text:
and demonstrate that it keeps time well. This technique, called gyrochronology, derives ages for low-mass main-sequence stars using only their rotation periods and colors. The technique is developed here and used to derive ages for illustrative groups of nearby field stars with measured rotation periods. We first demonstrate the reality of the interface sequence, the unifying feature of the rotational observations of cluster and field stars that makes the technique possible, and extend it beyond the proposal of Skumanich by specifying the mass dependence of rotation for these stars. We delineate which stars it cannot currently be used on. We then calibrate the age dependence using the Sun. The errors are propagated to understand their dependence on color and period. Representative age errors associated with the technique are estimated at \textasciitilde 15\% (plus possible systematic errors) for late F, G, K, and early M stars. Gyro ages for the Mount Wilson stars are shown to be in good agreement with chromospheric ages for all but the bluest stars, and probably superior. Gyro ages are then calculated for each of the active main-sequence field stars studied by Strassmeier and collaborators. These are shown to have a median age of 365 Myr. The sample of single field stars assembled by Pizzolato and collaborators is then assessed and shown to have gyro ages ranging from under 100 Myr to several Gyr, with a median age of 1.2 Gyr. Finally, we demonstrate that the individual components of the three wide binaries {$\xi$} Boo AB, 61 Cyg AB, and {$\alpha$} Cen AB yield substantially the same gyro ages.},
  file = {/Users/Oliver/Zotero/storage/HTMX4DAI/Barnes - 2007 - Ages for Illustrative Field Stars Using Gyrochrono.pdf;/Users/Oliver/Zotero/storage/ZGYAD5AX/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  keywords = {Core Gyrochronology},
  language = {en},
  number = {2}
}

@article{barnes2010,
  title = {A {{Simple Nonlinear Model}} for the {{Rotation}} of {{Main}}-Sequence {{Cool Stars}}. {{I}}. {{Introduction}}, {{Implications}} for {{Gyrochronology}}, and {{Color}}-{{Period Diagrams}}},
  author = {Barnes, Sydney A.},
  year = {2010},
  month = oct,
  volume = {722},
  pages = {222},
  doi = {10.1088/0004-637X/722/1/222},
  abstract = {We here introduce a simple nonlinear model to describe the rotational evolution of cool stars on the main sequence. It is formulated only in terms of the Rossby number (Ro = P/{$\tau$}), its inverse, and two dimensionless constants which we specify using solar and open-cluster data. The model has two limiting cases of stellar rotation, previously called C and I, that correspond to two observed sequences of fast and slowly rotating stars in young open clusters. The model describes the evolution of stars from C-type, with particular mass and age dependencies, to I-type, with different mass and age dependencies, through the rotational gap, g, separating them. The proposed model explains various aspects of stellar rotation, and provides an exact expression for the age of a rotating cool star in terms of P and {$\tau$}, thereby generalizing gyrochronology. Using it, we calculate the time interval required for stars to reach the rotational gap\textemdash a monotonically increasing, mildly nonlinear function of {$\tau$}. Beginning with the range of initial periods indicated by observations, we show that the (mass-dependent) dispersion in rotation period initially increases, and then decreases rapidly with the passage of time. The initial dispersion in period contributes up to 128 Myr to the gyro-age errors of solar-mass field stars. Finally, we transform to color-period space, calculate appropriate isochrones, and show that this model explains some detailed features in the observed color-period diagrams of open clusters, including the positions and shapes of the sequences, and the observed density of stars across these diagrams.},
  file = {/Users/Oliver/Zotero/storage/PBA3UWEZ/Barnes - 2010 - A Simple Nonlinear Model for the Rotation of Main-.pdf;/Users/Oliver/Zotero/storage/PNT29BCA/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{bastien+2013,
  title = {An Observational Correlation between Stellar Brightness Variations and Surface Gravity},
  author = {Bastien, Fabienne A. and Stassun, Keivan G. and Basri, Gibor and Pepper, Joshua},
  year = {2013},
  month = aug,
  volume = {500},
  pages = {427--430},
  issn = {0028-0836, 1476-4687},
  doi = {10.1038/nature12419},
  abstract = {Surface gravity is one of a star's basic properties, but it is difficult to measure accurately, with typical uncertainties of 25-50 per cent if measured spectroscopically and 90-150 per cent photometrically. Asteroseismology measures gravity with an uncertainty of about two per cent but is restricted to relatively small samples of bright stars, most of which are giants. The availability of high-precision measurements of brightness variations for {$>$}150,000 stars provides an opportunity to investigate whether the variations can be used to determine surface gravities. The Fourier power of granulation on a star's surface correlates physically with surface gravity; if brightness variations on timescales of hours arise from granulation, then such variations should correlate with surface gravity. Here we report an analysis of archival data that reveals an observational correlation between surface gravity and the root-mean-square brightness variations on timescales of less than eight hours for stars with temperatures of 4500-6750K, log of surface gravities of 2.5-4.5 (cgs units), and having overall brightness variations {$<$}3 parts per thousand. A straightforward observation of optical brightness variations therefore allows a determination of the surface gravity with a precision of {$<$}25 percent for inactive Sun-like stars at main-sequence to giant stages of evolution.},
  archivePrefix = {arXiv},
  eprint = {1308.4728},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/KNR9UVM9/Bastien et al. - 2013 - An observational correlation between stellar brigh.pdf;/Users/Oliver/Zotero/storage/UFVI2R7M/1308.html},
  journal = {Nature},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {7463}
}

@article{bastien+2016,
  title = {A {{Granulation}} "{{Flicker}}"-Based {{Measure}} of {{Stellar Surface Gravity}}},
  author = {Bastien, Fabienne A. and Stassun, Keivan G. and Basri, Gibor and Pepper, Joshua},
  year = {2016},
  month = feb,
  volume = {818},
  pages = {43},
  issn = {1538-4357},
  doi = {10.3847/0004-637X/818/1/43},
  abstract = {In Bastien et al. (2013) we found that high quality light curves, such as those obtained by Kepler, may be used to measure stellar surface gravity via granulation-driven light curve "flicker". Here, we update and extend the relation originally presented in Bastien et al. (2013) after calibrating flicker against a more robust set of asteroseismically derived surface gravities. We describe in detail how we extract the flicker signal from the light curves, including how we treat phenomena, such as exoplanet transits and shot noise, that adversely affect the measurement of flicker. We examine the limitations of the technique, and, as a result, we now provide an updated treatment of the flicker-based logg error. We briefly highlight further applications of the technique, such as astrodensity profiling or its use in other types of stars with convective outer layers. We discuss potential uses in current and upcoming space-based photometric missions. Finally, we supply flicker-based logg values, and their uncertainties, for 27 628 Kepler stars not identified as transiting-planet hosts, with 4500{$<$}teff{$<$}7150 K, 2.5{$<$}logg{$<$}4.6, Kepler magnitude {$<$}13.5, and overall photometric amplitudes {$<$}10 parts per thousand.},
  archivePrefix = {arXiv},
  eprint = {1512.03454},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/WAVNSHQ3/Bastien et al. - 2016 - A Granulation Flicker-based Measure of Stellar S.pdf;/Users/Oliver/Zotero/storage/QAUPZBXQ/1512.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{basu+1997,
  title = {Solar Internal Sound Speed as Inferred from Combined {{BiSON}} and {{LOWL}} Oscillation Frequencies},
  author = {Basu, Sarbani and {Christensen-Dalsgaard}, J. and Chaplin, W. J. and Elsworth, Y. and Isaak, G. R. and New, R. and Schou, J. and Thompson, M. J. and Tomczyk, S.},
  year = {1997},
  month = dec,
  volume = {292},
  pages = {243},
  issn = {0035-8711},
  doi = {10.1093/mnras/292.2.243},
  abstract = {Observations of the sun with the LOWL instrument provide a homogeneous
set of solar p-mode frequencies from low to intermediate degree that
allow one to determine the structure of much of the solar interior,
avoiding systematic errors that are introduced when different data sets
are combined, i.e., principally the effects of solar cycle changes on
the frequencies. Observations made by the Birmingham Solar-Oscillations
Network (BiSON) in integrated sunlight provide high-accuracy
measurements of a large number of low-degree modes. In this paper we
demonstrate that the low-degree mode set of the LOWL data can be
successfully combined with the more accurate BiSON data, provided the
observations are contemporaneous for those frequencies where the solar
cycle induced effects are important. We show that this leads to a factor
of 2 decrease in the error on the inferred sound speed in the solar
core. We find that the solar sound speed is higher than in solar models
for r less than 0.2 solar radius. The density of the solar core is,
however, lower than that in solar models.},
  file = {/Users/Oliver/Zotero/storage/U8AFE57Z/Basu et al. - 1997 - Solar internal sound speed as inferred from combin.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Astronomical Models,Error Analysis,Solar Cycles,Solar Diameter,Solar Interior,Solar Oscillations,Sound Propagation,Sunlight}
}

@article{basu+2009,
  title = {Fresh {{Insights}} on the {{Structure}} of the {{Solar Core}}},
  author = {Basu, Sarbani and Chaplin, William J. and Elsworth, Yvonne and New, Roger and Serenelli, Aldo M.},
  year = {2009},
  month = jul,
  volume = {699},
  pages = {1403--1417},
  issn = {0004-637X},
  doi = {10.1088/0004-637X/699/2/1403},
  abstract = {We present new results on the structure of the solar core, obtained with new sets of frequencies of solar low-degree p modes obtained from the BiSON network. We find that different methods used in extracting the different sets of frequencies cause shifts in frequencies, but the shifts are not large enough to affect solar structure results. We find that the BiSON frequencies show that the solar sound speed in the core is slightly larger than that inferred from data from Michelson Doppler Imager low-degree modes, and the uncertainties on the inversion results are smaller. Density results also change by a larger amount, and we find that solar models now tend to show smaller differences in density compared to the Sun. The result is seen at all radii, a result of the fact that conservation of mass implies that density differences in one region have to cancel out density differences in others, since our models are constructed to have the same mass as the Sun. The
uncertainties on the density results are much smaller too. We attribute the change in results to having more, and lower frequency, low-degree mode frequencies available. These modes provide greater sensitivity to conditions in the core.},
  file = {/Users/Oliver/Zotero/storage/YHM56XVN/Basu et al. - 2009 - Fresh Insights on the Structure of the Solar Core.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Sun: abundances,Sun: helioseismology,Sun: interior}
}

@article{basu+2009a,
  title = {Fresh {{Insights}} on the {{Structure}} of the {{Solar Core}}},
  author = {Basu, Sarbani and Chaplin, William J. and Elsworth, Yvonne and New, Roger and Serenelli, Aldo M.},
  year = {2009},
  month = jul,
  volume = {699},
  pages = {1403--1417},
  issn = {0004-637X},
  doi = {10.1088/0004-637X/699/2/1403},
  abstract = {We present new results on the structure of the solar core, obtained with new sets of frequencies of solar low-degree p modes obtained from the BiSON network. We find that different methods used in extracting the different sets of frequencies cause shifts in frequencies, but the shifts are not large enough to affect solar structure results. We find that the BiSON frequencies show that the solar sound speed in the core is slightly larger than that inferred from data from Michelson Doppler Imager low-degree modes, and the uncertainties on the inversion results are smaller. Density results also change by a larger amount, and we find that solar models now tend to show smaller differences in density compared to the Sun. The result is seen at all radii, a result of the fact that conservation of mass implies that density differences in one region have to cancel out density differences in others, since our models are constructed to have the same mass as the Sun. The
uncertainties on the density results are much smaller too. We attribute the change in results to having more, and lower frequency, low-degree mode frequencies available. These modes provide greater sensitivity to conditions in the core.},
  file = {/Users/Oliver/Zotero/storage/Q7GKWCFQ/Basu et al. - 2009 - Fresh Insights on the Structure of the Solar Core.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Sun: abundances,Sun: helioseismology,Sun: interior}
}

@article{batalha+2011,
  title = {Kepler's {{First Rocky Planet}}: {{Kepler}}-10b},
  shorttitle = {Kepler's {{First Rocky Planet}}},
  author = {Batalha, Natalie M. and Borucki, William J. and Bryson, Stephen T. and Buchhave, Lars A. and Caldwell, Douglas A. and {Christensen-Dalsgaard}, J{\o}rgen and Ciardi, David and Dunham, Edward W. and Fressin, Francois and Gautier, Thomas N. and Gilliland, Ronald L. and Haas, Michael R. and Howell, Steve B. and Jenkins, Jon M. and Kjeldsen, Hans and Koch, David G. and Latham, David W. and Lissauer, Jack J. and Marcy, Geoffrey W. and Rowe, Jason F. and Sasselov, Dimitar D. and Seager, Sara and Steffen, Jason H. and Torres, Guillermo and Basri, Gibor S. and Brown, Timothy M. and Charbonneau, David and Christiansen, Jessie and Clarke, Bruce and Cochran, William D. and Dupree, Andrea and Fabrycky, Daniel C. and Fischer, Debra and Ford, Eric B. and Fortney, Jonathan and Girouard, Forrest R. and Holman, Matthew J. and Johnson, John and Isaacson, Howard and Klaus, Todd C. and Machalek, Pavel and Moorehead, Althea V. and Morehead, Robert C. and Ragozzine, Darin and Tenenbaum, Peter and Twicken, Joseph and Quinn, Samuel and VanCleve, Jeffrey and Walkowicz, Lucianne M. and Welsh, William F. and Devore, Edna and Gould, Alan},
  year = {2011},
  month = mar,
  volume = {729},
  pages = {27},
  doi = {10.1088/0004-637X/729/1/27},
  abstract = {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 {$\pm$} 4 ppm dimming lasting 1.811 {$\pm$} 0.024 hr with ephemeris T [BJD] =2454964.57375\textsuperscript{+0.00060} \textsubscript{-0.00082} + N*0.837495\textsuperscript{+0.000004} \textsubscript{-0.000005} days and (2) a 376 {$\pm$} 9 ppm dimming lasting 6.86 {$\pm$} 0.07 hr with ephemeris T [BJD] =2454971.6761\textsuperscript{+0.0020} \textsubscript{-0.0023} + N*45.29485\textsuperscript{+0.00065} \textsubscript{-0.00076} 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 \>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 {$\pm$} 4.5 Gyr) but otherwise Sun-like main-sequence star with T \textsubscript{eff} = 5627 {$\pm$} 44 K, M \textsubscript{sstarf} = 0.895 {$\pm$} 0.060 M \textsubscript{sun}, and R \textsubscript{sstarf} = 1.056 {$\pm$} 0.021 R \textsubscript{sun}. 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 \textsubscript{P} = 4.56\textsuperscript{+1.17} \textsubscript{-1.29} M \textsubscript{{$\oplus$}}, R \textsubscript{P} = 1.416\textsuperscript{+0.033} \textsubscript{-0.036} R \textsubscript{{$\oplus$}}, and {$\rho$}\textsubscript{P} = 8.8\textsuperscript{+2.1} \textsubscript{-2.9} g cm\textsuperscript{-3}. Kepler-10b is the smallest transiting exoplanet discovered to date. 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.},
  file = {/Users/Oliver/Zotero/storage/IABSN2MG/Batalha et al. - 2011 - Kepler's First Rocky Planet Kepler-10b.pdf;/Users/Oliver/Zotero/storage/9EH767P3/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{batalha2014,
  title = {Exploring Exoplanet Populations with {{NASA}}'s {{Kepler Mission}}},
  author = {Batalha, Natalie M.},
  year = {2014},
  month = sep,
  volume = {111},
  pages = {12647--12654},
  issn = {0027-8424},
  doi = {10.1073/pnas.1304196111},
  abstract = {The Kepler Mission is exploring the diversity of planets and planetary systems. Its legacy will be a catalog of discoveries sufficient for computing planet occurrence rates as a function of size, orbital period, star type, and insolation flux. The mission has made significant progress toward achieving that goal. Over 3,500 transiting exoplanets have been identified from the analysis of the first 3 y of data, 100 planets of which are in the habitable zone. The catalog has a high reliability rate (85\textendash 90\% averaged over the period/radius plane), which is improving as follow-up observations continue. Dynamical (e.g., velocimetry and transit timing) and statistical methods have confirmed and characterized hundreds of planets over a large range of sizes and compositions for both single- and multiple-star systems. Population studies suggest that planets abound in our galaxy and that small planets are particularly frequent. Here, I report on the progress Kepler has made measuring the prevalence of exoplanets orbiting within one astronomical unit of their host stars in support of the National Aeronautics and Space Administration's long-term goal of finding habitable environments beyond the solar system.},
  file = {/Users/Oliver/Zotero/storage/CDDCT9KG/Batalha - 2014 - Exploring exoplanet populations with NASA’s Kepler.pdf},
  journal = {Proceedings of the National Academy of Sciences of the United States of America},
  number = {35},
  pmcid = {PMC4156715},
  pmid = {25049406}
}

@article{bayes+price1763,
  title = {An {{Essay}} towards {{Solving}} a {{Problem}} in the {{Doctrine}} of {{Chances}}. {{By}} the {{Late Rev}}. {{Mr}}. {{Bayes}}, {{F}}. {{R}}. {{S}}. {{Communicated}} by {{Mr}}. {{Price}}, in a {{Letter}} to {{John Canton}}, {{A}}. {{M}}. {{F}}. {{R}}. {{S}}.},
  author = {Bayes, Mr. and Price, Mr.},
  year = {1763},
  volume = {53},
  pages = {370--418},
  abstract = {Not Available},
  journal = {Philosophical Transactions of the Royal Society of London Series I}
}

@article{beck+2011,
  title = {Fast Core Rotation in Red-Giant Stars Revealed by Gravity-Dominated Mixed Modes},
  author = {Beck, Paul G. and Montalban, Josefina and Kallinger, Thomas and De Ridder, Joris and Aerts, Conny and Garc{\'i}a, Rafael A. and Hekker, Saskia and Dupret, Marc-Antoine and Mosser, Benoit and Eggenberger, Patrick and Stello, Dennis and Elsworth, Yvonne and Frandsen, S{\o}ren and Carrier, Fabien and Hillen, Michel and Gruberbauer, Michael and {Christensen-Dalsgaard}, J{\o}rgen and Miglio, Andrea and Valentini, Marica and Bedding, Timothy R. and Kjeldsen, Hans and Girouard, Forrest R. and Hall, Jennifer R. and Ibrahim, Khadeejah A.},
  year = {2011},
  month = dec,
  volume = {481},
  pages = {55--57},
  issn = {0028-0836, 1476-4687},
  doi = {10.1038/nature10612},
  abstract = {When the core hydrogen is exhausted during stellar evolution, the central region of a star contracts and the outer envelope expands and cools, giving rise to a red giant, in which convection occupies a large fraction of the star. Conservation of angular momentum requires that the cores of these stars rotate faster than their envelopes, and indirect evidence supports this. Information about the angular momentum distribution is inaccessible to direct observations, but it can be extracted from the effect of rotation on oscillation modes that probe the stellar interior. Here, we report the detection of non-rigid rotation in the interiors of red-giant stars by exploiting the rotational frequency splitting of recently detected mixed modes. We demonstrate an increasing rotation rate from the surface of the star to the stellar core. Comparing with theoretical stellar models, we conclude that the core must rotate at least ten times faster than the surface. This observational result confirms the theoretical prediction of a steep gradient in the rotation profile towards the deep stellar interior.},
  archivePrefix = {arXiv},
  eprint = {1112.2825},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/8BNRI68V/Beck et al. - 2011 - Fast core rotation in red-giant stars revealed by .pdf;/Users/Oliver/Zotero/storage/8KUVS6W4/1112.html},
  journal = {Nature},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {7379}
}

@article{beck+2012,
  title = {Constraining the Core-Rotation Rate in Red-Giant Stars from {{Kepler}} Space Photometry},
  author = {Beck, P. G. and De Ridder, J. and Aerts, C. and Kallinger, T. and Hekker, S. and Garc{\'i}a, R. A. and Mosser, B. and Davies, G. R.},
  year = {2012},
  month = dec,
  volume = {333},
  pages = {967},
  doi = {10.1002/asna.201211787},
  abstract = {Rotation plays a key role in stellar structure and its evolution. Through transport processes which induce rotational mixing of chemical species and the redistribution of angular momentum, internal stellar rotation influences the evolutionary tracks in the Hertzsprung-Russell diagram. In turn, evolution influences the rotational properties. Therefore, information on the rotational properties of the deep interior would help to better understand the stellar evolution. However, as the internal rotational profile cannot be measured directly, it remains a major unknown leaving this important aspect of models unconstrained. We can test for nonrigid rotation inside the stars with asteroseismology. Through the effect of rotational splitting of non-radial oscillation modes, we investigate the internal rotation profile indirectly. Red giants have very slow rotation rates leading to a rotational splitting on the level of a few tenth of a \textbackslash muHz. Only from more than 1.5 years of consecutive data from the NASA Kepler space telescope, these tiny variations could be resolved. A qualitative comparison to theoretical models allowed constraining the core-to-surface rotation rate for some of these evolved stars. In this paper, we report on the first results of a large sample study of splitting of individual dipole modes.},
  file = {/Users/Oliver/Zotero/storage/JQ54BZLW/Beck et al. - 2012 - Constraining the core-rotation rate in red-giant s.pdf;/Users/Oliver/Zotero/storage/UZ93VN4K/ui.adsabs.harvard.edu.html},
  journal = {Astronomische Nachrichten},
  language = {en},
  number = {10}
}

@article{beck2000,
  title = {A Comparison of Differential Rotation Measurements - ({{Invited Review}})},
  author = {Beck, John G.},
  year = {2000},
  month = jan,
  volume = {191},
  pages = {47--70},
  issn = {0038-0938},
  doi = {10.1023/A:1005226402796},
  abstract = {Observers have long measured solar rotation with different techniques and obtained different results. This paper compares differential rotation measurements from four techniques: Doppler shift, Doppler feature tracking, magnetic feature tracking, and p-mode splittings. The different rotation rates measured by the first three techniques are interpreted as rotation rates of solar phenomena which depend on the properties and depth of that which is measured. This interpretation is supported by comparison with rotation measurements obtained from p-mode splittings except for Doppler features. The rotation rate of the plasma corresponds to the surface rate obtained by inversions; the rates of magnetic features correspond to the rotation rate at various depths within the convection zone. Supergranulation rotates at a rate greater than the maximum rotation rate within the convection zone, suggesting that supergranules are not simple convection cells anchored at a particular depth.},
  journal = {Solar Physics}
}

@phdthesis{beck2013,
  title = {Asteroseismology of Red-Giant Stars: Mixed Modes, Differential Rotation, and Eccentric Binaries},
  shorttitle = {Asteroseismology of Red-Giant Stars},
  author = {Beck, Paul Gerhard},
  year = {2013},
  file = {/Users/Oliver/Zotero/storage/AY8GGEA4/Beck - 2013 - Asteroseismology of red-giant stars mixed modes, .pdf},
  isbn = {9789086496778},
  language = {en}
}

@article{bedding+2010,
  title = {Solar-like {{Oscillations}} in {{Low}}-Luminosity {{Red Giants}}: {{First Results}} from {{Kepler}}},
  shorttitle = {Solar-like {{Oscillations}} in {{Low}}-Luminosity {{Red Giants}}},
  author = {Bedding, T. R. and Huber, D. and Stello, D. and Elsworth, Y. P. and Hekker, S. and Kallinger, T. and Mathur, S. and Mosser, B. and Preston, H. L. and Ballot, J. and Barban, C. and Broomhall, A. M. and Buzasi, D. L. and Chaplin, W. J. and Garc{\'i}a, R. A. and Gruberbauer, M. and Hale, S. J. and De Ridder, J. and Frandsen, S. and Borucki, W. J. and Brown, T. and {Christensen-Dalsgaard}, J. and Gilliland, R. L. and Jenkins, J. M. and Kjeldsen, H. and Koch, D. and Belkacem, K. and Bildsten, L. and Bruntt, H. and Campante, T. L. and Deheuvels, S. and Derekas, A. and Dupret, M.-A. and Goupil, M.-J. and Hatzes, A. and Houdek, G. and Ireland, M. J. and Jiang, C. and Karoff, C. and Kiss, L. L. and Lebreton, Y. and Miglio, A. and Montalb{\'a}n, J. and Noels, A. and Roxburgh, I. W. and Sangaralingam, V. and Stevens, I. R. and Suran, M. D. and Tarrant, N. J. and Weiss, A.},
  year = {2010},
  month = apr,
  volume = {713},
  pages = {L176-L181},
  issn = {0004-637X},
  doi = {10.1088/2041-8205/713/2/L176},
  abstract = {We have measured solar-like oscillations in red giants using time-series photometry from the first 34 days of science operations of the Kepler Mission. The light curves, obtained with 30 minute sampling, reveal clear oscillations in a large sample of G and K giants, extending in luminosity from the red clump down to the bottom of the giant branch. We confirm a strong correlation between the large separation of the oscillations ({$\Delta\nu$}) and the frequency of maximum power
({$\nu$}max). We focus on a sample of 50 low-luminosity stars ({$\nu$}max {$>$} 100 {$\mu$}Hz, L {$<\sptilde$} 30 L sun) having
high signal-to-noise ratios and showing the unambiguous signature of solar-like oscillations. These are H-shell-burning stars, whose
oscillations should be valuable for testing models of stellar evolution and for constraining the star formation rate in the local disk. We use a new technique to compare stars on a single \'echelle diagram by
scaling their frequencies and find well-defined ridges corresponding to radial and non-radial oscillations, including clear evidence for modes with angular degree l = 3. Measuring the small separation between l = 0 and l = 2 allows us to plot the so-called C-D diagram of
{$\delta\nu$}02 versus {$\Delta\nu$}. The small separation
{$\delta\nu$}01 of l = 1 from the midpoint of adjacent l = 0
modes is negative, contrary to the Sun and solar-type stars. The ridge for l = 1 is notably broadened, which we attribute to mixed modes, confirming theoretical predictions for low-luminosity giants. Overall, the results demonstrate the tremendous potential of Kepler data for asteroseismology of red giants.},
  file = {/Users/Oliver/Zotero/storage/GR2XLMZT/Bedding et al. - 2010 - Solar-like Oscillations in Low-luminosity Red Gian.pdf},
  journal = {The Astrophysical Journal Letters},
  keywords = {stars: oscillations}
}

@article{bedding+2011,
  title = {Gravity Modes as a Way to Distinguish between Hydrogen- and Helium-Burning Red Giant Stars},
  author = {Bedding, Timothy R. and Mosser, Benoit and Huber, Daniel and Montalb{\'a}n, Josefina and Beck, Paul and {Christensen-Dalsgaard}, J{\o}rgen and Elsworth, Yvonne P. and Garc{\'i}a, Rafael A. and Miglio, Andrea and Stello, Dennis and White, Timothy R. and De Ridder, Joris and Hekker, Saskia and Aerts, Conny and Barban, Caroline and Belkacem, Kevin and Broomhall, Anne-Marie and Brown, Timothy M. and Buzasi, Derek L. and Carrier, Fabien and Chaplin, William J. and Mauro, Di and Pia, Maria and Dupret, Marc-Antoine and Frandsen, S{\o}ren and Gilliland, Ronald L. and Goupil, Marie-Jo and Jenkins, Jon M. and Kallinger, Thomas and Kawaler, Steven and Kjeldsen, Hans and Mathur, Savita and Noels, Arlette and Silva Aguirre, Victor and Ventura, Paolo},
  year = {2011},
  month = mar,
  volume = {471},
  pages = {608},
  doi = {10.1038/nature09935},
  abstract = {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 \textasciitilde 50seconds) and those that are also burning helium (period spacing \textasciitilde 100 to 300 seconds).},
  file = {/Users/Oliver/Zotero/storage/JS4W9GJ4/Bedding et al. - 2011 - Gravity modes as a way to distinguish between hydr.pdf;/Users/Oliver/Zotero/storage/JDU7FXI2/ui.adsabs.harvard.edu.html},
  journal = {Nature},
  language = {en},
  number = {7340}
}

@article{belkacem+2011a,
  title = {The Underlying Physical Meaning of the {$N$}max - {$N$}c Relation},
  author = {Belkacem, K. and Goupil, M. J. and Dupret, M. A. and Samadi, R. and Baudin, F. and Noels, A. and Mosser, B.},
  year = {2011},
  month = jun,
  volume = {530},
  pages = {A142},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201116490},
  abstract = {Asteroseismology of stars that exhibit solar-like oscillations are enjoying a growing interest with the wealth of observational results obtained with the CoRoT and Kepler missions. In this framework, scaling laws between asteroseismic quantities and stellar parameters are becoming essential tools to study a rich variety of stars. However, the physical underlying mechanisms of those scaling laws are still poorly known. Our objective is to provide a theoretical basis for the scaling between the frequency of the maximum in the power spectrum
({$\nu$}max) of solar-like oscillations and the cut-off
frequency ({$\nu$}c). Using the SoHO GOLF observations together with theoretical considerations, we first confirm that the maximum of the height in oscillation power spectrum is determined by the so-called plateau of the damping rates. The physical origin of the plateau can be traced to the destabilizing effect of the Lagrangian perturbation of entropy in the upper-most layers, which becomes important when the modal period and the local thermal relaxation time-scale are comparable. Based on this analysis, we then find a linear relation between
{$\nu$}max and {$\nu$}c, with a coefficient that depends on the ratio of the Mach number of the exciting turbulence to the third power to the mixing-length parameter.},
  file = {/Users/Oliver/Zotero/storage/43UBBNBN/Belkacem et al. - 2011 - The underlying physical meaning of the νmax - νc r.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {convection,stars: interiors,stars: oscillations,turbulence}
}

@article{belkacem+2013,
  title = {On the {{Seismic Scaling Relations}} {$\increment\nu$} \textemdash{} {$\rho$} and {$N$}{\textsubscript{max}} \textemdash{} {$N$}{\textsubscript{c}}},
  author = {Belkacem, K. and Samadi, R. and Mosser, B. and Goupil, M.-J. and Ludwig, H.-G.},
  year = {2013},
  month = dec,
  volume = {479},
  pages = {61},
  abstract = {Scaling relations between asteroseismic quantities and stellar parameters are essential tools for studying stellar structure and evolution. We will address two of them, namely, the relation between the large frequency separation ({$\increment\nu$}) and the mean density ({$\rho$}) as well as the relation between the frequency of the maximum in the power spectrum of solar-like oscillations ({$\nu$}\textsubscript{max}) and the cut-off frequency ({$\nu$}\textsubscript{c}). For the first relation, we will consider the possible sources of uncertainties and explore them with the help of a grid of stellar models. For the second one, we will show that the basic physical picture is understood and that departure from the observed relation arises from the complexity of non-adiabatic processes involving the time-dependent treatment of convection. This will be further discussed on the basis of a set of three-dimensional (3D) hydrodynamical simulations of surface convection.},
  file = {/Users/Oliver/Zotero/storage/9KAXUP8Z/Belkacem et al. - 2013 - On the Seismic Scaling Relations ∆ν — ρ and νSUB.pdf;/Users/Oliver/Zotero/storage/XUUTQ3SJ/ui.adsabs.harvard.edu.html},
  journal = {Progress in Physics of the Sun and Stars: A New Era in Helio- and Asteroseismology},
  language = {en}
}

@article{bell2020,
  title = {Pyriod: {{Frequency Analysis Software}} for {{Python}}},
  shorttitle = {Pyriod},
  author = {Bell, K. J.},
  year = {2020},
  month = jan,
  volume = {235},
  pages = {106.06},
  abstract = {Pyriod provides similar functionality as the widely used Period04 software for the modern Python workflow, including a GUI for interactive analysis that works within Jupyter notebooks. All basic functionality is implemented, with more advanced features under development. Code and examples are available at github.com/keatonb/Pyriod/.},
  file = {/Users/Oliver/Zotero/storage/VZVH42SY/Bell - 2020 - Pyriod Frequency Analysis Software for Python.pdf}
}

@article{bellinger+2018,
  title = {Stellar Ages, Masses and Radii from Asteroseismic Modelling Are Robust to Systematic Errors in Spectroscopy},
  author = {Bellinger, Earl P. and Hekker, Saskia and Angelou, George C. and Stokholm, Amalie and Basu, Sarbani},
  year = {2018},
  month = dec,
  pages = {arXiv:1812.06979},
  abstract = {The search for twins of the Sun and Earth relies on accurate characterization of stellar and exoplanetary parameters: i.e., ages, masses, and radii. In the modern era of asteroseismology, parameters of solar-like stars are derived by fitting theoretical models to observational data, which include measurements of their oscillation frequencies, metallicity [Fe/H], and effective temperature Teff. Combining this information with transit data furthermore yields the corresponding parameters for their exoplanets. While [Fe/H] and Teff are commonly stated to a precision of \textasciitilde 0.1 dex and \textasciitilde 100 K, the impact of errors in their measurement has not been studied in practice within the context of the parameters derived from them. Here we use the Stellar Parameters in an Instant (SPI) pipeline to estimate the parameters of nearly 100 stars observed by Kepler and Gaia, many of which are confirmed planet hosts. We adjust the reported spectroscopic measurements of these stars by introducing faux systematic errors and artificially increasing the reported uncertainties, and quantify the differences in the resulting parameters. We find that a systematic error of 0.1 dex in [Fe/H] translates to differences of only 4\%, 2\%, and 1\% on average in the resulting stellar ages, masses, and radii, which are well within their uncertainties (\textasciitilde 11\%, 3.5\%, 1.4\%) as derived by SPI. We also find that increasing the uncertainty of [Fe/H] measurements by 0.1 dex increases the uncertainties by only 0.01 Gyr, 0.02 M\_sun, and 0.01 R\_sun, which are again well below their reported uncertainties (0.5 Gyr, 0.04 M\_sun, 0.02 R\_sun). The results for Teff at 100 K are similar. Stellar parameters from SPI are unchanged within uncertainties by errors of up to 0.14 dex or 175 K, and are even more robust to errors in Teff than the seismic scaling relations. Consequently, the parameters for their exoplanets are robust as well.},
  file = {/Users/Oliver/Zotero/storage/EFFPY5EV/Bellinger et al. - 2018 - Stellar ages, masses and radii from asteroseismic .pdf;/Users/Oliver/Zotero/storage/SJT4WRNG/ui.adsabs.harvard.edu.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{bellinger+2019,
  title = {Testing Stellar Evolution with Asteroseismic Inversions of a Main Sequence Star Harboring a Small Convective Core},
  author = {Bellinger, Earl P. and Basu, Sarbani and Hekker, Saskia and {Christensen-Dalsgaard}, J{\o}rgen},
  year = {2019},
  month = oct,
  abstract = {The goal of stellar evolution theory is to predict the structure of stars throughout their lifetimes. Usually, these predictions can be assessed only indirectly, for example by comparing predicted and observed effective temperatures and luminosities. Thanks now to asteroseismology, which can reveal the internal structure of stars, it becomes possible to compare the predictions from stellar evolution theory to actual stellar structures. In this work, we present an inverse analysis of the oscillation data from the solar-type star KIC 6225718, which was observed by the \textbackslash emph\{Kepler\} space observatory during its nominal mission. As its mass is about 20\% greater than solar, this star is predicted to transport energy by convection in its nuclear-burning core. We find significant differences between the predicted and actual structure of the star in the radiative interior near to the convective core. In particular, the predicted sound speed is higher than observed in the deep interior of the star, and too low at a fractional radius of 0.25 and beyond. The cause of these discrepancies is unknown, and is not remedied by known physics in the form of convective overshooting or elemental diffusion.},
  archivePrefix = {arXiv},
  eprint = {1910.00603},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/7NLJNDB2/Bellinger et al. - 2019 - Testing stellar evolution with asteroseismic inver.pdf;/Users/Oliver/Zotero/storage/UAXYNTIH/1910.html},
  journal = {arXiv:1910.00603 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{bellinger2019,
  title = {A Seismic Scaling Relation for Stellar Age},
  author = {Bellinger, Earl Patrick},
  year = {2019},
  month = mar,
  abstract = {A simple solar scaling relation for estimating the ages of main-sequence stars from asteroseismic and spectroscopic data is developed. New seismic scaling relations for estimating mass and radius are presented as well, including a purely seismic radius scaling relation (i.e., no dependence on temperature). The relations show substantial improvement over the classical scaling relations and perform similarly well to grid-based modeling.},
  archivePrefix = {arXiv},
  eprint = {1903.03110},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/H5D355IX/Bellinger - 2019 - A seismic scaling relation for stellar age.pdf;/Users/Oliver/Zotero/storage/M93FW76D/1903.html},
  journal = {arXiv:1903.03110 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{bellinger2020,
  title = {A Seismic Scaling Relation for Stellar Age {{II}}: {{The}} Red Giant Branch},
  shorttitle = {A Seismic Scaling Relation for Stellar Age {{II}}},
  author = {Bellinger, Earl Patrick},
  year = {2020},
  month = feb,
  volume = {492},
  pages = {L50-L55},
  issn = {1745-3925, 1745-3933},
  doi = {10.1093/mnrasl/slz178},
  abstract = {Owing to their simplicity and ease of application, seismic scaling relations are widely used to determine the properties of stars exhibiting solar-like oscillations, such as solar twins and red giants. So far, no seismic scaling relations for determining the ages of red giant stars have been developed. Such relations would be desirable for galactic archaeology, which uses stellar ages to map the history of the Milky Way. The ages of red giants must instead be estimated with reference to grids of theoretical stellar models, which can be computationally intensive. Here I present an exhaustive search for scaling age relations involving different combinations of observable quantities. The candidate scaling relations are calibrated and tested using more than 1,000 red giant stars whose ages were obtained via grid-based modeling. I report multiple high-quality scaling relations for red giant branch stars, the best of which are shown to be approximately as accurate as grid-based modeling with typical uncertainties of 15\%. Additionally, I present new scaling mass and radius relations for red giants as well.},
  archivePrefix = {arXiv},
  eprint = {1911.11804},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/8GF5TACT/Bellinger - 2020 - A seismic scaling relation for stellar age II The.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society: Letters},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Instrumentation and Methods for Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  language = {en},
  number = {1}
}

@article{benbakoura+2019,
  title = {Evolution of Star-Planet Systems under Magnetic Braking and Tidal Interaction},
  author = {Benbakoura, M. and R{\'e}ville, V. and Brun, A. S. and {Le Poncin-Lafitte}, C. and Mathis, S.},
  year = {2019},
  month = jan,
  volume = {621},
  pages = {A124},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201833314},
  abstract = {Context. With the discovery over the last two decades of a large diversity of exoplanetary systems, it is now of prime importance to
characterize star-planet interactions and how such systems evolve. Aims: We address this question by studying systems formed by a
solar-like star and a close-in planet. We focus on the stellar wind
spinning down the star along its main-sequence phase and tidal
interaction causing orbital evolution of the systems. Despite recent
significant advances in these fields, all current models use parametric
descriptions to study at least one of these effects. Our objective is to
introduce ab initio prescriptions of the tidal and braking torques
simultaneously, so as to improve our understanding of the underlying
physics. Methods: We develop a one-dimensional (1D) numerical
model of coplanar circular star-planet systems taking into account
stellar structural changes, wind braking, and tidal interaction and
implement it in a code called ESPEM. We follow the secular evolution of
the stellar rotation and of the semi-major axis of the orbit, assuming a
bilayer internal structure for the former. After comparing our
predictions to recent observations and models, we perform tests to
emphasize the contribution of ab initio prescriptions. Finally, we
isolate four significant characteristics of star-planet systems: stellar
mass, initial stellar rotation period, planetary mass and initial
semi-major axis; and browse the parameter space to investigate the
influence of each of them on the fate of the system. Results: Our
secular model of stellar wind braking accurately reproduces the recent
observations of stellar rotation in open clusters. Our results show that
a planet can affect the rotation of its host star and that the resulting
spin-up or spin-down depends on the orbital semi-major axis and on the
joint influence of magnetic and tidal effects. The ab initio
prescription for tidal dissipation that we used predicts fast outward
migration of massive planets orbiting fast-rotating young stars.
Finally, we provide the reader with a criterion based on the
characteristics of the system that allows us to assess whether or not
the planet will undergo orbital decay due to tidal interaction.},
  file = {/Users/Oliver/Zotero/storage/C2665766/Benbakoura et al. - 2019 - Evolution of star-planet systems under magnetic br.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {planet-star interactions,planetary systems,stars: evolution,stars: low-mass,stars: rotation,stars: solar-type}
}

@article{benomar+2015,
  title = {Nearly Uniform Internal Rotation of Solar-like Main-Sequence Stars Revealed by Space-Based Asteroseismology and Spectroscopic Measurements},
  author = {Benomar, O. and Takata, M. and Shibahashi, H. and Ceillier, T. and Garc{\'i}a, R. A.},
  year = {2015},
  month = sep,
  volume = {452},
  pages = {2654--2674},
  issn = {0035-8711},
  doi = {10.1093/mnras/stv1493},
  abstract = {The rotation rates in the deep interior and at the surface of 22
main-sequence stars with masses between 1.0 and 1.6 M{$\odot$}
are constrained by combining asteroseismological analysis with
spectroscopic measurements. The asteroseismic data of each star are
taken by the Kepler or CoRoT space mission. It is found that the
difference between the surface rotation rate and the average rotation
rate (excluding the convective core) of most of stars is small enough to
suggest that an efficient process of angular momentum transport operates
during and/or before the main-sequence stage of stars. If each of the
surface convective zone and the underlying radiative zone, for
individual stars, is assumed to rotate uniformly, the difference in the
rotation rate between the two zones turns out to be no more than a
factor of 2 in most of the stars independently of their ages.},
  file = {/Users/Oliver/Zotero/storage/CMECLF4Q/Benomar et al. - 2015 - Nearly uniform internal rotation of solar-like mai.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {asteroseismology,methods: data analysis,stars: interiors,stars: oscillations,stars: rotation,stars: solar-type}
}

@article{benomar+2018,
  title = {Asteroseismic Detection of Latitudinal Differential Rotation in 13 {{Sun}}-like Stars},
  author = {Benomar, O. and Bazot, M. and Nielsen, M. B. and Gizon, L. and Sekii, T. and Takata, M. and Hotta, H. and Hanasoge, S. and Sreenivasan, K. R. and {Christensen-Dalsgaard}, J.},
  year = {2018},
  month = sep,
  volume = {361},
  pages = {1231},
  doi = {10.1126/science.aao6571},
  abstract = {The differentially rotating outer layers of stars are thought to play a role in driving their magnetic activity, but the underlying mechanisms that generate and sustain differential rotation are poorly understood. We report the measurement using asteroseismology of latitudinal differential rotation in the convection zones of 40 Sun-like stars. For the most significant detections, the stars' equators rotate approximately twice as fast as their midlatitudes. The latitudinal shear inferred from asteroseismology is much larger than predictions from numerical simulations.},
  file = {/Users/Oliver/Zotero/storage/WRXNWH7K/ui.adsabs.harvard.edu.html},
  journal = {Science},
  keywords = {Seismic rotation},
  language = {en},
  number = {6408}
}

@article{bera+bhattacharya2017,
  title = {Mass-Radius Relation of Strongly Magnetized White Dwarfs},
  author = {Bera, Prasanta and Bhattacharya, Dipankar},
  year = {2017},
  month = oct,
  abstract = {We study the strongly magnetized white dwarf configurations in a self-consistent manner as a progenitor of the over-luminous type-Ia supernovae. We compute static equilibria of white dwarf stars containing a strong magnetic field and present the modification of white dwarf mass-radius relation caused by the magnetic field. From a static equilibrium study, we find that a maximum white dwarf mass of about 1.9 M\$\_\textbackslash odot\$ may be supported if the interior poloidal field is as strong as approximately \$10\^\{10\}\$ T. On the other hand if the field is purely toroidal the maximum mass can be more than 5 M\$\_\textbackslash odot\$. All these modifications are mainly from the presence of Lorenz force. The effects of i) modification of equation of state due to Landau quantization, ii) electrostatic interaction due to ions, iii) general relativistic calculation on the stellar structure and, iv) field geometry are also considered. These strongly magnetised configurations are sensitive to magnetic instabilities where the perturbations grow at the corresponding Alfven time scales.},
  archivePrefix = {arXiv},
  eprint = {1710.08689},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/IHQVN72N/Bera and Bhattacharya - 2017 - Mass-radius relation of strongly magnetized white .pdf;/Users/Oliver/Zotero/storage/HGSTZRHF/1710.html},
  journal = {arXiv:1710.08689 [astro-ph]},
  keywords = {Astrophysics - High Energy Astrophysical Phenomena,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{berger+2020,
  title = {The \${{Gaia}}\$-\${{Kepler}}\$ {{Stellar Properties Catalog I}}: {{Homogeneous Fundamental Properties}} for 186,000 \${{Kepler}}\$ {{Stars}}},
  shorttitle = {The \${{Gaia}}\$-\${{Kepler}}\$ {{Stellar Properties Catalog I}}},
  author = {Berger, Travis A. and Huber, Daniel and {van Saders}, Jennifer L. and Gaidos, Eric and Tayar, Jamie and Kraus, Adam L.},
  year = {2020},
  month = jan,
  abstract = {An accurate and precise \$Kepler\$ Stellar Properties Catalog is essential for the interpretation of the \$Kepler\$ exoplanet survey results. Previous \$Kepler\$ Stellar Properties Catalogs have focused on reporting the best-available parameters for each star, but this has required combining data from a variety of heterogeneous sources. We present the \$Gaia\$-\$Kepler\$ Stellar Properties Catalog, a set of stellar properties of 186,301 \$Kepler\$ stars, homogeneously derived from isochrones and broadband photometry, \$Gaia\$ Data Release 2 parallaxes, and spectroscopic metallicities, where available. Our photometric effective temperatures, derived from \$g-K\_s\$ colors, are calibrated on stars with interferometric angular diameters. Median catalog uncertainties are 112 K for \$T\_\{\textbackslash mathrm\{eff\}\}\$, 0.05 dex for \$\textbackslash log g\$, 4\% for \$R\_\textbackslash star\$, 7\% for \$M\_\textbackslash star\$, 13\% for \$\textbackslash rho\_\textbackslash star\$, 10\% for \$L\_\textbackslash star\$, and 56\% for stellar age. These precise constraints on stellar properties for this sample of stars will allow unprecedented investigations into trends in stellar and exoplanet properties as a function of stellar mass and age. In addition, our homogeneous parameter determinations will permit more accurate calculations of planet occurrence and trends with stellar properties.},
  archivePrefix = {arXiv},
  eprint = {2001.07737},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/VIU8WYV2/Berger et al. - 2020 - The $Gaia$-$Kepler$ Stellar Properties Catalog I .pdf;/Users/Oliver/Zotero/storage/VHAMZF5I/2001.html},
  journal = {arXiv:2001.07737 [astro-ph]},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{bessell+2011,
  title = {{{SkyMapper Filter Set}}: {{Design}} and {{Fabrication}} of {{Large}}-{{Scale Optical Filters}}},
  shorttitle = {{{SkyMapper Filter Set}}},
  author = {Bessell, Michael and Bloxham, Gabe and Schmidt, Brian and Keller, Stefan and Tisserand, Patrick and Francis, Paul},
  year = {2011},
  volume = {123},
  pages = {789},
  file = {/Users/Oliver/Zotero/storage/DNTH25GY/pdf.pdf},
  journal = {Publications of the Astronomical Society of the Pacific},
  number = {905}
}

@article{betancourt+girolami2013,
  title = {Hamiltonian {{Monte Carlo}} for {{Hierarchical Models}}},
  author = {Betancourt, M. J. and Girolami, Mark},
  year = {2013},
  month = dec,
  abstract = {Hierarchical modeling provides a framework for modeling the complex interactions typical of problems in applied statistics. By capturing these relationships, however, hierarchical models also introduce distinctive pathologies that quickly limit the efficiency of most common methods of in- ference. In this paper we explore the use of Hamiltonian Monte Carlo for hierarchical models and demonstrate how the algorithm can overcome those pathologies in practical applications.},
  archivePrefix = {arXiv},
  eprint = {1312.0906},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/Y2V8MZ3B/Betancourt and Girolami - 2013 - Hamiltonian Monte Carlo for Hierarchical Models.pdf;/Users/Oliver/Zotero/storage/EBICQZM2/1312.html},
  journal = {arXiv:1312.0906 [stat]},
  keywords = {Statistics - Methodology},
  primaryClass = {stat}
}

@article{bilir+2008,
  title = {Transformations between {{2MASS}}, {{SDSS}} and {{BVRI}} Photometric Systems: Bridging the near-Infrared and Optical},
  shorttitle = {Transformations between {{2MASS}}, {{SDSS}} and {{BVRI}} Photometric Systems},
  author = {Bilir, S. and Ak, S. and Karaali, S. and {Cabrera-Lavers}, A. and Chonis, T. S. and Gaskell, C. M.},
  year = {2008},
  month = mar,
  volume = {384},
  pages = {1178--1188},
  issn = {0035-8711},
  doi = {10.1111/j.1365-2966.2007.12783.x},
  abstract = {We present colour transformations for the conversion of the Two Micron
All Sky Survey (2MASS) photometric system to the Johnson-Cousins UBVRI
system and further into the Sloan Digital Sky Survey (SDSS) ugriz
system. We have taken SDSS gri magnitudes of stars measured with the
2.5-m telescope from SDSS Data Release 5 (DR5), and BVRI and
JHKs magnitudes from Stetson's catalogue and Cutri et al.,
respectively. We matched thousands of stars in the three photometric
systems by their coordinates and obtained a homogeneous sample of 825
stars by the following constraints, which are not used in previous
transformations: (1) the data are dereddened, (2) giants are omitted and
(3) the sample stars selected are of the highest quality. We give
metallicity, population type and transformations dependent on two
colours. The transformations provide absolute magnitude and distance
determinations which can be used in space density evaluations at short
distances where some or all of the SDSS ugriz magnitudes are saturated.
The combination of these densities with those evaluated at larger
distances using SDSS ugriz photometry will supply accurate Galactic
model parameters, particularly the local space densities for each
population.},
  file = {/Users/Oliver/Zotero/storage/2GK4QBZA/Bilir et al. - 2008 - Transformations between 2MASS, SDSS and BVRI photo.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {catalgues: surveys,techniques: photometric}
}

@article{bonanno+frohlich2015,
  title = {A {{Bayesian}} Estimation of the Helioseismic Solar Age},
  author = {Bonanno, A. and Fr{\"o}hlich, H.-E.},
  year = {2015},
  month = aug,
  volume = {580},
  pages = {A130},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201526419},
  abstract = {Context. The helioseismic determination of the solar age has been a subject of several studies because it provides us with an independent estimation of the age of the solar system. Aims: We present the Bayesian estimates of the helioseismic age of the Sun, which are determined by means of calibrated solar models that employ different equations of state and nuclear reaction rates. Methods: We use 17 frequency separation ratios r02(n) = ({$\nu$}n,l =
0-{$\nu$}n-1,l = 2)/({$\nu$}n,l = 1-{$\nu$}n-1,l
= 1) from 8640 days of low-{$\mathscr{l}$}BiSON frequencies and consider three likelihood functions that depend on the handling of the errors of these r02(n) ratios. Moreover, we employ the 2010 CODATA recommended values for Newton's constant, solar mass, and radius to calibrate a large grid of solar models spanning a conceivable range of solar ages. Results: It is shown that the most constrained posterior distribution of the solar age for models employing Irwin EOS with NACRE reaction rates leads to t{$\odot$} = 4.587 {$\pm$}
0.007 Gyr, while models employing the Irwin EOS and Adelberger, et al. (2011, Rev. Mod. Phys., 83, 195) reaction rate have t{$\odot$} = 4.569 {$\pm$} 0.006 Gyr. Implementing OPAL EOS in the solar models
results in reduced evidence ratios (Bayes factors) and leads to an age that is not consistent with the meteoritic dating of the solar system. Conclusions: An estimate of the solar age that relies on an helioseismic age indicator such as r02(n) turns out to be essentially independent of the type of likelihood function. However, with respect to model selection, abandoning any information concerning the errors of the r02(n) ratios leads to inconclusive results, and this stresses the importance of evaluating the
trustworthiness of error estimates.},
  file = {/Users/Oliver/Zotero/storage/4I4RWXWU/Bonanno and Fröhlich - 2015 - A Bayesian estimation of the helioseismic solar ag.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {abundances,equation of state,methods: statistical,nuclear reactions,nucleosynthesis,Sun: helioseismology,Sun: interior,Sun: oscillations}
}

@article{bonanno2016,
  title = {Stellar Dynamo Models with Prominent Surface Toroidal Fields},
  author = {Bonanno, Alfio},
  year = {2016},
  month = dec,
  volume = {833},
  pages = {L22},
  issn = {2041-8213},
  doi = {10.3847/2041-8213/833/2/L22},
  abstract = {Recent spectro-polarimetric observations of solar-type stars have shown the presence of photospheric magnetic fields with a predominant toroidal component. If the external field is assumed to be current-free it is impossible to explain these observations within the framework of standard mean-field dynamo theory. In this work it will be shown that if the coronal field of these stars is assumed to be harmonic, the underlying stellar dynamo mechanism can support photospheric magnetic fields with a prominent toroidal component even in the presence of axisymmetric magnetic topologies. In particular it is argued that the observed increase in the toroidal energy in low mass fast rotating stars can be naturally explained with an underlying \$\textbackslash alpha\textbackslash Omega\$ mechanism.},
  archivePrefix = {arXiv},
  eprint = {1612.00253},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/AP444G7J/Bonanno - 2016 - Stellar dynamo models with prominent surface toroi.pdf;/Users/Oliver/Zotero/storage/U98ZFI8A/1612.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {2}
}

@inproceedings{borucki+2009,
  title = {{{KEPLER}}: {{Search}} for {{Earth}}-{{Size Planets}} in the {{Habitable Zone}}},
  shorttitle = {{{KEPLER}}},
  booktitle = {Transiting {{Planets}}},
  author = {Borucki, William and Koch, David and Batalha, Natalie and Caldwell, Douglas and {Christensen-Dalsgaard}, Jorgen and Cochran, William D. and Dunham, Edward and Gautier, Thomas N. and Geary, John and Gilliland, Ronald and Jenkins, Jon and Kjeldsen, Hans and Lissauer, Jack J. and Rowe, Jason},
  year = {2009},
  month = feb,
  volume = {253},
  pages = {289--299},
  doi = {10.1017/S1743921308026513},
  abstract = {The Kepler Mission is a space-based mission whose primary goal is to determine the frequency of Earth-size and larger planets in the
habitable zone of solar-like stars. The mission will monitor more than 100,000 stars for patterns of 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.

This paper provides a short overview of the mission, a brief history of the mission development, expected results, new investigations by the recently chosen Participating Scientists, and the plans for the Guest Observer and Astrophysical Data Programs.},
  file = {/Users/Oliver/Zotero/storage/3VVCVTV3/Borucki et al. - 2009 - KEPLER Search for Earth-Size Planets in the Habit.pdf},
  keywords = {C1}
}

@article{borucki+2010,
  title = {Kepler {{Planet Detection Mission}}: {{Highlights}} of the {{First Results}}},
  shorttitle = {Kepler {{Planet Detection Mission}}},
  author = {Borucki, William J. and Koch, D. and Team, Kepler Science},
  year = {2010},
  month = oct,
  volume = {42},
  pages = {47.03},
  abstract = {An important step in discovering the extent of life in our galaxy is to determine the number of terrestrial planets in the habitable zone (HZ) of solar-like stars. The Kepler Mission is designed specifically to determine the frequency of terrestrial planets in the HZ. It was launched on March 6, 2009 and is now measuring the brightness variations of 150,000 solar-like stars to detect patterns of transits that provide the size of the planet relative to the star and its orbital period. Combining these measurements with ground-based spectroscopy fixes the stellar parameters, the planet radius, orbital semi-major axis, and the location relative to the HZ. The first six weeks of data show the presence of hundreds of candidate planets, and thousands of eclipsing binary stars, and variable stars of amazing variety. Discoveries of five new exoplanets are shown and compared with known exoplanets with respect to mass, size, density, and orbital period. Over 750 planetary candidates found in the first year of data; with many smaller than Neptune.. The released data 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. Data for these discoveries were released in June. Examples of many of these discoveries and their distributions are presented and discussed. . Support by the NASA Astrophysics Division is gratefully acknowledged.},
  file = {/Users/Oliver/Zotero/storage/I3HFWADJ/ui.adsabs.harvard.edu.html},
  journal = {AAS/Division for Planetary Sciences Meeting Abstracts \#42},
  language = {en}
}

@article{bourrier+2017,
  title = {Reconnaissance of the {{TRAPPIST}}-1 Exoplanet System in the {{Lyman}}-\$\textbackslash alpha\$ Line},
  author = {Bourrier, V. and Ehrenreich, D. and Wheatley, P. J. and Bolmont, E. and Gillon, M. and {de Wit}, J. and Burgasser, A. J. and Jehin, E. and Queloz, D. and Triaud, A. H. M. J.},
  year = {2017},
  month = mar,
  volume = {599},
  pages = {L3},
  issn = {0004-6361, 1432-0746},
  doi = {10.1051/0004-6361/201630238},
  abstract = {The TRAPPIST-1 system offers the opportunity to characterize terrestrial, potentially habitable planets orbiting a nearby ultracool dwarf star. We performed a four-orbit reconnaissance with the Space Telescope Imaging Spectrograph onboard the Hubble Space Telescope to study the stellar emission at Lyman-\$\textbackslash alpha\$, to assess the presence of hydrogen exospheres around the two inner planets, and to determine their UV irradiation. We detect the Lyman-\$\textbackslash alpha\$ line of TRAPPIST-1, making it the coldest exoplanet host star for which this line has been measured. We reconstruct the intrinsic line profile, showing that it lacks broad wings and is much fainter than expected from the stellar X-ray emission. TRAPPIST-1 has a similar X-ray emission as Proxima Cen but a much lower Ly-\$\textbackslash alpha\$ emission. This suggests that TRAPPIST-1 chromosphere is only moderately active compared to its transition region and corona. We estimated the atmospheric mass loss rates for all planets, and found that despite a moderate extreme UV emission the total XUV irradiation could be strong enough to strip the atmospheres of the inner planets in a few billions years. We detect marginal flux decreases at the times of TRAPPIST-1b and c transits, which might originate from stellar activity, but could also hint at the presence of extended hydrogen exospheres. Understanding the origin of these Lyman-\$\textbackslash alpha\$ variations will be crucial in assessing the atmospheric stability and potential habitability of the TRAPPIST-1 planets.},
  archivePrefix = {arXiv},
  eprint = {1702.07004},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/89GEISZ3/Bourrier et al. - 2017 - Reconnaissance of the TRAPPIST-1 exoplanet system .pdf;/Users/Oliver/Zotero/storage/3RMD6CFV/1702.html},
  journal = {Astronomy \& Astrophysics},
  keywords = {Astrophysics - Earth and Planetary Astrophysics}
}

@article{boutle+2017,
  title = {Exploring the Climate of {{Proxima B}} with the {{Met Office Unified Model}}},
  author = {Boutle, Ian A. and Mayne, Nathan J. and Drummond, Benjamin and Manners, James and Goyal, Jayesh and Lambert, F. Hugo and Acreman, David M. and Earnshaw, Paul D.},
  year = {2017},
  month = feb,
  abstract = {We present results of simulations of the climate of the newly discovered planet Proxima Centauri B, performed using the Met Office Unified Model (UM). We examine the responses of both an `Earth-like' atmosphere and simplified nitrogen and trace carbon dioxide atmosphere to the radiation likely received by Proxima Centauri B. Additionally, we explore the effects of orbital eccentricity on the planetary conditions using a range of eccentricities guided by the observational constraints. Overall, our results are in agreement with previous studies in suggesting Proxima Centauri B may well have surface temperatures conducive to the presence of liquid water. Moreover, we have expanded the parameter regime over which the planet may support liquid water to higher values of eccentricity ({$>$}= 0.1) and lower incident fluxes (881.7 Wm-2) than previous work. This increased parameter space arises because of the low sensitivity of the planet to changes in stellar flux, a consequence of the stellar spectrum and orbital configuration. However, we also find interesting differences from previous simulations, such as cooler mean surface temperatures for the tidally-locked case. Finally, we have produced high resolution planetary emission and reflectance spectra, and highlight signatures of gases vital to the evolution of complex life on Earth (oxygen, ozone and carbon dioxide).},
  archivePrefix = {arXiv},
  eprint = {1702.08463},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/7EWAWVTM/Boutle et al. - 2017 - Exploring the climate of Proxima B with the Met Of.pdf;/Users/Oliver/Zotero/storage/SFK3I6GP/1702.html},
  journal = {arXiv:1702.08463 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics},
  primaryClass = {astro-ph}
}

@article{bovy+2014,
  title = {The {{APOGEE Red}}-Clump {{Catalog}}: {{Precise Distances}}, {{Velocities}}, and {{High}}-Resolution {{Elemental Abundances}} over a {{Large Area}} of the {{Milky Way}}'s {{Disk}}},
  shorttitle = {The {{APOGEE Red}}-Clump {{Catalog}}},
  author = {Bovy, Jo and Nidever, David L. and Rix, Hans-Walter and Girardi, L{\'e}o and Zasowski, Gail and Chojnowski, S. Drew and Holtzman, Jon and Epstein, Courtney and Frinchaboy, Peter M. and Hayden, Michael R. and Rodrigues, Tha{\'i}se S. and Majewski, Steven R. and Johnson, Jennifer A. and Pinsonneault, Marc H. and Stello, Dennis and Allende Prieto, Carlos and Andrews, Brett and Basu, Sarbani and Beers, Timothy C. and Bizyaev, Dmitry and Burton, Adam and Chaplin, William J. and Cunha, Katia and Elsworth, Yvonne and Garc{\'i}a, Rafael A. and {Garc{\'i}a-Her{\'n}andez}, Domingo A. and Garc{\'i}a P{\'e}rez, Ana E. and Hearty, Fred R. and Hekker, Saskia and Kallinger, Thomas and Kinemuchi, Karen and Koesterke, Lars and M{\'e}sz{\'a}ros, Szabolcs and Mosser, Beno{\^i}t and O'Connell, Robert W. and Oravetz, Daniel and Pan, Kaike and Robin, Annie C. and Schiavon, Ricardo P. and Schneider, Donald P. and Schultheis, Mathias and Serenelli, Aldo and Shetrone, Matthew and Silva Aguirre, Victor and Simmons, Audrey and Skrutskie, Michael and Smith, Verne V. and Stassun, Keivan and Weinberg, David H. and Wilson, John C. and Zamora, Olga},
  year = {2014},
  month = aug,
  volume = {790},
  pages = {127},
  issn = {0004-637X},
  doi = {10.1088/0004-637X/790/2/127},
  abstract = {The Sloan Digital Sky Survey III's Apache Point Observatory Galactic
Evolution Experiment (APOGEE) is a high-resolution near-infrared
spectroscopic survey covering all of the major components of the Galaxy,
including the dust-obscured regions of the inner Milky Way disk and
bulge. Here we present a sample of 10,341 likely red-clump stars (RC)
from the first two years of APOGEE operations, selected based on their
position in color-metallicity-surface-gravity-effective-temperature
space using a new method calibrated using stellar evolution models and
high-quality asteroseismology data. The narrowness of the RC locus in
color-metallicity-luminosity space allows us to assign distances to the
stars with an accuracy of 5\%-10\%. The sample extends to typical
distances of about 3 kpc from the Sun, with some stars out to 8 kpc, and
spans a volume of approximately 100 kpc3 over 5 kpc {$<\sptilde$} R
{$<\sptilde$} 14 kpc, |Z| {$<\sptilde$} 2 kpc, and -15\textdegree{} {$<\sptilde$} Galactocentric
azimuth {$<\sptilde$} 30\textdegree. The APOGEE red-clump (APOGEE-RC) catalog contains
photometry from the Two Micron All Sky Survey, reddening estimates,
distances, line-of-sight velocities, stellar parameters and elemental
abundances determined from the high-resolution APOGEE spectra, and
matches to major proper motion catalogs. We determine the survey
selection function for this data set and discuss how the RC selection
samples the underlying stellar populations. We use this sample to limit
any azimuthal variations in the median metallicity within the
{$\approx$}45\textdegree{} azimuthal region covered by the current sample to be
{$<$}=0.02 dex, which is more than an order of magnitude smaller than the
radial metallicity gradient. This result constrains coherent
non-axisymmetric flows within a few kiloparsecs from the Sun.},
  file = {/Users/Oliver/Zotero/storage/VP86VZXZ/Bovy et al. - 2014 - The APOGEE Red-clump Catalog Precise Distances, V.pdf},
  journal = {The Astrophysical Journal},
  keywords = {C4}
}

@article{bressan+2012,
  title = {{{PARSEC}}: Stellar Tracks and Isochrones with the {{PAdova}} and {{TRieste Stellar Evolution Code}}},
  shorttitle = {{{PARSEC}}},
  author = {Bressan, Alessandro and Marigo, Paola and Girardi, L{\'e}o and Salasnich, Bernardo and Dal Cero, Claudia and Rubele, Stefano and Nanni, Ambra},
  year = {2012},
  month = nov,
  volume = {427},
  pages = {127},
  doi = {10.1111/j.1365-2966.2012.21948.x},
  abstract = {We present the updated version of the code used to compute stellar evolutionary tracks in Padova. It is the result of a thorough revision of the major input physics, together with the inclusion of the pre-main sequence phase, not present in our previous releases of stellar models. Another innovative aspect is the possibility of promptly generating accurate opacity tables fully consistent with any selected initial chemical composition, by coupling the Opacity Project At Livermore (OPAL) data at high temperatures to the molecular opacities computed with our \ae SOPUS code. In this work, we present extended sets of stellar evolutionary models for various initial chemical compositions, while other sets with different metallicities and/or different distributions of heavy elements are being computed. For the present release of models, we adopt the solar distribution of heavy elements from the recent revision by Caffau et al., corresponding to a Sun's metallicity Z {$\simeq$} 0.0152. From all computed sets of stellar tracks, we also derive isochrones in several photometric systems. The aim is to provide the community with the basic tools to model star clusters and galaxies by means of population synthesis techniques.},
  file = {/Users/Oliver/Zotero/storage/PFZEJ97R/Bressan et al. - 2012 - PARSEC stellar tracks and isochrones with the PAd.pdf;/Users/Oliver/Zotero/storage/9T7VTFJI/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@article{brewer+2015,
  title = {Accurate {{Gravities}} of {{F}}, {{G}}, and {{K}} Stars from {{High Resolution Spectra Without External Constraints}}},
  author = {Brewer, John M. and Fischer, Debra A. and Basu, Sarbani and Valenti, Jeff A. and Piskunov, Nikolai},
  year = {2015},
  month = jun,
  volume = {805},
  pages = {126},
  doi = {10.1088/0004-637X/805/2/126},
  abstract = {We demonstrate a new procedure to derive accurate and precise surface gravities from high resolution spectra without the use of external constraints. Our analysis utilizes Spectroscopy Made Easy with robust spectral line constraints and uses an iterative process to mitigate degeneracies in the fitting process. We adopt an updated radiative transfer code, a new treatment for neutral perturber broadening, a line list with multiple gravity constraints and separate fitting for global stellar properties and abundance determinations. To investigate the sources of temperature dependent trends in determining log \{\textbackslash mkern 1mu\} g noted in previous studies, we obtained Keck HIRES spectra of 42 Kepler asteroseismic stars. In comparison to asteroseismically determined log \{\textbackslash mkern 1mu\} g our spectroscopic analysis has a constant offset of 0.01 dex with a rms scatter of 0.05 dex. We also analyzed 30 spectra which had published surface gravities determined using the a/\{\{R\}\vphantom\}\textsubscript{*}\vphantom\{\} technique from planetary transits and found a constant offset of 0.06 dex and rms scatter of 0.07 dex. The two samples covered effective temperatures between 5000 and 6700 K with log \{\textbackslash mkern 1mu\} g between 3.7 and 4.6.},
  file = {/Users/Oliver/Zotero/storage/TX5RFNIE/Brewer et al. - 2015 - Accurate Gravities of F, G, and K stars from High .pdf;/Users/Oliver/Zotero/storage/47LT5KN2/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{brogaard+2016,
  title = {Testing Asteroseismic Scaling Relations Using Eclipsing Binaries in Star Clusters and the Field},
  author = {Brogaard, K. and Jessen-Hansen, J. and Handberg, R. and Arentoft, T. and Frandsen, S. and Grundahl, F. and Bruntt, H. and Sandquist, E. L. and Miglio, A. and Beck, P. G. and Thygesen, A. O. and Kj{\ae}rgaard, K. L. and Haugaard, N. A.},
  year = {2016},
  volume = {337},
  pages = {793--798},
  issn = {1521-3994},
  doi = {10.1002/asna.201612374},
  abstract = {The accuracy of stellar masses and radii determined from asteroseismology is not known! We examine this issue for giant stars by comparing classical measurements of detached eclipsing binary systems (dEBs) with asteroseismic measurements from the Kepler mission. For star clusters, we extrapolate measurements of dEBs in the turn-off region to the red giant branch and the red clump where we investigate the giants as an ensemble. For the field stars, we measure dEBs with an oscillating giant component. These measurements allow a comparison of masses and radii calculated from a classical eclipsing binary analysis to those calculated from asteroseismic scaling relations and/or other asteroseismic methods. Our first results indicate small but significant systematic differences between the classical and asteroseismic measurements. In this contribution we show our latest results and summarize the current status and future plans. We also stress the importance of realizing that for giant stars mass cannot always be translated to age, since an unknown fraction of these evolved through a blue straggler phase with mass transfer in a binary system. Rough estimates of how many such stars to expect are given based on our findings in the open clusters NGC 6819 and NGC 6791.},
  file = {/Users/Oliver/Zotero/storage/U66DPI7R/Brogaard et al. - 2016 - Testing asteroseismic scaling relations using ecli.pdf;/Users/Oliver/Zotero/storage/6YTSTKGD/asna.html},
  journal = {Astronomische Nachrichten},
  keywords = {asteroseismology,binaries: eclipsing,NGC 6819),open clusters and associations: general,open clusters and associations: individual (NGC 6791,stars: fundamental parameters,stars: oscillations},
  language = {en},
  number = {8-9}
}

@article{brogaard+2017,
  title = {The Age of 47 {{Tuc}} from Self-Consistent Isochrone Fits to Colour-Magnitude Diagrams and the Eclipsing Member {{V69}}},
  author = {Brogaard, K. and VandenBerg, D. A. and Bedin, L. R. and Milone, A. P. and Thygesen, A. and Grundahl, F.},
  year = {2017},
  month = jun,
  volume = {468},
  pages = {645},
  doi = {10.1093/mnras/stx378},
  abstract = {Our aim is to derive a self-consistent age, distance and composition for the globular cluster 47 Tucanae (47 Tuc; NGC104). First, we re-evaluate the reddening towards the cluster resulting in a nominal E(B - V) = 0.03 {$\pm$} 0.01 as the best estimate. The T\textsubscript{eff} of the components of the eclipsing binary member V69 is found to be 5900 {$\pm$} 72 K from both photometric and spectroscopic evidence. This yields a true distance modulus (m - M)\textsubscript{0} = 13.21 {$\pm$} 0.06(random) {$\pm$}0.03(systematic) to 47 Tuc when combined with existing measurements of V69 radii and luminosity ratio. We then present a new completely self-consistent isochrone fitting method to ground-based and Hubble Space Telescope cluster colour-magnitude diagrams and the eclipsing binary member V69. The analysis suggests that the composition of V69, and by extension one of the populations of 47 Tuc, is given by [Fe/H]{\~ } -0.70, [O/Fe]{\~ } +0.60 and Y{\~ } 0.250 on the solar abundance scale of Asplund, Grevesse \& Sauval. However, this depends on the accuracy of the model T\textsubscript{eff} scale that is 50-75 K cooler than our best estimate but within measurement uncertainties. Our best estimate of the age of 47 Tuc is 11.8 Gyr, with firm (3{$\sigma$}) lower and upper limits of 10.4 and 13.4 Gyr, respectively, in satisfactory agreement with the age derived from the white dwarf cooling sequence if our determination of the distance modulus is adopted.},
  file = {/Users/Oliver/Zotero/storage/SI3LIPNY/Brogaard et al. - 2017 - The age of 47 Tuc from self-consistent isochrone f.pdf;/Users/Oliver/Zotero/storage/F99ZTW6F/abstract.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en}
}

@article{brogaard+2018,
  title = {Establishing the Accuracy of Asteroseismic Mass and Radius Estimates of Giant Stars - {{I}}. {{Three}} Eclipsing Systems at [{{Fe}}/{{H}}]{\~ } -0.3 and the Need for a Large High-Precision Sample},
  author = {Brogaard, K. and Hansen, C. J. and Miglio, A. and Slumstrup, D. and Frandsen, S. and {Jessen-Hansen}, J. and Lund, M. N. and Bossini, D. and Thygesen, A. and Davies, G. R. and Chaplin, W. J. and Arentoft, T. and Bruntt, H. and Grundahl, F. and Handberg, R.},
  year = {2018},
  month = may,
  volume = {476},
  pages = {3729},
  doi = {10.1093/mnras/sty268},
  abstract = {We aim to establish and improve the accuracy level of asteroseismic estimates of mass, radius, and age of giant stars. This can be achieved by measuring independent, accurate, and precise masses, radii, effective temperatures and metallicities of long period eclipsing binary stars with a red giant component that displays solar-like oscillations. We measured precise properties of the three eclipsing binary systems KIC 7037405, KIC 9540226, and KIC 9970396 and estimated their ages be 5.3 {$\pm$} 0.5, 3.1 {$\pm$} 0.6, and 4.8 {$\pm$} 0.5 Gyr. The measurements of the giant stars were compared to corresponding measurements of mass, radius, and age using asteroseismic scaling relations and grid modelling. We found that asteroseismic scaling relations without corrections to {$\increment\nu$} systematically overestimate the masses of the three red giants by 11.7 per cent, 13.7 per cent, and 18.9 per cent, respectively. However, by applying theoretical correction factors f\textsubscript{{$\increment\nu$}} according to Rodrigues et al. (2017), we reached general agreement between dynamical and asteroseismic mass estimates, and no indications of systematic differences at the precision level of the asteroseismic measurements. The larger sample investigated by Gaulme et al. (2016) showed a much more complicated situation, where some stars show agreement between the dynamical and corrected asteroseismic measures while others suggest significant overestimates of the asteroseismic measures. We found no simple explanation for this, but indications of several potential problems, some theoretical, others observational. Therefore, an extension of the present precision study to a larger sample of eclipsing systems is crucial for establishing and improving the accuracy of asteroseismology of giant stars.},
  file = {/Users/Oliver/Zotero/storage/CBP6GU7Z/Brogaard et al. - 2018 - Establishing the accuracy of asteroseismic mass an.pdf;/Users/Oliver/Zotero/storage/9DUI2TZP/abstract.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en}
}

@article{broomhall+2014,
  title = {Prospects for Asteroseismic Inference on the Envelope Helium Abundance in Red Giant Stars},
  author = {Broomhall, A.-M. and Miglio, A. and Montalban, J. and Eggenberger, P. and Chaplin, W. J. and Elsworth, Y. and Scuflaire, R. and Ventura, P. and Verner, G. A.},
  year = {2014},
  month = may,
  volume = {440},
  pages = {1828--1843},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stu393},
  abstract = {Regions of rapid variation in the internal structure of a star are often referred to as acoustic glitches since they create a characteristic periodic signature in the frequencies of p modes. Here we examine the localized disturbance arising from the helium second ionization zone in red giant branch and clump stars. More specifically, we determine how accurately and precisely the parameters of the ionization zone can be obtained from the oscillation frequencies of stellar models. We use models produced by three different generation codes that not only cover a wide range of stages of evolution along the red giant phase but also incorporate different initial helium abundances. We discuss the conditions under which such fits robustly and accurately determine the acoustic radius of the second ionization zone of helium. The determined radii of the ionization zones as inferred from the mode frequencies were found to be coincident with the local maximum in the first adiabatic exponent described by the models, which is associated with the outer edge of the second ionization zone of helium. Finally, we consider whether this method can be used to distinguish stars with different helium abundances. Although a definite trend in the amplitude of the signal is observed any distinction would be difficult unless the stars come from populations with vastly different helium abundances or the uncertainties associated with the fitted parameters can be reduced. However, application of our methodology could be useful for distinguishing between different populations of red giant stars in globular clusters, where distinct populations with very different helium abundances have been observed.},
  archivePrefix = {arXiv},
  eprint = {1403.7045},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/MHH3ABB4/Broomhall et al. - 2014 - Prospects for asteroseismic inference on the envel.pdf;/Users/Oliver/Zotero/storage/59GD84WA/1403.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {2}
}

@article{broomhall2017,
  title = {A {{Helioseismic Perspective}} on the {{Depth}} of the {{Minimum Between Solar Cycles}} 23 and 24},
  author = {Broomhall, A.-M.},
  year = {2017},
  month = feb,
  abstract = {The solar-activity-cycle minimum observed between Cycles 23 and 24 is generally regarded as being unusually deep and long. That minimum is being followed by one of the smallest amplitude cycles in recent history. We perform an in-depth analysis of this minimum with helioseismology. We use Global Oscillation Network Group (GONG) data to demonstrate that the frequencies of helioseismic oscillations are a sensitive probe of the Sun's magnetic field: The frequencies of the helioseismic oscillations were found to be systematically lower in the minimum following Cycle 23 than in the minimum preceding it. This difference is statistically significant and may indicate that the Sun's global magnetic field was weaker in the minimum following Cycle 23. The size of the shift in oscillation frequencies between the two minima is dependent on the frequency of the oscillation and takes the same functional form as the frequency dependence observed when the frequencies at cycle maximum are compared with the cycle-minimum frequencies. This implies that the same near-surface magnetic perturbation is responsible. Finally, we determine that the difference in the mean magnetic field between the minimum preceding Cycle 23 and that following it is approximately 1G.},
  archivePrefix = {arXiv},
  eprint = {1702.03149},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/MN95R3IU/1702.html},
  journal = {arXiv:1702.03149 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{brown+1991,
  title = {Detection of {{Possible}} P-{{Mode Oscillations}} on {{Procyon}}},
  author = {Brown, Timothy M. and Gilliland, Ronald L. and Noyes, Robert W. and Ramsey, Lawrence W.},
  year = {1991},
  month = feb,
  volume = {368},
  pages = {599},
  issn = {0004-637X},
  doi = {10.1086/169725},
  abstract = {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.},
  file = {/Users/Oliver/Zotero/storage/JIWBGVTS/Brown et al. - 1991 - Detection of Possible p-Mode Oscillations on Procy.pdf;/Users/Oliver/Zotero/storage/Y8RHNLLH/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en}
}

@article{brown+2016,
  title = {Gaia {{Data Release}} 1. {{Summary}} of the Astrometric, Photometric, and Survey Properties},
  author = {Brown, A. G. A. and Vallenari, A. and Prusti, T. and Bruijne, De and J, J. H. and Mignard, F. and Drimmel, R. and Babusiaux, C. and {Bailer-Jones}, C. a. L. and Bastian, U. and Biermann, M. and Evans, D. W. and Eyer, L. and Jansen, F. and Jordi, C. and Katz, D. and Klioner, S. A. and Lammers, U. and Lindegren, L. and Luri, X. and O'Mullane, W. and Panem, C. and Pourbaix, D. and Randich, S. and Sartoretti, P. and Siddiqui, H. I. and Soubiran, C. and Valette, V. and {van Leeuwen}, F. and Walton, N. A. and Aerts, C. and Arenou, F. and Cropper, M. and H{\o}g, E. and Lattanzi, M. G. and Grebel, E. K. and Holland, A. D. and Huc, C. and Passot, X. and Perryman, M. and Bramante, L. and Cacciari, C. and Casta{\~n}eda, J. and Chaoul, L. and Cheek, N. and De Angeli, F. and Fabricius, C. and Guerra, R. and Hern{\'a}ndez, J. and {Jean-Antoine-Piccolo}, A. and Masana, E. and Messineo, R. and Mowlavi, N. and Nienartowicz, K. and {Ord{\'o}{\~n}ez-Blanco}, D. and Panuzzo, P. and Portell, J. and Richards, P. J. and Riello, M. and Seabroke, G. M. and Tanga, P. and Th{\'e}venin, F. and Torra, J. and Els, S. G. and {Gracia-Abril}, G. and Comoretto, G. and {Garcia-Reinaldos}, M. and Lock, T. and Mercier, E. and Altmann, M. and Andrae, R. and Astraatmadja, T. L. and {Bellas-Velidis}, I. and Benson, K. and Berthier, J. and Blomme, R. and Busso, G. and Carry, B. and Cellino, A. and Clementini, G. and Cowell, S. and Creevey, O. and Cuypers, J. and Davidson, M. and De Ridder, J. and {de Torres}, A. and Delchambre, L. and Dell'Oro, A. and Ducourant, C. and Fr{\'e}mat, Y. and {Garc{\'i}a-Torres}, M. and Gosset, E. and Halbwachs, J.-L. and Hambly, N. C. and Harrison, D. L. and Hauser, M. and Hestroffer, D. and Hodgkin, S. T. and Huckle, H. E. and Hutton, A. and Jasniewicz, G. and Jordan, S. and Kontizas, M. and Korn, A. J. and Lanzafame, A. C. and Manteiga, M. and Moitinho, A. and Muinonen, K. and Osinde, J. and Pancino, E. and Pauwels, T. and Petit, J.-M. and {Recio-Blanco}, A. and Robin, A. C. and Sarro, L. M. and Siopis, C. and Smith, M. and Smith, K. W. and Sozzetti, A. and Thuillot, W. and {van Reeven}, W. and Viala, Y. and Abbas, U. and Abreu Aramburu, A. and Accart, S. and Aguado, J. J. and Allan, P. M. and Allasia, W. and Altavilla, G. and {\'A}lvarez, M. A. and Alves, J. and Anderson, R. I. and Andrei, A. H. and Anglada Varela, E. and Antiche, E. and Antoja, T. and Ant{\'o}n, S. and Arcay, B. and Bach, N. and Baker, S. G. and {Balaguer-N{\'u}{\~n}ez}, L. and Barache, C. and Barata, C. and Barbier, A. and Barblan, F. and {Barrado y Navascu{\'e}s}, D. and Barros, M. and Barstow, M. A. and Becciani, U. and Bellazzini, M. and Bello Garc{\'i}a, A. and Belokurov, V. and Bendjoya, P. and Berihuete, A. and Bianchi, L. and Bienaym{\'e}, O. and Billebaud, F. and Blagorodnova, N. and {Blanco-Cuaresma}, S. and Boch, T. and Bombrun, A. and Borrachero, R. and Bouquillon, S. and Bourda, G. and Bouy, H. and Bragaglia, A. and Breddels, M. A. and Brouillet, N. and Br{\"u}semeister, T. and Bucciarelli, B. and Burgess, P. and Burgon, R. and Burlacu, A. and Busonero, D. and Buzzi, R. and Caffau, E. and Cambras, J. and Campbell, H. and Cancelliere, R. and {Cantat-Gaudin}, T. and Carlucci, T. and Carrasco, J. M. and Castellani, M. and Charlot, P. and Charnas, J. and Chiavassa, A. and Clotet, M. and Cocozza, G. and Collins, R. S. and Costigan, G. and Crifo, F. and Cross, N. J. G. and Crosta, M. and Crowley, C. and Dafonte, C. and Damerdji, Y. and Dapergolas, A. and David, P. and David, M. and De Cat, P. and {de Felice}, F. and {de Laverny}, P. and De Luise, F. and De March, R. and {de Martino}, D. and {de Souza}, R. and Debosscher, J. and {del Pozo}, E. and Delbo, M. and Delgado, A. and Delgado, H. E. and Di Matteo, P. and Diakite, S. and Distefano, E. and Dolding, C. and Dos Anjos, S. and Drazinos, P. and Duran, J. and Dzigan, Y. and Edvardsson, B. and Enke, H. and Evans, N. W. and Eynard Bontemps, G. and Fabre, C. and Fabrizio, M. and Faigler, S. and Falc{\~a}o, A. J. and Farr{\`a}s Casas, M. and Federici, L. and Fedorets, G. and {Fern{\'a}ndez-Hern{\'a}ndez}, J. and Fernique, P. and Fienga, A. and Figueras, F. and Filippi, F. and Findeisen, K. and Fonti, A. and Fouesneau, M. and Fraile, E. and Fraser, M. and Fuchs, J. and Gai, M. and Galleti, S. and Galluccio, L. and Garabato, D. and {Garc{\'i}a-Sedano}, F. and Garofalo, A. and Garralda, N. and Gavras, P. and Gerssen, J. and Geyer, R. and Gilmore, G. and Girona, S. and Giuffrida, G. and Gomes, M. and {Gonz{\'a}lez-Marcos}, A. and {Gonz{\'a}lez-N{\'u}{\~n}ez}, J. and {Gonz{\'a}lez-Vidal}, J. J. and Granvik, M. and Guerrier, A. and Guillout, P. and Guiraud, J. and G{\'u}rpide, A. and {Guti{\'e}rrez-S{\'a}nchez}, R. and Guy, L. P. and Haigron, R. and Hatzidimitriou, D. and Haywood, M. and Heiter, U. and Helmi, A. and Hobbs, D. and Hofmann, W. and Holl, B. and Holland, G. and Hunt, J. a. S. and Hypki, A. and Icardi, V. and Irwin, M. and {Jevardat de Fombelle}, G. and Jofr{\'e}, P. and Jonker, P. G. and Jorissen, A. and Julbe, F. and Karampelas, A. and Kochoska, A. and Kohley, R. and Kolenberg, K. and Kontizas, E. and Koposov, S. E. and Kordopatis, G. and Koubsky, P. and {Krone-Martins}, A. and Kudryashova, M. and Kull, I. and Bachchan, R. K. and {Lacoste-Seris}, F. and Lanza, A. F. and Lavigne, J.-B. and {Le Poncin-Lafitte}, C. and Lebreton, Y. and Lebzelter, T. and Leccia, S. and Leclerc, N. and {Lecoeur-Taibi}, I. and Lemaitre, V. and Lenhardt, H. and Leroux, F. and Liao, S. and Licata, E. and Lindstr{\o}m, H. E. P. and Lister, T. A. and Livanou, E. and Lobel, A. and L{\"o}ffler, W. and L{\'o}pez, M. and Lorenz, D. and MacDonald, I. and Magalh{\~a}es Fernandes, T. and Managau, S. and Mann, R. G. and Mantelet, G. and Marchal, O. and Marchant, J. M. and Marconi, M. and Marinoni, S. and Marrese, P. M. and Marschalk{\'o}, G. and Marshall, D. J. and {Mart{\'i}n-Fleitas}, J. M. and Martino, M. and Mary, N. and Matijevi{\v c}, G. and Mazeh, T. and McMillan, P. J. and Messina, S. and Michalik, D. and Millar, N. R. and Miranda, B. M. H. and Molina, D. and Molinaro, R. and Molinaro, M. and Moln{\'a}r, L. and Moniez, M. and Montegriffo, P. and Mor, R. and Mora, A. and Morbidelli, R. and Morel, T. and Morgenthaler, S. and Morris, D. and Mulone, A. F. and Muraveva, T. and Musella, I. and Narbonne, J. and Nelemans, G. and Nicastro, L. and Noval, L. and Ord{\'e}novic, C. and {Ordieres-Mer{\'e}}, J. and Osborne, P. and Pagani, C. and Pagano, I. and Pailler, F. and Palacin, H. and Palaversa, L. and Parsons, P. and Pecoraro, M. and Pedrosa, R. and Pentik{\"a}inen, H. and Pichon, B. and Piersimoni, A. M. and Pineau, F.-X. and Plachy, E. and Plum, G. and Poujoulet, E. and Pr{\v s}a, A. and Pulone, L. and Ragaini, S. and Rago, S. and Rambaux, N. and {Ramos-Lerate}, M. and Ranalli, P. and Rauw, G. and Read, A. and Regibo, S. and Reyl{\'e}, C. and Ribeiro, R. A. and Rimoldini, L. and Ripepi, V. and Riva, A. and Rixon, G. and Roelens, M. and {Romero-G{\'o}mez}, M. and Rowell, N. and Royer, F. and {Ruiz-Dern}, L. and Sadowski, G. and Sagrist{\`a} Sell{\'e}s, T. and Sahlmann, J. and Salgado, J. and Salguero, E. and Sarasso, M. and Savietto, H. and Schultheis, M. and Sciacca, E. and Segol, M. and Segovia, J. C. and Segransan, D. and Shih, I.-C. and Smareglia, R. and Smart, R. L. and Solano, E. and Solitro, F. and Sordo, R. and Soria Nieto, S. and Souchay, J. and Spagna, A. and Spoto, F. and Stampa, U. and Steele, I. A. and Steidelm{\"u}ller, H. and Stephenson, C. A. and Stoev, H. and Suess, F. F. and S{\"u}veges, M. and Surdej, J. and Szabados, L. and {Szegedi-Elek}, E. and Tapiador, D. and Taris, F. and Tauran, G. and Taylor, M. B. and Teixeira, R. and Terrett, D. and Tingley, B. and Trager, S. C. and Turon, C. and Ulla, A. and Utrilla, E. and Valentini, G. and {van Elteren}, A. and Van Hemelryck, E. and {van Leeuwen}, M. and Varadi, M. and Vecchiato, A. and Veljanoski, J. and Via, T. and Vicente, D. and Vogt, S. and Voss, H. and Votruba, V. and Voutsinas, S. and Walmsley, G. and Weiler, M. and Weingrill, K. and Wevers, T. and Wyrzykowski, {\L} and Yoldas, A. and {\v Z}erjal, M. and Zucker, S. and Zurbach, C. and Zwitter, T. and Alecu, A. and Allen, M. and Allende Prieto, C. and Amorim, A. and {Anglada-Escud{\'e}}, G. and Arsenijevic, V. and Azaz, S. and Balm, P. and Beck, M. and Bernstein, H.-H. and Bigot, L. and Bijaoui, A. and Blasco, C. and Bonfigli, M. and Bono, G. and Boudreault, S. and Bressan, A. and Brown, S. and Brunet, P.-M. and Bunclark, P. and Buonanno, R. and Butkevich, A. G. and Carret, C. and Carrion, C. and Chemin, L. and Ch{\'e}reau, F. and Corcione, L. and Darmigny, E. and Boer, De and S, K. and {de Teodoro}, P. and Zeeuw, De and T, P. and Delle Luche, C. and Domingues, C. D. and Dubath, P. and Fodor, F. and Fr{\'e}zouls, B. and Fries, A. and Fustes, D. and Fyfe, D. and Gallardo, E. and Gallegos, J. and Gardiol, D. and Gebran, M. and Gomboc, A. and G{\'o}mez, A. and Grux, E. and Gueguen, A. and Heyrovsky, A. and Hoar, J. and Iannicola, G. and Isasi Parache, Y. and Janotto, A.-M. and Joliet, E. and Jonckheere, A. and Keil, R. and Kim, D.-W. and Klagyivik, P. and Klar, J. and Knude, J. and Kochukhov, O. and Kolka, I. and Kos, J. and Kutka, A. and Lainey, V. and LeBouquin, D. and Liu, C. and Loreggia, D. and Makarov, V. V. and Marseille, M. G. and Martayan, C. and {Martinez-Rubi}, O. and Massart, B. and Meynadier, F. and Mignot, S. and Munari, U. and Nguyen, A.-T. and Nordlander, T. and Ocvirk, P. and O'Flaherty, K. S. and Olias Sanz, A. and Ortiz, P. and Osorio, J. and Oszkiewicz, D. and Ouzounis, A. and Palmer, M. and Park, P. and Pasquato, E. and Peltzer, C. and Peralta, J. and P{\'e}turaud, F. and Pieniluoma, T. and Pigozzi, E. and Poels, J. and Prat, G. and Prod'homme, T. and Raison, F. and Rebordao, J. M. and Risquez, D. and {Rocca-Volmerange}, B. and Rosen, S. and {Ruiz-Fuertes}, M. I. and Russo, F. and Sembay, S. and Serraller Vizcaino, I. and Short, A. and Siebert, A. and Silva, H. and Sinachopoulos, D. and Slezak, E. and Soffel, M. and Sosnowska, D. and Strai{\v z}ys, V. and {ter Linden}, M. and Terrell, D. and Theil, S. and Tiede, C. and Troisi, L. and Tsalmantza, P. and Tur, D. and Vaccari, M. and Vachier, F. and Valles, P. and Van Hamme, W. and Veltz, L. and Virtanen, J. and Wallut, J.-M. and Wichmann, R. and Wilkinson, M. I. and Ziaeepour, H. and Zschocke, S.},
  year = {2016},
  month = nov,
  volume = {595},
  pages = {A2},
  doi = {10.1051/0004-6361/201629512},
  abstract = {Context. At about 1000 days after the launch of Gaia we present the first Gaia data release, Gaia DR1, consisting of astrometry and photometry for over 1 billion sources brighter than magnitude 20.7. \\
 Aims: A summary of Gaia DR1 is presented along with illustrations of the scientific quality of the data, followed by a discussion of the limitations due to the preliminary nature of this release. \\
 Methods: The raw data collected by Gaia during the first 14 months of the mission have been processed by the Gaia Data Processing and Analysis Consortium (DPAC) and turned into an astrometric and photometric catalogue. \\
 Results: Gaia DR1 consists of three components: a primary astrometric data set which contains the positions, parallaxes, and mean proper motions for about 2 million of the brightest stars in common with the Hipparcos and Tycho-2 catalogues - a realisation of the Tycho-Gaia Astrometric Solution (TGAS) - and a secondary astrometric data set containing the positions for an additional 1.1 billion sources. The second component is the photometric data set, consisting of mean G-band magnitudes for all sources. The G-band light curves and the characteristics of 3000 Cepheid and RR Lyrae stars, observed at high cadence around the south ecliptic pole, form the third component. For the primary astrometric data set the typical uncertainty is about 0.3 mas for the positions and parallaxes, and about 1 mas yr\textsuperscript{-1} for the proper motions. A systematic component of 0.3 mas should be added to the parallax uncertainties. For the subset of 94 000 Hipparcos stars in the primary data set, the proper motions are much more precise at about 0.06 mas yr\textsuperscript{-1}. For the secondary astrometric data set, the typical uncertainty of the positions is 10 mas. The median uncertainties on the mean G-band magnitudes range from the mmag level to 0.03 mag over the magnitude range 5 to 20.7. \\
 Conclusions: Gaia DR1 is an important milestone ahead of the next Gaia data release, which will feature five-parameter astrometry for all sources. Extensive validation shows that Gaia DR1 represents a major advance in the mapping of the heavens and the availability of basic stellar data that underpin observational astrophysics. Nevertheless, the very preliminary nature of this first Gaia data release does lead to a number of important limitations to the data quality which should be carefully considered before drawing conclusions from the data.},
  file = {/Users/Oliver/Zotero/storage/CZSESY6I/Brown et al. - 2016 - Gaia Data Release 1. Summary of the astrometric, p.pdf;/Users/Oliver/Zotero/storage/X8DEGNIS/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{brown+2018,
  title = {Gaia {{Data Release}} 2. {{Summary}} of the Contents and Survey Properties},
  author = {Brown, A. G. A. and Vallenari, A. and Prusti, T. and Bruijne, De and J, J. H. and Babusiaux, C. and {Bailer-Jones}, C. a. L. and Biermann, M. and Evans, D. W. and Eyer, L. and Jansen, F. and Jordi, C. and Klioner, S. A. and Lammers, U. and Lindegren, L. and Luri, X. and Mignard, F. and Panem, C. and Pourbaix, D. and Randich, S. and Sartoretti, P. and Siddiqui, H. I. and Soubiran, C. and {van Leeuwen}, F. and Walton, N. A. and Arenou, F. and Bastian, U. and Cropper, M. and Drimmel, R. and Katz, D. and Lattanzi, M. G. and Bakker, J. and Cacciari, C. and Casta{\~n}eda, J. and Chaoul, L. and Cheek, N. and De Angeli, F. and Fabricius, C. and Guerra, R. and Holl, B. and Masana, E. and Messineo, R. and Mowlavi, N. and Nienartowicz, K. and Panuzzo, P. and Portell, J. and Riello, M. and Seabroke, G. M. and Tanga, P. and Th{\'e}venin, F. and {Gracia-Abril}, G. and Comoretto, G. and {Garcia-Reinaldos}, M. and Teyssier, D. and Altmann, M. and Andrae, R. and Audard, M. and {Bellas-Velidis}, I. and Benson, K. and Berthier, J. and Blomme, R. and Burgess, P. and Busso, G. and Carry, B. and Cellino, A. and Clementini, G. and Clotet, M. and Creevey, O. and Davidson, M. and De Ridder, J. and Delchambre, L. and Dell'Oro, A. and Ducourant, C. and {Fern{\'a}ndez-Hern{\'a}ndez}, J. and Fouesneau, M. and Fr{\'e}mat, Y. and Galluccio, L. and {Garc{\'i}a-Torres}, M. and {Gonz{\'a}lez-N{\'u}{\~n}ez}, J. and {Gonz{\'a}lez-Vidal}, J. J. and Gosset, E. and Guy, L. P. and Halbwachs, J.-L. and Hambly, N. C. and Harrison, D. L. and Hern{\'a}ndez, J. and Hestroffer, D. and Hodgkin, S. T. and Hutton, A. and Jasniewicz, G. and {Jean-Antoine-Piccolo}, A. and Jordan, S. and Korn, A. J. and {Krone-Martins}, A. and Lanzafame, A. C. and Lebzelter, T. and L{\"o}ffler, W. and Manteiga, M. and Marrese, P. M. and {Mart{\'i}n-Fleitas}, J. M. and Moitinho, A. and Mora, A. and Muinonen, K. and Osinde, J. and Pancino, E. and Pauwels, T. and Petit, J.-M. and {Recio-Blanco}, A. and Richards, P. J. and Rimoldini, L. and Robin, A. C. and Sarro, L. M. and Siopis, C. and Smith, M. and Sozzetti, A. and S{\"u}veges, M. and Torra, J. and {van Reeven}, W. and Abbas, U. and Abreu Aramburu, A. and Accart, S. and Aerts, C. and Altavilla, G. and {\'A}lvarez, M. A. and Alvarez, R. and Alves, J. and Anderson, R. I. and Andrei, A. H. and Anglada Varela, E. and Antiche, E. and Antoja, T. and Arcay, B. and Astraatmadja, T. L. and Bach, N. and Baker, S. G. and {Balaguer-N{\'u}{\~n}ez}, L. and Balm, P. and Barache, C. and Barata, C. and Barbato, D. and Barblan, F. and Barklem, P. S. and Barrado, D. and Barros, M. and Barstow, M. A. and Bartholom{\'e} Mu{\~n}oz, S. and Bassilana, J.-L. and Becciani, U. and Bellazzini, M. and Berihuete, A. and Bertone, S. and Bianchi, L. and Bienaym{\'e}, O. and {Blanco-Cuaresma}, S. and Boch, T. and Boeche, C. and Bombrun, A. and Borrachero, R. and Bossini, D. and Bouquillon, S. and Bourda, G. and Bragaglia, A. and Bramante, L. and Breddels, M. A. and Bressan, A. and Brouillet, N. and Br{\"u}semeister, T. and Brugaletta, E. and Bucciarelli, B. and Burlacu, A. and Busonero, D. and Butkevich, A. G. and Buzzi, R. and Caffau, E. and Cancelliere, R. and Cannizzaro, G. and {Cantat-Gaudin}, T. and Carballo, R. and Carlucci, T. and Carrasco, J. 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