution of stars in the upper red giant branch. <BR
  /> Results: The resulting metallicity distribution function of both
  fields peaks around [Fe/H] ~ -0.1 dex, with the bulk of the stellar
  population having a metallicity within the range: -1 dex ≲ [Fe/H] ≲
  +0.4 dex, quite similar to that of other inner bulge fields. As for the
  previously explored inner fields, the color-magnitude diagrams of the
  two bar fields are consistent with their stellar population being older
  than ~10 Gyr, with no obvious evidence of younger population. <BR />
  Conclusions: The stellar population of the corners of the boxy bulge
  appears to be coeval with those within the innermost ~4° from the
  Galactic center. <P />Based on data taken at the ESO/VLT Telescope,
  within the observing program 081.B-0489(A).The derived photometric
  catalogs are only available at the CDS via anonymous ftp to <A
  href="http://cdsarc.u-strasbg.fr">http://cdsarc.u-strasbg.fr</A>
  (ftp://130.79.128.5) or via <A
  href="http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/559/A98">http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/559/A98</A>

Title: Las Cumbres Observatory Global Telescope Network
Authors: Brown, T. M.; Baliber, N.; Bianco, F. B.; Bowman, M.;
   Burleson, B.; Conway, P.; Crellin, M.; Depagne, É.; De Vera, J.;
   Dilday, B.; Dragomir, D.; Dubberley, M.; Eastman, J. D.; Elphick, M.;
   Falarski, M.; Foale, S.; Ford, M.; Fulton, B. J.; Garza, J.; Gomez,
   E. L.; Graham, M.; Greene, R.; Haldeman, B.; Hawkins, E.; Haworth,
   B.; Haynes, R.; Hidas, M.; Hjelstrom, A. E.; Howell, D. A.; Hygelund,
   J.; Lister, T. A.; Lobdill, R.; Martinez, J.; Mullins, D. S.; Norbury,
   M.; Parrent, J.; Paulson, R.; Petry, D. L.; Pickles, A.; Posner, V.;
   Rosing, W. E.; Ross, R.; Sand, D. J.; Saunders, E. S.; Shobbrook, J.;
   Shporer, A.; Street, R. A.; Thomas, D.; Tsapras, Y.; Tufts, J. R.;
   Valenti, S.; Vander Horst, K.; Walker, Z.; White, G.; Willis, M.
Bibcode: 2013PASP..125.1031B
Altcode: 2013arXiv1305.2437B
  Las Cumbres Observatory Global Telescope (LCOGT) is a young organization
  dedicated to time-domain observations at optical and (potentially)
  near-IR wavelengths. To this end, LCOGT is constructing a world-wide
  network of telescopes, including the two 2m Faulkes telescopes, as
  many as 17 x 1m telescopes, and as many as 23 x 40cm telescopes. These
  telescopes initially will be outfitted for imaging and (excepting the
  40cm telescopes) spectroscopy at wavelengths between the atmospheric
  UV cutoff and the roughly 1-micron limit of silicon detectors. Since
  the first of LCOGT's 1m telescopes are now being deployed, we lay
  out here LCOGT's scientific goals and the requirements that these
  goals place on network architecture and performance, we summarize
  the network's present and projected level of development, and we
  describe our expected schedule for completing it. In the bulk of
  the paper, we describe in detail the technical approaches that we
  have adopted to attain the desired performance. In particular, we
  discuss our choices for the number and location of network sites,
  for the number and sizes of telescopes, for the specifications of the
  first generation of instruments, for the software that will schedule
  and control the network's telescopes and reduce and archive its data,
  and for the structure of the scientific and educational programs for
  which the network will provide observations.

Title: VizieR Online Data Catalog: JK photometry in BUL<SUB>SC9 and
    BUL</SUB>SC29 (Valenti+,
Authors: Valenti, E.; Zoccali, M.; Renzini, A.; Brown, T. M.; Gonzalez,
   O.; Minniti, D.; Debattista, V. P.; Mayer, L.
Bibcode: 2013yCat..35590098V
Altcode: 2013yCat..35599098V
  Photometric catalogues of two bulge fields located at the edge of the
  edge of the Galactic bar. The J and K magnitudes have been calibrated
  onto the 2MASS photometric system. The position of the detected sources
  has been astrometrized by using 2MASS catalogs. <P />(2 data files).

Title: 2013 RT73
Authors: Okumura, S.; Hashimoto, N.; Manca, F.; Testa, A.; Pettarin,
   E.; Boattini, A.; Hill, R. E.; Christensen, E. J.; Gibbs, A. R.;
   Grauer, A. D.; Johnson, J. A.; Kowalski, R. A.; Larson, S. M.; Shelly,
   F. C.; Durig, D. T.; Boclair, C. A.; Schmidt, A. R.; Brown, T. M.;
   McCarthy Obs, J. J.; Polansky, M.; Robson, M.; Galli, G.; Mantero,
   A.; Holmes, R.; Vorobjov, T.; Buzzi, L.; Foglia, S.; Linder, T.; Hug,
   G.; Spagnotto, J.; Losse, F.; Birtwhistle, P.; Baj, G.
Bibcode: 2013MPEC....S...02O
Altcode:
  No abstract at ADS

Title: Transit Photometry with the LCOGT Network
Authors: Dragomir, Diana; Eastman, Jason; Brown, Tim; Street, Rachel;
   Lister, Tim; Tsapras, Yannis; Ross, Rachel; Fulton, Benjamin
Bibcode: 2013prpl.conf2K045D
Altcode:
  Within a single year, we deployed and commissioned a total of seven 1m
  telescopes to three sites (McDonald Observatory, CTIO and SAAO). These
  are complemented by two existing 2m telescopes, located in the northern
  (Haleakala) and southern (Siding Spring Observatory) hemispheres. Before
  the end of 2013, one additional 1m telescope will be deployed at
  McDonald Observatory, and two at Siding Spring Observatory, which will
  complete the southern ring and enable continuous LCOGT dark time in
  the southern hemisphere. We present transit observations acquired at
  each site with currently-deployed 1m telescopes. These data demonstrate
  some of the network's unique capabilities, such as simultaneous transit
  observations from multiple sites and construction of full transits by
  combining partial transit light curves from two sites. Such exercises
  pave the path toward searching for and characterizing transits of long
  period exoplanets, simultaneous multi-color transit observations, as
  well as studying spot distributions and rotation periods of exoplanet
  host stars using the LCOGT network.

Title: The Velocity Anisotropy of Distant Milky Way Halo Stars from
    Hubble Space Telescope Proper Motions
Authors: Deason, A. J.; Van der Marel, R. P.; Guhathakurta, P.; Sohn,
   S. T.; Brown, T. M.
Bibcode: 2013ApJ...766...24D
Altcode: 2013arXiv1302.5111D
  Based on long baseline (5-7 years) multi-epoch HST/ACS photometry,
  used previously to measure the proper motion of M31, we present the
  proper motions (PMs) of 13 main-sequence Milky Way halo stars. The
  sample lies at an average distance of r ~= 24 kpc from the Galactic
  center, with a root-mean-square spread of 6 kpc. At this distance,
  the median PM accuracy is 5 km s<SUP>-1</SUP>. We devise a maximum
  likelihood routine to determine the tangential velocity ellipsoid of
  the stellar halo. The velocity second moments in the directions of the
  Galactic (l, b) system are &lt; v^2_l &gt; ^{1/2} = 123^{+29}_{-23}
  km s<SUP>-1</SUP>, and &lt; v^2_b &gt; ^{1/2} = 83^{+24}_{-16} km
  s<SUP>-1</SUP>. We combine these results with the known line-of-sight
  second moment, &lt; v^2_los &gt; ^{1/2} = 105 +/- 5 km s<SUP>-1</SUP>,
  at this langrrang to study the velocity anisotropy of the halo. We
  find approximate isotropy between the radial and tangential velocity
  distributions, with anisotropy parameter β = 0.0^{+0.2}_{-0.4}. Our
  results suggest that the stellar halo velocity anisotropy out to r ~ 30
  kpc is less radially biased than solar neighborhood measurements. This
  is opposite to what is expected from violent relaxation, and may
  indicate the presence of a shell-type structure at r ~ 24 kpc. With
  additional multi-epoch HST data, the method presented here has the
  ability to measure the transverse kinematics of the halo for more stars,
  and to larger distances. This can yield new improved constraints on
  the stellar halo formation mechanism, and the mass of the Milky Way.

Title: VizieR Online Data Catalog: Kepler planetary
    candidates. III. (Batalha+, 2013)
Authors: Batalha, N. M.; Rowe, J. F.; Bryson, S. T.; Barclay, T.;
   Burke, C. J.; Caldwell, D. A.; Christiansen, J. L.; Mullally, F.;
   Thompson, S. E.; Brown, T. M.; Dupree, A. K.; Fabrycky, D. C.; Ford,
   E. B.; Fortney, J. J.; Gilliland, R. L.; Isaacson, H.; Latham,
   D. W.; Marcy, G. W.; Quinn, S. N.; Ragozzine, D.; Shporer, A.;
   Borucki, W. J.; Ciardi, D. R.; Gautier, T. N., III; Haas, M. R.;
   Jenkins, J. M.; Koch, D. G.; Lissauer, J. J.; Rapin, W.; Basri,
   G. S.; Boss, A. P.; Buchhave, L. A.; Carter, J. A.; Charbonneau, D.;
   Christensen-Dalsgaard, J.; Clarke, B. D.; Cochran, W. D.; Demory,
   B. -O.; Desert, J. -M.; DeVore, E.; Doyle, L. R.; Esquerdo, G. A.;
   Everett, M.; Fressin, F.; Geary, J. C.; Girouard, F. R.; Gould, A.;
   Hall, J. R.; Holman, M. J.; Howard, A. W.; Howell, S. B.; Ibrahim,
   K. A.; Kinemuchi, K.; Kjeldsen, H.; Klaus, T. C.; Li, J.; Lucas,
   P. W.; Meibom, S.; Morris, R. L.; Prsa, A.; Quintana, E.; Sanderfer,
   D. T.; Sasselov, D.; Seader, S. E.; Smith, J. C.; Steffen, J. H.;
   Still, M.; Stumpe, M. C.; Tarter, J. C.; Tenenbaum, P.; Torres, G.;
   Twicken, J. D.; Uddin, K.; van Cleve, J.; Walkowicz, L.; Welsh, W. F.
Bibcode: 2013yCat..22040024B
Altcode:
  The data employed for transit identification were acquired between 2009
  May 13 00:15 UTC and 2010 Sep 22 19:03 UTC (Q1-Q6). Over 190000 stars
  were observed at some time during this period. <P />(6 data files).

Title: Planetary Candidates Observed by Kepler. III. Analysis of
    the First 16 Months of Data
Authors: Batalha, Natalie M.; Rowe, Jason F.; Bryson, Stephen
   T.; Barclay, Thomas; Burke, Christopher J.; Caldwell, Douglas A.;
   Christiansen, Jessie L.; Mullally, Fergal; Thompson, Susan E.; Brown,
   Timothy M.; Dupree, Andrea K.; Fabrycky, Daniel C.; Ford, Eric B.;
   Fortney, Jonathan J.; Gilliland, Ronald L.; Isaacson, Howard; Latham,
   David W.; Marcy, Geoffrey W.; Quinn, Samuel N.; Ragozzine, Darin;
   Shporer, Avi; Borucki, William J.; Ciardi, David R.; Gautier, Thomas
   N., III; Haas, Michael R.; Jenkins, Jon M.; Koch, David G.; Lissauer,
   Jack J.; Rapin, William; Basri, Gibor S.; Boss, Alan P.; Buchhave,
   Lars A.; Carter, Joshua A.; Charbonneau, David; Christensen-Dalsgaard,
   Joergen; Clarke, Bruce D.; Cochran, William D.; Demory, Brice-Olivier;
   Desert, Jean-Michel; Devore, Edna; Doyle, Laurance R.; Esquerdo,
   Gilbert A.; Everett, Mark; Fressin, Francois; Geary, John C.; Girouard,
   Forrest R.; Gould, Alan; Hall, Jennifer R.; Holman, Matthew J.; Howard,
   Andrew W.; Howell, Steve B.; Ibrahim, Khadeejah A.; Kinemuchi, Karen;
   Kjeldsen, Hans; Klaus, Todd C.; Li, Jie; Lucas, Philip W.; Meibom,
   Søren; Morris, Robert L.; Prša, Andrej; Quintana, Elisa; Sanderfer,
   Dwight T.; Sasselov, Dimitar; Seader, Shawn E.; Smith, Jeffrey C.;
   Steffen, Jason H.; Still, Martin; Stumpe, Martin C.; Tarter, Jill C.;
   Tenenbaum, Peter; Torres, Guillermo; Twicken, Joseph D.; Uddin, Kamal;
   Van Cleve, Jeffrey; Walkowicz, Lucianne; Welsh, William F.
Bibcode: 2013ApJS..204...24B
Altcode: 2012arXiv1202.5852B
  New transiting planet candidates are identified in 16 months (2009
  May-2010 September) of data from the Kepler spacecraft. Nearly 5000
  periodic transit-like signals are vetted against astrophysical and
  instrumental false positives yielding 1108 viable new planet candidates,
  bringing the total count up to over 2300. Improved vetting metrics
  are employed, contributing to higher catalog reliability. Most notable
  is the noise-weighted robust averaging of multi-quarter photo-center
  offsets derived from difference image analysis that identifies likely
  background eclipsing binaries. Twenty-two months of photometry are used
  for the purpose of characterizing each of the candidates. Ephemerides
  (transit epoch, T <SUB>0</SUB>, and orbital period, P) are tabulated
  as well as the products of light curve modeling: reduced radius
  (R <SUB>P</SUB>/R <SUB>sstarf</SUB>), reduced semimajor axis (d/R
  <SUB>sstarf</SUB>), and impact parameter (b). The largest fractional
  increases are seen for the smallest planet candidates (201% for
  candidates smaller than 2 R <SUB>⊕</SUB> compared to 53% for
  candidates larger than 2 R <SUB>⊕</SUB>) and those at longer orbital
  periods (124% for candidates outside of 50 day orbits versus 86% for
  candidates inside of 50 day orbits). The gains are larger than expected
  from increasing the observing window from 13 months (Quarters 1-5)
  to 16 months (Quarters 1-6) even in regions of parameter space where
  one would have expected the previous catalogs to be complete. Analyses
  of planet frequencies based on previous catalogs will be affected by
  such incompleteness. The fraction of all planet candidate host stars
  with multiple candidates has grown from 17% to 20%, and the paucity of
  short-period giant planets in multiple systems is still evident. The
  progression toward smaller planets at longer orbital periods with each
  new catalog release suggests that Earth-size planets in the habitable
  zone are forthcoming if, indeed, such planets are abundant.

Title: LCOGT's New Telescopes and Instruments
Authors: Brown, Timothy M.; Becker, M.; Burleson, B.; De Vera, J.;
   Dragomir, D.; Dubberley, M.; Eastman, J.; Graham, M.; Haldeman, B.;
   Hawkins, E.; Haynes, R.; Hjelstrom, A.; Howell, D. A.; Hygelund,
   J.; Lister, T.; Lobdill, R.; Norbury, M.; Petry, D.; Pickles, A.;
   Posner, V.; Rosing, W.; Sand, D.; Street, R.; Tsapras, Y.; Tufts,
   J.; Valenti, S.
Bibcode: 2013AAS...22134523B
Altcode:
  Las Cumbres Observatory Global Telescope (LCOGT) is developing
  a world-wide network of robotic optical telescopes dedicated to
  time-domain astronomy. The last year has seen 3 major expansions in
  our observing capabilities. (1) We have deployed and commissioned
  4 new 1m telescopes at McDonald Observatory and at CTIO, and we are
  in the process of deploying 5 more at the South African Astronomical
  Observatory and at Siding Spring Observatory in Australia. (2) We have
  commissioned low-resolution spectrographs on the Faulkes 2m telescopes;
  these will become available to users in the 2013A semester, beginning 1
  April 2013. (3) We have commissioned the NRES Prototype cross-dispersed
  echelle spectrograph on our 0.8m telescope in California, giving
  LCOGT its first capability to perform radial-velocity and spectral
  classification observations. We describe here early science results
  from each of these 3 new systems.

Title: The Panchromatic Hubble Ultra Deep Field: Ultraviolet Coverage
Authors: Teplitz, Harry I.; Rafelski, M.; Grogin, N. A.; Koekemoer,
   A. M.; Siana, B. D.; Atek, H.; Bond, N. A.; Brown, T. M.; Coe, D. A.;
   Colbert, J. W.; De Mello, D. F.; Ferguson, H. C.; Finkelstein, S. L.;
   Gardner, J. P.; Gawiser, E. J.; Giavalisco, M.; Gronwall, C.; Hanish,
   D.; Kurczynski, P.; Lee, K.; Ravindranath, S.; Ryan, R. E.; Scarlata,
   C.; Voyer, E.; Wolfe, A. M.
Bibcode: 2013AAS...22122801T
Altcode:
  We present intial results from the UVUDF project: a Cycle 19 HST
  Treasury program that obtained ultraviolet imaging of the Hubble Ultra
  Deep Field. The data consist of 30 orbits with WFC3/UVIS in each of
  F225W, F275W, and F336W, divided between three epochs. The science
  goals of the UVUDF project are to: (i) Investigate the episode of peak
  star formation activity in galaxies at 1 &lt; z &lt; 2.5; (ii) Study the
  star formation properties of moderate redshift starburst galaxies; (iii)
  Probe the evolution of massive galaxies by resolving sub-galactic units
  (clumps); (iv) Examine the escape fraction of ionizing radiation from
  galaxies at 2-3; and (v) Measure the star formation rate efficiency of
  neutral atomic-dominated hydrogen gas at 1-3. In addition to the first
  UVUDF science results, we discuss technical lessons learned that may
  be of interst in planning future deep UV surveys with HST.

Title: The PTF Orion Project: A Possible Planet Transiting a
    T-Tauri Star
Authors: van Eyken, Julian C.; Ciardi, David R.; von Braun, Kaspar;
   Kane, Stephen R.; Plavchan, Peter; Bender, Chad F.; Brown, Timothy
   M.; Crepp, Justin R.; Fulton, Benjamin J.; Howard, Andrew W.; Howell,
   Steve B.; Mahadevan, Suvrath; Marcy, Geoffrey W.; Shporer, Avi; Szkody,
   Paula; Akeson, Rachel L.; Beichman, Charles A.; Boden, Andrew F.;
   Gelino, Dawn M.; Hoard, D. W.; Ramírez, Solange V.; Rebull, Luisa
   M.; Stauffer, John R.; Bloom, Joshua S.; Cenko, S. Bradley; Kasliwal,
   Mansi M.; Kulkarni, Shrinivas R.; Law, Nicholas M.; Nugent, Peter E.;
   Ofek, Eran O.; Poznanski, Dovi; Quimby, Robert M.; Walters, Richard;
   Grillmair, Carl J.; Laher, Russ; Levitan, David B.; Sesar, Branimir;
   Surace, Jason A.
Bibcode: 2012ApJ...755...42V
Altcode: 2012arXiv1206.1510V
  We report observations of a possible young transiting planet orbiting
  a previously known weak-lined T-Tauri star in the 7-10 Myr old
  Orion-OB1a/25-Ori region. The candidate was found as part of the
  Palomar Transient Factory (PTF) Orion project. It has a photometric
  transit period of 0.448413 ± 0.000040 days, and appears in both
  2009 and 2010 PTF data. Follow-up low-precision radial velocity (RV)
  observations and adaptive optics imaging suggest that the star is not
  an eclipsing binary, and that it is unlikely that a background source
  is blended with the target and mimicking the observed transit. RV
  observations with the Hobby-Eberly and Keck telescopes yield an RV
  that has the same period as the photometric event, but is offset in
  phase from the transit center by ≈ - 0.22 periods. The amplitude
  (half range) of the RV variations is 2.4 km s<SUP>-1</SUP> and is
  comparable with the expected RV amplitude that stellar spots could
  induce. The RV curve is likely dominated by stellar spot modulation
  and provides an upper limit to the projected companion mass of M
  <SUB>p</SUB>sin i <SUB>orb</SUB> &lt;~ 4.8 ± 1.2 M <SUB>Jup</SUB>;
  when combined with the orbital inclination, i <SUB>orb</SUB>, of the
  candidate planet from modeling of the transit light curve, we find an
  upper limit on the mass of the planetary candidate of M <SUB>p</SUB>
  &lt;~ 5.5 ± 1.4 M <SUB>Jup</SUB>. This limit implies that the planet
  is orbiting close to, if not inside, its Roche limiting orbital radius,
  so that it may be undergoing active mass loss and evaporation.

Title: Planet Occurrence within 0.25 AU of Solar-type Stars from
    Kepler
Authors: Howard, Andrew W.; Marcy, Geoffrey W.; Bryson, Stephen T.;
   Jenkins, Jon M.; Rowe, Jason F.; Batalha, Natalie M.; Borucki, William
   J.; Koch, David G.; Dunham, Edward W.; Gautier, Thomas N., III; Van
   Cleve, Jeffrey; Cochran, William D.; Latham, David W.; Lissauer,
   Jack J.; Torres, Guillermo; Brown, Timothy M.; Gilliland, Ronald
   L.; Buchhave, Lars A.; Caldwell, Douglas A.; Christensen-Dalsgaard,
   Jørgen; Ciardi, David; Fressin, Francois; Haas, Michael R.; Howell,
   Steve B.; Kjeldsen, Hans; Seager, Sara; Rogers, Leslie; Sasselov,
   Dimitar D.; Steffen, Jason H.; Basri, Gibor S.; Charbonneau, David;
   Christiansen, Jessie; Clarke, Bruce; Dupree, Andrea; Fabrycky,
   Daniel C.; Fischer, Debra A.; Ford, Eric B.; Fortney, Jonathan J.;
   Tarter, Jill; Girouard, Forrest R.; Holman, Matthew J.; Johnson,
   John Asher; Klaus, Todd C.; Machalek, Pavel; Moorhead, Althea V.;
   Morehead, Robert C.; Ragozzine, Darin; Tenenbaum, Peter; Twicken,
   Joseph D.; Quinn, Samuel N.; Isaacson, Howard; Shporer, Avi; Lucas,
   Philip W.; Walkowicz, Lucianne M.; Welsh, William F.; Boss, Alan;
   Devore, Edna; Gould, Alan; Smith, Jeffrey C.; Morris, Robert L.;
   Prsa, Andrej; Morton, Timothy D.; Still, Martin; Thompson, Susan E.;
   Mullally, Fergal; Endl, Michael; MacQueen, Phillip J.
Bibcode: 2012ApJS..201...15H
Altcode: 2011arXiv1103.2541H
  We report the distribution of planets as a function of planet radius,
  orbital period, and stellar effective temperature for orbital periods
  less than 50 days around solar-type (GK) stars. These results are based
  on the 1235 planets (formally "planet candidates") from the Kepler
  mission that include a nearly complete set of detected planets as
  small as 2 R <SUB>⊕</SUB>. For each of the 156,000 target stars,
  we assess the detectability of planets as a function of planet
  radius, R <SUB>p</SUB>, and orbital period, P, using a measure of the
  detection efficiency for each star. We also correct for the geometric
  probability of transit, R <SUB>sstarf</SUB>/a. We consider first
  Kepler target stars within the "solar subset" having T <SUB>eff</SUB>
  = 4100-6100 K, log g = 4.0-4.9, and Kepler magnitude Kp &lt; 15 mag,
  i.e., bright, main-sequence GK stars. We include only those stars
  having photometric noise low enough to permit detection of planets
  down to 2 R <SUB>⊕</SUB>. We count planets in small domains of R
  <SUB>p</SUB> and P and divide by the included target stars to calculate
  planet occurrence in each domain. The resulting occurrence of planets
  varies by more than three orders of magnitude in the radius-orbital
  period plane and increases substantially down to the smallest radius
  (2 R <SUB>⊕</SUB>) and out to the longest orbital period (50 days,
  ~0.25 AU) in our study. For P &lt; 50 days, the distribution of planet
  radii is given by a power law, df/dlog R = k<SUB>R</SUB>R <SUP>α</SUP>
  with k<SUB>R</SUB> = 2.9<SUP>+0.5</SUP> <SUB>- 0.4</SUB>, α = -1.92 ±
  0.11, and R ≡ R <SUB>p</SUB>/R <SUB>⊕</SUB>. This rapid increase
  in planet occurrence with decreasing planet size agrees with the
  prediction of core-accretion formation but disagrees with population
  synthesis models that predict a desert at super-Earth and Neptune
  sizes for close-in orbits. Planets with orbital periods shorter than
  2 days are extremely rare; for R <SUB>p</SUB> &gt; 2 R <SUB>⊕</SUB>
  we measure an occurrence of less than 0.001 planets per star. For all
  planets with orbital periods less than 50 days, we measure occurrence
  of 0.130 ± 0.008, 0.023 ± 0.003, and 0.013 ± 0.002 planets per
  star for planets with radii 2-4, 4-8, and 8-32 R <SUB>⊕</SUB>,
  in agreement with Doppler surveys. We fit occurrence as a function
  of P to a power-law model with an exponential cutoff below a critical
  period P <SUB>0</SUB>. For smaller planets, P <SUB>0</SUB> has larger
  values, suggesting that the "parking distance" for migrating planets
  moves outward with decreasing planet size. We also measured planet
  occurrence over a broader stellar T <SUB>eff</SUB> range of 3600-7100
  K, spanning M0 to F2 dwarfs. Over this range, the occurrence of 2-4 R
  <SUB>⊕</SUB> planets in the Kepler field increases with decreasing
  T <SUB>eff</SUB>, with these small planets being seven times more
  abundant around cool stars (3600-4100 K) than the hottest stars in
  our sample (6600-7100 K). <P />Based in part on observations obtained
  at the W. M. Keck Observatory, which is operated by the University of
  California and the California Institute of Technology.

Title: Ultraviolet Observations of the Hubble Ultra Deep Field
Authors: Rafelski, Marc; Teplitz, H.; Grogin, N.; Koekemoer, A.;
   Siana, B.; Atek, H.; Bond, N. A.; Brown, T. M.; Coe, D.; Colbert, J.;
   Ferguson, H. C.; Finkelstein, S. L.; Gardner, J. P.; Gawiser, E.;
   Giavalisco, M.; Gronwall, C.; Hanish, D.; Kurczynski, P.; Lee, K.;
   Ravindranath, S.; Scarlata, C.; Voyer, E.; Wolfe, A.; de Mello, D. F.
Bibcode: 2012AAS...22042104R
Altcode:
  We present details of a 90-orbit HST treasury program to obtain
  Ultraviolet (UV) imaging of the Hubble Ultra Deep Field (UDF) using
  the WFC3-UVIS detector with the F225W, F275W, and F336W filters. These
  UV images will reach point source detection limits of AB=29 at 10
  sigma. This survey is designed to: (i) Investigate the episode of peak
  star formation activity in galaxies at 1 &lt; z &lt; 2.5. (ii) Study the
  star formation properties of moderate redshift starburst galaxies. (iii)
  Probe the evolution of massive galaxies by resolving sub-galactic units
  (clumps). (iv) Examine the escape fraction of ionizing radiation from
  galaxies at z 2-3. (v) Measure the star formation rate efficiency
  of neutral atomic-dominated hydrogen gas at z 1-3. We will present
  preliminary results from the UVUDF team based on the first observations
  (beginning March 2012).

Title: Using HST to Detect Isolated Black Holes and Neutron Stars
    through Astrometric Microlensing
Authors: Sahu, Kailash C.; Albrow, M.; Anderson, J.; Bond, H. E.;
   Bond, I.; Brown, T. M.; Casertano, S.; Dominik, M.; Ferguson, H. C.;
   Fryer, C.; Livio, M.; Mao, S.; Perrott, Y.; Udalski, A.; Yock, P.
Bibcode: 2012AAS...22030703S
Altcode:
  To date, Black Hole (BH) and Neutron Star (NS) masses have been
  directly measured only in binaries; no isolated stellar-mass BH has
  been detected unambiguously within our Galaxy. We have underway a
  large, 3-year HST program (192 orbits) designed to detect microlensing
  events caused by non-luminous isolated BHs and NSs in the direction
  of the Galactic bulge. Our program consists of monitoring of 12
  fields in the Sagittarius window of the Galactic bulge, containing
  a total of 1.5 million stars down to V=28. Our observations have a
  typical cadence of one observation every two weeks, and are primarily
  targeted towards detecting microlensing events caused by non-luminous
  isolated BHs and NSs in the Galactic disk and bulge. <P />The unique
  capability of HST imaging for microlensing observations is the addition
  of high-precision astrometry, allowing detection of the astrometric
  shift of the source during the event. Combined with the lens parallax,
  which can be determined from the light curve as measured by HST (and
  supplemented by GEMINI) observations, the astrometric shift provides a
  direct measurement of the lens mass. Our program is optimized to detect
  long-duration events, which are more likely to be caused by massive
  lenses. We expect to detect a few dozen long-duration microlensing
  events, of which 45% will show astrometric deflections, leading to
  direct determinations of the lens masses.

Title: On using the beaming effect to measure spin-orbit alignment
    in stellar binaries with Sun-like components
Authors: Shporer, Avi; Brown, Tim; Mazeh, Tsevi; Zucker, Shay
Bibcode: 2012NewA...17..309S
Altcode: 2011arXiv1107.4458S
  The beaming effect (aka Doppler boosting) induces a variation in the
  observed flux of a luminous object, following its observed radial
  velocity variation. We describe a photometric signal induced by the
  beaming effect during eclipse of binary systems, where the stellar
  components are late type Sun-like stars. The shape of this signal is
  sensitive to the angle between the eclipsed star's spin axis and the
  orbital angular momentum axis, thereby allowing its measurement. We show
  that during eclipse there are in fact two effects, superimposed on the
  known eclipse light curve. One effect is produced by the rotation of
  the eclipsed star, and is the photometric analog of the spectroscopic
  Rossiter-McLaughlin effect, thereby it contains information about
  the sky-projected spin-orbit angle. The other effect is produced by
  the varying weighted difference, during eclipse, between the beaming
  signals of the two stars. We give approximated analytic expressions for
  the amplitudes of the two effects, and present a numerical simulation
  where we show the light curves for the two effects for various orbital
  orientations, for a low mass ratio stellar eclipsing binary system. We
  show that although the overall signal is small, it can be detected
  in the primary eclipse when using Kepler Long Cadence data of bright
  systems accumulated over the mission lifetime.

Title: New Observational Evidence of Flash Mixing on the White Dwarf
    Cooling Curve
Authors: Brown, T. M.; Lanz, T.; Sweigart, A. V.; Cracraft, M.;
   Hubeny, I.; Landsman, W. B.
Bibcode: 2012ASPC..452...23B
Altcode: 2012arXiv1201.4204B
  Blue hook stars are a class of subluminous extreme horizontal branch
  stars that were discovered in UV images of the massive globular clusters
  ω Cen and NGC 2808. These stars occupy a region of the HR diagram
  that is unexplained by canonical stellar evolution theory. Using
  new theoretical evolutionary and atmospheric models, we have shown
  that the blue hook stars are very likely the progeny of stars that
  undergo extensive internal mixing during a late helium-core flash
  on the white dwarf cooling curve. This “flash mixing” produces
  hotter-than-normal EHB stars with atmospheres significantly enhanced
  in helium and carbon. The larger bolometric correction, combined with
  the decrease in hydrogen opacity, makes these stars appear subluminous
  in the optical and UV. Flash mixing is more likely to occur in stars
  born with a high helium abundance, due to their lower mass at the
  main sequence turnoff. For this reason, the phenomenon is more common
  in those massive globular clusters that show evidence for secondary
  populations enhanced in helium. However, a high helium abundance does
  not, by itself, explain the presence of blue hook stars in massive
  globular clusters. Here, we present new observational evidence for flash
  mixing, using recent HST observations. These include UV color-magnitude
  diagrams of six massive globular clusters and far-UV spectroscopy of
  hot subdwarfs in one of these clusters (NGC 2808).

Title: An eclipsing post-common-envelope binary in the field of the
    Kepler mission
Authors: Almenara, J. M.; Alonso, R.; Rabus, M.; Lázaro, C.; Arévalo,
   M. J.; Belmonte, J. A.; Deeg, H. J.; Brown, T. M.; Vázquez Ramió, H.
Bibcode: 2012MNRAS.420.3017A
Altcode:
  We present a new eclipsing post-common-envelope binary,
  identified inside the Kepler field prior to the launch of the
  spacecraft. Multifilter photometry and radial velocity data are analysed
  with an eclipsing-binary modelling code to determine the physical
  parameters of the binary. Spectra of the system within the primary
  eclipse and uneclipsed allow us to identify the spectral characteristics
  of the primary and secondary components. The primary component of
  the binary is a DA white dwarf, with M≃ 0.61 M<SUB>⊙</SUB>, log
  g≃ 7.95 and T<SUB>eff</SUB>≃ 20 500 K. <P />The detection of two
  flares and the emission signatures displayed in the spectra show that
  the secondary component of the system is chromospherically active and
  is classified as an active M4 main-sequence star. Its mass, radius
  and temperature are estimated as M≃ 0.39 M<SUB>⊙</SUB>, R≃
  0.37 R<SUB>⊙</SUB> and T<SUB>eff</SUB>≃ 3200 K. The ephemeris
  of the system is HJD = 245 3590.436 126(10) + 0.350 468 722(6)
  ×E. <P />This binary is a new post-common-envelope binary (PCEB),
  with physical parameters within the range found in other systems of
  this small group of evolved binaries.

Title: VizieR Online Data Catalog: Masses and radii of eclipsing
    binaries (Brown, 2010)
Authors: Brown, T. M.
Bibcode: 2012yCat..17090535B
Altcode:
  I implemented the {rho}<SUB>*</SUB> method, using the Yonsei-Yale evo
  tracks (Yi et al. 2001ApJS..136..417Y; Kim et al. 2002ApJS..143..499K;
  Yi et al. 2003ApJS..144..259Y; Demarque et al. 2004ApJS..155..667D)
  as the needed stellar evolution models, and I then applied it to the
  Torres et al., (2009, Cat. J/other/A+ARV/18.67) tabulation of EBs and
  to 15 stars with asteroseismic measurements. <P />(1 data file).

Title: Spectroscopy at LCOGT
Authors: Brown, Timothy M.; Becker, M.; Burleson, B.; De Vera, J.;
   Dubberley, M.; Eastman, J.; Haldeman, B.; Hawkins, E.; Haynes, R.;
   Hygelund, J.; Lister, T.; Lobdill, R.; Norbury, M.; Pickles, A.;
   Rosing, W.; Sand, D.; Tufts, J.
Bibcode: 2012AAS...21942203B
Altcode:
  Las Cumbres Observatory Global Telescope (LCOGT) is developing a
  world-wide network of optical telescopes dedicated to time-domain
  astronomy. In a few years, the network will consist of more than twenty
  0.4m telescopes, about fifteen 1m telescopes, and two 2m telescopes. We
  are now developing spectrographs to use with this network; here we
  describe the performance goals and status of these instruments. Furthest
  along is FLOYDS, a low-resolution spectrograph that will cover 330nm -
  1040 nm in one shot, using two diffraction orders. FLOYDS is intended
  mostly for SN classification and time-evolution studies. We will install
  copies of this spectrograph on each of LCOGT's 2m Faulkes telescopes,
  beginning with FTN early in 2012. Still in the prototype stage is
  MRES, a medium-resolution (R=45,000) fiber-fed cross-dispersed echelle
  covering 380nm-850nm. It will accept fibers from up to 3 co-located
  1m telescopes, so that we can observe multiple targets at once, or
  gain S/N by devoting multiple telescopes to a single target. The
  spectrograph is designed for easy control of its light path and
  environment, to facilitate accurate and repeatable measurements. MRES
  will be used mostly for validation and study of extrasolar planets,
  and for time-domain studies of pulsating and magnetically active stars.

Title: The Atmospheres of the Hot-Jupiters Kepler-5b and Kepler-6b
    Observed during Occultations with Warm-Spitzer and Kepler
Authors: Désert, Jean-Michel; Charbonneau, David; Fortney, Jonathan
   J.; Madhusudhan, Nikku; Knutson, Heather A.; Fressin, François;
   Deming, Drake; Borucki, William J.; Brown, Timothy M.; Caldwell,
   Douglas; Ford, Eric B.; Gilliland, Ronald L.; Latham, David W.; Marcy,
   Geoffrey W.; Seager, Sara
Bibcode: 2011ApJS..197...11D
Altcode: 2011arXiv1102.0555D
  This paper reports the detection and the measurements of occultations of
  the two transiting hot giant exoplanets Kepler-5b and Kepler-6b by their
  parent stars. The observations are obtained in the near-infrared with
  Warm-Spitzer Space Telescope and at optical wavelengths by combining
  more than a year of Kepler photometry. The investigation consists of
  constraining the eccentricities of these systems and of obtaining
  broadband emergent photometric data for individual planets. For
  both targets, the occultations are detected at the 3σ level at
  each wavelength with mid-occultation times consistent with circular
  orbits. The brightness temperatures of these planets are deduced from
  the infrared observations and reach T <SUB>Spitzer</SUB> = 1930 ± 100 K
  and T <SUB>Spitzer</SUB> = 1660 ± 120 K for Kepler-5b and Kepler-6b,
  respectively. We measure optical geometric albedos A<SUB>g</SUB>
  in the Kepler bandpass and find A<SUB>g</SUB> = 0.12 ± 0.04 for
  Kepler-5b and A<SUB>g</SUB> = 0.11 ± 0.04 for Kepler-6b, leading to
  upper an limit for the Bond albedo of A <SUB>B</SUB> &lt;= 0.17 in both
  cases. The observations for both planets are best described by models
  for which most of the incident energy is redistributed on the dayside,
  with only less than 10% of the absorbed stellar flux redistributed to
  the nightside of these planets.

Title: Kepler-10 c: a 2.2 Earth Radius Transiting Planet in a
    Multiple System
Authors: Fressin, François; Torres, Guillermo; Désert, Jean-Michel;
   Charbonneau, David; Batalha, Natalie M.; Fortney, Jonathan J.; Rowe,
   Jason F.; Allen, Christopher; Borucki, William J.; Brown, Timothy M.;
   Bryson, Stephen T.; Ciardi, David R.; Cochran, William D.; Deming,
   Drake; Dunham, Edward W.; Fabrycky, Daniel C.; Gautier, Thomas N.,
   III; Gilliland, Ronald L.; Henze, Christopher E.; Holman, Matthew
   J.; Howell, Steve B.; Jenkins, Jon M.; Kinemuchi, Karen; Knutson,
   Heather; Koch, David G.; Latham, David W.; Lissauer, Jack J.; Marcy,
   Geoffrey W.; Ragozzine, Darin; Sasselov, Dimitar D.; Still, Martin;
   Tenenbaum, Peter; Uddin, Kamal
Bibcode: 2011ApJS..197....5F
Altcode: 2011arXiv1105.4647F
  The Kepler mission has recently announced the discovery of Kepler-10
  b, the smallest exoplanet discovered to date and the first rocky
  planet found by the spacecraft. A second, 45 day period transit-like
  signal present in the photometry from the first eight months of data
  could not be confirmed as being caused by a planet at the time of that
  announcement. Here we apply the light curve modeling technique known as
  BLENDER to explore the possibility that the signal might be due to an
  astrophysical false positive (blend). To aid in this analysis we report
  the observation of two transits with the Spitzer Space Telescope at 4.5
  μm. When combined, they yield a transit depth of 344 ± 85 ppm that
  is consistent with the depth in the Kepler passband (376 ± 9 ppm,
  ignoring limb darkening), which rules out blends with an eclipsing
  binary of a significantly different color than the target. Using these
  observations along with other constraints from high-resolution imaging
  and spectroscopy, we are able to exclude the vast majority of possible
  false positives. We assess the likelihood of the remaining blends, and
  arrive conservatively at a false alarm rate of 1.6 × 10<SUP>-5</SUP>
  that is small enough to validate the candidate as a planet (designated
  Kepler-10 c) with a very high level of confidence. The radius of
  this object is measured to be R<SUB>p</SUB> = 2.227<SUP>+0.052</SUP>
  <SUB>-0.057</SUB> R <SUB>⊕</SUB> (in which the error includes
  the uncertainty in the stellar properties), but currently available
  radial-velocity measurements only place an upper limit on its mass
  of about 20 M <SUB>⊕</SUB>. Kepler-10 c represents another example
  (with Kepler-9 d and Kepler-11 g) of statistical "validation" of a
  transiting exoplanet, as opposed to the usual "confirmation" that
  can take place when the Doppler signal is detected or transit timing
  variations are measured. It is anticipated that many of Kepler's
  smaller candidates will receive a similar treatment since dynamical
  confirmation may be difficult or impractical with the sensitivity of
  current instrumentation.

Title: Kepler-14b: A Massive Hot Jupiter Transiting an F Star in a
    Close Visual Binary
Authors: Buchhave, Lars A.; Latham, David W.; Carter, Joshua A.;
   Désert, Jean-Michel; Torres, Guillermo; Adams, Elisabeth R.; Bryson,
   Stephen T.; Charbonneau, David B.; Ciardi, David R.; Kulesa, Craig;
   Dupree, Andrea K.; Fischer, Debra A.; Fressin, François; Gautier,
   Thomas N., III; Gilliland, Ronald L.; Howell, Steve B.; Isaacson,
   Howard; Jenkins, Jon M.; Marcy, Geoffrey W.; McCarthy, Donald W.;
   Rowe, Jason F.; Batalha, Natalie M.; Borucki, William J.; Brown,
   Timothy M.; Caldwell, Douglas A.; Christiansen, Jessie L.; Cochran,
   William D.; Deming, Drake; Dunham, Edward W.; Everett, Mark; Ford,
   Eric B.; Fortney, Jonathan J.; Geary, John C.; Girouard, Forrest R.;
   Haas, Michael R.; Holman, Matthew J.; Horch, Elliott; Klaus, Todd C.;
   Knutson, Heather A.; Koch, David G.; Kolodziejczak, Jeffrey; Lissauer,
   Jack J.; Machalek, Pavel; Mullally, Fergal; Still, Martin D.; Quinn,
   Samuel N.; Seager, Sara; Thompson, Susan E.; Van Cleve, Jeffrey
Bibcode: 2011ApJS..197....3B
Altcode: 2011arXiv1106.5510B
  We present the discovery of a hot Jupiter transiting an F star in
  a close visual (0farcs3 sky projected angular separation) binary
  system. The dilution of the host star's light by the nearly equal
  magnitude stellar companion (~0.5 mag fainter) significantly affects
  the derived planetary parameters, and if left uncorrected, leads
  to an underestimate of the radius and mass of the planet by 10%
  and 60%, respectively. Other published exoplanets, which have not
  been observed with high-resolution imaging, could similarly have
  unresolved stellar companions and thus have incorrectly derived
  planetary parameters. Kepler-14b (KOI-98) has a period of P = 6.790
  days and, correcting for the dilution, has a mass of M<SUB>p</SUB> =
  8.40<SUP>+0.35</SUP> <SUB> - 0.34</SUB> M <SUB>J</SUB> and a radius
  of R<SUB>p</SUB> = 1.136<SUP>+0.073</SUP> <SUB> - 0.054</SUB> R
  <SUB>J</SUB>, yielding a mean density of ρ<SUB> p </SUB> = 7.1 ±
  1.1 g cm<SUP>-3</SUP>.

Title: The Hot-Jupiter Kepler-17b: Discovery, Obliquity from
    Stroboscopic Starspots, and Atmospheric Characterization
Authors: Désert, Jean-Michel; Charbonneau, David; Demory,
   Brice-Olivier; Ballard, Sarah; Carter, Joshua A.; Fortney, Jonathan
   J.; Cochran, William D.; Endl, Michael; Quinn, Samuel N.; Isaacson,
   Howard T.; Fressin, François; Buchhave, Lars A.; Latham, David W.;
   Knutson, Heather A.; Bryson, Stephen T.; Torres, Guillermo; Rowe,
   Jason F.; Batalha, Natalie M.; Borucki, William J.; Brown, Timothy
   M.; Caldwell, Douglas A.; Christiansen, Jessie L.; Deming, Drake;
   Fabrycky, Daniel C.; Ford, Eric B.; Gilliland, Ronald L.; Gillon,
   Michaël; Haas, Michaël R.; Jenkins, Jon M.; Kinemuchi, Karen; Koch,
   David; Lissauer, Jack J.; Lucas, Philip; Mullally, Fergal; MacQueen,
   Phillip J.; Marcy, Geoffrey W.; Sasselov, Dimitar D.; Seager, Sara;
   Still, Martin; Tenenbaum, Peter; Uddin, Kamal; Winn, Joshua N.
Bibcode: 2011ApJS..197...14D
Altcode: 2011arXiv1107.5750D
  This paper reports the discovery and characterization of the
  transiting hot giant exoplanet Kepler-17b. The planet has an orbital
  period of 1.486 days, and radial velocity measurements from the
  Hobby-Eberly Telescope show a Doppler signal of 419.5<SUP>+13.3</SUP>
  <SUB>-15.6</SUB> m s<SUP>-1</SUP>. From a transit-based estimate
  of the host star's mean density, combined with an estimate of the
  stellar effective temperature T <SUB>eff</SUB> = 5630 ± 100 from
  high-resolution spectra, we infer a stellar host mass of 1.06 ± 0.07 M
  <SUB>⊙</SUB> and a stellar radius of 1.02 ± 0.03 R <SUB>⊙</SUB>. We
  estimate the planet mass and radius to be M <SUB>P</SUB> = 2.45 ± 0.11
  M <SUB>J</SUB> and R <SUB>P</SUB> = 1.31 ± 0.02 R <SUB>J</SUB>. The
  host star is active, with dark spots that are frequently occulted by
  the planet. The continuous monitoring of the star reveals a stellar
  rotation period of 11.89 days, eight times the planet's orbital period;
  this period ratio produces stroboscopic effects on the occulted
  starspots. The temporal pattern of these spot-crossing events shows
  that the planet's orbit is prograde and the star's obliquity is smaller
  than 15°. We detected planetary occultations of Kepler-17b with both
  the Kepler and Spitzer Space Telescopes. We use these observations to
  constrain the eccentricity, e, and find that it is consistent with
  a circular orbit (e &lt; 0.011). The brightness temperatures of the
  planet's infrared bandpasses are T_{3.6\, {\mu m}} = 1880 ± 100 K and
  T_{4.5\, {\mu m}} = 1770 ± 150 K. We measure the optical geometric
  albedo A<SUB>g</SUB> in the Kepler bandpass and find A<SUB>g</SUB>
  = 0.10 ± 0.02. The observations are best described by atmospheric
  models for which most of the incident energy is re-radiated away from
  the day side.

Title: Discovery and Atmospheric Characterization of Giant Planet
Kepler-12b: An Inflated Radius Outlier
Authors: Fortney, Jonathan J.; Demory, Brice-Olivier; Désert,
   Jean-Michel; Rowe, Jason; Marcy, Geoffrey W.; Isaacson, Howard;
   Buchhave, Lars A.; Ciardi, David; Gautier, Thomas N.; Batalha, Natalie
   M.; Caldwell, Douglas A.; Bryson, Stephen T.; Nutzman, Philip; Jenkins,
   Jon M.; Howard, Andrew; Charbonneau, David; Knutson, Heather A.;
   Howell, Steve B.; Everett, Mark; Fressin, François; Deming, Drake;
   Borucki, William J.; Brown, Timothy M.; Ford, Eric B.; Gilliland,
   Ronald L.; Latham, David W.; Miller, Neil; Seager, Sara; Fischer, Debra
   A.; Koch, David; Lissauer, Jack J.; Haas, Michael R.; Still, Martin;
   Lucas, Philip; Gillon, Michael; Christiansen, Jessie L.; Geary, John C.
Bibcode: 2011ApJS..197....9F
Altcode: 2011arXiv1109.1611F
  We report the discovery of planet Kepler-12b (KOI-20), which at 1.695 ±
  0.030 R <SUB>J</SUB> is among the handful of planets with super-inflated
  radii above 1.65 R <SUB>J</SUB>. Orbiting its slightly evolved G0 host
  with a 4.438 day period, this 0.431 ± 0.041 M <SUB>J</SUB> planet
  is the least irradiated within this largest-planet-radius group,
  which has important implications for planetary physics. The planet's
  inflated radius and low mass lead to a very low density of 0.111 ±
  0.010 g cm<SUP>-3</SUP>. We detect the occultation of the planet at a
  significance of 3.7σ in the Kepler bandpass. This yields a geometric
  albedo of 0.14 ± 0.04; the planetary flux is due to a combination of
  scattered light and emitted thermal flux. We use multiple observations
  with Warm Spitzer to detect the occultation at 7σ and 4σ in the 3.6
  and 4.5 μm bandpasses, respectively. The occultation photometry timing
  is consistent with a circular orbit at e &lt; 0.01 (1σ) and e &lt;
  0.09 (3σ). The occultation detections across the three bands favor an
  atmospheric model with no dayside temperature inversion. The Kepler
  occultation detection provides significant leverage, but conclusions
  regarding temperature structure are preliminary, given our ignorance of
  opacity sources at optical wavelengths in hot Jupiter atmospheres. If
  Kepler-12b and HD 209458b, which intercept similar incident stellar
  fluxes, have the same heavy-element masses, the interior energy
  source needed to explain the large radius of Kepler-12b is three times
  larger than that of HD 209458b. This may suggest that more than one
  radius-inflation mechanism is at work for Kepler-12b or that it is
  less heavy-element rich than other transiting planets.

Title: Kepler-18b, c, and d: A System of Three Planets Confirmed
    by Transit Timing Variations, Light Curve Validation, Warm-Spitzer
    Photometry, and Radial Velocity Measurements
Authors: Cochran, William D.; Fabrycky, Daniel C.; Torres, Guillermo;
   Fressin, François; Désert, Jean-Michel; Ragozzine, Darin; Sasselov,
   Dimitar; Fortney, Jonathan J.; Rowe, Jason F.; Brugamyer, Erik J.;
   Bryson, Stephen T.; Carter, Joshua A.; Ciardi, David R.; Howell,
   Steve B.; Steffen, Jason H.; Borucki, William. J.; Koch, David G.;
   Winn, Joshua N.; Welsh, William F.; Uddin, Kamal; Tenenbaum, Peter;
   Still, M.; Seager, Sara; Quinn, Samuel N.; Mullally, F.; Miller, Neil;
   Marcy, Geoffrey W.; MacQueen, Phillip J.; Lucas, Phillip; Lissauer,
   Jack J.; Latham, David W.; Knutson, Heather; Kinemuchi, K.; Johnson,
   John A.; Jenkins, Jon M.; Isaacson, Howard; Howard, Andrew; Horch,
   Elliott; Holman, Matthew J.; Henze, Christopher E.; Haas, Michael R.;
   Gilliland, Ronald L.; Gautier, Thomas N., III; Ford, Eric B.; Fischer,
   Debra A.; Everett, Mark; Endl, Michael; Demory, Brice-Oliver; Deming,
   Drake; Charbonneau, David; Caldwell, Douglas; Buchhave, Lars; Brown,
   Timothy M.; Batalha, Natalie
Bibcode: 2011ApJS..197....7C
Altcode: 2011arXiv1110.0820C
  We report the detection of three transiting planets around a Sun-like
  star, which we designate Kepler-18. The transit signals were detected in
  photometric data from the Kepler satellite, and were confirmed to arise
  from planets using a combination of large transit-timing variations
  (TTVs), radial velocity variations, Warm-Spitzer observations, and
  statistical analysis of false-positive probabilities. The Kepler-18 star
  has a mass of 0.97 M <SUB>sun</SUB>, a radius of 1.1 R <SUB>sun</SUB>,
  an effective temperature of 5345 K, and an iron abundance of [Fe/H] =
  +0.19. The planets have orbital periods of approximately 3.5, 7.6, and
  14.9 days. The innermost planet "b" is a "super-Earth" with a mass of
  6.9 ± 3.4 M <SUB>⊕</SUB>, a radius of 2.00 ± 0.10 R <SUB>⊕</SUB>,
  and a mean density of 4.9 ± 2.4 g cm<SUP>3</SUP>. The two outer planets
  "c" and "d" are both low-density Neptune-mass planets. Kepler-18c has
  a mass of 17.3 ± 1.9 M <SUB>⊕</SUB>, a radius of 5.49 ± 0.26 R
  <SUB>⊕</SUB>, and a mean density of 0.59 ± 0.07 g cm<SUP>3</SUP>,
  while Kepler-18d has a mass of 16.4 ± 1.4 M <SUB>⊕</SUB>, a radius
  of 6.98 ± 0.33 R <SUB>⊕</SUB> and a mean density of 0.27 ± 0.03 g
  cm<SUP>3</SUP>. Kepler-18c and Kepler-18d have orbital periods near
  a 2:1 mean-motion resonance, leading to large and readily detected
  TTVs. <P />Based in part on observations obtained at the W. M. Keck
  Observatory, which is operated by the University of California and
  the California Institute of Technology.

Title: TrES-5: A Massive Jupiter-sized Planet Transiting a Cool
    G Dwarf
Authors: Mandushev, Georgi; Quinn, Samuel N.; Buchhave, Lars A.;
   Dunham, Edward W.; Rabus, Markus; Oetiker, Brian; Latham, David W.;
   Charbonneau, David; Brown, Timothy M.; Belmonte, Juan A.; O'Donovan,
   Francis T.
Bibcode: 2011ApJ...741..114M
Altcode: 2011arXiv1108.3572M
  We report the discovery of TrES-5, a massive hot Jupiter that transits
  the star GSC 03949-00967 every 1.48 days. From spectroscopy of the
  star we estimate a stellar effective temperature of T <SUB>eff</SUB>
  = 5171 ± 36 K, and from high-precision B, R, and I photometry of
  the transit we constrain the ratio of the semimajor axis a and the
  stellar radius R <SUB>sstarf</SUB> to be a/R <SUB>sstarf</SUB> =
  6.07 ± 0.14. We compare these values to model stellar isochrones
  to obtain a stellar mass of M <SUB>sstarf</SUB> = 0.893 ± 0.024 M
  <SUB>⊙</SUB>. Based on this estimate and the photometric time series,
  we constrain the stellar radius to be R <SUB>sstarf</SUB> = 0.866 ±
  0.013 R <SUB>⊙</SUB> and the planet radius to be R <SUB>p</SUB>
  = 1.209 ± 0.021 R <SUB>J</SUB>. We model our radial-velocity data
  assuming a circular orbit and find a planetary mass of 1.778 ± 0.063 M
  <SUB>J</SUB>. Our radial-velocity observations rule out line-bisector
  variations that would indicate a specious detection resulting from
  a blend of an eclipsing binary system. TrES-5 orbits one of the
  faintest stars with transiting planets found to date from the ground
  and demonstrates that precise photometry and followup spectroscopy
  are possible, albeit challenging, even for such faint stars.

Title: KOI-54: The Kepler Discovery of Tidally Excited Pulsations
    and Brightenings in a Highly Eccentric Binary
Authors: Welsh, William F.; Orosz, Jerome A.; Aerts, Conny; Brown,
   Timothy M.; Brugamyer, Erik; Cochran, William D.; Gilliland, Ronald L.;
   Guzik, Joyce Ann; Kurtz, D. W.; Latham, David W.; Marcy, Geoffrey W.;
   Quinn, Samuel N.; Zima, Wolfgang; Allen, Christopher; Batalha, Natalie
   M.; Bryson, Steve; Buchhave, Lars A.; Caldwell, Douglas A.; Gautier,
   Thomas N., III; Howell, Steve B.; Kinemuchi, K.; Ibrahim, Khadeejah
   A.; Isaacson, Howard; Jenkins, Jon M.; Prsa, Andrej; Still, Martin;
   Street, Rachel; Wohler, Bill; Koch, David G.; Borucki, William J.
Bibcode: 2011ApJS..197....4W
Altcode: 2011arXiv1102.1730W
  Kepler observations of the star HD 187091 (KIC 8112039, hereafter
  KOI-54) revealed a remarkable light curve exhibiting sharp
  periodic brightening events every 41.8 days with a superimposed
  set of oscillations forming a beating pattern in phase with the
  brightenings. Spectroscopic observations revealed that this is a binary
  star with a highly eccentric orbit, e = 0.83. We are able to match the
  Kepler light curve and radial velocities with a nearly face-on (i =
  5fdg5) binary star model in which the brightening events are caused by
  tidal distortion and irradiation of nearly identical A stars during
  their close periastron passage. The two dominant oscillations in the
  light curve, responsible for the beating pattern, have frequencies
  that are the 91st and 90th harmonic of the orbital frequency. The power
  spectrum of the light curve, after removing the binary star brightening
  component, reveals a large number of pulsations, 30 of which have
  a signal-to-noise ratio gsim7. Nearly all of these pulsations have
  frequencies that are either integer multiples of the orbital frequency
  or are tidally split multiples of the orbital frequency. This pattern
  of frequencies unambiguously establishes the pulsations as resonances
  between the dynamic tides at periastron and the free oscillation
  modes of one or both of the stars. KOI-54 is only the fourth star to
  show such a phenomenon and is by far the richest in terms of excited
  modes. <P />Based in part on observations obtained at the W. M. Keck
  Observatory, which is operated by the University of California and
  the California Institute of Technology.

Title: VizieR Online Data Catalog: Kepler planetary
    candidates. I. (Borucki+, 2011)
Authors: Borucki, W. J.; Koch, D. G.; Basri, G.; Batalha, N.; Boss,
   A.; Brown, T. M.; Caldwell, D.; Christensen-Dalsgaard, J.; Cochran,
   W. D.; DeVore, E.; Dunham, E. W.; Dupree, A. K.; Gautier, T. N.,
   III; Geary, J. C.; Gilliland, R.; Gould, A.; Howell, S. B.; Jenkins,
   J. M.; Kjeldsen, H.; Latham, D. W.; Lissauer, J. J.; Marcy, G. W.;
   Monet, D. G.; Sasselov, D.; Tarter, J.; Charbonneau, D.; Doyle, L.;
   Ford, E. B.; Fortney, J.; Holman, M. J.; Seager, S.; Steffen, J. H.;
   Welsh, W. F.; Allen, C.; Bryson, S. T.; Buchhave, L.; Chandrasekaran,
   H.; Christiansen, J. L.; Ciardi, D.; Clarke, B. D.; Dotson, J. L.;
   Endl, M.; Fischer, D.; Fressin, F.; Haas, M.; Horch, E.; Howard,
   A.; Isaacson, H.; Kolodziejczak, J.; Li, J.; MacQueen, P.; Meibom,
   S.; Prsa, A.; Quintana, E. V.; Rowe, J.; Sherry, W.; Tenenbaum, P.;
   Torres, G.; Twicken, J. D.; van Cleve, J.; Walkowicz, L.; Wu, H.
Bibcode: 2011yCat..17280117B
Altcode:
  In the spring of 2009, the Kepler Mission commenced high-precision
  photometry on nearly 156000 stars to determine the frequency and
  characteristics of small exoplanets, conduct a guest observer program,
  and obtain asteroseismic data on a wide variety of stars. On 2010
  June 15, the Kepler Mission released most of the data from the first
  quarter of observations. At the time of this data release, 705 stars
  from this first data set have exoplanet candidates with sizes from as
  small as that of Earth to larger than that of Jupiter. Here we give
  the identity and characteristics of 305 released stars with planetary
  candidates. Data for the remaining 400 stars with planetary candidates
  will be released in 2011 February. More than half the candidates on
  the released list have radii less than half that of Jupiter. Five
  candidates are present in and near the habitable zone; two near
  super-Earth size, and three bracketing the size of Jupiter. The
  released stars also include five possible multi-planet systems. One
  of these has two Neptune-size (2.3 and 2.5 Earth radius) candidates
  with near-resonant periods. <P />(1 data file).

Title: The LCOGT Network
Authors: Shporer, Avi; Brown, Tim; Lister, Tim; Street, Rachel;
   Tsapras, Yiannis; Bianco, Federica; Fulton, Benjamin; Howell, Andy
Bibcode: 2011IAUS..276..553S
Altcode: 2010arXiv1011.6394S
  Motivated by the increasing need for observational resources for the
  study of time varying astronomy, the Las Cumbres Observatory Global
  Telescope (LCOGT) is a private foundation, whose goal is to build
  a global network of robotic telescopes for scientific research and
  education. Once completed, the network will become a unique tool,
  capable of continuous monitoring from both the Northern and Southern
  Hemispheres. The network currently includes 2 × 2.0 m telescopes,
  already making an impact in the field of exoplanet research. In the next
  few years they will be joined by at least 12 × 1.0 m and 20 × 0.4 m
  telescopes. The increasing amount of LCOGT observational resources in
  the coming years will be of great service to the astronomical community
  in general, and the exoplanet community in particular.

Title: VizieR Online Data Catalog: Kepler planetary
    candidates. II. (Borucki+, 2011)
Authors: Borucki, W. J.; Koch, D. G.; Basri, G.; Batalha, N.; Brown,
   T. M.; Bryson, S. T.; Caldwell, D.; Christensen-Dalsgaard, J.;
   Cochran, W. D.; DeVore, E.; Dunham, E. W.; Gautier, T. N.; Geary,
   J. C.; Gilliland, R.; Gould, A.; Howell, S. B.; Jenkins, J. M.;
   Latham, D. W.; Lissauer, J. J.; Marcy, G. W.; Rowe, J.; Sasselov,
   D.; Boss, A.; Charbonneau, D.; Ciardi, D.; Doyle, L.; Dupree, A. K.;
   Ford, E. B.; Fortney, J.; Holman, M. J.; Seager, S.; Steffen, J. H.;
   Tarter, J.; Welsh, W. F.; Allen, C.; Buchhave, L. A.; Christiansen,
   J. L.; Clarke, B. D.; Das, S.; Desert, J. -M.; Endl, M.; Fabrycky,
   D.; Fressin, F.; Haas, M.; Horch, E.; Howard, A.; Isaacson, H.;
   Kjeldsen, H.; Kolodziejczak, J.; Kulesa, C.; Li, J.; Lucas, P. W.;
   Machalek, P.; McCarthy, D.; MacQueen, P.; Meibom, S.; Miquel, T.;
   Prsa, A.; Quinn, S. N.; Quintana, E. V.; Ragozzine, D.; Sherry, W.;
   Shporer, A.; Tenenbaum, P.; Torres, G.; Twicken, J. D.; van Cleve,
   J.; Walkowicz, L.; Witteborn, F. C.; Still, M.
Bibcode: 2011yCat..17360019B
Altcode:
  The results discussed in this paper are based on three data segments:
  the first segment (labeled Q0) started on JD 2454953.53 and ended on
  2454963.25 and was taken during commissioning operations, the second
  data segment (labeled Q1) taken at the beginning of science operations
  that started on JD 2454964.50 and finished on JD 2454997.99, and a
  third segment (labeled Q2) starting on JD 2455002.51 and finishing on
  JD 2455091.48. The durations of the segments are 9.7, 33.5, and 89.0
  days, respectively. The observations span a total period of 137.95
  days including the gaps. A total of 156097 long cadence (LC) targets
  in Q1, and 166247 LC and 1492 short cadence (SC) targets in Q2 were
  observed. The results reported here are for the LC observations of
  153196 stars observed during Q2. The selected stars are primarily
  main-sequence dwarfs chosen from the Kepler Input Catalog (KIC,
  Cat. V/133). <P />(4 data files).

Title: Kepler Input Catalog: Photometric Calibration and Stellar
    Classification
Authors: Brown, Timothy M.; Latham, David W.; Everett, Mark E.;
   Esquerdo, Gilbert A.
Bibcode: 2011AJ....142..112B
Altcode: 2011arXiv1102.0342B
  We describe the photometric calibration and stellar classification
  methods used by the Stellar Classification Project to produce the Kepler
  Input Catalog (KIC). The KIC is a catalog containing photometric and
  physical data for sources in the Kepler mission field of view; it is
  used by the mission to select optimal targets. Four of the visible-light
  (g, r, i, z) magnitudes used in the KIC are tied to Sloan Digital Sky
  Survey magnitudes; the fifth (D51) is an AB magnitude calibrated to be
  consistent with Castelli &amp; Kurucz (CK) model atmosphere fluxes. We
  derived atmospheric extinction corrections from hourly observations of
  secondary standard fields within the Kepler field of view. For these
  filters and extinction estimates, repeatability of absolute photometry
  for stars brighter than magnitude 15 is typically 2%. We estimated
  stellar parameters {T <SUB>eff</SUB>, log (g), log (Z), E <SUB> B -
  V </SUB>} using Bayesian posterior probability maximization to match
  observed colors to CK stellar atmosphere models. We applied Bayesian
  priors describing the distribution of solar-neighborhood stars in the
  color-magnitude diagram, in log (Z), and in height above the galactic
  plane. Several comparisons with samples of stars classified by other
  means indicate that for 4500 K &lt;=T <SUB>eff</SUB> &lt;= 6500 K, our
  classifications are reliable within about ±200 K and 0.4 dex in log (g)
  for dwarfs, with somewhat larger log (g) uncertainties for giants. It
  is difficult to assess the reliability of our log (Z) estimates, but
  there is reason to suspect that it is poor, particularly at extreme T
  <SUB>eff</SUB>. Comparisons between the CK models and observed colors
  are generally satisfactory with some exceptions, notably for stars
  cooler than 4500 K. Of great importance for the Kepler mission, for
  T <SUB>eff</SUB> &lt;= 5400 K, comparison with asteroseismic results
  shows that the distinction between main-sequence stars and giants is
  reliable with about 98% confidence. Larger errors in log (g) occur
  for warmer stars, for which our filter set provides inadequate gravity
  diagnostics. The KIC is available through the MAST data archive.

Title: Verification of the Kepler Input Catalog from Asteroseismology
    of Solar-type Stars
Authors: Verner, G. A.; Chaplin, W. J.; Basu, S.; Brown, T. M.;
   Hekker, S.; Huber, D.; Karoff, C.; Mathur, S.; Metcalfe, T. S.;
   Mosser, B.; Quirion, P. -O.; Appourchaux, T.; Bedding, T. R.; Bruntt,
   H.; Campante, T. L.; Elsworth, Y.; García, R. A.; Handberg, R.;
   Régulo, C.; Roxburgh, I. W.; Stello, D.; Christensen-Dalsgaard, J.;
   Gilliland, R. L.; Kawaler, S. D.; Kjeldsen, H.; Allen, C.; Clarke,
   B. D.; Girouard, F. R.
Bibcode: 2011ApJ...738L..28V
Altcode: 2011arXiv1109.0869V
  We calculate precise stellar radii and surface gravities from the
  asteroseismic analysis of over 500 solar-type pulsating stars observed
  by the Kepler space telescope. These physical stellar properties
  are compared with those given in the Kepler Input Catalog (KIC),
  determined from ground-based multi-color photometry. For the stars
  in our sample, we find general agreement but we detect an average
  overestimation bias of 0.23 dex in the KIC determination of log (g)
  for stars with log (g)<SUB>KIC</SUB> &gt; 4.0 dex, and a resultant
  underestimation bias of up to 50% in the KIC radii estimates for stars
  with R <SUB>KIC</SUB> &lt; 2 R <SUB>sun</SUB>. Part of the difference
  may arise from selection bias in the asteroseismic sample; nevertheless,
  this result implies there may be fewer stars characterized in the KIC
  with R ~ 1 R <SUB>sun</SUB> than is suggested by the physical properties
  in the KIC. Furthermore, if the radius estimates are taken from the
  KIC for these affected stars and then used to calculate the size of
  transiting planets, a similar underestimation bias may be applied to
  the planetary radii.

Title: The GHOSTS Survey. I. Hubble Space Telescope Advanced Camera
    for Surveys Data
Authors: Radburn-Smith, D. J.; de Jong, R. S.; Seth, A. C.; Bailin,
   J.; Bell, E. F.; Brown, T. M.; Bullock, J. S.; Courteau, S.; Dalcanton,
   J. J.; Ferguson, H. C.; Goudfrooij, P.; Holfeltz, S.; Holwerda, B. W.;
   Purcell, C.; Sick, J.; Streich, D.; Vlajic, M.; Zucker, D. B.
Bibcode: 2011ApJS..195...18R
Altcode:
  We present an overview of the GHOSTS survey, the largest study to
  date of the resolved stellar populations in the outskirts of disk
  galaxies. The sample consists of 14 disk galaxies within 17 Mpc,
  whose outer disks and halos are imaged with the Hubble Space Telescope
  Advanced Camera for Surveys (ACS). In the first paper of this series,
  we describe the sample, explore the benefits of using resolved stellar
  populations, and discuss our ACS F606W and F814W photometry. We use
  artificial star tests to assess completeness and use overlapping regions
  to estimate photometric uncertainties. The median depth of the survey
  at 50% completeness is 2.7 mag below the tip of the red giant branch
  (TRGB). We comprehensively explore and parameterize contamination from
  unresolved background galaxies and foreground stars using archival
  fields of high-redshift ACS observations. Left uncorrected, these
  would account for 10<SUP>0.65 × F814W - 19.0</SUP> detections per
  mag per arcsec<SUP>2</SUP>. We therefore identify several selection
  criteria that typically remove 95% of the contaminants. Even with these
  culls, background galaxies are a significant limitation to the surface
  brightness detection limit which, for this survey, is typically V ~ 30
  mag arcsec<SUP>-2</SUP>. The resulting photometric catalogs are publicly
  available and contain some 3.1 million stars across 76 ACS fields,
  predominantly of low extinction. The uniform magnitudes of TRGB stars
  in these fields enable galaxy distance estimates with 2%-7% accuracy.

Title: The pulsations of PG 1351+489
Authors: Redaelli, M.; Kepler, S. O.; Costa, J. E. S.; Winget, D. E.;
   Handler, G.; Castanheira, B. G.; Kanaan, A.; Fraga, L.; Henrique,
   P.; Giovannini, O.; Provencal, J. L.; Shipman, H. L.; Dalessio, J.;
   Thompson, S. E.; Mullally, F.; Brewer, M. M.; Childers, D.; Oksala,
   M. E.; Rosen, R.; Wood, M. A.; Reed, M. D.; Walter, B.; Strickland,
   W.; Chandler, D.; Watson, T. K.; Nather, R. E.; Montgomery, M. H.;
   Bischoff-Kim, A.; Hansen, C. J.; Nitta, A.; Kleinman, S. J.; Claver,
   C. F.; Brown, T. M.; Sullivan, D. J.; Kim, S. -L.; Chen, W. -P.;
   Yang, M.; Shih, C. -Y.; Zhang, X.; Jiang, X.; Fu, J. N.; Seetha,
   S.; Ashoka, B. N.; Marar, T. M. K.; Baliyan, K. S.; Vats, H. O.;
   Chernyshev, A. V.; Ibbetson, P.; Leibowitz, E.; Hemar, S.; Sergeev,
   A. V.; Andreev, M. V.; Janulis, R.; Meištas, E. G.; Moskalik, P.;
   Pajdosz, G.; Baran, A.; Winiarski, M.; Zola, S.; Ogloza, W.; Siwak, M.;
   Bognár, Zs.; Solheim, J. -E.; Sefako, R.; Buckley, D.; O'Donoghue,
   D.; Nagel, T.; Silvotti, R.; Bruni, I.; Fremy, J. R.; Vauclair, G.;
   Chevreton, M.; Dolez, N.; Pfeiffer, B.; Barstow, M. A.; Creevey,
   O. L.; Kawaler, S. D.; Clemens, J. C.
Bibcode: 2011MNRAS.415.1220R
Altcode: 2011MNRAS.tmp..999R
  PG 1351+489 is one of the 20 DBVs - pulsating helium-atmosphere white
  dwarf stars - known and has the simplest power spectrum for this class
  of star, making it a good candidate to study cooling rates. We report
  accurate period determinations for the main peak at 489.334 48 s and
  two other normal modes using data from the Whole Earth Telescope
  (WET) observations of 1995 and 2009. In 2009, we detected a new
  pulsation mode and the main pulsation mode exhibited substantial
  change in its amplitude compared to all previous observations. We were
  able to estimate the star's rotation period, of 8.9 h, and discuss a
  possible determination of the rate of period change of (2.0 ± 0.9) ×
  10<SUP>-13</SUP> s s <SUP>-1</SUP>, the first such estimate for a DBV.

Title: Characteristics of Planetary Candidates Observed by
    Kepler. II. Analysis of the First Four Months of Data
Authors: Borucki, William J.; Koch, David G.; Basri, Gibor; Batalha,
   Natalie; Brown, Timothy M.; Bryson, Stephen T.; Caldwell, Douglas;
   Christensen-Dalsgaard, Jørgen; Cochran, William D.; DeVore, Edna;
   Dunham, Edward W.; Gautier, Thomas N., III; Geary, John C.; Gilliland,
   Ronald; Gould, Alan; Howell, Steve B.; Jenkins, Jon M.; Latham, David
   W.; Lissauer, Jack J.; Marcy, Geoffrey W.; Rowe, Jason; Sasselov,
   Dimitar; Boss, Alan; Charbonneau, David; Ciardi, David; Doyle,
   Laurance; Dupree, Andrea K.; Ford, Eric B.; Fortney, Jonathan; Holman,
   Matthew J.; Seager, Sara; Steffen, Jason H.; Tarter, Jill; Welsh,
   William F.; Allen, Christopher; Buchhave, Lars A.; Christiansen,
   Jessie L.; Clarke, Bruce D.; Das, Santanu; Désert, Jean-Michel;
   Endl, Michael; Fabrycky, Daniel; Fressin, Francois; Haas, Michael;
   Horch, Elliott; Howard, Andrew; Isaacson, Howard; Kjeldsen, Hans;
   Kolodziejczak, Jeffery; Kulesa, Craig; Li, Jie; Lucas, Philip W.;
   Machalek, Pavel; McCarthy, Donald; MacQueen, Phillip; Meibom, Søren;
   Miquel, Thibaut; Prsa, Andrej; Quinn, Samuel N.; Quintana, Elisa V.;
   Ragozzine, Darin; Sherry, William; Shporer, Avi; Tenenbaum, Peter;
   Torres, Guillermo; Twicken, Joseph D.; Van Cleve, Jeffrey; Walkowicz,
   Lucianne; Witteborn, Fred C.; Still, Martin
Bibcode: 2011ApJ...736...19B
Altcode: 2011arXiv1102.0541B
  On 2011 February 1 the Kepler mission released data for 156,453
  stars observed from the beginning of the science observations on
  2009 May 2 through September 16. There are 1235 planetary candidates
  with transit-like signatures detected in this period. These are
  associated with 997 host stars. Distributions of the characteristics
  of the planetary candidates are separated into five class sizes:
  68 candidates of approximately Earth-size (R <SUB>p</SUB> &lt;
  1.25 R <SUB>⊕</SUB>), 288 super-Earth-size (1.25 R <SUB>⊕</SUB>
  &lt;= R <SUB>p</SUB> &lt; 2 R <SUB>⊕</SUB>), 662 Neptune-size
  (2 R <SUB>⊕</SUB> &lt;= R <SUB>p</SUB> &lt; 6 R <SUB>⊕</SUB>),
  165 Jupiter-size (6 R <SUB>⊕</SUB> &lt;= R <SUB>p</SUB> &lt;
  15 R <SUB>⊕</SUB>), and 19 up to twice the size of Jupiter (15 R
  <SUB>⊕</SUB> &lt;= R <SUB>p</SUB> &lt; 22 R <SUB>⊕</SUB>). In the
  temperature range appropriate for the habitable zone, 54 candidates
  are found with sizes ranging from Earth-size to larger than that
  of Jupiter. Six are less than twice the size of the Earth. Over 74%
  of the planetary candidates are smaller than Neptune. The observed
  number versus size distribution of planetary candidates increases to a
  peak at two to three times the Earth-size and then declines inversely
  proportional to the area of the candidate. Our current best estimates
  of the intrinsic frequencies of planetary candidates, after correcting
  for geometric and sensitivity biases, are 5% for Earth-size candidates,
  8% for super-Earth-size candidates, 18% for Neptune-size candidates,
  2% for Jupiter-size candidates, and 0.1% for very large candidates; a
  total of 0.34 candidates per star. Multi-candidate, transiting systems
  are frequent; 17% of the host stars have multi-candidate systems,
  and 34% of all the candidates are part of multi-candidate systems.

Title: A First Comparison of Kepler Planet Candidates in Single and
    Multiple Systems
Authors: Latham, David W.; Rowe, Jason F.; Quinn, Samuel N.; Batalha,
   Natalie M.; Borucki, William J.; Brown, Timothy M.; Bryson, Stephen
   T.; Buchhave, Lars A.; Caldwell, Douglas A.; Carter, Joshua A.;
   Christiansen, Jessie L.; Ciardi, David R.; Cochran, William D.;
   Dunham, Edward W.; Fabrycky, Daniel C.; Ford, Eric B.; Gautier,
   Thomas N., III; Gilliland, Ronald L.; Holman, Matthew J.; Howell,
   Steve B.; Ibrahim, Khadeejah A.; Isaacson, Howard; Jenkins, Jon M.;
   Koch, David G.; Lissauer, Jack J.; Marcy, Geoffrey W.; Quintana,
   Elisa V.; Ragozzine, Darin; Sasselov, Dimitar; Shporer, Avi; Steffen,
   Jason H.; Welsh, William F.; Wohler, Bill
Bibcode: 2011ApJ...732L..24L
Altcode: 2011arXiv1103.3896L
  In this Letter, we present an overview of the rich population of systems
  with multiple candidate transiting planets found in the first four
  months of Kepler data. The census of multiples includes 115 targets
  that show two candidate planets, 45 with three, eight with four,
  and one each with five and six, for a total of 170 systems with 408
  candidates. When compared to the 827 systems with only one candidate,
  the multiples account for 17% of the total number of systems, and
  one-third of all the planet candidates. We compare the characteristics
  of candidates found in multiples with those found in singles. False
  positives due to eclipsing binaries are much less common for the
  multiples, as expected. Singles and multiples are both dominated by
  planets smaller than Neptune; 69<SUP>+2</SUP> <SUB> - 3</SUB>% for
  singles and 86<SUP>+2</SUP> <SUB> - 5</SUB>% for multiples. This result,
  that systems with multiple transiting planets are less likely to include
  a transiting giant planet, suggests that close-in giant planets tend
  to disrupt the orbital inclinations of small planets in flat systems,
  or maybe even prevent the formation of such systems in the first place.

Title: Constraining the Properties of Delta Scuti Stars Using
    Spectroscopic Eclipsing Binary Systems
Authors: Creevey, O. L.; Metcalfe, T. S.; Brown, T. M.; Jiménez-Reyes,
   S.; Belmonte, J. A.
Bibcode: 2011ApJ...733...38C
Altcode: 2011arXiv1105.1045C
  Many stars exhibit stellar pulsations, favoring them for asteroseismic
  analyses. Interpreting the oscillations requires some knowledge
  of the oscillation mode geometry (spherical degree, radial, and
  azimuthal orders). The δ Scuti stars (1.5-2.5 M <SUB>sun</SUB>)
  often show just one or few pulsation frequencies. Although this may
  promise a successful seismological analysis, we may not know enough
  about either the mode or the star to use the oscillation frequency to
  improve the determination of the stellar model or to probe the star's
  structure. For the observed frequencies to be used successfully as
  seismic probes of these objects, we need to concentrate on stars for
  which we can reduce the number of free parameters in the problem,
  such as binary systems or open clusters. We investigate how much
  our understanding of a δ Scuti star is improved when it is in a
  detached eclipsing binary system instead of being a single field
  star. We use singular value decomposition to explore the precision
  we expect in stellar parameters (mass, age, and chemical composition)
  for both cases. We examine how the parameter uncertainties propagate
  to the luminosity-effective temperature diagram and determine when the
  effort of obtaining a new measurement is justified. We show that for
  the single star, a correct identification of the oscillation mode is
  necessary to produce strong constraints on the stellar model properties,
  while for the binary system the observations without the pulsation mode
  provide the same or better constraints on the stellar parameters. In
  the latter case, the strong constraints provided by the binary system
  not only allow us to detect an incorrectly identified oscillation mode,
  but we can also constrain the oscillation mode geometry by comparing
  the distribution of possible solutions with and without including the
  oscillation frequency as a constraint.

Title: HST/ACS Observations of RR Lyrae Stars in Six Ultra-deep
    Fields of M31
Authors: Jeffery, E. J.; Smith, E.; Brown, T. M.; Sweigart, A. V.;
   Kalirai, J. S.; Ferguson, H. C.; Guhathakurta, P.; Renzini, A.; Rich,
   R. M.
Bibcode: 2011AJ....141..171J
Altcode: 2011arXiv1103.1400J
  We present HST/ACS observations of RR Lyrae variable stars in six
  ultra-deep fields of the Andromeda galaxy (M31), including parts
  of the halo, disk, and giant stellar stream. Past work on the RR
  Lyrae stars in M31 has focused on various aspects of the stellar
  populations that make up the galaxy's halo, including their distances
  and metallicities. This study builds upon this previous work by
  increasing the spatial coverage (something that has been lacking
  in previous studies) and by searching for these variable stars in
  constituents of the galaxy not yet explored. Besides the 55 RR Lyrae
  stars we found in our initial field located 11 kpc from the galactic
  nucleus, we find additional RR Lyrae stars in four of the remaining
  five ultra-deep fields as follows: 21 in the disk, 24 in the giant
  stellar stream, three in the halo field 21 kpc from the galactic
  nucleus, and five in one of the halo fields at 35 kpc. No RR Lyrae
  stars were found in the second halo field at 35 kpc. The RR Lyrae
  populations of these fields appear to be mostly of Oosterhoff I type,
  although the 11 kpc field appears to be intermediate or mixed. We will
  discuss the properties of these stars including period and reddening
  distributions. We calculate metallicities and distances for the stars in
  each of these fields using different methods and compare the results,
  to an extent that has not yet been done. We compare these methods not
  just on RR Lyrae stars in our M31 fields, but also on a data set of
  Milky Way field RR Lyrae stars. <P />Based on observations made with
  the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope
  Science Institute, which is operated by the Association of Universities
  for Research in Astronomy, Incorporated, under NASA contract NAS5-26555.

Title: The Impact of the Convective Blueshift Effect on Spectroscopic
    Planetary Transits
Authors: Shporer, Avi; Brown, Tim
Bibcode: 2011ApJ...733...30S
Altcode: 2011arXiv1103.0775S
  We present here a small anomalous radial velocity (RV) signal expected
  to be present in RV curves measured during planetary transits. This
  signal is induced by the convective blueshift (CB) effect—a net
  blueshift emanating from the stellar surface, resulting from a larger
  contribution of rising hot and bright gas relative to the colder and
  darker sinking gas. Since the CB radial component varies across the
  stellar surface, the light blocked by the planet during a transit
  will have a varying RV component, resulting in a small shift of
  the measured RVs. The CB-induced anomalous RV curve is different
  than, and independent of, the well-known Rossiter-McLaughlin (RM)
  effect, where the latter is used for determining the sky-projected
  angle between the host star rotation axis and the planet's orbital
  angular momentum axis. The observed RV curve is the sum of the CB
  and RM signals, and they are both superposed on the orbital Keplerian
  curve. If not accounted for, the presence of the CB RV signal in the
  spectroscopic transit RV curve may bias the estimate of the spin-orbit
  angle. In addition, future very high precision RVs will allow the use
  of transiting planets to study the CB of their host stars.

Title: The First Detection of Blue Straggler Stars in the Milky
    Way Bulge
Authors: Clarkson, Will; Sahu, K. C.; Anderson, J.; Rich, M.; Smith,
   E.; Brown, T. M.; Bond, H. E.; Livio, M.; Minniti, D.; Renzini, A.;
   Zoccali, M.
Bibcode: 2011AAS...21821705C
Altcode: 2011BAAS..43G21705C
  We report the first detections of Blue Straggler Stars (BSS) in
  the bulge of the Milky Way galaxy. Proper motions from extensive
  space-based observations along a single sight-line allow us to separate
  a sufficiently clean and well-characterized bulge sample that we are
  able to detect a small population of bulge objects in the region of
  the color-magnitude diagram commonly occupied young objects and blue
  strgglers. However, variability measurements of these objects clearly
  establish that a fraction of them are blue stragglers. Out of the 42
  objects found in this region of the CMD, we estimate that at least 18
  are genuine BSS. We normalize the BSS population by our estimate of the
  number of horizontal branch stars in the bulge in order to compare the
  bulge to other stellar systems. The BSS fraction is clearly discrepant
  from that found in stellar clusters. The blue straggler population
  of dwarf spheroidals remains a subject of debate; some authors claim
  an anticorrelation between the normalised blue straggler fraction
  and integrated light. If this trend is real, then the bulge extends
  it by three orders of magnitude in mass. Conversely, we find that the
  genuinely young (&lt; 5Gy) population in the bulge, must be at most 3.3%
  under the most conservative scenario for the BSS population.

Title: Validating the First Habitable-Zone Planet Candidates
    Identified by the NASA Kepler Mission
Authors: Charbonneau, David; Desert, Jean-Michel; Fressin, Francois;
   Ballard, Sarah; Borucki, William; Latham, David; Gilliland, Ronald;
   Seager, Sara; Knutson, Heather; Fortney, Jonathan; Brown, Timothy;
   Ford, Eric; Deming, Drake; Torres, Guillermo
Bibcode: 2011sptz.prop80117C
Altcode:
  At the beginning of Cycle 8, the NASA Kepler Mission will have completed
  two years of science observations, the minimum baseline sufficient
  to identify candidate transiting exoplanets orbiting within the
  habitable-zones of Sun-like stars. The principal task that lies ahead
  is to reject from this sample the false positives (blends of eclipsing
  binaries that precisely mimic the signal of a transiting exoplanet), and
  to confirm the planetary nature of the remaining candidates. For planets
  more massive than Neptune, the direct confirmation of their planetary
  status can be accomplished by radial-velocity measurements. However,
  such planets possess primordial envelopes of hydrogen and helium
  that make them unsuitable to life as we know it. The most exciting
  candidates -- and the ones that Kepler is specifically tasked with
  finding -- are super-Earth and Earth-sized planets orbiting within their
  stellar habitable zones. Kepler has just begun to identify such planet
  candidates, and it will identify many more as its baseline increases
  throughout the coming year. While the Kepler team has developed powerful
  tools to weed out the impostors, Spitzer possesses the unique ability
  to provide the final validation of these candidates as planets, namely
  by measuring the depth of the transit at infrared wavelengths. By
  combining the infrared and optical measurements of the transit depth
  with models of hypothetical stellar blends, we can definitively test
  the stellar-blend hypothesis. We propose to observe the transits of 20
  candidate habitable-zone super-Earths to be identified by the Kepler
  Mission. The results from this Exploration Science Program will be
  twofold: First, we will definitively validate the first potentially
  habitable planets ever identified. Second, we will determine the rate
  of occurrence of impostors. This rate of false positives can then be
  applied to the much larger sample of candidates identified by Kepler,
  to deduce the true rate of planetary companions.

Title: Predicting the Detectability of Oscillations in Solar-type
    Stars Observed by Kepler
Authors: Chaplin, W. J.; Kjeldsen, H.; Bedding, T. R.;
   Christensen-Dalsgaard, J.; Gilliland, R. L.; Kawaler, S. D.;
   Appourchaux, T.; Elsworth, Y.; García, R. A.; Houdek, G.; Karoff, C.;
   Metcalfe, T. S.; Molenda-Żakowicz, J.; Monteiro, M. J. P. F. G.;
   Thompson, M. J.; Verner, G. A.; Batalha, N.; Borucki, W. J.;
   Brown, T. M.; Bryson, S. T.; Christiansen, J. L.; Clarke, B. D.;
   Jenkins, J. M.; Klaus, T. C.; Koch, D.; An, D.; Ballot, J.; Basu,
   S.; Benomar, O.; Bonanno, A.; Broomhall, A. -M.; Campante, T. L.;
   Corsaro, E.; Creevey, O. L.; Esch, L.; Gai, N.; Gaulme, P.; Hale,
   S. J.; Handberg, R.; Hekker, S.; Huber, D.; Mathur, S.; Mosser, B.;
   New, R.; Pinsonneault, M. H.; Pricopi, D.; Quirion, P. -O.; Régulo,
   C.; Roxburgh, I. W.; Salabert, D.; Stello, D.; Suran, M. D.
Bibcode: 2011ApJ...732...54C
Altcode: 2011arXiv1103.0702C
  Asteroseismology of solar-type stars has an important part to play
  in the exoplanet program of the NASA Kepler Mission. Precise and
  accurate inferences on the stellar properties that are made possible
  by the seismic data allow very tight constraints to be placed on the
  exoplanetary systems. Here, we outline how to make an estimate of the
  detectability of solar-like oscillations in any given Kepler target,
  using rough estimates of the temperature and radius, and the Kepler
  apparent magnitude.

Title: LCOGT Imaging Capabilities
Authors: Brown, Timothy M.; Burleson, B.; De Vera, J.; Dubberley,
   M.; Haldeman, B.; Hawkins, E.; Haynes, R.; Hjelstrom, A.; Hygelund,
   J.; Lister, T.; Lobdill, R.; Pickles, A.; Rosing, W.; Tufts, J.
Bibcode: 2011AAS...21813202B
Altcode: 2011BAAS..43G13202B
  Las Cumbres Observatory Global Telescope (LCOGT) is developing a
  world-wide network of optical telescopes dedicated to time-domain
  astronomy. In a few years, the network will consist of more than twenty
  0.4m telescopes, about fifteen 1m telescopes, and two 2m telescopes, all
  of which will initially be equipped for both high-speed and traditional
  CCD imaging. Instruments for high-speed applications are described
  in Bianco et al. (this session). Here we describe LCOGT's instruments
  for relatively wide-field imaging at moderate time cadence. The most
  notable of these is the "Sinistro" camera system being built for the 1m
  network. It consists of corrector optics, filter changer, photometric
  shutter, 16 Mpix CCD camera, and custom CCD controller. Each Sinistro
  component is optimized for precision photometric measurements, and the
  system provides a large critically sampled field to the full CCD, rapid
  access to as many as 21 different filters, minimized shutter overhead,
  flexible high-speed readout, support for multiple independent regions
  of interest, the ability to autoguide independently of camera focus,
  precision CCD temperature control and telemetry, and a dry nitrogen
  filter environment.

Title: Ensemble Asteroseismology of Solar-Type Stars with the NASA
    Kepler Mission
Authors: Chaplin, W. J.; Kjeldsen, H.; Christensen-Dalsgaard, J.;
   Basu, S.; Miglio, A.; Appourchaux, T.; Bedding, T. R.; Elsworth, Y.;
   García, R. A.; Gilliland, R. L.; Girardi, L.; Houdek, G.; Karoff,
   C.; Kawaler, S. D.; Metcalfe, T. S.; Molenda-Żakowicz, J.; Monteiro,
   M. J. P. F. G.; Thompson, M. J.; Verner, G. A.; Ballot, J.; Bonanno,
   A.; Brandão, I. M.; Broomhall, A. -M.; Bruntt, H.; Campante, T. L.;
   Corsaro, E.; Creevey, O. L.; Doğan, G.; Esch, L.; Gai, N.; Gaulme,
   P.; Hale, S. J.; Handberg, R.; Hekker, S.; Huber, D.; Jiménez, A.;
   Mathur, S.; Mazumdar, A.; Mosser, B.; New, R.; Pinsonneault, M. H.;
   Pricopi, D.; Quirion, P. -O.; Régulo, C.; Salabert, D.; Serenelli,
   A. M.; Silva Aguirre, V.; Sousa, S. G.; Stello, D.; Stevens, I. R.;
   Suran, M. D.; Uytterhoeven, K.; White, T. R.; Borucki, W. J.; Brown,
   T. M.; Jenkins, J. M.; Kinemuchi, K.; Van Cleve, J.; Klaus, T. C.
Bibcode: 2011Sci...332..213C
Altcode: 2011arXiv1109.4723C
  In addition to its search for extrasolar planets, the NASA Kepler
  mission provides exquisite data on stellar oscillations. We report the
  detections of oscillations in 500 solar-type stars in the Kepler field
  of view, an ensemble that is large enough to allow statistical studies
  of intrinsic stellar properties (such as mass, radius, and age) and
  to test theories of stellar evolution. We find that the distribution
  of observed masses of these stars shows intriguing differences to
  predictions from models of synthetic stellar populations in the Galaxy.

Title: Kepler Detected Gravity-Mode Period Spacings in a Red
    Giant Star
Authors: Beck, P. G.; Bedding, T. R.; Mosser, B.; Stello, D.; Garcia,
   R. A.; Kallinger, T.; Hekker, S.; Elsworth, Y.; Frandsen, S.; Carrier,
   F.; De Ridder, J.; Aerts, C.; White, T. R.; Huber, D.; Dupret, M. -A.;
   Montalbán, J.; Miglio, A.; Noels, A.; Chaplin, W. J.; Kjeldsen, H.;
   Christensen-Dalsgaard, J.; Gilliland, R. L.; Brown, T. M.; Kawaler,
   S. D.; Mathur, S.; Jenkins, J. M.
Bibcode: 2011Sci...332..205B
Altcode:
  Stellar interiors are inaccessible through direct observations. For
  this reason, helioseismologists made use of the Sun’s acoustic
  oscillation modes to tune models of its structure. The quest to detect
  modes that probe the solar core has been ongoing for decades. We
  report the detection of mixed modes penetrating all the way to the
  core of an evolved star from 320 days of observations with the Kepler
  satellite. The period spacings of these mixed modes are directly
  dependent on the density gradient between the core region and the
  convective envelope.

Title: Gravity modes as a way to distinguish between hydrogen-
    and helium-burning red giant stars
Authors: Bedding, Timothy R.; Mosser, Benoit; Huber, Daniel;
   Montalbán, Josefina; Beck, Paul; Christensen-Dalsgaard, Jørgen;
   Elsworth, Yvonne P.; García, Rafael A.; Miglio, Andrea; Stello,
   Dennis; White, Timothy R.; De Ridder, Joris; Hekker, Saskia; Aerts,
   Conny; Barban, Caroline; Belkacem, Kevin; Broomhall, Anne-Marie;
   Brown, Timothy M.; Buzasi, Derek L.; Carrier, Fabien; Chaplin,
   William J.; di Mauro, Maria Pia; Dupret, Marc-Antoine; Frandsen,
   Søren; Gilliland, Ronald L.; Goupil, Marie-Jo; Jenkins, Jon M.;
   Kallinger, Thomas; Kawaler, Steven; Kjeldsen, Hans; Mathur, Savita;
   Noels, Arlette; Silva Aguirre, Victor; Ventura, Paolo
Bibcode: 2011Natur.471..608B
Altcode: 2011arXiv1103.5805B
  Red giants are evolved stars that have exhausted the supply of hydrogen
  in their cores and instead burn hydrogen in a surrounding shell. Once a
  red giant is sufficiently evolved, the helium in the core also undergoes
  fusion. Outstanding issues in our understanding of red giants include
  uncertainties in the amount of mass lost at the surface before helium
  ignition and the amount of internal mixing from rotation and other
  processes. Progress is hampered by our inability to distinguish between
  red giants burning helium in the core and those still only burning
  hydrogen in a shell. Asteroseismology offers a way forward, being
  a powerful tool for probing the internal structures of stars using
  their natural oscillation frequencies. Here we report observations of
  gravity-mode period spacings in red giants that permit a distinction
  between evolutionary stages to be made. We use high-precision
  photometry obtained by the Kepler spacecraft over more than a year
  to measure oscillations in several hundred red giants. We find many
  stars whose dipole modes show sequences with approximately regular
  period spacings. These stars fall into two clear groups, allowing us
  to distinguish unambiguously between hydrogen-shell-burning stars
  (period spacing mostly ~50seconds) and those that are also burning
  helium (period spacing ~100 to 300 seconds).

Title: Kepler's First Rocky Planet: Kepler-10b
Authors: Batalha, Natalie M.; Borucki, William J.; Bryson, Stephen
   T.; Buchhave, Lars A.; Caldwell, Douglas A.; Christensen-Dalsgaard,
   Jørgen; Ciardi, David; Dunham, Edward W.; Fressin, Francois;
   Gautier, Thomas N., III; Gilliland, Ronald L.; Haas, Michael R.;
   Howell, Steve B.; Jenkins, Jon M.; Kjeldsen, Hans; Koch, David G.;
   Latham, David W.; Lissauer, Jack J.; Marcy, Geoffrey W.; Rowe, Jason
   F.; Sasselov, Dimitar D.; Seager, Sara; Steffen, Jason H.; Torres,
   Guillermo; Basri, Gibor S.; Brown, Timothy M.; Charbonneau, David;
   Christiansen, Jessie; Clarke, Bruce; Cochran, William D.; Dupree,
   Andrea; Fabrycky, Daniel C.; Fischer, Debra; Ford, Eric B.; Fortney,
   Jonathan; Girouard, Forrest R.; Holman, Matthew J.; Johnson, John;
   Isaacson, Howard; Klaus, Todd C.; Machalek, Pavel; Moorehead, Althea
   V.; Morehead, Robert C.; Ragozzine, Darin; Tenenbaum, Peter; Twicken,
   Joseph; Quinn, Samuel; VanCleve, Jeffrey; Walkowicz, Lucianne M.;
   Welsh, William F.; Devore, Edna; Gould, Alan
Bibcode: 2011ApJ...729...27B
Altcode: 2011arXiv1102.0605B
  NASA's Kepler Mission uses transit photometry to determine
  the frequency of Earth-size planets in or near the habitable
  zone of Sun-like stars. The mission reached a milestone toward
  meeting that goal: the discovery of its first rocky planet,
  Kepler-10b. Two distinct sets of transit events were detected: (1)
  a 152 ± 4 ppm dimming lasting 1.811 ± 0.024 hr with ephemeris
  T [BJD] =2454964.57375<SUP>+0.00060</SUP> <SUB>-0.00082</SUB> +
  N*0.837495<SUP>+0.000004</SUP> <SUB>-0.000005</SUB> days and (2)
  a 376 ± 9 ppm dimming lasting 6.86 ± 0.07 hr with ephemeris
  T [BJD] =2454971.6761<SUP>+0.0020</SUP> <SUB>-0.0023</SUB> +
  N*45.29485<SUP>+0.00065</SUP> <SUB>-0.00076</SUB> days. Statistical
  tests on the photometric and pixel flux time series established the
  viability of the planet candidates triggering ground-based follow-up
  observations. Forty precision Doppler measurements were used to confirm
  that the short-period transit event is due to a planetary companion. The
  parent star is bright enough for asteroseismic analysis. Photometry was
  collected at 1 minute cadence for &gt;4 months from which we detected
  19 distinct pulsation frequencies. Modeling the frequencies resulted in
  precise knowledge of the fundamental stellar properties. Kepler-10 is
  a relatively old (11.9 ± 4.5 Gyr) but otherwise Sun-like main-sequence
  star with T <SUB>eff</SUB> = 5627 ± 44 K, M <SUB>sstarf</SUB> = 0.895
  ± 0.060 M <SUB>sun</SUB>, and R <SUB>sstarf</SUB> = 1.056 ± 0.021 R
  <SUB>sun</SUB>. Physical models simultaneously fit to the transit light
  curves and the precision Doppler measurements yielded tight constraints
  on the properties of Kepler-10b that speak to its rocky composition: M
  <SUB>P</SUB> = 4.56<SUP>+1.17</SUP> <SUB>-1.29</SUB> M <SUB>⊕</SUB>,
  R <SUB>P</SUB> = 1.416<SUP>+0.033</SUP> <SUB>-0.036</SUB> R
  <SUB>⊕</SUB>, and ρ<SUB>P</SUB> = 8.8<SUP>+2.1</SUP> <SUB>-2.9</SUB>
  g cm<SUP>-3</SUP>. Kepler-10b is the smallest transiting exoplanet
  discovered to date. <P />Based in part on observations obtained at
  the W. M. Keck Observatory, which is operated by the University of
  California and the California Institute of Technology.

Title: LCOGT Sites and Facilities
Authors: Martinez, John; Brown, Timothy M.; Conway, Patrick; Elphick,
   Mark; Falarski, Michael; Hawkins, Eric; Rosing, Wayne; Shobbrook, John
Bibcode: 2011tfa..confE..32M
Altcode:
  LCOGT is currently building and deploying a world-wide network of
  at least twelve 1-meter and twenty-four 0.4-meter telescopes to as
  many as 4 sites in the Southern hemisphere (Chile, South Africa,
  Eastern Australia) and 4 in the Northern hemisphere (Hawaii, West
  Texas, Canary Islands). Our deployment and operations model emphasizes
  modularity and interchangeability of major components, maintenance and
  troubleshooting personnel who are local to the site, and autonomy of
  operation. We plan to ship, install, and spare large units (in many
  cases entire telescopes), with minimal assembly on site.

Title: White-light Flares on Cool Stars in the Kepler Quarter 1 Data
Authors: Walkowicz, Lucianne M.; Basri, Gibor; Batalha, Natalie;
   Gilliland, Ronald L.; Jenkins, Jon; Borucki, William J.; Koch, David;
   Caldwell, Doug; Dupree, Andrea K.; Latham, David W.; Meibom, Soeren;
   Howell, Steve; Brown, Timothy M.; Bryson, Steve
Bibcode: 2011AJ....141...50W
Altcode: 2010arXiv1008.0853W
  We present the results of a search for white-light flares on ~23,000
  cool dwarfs in the Kepler Quarter 1 long cadence data. We have
  identified 373 flaring stars, some of which flare multiple times during
  the observation period. We calculate relative flare energies, flare
  rates, and durations and compare these with the quiescent photometric
  variability of our sample. We find that M dwarfs tend to flare more
  frequently but for shorter durations than K dwarfs and that they emit
  more energy relative to their quiescent luminosity in a given flare than
  K dwarfs. Stars that are more photometrically variable in quiescence
  tend to emit relatively more energy during flares, but variability is
  only weakly correlated with flare frequency. We estimate distances for
  our sample of flare stars and find that the flaring fraction agrees
  well with other observations of flare statistics for stars within
  300 pc above the Galactic plane. These observations provide a more
  rounded view of stellar flares by sampling stars that have not been
  pre-selected by their activity, and are informative for understanding
  the influence of these flares on planetary habitability.

Title: Characteristics of Kepler Planetary Candidates Based on the
    First Data Set
Authors: Borucki, William J.; Koch, David G.; Basri, Gibor;
   Batalha, Natalie; Boss, Alan; Brown, Timothy M.; Caldwell, Douglas;
   Christensen-Dalsgaard, Jørgen; Cochran, William D.; DeVore, Edna;
   Dunham, Edward W.; Dupree, Andrea K.; Gautier, Thomas N., III;
   Geary, John C.; Gilliland, Ronald; Gould, Alan; Howell, Steve B.;
   Jenkins, Jon M.; Kjeldsen, Hans; Latham, David W.; Lissauer, Jack
   J.; Marcy, Geoffrey W.; Monet, David G.; Sasselov, Dimitar; Tarter,
   Jill; Charbonneau, David; Doyle, Laurance; Ford, Eric B.; Fortney,
   Jonathan; Holman, Matthew J.; Seager, Sara; Steffen, Jason H.; Welsh,
   William F.; Allen, Christopher; Bryson, Stephen T.; Buchhave, Lars;
   Chandrasekaran, Hema; Christiansen, Jessie L.; Ciardi, David; Clarke,
   Bruce D.; Dotson, Jessie L.; Endl, Michael; Fischer, Debra; Fressin,
   Francois; Haas, Michael; Horch, Elliott; Howard, Andrew; Isaacson,
   Howard; Kolodziejczak, Jeffery; Li, Jie; MacQueen, Phillip; Meibom,
   Søren; Prsa, Andrej; Quintana, Elisa V.; Rowe, Jason; Sherry, William;
   Tenenbaum, Peter; Torres, Guillermo; Twicken, Joseph D.; Van Cleve,
   Jeffrey; Walkowicz, Lucianne; Wu, Hayley
Bibcode: 2011ApJ...728..117B
Altcode: 2010arXiv1006.2799B
  In the spring of 2009, the Kepler Mission commenced high-precision
  photometry on nearly 156,000 stars to determine the frequency and
  characteristics of small exoplanets, conduct a guest observer program,
  and obtain asteroseismic data on a wide variety of stars. On 2010
  June 15, the Kepler Mission released most of the data from the first
  quarter of observations. At the time of this data release, 705 stars
  from this first data set have exoplanet candidates with sizes from as
  small as that of Earth to larger than that of Jupiter. Here we give
  the identity and characteristics of 305 released stars with planetary
  candidates. Data for the remaining 400 stars with planetary candidates
  will be released in 2011 February. More than half the candidates on
  the released list have radii less than half that of Jupiter. Five
  candidates are present in and near the habitable zone; two near
  super-Earth size, and three bracketing the size of Jupiter. The
  released stars also include five possible multi-planet systems. One
  of these has two Neptune-size (2.3 and 2.5 Earth radius) candidates
  with near-resonant periods.

Title: Modeling Kepler Transit Light Curves as False Positives:
    Rejection of Blend Scenarios for Kepler-9, and Validation of Kepler-9
    d, A Super-earth-size Planet in a Multiple System
Authors: Torres, Guillermo; Fressin, François; Batalha, Natalie M.;
   Borucki, William J.; Brown, Timothy M.; Bryson, Stephen T.; Buchhave,
   Lars A.; Charbonneau, David; Ciardi, David R.; Dunham, Edward W.;
   Fabrycky, Daniel C.; Ford, Eric B.; Gautier, Thomas N., III; Gilliland,
   Ronald L.; Holman, Matthew J.; Howell, Steve B.; Isaacson, Howard;
   Jenkins, Jon M.; Koch, David G.; Latham, David W.; Lissauer, Jack J.;
   Marcy, Geoffrey W.; Monet, David G.; Prsa, Andrej; Quinn, Samuel N.;
   Ragozzine, Darin; Rowe, Jason F.; Sasselov, Dimitar D.; Steffen,
   Jason H.; Welsh, William F.
Bibcode: 2011ApJ...727...24T
Altcode: 2010arXiv1008.4393T
  Light curves from the Kepler Mission contain valuable information on the
  nature of the phenomena producing the transit-like signals. To assist
  in exploring the possibility that they are due to an astrophysical
  false positive, we describe a procedure (BLENDER) to model the
  photometry in terms of a "blend" rather than a planet orbiting a
  star. A blend may consist of a background or foreground eclipsing
  binary (or star-planet pair) whose eclipses are attenuated by the
  light of the candidate and possibly other stars within the photometric
  aperture. We apply BLENDER to the case of Kepler-9 (KIC 3323887), a
  target harboring two previously confirmed Saturn-size planets (Kepler-9
  b and Kepler-9 c) showing transit timing variations, and an additional
  shallower signal with a 1.59 day period suggesting the presence of a
  super-Earth-size planet. Using BLENDER together with constraints from
  other follow-up observations we are able to rule out all blends for
  the two deeper signals and provide independent validation of their
  planetary nature. For the shallower signal, we rule out a large
  fraction of the false positives that might mimic the transits. The
  false alarm rate for remaining blends depends in part (and inversely)
  on the unknown frequency of small-size planets. Based on several
  realistic estimates of this frequency, we conclude with very high
  confidence that this small signal is due to a super-Earth-size planet
  (Kepler-9 d) in a multiple system, rather than a false positive. The
  radius is determined to be 1.64<SUP>+0.19</SUP> <SUB>-0.14</SUB>
  R <SUB>⊕</SUB>, and current spectroscopic observations are as yet
  insufficient to establish its mass.

Title: Photometric Variability in Kepler Target Stars. II. An Overview
    of Amplitude, Periodicity, and Rotation in First Quarter Data
Authors: Basri, Gibor; Walkowicz, Lucianne M.; Batalha, Natalie;
   Gilliland, Ronald L.; Jenkins, Jon; Borucki, William J.; Koch, David;
   Caldwell, Doug; Dupree, Andrea K.; Latham, David W.; Marcy, Geoffrey
   W.; Meibom, Soeren; Brown, Tim
Bibcode: 2011AJ....141...20B
Altcode: 2010arXiv1008.1092B
  We provide an overview of stellar variability in the first quarter
  data from the Kepler mission. The intent of this paper is to examine
  the entire sample of over 150,000 target stars for periodic behavior
  in their light curves and relate this to stellar characteristics. This
  data set constitutes an unprecedented study of stellar variability
  given its great precision and complete time coverage (with a half
  hour cadence). Because the full Kepler pipeline is not currently
  suitable for a study of stellar variability of this sort, we describe
  our procedures for treating the "raw" pipeline data. About half of
  the total sample exhibits convincing periodic variability up to two
  weeks, with amplitudes ranging from differential intensity changes of
  less than 10<SUP>-4</SUP> up to more than 10%. K and M dwarfs have a
  greater fraction of period behavior than G dwarfs. The giants in the
  sample have distinctive quasi-periodic behavior, but are not periodic
  in the way we define it. Not all periodicities are due to rotation,
  and the most significant period is not necessarily the rotation
  period. We discuss properties of the light curves, and in particular
  look at a sample of very clearly periodic G dwarfs. It is clear that
  a large number of them do vary because of rotation and starspots,
  but it will take further analysis to fully exploit this.

Title: Asteroseismology of the Transiting Exoplanet Host HD 17156
    with Hubble Space Telescope Fine Guidance Sensor
Authors: Gilliland, Ronald L.; McCullough, Peter R.; Nelan,
   Edmund P.; Brown, Timothy M.; Charbonneau, David; Nutzman, Philip;
   Christensen-Dalsgaard, Jørgen; Kjeldsen, Hans
Bibcode: 2011ApJ...726....2G
Altcode: 2010arXiv1011.0435G
  Observations conducted with the Fine Guidance Sensor on the Hubble
  Space Telescope (HST) providing high cadence and precision time-series
  photometry were obtained over 10 consecutive days in 2008 December on
  the host star of the transiting exoplanet HD 17156b. During this time,
  1.0 × 10<SUP>12</SUP> photons (corrected for detector dead time) were
  collected in which a noise level of 163 parts per million per 30 s sum
  resulted, thus providing excellent sensitivity to the detection of the
  analog of the solar 5-minute p-mode oscillations. For HD 17156, robust
  detection of p modes supports the determination of the stellar mean
  density of langρ<SUB>*</SUB>rang = 0.5301 ± 0.0044 g cm<SUP>-3</SUP>
  from a detailed fit to the observed frequencies of modes of degree l =
  0, 1, and 2. This is the first star for which the direct determination
  of langρ<SUB>*</SUB>rang has been possible using both asteroseismology
  and detailed analysis of a transiting planet light curve. Using
  the density constraint from asteroseismology, and stellar evolution
  modeling results in M <SUB>*</SUB> = 1.285 ± 0.026 M <SUB>sun</SUB>,
  R <SUB>*</SUB> = 1.507 ± 0.012 R <SUB>sun</SUB>, and a stellar age of
  3.2 ± 0.3 Gyr. <P />Based on observations with the NASA/ESA Hubble
  Space Telescope, obtained at the Space Telescope Science Institute,
  which is operated by AURA, Inc., under NASA contract NAS 5-26555.

Title: Precise Estimates of the Physical Parameters for the Exoplanet
    System HD 17156 Enabled by Hubble Space Telescope Fine Guidance
    Sensor Transit and Asteroseismic Observations
Authors: Nutzman, Philip; Gilliland, Ronald L.; McCullough, Peter R.;
   Charbonneau, David; Christensen-Dalsgaard, Jørgen; Kjeldsen, Hans;
   Nelan, Edmund P.; Brown, Timothy M.; Holman, Matthew J.
Bibcode: 2011ApJ...726....3N
Altcode: 2010arXiv1011.0440N
  We present observations of three distinct transits of HD 17156b
  obtained with the Fine Guidance Sensors on board the Hubble Space
  Telescope. We analyzed both the transit photometry and previously
  published radial velocities to find the planet-star radius ratio
  R<SUB>p</SUB> /R <SUB>sstarf</SUB> = 0.07454 ± 0.00035, inclination i =
  86.49<SUP>+0.24</SUP> <SUB>-0.20</SUB> deg, and scaled semimajor axis
  a/R <SUB>sstarf</SUB> = 23.19<SUP>+0.32</SUP> <SUB>-0.27</SUB>. This
  last value translates directly to a mean stellar density determination
  ρ<SUB>sstarf</SUB> = 0.522<SUP>+0.021</SUP> <SUB>-0.018</SUB>
  g cm<SUP>-3</SUP>. Analysis of asteroseismology observations by
  the companion paper of Gilliland et al. provides a consistent but
  significantly refined measurement of ρ<SUB>sstarf</SUB> = 0.5308 ±
  0.0040. We compare stellar isochrones to this density estimate and find
  M <SUB>sstarf</SUB> = 1.275 ± 0.018 M <SUB>sun</SUB> and a stellar
  age of 3.37<SUP>+0.20</SUP> <SUB>-0.47</SUB> Gyr. Using this estimate
  of M <SUB>sstarf</SUB> and incorporating the density constraint from
  asteroseismology, we model both the photometry and published radial
  velocities to estimate the planet radius R<SUB>p</SUB> = 1.0870 ±
  0.0066 R<SUB>J</SUB> and the stellar radius R <SUB>sstarf</SUB> =
  1.5007 ± 0.0076 R <SUB>sun</SUB>. The planet radius is larger than
  that found in previous studies and consistent with theoretical models
  of a solar-composition gas giant of the same mass and equilibrium
  temperature. For the three transits, we determine the times of
  mid-transit to a precision of 6.2 s, 7.6 s, and 6.9 s, and the
  transit times for HD 17156 do not show any significant departures
  from a constant period. The joint analysis of transit photometry and
  asteroseismology presages similar studies that will be enabled by the
  NASA Kepler Mission. <P />Based on observations with the NASA/ESA Hubble
  Space Telescope obtained at the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in
  Astronomy, Incorporated, under NASA contract NAS5-26555.

Title: KOI-54: The Remarkable Pulsating, Periastron-Pumped Binary Star
Authors: Welsh, William F.; Orosz, J. A.; Gilliland, R. L.; Aerts,
   C.; Brown, T. M.; Brugamyer, E.; Cochran, W. D.; Guzik, J. A.; Kurtz,
   D. W.; Latham, D. W.; Marcy, G. W.; Quinn, S. A.; Zima, W.; Koch,
   D. G.; Borucki, W. J.; Kepler Science Team
Bibcode: 2011AAS...21710307W
Altcode: 2011BAAS...4310307W
  A previously-known unremarkable A star has been discovered by Kepler
  to be a fascinating object: KOI-54 exhibits sharp brightening events
  every 42 days and a beat-pattern of pulsations locked in phase with the
  brightenings. We have determined that this is a highly eccentric face-on
  binary star system and the brightenings are due to tidal distortion
  plus mutual irradiation of the stars at periastron passage. The periodic
  driving produces a rich set of tidally-induced g-mode pulsations locked
  to the orbital period. We present spectral analysis, radial velocities,
  the exquisite Kepler photometry of KOI-54, and a model that successfully
  reproduces these observations. <P />Kepler was selected as the 10th
  mission of the Discovery Program. Funding for this mission is provided
  by NASA, Science Mission Directorate.

Title: Kepler observations: Light shed on the hybrid γ Doradus -
    δ Scuti pulsation phenomenon
Authors: Grigahcène, A.; Uytterhoeven, K.; Antoci, V.; Balona, L.;
   Catanzaro, G.; Daszyńska-Daszkiewicz, J.; Guzik, J. A.; Handler, G.;
   Houdek, G.; Kurtz, D. W.; Marconi, M.; Monteiro, M. J. P. F. G.;
   Moya, A.; Ripepi, V.; Suárez, J. -C.; Borucki, W. J.; Brown,
   T. M.; Christensen-Dalsgaard, J.; Gilliland, R. L.; Jenkins, J. M.;
   Kjeldsen, H.; Koch, D.; Bernabei, S.; Bradley, P.; Breger, M.; Di
   Criscienzo, M.; Dupret, M. -A.; García, R. A.; García Hernández, A.;
   Jackiewicz, J.; Kaiser, A.; Lehmann, H.; Martín-Ruiz, S.; Mathias,
   P.; Molenda-Żakowicz, J.; Nemec, J. M.; Nuspl, J.; Paparó, M.;
   Roth, M.; Szabó, R.; Suran, M. D.; Ventura, R.
Bibcode: 2010AN....331..989G
Altcode:
  Through the observational study of stellar pulsations, the internal
  structure of stars can be probed and theoretical models can be
  tested. The main sequence γ Doradus (Dor) and δ Scuti (Sct) stars
  with masses 1.2-2.5 M<SUB>⊙</SUB> are particularly interesting for
  asteroseismic study. The γ Dor stars pulsate in high-order gravity (g)
  modes, with pulsational periods of order of one day. The δ Sct stars,
  on the other hand, show low-order g and pressure (p) modes with periods
  of order of 2 hours. Theory predicts the existence of `hybrid' stars,
  i.e. stars pulsating in both types of modes, in an overlap region
  between the instability strips of γ Dor and δ Sct stars in the
  Hertzsprung-Russell diagram. Hybrid stars are particularly interesting
  as the two types of modes probe different regions of the stellar
  interior and hence provide complementary model constraints. Before
  the advent of Kepler, only a few hybrid stars had been confirmed. The
  {{Kepler}} satellite is providing a true revolution in the study
  of and search for hybrid stars. Analysis of the first 50 days of
  {{Kepler}} data of hundreds of γ Dor and δ Sct candidates reveals
  extremely rich frequency spectra, with most stars showing frequencies
  in both the δ Sct and γ Dor frequency range. As these results show
  that there are practically no pure δ Sct or γ Dor pulsators, a new
  observational classification scheme is proposed by \cite{Grig10}. We
  present their results and characterize 234 stars in terms of δ Sct,
  γ Dor, δ Sct/γ Dor or γ Dor/δ Sct hybrids.

Title: The Kepler Asteroseismic Investigation: Scientific goals and
    first results
Authors: Kjeldsen, H.; Christensen-Dalsgaard, J.; Handberg, R.; Brown,
   T. M.; Gilliland, R. L.; Borucki, W. J.; Koch, D.
Bibcode: 2010AN....331..966K
Altcode: 2010arXiv1007.1816K
  Kepler is a NASA mission designed to detect exoplanets and characterize
  the properties of exoplanetary systems. Kepler also includes an
  asteroseismic programme which is being conducted through the Kepler
  Asteroseismic Science Consortium (KASC), whose 400 members are organized
  into 13 working groups by type of variable star. So far data have been
  available from the first 7 month of the mission containing a total of
  2937 targets observed at a 1-min cadence for periods between 10 days and
  7 months. The goals of the asteroseismic part of the Kepler project is
  to perform detailed studies of stellar interiors. The first results of
  the asteroseismic analysis are orders of magnitude better than seen
  before, and this bodes well for how the future analysis of Kepler
  data for many types of stars will impact our general understanding of
  stellar structure and evolution.

Title: Discovery and Rossiter-Mclaughlin Effect of Exoplanet Kepler-8b
Authors: Jenkins, Jon M.; Borucki, William J.; Koch, David G.;
   Marcy, Geoffrey W.; Cochran, William D.; Welsh, William F.; Basri,
   Gibor; Batalha, Natalie M.; Buchhave, Lars A.; Brown, Timothy M.;
   Caldwell, Douglas A.; Dunham, Edward W.; Endl, Michael; Fischer,
   Debra A.; Gautier, Thomas N., III; Geary, John C.; Gilliland,
   Ronald L.; Howell, Steve B.; Isaacson, Howard; Johnson, John Asher;
   Latham, David W.; Lissauer, Jack J.; Monet, David G.; Rowe, Jason F.;
   Sasselov, Dimitar D.; Howard, Andrew W.; MacQueen, Phillip; Orosz,
   Jerome A.; Chandrasekaran, Hema; Twicken, Joseph D.; Bryson, Stephen
   T.; Quintana, Elisa V.; Clarke, Bruce D.; Li, Jie; Allen, Christopher;
   Tenenbaum, Peter; Wu, Hayley; Meibom, Søren; Klaus, Todd C.; Middour,
   Christopher K.; Cote, Miles T.; McCauliff, Sean; Girouard, Forrest R.;
   Gunter, Jay P.; Wohler, Bill; Hall, Jennifer R.; Ibrahim, Khadeejah;
   Kamal Uddin, AKM; Wu, Michael S.; Bhavsar, Paresh A.; Van Cleve,
   Jeffrey; Pletcher, David L.; Dotson, Jessie L.; Haas, Michael R.
Bibcode: 2010ApJ...724.1108J
Altcode: 2010arXiv1001.0416J
  We report on the discovery and the Rossiter-McLaughlin (R-M) effect
  of Kepler-8b, a transiting planet identified by the NASA Kepler
  Mission. Kepler photometry and Keck-HIRES radial velocities yield the
  radius and mass of the planet around this F8IV subgiant host star. The
  planet has a radius R <SUB>P</SUB> = 1.419 R <SUB>J</SUB> and a mass
  M <SUB>P</SUB> = 0.60 M <SUB>J</SUB>, yielding a density of 0.26 g
  cm<SUP>-3</SUP>, one of the lowest planetary densities known. The
  orbital period is P = 3.523 days and the orbital semimajor axis is
  0.0483<SUP>+0.0006</SUP> <SUB>-0.0012</SUB> AU. The star has a large
  rotational vsin i of 10.5 ± 0.7 km s<SUP>-1</SUP> and is relatively
  faint (V ≈ 13.89 mag); both properties are deleterious to precise
  Doppler measurements. The velocities are indeed noisy, with scatter of
  30 m s<SUP>-1</SUP>, but exhibit a period and phase that are consistent
  with those implied by transit photometry. We securely detect the R-M
  effect, confirming the planet's existence and establishing its orbit
  as prograde. We measure an inclination between the projected planetary
  orbital axis and the projected stellar rotation axis of λ = -26fdg4 ±
  10fdg1, indicating a significant inclination of the planetary orbit. R-M
  measurements of a large sample of transiting planets from Kepler will
  provide a statistically robust measure of the true distribution of
  spin-orbit orientations for hot Jupiters around F and early G stars. <P
  />Based in part on observations obtained at the W. M. Keck Observatory,
  which is operated as a scientific partnership between the California
  Institute of Technology, the University of California, and the National
  Aeronautics and Space Administration. The Observatory was made possible
  by the generous financial support of the W. M. Keck Foundation.

Title: Constraints of a pulsation frequency on stellar parameters
    in the eclipsing spectroscopic binary system V577 Oph
Authors: Creevey, O. L.; Telting, J.; Belmonte, J. A.; Brown, T. M.;
   Handler, G.; Metcalfe, T. S.; Pinheiro, F.; Sousa, S.; Terrell, D.;
   Zhou, A.
Bibcode: 2010AN....331..952C
Altcode: 2010arXiv1011.3028C
  We present a preliminary spectroscopic analysis of the binary system
  V577Oph, observed during the summer of 2007 on the 2.6 m NOT telescope
  on La Palma. We have obtained time series spectroscopic observations,
  which show clear binary motion as well as radial velocity variations due
  to pulsation in the primary star. By modelling the radial velocities
  we determine a full orbital solution of the system, which yields
  {M_A sin<SUP>3</SUP> i = 1.562 ± 0.012} M<SUB>⊙</SUB> and {M_B
  sin<SUP>3</SUP> i = 1.461 ± 0.020} M<SUB>⊙</SUB>. An estimate
  of inclination from photometry yields a primary mass of ∼ 1.6
  M<SUB>⊙</SUB>. Using this derived mass, and the known pulsation
  frequency we can impose a lower limit of 1 Gyr on the age of the system,
  and constrain the parameters of the oscillation mode. We show that with
  further analysis of the spectra (extracting the atmospheric parameters),
  tighter constraints could be imposed on the age, metallicity and the
  mode parameters. This work emphasizes the power that a single pulsation
  frequency can have for constraining stellar parameters in an eclipsing
  binary system.

Title: A Precise Asteroseismic Age and Radius for the Evolved Sun-like
    Star KIC 11026764
Authors: Metcalfe, T. S.; Monteiro, M. J. P. F. G.; Thompson, M. J.;
   Molenda-Żakowicz, J.; Appourchaux, T.; Chaplin, W. J.; Doǧan, G.;
   Eggenberger, P.; Bedding, T. R.; Bruntt, H.; Creevey, O. L.; Quirion,
   P. -O.; Stello, D.; Bonanno, A.; Silva Aguirre, V.; Basu, S.; Esch,
   L.; Gai, N.; Di Mauro, M. P.; Kosovichev, A. G.; Kitiashvili, I. N.;
   Suárez, J. C.; Moya, A.; Piau, L.; García, R. A.; Marques, J. P.;
   Frasca, A.; Biazzo, K.; Sousa, S. G.; Dreizler, S.; Bazot, M.; Karoff,
   C.; Frandsen, S.; Wilson, P. A.; Brown, T. M.; Christensen-Dalsgaard,
   J.; Gilliland, R. L.; Kjeldsen, H.; Campante, T. L.; Fletcher, S. T.;
   Handberg, R.; Régulo, C.; Salabert, D.; Schou, J.; Verner, G. A.;
   Ballot, J.; Broomhall, A. -M.; Elsworth, Y.; Hekker, S.; Huber, D.;
   Mathur, S.; New, R.; Roxburgh, I. W.; Sato, K. H.; White, T. R.;
   Borucki, W. J.; Koch, D. G.; Jenkins, J. M.
Bibcode: 2010ApJ...723.1583M
Altcode: 2010arXiv1010.4329M
  The primary science goal of the Kepler Mission is to provide
  a census of exoplanets in the solar neighborhood, including the
  identification and characterization of habitable Earth-like planets. The
  asteroseismic capabilities of the mission are being used to determine
  precise radii and ages for the target stars from their solar-like
  oscillations. Chaplin et al. published observations of three bright
  G-type stars, which were monitored during the first 33.5 days of science
  operations. One of these stars, the subgiant KIC 11026764, exhibits a
  characteristic pattern of oscillation frequencies suggesting that it
  has evolved significantly. We have derived asteroseismic estimates of
  the properties of KIC 11026764 from Kepler photometry combined with
  ground-based spectroscopic data. We present the results of detailed
  modeling for this star, employing a variety of independent codes and
  analyses that attempt to match the asteroseismic and spectroscopic
  constraints simultaneously. We determine both the radius and the age
  of KIC 11026764 with a precision near 1%, and an accuracy near 2%
  for the radius and 15% for the age. Continued observations of this
  star promise to reveal additional oscillation frequencies that will
  further improve the determination of its fundamental properties.

Title: Characteristics of the Kepler target stars
Authors: Batalha, Natalie M.; Borucki, William J.; Koch, David G.;
   Brown, Timothy M.; Caldwell, Douglas A.; Latham, David W.
Bibcode: 2010HiA....15..712B
Altcode:
  The Kepler Mission successfully launched March 6, 2009, beginning
  its 3.5-year mission to determine the frequency of Earth-size planets
  in the habitable zones of late-type stars. The brightnesses of over
  100,000 stars are currently being monitored for transit events with
  an expected differential photometric precision of 20 ppm at V=12 for a
  6.5-hour transit. The same targets will be observed continuously over
  the mission duration in order to broaden the detection space to orbital
  periods comparable to that of Earth. This paper provides an overview
  of the selection and prioritization criteria used to choose the stars
  that Kepler is observing from the &gt; 4.5 million objects in the 100
  square degree field of view. The characteristics of the Kepler targets
  are described as well as the implications for detectability of planets
  in the habitable zone smaller than 2R<SUB>⊕</SUB>.

Title: Observational detection of eclipses of J5 Amalthea by the
    Galilean satellites
Authors: Christou, A. A.; Lewis, F.; Roche, P.; Hidas, M. G.; Brown,
   T. M.
Bibcode: 2010A&A...522A...6C
Altcode: 2011arXiv1104.0042C
  <BR /> Aims: We carried out observations of the small jovian satellite
  Amalthea (J5) as it was being eclipsed by the Galilean satellites near
  the 2009 equinox of Jupiter in order to apply the technique of mutual
  event photometry to the astrometric determination of this satellite's
  position. <BR /> Methods: The observations were carried out during
  the period 06/2009-09/2009 from the island of Maui, Hawaii and Siding
  Spring, Australia with the 2m Faulkes Telescopes North and South
  respectively. We observed in the near-infrared part of the spectrum
  using a PanStarrs-Z filter with Jupiter near the edge of the field
  in order to mitigate against the glare from the planet. Frames were
  acquired at rates &gt; 1/min during eclipse times predicted using
  recent JPL ephemerides for the satellites. Following subtraction
  of the sky background from these frames, differential aperture
  photometry was carried out on Amalthea and a nearby field star. <BR />
  Results: We have obtained three lightcurves which show a clear drop
  in the flux from Amalthea, indicating that an eclipse took place as
  predicted. These were model-fitted to yield best estimates of the time
  of maximum flux drop and the impact parameter. These are consistent with
  Amalthea's ephemeris but indicate that Amalthea is slightly ahead of,
  and closer to Jupiter than, its predicted position by approximately
  half the ephemeris uncertainty in these directions. We argue that a
  ground-based campaign of higher-cadence photometry accurate at the 5%
  level or better during the next season of eclipses in 2014-15 should
  yield positions to within 0.05 arcsec and affect a corresponding
  improvement in Amalthea's ephemeris.

Title: Kepler-9: A System of Multiple Planets Transiting a Sun-Like
    Star, Confirmed by Timing Variations
Authors: Holman, Matthew J.; Fabrycky, Daniel C.; Ragozzine, Darin;
   Ford, Eric B.; Steffen, Jason H.; Welsh, William F.; Lissauer,
   Jack J.; Latham, David W.; Marcy, Geoffrey W.; Walkowicz, Lucianne
   M.; Batalha, Natalie M.; Jenkins, Jon M.; Rowe, Jason F.; Cochran,
   William D.; Fressin, Francois; Torres, Guillermo; Buchhave, Lars A.;
   Sasselov, Dimitar D.; Borucki, William J.; Koch, David G.; Basri,
   Gibor; Brown, Timothy M.; Caldwell, Douglas A.; Charbonneau, David;
   Dunham, Edward W.; Gautier, Thomas N.; Geary, John C.; Gilliland,
   Ronald L.; Haas, Michael R.; Howell, Steve B.; Ciardi, David R.;
   Endl, Michael; Fischer, Debra; Fürész, Gábor; Hartman, Joel D.;
   Isaacson, Howard; Johnson, John A.; MacQueen, Phillip J.; Moorhead,
   Althea V.; Morehead, Robert C.; Orosz, Jerome A.
Bibcode: 2010Sci...330...51H
Altcode:
  The Kepler spacecraft is monitoring more than 150,000 stars for
  evidence of planets transiting those stars. We report the detection of
  two Saturn-size planets that transit the same Sun-like star, based on
  7 months of Kepler observations. Their 19.2- and 38.9-day periods are
  presently increasing and decreasing at respective average rates of 4 and
  39 minutes per orbit; in addition, the transit times of the inner body
  display an alternating variation of smaller amplitude. These signatures
  are characteristic of gravitational interaction of two planets near a
  2:1 orbital resonance. Six radial-velocity observations show that these
  two planets are the most massive objects orbiting close to the star and
  substantially improve the estimates of their masses. After removing the
  signal of the two confirmed giant planets, we identified an additional
  transiting super-Earth-size planet candidate with a period of 1.6 days.

Title: Scheduling observations on the LCOGT network
Authors: Hawkins, Eric; Baliber, Nairn; Bowman, Mark; Brown, Timothy;
   Burleson, Benjamin; Foale, Steven; Ford, Martyn; Lister, Timothy;
   Norbury, Martin; Saunders, Eric; Walker, Zachary
Bibcode: 2010SPIE.7737E..0PH
Altcode: 2010SPIE.7737E..17H
  LCOGT is deploying a world-wide telescope network to enable
  near-continuous coverage of variable or transient sources. We desire the
  telescopes in this network to be scheduled for efficiency with respect
  to a coherent set of science goals. To achieve this, we are developing
  a software structure to carry observing programs from initial proposal
  through data acquisition and feedback to the schedule. Key elements in
  this structure are a database of observation requests, requirements,
  and status, a protocol to describe observations, and a set of planners
  that work by successive refinement of the schedule.

Title: LCOGT Telescope network capabilities
Authors: Pickles, A.; Rosing, W.; Brown, T. M.; de Vera, J.; Dubberley,
   M.; Haldeman, B.; Hausler, S.; Haynes, R.; Hjelstrom, A.; Lobdill,
   R.; Mullins, D.; Posner, V.; Tufts, J.; Walker, Z.
Bibcode: 2010SPIE.7733E..2XP
Altcode: 2010SPIE.7733E..90P
  LCOGT are currently building and deploying a worldwide network of at
  least fifteen 1-meter and twenty-four 0.4-meter telescopes to three
  sites in each hemisphere, enabling extended, redundant and optimally
  continuous coverage of time variable or transient sources. Each
  site will support two or more 1m telescopes and four or more 0.4m
  telescopes. All telescope classes provide a full range of optical
  narrow-band and broad-band UBVRI and ugriZY imaging filters. All
  telescopes are being equipped with a moving light-bar flatfielding
  system called Lambert. The 1m network is intended primarily for science
  observing while the 0.4m network additionally provides educational
  opportunities to participating schools and institutes. The global
  network is designed to accommodate multiple science, educational and
  rapid response capabilities. For LCOGT, the network IS the telescope.

Title: LCOGT sites and site operations
Authors: Martinez, John J.; Brown, Timothy M.; Conway, Patrick;
   Elphick, Mark; Falarski, Michael; Hawkins, Eric; Rosing, Wayne;
   Shobbrook, John
Bibcode: 2010SPIE.7737E..0OM
Altcode: 2010SPIE.7737E..16M
  LCOGT is currently building and deploying a world-wide network of at
  least twelve 1-meter and twenty-four 0.4-meter telescopes to as many
  as 4 sites in the Southern hemisphere (Chile, South Africa, Eastern
  Australia; 4 in the Northern hemisphere (Hawaii, West Texas, Canary
  Islands). Our deployment and operations model emphasizes modularity and
  interchangeability of major components, maintenance and troubleshooting
  personnel who are local to the site, and autonomy of operation. We
  plan to ship, install, and spare large units (in many cases entire
  telescopes), with minimal assembly on site.

Title: Non-Axisymmetric Structure in the Inner Disks of YSOs --
    Signposts of Planet Formation?
Authors: Stauffer, John; Morales-Calderon, Maria; Rebull, Luisa;
   Barrado, David; Bouvier, Jerome; Brown, Tim; Carey, Sean; Carpenter,
   John; Grankin, Konstantin; Gutermuth, Rob; Hartmann, Lee; Hillenbrand,
   Lynne; Holtzman, Jon; Hora, Joe; Ibrahimov, Mansur; James, David;
   Megeath, S. Tom; Skrutzkie, Mike; Vrba, Fred; Wasserman, Lawrence;
   Whitney, Barb
Bibcode: 2010sptz.prop70025S
Altcode:
  We have identified a well-populated class of young stellar objects
  (YSOs) in the Orion Nebula cluster whose light curves show narrow (few
  day timescale) flux dips. Based on comparison to the only previously
  well-documented member of this class (AA Tau), we believe these flux
  dips are due to 'clouds' in the inner circumstellar disk of these
  stars that pass through our line of sight. Our 2009 data suggest that
  most YSO disks have similar structures and that those which exhibit
  these flux dips are simply those whose disks are close to edge-on to
  our line of sight. We propose here to obtain IRAC time series data
  of much higher cadence and significantly better RMS noise for twelve
  members of this class over a 10 day timespan. These data will allow
  us to constrain better the size distribution of the occulting bodies,
  their grain properties and their internal density structure. These
  data will therefore provide quantitative inputs to realistic models
  of circumstellar disk evolution and planet formation/migration.

Title: Photometric Variability in Kepler Target Stars: The Sun Among
    Stars—a First Look
Authors: Basri, Gibor; Walkowicz, Lucianne M.; Batalha, Natalie;
   Gilliland, Ronald L.; Jenkins, Jon; Borucki, William J.; Koch, David;
   Caldwell, Doug; Dupree, Andrea K.; Latham, David W.; Meibom, Søren;
   Howell, Steve; Brown, Tim
Bibcode: 2010ApJ...713L.155B
Altcode: 2010arXiv1001.0414B
  The Kepler mission provides an exciting opportunity to study the
  light curves of stars with unprecedented precision and continuity
  of coverage. This is the first look at a large sample of stars with
  photometric data of a quality that has heretofore been only available
  for our Sun. It provides the first opportunity to compare the irradiance
  variations of our Sun to a large cohort of stars ranging from very
  similar to rather different stellar properties, at a wide variety of
  ages. Although Kepler data are in an early phase of maturity, and we
  only analyze the first month of coverage, it is sufficient to garner the
  first meaningful measurements of our Sun's variability in the context
  of a large cohort of main-sequence stars in the solar neighborhood. We
  find that nearly half of the full sample is more active than the active
  Sun, although most of them are not more than twice as active. The active
  fraction is closer to a third for the stars most similar to the Sun, and
  rises to well more than half for stars cooler than mid-K spectral types.

Title: Asteroseismic Investigation of Known Planet Hosts in the
    Kepler Field
Authors: Christensen-Dalsgaard, J.; Kjeldsen, H.; Brown, T. M.;
   Gilliland, R. L.; Arentoft, T.; Frandsen, S.; Quirion, P. -O.; Borucki,
   W. J.; Koch, D.; Jenkins, J. M.
Bibcode: 2010ApJ...713L.164C
Altcode: 2010arXiv1001.0032C
  In addition to its great potential for characterizing extra-solar
  planetary systems, the Kepler Mission is providing unique data on
  stellar oscillations. A key aspect of Kepler asteroseismology is the
  application to solar-like oscillations of main-sequence stars. As
  an example, we here consider an initial analysis of data for three
  stars in the Kepler field for which planetary transits were known
  from ground-based observations. For one of these, HAT-P-7, we obtain
  a detailed frequency spectrum and hence strong constraints on the
  stellar properties. The remaining two stars show definite evidence
  for solar-like oscillations, yielding a preliminary estimate of their
  mean densities.

Title: Kepler Observations of Transiting Hot Compact Objects
Authors: Rowe, Jason F.; Borucki, William J.; Koch, David; Howell,
   Steve B.; Basri, Gibor; Batalha, Natalie; Brown, Timothy M.; Caldwell,
   Douglas; Cochran, William D.; Dunham, Edward; Dupree, Andrea K.;
   Fortney, Jonathan J.; Gautier, Thomas N., III; Gilliland, Ronald L.;
   Jenkins, Jon; Latham, David W.; Lissauer, Jack J.; Marcy, Geoff;
   Monet, David G.; Sasselov, Dimitar; Welsh, William F.
Bibcode: 2010ApJ...713L.150R
Altcode: 2010arXiv1001.3420R
  Kepler photometry has revealed two unusual transiting companions: one
  orbiting an early A-star and the other orbiting a late B-star. In both
  cases, the occultation of the companion is deeper than the transit. The
  occultation and transit with follow-up optical spectroscopy reveal a
  9400 K early A-star, KOI-74 (KIC 6889235), with a companion in a 5.2
  day orbit with a radius of 0.08 R <SUB>sun</SUB> and a 10,000 K late
  B-star KOI-81 (KIC 8823868) that has a companion in a 24 day orbit with
  a radius of 0.2 R <SUB>sun</SUB>. We infer a temperature of 12,250 K
  for KOI-74b and 13,500 K for KOI-81b. We present 43 days of high duty
  cycle, 30 minute cadence photometry, with models demonstrating the
  intriguing properties of these objects, and speculate on their nature.

Title: Automated Classification of Variable Stars in the
    Asteroseismology Program of the Kepler Space Mission
Authors: Blomme, J.; Debosscher, J.; De Ridder, J.; Aerts, C.;
   Gilliland, R. L.; Christensen-Dalsgaard, J.; Kjeldsen, H.; Brown,
   T. M.; Borucki, W. J.; Koch, D.; Jenkins, J. M.; Kurtz, D. W.; Stello,
   D.; Stevens, I. R.; Suran, M. D.; Derekas, A.
Bibcode: 2010ApJ...713L.204B
Altcode: 2010arXiv1001.0507B
  We present the first results of the application of supervised
  classification methods to the Kepler Q1 long-cadence light curves of a
  subsample of 2288 stars measured in the asteroseismology program of the
  mission. The methods, originally developed in the framework of the CoRoT
  and Gaia space missions, are capable of identifying the most common
  types of stellar variability in a reliable way. Many new variables have
  been discovered, among which a large fraction are eclipsing/ellipsoidal
  binaries unknown prior to launch. A comparison is made between our
  classification from the Kepler data and the pre-launch class based
  on data from the ground, showing that the latter needs significant
  improvement. The noise properties of the Kepler data are compared to
  those of the exoplanet program of the CoRoT satellite. We find that
  Kepler improves on CoRoT by a factor of 2-2.3 in point-to-point scatter.

Title: Kepler-6b: A Transiting Hot Jupiter Orbiting a Metal-rich Star
Authors: Dunham, Edward W.; Borucki, William J.; Koch, David G.;
   Batalha, Natalie M.; Buchhave, Lars A.; Brown, Timothy M.; Caldwell,
   Douglas A.; Cochran, William D.; Endl, Michael; Fischer, Debra;
   Fűrész, Gabor; Gautier, Thomas N., III; Geary, John C.; Gilliland,
   Ronald L.; Gould, Alan; Howell, Steve B.; Jenkins, Jon M.; Kjeldsen,
   Hans; Latham, David W.; Lissauer, Jack J.; Marcy, Geoffrey W.; Meibom,
   Søren; Monet, David G.; Rowe, Jason F.; Sasselov, Dimitar D.
Bibcode: 2010ApJ...713L.136D
Altcode: 2010arXiv1001.0333D
  We announce the discovery of Kepler-6b, a transiting hot Jupiter
  orbiting a star with unusually high metallicity, {[Fe/H]}= +0.34+/-
  0.04. The planet's mass is about 2/3 that of Jupiter, M <SUB>P</SUB>
  = 0.67 M <SUB>J</SUB>, and the radius is 30% larger than that
  of Jupiter, R <SUB>P</SUB> = 1.32 R <SUB>J</SUB>, resulting in a
  density of ρ<SUB>P</SUB> = 0.35 g cm<SUP>-3</SUP>, a fairly typical
  value for such a planet. The orbital period is P = 3.235 days. The
  host star is both more massive than the Sun, M <SUB>sstarf</SUB> =
  1.21 M <SUB>sun</SUB>, and larger than the Sun, R <SUB>sstarf</SUB>
  = 1.39 R <SUB>sun</SUB>. <P />Based in part on observations obtained
  at the W. M. Keck Observatory, which is operated by the University of
  California and the California Institute of Technology.

Title: Detection of Solar-like Oscillations from Kepler Photometry
    of the Open Cluster NGC 6819
Authors: Stello, Dennis; Basu, Sarbani; Bruntt, Hans; Mosser, Benoît;
   Stevens, Ian R.; Brown, Timothy M.; Christensen-Dalsgaard, Jørgen;
   Gilliland, Ronald L.; Kjeldsen, Hans; Arentoft, Torben; Ballot,
   Jérôme; Barban, Caroline; Bedding, Timothy R.; Chaplin, William
   J.; Elsworth, Yvonne P.; García, Rafael A.; Goupil, Marie-Jo;
   Hekker, Saskia; Huber, Daniel; Mathur, Savita; Meibom, Søren;
   Sangaralingam, Vinothini; Baldner, Charles S.; Belkacem, Kevin;
   Biazzo, Katia; Brogaard, Karsten; Suárez, Juan Carlos; D'Antona,
   Francesca; Demarque, Pierre; Esch, Lisa; Gai, Ning; Grundahl, Frank;
   Lebreton, Yveline; Jiang, Biwei; Jevtic, Nada; Karoff, Christoffer;
   Miglio, Andrea; Molenda-Żakowicz, Joanna; Montalbán, Josefina; Noels,
   Arlette; Roca Cortés, Teodoro; Roxburgh, Ian W.; Serenelli, Aldo M.;
   Silva Aguirre, Victor; Sterken, Christiaan; Stine, Peter; Szabó,
   Robert; Weiss, Achim; Borucki, William J.; Koch, David; Jenkins, Jon M.
Bibcode: 2010ApJ...713L.182S
Altcode: 2010arXiv1001.0026S
  Asteroseismology of stars in clusters has been a long-sought goal
  because the assumption of a common age, distance, and initial chemical
  composition allows strong tests of the theory of stellar evolution. We
  report results from the first 34 days of science data from the Kepler
  Mission for the open cluster NGC 6819—one of the four clusters in
  the field of view. We obtain the first clear detections of solar-like
  oscillations in the cluster red giants and are able to measure
  the large frequency separation, Δν, and the frequency of maximum
  oscillation power, ν<SUB>max</SUB>. We find that the asteroseismic
  parameters allow us to test cluster membership of the stars, and
  even with the limited seismic data in hand, we can already identify
  four possible non-members despite their having a better than 80%
  membership probability from radial velocity measurements. We are also
  able to determine the oscillation amplitudes for stars that span about
  2 orders of magnitude in luminosity and find good agreement with the
  prediction that oscillation amplitudes scale as the luminosity to the
  power of 0.7. These early results demonstrate the unique potential of
  asteroseismology of the stellar clusters observed by Kepler.

Title: First Kepler Results on RR Lyrae Stars
Authors: Kolenberg, K.; Szabó, R.; Kurtz, D. W.; Gilliland, R. L.;
   Christensen-Dalsgaard, J.; Kjeldsen, H.; Brown, T. M.; Benkő,
   J. M.; Chadid, M.; Derekas, A.; Di Criscienzo, M.; Guggenberger, E.;
   Kinemuchi, K.; Kunder, A.; Kolláth, Z.; Kopacki, G.; Moskalik, P.;
   Nemec, J. M.; Nuspl, J.; Silvotti, R.; Suran, M. D.; Borucki, W. J.;
   Koch, D.; Jenkins, J. M.
Bibcode: 2010ApJ...713L.198K
Altcode: 2010arXiv1001.0417K
  We present the first results of our analyses of selected RR Lyrae stars
  for which data have been obtained by the Kepler Mission. As expected,
  we find a significant fraction of the RRab stars to show the Blazhko
  effect, a still unexplained phenomenon that manifests itself as periodic
  amplitude and phase modulations of the light curve, on timescales of
  typically tens to hundreds of days. The long time span of the Kepler
  Mission of 3.5 yr and the unprecedentedly high precision of its data
  provide a unique opportunity for the study of RR Lyrae stars. Using
  data of a modulated star observed in the first roll as a showcase, we
  discuss the data, our analyses, findings, and their implications for our
  understanding of RR Lyrae stars and the Blazhko effect. With at least
  40% of the RR Lyrae stars in our sample showing modulation, we confirm
  the high incidence rate that was only found in recent high-precision
  studies. Moreover, we report the occurrence of additional frequencies,
  beyond the main pulsation mode and its modulation components. Their
  half-integer ratio to the main frequency is reminiscent of a period
  doubling effect caused by resonances, observed for the first time in
  RR Lyrae stars.

Title: Hybrid γ Doradus-δ Scuti Pulsators: New Insights into the
    Physics of the Oscillations from Kepler Observations
Authors: Grigahcène, A.; Antoci, V.; Balona, L.; Catanzaro, G.;
   Daszyńska-Daszkiewicz, J.; Guzik, J. A.; Handler, G.; Houdek,
   G.; Kurtz, D. W.; Marconi, M.; Monteiro, M. J. P. F. G.; Moya, A.;
   Ripepi, V.; Suárez, J. -C.; Uytterhoeven, K.; Borucki, W. J.; Brown,
   T. M.; Christensen-Dalsgaard, J.; Gilliland, R. L.; Jenkins, J. M.;
   Kjeldsen, H.; Koch, D.; Bernabei, S.; Bradley, P.; Breger, M.; Di
   Criscienzo, M.; Dupret, M. -A.; García, R. A.; García Hernández, A.;
   Jackiewicz, J.; Kaiser, A.; Lehmann, H.; Martín-Ruiz, S.; Mathias,
   P.; Molenda-Żakowicz, J.; Nemec, J. M.; Nuspl, J.; Paparó, M.;
   Roth, M.; Szabó, R.; Suran, M. D.; Ventura, R.
Bibcode: 2010ApJ...713L.192G
Altcode: 2010arXiv1001.0747G
  Observations of the pulsations of stars can be used to infer their
  interior structure and test theoretical models. The main-sequence
  γ Doradus (Dor) and δ Scuti (Sct) stars with masses 1.2-2.5 M
  <SUB>sun</SUB> are particularly useful for these studies. The γ
  Dor stars pulsate in high-order g-modes with periods of order 1
  day, driven by convective blocking at the base of their envelope
  convection zone. The δ Sct stars pulsate in low-order g- and p-modes
  with periods of order 2 hr, driven by the κ mechanism operating in
  the He II ionization zone. Theory predicts an overlap region in the
  Hertzsprung-Russell diagram between instability regions, where "hybrid"
  stars pulsating in both types of modes should exist. The two types of
  modes with properties governed by different portions of the stellar
  interior provide complementary model constraints. Among the known γ
  Dor and δ Sct stars, only four have been confirmed as hybrids. Now,
  analysis of combined Quarter 0 and Quarter 1 Kepler data for hundreds of
  variable stars shows that the frequency spectra are so rich that there
  are practically no pure δ Sct or γ Dor pulsators, i.e., essentially
  all of the stars show frequencies in both the δ Sct and the γ Dor
  frequency range. A new observational classification scheme is proposed
  that takes into account the amplitude as well as the frequency and is
  applied to categorize 234 stars as δ Sct, γ Dor, δ Sct/γ Dor or
  γ Dor/δ Sct hybrids.

Title: Kepler-7b: A Transiting Planet with Unusually Low Density
Authors: Latham, David W.; Borucki, William J.; Koch, David G.;
   Brown, Timothy M.; Buchhave, Lars A.; Basri, Gibor; Batalha, Natalie
   M.; Caldwell, Douglas A.; Cochran, William D.; Dunham, Edward W.;
   Fűrész, Gabor; Gautier, Thomas N., III; Geary, John C.; Gilliland,
   Ronald L.; Howell, Steve B.; Jenkins, Jon M.; Lissauer, Jack J.; Marcy,
   Geoffrey W.; Monet, David G.; Rowe, Jason F.; Sasselov, Dimitar D.
Bibcode: 2010ApJ...713L.140L
Altcode: 2010arXiv1001.0190L
  We report on the discovery and confirmation of Kepler-7b, a transiting
  planet with unusually low density. The mass is less than half that of
  Jupiter, M <SUB>P</SUB> = 0.43 M <SUB>J</SUB>, but the radius is 50%
  larger, R <SUB>P</SUB> = 1.48 R <SUB>J</SUB>. The resulting density,
  ρ<SUB>P</SUB> = 0.17 g cm<SUP>-3</SUP>, is the second lowest reported
  so far for an extrasolar planet. The orbital period is fairly long,
  P = 4.886 days, and the host star is not much hotter than the Sun, T
  <SUB>eff</SUB> = 6000 K. However, it is more massive and considerably
  larger than the Sun, M <SUB>sstarf</SUB> = 1.35 M <SUB>sun</SUB> and
  R <SUB>sstarf</SUB> = 1.84 R <SUB>sun</SUB>, and must be near the end
  of its life on the main sequence. <P />Based in part on observations
  obtained at the W. M. Keck Observatory, which is operated by the
  University of California and the California Institute of Technology.

Title: The Asteroseismic Potential of Kepler: First Results for
    Solar-Type Stars
Authors: Chaplin, W. J.; Appourchaux, T.; Elsworth, Y.; García,
   R. A.; Houdek, G.; Karoff, C.; Metcalfe, T. S.; Molenda-Żakowicz,
   J.; Monteiro, M. J. P. F. G.; Thompson, M. J.; Brown, T. M.;
   Christensen-Dalsgaard, J.; Gilliland, R. L.; Kjeldsen, H.; Borucki,
   W. J.; Koch, D.; Jenkins, J. M.; Ballot, J.; Basu, S.; Bazot, M.;
   Bedding, T. R.; Benomar, O.; Bonanno, A.; Brandão, I. M.; Bruntt,
   H.; Campante, T. L.; Creevey, O. L.; Di Mauro, M. P.; Doǧan,
   G.; Dreizler, S.; Eggenberger, P.; Esch, L.; Fletcher, S. T.;
   Frandsen, S.; Gai, N.; Gaulme, P.; Handberg, R.; Hekker, S.; Howe,
   R.; Huber, D.; Korzennik, S. G.; Lebrun, J. C.; Leccia, S.; Martic,
   M.; Mathur, S.; Mosser, B.; New, R.; Quirion, P. -O.; Régulo, C.;
   Roxburgh, I. W.; Salabert, D.; Schou, J.; Sousa, S. G.; Stello, D.;
   Verner, G. A.; Arentoft, T.; Barban, C.; Belkacem, K.; Benatti, S.;
   Biazzo, K.; Boumier, P.; Bradley, P. A.; Broomhall, A. -M.; Buzasi,
   D. L.; Claudi, R. U.; Cunha, M. S.; D'Antona, F.; Deheuvels, S.;
   Derekas, A.; García Hernández, A.; Giampapa, M. S.; Goupil, M. J.;
   Gruberbauer, M.; Guzik, J. A.; Hale, S. J.; Ireland, M. J.; Kiss,
   L. L.; Kitiashvili, I. N.; Kolenberg, K.; Korhonen, H.; Kosovichev,
   A. G.; Kupka, F.; Lebreton, Y.; Leroy, B.; Ludwig, H. -G.; Mathis, S.;
   Michel, E.; Miglio, A.; Montalbán, J.; Moya, A.; Noels, A.; Noyes,
   R. W.; Pallé, P. L.; Piau, L.; Preston, H. L.; Roca Cortés, T.;
   Roth, M.; Sato, K. H.; Schmitt, J.; Serenelli, A. M.; Silva Aguirre,
   V.; Stevens, I. R.; Suárez, J. C.; Suran, M. D.; Trampedach, R.;
   Turck-Chièze, S.; Uytterhoeven, K.; Ventura, R.; Wilson, P. A.
Bibcode: 2010ApJ...713L.169C
Altcode: 2010arXiv1001.0506C
  We present preliminary asteroseismic results from Kepler on three G-type
  stars. The observations, made at one-minute cadence during the first
  33.5 days of science operations, reveal high signal-to-noise solar-like
  oscillation spectra in all three stars: about 20 modes of oscillation
  may be clearly distinguished in each star. We discuss the appearance of
  the oscillation spectra, use the frequencies and frequency separations
  to provide first results on the radii, masses, and ages of the stars,
  and comment in the light of these results on prospects for inference
  on other solar-type stars that Kepler will observe.

Title: Discovery of the Transiting Planet Kepler-5b
Authors: Koch, David G.; Borucki, William J.; Rowe, Jason F.; Batalha,
   Natalie M.; Brown, Timothy M.; Caldwell, Douglas A.; Caldwell, John;
   Cochran, William D.; DeVore, Edna; Dunham, Edward W.; Dupree, Andrea
   K.; Gautier, Thomas N., III; Geary, John C.; Gilliland, Ron L.; Howell,
   Steve B.; Jenkins, Jon M.; Latham, David W.; Lissauer, Jack J.; Marcy,
   Geoff W.; Morrison, David; Tarter, Jill
Bibcode: 2010ApJ...713L.131K
Altcode: 2010arXiv1001.0913K
  We present 44 days of high duty cycle, ultra precise photometry of
  the 13th magnitude star Kepler-5 (KIC 8191672, T <SUB>eff</SUB>=
  6300 K, log g= 4.1), which exhibits periodic transits with a depth
  of 0.7%. Detailed modeling of the transit is consistent with a
  planetary companion with an orbital period of 3.548460 ± 0.000032
  days and a radius of 1.431<SUP>+0.041</SUP> <SUB>-0.052</SUB>
  R <SUB>J</SUB>. Follow-up radial velocity measurements with the
  Keck HIRES spectrograph on nine separate nights demonstrate that
  the planet is more than twice as massive as Jupiter with a mass of
  2.114<SUP>+0.056</SUP> <SUB>-0.059</SUB> M <SUB>J</SUB> and a mean
  density of 0.894 ± 0.079 g cm<SUP>-3</SUP>.

Title: Kepler-4b: A Hot Neptune-like Planet of a G0 Star Near
    Main-sequence Turnoff
Authors: Borucki, William J.; Koch, David G.; Brown, Timothy M.;
   Basri, Gibor; Batalha, Natalie M.; Caldwell, Douglas A.; Cochran,
   William D.; Dunham, Edward W.; Gautier, Thomas N., III; Geary, John
   C.; Gilliland, Ronald L.; Howell, Steve B.; Jenkins, Jon M.; Latham,
   David W.; Lissauer, Jack J.; Marcy, Geoffrey W.; Monet, David; Rowe,
   Jason F.; Sasselov, Dimitar
Bibcode: 2010ApJ...713L.126B
Altcode: 2010arXiv1001.0604B
  Early time-series photometry from NASA's Kepler spacecraft
  has revealed a planet transiting the star we term Kepler-4,
  at R.A. = 19<SUP>h</SUP>02<SUP>m</SUP>27.<SUP>s</SUP>68, δ =
  +50°08'08farcs7. The planet has an orbital period of 3.213 days
  and shows transits with a relative depth of 0.87 × 10<SUP>-3</SUP>
  and a duration of about 3.95 hr. Radial velocity (RV) measurements
  from the Keck High Resolution Echelle Spectrometer show a reflex
  Doppler signal of 9.3<SUP>+1.1</SUP> <SUB>-1.9</SUB> m s<SUP>-1</SUP>,
  consistent with a low-eccentricity orbit with the phase expected from
  the transits. Various tests show no evidence for any companion star
  near enough to affect the light curve or the RVs for this system. From
  a transit-based estimate of the host star's mean density, combined
  with analysis of high-resolution spectra, we infer that the host
  star is near turnoff from the main sequence, with estimated mass and
  radius of 1.223<SUP>+0.053</SUP> <SUB>-0.091</SUB> M <SUB>sun</SUB> and
  1.487<SUP>+0.071</SUP> <SUB>-0.084</SUB> R <SUB>sun</SUB>. We estimate
  the planet mass and radius to be {M <SUB>P</SUB>, R <SUB>P</SUB>} =
  {24.5 ± 3.8 M <SUB>⊕</SUB>, 3.99 ± 0.21 R <SUB>⊕</SUB>}. The
  planet's density is near 1.9 g cm<SUP>-3</SUP> it is thus slightly
  denser and more massive than Neptune, but about the same size. <P
  />Some of the data presented herein were obtained at the W. M. Keck
  Observatory, which is operated as a scientific partnership among the
  California Institute of Technology, the University of California,
  and the National Aeronautics and Space Administration. The Observatory
  was made possible by the generous financial support of the W. M. Keck
  Foundation.

Title: Discovery of a Red Giant with Solar-like Oscillations in an
    Eclipsing Binary System from Kepler Space-based Photometry
Authors: Hekker, S.; Debosscher, J.; Huber, D.; Hidas, M. G.; De
   Ridder, J.; Aerts, C.; Stello, D.; Bedding, T. R.; Gilliland, R. L.;
   Christensen-Dalsgaard, J.; Brown, T. M.; Kjeldsen, H.; Borucki, W. J.;
   Koch, D.; Jenkins, J. M.; Van Winckel, H.; Beck, P. G.; Blomme,
   J.; Southworth, J.; Pigulski, A.; Chaplin, W. J.; Elsworth, Y. P.;
   Stevens, I. R.; Dreizler, S.; Kurtz, D. W.; Maceroni, C.; Cardini,
   D.; Derekas, A.; Suran, M. D.
Bibcode: 2010ApJ...713L.187H
Altcode: 2010arXiv1001.0399H
  Oscillating stars in binary systems are among the most interesting
  stellar laboratories, as these can provide information on the stellar
  parameters and stellar internal structures. Here we present a red
  giant with solar-like oscillations in an eclipsing binary observed
  with the NASA Kepler satellite. We compute stellar parameters of the
  red giant from spectra and the asteroseismic mass and radius from
  the oscillations. Although only one eclipse has been observed so far,
  we can already determine that the secondary is a main-sequence F star
  in an eccentric orbit with a semi-major axis larger than 0.5 AU and
  orbital period longer than 75 days.

Title: Selection, Prioritization, and Characteristics of Kepler
    Target Stars
Authors: Batalha, Natalie M.; Borucki, William J.; Koch, David G.;
   Bryson, Stephen T.; Haas, Michael. R.; Brown, Timothy M.; Caldwell,
   Douglas A.; Hall, Jennifer R.; Gilliland, Ronald L.; Latham, David W.;
   Meibom, Soren; Monet, David G.
Bibcode: 2010ApJ...713L.109B
Altcode: 2010arXiv1001.0349B
  The Kepler Mission began its 3.5 year photometric monitoring campaign in
  2009 May on a select group of approximately 150,000 stars. The stars
  were chosen from the ~ half million in the field of view that are
  brighter than 16th magnitude. The selection criteria are quantitative
  metrics designed to optimize the scientific yield of the mission
  with regard to the detection of Earth-size planets in the habitable
  zone. This yields more than 90,000 G-type stars on or close to the main
  sequence, &gt;20, 000 of which are brighter than 14th magnitude. At the
  temperature extremes, the sample includes approximately 3000 M-type
  dwarfs and a small sample of O- and B-type MS stars (&lt;200). The
  small numbers of giants are included in the sample: ~5000 stars with
  surface gravities log(g) &lt; 3.5. We present a brief summary of the
  selection process and the stellar populations it yields in terms of
  surface gravity, effective temperature, and apparent magnitude. In
  addition to the primary, statistically derived target set, several
  ancillary target lists were manually generated to enhance the science
  of the mission, examples being: known eclipsing binaries, open cluster
  members, and high proper motion stars.

Title: Kepler Mission Design, Realized Photometric Performance,
    and Early Science
Authors: Koch, David G.; Borucki, William J.; Basri, Gibor;
   Batalha, Natalie M.; Brown, Timothy M.; Caldwell, Douglas;
   Christensen-Dalsgaard, Jørgen; Cochran, William D.; DeVore, Edna;
   Dunham, Edward W.; Gautier, Thomas N., III; Geary, John C.; Gilliland,
   Ronald L.; Gould, Alan; Jenkins, Jon; Kondo, Yoji; Latham, David W.;
   Lissauer, Jack J.; Marcy, Geoffrey; Monet, David; Sasselov, Dimitar;
   Boss, Alan; Brownlee, Donald; Caldwell, John; Dupree, Andrea K.;
   Howell, Steve B.; Kjeldsen, Hans; Meibom, Søren; Morrison, David;
   Owen, Tobias; Reitsema, Harold; Tarter, Jill; Bryson, Stephen T.;
   Dotson, Jessie L.; Gazis, Paul; Haas, Michael R.; Kolodziejczak,
   Jeffrey; Rowe, Jason F.; Van Cleve, Jeffrey E.; Allen, Christopher;
   Chandrasekaran, Hema; Clarke, Bruce D.; Li, Jie; Quintana, Elisa V.;
   Tenenbaum, Peter; Twicken, Joseph D.; Wu, Hayley
Bibcode: 2010ApJ...713L..79K
Altcode: 2010arXiv1001.0268K
  The Kepler Mission, launched on 2009 March 6, was designed with the
  explicit capability to detect Earth-size planets in the habitable zone
  of solar-like stars using the transit photometry method. Results from
  just 43 days of data along with ground-based follow-up observations
  have identified five new transiting planets with measurements of their
  masses, radii, and orbital periods. Many aspects of stellar astrophysics
  also benefit from the unique, precise, extended, and nearly continuous
  data set for a large number and variety of stars. Early results for
  classical variables and eclipsing stars show great promise. To fully
  understand the methodology, processes, and eventually the results from
  the mission, we present the underlying rationale that ultimately led
  to the flight and ground system designs used to achieve the exquisite
  photometric performance. As an example of the initial photometric
  results, we present variability measurements that can be used to
  distinguish dwarf stars from red giants.

Title: VizieR Online Data Catalog: The Lick AGN monitoring project
    (Walsh+, 2009)
Authors: Walsh, J. L.; Minezaki, T.; Bentz, M. C.; Barth, A. J.;
   Baliber, N.; Li, W.; Stern, D.; Bennert, V. N.; Brown, T. M.; Canalizo,
   G.; Filippenko, A. V.; Gates, E. L.; Greene, J. E.; Malkan, M. A.;
   Sakata, Y.; Street, R. A.; Treu, T.; Woo, J. -H.; Yoshii, Y.
Bibcode: 2010yCat..21850156W
Altcode:
  The Lick AGN Monitoring Project targeted 13 nearby Seyfert 1
  galaxies with the intent of measuring the masses of their central
  black holes using reverberation mapping. The sample includes 12
  galaxies selected to have black holes with masses roughly in the range
  106<SUP>-107</SUP>M<SUB>⊙</SUB>, as well as the well-studied active
  galactic nucleus (AGN) NGC 5548. In conjunction with a spectroscopic
  monitoring campaign, we obtained broadband B and V images on most
  nights from 2008 February through 2008 May. The imaging observations
  were carried out by four telescopes: the 0.76m Katzman Automatic
  Imaging Telescope, the 2m Multicolor Active Galactic Nuclei Monitoring
  telescope, the Palomar 60 inch (1.5m) telescope, and the 0.80m Tenagra
  II telescope. Having well-sampled light curves over the course of a
  few months is useful for obtaining the broad-line reverberation lag and
  black hole mass, and also allows us to examine the characteristics of
  the continuum variability. In this paper, we discuss the observational
  methods and the photometric measurements, and present the AGN continuum
  light curves. We measure various variability characteristics of each
  of the light curves. We do not detect any evidence for a time lag
  between the B- and V-band variations, and we do not find significant
  color variations for the AGNs in our sample. <P />(2 data files).

Title: VizieR Online Data Catalog: Deep optical photometry in M31
    (Brown+, 2009)
Authors: Brown, T. M.; Smith, E.; Ferguson, H. C.; Guhathakurta, P.;
   Kalirai, J. S.; Kimble, R. A.; Renzini, A.; Rich, R. M.; Sweigart,
   A. V.; Vandenberg, D. A.
Bibcode: 2010yCat..21840152B
Altcode:
  Images were obtained using the Wide Field Camera on the ACS, in the
  F606W (broad V) and F814W (I) filters. The characteristics of the six
  fields observed are summarized in Table 1. <P />(7 data files).

Title: Kepler Asteroseismology Program: Introduction and First Results
Authors: Gilliland, Ronald L.; Brown, Timothy M.;
   Christensen-Dalsgaard, Jørgen; Kjeldsen, Hans; Aerts, Conny;
   Appourchaux, Thierry; Basu, Sarbani; Bedding, Timothy R.; Chaplin,
   William J.; Cunha, Margarida S.; De Cat, Peter; De Ridder, Joris;
   Guzik, Joyce A.; Handler, Gerald; Kawaler, Steven; Kiss, László;
   Kolenberg, Katrien; Kurtz, Donald W.; Metcalfe, Travis S.; Monteiro,
   Mario J. P. F. G.; Szabó, Robert; Arentoft, Torben; Balona, Luis;
   Debosscher, Jonas; Elsworth, Yvonne P.; Quirion, Pierre-Olivier;
   Stello, Dennis; Suárez, Juan Carlos; Borucki, William J.; Jenkins,
   Jon M.; Koch, David; Kondo, Yoji; Latham, David W.; Rowe, Jason F.;
   Steffen, Jason H.
Bibcode: 2010PASP..122..131G
Altcode: 2010arXiv1001.0139G
  Asteroseismology involves probing the interiors of stars and quantifying
  their global properties, such as radius and age, through observations of
  normal modes of oscillation. The technical requirements for conducting
  asteroseismology include ultrahigh precision measured in photometry
  in parts per million, as well as nearly continuous time series over
  weeks to years, and cadences rapid enough to sample oscillations with
  periods as short as a few minutes. We report on results from the first
  43 days of observations, in which the unique capabilities of Kepler
  in providing a revolutionary advance in asteroseismology are already
  well in evidence. The Kepler asteroseismology program holds intrinsic
  importance in supporting the core planetary search program through
  greatly enhanced knowledge of host star properties, and extends well
  beyond this to rich applications in stellar astrophysics.

Title: Kepler Planet-Detection Mission: Introduction and First Results
Authors: Borucki, William J.; Koch, David; Basri, Gibor; Batalha,
   Natalie; Brown, Timothy; Caldwell, Douglas; Caldwell, John;
   Christensen-Dalsgaard, Jørgen; Cochran, William D.; DeVore, Edna;
   Dunham, Edward W.; Dupree, Andrea K.; Gautier, Thomas N.; Geary, John
   C.; Gilliland, Ronald; Gould, Alan; Howell, Steve B.; Jenkins, Jon M.;
   Kondo, Yoji; Latham, David W.; Marcy, Geoffrey W.; Meibom, Søren;
   Kjeldsen, Hans; Lissauer, Jack J.; Monet, David G.; Morrison, David;
   Sasselov, Dimitar; Tarter, Jill; Boss, Alan; Brownlee, Don; Owen,
   Toby; Buzasi, Derek; Charbonneau, David; Doyle, Laurance; Fortney,
   Jonathan; Ford, Eric B.; Holman, Matthew J.; Seager, Sara; Steffen,
   Jason H.; Welsh, William F.; Rowe, Jason; Anderson, Howard; Buchhave,
   Lars; Ciardi, David; Walkowicz, Lucianne; Sherry, William; Horch,
   Elliott; Isaacson, Howard; Everett, Mark E.; Fischer, Debra; Torres,
   Guillermo; Johnson, John Asher; Endl, Michael; MacQueen, Phillip;
   Bryson, Stephen T.; Dotson, Jessie; Haas, Michael; Kolodziejczak,
   Jeffrey; Van Cleve, Jeffrey; Chandrasekaran, Hema; Twicken, Joseph
   D.; Quintana, Elisa V.; Clarke, Bruce D.; Allen, Christopher; Li,
   Jie; Wu, Haley; Tenenbaum, Peter; Verner, Ekaterina; Bruhweiler,
   Frederick; Barnes, Jason; Prsa, Andrej
Bibcode: 2010Sci...327..977B
Altcode:
  The Kepler mission was designed to determine the frequency of
  Earth-sized planets in and near the habitable zone of Sun-like
  stars. The habitable zone is the region where planetary temperatures
  are suitable for water to exist on a planet’s surface. During the
  first 6 weeks of observations, Kepler monitored 156,000 stars, and
  five new exoplanets with sizes between 0.37 and 1.6 Jupiter radii and
  orbital periods from 3.2 to 4.9 days were discovered. The density of
  the Neptune-sized Kepler-4b is similar to that of Neptune and GJ 436b,
  even though the irradiation level is 800,000 times higher. Kepler-7b
  is one of the lowest-density planets (~0.17 gram per cubic centimeter)
  yet detected. Kepler-5b, -6b, and -8b confirm the existence of planets
  with densities lower than those predicted for gas giant planets.

Title: Transiting Exoplanet Survey Satellite (TESS)
Authors: Ricker, George R.; Latham, D. W.; Vanderspek, R. K.; Ennico,
   K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau,
   D.; Clampin, M.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot,
   J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai,
   N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.;
   Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.; Villasenor, J. N.;
   Winn, J. N.; Worden, S. P.
Bibcode: 2010AAS...21545006R
Altcode: 2010BAAS...42..459R
  TESS is a low-cost SMEX-class satellite mission. In a two-year all-sky
  survey, TESS will observe more than 2,000,000 nearby stars, searching
  for temporary drops in brightness caused by planetary transits. <P
  />TESS is expected to identify more than 1000 transiting exoplanet
  candidates, including a sample of about 100 Super Earths---small
  rock-and-ice planets in the range 1 to 10 Earth masses---orbiting F,
  G, K, and M dwarfs. TESS's "wide-shallow” survey complements the
  "narrow-deep” CoRoT and Kepler surveys. TESS-discovered transiting
  systems will be nearby (&lt; 50 pc), and typically 10-20 x brighter than
  those discovered by CoRoT and Kepler. Thus, the resulting TESS Transit
  Catalog will comprise all of the best transiting systems for follow-up
  observations. TESS will identify Super Earths orbiting IR-bright stars,
  within reach of JWST spectroscopic searches for planetary water and
  carbon dioxide. <P />TESS is a collaborative effort led by researchers
  at the Massachusetts Institute of Technology, the Harvard-Smithsonian
  Center for Astrophysics, and the NASA Ames Research Center. Additional
  TESS scientific partners include Las Cumbres Observatory Global
  Telescope, Lowell Observatory, the NASA Goddard Space Flight Center,
  the Infrared Processing and Analysis Center at the California Institute
  of Technology, the Geneva Observatory (Switzerland), the Tokyo Institute
  of Technology (Japan), and Institut Supérieur de l'Aéronautique et
  de l'Espace (France). <P />TESS was funded by NASA for a Phase A study
  from May 2008 - June 2009, but was not selected for flight. Additional
  funding leading to a flight opportunity is being sought. Support has
  also been provided by the Kavli Foundation, Google, and the Smithsonian
  Institution. TESS could launch as early as 2013-2014.

Title: Radii of Rapidly Rotating Stars, with Application to
    Transiting-Planet Hosts
Authors: Brown, Timothy M.
Bibcode: 2010ApJ...709..535B
Altcode: 2009arXiv0912.1639B
  The currently favored method for estimating radii and other parameters
  of transiting-planet host stars is to match theoretical models to
  observations of the stellar mean density ρ<SUB>*</SUB>, the effective
  temperature T <SUB>eff</SUB>, and the composition parameter [Z]. This
  explicitly model-dependent approach is based on readily available
  observations, and results in small formal errors. Its performance
  will be central to the reliability of results from ground-based
  transit surveys such as TrES, HAT, and SuperWASP, as well as to
  the space-borne missions MOST, CoRoT, and Kepler. Here, I use two
  calibration samples of stars (eclipsing binaries (EBs) and stars for
  which asteroseismic analyses are available) having well-determined
  masses and radii to estimate the accuracy and systematic errors
  inherent in the ρ<SUB>*</SUB> method. When matching to the Yonsei-Yale
  stellar evolution models, I find the most important systematic error
  results from selection bias favoring rapidly rotating (hence probably
  magnetically active) stars among the EB sample. If unaccounted for,
  this bias leads to a mass-dependent underestimate of stellar radii
  by as much as 4% for stars of 0.4 M <SUB>sun</SUB>, decreasing to
  zero for masses above about 1.4 M <SUB>sun</SUB>. Relative errors
  in estimated stellar masses are three times larger than those in
  radii. The asteroseismic sample suggests (albeit with significant
  uncertainty) that systematic errors are small for slowly rotating,
  inactive stars. Systematic errors arising from failings of the
  Yonsei-Yale models of inactive stars probably exist, but are difficult
  to assess because of the small number of well-characterized comparison
  stars having low mass and slow rotation. Poor information about [Z]
  is an important source of random error, and may be a minor source of
  systematic error as well. With suitable corrections for rotation, it
  is likely that systematic errors in the ρ<SUB>*</SUB> method can be
  comparable to or smaller than the random errors, yielding radii that
  are accurate to about 2% for most stars.

Title: The Kepler Mission and Early Results
Authors: Koch, David; Borucki, William; Jenkins, Jon; Basri,
   Gibor; Batalha, Natalie M.; Brown, Timothy M.; Caldwell, Douglas;
   Christensen-Dalsgaard, Jørgen; Cochran, William D.; Devore, Edna;
   Dunham, Edward W.; Gautier, Thomas N., III; Geary, John C.; Gilliland,
   Ronald L.; Gould, Alan; Jenkins, Jon; Latham, David W.; Lissauer,
   Jack J.; Marcy, Geoffrey; Monet, David; Sasselov, Dimitar; Boss, Alan;
   Caldwell, John; Dupree, Andrea K.; Howell, Steve B.; Kjeldsen, Hans;
   Meibom, Søren; Morrison, David; Tarter, Jill; Bryson, Stephen T.;
   Dotson, Jessie L.; Haas, Michael R.; Kolodziejczak, Jeffrey; Rowe,
   Jason F.; van Cleve, Jeffrey E.; Buzasi, Derek; Charbonneau, David;
   Doyle, Lau-Rance; Ford, Eric; Fortney, Jonathan; Holman, Matthew;
   Seager, Sara; Steffen, Jason; Welsh, William
Bibcode: 2010cosp...38.2513K
Altcode: 2010cosp.meet.2513K
  Kepler is a Discovery-class mission designed to determine the frequency
  of Earth-size planets in and near the habitable zone of solar-like
  stars. The instrument consists of a 0.95 m aperture photometer designed
  to obtain high-precision photometric measurement for more than 3.5
  years of more than 100,000 stars to search for patterns of transits
  of exoplanets. The focal plane of the Schmidt telescope contains 42
  CCDs with a total of 95 megapixels that cover 115 square degrees of
  sky. The single star field will be viewed for the entire duration
  of the mission. The photometer was launched into an Earth-trailing
  heliocentric orbit on March 6, 2009, finished its commissioning on May
  12, and is now in the science operations mode. The bases for a number of
  the design choices are described. Although the data have not yet been
  fully corrected for the presence of systematic errors and artifacts,
  the data show the presence of thousands of eclipsing binaries and
  variable stars of amazing variety. The character of stellar variability
  allows us to distinguish dwarf stars from giants. Astrometric stability
  at the sub-millipixel level of the photocenters of stars allows us in
  many cases to distinguish transit candidates from background eclipsing
  binaries. Analysis of the early data shows transits, occultations and
  even visible light emission from the hot exoplanet HAT-P-7b. The latest
  results on exoplanet detections from Kepler will be presented. Funding
  for this mission is provided by NASA's Science Mission Directorate.

Title: The Kepler Short Cadence Data and Applications for
    Asteroseismology and Transit Light Curves
Authors: Gilliland, Ronald L.; Brown, T. M.; Christensen-Dalsgaard,
   J.; Kjeldsen, H.; Borucki, W. J.; Bryson, S.; Caldwell, D. A.; Jenkins,
   J. M.; Koch, D.; Kepler Team
Bibcode: 2010AAS...21530504G
Altcode: 2010BAAS...42..302G
  The Kepler data acquisition allows 512 targets to be followed in a
  'short cadence' mode with roughly 1-minute integrations as needed for
  asteroseismology of solar analogs having p-mode oscillations of a few
  minutes, and to study fine details of high S/N transits. Characteristics
  of these data will be described. An application of asteroseismology in
  support of the core Kepler mission of characterizing detected planets
  follows from stellar radius determinations needed to in turn provide
  radii for the planets. The steps from processing of Kepler short cadence
  data, derivation of asteroseismic frequencies from power spectra of
  these time series, constraint on the mean stellar density and ultimately
  stellar radius will be illustrated for a few planet host stars yielding
  radii to accuracies approaching 1%. Analysis of individual oscillation
  frequencies will provide information about the properties of stellar
  interiors, resulting in some cases in determinations of ages to about
  10%. Asteroseismic results will ultimately be expected for several
  thousand stars ranging from the solar analog oscillations mentioned
  above, to oscillations in red giants and a full spectrum of classical
  variable stars (both at short, and the 30-minute long cadence) including
  delta Scuti, RR Lyrae, RoAp stars etc. <P />Kepler was selected as
  the 10th mission of the Discovery Program. Funding for this mission
  is provided by NASA, Science Mission Directorate.

Title: Estimates of the Population of Exoplanets Discoverable by
    the Transiting Exoplanet Survey Satellite (TESS)
Authors: Seager, Sara; Winn, J. N.; Ricker, G. R.; Latham, D. W.;
   Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.; Burgasser,
   A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.; Doty, J. P.;
   Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins,
   J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.;
   Martel, F.; Sasselov, D. D.; Schingler, R. H.; Torres, G.; Udry, S.;
   Villasenor, J. N.; Worden, S. P.
Bibcode: 2010AAS...21545004S
Altcode: 2010BAAS...42R.458S
  In a two year survey, the Transiting Exoplanet Survey Satellite
  (TESS) will search the entire sky for planets orbiting nearby,
  bright stars. In this paper, we calculate the number of transiting
  planets that TESS will detect, as a function of the properties of the
  planet and the properties of the host star. The ingredients in this
  calculation are divided into five groups: <P />The properties of the
  planet: its radius r and orbital distance a. <P />The properties of
  the star: its luminosity L, mass M, radius R, and number density n in
  our Galactic neighborhood. <P />The TESS instrumental parameters: its
  effective area, bandpass, and limiting photometric precision. <P />The
  TESS survey parameters: the characteristics of the input catalog (2.5
  million V &lt; 13.5 dwarfs over the whole sky), observing duty cycle
  (observing a given star 10.3% of the time), and duration of observations
  for a given star (72 days). <P />The abundance of planets around stars,
  which may depend on r, a, and L <P />The calculation is performed for
  a three-dimensional grid of planet/star/orbit combinations, in which
  the three parameters are the planet radius r, the stellar luminosity L,
  and the orbital distance a. For the range of instrument and population
  parameters and assumptions considered, we estimate that TESS will detect
  1600-2700 planets in total, of which 100-300 should be small planets:
  SuperEarths or Earths. <P />Support for this work has been provided
  by NASA, the Kavli Foundation, Google, and the Smithsonian Institution.

Title: Monte Carlo Simulations of Transit Light Curves for the
    Transiting Exoplanet Survey Satellite (TESS)
Authors: Jernigan, J. G.; Villasenor, J. N.; Ricker, G. R.; Latham,
   D. W.; Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.;
   Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.;
   Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.;
   Jenkins, J. M.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel,
   F.; Sasselov, D. D.; Schingler, R. H.; Seager, S.; Torres, G.; Udry,
   S.; Winn, J. N.; Worden, S. P.
Bibcode: 2010AAS...21545003J
Altcode: 2010BAAS...42..458J
  During the Phase A for TESS, simulations of planetary transits were
  performed to confirm the instrument's ability to detect transits. The
  simulations cover the full TESS discovery space in the planet
  period-transit duration plane. Examples included a 36-day period planet,
  two previously known systems (HAT-P-11 and CoRoT 7B), and one Earth
  and one SuperEarth. In addition, a broad matrix of planetary periods
  and transit depths were also simulated. We present simulated light
  curves of transiting planets that are typical of those that TESS will
  detect. Each light curve is computed via a Monte Carlo algorithm. The
  timing of the optical emission includes the parameters of orbital
  motion for the planet-star system. All simulations include estimates
  of the noise from the following effects: spacecraft pointing jitter,
  vignetting, optical PSF wings, background effects, CCD gain and bias
  instability, sky background, and intrinsic stellar variability. The
  stellar variability includes a scaled, full temporal power spectrum
  of the Sun. Typical light curves of planet-star systems are simulated
  for a 72 day duration with a 10 minute time resolution of each TESS
  sample. These simulated light curves are analyzed to determine estimates
  of the S/N for detection for each simulated system. Support for this
  work has been provided by NASA, the Kavli Foundation, Google, and the
  Smithsonian Institution.

Title: High-Precision Imaging Photometers for the Transient Exoplanet
    Survey Satellite
Authors: Kraft Vanderspek, Roland; Ricker, G. R.; Latham, D. W.;
   Ennico, K.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau,
   D.; Clampin, M.; Deming, L.; Doty, J. P.; Dunham, E. W.; Elliot,
   J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.;
   Kawai, N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov,
   D. D.; Schingler, R. H.; Seager, S.; Szentgyorgyi, A.; Torres, G.;
   Udry, S.; Villasenor, J. N.; Winn, J. N.; Worden, S. P.
Bibcode: 2010AAS...21545007K
Altcode: 2010BAAS...42..459K
  The Transient Exoplanet Survey Satellite (TESS) is designed to
  search for transiting exoplanet systems around all stars with V &lt;
  12. The TESS payload consists of a bank of six identical, wide-field,
  high-precision imaging photometers. When deployed on the highly-stable
  TESS satellite platform, these photometers can perform &lt;200 ppm
  photometry for V=8 stars (∼100 ppm for V=6 stars) in a 10-minute
  observation. We describe the components of the TESS imaging photometers:
  the custom, wide-field optics; the large-area CCD arrays; and the
  low-power, high precision CCD electronics. Support for TESS has been
  provided by NASA, the Kavli Foundation, Google, and the Smithsonian
  Institution.

Title: Characteristics of the Kepler Target Stars
Authors: Batalha, Natalie M.; Borucki, W. J.; Koch, D. G.; Brown,
   T. M.; Bryson, S. T.; Caldwell, D. A.; Gilliland, R. L.; Latham,
   D. W.; Meibom, S.; Monet, D. G.; Kepler Team
Bibcode: 2010AAS...21530506B
Altcode: 2010BAAS...42Q.303B
  In May, 2009, the Kepler spacecraft began its 3.5-year photometric
  monitoring campaign on a select group of approximately 150,000
  stars. The stars were chosen from the ∼half million in the field of
  view that are brighter than 16th magnitude. The selection criteria
  are quantitative metrics designed to optimize the scientific yield
  of the mission with regards to the detection of earth-size planets
  in the habitable zone. This yields more than 90,000 G-type stars
  on or close to the Main Sequence, ∼20,000 of which are brighter
  than 14th magnitude. At the temperature extremes, the sample includes
  approximately 3,000 M-type dwarfs and a small sample of O and B-type MS
  stars (&lt; 200). The brightest giants are captured in the sample with
  ∼16,000 stars with surface gravities less than 3.5 dex. We present a
  brief summary of the selection process and the stellar populations it
  yields in terms of surface gravity, effective temperature, and apparent
  magnitude. In addition to the primary, statistically derived, target
  set, several ancillary target lists were manually generated to enhance
  the science of the mission, examples being: known eclipsing binaries,
  open cluster members, and high proper-motion stars. To highlight
  the stellar sample, we present light curves from the first months of
  science operations of the twenty brightest G, K, and M dwarfs as well
  as a direct comparison with the solar irradiance variations at maximum
  and minimum activity levels. This cursory look at the data suggests that
  stars as photometrically quiet as the Sun are not a rarity. <P />Kepler
  was selected as the 10th mission of the Discovery Program. Funding
  for this mission is provided by NASA, Science Mission Directorate.

Title: Data Network for the TESS Mission
Authors: Martel, Francois; Villasenor, J. N.; Ricker, G. R.; Latham,
   D. W.; Vanderspek, R. K.; Ennico, K. A.; Bakos, G.; Brown, T. M.;
   Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming, L. D.; Doty,
   J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida, S.; Jenkins,
   J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.; Lissauer, J. J.;
   Sasselov, D. D.; Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.;
   Winn, J. N.; Worden, S. P.
Bibcode: 2010AAS...21545002M
Altcode: 2010BAAS...42..458M
  The Transiting Exoplanet Survey Satellite (TESS) is designed for an
  all-sky photometric survey of bright stars, extending&amp;nbspover the
  entire celestial sphere.&amp;nbspTESS will catalog planetary transits
  of nearby stars that can be followed-up with ground observatories. The
  satellite cameras will perform measurements of 2,500,000 stars with
  brightness ranging from V=4.5 to V=13.5 within two years, and download
  typically 4.7 G Bytes of data per day.&amp;nbspWe describe the TESS
  operation plan and the communication and ground system designed to
  download and process the TESS data. The dedicated ground system uses
  a network of S-band ground stations spaced around the equator which
  allows three communications passes per orbit, at data rates of 3.5
  Mbit/sec, for up to 45 data downloads per day. Satellite operations
  and data download are controlled remotely through the internet by
  the TESS Mission Operation Center at NASA Ames Research Center, which
  transfers the TESS observation data for processing and distribution to
  the Science Operation Center managed by &amp;nbspMIT and Harvard-SAO
  in Cambridge. Support for this work has been provided by NASA, the
  Kavli Foundation, Google, and the Smithsonian Institution.

Title: Transiting Exoplanet Survey Satellite (TESS) Community Observer
    Program including the Science Enhancement Option Box (SEO Box) -
    12 TB On-board Flash Memory for Serendipitous Science
Authors: Schingler, Robert; Villasenor, J. N.; Ricker, G. R.; Latham,
   D. W.; Vanderspek, R. K.; Ennico, K. A.; Lewis, B. S.; Bakos, G.;
   Brown, T. M.; Burgasser, A. J.; Charbonneau, D.; Clampin, M.; Deming,
   L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman, M. J.; Ida,
   S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin, G. P.;
   Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Seager, S.; Torres,
   G.; Udry, S.; Winn, J. N.; Worden, S. P.
Bibcode: 2010AAS...21545001S
Altcode: 2010BAAS...42Q.458S
  The Transiting Exoplanet Survey Satellite (TESS) will perform an
  all-sky survey in a low-inclination, low-Earth orbit. TESS's 144
  GB of raw data collected each orbit will be stacked, cleaned, cut,
  compressed and downloaded. The Community Observer Program is a Science
  Enhancement Option (SEO) that takes advantage of the low-radiation
  environment, technology advances in flash memory, and the vast amount
  of astronomical data collected by TESS. The Community Observer Program
  requires the addition of a 12 TB "SEO Box” inside the TESS Bus. The
  hardware can be built using low-cost Commercial Off-The-Shelf (COTS)
  components and fits within TESS's margins while accommodating GSFC
  gold rules. <P />The SEO Box collects and stores a duplicate of the
  TESS camera data at a "raw” stage ( 4.3 GB/orbit, after stacking and
  cleaning) and makes them available for on-board processing. The sheer
  amount of onboard storage provided by the SEO Box allows the stacking
  and storing of several months of data, allowing the investigator
  to probe deeper in time prior to a given event. Additionally, with
  computation power and data in standard formats, investigators can
  utilize data-mining techniques to investigate serendipitous phenomenon,
  including pulsating stars, eclipsing binaries, supernovae or other
  transient phenomena. <P />The Community Observer Program enables ad-hoc
  teams of citizen scientists to propose, test, refine and rank algorithms
  for on-board analysis to support serendipitous science. Combining
  "best practices” of online collaboration, with careful moderation
  and community management, enables this `crowd sourced’ participatory
  exploration with a minimal risk and impact on the core TESS Team. This
  system provides a powerful and independent tool opening a wide range of
  opportunity for science enhancement and secondary science. <P />Support
  for this work has been provided by NASA, the Kavli Foundation, Google,
  and the Smithsonian Institution.

Title: HST/ACS Observations of RR Lyrae Stars in Six Ultra-deep
    Fields of M31
Authors: Jeffery, Elizabeth; Brown, T. M.; Smith, E.; Ferguson, H. C.;
   Guhathakurta, P.; Kalirai, J. S.; Kimble, R. A.; Renzini, A.; Rich,
   R. M.; Sweigart, A. V.; VandenBerg, D. A.
Bibcode: 2010AAS...21541713J
Altcode: 2010BAAS...42..273J
  We present HST/ACS observations of RR Lyrae variable stars obtained
  in ultra-deep observations of the Andromeda galaxy (M31). These
  observations probe the disk, giant stellar stream, and several halo
  fields with distinct star formation histories. Earlier RR Lyrae data
  from this series of observing programs have probed various aspects
  of the populations that make up Andromeda's inner halo, including
  distances and metallicities. The current study builds and expands
  on that earlier work, investigating a sample of substructures and
  environments that is much more diverse. The quality of the light curves
  is akin to that usually associated with RR Lyrae stars of the Milky Way,
  both in terms of photometric accuracy and time series sampling. These
  data will provide additional insights into the stellar populations
  with techniques that are independent of the traditional fitting of
  color-magnitude diagrams.

Title: WFC3: The Photometric Performance Of The UVIS And IR Cameras
Authors: Borders, Tiffany M.; Kalirai, J.; Brown, T. M.; Deustua,
   S.; Rajan, A.; Riess, A.; WFC3 Team
Bibcode: 2010AAS...21546313B
Altcode: 2010BAAS...42S.496B
  The on-orbit throughput of WFC3 has been measured by observing bright
  spectrophotometric standard stars during SMOV4. For the UVIS channel,
  we observed the hot white dwarf GD 153 in 37 of 62 filters, and on
  the IR channel we observed both GD 153 and the solar analogue P330 in
  all 15 filters. Repeat measurements, at multiple dither positions,
  confirm that the throughput of both cameras is stable to &lt;1% in
  wide and medium band filters. Relative to the calibrations determined
  during ground tests in Thermal Vacuum Test #3, the instrument is
  performing more efficiently in all filters. For the UVIS channel,
  we measure efficiencies that are higher than ground tests by 15-20%
  at central wavelengths and 5-10% at the blue and red ends of the UVIS
  spectral range. For the IR channel, the instrument throughput is 10-15%
  higher in all filters. New photometric zero points have been calculated,
  and updates to the exposure time calculator have been implemented.

Title: WFC3: SMOV and Cycle 17 Calibration Programs
Authors: Deustua, Susana E.; MacKenty, J.; Kimble, R.; Martel,
   A. R.; Baggett, S.; Barker, E.; Borders, T.; Bushouse, H.; Brown,
   T. M.; Dressel, L.; Dulude, M.; Hartig, G.; Hilbert, B.; Kalirai, J.;
   Quijano, J. Kim; Kozhurina-Platais, V.; McLean, B.; McCullough, P.;
   Pavlovsky, C.; Petro, L.; Pirzkal, N.; Rajan, A.; Riess, A.; Sabbi,
   E.; Viana, A.; Wheeler, T.; Wong, M. H.; Kuemmel, M.; Kuntschner,
   H.; Walsh, J.; WFC3 Team
Bibcode: 2010AAS...21546319D
Altcode: 2010BAAS...42R.497D
  The Servicing Mission Observatory Verification (SMOV4) commissioning
  activities were carried out over 3 months following the installation
  of Wide Field Camera 3 (WFC3) into HST during Servicing Mission
  4. Following SMOV4, once WFC3 was enabled for routine science
  observations, the WFC3 Cycle 17 Calibration program began. Both
  SMOV4 and Cycle 17 calibration programs characterize the UVIS and IR
  channels, monitor their behavior with time, and provide the reference
  files used in the data reduction pipeline. Comprising 43 SMOV4 and 35
  Cycle 17 programs, the commissioning and calibration of WFC3 require
  approximately 400 orbits during its first 15 months on-orbit. This
  paper discusses the contents, rationale, and initial results of WFC3
  SMOV4 and Cycle 17 Calibration Programs. We also highlight some issues
  that may affect GO programs.

Title: Las Cumbres Observatory Global Telescope 1-meter Telescope
Project: Design, Deployment Plans, Status
Authors: Brown, Timothy M.; Burleson, B.; Crellin, M.; De Vera, J.;
   Dubberly, M.; Greene, R.; Falarski, M.; Haldeman, B.; Hausler, S.;
   Haynes, R.; Hjelstrom, A.; Hygelund, J.; Johnson, D.; Lobdill, R.;
   Martinez, J.; Mullins, D.; Pickles, A.; Posner, V.; Rosing, W.; Tufts,
   J.; Vander Horst, K.; Vanderhyden, B.; Walker, Z.
Bibcode: 2010AAS...21544106B
Altcode: 2010BAAS...42..401B
  Las Cumbres Observatory Global Telescope (LCOGT) is a privately-funded
  observatory dedicated to time-domain astronomy. Our main observing tool
  will be a homogeneous world-wide network of 12 x 1m optical telescopes,
  each equipped for both imaging and spectroscopy. Here we describe
  the LCOGT 1m telescope design, its development status, and our plans
  for deploying a dozen or so such telescopes in a worldwide network
  capable of continuous observing. We also describe the 80 cm Sedgwick
  telescope, which is now in regular operation as a research instrument,
  and which has served as a prototype for many of the 1m mechanical and
  control systems.

Title: The Star Formation Histories of the M31 and M33 Spheroids
Authors: Brown, T. M.
Bibcode: 2009ASPC..419..110B
Altcode: 2009arXiv0901.2577B
  I review the observational constraints on the star formation histories
  in the spheroids of M33 and M31, the other two spiral galaxies in the
  Local Group. M33 does not possess a traditional bulge; instead, it has a
  small nuclear region hosting stars with a wide range of ages. The star
  formation history of the M33 halo is poorly constrained, but composite
  spectra of its halo globular clusters imply a wide age spread of 5-7
  years, while the presence of RR Lyrae stars in the halo implies at least
  some of the population is ancient. Although it is possible to obtain the
  detailed star formation history of the M33 halo via deep photometry,
  this has not been done to date. M31 hosts a traditional bulge that is
  apparently dominated by stars older than 10 Gyr. Deep photometry of
  the M31 halo demonstrates that it hosts both a population of ancient
  metal-poor stars and a significant population extending to younger
  ages and high metallicity, apparently due to its active merger history.

Title: The Palomar Transient Factory: System Overview, Performance,
    and First Results
Authors: Law, Nicholas M.; Kulkarni, Shrinivas R.; Dekany, Richard G.;
   Ofek, Eran O.; Quimby, Robert M.; Nugent, Peter E.; Surace, Jason;
   Grillmair, Carl C.; Bloom, Joshua S.; Kasliwal, Mansi M.; Bildsten,
   Lars; Brown, Tim; Cenko, S. Bradley; Ciardi, David; Croner, Ernest;
   Djorgovski, S. George; van Eyken, Julian; Filippenko, Alexei V.;
   Fox, Derek B.; Gal-Yam, Avishay; Hale, David; Hamam, Nouhad; Helou,
   George; Henning, John; Howell, D. Andrew; Jacobsen, Janet; Laher,
   Russ; Mattingly, Sean; McKenna, Dan; Pickles, Andrew; Poznanski,
   Dovi; Rahmer, Gustavo; Rau, Arne; Rosing, Wayne; Shara, Michael;
   Smith, Roger; Starr, Dan; Sullivan, Mark; Velur, Viswa; Walters,
   Richard; Zolkower, Jeff
Bibcode: 2009PASP..121.1395L
Altcode: 2009arXiv0906.5350L
  The Palomar Transient Factory (PTF) is a fully-automated, wide-field
  survey aimed at a systematic exploration of the optical transient
  sky. The transient survey is performed using a new 8.1 square degree
  camera installed on the 48 inch Samuel Oschin telescope at Palomar
  Observatory; colors and light curves for detected transients are
  obtained with the automated Palomar 60 inch telescope. PTF uses 80%
  of the 1.2 m and 50% of the 1.5 m telescope time. With an exposure
  of 60 s the survey reaches a depth of m<SUB>g<SUP>‧</SUP></SUB>
  ≈ 21.3 and m<SUB>R</SUB> ≈ 20.6 (5σ, median seeing). Four major
  experiments are planned for the five-year project: (1) a 5 day cadence
  supernova search; (2) a rapid transient search with cadences between 90
  s and 1 day (3) a search for eclipsing binaries and transiting planets
  in Orion; and (4) a 3π sr deep H-alpha survey. PTF provides automatic,
  real-time transient classification and follow-up, as well as a database
  including every source detected in each frame. This paper summarizes
  the PTF project, including several months of on-sky performance tests
  of the new survey camera, the observing plans, and the data reduction
  strategy. We conclude by detailing the first 51 PTF optical transient
  detections, found in commissioning data.

Title: The Lick AGN Monitoring Project: Photometric Light Curves
    and Optical Variability Characteristics
Authors: Walsh, Jonelle L.; Minezaki, Takeo; Bentz, Misty C.; Barth,
   Aaron J.; Baliber, Nairn; Li, Weidong; Stern, Daniel; Bennert, Vardha
   Nicola; Brown, Timothy M.; Canalizo, Gabriela; Filippenko, Alexei V.;
   Gates, Elinor L.; Greene, Jenny E.; Malkan, Matthew A.; Sakata, Yu;
   Street, Rachel A.; Treu, Tommaso; Woo, Jong-Hak; Yoshii, Yuzuru
Bibcode: 2009ApJS..185..156W
Altcode: 2009arXiv0909.5455W
  The Lick AGN Monitoring Project targeted 13 nearby Seyfert 1
  galaxies with the intent of measuring the masses of their central
  black holes using reverberation mapping. The sample includes 12
  galaxies selected to have black holes with masses roughly in the
  range 10<SUP>6</SUP>-10<SUP>7</SUP> M <SUB>sun</SUB>, as well as the
  well-studied active galactic nucleus (AGN) NGC 5548. In conjunction
  with a spectroscopic monitoring campaign, we obtained broadband B
  and V images on most nights from 2008 February through 2008 May. The
  imaging observations were carried out by four telescopes: the 0.76 m
  Katzman Automatic Imaging Telescope, the 2 m Multicolor Active Galactic
  Nuclei Monitoring telescope, the Palomar 60 inch (1.5 m) telescope,
  and the 0.80 m Tenagra II telescope. Having well-sampled light curves
  over the course of a few months is useful for obtaining the broad-line
  reverberation lag and black hole mass, and also allows us to examine
  the characteristics of the continuum variability. In this paper, we
  discuss the observational methods and the photometric measurements, and
  present the AGN continuum light curves. We measure various variability
  characteristics of each of the light curves. We do not detect any
  evidence for a time lag between the B- and V-band variations, and we
  do not find significant color variations for the AGNs in our sample.

Title: The Kepler mission
Authors: Christensen-Dalsgaard, J.; Arentoft, T.; Brown, T. M.;
   Gilliland, R. L.; Kjeldsen, H.; Borucki, W. J.; Koch, D.
Bibcode: 2009CoAst.158..328C
Altcode:
  The Kepler mission will provide a vast improvement in the
  characterization of extrasolar planetary systems, and in addition give
  a dramatic increase in the data available for asteroseismology. The
  present paper gives a brief overview of the mission, emphasizing
  the asteroseismic aspects, and with references to more detailed
  presentations.

Title: Las Cumbres Observatory Global Telescope
Authors: Brown, Timothy M.; Rosing, W.; Pickles, A.; Howell, D. A.
Bibcode: 2009AAS...21440914B
Altcode:
  Las Cumbres Observatory Global Telescope (LCOGT) is a privately-funded
  observatory dedicated to time-domain astronomy. Our main observing
  tool will be a homogeneous world-wide network of 12 x 1m optical
  telescopes, each equipped for both imaging and spectroscopy. We will
  also continue to operate 2m telscopes in Hawaii and Australia, and we
  plan to deploy a few tens of 0.4m imaging telescopes for education and
  for bright-object research. LCOGT has membership in the Pan-STARRS1
  consortium, in the Palomar Transient Factory (PTF), and in LSST. In
  accord with these affiliations, our staff's scientific interests are
  concentrated in (but not restricted to) the areas of extrasolar planets,
  extragalactic transients (especially SNe), and pulsating stars. <P />In
  this poster we describe the observatory in general terms, including
  its research agenda, its telescope deployment plans and schedule, its
  notable technical challenges, and its anticipated methods of working
  with the wider astronomical community. For more detailed information
  about LCOGT's aims and projects, please see the related posters in
  this session.

Title: Transiting Exoplanet Survey Satellite (TESS)
Authors: Ricker, George R.; Latham, D. W.; Vanderspek, R. K.; Ennico,
   K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau,
   D.; Clampin, M.; Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot,
   J. L.; Holman, M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai,
   N.; Laughlin, G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.;
   Schingler, R. H.; Seager, S.; Torres, G.; Udry, S.; Villasenor, J. S.;
   Winn, J. N.; Worden, S. P.
Bibcode: 2009AAS...21430605R
Altcode:
  The Transiting Exoplanet Survey Satellite (TESS) is a low
  cost, SMEX-class planet finder. In a two year all-sky survey,
  TESS will observe more than two million bright, nearby stars,
  searching for temporary drops in brightness that are caused by
  planetary transits. Such transits not only provide the means of
  identifying the planet, but also provide knowledge of the planet's
  diameter, mass density, surface gravity, temperature, and other key
  properties. TESS is expected to detect more than 1000 transiting
  exoplanet candidates. These detections will include a sample of
  100 Super Earths -- small rock-and-ice planets with masses in the
  range 1 to 10 Earth masses -- orbiting nearby stars with spectral
  types spanning a broad range, including F, G, K, and M dwarfs. No
  ground-based survey can achieve this feat. TESS's "wide-shallow" survey
  complements the "narrow-deep" Corot and Kepler mission surveys. The
  resulting TESS Transit Catalog of the nearest and brightest stars
  in the sky will constitute a unique scientific legacy for followup
  observations. TESS will identify Super Earths orbiting IR-bright stars,
  ideal for JWST searches for planetary water and carbon dioxide. <P
  />The TESS mission is a collaborative effort led by researchers at
  the Massachusetts Institute of Technology, the Harvard-Smithsonian
  Center for Astrophysics, and the NASA Ames Research Center. Additional
  TESS partners include ATK Space Systems, the Las Cumbres Observatory
  Global Telescope Network, Lowell Observatory, the NASA Goddard Space
  Flight Center, the Infrared Processing and Analysis Center at the
  California Institute of Technology, the University of California
  (Berkeley and Santa Cruz), the SETI Institute, Espace Incorporated,
  the Geneva Observatory (Switzerland), the Tokyo Institute of Technology
  (Japan), and Institut Supérieur de l'Aéronautique et de l'Espace
  (France). <P />TESS is currently completing a NASA-funded Phase A study,
  and is proposed for launch in December 2012.

Title: Observational detection of eight mutual eclipses and
    occultations between the satellites of Uranus
Authors: Christou, A. A.; Lewis, F.; Roche, P.; Hashimoto, Y.;
   O'Donoghue, D.; Worters, H.; Buckley, D. A. H.; Michalowski, T.;
   Asher, D. J.; Bitsaki, A.; Psalidas, A.; Tsamis, V.; Gourgouliatos,
   K. N.; Liakos, A.; Hidas, M. G.; Brown, T. M.
Bibcode: 2009A&A...497..589C
Altcode: 2009arXiv0902.4582C
  Aims: We carried out observations, with five different instruments
  ranging in aperture from 0.4 m to 10 m, of the satellites of
  Uranus during that planet's 2007 Equinox. Our observations covered
  specific intervals of time when mutual eclipses and occultations were
  predicted. <BR />Methods: The observations were carried out in the
  near-infrared part of the spectrum to mitigate the glare from the
  planet. Frames were acquired at rates &gt;1/min. Following modelling
  and subtraction of the planetary source from these frames, differential
  aperture photometry was carried out on the satellite pairs involved in
  the predicted events. In all cases but one, nearby bright satellites
  were used as reference sources. <BR />Results: We have obtained
  fifteen individual lightcurves, eight of which show a clear drop in
  the flux from the satellite pair, indicating that a mutual event took
  place. Three of these involve the faint satellite Miranda. All eight
  lightcurves were model-fitted to yield best estimates of the time of
  maximum flux drop and the impact parameter. In three cases best-fit
  albedo ratios were also derived. We used these estimates to generate
  intersatellite astrometric positions with typical formal uncertainties
  of &lt;0.01 arcsec, several times better than conventional astrometry of
  these satellites. The statistics of our estimated event midtimes show
  a systematic lag, with the observations later than predictions. In
  addition, lightcurves of two partial eclipses of Miranda show no
  statistically significant evidence of a light drop, at variance with
  the predictions. These indicate that new information about the Uranian
  satellite system is contained in observations of mutual events acquired
  here and by other groups.

Title: Transit timing variability in TrES-1
Authors: Rabus, M.; Alonso, R.; Deeg, H. J.; Belmonte, J. A.; Almenara,
   J. M.; Gilliland, R. L.; Brown, T. M.
Bibcode: 2009IAUS..253..432R
Altcode:
  We observed several transits of the exoplanet TrES-1 distributed over
  four years from 2004 to 2007. On the basis of these observations and
  additional published data, we present a mid-transit time analysis. The
  aim is to find indications of the presence of a third body by analysing
  the difference between the calculated and observed transit times.

Title: Transiting Planets in the Galactic Bulge from SWEEPS Survey
    and Implications
Authors: Sahu, Kailash C.; Casertano, Stefano; Valenti, Jeff; Bond,
   Howard E.; Brown, Thomas M.; Smith, T. Ed; Clarkson, Will; Minniti,
   Dante; Zoccali, Manuela; Livio, Mario; Renzini, Alvio; Rich, R. M.;
   Panagia, Nino; Lubow, Stephen; Brown, Timothy; Piskunov, Nikolai
Bibcode: 2009IAUS..253...45S
Altcode:
  The SWEEPS (Sagittarius Window Eclipsing Extrasolar Planet Search)
  program was aimed at detecting planets around stars in the Galactic
  bulge, not only to determine their physical properties, but also
  to determine whether the properties of planets found in the solar
  neighborhood, such as their frequency and the metallicity dependence,
  also hold for the planets in the Galactic bulge. We used the Hubble
  Space Telescope to monitor 180,000 F, G, K, and M dwarfs in the
  Galactic bulge continuously for 7 days in order to look for transiting
  planets. We discovered 16 candidate transiting extrasolar planets
  with periods of 0.6 to 4.2 days, including a possible new class of
  ultra-short period planets (USPPs) with P &lt; 1 day. The facts that
  (i) the coverage in the monitoring program is continuous, (ii) most
  of the stars are at a known distance (in the Galctic bulge), (iii)
  monitoring was carried out in 2 passbands, and (iv) the images have
  high spatial resolution, were crucial in minimizing and estimating the
  false positive rates. We estimate that at least 45% of the candidates
  are genuine planets. Radial velocity observations of the two brightest
  host stars further support the planetary nature of the transiting
  companions. These results suggest that the planet frequency in the
  Galactic bulge is similar to that in the solar neighborhood. They
  also suggest that higher metallicity favors planet formation even
  in the Galactic bulge. The USPPs occur only around low-mass stars
  which may suggest that close-in planets around higher-mass stars are
  irradiately evaporated, or that planets are able to migrate to and
  survive in close-in orbits only around such old and low-mass stars.

Title: The Transiting Exoplanet Survey Satellite (TESS)
Authors: Ricker, George R.; Latham, D. W.; Vanderspek, R. K.; Ennico,
   K. A.; Bakos, G.; Brown, T. M.; Burgasser, A. J.; Charbonneau, D.;
   Deming, L. D.; Doty, J. P.; Dunham, E. W.; Elliot, J. L.; Holman,
   M. J.; Ida, S.; Jenkins, J. M.; Jernigan, J. G.; Kawai, N.; Laughlin,
   G. P.; Lissauer, J. J.; Martel, F.; Sasselov, D. D.; Schingler,
   R. H.; Seager, S.; Torres, G.; Udry, S.; Villasenor, J. S.; Winn,
   J. N.; Worden, S. P.
Bibcode: 2009AAS...21340301R
Altcode: 2009BAAS...41..193R
  The Transiting Exoplanet Survey Satellite (TESS) is a low cost,
  SMEX-class planet finder. In a two year all-sky survey, TESS will
  observe more than two million bright, nearby stars, searching for
  temporary drops in brightness that are caused by planetary transits,
  which occur when a planet's orbit carries it directly in front of its
  parent star. Such transits not only provide the means of identifying
  the planet, but also provide knowledge of the planet's diameter, mass
  density, surface gravity, temperature, and other key properties. <P
  />TESS is expected to catalog more than 1000 transiting exoplanet
  candidates--20 times as many as are presently known, including a
  sample of 'super Earths'. The TESS "wide-shallow" survey will be
  complementary to the "narrow-deep" ones of the Corot and Kepler
  missions: its sky coverage will exceed that of Corot by 1000 times,
  and that of Kepler by 400 times. Because the TESS all-sky survey will
  systematically examine every interesting bright star likely to harbor an
  exoplanet, the resulting TESS Transit Catalog will constitute a unique
  scientific legacy. High resolution, follow-up ground-based optical and
  space-based IR spectroscopy of exoplanets demands bright targets. Thus,
  TESS should identify those new exoplanets that are ideal for study
  with the world's largest ground-based telescopes, as well as with
  NASA's upcoming James Webb Space Telescope. <P />The TESS mission is a
  collaborative effort led by researchers at MIT, the Harvard-Smithsonian
  Center for Astrophysics, and the NASA Ames Research Center. Additional
  TESS partners include the NASA Goddard Space Flight Center, the Harvard
  Origins of Life Initiative, Lowell Observatory, Caltech's IPAC, the
  SETI Institute, Geneva Observatory in Switzerland, Tokyo Institute
  of Technology, SUPAERO in France, ATK Space, Espace Inc, and the Las
  Cumbres Observatory Global Telescope Network. TESS has been accepted
  for Phase A study by NASA, and is proposed for launch in late 2012.

Title: NStED: Exo-Planet Transit Survey TrES Lyr1
Authors: O'Donovan, Francis T.; Charbonneau, David; Mandushev,
   Georgi; Dunham, Edward W.; Latham, David W.; Torres, Guillermo;
   Sozzetti, Alessandro; Brown, Timothy M.; Trauger, John T.; Belmonte,
   Juan A.; Rabus, Markus; Almenara, José M.; Alonso, Roi; Deeg, Hans
   J.; Esquerdo, Gilbert A.; Falco, Emilio E.; Hillenbrand, Lynne A.;
   Roussanova, Anna; Stefanik, Robert P.; Winn, Joshua N.
Bibcode: 2009nsted.cat....6O
Altcode:
  The Trans-atlantic Exoplanet Survey (TrES) attempts to find planetary
  transits among bright stars. The two telescope used are the 10cm Sleuth
  Telescope (Palomar Observatory, California) and the 10cm Planet Search
  Survey Telescope (PSST) at Lowell Observatory, Arizona. The survey
  area covers 5.7 degrees by 5.7 degrees and is centered on the star
  16 Lyr (19h 01m 26.3713s +46d 56m 05.325s). NStED provides access to
  high precision time-series photometry from stars observed by various
  transit survey programs. The data presented here are the result of
  the Lyra 1 campaign with TrES telescopes.

Title: Research Science and Education: The NSF’s Astronomy and
    Astrophysics Postdoctoral Fellowship
Authors: Norman, Dara; Agueros, Marcel; Brown, Timothy M.; Browning,
   Matthew; Chakrabarti, Sukanya; Cobb, Bethany; Coble, Kim; Conselice,
   Christopher; Cruz, Kelle; Danly, Laura; Frinchaboy, Peter M.; Gawiser,
   Eric; Gelfand, Joseph; Gonzalez, Anthony; Hoffman, Jennifer L.;
   Huterer, Dragan; Johnson, John; Johnson, Roberta M.; Kannappan,
   Sheila; Kuzio de Naray, Rachel; Lai, David; Leonard, Douglas C.;
   Lystrup, Makenzi; Markoff, Sera; Menendez-Delmestre, Karin; Muchovej,
   Stephan; McSwain, M. Virginia; Rhode, Katherine; Smecker-Hane, Tammy;
   Smith, Malcolm; Sokoloski, Jennifer; Tran, Kim-Vy
Bibcode: 2009astro2010P..41N
Altcode: 2009arXiv0903.4509N
  The NSF's Astronomy and Astrophysics Postdoctoral Fellowship (AAPF)
  is exceptional among the available postdoctoral awards in Astronomy and
  Astrophysics. The fellowship is one of the few that allows postdoctoral
  researchers to pursue an original research program, of their own design,
  at the U.S. institution of their choice. However, what makes this
  fellowship truly unique is the ability of Fellows to lead an equally
  challenging, original educational program simultaneously. The legacy
  of this singular fellowship has been to encourage and advance leaders
  in the field who are equally as passionate about their own research as
  they are about sharing that research and their passion for astronomy
  with students and the public. In this positional paper we address the
  importance of fellowships like the AAPF to the astronomical profession
  by identifying the science and educational contributions that Fellows
  have made to the community. Further, we recommend that fellowships that
  encourage leading postdoctoral researchers to also become leaders in
  Astronomy education be continued and expanded.

Title: A cool starspot or a second transiting planet in the TrES-1
    system?
Authors: Rabus, M.; Alonso, R.; Belmonte, J. A.; Deeg, H. J.;
   Gilliland, R. L.; Almenara, J. M.; Brown, T. M.; Charbonneau, D.;
   Mandushev, G.
Bibcode: 2009A&A...494..391R
Altcode: 2008arXiv0812.1799R
  Aims: We investigate the origin of a flux increase found during a
  transit of TrES-1, observed with the HST (Hubble Space Telescope). This
  feature in the HST light curve cannot be attributed to noise and is
  supposedly a dark area on the stellar surface of the host star eclipsed
  by TrES-1 during its transit. We investigate the likelihood of two
  possible hypotheses for its origin. A starspot or a second transiting
  planet. <BR />Methods: We made use of several transit observations of
  TrES-1 from space with the HST and from ground with the IAC 80-cm
  telescope (IAC-80). On the basis of these observations we did a
  statistical study of flux variations in each of the observed events to
  investigate whether similar flux increases are present in other parts
  of the data set. <BR />Results: The HST observation presents a single
  clear flux rise during a transit, whereas the ground observations
  lead to detecting two such events but with low significance. In the
  case of having observed a starspot in the HST data, assuming a central
  impact between the spot and TrES-1, we would obtain a lower limit for
  the spot radius of 42 000 km. For this radius the spot temperature
  would be 4690 K, 560 K lower then the stellar surface of 5250 K. For
  a putative second transiting planet, we can set a lower limit for its
  radius at 0.37 R<SUB>J</SUB> and for periods of less than 10.5 days,
  we can set an upper limit at 0.72 R<SUB>J</SUB>. <BR />Conclusions:
  Assuming a conventional interpretation, this HST observation then
  constitutes the detection of a starspot. Alternatively, this flux rise
  might also be caused by an additional transiting planet. The true nature
  of the origin can be revealed if a wavelength dependency of the flux
  rise can be shown or discarded with higher certainty. Additionally,
  the presence of a second planet can be detected by radial velocity
  measurements. <P />Based on observations made with the NASA/ESA Hubble
  Space Telescope, obtained at the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in
  Astronomy, Inc., under NASA contract NAS 5-26555.

Title: Asteroseismology: The Next Frontier in Stellar Astrophysics
Authors: Giampapa, Mark S.; Aerts, Conny; Bedding, Tim; Bonanno,
   Alfio; Brown, Timothy M.; Christensen-Dalsgaard, Jorgen; Dominik,
   Martin; Ge, Jian; Gilliland, Ronald L.; Harvey, J. W.; Hill, Frank;
   Kawaler, Steven D.; Kjeldsen, Hans; Kurtz, D. W.; Marcy, Geoffrey W.;
   Matthews, Jaymie M.; Monteiro, Mario Joao P. F. G.; Schou, Jesper
Bibcode: 2009astro2010S..91G
Altcode:
  No abstract at ADS

Title: The Lyman Continuum Escape Fraction at z 0.7
Authors: Bridge, Carrie; Teplitz, H.; Siana, B.; Ferguson, H.;
   Conselice, C.; Brown, T. M.; De Mello, D. F.; Dickinson, M.; Gardner,
   J.; Giavalisco, M.; Claudia, S.; Colbert, J.
Bibcode: 2009AAS...21334805B
Altcode: 2009BAAS...41R.484B
  Lyman continuum photons produced in massive starbursts likely played
  an important role in the reionization of the Universe. However, their
  contribution depends upon the fraction of ionizing radiation that
  escapes from the intrinsic opacity of the galaxies below the Lyman
  limit. We present the results of deep HST rest-frame, UV slitless
  spectroscopy of 14 z 0.7 Lyman break galaxy (LBG) analogs in the COSMOS
  field. While there are no <P />detections of the Lyman Continuum we
  achieve individual limits of 5-21% and a stacked limit for the escape
  fraction of &lt;5%. These UV spectra from the ACS Solar Blind channel
  have achieved the deepest limits to date of the escape fraction in
  individual sources below z 1.

Title: Temporal Variability of Stars and Stellar Systems
Authors: Lister, Tim; Metcalfe, Travis; Brown, Tim; Street, Rachel
Bibcode: 2009astro2010S.184L
Altcode: 2009arXiv0902.2966L
  Although the Sun is our closest star by many orders of magnitude and
  despite having sunspot records stretching back to ancient China, our
  knowledge of the Sun's magnetic field is far from complete. Indeed,
  even now, after decades of study, the most obvious manifestations of
  magnetic fields in the Sun (e.g. sunspots, flares and the corona)
  are scarcely understood at all. These failures in spite of intense
  effort suggest that to improve our grasp of magnetic fields in stars
  and of astrophysical dynamos in general, we must broaden our base of
  examples beyond the Sun; we must study stars with a variety of ages,
  masses, rotation rates, and other properties, so we can test models
  against as broad a range of circumstances as possible. Over the next
  decade, an array of indirect techniques will be supplemented by rapidly
  maturing new capabilities such as gyrochronology, asteroseismology and
  precision photometry from space, which will transform our understanding
  of the temporal variability of stars and stellar systems. In this White
  Paper we will outline some of the key science questions in this area
  along with the techniques that could be used to bring new insights to
  these questions.

Title: Confirmation and Characterization of Kepler Mission Exoplanets:
    The Era of Rock and Ice Exoplanets
Authors: Charbonneau, David; Borucki, William; Brown, Timothy; Deming,
   Drake; Ford, Eric; Fortney, Jonathan; Gilliland, Ronald; Knutson,
   Heather; Latham, David; Seager, Sara
Bibcode: 2008sptz.prop60028C
Altcode:
  In the past 4 years, the combination of ground-based transit surveys
  and the remarkable stability of the Spitzer Space Telescope permitted
  the direct investigation of the atmospheres of one specific class
  of exoplanet, namely the Hot Jupiters. The power of the NASA Kepler
  Mission will be to discover dozens of transiting exoplanets that
  are not detectable from the ground either due to the shallow transit
  depth or the low transit frequency resulting from their longer orbital
  periods. Kepler will find large numbers of transiting hot Neptunes
  and hot SuperEarth exoplanets, as well as cooler Jupiters, each of
  which are nonetheless amenable to direct study of their infrared
  emission. We propose to use Spitzer to observe Kepler-detected
  exoplanets and candidates to pursue two goals. First, we will measure
  the two-color planetary emission for 20 representative members
  of these previously inaccessible cexoplanets. Such observations
  will permit the first opportunity to directly test theoretical
  models of exoplanetary atmospheres of varying compositions (notably
  SuperEarths and Neptunes) and under differing levels of irradiation
  (cooler Jovian companions). The same data will permit an estimate of
  the orbital eccentricities, thus providing a test of models of the
  orbital migration, and tidal dissipation for these various types of
  exoplanets. Second, we will use Spitzer to follow up Kepler-identified
  candidate terrestrial exoplanets to prove that these signals are indeed
  planetary in origin. By gathering single color time series spanning
  times of primary transit, we will exclude a significant source of
  astrophysical false positives (resulting from blends of triple stars
  systems containing an eclipsing binary) that will precisely mimic an
  exoplanetary signature in the Kepler data. These infrared data will
  provide a crucial step in confirming the planetary nature of many of
  the most exciting candidates, namely the planets with the smallest
  radii that are likely rocky in composition.

Title: Expected Planet and False Positive Detection Rates for the
    Transiting Exoplanet Survey Satellite
Authors: Brown, Timothy M.; Latham, David W.
Bibcode: 2008arXiv0812.1305B
Altcode:
  The proposed Transiting Exoplanet Survey Satellite (TESS) will survey
  the entire sky to locate the nearest and brightest transiting extrasolar
  planets with orbital periods up to about 36 days. Here we estimate
  the number and kind of astrophysical false positives that TESS will
  report, along with the number of extrasolar planets. These estimates
  are then used to size the ground-based follow-up observing efforts
  needed to confirm and characterize the planets. We estimate that the
  needed observing resources will be about 1400 telescope-nights of
  imaging with 0.5m to 1m-class telescopes, 300 telescope-nights with
  1m to 2m-class telescopes for the classification of the host stars
  and for radial velocity measurements with roughly 1 km/s precision,
  and 380 telescope-nights with 2m to 4m-class telescopes for radial
  velocity studies with precision of a few m/s. Follow-up spectroscopy of
  the smallest planets discovered by TESS at the best possible velocity
  precision will be limited by the number of telescope nights available
  on 4m to 10m class telescopes with instruments such as HARPS and HIRES,
  but the pay-off of such efforts will be the determination of masses
  for Super Earths with sufficient accuracy to distinguish rocky desert
  planets from water worlds.

Title: Kepler
Authors: Christensen-Dalsgaard, J.; Arentoft, T.; Brown, T. M.;
   Gilliland, R. L.; Kjeldsen, H.; Borucki, W. J.; Koch, D.
Bibcode: 2008CoAst.157..266C
Altcode:
  Kepler is a NASA mission, scheduled for launch in April 2009, whose
  principal purpose is to investigate extra-solar planetary systems,
  through the detection of planetary transits across their parent
  star. An important goal is to determine the prevalence of Earth-size
  planets in Earth-like orbits. The required photometric precision also
  makes the mission very well- suited for asteroseismology, with the
  important purpose of characterizing the central stars in planetary
  systems. An extensive asteroseismic programme is planned for Kepler,
  organized in an international collaboration in the Kepler Asteroseismic
  Science Consortium.

Title: The Kepler asteroseismic investigation
Authors: Christensen-Dalsgaard, J.; Arentoft, T.; Brown, T. M.;
   Gilliland, R. L.; Kjeldsen, H.; Borucki, W. J.; Koch, D.
Bibcode: 2008JPhCS.118a2039C
Altcode:
  The NASA Kepler mission for studies of extra-solar planets, with
  expected launch early in 2009, will provide a large set of excellent
  data for asteroseismology. Here we provide a brief presentation of
  the mission and discuss some aspects of the expected results of the
  asteroseismic investigations and the organization of the effort in
  the Kepler Asteroseismic Science Consortium (KASC).

Title: Mutual Events of the Uranian Satellites Observed with the
    Faulkes Telescopes
Authors: Christou, Apostolos; Lewis, F.; Hidas, M. G.; Brown, T. M.;
   Roche, P.
Bibcode: 2008DPS....40.4601C
Altcode: 2008BAAS...40..480C
  The 2007 Uranian Equinox allowed unique observations of the planet,
  its rings and satellites, possible only twice during the planet's 84
  year orbit. <P />Among these were mutual eclipses and occultations
  between the 5 classical satellites Ariel, Umbriel, Titania, Oberon and
  Miranda. These ``mutual'' events are extremely useful as reality checks
  of satellite ephemerides. In addition, they provide an opportunity
  to improve our knowledge of the satellite orbits and the system
  constants. <P />We observed several mutual events in 2007 using the 2m
  Faulkes Telescopes North (FTN) and South (FTS) located in Haleakala,
  Maui and Siding Spring, Australia respectively, operated by the Las
  Cumbres Observatory Global Telescope (LCOGT) network. To mitigate
  against Uranus' glare, we utilized wide-band imaging in the near-IR,
  a small image scale and a posteriori subtraction of the planet's
  PSF. <P />We obtained positive detections of six mutual events, three
  occultations and three eclipses, among these satellites. Three of
  these events involved Miranda, a difficult target due to its proximity
  to Uranus. Furthermore, we recorded at least two events that were
  predicted to occur with high confidence but did not, in fact, occur. <P
  />During this presentation we will describe our observing strategy,
  operational setup and data reduction techniques and present examples
  of obtained lightcurves. Our observational results have been compared
  with predictions based on ephemerides by Laskar and Jacobson (1987;
  GUST86), by Lainey and Arlot (2006; LA06) and by Rush and Jacobson
  (2007; RJ07). Offsets with respect to the Voyager-era GUST86 are quite
  significant, of the order of minutes in the event midtimes. Smaller,
  yet significant trends in the data also appear with respect to LA06
  and RJ07. <P />We will discuss the nature of these trends and how they
  can be interpreted in terms of potential improvements in our knowledge
  of the Uranian system.

Title: The Wide-Field Camera 3 detectors
Authors: Baggett, S. M.; Hill, R. J.; Kimble, R. A.; MacKenty, J. W.;
   Waczynski, A.; Bushouse, H. A.; Boehm, N.; Bond, H. E.; Brown, T. M.;
   Collins, N. R.; Delo, G.; Dressel, L.; Foltz, R.; Hartig, G.; Hilbert,
   B.; Kan, E.; Kim-Quijano, J.; Malumuth, E.; Martel, A.; McCullough,
   P.; Petro, L.; Robberto, M.; Wen, Y.
Bibcode: 2008SPIE.7021E..1QB
Altcode: 2008SPIE.7021E..50B
  The Wide-field Camera 3 (WFC3) is a fourth-generation instrument
  planned for installation in Hubble Space Telescope (HST). Designed as
  a panchromatic camera, WFC3's UVIS and IR channels will complement the
  other instruments onboard HST and enhance the observatory's scientific
  performance. UVIS images are obtained via two 4096×2051 pixel e2v CCDs
  while the IR images are taken with a 1024×1024 pixel HgCdTe focal plane
  array from Teledyne Imaging Sensors. Based upon characterization tests
  performed at NASA/GSFC, the final flight detectors have been chosen
  and installed in the instrument. This paper summarizes the performance
  characteristics of the WFC3 flight detectors based upon component and
  instrument-level testing in ambient and thermal vacuum environments.

Title: Parameters and Predictions for the Long-Period Transiting
    Planet HD 17156b
Authors: Irwin, Jonathan; Charbonneau, David; Nutzman, Philip; Welsh,
   William F.; Rajan, Abhijith; Hidas, Marton; Brown, Timothy M.; Lister,
   Timothy A.; Davies, Donald; Laughlin, Gregory; Langton, Jonathan
Bibcode: 2008ApJ...681..636I
Altcode: 2008arXiv0801.1496I
  We report high-cadence time series photometry of the recently
  discovered transiting exoplanet system HD 17156, spanning the time of
  transit on UT 2007 October 1, from three separate observatories. We
  present a joint analysis of our photometry, previously published
  radial velocity measurements, and times of transit center for three
  additional events. Adopting the spectroscopically determined values
  and uncertainties for the stellar mass and radius, we estimate a
  planet radius of R<SUB>p</SUB> = 1.01 +/- 0.09 R<SUB>Jup</SUB> and an
  inclination of i = 86.5<SUP>+ 1.1</SUP><SUB>-0.7</SUB> deg. We find a
  time of transit center of T<SUB>c</SUB> = 2,454,374.8338 +/- 0.0020 HJD
  and an orbital period of P = 21.21691 +/- 0.00071 days and note that
  the four transits reported to date show no sign of timing variations
  that would indicate the presence of a third body in the system. Our
  results do not preclude the existence of a secondary eclipse, but
  imply that there is only a 9.2% chance for this to be present and an
  even lower probability (6.9%) that the secondary eclipse would be a
  nongrazing event. Due to its eccentric orbit and long period, HD 17156b
  is a fascinating object for the study of the dynamics of exoplanet
  atmospheres. To aid such future studies, we present theoretical light
  curves for the variable infrared emission from the visible hemisphere
  of the planet throughout its orbit.

Title: Stellar proper motions in the Galactic bulge with ACS/WFC
    on HST
Authors: Clarkson, Will; Sahu, Kailash; Anderson, Jay; Smith, T. Ed;
   Brown, Thomas M.; Casertano, Stefano; Rich, R. Michael; Bond, Howard
   E.; Brown, Timothy; Livio, Mario; Minniti, Dante; Panagia, Nino;
   Renzini, Alvio; Valenti, Jeff; Zoccali, Manuela
Bibcode: 2008IAUS..245..361C
Altcode:
  In 2004 the Sagittarius Window Eclipsing Extrasolar Planet Search
  (SWEEPS) project undertook a very deep ACS/WFC exposure-set of the Sgr-I
  low-reddening window in the Galactic Bulge, with repeat observations
  2.04 years later. The combination of superb first-epoch sampling,
  wide field of view and high PSF stability of ACS/WFC on Hubble allows
  proper motions to be extracted for more than 137,000 objects, over
  85,000 to accuracy better than 0.3 mas yr<SUP>-1</SUP>. We present
  these proper motions and outline some of the uses to which they have
  been put, including the separation of a pure-Bulge sample and the
  inner Galactic rotation curve.

Title: Observations of the atmospheres of extrasolar planets
Authors: Brown, T. M.; Alonso, R.; Knölker, M.; Rauer, H.; Schmidt, W.
Bibcode: 2008depn.conf...50B
Altcode:
  No abstract at ADS

Title: Finding Earth-size planets in the habitable zone: the Kepler
    Mission
Authors: Borucki, William; Koch, David; Basri, Gibor; Batalha, Natalie;
   Brown, Timothy; Caldwell, Douglas; Christensen-Dalsgaard, Jørgen;
   Cochran, William; Dunham, Edward; Gautier, Thomas N.; Geary, John;
   Gilliland, Ronald; Jenkins, Jon; Kondo, Yoji; Latham, David; Lissauer,
   Jack J.; Monet, David
Bibcode: 2008IAUS..249...17B
Altcode: 2007IAUS..249...17B
  The Kepler Mission is a space-based mission whose primary goal is
  to detect Earth-size and smaller planets in the habitable zone of
  solar-like stars. The mission will monitor more than 100,000 stars
  for transits with a differential photometric precision of 20 ppm
  at V=12 for a 6.5 hour transit. It will also provide asteroseismic
  results on several thousand dwarf stars. It is specifically designed
  to continuously observe a single field of view of greater than 100
  square degrees for 3.5 or more years. <P />This overview describes the
  mission design, its goals and capabilities, the measured performance
  for those photometer components that have now been tested, the Kepler
  Input Catalog, an overview of the analysis pipeline, the plans for the
  Follow-up Observing Program to validate the detections and characterize
  the parent stars, and finally, the plans for the Guest Observer and
  Astrophysical Data Program.

Title: Las Cumbres Observatory Global Telescope: A homogeneous
    telescope network
Authors: Hidas, M. G.; Hawkins, E.; Walker, Z.; Brown, T. M.; Rosing,
   W. E.
Bibcode: 2008AN....329..269H
Altcode:
  Las Cumbres Observatory Global Telescope is a research organisation in
  the process of designing and building a network of robotic telescopes
  to be used for research in time-domain astrophysics and education. The
  network will have complete latitude coverage in both hemispheres to
  allow continuous observations of any target. In other words, we will
  keep you in the dark. We describe the current status of our facilities
  and our vision for the full network.

Title: An observation of a mutual event between two satellites
    of Uranus
Authors: Hidas, M. G.; Christou, A. A.; Brown, T. M.
Bibcode: 2008MNRAS.384L..38H
Altcode: 2008MNRAS.tmpL...2H; 2007arXiv0711.2095H
  We present observations of the occultation of Umbriel by Oberon on
  2007 May 4. We believe this is the first observed mutual event between
  satellites of Uranus. Fitting a simple geometric model to the light
  curve, we measure the mid-event time with a precision of 4 s. We assume
  previously measured values for the albedos of the two satellites, and
  measure the impact parameter to be 500 +/- 80 km. These measurements
  are more precise than estimates based on current ephemerides for these
  satellites. Therefore observations of additional mutual events during
  the 2007-2008 Uranian equinox will provide improved estimates of their
  orbital and physical parameters.

Title: Planets in the Galactic Bulge: Results from the SWEEPS Project
Authors: Sahu, K. C.; Casertano, S.; Valenti, J.; Bond, H. E.; Brown,
   T. M.; Smith, T. E.; Clarkson, W.; Minniti, D.; Zoccali, M.; Livio,
   M.; Renzini, A.; Rich, R. M.; Panagia, N.; Lubow, S.; Brown, T.;
   Piskunov, N.
Bibcode: 2008ASPC..398...93S
Altcode: 2007arXiv0711.4059S
  The exoplanets discovered so far have been mostly around relatively
  nearby and bright stars. As a result, the host stars are mostly (i)
  in the Galactic disk, (ii) relatively massive, and (iii) relatively
  metal rich. The aim of the SWEEPS project is to extend our knowledge
  to stars which (i) are in a different part of the Galaxy, (ii) have
  low masses, and (iii) have a large range of metallicities. To achieve
  this goal, we used the Hubble Space Telescope and its Advanced Camera
  for Surveys to look for transiting planets around F, G, K, and and M
  dwarfs in the Galactic bulge. We photometrically monitored ∼180,000
  stars in a dense stellar field in the Galactic bulge continuously for
  7 days. We discovered 16 candidate transiting extrasolar planets with
  periods of 0.6 to 4.2 days, including a new class of ultra-short period
  planets (USPPs) with P&lt;1.2 days. Radial velocity observations of
  two brightest candidates support the planetary nature. These results
  suggest that planets are equally abundant in the Galactic bulge and
  around low-mass stars (within a factor ∼2), and the metallicity
  distribution holds even for the stars in the Galactic bulge. The USPPs
  occur only around low-mass stars which suggest that close-in planets
  around higher-mass stars are either irradiately evaporated, or that
  the size of the inner disk hole decreases with decreasing mass of the
  host stars.

Title: Characterizing extrasolar planets
Authors: Brown, Timothy M.
Bibcode: 2008expl.conf...65B
Altcode:
  Transiting extrasolar planets provide the best current opportunities
  for characterizing the physical properties of extrasolar planets. In
  this review, I first describe the geometry of planetary transits, and
  methods for detecting and refining the observations of such transits. I
  derive the methods by which transit light curves and radial velocity
  data can be analyzed to yield estimates of the planetary radius,
  mass, and orbital parameters. I also show how visible-light and
  infrared spectroscopy can be valuable tools for understanding the
  composition, temperature, and dynamics of the atmospheres of transiting
  planets. Finally, I relate the outcome of a participatory lecture-hall
  exercise relating to one term in the Drake equation, namely the lifetime
  of technical civilizations.

Title: The Lyman Continuum Escape Fraction at Moderate Redshift
Authors: Teplitz, Harry I.; Siana, B.; Bridge, C.; Ferguson, H.;
   Giavalisco, M.; Dickinson, M.; Gardner, J. P.; de Mello, D.; Brown,
   T. M.; Colbert, J.
Bibcode: 2007AAS...21114306T
Altcode: 2007BAAS...39..996T
  Massive starbursts may have played a dominant role in the reionization
  of the Universe. Their contribution depends in part upon the fraction of
  ionizing radiation that escapes from the intrinsic opacity of galaxies
  below the Lyman limit. Current surveys suggest that the escape fraction
  is low in all but 15-25% of galaxies, even among young starbursts. We
  present new HST ultraviolet imaging of moderate redshift starbursts
  to constrain how close to zero the escape fraction is in galaxies
  that are similar to those which may have reinoized the Universe. We
  targeted 15 bright, blue galaxies at z 1.3 in the GOODS fields for 5
  orbits each using the Solar Blind Channel of the ACS, achieving the
  deepest limits to date on the escape fraction in individual sources.

Title: Hubble Space Telescope time-series photometry of the planetary
transit of HD 189733: no moon, no rings, starspots
Authors: Pont, F.; Gilliland, R. L.; Moutou, C.; Charbonneau, D.;
   Bouchy, F.; Brown, T. M.; Mayor, M.; Queloz, D.; Santos, N.; Udry, S.
Bibcode: 2007A&A...476.1347P
Altcode: 2007arXiv0707.1940P
  We monitored three transits of the giant gas planet around the nearby K
  dwarf HD 189733 with the ACS camera on the Hubble Space Telescope. The
  resulting very-high accuracy lightcurve (signal-to-noise ratio near
  15 000 on individual measurements, 35 000 on 10-min averages) allows a
  direct geometric measurement of the orbital inclination, radius ratio
  and scale of the system: i = 85.68 ± 0.04, R_pl/R<SUB>*</SUB> = 0.1572
  ± 0.0004, a/R<SUB>*</SUB> = 8.92 ± 0.09. We derive improved values
  for the stellar and planetary radius, R<SUB>*</SUB> = 0.755 ± 0.011
  R_⊙, R_pl = 1.154 ± 0.017 R_J, and the transit ephemerides, T_tr =
  2453931.12048 ± 0.00002 + n\cdot2.218581 ± 0.000002. The HST data also
  reveal clear evidence of the planet occulting spots on the surface of
  the star. At least one large spot complex (&gt;80 000 km) is required to
  explain the observed flux residuals and their colour evolution. This
  feature is compatible in amplitude and phase with the variability
  observed simultaneously from the ground. No evidence for satellites
  or rings around HD 189733b is seen in the HST lightcurve. This allows
  us to exlude with a high probability the presence of Earth-sized
  moons and Saturn-type debris rings around this planet. The timing of
  the three transits sampled is stable to the level of a few seconds,
  excluding a massive second planet in outer 2:1 resonance. <P />The
  full version of Table ? is only available in electronic form at the
  CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via
  http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/476/1347

Title: Selection and Prioritization of Targets for the Kepler Mission
Authors: Batalha, Natalie M.; Borucki, W. J.; Brown, T. M.; Bryson,
   S. T.; Caldwell, D. A.; Everett, M. E.; Jenkins, J. M.; Koch, D. G.;
   Latham, D. W.
Bibcode: 2007AAS...21113516B
Altcode: 2007BAAS...39R.974B
  The Kepler mission is designed to detect and characterize Earth-size
  planets in the habitable zone of their parent stars. This will be
  possible for the brightest late-type Main Sequence stars (e.g. 12th
  magnitude for sun-like stars, 15-16th magnitude for M-type stars). There
  are nearly a half million stars brighter than 16th magnitude in the
  Kepler field of view, most of which are too large or too faint for
  detection of an Earth-like planet. The Kepler Stellar Classification
  Program (SCP) is a pre-launch effort to characterize every star in the
  field (with reasonable completeness down to m=20) using ground-based
  multi-color photometry to determine the surface gravity and effective
  temperature. The SCP products will allow us to pre-select and prioritize
  targets based on the predicted SNR of an Earth-like transit. The
  methodology is designed to maximize the science yield of the mission
  by quantifying, for every potential target, the minimum detectable
  planet radius as a function of semi-major axis. The metric considers
  issues of crowding by quantifying the amount of contamination from
  background stars that works to dilute the transit signal. We describe
  the selection/prioritization methodology and present the magnitude
  and spectral type distribution for a target list generated from a
  preliminary release of the Kepler Input Catalog. <P />Support for this
  work came from NASA's Discovery Program.

Title: Towards A Scheduler For The LCOGT Multi-telescope Network
Authors: Brown, Timothy M.; Baliber, N.
Bibcode: 2007AAS...211.4726B
Altcode: 2007BAAS...39..807B
  Las Cumbres Observatory Global Telescope (LCOGT) is building a
  world-wide network of telescopes optimized for time-domain astronomy. A
  key part of this effort is the scheduler, which converts allocations
  of telescope time, judgments about scientific importance, and a
  multitude of practical considerations into commands for the pointing
  and instrument configuration of each network telescope. Among telescope
  schedulers, this one will be unusual in two respects: it must deal
  with multiple telescopes, and the mix of desired observations will
  be dominated by lengthy observations of time-critical (but often
  predictable) events. Here we describe the program BLOCKHEAD, intended
  as a step toward the final scheduler. BLOCKHEAD uses a randomized
  multi-pass procedure to distribute 30-minute blocks of observing time
  among many observing projects and across multiple telescopes, for a
  1-month planning interval. For automated scheduling of a full network,
  BLOCKHEAD is intended to be preceded by a monthly time-allocation
  process, and followed by a module that adapts the nominal schedule
  to cope with weather, targets of opportunity, and other real-time
  schedule-driving events. It does not attempt global optimization of the
  schedule, but it is fast enough that many independent schedules may
  easily be intercompared for optimization against any desired figure
  of merit. BLOCKHEAD is now being tested using simulated observing
  requests on telescope networks, and also as an element in scheduling
  our existing telescopes on Haleakala and at Siding Spring.

Title: Asteroseismology and interferometry
Authors: Cunha, M. S.; Aerts, C.; Christensen-Dalsgaard, J.;
   Baglin, A.; Bigot, L.; Brown, T. M.; Catala, C.; Creevey, O. L.;
   Domiciano de Souza, A.; Eggenberger, P.; Garcia, P. J. V.; Grundahl,
   F.; Kervella, P.; Kurtz, D. W.; Mathias, P.; Miglio, A.; Monteiro,
   M. J. P. F. G.; Perrin, G.; Pijpers, F. P.; Pourbaix, D.; Quirrenbach,
   A.; Rousselet-Perraut, K.; Teixeira, T. C.; Thévenin, F.; Thompson,
   M. J.
Bibcode: 2007A&ARv..14..217C
Altcode: 2007arXiv0709.4613C
  Asteroseismology provides us with a unique opportunity to improve
  our understanding of stellar structure and evolution. Recent
  developments, including the first systematic studies of solar-like
  pulsators, have boosted the impact of this field of research within
  astrophysics and have led to a significant increase in the size of
  the research community. In the present paper we start by reviewing
  the basic observational and theoretical properties of classical and
  solar-like pulsators and present results from some of the most recent
  and outstanding studies of these stars. We centre our review on those
  classes of pulsators for which interferometric studies are expected
  to provide a significant input. We discuss current limitations to
  asteroseismic studies, including difficulties in mode identification
  and in the accurate determination of global parameters of pulsating
  stars, and, after a brief review of those aspects of interferometry
  that are most relevant in this context, anticipate how interferometric
  observations may contribute to overcome these limitations. Moreover,
  we present results of recent pilot studies of pulsating stars involving
  both asteroseismic and interferometric constraints and look into the
  future, summarizing ongoing efforts concerning the development of
  future instruments and satellite missions which are expected to have
  an impact in this field of research.

Title: VizieR Online Data Catalog: HST/ACS flux time series for HD
    189733 (Pont+, 2007)
Authors: Pont, F.; Gilliland, R. L.; Moutou, C.; Charbonneau, D.;
   Bouchy, F.; Brown, T. M.; Mayor, M.; Queloz, D.; Santos, N.; Udry, S.
Bibcode: 2007yCat..34761347P
Altcode:
  We monitored three transits of the giant gas planet around the nearby K
  dwarf HD 189733 with the ACS camera on the Hubble Space Telescope. The
  resulting very-high accuracy light-curve (signal-to-noise ratio near
  15000 on individual measurements, 35000 on 10-min averages) allows
  a direct geometric measurement of the orbital inclination, radius
  ratio and scale of the system: i=85.68+/-0.04, Rpl/R*=0.1572+/-0.0004,
  a/R*=8.92+/-0.09. <P />(1 data file).

Title: TrES-4: A Transiting Hot Jupiter of Very Low Density
Authors: Mandushev, Georgi; O'Donovan, Francis T.; Charbonneau, David;
   Torres, Guillermo; Latham, David W.; Bakos, Gáspár Á.; Dunham,
   Edward W.; Sozzetti, Alessandro; Fernández, José M.; Esquerdo,
   Gilbert A.; Everett, Mark E.; Brown, Timothy M.; Rabus, Markus;
   Belmonte, Juan A.; Hillenbrand, Lynne A.
Bibcode: 2007ApJ...667L.195M
Altcode: 2007arXiv0708.0834M
  We report the discovery of TrES-4, a hot Jupiter that transits
  the star GSC 02620-00648 every 3.55 days. From high-resolution
  spectroscopy of the star, we estimate a stellar effective temperature of
  T<SUB>eff</SUB>=6100+/-150 K, and from high-precision z and B photometry
  of the transit we constrain the ratio of the semimajor axis a and the
  stellar radius R<SUB>*</SUB> to be a/R<SUB>*</SUB>=6.03+/-0.13. We
  compare these values to model stellar isochrones to constrain the
  stellar mass to be M<SUB>*</SUB>=1.22+/-0.17 M<SUB>solar</SUB>. Based
  on this estimate and the photometric time series, we constrain the
  stellar radius to be R<SUB>*</SUB>=1.738+/-0.092 R<SUB>solar</SUB> and
  the planet radius to be R<SUB>p</SUB>=1.674+/-0.094 R<SUB>Jup</SUB>. We
  model our radial velocity data assuming a circular orbit and find a
  planetary mass of 0.84+/-0.10 M<SUB>Jup</SUB>. Our radial velocity
  observations rule out line-bisector variations that would indicate
  a specious detection resulting from a blend of an eclipsing binary
  system. TrES-4 has the largest radius and lowest density of any of the
  known transiting planets. It presents a challenge to current models of
  the physical structure of hot Jupiters and indicates that the diversity
  of physical properties among the members of this class of exoplanets
  has yet to be fully explored.

Title: Stellar Populations across the NGC 4244 Truncated Galactic Disk
Authors: de Jong, Roelof S.; Seth, A. C.; Radburn-Smith, D. J.; Bell,
   E. F.; Brown, T. M.; Bullock, J. S.; Courteau, S.; Dalcanton, J. J.;
   Ferguson, H. C.; Goudfrooij, P.; Holfeltz, S.; Holwerda, B. W.;
   Purcell, C.; Sick, J.; Zucker, D. B.
Bibcode: 2007ApJ...667L..49D
Altcode: 2007arXiv0708.0826D
  We use the Hubble Space Telescope ACS to study the resolved stellar
  populations of the nearby, nearly edge-on galaxy NGC 4244 across its
  outer disk surface density break. The stellar photometry allows us to
  study the distribution of different stellar populations and reach very
  low equivalent surface brightnesses. We find that the break occurs
  at the same radius for young, intermediate-age, and old stars. The
  stellar density beyond the break drops sharply by a factor of at least
  600 in 5 kpc. The break occurs at the same radius independent of height
  above the disk, but is sharpest in the midplane and nearly disappears
  at large heights. These results make it unlikely that truncations are
  caused by a star formation threshold alone: the threshold would have
  to keep the same radial position from less than 100 Myr to 10 Gyr ago,
  in spite of potential disturbances such as infall and redistribution
  of gas by internal processes. A dynamical interpretation of truncation
  formation is more likely, such as due to angular momentum redistribution
  by bars or density waves, or heating and stripping of stars caused
  by the bombardment of dark matter subhalos. The latter explanation
  is also in quantitative agreement with the small diffuse component we
  see around the galaxy.

Title: GHOSTS: The Resolved Stellar Outskirts of Massive Disk Galaxies
Authors: de Jong, Roelof S.; Seth, A. C.; Bell, E. F.; Brown,
   T. M.; Bullock, J. S.; Courteau, S.; Dalcanton, J. J.; Ferguson,
   H. C.; Goudfrooij, P.; Holfeltz, S.; Purcell, C.; Radburn-Smith, D.;
   Zucker, D.
Bibcode: 2007IAUS..241..503D
Altcode: 2007astro.ph..2168D
  We show initial results from our ongoing HST GHOSTS survey of the
  resolved stellar envelopes of 14 nearby, massive disk galaxies. In
  hierarchical galaxy formation the stellar halos and thick disks of
  galaxies are formed by accretion of minor satellites and therefore
  contain valuable information about the (early) assembly process
  of galaxies. We detect for the first time the very small halo of
  NGC4244, a low mass edge-on galaxy. We find that massive galaxies
  have very extended halos, with equivalent surface brightnesses of
  28-29 V-mag/arcsec^2 at 20-30 kpc from the disk. The old RGB stars of
  the thick disk in the NGC891 and NGC4244 edge-on galaxies truncate at
  the same radius as the young thin disk stars, providing insights into
  the formation of both disk truncations and thick disks. We furthermore
  present the stellar populations of a very low surface brightness stream
  around M83, the first such a stream resolved into stars beyond those
  of the Milky Way and M31.

Title: The Kepler Mission and Eclipsing Binaries
Authors: Koch, David; Borucki, William; Basri, Gibor; Brown, Timothy;
   Caldwell, Douglas; Christensen-Dalsgaard, Jorgen; Cochran, William;
   Devore, Edna; Dunham, Edward; Gautier, Thomas N.; Geary, John;
   Gilliland, Ronald; Gould, Alan; Jenkins, Jon; Kondo, Yoji; Latham,
   David; Lissauer, Jack; Monet, David
Bibcode: 2007IAUS..240..236K
Altcode: 2006IAUS..240E..21K
  The Kepler Mission is a photometric mission with a precision of 14 ppm
  ( at R= 12) that is designed to continuously observe a single field of
  view (FOV) of greater 100 sq deg in the Cygnus-Lyra region for four or
  more years. The primary goal of the mission is to monitor &gt;100,000
  stars for transits of Earth-size and smaller planets in the habitable
  zone of solar-like stars. In the process, many eclipsing binaries
  (EB) will also be detected and light curves produced. To enhance and
  optimize the mission results, the stellar characteristics for all
  the stars in the FOV with R&lt;16 will have been determined prior
  to launch. As part of the verification process, stars with transit
  candidates will have radial velocity follow-up observations performed to
  determine the component masses and thereby separate eclipses caused by
  stellar companions from transits caused by planets. The result will be
  a rich database on EBs. The community will have access to the archive
  for further analysis, such as, for EB modeling of the high-precision
  light curves. A guest observer program is also planned to allow for
  photometric observations of objects not on the target list but within
  the FOV, since only the pixels of interest from those stars monitored
  will be transmitted to the ground.

Title: The Transatlantic Exoplanet Survey (TrES): A Review
Authors: Alonso, R.; Brown, T. M.; Charbonneau, D.; Dunham, E. W.;
   Belmonte, J. A.; Deeg, H. J.; Fernández, J. M.; Latham, D. W.;
   Mandushev, G.; O'Donovan, F. T.; Rabus, M.; Torres, G.
Bibcode: 2007ASPC..366...13A
Altcode:
  The TrES project is designed to search for exoplanetary transits
  using three wide-field optical telescopes of 10-cm in diameter,
  in three different observatories. We describe the instruments and
  strategies used by the team, which has been working as a network since
  2003. We summarize the major findings and difficulties faced during
  these years, which include the discovery of two transiting planets,
  a pair of eclipsing M stars, and many configurations of stars that
  mimic the signal of transiting planets.

Title: Precise Photometry of Extrasolar Planet Transits with SOFIA
Authors: Dunham, E. W.; Elliot, J. L.; Brown, T. M.; Charbonneau,
   D.; McLean, I. S.
Bibcode: 2007ASPC..366..256D
Altcode:
  Precise photometric observations of transiting extrasolar planets
  can provide a wealth of data on the nature of these objects. Results
  such as planetary radius, orbital inclination, stellar limb darkening,
  evidence for planetary satellites or rings, and atmospheric composition
  can be found from the transit observation alone. When combined with high
  quality radial velocity data the mass and density of the planet can be
  determined. Infrared observations of the secondary minimum provide a
  means to determine the temperature of the planet and allow limits on
  the orbital eccentricity to be defined. Perturbations by other planets
  in the system can be found by variations in transit timing over a period
  of years. <P />We anticipate that very high quality transit data can be
  obtained with SOFIA using the HIPO and FLITECAM science instruments. At
  present this work is limited to the nine brightest known transiting
  planets, but the field is so active that many additional targets will
  be found. The ongoing spectroscopic planet search programs and several
  ongoing transit search programs designed specifically to find objects
  bright enough for detailed follow-up work are expected to add numerous
  objects to this list over SOFIA's lifetime. The Kepler mission will
  be launched and complete its mission while SOFIA is flying, producing
  numerous exciting opportunities for additional work.

Title: Update and Recent Results of the STARE Instrument
Authors: Rabus, M.; Brown, T. M.; Deeg, H. J.; Belmonte Avilés,
   J. A.; Almenara Villa, J. M.; Alonso, R.
Bibcode: 2007ASPC..366...96R
Altcode:
  The STARE telescope of the High Altitude Observatory (HAO), Boulder
  is maintained by the Instituto de Astrofísica de Canarias (IAC)
  at the Observatorio del Teide (OT) on Tenerife. The STARE instrument
  has been updated in spring 2006 and forms part of the TrES network,
  which consists of two more telescopes located in the USA (PSST, Lowell
  Observatory; Sleuth Mt. Palomar). In this paper an overview over
  STARE's update and first results from recent observations are given.

Title: TrES-3: A Nearby, Massive, Transiting Hot Jupiter in a 31
    Hour Orbit
Authors: O'Donovan, Francis T.; Charbonneau, David; Bakos, Gáspár
   Á.; Mandushev, Georgi; Dunham, Edward W.; Brown, Timothy M.; Latham,
   David W.; Torres, Guillermo; Sozzetti, Alessandro; Kovács, Géza;
   Everett, Mark E.; Baliber, Nairn; Hidas, Márton G.; Esquerdo, Gilbert
   A.; Rabus, Markus; Deeg, Hans J.; Belmonte, Juan A.; Hillenbrand,
   Lynne A.; Stefanik, Robert P.
Bibcode: 2007ApJ...663L..37O
Altcode: 2007arXiv0705.2004O
  We describe the discovery of a massive transiting hot Jupiter
  with a very short orbital period (1.30619 days), which we name
  TrES-3. From spectroscopy of the host star GSC 03089-00929,
  we measure T<SUB>eff</SUB>=5720+/-150 K, logg=4.6+/-0.3, and
  vsini&lt;2 km s<SUP>-1</SUP> and derive a stellar mass of 0.90+/-0.15
  M<SUB>solar</SUB>. We estimate a planetary mass of 1.92+/-0.23
  M<SUB>Jup</SUB>, based on the sinusoidal variation of our high-precision
  radial velocity measurements. This variation has a period and phase
  consistent with our transit photometry. Our spectra show no evidence of
  line bisector variations that would indicate a blended eclipsing binary
  star. From detailed modeling of our B and z photometry of the 2.5% deep
  transits, we determine a stellar radius 0.802+/-0.046 R<SUB>solar</SUB>
  and a planetary radius 1.295+/-0.081 R<SUB>Jup</SUB>. TrES-3 has one
  of the shortest orbital periods of the known transiting exoplanets,
  facilitating studies of orbital decay and mass loss due to evaporation,
  and making it an excellent target for future studies of infrared
  emission and reflected starlight. <P />Some of the data presented herein
  were obtained at the W. M. Keck Observatory, which is operated as a
  scientific partnership among Caltech, the University of California,
  and NASA. The Observatory was made possible by the generous financial
  support of the W. M. Keck Foundation.

Title: Outcome of Six Candidate Transiting Planets from a TrES Field
    in Andromeda
Authors: O'Donovan, Francis T.; Charbonneau, David; Alonso, Roi;
   Brown, Timothy M.; Mandushev, Georgi; Dunham, Edward W.; Latham,
   David W.; Stefanik, Robert P.; Torres, Guillermo; Everett, Mark E.
Bibcode: 2007ApJ...662..658O
Altcode: 2006astro.ph.10603O
  Driven by the incomplete understanding of the formation of gas giant
  extrasolar planets and of their mass-radius relationship, several
  ground-based, wide-field photometric campaigns are searching the skies
  for new transiting extrasolar gas giants. As part of the Trans-atlantic
  Exoplanet Survey (TrES), in 2003/2004 we monitored approximately 30,000
  stars (9.5&lt;=V&lt;=15.5) in a 5.7<SUP>deg</SUP>×5.7<SUP>deg</SUP>
  field in Andromeda with three telescopes over 5 months. We identified
  six candidate transiting planets from the stellar light curves. From
  subsequent follow-up observations we rejected each of these as an
  astrophysical false positive, i.e., a stellar system containing an
  eclipsing binary, whose light curve mimics that of a Jupiter-sized
  planet transiting a Sunlike star. We discuss here the procedures
  followed by the TrES team to reject false positives from our list of
  candidate transiting hot Jupiters. We present these candidates as early
  examples of the various types of astrophysical false positives found
  in the TrES campaign, and discuss what we learned from the analysis.

Title: Asteroseismology with the Kepler mission
Authors: Christensen-Dalsgaard, J.; Arentoft, T.; Brown, T. M.;
   Gilliland, R. L.; Kjeldsen, H.; Borucki, W. J.; Koch, D.
Bibcode: 2007CoAst.150..350C
Altcode: 2007astro.ph..1323C
  NASA's Kepler mission will fly a photometer based on a wide-field
  Schmidt camera with a 0.95 m aperture, staring at a single field
  continuously for at least 4 years. Although the mission's principal
  aim is to locate transiting extrasolar planets, it will provide an
  unprecedented opportunity to make asteroseismic observations on a
  wide variety of stars. Plans are now being developed to exploit this
  opportunity to the fullest.

Title: Surveys, Temporal Variability, and the Las Cumbres Observatory
    Global Telescope
Authors: Brown, Tim; Rosing, W. E.; Baliber, N.; Hidas, M.; Street, R.
Bibcode: 2007AAS...210.6601B
Altcode: 2007BAAS...39..173B
  Upcoming wide-field surveys such as Pan-STARRS, LSST, and Skymapper
  will detect large numbers of objects that vary photometrically,
  or that move. These objects will include small bodies in the solar
  systema, eclipsing binary stars, transiting extrasolar planets,
  pulsating stars, dwarf novae, novae, supernovae, active galactic
  nuclei, and quite possibly other transient phenomena for which we
  have no names as yet. Although they will be a fertile source of such
  transient detections, wide-field surveys themselves ordinarily will
  have neither the observing cadence nor the (e.g., spectroscopic)
  observing capabilities to perform adequate follow-up observations of
  these variable objects. The Las Cumbres Observatory Global Telescope
  (LCOGT) will be a global network of moderate-aperture (2m and smaller)
  telescopes, instrumented and interconnected so as to <P />facilitate
  such in-depth variability studies. <P />The LCOGT now operates the
  two 2m Faulkes Telescopes: FT North located on the island of Maui,
  and FT South at the Siding Spring site in Australia. These telescopes
  will anchor a network of about 7 clusters of 1m-class telescopes,
  each cluster containing 4 telescopes. First-light instruments will
  provide visible-light and NIR imaging; spectroscopic capabilities
  will come later, and will likely include both low- and high-resolution
  visible-light spectrographs. Scheduling and coordination of observations
  will be provided from a central site, in pursuit of a single set of
  scientific goals.

Title: New Constraints on the Escape Fraction at z 1
Authors: Siana, Brian D.; Teplitz, H. I.; Colbert, J.; Ferguson,
   H. C.; Brown, T. M.; Conselice, C. J.; de Mello, D. F.; Dickinson,
   M.; Gardner, J. P.; Giavalisco, M.; Menantau, F.
Bibcode: 2007AAS...20925205S
Altcode: 2007BAAS...39Q.273S
  We examine deep far-ultraviolet imaging (m_AB(1600 Å) &lt; 29) of the
  Hubble Deep Field-North (HDF-N) and the Hubble Ultra Deep Field (UDF)
  to search for escaping Lyman continuum radiation from star-forming
  galaxies at z 1.3. Of the 20 galaxies sufficiently bright for possible
  detection in the far-UV, none are detected. Once the starburst age and
  intergalactic HI absorption are accounted for, we derive 3σ limits
  to the relative escape fractions between 0.16 &lt; f_esc,rel &lt; 1.0
  and a stacked limit of f_esc,rel &lt; 0.11. Our stacked limit is about
  equal to the average detected relative escape fraction at z 3 so deeper
  observations are required to determine if f_esc is evolving. We see no
  indication of any galaxies with a relative escape fraction near unity,
  as seen in individual z 3 galaxies in deep spectroscopic studies. The
  difference may be attributed to luminosity differences in the samples
  or due to the different regions of the Lyman continuum that are observed
  (700 Å for our study and 900 Å with spectroscopy at z 3).

Title: The Complementary Roles of Interferometry and Asteroseismology
    in Determining the Mass of Solar-Type Stars
Authors: Creevey, O. L.; Monteiro, M. J. P. F. G.; Metcalfe, T. S.;
   Brown, T. M.; Jiménez-Reyes, S. J.; Belmonte, J. A.
Bibcode: 2007ApJ...659..616C
Altcode: 2007astro.ph..2270C
  How important is an independent diameter measurement for the
  determination of stellar parameters of solar-type stars? When coupled
  with seismic observables, how well can we determine the stellar mass? If
  we can determine the radius of the star to between 1% and 4%, how does
  this affect the theoretical uncertainties? Interferometry can provide
  an independent radius determination, and it has been suggested that
  we should expect at least a 4% precision on such a measurement for
  nearby solar-type stars. This study aims to provide both qualitative
  and quantitative answers to these questions for a star, such as our Sun,
  where seismic information will be available. We show that the importance
  of an independent radius measurement depends on the combination of
  observables available and the size of the measurement errors. It is
  important for determining all stellar parameters and in particular the
  mass, where a good radius measurement can even allow us to determine
  the mass with a precision better than 2%. Our results also show that
  measuring the small frequency separation δν significantly improves
  the determination of the evolutionary stage τ and the mixing-length
  parameter α.

Title: When Extrasolar Planets Transit Their Parent Stars
Authors: Charbonneau, D.; Brown, T. M.; Burrows, A.; Laughlin, G.
Bibcode: 2007prpl.conf..701C
Altcode: 2006astro.ph..3376C
  When extrasolar planets are observed to transit their parent stars,
  we are granted unprecedented access to their physical properties. It
  is only for transiting planets that we are permitted direct estimates
  of the planetary masses and radii, which provide the fundamental
  constraints on models of their physical structure. In particular,
  precise determination of the radius may indicate the presence (or
  absence) of a core of solid material, which in turn would speak to the
  canonical formation model of gas accretion onto a core of ice and rock
  embedded in a protoplanetary disk. Furthermore, the radii of planets in
  close proximity to their stars are affected by tidal effects and the
  intense stellar radiation. As a result, some of these "hot Jupiters"
  are significantly larger than Jupiter in radius. Precision follow-up
  studies of such objects (notably with the spacebased platforms of the
  Hubble and Spitzer Space Telescopes) have enabled direct observation
  of their transmission spectra and emitted radiation. These data
  provide the first observational constraints on atmospheric models of
  these extrasolar gas giants, and permit a direct comparison with the
  gas giants of the solar system. Despite significant observational
  challenges, numerous transit surveys and quick-look radial velocity
  surveys are active, and promise to deliver an ever-increasing number
  of these precious objects. The detection of transits of short-period
  Neptune-sized objects, whose existence was recently uncovered by the
  radialvelocity surveys, is eagerly anticipated. Ultraprecise photometry
  enabled by upcoming space missions offers the prospect of the first
  detection of an extrasolar Earth-like planet in the habitable zone of
  its parent star, just in time for Protostars and Planets VI.

Title: Using Stellar Limb-Darkening to Refine the Properties of
    HD 209458b
Authors: Knutson, Heather A.; Charbonneau, David; Noyes, Robert W.;
   Brown, Timothy M.; Gilliland, Ronald L.
Bibcode: 2007ApJ...655..564K
Altcode: 2006astro.ph..3542K
  We use multiband photometry to refine estimates for the planetary
  radius and orbital inclination of the transiting planet system HD
  209458. We gathered 1066 spectra over four distinct transits with the
  STIS spectrometer on the Hubble Space Telescope using two gratings
  with a resolution R=1500 and a combined wavelength range of 290-1030
  nm. We divide the spectra into 10 spectrophotometric bandpasses,
  five for each grating, of equal wavelength span within each grating,
  and fit a transit curve over all bandpasses simultaneously. In our fit
  we use theoretical values for the stellar limb-darkening to further
  constrain the planetary radius. We find that the radius of HD 209458b is
  (1.320+/-0.025)R<SUB>Jup</SUB>, which is a factor of 2 more precise
  than current estimates. We also obtain improved estimates for the
  orbital period P and time of center of transit T<SUB>C</SUB>. Although
  in principle the photon-limited precision of the STIS data should allow
  us to measure the timing of individual transits to a precision of 2-7 s,
  we find that uncertainties in the stellar limb-darkening coefficients
  and residual noise in the data degrade these measurements to a typical
  precision of +/-14 s. Within this level of error, we find no significant
  variations in the timing of the eight events examined in this work.

Title: Report of the Working Group on Detection Methods
Authors: Brown, T. M.; de Medeiros, J. -R.
Bibcode: 2006psps.conf..227B
Altcode:
  No abstract at ADS

Title: Keck/Deimos Spectroscopy of Distant M31 fields with Deep
    HST Imaging
Authors: Rich, Robert M.; Brown, T. M.; Reitzel, D. B.; Ferguson,
   H.; Koch, A.; Smith, E.; Guhathakurta, P.; Kalirai, J.; Renzini, A.;
   Kimble, R.; Sweigart, A.; Gilbert, K.; Chiba, M.; Iye, M.; Komiyama,
   Y.; Tanaka, M.
Bibcode: 2006AAS...20917708R
Altcode: 2006BAAS...38.1155R
  We are undertaking a program to obtain the radial velocities and
  abundances of red giants in the vicinity of M31 fields with deep HST
  imaging. Our goal is to obtain complementary spectroscopy for fields
  at 22 and 35 kpc on the minor axis, where the M31 halo may be in a
  transition in metallicity and surface brightness from relatively metal
  rich and intermediate age, to metal poor and old. We will describe
  existing deep M31 fields with Keck spectroscopy and HST imaging and
  compare our findings with observations in other M31 deep fields.

Title: Las Cumbres Observatory Global Telescope Network: Keeping
    Education in the Dark
Authors: Ross, Rachel J.; Geibink, W.; Rosing, W. E.; Brown, T. M.
Bibcode: 2006AAS...20921803R
Altcode: 2006BAAS...38.1199R
  The Las Cumbres Observatory Global Telescope Network is a privately
  funded, non-profit organization that is constructing two overlapping
  networks of robotic telescopes for scientific and educational uses. The
  educational network will consist of at least thirty 0.4 1.0 meter
  telescopes that will be longitudinally spaced around the world so
  that there will always be at least one (more likely several) in the
  dark at any given time. All will be equipped with high quality CCD
  imagers, with the 1.0 meters having spectrographs and possible infrared
  capabilities. All networked telescopes will have identical, completely
  online interfaces that allow you to control the telescope and use
  different imaging instruments in either real-time or queued modes. Any
  registered school or group will have the capability to remotely observe
  using a telescope that is currently in the dark from the comfort of
  their classroom or science center, half a world away. Accompanying the
  robotic observations will be a library of resources and activities that
  will be usable in the formal classroom setting, informal groups and
  clubs, and for public outreach in the community for all age-groups
  and levels of science. Using the LCOGT network as a tool to enjoy
  real astronomical research will not only create a new awareness for
  science and technology, but also create connections between science
  and humanities. We aim to always keep astronomy education in the dark.

Title: LCOGT.net: A Global Telescope Network to Keep Astronomers in
    the Dark
Authors: Taylor, Stuart F.; Brown, T. M.; Rosing, W.; Ross, R.;
   Farrell, J.
Bibcode: 2006AAS...209.2213T
Altcode: 2006BAAS...38..930T
  The Las Cumbres Observatory Global Telescope is a privately supported
  planned network of medium-sized (2m) telescopes, longitudinally located
  to "keep you in the dark all of the time''. The observatory is in
  the process of completing major upgrades to its two 2m telescopes,
  FTN and FTS. These are the two telescopes that have been completed,
  among the nearly identical telescopes that will eventually form
  a global network longitudinally distributed to provide continuous
  night-time coverage. The upgrades of FTN and FTS are intended to
  improve image quality and reduce noise from the CCD cameras. FTN and
  FTS are being fitted with new CCD cameras, work on the enclosures will
  provide improved thermal control, and a warping harness has been used
  to reduce the astigmatism of the FTN secondary. We are in the process
  of evaluating the impact of these improvements on the performance of
  our telescopes.

Title: TrES-2: The First Transiting Planet in the Kepler Field
Authors: O'Donovan, Francis T.; Charbonneau, David; Mandushev,
   Georgi; Dunham, Edward W.; Latham, David W.; Torres, Guillermo;
   Sozzetti, Alessandro; Brown, Timothy M.; Trauger, John T.; Belmonte,
   Juan A.; Rabus, Markus; Almenara, José M.; Alonso, Roi; Deeg, Hans
   J.; Esquerdo, Gilbert A.; Falco, Emilio E.; Hillenbrand, Lynne A.;
   Roussanova, Anna; Stefanik, Robert P.; Winn, Joshua N.
Bibcode: 2006ApJ...651L..61O
Altcode: 2006astro.ph..9335O
  We announce the discovery of the second transiting hot Jupiter
  discovered by the Trans-atlantic Exoplanet Survey. The
  planet, which we dub TrES-2, orbits the nearby star GSC
  03549-02811 every 2.47063 days. From high-resolution spectra,
  we determine that the star has T<SUB>eff</SUB>=5960+/-100 K and
  logg=4.4+/-0.2, implying a spectral type of G0 V and a mass of
  1.08<SUP>+0.11</SUP><SUB>-0.05</SUB> M<SUB>solar</SUB>. High-precision
  radial velocity measurements confirm a sinusoidal variation with
  the period and phase predicted by the photometry, and rule out the
  presence of line bisector variations that would indicate that the
  spectroscopic orbit is spurious. We estimate a planetary mass
  of 1.28<SUP>+0.09</SUP><SUB>-0.04</SUB>M<SUB>Jup</SUB>. We
  model B, r, R, and I photometric time series of
  the 1.4% deep transits and find a planetary radius of
  1.24<SUP>+0.09</SUP><SUB>-0.06</SUB>R<SUB>Jup</SUB>. This planet lies
  within the field of view of the NASA Kepler mission, ensuring that
  hundreds of upcoming transits will be monitored with exquisite precision
  and permitting a host of unprecedented investigations. <P />Some of
  the data presented herein were obtained at the W. M. Keck Observatory,
  which is operated as a scientific partnership among Caltech, the
  University of California, and NASA. The Observatory was made possible
  by the generous financial support of the W. M. Keck Foundation.

Title: Transiting extrasolar planetary candidates in the Galactic
    bulge
Authors: Sahu, Kailash C.; Casertano, Stefano; Bond, Howard E.;
   Valenti, Jeff; Ed Smith, T.; Minniti, Dante; Zoccali, Manuela;
   Livio, Mario; Panagia, Nino; Piskunov, Nikolai; Brown, Thomas M.;
   Brown, Timothy; Renzini, Alvio; Rich, R. Michael; Clarkson, Will;
   Lubow, Stephen
Bibcode: 2006Natur.443..534S
Altcode: 2006astro.ph.10098S
  More than 200 extrasolar planets have been discovered around relatively
  nearby stars, primarily through the Doppler line shifts owing to reflex
  motions of their host stars, and more recently through transits of
  some planets across the faces of the host stars. The detection of
  planets with the shortest known periods, 1.2-2.5 days, has mainly
  resulted from transit surveys which have generally targeted stars
  more massive than 0.75M<SUB>solar</SUB>, where M<SUB>solar</SUB>
  is the mass of the Sun. Here we report the results from a planetary
  transit search performed in a rich stellar field towards the Galactic
  bulge. We discovered 16 candidates with orbital periods between
  0.4 and 4.2 days, five of which orbit stars of masses in the range
  0.44-0.75M<SUB>solar</SUB>. In two cases, radial-velocity measurements
  support the planetary nature of the companions. Five candidates
  have orbital periods below 1.0 day, constituting a new class of
  ultra-short-period planets, which occur only around stars of less than
  0.88M<SUB>solar</SUB>. This indicates that those orbiting very close
  to more-luminous stars might be evaporatively destroyed or that jovian
  planets around stars of lower mass might migrate to smaller radii.

Title: The complementary roles of interferometry and asteroseismology
Authors: Creevey, O. L.; Monteiro, M. J. P. F. G.; Metcalfe, T. S.;
   Brown, T. M.
Bibcode: 2006ESASP.624E.114C
Altcode: 2006soho...18E.114C
  How important is an independent diameter measurement for the
  determination of stellar parameters of a solar-type star? If we can
  determine the radius of the star to between 1% and 4% how does this
  effect the theoretical uncertainties? Interferometry can provide this
  independent measurement and it has been suggested that we should expect
  at least a 4% precision on this measurement for solartype stars. This
  study aims to provide both qualitive and quantitive answers to the
  posed questions for a star such as our sun, one to which seismology
  can be applied. We find that the radius is fundamental for the
  determination of all stellar parameters and in particular the mass
  and the initial hydrogen abundance. Its influence depends not only
  on the size of the error in the radius but also on the errors in the
  seismic observables. The combination of observables available is also
  important for determining how influential the radius measurement can be.

Title: Kepler Mission: Mission Progress
Authors: Borucki, William J.; Koch, D. G.; Lissauer, J. J.; Basri,
   G. S.; Caldwell, D. A.; DeVore, E.; Jenkins, J. M.; Caldwell, J. J.;
   Christensen-Dalsgaard, J.; Cochran, W. D.; Dunham, E. W.; Gautier,
   T. N.; Geary, J. C.; Latham, D. A.; Sasselov, D.; Gilliland, R. L.;
   Gould, A.; Howell, S. B.; Brown, T. M.; Kondo, Y.; Monet, D. G.;
   Batalha, N.
Bibcode: 2006DPS....38.4501B
Altcode: 2006BAAS...38..567B
  Kepler is a Discovery-class mission designed to determine the
  frequency of Earth-size planets in and near the habitable zone (HZ)
  of solar-like stars. The instrument consists of a 0.95 m aperture
  photometer designed to obtain high precision photometric measurements
  of &gt;100,000 stars to search for patterns of transits. The focal
  plane of the Schmidt-telescope contains 42 CCDs with a total of 96
  megapixels that cover 100 square degrees of sky. <P />Both the Schmidt
  corrector and 1.4 m aperture primary mirror have been fabricated and
  polished. All 50 CCD detectors have been delivered, tested and found to
  perform better than required, and are now being mounted in modules to be
  installed in the focal plane. Measurements of the ability of the first
  module to detect transit amplitudes expected from Earth-size planets
  are scheduled to start this month. A preliminary catalog classifying
  11 million stars in the FOV has been produced. The science descope
  that replaced the articulated antenna with a body-fixed antenna still
  provides performance above the baseline design. A concise description of
  the current mission design and expected science results are presented.

Title: Far-Ultraviolet Imaging of the Hubble Deep Field-North:
    Star Formation in Normal Galaxies at z&lt;1
Authors: Teplitz, H. I.; Siana, B.; Brown, T. M.; Chary, R.; Colbert,
   J. W.; Conselice, C. J.; de Mello, D. F.; Dickinson, M.; Ferguson,
   H. C.; Gardner, Jonathan P.; Menanteau, F.
Bibcode: 2006AJ....132..853T
Altcode: 2006astro.ph..6244T
  We present far-ultraviolet (FUV) imaging of the Hubble Deep Field-North
  (HDF-N) taken with the Solar Blind Channel of the Advanced Camera for
  Surveys (ACS SBC) and the FUV MAMA detector of the Space Telescope
  Imaging Spectrograph onboard the Hubble Space Telescope. The full
  WFPC2 deep field has been observed at 1600 Å. We detect 134 galaxies
  and one star down to a limit of FUV<SUB>AB</SUB>~29. All sources
  have counterparts in the WFPC2 image. Redshifts (spectroscopic or
  photometric) for the detected sources are in the range 0&lt;z&lt;1. We
  find that the FUV galaxy number counts are higher than those reported
  by GALEX, which we attribute at least in part to cosmic variance in the
  small HDF-N field of view. Six of the 13 Chandra sources at z&lt;0.85
  in the HDF-N are detected in the FUV, and those are consistent with
  starbursts rather than active galactic nuclei. Cross-correlating with
  Spitzer sources in the field, we find that the FUV detections show
  general agreement with the expected L<SUB>IR</SUB>/L<SUB>UV</SUB>
  versus β relationship. We infer star formation rates (SFRs),
  corrected for extinction using the UV slope, and find a median value
  of 0.3 M<SUB>solar</SUB> yr<SUP>-1</SUP> for FUV-detected galaxies,
  with 75% of detected sources having SFR&lt;1 M<SUB>solar</SUB>
  yr<SUP>-1</SUP>. Examining the morphological distribution of sources,
  we find that about half of all FUV-detected sources are identified as
  spiral galaxies. Half of morphologically selected spheroid galaxies
  at z&lt;0.85 are detected in the FUV, suggesting that such sources
  have had significant ongoing star formation in the epoch since z~1. <P
  />Based on observations made with the NASA/ESA Hubble Space Telescope,
  obtained from the Space Telescope Science Institute, which is operated
  by the Association of Universities for Research in Astronomy (AURA),
  Inc., under NASA contract NAS5-26555. These observations are associated
  with proposals 7410 and 9478.

Title: Does the Line of Sight to M5 Intersect a Highly-Ionized
    High-Velocity Cloud?
Authors: Dixon, W. V.; Brown, T. M.; Howk, J. C.; Landsman, W. B.
Bibcode: 2006ASPC..348..218D
Altcode:
  FUSE and HST/STIS observations of the post-asymptotic giant branch
  (PAGB) star ZNG 1 in the globular cluster M5 (NGC 5904) reveal
  high-velocity absorption in O VI, C IV, Si IV, and other species. With
  LSR velocities between -150 and -100 km s<SUP>-1</SUP>, this complex of
  absorbing components is blue-shifted by roughly -180 km s<SUP>-1</SUP>
  relative to the stellar photosphere. The absorption represents either
  circumstellar material (e.g., gas ejected during the star's AGB
  phase and now shock-heated by the fast PAGB wind) or a high-ionization
  high-velocity cloud (HVC) along the line of sight to M5. If the latter,
  it would be the first evidence that highly-ionized HVCs may be found
  near the Galactic disk.

Title: Rejecting Astrophysical False Positives from the TrES
Transiting Planet Survey: The Example of GSC 03885-00829
Authors: O'Donovan, Francis T.; Charbonneau, David; Torres, Guillermo;
   Mandushev, Georgi; Dunham, Edward W.; Latham, David W.; Alonso, Roi;
   Brown, Timothy M.; Esquerdo, Gilbert A.; Everett, Mark E.; Creevey,
   Orlagh L.
Bibcode: 2006ApJ...644.1237O
Altcode: 2006astro.ph..3005O
  Ground-based wide-field surveys for nearby transiting gas giants are
  yielding far fewer true planets than astrophysical false positives, some
  of which are difficult to reject. Recent experience has highlighted
  the need for careful analysis to eliminate astronomical systems in
  which light from a faint eclipsing binary is blended with that from a
  bright star. During the course of the Transatlantic Exoplanet Survey,
  we identified a system presenting a transit-like periodic signal. We
  obtained the proper motion and infrared color of this target (GSC
  03885-00829) from publicly available catalogs, which suggested this
  star is an F dwarf, supporting our transit hypothesis. This spectral
  classification was confirmed using spectroscopic observations from which
  we determined the stellar radial velocity. The star did not exhibit
  any signs of a stellar mass companion. However, subsequent multicolor
  photometry displayed a color-dependent transit depth, indicating that a
  blend was the likely source of the eclipse. We successfully modeled our
  initial photometric observations of GSC 03885-00829 as the light from
  a K dwarf binary system superimposed on the light from a late F dwarf
  star. High-dispersion spectroscopy confirmed the presence of light from
  a cool stellar photosphere in the spectrum of this system. With this
  candidate, we demonstrate both the difficulty in identifying certain
  types of false positives in a list of candidate transiting planets and
  our procedure for rejecting these imposters, which may be useful to
  other groups performing wide-field transit surveys. <P />Some of the
  data presented herein were obtained at the W. M. Keck Observatory,
  which is operated as a scientific partnership among the California
  Institute of Technology, the University of California, and the National
  Aeronautics and Space Administration. The Observatory was made possible
  by the generous financial support of the W.M. Keck Foundation.

Title: Keeping Astronomy in the Dark Around the Clock: Introducing
    LCOGT.net
Authors: Brown, Timothy M.; Taylor, S. F.; Rosing, W.; Mann, R.;
   Trimble, V.; Farrell, J. A.
Bibcode: 2006AAS...208.5605B
Altcode: 2006BAAS...38..136B
  The Las Cumbres Observatory Global Telescope is a privately supported
  planned network of medium-sized (2m) telescopes, longitudinally
  located to "keep you in the dark all of the time". Since it will be
  able to perform continuous optical observations unbroken by the usual
  day/night cycle, LCOGT will have a capability to do astronomy in the
  24+ hour time-domain, a function that does not currently exist in
  a manner dedicated to doing time-varying astronomy. By having such
  telescopes distributed in northern- and southern-hemisphere sets of
  nearly-identical facilities, LCOGT will also have a uniqe ability to
  perform target-of-opportunity observing. Finally, LCOGT will have
  sufficient telescope time to address a small number of key science
  questions that require large observing resources. A major educational
  outreach effort will accompany LCOGT science, building upon the
  educational work started by the Dill Faulkes Foundation.

Title: Interested in observing TrES-Her0-07621?
Authors: Creevey, O. L.; Brown, T. M.; Jiménez-Reyes, S.; Belmonte,
   J. A.
Bibcode: 2006ASPC..349..387C
Altcode: 2006astro.ph..5176C
  TrES-Her0-07621 is a recently discovered detached M Dwarf eclipsing
  binary system. We present some follow-up observations of this system
  including new minima times and a refined orbital period. We have also
  obtained better estimates of the stellar radii and inclination.

Title: Understanding the Relationship between Observations and
    Stellar Parameters in an Eclipsing Binary System
Authors: Creevey, O. L.; Brown, T. M.; Jiménez-Reyes, S.; Belmonte,
   J. A.
Bibcode: 2006ASPC..349..211C
Altcode: 2006astro.ph..5177C
  We investigate the information contained in observations and to what
  extent each of them contributes individually to constraining the
  physical parameters of the system we are investigating. To do this, we
  present a study involving the technique of Singular Value Decomposition
  using as a simple example a detached eclipsing binary system. We intend
  to apply an extension of this technique to asteroseismic measurements
  of Delta Scuti stars that are members of eclipsing binary systems.

Title: The Kepler Mission: A Transit-Photometry Mission to Discover
    Terrestrial Planets
Authors: Borucki, William J.; Koch, David; Basri, Gibor; Brown,
   Timothy; Caldwell, Douglas; Devore, Edna; Dunham, Edward; Gautier,
   Thomas; Geary, John; Gilliland, Ronald; Gould, Alan; Howell, Steve;
   Jenkins, Jon
Bibcode: 2006ISSIR...6..207B
Altcode:
  The Kepler Mission is a NASA Discovery-class mission designed to
  continuously monitor the brightness of 100,000 main sequence stars
  to detect the transit of Earth-size and larger planets. It is a wide
  field of view photometer with a Schmidt-type telescope and an array
  of 42 CCDs covering the 100 sq. degree field-of-view (FOV). It has
  a 0.95 m aperture and a 1.4 m primary and is designed to attain a
  photometric precision of 20 parts per million (ppm) for 12th magnitude
  solar-like stars for a 6.5-hour transit duration. It will continuously
  observe 100,000 main sequence stars from 9th to 15th magnitude in the
  Cygnus constellation for a period of four years with a cadence of
  4 measurements per hour. Kepler is Discovery Mission #10 and is on
  schedule for launch in 2007 into heliocentric orbit. A ground-based
  program to classify all 450,000 stars brighter than 15th magnitude
  in the FOV and to conduct a detailed examination of a subset of
  the stars that show planetary companions is also planned. Hundreds
  of Earth-size planets should be detected if they are common around
  solarlike stars. Ground-based spectrometric observations of those stars
  with planetary companions will be made to determine the dependences of
  the frequency and size of terrestrial planets on stellar characteristics
  such as type and metallicity. A null result would imply that terrestrial
  planets are rare.

Title: Report of the Working Group on Detection Methods
Authors: Brown, T. M.; de Medeiros, J. -R.
Bibcode: 2006ISSIR...6..227B
Altcode:
  A group of about fifteen interested scientists spent two long sessions
  discussing issues related to detecting extrasolar planets, particularly
  ones of roughly terrestrial size. We arrived at several recommendations,
  principally: (1) Radial velocity measurement precision should be pushed
  to its limits, presumably those set by the astrophysics of stars. (2)
  Data policies for upcoming planet-finding space missions must be
  written so they do not encourage premature or mistaken discovery
  announcements. (3) Ground-based transit searches would benefit
  enormously if some adequately-funded institution would take the lead in
  fielding a coherent and well-engineered world-wide network of telescopes
  for this purpose. We should attempt to build international consensus
  and support for this idea.

Title: Star Classification for the Kepler Input Catalog: From Images
    to Stellar Parameters
Authors: Brown, T. M.; Everett, M.; Latham, D. W.; Monet, D. G.
Bibcode: 2005AAS...20711012B
Altcode: 2005BAAS...37.1340B
  The Stellar Classification Project is a ground-based effort to
  screen stars within the Kepler field of view, to allow removal
  of stars with large radii (and small potential transit signals)
  from the target list. Important components of this process are: (1)
  An automated photometry pipeline estimates observed magnitudes both
  for target stars and for stars in several calibration fields. (2)
  Data from calibration fields yield extinction-corrected AB magnitudes
  (with g, r, i, z magnitudes transformed to the SDSS system). We merge
  these with 2MASS J, H, K magnitudes. (3) The Basel grid of stellar
  atmosphere models yields synthetic colors, which are transformed to
  our photometric system by calibration against observations of stars in
  M67. (4) We combine the r magnitude and stellar galactic latitude with a
  simple model of interstellar extinction to derive a relation connecting
  {Teff, luminosity} to distance and reddening. For models satisfying
  this relation, we compute a chi-squared statistic describing the match
  between each model and the observed colors. (5) We create a merit
  function based on the chi-squared statistic, and on a Bayesian prior
  probability distribution which gives probability as a function of Teff,
  luminosity, log(Z), and height above the galactic plane. The stellar
  parameters ascribed to a star are those of the model that maximizes
  this merit function. (6) Parameter estimates are merged with positional
  and other information from extant catalogs to yield the Kepler Input
  Catalog, from which targets will be chosen. Testing and validation of
  this procedure are underway, with encouraging initial results.

Title: Kepler Mission Design
Authors: Koch, D. G.; Borucki, W. J.; Lissauer, J. J.; Basri, G. S.;
   Gould, A. D.; Brown, T. M.; Caldwell, D. A.; DeVore, E. K.; Jenkins,
   J. M.; Christensen-Dalsgaard, J.; Cochran, W. D.; Dunham, E. W.;
   Gautier, T. N.; Geary, J. C.; Latham, D. W.; Gilliland, R. L.; Kondo,
   Y.; Monet, D. G.
Bibcode: 2005AAS...20711009K
Altcode: 2005BAAS...37.1339K
  The Kepler Mission is in the development phase with launch planned for
  2008. The mission goal is to reliably detect a significant number of
  Earth-size and smaller planets in the habitable zone of solar-like
  stars. (see W. Borucki, et al, this meeting.) The mission design
  allows for exploring the diversity of planetary sizes and orbital
  periods for a wide variety of stellar spectral types, (see posters by
  D. Latham, et al and T. Brown, et al, this meeting on stellar catalog
  preparation). In this poster we describe the technical approach taken
  for the mission design; describing the flight and ground system, the
  detection methodology, the photometer design and capabilities, the way
  the data are taken and processed, the Guest Observer opportunity and
  the EPO aspects (see paper by E. DeVore, et al). Finally the detection
  capability in terms of planet size is presented as a function of
  planetary orbital period, mission duration, stellar type and combined
  differential photometric precision.

Title: The Violent History of Andromeda
Authors: Brown, T. M.; Smith, E.; Guhathakurta, P.; Rich, R. M.;
   Ferguson, H. C.; Renzini, A.; Sweigart, A. V.; Kimble, R. A.
Bibcode: 2005AAS...20713505B
Altcode: 2005BAAS...37R1387B
  Using the Advanced Camera for Surveys on the Hubble Space Telescope,
  Andromeda has now been imaged well below the main sequence turnoff
  in three structures: the spheroid, the outer disk, and the tidal
  stream. These data allow a complete reconstruction of the star formation
  histories in these structures. Although the disk is significantly
  different from the other two fields, the stream and spheroid look
  remarkably similar. Each of the fields has an extended star formation
  history that was largely finished approximately 5 Gyr ago. At the same
  time, other observing programs are providing important constraints on
  the spatial morphologies and kinematics of these structures. Taken
  together, the extant data suggest a violent history in Andromeda,
  with significant disruption of the disk population into the outskirts
  of the galaxy.

Title: HST Far-Ultraviolet Imaging of the Hubble Ultra Deep Field
Authors: Siana, B. D.; Teplitz, H. I.; Chary, R.; Colbert, J. W.;
   Brown, T. M.; de Mello, D. F.; Ferguson, H. C.; Conselice, C.; Gardner,
   J. P.; Menanteau, F.; Dickinson, M. E.
Bibcode: 2005AAS...207.2205S
Altcode: 2005BAAS...37.1193S
  We present far-UV (1500Å) imaging of the Ultra Deep Field (UDF)
  taken with the Solar Blind Channel of the Advanced Camera for Surveys
  (ACS/SBC) on HST. Combined with data from a previous campaign covering
  the Hubble Deep Field North (HDF-N), we detect more than 200 galaxies
  over 12 arcmin<SUP>2</SUP> with Far-UV mags to m(AB)=29. The derived
  number counts extend nearly four magnitudes fainter than the GALEX
  ultra-deep fields. We use Spitzer infrared photometry from the GOODS
  Legacy survey to examine the F(IR)/F(UV) vs. β relation. We find
  that this relation, although derived with a local sample, holds
  for starburst galaxies at moderate redshift between 0.3-0.9. We
  detect about half of all morphologically selected ellipticals with
  z&lt;0.8, indicating significant ongoing star-formation at z&lt;1 in
  this population. Furthermore, our detection rate of ellipticals is
  correlated with their dispersion in optical color across the galaxy
  with nearly all of the "blue core" ellipticals (δ (V-I)&gt;0.05)
  detected in the far-UV.

Title: A ∼7.5 Earth-Mass Planet Orbiting the Nearby Star, GJ 876
Authors: Rivera, E. J.; Lissauer, J. J.; Butler, R. P.; Marcy, G. W.;
   Vogt, S. S.; Fischer, D. A.; Brown, T. M.; Laughlin, G.; Henry, G. W.
Bibcode: 2005AAS...20719103R
Altcode: 2005BAAS...37Q1487R
  High precision, high cadence radial velocity monitoring over the past
  8 years at the W. M. Keck Observatory reveals evidence for a third
  planet orbiting the nearby (4.69 pc) dM4 star GJ 876. The residuals
  of three-body Newtonian fits, which include GJ 876 and Jupiter mass
  companions b and c, show significant power at a periodicity of 1.9379
  days. Self-consistently fitting the radial velocity data with a model
  that includes an additional body with this period significantly
  improves the quality of the fit. These four-body (three-planet)
  Newtonian fits find that the minimum mass of companion ``d'' is m
  sin {i}=5.89 ± 0.54 M<SUB>⊕ </SUB> and that its orbital period is
  1.93776 (± 7×10<SUP>-5</SUP>) days. Assuming coplanar orbits, an
  inclination of the GJ 876 planetary system to the plane of the sky of
  ∼50<SUP>o</SUP> gives the best fit. This inclination yields a mass
  for companion d of m=7.53 ± 0.70 M<SUB>⊕ </SUB>, making it by far
  the lowest mass companion yet found around a main sequence star other
  than our Sun. Precise photometric observations at Fairborn Observatory
  confirm low-level brightness variability in GJ 876 and provide the first
  explicit determination of the star's 96.7-day rotation period. Even
  higher precision short-term photometric measurements obtained at Las
  Campanas imply that planet d does not transit GJ 876.

Title: The Kepler Input Catalog
Authors: Latham, D. W.; Brown, T. M.; Monet, D. G.; Everett, M.;
   Esquerdo, G. A.; Hergenrother, C. W.
Bibcode: 2005AAS...20711013L
Altcode: 2005BAAS...37.1340L
  The Kepler mission will monitor 170,000 planet-search targets during
  the first year, and 100,000 after that. The Kepler Input Catalog (KIC)
  will be used to select optimum targets for the search for habitable
  earth-like transiting planets. The KIC will include all known catalogued
  stars in an area of about 177 square degrees centered at RA 19:22:40 and
  Dec +44:30 (l=76.3 and b=+13.5). 2MASS photometry will be supplemented
  with new ground-based photometry obtained in the SDSS g, r, i, and z
  bands plus a custom filter centered on the Mg b lines, using KeplerCam
  on the 48-inch telescope at the Whipple Observatory on Mount Hopkins,
  Arizona. The photometry will be used to estimate stellar characteristics
  for all stars brighter than K 14.5 mag. The KIC will include effective
  temperature, surface gravity, metallicity, reddening, distance,
  and radius estimates for these stars. The CCD images are pipeline
  processed to produce instrumental magnitudes at PSI. The photometry
  is then archived and transformed to the SDSS system at HAO, where
  the astrophysical analysis of the stellar characteristics is carried
  out. The results are then merged with catalogued data at the USNOFS to
  produce the KIC. High dispersion spectroscopy with Hectochelle on the
  MMT will be used to supplement the information for many of the most
  interesting targets. The KIC will be released before launch for use by
  the astronomical community and will be available for queries over the
  internet. Support from the Kepler mission is gratefully acknowledged.

Title: A ~7.5 M<SUB>⊕</SUB> Planet Orbiting the Nearby Star, GJ 876
Authors: Rivera, Eugenio J.; Lissauer, Jack J.; Butler, R. Paul; Marcy,
   Geoffrey W.; Vogt, Steven S.; Fischer, Debra A.; Brown, Timothy M.;
   Laughlin, Gregory; Henry, Gregory W.
Bibcode: 2005ApJ...634..625R
Altcode: 2005astro.ph.10508R
  High-precision, high-cadence radial velocity monitoring over the
  past 8 yr at the W. M. Keck Observatory reveals evidence for a third
  planet orbiting the nearby (4.69 pc) dM4 star GJ 876. The residuals
  of three-body Newtonian fits, which include GJ 876 and Jupiter-mass
  companions b and c, show significant power at a periodicity of 1.9379
  days. Self-consistently fitting the radial velocity data with a model
  that includes an additional body with this period significantly
  improves the quality of the fit. These four-body (three-planet)
  Newtonian fits find that the minimum mass of companion ``d'' is
  msini=5.89+/-0.54 M<SUB>⊕</SUB> and that its orbital period is
  1.93776 (+/-7×10<SUP>-5</SUP>) days. Assuming coplanar orbits,
  an inclination of the GJ 876 planetary system to the plane of the
  sky of ~50° gives the best fit. This inclination yields a mass for
  companion d of m=7.53+/-0.70 M<SUB>⊕</SUB>, making it by far the
  lowest mass companion yet found around a main-sequence star other
  than our Sun. Precise photometric observations at Fairborn Observatory
  confirm low-level brightness variability in GJ 876 and provide the first
  explicit determination of the star's 96.7 day rotation period. Even
  higher precision short-term photometric measurements obtained at Las
  Campanas imply that planet d does not transit GJ 876. <P />Based on
  observations obtained at the W. M. Keck Observatory, which is operated
  jointly by the University of California and the California Institute
  of Technology.

Title: Halos of Spiral Galaxies. II. Halo Metallicity-Luminosity
    Relation
Authors: Mouhcine, M.; Ferguson, H. C.; Rich, R. M.; Brown, T. M.;
   Smith, T. E.
Bibcode: 2005ApJ...633..821M
Altcode: 2005astro.ph.10254M
  Using the Hubble Space Telescope, we have resolved individual red giant
  branch stars in the halos of eight nearby spiral galaxies. The fields
  lie at projected distances between 2 and 13 kpc along the galaxies'
  minor axes. The data set allows a first look at the systematic trends
  in halo stellar populations. We have found that bright galaxies tend to
  have broad red giant branch star color distributions with redder mean
  colors, suggesting that the heavy-element abundance spread increases
  with the parent galaxy luminosity. The mean metallicity of the stellar
  halo, estimated using the mean colors of red giant branch stars,
  correlates with the parent galaxy luminosity. The metallicity of the
  Milky Way halo falls nearly 1 dex below this luminosity-metallicity
  relation, suggesting that the halo of the Galaxy is more the exception
  than the rule for spiral galaxies; i.e., massive spirals with metal-poor
  halos are unusual. The luminosity-halo stellar abundance relation
  is consistent with the scaling relation expected for stellar systems
  embedded in dominant halos, suggesting that the bulk of the halo stellar
  population may have formed in situ. <P />Based on observations with
  the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope
  Science Institute, which is operated by the Association of Universities
  for Research in Astronomy, Inc., under NASA contract NAS 5-26555.

Title: Halos of Spiral Galaxies. III. Metallicity Distributions
Authors: Mouhcine, M.; Rich, R. M.; Ferguson, H. C.; Brown, T. M.;
   Smith, T. E.
Bibcode: 2005ApJ...633..828M
Altcode: 2005astro.ph.10255M
  We report results of a campaign to image the stellar populations
  in the halos of highly inclined spiral galaxies, with the fields
  roughly 10 kpc (projected) from the nuclei. We use the F814W (I) and
  F606W (V) filters in the Wide Field Planetary Camera 2 on board the
  Hubble Space Telescope. We unambiguously resolve the stellar halos
  1 to 2 mag fainter than the tip of the red giant branch. Extended
  halo populations are detected in all galaxies. The color-magnitude
  diagrams appear to be completely dominated by giant branch stars,
  with no evidence for the presence of young stellar populations in any
  of the fields. The metallicity distribution function for the galaxy
  sample is derived from interpolation within an extensive grid of red
  giant branch loci. These loci are derived from theoretical sequences
  that are calibrated using the Galactic globular clusters and from
  empirical sequences for metal-rich stellar populations. We find that
  the metallicity distribution functions are dominated by metal-rich
  populations, with a tail extending toward the metal-poor end. To first
  order, the overall shapes of the metallicity distribution functions
  are similar to what is predicted by a simple, single-component model
  of chemical evolution with the effective yields increasing with galaxy
  luminosity. However, metallicity distributions significantly narrower
  than the simple model are observed for a few of the most luminous
  galaxies in the sample. The discrepancies are similar to those
  previously observed for NGC 5128, the halo of M31, and the Galactic
  bulge. Our observations can be used to help distinguish between
  models for the formation of spiral galaxies. It appears that more
  luminous spiral galaxies also have more metal-rich stellar halos. The
  increasingly significant departures from the closed-box model for
  the more luminous galaxies indicate that a parameter in addition
  to a single yield is required to describe chemical evolution. This
  parameter, which could be related to gas infall or outflow either
  in situ or in progenitor dwarf galaxies that later merge to form the
  stellar halo, tends to make the metallicity distributions narrower at
  high metallicity. <P />Based on observations with the NASA/ESA Hubble
  Space Telescope, obtained at the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in
  Astronomy, Inc., under NASA contract NAS 5-26555.

Title: Halos of Spiral Galaxies. I. The Tip of the Red Giant Branch
    as a Distance Indicator
Authors: Mouhcine, M.; Ferguson, H. C.; Rich, R. M.; Brown, T. M.;
   Smith, T. E.
Bibcode: 2005ApJ...633..810M
Altcode: 2005astro.ph.10253M
  We have imaged the halo populations of a sample of nearby spiral
  galaxies using the Wide Field Planetary Camera 2 on board the Hubble
  Space Telescope with the aim of studying the stellar population
  properties and relating them to those of the host galaxies. In four
  galaxies, the red giant branch is sufficiently well populated to measure
  the magnitude of the tip of the red giant branch (TRGB), a well-known
  distance indicator. Using both the Sobel edge-detection technique and
  maximum likelihood analysis to measure the I-band magnitude of the TRGB,
  we determine distances to four nearby galaxies: NGC 253, NGC 4244, NGC
  4945, and NGC 4258. For the first three galaxies, the TRGB distance is
  here determined more directly, and is likely to be more accurate, than
  previous distance estimates. In the case of NGC 4258, our TRGB distance
  is in good agreement with the geometrical maser distance, supporting the
  Large Magellanic Cloud distance modulus (m-M)<SUB>0</SUB>=18.50 that
  is generally adopted in recent estimates of the Hubble constant. <P
  />Based on observations with the NASA/ESA Hubble Space Telescope,
  obtained at the Space Telescope Science Institute, which is operated
  by the Association of Universities for Research in Astronomy, Inc.,
  under NASA contract NAS 5-26555.

Title: The Frequency of WFC3/IR Saturations
Authors: Brown, T. M.
Bibcode: 2005wfc..rept...28B
Altcode:
  The WFC3/IR channel will combine sensitivity with a wide field of view,
  such that all long exposures will contain some saturated stars, even
  in sparse fields near the Galactic poles. Because such saturations in
  IR detectors can result in persistence (particularly when a pixel is
  over-saturated by factors of 10 to 100), I quantify here the frequency
  of 1x, 10x, and 100x saturations, as a function of position on the
  sky. I use the 2MASS and GSC2 catalogs for this analysis, although each
  has its limitations for this purpose. Away from the Galactic plane,
  the greater depth of the GSC2 is required to quantify the frequency of
  moderate saturations (1-10x). If, however, one is only interested in
  extreme saturations (&gt;100x), the 2MASS catalog is more appropriate,
  because it is sufficiently deep for such sources and it avoids the
  large systematic errors (by factors of 200) that can arise due to an
  incorrect assumption of spectral type and extinction when extrapolating
  from the GSC2 optical bands into the IR. Both catalogs suffer from
  serious incompleteness in the Galactic plane, especially toward the
  Galactic center, but for such fields the 2MASS catalog would still be
  preferred over the GSC2 when checking for saturating objects.

Title: Thermal Emission from the Newest, Closest, and Brightest
    Transiting Planet
Authors: Charbonneau, David; Allen, Lori; Barman, Travis; Bouchy,
   Francois; Brown, Timothy; Mayor, Michel; Megeath, Tom; Moutou, Claire;
   Queloz, Didier; Udry, Stephane
Bibcode: 2005sptz.prop..261C
Altcode:
  We propose to observe the newly-discovered transiting-planet system
  HD 189733 during two times of secondary eclipse, corresponding to
  the passage of the planet behind the star. Of the 4 known transiting
  planets accessible to Spitzer, this object offers by far the greatest
  signal-to-noise ratio, owing to both the apparent brightness of the
  system and the favorable ratio of the planetary flux to that of the
  star. By measuring the planetary flux in 5 band passes (3.6, 4.5, 5.8,
  8.0, &amp; 24 um), we will directly constrain models of the planetary
  emission, which in turn should allow identification of the molecules
  that dominate its spectrum. Moreover, high-cadence observations with
  IRAC during times of ingress and egress may permit us to spatially
  resolve the planetary emission over the surface of the planet,
  providing an unprecedented probe of the dynamics of these strongly
  irradiated exoplanet atmospheres. These observations will firmly
  establish Spitzer as the primary observatory in the nascent field of
  comparative exoplanetology.

Title: A New Detached M Dwarf Eclipsing Binary
Authors: Creevey, O. L.; Benedict, G. F.; Brown, T. M.; Alonso,
   R.; Cargile, P.; Mandushev, G.; Charbonneau, D.; McArthur, B. E.;
   Cochran, W.; O'Donovan, F. T.; Jiménez-Reyes, S. J.; Belmonte, J. A.;
   Kolinski, D.
Bibcode: 2005ApJ...625L.127C
Altcode: 2005astro.ph..4490C
  We describe a newly discovered detached M dwarf eclipsing binary
  system. This system was first observed by the TrES network during a
  long-term photometry campaign of 54 nights. Analysis of the folded
  light curve indicates two very similar components orbiting each other
  with a period of 1.12079 +/- 0.00001 days. Spectroscopic observations
  with the Hobby-Eberly Telescope show the system to consist of two M3e
  dwarfs in a near-circular orbit. Double-line radial velocity amplitudes,
  combined with the orbital inclination derived from light-curve fitting,
  yield M<SUB>total</SUB> = 0.983 +/- 0.007 M<SUB>solar</SUB>, with
  component masses of M<SUB>1</SUB>=0.493+/-0.003 M<SUB>solar</SUB>
  and M<SUB>2</SUB>=0.489+/-0.003 M<SUB>solar</SUB>. The light-curve fit
  yields component radii of R<SUB>1</SUB>=0.453+/-0.060 R<SUB>solar</SUB>
  and R<SUB>2</SUB>=0.452+/-0.050 R<SUB>solar</SUB>. Although a precise
  parallax is lacking, broadband VJHK colors and spectral typing suggest
  component absolute magnitudes of M<SUB>V</SUB>(1)=11.18+/-0.30 and
  M<SUB>V</SUB>(2)=11.28+/-0.30.

Title: Results of WFC3 Thermal Vacuum Testing - IR Channel Ghosts
    &amp; Baffle Scatter
Authors: Brown, T. M.
Bibcode: 2005wfc..rept...22B
Altcode:
  During the Fall 2004 campaign of thermal-vacuum tests on WFC3, we looked
  for optical ghosts in the IR channel by imaging a saturated point source
  at various positions on the detector. For the F110W and F160W filters,
  34 positions were checked on and off the detector, while the remaining
  filters were checked at one position in each quadrant. Although the
  primary image was 10x oversaturated in these checks, no signs of
  optical ghosts were seen. In an additional test, we scanned a bright
  point source across the baffle edges, immediately outside of the IR
  field of view. These scans showed that strong scattering can occur from
  the baffle edge, especially along the upper baffle edge. The strongest
  glints from the baffle edge contained ~20% of the source flux and were
  spread over a large area of the detector. The baffle installation is
  under investigation.

Title: Detection of Thermal Emission from an Extrasolar Planet
Authors: Charbonneau, David; Allen, Lori E.; Megeath, S. Thomas;
   Torres, Guillermo; Alonso, Roi; Brown, Timothy M.; Gilliland, Ronald
   L.; Latham, David W.; Mandushev, Georgi; O'Donovan, Francis T.;
   Sozzetti, Alessandro
Bibcode: 2005ApJ...626..523C
Altcode: 2005astro.ph..3457C
  We present Spitzer Space Telescope infrared photometric time series
  of the transiting extrasolar planet system TrES-1. The data span a
  predicted time of secondary eclipse, corresponding to the passage of the
  planet behind the star. In both bands of our observations, we detect a
  flux decrement with a timing, amplitude, and duration as predicted by
  published parameters of the system. This signal represents the first
  direct detection of (i.e., the observation of photons emitted by) a
  planet orbiting another star. The observed eclipse depths (in units of
  relative flux) are 0.00066+/-0.00013 at 4.5 μm and 0.00225+/-0.00036
  at 8.0 μm. These estimates provide the first observational constraints
  on models of the thermal emission of hot Jupiters. Assuming that the
  planet emits as a blackbody, we estimate an effective temperature of
  T<SUB>p</SUB>=1060+/-50 K. Under the additional assumptions that the
  planet is in thermal equilibrium with the radiation from the star and
  emits isotropically, we find a Bond albedo of A=0.31+/-0.14. This would
  imply that the planet absorbs the majority of stellar radiation incident
  upon it, a conclusion of significant impact to atmospheric models of
  these objects. We also compare our data to a previously published
  model of the planetary thermal emission, which predicts prominent
  spectral features in our observational bands due to water and carbon
  monoxide. This model adequately reproduces the observed planet-to-star
  flux ratio at 8.0 μm however, it significantly overpredicts the ratio
  at 4.5 μm. We also present an estimate of the timing of the secondary
  eclipse, which we use to place a strong constraint on the expression
  ecosω, where e is the orbital eccentricity and ω is the longitude of
  periastron. The resulting upper limit on e is sufficiently small that
  we conclude that tidal dissipation is unlikely to provide a significant
  source of energy interior to the planet.

Title: Results of WFC3 Thermal Vacuum Testing - Repeatability of
    the Channel Select Mechanism
Authors: Brown, T. M.
Bibcode: 2005wfc..rept...18B
Altcode:
  The channel select mechanism (CSM) on WFC3 is used to divert the optical
  path of the incoming beam to the WFC3 IR channel. The contract end item
  (CEI) specification for the CSM is that the position of point sources in
  the IR channel should vary by less than 20 milliarcsec after movement
  of the CSM. As part of the 2004 campaign of WFC3 thermal-vacuum tests,
  the image stability of both WFC3 channels (UVIS &amp; IR) was measured
  over a wide range of environmental temperatures, simulating thermal
  variations that could occur in flight due to orbital occultations and
  slewing between hot and cold orientations. Some of these tests involved
  rapid switching between the WFC3 channels to track the image stability
  over large slews in temperature. These data imply that the CSM meets
  its CEI specification for repeatability.

Title: Far-Ultraviolet imaging of the Hubble Deep Field North
Authors: Teplitz, H. I.; Brown, T. M.; Conselice, C.; de Mello, D. F.;
   Dickinson, M. E.; Ferguson, H. C.; Gardner, J. P.; Giavalisco, M.;
   Menanteau, F.
Bibcode: 2005ASSL..329P..79T
Altcode: 2005sdlb.procP..79T
  We present far-UV imaging of the Hubble Deep Field North (HDF-N)
  taken with the Solar Blind Channel of the Advanced Camera for Surveys
  (ACS/SBC) on board HST. Combined with archival STIS imaging, the
  full WFPC2 deep field has now been observed at 1500 Å. We detect
  111 objects, with redshifts 0.07 &lt; z &lt; 0.85. A high fraction
  of galaxies previously identified as ``blue-core ellipticals'' show
  significant UV flux, presumably due to star-formation activity. Number
  counts to AB=29 have a surprisingly flat slope, consistent with a
  larger-than-predicted population of starburst galaxies at intermediate
  redshift. We examine the morphology of starburst galaxies as a function
  of redshift, and compare FUV, optical and NIR properties.

Title: A New Search for Carbon Monoxide Absorption in the Transmission
    Spectrum of the Extrasolar Planet HD 209458b
Authors: Deming, Drake; Brown, Timothy M.; Charbonneau, David;
   Harrington, Joseph; Richardson, L. Jeremy
Bibcode: 2005ApJ...622.1149D
Altcode: 2004astro.ph.12436D
  We have revisited the search for carbon monoxide absorption features in
  transmission during the transit of the extrasolar planet HD 209458b. In
  2002 August-September we acquired a total of 1077 high-resolution
  spectra (λ/δλ~25,000) in the K-band (2 μm) wavelength region using
  NIRSPEC on the Keck II telescope during three transits. These data
  are more numerous and of better quality than the data analyzed in an
  initial search by Brown et al. Our analysis achieves a sensitivity
  sufficient to test the degree of CO absorption in the first-overtone
  bands during transit on the basis of plausible models of the planetary
  atmosphere. We analyze our observations by comparison with theoretical
  tangent geometry absorption spectra, computed by adding height-invariant
  ad hoc temperature perturbations to the model atmosphere of Sudarsky
  et al. and by treating cloud height as an adjustable parameter. We do
  not detect CO absorption. The strong 2-0 R-branch lines between 4320
  and 4330 cm<SUP>-1</SUP> have depths during transit less than 1.6 parts
  in 10<SUP>4</SUP> in units of the stellar continuum (3 σ limit) at a
  spectral resolving power of 25,000. Our analysis indicates a weakening
  similar to that found in the case of sodium, suggesting that a general
  masking mechanism is at work in the planetary atmosphere. Under
  the interpretation that this masking is provided by high clouds,
  our analysis defines the maximum cloud-top pressure (i.e., minimum
  height) as a function of the model atmospheric temperature. For the
  relatively hot model used by Charbonneau et al. to interpret their
  sodium detection, our CO limit requires cloud tops at or above 3.3
  mbar, and these clouds must be opaque at a wavelength of 2 μm. High
  clouds comprised of submicron-sized particles are already present
  in some models but may not provide sufficient opacity to account for
  our CO result. Cooler model atmospheres, having smaller atmospheric
  scale heights and lower CO mixing ratios, may alleviate this problem
  to some extent. However, even models 500 K cooler than the Sudarsky et
  al. model require clouds above the 100 mbar level to be consistent with
  our observations. Our null result therefore requires clouds to exist at
  an observable level in the atmosphere of HD 209458b, unless this planet
  is dramatically colder than current belief. <P />Data presented herein
  were obtained at the W. M. Keck Observatory, which is operated as a
  scientific partnership among the California Institute of Technology,
  the University of California and the National Aeronautics and Space
  Administration. The Observatory was made possible by the generous
  financial support of the W. M. Keck Foundation.

Title: The Challenge of Wide-Field Transit Surveys: The Case of
    GSC 01944-02289
Authors: Mandushev, Georgi; Torres, Guillermo; Latham, David W.;
   Charbonneau, David; Alonso, Roi; White, Russel J.; Stefanik, Robert
   P.; Dunham, Edward W.; Brown, Timothy M.; O'Donovan, Francis T.
Bibcode: 2005ApJ...621.1061M
Altcode: 2005astro.ph..1554M
  Wide-field searches for transiting extrasolar giant planets face
  the difficult challenge of separating true transit events from the
  numerous false positives caused by isolated or blended eclipsing
  binary systems. We describe here the investigation of GSC 01944-02289,
  a very promising candidate for a transiting brown dwarf detected by
  the Trans-Atlantic Exoplanet Survey (TrES) network. The photometry
  and radial velocity observations suggested that the candidate was an
  object of substellar mass in orbit around an F star. However, careful
  analysis of the spectral line shapes revealed a pattern of variations
  consistent with the presence of another star whose motion produced
  the asymmetries observed in the spectral lines of the brightest
  star. Detailed simulations of blend models composed of an eclipsing
  binary plus a third star diluting the eclipses were compared with
  the observed light curve and used to derive the properties of the
  three components. Using the predicted stellar parameters, we were
  able to identify a second set of spectral lines corresponding to the
  primary of the eclipsing binary and derive its spectroscopic orbit. Our
  photometric and spectroscopic observations are fully consistent with
  a blend model of a hierarchical triple system composed of an eclipsing
  binary with G0 V and M3 V components in orbit around a slightly evolved
  F5 dwarf. The rotational broadening of the spectral lines of the F5
  primary (vsini~34 km s<SUP>-1</SUP>) and its brightness relative to
  the eclipsing binary (~89% of the total light) made the discovery of
  the true nature of the system particularly difficult. We believe that
  this investigation will be helpful to other groups pursuing wide-field
  transit searches as this type of false detection could be more common
  than true transiting planets and difficult to identify.

Title: Results of WFC3 Thermal Vacuum
Authors: Brown, T. M.; Reid, I. N.; Figer, D. F.
Bibcode: 2005wfc..rept...12B
Altcode:
  The throughput measurements for the WFC3 IR channel, taken during
  the Fall 2004 thermal-vacuum test, show that the IR throughput is
  approximately 15% lower than expected at all wavelengths. These
  measurements were obtained through all of the IR filters, scanning
  a monochromatic source through the central wavelengths of each
  filter, from 930 to 1670 nm. The source of this discrepancy is under
  investigation.

Title: Results of WFC3 Thermal Vacuum Testing - Image Stability
Authors: Brown, T. M.
Bibcode: 2005wfc..rept...11B
Altcode:
  As part of the 2004 campaign of WFC3 thermal-vacuum tests, the image
  stability of both WFC3 channels (UVIS &amp; IR) was measured over a
  wide range of environmental temperatures, simulating thermal variations
  that could occur in flight due to orbital occultations and slewing
  between hot and cold orientations. During orbital temperature cycles,
  the drift in the UVIS channel slightly exceeded its specification
  of 10 milliarcsec per 200 minutes, while the drift in the IR channel
  met its specification of 20 milliarcsec per 200 minutes. During large
  temperature slews, the UVIS channel drift exceeded its specification by
  a factor of 6, while the IR channel drift exceeded its specification
  by a factor of 3, and the alignment of the two channels diverged
  significantly. Alternative versions of these tests showed that much of
  this motion may be associated with the test apparatus instead of WFC3,
  but this is still under investigation.

Title: Results of WFC3 Thermal Vacuum Testing - UVIS Channel Ghosts
Authors: Brown, T. M.
Bibcode: 2005wfc..rept....1B
Altcode:
  The optical ghosts in the WFC3 UVIS channel, measured during the Fall
  2004 thermalvacuum test, show the same morphologies and strengths as
  characterized previously while under ambient conditions. All filters
  previously showing optical ghosts were tested: F225W, F280N, F606W,
  F218W, F275W, F300X, F410M, F467M, F547M, F621M, F625M, F689M, F775W,
  F814W, FQ232N, FQ243N, F656N, F658N, F665N, F673N, and F680N. F225W,
  F280N, and F606W are representative of all ghost behavior, and were
  tested at 8 field points; the remaining filters were tested at one
  field point.

Title: Results of WFC3 Thermal Vacuum Testing - UVIS Channel
    Throughput
Authors: Brown, T. M.; Reid, I. N.
Bibcode: 2005wfc..rept....2B
Altcode:
  The throughput measurements for the WFC3 UVIS channel, taken during
  the Fall 2004 thermal-vacuum test, show that the UVIS throughput is
  excellent, meeting or exceeding expectations at most wavelengths. These
  measurements were obtained through both the "clear" aperture and
  through a subset of the broad-band UVIS filters. The clear throughput
  was obtained on each detector chip, scanning a monochromatic source from
  the near- UV (200 nm) to the near-IR (1000 nm). The filtered throughput
  was obtained at one field point using a monochromatic source at the
  central wavelength of each tested filter.

Title: High-Resolution Spectroscopy of the Transiting Planet Host
    Star TrES-1
Authors: Sozzetti, Alessandro; Yong, David; Torres, Guillermo;
   Charbonneau, David; Latham, David W.; Allende Prieto, Carlos; Brown,
   Timothy M.; Carney, Bruce W.; Laird, John B.
Bibcode: 2004ApJ...616L.167S
Altcode: 2004astro.ph.10483S
  We report on a spectroscopic determination of the stellar parameters
  and chemical abundances for the parent star of the transiting planet
  TrES-1. Based on a detailed analysis of iron lines in our Keck and
  Hobby-Eberly Telescope spectra, we derive T<SUB>eff</SUB>=5250+/-75
  K, logg=4.6+/-0.2, and [Fe/H]=0.00+/-0.09. By measuring the Ca
  II activity indicator and by putting useful upper limits on the
  Li abundance, we constrain the age of TrES-1 to be 2.5+/-1.5
  Gyr. By comparing theoretical stellar evolution models with the
  observational parameters, we obtain M<SUB>*</SUB>=0.89+/-0.05
  M<SUB>solar</SUB> and R<SUB>*</SUB>=0.83+/-0.05 R<SUB>solar</SUB>. Our
  improved estimates of the stellar parameters are utilized in
  a new analysis of the transit photometry of TrES-1 to derive
  a mass M<SUB>p</SUB>=(0.76+/-0.05)M<SUB>J</SUB>, a radius
  R<SUB>p</SUB>=1.04<SUP>+0.08</SUP><SUB>-0.05</SUB>R<SUB>J</SUB>, and
  an inclination i=89.5<SUP>+0.5</SUP><SUB>-1.3</SUB> deg. The improved
  planetary mass and radius estimates provide the grounds for new crucial
  tests of theoretical models of evolution and evaporation of irradiated
  extrasolar giant planets.

Title: FUSE and STIS Observations of the Post-AGB Star ZNG 1 in the
    Globular Cluster M5
Authors: Dixon, W. V.; Brown, T. M.; Howk, J. C.; Landsman, W. B.
Bibcode: 2004AAS...205.5309D
Altcode: 2004BAAS...36.1426D
  FUSE and HST/STIS observations of the UV-bright star ZNG 1 in
  the globular cluster M5 (NGC 5904) reveal it to be a helium-rich,
  post-asymptotic giant branch (PAGB) star enhanced in carbon, nitrogen,
  and oxygen, with a high rotational velocity (170 km/s) and a fast
  stellar wind (1000 km/s). Its spectrum exhibits high-velocity
  absorption by both neutral and high-ionization (O VI, C IV, and
  Si IV) species. Blue-shifted by approximately 180 km/s relative to
  the stellar photosphere and by 100 to 150 km/s relative to the LSR,
  the absorption represents either circumstellar material (e.g., gas
  ejected during the star's AGB phase and now shock-heated by the fast
  PAGB wind) or a high-ionization high-velocity cloud (HVC) along the
  line of sight to M5. If the latter, it would be the first evidence
  that highly-ionized HVCs may be found near the Galactic disk. In this
  poster, we use these data to improve previous estimates of the stellar
  parameters and test the possibility that the star is a merger remnant;
  to determine the star's iron abundance and compare it to the cluster
  mean; and to investigate the origin of the blue-shifted absorption. <P
  />This work is supported by NASA grant NNG04GC44G6.

Title: FUSE Observations of the Hot Post-AGB Star ZNG 1 in the
    Globular Cluster M5
Authors: Dixon, W. V.; Brown, T. M.; Landsman, W. B.
Bibcode: 2004ASSL..315..382D
Altcode: 2004hdgw.conf..382D
  No abstract at ADS

Title: STARE operations experience and its data quality control
Authors: Alonso, R.; Deeg, H. J.; Brown, T. M.; Belmonte, J. A.
Bibcode: 2004AN....325..594A
Altcode:
  The STARE instrument was the first to detect the transits of an
  extrasolar planet in 1999. To date it has performed one of the longest
  running searches for transits, being in nearly continous operations
  since July 2001 at Teide Observatory, Tenerife. We describe the
  instrumental setup and the scheme that is used for data acquisition,
  handling and analysis. To this end, we first review the conditions
  under which we obtained data suggestive of transits, and we then
  follow a chain of verification and follow-up measures, progressing
  from fairly simple ones of low cost and effort towards more involved
  ones, which may be needed to positively verify the existence of a true
  planetary transit.

Title: Asteroseismology of Sun-Like Stars
Authors: Metcalfe, T. S.; Brown, T. M.; Christensen-Dalsgaard, J.
Bibcode: 2004ESASP.559..567M
Altcode: 2004soho...14..567M; 2004astro.ph..8127M
  In the past decade, helioseismology has revolutionized our
  understanding of the interior structure of the Sun. In the next decade,
  asteroseismology will place this knowledge into context, by providing
  structural information for dozens of pulsating stars across the H-R
  diagram. Solar-like oscillations have already been detected from
  the ground in a few stars, and several current and planned satellite
  missions will soon unleash a flood of stellar pulsation data. Deriving
  reliable seismological constraints from these observations will
  require a significant improvement to our current analysis methods. We
  are adapting a computational method, based on a parallel genetic
  algorithm, to help interpret forthcoming observations of Sun-like
  stars. This approach was originally developed for white dwarfs and
  ultimately led to several interesting tests of fundamental physics,
  including a key astrophysical nuclear reaction rate and the theory of
  stellar crystallization. The impact of this method on the analysis of
  pulsating white dwarfs suggests that seismological modeling of Sun-like
  stars will also benefit from this approach.

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
Bibcode: 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: TrES-1: The Transiting Planet of a Bright K0 V Star
Authors: Alonso, Roi; Brown, Timothy M.; Torres, Guillermo; Latham,
   David W.; Sozzetti, Alessandro; Mandushev, Georgi; Belmonte, Juan
   A.; Charbonneau, David; Deeg, Hans J.; Dunham, Edward W.; O'Donovan,
   Francis T.; Stefanik, Robert P.
Bibcode: 2004ApJ...613L.153A
Altcode: 2004astro.ph..8421A
  We report the detection of a transiting Jupiter-sized planet
  orbiting a relatively bright (V=11.79) K0 V star. We detected
  the transit light-curve signature in the course of the TrES
  multisite transiting planet survey and confirmed the planetary
  nature of the companion via multicolor photometry and precise
  radial velocity measurements. We designate the planet TrES-1
  its inferred mass is (0.75+/-0.07)M<SUB>Jup</SUB>, its radius is
  1.08<SUP>+0.18</SUP><SUB>-0.04</SUB>R<SUB>Jup</SUB>, and its orbital
  period is 3.030065+/-0.000008 days. This planet has an orbital period
  similar to that of HD 209458b but about twice as long as those of
  the OGLE transiting planets. Its mass is indistinguishable from that
  of HD 209458b, but its radius is significantly smaller and fits the
  theoretical models without the need for an additional source of heat
  deep in the atmosphere, as has been invoked by some investigators for
  HD 209458b.

Title: Taking the Temperature of the New Planet TrES-1
Authors: Charbonneau, David; Allen, Lori; Brown, Timothy; Gilliland,
   Ronald; Latham, David; Mandushev, Georgi; Megeath, Tom; Torres,
   Guillermo; Alonso Sobrino, Roi; O'Donovan, Francis; Sozzetti,
   Alessandro
Bibcode: 2004sptz.prop..227C
Altcode:
  We propose to observe the newly-discovered transiting planet TrES-1
  during the time of secondary eclipse (when the planet passes behind
  the star). A successful measurement of this eclipse would constitute
  the first direct detection of emission from an extrasolar planet. The
  secondary eclipse will reveal two key quantities of the planet: its
  temperature (from the eclipse depth), and its orbital eccentricity
  (from the eclipse timing). Moreover, these observations will enable
  us to characterize the high-precision, rapid-cadence photometric
  performance of IRAC. A successful demonstration of this innovative use
  of IRAC would open a new observing mode for Spitzer with applications
  extending well beyond the study of extrasolar planets.

Title: Characterizing a Newly-Found Extrasolar Planet
Authors: Brown, Timothy
Bibcode: 2004hst..prop10441B
Altcode: 2004hst..prop.6754B
  We propose to observe transits of the newly-discovered extrasolar planet
  TRES-1 using {1} ACS/HRC to obtain precise time-series photometry of
  the transit, and {2} NICMOS to measure the strength of water vapor
  absorption in the planetary atmosphere. The visible light curve will
  permit an accurate estimate of the planet's diameter by resolving
  uncertainty concerning the diameter of the parent star, and the water
  vapor observation can be used to test models of the structure, clouds
  and composition in the planet's upper atmosphere.

Title: Astrophysical False Positives Encountered in Wide-Field
    Transit Searches
Authors: Charbonneau, David; Brown, Timothy M.; Dunham, Edward W.;
   Latham, David W.; Looper, Dagny L.; Mandushev, Georgi
Bibcode: 2004AIPC..713..151C
Altcode: 2004astro.ph..1063C
  Wide-field photometric transit surveys for Jupiter-sized planets
  are inundated by astrophysical false positives, namely systems
  that contain an eclipsing binary and mimic the desired photometric
  signature. We discuss several examples of such false alarms. These
  systems were initially identified as candidates by the PSST instrument
  at Lowell Observatory. For three of the examples, we present follow-up
  spectroscopy that demonstrates that these systems consist of (1) an
  M-dwarf in eclipse in front of a larger star, (2) two main-sequence
  stars presenting grazing-incidence eclipses, and (3) the blend of
  an eclipsing binary with the light of a third, brighter star. For
  an additional candidate, we present multi-color follow-up photometry
  during a subsequent time of eclipse, which reveals that this candidate
  consists of a blend of an eclipsing binary and a physically unassociated
  star. We discuss a couple indicators from publicly-available catalogs
  that can be used to identify which candidates are likely giant stars,
  a large source of the contaminants in such surveys.

Title: HST Photometry of 47 Tucanae: Time Series Analysis and Search
    for Giant Planets
Authors: Brown, Timothy M.; Charbonneau, David; Gilliland, Ronald L.;
   Albrow, M. D.; Burrows, A.; Cochran, W. D.; Baliber, N.; Edmonds,
   P. D.; Frandsen, S.; Bruntt, S.; Guhathakurta, P.; Choi, P.; Lin,
   D. N. C.; Vogt, S. S.; Marcy, G. W.; Mayor, M.; Naef, D.; Milone,
   E. F.; Stagg, C. R.; Williams, M. D.; Sarajedini, A.; Sigurdsson,
   S.; Vandenberg, D. A.
Bibcode: 2004IAUS..202...66B
Altcode:
  No abstract at ADS

Title: Probing the Outskirts of an Extrasolar Planet with HST
    Time-Series Photometry
Authors: Charbonneau, David; Brown, Timothy M.; Gilliland, Ronald L.;
   Noyes, Robert W.; Burrows, Adam
Bibcode: 2004IAUS..202...72C
Altcode:
  No abstract at ADS

Title: Extrasolar Planet Transit Observations-Findings and Prospects
    (Invited Review)
Authors: Brown, Timothy M.
Bibcode: 2004IAUS..202...52B
Altcode:
  No abstract at ADS

Title: Strategies to recognize false alarms in transit experiments:
    experiences from the STARE project
Authors: Alonso, R.; Deeg, H. J.; Brown, T. M.; Belmonte, J. A.
Bibcode: 2004ESASP.538..255A
Altcode: 2004sshp.conf..255A
  In this contribution, we study the different stellar configurations
  that can produce signals resembling those produced by a transiting
  planet. We list several strategies to recognize these false alarms. For
  the most common configurations, we delineate which of these strategies
  are able to detect them. The case of an eclipsing binary of similar
  components, whose light is diluted by a third star, is discussed in
  some detail. Multicolor photometry is considered as a useful tool
  to recognize this common case. Two example of false alarms obtained
  by the STARE project, the different techniques used to study them,
  and the most probable configurations producing them are shown.

Title: Far-Ultraviolet Imaging of the Hubble Deep Field North
Authors: Teplitz, H. I.; Brown, T. M.; de Mello, D. F.; Dickinson,
   M. E.; Ferguson, H. C.; Gardner, J. P.; Giavalisco, M.; Heap, S. R.
Bibcode: 2003AAS...203.9003T
Altcode: 2003BAAS...35R1350T
  We present far-UV imaging of the Hubble Deep Field North (HDF-N)
  taken with the Solar Blind Channel of the Advanced Camera for Surveys
  (ACS/SBC) onboard HST. Combined with archival STIS imaging, the full
  WFPC2 deep field has now been observed at 1500 Angstroms. In the
  mosaic of 14 ACS/SBC pointings, we detect more than 80 galaxies. No
  sources are found without counterparts in the WFPC2 image. Redshifts
  (spectroscopic or photometric) for the detected sources are in the
  range z=0.07 to z=0.85. We compare morphological properties in the
  FUV, optical, and near-IR. We investigate the population of UV-bright,
  intermediate redshift starbursts by measuring the FUV number counts. The
  galaxy counts reach fainter than AB=28, but dark current glow causes
  the detection area and completeness to be a strong function of position
  on the detector.

Title: Iron Abundances of Hot Post-AGB Stars in Globular Clusters
Authors: Dixon, W. V.; Brown, T. M.; Landsman, W. B.
Bibcode: 2003AAS...203.5214D
Altcode: 2003BAAS...35Q1291D
  Only two hot post-asymptotic giant branch (PAGB) stars in globular
  clusters, Barnard 29 in M13 and ROA 5701 in Omega Cen, have
  well-determined iron abundances, and in both cases [Fe/H] is more than
  0.5 dex below the cluster mean. The stars apparently lost a significant
  fraction of their photospheric iron while on the AGB, perhaps through
  the selective condensation of iron onto dust grains. To determine
  the frequency of iron depletion among cluster PAGB stars and to test
  scenarios for this depletion, we have begun a project to re-analyze
  archival spectra of cluster PAGB stars obtained with the Hopkins
  Ultraviolet Telescope. (HUT flew on the Astro-1 and 2 Space Shuttle
  missions in 1990 and 1995. Its first-order sensitivity ranged from 820
  to 1840 Å with a resolution of about 3 Å.) Using state-of-the-art
  non-LTE line-blanketed stellar atmosphere models, we determine the
  effective temperature, surface gravity and iron abundance of each
  star. In this poster, we present preliminary results for the stars
  BS in 47 Tuc, vZ 1128 in M3, and UV5 in NGC 1851. <P />This work is
  supported by NASA grant NAG 5-10916.

Title: The ELODIE survey for northern extra-solar planets. II. A
    Jovian planet on a long-period orbit around GJ 777 A
Authors: Naef, D.; Mayor, M.; Korzennik, S. G.; Queloz, D.; Udry,
   S.; Nisenson, P.; Noyes, R. W.; Brown, T. M.; Beuzit, J. L.; Perrier,
   C.; Sivan, J. P.
Bibcode: 2003A&A...410.1051N
Altcode: 2003astro.ph..6586N
  We present radial-velocity measurements obtained with the ELODIE
  and AFOE spectrographs for <ASTROBJ>GJ 777 A</ASTROBJ> (<ASTROBJ>HD
  190360</ASTROBJ>), a metal-rich ([Fe/H] = 0.25) nearby (d = 15.9 pc)
  star in a stellar binary system. A long-period low radial-velocity
  amplitude variation is detected revealing the presence of a Jovian
  planetary companion. Some of the orbital elements remain weakly
  constrained because of the smallness of the signal compared to our
  instrumental precision. The detailed orbital shape is therefore
  not well established. We present our best fitted orbital solution:
  an eccentric (e = 0.48) 10.7-year orbit. The minimum mass of the
  companion is 1.33 M<SUB>Jup</SUB>. <P />Based on observations made
  with the ELODIE echelle spectrograph mounted on the 1.93-m Telescope
  at the Observatoire de Haute-Provence (CNRS) and with the AFOE
  spectrograph mounted on the 1.5-m Telescope at the Fred Lawrence
  Whipple Observatory (SAO). <P />The ELODIE and AFOE measurements
  discussed in this paper are only available in electronic form at the
  CDS via anonymous ftp to cdsarc.u-strasbg.fr (130.79.128.5) or via
  http://cdsweb.u-strasbg.fr/cgi-bin/qcat?J/A+A/410/1051

Title: Kepler Mission: a mission to find Earth-size planets in the
    habitable zone
Authors: Borucki, William J.; Koch, David; Basri, Gibor; Brown,
   Timothy; Caldwell, Douglas; Devore, Edna; Dunham, Edward; Gautier,
   Thomas; Geary, John; Gilliland, Ronald; Gould, Alan; Howell, Steve;
   Jenkins, Jon
Bibcode: 2003ESASP.539...69B
Altcode: 2003toed.conf...69B
  The Kepler Mission is a NASA Discovery-class mission designed to
  continuously monitor the brightness of 100,000 main sequence stars
  to detect the transit of Earth-size and larger planets. It is a wide
  field of view photometer with a Schmidt-type telescope and an array
  of 42 CCDs covering the 100 sq. degree field-of-view (FOV). It has
  a 0.95 m aperture and a 1.4 m primary and is designed to attain a
  photometric precision of 20 parts per million (ppm) for 12th magnitude
  solar-like stars for a 6.5-hour transit duration. It will continuously
  observe 100,000 main sequence stars from 9th to 15th magnitude in the
  Cygnus constellation for a period of four years with a cadence of 4
  measurements per hour. The photometer is scheduled to be launched in
  2007 into heliocentric orbit. A ground-based program to classify all
  450,000 stars brighter than 15th magnitude in the FOV and to conduct
  a detailed examination of a subset of the stars that show planetary
  companions is also planned. Hundreds of Earth-size planets should
  be detected if they are common around solar-like stars. Ground-based
  spectrometric observations of those stars with planetary companions
  will be made to determine the dependences of the frequency and size
  of terrestrial planets on stellar characteristics such as type and
  metallicity. A null result would imply that terrestrial planets
  are rare.

Title: VizieR Online Data Catalog: ELODIE survey for northern
    extra-solar planets. II. (Naef+, 2003)
Authors: Naef, D.; Mayor, M.; Korzennik, S. G.; Queloz, D.; Udry,
   S.; Nisenson, P.; Noyes, R. W.; Brown, T. M.; Beuzit, J. L.; Perrier,
   C.; Sivan, J. P.
Bibcode: 2003yCat..34101051N
Altcode:
  Here are the 69 radial-velocity measurements of GJ 777A (HD 190360)
  used for deriving the orbital solution of this star. These velocities
  were obtained using the ELODIE echelle spectrograph mounted on the
  1.93-m Telescope at Observatoire de Haute-Provence (France) and the
  AFOE spectrograph mounted on the 1.5-m Telescope at the Fred Lawrence
  Whipple Observatory (USA). <P />(1 data file).

Title: Expected Detection and False Alarm Rates for Transiting
    Jovian Planets
Authors: Brown, Timothy M.
Bibcode: 2003ApJ...593L.125B
Altcode: 2003astro.ph..7256B
  Ground-based searches for transiting Jupiter-sized planets have so far
  produced few detections of planets but many of stellar systems with
  eclipse depths, durations, and orbital periods that resemble those
  expected from planets. The detection rates prove to be consistent
  with our present knowledge of binary and multiple-star systems
  and of Jovian-mass extrasolar planets. Space-based searches for
  transiting Earth-sized planets will be largely unaffected by the
  false alarm sources that afflict ground-based searches, except for
  distant eclipsing binaries whose light is strongly diluted by that of
  a foreground star. A by-product of the rate estimation is evidence
  that the period distribution of extrasolar planets is depressed for
  periods between 5 and 200 days.

Title: A Search for Water Vapor in the Atmosphere of an Extrasolar
    Planet
Authors: Brown, Timothy
Bibcode: 2003hst..prop.9832B
Altcode:
  We propose to search for evidence of water vapor in the transmission
  spectrum of the transiting planet of HD 209458. A successful detection
  would not only establish the presence of this important atmospheric
  constituent, but would also constrain other key properties of this
  close-in, Jupiter-sized planet. Specifically, relating the absorption
  caused by water to that already observed from atomic sodium would
  help establish the height of the atmosphere's uppermost cloud layer
  {if any}. Also, the abundance of water will provide information about
  that of oxygen, and by extension, that of all heavy elements. To make
  this measurement, we propose a doubly-differential procedure in which
  we will use NICMOS in spectroscopic mode to detect the small spectral
  changes that occur during planetary transits, and that result from
  absorption of starlight as it passes through the outer parts of the
  planet's atmosphere. We search for water because it is expected to
  produce by far the strongest spectrum features within the wavelength
  range accessible to HST.

Title: Mapping the Star Formation History of the Local Group with NHST
Authors: Brown, T. M.
Bibcode: 2003AAS...202.4903B
Altcode: 2003BAAS...35..768B
  The color-magnitude diagram (CMD) is the most fundamental
  tool for studying the star formation history of nearby stellar
  populations. Strong constraints on the ages of stellar populations
  come from CMDs reaching the main sequence, and with the Hubble Space
  Telescope (HST), it is possible to produce such a CMD for stars at
  any distance within the Local Group. Unfortunately, resolving the
  main sequence in old populations beyond the satellites of the Milky
  Way requires an enormous investment of HST time, meaning that only a
  few pencil beams can be explored within the remaining HST mission. In
  strong contrast, an 8 meter UV-optical space telescope, diffraction
  limited at 0.5 microns, could map the star formation history of all
  galaxies in the Local Group: It would take only one hour to resolve
  the main sequence in any Local Group galaxy, allowing the exploration
  of hundreds of sight-lines in a reasonable program.

Title: Flux Calibration of the STIS CCD: Correcting for Charge
    Transfer Inefficiency and Time-Dependent Sensitivity
Authors: Davies, J.; Goudfrooij, P.; Bohlin, R. C.; Stys, D. J.;
   Brown, T. M.; Walborn, N. R.; Proffitt, C. R.
Bibcode: 2003AAS...202.0407D
Altcode: 2003BAAS...35Q.704D; 2003AAS...202..407D
  A variety of on-orbit imaging and spectroscopic observations have
  been used to characterize the Charge Transfer Efficiency (CTE) of the
  Charge-Coupled Device (CCD) of the Space Telescope Imaging Spectrograph
  (STIS) aboard the Hubble Space Telescope. A set of formulae has been
  developed to correct aperture photometry and spectrophotometry of
  point sources for CTE-related loss, with dependencies on X and Y
  positions, the source signal, the background counts, and the time
  of observation. Application of the new formulae leads to a CCD flux
  calibration that is accurate to within one percent, independent
  of source signal. <P />The analysis of the STIS Sensitivity Monitor
  observations from 1997 through January 2003 shows continuing sensitivity
  trends correlated with time for all first-order, low- and medium
  resolution spectroscopic modes as well as a temperature dependance
  in the FUV and recently in the CCD detectors. The newly available
  CTE corrections allow for the proper determination of time-dependent
  sensitivity (TDS) trends in CCD modes. The wavelength-averaged rates
  of sensitivity loss for the CCD modes range from 0%/yr (G750L grating)
  to 1.5%/yr (G230LB grating). These sensitivity losses are wavelength
  dependent and will be corrected for within the STIS data reduction
  pipeline by means of the delivery of new reference files.

Title: Hubble Space Telescope and Ground-based Optical and Ultraviolet
    Observations of GRB 010222
Authors: Galama, T. J.; Reichart, D.; Brown, T. M.; Kimble, R. A.;
   Price, P. A.; Berger, E.; Frail, D. A.; Kulkarni, S. R.; Yost,
   S. A.; Gal-Yam, A.; Bloom, J. S.; Harrison, F. A.; Sari, R.; Fox,
   D.; Djorgovski, S. G.
Bibcode: 2003ApJ...587..135G
Altcode: 2003astro.ph..1059G
  We report on Hubble Space Telescope (HST) Wide Field Planetary Camera 2
  optical and Space Telescope Imaging Spectrograph (STIS) near-ultraviolet
  MAMA observations and ground-based optical observations of GRB 010222,
  spanning 15 hr to 71 days. The observations are well described by a
  relativistic blast wave model with a hard electron energy distribution,
  p=1.57<SUP>+0.04</SUP><SUB>-0.03</SUB>, and a jet transition at
  t<SUB>*</SUB>=0.93<SUP>+0.15</SUP><SUB>-0.06</SUB> days. These values
  are slightly larger than previously found as a result of a correction
  for the contribution from the host galaxy to the late-time ground-based
  observations and the larger temporal baseline provided by the HST
  observations. The host galaxy is found to contain a very compact core
  (size &lt;0.25"), which coincides with the position of the optical
  transient. The STIS near-ultraviolet MAMA observations allow for an
  investigation of the extinction properties along the line of sight
  to GRB 010222. We find that the far-ultraviolet curvature component
  c<SUB>4</SUB> is rather large. In combination with the low optical
  extinction, A<SUB>V</SUB>=0.110<SUP>+0.010</SUP><SUB>-0.021</SUB> mag,
  when compared with the hydrogen column inferred from X-ray observations,
  we suggest that this is evidence for dust destruction.

Title: FUSE Observations of the Post-AGB Star ZNG 1 in the Globular
    Cluster M5 (NGC 5904)
Authors: Dixon, W. Van Dyke; Brown, T. M.; Landsman, W. B.
Bibcode: 2003ASPC..296..236D
Altcode: 2003ASPC..296..236V; 2002astro.ph..9344D; 2003nhgc.conf..236D
  We report observations of the hot post-asymptotic giant branch
  (PAGB) star ZNG 1 in the globular cluster M5 (NGC 5904) with the Far
  Ultraviolet Spectroscopic Explorer (FUSE). From the resulting spectrum,
  we derive an effective temperature T<SUB>eff</SUB> = 45 +/- 1 kK, a
  surface gravity log g = 4.3 +/- 0.1, and a rotational velocity v sin i =
  170 +/- 20 km/s. The star's luminosity, log (L/L<SUB>sun</SUB>) = 3.54
  +/- 0.06, is consistent with its PAGB classification. The atmosphere is
  helium-rich (Y = 0.92), with enhanced carbon (2.9% by mass), nitrogen
  (0.43%), and oxygen (0.37%) abundances. The spectrum shows evidence for
  a stellar wind with terminal velocity near 1000 km/s and an expanding
  shell of carbon- and nitrogen-rich material. This work is supported
  by NASA grant NAG 5-10405.

Title: A New Formation Mechanism for the Hottest Horizontal-Branch
    Stars
Authors: Sweigart, A. V.; Brown, T. M.; Lanz, T.; Landsman, W. B.;
   Hubeny, I.
Bibcode: 2003ASPC..296..313S
Altcode: 2003nhgc.conf..313S; 2002astro.ph..7343S
  Stars with very large mass loss on the red-giant branch can undergo
  the helium flash while descending the white-dwarf cooling curve. Under
  these conditions the flash convection zone will mix the hydrogen
  envelope with the hot helium- burning core. Such ``flash-mixed''
  stars will arrive on the extreme horizontal branch (EHB) with helium-
  and carbon-rich envelopes and will lie at higher temperatures than the
  hottest canonical (i.e., unmixed) EHB stars. Flash mixing provides a
  new evolutionary channel for populating the hot end of the EHB and may
  explain the origin of the high gravity, helium-rich sdO and sdB stars.

Title: Using M32 to Study Rapid Phases of Stellar Evolution
Authors: Brown, T. M.; Ferguson, H. C.
Bibcode: 2003ASPC..296..199B
Altcode: 2002astro.ph..7211B; 2003nhgc.conf..199B
  The compact elliptical galaxy M32 offers a unique testing ground for
  theories of stellar evolution. Because of its proximity, solar-blind
  UV observations can resolve the hot evolved stars in its center. Some
  of these late evolutionary phases are too rapid to study adequately
  in globular clusters, and their study in the Galactic field is often
  complicated by uncertainties in distance and reddening. Using the UV
  cameras on the Space Telescope Imaging Spectrograph, we have obtained a
  deep color-magnitude diagram (CMD) of the M32 center. Although the hot
  horizontal branch is well-detected, our CMD shows a striking scarcity
  of the brighter post-asymptotic giant branch (PAGB) and post-early AGB
  stars expected for a population of this size. This dearth suggests
  that the evolution to the white dwarf phase may be much more rapid
  than that predicted by canonical evolutionary tracks for low-mass stars.

Title: Recent Improvements to STIS Pipeline Calibration
Authors: Diaz-Miller, R. I.; Quijano, J. Kim; Valenti, J.; Proffitt,
   C. R.; Sahu, K. C.; Bohlin, R. C.; Brown, T. M.; Lindler, D.
Bibcode: 2003hstc.conf..189D
Altcode:
  In the last few months a number of improvements to the STIS pipeline
  calibration have been developed and implemented, which include the
  following. <P />We have released new low order flat files for use
  with the G140L observations. These flats should reduce uncertainties
  of the extracted flux with position from 12% to 2%. <P />To better
  reflect the change with time in the overall shape of the NUV MAMA
  dark current, new dark reference files were created for different
  epochs. To further improve the dark subtraction, these darks are also
  scaled using an improved algorithm, which takes into account long term
  changes in the behavior of the NUV MAMA dark current. <P />Additional
  improvements which have been implemented are described in the posters
  by Stys et al., Valenti et al., Davies et al. and Lindler et al. Future
  improvements include background smoothing for low signal spectroscopic
  data, and updating the Pixel-to-Pixel flat library and the current
  CCD bad pixel table.

Title: STIS Status after the Switch to Side 2
Authors: Brown, T. M.; Davies, J. E.
Bibcode: 2003hstc.conf..180B
Altcode:
  Since July 2001, STIS has been operating on its secondary (Side-2)
  electronics, due to the failure of the primary (Side-1) system. The
  change to Side 2 has required new calibration work. The dark rate of
  the STIS CCD varies since the switch to Side 2, as it depends on the
  temperature of the CCD (which cannot be regulated precisely using Side-2
  electronics). We find that the dark rate is a linear function of the
  housing temperature for pixels at a given dark rate, but the slope of
  this relation varies for pixels with different dark rates. Scaling of
  the darks as a function of the temperature has been incorporated into
  the STIS pipeline. An additional feature of the switch to Side-2 is
  that the STIS CCD read noise has increased by 1 e^{-} sec^{-1} for all
  four amplifiers when using a gain of 1. This increased read noise is due
  to electronic pick-up pattern noise (on Side 1 the noise was primarily
  white noise). Although an algorithm exists for filtering this additional
  pattern noise, it will not be incorporated into the STIS pipeline.

Title: Astronomy: Distant planet is the hottest yet
Authors: Brown, Timothy M.
Bibcode: 2003Natur.421..488B
Altcode:
  The first planet beyond our Solar System to be detected by means of
  the transit method has now been found to orbit its star almost twenty
  times closer than Mercury orbits the Sun.

Title: Absolute Flux Calibration of STIS MAMA Imaging Modes
Authors: Proffitt, C. R.; Brown, T. M.; Mobasher, B.; Davies, J.
Bibcode: 2003stis.rept....1P
Altcode:
  The absolute flux calibration of STIS MAMA imaging modes is tested
  by comparison of observed and predicted count rates. As part of this
  work, we have derived new, wavelength- dependent aperture corrections
  for MAMA imaging, and have revised the NUVMAMA imaging throughput at
  short wavelengths. FUV-MAMA imaging modes clearly show a time dependent
  sensitivity loss that is consistent with the time dependent sensitivity
  changes seen in G140L spectra. Once this time dependence is taken
  into account, count rates measured using 1" apertures for FUV 25MAMA,
  F25LYA, F25ND3, and F25SRF2 observations are within 5% of predictions
  made using the prelaunch throughput determination. However, FUV F25QTZ
  observations show a much larger scatter than expected from Poisson
  statistics. NUV-MAMA imaging modes also appear to be consistent with
  the time dependence observed for G230L spectra, although this effect
  is not as large as for the FUV-MAMA. While most NUV-MAMA imaging
  modes show adequate agreement with the tabulated sensitivity curve,
  results for the F25CN182 mode are discrepant. We suggest a revision
  of the short wavelength throughput of the NUV-MAMA imaging modes to
  fix this problem. This revision brings the results for all NUV imaging
  modes to within 5% of predictions.

Title: Absolute Flux Calibration of STIS Imaging Modes
Authors: Proffitt, C. R.; Davies, J. E.; Brown, T. M.; Mobasher, B.
Bibcode: 2003hstc.conf..201P
Altcode:
  The absolute flux calibration of STIS imaging photometry presents
  a number of unique challenges. The very wide wavelength coverage
  of most STIS imaging modes leads to significant color dependence in
  both the throughputs and the aperture corrections, complicating the
  determination of detector sensitivity. For CCD imaging modes, these
  difficulties are further complicated by the very broad scattered light
  halo at long wavelengths. For MAMA imaging modes, it is also necessary
  to take the time and wavelength dependent sensitivity changes of the
  detectors into account. We present deep imaging observations of a number
  of stars with well measured spectral energy distributions. These data
  have been used to derive improved color dependent aperture corrections
  for all STIS imaging configurations, and to revise the wavelength
  dependent detector sensitivities. These new aperture corrections and
  sensitivity revisions should allow absolute flux calibration of imaging
  observations with better than 5% accuracy for most STIS imaging modes.

Title: 100 Times Faster and 3 Times Sharper: Background-Dominated
    Observations of Stellar Populations with an 8-meter Optical-UV
    Space Telescope
Authors: Brown, T. M.
Bibcode: 2003ASPC..291..351B
Altcode: 2002astro.ph..7212B; 2003hslf.conf..351B
  An 8 m successor to the Hubble Space Telescope (HST) would make
  incredible gains in the study of stellar populations, especially in
  the Local Group. If diffraction-limited at 0.5 microns, the "Next HST"
  could produce high-resolution imaging of faint sources over a wide field
  in 1 percent of the time needed with the HST. With these capabilities,
  photometry of the ancient main sequence could be obtained for many
  sight-lines through Local Group galaxies, thus determining directly
  the ages of their structures and providing a formation history for
  the Local Group populations.

Title: Possible Transiting Planet Candidates from the EXPLORE Project
Authors: Mallén-Ornelas, G.; Seager, S.; Yee, H. K. C.; Gladders,
   M. D.; Brown, T. M.; Minniti, D.; Ellison, S. L.; Mallén-Fullerton,
   G. M.
Bibcode: 2003ASPC..294..391M
Altcode: 2002astro.ph..9589M
  The EXPLORE Project is a series of searches for transiting
  extrasolar planets using large-format mosaic CCD cameras on 4-m class
  telescopes. Radial velocity follow-up is done on transiting planet
  candidates with 8--10m class telescopes. We present a summary of
  transit candidates from the EXPLORE Project for which we have radial
  velocity data.

Title: The EXPLORE Project. I. A Deep Search for Transiting Extrasolar
    Planets
Authors: Mallén-Ornelas, G.; Seager, S.; Yee, H. K. C.; Minniti,
   D.; Gladders, Michael D.; Mallén-Fullerton, G. M.; Brown, T. M.
Bibcode: 2003ApJ...582.1123M
Altcode: 2002astro.ph..3218M
  Planet transit searches promise to be the next breakthrough for
  extrasolar planet detection and will bring the characterization of
  short-period planets into a new era. Every transiting planet discovered
  will have a measured radius, which will provide constraints on planet
  composition, evolution, and migration history. Together with radial
  velocity measurements, the absolute mass of every transiting planet
  will be determined. In this paper we discuss the design considerations
  of the Extrasolar Planet Occultation Research (EXPLORE) project,
  a series of transiting planet searches using 4 m class telescopes to
  continuously monitor a single field of stars in the Galactic plane in
  each ~2 week observing campaign. We discuss the general factors that
  determine the efficiency and the number of planets found by a transit
  search, including time sampling strategy and field selection. The
  primary goal is to select the most promising planet candidates for
  radial velocity follow-up observations. We show that with very high
  photometric precision light curves that have frequent time sampling and
  at least two detected transits, it is possible to uniquely solve for
  the main parameters of the eclipsing system (including planet radius),
  based on several important assumptions about the central star. Together
  with a measured spectral type for the star, this unique solution for
  orbital parameters provides a powerful method for ruling out most
  contaminants to transiting planet candidates. For the EXPLORE project,
  radial velocity follow-up observations for companion mass determination
  of the best candidates are done on 8 m class telescopes within 2 or
  3 months of the photometric campaigns. This same-season follow-up is
  made possible by the use of efficient pipelines to produce high-quality
  light curves within weeks of the observations. We conclude by presenting
  early results from our first search, EXPLORE I, in which we reached
  better than 1% rms photometric precision (measured over a full night)
  on ~37,000 stars with 14.5&lt;=I&lt;=18.2.

Title: STARE Results on a Single Field: Tens of New Pulsating Stars
Authors: Alonso, Roi; Belmonte, Juan Antonio; Brown, Tim
Bibcode: 2003Ap&SS.284...13A
Altcode:
  We present preliminary results on variable stars of a STARE's three
  month observational run centered at the Cygnus constellation. A total
  amount of aprox. 14000 stars with 9&lt;R&lt;12.5 magnitude, in STARE's
  6.1×6.1<SUP>̂2</SUP> FOV, have been analyzed to obtain lightcurves
  for each of these stars. The data spans for ~90 nights. In this single
  field, we detect more that 40 stars with pulsation modes between 5
  and 40 c/d, the vast mayority previously unknown to be variables.

Title: STIS Calibration Status
Authors: Proffitt, C. R.; Goudfrooij, P.; Brown, T. M.; Davies, J. E.;
   Diaz-Miller, R. I.; Dressel, L.; Quijano, J. Kim; Maíz-Apellániz,
   J.; Mobasher, B.; Potter, M.; Sahu, K. C.; Stys, D. J.; Valenti, J.;
   Walborn, N. R.; Bohlin, R. C.; Barrett, P.; Busko, I.; Hodge, P.
Bibcode: 2003hstc.conf...97P
Altcode:
  Last year's failure of the STIS Side-1 electronics temporarily suspended
  use of the instrument. The Side-1 electronics are not repairable, but
  operations were resumed in August of 2001 using the redundant Side-2
  electronics. STIS was fully returned to operation, with only minimal
  impacts on scientific performance. <P />MAMA detector performance
  continues to be very good, with sensitivity changes of 1 to 2 percent
  per year. Although the detailed relation between the NUV MAMA detector
  temperature and dark current has changed, typical NUV dark current
  levels are similar to those in previous cycles. The FUV dark current
  varies irregularly, and it is now usually significantly higher than
  it had been during the first two years of STIS operations. <P />The
  effects of radiation damage on the STIS CCD detector continue to follow
  previous trends, with declining charge transfer efficiency, increasing
  dark current, and increasing numbers of hot pixels. We also review the
  use and calibration of the E1 aperture positions which can be used to
  ameliorate CTE effects.

Title: An Aluminum Secondary Mirror for the SOFIA Telescope
Authors: Erickson, E. F.; Kunz, N.; Brivkalns, C. A.; Brown, T. M.;
   Honaker, M.
Bibcode: 2002AAS...201.1808E
Altcode: 2002BAAS...34.1131E
  The secondary mirror for the SOFIA telescope is made from silicon
  carbide. It is 352 mm in diameter, weighs 1.8 kg, and is finished to
  good optical tolerances. The light weight is essential for chopping
  with the secondary support mechanism to suppress low frequency "sky"
  noise. To achieve the light weight, the back side of the mirror is
  structured with thin-walled pockets; the face plate is 2.3 mm thick. The
  material is stiff, has low density and high thermal conductance, but is
  brittle. The latter is a concern because failure of this mirror would
  render the telescope inoperable. For this reason we are designing a
  spare secondary mirror. The spare must match the mass and moments of
  inertia of the SiC mirror (to permit effective chopping), but should be
  more robust and much cheaper. The spare should permit continuation of
  much of the observing program, and since many of SOFIA's observations
  will be made in the far-infrared, the optical quality of the spare
  can be significantly lower than that of the SiC secondary. Currently
  it appears that a bare aluminum secondary can be made to meet the
  requirements, while achieving a diffraction-limited wavelength of 20
  microns or less. The design details will be described and discussed
  in the paper. We gratefully acknowledge NASA support of this work.

Title: FUSE Observations of He-rich sdB Stars
Authors: Lanz, T.; Brown, T. M.; Sweigart, A. V.; Hubeny, I.; Landsman,
   W. B.
Bibcode: 2002AAS...20111308L
Altcode: 2002BAAS...34.1285L
  Subdwarf B stars all show significant abundance anomalies. Most are
  extremely deficient in helium and selected light elements, but a
  minority are helium-rich. Deficiencies in helium and heavier elements
  have been attributed to gravitational settling, but the helium-enriched
  members of the class present a puzzling exception, because radiative
  levitation should be too weak to prevent gravitational settling. New
  evolutionary calculations suggest that these helium-rich sdB stars are
  the result of a delayed helium-core flash on the white dwarf cooling
  curve. The convective zone produced by this flash will penetrate
  the hydrogen envelope, mixing hydrogen into the hot helium-burning
  interior, where it is rapidly consumed. The resulting star should show
  greatly enhanced helium and carbon with respect to the other heavy
  elements. This phenomenon is analogous to the born again scenario
  for producing hydrogen-deficient R CrB stars following a very late
  helium-shell flash. We have recently obtained FUSE spectra of two
  helium-rich sdB stars, revealing huge C III lines at 977 and 1176
  Å. Our preliminary analysis yields a surface composition of 97% He
  and 3% C, in agreement with the new evolutionary scenario. This work
  is supported in part by NASA grant NAG5-12383.

Title: FUSE Observations of the Post-AGB Star ZNG 1 in the Globular
    Cluster M5
Authors: Dixon, W. V.; Brown, T. M.; Landsman, W. B.
Bibcode: 2002AAS...20111306D
Altcode: 2002BAAS...34.1284D
  We have observed the hot post-AGB star ZNG 1 in the globular
  cluster M5 (NGC 5904) with the Far Ultraviolet Spectroscopic Explorer
  (FUSE). From the resulting spectrum, we derive an effective temperature
  T<SUB>eff</SUB> ~ 45,000K, a rotational velocity v<SUB>rot</SUB> ~
  100km/s, carbon and nitrogen abundances approximately ten times solar,
  a wind with terminal velocity near 1000 km/s, and evidence for an
  expanding shell of material around the star. The carbon and nitrogen
  enhancements suggest dredge-up of nuclear-processed material on the
  AGB. The high rotational velocity may reflect a previous merger with
  a binary companion. This research is supported by NASA grant NAG5-10405.

Title: The EXPLORE Project: A Deep Search for Transiting Extrasolar
    Planets at the KPNO and CTIO 4m Telescopes.
Authors: Mallen-Ornelas, G.; Seager, S.; Yee, H. K. C.; von Braun,
   K.; Brown, T. M.; Gladders, M. D.; Lee, B.; Ellison, S. L.; Eyer,
   L.; Blake, C.; Mallen-Fullerton, G.
Bibcode: 2002AAS...20110410M
Altcode: 2002BAAS...34.1273M
  We present preliminary results of our October 2002 campaign at
  the KPNO 4m telescope as part of an ongoing search for transiting
  extrasolar planets. Our goal is to detect transiting planets and to
  derive statistics of planet frequency, radius, and mass for stars
  ranging from types early G to late K. Planet transits will be detected
  via 1% photometric precision lightcurves with 4 minute time sampling
  spanning 18 nights per run. Transit searches will mark a new era in
  planetary discovery and characterization. Planet radii, which provide
  constraints on composition, evolution, and migration history, can only
  be measured for transiting planets. In addition absolute planet mass
  can be determined with follow-up radial velocity measurements. Our
  lightcurve database will have unprecedented time sampling and very
  high photometric precision for hundreds of thousands of stars, enabling
  new research on variable and binary stars, short microlensing events,
  and moving objects such as asteroids.

Title: Possible Transiting Planet Candidates from the Explore Project
Authors: Mallen-Ornelas, G.; Seager, S.; Yee, H. K. C.; Gladders,
   M. D.; Brown, T. M.; von Braun, K.; Minniti, D.; Ellison, S. L.;
   Mallen-Fullerton, G. M.
Bibcode: 2002AAS...201.9604M
Altcode: 2002BAAS...34.1263M
  Planet transit searches promise to be the next big step forward in
  short-period extrasolar planet detection and characterization. Every
  transiting planet discovered will have a measured radius, and radial
  velocity observations will lead to an absolute mass measurement (since
  orbital inclination is known). Transiting planets can be discovered
  around distant stars and in a variety of stellar environments. Many
  transit searches are now ongoing. The EXPLORE Project is a series
  of transit searches using wide-field CCD mosaic cameras on 4m-class
  telescopes, with radial velocity follow-up of transit candidates done
  using 8m-class telescopes. We continuously monitor a Galactic plane
  field for as long as 18 consecutive nights with 3-minute time sampling,
  and perform 0.2-1 tens of thousands of stars in our field. We have a
  pipeline to completely reduce the data in a few weeks after the imaging
  observations, which allows same-semester radial-velocity follow-up
  observations. We present results from our 2001 and 2002 observing
  campaigns at CTIO, CFHT, and KPNO, and show transit candidates for
  which radial velocity follow-up has been done.

Title: A Search for CO Absorption in the Transmission Spectrum of
    HD 209458b
Authors: Brown, Timothy M.; Libbrecht, Kenneth G.; Charbonneau, David
Bibcode: 2002PASP..114..826B
Altcode: 2002astro.ph..5246B
  We observed one transit of the extrasolar planet HD 209458b with the
  NIRSPEC spectrograph on the Keck II telescope. Using time series of
  low-noise observations in the wavelength range 2.0-2.5 μm, we searched
  for extra absorption from the first-overtone rotation-vibration band
  of CO near 2.3 μm. This was not detected with a detection limit that
  fails to test simple models of the planetary atmosphere by a factor
  of about 3. Great improvements in the detectability of the CO spectrum
  features could be realized by observing a transit that is centered near
  stellar meridian passage, and in better weather. Since it appears that
  similar observations taken under better circumstances might succeed,
  we describe our analysis procedures in detail.

Title: Detection of an Extrasolar Planet Atmosphere
Authors: Charbonneau, David; Brown, Timothy M.; Noyes, Robert W.;
   Gilliland, Ronald L.
Bibcode: 2002ApJ...568..377C
Altcode: 2001astro.ph.11544C
  We report high-precision spectrophotometric observations of four
  planetary transits of HD 209458, in the region of the sodium resonance
  doublet at 589.3 nm. We find that the photometric dimming during
  transit in a bandpass centered on the sodium feature is deeper by
  (2.32+/-0.57)×10<SUP>-4</SUP> relative to simultaneous observations
  of the transit in adjacent bands. We interpret this additional dimming
  as absorption from sodium in the planetary atmosphere, as recently
  predicted from several theoretical modeling efforts. Our model for
  a cloudless planetary atmosphere with a solar abundance of sodium in
  atomic form predicts more sodium absorption than we observe. There are
  several possibilities that may account for this reduced amplitude,
  including reaction of atomic sodium into molecular gases and/or
  condensates, photoionization of sodium by the stellar flux, a low
  primordial abundance of sodium, and the presence of clouds high in
  the atmosphere. Based on observations with the NASA/ESA Hubble Space
  Telescope (HST), obtained at the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in
  Astronomy, Inc. under NASA contract NAS 5-26555.

Title: A Deep Search for Transiting Extrasolar Planets
Authors: Seager, Sara; Mallen-Ornelas, Gabriela; Yee, Howard; Minniti,
   Dante; Gladders, Michael; Brown, Tim
Bibcode: 2002noao.prop..336S
Altcode:
  We propose to continue our deep search for transiting close-in
  extrasolar planets using the MOSAIC II wide-field imager on the CTIO 4m
  telescope. We will take repeated short I-band exposures during 9 nights
  (4 Chilean time and 5 USA time) of a single well-chosen field with
  ~100,000 stars with I≲18.2. Relative photometry accurate to 0.2-1%
  rms will yield light curves which will allow the identification of
  transiting planets. We have already analysed the best 37,000 lightcurves
  (0.2%-1% rms) and found several planet candidates. However, due to
  bad weather and seeing, we effectively had only 5-6 good nights out
  of 11, and two nights were completely lost. The reduced time coverage
  resulted in a loss of 3.5 times of planet-detection efficiency. We
  are requesting additional time to compensate for this loss. Note
  that the proposed observations - to be conducted a year after the
  first run - will allow us to obtain a very accurate period and phase
  measurement for those planet candidates for which we already have 2
  transits detected, since we will have a large time baseline equivalent
  to ~100 orbits of the planet. A detection of a second transit in a
  light-curve with currently only one transit will result in new planet
  candidates. Finally, there will be new candidates for which 2 transits
  will be visible in the second run.

Title: The Origin of Hot Subluminous Horizontal-Branch Stars in ω
    Centauri and NGC 2808
Authors: Sweigart, A. V.; Brown, T. M.; Lanz, T.; Landsman, W. B.;
   Hubeny, I.
Bibcode: 2002ASPC..265..261S
Altcode: 2002ocuw.conf..261S; 2002astro.ph..3063S
  Hot subluminous stars lying up to 0.7 mag below the extreme horizontal
  branch (EHB) are found in the UV color-magnitude diagrams of omega Cen
  and NGC 2808. Such stars are unexplained by canonical HB theory. In
  order to explore the origin of these subluminous stars, we evolved a
  set of low-mass stars from the main sequence through the helium-core
  flash to the HB for a wide range in the mass loss along the red-giant
  branch (RGB). Stars with the largest mass loss evolve off the RGB to
  high effective temperatures before igniting helium in their cores. Our
  results indicate that the subluminous EHB stars, as well as the gap
  within the EHB of NGC 2808, can be explained if these stars undergo
  a late helium-core flash on the white-dwarf cooling curve. Under
  these conditions the flash convection will penetrate into the stellar
  envelope, thereby mixing most, if not all, of the envelope hydrogen
  into the hot helium- burning interior. This phenomenon is analogous
  to the "born-again" scenario for producing hydrogen-deficient stars
  during a very late helium-shell flash. "Flash mixing" greatly enhances
  the envelope helium and carbon abundances and, as a result, leads to
  an abrupt increase in the HB effective temperature. We argue that
  the EHB gap in NGC 2808 is caused by this theoretically predicted
  dichotomy in the HB morphology. Using new helium- and carbon-rich
  stellar atmospheres, we show that the flash-mixed stars have the same
  reduced UV flux as the subluminous EHB stars. Moreover, we demonstrate
  that models without flash mixing lie, at most, ~0.1 mag below the EHB
  and hence fail to explain the observations. Flash mixing may also
  provide a new evolutionary channel for producing the high gravity,
  He-rich sdO and sdB stars.

Title: δ Scuti stars with STARE: a project on planetary transits
    and stellar variability
Authors: Alonso, R.; Brown, T. M.; Belmonte, J. A.; Charbonneau, D.;
   Fox Machado, L.; Pallé, P. L.
Bibcode: 2002ESASP.485..245A
Altcode: 2002sshp.conf..245A
  In this contribution, we show the capability of STARE to obtain
  frequencies and amplitudes from high temporal resolution δ Scuti
  spectra. Lightcurves of 13 new field δ Scuti stars are analyzed and a
  total of 21 oscillation modes are found in a single field. Noise level
  in the spectra falls bellow 3 mmag for stars fainter than magnitude
  9. Subsequent analysis of the other observed fields, a new location
  for STARE, as well as the sharing of data with similar projects will
  provide higher-quality results and a valuable δ Scuti database,
  which would be useful for follow-up observations.

Title: The Origin of Hot Subluminous Horizontal-Branch Stars in ω
    Cen and NGC 2808
Authors: Sweigart, A. V.; Brown, T. M.; Moehler, S.; Lanz, T.;
   Landsman, W. B.; Hubeny, I.; Dreizler, S.; Napiwotzki, R.
Bibcode: 2001AAS...19913704S
Altcode: 2001BAAS...33.1512S
  Ultraviolet (UV) observations of the globular clusters ω Cen and NGC
  2808 have revealed an unexpected population of hot subluminous stars
  lying up to 0.7 mag below the extreme horizontal branch (EHB) in the
  UV, which are not explained by canonical stellar models. In order to
  explore the evolutionary status of these stars, we have evolved a set
  of low-mass stars from the main sequence through the helium flash to
  the horizontal branch (HB) for a wide range in the mass loss along the
  red-giant branch (RGB). Stars with the largest mass loss evolve off
  the RGB to high effective temperatures before igniting helium in their
  cores. Our results indicate that the subluminous stars can be explained
  if these stars undergo a late helium flash while descending the white
  dwarf cooling curve. Under these conditions the convection zone produced
  by the helium flash will penetrate into the stellar envelope, thereby
  mixing the envelope hydrogen into the hot helium-burning interior, where
  it is rapidly consumed. Such ``flash-mixed'' stars will have helium-
  and carbon-rich envelopes and will lie at higher effective temperatures
  than the hottest canonical (i.e., unmixed) EHB stars. Using new stellar
  atmospheres, we show that these changes in the envelope abundances
  will suppress the UV flux in the spectra of the flash-mixed stars by
  the amount needed to explain the hot subluminous stars in ω Cen and
  NGC 2808. To test this evolutionary scenario, we have obtained medium
  resolution spectra of a sample of the hottest HB stars in ω Cen. We
  find that these stars are indeed helium-rich compared to classical
  EHB stars and also considerably hotter than the hottest EHB models
  without flash mixing.

Title: Photospheric Abundances of the Hot Stars in NGC 1399
Authors: Brown, T. M.; Ferguson, H. C.; O'Connell, R. W.; Ohl, R. G.
Bibcode: 2001AAS...199.2002B
Altcode: 2001BAAS...33Q1339B
  We present far-UV spectroscopy of the giant elliptical galaxy NGC1399,
  obtained with the Far Ultraviolet Spectroscopic Explorer. Of all
  quiescent ellipticals with measured UV emission, NGC1399 has the
  strongest known ``UV upturn'' - a sharp rise in the spectrum shortward
  of 2500 Å. It is now well-established that this emission comes from hot
  horizontal branch (HB) stars and their progeny; however, the chemical
  composition of these stars has been the subject of a long-standing
  debate. Our spectra, covering 900 - 1200 Å, clearly show photospheric
  absorption lines from the hot HB stars in this galaxy. The abundance
  of N appears nearly solar, Si is at 30% of the solar value, and C is
  at 4% of the solar value. Such abundances anomalies are a natural
  consequence of gravitational diffusion, and are also observed in
  subdwarf B stars of the Galactic field. Our spectra suggest that the
  hot stars responsible for the UV upturn are drawn from a metal-rich
  population. Although NGC1399 is at the center of the Fornax cluster,
  we find no evidence for OVI cooling flow emission. The upper limit to
  λ λ 1032,1038 emission is 3.6 x 10<SUP>-15</SUP> erg s<SUP>-1</SUP>
  cm<SUP>-2</SUP>, equivalent to 0.1 M<SUB>sun</SUB> yr<SUP>-1</SUP>. This
  OVI emission is far less than that predicted by cooling flow models
  of the observed NGC1399 X-ray luminosity.

Title: STIS Status after the Switch to Side-2, Calibration and
    Time-Tag Fixes
Authors: Davies, J. E.; Brown, T. M.; Goudfrooij, P.; Proffitt, C.;
   Sahu, K. C.; Stys, D.; Valenti, J.
Bibcode: 2001AAS...199.0803D
Altcode: 2001BAAS...33.1316D
  Since July 2001, STIS has been operating on its secondary (Side-2)
  electronics due to the failure of the primary (Side-1) system. The
  change to Side-2 has required new calibration work. The dark rate of
  the STIS CCD varies after the switch to Side-2, as it depends on the
  temperature of the CCD which cannot be regulated precisely using Side-2
  electronics. By tracking the CCD housing temperature, the relation of
  this dark rate to the housing temperature is found to be linear for
  pixels at a fixed dark rate, but the relation also depends (slightly) on
  the dark rate. The STIS CCD read noise has increased by 1 electron/sec
  for all four amplifiers after the switch to Side-2. This increased
  read noise is due to electronic pick-up noise, unlike before when it
  was consistent with white noise. Work towards reducing or removing
  this pattern noise is ongoing. The sensitivity of STIS in the imaging
  modes has been recalibrated and updated. This has also resulted in new
  aperature throughputs. Since the switch to Side-2, the sensitivity seems
  to have remained the same based on initial data. MAMA TIME-TAG data
  retrieved from the archive prior to 13 Sep 2001 may contain erroneous
  temporal gaps and jumps, potentially affecting the flux calibration
  of extracted spectra. New archive software installed on 13 Sep 2001
  fixes all known problems with TIME-TAG data.

Title: The Stellar Halos of Spiral Galaxies beyond the Local Group
Authors: Ferguson, H. C.; Rich, R. M.; Brown, T. M.; Smith, T. E.;
   Mouhcine, M.
Bibcode: 2001AAS...199.5212F
Altcode: 2001BAAS...33.1380F
  Were the extended stellar halos the first stellar populations to
  form in spiral galaxies, or have they been accreted over time from
  dwarf galaxies? What are the systematic relations between the disk,
  the bulge and the halo? Does stellar mass of the halo scale with the
  mass of the bulge or the mass of the entire galaxy? To begin to address
  such questions we observed nine nearby spiral galaxies with WFPC2 and
  resolved the top few magnitudes of the red-giant branch in the halo
  population. Specifically, the WFPC2 fields were placed 2 to 13 kpc
  off the minor-axis of the disks of NGC55, 247, 253, 300, 2903, 3031,
  4244, 4258, and 4945. These observations allow the first systematic
  study of the spatial distributions, metallicities and metallicity
  distributions of halo stars in normal spiral galaxies outside of the
  Local Group. We present a preliminary analysis of the color-magnitude
  diagrams including: estimates of the mean metallicities and metallicity
  distributions of each galaxy, estimates of the TRGB distances, estimates
  of the radial density profiles and a search for metallicity gradients,
  and first look at systematic trends within the sample of galaxies. This
  work is supported by a grant from STScI which is operated by AURA
  for NASA.

Title: HST Studies of the Core of 47 Tucanae
Authors: Howell, J. H.; Warren, J. A.; Guhathakurta, P.; Gilliland,
   R. L.; Albrow, M. D.; Sarajedini, A.; Brown, T. M.; Charbonneau, D.;
   Burrows, A. S.; Cochran, W. D.; Baliber, N.; Edmonds, P. D.; Frandsen,
   S.; Bruntt, H.; Lin, D. N. C.; Vogt, S. S.; Choi, P.; Marcy, G. W.;
   Mayor, M.; Naef, D.; Milone, E. F.; Stagg, C. R.; Williams, M. D.;
   Sigurdsson, S.; VandenBerg, D. A.
Bibcode: 2001AAS...198.9505H
Altcode: 2001BAAS...33.1182H
  The 8.3 day HST experiment described by R. L. Gilliland, et al. 2000
  is aimed at detecting planetary transits in the globular cluster
  47 Tucanae. An important by-product is a set of extremely deep
  WFPC2 images in F555W (V) and F814W (I) of the dense cluster core
  region. The effective exposure times in each of these bands is over
  100,000 s, and extensive sub-pixel dithers between individual exposures
  supports the creation of 4x oversampled images in which the FWHM of
  the point spread function is &lt; ~70 mas (PC) and &lt; ~140 mas
  (WF CCDs). Limited use is made of the shorter exposure time F336W
  (U) data. This poster describes several studies underway using this
  outstanding data set. First is a study of mass segregation in the core
  of 47 Tuc using this extremely deep WFPC2 data set. The degree of mass
  segregation is characterized by the slope x of the best fitting stellar
  mass function, where x=+1.35 is the Salpeter value. The mass function
  slope is found to vary from x=-5 in the cluster center to x=-2 at the
  edge of the WFPC2 field of view at a radius around 100'', indicating
  extreme mass segregation in the core of 47 Tuc. We also examine nearly
  100 blue stragglers in 47 Tuc's core. These include: a bright, strongly
  centrally concentrated population, and a faint population whose radial
  distribution is similar to that of the giants. The luminosity function
  and photometric properties of these two kinds of 47 Tuc blue stragglers
  are compared to predictions of blue straggler formation models. Blue
  stragglers are also discussed in relation to millisecond pulsars and
  other exotic objects in the cluster core. The binary sequence in 47
  Tuc will be examined in future work. Funding has been provided via a
  NASA/STScI grant for GO-8267.

Title: The Frequency of Binary Stars in the Core of 47 Tucanae
Authors: Albrow, Michael D.; Gilliland, Ronald L.; Brown, Timothy M.;
   Edmonds, Peter D.; Guhathakurta, Puragra; Sarajedini, Ata
Bibcode: 2001ApJ...559.1060A
Altcode: 2001astro.ph..5441A
  Differential time series photometry has been derived for 46,422
  main-sequence stars in the core of 47 Tucanae. The observations
  consisted of near-continuous 160 s exposures alternating between the
  F555W and F814W filters for 8.3 days in 1999 July with the Wide Field
  Planetary Camera 2 on the Hubble Space Telescope. Using Fourier and
  other search methods, 11 detached eclipsing binaries and 15 W Ursa
  Majoris stars have been discovered plus an additional 10 contact or
  near-contact noneclipsing systems. After correction for nonuniform area
  coverage of the survey, the observed frequencies of detached eclipsing
  binaries and W UMa stars within 90" of the cluster center are 0.022% and
  0.031%, respectively. The observed detached eclipsing binary frequency,
  the assumptions of a flat binary distribution with log period, and
  assuming that the eclipsing binaries with periods longer than about 4
  days have essentially their primordial periods imply an overall binary
  frequency of 13%+/-6%. The observed W UMa frequency and the additional
  assumptions that W UMa stars have evolved to contact according to
  tidal circularization and angular momentum loss theory and that the
  contact binary lifetime is 10<SUP>9</SUP> yr imply an overall binary
  frequency of 14%+/-4%. An additional 71 variables with periods from 0.4
  to 10 days have been found, which are likely to be BY Draconis stars in
  binary systems. The radial distribution of these stars is the same as
  that of the eclipsing binaries and W UMa stars and is more centrally
  concentrated than average stars but less so than the blue straggler
  stars. A distinct subset of six of these stars falls in an unexpected
  domain of the color-magnitude diagram, comprising what we propose to
  call red stragglers. Based on observations with the NASA/ESA Hubble
  Space Telescope obtained at the Space Telescope Science Institute,
  which is operated by AURA, Inc. under NASA contract NAS 5-26555.

Title: Transmission Spectra as Diagnostics of Extrasolar Giant
    Planet Atmospheres
Authors: Brown, Timothy M.
Bibcode: 2001ApJ...553.1006B
Altcode: 2001astro.ph..1307B
  Atmospheres of transiting extrasolar giant planets (EGPs) such as
  HD 209458b must impose features on the spectra of their parent stars
  during transits; these features contain information about the physical
  conditions and chemical composition of the atmospheres. The most
  convenient observational index showing these features is the ``spectrum
  ratio'' ℜ(λ), defined as the wavelength-dependent ratio of spectra
  taken in and out of transit. The principal source of structure in ℜ is
  the variation with wavelength of the height at which the EGP atmosphere
  first becomes opaque to tangential rays-one may think of the planet
  as having different radii, and hence different transit depths, at each
  wavelength. The characteristic depth of absorption lines in ℜ scales
  with the atmospheric scale height and with the logarithm of the opacity
  ratio between continuum and strong lines. For close-in EGPs, line depths
  of 10<SUP>-3</SUP> relative to the stellar continuum can occur. The
  atmospheres of EGPs probably consist mostly of molecular species,
  including H<SUB>2</SUB>, CO, H<SUB>2</SUB>O, and CH<SUB>4</SUB>, while
  the illuminating flux is characteristic of a Sun-like star. Thus,
  the most useful diagnostics are likely to be the near-infrared bands
  of these molecules, and the visible/near-IR resonance lines of the
  alkali metals. I describe a model that estimates ℜ(λ) for EGPs with
  prescribed radius, mass, temperature structure, chemical composition,
  and cloud properties. This model assumes hydrostatic and chemical
  equilibrium in an atmosphere with chemistry involving only H, C, N,
  and O. Other elements (He, Na, K, Si) are included as nonreacting
  minor constituents. Opacity sources include Rayleigh scattering,
  the strongest lines of Na and K, collision-induced absorption by
  H<SUB>2</SUB>, scattering by cloud particles, and molecular lines of CO,
  H<SUB>2</SUB>O, and CH<SUB>4</SUB>. The model simulates Doppler shifts
  from height-dependent winds and from planetary rotation, and deals in
  a schematic way with photoionization of Na and K by the stellar UV
  flux. Using this model, I investigated the diagnostic potential of
  various spectral features for planets similar to HD 209458b. Clouds
  are the most important determinants of the depth of features in ℜ
  they decrease the strength of all features as they reach higher in
  the atmosphere. The relative strengths of molecular lines provide
  diagnostics for the heavy-element abundance, temperature, and the
  vertical temperature structure, although diagnostics for different
  physical properties tend to be somewhat degenerate. Planetary rotation
  with likely periods leaves a clear signature on the line profiles,
  as do winds with speeds comparable to that of rotation. Successful
  use of these diagnostics will require spectral observations with
  signal-to-noise ratio (S/N) of 10<SUP>3</SUP> or better and resolving
  power R=λ/δλ ranging from 10<SUP>3</SUP> to 10<SUP>6</SUP>,
  depending on the application. Because of these stringent demands, it
  will be important to evolve analysis methods that combine information
  from many lines into a few definitive diagnostic indices.

Title: Hubble Space Telescope Time-Series Photometry of the Transiting
    Planet of HD 209458
Authors: Brown, Timothy M.; Charbonneau, David; Gilliland, Ronald L.;
   Noyes, Robert W.; Burrows, Adam
Bibcode: 2001ApJ...552..699B
Altcode: 2001astro.ph..1336B
  We have observed four transits of the planet of HD 209458 using
  the STIS spectrograph on the Hubble Space Telescope (HST). Summing
  the recorded counts over wavelength between 582 and 638 nm yields a
  photometric time series with 80 s time sampling and relative precision
  of about 1.1×10<SUP>-4</SUP> per sample. The folded light curve can
  be fitted within observational errors using a model consisting of an
  opaque circular planet transiting a limb-darkened stellar disk. In
  this way we estimate the planetary radius R<SUB>p</SUB>=1.347+/-0.060
  R<SUB>Jup</SUB>, the orbital inclination i=86.6d+/-0.14d, the stellar
  radius R<SUB>*</SUB>=1.146+/-0.050 R<SUB>solar</SUB>, and one parameter
  describing the stellar limb darkening. Our estimated radius is smaller
  than those from earlier studies but is consistent within measurement
  errors and also with theoretical estimates of the radii of irradiated
  Jupiter-like planets. Satellites or rings orbiting the planet would, if
  large enough, be apparent from distortions of the light curve or from
  irregularities in the transit timings. We find no evidence for either
  satellites or rings, with upper limits on satellite radius and mass
  of 1.2 R<SUB>⊕</SUB> and 3 M<SUB>⊕</SUB>, respectively. Opaque
  rings, if present, must be smaller than 1.8 planetary radii in
  radial extent. The high level of photometric precision attained in
  this experiment confirms the feasibility of photometric detection of
  Earth-sized planets circling Sun-like stars. Based on observations with
  the NASA/ESA Hubble Space Telescope, obtained at the Space Telescope
  Science Institute, which is operated by the Association of Universities
  for Research in Astronomy, Inc. under NASA contract NAS 5-26555.

Title: FUSE Observations of the UV-Bright Star ZNG 1 in M5 (NGC 5904)
Authors: Dixon, W. V.; Brown, T. M.; Landsman, W. B.
Bibcode: 2001AAS...198.4505D
Altcode: 2001BAAS...33Q.847D
  Hot post-AGB stars in globular clusters typically exhibit Fe abundances
  considerably lower than the cluster mean. This anomaly may reflect
  selective condensation of metals onto dust grains at the end of the
  AGB phase, a mechanism first suggested for cooler post-AGB stars
  with peculiar Fe abundances. To investigate this phenomenon, we have
  observed several UV-bright stars in globular clusters with FUSE, the
  Far Ultraviolet Spectroscopic Explorer. In this poster, we present
  first results for the post-AGB star ZNG 1 in M5 (NGC 5904). Previous
  studies have shown the star to have an effective temperature of
  about 41,000 K and a surface gravity of log g = 4.5. Using the TLUSTY
  and SYNSPEC routines of Ivan Hubeny, we construct a set of non-LTE
  stellar atmosphere models and synthetic spectra, with which we derive
  the star's photospheric parameters and abundances. We present our
  results and discuss their implications for AGB and post-AGB stellar
  evolution. This research is supported by NASA grant NAG5-8962.

Title: Understanding Horizontal Branch Anomalies in NGC 2808
Authors: Brown, T. M.; Sweigart, A. V.; Lanz, T.; Landsman, W. B.;
   Hubeny, I.
Bibcode: 2001AAS...198.4302B
Altcode: 2001BAAS...33..844B
  We present an ultraviolet color-magnitude diagram (CMD) spanning the hot
  horizontal branch (HB), blue straggler, and white dwarf populations
  of the globular cluster NGC 2808. These data, obtained with the
  Space Telescope Imaging Spectrograph (STIS), demonstrate that NGC
  2808 harbors a significant population of hot subluminous HB stars,
  an anomaly only previously reported for the globular cluster Omega
  Cen. Our theoretical modeling indicates that the location of these
  subluminous stars in the CMD, as well as the high temperature gap along
  the HB of NGC 2808, can be explained if these stars underwent a late
  helium-core flash while descending the white dwarf cooling curve. We
  show that the convective zone produced by such a late helium flash will
  penetrate into the hydrogen envelope, thereby mixing hydrogen into
  the hot helium-burning interior, where it is rapidly consumed. This
  phenomenon is analogous to the "born again" scenario for producing
  hydrogen-deficient stars following a late helium-shell flash. The flash
  mixing of the envelope greatly enhances the envelope helium and carbon
  abundances that, in turn, leads to a discontinuous increase in the HB
  effective temperatures. We argue that the hot HB gap is associated with
  this theoretically predicted dichotomy in the HB properties. Moreover,
  the changes in the emergent spectral energy distribution caused by
  these abundance changes are primarily responsible for explaining
  the hot subluminous HB stars. Although further evidence is needed to
  confirm that a late helium-core flash can account for the subluminous HB
  stars and the hot HB gap, we demonstrate that an understanding of these
  stars requires use of sophisticated models for the stellar evolution,
  atmospheres, and synthetic spectra.

Title: A Lack of Planets in 47 Tucanae from a Hubble Space Telescope
    Search
Authors: Gilliland, Ronald L.; Brown, T. M.; Guhathakurta, P.;
   Sarajedini, A.; Milone, E. F.; Albrow, M. D.; Baliber, N. R.; Bruntt,
   H.; Burrows, A.; Charbonneau, D.; Choi, P.; Cochran, W. D.; Edmonds,
   P. D.; Frandsen, S.; Howell, J. H.; Lin, D. N. C.; Marcy, G. W.; Mayor,
   M.; Naef, D.; Sigurdsson, S.; Stagg, C. R.; Vandenberg, D. A.; Vogt,
   S. S.; Williams, M. D.
Bibcode: 2000ApJ...545L..47G
Altcode:
  We report results from a large Hubble Space Telescope project to observe
  a significant (~34,000) ensemble of main-sequence stars in the globular
  cluster 47 Tucanae with a goal of defining the frequency of inner
  orbit, gas giant planets. Simulations based on the characteristics of
  the 8.3 days of time series data in the F555W and F814W Wide Field
  Planetary Camera 2 (WFPC2) filters show that ~17 planets should
  be detected by photometric transit signals if the frequency of hot
  Jupiters found in the solar neighborhood is assumed to hold for 47
  Tuc. The experiment provided high-quality data sufficient to detect
  planets. A full analysis of these WFPC2 data reveals ~75 variables,
  but no light curves resulted for which a convincing interpretation as
  a planet could be made. The planet frequency in 47 Tuc is at least
  an order of magnitude below that for the solar neighborhood. The
  cause of the absence of close-in planets in 47 Tuc is not yet known;
  presumably the low metallicity and/or crowding of 47 Tuc interfered
  with planet formation, with orbital evolution to close-in positions,
  or with planet survival. Based on observations with the NASA/ESA Hubble
  Space Telescope obtained at STScI, which is operated by AURA, Inc.,
  under NASA contract NAS5-26555.

Title: Seeking the Atmospheric Transmission Spectrum of HD209458b
Authors: Brown, T. M.; Butler, R. P.; Charbonneau, D.; Noyes, R. W.;
   Sasselov, D.; Libbrecht, K. G.; Marcy, G. W.; Seager, S.; Vogt, S. S.
Bibcode: 2000AAS...197.1105B
Altcode: 2000BAAS...32Q1417B
  Transiting extrasolar giant planets such as HD209458b should impress
  a spectroscopic signature on the light that is transmitted through
  the outer parts of their atmospheres. Theory suggests that the depths
  of absorption features resulting from this effect may be as large as
  about 10<SUP>-3</SUP> of the parent star's continuum intensity. Such
  spectral features could provide important diagnostics concerning the
  composition and physical state of the planetary atmosphere. Accordingly,
  we have obtained low-noise spectra of HD209458 during two transits
  of its planet, once in visible light using the HIRES spectrograph at
  the Keck I telescope, and once in the near infrared using the NIRSPEC
  spectrograph at Keck II. We describe the methods employed and the
  results of searches for spectral signatures of neutral atomic sodium,
  carbon monoxide, and other atomic and molecular species.

Title: Searching for Shadows of Other Earths
Authors: Doyle, L. R.; Deeg, H. J.; Brown, T. M.
Bibcode: 2000SciAm.283c..58D
Altcode: 2000SciAm.283c..38D
  No abstract at ADS

Title: Multicolor Observations of a Planetary Transit of HD 209458
Authors: Jha, Saurabh; Charbonneau, David; Garnavich, Peter M.;
   Sullivan, Denis J.; Sullivan, Tiri; Brown, Timothy M.; Tonry, John L.
Bibcode: 2000ApJ...540L..45J
Altcode: 2000astro.ph..7245J
  We present BVRIZ photometric observations of HD 209458 during the
  transit by its planetary companion on UT 1999 November 15 with the
  University of Hawaii 0.6 and 2.2 m telescopes and the High Altitude
  Observatory STARE telescope. The detailed shape of the transit
  curve is predicted to vary with color primarily as a result of the
  color-dependent limb darkening of the star but potentially due as well
  to the effect of color-dependent opacity in the planetary atmosphere. We
  model the light curves and present refined values for the transit timing
  and orbital period, useful for planning future observations of the
  planetary transit. We also derive significantly improved measurements
  of the planetary radius, R<SUB>p</SUB>=1.55+/-0.10 R<SUB>Jup</SUB>,
  stellar radius, R<SUB>s</SUB>=1.27+/-0.05 R<SUB>solar</SUB>, and
  orbital inclination, i=85.9d+/-0.5d. The derived planetary radius
  favors evolutionary models in which the planet has a low albedo.

Title: A Lack of Planets in 47 Tucanae from an HST Search
Authors: Gilliland, Ronald L.; Brown, T. M.; Guhathakurta, P.;
   Sarajedini, A.; Milone, E. F.; Albrow, M. D.; Baliber, N. R.; Bruntt,
   H.; Burrows, A.; Charbonneau, D.; Choi, P.; Cochran, W. D.; Edmonds,
   P. D.; Frandsen, S.; Howell, J. H.; Lin, D. N. C.; Marcy, G. W.; Mayor,
   M.; Naef, D.; Sigurdsson, S.; Stagg, C. R.; VandenBerg, D. A.; Vogt,
   S. S.; Williams, M. D.
Bibcode: 2000astro.ph..9397G
Altcode:
  We report results from a large Hubble Space Telescope project to observe
  a significant (~34,000) ensemble of main sequence stars in the globular
  cluster 47 Tucanae with a goal of defining the frequency of inner-orbit,
  gas-giant planets. Simulations based on the characteristics of the 8.3
  days of time-series data in the F555W and F814W WFPC2 filters show
  that ~17 planets should be detected by photometric transit signals
  if the frequency of hot Jupiters found in the solar neighborhood is
  assumed to hold for 47 Tuc. The experiment provided high-quality
  data sufficient to detect planets. A full analysis of these WFPC2
  data reveals ~75 variables, but NO light curves resulted for which
  a convincing interpretation as a planet could be made. The planet
  frequency in 47 Tuc is at least an order of magnitude below that for
  the solar neighborhood. The cause of the absence of close-in planets in
  47 Tuc is not yet known; presumably the low metallicity and/or crowding
  of 47 Tuc interfered with planet formation, with orbital evolution to
  close-in positions, or with planet survival.

Title: Eclipsing Binaries in 47 Tuc: Bonus of an HST Planetary Search
Authors: Milone, E. F.; Stagg, C. R.; Williams, M. D.; Brown, T. M.;
   Charbonneau, D.; Gilliland, R. L.; Albrow, M. D.; Burrows, A. S.;
   Cochran, W. D.; Baliber, N.; Edmonds, P. D.; Frandsen, S.; Bruntt,
   H.; Guhathakurta, P.; Choi, P.; Lin, D. N. C.; Vogt, S. S.; Howell,
   J. H.; Marcy, G. W.; Mayor, M.; Naef, D.; Sarajedini, A.; Sigurdsson,
   S.; VandenBerg, D. A.
Bibcode: 2000AAS...196.4603M
Altcode: 2000BAAS...32..746M
  A direct benefit of the 8.3 d HST experiment described by
  R. L. Gilliland, et al. (see their poster), is the opportunity to obtain
  fundamental stellar data from an earlier generation of stars than are
  found in the local field and in (relatively young) open clusters, the
  sources of almost all our current knowledge of stellar parameters. Of 32
  variables examined thus far from time-series detections (see the Brown,
  et al., poster), 9 were previously known; of the 23 remaining, one
  remains a possible (though unlikely) planetary transit candidate. At
  present writing, 17 confirmed or potential eclipsing binary systems
  have been closely examined: five contact/over-contact; two short-period
  β Lyrae-type, four Algol-type; one asymmetric (O'Connell effect)
  light curve-, but likely eclipsing, variable; one possible ellipsoidal
  variable; and four others with asymmetric low-amplitude variation,
  still under investigation. Preliminary modeling is nearly complete for
  six binaries in this still incomplete sample, and is underway for the
  others. Unadjusted and starting parameters are from VandenBerg's recent
  isochrone models and from an eclipsing binary simulation database
  of more than 8000 models created by Calgary students M. McClure,
  and B. Desnoyers-Winmill. Kurucz limb-darkening and atmospheric
  models straddling the metallicity range of the cluster are used in
  conjunction with Calgary versions of the Wilson-Devinney code, WD98
  &amp; wd98k93; the time-based mode is used to improve the periods and
  epochs. J Kallrath (BASF) developed and D. Terrell (SwRI) and W. Van
  Hamme (FIU) contributed to the value of these tools. The eclipsing
  binary modeling is funded by NSERC of Canada and by the Univ. of
  Calgary Research Grants Committee through grants to EFM.

Title: An HST Search for Planets in the Globular Cluster 47 Tucanae
Authors: Gilliland, R. L.; Albrow, M. D.; Brown, T. M.; Charbonneau,
   D.; Burrows, A.; Cochran, W. D.; Baliber, N.; Edmonds, P. D.; Frandsen,
   S.; Bruntt, H.; Guhathakurta, P.; Choi, P.; Howell, J. H.; Lin,
   D. N. C.; Vogt, S. S.; Marcy, G. W.; Mayor, M.; Naef, D.; Milone,
   E. F.; Stagg, C. R.; Williams, M. D.; Sarajedini, A.; Sigurdsson,
   S.; VandenBerg, D. A.
Bibcode: 2000AAS...196.0202G
Altcode: 2000BAAS...32R.675G
  HST was used for 8.3 days in July '99 to monitor over 30,000 stars on
  the main sequence of 47 Tuc photometrically with a goal of detecting
  planets via transit signals. Expected transit depths for 1.3 Jupiter
  radii planets increase from 1% near main sequence turnoff to 6% at 4
  magnitudes fainter due to decreasing stellar radii. Over this domain
  realized time series rms, obtained with PSF fitting in difference
  images, smoothly increases from 0.3% to 2.5%. With ~645 data points
  in each of WFPC2 F555W and F814W filters any planet with P &lt; 4.2
  days should provide securely detectable transits lasting 2-4 hours
  twice in each of V and I. Based on the frequency of inner-orbit,
  gas-giant planets from solar neighborhood radial velocity surveys we
  expect to detect 15 to 20 candidate planets, but see none (with 75%
  search completion) in this low metalicity, crowded stellar system;
  see also T.M. Brown poster. Many eclipsing binaries and variable
  stars are detected; see also E.F. Milone poster. We provide a project
  overview and details on: (1) reduction steps and resulting deep
  (&gt; 100,000s in V, I; 14,360s U) co-added, over-sampled images,
  (2) key analysis steps that provide near-Poisson limited photometric
  time-series precisions for dithered, under-sampled, crowded-field images
  with significant focus variations in time, (3) global summaries of
  time series precisions and sensitivity to detecting planets, and (4)
  a few time series of particular interest. Funding has been provided
  via a NASA/STScI grant for GO-8267.

Title: Extreme Mass Segregation in the Core of 47 Tucanae (NGC 104):
    Bonus of an HST Planetary Search
Authors: Howell, J. H.; Guhathakurta, P.; Sarajedini, A.; Gilliland,
   R. L.; Albrow, M. D.; Brown, T. M.; Charbonneau, D.; Burrows, A. S.;
   Cochran, W. D.; Baliber, N.; Edmonds, P. D.; Frandsen, S.; Bruntt,
   H.; Lin, D. N. C.; Vogt, S. S.; Choi, P.; Marcy, G. W.; Mayor, M.;
   Naef, D.; Milone, E. F.; Stagg, C. R.; Williams, M. D.; Sigurdsson,
   S.; VandenBerg, D. A.
Bibcode: 2000AAS...196.4108H
Altcode: 2000BAAS...32..740H
  The 8.3 d HST experiment described by R. L. Gilliland, et al. (see
  their poster) is aimed at detecting planetary transits in the globular
  cluster 47 Tucanae. An important by-product is a set of extremely
  deep WFPC2 images in F555W (V) and F814W (I) of the dense cluster
  core region. The effective exposure times in each of these bands is
  over 100,000 s, and extensive sub-pixel dithers between individual
  exposures supports the creation of 4x oversampled images in which the
  FWHM of the point spread function is &lt; ~70 mas (PC) and &lt; ~140 mas
  (WF CCDs). Limited use is made of the shorter exposure time F336W (U)
  data. This poster describes a study of mass segregation in the core of
  47 Tuc using this extremely deep WFPC2 data set. Luminosity functions
  are constructed in a sequence of radial bins, and are compared with
  theoretical luminosity functions (Bergbusch &amp; VandenBerg 1992)
  based on a variety of power-law stellar mass functions. The degree of
  mass segregation is characterized by the slope x of the best fitting
  stellar mass function, where x=+1.35 is the Salpeter value. The mass
  function slope is found to vary from x ~-5 in the cluster center to x
  ~-2 at the edge of the WFPC2 field of view, r ~100'', indicating extreme
  mass segregation in the core of 47 Tuc. The results are coupled with
  image simulations and results derived from a set of archival short WFPC2
  exposures to assess the effect of faint end incompleteness in the latter
  data set. Funding has been provided via a NASA/STScI grant for GO-8267.

Title: Ultraviolet Galaxy Counts from STIS Observations of the Hubble
    Deep Fields
Authors: Gardner, J. P.; Brown, T. M.; Ferguson, H. C.
Bibcode: 2000AAS...196.0607G
Altcode: 2000BAAS...32..685G
  We present galaxy counts in the near and far ultraviolet (NUV and FUV)
  obtained from Space Telescope Imaging Spectrograph (STIS) observations
  of portions of the Hubble Deep Field North, (HDFN), the Hubble Deep
  Field South, (HDFS) and a parallel field near the HDFN. All three fields
  have deep (AB&gt;29) optical imaging, and we determine magnitudes
  by taking the ultraviolet flux detected within the limiting optical
  isophote. An analysis of the UV-optical colors of detected objects,
  combined with a visual inspection of the UV images, indicates that
  there are no detectable objects in the UV images which are not also
  detected in the optical. We measure the detection area and completeness
  as a function of magnitude by taking the size-magnitude distribution
  of galaxies in the entire HDFN WFPC2 V+I image, applying the measured
  UV-optical colors from the detected galaxies, and determining the
  total area over which each galaxy would have been detected in the UV
  images. The average area for the simulated galaxies in each UV magnitude
  bin, (including galaxies which would not be detected at all), provides
  the effective area and completeness for the bin. We test this procedure
  with Monte Carlo simulations. The galaxy counts reach to AB=29 in
  both the NUV and FUV; 1 magnitude fainter than the HDF F300W counts,
  and 7 magnitudes fainter than balloon-based counts. We compare our
  measured counts to various models.

Title: Blue Stragglers in the Core of 47 Tucanae (NGC 104): Bonus
    of an HST Planetary Search
Authors: Guhathakurta, P.; Howell, J. H.; Sarajedini, A.; Gilliland,
   R. L.; Albrow, M. D.; Brown, T. M.; Charbonneau, D.; Burrows, A. S.;
   Cochran, W. D.; Baliber, N.; Edmonds, P. D.; Frandsen, S.; Bruntt,
   H.; Lin, D. N. C.; Vogt, S. S.; Choi, P.; Marcy, G. W.; Mayor, M.;
   Naef, D.; Milone, E. F.; Stagg, C. R.; Williams, M. D.; Sigurdsson,
   S.; VandenBerg, D. A.
Bibcode: 2000AAS...196.4107G
Altcode: 2000BAAS...32..740G
  A secondary data product from the 8.3 d HST campaign to search
  for planetary transits in 47 Tucanae is a set of coadded F555W (V),
  F814W (I), and F336W (U) images with WFPC2 of unprecedented depth and
  resolution (see the poster by R. L. Gilliland, et al.). The pointings
  cover about 100 sub-pixel dither positions so that it is possible to
  construct 4x oversampled images with FWHM&lt; ~70 mas and &lt; ~140
  mas point spread functions in the PC and WF CCDs, respectively. This
  poster uses this high quality data set to study ~100 blue stragglers in
  47 Tuc's core. These include: a bright, strongly centrally concentrated
  population, and a faint population whose radial distribution is similar
  to that of the giants. The faint straggler region of the color-magnitude
  diagram tends to be contaminated by subgiant/turnoff star blend
  artifacts even in ``normal resolution'' (i.e., non-oversampled) WFPC2
  images; this is illustrated using archival short WFPC2 images of 47
  Tuc. A statistical technique is used to separate blend artifacts from
  true faint blue stragglers---the ultra deep WFPC2 data set provides
  a cross check. The technique should be useful for blue straggler
  studies of other clusters for which only normal resolution WFPC2 data
  are available. The luminosity function and photometric properties of
  these two kinds of 47 Tuc blue stragglers are compared to predictions of
  blue straggler formation models. Blue stragglers are also discussed in
  relation to millisecond pulsars and other exotic objects in the cluster
  core. Funding has been provided via a NASA/STScI grant for GO-8267.

Title: HST Photometry of 47 Tucanae: Time Series Analysis and Search
    for Giant Planets
Authors: Brown, T. M.; Charbonneau, D.; Gilliland, R. L.; Albrow,
   M. D.; Burrows, A. S.; Cochran, W. D.; Baliber, N.; Edmonds, P. D.;
   Frandsen, S.; Bruntt, H.; Guhathakurta, P.; Choi, P.; Howell, J. H.;
   Lin, D. N. C.; Vogt, S. S.; Marcy, G. W.; Mayor, M.; Naef, D.; Milone,
   E. F.; Stagg, C. R.; Williams, M. D.; Sarajedini, A.; Sigurdsson,
   S.; VandenBerg, D. A.
Bibcode: 2000AAS...196.0203B
Altcode: 2000BAAS...32..676B
  We have analyzed HST time series data of more than 34000 stars in the
  globular cluster 47 Tuc in a search for transiting Jupiter-sized planets
  in small orbits. The data consist of roughly 645 time samples each
  in bands centered at 555 nm and 814 nm, with fairly uniform sampling
  (except for orbital gaps) over an 8.3-day interval. They are described
  in detail in a poster by Gilliland et al. We used a matched-filter
  technique to search for periodic transit events in these time series
  over a period range between 0.5 and 8.3 days. Blind tests with injected
  artificial transits yielded recovery rates of about 85% for planets
  of 1.3 Jupiter radii, and above 60% for planets of 1.0 Jupiter radii,
  in a sample spanning 4 magnitudes below main sequence turnoff. At
  abstract time, analysis was complete for 27000 stars. These data
  reveal no convincing planet candidates; 15 to 20 detections would be
  expected if the occurrence rate in 47 Tuc were the same as indicated
  by radial velocity searches of stars in the solar neighborhood, and
  if planet radii are indeed above 1 R<SUB>Jup</SUB>. This discrepancy
  suggests that at least one of the processes of formation, migration,
  or survival of close-in planets may be significantly altered in the
  cluster environment. Many elipsing binaries and other variables were
  found in this analysis. Some of them are described by Milone et al. in
  an accompanying poster. Funding has been provided via a NASA/STScI
  GO grant.

Title: A High-Eccentricity Low-Mass Companion to HD 89744
Authors: Korzennik, Sylvain G.; Brown, Timothy M.; Fischer, Debra A.;
   Nisenson, Peter; Noyes, Robert W.
Bibcode: 2000ApJ...533L.147K
Altcode: 2000astro.ph..3045K
  HD 89744 is an F7 V star with a mass of 1.4 M<SUB>solar</SUB>, an
  effective temperature of 6166 K, an age of 2.0 Gyr, and metallicity
  [Fe/H]=0.18. The radial velocity of the star has been monitored
  with the Advanced Fiber-Optic Echelle spectrograph at the Whipple
  Observatory since 1996, and evidence has been found for a low-mass
  companion. The data were complemented by additional data from the
  Hamilton spectrograph at Lick Observatory during the companion's
  periastron passage in the fall of 1999. As a result, we have
  determined the star's orbital wobble to have a period P=256 days,
  an orbital amplitude K=257 m s<SUP>-1</SUP>, and an eccentricity
  e=0.7. From the stellar mass, we infer that the companion has a
  minimum mass m<SUB>2</SUB>sini=7.2 M<SUB>J</SUB> in an orbit with a
  semimajor axis a<SUB>2</SUB>=0.88 AU. The eccentricity of the orbit,
  among the highest known for extrasolar planets, continues the trend
  that extrasolar planets with semimajor axes greater than about 0.15 AU
  tend to have much higher eccentricities than are found in our solar
  system. The high metallicity of the parent star reinforces the trend
  that parent stars of extrasolar planets tend to have high metallicity.

Title: Progress in Observational Asteroseismology
Authors: Brown, T. M.
Bibcode: 2000mons.proc....1B
Altcode:
  No abstract at ADS

Title: Photometric Detection of Transits by Extrasolar Planets
Authors: Brown, T. M.
Bibcode: 2000mons.proc...71B
Altcode:
  Transit photometry provides an efficient way to detect and to study
  extrasolar planets. As the recent detection of transits in HD 209458
  demonstrates, the intensity diminution as a giant planet crosses the
  disk of its star is about 1%, a signal that is easily large enough to
  detect using groundbased telescopes. With spaceborne photometers such as
  MONS, planets of the Earth's size or smaller might be detected. Most
  importantly, planets in transit can be studied in ways that other
  extrasolar planets cannot; in some cases it should be possible to
  derive fairly detailed information about the physical nature of the
  planets from these follow-up studies.

Title: The Spectroscopic Orbit of the Planetary Companion Transiting
    HD 209458
Authors: Mazeh, Tsevi; Naef, Dominique; Torres, Guillermo; Latham,
   David W.; Mayor, Michel; Beuzit, Jean-Luc; Brown, Timothy M.; Buchhave,
   Lars; Burnet, Michel; Carney, Bruce W.; Charbonneau, David; Drukier,
   Gordon A.; Laird, John B.; Pepe, Francesco; Perrier, Christian;
   Queloz, Didier; Santos, Nuno C.; Sivan, Jean-Pierre; Udry, Stéphane;
   Zucker, Shay
Bibcode: 2000ApJ...532L..55M
Altcode: 2000astro.ph..1284M
  We report a spectroscopic orbit with period P=3.52433+/-0.00027 days
  for the planetary companion that transits the solar-type star HD
  209458. For the metallicity, mass, and radius of the star, we derive
  [Fe/H]=0.00+/-0.02, M<SUB>*</SUB>=1.1+/-0.1 M<SUB>solar</SUB>, and
  R<SUB>*</SUB>=1.2+/-0.1 R<SUB>solar</SUB>. This is based on a new
  analysis of the iron lines in our HIRES template spectrum and also on
  the absolute magnitude, effective temperature, and color of the star,
  and it uses isochrones from four different sets of stellar evolution
  models. Using these values for the stellar parameters, we reanalyze the
  transit data and derive an orbital inclination of i=86.1d+/-1.6d. For
  the planet, we derive a mass of M<SUB>p</SUB>=0.69+/-0.05
  M<SUB>Jup</SUB>, a radius of R<SUB>p</SUB>=1.40+/-0.17 R<SUB>Jup</SUB>,
  and a density of ρ=0.31+/-0.07 g cm<SUP>-3</SUP>. Some of the data
  presented herein were obtained at the W. M. Keck Observatory, which is
  operated as a scientific partnership among the California Institute of
  Technology, the University of California, and the National Aeronautics
  and Space Administration. The Observatory was made possible by the
  generous financial support of the W. M. Keck Foundation. The other data
  were obtained at Observatoire de Haute-Provence (France) and with the
  1.2 m Euler Swiss telescope at La Silla Observatory, ESO Chile.

Title: Detecting Planets Using Transit Observations (Invited Review)
Authors: Brown, T. M.
Bibcode: 2000ASPC..219..557B
Altcode: 2000dpp..conf..557B
  No abstract at ADS

Title: The STARE Project: a Transit Search for Hot Jupiters
Authors: Brown, T. M.; Charbonneau, D.
Bibcode: 2000ASPC..219..584B
Altcode: 2000dpp..conf..584B; 2000astro.ph..5009B
  The STARE instrument is a small aperture, wide-field, CCD-based
  telescope that delivers high cadence time series photometry on roughly
  40,000 stars in a typical field centered on the galactic plane. In a
  two-month observing run on a field, we obtain sufficient precision on
  roughly 4,000 stars to detect a close-in Jupiter-sized companion in an
  edge-on orbit. We also used this instrument to detect the planetary
  transits across the Sun-like star HD209458. The project is now in
  its third season, and we have acquired a large dataset on several
  fields. Given the frequency of close-in extrasolar planets found by
  the radial velocity surveys, and the recent confirmation that at least
  some of these are indeed gas giants, the STARE project should be able
  to detect roughly a dozen Jupiter-sized planets in its existing dataset.

Title: Asteroseismology
Authors: Brown, T. M.
Bibcode: 2000upse.conf..141B
Altcode:
  No abstract at ADS

Title: Detection of Planetary Transits Across a Sun-like Star
Authors: Charbonneau, David; Brown, Timothy M.; Latham, David W.;
   Mayor, Michel
Bibcode: 2000ApJ...529L..45C
Altcode: 1999astro.ph.11436C
  We report high-precision, high-cadence photometric measurements of
  the star HD 209458, which is known from radial velocity measurements
  to have a planetary-mass companion in a close orbit. We detect two
  separate transit events at times that are consistent with the radial
  velocity measurements. In both cases, the detailed shape of the transit
  curve due to both the limb darkening of the star and the finite size
  of the planet is clearly evident. Assuming stellar parameters of 1.1
  R<SUB>solar</SUB> and 1.1 M<SUB>solar</SUB>, we find that the data
  are best interpreted as a gas giant with a radius of 1.27+/-0.02
  R<SUB>Jup</SUB> in an orbit with an inclination of 87.1d+/-0.2d. We
  present values for the planetary surface gravity, escape velocity, and
  average density and discuss the numerous observations that are warranted
  now that a planet is known to transit the disk of its parent star.

Title: Evidence for Multiple Companions to υ Andromedae
Authors: Butler, R. Paul; Marcy, Geoffrey W.; Fischer, Debra A.;
   Brown, Timothy M.; Contos, Adam R.; Korzennik, Sylvain G.; Nisenson,
   Peter; Noyes, Robert W.
Bibcode: 1999ApJ...526..916B
Altcode:
  The bright F8 V star υ Andromedae was previously reported to have
  a 4.6 day Doppler velocity periodicity, consistent with having a
  Jupiter-mass companion orbiting at 0.059 AU. Follow-up observations
  by both the Lick and Advanced Fiber-Optic Echelle spectrometer (AFOE)
  planet survey programs confirm this periodicity and reveal additional
  periodicities at 241 and 1267 days. These periodicities are consistent
  with Keplerian orbital motion and imply two additional companions
  orbiting at 0.83 and 2.5 AU, with minimum (Msini) masses of 2.0 and
  4.6 M<SUB>JUP</SUB>, respectively. Non-Keplerian explanations for the
  observed Doppler velocity variations, including radial and nonradial
  pulsations, rotational modulation of surface features, and stellar
  magnetic cycles, are examined. These explanations seem unlikely
  based on the observed photometric and chromospheric stability of the
  star. This putative three-planet system is found to be dynamically
  stable by both analytic techniques and numerical simulations. The
  outer two companions both reside in eccentric orbits, as do all nine
  known extrasolar planet candidates in distant orbits. If real, this
  multiple-planet system is the first around a main-sequence star, and
  its study should offer insights into planet formation, planet-planet
  interactions, and the observed eccentricities of planetary orbits. <P
  />Based on observations obtained at Lick Observatory, operated by the
  University of California, and at the Whipple Observatory, operated by
  the Smithsonian Astrophysical Observatory.

Title: The Evolution of Far-UV Emission in Elliptical Galaxies
Authors: Brown, T. M.; Bowers, C. W.; Kimble, R. A.; Ferguson, H. C.
Bibcode: 1999AAS...195.0912B
Altcode: 1999BAAS...31.1385B
  The restframe UV-to-optical flux ratio, characterizing the ``UV
  upturn'' phenomenon, is potentially the most sensitive tracer of age
  in elliptical galaxies; models predict that it may change by orders
  of magnitude over the course of a few Gyr. In order to trace the
  evolution of the UV upturn as a function of redshift, we have used the
  far-UV camera on the Space Telescope Imaging Spectrograph to image the
  galaxy cluster CL0016+16 at z=0.55. Our 25 " x 25 " field includes four
  bright elliptical galaxies, spectroscopically confirmed to be passively
  evolving cluster members. The weak UV emission from the galaxies in our
  image demonstrates that the UV upturn is very weak at a lookback time
  5.6 Gyr earlier than our own, as compared to measurements of the UV
  upturn in cluster E and S0 galaxies at z=0 and z=0.375. These images
  are the first with sufficient depth to demonstrate the fading of the
  UV upturn expected at moderate redshifts. We discuss these observations
  and the implications for the formation history of galaxies.

Title: Stellar and Planetary Explorer (SPEX)
Authors: Schou, J.; Bogart, R. S.; Bush, R. I.; Hoeksema, J. T.;
   Scherrer, P. H.; Brown, T. M.; Buzasi, D. L.; Horner, S. D.; Korzennik,
   S. G.
Bibcode: 1999AAS...195.8808S
Altcode: 1999BAAS...31.1506S
  The Stellar and Planetary Explorer (SPEX) mission will search for
  terrestrial inner planets around Sun-like (FGK, main sequence) stars
  using photometric techniques as well as provide very long time series
  for asteroseismology. If every Sun-like star had a planetary system
  similar to ours, the proposed instrumentation would detect at least
  100 terrestrial planets similar to the Earth or Venus and be able to
  provide statistics on their diameters and orbital periods. SPEX will
  accomplish this by continuously observing a large number of field stars
  to detect planetary transits. The instrument consists of a fast Schmidt
  camera with a mosaic of large CCD detectors. SPEX will observe a field
  near the galactic plane from a geosynchronous orbit for a minimum of 3
  years. The very long asteroseismic time series will allow inferences
  on the interiors of more than 100 Sun-like stars with a variety of
  masses and ages. This will allow us to substantially refine stellar
  model calculations and in particular improve on the age estimates of
  stars. This in turn is of considerable interest for the understanding
  of the evolution of our galaxy and the universe as a whole. SPEX will
  also provide new data for stellar activity and will be able to detect
  the reflected light from large inner planets, such as those detected
  using ground based Doppler velocity searches.

Title: The STARE Project; A Transit Search for Hot Jupiters
Authors: Brown, T. M.; Charbonneau, D.
Bibcode: 1999AAS...19510907B
Altcode: 1999BAAS...31.1534B
  Radial velocity surveys of nearby, solar-type stars have revealed
  nine planets that orbit their parent stars with a separation of a
  ≲ 0.1 A.U. Close-in, extrasolar giant planets such as these will
  produce a measurable photometric dimming of the star as the planet
  transits the stellar disk. The motivation to undertake a transit
  search is strong: It may be the first detection of extrasolar planets
  by a method other than the radial velocity technique. Furthermore,
  it would be the first survey of planets that is not strongly biased
  toward solar-type stars. In combination with follow-up radial velocity
  observations, transit measurements will yield a direct measurement
  of the planetary radius and mass, which can be combined to calculate
  the average density and surface gravity. These would provide the
  first measurements of the physical characteristics of the planet,
  and provide the first constraints on the structural models. The
  STARE instrument is a small aperture (10 cm), wide-field (6 degree
  square), CCD-based telescope that delivers high cadence (2 minute)
  time series photometry on roughly 40,000 stars (9 &lt; V &lt; 14) in a
  typical field centered on the galactic plane. In a typical two-month
  observing run on a single field, sufficient precision is obtained
  on roughly 4,000 stars to detect a close-in Jupiter-sized companion
  in a near edge-on orbit. The project is now in its third season, and
  has acquired a large dataset on several fields. Based on the results
  of the radial velocity projects, roughly one star in 1,500 surveyed
  should show transits due to a hot Jupiter. Thus, the STARE project
  should either detect numerous Jupiter-sized planets, or, in the event
  of a non-detection, establish that the radial velocity signatures are
  not due to large-radius, planetary-mass orbital companions. The STARE
  project is funded by the NASA Origins of Solar Systems program.

Title: HD 209458
Authors: Latham, D. W.; Charbonneau, D.; Brown, T. M.; Mayor, M.;
   Mazeh, T.; Torres, G.; Beuzit, J. L.; Burnet, M.; Druckier, G. A.;
   Naef, D.; Pepe, F.; Perrier, C.; Queloz, D.; Santos, N.; Sivan, J. P.;
   Udry, S.; Zucker, S.
Bibcode: 1999IAUC.7315....1L
Altcode: 1999IAUC.7315A...1L; 1999IAUC.7315Q...1L
  In response to a request from the Central Bureau, D. W. Latham,
  Harvard-Smithsonian Center for Astrophysics, communicates on behalf
  also of D. Charbonneau, T. M. Brown, M. Mayor, and T. Mazeh: "We
  have prepared an updated ephemeris for the transits of HD 209458. This
  ephemeris is based on 150 velocity observations dating back to Aug. 1997
  (made with HIRES on Keck I, as part of the G Dwarf Planet Search under
  NASA time, with ELODIE on the 1.93-m telescope at Observatoire de Haute
  Provence, and with CORALIE on the new Swiss 1.2-m telescope at La Silla;
  a paper describing the spectroscopic results is in preparation) and
  on two complete transit observations obtained on 1999 Sept. 8 and 15
  (made by Charbonneau and Brown with the STARE instrument at the High
  Altitude Observatory, National Center for Atmospheric Research, Boulder,
  and reported in a paper submitted to Ap.J. Lett. by Charbonneau, Brown,
  Latham, and Mayor). G. Torres has carried out a simultaneous solution
  of the radial velocities and the transit observations and provided the
  following orbital period and epoch of transit center: P = 3.52433 +/-
  0.00027 days, T_c = 2451430.8238 +/- 0.0033 (HJD). Predictions for
  the center of the transits through the end of Dec. 1999 are: HJD
  2451508.3590 +/- 0.0080, 2451511.8833 +/- 0.0083, 2451515.4077 +/-
  0.0086, 2451518.9320 +/- 0.0089, 2451522.4563 +/- 0.0091, 2451525.9806
  +/- 0.0094, 2451529.5050 +/- 0.0097, 2451533.0293 +/- 0.010, 2451536.554
  +/- 0.010, 2451540.078 +/- 0.011, 2451543.602 +/- 0.011. Observers
  should plan to monitor the star for at least 2 hr before and after
  these times of transit center. Our identification of HD 209458 as a
  prime target for transit observations was made possible by the many
  contributions of the G Dwarf Planet Search, ELODIE, and CORALIE teams:
  J. L. Beuzit, M. Burnet, G. A. Druckier, D. Naef, F. Pepe, C. Perrier,
  D. Queloz, N. Santos, J. P. Sivan, G. Torres, S. Udry, and S. Zucker."

Title: Evidence for a system of planets orbiting Upsilon Andromedae.
Authors: Noyes, R. W.; Korzennik, S. G.; Nisenson, P.; Holman, M. J.;
   Contos, A.; Brown, T. M.
Bibcode: 1999BAAS...31.1236N
Altcode:
  No abstract at ADS

Title: Evidence for a System of Planets Orbiting Upsilon Andromedae
Authors: Noyes, R. W.; Korzennik, S. G.; Nisenson, P.; Holman, M. J.;
   Contos, A.; Brown, T. M.
Bibcode: 1999AAS...194.1404N
Altcode: 1999BAAS...31..847N
  Using the Advanced Fiber Optic Echelle (AFOE) spectrograph at SAO's
  Whipple Observatory, we have monitored the radial velocity of Upsilon
  Andromedae since September 1994. Similar observations were made by the
  "Lick" group (P. Butler, G. Marcy, D. Fischer; see Paper 14.02).The AFOE
  data show, in addition to the already known close-in ``hot Jupiter''
  in a 4.6-day circular orbit, two additional companions. The middle
  companion has a well-defined orbit, with semi-major axis about
  0.83 AU, period 243.5 days, eccentricity 0.22, and minimum mass
  (M sin i) of 2 Jupiter masses. This is in very close agreement with
  independent findings by the Lick group. The AFOE data alone do not
  yield well-determined orbital parameters for the outer companion,
  because the total observing span encompasses only about one period of
  its orbit. However, the data are consistent with parameters derived
  for that companion by the Lick group from data with a longer time span,
  and when combined with the Lick data yield a semi-major axis of 2.5 AU,
  orbital period of 1267 days, eccentricity of 0.41, and minimum mass
  about 4.6 Jupiter masses. These results, independently obtained by two
  different groups with different instruments and analysis methodologies,
  together give strong indications that a true planetary ``system'' has
  now been discovered around a star like our own. We have carried out
  numerical integrations which show that this system can be stable, but
  only for certain combinations of periods, masses, and eccentricities
  of the outer two companions. The stability requirement thus provides
  a prediction that can be tested as the orbital elements of the outer
  companion are refined. In addition, it imposes an upper limit on the
  actual planetary masses, and on the difference in orbital inclination of
  the two outer planets. Finally, the numerical integrations imply that
  the longitudes of periastron of the two outer companions are locked to
  nearly the same value, in accord with the present observations. This
  work was supported by NASA, NSF, and the Smithsonian Institution.

Title: Probing the Outskirts of an Extrasolar Planet: Photometry
    and Spectroscopy
Authors: Brown, Timothy
Bibcode: 1999hst..prop.8789B
Altcode: 1999hst..prop.4860B
  HD 209458 is the first extrasolar planet known to transit the disk
  of its parent star. HST can provide unique probes of this system
  for moons, rings and atmospheric composition that are unlikely to be
  feasible with ground-based observations. Furthermore, we note that
  since HD 209458 will come out of the solar avoidance zone in mid-
  April 2000, it will be observable to HST several months before the
  first decent transits can be followed from the ground. The field of
  extrasolar planets is one that proceeds with breakneck speed {the
  entire field is only four years old}, and next fall HD 209458 will
  no doubt be the subject of intensive study. The analysis of the data
  acquired by this project may be critically important in its own right,
  and should help significantly to define optimum follow-on observations
  during the coming year. Timely analysis and publication of the data
  will clearly be a top priority to the authors of this proposal. HST
  is thus in a unique position to deliver a wealth of science on this
  first transiting extrasolar planet early next year.

Title: A Deep UV STIS Image of Hot Horizontal Branch Stars in M32
Authors: Brown, T. M.; Bowers, C. W.; Kimble, R. A.; Sweigart, A. V.;
   Ferguson, H. C.
Bibcode: 1999AAS...194.0713B
Altcode: 1999BAAS...31Q.833B
  We present the deepest near-UV image of M32, which for the first time
  resolves hot horizontal branch (HB) stars in an elliptical galaxy. Given
  the near-solar metallicity of M32, much larger than that of globular
  clusters, the existence of an extended horizontal branch is a striking
  example of the second parameter effect, and, most importantly,
  provides direct evidence that hot HB stars are the major contributors
  to the UV upturn phenomenon observed in elliptical galaxies. Our image,
  obtained with the Space Telescope Imaging Spectrograph (STIS), detects
  approximately 8000 stars in a 25x25 arcsec field, centered 7.7 arcsec
  from the galaxy core. These stars span a range of 21-28 mag in the
  STMAG system, and in the deepest parts of the image, our catalog is
  reasonably complete (&gt; 25%) to a magnitude of 27. The hot HB spans
  a magnitude range of 25-27 at effective temperatures hotter than 8500
  K. We interpret the luminosity function with an extensive set of HB
  and post-HB evolutionary tracks.

Title: The Lyα Forest of the Quasar in the Hubble Deep Field South
Authors: Savaglio, S.; Ferguson, H. C.; Brown, T. M.; Espey, B. R.;
   Sahu, K. C.; Baum, S. A.; Carollo, C. M.; Kaiser, M. E.; Stiavelli,
   M.; Williams, R. E.; Wilson, J.
Bibcode: 1999ApJ...515L...5S
Altcode: 1999astro.ph..1022S
  The quasar in the Hubble Deep Field South (HDF-S), J2233-606
  (z<SUB>em</SUB>=2.23), has been observed exhaustively by ground-based
  telescopes and by the Space Telescope Imaging Spectrograph on board
  the Hubble Space Telescope at low, medium, and high resolution in
  the spectral interval from 1120 to 10000 Å. The combined data give
  continuous coverage of the Lyα forest from redshift 0.9 to 2.24. This
  very large baseline represents a unique opportunity to study in detail
  the distribution of clouds associated with emitting structures in the
  field of the quasar and in nearby fields already observed as part of
  the HDF-S campaign. Here we report on the main properties obtained from
  the large spectroscopic data set that is available for the Lyα clouds
  in the intermediate-redshift range of 1.20-2.20, where our present
  knowledge has been complicated by the difficulty in producing good
  data. The number density is shown to be higher than what is expected
  by extrapolating the results from both lower and higher redshifts:
  63+/-8 lines with logN<SUB>HI</SUB>&gt;=14.0 are found (including
  metal systems) at =1.7, compared with the ~40 lines predicted by
  extrapolating from previous studies. The redshift distribution of the
  Lyα clouds shows a region spanning z~=1.383-1.460 (comoving size of 94
  h<SUP>-1</SUP><SUB>65</SUB> Mpc, Ω<SUB>0</SUB>=1) with a low density
  of absorption lines; we detect five lines in this region, compared with
  the 16 expected from an average density along the line of sight. The
  two-point correlation function shows a positive signal up to scales
  of about 3 h<SUP>-1</SUP><SUB>65</SUB> Mpc and an amplitude that is
  larger for larger H I column densities. The average Doppler parameter
  is about 27 km s<SUP>-1</SUP>, which is comparable to the mean value
  found at z&gt;3, thus casting doubts on the temperature evolution of
  the Lyα clouds. <P />Based on observations made with the NASA/ESA
  Hubble Space Telescope by the Space Telescope Science Institute,
  which is operated by AURA, Inc., under NASA contract NAS5-26555.

Title: Doppler Imaging of Stellar Oscillations: Multi-Site
    Observations of Epsilon Cephei
Authors: Kennelly, E. J.; Brown, T. M.; Ehrenfreund, P.; Foing,
   B.; Hao, J.; Horner, S.; Korzennik, S.; Nisenson, P.; Noyes, R.;
   Sonnentrucker, P.
Bibcode: 1999ASPC..185..264K
Altcode: 1999IAUCo.170..264K; 1999psrv.conf..264K
  We investigate the oscillation properties of ɛ Cep using a series of
  specialized techniques designed to extract and analyze time variations
  in absorption line profiles. To obtain the necessary temporal coverage
  for this investigation, multi-site observations were collected at
  3 sites (China, France, Arizona) all equipped with high-resolution
  echelle spectrographs. From these observations, we find evidence for
  a very rich spectrum of modes in ɛ Cep.

Title: Dating intermediate-age populations with main-sequence A and
    F-type stars
Authors: Lanz, T.; Heap, S.; Brown, T. M.; Hubeny, I.; Yi, S.
Bibcode: 1999ASPC..192..106L
Altcode: 1999sdsg.conf..106L
  No abstract at ADS

Title: On the Age Estimation of High Redshift Galaxies
Authors: Yi, S.; Brown, T. M.; Heap, S.; Hubeny, I.; Landsman, W.;
   Lanz, T.; Sweigart, A.
Bibcode: 1999ASPC..192..126Y
Altcode: 1999sdsg.conf..126Y
  No abstract at ADS

Title: Measurements of the UV Upturn in Local and
    Intermediate-Redshift Ellipticals
Authors: Brown, T. M.
Bibcode: 1999ASPC..192..315B
Altcode: 1999sdsg.conf..315B; 1999astro.ph..5377B
  The rest-frame UV contains the most sensitive indicators of age for
  elliptical galaxies. While the near-UV flux from young ellipticals
  isolates the main sequence turnoff, the far-UV flux in old ellipticals
  is dominated by hot horizontal branch (HB) stars. This evolved
  population was first revealed by early UV observations showing a sharp
  flux increase shortward of rest-frame 2500 A, subsequently dubbed the
  "UV upturn." The phenomenon has since been characterized in many
  local ellipticals, and measurements at intermediate redshifts are
  now underway. Once ellipticals reach ages of 5-10 Gyr, stellar and
  galactic evolution theories predict that the UV-to-optical flux ratio
  can increase by orders of magnitude over timescales of a few Gyr, making
  the UV upturn the most rapidly evolving feature of these galaxies. It is
  thus expected to fade dramatically with increasing redshift. I review
  the imaging and spectroscopic evidence for the nature of the UV upturn
  in nearby ellipticals, and then present observations that measure the
  UV upturn at an epoch significantly earlier than our own. Far-UV data
  from the HUT demonstrate that the spectra of nearby ellipticals are
  dominated by hot HB stars. FOC UV imaging of M32 and the M31 bulge
  detected the UV-bright phases of post-HB stars, but did not reach the
  HB itself. Recent STIS observations were the first to image the hot
  HB and post-HB stars in the center of the nearest elliptical galaxy,
  M32; these observations also show a striking lack of UV-bright post-AGB
  stars. FOC observations of Abell 370, a rich galaxy cluster at z=0.375,
  show that giant ellipticals at a lookback time of 4 Gyr can exhibit
  strong UV luminosity, with no evidence of evolution in the UV upturn
  between this epoch and our own, thus implying a high redshift of
  formation (z_f &gt; 4).

Title: Color-Luminosity Relations for the Resolved Hot Stellar
    Populations in the Centers of M31 and M32
Authors: Brown, T. M.; Ferguson, H. C.; Stanford, S. A.; Deharveng, J.
Bibcode: 1999IAUS..192..195B
Altcode:
  We present Faint Object Camera (FOC) ultraviolet images of the central
  14 x 14'' of Messier 31 and Messier 32. The hot stellar population
  detected in the composite UV spectra of these nearby galaxies is
  partially resolved into individual stars, and their individual colors
  and apparent magnitudes are measured. We detect 433 stars in M31
  and 138 stars in M32, down to detection limits of m<SUB>F275W</SUB>
  = 25.5 mag and m<SUB>F175W</SUB> = 24.5 mag. We investigate the
  luminosity functions of the sources, their spatial distribution,
  their color-magnitude diagrams, and their total integrated far-UV
  flux. Although M32 has a weaker UV upturn than M31, the luminosity
  functions and color-magnitude diagrams of M31 and M32 are surprisingly
  similar, and are inconsistent with a majority contribution from any
  of the following: PAGB stars more massive than 0.56 M<SUB>odot</SUB>,
  main sequence stars, or blue stragglers. Both the luminosity functions
  and color-magnitude diagrams are consistent with a dominant population
  of stars that have evolved from the extreme horizontal branch (EHB)
  along tracks with masses between 0.47 and 0.53 M<SUB>odot</SUB>. These
  stars are well below the detection limits of our images while on the
  zero-age EHB, but become detectable while in the more luminous (but
  shorter) AGB-Manque and post-early asymptotic giant branch (PEAGB)
  phases. The FOC observations require that only a very small fraction of
  the main sequence population (2% in M31 and 0.5% in M32) in these two
  galaxies evolve though the EHB and post-EHB phases, with the remainder
  evolving through bright PAGB evolution that is so rapid that few if
  any stars are expected in the small field of view covered by the FOC.

Title: The Planet Orbiting ρ Coronae Borealis
Authors: Noyes, R. W.; Contos, A. R.; Korzennik, S. G.; Nisenson,
   P.; Brown, T. M.; Horner, S. D.
Bibcode: 1999ASPC..185..162N
Altcode: 1999IAUCo.170..162N; 1999psrv.conf..162N
  Continuing precise radial velocity observations of ρ Coronae Borealis
  have allowed the determination of updated parameters of the 40-day
  orbit of its Jupiter-mass companion. This confirms the near-zero
  eccentricity of the orbit, and provides improved predictions for the
  times of possible transit of the companion in front of the star. The
  new data provide more stringent upper limits to the mass of a possible
  second companion to the system. The orbital parameters are discussed in
  the light of several different scenarios for the origin and migration
  of extra-solar giant planets.

Title: Age and Metallicity of F-type Stars
Authors: Lanz, T.; Heap, S. R.; Brown, T. M.; Hubeny, I.; Yi, S.
Bibcode: 1998AAS...193.0302L
Altcode: 1998BAAS...30.1246L
  The rest-frame ultraviolet spectrum of intermediate-age stellar
  populations (1 to few Gyr) is dominated by the UV flux of F-type
  stars at the main sequence turn-off. We have obtained high-resolution
  spectra of four well-studied F stars with STIS aboard HST to calibrate
  ultraviolet spectral features in terms of age and metallicity. The UV
  spectrum is mostly degenerate in terms of effective temperature and
  metallicity, but we found that two spectral indices, [2850/2770] and
  [2310/3040], allow a discrimination between these two parameters. The
  first index measures mainly the strength of Mg I 2852, while the second
  index is the mid-UV color. We find that the Mg I index is sensitive
  to the effective temperature, but insensitive to metallicity; the
  UV color is sensitive to both metallicity and T_eff. We discuss the
  importance of departures from LTE and chromospheric activity on these
  two spectral indices. We apply our results to estimate the time since
  the last major star formation episode in the early-type galaxy LBDS
  53W091 at redshift z=1.55.

Title: Measurements of Far-UV Emission from Elliptical Galaxies
    at z=0.375
Authors: Brown, T. M.; Ferguson, H. C.; Deharveng, J. -M.;
   Jedrzejewski, R. I.
Bibcode: 1998AAS...193.0907B
Altcode: 1998BAAS...30R1261B
  The ``UV upturn'' is a sharp rise in spectra of elliptical galaxies
  shortward of rest-frame 2500 Angstroms. It is a ubiquitous phenomenon
  in nearby giant ellipticals, and is thought to arise primarily
  from low-mass evolved stars on the extreme horizontal branch and
  beyond. Models suggest that the UV upturn is a very strong function of
  age for these old stellar populations, increasing as the galaxy gets
  older. In some models the change in UV/optical flux ratio is a factor
  of 25 over timescales of less than 3 Gyr. To test the predictions
  for rapid evolution of the UV upturn, we have observed a sample of
  normal elliptical galaxies in the z=0.375 cluster Abell 370 with the
  Faint Object Camera aboard the Hubble Space Telescope. A combination
  of two long-pass filters was used to isolate wavelengths shortward of
  rest-frame 2700 Angstroms, providing a measurement of the UV upturn at a
  lookback time of approximately 4 Gyr. Surprisingly, the four ellipticals
  observed show a range of UV upturn strength that is similar to that
  seen in nearby ellipticals, with an equivalent m<SUB>1550</SUB>-V
  color ranging from 2.9--3.4 mag. Our result is inconsistent with some
  models for the UV upturn; other models are consistent only for a high
  redshift of formation (z_f &gt;= 4).

Title: The Hubble Deep Field South: Flanking Fields
Authors: Lucas, R. A.; Baum, S. A.; Casertano, S.; de Mello, D.;
   Dickinson, M.; Ferguson, H. C.; Fruchter, A. S.; Gonzalez-Lopezlira,
   R.; Heyer, I.; Mack, J.; Makidon, R.; Martin, C. L.; Mutchler, M.;
   Smith, E.; Stiavelli, M.; Teplitz, H. I.; Wiggs, M. S.; Williams,
   R.; Zurek, D.; Brown, T. M.; Gardner, J. P.; Kaiser, M. E.; Hook, R. N.
Bibcode: 1998AAS...193.7506L
Altcode: 1998BAAS...30.1367L
  Due to the availability of the STIS and NICMOS instruments at the time
  of the observations, the Hubble Deep Field - South Flanking Fields
  are more complex and varied than those of the Hubble Deep Field -
  North. In addition to the WFPC2 Flanking Fields, there are parallel
  observations in STIS and NICMOS for each, and there are also a series
  of STIS observations of the NICMOS deep field, and associated WFPC2 and
  NICMOS parallels as well. In this paper, we will present the data and
  describe the data reduction process used for the HDF-S Flanking Fields.

Title: The Hubble Deep Field South: UV Spectroscopy of QSO J2233-606
Authors: Ferguson, H. C.; Baum, S. A.; Busko, I.; Espey, B. R.;
   Gonnella, A.; Hayes, J.; Hodge, P.; Martin, C. L.; Sahu, K. C.;
   Savaglio, S.; Smith, E.; Williams, R.; Wilson, J.; Brown, T. M.;
   Gardner, J. P.; Carollo, C. M.; Kaiser, M. E.
Bibcode: 1998AAS...193.7502F
Altcode: 1998BAAS...30Q1366F
  QSO J2233-606 was observed with the Space Telescope Imaging Spectrograph
  during the HDF-South campaign. The spectroscopic observations
  covered wavelengths from 1150 to 3560 { Angstroms} at a range of
  resolutions. The QSO spectrum is attenuated by a Lyman-limit absorption
  line system at z ~ 1.9, but the flux recovers in the far-UV. Most of
  the spectroscopic observing time (155 ks) was devoted to obtaining
  observations with the medium-resolution echelle grating at a resolution
  of 10 km/s. The spectra show a rich forest of absorption lines, some
  arising from Lyman alpha in the redshift range 1.2 to 1.5, and others
  from higher order Lyman series lines of higher-redshift systems. At
  shorter wavelengths, some strong absorption line systems are seen
  at the 250-400 km/s resolution with the low-resolution gratings. The
  higher-redshift Lyman alpha forest is detected at 50 km/s resolution
  in the 3100-3560 { Angstroms} region.

Title: The Hubble Deep Field -- South: STIS Imaging
Authors: Gardner, J. P.; Brown, T. M.; Teplitz, H. I.; Baum, S. A.;
   Espey, B. R.; Ferguson, H. C.; Fruchter, A. S.; Gonnella, A.; Hayes,
   J.; Martin, C. L.; Sahu, K. C.; Savaglio, S.; Smith, E.; Williams,
   R.; Wilson, J.; Carollo, C. M.; Kaiser, M. E.; Hook, R. N.
Bibcode: 1998AAS...193.7503G
Altcode: 1998BAAS...30.1366G
  We present the imaging observations made with the Space Telescope
  Imaging Spectrograph of the Hubble Deep Field -- South. The field was
  imaged in 4 bandpasses, a clear CCD bandpass for 156 ksec, a long-pass
  filter for 25 ksec, a Near-UV bandpass for 23 ksec and a Far-UV bandpass
  for 52 ksec. The clear visible image is the deepest observation ever
  made in the UV-NIR wavelength region. The field contains QSO J2233-606,
  the target of the STIS spectroscopy, and extends 50arcsec x 50arcsec
  for the visible images, and 25arcsec x 25arcsec for the ultraviolet
  images. We present the images, catalog of objects, and galaxy counts
  obtained in the field.

Title: The Southern Hubble Deep Field: HDF-S
Authors: Williams, R.; Baum, S. A.; Bergeron, L. E.; Blacker, B.;
   Boyle, B. J.; Brown, T. M.; Bernstein, N.; Carollo, C. M.; Casertano,
   S.; de Mello, D.; Dickinson, M.; Espey, B. R.; Ferguson, H. C.;
   Fruchter, A. S.; Gardner, J. P.; Gonnella, A.; Gonzalez, R.; Hayes, J.;
   Hewett, P.; Heyer, I.; Hook, R. N.; Jones, D.; Kaiser, M. E.; Lubenow,
   A.; Lucas, R. A.; Mack, J.; MacKenty, J. W.; Madau, P.; Makidon, R.;
   Martin, C. L.; Mazzuca, L.; Mutchler, M.; Norris, R. P.; Perriello,
   B.; Postman, M.; Royle, P.; Sahu, K. C.; Savaglio, S.; Sherwin, A.;
   Smith, E.; Stiavelli, M.; Teplitz, H. I.; van der Marel, R.; Weymann,
   R. J.; Wiggs, M. S.; Williger, G. M.; Wilson, J.; Zurek, D.
Bibcode: 1998AAS...193.7501W
Altcode: 1998BAAS...30.1366W
  177 orbits of HST imaging and spectroscopy were devoted to three
  adjacent fields plus flanking fields in the southern CVZ in October
  1998, in an observing program similar to the original northern HDF. Two
  important features of the HDF-S make it distinct from the HDF-N: (1)
  simultaneous observations with WFPC2, STIS, and NICMOS in parallel
  observing modes, leading to imaging of three separate fields, and (2)
  the inclusion of a z<SUB>em</SUB>=2.2 quasar in the line of sight for
  the STIS field. The HDF-S observations produced WFPC2 images in U,
  B, V, and I; a deep STIS image of the field surrounding the quasar;
  spectroscopy of the quasar with STIS from 1150-3560 Angstroms; and deep
  imaging of an adjacent field with NICMOS in the J, H, and K bands. All
  of the data, both raw and reduced, have been made public on 23 November
  1998 and are available from the HST archive for analysis.

Title: The Hubble Deep Field South: Deep uBVRI Imaging of 1/2
    Square Degree
Authors: Teplitz, H. I.; Gardner, J. P.; Palunas, P.; Sahu, M. S.;
   Malumuth, E. M.; Woodgate, B. E.; Heap, S. R.; Williger, G. M.; Danks,
   A. C.; Smette, A.; Brown, T. M.; Kaiser, M. E.; Gull, T. R.
Bibcode: 1998AAS...193.7507T
Altcode: 1998BAAS...30.1367T
  We present 1/2 square degree uBVRI imaging around the Hubble Deep Field
  -- South. The images were obtained with the Big Throughput Camera at
  CTIO in 1998 September. We will discuss the broad-band photometry of
  this field and present the statistics of ~ 50000 galaxies, including
  number-magnitude counts and clustering properties. The deep field was
  chosen for the presence of the z=2.25 QSO J2233-606, which has multiple
  absorption systems that may mark large scale structures. We also discuss
  the color distribution of galaxies and u-band dropouts. We compare our
  photometric measurements with the high resolution images available from
  the HST observations. We will make the images and catalogs presented
  here available over the WWW.

Title: Acoustic Power Maps of Solar Active Regions
Authors: Hindman, Bradley W.; Brown, Timothy M.
Bibcode: 1998ApJ...504.1029H
Altcode:
  Using observations made by the Michelson Doppler Imager (MDI), we find
  that within solar active regions the spatial distributions of Doppler
  velocity power and continuum intensity power differ. The oscillation
  power within any pixel is a strong function of the magnetic field
  strength within that pixel. The amplitudes of oscillations with
  frequencies less than 5.2 mHz decrease with field strength for both
  velocity and continuum intensity measurements. However, within active
  regions oscillations with frequencies between 5.2 and 7.0 mHz have
  suppressed continuum intensity amplitudes but enhanced velocity
  amplitudes. The enhancement of the high-frequency velocity signal
  is largest in pixels with intermediate field strength (50-250 G)
  and is a manifestation of the high-frequency acoustic halos. We find
  that the high-frequency halos are absent in MDI observations of the
  continuum intensity.

Title: Exoplanets or Dynamic Atmospheres? The Radial Velocity and
    Line Shape Variations of 51 Pegasi and τ Bootis
Authors: Brown, Timothy M.; Kotak, Rubina; Horner, Scott D.;
   J. Kennelly, Edward; Korzennik, Sylvain; Nisenson, P.; Noyes, Robert W.
Bibcode: 1998ApJS..117..563B
Altcode: 1998astro.ph..1166B
  The stars 51 Pegasi and τ Bootis show radial velocity variations that
  have been interpreted as resulting from companions with roughly Jovian
  mass and orbital periods of a few days. Gray and Gray &amp; Hatzes
  reported that the radial velocity signal of 51 Peg is synchronous with
  variations in the shape of the line λ6253 Fe I; thus, they argue that
  the velocity signal arises not from a companion of planetary mass but
  from dynamic processes in the atmosphere of the star, possibly nonradial
  pulsations. Here we seek confirming evidence for line shape or strength
  variations in both 51 Peg and τ Boo, using R = 50,000 observations
  taken with the Advanced Fiber Optic Echelle. Because of our relatively
  low spectral resolution, we compare our observations with Gray's line
  bisector data by fitting observed line profiles to an expansion in terms
  of orthogonal (Hermite) functions. To obtain an accurate comparison,
  we model the emergent line profiles from rotating and pulsating stars,
  taking the instrumental point-spread function into account. We describe
  this modeling process in detail. We find no evidence for line profile or
  strength variations at the radial velocity period in either 51 Peg or in
  τ Boo. For 51 Peg, our upper limit for line shape variations with 4.23
  day periodicity is small enough to exclude with 10 σ confidence the
  bisector curvature signal reported by Gray &amp; Hatzes; the bisector
  span and relative line depth signals reported by Gray are also not seen,
  but in this case with marginal (2 σ) confidence. We cannot, however,
  exclude pulsations as the source of 51 Peg's radial velocity variation
  because our models imply that line shape variations associated with
  pulsations should be much smaller than those computed by Gray &amp;
  Hatzes; these smaller signals are below the detection limits both for
  Gray &amp; Hatzes's data and for our own. τ Boo's large radial velocity
  amplitude and v sin i make it easier to test for pulsations in this
  star. Again we find no evidence for periodic line shape changes, at a
  level that rules out pulsations as the source of the radial velocity
  variability. We conclude that the planet hypothesis remains the most
  likely explanation for the existing data.

Title: Accurate Determination of the Solar Photospheric Radius
Authors: Brown, T. M.; Christensen-Dalsgaard, J.
Bibcode: 1998ApJ...500L.195B
Altcode: 1998astro.ph..3131B
  The Solar Diameter Monitor measured the duration of solar meridian
  transits during the 6 years 1981-1987, spanning the declining half of
  solar cycle 21. We have combined these photoelectric measurements with
  models of the solar limb-darkening function, deriving a mean value for
  the solar near-equatorial radius of 695.508+/-0.026 Mm. Annual averages
  of the radius are identical within the measurement error of +/-0.037 Mm.

Title: Detection of Extrasolar Planets by Transit Photometry in
    the Antarctic
Authors: Borucki, William J.; Koch, David G.; Lissauer, Jack J.;
   Brown, Timothy M.; Jenkins, Jon M.; Dunham, Edward T.
Bibcode: 1998AAS...192.6223B
Altcode: 1998BAAS...30R.909B
  The recent discovery by the Doppler velocity technique that
  approximately 2% to 3% of the solar-like stars possess giant planets
  demonstrates that ground-based detection of extrasolar planets is
  feasible. Photometric detection of transits can provide the size of
  planetary companions and determine both orbital period and inclination
  angle. Subsequent Doppler velocity measurements can then estimate the
  mass since the inclination angle is known. The combination of mass
  and size allows the density of these objects to be determined. These
  data can then be used to compare with theoretical predictions of
  the inflation of a planet's atmosphere as a function of its distance
  from the primary. Follow on observations at major observatories using
  high resolution spectrographs can be made to determine the spectral
  class and metallicity of the stars found to have planets so that
  correlations with these quantities and the frequency of planets and
  their orbital radii can be investigated. Only a small aperture (i.e.,
  10 cm to 30 cm), wide-field-of-view telescope with a CCD detector and
  several weeks of continuous observation are required to detect planets
  around a variety of stars. By observing approximately 4,000 stars
  continuously, approximately four giant inner planets (like 51 Peg b)
  with orbital periods near 4 days should be discovered each month;
  i.e. approximately 16 planets during the four month winter period in
  Antarctica. The availability of continuous observing would dramatically
  improve the yield of searches now being conducted at other locations
  in the presence of day/night cycles.

Title: The Oscillations of Tau Pegasi
Authors: Kennelly, E. J.; Brown, T. M.; Kotak, R.; Sigut, T. A. A.;
   Horner, S. D.; Korzennik, S. G.; Nisenson, P.; Noyes, R. W.; Walker,
   A.; Yang, S.
Bibcode: 1998ApJ...495..440K
Altcode:
  We present extensive spectroscopic time series observations of the
  multiperiodic, rapidly rotating, δ Scuti star τ Pegasi. Information
  about the oscillations is contained within the patterns of line-profile
  variation of the star's blended absorption-line spectrum. We introduce
  the new technique of Doppler deconvolution with which to extract these
  patterns by modeling the intrinsic stellar spectrum and the broadening
  functions for each spectrum in the time series. Frequencies and modes
  of oscillation are identified from the variations using the technique
  of Fourier-Doppler imaging and a two-dimensional least-squares cleaning
  algorithm. We find a rich mode spectrum with degrees up to l = 20 and
  with frequencies below about 35 cycles day<SUP>-1</SUP>. Those modes
  with the largest amplitudes have frequencies that lie within a narrow
  band. We conclude that the observed spectrum can be explained if the
  modes of τ Peg propagate in the prograde direction with l ~= |m| and
  with frequencies that are about equal in the corotating frame of the
  star. We discuss the implications of these results for the prospect
  of δ Scuti seismology.

Title: A Search for Line Shape and Depth Variations in 51 Pegasi
    and τ Bootis
Authors: Brown, Timothy M.; Kotak, Rubina; Horner, Scott D.; Kennelly,
   Edward J.; Korzennik, Sylvain; Nisenson, P.; Noyes, Robert W.
Bibcode: 1998ApJ...494L..85B
Altcode: 1997astro.ph.12279B
  Spectroscopic observations of 51 Pegasi and τ Bootis show no periodic
  changes in the shapes of their line profiles; these results for 51
  Peg are in significant conflict with those reported by Gray &amp;
  Hatzes. Our detection limits are small enough to rule out nonradial
  pulsations as the cause of the variability in τ Boo, but not in 51
  Peg. The absence of line shape changes is consistent with these stars'
  radial velocity variability arising from planetary mass companions.

Title: The Stellar and Planetary Explorer (SPEX) Mission
Authors: Schou, J.; Scherrer, P. H.; Brown, T. M.; Frandsen, S.;
   Horner, S. D.; Korzennik, S. G.; Noyes, R. W.; Tarbell, T. D.; Title,
   A. M.; Walker, A. B. C., II; Weiss, W. W.; Bogart, R. S.; Bush, R. I.;
   Christensen-Dalsgaard, J.; Hoeksema, J. T.; Jones, A.; Kjeldsen, H.
Bibcode: 1998ESASP.418..401S
Altcode: 1998soho....6..401S
  The Stellar and Planetary Explorer (SPEX) is a mission designed
  to search for terrestrial sized planets around sun-like stars using
  precise photometry. The planets will be detected by searching for the
  decrease in brightness associated with transits of the planets in front
  of their parent stars. One of the secondary scientific objective of
  SPEX is to do asteroseismology on a number of sun-like stars. SPEX
  is designed as a secondary payload on a commercial communications
  satellite and will have a design life time of three years. We will
  provide an overview of the SPEX scientific objectives and design,
  with particular emphasis on the prospects for doing asteroseismology.

Title: Observational Challenges in Asteroseismology
Authors: Brown, Timothy M.
Bibcode: 1998ASPC..154..289B
Altcode: 1998csss...10..289B
  Asteroseismology of Sun-like stars will probably be done best by means
  of CCD photometry from space. However, making this happen is going to
  take hard work and organization. In the meantime, significant progress
  is being made on spectroscopic studies of F- and G-type subgiants,
  and important advances are being made in techniques for measuring
  modes in delta Scuti stars.

Title: Ultraviolet Spectral Dating of Stars and Galaxies
Authors: Heap, S. R.; Brown, T. M.; Hubeny, I.; Landsman, W.; Yi,
   S.; Fanelli, M.; Gardner, J. P.; Lanz, T.; Maran, S. P.; Sweigart,
   A.; Kaiser, M. E.; Linsky, J.; Timothy, J. G.; Lindler, D.; Beck,
   T.; Bohlin, R. C.; Clampin, M.; Grady, J.; Loiacono, J.; Krebs, C.
Bibcode: 1998ApJ...492L.131H
Altcode:
  An echelle spectrogram (R = 30,000) of the 2300-3100 Å region in
  the ultraviolet spectrum of the F8 V star 9 Comae is presented. The
  observation is used to calibrate features in the mid-ultraviolet spectra
  of similar stars according to age and metal content. In particular, the
  spectral break at 2640 Å is interpreted using the spectral synthesis
  code SYNSPEC. We use this feature to estimate the time since the last
  major star formation episode in the early-type galaxy LBDS 53W091 at
  redshift z=1.55, whose rest-frame mid-ultraviolet spectrum, observed
  with the Keck Telescope, is dominated by the flux from similar stars
  that are at or near the main-sequence turnoff in that system (Spinrad
  et al.). Our result, 1 Gyr if the flux-dominating stellar population
  has a metallicity twice solar, or 2 Gyr for a more plausible solar
  metallicity, is significantly lower than the previous estimate and
  thereby relaxes constraints on cosmological parameters that were implied
  by the earlier work. <P />Based on observations with the NASA/ESA Hubble
  Space Telescope, obtained at the Space Telescope Science Institute,
  which is operated by the Association of Universities for Research in
  Astronomy, Inc., under NASA contract NAS5-2655.

Title: Exoplanet Research with the Advanced Fiber Optic Echelle
Authors: Korzennik, S. G.; Brown, T. M.; Contos, A. R.; Horner, S.;
   Jha, S.; Kennelly, T.; Krockenberger, M.; Nisenson, P.; Noyes, R. W.
Bibcode: 1998ASPC..154.1876K
Altcode: 1998csss...10.1876K
  The AFOE is a fiber-fed bench-top echelle spectrometer installed
  at the Mt. Hopkins 1.5 m telescope for research in exoplanets,
  asteroseismology, and other topics requiring precise radial velocity
  measurements. Here we describe the instrumentation, observing programs,
  and data reduction techniques for exoplanet research with the AFOE. We
  also summarize recent results of our search for and characterization
  of exoplanets. Further information on the AFOE can be found on the
  Web at http://cfa-www.harvard.edu/afoe.

Title: 51 Pegasi and Tau Bootis: Planets or Pulsations?
Authors: Horner, S. D.; Brown, T. M.; Kennelly, E. J.; Kotak, R.; Jha,
   S.; Korzennik, S. G.; Krockenberger, M.; Nisenson, P.; Noyes, R. W.
Bibcode: 1998ASPC..135..206H
Altcode: 1998hcsp.conf..206H
  It has recently been suggested (Gray 1997) that the radial velocity
  variations observed in the spectra of 51 Pegasi are the result of
  stellar pulsations as opposed to the reflex motion due to an orbital
  companion. The AFOE group has confirmed the radial velocity variations
  in 51 Pegasi and t Bootis. Here we discuss the results of a search for
  evidence of pulsations in the AFOE data for these two stars, as well
  as attempt to clear up misconceptions regarding pulsations circulated
  as a result of the current debate about the nature of the 51 Pegasi
  radial velocity variations.

Title: 51 Pegasi and Tau Bootis: Planets or Pulsations?
Authors: Horner, S. D.; Brown, T. M.; Kennedy, E. J.; Kotak, R.; Jha,
   S.; Korzennik, S. G.; Krockenberger, M.; Nisenson, P.; Noyes, R. W.
Bibcode: 1998ASPC..154.1860H
Altcode: 1998csss...10.1860H
  Using data from the AFOE and simulations of pulsating stars, we are able
  to rule out pulsations as the cause of the radial velocity variations
  seen in tau Bootis and conclude that it is unlikely that pulsations
  are the cause of radial velocity variations seen in 51 Pegasi. Orbital
  companions are still the most probable causes of the radial velocity
  variations observed in these systems.

Title: Asteroseismology of Procyon with the AFOE
Authors: Horner, S. D.; Brown, T. M.; Kennelly, E. J.; Korzennik,
   S.; Nisenson, P.; Noyes, R. W.
Bibcode: 1997AAS...191.4310H
Altcode: 1997BAAS...29R1276H
  The Advanced Fiber Optic Echelle (AFOE) is a bench-mounted,
  fiber-fed echelle spectrograph designed for precision radial velocity
  observations. Located at the 1.5m Tillinghast telescope at Whipple
  Observatory, the AFOE is used to detect exoplanets and is involved in
  several projects in asteroseismology, including asteroseismology of
  Sun-like stars. Procyon has been a prime target for asteroseismology
  of Sun-like stars due to its proximity and its spectral type
  (F5 IV-V). Theory predicts that due to its low surface gravity
  and inefficient surface convection, the amplitudes of its p-mode
  pulsation modes should be relatively large, though still less than 1
  m\ s(-1) . While the velocity of individual modes is extremely small,
  observations of Procyon with the AFOE show excess power in the frequency
  range between 0.5 to 1.5 MHz. This power may be the result of p-mode
  oscillations on Procyon, and is consistent with previous results (Brown
  et al. 1991). However, mode identification is required to interpret
  the ramifications of the observations for the star's structure, which
  is the goal of asteroseismology. These single-site data are limited
  in frequency resolution, which may prevent clear identification of
  individual modes.

Title: Color--Luminosity Relations for the Resolved Hot Stellar
    Populations in the Centers of M31 and M32
Authors: Brown, T. M.; Ferguson, H. C.; Stanford, S. A.; Deharveng,
   J. -M.; Davidsen, A. F.
Bibcode: 1997AAS...191.8219B
Altcode: 1997BAAS...29R1345B
  We present Faint Object Camera ultraviolet images of Messier 31 and
  Messier 32. The hot stellar population detected in the composite
  UV spectra of these nearby galaxies is partially resolved into
  individual stars, and their individual colors and luminosities are
  measured. Although our photometry does not extend to the horizontal
  branch (HB) itself, we can detect and characterize stars that are
  in the bright phases of post-HB evolution for the entire range of
  mass on the HB. Many of our detected stars imply the existence of an
  extended HB in the cores of these galaxies. These hot stars are the
  extragalactic counterparts to the hot subdwarfs in our own Galactic
  field, and their confirmed existence in neighboring galaxies supplies
  an important validation to explanations of the ultraviolet upturn
  phenomenon found in ellipticals and spiral bulges.

Title: STIS Ultraviolet Imagery of the Globular Cluster NGC 6681
Authors: Landsman, W.; Bowers, C.; Heap, S.; Kimble, R.; Sweigart,
   A.; Brown, T. M.; Catelan, M.; Yi, S.
Bibcode: 1997AAS...191.8003L
Altcode: 1997BAAS...29.1338L
  The post--core-collapse globular cluster NGC 6681 (M70) is characterized
  by an intermediate metallicity ([Fe/H] = --1.5), a low reddening
  (E(B--V) = 0.06), and a blue horizontal branch (HB). STIS ultraviolet
  images of NGC 6681 have recently been obtained as part of the
  Servicing Mission Observatory Verification (SMOV) testing. The images
  were obtained in five ultraviolet filters (25MAMA, F25QTZ, F25SRF2,
  F25CN182, and F25CN270), and reach a typical limiting monochromatic
  magnitude of m(UV) ~ 22. Photometry of the blue HB stars in the
  far-ultraviolet ( ~ 1600 Angstroms) images is in good agreement with
  the WFPC2 Woods filter photometry of Watson et al. (1994, ApJL, 435,
  L55). The F25CN182 -- F25CN270 color-magnitude diagram shows a tight
  cluster of blue HB stars, a pronounced blue straggler sequence, and
  several white dwarf candidates.

Title: Erratum: A Planet Orbiting the Star Rho Coronae Borealis:
Authors: Noyes, Robert W.; Jha, Saurabh; Korzennik, Sylvain G.;
   Krockenberger, Martin; Nisenson, Peter; Brown, Timothy M.; Kennelly,
   Edward J.; Horner, Scott D.
Bibcode: 1997ApJ...487L.195N
Altcode:
  In the Letter, ``A Planet Orbiting the Star ρ Coronae Borealis''
  by Robert W. Noyes, Saurabh Jha, Sylvain G. Korzennik, Martin
  Krockenberger, Peter Nisenson, Timothy M. Brown, Edward J. Kennelly,
  and Scott D. Horner (ApJ, 483, L111 [1997]), a software error caused
  the sign of the reported radial velocity variations of ρ Coronae
  Borealis to be reversed. This error has no effect on the period,
  amplitude, or eccentricity of the derived orbit and thus does not
  affect the main conclusion of the paper. However, the longitude ω
  of periastron reported in Table 1 is off by 180°, and the predicted
  time of a possible planetary transit T<SUB>transit</SUB> is off by
  approximately 1/2 period. The correct values are ω = 30° +/- 74°
  and T<SUB>transit</SUB> = 2,450,657.88 +/- 0.54 HJD.

Title: A Planet Orbiting the Star ρ Coronae Borealis
Authors: Noyes, Robert W.; Jha, Saurabh; Korzennik, Sylvain G.;
   Krockenberger, Martin; Nisenson, Peter; Brown, Timothy M.; Kennelly,
   Edward J.; Horner, Scott D.
Bibcode: 1997ApJ...483L.111N
Altcode: 1997astro.ph..4248N
  We report the discovery of near-sinusoidal radial velocity variations
  of the G0V star ρ CrB, with period 39.6 days and amplitude 67 m
  s<SUP>-1</SUP>. These variations are consistent with the existence
  of an orbital companion in a circular orbit. Adopting a mass of 1.0
  M<SUB>solar</SUB> for the primary, the companion has minimum mass
  about 1.1 Jupiter masses and orbital radius about 0.23 AU. Such an
  orbital radius is too large for tidal circularization of an initially
  eccentric orbit during the lifetime of the star, and hence we suggest
  that the low eccentricity is primordial, as would be expected for a
  planet formed in a dissipative circumstellar disk.

Title: Hot Evolved Stars in the Centers of M31 and M32
Authors: Brown, T. M.; Ferguson, H. C.; Standford, S. A.; Deharveng,
   J. -M.; Davidsen, A. F.
Bibcode: 1997AAS...190.0303B
Altcode: 1997BAAS...29Q.781B
  We present UV images of M31 and M32, as observed by HST with the
  refurbished FOC. The galaxies were observed through the F175W and F275W
  filters, allowing the construction of color magnitude diagrams (CMDs)
  for the hundreds of detected sources found in each image. Comparison of
  these data with the stellar evolutionary tracks of horizontal branch
  stars and their progeny shows that for the first time outside of our
  own Galaxy, we are measuring the colors of individual stars that are
  evolving along post asymptotic giant branch (PAGB), post-early AGB,
  and AGB-Manque' paths. Searching to the 6-sigma detection limit,
  we find 986 sources in M31 and 183 sources in M32. We compare the
  distribution of stars in the CMDs with the expectations from theory.

Title: A Radial Velocity Search for p-Mode Pulsations in η Bootis
Authors: Brown, Timothy M.; Kennelly, Edward J.; Korzennik, Sylvain
   G.; Nisenson, Peter; Noyes, Robert W.; Horner, Scott D.
Bibcode: 1997ApJ...475..322B
Altcode:
  The subgiant η Boo (G5 IV) has been reported to show p-mode pulsations,
  as evidenced by variations in the equivalent width of its hydrogen
  Balmer lines (reported by Kjeldsen et al.). In an attempt to confirm
  this report, we observed η Boo's radial velocity with the AFOE
  spectrograph for a total of 22 hours spread over seven successive
  nights in 1995 March. We find no evidence for the presence of excess
  power at the frequencies reported by Kjeldsen et al.; our upper limit
  corresponds to typical mode amplitudes of 0.5 m s<SUP>-1</SUP>, about 3
  times smaller than the velocity amplitudes they inferred. Signals with
  amplitudes larger than 0.5 m s<SUP>-1</SUP> may be present at other
  frequencies within the 0-1000 μHz range, but evidence for such signals
  is scanty, and typical mode amplitudes greater than 1.5 m s<SUP>-1</SUP>
  are clearly inconsistent with our observations.

Title: A Far Ultraviolet Analysis of the Stellar Populations in
    Elliptical and S0 Galaxies
Authors: Brown, T. M.
Bibcode: 1996AAS...189.6204B
Altcode: 1996BAAS...28.1351B
  We have analyzed the far-ultraviolet (FUV) spectra of six elliptical and
  S0 galaxies in order to characterize their hot stellar populations. The
  spectra were obtained using the Hopkins Ultraviolet Telescope (HUT)
  in March 1995. These data, together with the spectra of two galaxies
  observed with HUT in 1990, represent the only FUV spectra of early type
  galaxies that extend to the Lyman limit at 912 Angstroms and therefore
  include the ``turnover'' in the spectral energy distribution below
  Lyman alpha. Using an extensive new grid of synthetic spectra which
  match the HUT resolution and cover the relevant parameter space of
  temperature and gravity, we have constructed synthetic spectral energy
  distributions by integrating over predicted stellar evolutionary tracks
  for horizontal branch stars and their progeny. When the models are
  compared with the HUT data, we find that those with supersolar metal
  abundances and helium best reproduce the flux across the entire HUT
  wavelength range, while those with subsolar Z &amp; Y fit less well,
  partly because of a significant flux deficit shortward of 970 Angstroms
  in the models. We find that AGB-Manquacutee evolution is required in
  all fits to the HUT spectra, suggesting that all of the galaxies have
  some subdwarf B star population. At any Z &amp; Y, the models that
  best match the HUT flux are dominated by stars evolving from a narrow
  range of envelope mass on the blue end of the horizontal branch. We
  find that most absorption features in the spectra are consistent with
  Z = 0.1 Z_⊙, significantly lower than the abundances implied by the
  best-fitting spectral energy distributions. However, given the strong
  observational and theoretical evidence for diffusion processes in the
  atmospheres of evolved stars, the observed atmospheric abundances may
  not reflect the interior abundances in the population producing the
  ultraviolet flux in elliptical galaxies.

Title: Asteroseismological calibration of open clusters
Authors: Audard, N.; Brown, T. M.; Christensen-Dalsgaard, J.; Frandsen,
   S.; Kjeldsen, H.
Bibcode: 1996BASI...24..305A
Altcode:
  No abstract at ADS

Title: A radial velocity search for p-modes in Procyon.
Authors: Brown, T. M.; Kennelly, E. J.; Noyes, R. W.; Korzennik,
   S. G.; Nisenson, P.; Horner, S. D.; Catala, C.
Bibcode: 1996BAAS...28..917B
Altcode:
  No abstract at ADS

Title: The oscillation modes of ɛ Cep and τ Peg.
Authors: Horner, S. D.; Kennelly, E. J.; Brown, T. M.; Noyes, R. W.;
   Korzennik, S. G.; Nisenson, P.; Yang, S.; Walker, A. R.
Bibcode: 1996BAAS...28..916H
Altcode:
  No abstract at ADS

Title: A Grid of Model Atmospheres and Synthetic Spectra for the
    Far Ultraviolet Analysis of Old Stellar Populations
Authors: Brown, T. M.; Davidsen, A. F.; Ferguson, H. C.
Bibcode: 1996AAS...188.1106B
Altcode: 1996BAAS...28..840B
  We present a grid of stellar synthetic spectra suitable for detailed
  comparison to far-ultraviolet (FUV) observations obtained with the
  Hopkins Ultraviolet Telescope, IUE, and HST. Our specific application
  is to study the hot stellar populations in elliptical galaxies, but we
  anticipate that the models will be useful for other purposes. The 1,497
  spectra span a range of 10,000 K &lt;= T<SUB>eff</SUB> &lt;= 250,000 K
  and 2 &lt;= log g &lt;= 8.5, with three metallicities: Z = Z_⊙, Z =
  0.1 Z_⊙, and Z = 0.01 Z_⊙. A variety of simplifying assumptions
  have been made to reduce computer time and improve convergence, at
  the inevitable expense of some accuracy. Nevertheless, models in the
  grid reproduce the overall continuum shape and most of the absorption
  features seen in HUT spectra of four evolved stars at temperatures
  of 17000, 29900, 36100, and 55000 K. The most serious discrepancy is
  in the cores of the Lyman series lines, where the observed lines are
  not as deep as those obtained from the models. Until this problem is
  resolved, the Lyman series lines will not provide a reliable measure of
  T<SUB>eff</SUB> or log g. While the synthetic spectra in this grid may
  not be appropriate for detailed analysis of high S/N stellar spectra,
  they are sufficiently similar to the observed stars to provide a
  considerable advantage over existing models for the analysis of the FUV
  spectra of composite systems, such as elliptical galaxies and globular
  clusters, where the advantages of having a large, well-sampled grid
  of models tend to outweigh the known inadequacies of the individual
  grid points.

Title: The Oscillation Modes of epsilon CEP and tau Peg
Authors: Horner, S. D.; Kennelly, E. J.; Brown, T. M.; Noyes, R. W.;
   Korzennik, S. G.; Nisenson, P.; Yang, S.; Walker, A.
Bibcode: 1996AAS...188.5901H
Altcode: 1996BAAS...28Q.917H
  Asteroseismology of delta Scuti stars offers an attractive prospect for
  determining the interior properties of main sequence and slightly more
  evolved A- and F-type stars. Here we present detailed identifications
  of oscillation modes in the rapidly rotating delta Scuti stars epsilon
  Cep and tau Peg based on extensive observations carried out at two
  North American sites. Using cross-correlation and Fourier techniques
  we analyze the line-profile variations and the variations in the
  line-profile moments. A solution to the mode spectrum is sought using
  a genetic-based search algorithm and a line profile simulation model
  to reproduce the observed variations.

Title: The Solar Acoustic Spectrum and Eigenmode Parameters
Authors: Hill, F.; Stark, P. B.; Stebbins, R. T.; Anderson, E. R.;
   Antia, H. M.; Brown, T. M.; Duvall, T. L., Jr.; Haber, D. A.;
   Harvey, J. W.; Hathaway, D. H.; Howe, R.; Hubbard, R. P.; Jones,
   H. P.; Kennedy, J. R.; Korzennik, S. G.; Kosovichev, A. G.; Leibacher,
   J. W.; Libbrecht, K. G.; Pintar, J. A.; Rhodes, E. J., Jr.; Schou, J.;
   Thompson, M. J.; Tomczyk, S.; Toner, C. G.; Toussaint, R.; Williams,
   W. E.
Bibcode: 1996Sci...272.1292H
Altcode:
  The Global Oscillation Network Group (GONG) project estimates
  the frequencies, amplitudes, and linewidths of more than 250,000
  acoustic resonances of the sun from data sets lasting 36 days. The
  frequency resolution of a single data set is 0.321 microhertz. For
  frequencies averaged over the azimuthal order m, the median formal
  error is 0.044 microhertz, and the associated median fractional error
  is 1.6 x 10<SUP>-5</SUP>. For a 3-year data set, the fractional error
  is expected to be 3 x 10<SUP>-6</SUP>. The GONG m-averaged frequency
  measurements differ from other helioseismic data sets by 0.03 to 0.08
  microhertz. The differences arise from a combination of systematic
  errors, random errors, and possible changes in solar structure.

Title: A Radial Velocity Search for p-modes in Procyon
Authors: Brown, T. M.; Kennelly, E. J.; Noyes, R. W.; Korzennik,
   S. G.; Nisenson, P.; Horner, S. D.; Catala, C.
Bibcode: 1996AAS...188.5902B
Altcode: 1996BAAS...28R.917B
  Procyon (alpha CMi F5 IV) has long been a promising candidate for
  detection of solar-like p-modes. Although several authors have reported
  evidence for low-amplitude (&lt;= 10) m/s pulsations in this star,
  none of the existing observations are conclusive. A clear detection
  of such pulsations would be a significant step for asteroseismology
  of Sun-like stars, allowing refined estimates of the star's properties
  and paving the way for the study of fainter stars of similar spectral
  type. Identification of oscillation modes in subgiants like Procyon is
  expected to be difficult, however, because both the amplitudes and the
  frequency separations of the modes are expected to be small. To address
  these difficulties, we organized a joint observing campaign involving
  the AFOE spectrograph located at the Whipple Observatory (Mt. Hopkins,
  AZ) and the MUSICOS spectrograph located at Pic du Midi. Both
  instruments are capable of providing Doppler measurements with the
  required precision of a few m/s, and the 7 hour longitude separation
  between them allows the acquisition of relatively long uninterrupted
  data strings. In the event, bad weather prevented more than sporadic
  observations from Pic du Midi. At Mt. Hopkins, however, we obtained
  good observations on each of 6 consecutive nights 3-8 Feb 1996, for
  a total of 47 h of observing time. We discuss here the interpretation
  of this data set in terms of possible p-mode oscillations.

Title: Techniques for observing solar oscillations.
Authors: Brown, T. M.
Bibcode: 1996stsu.conf....1B
Altcode:
  The following topics were dealt with: analysis tools and the solar
  noise background; instrumentation for measuring solar p-modes; analysis
  tools for helioseismology; local analysis methods.

Title: Far-UV Line Strengths in Elliptical Galaxies
Authors: Ferguson, H. C.; Brown, T. M.; Davidsen, A. F.
Bibcode: 1996ASPC...98..486F
Altcode: 1996fstg.conf..486F; 1996astro.ph..4008F
  Much of the far-UV emission from elliptical galaxies is thought to
  arise from extreme horizontal branch stars and related objects. Only
  about 10% of the stellar population needs to evolve through this phase
  even in galaxies with the strongest UV upturn. However it is not yet
  clear if this population represents the extreme low-metallicity or
  high-metallicty tail of the distribution, or rather arises from the
  overall population through some metallicity-insensitive mechanism
  that causes increased mass loss in a small fraction of RGB stars. We
  investigate the utility of far-UV line strengths for deciding between
  these possiblities. Complications include the fact that the line
  strengths reflect both the temperature distribution and the metallicity
  distribution of the stars, that there may be abundance anomalies
  introduced on the RGB, and that metals are likely to be redistributed
  by gravitational settling and radiative diffusion in the atmospheres
  of hot high-gravity stars. Line-strength measurements from Astro-2
  HUT spectra are considered in this context.

Title: A Radial Velocity Search for p-mode Pulsations in eta Bootis
Authors: Noyes, R. W.; Korzennik, S. G.; Nisenson, P.; Brown, T. M.;
   Kennelly, E. J.; Horner, S. D.
Bibcode: 1995AAS...18710211N
Altcode: 1995BAAS...27.1429N
  Kjeldsen et al. 1994 (Astron. J 109, 1313 ) have reported the presence
  of p-mode pulsations in Balmer line equivalent widths measured in
  the spectrum of eta Boo (G5 IV); they give accurate frequencies for
  13 modes of oscillation, and estimate velocity amplitudes for these
  modes of typically 1.6 m/s. We report here time-series observations of
  the radial velocity of eta Boo obtained with the Advanced Fiber Optic
  Echelle (AFOE) spectrograph. In March 1995 we obtained 555 spectra
  of eta Boo for a total of 21.6 hours of observing time spread over
  7 consecutive nights. The radial velocity time series clearly shows
  the night-to-night orbital motion of eta Boo; the residual velocities
  after removing this motion are typically 10 m/s for single spectra,
  a value that is roughly consistent with shot noise limits. The power
  spectrum of the time series shows no evidence for Kjeldsen et al.'s
  frequencies. With 95 % confidence, we can rule out the presence of these
  13 frequencies with typical amplitudes of 0.5 m/s or more. The spectrum
  is consistent with pure photon noise, but also with the presence of
  pulsations having other frequencies (not those given by Kjeldsen et
  al.) and with typical amplitudes as large as about 1.5 m/s. Possible
  explanations for the discrepancy between the two results are (a) an
  incorrect conversion between the amplitudes of equivalent width and
  Doppler pulsations, and (b) a fluke in the noise behavior of one or
  both observations.

Title: Determining the AFOE's Radial Velocity Precision with Solar
    Observations
Authors: Horner, S. D.; Brown, T. M.; Kennelly, E. J.; Noyes, R. W.;
   Korzennik, S. G.; Nisenson, P.; Krockenberger, M.
Bibcode: 1995AAS...187.7006H
Altcode: 1995BAAS...27.1380H
  The Advanced Fiber Optic Echelle (AFOE) is an instrument designed
  for high precision radial velocity observations to detect extra-solar
  planets and study stellar structure through asteroseismology. A 320 mu
  m optical fiber is used to obtain solar observations during the day to
  determine the precision of the instrument, and to study the relationship
  between stellar activity and measured radial velocities. Here we
  present the results of our analysis of solar data to determine the
  short and long term radial velocity precision of the AFOE.

Title: Precise Photometry Mission -- Measuring Stellar
    Microvariability from Space
Authors: Brown, T. M.; Borucki, W.; Frandsen, S.; Gilliland, R. L.;
   Jones, A.; Noyes, R. W.; Tarbell, T.; Title, A.; Ulrich, R. K.
Bibcode: 1995AAS...187.7111B
Altcode: 1995BAAS...27R1385B
  Atmospheric scintillation limits the precision attainable by
  ground-based photometry; this limitation is a major obstacle to
  progress in several fields, notably asteroseismology of Sun-like
  stars. A space-borne photometric telescope could operate near the shot
  noise limit, removing this obstacle and providing new opportunities
  for inquiry. As part of the program for New Mission Concepts in
  Astrophysics, we are studying the scientific rewards and technological
  challenges associated with a Precise Photometry Mission (PPM). The
  baseline performance goal for the PPM is to measure solar-like
  pulsations (amplitude 3 mu mag) in G stars in the Hyades with a S/N
  ratio of 4 in 10 days of observing time. This performance would also
  allow detection of transits of Earth-sized planets of main-sequence
  stars, extremely precise characterization of the light curves of
  micro-lensing events, and other novel applications. The technical
  approach envisioned for the PPM is wide-band CCD photometry. The study
  that is underway focuses on two aspects of the required technology: (1)
  Are CCD detectors able to provide the necessary very high S/N within
  the spacecraft operating environment? (2) Can new lightweight mirror
  and telescope structure technology be applied to yield significant
  reductions in mission cost? We are addressing both questions with
  laboratory tests, including time-series performance tests of suitable
  CCDs, and thermal and mechanical tests of a SiC telescope mirror. In
  addition to describing PPM's scientific aims and technical rationale,
  we report preliminary results of the CCD tests.

Title: Hopkins Ultraviolet Telescope Observations of Six E and
    S0 Galaxies
Authors: Brown, T. M.; Ferguson, H. C.; Davidsen, A. F.
Bibcode: 1995AAS...186.2004B
Altcode: 1995BAAS...27..834B
  In order to better understand the hot stellar populations of E and
  S0 galaxies, we observed six objects using the Hopkins Ultraviolet
  Telescope. Through our 11'' times 60'' aperture, we obtained one
  observation each of M 49 (1346 s), M 87 (950 s), M 89 (1682 s), and
  NGC 3115 (1634 s), two observations of NGC 3379 (3074 s), and four
  observations of M 60 (5824 s). The far-ultraviolet (FUV) spectra
  were obtained during orbital night as part of the Astro-2 mission
  on the space shuttle Endeavor in March 1995, and cover the spectral
  range of 912 Angstroms to 1850 Angstroms with a resolution of 2--4
  Angstroms. This sample quadruples the number of early-type galaxies
  studied to the Lyman limit. After correcting for geocoronal emission
  and interstellar extinction in our own Galaxy, all the spectra are
  similar, even though the ``UV upturn'' strength, as characterized by
  the parameter m<SUB>1550</SUB>-V, varies over the range of 2.04 mag to
  3.86 mag for these galaxies. Comparison with models of evolved stellar
  populations confirms the conclusion from Astro-1 data that the FUV
  flux can be explained by stars with a narrow range of temperature and
  envelope mass on the extreme horizontal branch (EHB). This work was
  supported by NASA contract NAS 5-27000 to the Johns Hopkins University.

Title: Asteroseismology
Authors: Brown, T. M.
Bibcode: 1995ESASP.376a.177B
Altcode: 1995heli.conf..177B; 1995soho....1..177B
  Asteroseismology is already being successfully practiced on white
  dwarfs. To make progress applying it to stars that are more like the
  Sun, advances are needed in both observation and theory. Observations of
  the subgiant η Boo may point the way to a new low-noise spectroscopic
  technique for studying the very small-amplitude pulsations in stars
  with surface temperatures similar to that of the Sun. In the longer
  term, photometric observations from spacecraft probably hold the most
  promise for studying such stars. Several such missions are now being
  studied or actively pursued.

Title: The AFOE: A Spectrograph for Precision Doppler Studies
Authors: Brown, Timothy M.; Noyes, Robert W.; Nisenson, Peter;
   Korzennik, Sylvain G.; Horner, Scott
Bibcode: 1994PASP..106.1285B
Altcode:
  The Advanced Fiber Optic Echelle (AFOE) is a fiber-fed echelle
  spectrograph designed for the measurement of stellar Doppler
  shifts. Using a 2k x 2k CCD detector, it samples about 55% of the
  wavelength range between 450 nm and 700 nm (20 echelle orders) at a
  single shot, with spectral resolution R = 32000 to 70000 at 500 nm,
  depending on the slit width employed. The AFOE employs a number of
  devices to assure that the calibrations necessary for accurate Doppler
  measurements can be properly performed. The most important of these
  are: (1) coupling to the telescope via a double-scrambling optical
  fiber system; (2) continuous calibration of the wavelength scale and
  point-spread function by means of an atomic emission lamp entering the
  spectrograph via a separate fiber and/or a molecular iodine absorption
  cell; (3) availability of fiber-coupled sunlight for regular calibration
  against the solar spectrum; (4) appropriate mechanical design and active
  thermal control, yielding good mechanical stability. The AFOE is coupled
  to the Tillinghast 1.5-m telescope at the F. L. Whipple Observatory. It
  presently achieves S/N = 500 in the continuum near 500 nm in 60s when
  observing Arcturus (alpha-Boo, m_V = -0.04). This noise level sets
  a limit of about 0.7 ms^-1 to the Doppler precision attainable in
  this length of observing time. Currently, our actual frame-to-frame
  repeatability is worse than the photon noise limited value by about a
  factor of 3 for this bright star, and about 1.5 for stars with m_V =
  4. Work is continuing to refine data processing methods so that the
  ultimate noise limit may be approached more closely, and to improve
  the spectrograph's relatively low efficiency. (SECTION: Astronomical
  Instrumentation )

Title: Generation of artificial helioseismic time-series.
Authors: Schou, J.; Brown, T. M.
Bibcode: 1994A&AS..107..541S
Altcode:
  We present an outline of an algorithm to generate artificial
  helioseismic time-series, taking into account as much as possible of
  the knowledge we have on solar oscillations. The hope is that it will
  be possible to find the causes of some of the systematic errors in
  analysis algorithms by testing them with such artificial time-series.

Title: On the Rotation Rate in the Solar Convection Zone
Authors: Schou, Jesper; Brown, Timothy M.
Bibcode: 1994ApJ...434..378S
Altcode:
  Recently Gough et al. (1993) have argued that the rotation rate in parts
  of the solar convection zone may be constant on cylinders as predicted
  by models of the convection zone, contrary to the inferences generally
  made from helioseismology. Here we consider models similar to those
  suggested by Gough et al. and show that they are either inconsistent
  with observations made by Fourier Tachometer or require unphysical
  rotation rates in other parts of the Sun. These observations use a more
  detailed model of the effects of the solar rotation on the observed
  frequencies than that used in reducing previous observations. We
  also show the results of an inversion of the Fourier Tachometer
  observations and compare it with an inversion of data similar to that
  used previously. The result of this inversion generally confirms the
  conclusions from previous inversions.

Title: Asteroseismology: Theory and phenomenology
Authors: Brown, Timothy M.
Bibcode: 1994spmt.nasa...17B
Altcode:
  Seismic studies of the Sun have succeeded in mapping the variation of
  sound speed with depth in the Sun, and variation of angular velocity
  with both depth and latitude. Many stars besides the Sun may also be
  amenable to asteroseismic analysis. Stars of roughly solar type should
  of course behave in ways similar to the sun, and stars of this sort form
  a large fraction of the potential targets for asteroseismology. But
  several other types of stars (delta scuti stars, roAP stars,
  and the pulsating white dwarfs) also have the desired pulsation
  characteristics. Pulsations in some of these stars are, for various
  reasons, much easier to observe than in the Sun-like stars. Virtually
  all unambiguous observations of multi-mode pulsators relate to these
  other categories of stars. Since oscillation mode frequencies are
  arguably the most precise measurement relating to a star that we can
  make, a few tens of such frequencies may still be of great importance
  to our understanding of the stellar structure and evolution.

Title: The Effectiveness of Oscillation Frequencies in Constraining
    Stellar Model Parameters
Authors: Brown, Timothy M.; Christensen-Dalsgaard, J.; Weibel-Mihalas,
   Barbara; Gilliland, Ronald L.
Bibcode: 1994ApJ...427.1013B
Altcode:
  Recent observational advances suggest that it may soon be possible to
  measure the frequencies of p-mode oscillations on distant Sun-like
  stars. We investigate the potential utility of such oscillation
  frequencies in determining the fundamental stellar structure parameters
  of these stars, in the case in which frequencies may be measured
  for both members of a visual binary system. To utilize all of the
  observations presumed to be available in an optimal way, we develop a
  formalism based on singular value decomposition (SVD) to relate errors
  in observed quantities to those in model parameters. As a particularly
  interesting example, we consider the alpha Cen system as it would
  be seen from distances between 1.3 pc (its true distance) and 100
  pc. We find that for the nearest case, adding oscillation frequency
  separations with plausible errors to the available astrometric,
  photometric, and spectroscopic data allows one to reduce the formal
  errors in estimates of the helium abundance, heavy-element abundance,
  and mixing length by roughly a factor of 2. Estimates of the stellar
  masses and the system's age and distance are not markedly improved,
  mostly because of the very high quality astrometric data that can
  be obtained on such a nearby object. If the system were located at a
  signifcantly larger distance, the addition of oscillation information
  would allow drastic reductions in the formal error applicable to all
  of the stellar parameters except the helium abundance. These results
  suggest that accurately measured oscillation frequencies for visual
  binaries might allow tests of stellar structure theory at a level of
  precision that has hitherto been obtainable only for a few eclipsing
  binaries. Reducing the observational errors in photometry or astrometry
  by a factor of 3 does not provide the same level of improvement,
  especially for relatively distant systems. We show that the extra
  information contained in the oscillation frequencies for a reasonable
  set of modes would easily allow one to distinguish between models using
  opacity laws obtained from the Los Alamos Opacity Library and from
  the more recent Livermore OPAL tables. Different formulations of the
  equation of state (without and with Coulomb effects) lead to models
  that are marginally distinguishable, while models with and without
  helium settling from the convection zone are not distinguishable,
  given observations with errors as large as we assume.

Title: Asteroseismology
Authors: Brown, Timothy M.; Gilliland, Ronald L.
Bibcode: 1994ARA&A..32...37B
Altcode:
  No abstract at ADS

Title: A Search for Solar-Like Oscillations in the Stars of M67 With
    CCD Ensemble Photometry on a Network of 4m Telescopes
Authors: Gilliland, R. L.; Brown, T. M.; Kjeldsen, H.; McCarthy,
   J. K.; Peri, M. L.; Belmonte, J. A.; Vidal, I.; Cram, L. E.; Palmer,
   J.; Frandsen, S.; Parthasarathy, M.; Petro, L.; Schneider, H.; Stetson,
   P. B.; Weiss, W. W.
Bibcode: 1993AJ....106.2441G
Altcode:
  Results are presented from a large observational project directed
  toward the detection of solar-like oscillations in an ensemble of
  open cluster stars. Seven groups collaborated in 1992 January to
  observe twelve stars in M67 with 4 m class telescopes for a one week
  period. High quality time series were collected on 22 telescope nights
  for a total of 156 h. The technique of CCD ensemble photometry allowed
  precisions of about 250 micro-mag per minute to be reached in the best
  cases, and provided robust results in conditions that sometimes were
  far from 'photometric.' The longitude-distributed network, coupled
  with generally low noise levels, provided a good window function and
  yielded detection thresholds of about 20 micro-mag (five times solar)
  for solar-like oscillations in the best ensembled stars. Sensitivity
  to solar-like oscillations over our twelve ensemble stars ranges
  from 30% to a factor of three better than obtained previously by any
  group. When our simulations results for 12 stars is taken into account
  this project provides a (multiplexed) factor of 20 to 30 gain over
  previous experiments. For two stars we derive interesting upper limits
  for oscillation amplitudes that are near the lower range predicted by
  theory. Over half the stars in the ensemble show suggestive evidence for
  oscillations; we develop the evidence for, and the cautions against,
  claiming detections in these cases. We argue that a more aggressive
  network campaign could provide a factor of two sensitivity gain with
  a resulting high probability of attaining unambiguous oscillation
  detections on most of the stars in the M67 ensemble.

Title: Generation of artificial helioseismic time-series
Authors: Schou, J.; Brown, T. M.
Bibcode: 1993STIN...9415968S
Altcode:
  We present an outline of an algorithm to generate artificial
  helioseismic time-series, taking into account as much as possible of
  the knowledge we have on solar oscillations. The hope is that it will
  be possible to find the causes of some of the systematic errors in
  analysis algorithms by testing them with such artificial time-series.

Title: Observations of Intermediate Degree Solar Oscillations:
    1989 April--June
Authors: Bachmann, Kurt T.; Schou, Jesper; Brown, Timothy M.
Bibcode: 1993ApJ...412..870B
Altcode:
  Frequencies, splittings, and line widths from 85 d of full disk
  Doppler observations of solar p-modes taken between April 4 and June
  30, 1989 are presented. Comparison of the present mode parameters
  with published Big Bear Solar Observatory (BBSO) results yields good
  agreement in general and is thus a confirmation of their work using an
  independent instrument and set of analysis routines. Average differences
  in p-mode frequencies measured by the two experiments in spring-summer
  1989 are explained as a result of differences in the exact periods of
  data collection during a time of rapidly changing solar activity. It
  is shown that the present a(1) splitting coefficients for p-modes
  with nu/L less than 45 micro-Hz suffer from a significant systematic
  error. Evidence is presented to the effect that a detector distortion
  or alignment problem, not a problem with the power spectra analysis,
  is the most likely explanation of this a(1) anomaly.

Title: P-Mode Frequency Variation in Relation to Global Solar Activity
Authors: Bachmann, Kurt T.; Brown, Timothy M.
Bibcode: 1993ApJ...411L..45B
Altcode:
  We show that p-mode frequency variations correlate remarkably well with
  the variations of six solar activity indices over a 6 yr period from
  1984 October to 1990 November, including both the large variation from
  solar minimum to solar maximum and smaller variations observed over
  approximately 1 month intervals during solar maximum. The quality of
  correlation as seen visually and as measured by two statistical tests
  differs significantly among the six activity indices, and we briefly
  speculate on possible reasons for this. Observations used in this
  study come from the HAO/NSO Fourier tachometer (FTACH) and include
  the spherical harmonic degree range l greater than 20 and equal to 60
  or less and frequency range between 2600 and 3200 micro-Hz. The data
  are divided into 18 separate epochs with time string duration ranging
  from a minimum of 18 days to a maximum of 45 days. We have particularly
  good coverage during the early part of solar maximum of cycle 22.

Title: The Absorption of p-Modes by Sunspots: Variations with Degree
    and Order
Authors: Bogdan, Thomas J.; Brown, Timothy M.; Lites, Bruce W.;
   Thomas, John H.
Bibcode: 1993ApJ...406..723B
Altcode:
  A spherical harmonic decomposition of the p-modes into inward and
  outward propagating waves is employed to investigate the absorption
  of solar p-modes by an isolated sunspot. The absorption coefficient
  (averaged over frequency and azimuthal order) is found to increase
  with increasing horizontal wavenumber k over the range 0-0.8/Mm. For
  larger horizontal wavenumbers, in the range 0.8-1.5/Mm, the absorption
  coefficient decreases with increasing k. The absorption along each
  individual p-mode ridge tends to peak at an intermediate value of the
  spherical harmonic degree in the range 200-400. The highest absorption
  is found along the p(1) ridge, and the absorption decreases with
  increasing radial order.

Title: A search for solar-like oscillations in the stars of M67
Authors: Gilliland, R. L.; Brown, T. M.; Kjeldsen, H.; Belmonte,
   J. A.; Cram, L. E.; Frandsen, S.; McCarthy, J. K.; Parthasarathy,
   M.; Peri, M. L.; Petro, L.; Schneider, H.; Stetson, P. B.; Vidal,
   I.; Weiss, W. W.
Bibcode: 1993prph.conf..145G
Altcode:
  No abstract at ADS

Title: The Search for Pulsations in Late-Type Giants - Preliminary
    Results
Authors: Horner, S. D.; Brown, T. M.
Bibcode: 1993ASPC...42..391H
Altcode: 1993gong.conf..391H
  No abstract at ADS

Title: Ring Diagram Analysis of MT.WILSON Data
Authors: Patron, J.; Hill, F.; Rhodes, E. J., Jr.; Korzennik, S. G.;
   Cacciani, A.; Brown, T. M.
Bibcode: 1993ASPC...42..437P
Altcode: 1993gong.conf..437P
  No abstract at ADS

Title: How may seismological measurements constrain parameters of
    stellar structure?
Authors: Brown, T. M.; Christensen-Dalsgaard, J.; Mihalas, B. W.
Bibcode: 1993ASPC...40..554B
Altcode: 1993IAUCo.137..554B; 1993ist..proc..554B
  No abstract at ADS

Title: Observations of Intermediate Degree Solar Oscillations -
    1989APR-JUN
Authors: Bachmann, K. T.; Schou, J.; Brown, T. M.
Bibcode: 1993ASPC...42..197B
Altcode: 1993gong.conf..197B
  No abstract at ADS

Title: GONG 1992 : seismic investigation of the sun and stars :
    proceedings of a conference held in Boulder, Colorado, August
    11-14, 1993
Authors: Brown, Timothy M.
Bibcode: 1993ASPC...42.....B
Altcode: 1993gong.conf.....B; 1993QB539.O83G66...
  Various papers on the seismic investigation of the sun and stars are
  presented. Individual topics addressed include: excitation of solar
  p-modes, cause of cycle-related global solar changes, ionization effects
  on solar granulation dynamics, turbulent compressible convection with
  rotation, convective overshooting in stars, local helioseismology of
  subsurface structure, observations of high-frequency solar oscillations,
  high-frequency P-mode spectrum, high-frequency solar velocity noise,
  isothermal waves in solar atmosphere, detection of convective overshoot,
  2D helioseismic inversions, seismic limits on the sun's internal
  toroidal field, faster formulations of the OLA method, torsional
  oscillations and internal rotation. Also discussed are: solar g-mode
  signatures in p-mode signals, theory of Delta Scuti stars, the Whole
  Earth Telescope, phase function for solar-like stars, asteroseismic
  HR diagram, seismic analysis of stellar P-mode spectra, asteroseismic
  calibration of stellar clusters, observations of Delta Scuti stars from
  Arhus, seismology of Procyon, seismological modeling of PG1159-035, GONG
  Project update, ring diagram analysis of Mt. Wilson data, gap filling
  the GONG data set, helioseismic prospects in the MIR, multicolor CCD
  photometer, new echelle spectrograph for asteroseismology.

Title: Preliminary results from observations with the Fourier
    tachometer.
Authors: Schou, J.; Brown, T. M.; Bachman, K. T.
Bibcode: 1993ASPC...40...90S
Altcode: 1993IAUCo.137...90S; 1993ist..proc...90S
  The authors present preliminary results from an analysis of two ≍3
  month observation runs with the Fourier Tachometer (which was operated
  by HAO and NSO) from 1987 and 1989. The analysis was done with two
  different methods in order to test for systematic errors. It is shown
  that the mode frequencies change in a manner similar to that reported
  by Libbrecht and Woodard. The authors also present results for the
  frequency splittings caused by the solar rotation.

Title: An Advanced Fiber Optic Echelle Spectrograph for
    Asteroseismology
Authors: Noyes, R. W.; Brown, T. M.; Horner, S.; Korzennik, S.;
   Nisenson, P.
Bibcode: 1993ASPC...42..485N
Altcode: 1993gong.conf..485N
  No abstract at ADS

Title: The AFOE - a new instrument for asteroseismology
Authors: Noyes, R. W.; Brown, T. M.; Horner, S.; Korzennik, S.;
   Nisenson, P.
Bibcode: 1993ASPC...40..752N
Altcode: 1993IAUCo.137..752N; 1993ist..proc..752N
  No abstract at ADS

Title: Data analysis techniques for determining high precision
    doppler shifts using Iodine absorption cells
Authors: Horner, S. D.; Brown, T. M.
Bibcode: 1993ASPC...40..764H
Altcode: 1993ist..proc..764H; 1993IAUCo.137..764H
  No abstract at ADS

Title: Key issues - A round table discussion
Authors: Brown, T. M.; Demarque, P.; Noyes, R.; Praderie, F.; Roxburgh,
   I. W.; Schatzman, E.
Bibcode: 1993ASPC...40..776B
Altcode: 1993ist..proc..776B; 1993IAUCo.137..776B
  An overview of a round table discussion on the internal dynamics of
  stars, some problems in stellar structure and evolution, a study of
  stellar activity mechanisms using PRISMA, the seismology of sunlike
  stars, and directions of future research is presented. It is concluded
  that models that take into account just one physical process generally
  do not agree with the observations. This provides evidence for the
  presence of other physical processes. In each phenomenon which is
  considered, a variety of physical processes are involved. All physical
  processes should be taken into account simultaneously. Stars need to
  be considered globally. It is recommended that attention be given to
  such unsolved problems as the helium content of the sun, the abundance
  of lithium in fast rotating stars, and the origin and evolution of
  stellar magnetic fields.

Title: Tests of a Simple GONG P-Mode Merging Algorithm
Authors: Williams, W.; Hill, F.; Toner, C.; Brown, T. M.
Bibcode: 1993ASPC...42..441W
Altcode: 1993gong.conf..441W
  No abstract at ADS

Title: Localized Sources of Propagating Acoustic Waves in the Solar
    Photosphere
Authors: Brown, Timothy M.; Bogdan, Thomas J.; Lites, Bruce W.;
   Thomas, John H.
Bibcode: 1992ApJ...394L..65B
Altcode:
  A time series of Doppler measurements of the solar photosphere with
  moderate spatial resolution is described which covers a portion of the
  solar disk surrounding a small sunspot group. At temporal frequencies
  above 5.5 mHz, the Doppler field probes the spatial and temporal
  distribution of regions that emit acoustic energy. In the frequency
  range between 5.5 and 7.5 mHz, inclusive, a small fraction of the
  surface area emits a disproportionate amount of acoustic energy. The
  regions with excess emission are characterized by a patchy structure
  at spatial scales of a few arcseconds and by association (but not
  exact co-location) with regions having substantial magnetic field
  strength. These observations bear on the conjecture that most of the
  acoustic energy driving solar p-modes is created in localized regions
  occupying a small fraction of the solar surface area.

Title: Limits to CCD Ensemble Photometry Precision, and Prospects
    for Asteroseismology
Authors: Gilliland, Ronald L.; Brown, Timothy M.
Bibcode: 1992PASP..104..582G
Altcode:
  We report results of CCD ensemble, time-resolved photometry with
  the KPNO 2.1-m telescope yielding precision of 400 umag per minute
  of integration. Previous experience on 1-m class telescopes and
  well-known scaling laws for the limiting noise sources indicate
  that current 4-m class telescopes and existing detectors, operated
  as a network for about five days, would allow detection of coherent
  (solar-like) oscillations at an amplitude of 15 umag. We provide
  detailed stellar-evolution modeling and eigenfrequency-analysis results
  for the stars of the old open cluster M67. Using observed amplitudes
  of solar p-mode oscillations, and published scaling laws with spectral
  type, we show that direct detection of solar-analog oscillations on
  13th-magnitude M67 stars is possible with a several-night 4-m network
  campaign. Asteroseismology on a substantial ensemble of cluster stars
  promises to allow fundamental new tests of stellar structure and
  evolution theory. (SECTION: Instrumentation and Data Analysis)

Title: The Oscillating Blue Stragglers in the Open Cluster M67
Authors: Gilliland, Ronald L.; Brown, Timothy M.
Bibcode: 1992AJ....103.1945G
Altcode:
  Results from high-precision, time-resolved CCD photometry of two
  oscillating blue stragglers in M67 are presented. By comparing similar
  observations obtained two years apart, ten independent modes in one
  of these Delta Scuti stars, and five modes in the other have been
  detected. Results from stellar evolution computations and theoretical
  eigenfrequency analyses are discussed in attempts to make definitive
  mode identifications. For both oscillating blue stragglers, nonradial
  p modes are present that carry information on internal structure,
  rotation, and inclination of the stars. The implications of oscillation
  frequency analyses for theories of the origin of blue stragglers
  are discussed.

Title: Wide-field f /3.5 Rosin camera
Authors: Brown, Timothy M.
Bibcode: 1992ApOpt..31.2314B
Altcode:
  A relatively fast wide-field f/3.5 camera with an aperture of 15 cm and
  a focal length of 52 cm was constructed by modifying wide-field Rosin's
  (1961) design. The camera yields 2.5-arcsec resolution over a 5-deg-diam
  flat field. No ghost images arising from multiple reflections were
  detected within the antireflection-coated corrector system or from
  light reflected backward from the focal plane.

Title: On the Analysis of Helioseismic Time-Series
Authors: Schou, J.; Brown, T. M.
Bibcode: 1991BAAS...23.1390S
Altcode:
  No abstract at ADS

Title: High Precision Doppler Measurements Using Iodine Absorption
    Cells
Authors: Horner, S. D.; Brown, T. M.
Bibcode: 1991BAAS...23.1315H
Altcode:
  No abstract at ADS

Title: The Source of Solar High-Frequency Acoustic Modes: Theoretical
    Expectations
Authors: Brown, Timothy M.
Bibcode: 1991ApJ...371..396B
Altcode:
  The source exciting the solar p-modes is likely to be acoustic noise
  generated in the top part of the sun's convection zone. If so, then
  simple arguments suggest that most of the emitted energy may come
  from rare localized events that are well separated from one another in
  space and time. This note describes the acoustic emission that would
  be expected from such events, based on a ray-theory analysis. Most
  of the acoustic energy is found to emerge very close to the source,
  so that observations to identify emission events will require high
  spatial resolution.

Title: Detection of Possible p-Mode Oscillations on Procyon
Authors: Brown, Timothy M.; Gilliland, Ronald L.; Noyes, Robert W.;
   Ramsey, Lawrence W.
Bibcode: 1991ApJ...368..599B
Altcode:
  In the course of a search for solar-like oscillations in bright
  late-type stars, Doppler variability was observed in the F5 subgiant
  Procyon. The variations have frequencies within a 1.1 mHz range
  centered at 0.9 mHz, and a total rms amplitude within that range
  of 2.5 m/s. Observations of Arcturus and scattered sunlight made
  with the same equipment during the same time interval show no such
  variation, indicating that the variations seen on Procyon are of stellar
  origin. The Doppler signal seen is entirely consistent with solar-like
  p-modes on Procyon, with maximum mode amplitudes of about 50 cm/s
  and periods around 20 minutes. Several statistical tests support the
  identification for the signal with narrow-band oscillations, but none
  does so conclusively. Assuming that the signal does arise from p-modes,
  there is evidence that the frequency splitting nu(0) is 71 micro-Hz. The
  data do not permit a definite estimate of this quantity, and other
  values of nu(0) fit the observations about equally well. In order to
  clarify the sources of ambiguity in this and similar observations,
  the data acquisition, reduction, and interpretation are described.

Title: Time-Resolved CCD Photometry of an Ensemble of Stars in the
    Open Cluster M67
Authors: Gilliland, Ronald L.; Brown, Timothy M.; Duncan, Douglas K.;
   Suntzeff, Nicholas B.; Lockwood, G. Wesley; Thompson, Don T.; Schild,
   Rudolph E.; Jeffrey, William A.; Penprase, Bryan E.
Bibcode: 1991AJ....101..541G
Altcode:
  Stars in the central region of the old open cluster M67 were monitored
  for stability using CCD, time-resolved photometry. Five sites
  with 1 m class telescopes participated in an intensive monitoring
  effort, yielding contiguous 14 night coverage with 1 min temporal
  resolution. Noise levels to 0.0008 mag variation relative to an
  ensemble mean were attained at 13th mag over 9 hr time series. Limits
  to detection of coherent oscillations with periods of 3-20 min,
  assuming a solarlike spectrum of frequencies, are 100 micromag
  (30 times solar amplitude) for the best cases. Evidence suggestive
  of p-mode oscillations is shown for a few stars, but an unambiguous
  detection is not claimed. Serendipitous detection was made of two new
  W UMa stars in M67, two oscillating blue stragglers (with multiple
  modes) a likely AM Her cataclysmic variable with a 2.091 hr period,
  and several stars with low-amplitude intensity changes over timescales
  of 1-10 days, that presumably result from rotation or orbital motion.

Title: Solar Oscillation Ring Diagrams from Mt. Wilson Full-Disk
    Magneto-Optical Dopplergrams
Authors: Hill, Frank; Rhodes, Edward J.; Korzennik, Sylvain G.;
   Cacciani, Alessandro; Brown, Timothy M.
Bibcode: 1991LNP...388..271H
Altcode: 1991ctsm.conf..271H
  Three-dimensional power spectra of solar oscillations have been
  computed from moderate-resolution full disk Doppler images obtained
  with the Magneto-Optical Filter at Mt. Wilson. Slices of the spectra
  at constant frequency reveal the ring structures that are analogous
  to the ridges in two-dimensional spectra. Ring diagrams obtained
  at different heliographic positions show large differences in the
  structure of the rings. These variations can be attributed to the
  changing effective spatial resolution of the observations across the
  disk. After correction for this effect, and .for terrestrial seeing,
  the rings will be used to map the horizontal flows in the convection
  zone as a function of position and depth.

Title: Improvements to solar oscillations time series analysis
    methods.
Authors: Brown, T. M.
Bibcode: 1991dsoo.conf....3B
Altcode:
  At HAO, one is in the process of performing a comprehensive and
  critical evaluation of several methods for analyzing time series
  data related to helioseismology. The purpose is to understand the
  random and systematic errors that may be introduced into estimates
  of p-mode frequencies, amplitudes, and linewidths by the time series
  analysis, and, where possible, to devise means for minimizing these
  errors. The methods will be directly applicable to data obtained by
  extant experiments, as well as to that expected from the GONG network,
  and from the helioseismology instruments on the SOHO spacecraft.

Title: Measurements of Intermediate- and High-Degree (20&lt;1&lt;600)
    p-Mode Solar Oscillation Power and Energy
Authors: Rhodes, Edward J.; Brown, Timothy M.; Cacciani, Alessandro;
   Korzennik, Sylvain G.; Ulrich, Roger K.
Bibcode: 1991LNP...388..277R
Altcode: 1991ctsm.conf..277R
  We present measurements of the total modal power and energy of
  both intermediate- and high-degree (20&lt; l &lt;600) solar p-mode
  oscillations which have been corrected to first order for the combined
  effects of atmospheric seeing, image motion due to imperfect tracking,
  and the point spread function of our optics. These power and energy
  estimates have been obtained from an average of 20 separate zonal l -
  n power spectra, which were obtained from observations obtained at the
  60-Foot Solar Tower of the Mt. Wilson Observatory between July 1 and 20,
  1988. The raw total power values were obtained from a least-squares
  fitting of Lorentzian profiles to the p-mode ridges in the average
  zonal power spectrum. As an initial method of correcting the observed
  power levels, we adopted the procedure described by Kaufman (1988)
  and deconvolved measurements of the observed limb profiles from one
  of our images using two slightly different theoretical unblurred limb
  profiles in order to obtain two estimates of the modulation transfer
  function (mtf) of our experiment. The corrected power values which
  resulted show systematic variations with both frequency and degree
  which are similar to those obtained by Kaufman. For example, between
  l = 100 and 600 our corrected power values drop by a factor of at
  least 4.5, although the magnitude of our correction becomes less
  certain as the degree is increased above 300. We also convert these
  power values into estimates of the total energy of the modes to show
  that the modal energies decrease by a factor of at least 15 over the
  same range in l. Even given the uncertainty of our correction at the
  higher degrees, the consistency of the l-dependent decrease in the
  modal energies with similar results by Kaufman (1990) suggests that,
  at least above l = 100, the modes are not in energy equipartition with
  turbulent convective eddies.

Title: The Sun and Asteroseismology
Authors: Brown, Timothy M.
Bibcode: 1991ASPC...20..139B
Altcode:
  Helioseismological studies of the p-mode solar oscillations can
  be extended to similar oscillations on more distant stars, thereby
  constituting the field of asteroseismology. An evaluation is presented
  of the current and future prospects for such studies in the cases of
  stars of approximately solar type; general agreement has not yet been
  reached as to the detection of p-modes in stars other than the sun,
  but such detections appear likely in the near future through powerful
  new telescopic techniques. There are also suggestive theoretical
  indications as to how much would be learned about stellar interiors
  through detailed studies of stellar oscillation.

Title: The Variability of the Solar Diameter
Authors: Ribes, E.; Beardsley, B.; Brown, T. M.; Delache, Ph.; Laclare,
   F.; Kuhn, J. R.; Leister, N. V.
Bibcode: 1991suti.conf...59R
Altcode:
  It is argued here that most of the variation in observations of
  the solar radius of over three centuries measure properties of the
  sun's limb darkening function and are affected by many sources of
  degradation of the solar image. They do not directly measure a true
  solar radius. From a long series of visual observations made by a
  single observer as well as recent photoelectric observations, evidence
  is found for periodicities in the apparent radius that occur in both
  modern and historical records. The magnitude of the observed variations
  is quite different in visual and photoelectric observations, suggesting
  that the process responsible for the periodicities is either one that
  modifies the solar limb darkening function or one that causes systematic
  variations in image blurring by the earth's atmosphere. A connection
  between solar magnetic activity an apparent radius seems likely, with
  evidence for such a relation dating back as fast as the Maunder minimum.

Title: A Computer Model of Echelle Spectrograph Efficiency
Authors: Horner, S. D.; Brown, T. M.; Ramsey, L. W.
Bibcode: 1990BAAS...22.1260H
Altcode:
  No abstract at ADS

Title: An Inverse Method for P-Mode Scattering Measurements
Authors: Brown, Timothy M.
Bibcode: 1990SoPh..128..133B
Altcode: 1990IAUCo.121P.133B
  Observations of acoustic waves propagating into and out of solar active
  regions (Braun, Duvall, and LaBonte, 1987a, b) show that for moderately
  large horizontal wavenumbers, sunspots may absorb as much as 50% of
  the acoustic energy incident on them. If the absorption process can be
  parameterized adequately, it should be possible to use such observations
  to learn something about the subsurface structure of magnetized
  regions. One way to do this is to treat the inhomogeneities seen by the
  propagating sound waves as a collection of point scatterers. Starting
  from this approximation, and assuming that multiple scattering is
  unimportant, it is possible to use the ingoing and outgoing wave
  fields observed at the solar surface to infer a 3-dimensional map of
  the active region structure. The inversion technique used to do this is
  a departure from usual practice in helioseismology, in that the input
  data it requires are mode amplitudes and phases, not frequencies. An
  advantage resulting from this difference is that one can attain high
  spatial resolution (comparable to the local acoustic wavelength)
  with small noise amplification.

Title: A Search for Solar-like Oscillations in alpha Centauri A
Authors: Brown, Timothy M.; Gilliland, Ronald L.
Bibcode: 1990ApJ...350..839B
Altcode:
  Spectrographic observations made in the course of a search for
  solar-like acoustic oscillations in Alpha Cen A are described. The
  observational method was to search for periodic Doppler-shift variations
  in all of the spectrum lines within the wavelength range accessible
  to a high-dispersion echelle spectrograph - about 30 nm centered on
  427.5 nm, in this case. A search was also conducted for variations in
  the ratio of line core to continuum intensity, again averaged over all
  the available lines. No convincing oscillations were found in either
  case, with upper limits for typical single oscillation modes of 70
  cm/s in Doppler shift and 4 x 10 to the -5th for continuum intensity
  variations inferred from line core intensities.

Title: A Technique for Estimating Complicated Power Spectra from
    Time Series with Gaps
Authors: Brown, Timothy M.; Christensen-Dalsgaard, Jorgen
Bibcode: 1990ApJ...349..667B
Altcode:
  Fahlman and Ulrych (1982) describe a method for estimating the power
  and phase spectra of gapped time series, using a maximum-entropy
  reconstruction of the data in the gaps. It has proved difficult to
  apply this technique to solar oscillations data, because of the great
  complexity of the solar oscillations spectrum. A means for avoiding
  this difficulty is described, and the results of a series of blind
  tests of the modified technique are reported. The main results of
  these tests are: (1) gap filling gives good results, provided that
  the signal-to-noise ratio in the original data is large enough, and
  provided the gaps are short enough. For low-noise data, the duty cycle
  of the observations should not be less than about 50 percent. (2) the
  frequencies and widths of narrow spectrum features are well reproduced
  by the technique. (3) The technique systematically reduces the apparent
  amplitudes of small features in the spectrum relative to large ones.

Title: High precision Doppler measurements via echelle spectroscopy.
Authors: Brown, Timothy M.
Bibcode: 1990ASPC....8..335B
Altcode: 1990ccd1.proc..335B; 1990LDP....13..335B; 1990ccda.proc..335B
  With modern echelle spectrographs and CCD detectors, photon noise
  permits one to measure the radial velocity of bright stars with
  precision as good as 1 m/s in 60 s of observing time. In order to
  achieve this precision in practice, one must take measures to control
  several sources of instrumental noise. Two distinct methods have evolved
  to do this: (1) one may use a molecular absorption cell to impress lines
  of constant wavelength on the incoming starlight, or (2) one may use a
  fiber optic feed for the starlight, in conjunction with a second fiber
  carrying light from a stable wavelength source. At the current state of
  development, the first method yields better long-term stability (useful,
  e.g., for planetary detection), while the second method provides better
  S/N per unit time in circumstances where low-frequency stability is
  not required (such as observation of stellar oscillations). For both
  methods, details of instrument setup, data acquisition, and data
  analysis are important for getting the best results.

Title: Oscillating Blue Stragglers in the Old open Cluster M67
Authors: Gilliland, R. L.; Brown, T. M.; Duncan, D. K.; Suntzeff,
   N. B.; Lockwood, G. W.; Schild, R. E.; Jeffrey, W. A.; Penprase, B. E.
Bibcode: 1989BAAS...21.1119G
Altcode:
  No abstract at ADS

Title: Inferring the Sun's Internal Angular Velocity from Observed
    p-Mode Frequency Splittings
Authors: Brown, Timothy M.; Christensen-Dalsgaard, Jorgen; Dziembowski,
   Wojciech A.; Goode, Philip; Gough, Douglas O.; Morrow, Cherilynn A.
Bibcode: 1989ApJ...343..526B
Altcode:
  The sun's internal solar velocity Omega is studied as a function of
  latitude and radius using the solar oscillation data of Brown and
  Morrow (1987). An attempt is made to separate robust inferences about
  the sun from artifacts of the analysis. It is found that a latitudinal
  variation of Omega similar to that observed at the solar surface exists
  throughout the sun's convection zone and that the variation of Omega
  with latitude persists to some extent even beneath the convection zone.

Title: The GONG data reduction and analysis system.
Authors: Pintar, J. A.; Andersen, B.; Anderson, E. R.; Armet, D. B.;
   Brown, T. M.; Hathaway, D. H.; Hill, F.; Jones, H. P.; GONG Data Team
Bibcode: 1988ESASP.286..217P
Altcode:
  Each of the six GONG observing stations will produce three, 16-bit,
  256×256 images of the Sun every 60 seconds of sunlight. These
  data will be transferred from the observing sites to the GONG Data
  Management and Analysis Center (DMAC), in Tucson, on high-density tapes
  at a combined rate of over 1 gigabyte per day. The contemporaneous
  processing of these data will produce several standard data products
  and will require a sustained throughput in excess of 7 megaflops. Peak
  rates may exceed 50 megaflops. Archives will accumulate at the rate
  of approximately 1 terabyte per year, reaching nearly 3 terabytes in
  three years of observing. Researchers will access the data products
  with a machine-independent GONG Reduction and Analysis Software
  Package (GRASP). Based on the Image Reduction and Analysis Facility
  (IRAF), this package will include database facilities and helioseismic
  analysis tools. Users may access the data as visitors in Tucson, or
  may access DMAC remotely through networks, or may process subsets of
  the data at their local institutions using GRASP or other systems of
  their choice. Elements of the system will reach the prototype stage
  by the end of 1988. Full operation is expected in 1992 when data
  acquisition begins.

Title: Time-Resolved CCD Photometry of an Ensemble of Stars
Authors: Gilliland, Ronald L.; Brown, Timothy M.
Bibcode: 1988PASP..100..754G
Altcode:
  A technique for obtaining CCD photometry of a large ensemble of
  stars, with precision limited by atmospheric scintillation and photon
  statistics is presented. Under bright-sky conditions with a 0.9-m
  telescope, a precision of about 0.0015 mag relative to an ensemble
  average standard was obtained for 12th-13th mag stars in M 67 with
  exposure times of 1 min. The increase in noise level due to variable
  cirrus clouds is minimal. Effective noise levels for the detection of
  coherent oscillations with periods of 5-20 min could thus be reduced
  to about 30 micromag over ten nights of observing for stars of this
  brightness. A much larger ensemble of faint stars could be followed at
  lower precision with sky background and photon statistics as dominant
  error sources. Four probable-cluster DA white dwarfs were detected in
  the old galactic cluster M 67, using B, V calibration photometry.

Title: A Bayesian Approach to Ridge Fitting in the Omega-K Diagram
    of the Solar 5-MINUTE Oscillations
Authors: Morrow, C. A.; Brown, T. M.
Bibcode: 1988IAUS..123..485M
Altcode:
  The acoustic oscillation modes of the Sun cluster along ridges of power
  in the frequency (ω), horizontal wave number (k) plane. Fitting curves
  to these ridges provides input for methods that reveal information
  about the Sun's interior. The Bayesian approach allows one to make
  systematic use of prior physical and phenomenological information to
  assign a prior probability that a candidate curve gives the best fit
  to a ridge. Bayes' rule then permits one to update this probability
  using the new ridge power data. The maximally probable candidate curve
  giving both new and prior information is chosen as the best fit.

Title: Automated P-Mode Identification Using Bayes' Theorem
Authors: Brown, T. M.
Bibcode: 1988IAUS..123..491B
Altcode:
  The task of interpreting p-mode spectra is complicated by the
  presence of a very large number of oscillation modes, each of which
  may appear in the power spectra corresponding to several values of l
  and m. Identifying peaks in a power spectrum with particular modes in
  an interactive fashion thus quickly becomes impractical. The author
  describes an automated method for doing this identification. The
  method is based on an application of Bayes' theorem. The method takes
  as input the observed power spectra, and a model of the amplitudes
  and frequencies one expects to see.

Title: Techniques for Observing Solar Oscillations
Authors: Brown, T. M.
Bibcode: 1988IAUS..123..453B
Altcode:
  The author discusses first the instrumental techniques used to observe
  solar p-modes, with attention given both to low- and no-resolution
  systems, and to systems with spatial resolution. Then he describes
  the reduction techniques that are used to convert the raw observations
  into useful form.

Title: Depth and Latitude Dependence of Solar Rotation
Authors: Brown, Timothy M.; Morrow, Cherilynn A.
Bibcode: 1987ApJ...314L..21B
Altcode:
  A 15-day time series of spatially resolved full-disk Doppler
  observations is used to measure the dependence of p-mode oscillation
  frequencies on the mode azimuthal order m. This dependence may be used
  to infer the depth and latitude variation of the solar rotation. The
  results are consistent with solar models that have approximately the
  surface latitudinal differential rotation within the convection zone,
  but no latitudinal differential rotation in the radiative interior. The
  data do not make it possible to distinguish between models for which
  the angular rotation rate within the convection zone is a function
  of latitude alone, and those for which it is constant on cylindrical
  surfaces. Weak evidence for a pole-equator asymmetry in the sound
  speed is found.

Title: Observations of Solar P-Mode Rotational Splittings
Authors: Brown, Timothy M.; Morrow, Cherilynn A.
Bibcode: 1987ASSL..137....7B
Altcode: 1987isav.symp....7B
  The results of a new set of observations of solar p-mode rotational
  splittings obtained with the Fourier Tachometer at NSO/Sunspot (Brown
  and Morrow, 1986) are described. The rotational splittings from
  these observations fall between those of Brown (1985) and Duvall et
  al. (1986). They are apparently consistent with a model in which the
  differential rotation resembles that seen at the surface throughout
  the convective zone, but becomes constant on spherical surfaces within
  the radiative interior.

Title: Some current problems in helioseismology
Authors: Brown, Timothy M.
Bibcode: 1987LNP...274..298B
Altcode: 1987stpu.conf..298B
  Helioseismology is enjoying a tremendous surge of activity, spurred
  by the combination of reliable data and effective interpretation
  methods. Since I cannot do justice to the entire field, I attempt in
  this review to describe two current topics that I find interesting. (1)
  Several workers have now made measurements relating to the variation
  of rotation with depth and latitude inside the Sun. Most of the
  observations agree fairly well on the depth dependence, but not so
  well on the latitude dependence. I explain how such measurements
  are made, and discuss the current state of this controversy. (2)
  The driving mechanism for solar p-modes remains a mystery. The best
  (in my view) explanation involves stochastic driving of the modes by
  turbulent convection. This theory (proposed by Goldreich and Keeley)
  has recently been extended by Goldreich and Kumar in a way that
  illuminates some issues and obscures others. I attempt to provide a
  simple introduction to these ideas.

Title: An Asteroseismology Explorer
Authors: Brown, Timothy M.; Cox, Arthur N.
Bibcode: 1987LNP...274..415B
Altcode: 1987stpu.conf..415B
  In response to a NASA opportunity, a proposal has been made to study
  the concept of an Asteroseismology Explorer (ASE). The goal of the
  ASE would be to measure solar-like oscillations on many (perhaps
  hundreds) of stars during a 1-year mission, including many members
  of open clusters. We describe this proposal's observational goals,
  a strawman technical approach, and likely scientific rewards.

Title: Phase recovery with dual nonredundant arrays
Authors: Zirker, J. B.; Brown, T. M.
Bibcode: 1986JOSAA...3.2077Z
Altcode: 1986OSAJ....3.2077Z
  Nonredundant arrays inserted at the pupil plane of a telescope permit
  recovery of both amplitude and phase of numerous Fourier components of a
  small target. A single array, however, yields insufficient information
  with which to solve for all the Fourier components to which that array
  responds. A method is proposed here for selecting pairs of arrays that
  yield complete information within some passband of spatial frequencies.

Title: Solar waves and oscillations.
Authors: Brown, T. M.; Mihalas, B. W.; Rhodes, E. J., Jr.
Bibcode: 1986psun....1..177B
Altcode:
  Contents: Theory of waves and oscillations (basic equations: full
  hydromagnetic equations, linearized equations; waves: nonmagnetic waves,
  magnetohydrodynamic waves; general properties of solar oscillations:
  equations and spheroidal mode solutions, Cowling approximation,
  asymptotic behavior of p- and g-mode frequencies, radial oscillations,
  properties of nonadiabatic solutions, toroidal oscillations; excitation
  and damping of solar pulsations: excitation and damping mechanisms,
  mode lifetimes, stability of solar pulsation modes; detailed solutions
  for frequencies and frequency splitting: effects of structure on
  unperturbed frequencies, effects of rotation, effects of internal
  magnetic fields; future theoretical needs). Observations (observational
  techniques: diagnostics of spectrum lines, techniques for observing
  oscillations and trapped waves; oscillations observed: observations
  of 5 minute period p-mode oscillations, the 160 minute oscillation,
  torsional oscillations, localized brightness oscillations; wave
  observations; waves and oscillations in sunspots; future observational
  needs). Oscillations as probes of the solar interior (direct method:
  technique and results; inversion methods: technique and applications).

Title: Measuring the Sun's internal rotation using solar p-mode
    oscillations.
Authors: Brown, Timothy M.
Bibcode: 1986ASIC..169..199B
Altcode: 1986ssds.proc..199B
  2-dimensional velocity images of the Sun were obtained for 5 days in
  June, 1984. This time series of images has been analyzed to obtain
  frequencies of solar p-mode oscillations with degrees between 8 and 50,
  with all azimuthal orders for each degree. The principal results of the
  analysis are measurements of the frequency splitting between modes with
  the same degree and radial order; these are related to the latitudinal
  variation of solar rotation. The observed splittings suggest that for
  0.3 R_sun; ≤ r ≤ 0.7 R_sun;, the solar latitudinal differential
  rotation is much smaller than at the surface, and moreover than the
  rotation rate is close to the surface equatorial value.

Title: Solar rotation as a function of depth and latitude
Authors: Brown, T. M.
Bibcode: 1985Natur.317..591B
Altcode:
  A 5-day series of two-dimensional velocity images of the Sun
  is analysed to yield frequencies of solar p-mode oscillations
  with degrees between 8 and 50, with all azimuthal orders for each
  degree. The frequency splitting between modes with the same degree
  and radial order is related to the latitudinal variation of rotation,
  averaged over a depth range that depends on the degree. The observed
  splittings indicate that for 0.3Rsolar &lt;~r&lt;~0.7Rsolar the solar
  latitudinal differential rotation is much smaller than at the surface
  (rotation roughly constant on spheres), and moreover that the rotation
  rate is close to the surface equatorial value.

Title: Analysis and interpretation of synthetic time strings of
    oscillation data.
Authors: Mihalas, B. W.; Christensen-Dalsgaard, J.; Brown, T. M.
Bibcode: 1984sses.nasa..279M
Altcode: 1984sss..conf..279M
  Artificial strings of solar oscillation data with gaps and noise,
  corresponding to the output of different spatial filter functions,
  were analyzed. Peaks in the power spectrum are identified for values of
  the degree l from 0 to 18, and rotational splitting is estimated. The
  filters prove effective in facilitating identification of essentially
  all the real peaks in the power spectrum. Estimates of peak frequencies
  and amplitudes and rotational splitting frequencies are in reasonably
  good agreement with the input values. Spurious peaks in autocorrelation
  spectra correspond to the frequency spacing between power peaks with
  the same order n, differing by one or two in the degree l.

Title: The Fourier Tachometer II - an instrument for measuring global
    solar velocity fields.
Authors: Brown, T. M.
Bibcode: 1984sses.nasa..157B
Altcode: 1984sss..conf..157B
  The High Altitude Observatory and Sacramento Peak Observatory have
  jointly constructed a second version of the Fourier Tachometer,
  which is now undergoing final integration and testing. This is an
  interferometric instrument for measuring the Doppler shift of solar
  spectrum lines. The principal features and performance goals of this
  instrument are: simultaneous velocity observations over a 2-dimensional,
  100 x 100 pixel field of view; measurement of absolute Doppler shifts
  with 1 m/s accuracy; noise level for moderate-1 oscillation modes of
  1 cm/s for a 1-day observing run; flexibility and ease of use. Early
  (though incomplete) testing suggests that these goals should be
  attainable with the current instrument.

Title: Solar p-Mode Eigenfrequencies are Decreased by Turbulent
    Convection
Authors: Brown, T. M.
Bibcode: 1984Sci...226..687B
Altcode:
  Average solar p-mode eigenfrequencies are decreased by large fluctuating
  velocity fields in the upper convection zone. This effect is greatest
  for modes with large horizontal wave numbers and frequencies. It
  is large enough to affect estimates of the depth of the convection
  zone and may carry useful information about the structure of solar
  convective turbulence.

Title: Techniques for detecting giant cells using spatially resolved
    solar velocity data
Authors: Brown, T. M.; Gilman, P. A.
Bibcode: 1984ApJ...286..804B
Altcode:
  Whether giant cells exist in the convection zone of the sun, and what
  their properties might be, are matters of great importance for the
  understanding of the dynamics of the solar interior. So far, such cells
  have escaped detection, probably because of the small amplitude of their
  associated velocity fields and the large amplitudes of shorter-lived
  flows. Techniques for improving the detectability of giant cells are
  presented. These methods are based on the spatial extent and symmetry
  properties of giant cells as seen in self-consistent dynamical models
  of the solar convection zone. Simulations suggest that these techniques
  allow detection of giant cells with photospheric rms velocities of 2
  m/s (0.4 m/s per longitudinal wavenumber), given observations spanning
  about one year.

Title: Solar Oscillations Observations with the Fourier Tachometer II
Authors: Brown, T. M.
Bibcode: 1984BAAS...16..978B
Altcode:
  No abstract at ADS

Title: Life history of a fossil: An introduction to taphonomy and
    paleoecology
Authors: Brown, T. M.
Bibcode: 1983ESRv...19..356B
Altcode:
  No abstract at ADS

Title: Seeing-independent definitions of the solar limb position
Authors: Brown, T. M.
Bibcode: 1982A&A...116..260B
Altcode:
  The most important of the advantages of the finite Fourier transform
  definition (FFTD) is a low sensitivity to changes in the width of
  the atmospheric point spread function. This paper describes a class
  of similar edge definitions which share the advantages of the FFTD
  and which may be tailored to any desired limb darkening function or
  set of observing conditions. For some limb darkening functions, edge
  definitions may be obtained which are substantially less sensitive to
  seeing than the FFTD.

Title: Solar diameter monitor: an instrument to measure long-term
    changes
Authors: Brown, Timothy M.; Elmore, D. F.; Lacey, L.; Hull, H.
Bibcode: 1982ApOpt..21.3588B
Altcode:
  No abstract at ADS

Title: Information theory and the spectrum of isotropic turbulence
Authors: Brown, T. M.
Bibcode: 1982JPhA...15.2285B
Altcode:
  A method of closing the equation set describing turbulent flows is
  presented in which the flow behaves in such a way that an entropy
  defined in terms suggested by information theory is maximized. The
  relevant constraints are taken to be the Reynolds number and energy
  dissipation rate of the flow, energy balance at every point in
  wavenumber space, and adherence to the Navier-Stokes equations. It is
  shown that the maximum entropy formalism leads to a pair of coupled
  equations describing the distribution of energy in the turbulent
  spectrum, and the correlations between the amplitudes of velocity
  components with nearly identical wavenumbers. It develops that if
  a power-law solution exists, it can only be the Kolmogorov law. The
  turbulent temperature, defined as the reciprocal of the derivative
  of the entropy with respect to the local energy dissipation rate,
  is virtually constant within the spectrum's inertial subrange.

Title: The HAO Solar Diameter Monitor
Authors: Brown, T. M.
Bibcode: 1981BAAS...13..878B
Altcode:
  No abstract at ADS

Title: Evidence for trapped gravity waves in the solar atmosphere
Authors: Brown, T. M.; Harrison, R. L.
Bibcode: 1980ApJ...236L.169B
Altcode:
  Observations of disk-center solar continuum brightness fluctuations are
  reported. These observations show features that may be interpreted
  as internal gravity waves trapped in the solar photosphere and
  chromosphere. The reasons for this interpretation, and some of its
  implications are discussed.

Title: Are Gravity Waves Trapped in the Solar Photosphere?
Authors: Brown, T. M.
Bibcode: 1980BAAS...12..475B
Altcode:
  No abstract at ADS

Title: The Opportunities Offered by SCADM for the Study of Surface
    Phenomena Related to Interior Structure and Dynamics
Authors: Brown, T. M.
Bibcode: 1980NASCP2098..101B
Altcode: 1980sscs.nasa..101B
  The physical processes to be probed by experiments may be grouped
  as large scale flows, oscillations, and chromospheric/coronal
  diagnostics. While the fundamental concerns and observational equipments
  are similar within each class, different investigations may tell
  different things about the Sun. Observational requirements are listed
  for experiments to study (1) plasma-magnetic field interactions; (2)
  interior structure via oscillations; (3) chromospheric and coronal
  tracers; (4) rotation, meridional flows, and giant cells; (5) the depth
  dependence of rotation; (6) EUV luminosity; (7) intensity fluctuations
  and tracers; and (8) diameter oscillations, the effects of noise and
  time-string on experiment results are assessed.

Title: Solar circulation measurements: consideration and plans
Authors: Beckers, J. M.; Brown, T. M.
Bibcode: 1980fsoo.conf..189B
Altcode:
  No abstract at ADS

Title: Solar continuum brightness oscillations - A progress report
Authors: Brown, T. M.; Harrison, R. L.
Bibcode: 1980LNP...125..200B
Altcode: 1980nnsp.work..200B
  Solar brightness oscillations were observed in the continuum, and
  results achieved to date are summarized for two distinct groups of
  data. One deals with oscillations at the extreme solar limb, while
  the other involves oscillations at the disk center. Some preliminary
  interpretations are offered pending further data collection.

Title: Observed brightness oscillations at the solar limb.
Authors: Brown, T. M.
Bibcode: 1979ApJ...230..255B
Altcode:
  Observations of the continuum intensity near the solar limb are used to
  estimate the power in fluctuating brightness as a function of spatial
  and temporal frequency and distance from the limb. This presentation of
  the data clearly discriminates between atmospheric and solar effects,
  and shows that brightness oscillations are indeed present on the
  sun. Most power lies below 1.5 mHz or betweeen 3.0 and 5.0 mHz, and
  at wavelengths longer than 5 Mm. Amplitudes per frequency-wavenumber
  resolution element range downward from one thousandth the disk-center
  intensity. The oscillation amplitude apparently increases with distance
  inward from the limb, indicating that the contribution from a high,
  optically thin shell cannot be very important.

Title: Solar circulation measurements: considerations and plans.
Authors: Beckers, J. M.; Brown, T. M.
Bibcode: 1979MmArc.106..189B
Altcode:
  No abstract at ADS

Title: Solar limb brightness oscillations.
Authors: Brown, T. M.
Bibcode: 1978BAAS...10..729B
Altcode:
  No abstract at ADS

Title: Long-period oscillations of the apparent solar diameter:
    observations.
Authors: Brown, T. M.; Stebbins, R. T.; Hill, H. A.
Bibcode: 1978ApJ...223..324B
Altcode:
  New observations of the time-varying component of the apparent solar
  diameter are reported. Power spectra derived from these observations
  reveal narrow-band oscillations at frequencies consistent with the
  normal mode frequencies of a standard solar model. The amplitudes of
  these oscillations are discussed and related to the observations of
  other investigators. A detailed analysis of the experiment and its
  associated sources of error is presented and used to show that there
  is a very small likelihood that the power spectrum peaks are due to
  nonsolar causes.

Title: Solar circulation measurements: consideration and plans
Authors: Beckers, J. M.; Brown, T. M.
Bibcode: 1978fsoo.conf..189B
Altcode:
  No abstract at ADS

Title: Performance of image-plane sharpness criteria in image
    reconstruction
Authors: Brown, T. M.
Bibcode: 1978JOSA...68..890B
Altcode: 1978OSAJ...68..890B
  The performance of image-plane sharpness criteria for purposes of image
  reconstruction is discussed in terms of a probabilistic model. This
  model provides a general framework for understanding sharpness criteria
  and predicts that the accuracy of the phase compensation process is
  proportional to the number of discrete phase correcting elements.

Title: Reconstruction of turbulence-degraded images using nonredundant
    aperture arrays
Authors: Brown, T. M.
Bibcode: 1978JOSA...68..883B
Altcode: 1978OSAJ...68..883B
  A technique is described which allows the removal of seeing distortions
  from a single frame of speckle-type imagery, provided that this frame
  is obtained using an aperture consisting of a nonredundant array of
  subapertures, each smaller than the seeing correlation length. Although
  performed a posteriori, the method is related to those already proposed
  for use with active optical systems. Computer simulations are described
  which verify the basic features of this technique. The simulations
  indicate that reconstructed images of diffraction-limited quality should
  be obtainable for starlike objects as dim as eighth magnitude. For
  more extended objects, the limiting magnitude depends somewhat on the
  object structure. The technique described is immediately applicable to
  any large telescope, and because the processing is done after the fact,
  a frame containing many isoplanatic patches may be processed piecewise,
  allowing the reconstruction of large areas

Title: An Observational Investigation of Long-Period Oscillations
    in the Apparent Solar Diameter.
Authors: Brown, T. M.
Bibcode: 1977PhDT.........5B
Altcode:
  A power spectrum analysis of eleven individual time series observations
  of the apparent solar diameter reveals oscillations throughout the
  three minute to 70 minute period range, with typical amplitudes of
  .000002 of the solar diameter. Many of the long period peaks in the
  power spectrum appear to be narrow-band features, with damping times
  long compared to the length of a typical time series. At least ten of
  the observed peaks show repeatable power levels that are significant
  at the 0.999 confidence level, and two of them appear to show good
  phase coherence over the entire 30 day observation period.

Title: Observed Oscillations of the Apparent Solar Diameter
Authors: Brown, T. M.; Stebbins, R. T.; Hill, H. A.
Bibcode: 1976ssp..conf....1B
Altcode:
  No abstract at ADS

Title: INVITED PAPER - Recent Progress in Solar Oblateness Studies
Authors: Hill, H. A.; Stebbins, R. T.; Brown, T. M.
Bibcode: 1975BAAS....7R.478H
Altcode:
  No abstract at ADS

Title: The Dispersal of the Shell of Zeta Ophiuchi
Authors: Barker, Paul K.; Brown, Timothy
Bibcode: 1974ApJ...192L..11B
Altcode:
  Observations are presented showing that the shell recently ejected by
  Oph has now disappeared. Spectral changes, including the disappearance
  of Ha emission, are described. Subject headings: circumstellar shells -
  early-type stars - line profiles