text:
author = {Santos, A. R. G. and Cunha, M. S. and Avelino, P. P. and Garc{\'i}a, R. A. and Mathur, S.},
  year = {2016},
  month = nov,
  abstract = {Quasi-periodic modulations of the stellar light curve may result from dark spots crossing the visible stellar disc. Due to differential rotation, spots at different latitudes generally have different rotation periods. Hence, by studying spot-induced modulations, one can learn about stellar surface (differential) rotation and magnetic activity. Recently, Reinhold \& Arlt (2015) proposed a method based on the Lomb-Scargle periodogram of light curves to identify the sign of the differential rotation at the stellar surface. Our goal is to understand how the modulation of the stellar light curve due to the presence of spots and the corresponding periodogram are affected by both the stellar and spot properties. We generate synthetic light curves of stars with different properties (inclination angle, limb darkening, and rotation rate) and spot configurations (number of spots, latitude, intensity contrast, and size). By analysing their Lomb-Scargle periodograms, we compute the ratio between the heights of the second and first harmonics of the rotation period (peak-height-ratio). We find that the peak-height ratios are essentially a function of a single parameter, the fraction of time the spot is visible, which is related to the sinusoidality of the spot modulation. We identify the conditions under which the periodogram analysis can actually provide an estimate of the spot latitudes and/or the stellar inclination angle. We also identify possible sources of error in the identification of the sign of the differential rotation.},
  archivePrefix = {arXiv},
  eprint = {1611.07461},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/SE9V2W3E/Santos et al. - 2016 - Starspot signature on the light curve Learning ab.pdf;/Users/Oliver/Zotero/storage/KWMRTECB/1611.html},
  journal = {arXiv:1611.07461 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{santos+2016b,
  title = {A Thorough Analysis of the Short- and Mid-Term Activity-Related Variations in the Solar Acoustic Frequencies},
  author = {Santos, A. R. G. and Cunha, M. S. and Avelino, P. P. and Chaplin, W. J. and Campante, T. L.},
  year = {2016},
  month = oct,
  abstract = {The frequencies of the solar acoustic oscillations vary over the activity cycle. The variations in other activity proxies are found to be well correlated with the variations in the acoustic frequencies. However, each proxy has a slightly different time behaviour. Our goal is to characterize the differences between the time behaviour of the frequency shifts and of two other activity proxies, namely, the area covered by sunspots and the 10.7cm flux. We define a new observable that is particularly sensitive to the short-term frequency variations. We then compare the observable when computed from model frequency shifts and from observed frequency shifts obtained with the Global Oscillation Network Group (GONG) for cycle 23. Our analysis shows that on the shortest time-scales the variations in the frequency shifts seen in the GONG observations are strongly correlated with the variations in the area covered by sunspots. However, a significant loss of correlation is still found. We verify that the times when the frequency shifts and the sunspot area do not vary in a similar way tend to coincide with the times of the maxima of the quasi-biennial variations seen in the solar seismic data. A similar analysis of the relation between the 10.7cm flux and the frequency shifts reveals that the short-time variations in the frequency shifts follow even more closely those of the 10.7cm flux than those of the sunspot area. However, a loss of correlation between frequency shifts and 10.7cm flux variations is still found around the same times.},
  archivePrefix = {arXiv},
  eprint = {1610.06872},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/KX2TWFAH/Santos et al. - 2016 - A thorough analysis of the short- and mid-term act.pdf;/Users/Oliver/Zotero/storage/HRUB4XV4/1610.html},
  journal = {arXiv:1610.06872 [astro-ph]},
  keywords = {AR 01/11/16,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{santos+2018,
  title = {Signatures of {{Magnetic Activity}} in the {{Seismic Data}} of {{Solar}}-Type {{Stars Observed}} by {{{\emph{Kepler}}}}},
  author = {Santos, A. R. G. and Campante, T. L. and Chaplin, W. J. and Cunha, M. S. and Lund, M. N. and Kiefer, R. and Salabert, D. and Garc{\'i}a, R. A. and Davies, G. R. and Elsworth, Y. and Howe, R.},
  year = {2018},
  month = jul,
  volume = {237},
  pages = {17},
  issn = {1538-4365},
  doi = {10.3847/1538-4365/aac9b6},
  file = {/Users/Oliver/Zotero/storage/YIE7R2DV/Santos et al. - 2018 - Signatures of Magnetic Activity in the Seismic Dat.pdf},
  journal = {The Astrophysical Journal Supplement Series},
  number = {1}
}

@article{santos+2019,
  title = {Surface {{Rotation}} and {{Photometric Activity}} for {{Kepler Targets}}. {{I}}. {{M}} and {{K Main}}-Sequence {{Stars}}},
  author = {Santos, A. R. G. and Garc{\'i}a, R. A. and Mathur, S. and Bugnet, L. and {van Saders}, J. L. and Metcalfe, T. S. and Simonian, G. V. A. and Pinsonneault, M. H.},
  year = {2019},
  month = sep,
  volume = {244},
  pages = {21},
  doi = {10.3847/1538-4365/ab3b56},
  abstract = {Brightness variations due to dark spots on the stellar surface encode information about stellar surface rotation and magnetic activity. In this work, we analyze the Kepler long-cadence data of 26,521 main-sequence stars of spectral types M and K in order to measure their surface rotation and photometric activity level. Rotation-period estimates are obtained by the combination of a wavelet analysis and autocorrelation function of the light curves. Reliable rotation estimates are determined by comparing the results from the different rotation diagnostics and four data sets. We also measure the photometric activity proxy \{S\}\textsubscript{ph}\vphantom\{\} using the amplitude of the flux variations on an appropriate timescale. We report rotation periods and photometric activity proxies for about 60\% of the sample, including 4431 targets for which McQuillan et al. did not report a rotation period. For the common targets with rotation estimates in this study and in McQuillan et al., our rotation periods agree within 99\%. In this work, we also identify potential polluters, such as misclassified red giants and classical pulsator candidates. Within the parameter range we study, there is a mild tendency for hotter stars to have shorter rotation periods. The photometric activity proxy spans a wider range of values with increasing effective temperature. The rotation period and photometric activity proxy are also related, with \{S\}\textsubscript{ph}\vphantom\{\} being larger for fast rotators. Similar to McQuillan et al., we find a bimodal distribution of rotation periods.},
  file = {/Users/Oliver/Zotero/storage/CS77D2ST/abstract.html},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en}
}

@article{scargle1982,
  title = {Studies in Astronomical Time Series Analysis. {{II}}. {{Statistical}} Aspects of Spectral Analysis of Unevenly Spaced Data.},
  author = {Scargle, J. D.},
  year = {1982},
  month = dec,
  volume = {263},
  pages = {835},
  doi = {10.1086/160554},
  abstract = {Detection of a periodic signal hidden in noise is frequently a goal in astronomical data analysis. This paper does not introduce a new detection technique, but instead studies the reliability and efficiency of detection with the most commonly used technique, the periodogram, in the case where the observation times are unevenly spaced. This choice was made because, of the methods in current use, it appears to have the simplest statistical behavior. A modification of the classical definition of the periodogram is necessary in order to retain the simple statistical behavior of the evenly spaced case. With this modification, periodogram analysis and least-squares fitting of sine waves to the data are exactly equivalent. Certain difficulties with the use of the periodogram are less important than commonly believed in the case of detection of strictly periodic signals. In addition, the standard method for mitigating these difficulties (tapering) can be used just as well if the sampling is uneven. An analysis of the statistical significance of signal detections is presented, with examples},
  file = {/Users/Oliver/Zotero/storage/EXGIVL5I/Scargle - 1982 - Studies in astronomical time series analysis. II. .pdf;/Users/Oliver/Zotero/storage/BIMXNZHL/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en}
}

@article{schlaufman2010,
  title = {Evidence of {{Possible Spin}}-Orbit {{Misalignment Along}} the {{Line}} of {{Sight}} in {{Transiting Exoplanet Systems}}},
  author = {Schlaufman, Kevin C.},
  year = {2010},
  month = aug,
  volume = {719},
  pages = {602},
  doi = {10.1088/0004-637X/719/1/602},
  abstract = {Of the 26 transiting exoplanet systems with measurements of the Rossiter-McLaughlin (RM) effect, eight have now been found to be significantly spin-orbit misaligned in the plane of the sky (i.e., RM misalignment angle |{$\lambda$}| \>\textasciitilde{} 30\textdegree{} and inconsistent with {$\lambda$} = 0\textdegree ). Unfortunately, the RM effect does not constrain the complement misalignment angle between the orbit of the planet and the spin of its host star along the line of sight (LOS). I use a simple model of stellar rotation benchmarked with observational data to statistically identify 10 exoplanet systems from a sample of 75 for which there is likely a significant degree of spin-orbit misalignment along the LOS: HAT-P-7, HAT-P-14, HAT-P-16, HD 17156, Kepler-5, Kepler-7, TrES-4, WASP-1, WASP-12, and WASP-14. All 10 systems have host stellar masses M \textsubscript{*} in the range 1.2 M \textsubscript{sun} \<\textasciitilde{} M \textsubscript{*} \<\textasciitilde{} 1.5 M \textsubscript{sun}, and the probability of this occurrence by chance is less than one in ten thousand. In addition, the planets in the candidate-misaligned systems are preferentially massive and eccentric. The coupled distribution of misalignment from the RM effect and from this analysis suggests that transiting exoplanets are more likely to be spin-orbit aligned than expected given predictions for a transiting planet population produced entirely by planet-planet scattering or Kozai cycles and tidal friction. For that reason, there are likely two populations of close-in exoplanet systems: a population of aligned systems and a population of apparently misaligned systems in which the processes that lead to misalignment or to the survival of misaligned systems operate more efficiently in systems with massive stars and planets.},
  file = {/Users/Oliver/Zotero/storage/W5N5HEPT/Schlaufman - 2010 - Evidence of Possible Spin-orbit Misalignment Along.pdf;/Users/Oliver/Zotero/storage/SJIB9WU6/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  keywords = {Core Gyrochronology},
  language = {en},
  number = {1}
}

@article{schleicher+mennickent2017,
  title = {A Dynamo Mechanism as the Potential Origin of the Long Cycle in {{Double Periodic Variables}}},
  author = {Schleicher, Dominik R. G. and Mennickent, Ronald E.},
  year = {2017},
  month = mar,
  abstract = {The class of Double Period Variables (DPVs) consists of close interacting binaries, with a characteristic long period that is an order of magnitude longer than the corresponding orbital period, many of them with a characteristic ratio of about 3.5x10\^1. We consider here the possibility that the accretion flow is modulated as a result of a magnetic dynamo cycle. Due to the short binary separations, we expect the rotation of the donor star to be synchronized with the rotation of the binary due to tidal locking. We here present a model to estimate the dynamo number and the resulting relation between the activity cycle length and the orbital period, as well as an estimate for the modulation of the mass transfer rate. The latter is based on Applegate's scenario, implying cyclic changes in the radius of the donor star and thus in the mass transfer rate as a result of magnetic activity. Our model is applied to a sample of 17 systems with known physical parameters, 10 also with known orbital periods. In spite of the uncertainties of our simplified framework, the results show a reasonable agreement, indicating that a dynamo interpretation is potentially feasible. At the same time, we note that the orbital period variations resulting from Applegate's model are sufficiently small to be consistent with the data. We conclude that both larger samples with known physical parameters as well as potential direct probes of the magnetism of the donor star, including cold spots as well as polarization, will be valuable to further constrain the nature of these systems.},
  archivePrefix = {arXiv},
  eprint = {1703.03876},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/QPKJGW9Q/Schleicher and Mennickent - 2017 - A dynamo mechanism as the potential origin of the .pdf;/Users/Oliver/Zotero/storage/KHBFRPRQ/1703.html},
  journal = {arXiv:1703.03876 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{schofield+2019,
  title = {The {{Asteroseismic Target List}} for {{Solar}}-like {{Oscillators Observed}} in 2 Minute {{Cadence}} with the {{Transiting Exoplanet Survey Satellite}}},
  author = {Schofield, Mathew and Chaplin, William J. and Huber, Daniel and Campante, Tiago L. and Davies, Guy R. and Miglio, Andrea and Ball, Warrick H. and Appourchaux, Thierry and Basu, Sarbani and Bedding, Timothy R. and {Christensen-Dalsgaard}, J{\o}rgen and Creevey, Orlagh and Garc{\'i}a, Rafael A. and Handberg, Rasmus and Kawaler, Steven D. and Kjeldsen, Hans and Latham, David W. and Lund, Mikkel N. and Metcalfe, Travis S. and Ricker, George R. and Serenelli, Aldo and Silva Aguirre, Victor and Stello, Dennis and Vanderspek, Roland},
  year = {2019},
  month = mar,
  volume = {241},
  pages = {12},
  doi = {10.3847/1538-4365/ab04f5},
  abstract = {We present the target list of solar-type stars to be observed in short-cadence (2 minute) for asteroseismology by the NASA Transiting Exoplanet Survey Satellite (TESS) during its 2 year nominal survey mission. The solar-like Asteroseismic Target List (ATL) is comprised of bright, cool main-sequence and subgiant stars and forms part of the larger target list of the TESS Asteroseismic Science Consortium. The ATL uses the Gaia Data Release 2 and the Extended Hipparcos Compilation (XHIP) to derive fundamental stellar properties, to calculate detection probabilities, and to produce a rank-ordered target list. We provide a detailed description of how the ATL was produced and calculate expected yields for solar-like oscillators based on the nominal photometric performance by TESS. We also provide a publicly available source code that can be used to reproduce the ATL, thereby enabling comparisons of asteroseismic results from TESS with predictions from synthetic stellar populations.},
  file = {/Users/Oliver/Zotero/storage/MPLZTXBQ/Schofield et al. - 2019 - The Asteroseismic Target List for Solar-like Oscil.pdf;/Users/Oliver/Zotero/storage/U9TC2ZMV/abstract.html},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en},
  number = {1}
}

@article{schonrich+2019,
  title = {Distances and Parallax Bias in {{Gaia DR2}}},
  author = {Sch{\"o}nrich, Ralph and McMillan, Paul and Eyer, Laurent},
  year = {2019},
  month = feb,
  pages = {arXiv:1902.02355},
  abstract = {We derive Bayesian distances for all stars in the RV sample of Gaia DR2, and use the statistical method of Schoenrich, Binney \& Asplund(2012) to validate the distances and test the Gaia parallaxes. In contrast to other methods, which rely on special sources, our method directly tests the distances to all stars in our sample. We find clear evidence for a near-linear trend of distance bias f with distance s, proving a parallax offset delta p. On average, we find delta p = 0.054 mas (parallaxes in Gaia DR2 need to be increased) when accounting for the parallax uncertainty under-estimate in the Gaia set (delta p = 0.048 mas on the raw parallax errors) with negligible formal error and a systematic uncertainty of about 0.006 mas. The value is in concordance with results from asteroseismic measurements, but differs from the much lower bias found on quasar samples. We further use our method to compile a comprehensive set of quality cuts in colour, apparent magnitude, and astrometric parameters. Last, we find that for this sample delta p appears to strongly depend on the parallax uncertainty sigma\_p (when including the additional 0.043 mas) with a statistical confidence far in excess of 10\textbackslash sigma and a proportionality factor close to 1, though the dependence varies somewhat with sigma\_p. Correcting for the sigma\_p dependence also resolves otherwise unexplained correlations of the offset with the number of observation periods n\_\{vis\} and ecliptic latitude.},
  file = {/Users/Oliver/Zotero/storage/5FUAYPEK/Schönrich et al. - 2019 - Distances and parallax bias in Gaia DR2.pdf;/Users/Oliver/Zotero/storage/JGRSVNQU/ui.adsabs.harvard.edu.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{schou+buzasi2001,
  title = {Observations of P-Modes in {$\alpha$} {{Cen}}},
  author = {Schou, Jesper and Buzasi, Derek L.},
  year = {2001},
  month = jan,
  volume = {464},
  pages = {391--394},
  abstract = {We present the results of an analysis of a 50 day time-series of
photometry of {$\alpha$} Cen taken by the WIRE spacecraft. We see evidence
of p-modes similar to those observed in the Sun and present the results
obtained. We also discuss some of the implications of the measurements
and what can be observed in other stars.},
  file = {/Users/Oliver/Zotero/storage/3GHXPZP8/Schou and Buzasi - 2001 - Observations of p-modes in α Cen.pdf},
  keywords = {INDIVIDUAL STARS,P-MODES,STELLAR OSCILLATIONS}
}

@article{schultheis+2017,
  title = {Baade's Window with {{APOGEE}}: {{Metallicities}}, Ages and Chemical Abundances},
  shorttitle = {Baade's Window with {{APOGEE}}},
  author = {Schultheis, M. and {Rojas-Arriagada}, A. and P{\'e}rez, A. E. Garc{\'i}a and J{\"o}nsson, H. and Hayden, M. and Nandakumar, G. and Cunha, K. and Prieto, C. Allende and Holtzman, J. A. and Beers, T. C. and Bizyaev, D. and Brinkmann, J. and Carrera, R. and Cohen, R. E. and Geisler, D. and Hearty, F. R. and {Fern{\'a}ndez-Trincado}, J. G. and Maraston, C. and Minniti, D. and Nitschelm, C. and {Roman-Lopes}, A. and Schneider, D. P. and Tang, B. and Villanova, S. and Zasowski, G. and Majewski, S. R.},
  year = {2017},
  month = feb,
  abstract = {Baade's window (BW) is one of the most observed Galactic bulge fields in terms of chemical abundances. Due to its low and homogeneous interstellar absorption it is considered as a calibration field for Galactic bulge studies. In the era of large spectroscopic surveys, calibration fields such as BW are necessary to cross calibrate the stellar parameters and individual abundances of the APOGEE survey. We use the APOGEE BW stars to derive their metallicity distribution function (MDF) and individual abundances, for \$\textbackslash alpha\$- and iron-peak elements of the APOGEE ASPCAP pipeline (DR13), as well as the age distribution for stars in BW. We determine the MDF of APOGEE stars in BW and find a remarkable agreement with that of the Gaia-ESO survey (GES). Both exhibit a clear bimodal distribution. We also find that the Mg-metallicity planes of both surveys agree well, except for the metal-rich part ([Fe/H] {$>$}0.1), where APOGEE finds systematically higher Mg abundances with respect to the GES. The ages based on the [C/N] ratio reveal a bimodal age distribution, with a major old population at 10 Gyr, with a decreasing tail towards younger stars. A comparison between APOGEE estimates and stellar parameters, and those determined by other sources reveals detectable systematic offsets, in particular for spectroscopic surface gravity estimates. In general, we find a good agreement between individual abundances of O, Na, Mg, Al, Si, K, Ca, Cr, Mn, Co, and Ni from APOGEE with that of literature values. We have shown that in general APOGEE data show a good agreement in terms of MDF and individual chemical abundances with respect to literature works. Using the [C/N] ration we found a significant fraction of young stars in BW which is in agreement with the model of Haywood et al. (2016).},
  archivePrefix = {arXiv},
  eprint = {1702.01547},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/X54H7EB6/Schultheis et al. - 2017 - Baade's window with APOGEE Metallicities, ages an.pdf;/Users/Oliver/Zotero/storage/KH9F45MZ/1702.html},
  journal = {arXiv:1702.01547 [astro-ph]},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{schunker+2018,
  title = {Fragile {{Detection}} of {{Solar}} G-{{Modes}} by {{Fossat}} et Al.},
  author = {Schunker, Hannah and Schou, Jesper and Gaulme, Patrick and Gizon, Laurent},
  year = {2018},
  month = jun,
  volume = {293},
  pages = {95},
  issn = {0038-0938},
  doi = {10.1007/s11207-018-1313-6},
  abstract = {The internal gravity modes of the Sun are notoriously difficult to detect, and the claimed detection of gravity modes presented by Fossat et al. ( Astron. Astrophys. 604, A40, 2017) is thus very exciting. Given the importance of these modes for understanding solar structure and dynamics, the results must be robust. While Fossat et al. described their method and parameter choices in detail, the sensitivity of their results to several parameters was not presented. Therefore, we test the sensitivity of the results to a selection of the parameters. The most concerning result is that the detection vanishes when we adjust the start time of the 16.5-year velocity time-series by a few hours. We conclude that this reported detection of gravity modes is extremely fragile and should be treated with utmost caution.},
  file = {/Users/Oliver/Zotero/storage/5VQ5GSVU/Schunker et al. - 2018 - Fragile Detection of Solar g-Modes by Fossat et al.pdf},
  journal = {Solar Physics},
  keywords = {Helioseismology,Interior,observations,Oscillations}
}

@article{schuster1898,
  title = {On the Investigation of Hidden Periodicities with Application to a Supposed 26 Day Period of Meteorological Phenomena},
  author = {Schuster, Arthur},
  year = {1898},
  volume = {3},
  pages = {13},
  doi = {10.1029/TM003i001p00013},
  abstract = {1. Obvious and hidden periodicities. A variable quantity may show
periodic changes which become obvious as soon as a sufficient record has
been obtained; such are the semi-diurnal changes of the tides, or the
eleven years recurrence of sunspot maxima. We may call these obvious
periodicities. Most often, however, small periodic variations are hidden
behind irregular fluctuations, and their investigation then becomes a
matter of considerable difficulty.},
  journal = {Terrestrial Magnetism (Journal of Geophysical Research)}
}

@article{scuflaire1974,
  title = {The {{Non Radial Oscillations}} of {{Condensed Polytropes}}},
  author = {Scuflaire, R.},
  year = {1974},
  month = nov,
  volume = {36},
  pages = {107},
  issn = {0004-6361},
  abstract = {Abstract image available at:
http://adsabs.harvard.edu/abs/1974A\&A....36..107S},
  file = {/Users/Oliver/Zotero/storage/IZIW3HB5/Scuflaire - 1974 - The Non Radial Oscillations of Condensed Polytrope.pdf},
  journal = {Astronomy and Astrophysics}
}

@article{seabold+perktold2010,
  title = {Statsmodels: {{Econometric}} and {{Statistical Modeling}} with {{Python}}},
  author = {Seabold, Skipper and Perktold, Josef},
  year = {2010},
  pages = {5},
  abstract = {Statsmodels is a library for statistical and econometric analysis in Python. This paper discusses the current relationship between statistics and Python and open source more generally, outlining how the statsmodels package fills a gap in this relationship. An overview of statsmodels is provided, including a discussion of the overarching design and philosophy, what can be found in the package, and some usage examples. The paper concludes with a look at what the future holds.},
  file = {/Users/Oliver/Zotero/storage/7V785QB4/Seabold and Perktold - 2010 - Statsmodels Econometric and Statistical Modeling .pdf},
  language = {en}
}

@article{see+2019,
  title = {Do {{Non}}-Dipolar {{Magnetic Fields Contribute}} to {{Spin}}-down {{Torques}}?},
  author = {See, Victor and Matt, Sean P. and Finley, Adam J. and Folsom, Colin P. and Boro Saikia, Sudeshna and Donati, Jean-Francois and Fares, Rim and H{\'e}brard, {\'E}lodie M. and Jardine, Moira M. and Jeffers, Sandra V. and Marsden, Stephen C. and Mengel, Matthew W. and Morin, Julien and Petit, Pascal and Vidotto, Aline A. and Waite, Ian A. and {the BCool Collaboration}},
  year = {2019},
  month = dec,
  volume = {886},
  pages = {120},
  issn = {0004-637X},
  doi = {10.3847/1538-4357/ab46b2},
  abstract = {Main-sequence low-mass stars are known to spin down as a consequence of their magnetized stellar winds. However, estimating the precise rate of this spin-down is an open problem. The mass-loss rate, angular momentum loss rate, and magnetic field properties of low-mass stars are
fundamentally linked, making this a challenging task. Of particular interest is the stellar magnetic field geometry. In this work, we consider whether non-dipolar field modes contribute significantly to the spin-down of low-mass stars. We do this using a sample of stars that have all been previously mapped with Zeeman\textendash Doppler imaging. For a given star, as long as its mass-loss rate is below some critical mass-loss rate, only the dipolar fields contribute to its spin-down torque. However, if it has a larger mass-loss rate, higher-order modes need to be considered. For each star, we calculate this critical mass-loss rate, which is a simple function of the field geometry. Additionally, we use two methods of estimating mass-loss rates for our sample of stars. In the majority of cases, we find that the estimated mass-loss rates do not exceed the critical mass-loss rate; hence, the dipolar magnetic field alone is sufficient to determine the spin-down torque. However, we find some evidence that, at large Rossby numbers, non-dipolar modes may start to contribute.},
  file = {/Users/Oliver/Zotero/storage/PZPTY2KT/See et al. - 2019 - Do Non-dipolar Magnetic Fields Contribute to Spin-.pdf},
  journal = {The Astrophysical Journal},
  keywords = {magnetohydrodynamics: MHD,outflows,stars: evolution,stars: low-mass,stars: magnetic field,stars: rotation,stars: winds}
}

@article{serenelli+2017,
  title = {The {{First APOKASC Catalog}} of {{Kepler Dwarf}} and {{Subgiant Stars}}},
  author = {Serenelli, Aldo and Johnson, Jennifer and Huber, Daniel and Pinsonneault, Marc and Ball, Warrick H. and Tayar, Jamie and Silva Aguirre, Victor and Basu, Sarbani and Troup, Nicholas and Hekker, Saskia and Kallinger, Thomas and Stello, Dennis and Davies, Guy R. and Lund, Mikkel N. and Mathur, Savita and Mosser, Benoit and Stassun, Keivan G. and Chaplin, William J. and Elsworth, Yvonne and Garc{\'i}a, Rafael A. and Handberg, Rasmus and Holtzman, Jon and Hearty, Fred and {Garc{\'i}a-Hern{\'a}ndez}, D. A. and Gaulme, Patrick and Zamora, Olga},
  year = {2017},
  month = dec,
  volume = {233},
  pages = {23},
  doi = {10.3847/1538-4365/aa97df},
  abstract = {We present the first APOKASC catalog of spectroscopic and asteroseismic data for dwarfs and subgiants. Asteroseismic data for our sample of 415 objects have been obtained by the Kepler mission in short (58.5 s) cadence, and light curves span from 30 up to more than 1000 days. The spectroscopic parameters are based on spectra taken as part of the Apache Point Observatory Galactic Evolution Experiment and correspond to Data Release 13 of the Sloan Digital Sky Survey. We analyze our data using two independent \{T\}\textsubscript{\{eff\vphantom\}}\vphantom\{\} scales, the spectroscopic values from DR13 and those derived from SDSS griz photometry. We use the differences in our results arising from these choices as a test of systematic temperature uncertainties and find that they can lead to significant differences in the derived stellar properties. Determinations of surface gravity (\{log\}g), mean density (\< {$\rho$} \> ), radius (R), mass (M), and age ({$\tau$}) for the whole sample have been carried out by means of (stellar) grid-based modeling. We have thoroughly assessed random and systematic error sources in the spectroscopic and asteroseismic data, as well as in the grid-based modeling determination of the stellar quantities provided in the catalog. We provide stellar properties determined for each of the two \{T\}\textsubscript{\{eff\vphantom\}}\vphantom\{\} scales. The median combined (random and systematic) uncertainties are 2\% (0.01 dex; \{log\}g), 3.4\% (\< {$\rho$} \> ), 2.6\% (R), 5.1\% (M), and 19\% ({$\tau$}) for the photometric \{T\}\textsubscript{\{eff\vphantom\}}\vphantom\{\} scale and 2\% (\{log\}g), 3.5\% (\< {$\rho$} \> ), 2.7\% (R), 6.3\% (M), and 23\% ({$\tau$}) for the spectroscopic scale. We present comparisons with stellar quantities in the asteroseismic catalog by Chaplin et al. that highlight the importance of having metallicity measurements for determining stellar parameters accurately. Finally, we compare our results with those coming from a variety of sources, including stellar radii determined from TGAS parallaxes and asteroseismic analyses based on individual frequencies. We find a very good agreement for all inferred quantities. The latter comparison, in particular, gives strong support to the determination of stellar quantities based on global seismology, a relevant result for future missions such as TESS and PLATO.},
  file = {/Users/Oliver/Zotero/storage/H47IHD6W/Serenelli et al. - 2017 - The First APOKASC Catalog of Kepler Dwarf and Subg.pdf;/Users/Oliver/Zotero/storage/2QSF68ZH/abstract.html},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en},
  number = {2}
}

@article{sesar+2016,
  title = {A {{Probabilistic Approach}} to {{Fitting Period}}-{{Luminosity Relations}} and {{Validating Gaia Parallaxes}}},
  author = {Sesar, Branimir and Fouesneau, Morgan and {Price-Whelan}, Adrian M. and {Bailer-Jones}, Coryn A. L. and Gould, Andy and Rix, Hans-Walter},
  year = {2016},
  month = nov,
  abstract = {Pulsating stars, such as Cepheids, Miras, and RR Lyrae stars, are important distance indicators and calibrators of the "cosmic distance ladder", and yet their period-luminosity-metallicity (PLZ) relations are still constrained using simple statistical methods that cannot take full advantage of available data. To enable optimal usage of data provided by the Gaia mission, we present a probabilistic approach that simultaneously constrains parameters of PLZ relations and uncertainties in Gaia parallax measurements. We demonstrate this approach by constraining PLZ relations of RR Lyrae stars in near-infrared W1 and W2 bands, using Tycho-Gaia Astrometric Solution (TGAS) parallax measurements for a sample of 123 RR Lyrae stars located within 2.5 kpc of the Sun. The fitted PLZ relations are consistent with previous studies, and in combination with other data, deliver distances precise to 6\% (once various sources of uncertainty are taken into account). To a precision of 0.03 mas (\$1\textbackslash sigma\$), we do not find a statistically significant offset in TGAS parallaxes for this sample of distant RR Lyrae stars (median parallax of 0.8 mas and distance of 1.4 kpc). With only minor modifications, our probabilistic approach can be used to constrain PLZ relations of other pulsating stars, and we intend to apply it to Cepheid and Mira stars in the near future.},
  archivePrefix = {arXiv},
  eprint = {1611.07035},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/B9F8FQ4Z/Sesar et al. - 2016 - A Probabilistic Approach to Fitting Period-Luminos.pdf;/Users/Oliver/Zotero/storage/FINWB2IW/1611.html},
  journal = {arXiv:1611.07035 [astro-ph]},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Instrumentation and Methods for Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{shallue+vanderburg2017,
  title = {Identifying {{Exoplanets}} with {{Deep Learning}}: {{A Five Planet Resonant Chain}} around {{Kepler}}-80 and an {{Eighth Planet}} around {{Kepler}}-90},
  shorttitle = {Identifying {{Exoplanets}} with {{Deep Learning}}},
  author = {Shallue, Christopher J. and Vanderburg, Andrew},
  year = {2017},
  file = {/Users/Oliver/Zotero/storage/QKQNNC9W/kepler90i.pdf},
  journal = {arXiv preprint arXiv:1712.05044}
}

@article{shanks+2018,
  title = {{{GAIA Cepheid}} Parallaxes and '{{Local Hole}}' Relieve \${{H}}\_0\$ Tension},
  author = {Shanks, Tom and Hogarth, Lucy and Metcalfe, Nigel},
  year = {2018},
  month = oct,
  pages = {arXiv:1810.02595},
  abstract = {There has been much discussion of the tension between the values of Hubble's Constant \$H\_0\$ implied by the distance scale and fits to the microwave background's primordial power spectrum. While the latter is fitted by standard cosmological models with \$H\_0=67.4\textbackslash pm0.5\$kms\$\^\{-1\}\$Mpc\$\^\{-1\}\$, the distance scale gives \$H\_0=73.45\textbackslash pm1.66\$kms\$\^\{-1\}\$Mpc\$\^\{-1\}\$, an \$\textbackslash approx10\$\%, \$\textbackslash approx3.5\textbackslash sigma\$ discrepancy. Here we first show that GAIA parallax distances of Milky Way Cepheids may be between \$\textbackslash approx7-18\$\% larger than previously estimated, with the potential to produce a corresponding reduction in the value of \$H\_0\$. Then we show that the existence of an \$\textbackslash approx150\$h\$\^\{-1\}\$Mpc `Local Hole' in the galaxy distribution around our position implies an outflow of \$\textbackslash approx500\$kms\$\^\{-1\}\$ averaging over direction. Accounting for this in the recession velocities of SNIa standard candles out to \$z\textbackslash approx0.1\$ reduces \$H\_0\$ by a further \$\textbackslash approx1.8\$\%, while maintaining reasonable consistency with the supernova Hubble diagram. Combining this result with even an \$\textbackslash approx7\$\% increase in the Cepheid distance scale due to GAIA implies an \$\textbackslash approx9\$\% reduction in the value of the Hubble Constant, decreasing from \$H\_0\textbackslash approx73.45\$ to 67.6 kms\$\^\{-1\}\$Mpc\$\^\{-1\}\$. This would leave the distance scale and Planck Cosmic Microwave Background values entirely consistent, thus potentially relieving the previous \$H\_0\$ tension.},
  file = {/Users/Oliver/Zotero/storage/46PV3NT2/Shanks et al. - 2018 - GAIA Cepheid parallaxes and 'Local Hole' relieve $.pdf;/Users/Oliver/Zotero/storage/VQ9J6IIY/ui.adsabs.harvard.edu.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{sharma+2016,
  title = {Stellar {{Population Synthesis Based Modeling}} of the {{Milky Way Using Asteroseismology}} of 13,000 {{Kepler Red Giants}}},
  author = {Sharma, Sanjib and Stello, Dennis and {Bland-Hawthorn}, Joss and Huber, Daniel and Bedding, Timothy R.},
  year = {2016},
  month = may,
  volume = {822},
  pages = {15},
  doi = {10.3847/0004-637X/822/1/15},
  abstract = {With current space-based missions it is now possible to obtain age-sensitive asteroseismic information for tens of thousands of red giants. This provides a promising opportunity to study the Galactic structure and evolution. We use asteroseismic data of red giants, observed by Kepler, to test the current theoretical framework of modeling the Galaxy based on population synthesis modeling and the use of asteroseismic scaling relations for giants. We use the open source code Galaxia to model the Milky Way and find the distribution of the masses predicted by Galaxia to be systematically offset with respect to the seismically inferred observed masses. The Galactic model overestimates the number of low-mass stars, and these stars are predominantly old and of low metallicity. Using corrections to the \{\{{$\increment$} \}\}{$\nu$} scaling relation suggested by stellar models significantly reduces the disagreement between predicted and observed masses. For a few cases where non-seismic mass estimates are available, the corrections to \{\{{$\increment$} \}\}{$\nu$} also improve the agreement between seismic and non-seismic mass estimates. The disagreement between predictions of the Galactic model and the observations is most pronounced for stars with \{\{[Fe/H]\}\}\textbackslash lt -0.5 and \{\{[Fe/H]\}\}\textbackslash gt 0 or for \{T\}\textsubscript{\{\{eff\vphantom{\}\}}}\vphantom\{\}\vphantom\{\}\textbackslash gt 4700 K. Altering the star formation rate in order to suppress stars older than 10 Gyr improves the agreement for mass but leads to inconsistent color distributions. We also tested the predictions of the TRILEGAL Galactic model. However, unlike Galaxia, it had difficulties in reproducing the photometric properties of the Kepler Input Catalog because it overestimates the number of blue stars. We conclude that either the scaling relations and/or the Galactic models need to be revised to reconcile predictions of theory with asteroseismic observations.},
  file = {/Users/Oliver/Zotero/storage/JSPFKLSQ/Sharma et al. - 2016 - Stellar Population Synthesis Based Modeling of the.pdf;/Users/Oliver/Zotero/storage/KFVPZ5JS/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{sharma+2017,
  title = {Stellar Population Synthesis Based Modelling of the {{Milky Way}} Using Asteroseismology of Dwarfs and Subgiants from {{Kepler}}},
  author = {Sharma, Sanjib and Stello, Dennis and Huber, Daniel and {Bland-Hawthorn}, Joss and Bedding, Timothy R.},
  year = {2017},
  file = {/Users/Oliver/Zotero/storage/D8RQPP4C/1701.02464v1.pdf},
  journal = {arXiv preprint arXiv:1701.02464}
}

@article{sharma+stello2016,
  title = {Asfgrid: {{Asteroseismic}} Parameters for a Star},
  shorttitle = {Asfgrid},
  author = {Sharma, Sanjib and Stello, Dennis},
  year = {2016},
  month = mar,
  pages = {ascl:1603.009},
  abstract = {asfgrid computes asteroseismic parameters for a star with given stellar parameters and vice versa. Written in Python, it determines delta\_nu, nu\_max or masses via interpolation over a grid.},
  file = {/Users/Oliver/Zotero/storage/F2ZI7LC5/ui.adsabs.harvard.edu.html},
  journal = {Astrophysics Source Code Library},
  language = {en}
}

@article{shibahashi+takata1993,
  title = {Theory for the Distorted Dipole Modes of the Rapidly Oscillating {{AP}} Stars: {{A}} Refinement of the Oblique Pulsator Model},
  shorttitle = {Theory for the Distorted Dipole Modes of the Rapidly Oscillating {{AP}} Stars},
  author = {Shibahashi, Hiromoto and Takata, Masao},
  year = {1993},
  month = aug,
  volume = {45},
  pages = {617--641},
  issn = {0004-6264},
  abstract = {Recently, one of the rapidly oscillating Ap stars, HR 3831, has been
found to have an equally split frequency septuplet, though its
oscillation seems to be essentially an axisymmetric dipole mode with
respect to the magnetic axis, which is oblique to the rotation axis
(Kurtz 1992, Kurtz et al. 1993). In order to explain this fine
structure, we consider the magnetic stars by taking account of the
perturbations due to the magnetic fields and the rotation. We show that
the effect of the magnetic field on the axisymmetric dipole modes
distorts the dipole oscillation pattern to have axisymmetric octupole
components, so that the frequency pattern becomes a septuplet rather
than a triplet, and that the additional effect of the rotation causes
the frequency pattern to be asymmetric. The formula allow us to obtain
information concerning the magnetic fields, rotation, and geometrical
configuration of the star from the oscillation data.},
  file = {/Users/Oliver/Zotero/storage/6Z8SGQZZ/Shibahashi and Takata - 1993 - Theory for the distorted dipole modes of the rapid.pdf},
  journal = {Publications of the Astronomical Society of Japan},
  keywords = {A Stars,Eigenvalues,Eigenvectors,Magnetic Dipoles,Magnetic Stars,Peculiar Stars,Perturbation Theory,Seismology,Stellar Magnetic Fields,Stellar Oscillations,Stellar Rotation,Stellar Structure}
}

@article{silvaaguirre+2012,
  title = {Verifying {{Asteroseismically Determined Parameters}} of {{Kepler Stars Using Hipparcos Parallaxes}}: {{Self}}-Consistent {{Stellar Properties}} and {{Distances}}},
  shorttitle = {Verifying {{Asteroseismically Determined Parameters}} of {{Kepler Stars Using Hipparcos Parallaxes}}},
  author = {Silva Aguirre, V. and Casagrande, L. and Basu, S. and Campante, T. L. and Chaplin, W. J. and Huber, D. and Miglio, A. and Serenelli, A. M. and Ballot, J. and Bedding, T. R. and {Christensen-Dalsgaard}, J. and Creevey, O. L. and Elsworth, Y. and Garc{\'i}a, R. A. and Gilliland, R. L. and Hekker, S. and Kjeldsen, H. and Mathur, S. and Metcalfe, T. S. and Monteiro, M. J. P. F. G. and Mosser, B. and Pinsonneault, M. H. and Stello, D. and Weiss, A. and Tenenbaum, P. and Twicken, J. D. and Uddin, K.},
  year = {2012},
  month = sep,
  volume = {757},
  pages = {99},
  issn = {0004-637X},
  doi = {10.1088/0004-637X/757/1/99},
  abstract = {Accurately determining the properties of stars is of prime importance
for characterizing stellar populations in our Galaxy. The field of
asteroseismology has been thought to be particularly successful in such
an endeavor for stars in different evolutionary stages. However, to
fully exploit its potential, robust methods for estimating stellar
parameters are required and independent verification of the results is
mandatory. With this purpose, we present a new technique to obtain
stellar properties by coupling asteroseismic analysis with the InfraRed
Flux Method. By using two global seismic observables and multi-band
photometry, the technique allows us to obtain masses, radii, effective
temperatures, bolometric fluxes, and hence distances for field stars in
a self-consistent manner. We apply our method to 22 solar-like
oscillators in the Kepler short-cadence sample, that have accurate
Hipparcos parallaxes. Our distance determinations agree to better than
5\%, while measurements of spectroscopic effective temperatures and
interferometric radii also validate our results. We briefly discuss the
potential of our technique for stellar population analysis and models of
Galactic Chemical Evolution.},
  file = {/Users/Oliver/Zotero/storage/WU5V5V33/Silva Aguirre et al. - 2012 - Verifying Asteroseismically Determined Parameters .pdf},
  journal = {The Astrophysical Journal},
  keywords = {asteroseismology,parallaxes,stars: distances,stars: fundamental parameters,stars: oscillations}
}

@article{silvaaguirre+2013,
  title = {Stellar {{Ages}} and {{Convective Cores}} in {{Field Main}}-Sequence {{Stars}}: {{First Asteroseismic Application}} to {{Two Kepler Targets}}},
  shorttitle = {Stellar {{Ages}} and {{Convective Cores}} in {{Field Main}}-Sequence {{Stars}}},
  author = {Silva Aguirre, V. and Basu, S. and Brand{\~a}o, I. M. and {Christensen-Dalsgaard}, J. and Deheuvels, S. and Do{\u g}an, G. and Metcalfe, T. S. and Serenelli, A. M. and Ballot, J. and Chaplin, W. J. and Cunha, M. S. and Weiss, A. and Appourchaux, T. and Casagrande, L. and Cassisi, S. and Creevey, O. L. and Garc{\'i}a, R. A. and Lebreton, Y. and Noels, A. and Sousa, S. G. and Stello, D. and White, T. R. and Kawaler, S. D. and Kjeldsen, H.},
  year = {2013},
  month = jun,
  volume = {769},
  pages = {141},
  doi = {10.1088/0004-637X/769/2/141},
  abstract = {Using asteroseismic data and stellar evolution models we obtain the first detection of a convective core in a Kepler field main-sequence star, putting a stringent constraint on the total size of the mixed zone and showing that extra mixing beyond the formal convective boundary exists. In a slightly less massive target the presence of a convective core cannot be conclusively discarded, and thus its remaining main-sequence lifetime is uncertain. Our results reveal that best-fit models found solely by matching individual frequencies of oscillations corrected for surface effects do not always properly reproduce frequency combinations. Moreover, slightly different criteria to define what the best-fit model is can lead to solutions with similar global properties but very different interior structures. We argue that the use of frequency ratios is a more reliable way to obtain accurate stellar parameters, and show that our analysis in field main-sequence stars can yield an overall precision of 1.5\%, 4\%, and 10\% in radius, mass, and age, respectively. We compare our results with those obtained from global oscillation properties, and discuss the possible sources of uncertainties in asteroseismic stellar modeling where further studies are still needed.},
  file = {/Users/Oliver/Zotero/storage/MNUL3X6L/Silva Aguirre et al. - 2013 - Stellar Ages and Convective Cores in Field Main-se.pdf;/Users/Oliver/Zotero/storage/3QJUGH7C/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{silvaaguirre+2015,
  title = {Ages and Fundamental Properties of {{Kepler}} Exoplanet Host Stars from Asteroseismology},
  author = {Silva Aguirre, V. and Davies, G. R. and Basu, S. and {Christensen-Dalsgaard}, J. and Creevey, O. and Metcalfe, T. S. and Bedding, T. R. and Casagrande, L. and Handberg, R. and Lund, M. N. and Nissen, P. E. and Chaplin, W. J. and Huber, D. and Serenelli, A. M. and Stello, D. and Van Eylen, V. and Campante, T. L. and Elsworth, Y. and Gilliland, R. L. and Hekker, S. and Karoff, C. and Kawaler, S. D. and Kjeldsen, H. and Lundkvist, M. S.},
  year = {2015},
  month = sep,
  volume = {452},
  pages = {2127},
  doi = {10.1093/mnras/stv1388},
  abstract = {We present a study of 33 Kepler planet-candidate host stars for which asteroseismic observations have sufficiently high signal-to-noise ratio to allow extraction of individual pulsation frequencies. We implement a new Bayesian scheme that is flexible in its input to process individual oscillation frequencies, combinations of them, and average asteroseismic parameters, and derive robust fundamental properties for these targets. Applying this scheme to grids of evolutionary models yields stellar properties with median statistical uncertainties of 1.2 per cent (radius), 1.7 per cent (density), 3.3 per cent (mass), 4.4 per cent (distance), and 14 per cent (age), making this the exoplanet host-star sample with the most precise and uniformly determined fundamental parameters to date. We assess the systematics from changes in the solar abundances and mixing-length parameter, showing that they are smaller than the statistical errors. We also determine the stellar properties with three other fitting algorithms and explore the systematics arising from using different evolution and pulsation codes, resulting in 1 per cent in density and radius, and 2 per cent and 7 per cent in mass and age, respectively. We confirm previous findings of the initial helium abundance being a source of systematics comparable to our statistical uncertainties, and discuss future prospects for constraining this parameter by combining asteroseismology and data from space missions. Finally, we compare our derived properties with those obtained using the global average asteroseismic observables along with effective temperature and metallicity, finding excellent level of agreement. Owing to selection effects, our results show that the majority of the high signal-to-noise ratio asteroseismic Kepler host stars are older than the Sun.},
  file = {/Users/Oliver/Zotero/storage/3L65BP3A/Silva Aguirre et al. - 2015 - Ages and fundamental properties of Kepler exoplane.pdf;/Users/Oliver/Zotero/storage/ETG2LLJV/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Seismic Age},
  language = {en},
  number = {2}
}

@article{silvaaguirre+2017,
  title = {Standing on the {{Shoulders}} of {{Dwarfs}}: The {{Kepler Asteroseismic LEGACY Sample}}. {{II}}.{{Radii}}, {{Masses}}, and {{Ages}}},
  shorttitle = {Standing on the {{Shoulders}} of {{Dwarfs}}},
  author = {Silva Aguirre, V{\'i}ctor and Lund, Mikkel N. and Antia, H. M. and Ball, Warrick H. and Basu, Sarbani and {Christensen-Dalsgaard}, J{\o}rgen and Lebreton, Yveline and Reese, Daniel R. and Verma, Kuldeep and Casagrande, Luca and Justesen, Anders B. and Mosumgaard, Jakob R. and Chaplin, William J. and Bedding, Timothy R. and Davies, Guy R. and Handberg, Rasmus and Houdek, G{\"u}nter and Huber, Daniel and Kjeldsen, Hans and Latham, David W. and White, Timothy R. and Coelho, Hugo R. and Miglio, Andrea and Rendle, Ben},
  year = {2017},
  month = feb,
  volume = {835},
  pages = {173},
  doi = {10.3847/1538-4357/835/2/173},
  abstract = {We use asteroseismic data from the Kepler satellite to determine fundamental stellar properties of the 66 main-sequence targets observed for at least one full year by the mission. We distributed tens of individual oscillation frequencies extracted from the time series of each star among seven modeling teams who applied different methods to determine radii, masses, and ages for all stars in the sample. Comparisons among the different results reveal a good level of agreement in all stellar properties, which is remarkable considering the variety of codes, input physics, and analysis methods employed by the different teams. Average uncertainties are of the order of{\~ }2\% in radius,{\~ }4\% in mass, and{\~ }10\% in age, making this the best-characterized sample of main-sequence stars available to date. Our predicted initial abundances and mixing-length parameters are checked against inferences from chemical enrichment laws {$\increment$}Y/{$\increment$}Z and predictions from 3D atmospheric simulations. We test the accuracy of the determined stellar properties by comparing them to the Sun, angular diameter measurements, Gaia parallaxes, and binary evolution, finding excellent agreement in all cases and further confirming the robustness of asteroseismically determined physical parameters of stars when individual frequencies of oscillation are available. Baptised as the Kepler dwarfs LEGACY sample, these stars are the solar-like oscillators with the best asteroseismic properties available for at least another decade. All data used in this analysis and the resulting stellar parameters are made publicly available for the community.},
  file = {/Users/Oliver/Zotero/storage/KB2T6A8A/Silva Aguirre et al. - 2017 - Standing on the Shoulders of Dwarfs the Kepler As.pdf;/Users/Oliver/Zotero/storage/YYCS8VYG/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  keywords = {Seismic Age},
  language = {en},
  number = {2}
}

@article{silvaaguirre+2020,
  title = {Detection and Characterisation of Oscillating Red Giants: First Results from the {{TESS}} Satellite},
  shorttitle = {Detection and Characterisation of Oscillating Red Giants},
  author = {Silva Aguirre, V. and Stello, Dennis and Stokholm, Amalie and Mosumgaard, Jakob R. and Ball, Warrick and Basu, Sarbani and Bossini, Diego and Bugnet, Lisa and Buzasi, Derek and Campante, Tiago L. and Carboneau, Lindsey and Chaplin, William J. and Corsaro, Enrico and Davies, Guy R. and Elsworth, Yvonne and Garc{\'i}a, Rafael A. and Gaulme, Patrick and Hall, Oliver J. and Handberg, Rasmus and Hon, Marc and Kallinger, Thomas and Kang, Liu and Lund, Mikkel N. and Mathur, Savita and Mints, Alexey and Mosser, Benoit and Orhan, Zeynep {\c C}elik and Rodrigues, Tha{\'i}se S. and Vrard, Mathieu and Y{\i}ld{\i}z, Mutlu and Zinn, Joel C. and {\"O}rtel, Sibel and Beck, Paul G. and Bell, Keaton J. and Guo, Zhao and Jiang, Chen and Kuszlewicz, James S. and Kuehn, Charles A. and Li, Tanda and Lundkvist, Mia S. and Pinsonneault, Marc and Tayar, Jamie and Cunha, Margarida S. and Hekker, Saskia and Huber, Daniel and Miglio, Andrea and Monteiro, Mario J. P. F. G. and Slumstrup, Ditte and Winther, Mark L. and Angelou, George and Benomar, Othman and B{\'o}di, Attila and De Moura, Bruno L. and Deheuvels, S{\'e}bastien and Derekas, Aliz and Di Mauro, Maria Pia and Dupret, Marc-Antoine and Jim{\'e}nez, Antonio and Lebreton, Yveline and Matthews, Jaymie and Nardetto, Nicolas and Nascimento, Jr and Pereira, Filipe and D{\'i}az, Luisa F. Rodr{\'i}guez and Serenelli, Aldo M. and Spitoni, Emanuele and Stonkut{\.e}, Edita and Su{\'a}rez, Juan Carlos and Szab{\'o}, Robert and Van Eylen, Vincent and Ventura, Rita and Verma, Kuldeep and Weiss, Achim and Wu, Tao and Barclay, Thomas and {Christensen-Dalsgaard}, J{\o}rgen and Jenkins, Jon M. and Kjeldsen, Hans and Ricker, George R. and Seager, Sara and Vanderspek, Roland},
  year = {2020},
  month = jan,
  volume = {889},
  pages = {L34},
  issn = {2041-8213},
  doi = {10.3847/2041-8213/ab6443},
  abstract = {Since the onset of the `space revolution' of high-precision high-cadence photometry, asteroseismology has been demonstrated as a powerful tool for informing Galactic archaeology investigations. The launch of the NASA TESS mission has enabled seismic-based inferences to go full sky \textendash{} providing a clear advantage for large ensemble studies of the different Milky Way components. Here we demonstrate its potential for investigating the Galaxy by carrying out the first asteroseismic ensemble study of red giant stars observed by TESS. We use a sample of 25 stars for which we measure their global asteroseimic observables and estimate their fundamental stellar properties, such as radius, mass, and age. Significant improvements are seen in the uncertainties of our estimates when combining seismic observables from TESS with astrometric measurements from the Gaia mission compared to when the seismology and astrometry are applied separately. Specifically, when combined we show that stellar radii can be determined to a precision of a few percent, masses to 5-10\% and ages to the 20\% level. This is comparable to the precision typically obtained using end-of-mission Kepler data.},
  archivePrefix = {arXiv},
  eprint = {1912.07604},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/PVPHIIGH/Aguirre et al. - 2020 - Detection and characterisation of oscillating red .pdf},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  language = {en},
  number = {2}
}

@article{simonian+2019,
  title = {Rapid {{Rotation}} in the {{Kepler Field}}: {{Not}} a {{Single Star Phenomenon}}},
  shorttitle = {Rapid {{Rotation}} in the {{Kepler Field}}},
  author = {Simonian, Gregory V. A. and Pinsonneault, Marc H. and Terndrup, Donald M.},
  year = {2019},
  month = feb,
  volume = {871},
  pages = {174},
  doi = {10.3847/1538-4357/aaf97c},
  abstract = {Tens of thousands of rotation periods have been measured in the Kepler fields, including a substantial fraction of rapid rotators. We use Gaia parallaxes to distinguish photometric binaries (PBs; from single stars on the unevolved lower main sequence, and compare their distribution of rotation properties to those of single stars both with and without Apache Point Observatory Galactic Evolution Experiment spectroscopic characterization. We find that 59\% of stars with 1.5 day \< P \< 7 day lie 0.3 mag above the main sequence, compared with 28\% of the full rotation sample. The fraction of stars in the same period range is 1.7 {$\pm$} 0.1\% of the total sample analyzed for rotation periods. Both the PB fraction and the fraction of rapid rotators are consistent with a population of non-eclipsing short-period binaries inferred from Kepler eclipsing binary data after correcting for inclination. This suggests that the rapid rotators are dominated by tidally synchronized binaries rather than single stars obeying traditional angular momentum evolution. We caution against interpreting rapid rotation in the Kepler field as a signature of youth. Following up on this new sample of 217 candidate tidally synchronized binaries will help further understand tidal processes in stars.},
  file = {/Users/Oliver/Zotero/storage/8LPF9SZR/Simonian et al. - 2019 - Rapid Rotation in the Kepler Field Not a Single S.pdf;/Users/Oliver/Zotero/storage/P3CM8SWT/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en}
}

@article{simonian+2020,
  title = {Rotation of {{Kepler}} Field Dwarfs and Sub Giants: {{Spectroscopic}} \$v \textbackslash sin {{I}}\$ from {{APOGEE}}},
  shorttitle = {Rotation of {{Kepler}} Field Dwarfs and Sub Giants},
  author = {Simonian, Gregory V. A. and Pinsonneault, Marc H. and Terndrup, Donald M. and {van Saders}, Jennifer L.},
  year = {2020},
  month = jun,
  abstract = {We use 5,337 spectroscopic \$v \textbackslash sin i\$ measurements of Kepler dwarfs and subgiants from the APOGEE survey to study stellar rotation trends. We find a detection threshold of 10 km/s, which allows us to explore the spindown of intermediate-mass stars leaving the main sequence, merger products, young stars, and tidally-synchronized binaries. We see a clear distinction between blue stragglers and the field turnoff in \$\textbackslash alpha\$-rich stars, with a sharp rapid rotation cutoff for blue stragglers consistent with the Kraft break. We also find rapid rotation and RV variability in a sample of red straggler stars, considerably cooler than the giant branch, lending credence to the hypothesis that these are active, tidally-synchronized binaries. We see clear evidence for a transition between rapid and slow rotation on the subgiant branch in the domain predicted by modern angular momentum evolution models. We find substantial agreement between the spectroscopic and photometric properties of KIC targets added by Huber et al (2014) based on 2MASS photometry. For the unevolved lower main sequence, we see the same concentration toward rapid rotation in photometric binaries as that observed in rotation period data, but at an enhanced rate. We attribute this difference to unresolved near-equal luminosity spectroscopic binaries with velocity displacements on the order of the APOGEE resolution. Among cool unevolved stars we find an excess rapid rotator fraction of 4\% caused by pipeline issues with photometric binaries.},
  archivePrefix = {arXiv},
  eprint = {2006.14642},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/XXNX9XKS/Simonian et al. - 2020 - Rotation of Kepler field dwarfs and sub giants Sp.pdf;/Users/Oliver/Zotero/storage/FWSQQ58F/2006.html},
  journal = {arXiv:2006.14642 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{skrutskie+2006,
  title = {The {{Two Micron All Sky Survey}} ({{2MASS}})},
  author = {Skrutskie, M. F. and Cutri, R. M. and Stiening, R. and Weinberg, M. D. and Schneider, S. and Carpenter, J. M. and Beichman, C. and Capps, R. and Chester, T. and Elias, J. and Huchra, J. and Liebert, J. and Lonsdale, C. and Monet, D. G. and Price, S. and Seitzer, P. and Jarrett, T. and Kirkpatrick, J. D. and Gizis, J. E. and Howard, E. and Evans, T. and Fowler, J. and Fullmer, L. and Hurt, R. and Light, R. and Kopan, E. L. and Marsh, K. A. and McCallon, H. L. and Tam, R. and Van Dyk, S. and Wheelock, S.},
  year = {2006},
  month = feb,
  volume = {131},
  pages = {1163},
  doi = {10.1086/498708},
  abstract = {Between 1997 June and 2001 February the Two Micron All Sky Survey (2MASS) collected 25.4 Tbytes of raw imaging data covering 99.998\% of the celestial sphere in the near-infrared J (1.25 {$\mu$}m), H (1.65 {$\mu$}m), and K\textsubscript{s} (2.16 {$\mu$}m) bandpasses. Observations were conducted from two dedicated 1.3 m diameter telescopes located at Mount Hopkins, Arizona, and Cerro Tololo, Chile. The 7.8 s of integration time accumulated for each point on the sky and strict quality control yielded a 10 {$\sigma$} point-source detection level of better than 15.8, 15.1, and 14.3 mag at the J, H, and K\textsubscript{s} bands, respectively, for virtually the entire sky. Bright source extractions have 1 {$\sigma$} photometric uncertainty of {$<$}0.03 mag and astrometric accuracy of order 100 mas. Calibration offsets between any two points in the sky are {$<$}0.02 mag. The 2MASS All-Sky Data Release includes 4.1 million compressed FITS images covering the entire sky, 471 million source extractions in a Point Source Catalog, and 1.6 million objects identified as extended in an Extended Source Catalog.},
  file = {/Users/Oliver/Zotero/storage/6AD4QWJ9/Skrutskie et al. - 2006 - The Two Micron All Sky Survey (2MASS).pdf;/Users/Oliver/Zotero/storage/59XUDTTN/ui.adsabs.harvard.edu.html},
  journal = {The Astronomical Journal},
  language = {en},
  number = {2}
}

@article{skumanich1972,
  title = {{{TIME SCALES FOR Ca}} n {{EMISSION DECAY}}, {{ROTATIONAL BRAKING}}, {{AND LITHIUM DEPLETION}}},
  author = {Skumanich, A},
  year = {1972},
  pages = {4},
  abstract = {A comparison of the Ca+ emission luminosity\textemdash after correction for spectral-type effects\textemdash for the Pleiades, Ursa Major, and Hyades stars and the Sun indicate an emission decay which varies as the inverse square root of the age. Further, the rotational decay curve is found to satisfy the same law. It is further suggested that lithium depletion follows the same law but only as far as the Hyades age, after which the depletion proceeds exponentially. Since Ca+ emission is linearly proportional to magnetic field strength at the surface, one can predict that the surface fields are proportional to angular velocity and decay as the inverse square root. The above results are predicated on the standard Hyades age (0.4 billion years).},
  file = {/Users/Oliver/Zotero/storage/SYGPJ843/Skumanich - TIME SCALES FOR Ca n EMISSION DECAY, ROTATIONAL BR.pdf},
  journal = {ApJ. . .},
  language = {en}
}

@article{slumstrup+2018,
  title = {Systematic {{Differences}} in {{Spectroscopic Analysis}} of {{Red Giants}}},
  author = {Slumstrup, Ditte and Grundahl, Frank and Aguirre, Victor Silva and Brogaard, Karsten},
  year = {2018},
  month = dec,
  pages = {arXiv:1812.05630},
  abstract = {A spectroscopic analysis of stellar spectra can be carried out using different approaches; different methods, line lists, atomic parameters, solar abundances etc. The resulting atmospheric parameters from these choices can vary beyond quoted uncertainties in the literature. Here we characterize these differences by systematically comparing some of the commonly adopted ingredients; line lists, equivalent width measurements and atomic parameters. High resolution and high signal-to-noise spectroscopic data of one helium-core-burning red giant star in each of the three open clusters, NGC6819, M67 and NGC188 have been obtained with the FIES spectrograph at the Nordic Optical Telescope. The M67 target has been used to benchmark the analysis, as it is a well studied cluster with asteroseismic data from the K2 mission. For the other two clusters we have obtained higher quality data than previously analyzed, which allows us to establish their chemical composition more securely. Using a line by line analysis, we tested several different combinations of line lists and programs to measure equivalent widths of absorption lines to characterize systematic differences within the same spectroscopic method. The obtained parameters for the benchmark star in M67 vary up to \textasciitilde 170 K in T\_eff, \textasciitilde 0.4 dex in log g and \textasciitilde 0.25 dex in [Fe/H] between the tested setups. Using the combination of equivalent width measurement program and line list that best reproduce the inferred log g from asteroseismology, we determined the atmospheric parameters for the three stars and securely established the chemical composition of NGC6819 to be \textasciitilde solar, [Fe/H]=-0.02+-0.01 dex. We have highlighted the significantly different results obtained with different combinations of line lists, programs and atomic parameters, which emphasize the importance of benchmark stars studied with several different methods to anchor spectroscopic analyses.},
  file = {/Users/Oliver/Zotero/storage/QEIINJ2F/Slumstrup et al. - 2018 - Systematic Differences in Spectroscopic Analysis o.pdf;/Users/Oliver/Zotero/storage/ZGF5DXIC/ui.adsabs.harvard.edu.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{soderblom2010,
  title = {The {{Ages}} of {{Stars}}},
  author = {Soderblom, David R.},
  year = {2010},
  month = sep,
  volume = {48},
  pages = {581},
  doi = {10.1146/annurev-astro-081309-130806},
  abstract = {The age of an individual star cannot be measured, only estimated through mostly model-dependent or empirical methods, and no single method works well for a broad range of stellar types or for a full range in age. This review presents a summary of the available techniques for age-dating stars and ensembles of stars, their realms of applicability, and their strengths and weaknesses. My emphasis is on low-mass stars because they are present from all epochs of star formation in the Galaxy and because they present both special opportunities and problems. The ages of open clusters are important for understanding the limitations of stellar models and for calibrating empirical age indicators. For individual stars, a hierarchy of quality for the available age-dating methods is described. Although our present ability to determine the ages of even the nearest stars is mediocre, the next few years hold great promise as asteroseismology probes beyond stellar surfaces and starts to provide precise interior properties of stars and as models continue to improve when stressed by better observations.},
  file = {/Users/Oliver/Zotero/storage/A5WHRAWP/Soderblom - 2010 - The Ages of Stars.pdf;/Users/Oliver/Zotero/storage/PEGBPJEB/ui.adsabs.harvard.edu.html},
  journal = {Annual Review of Astronomy and Astrophysics},
  language = {en}
}

@article{sonoi+2017,
  title = {On the Computation of Eigenfrequencies for Equilibrium Models Including Turbulent Pressure},
  author = {Sonoi, T. and Belkacem, K. and Dupret, M.-A. and Samadi, R. and Ludwig, H.-G. and Caffau, E. and Mosser, B.},
  year = {2017},
  file = {/Users/Oliver/Zotero/storage/6Q2558UE/1701.07244.pdf},
  journal = {arXiv preprint arXiv:1701.07244}
}

@article{southworth+2016,
  title = {Detection of the Atmosphere of the 1.6 {{Earth}} Mass Exoplanet {{GJ}} 1132b},
  author = {Southworth, John and Mancini, Luigi and Madhusudhan, Nikku and Molliere, Paul and Ciceri, Simona and Henning, Thomas},
  year = {2016},
  month = dec,
  volume = {1612},
  pages = {arXiv:1612.02425},
  abstract = {Detecting the atmospheres of low-mass low-temperature exoplanets is a high-priority goal on the path to ultimately detect biosignatures in the atmospheres of habitable exoplanets. High-precision HST observations of several super-Earths with equilibrium temperatures below 1000 K have to date all resulted in featureless transmission spectra, which have been suggested to be due to high-altitude clouds. We report the detection of an atmospheric feature in the atmosphere of a 1.6 Mearth transiting exoplanet, GJ 1132b, with an equilibrium temperature of \textasciitilde 600 K and orbiting a nearby M dwarf. We present observations of nine transits of the planet obtained simultaneously in the griz and JHK passbands. We find an average radius of 1.44 +/- 0.21 Rearth for the planet, averaged over all the passbands, which can be decomposed into a "surface radius" at \textasciitilde 1.35 Rearth, and higher contributions in the z and K bands. The z-band radius is 4 sigma higher than the continuum, suggesting a strong detection of an atmosphere. We deploy a suite of tests to verify the reliability of the transmission spectrum, which are greatly helped by the existence of repeat observations. The large z-band transit depth indicates strong opacity from H2O and/or CH4 or an hitherto unconsidered opacity. A surface radius of 1.35 +/- 0.21 Rearth allows for a wide range of interior compositions ranging from a nearly Earth-like rocky interior, with \textasciitilde 70\% silicate and \textasciitilde 30\% Fe, to a substantially H2O-rich water world. New observations with HST and existing ground-based facilities would be able to confirm the present detection and further constrain the atmospheric composition of the planet.},
  journal = {ArXiv e-prints},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics}
}

@article{stassun+2017,
  title = {Empirical, {{Accurate Masses}} and {{Radii}} of {{Single Stars}} with {{TESS}} and {{Gaia}}},
  author = {Stassun, Keivan G. and Corsaro, Enrico and Pepper, Joshua and Gaudi, Scott},
  year = {2017},
  month = oct,
  abstract = {We present a methodology for the determination of empirical masses of single stars through the combination of three direct observables with Gaia and TESS: (i) the surface gravity via granulation-driven variations in the TESS light curve, (ii) the bolometric flux at Earth via the broadband spectral energy distribution, and (iii) the distance via the Gaia parallax. We demonstrate the method using 675 Kepler stars for which these measures are available in the literature, and show that the stellar masses can be measured with this method to a precision of \$\textbackslash sim\$25\%, limited by the surface-gravity precision of the granulation "flicker" method (\$\textbackslash sim\$0.1 dex) and by the parallax uncertainties (\$\textbackslash sim\$10\% for the Kepler sample). We explore the impact of expected improvements in the surface gravity determinations---through the application of granulation background fitting and the use of recently published granulation-metallicity relations---and improvements in the parallaxes with the arrival of the Gaia second data release. We show that the application of this methodology to stars that will be observed by TESS should yield radii good to a few percent and masses good to \$\textbackslash approx\$10\%. Importantly, the method does not require the presence of an orbiting, eclipsing, or transiting body, nor does it require spatial resolution of the stellar surface. Thus we can anticipate the determination of fundamental, accurate stellar radii and masses for millions of bright single stars---across the entire sky and spanning the Hertzsprung-Russell diagram---including those that will ultimately be found to host planets.},
  archivePrefix = {arXiv},
  eprint = {1710.01460},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/VNDXW5ZT/Stassun et al. - 2017 - Empirical, Accurate Masses and Radii of Single Sta.pdf;/Users/Oliver/Zotero/storage/4EZF5HDJ/1710.html},
  journal = {arXiv:1710.01460 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{stassun+torres2016,
  title = {Evidence for a Systematic Offset of \$-\$0.25 Mas in the {{Gaia DR1}} Parallaxes},
  author = {Stassun, Keivan G. and Torres, Guillermo},
  year = {2016},
  month = sep,
  pages = {arXiv:1609.05390},
  abstract = {We test the parallaxes reported in the Gaia first data release using the sample of eclipsing binaries with accurate, empirical distances from Stassun \textbackslash\& Torres (2016). We find an average offset of \$-\$0.25\$\textbackslash pm\$0.05 mas in the sense of the Gaia parallaxes being too small (i.e., the distances too long). The offset does not depend strongly on obvious parameters such as color or brightness. However, we find with high confidence that the offset may depend on ecliptic latitude: the mean offset is \$-\$0.38\$\textbackslash pm\$0.06 mas in the ecliptic north and \$-\$0.05\$\textbackslash pm\$0.09 mas in the ecliptic south. The ecliptic latitude dependence may also be represented by the linear relation, \$\textbackslash Delta\textbackslash pi \textbackslash approx -0.22(\textbackslash pm0.05) -0.003(\textbackslash pm0.001)\textbackslash times\textbackslash beta\$ mas (\$\textbackslash beta\$ in degrees). Finally, there is a possible dependence of the parallax offset on distance, with the offset becoming negligible for \$\textbackslash pi\textbackslash lesssim 1\$ mas; we discuss whether this could be caused by a systematic error in the eclipsing binary distance scale, and reject this interpretation as unlikely.},
  file = {/Users/Oliver/Zotero/storage/C2QCATFY/Stassun and Torres - 2016 - Evidence for a systematic offset of $-$0.25 mas in.pdf;/Users/Oliver/Zotero/storage/JQQ2VGYH/ui.adsabs.harvard.edu.html},
  journal = {ArXiv e-prints},
  language = {en}
}

@article{stassun+torres2018,
  title = {Evidence for a {{Systematic Offset}} of -80 {$M$}as in the {{Gaia DR2 Parallaxes}}},
  author = {Stassun, Keivan G. and Torres, Guillermo},
  year = {2018},
  month = jul,
  volume = {862},
  pages = {61},
  doi = {10.3847/1538-4357/aacafc},
  abstract = {We reprise the analysis of Stassun \& Torres, comparing the parallaxes of the eclipsing binaries reported in that paper to the parallaxes newly reported in the Gaia second data release (DR2). We find evidence for a systematic offset of -82 {$\pm$} 33 {$\mu$}as, in the sense of the Gaia parallaxes being too small, for brightnesses (G {$\lessequivlnt$} 12) and for distances (0.03-3 kpc) in the ranges spanned by the eclipsing binary sample. The offset does not appear to depend strongly on distance within this range, though there is marginal evidence that the offset increases (becomes slightly more negative) for distances {$\greaterequivlnt$}1 kpc, up to the 3 kpc distances probed by the test sample. The offset reported here is consistent with the expectation that global systematics in the Gaia DR2 parallaxes are below 100 {$\mu$}as.},
  file = {/Users/Oliver/Zotero/storage/6YHQSRZY/Stassun and Torres - 2018 - Evidence for a Systematic Offset of −80 μas in the.pdf;/Users/Oliver/Zotero/storage/H4PGZN55/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{stello+2008,
  title = {Oscillating {{K Giants}} with the {{WIRE Satellite}}: {{Determination}} of {{Their Asteroseismic Masses}}},
  shorttitle = {Oscillating {{K Giants}} with the {{WIRE Satellite}}},
  author = {Stello, D. and Bruntt, H. and Preston, H. and Buzasi, D.},
  year = {2008},
  month = feb,
  volume = {674},
  pages = {L53},
  issn = {0004-637X},
  doi = {10.1086/528936},
  abstract = {Mass estimates of K giants are generally very uncertain. Traditionally,
stellar masses of single field stars are determined by comparing their
location in the Hertzsprung-Russell diagram with stellar evolutionary
models. Applying an additional method to determine the mass is therefore
of significant interest for understanding stellar evolution. We present
the time series analysis of 11 K giants recently observed with the WIRE
satellite. With this comprehensive sample, we report the first
confirmation that the characteristic acoustic frequency,
{$\nu$}max, can be predicted for K giants by scaling from the
solar acoustic cutoff frequency. We are further able to utilize our
measurements of {$\nu$}max to determine an asteroseismic mass
for each star with a lower uncertainty compared to the traditional
method, for most stars in our sample. This indicates good prospects for
the application of our method on the vast amounts of data that will soon
come from the COROT and Kepler space missions.},
  file = {/Users/Oliver/Zotero/storage/D6AV8XCV/Stello et al. - 2008 - Oscillating K Giants with the WIRE Satellite Dete.pdf},
  journal = {The Astrophysical Journal Letters},
  keywords = {stars: fundamental parameters,stars: interiors,stars: oscillations}
}

@article{stello+2009,
  title = {Radius Determination of Solar-Type Stars Using Asteroseismology: {{What}} to Expect from the {{Kepler}} Mission},
  shorttitle = {Radius Determination of Solar-Type Stars Using Asteroseismology},
  author = {Stello, D. and Chaplin, W. J. and Bruntt, H. and Creevey, O. L. and {Garc{\'i}a-Hern{\'a}ndez}, A. and Monteiro, M. J. P. F. G. and Moya, A. and Quirion, P.-O. and Sousa, S. G. and Su{\'a}rez, J.-C. and Appourchaux, T. and Arentoft, T. and Ballot, J. and Bedding, T. R. and {Christensen-Dalsgaard}, J. and Elsworth, Y. and Fletcher, S. T. and Garc{\'i}a, R. A. and Houdek, G{\"u}nter and {Jim{\'e}nez-Reyes}, S. J. and Kjeldsen, H. and New, R. and R{\'e}gulo, C. and Salabert, D. and Toutain, T.},
  year = {2009},
  month = aug,
  volume = {700},
  pages = {1589--1602},
  issn = {0004-637X, 1538-4357},
  doi = {10.1088/0004-637X/700/2/1589},
  abstract = {For distant stars, as observed by the NASA Kepler satellite, parallax information is currently of fairly low quality and is not complete. This limits the precision with which the absolute sizes of the stars and their potential transiting planets can be determined by traditional methods. Asteroseismology will be used to aid the radius determination of stars observed during NASA's Kepler mission. We report on the recent asteroFLAG hare-and-hounds Exercise\#2, where a group of `hares' simulated data of F-K main-sequence stars that a group of `hounds' sought to analyze, aimed at determining the stellar radii. Based on the asteroseismic large frequency spacing, obtained from simulations of 4-year time series data from the Kepler mission, we demonstrate that the stellar radii can be correctly and precisely determined, when combined with traditional stellar parameters from the Kepler Input Catalogue. The radii found by the various methods used by each independent hound generally agree with the true values of the artificial stars to within 3\%, when the large frequency spacing is used. This is 5--10 times better than the results where seismology is not applied. These results give strong confidence that radius estimation can be performed to better than 3\% for solar-like stars using automatic pipeline reduction. Even when the stellar distance and luminosity are unknown we can obtain the same level of agreement.},
  archivePrefix = {arXiv},
  eprint = {0906.0766},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/VC8PECA4/Stello et al. - 2009 - Radius determination of solar-type stars using ast.pdf;/Users/Oliver/Zotero/storage/N2NL7CD7/0906.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {2}
}

@article{stello+2009a,
  title = {The Relation between \$\textbackslash{{Delta}}\textbackslash nu\$ and \$\textbackslash nu\_\{max\}\$ for Solar-like Oscillations},
  author = {Stello, D. and Chaplin, W. J. and Basu, S. and Elsworth, Y. and Bedding, T. R.},
  year = {2009},
  month = nov,
  volume = {400},
  pages = {L80-L84},
  issn = {17453925, 17453933},
  doi = {10.1111/j.1745-3933.2009.00767.x},
  abstract = {Establishing relations between global stellar parameters and asteroseismic quantities can help improve our understanding of stellar astrophysics and facilitate the interpretation of observations. We present an observed relation between the large frequency separation, \$\textbackslash Delta\textbackslash nu\$, and the frequency of maximum power, \$\textbackslash nu\_\{max\}\$. We find that \$\textbackslash Delta\textbackslash nu\$ is proportional to \$(\textbackslash nu\_\{max\})\^0.77\$, allowing prediction of \$\textbackslash Delta\textbackslash nu\$ to about 15 per cent given \$\textbackslash nu\_\{max\}\$. Our result is further supported by established scaling relations for \$\textbackslash Delta\textbackslash nu\$ and \$\textbackslash nu\_\{max\}\$ and by extended stellar model calculations, which confirm that \$\textbackslash Delta\textbackslash nu\$ can be estimated using this relation for basically any star showing solar-like oscillations in the investigated range (0.5},
  archivePrefix = {arXiv},
  eprint = {0909.5193},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/PZSFXLL6/Stello et al. - 2009 - The relation between $Deltanu$ and $nu_ max $ f.pdf;/Users/Oliver/Zotero/storage/QG3QYB3V/0909.html},
  journal = {Monthly Notices of the Royal Astronomical Society: Letters},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{stello+2011,
  title = {An Asteroseismic Membership Study of the Red Giants in Three Open Clusters Observed by {{Kepler}}: {{NGC6791}}, {{NGC6819}}, and {{NGC6811}}},
  shorttitle = {An Asteroseismic Membership Study of the Red Giants in Three Open Clusters Observed by {{Kepler}}},
  author = {Stello, D. and Meibom, S. and Gilliland, R. L. and Grundahl, F. and Hekker, S. and Mosser, B. and Kallinger, T. and Mathur, S. and Garc{\'i}a, R. A. and Huber, D. and Basu, S. and Bedding, T. R. and Brogaard, K. and Chaplin, W. J. and Elsworth, Y. P. and {Molenda-{\.Z}akowicz}, J. and Szab{\'o}, R. and Still, M. and Jenkins, J. M. and {Christensen-Dalsgaard}, J. and Kjeldsen, H. and Serenelli, A. M. and Wohler, B.},
  year = {2011},
  month = sep,
  volume = {739},
  pages = {13},
  issn = {0004-637X, 1538-4357},
  doi = {10.1088/0004-637X/739/1/13},
  abstract = {Studying star clusters offers significant advances in stellar astrophysics due to the combined power of having many stars with essentially the same distance, age, and initial composition. This makes clusters excellent test benches for verification of stellar evolution theory. To fully exploit this potential, it is vital that the star sample is uncontaminated by stars that are not members of the cluster. Techniques for determining cluster membership therefore play a key role in the investigation of clusters. We present results on three clusters in the Kepler field of view based on a newly established technique that uses asteroseismology to identify fore- or background stars in the field, which demonstrates advantages over classical methods such as kinematic and photometry measurements. Four previously identified seismic non-members in NGC6819 are confirmed in this study, and three additional non-members are found -- two in NGC6819 and one in NGC6791. We further highlight which stars are, or might be, affected by blending, which needs to be taken into account when analysing these Kepler data.},
  archivePrefix = {arXiv},
  eprint = {1107.1234},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/WMEQ99ZC/Stello et al. - 2011 - An asteroseismic membership study of the red giant.pdf;/Users/Oliver/Zotero/storage/S94HRJF5/1107.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{stello+2013,
  title = {Period {{Spacings}} of {{Most Red Giants Observed}} by {{Kepler}}},
  author = {Stello, D. and Huber, D. and Bedding, T. R. and Benomar, O. and Bildsten, L. and Elsworth, Y. and Gilliland, R. L. and Mosser, B. and Paxton, B. and White, T. R.},
  year = {2013},
  month = dec,
  volume = {479},
  pages = {167},
  abstract = {Of the more than 150 000 targets followed by the Kepler mission, about 10\% were selected as red giants. Due to their high scientific value, in particular for Galaxy population studies and stellar structure and evolution, their Kepler light curves were made public in late 2011. More than 13 000 (over 85\%) of these stars show intrinsic flux variability caused by solar-like oscillations making them ideal for large scale asteroseismic investigations. We automatically extracted individual frequencies and measured the period spacings of the dipole modes in nearly every red giant. These measurements naturally classify the stars into various populations, such as the Red Giant Branch, the low-mass (M / M\textsubscript{{$\Sun$}} {$\lessequivlnt$} 1.8) helium-core-burning Red Clump, and the higher-mass (M / M\textsubscript{{$\Sun$}} {$\greaterequivlnt$} 1.8) secondary clump. The period spacings also reveal that a large fraction of the stars show rotationally induced frequency splittings. This sample of stars will undoubtedly provide an extremely valuable source for studying the stellar population in the direction of the Kepler field, in particular when combined with complementary spectroscopic surveys.},
  file = {/Users/Oliver/Zotero/storage/4ZJAHIHG/Stello et al. - 2013 - Period Spacings of Most Red Giants Observed by Kep.pdf;/Users/Oliver/Zotero/storage/NV8EZWIZ/ui.adsabs.harvard.edu.html},
  journal = {Progress in Physics of the Sun and Stars: A New Era in Helio- and Asteroseismology},
  language = {en}
}

@article{stello+2015,
  title = {Oscillating {{Red Giants Observed}} during {{Campaign}} 1 of the {{Kepler K2 Mission}}: {{New Prospects}} for {{Galactic Archaeology}}},
  shorttitle = {Oscillating {{Red Giants Observed}} during {{Campaign}} 1 of the {{Kepler K2 Mission}}},
  author = {Stello, Dennis and Huber, Daniel and Sharma, Sanjib and Johnson, Jennifer and Lund, Mikkel N. and Handberg, Rasmus and Buzasi, Derek L. and Silva Aguirre, Victor and Chaplin, William J. and Miglio, Andrea and Pinsonneault, Marc and Basu, Sarbani and Bedding, Tim R. and {Bland-Hawthorn}, Joss and Casagrande, Luca and Davies, Guy and Elsworth, Yvonne and Garcia, Rafael A. and Mathur, Savita and Mauro, Di and Pia, Maria and Mosser, Benoit and Schneider, Donald P. and Serenelli, Aldo and Valentini, Marica},
  year = {2015},
  month = aug,
  volume = {809},
  pages = {L3},
  doi = {10.1088/2041-8205/809/1/L3},
  abstract = {NASA's re-purposed Kepler mission\textemdash dubbed K2\textemdash has brought new scientific opportunities that were not anticipated for the original Kepler mission. One science goal that makes optimal use of K2's capabilities, in particular its 360\textdegree{} ecliptic field of view, is galactic archaeology\textemdash the study of the evolution of the Galaxy from the fossil stellar record. The thrust of this research is to exploit high-precision, time-resolved photometry from K2 in order to detect oscillations in red giant stars. This asteroseismic information can provide estimates of stellar radius (hence distance), mass, and age of vast numbers of stars across the Galaxy. Here we present the initial analysis of a subset of red giants, observed toward the north galactic gap, during the mission's first full science campaign. We investigate the feasibility of using K2 data for detecting oscillations in red giants that span a range in apparent magnitude and evolutionary state (hence intrinsic luminosity). We demonstrate that oscillations are detectable for essentially all cool giants within the \{log\}g range{\~ }1.9-3.2. Our detection is complete down to \{\textbackslash text\{Kp\}\}{\~ } 14.5, which results in a seismic sample with little or no detection bias. This sample is ideally suited to stellar population studies that seek to investigate potential shortcomings of contemporary Galaxy models.},
  file = {/Users/Oliver/Zotero/storage/FWLHV97C/Stello et al. - 2015 - Oscillating Red Giants Observed during Campaign 1 .pdf;/Users/Oliver/Zotero/storage/7V32NMRF/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{stello+2016,
  title = {The {{K2 M67 Study}}: {{Revisiting Old Friends}} with {{K2 Reveals Oscillating Red Giants}} in the {{Open Cluster M67}}},
  shorttitle = {The {{K2 M67 Study}}},
  author = {Stello, Dennis and Vanderburg, Andrew and Casagrande, Luca and Gilliland, Ron and Silva Aguirre, Victor and Sandquist, Eric and Leiner, Emily and Mathieu, Robert and Soderblom, David R.},
  year = {2016},
  month = dec,
  volume = {832},
  pages = {133},
  doi = {10.3847/0004-637X/832/2/133},
  abstract = {Observations of stellar clusters have had a tremendous impact in forming our understanding of stellar evolution. The open cluster M67 has a particularly important role as a calibration benchmark for stellar evolution theory due to its near-solar composition and age. As a result, it has been observed extensively, including attempts to detect solar-like oscillations in its main sequence and red giant stars. However, any asteroseismic inference has so far remained elusive due to the difficulty in measuring these extremely low-amplitude oscillations. Here we report the first unambiguous detection of solar-like oscillations in the red giants of M67. We use data from the Kepler ecliptic mission, K2, to measure the global asteroseismic properties. We find a model-independent seismic-informed distance of 816 {$\pm$} 11 pc, or \{(m-M)\}\textsubscript{0} = 9.57+/- 0.03 mag, an average red giant mass of 1.36+/- 0.01 \{M\}\textsubscript{{$\Sun$} }, in agreement with the dynamical mass from an eclipsing binary near the cluster turn-off, and ages of individual stars compatible with isochrone fitting. We see no evidence of strong mass loss on the red giant branch. We also determine seismic \{log\}g of all the cluster giants with a typical precision of{\~ } 0.01 dex. Our results generally show good agreement with independent methods and support the use of seismic scaling relations to determine global properties of red giant stars with near-solar metallicity. We further illustrate that the data are of such high quality that future work on individual mode frequencies should be possible, which would extend the scope of seismic analysis of this cluster.},
  file = {/Users/Oliver/Zotero/storage/62ABTP65/Stello et al. - 2016 - The K2 M67 Study Revisiting Old Friends with K2 R.pdf;/Users/Oliver/Zotero/storage/G3RAJ3GB/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{stello+2017,
  title = {The {{K2 Galactic Archaeology Program Data Release}} 1: {{Asteroseismic}} Results from {{Campaign}} 1},
  shorttitle = {The {{K2 Galactic Archaeology Program Data Release}} 1},
  author = {Stello, D. and Zinn, J. and Elsworth, Y. and Garcia, R. A. and Kallinger, T. and Mathur, S. and Mosser, B. and Sharma, S. and Chaplin, W. J. and Davies, G. and Huber, D. and Jones, C. D. and Miglio, A. and Aguirre, V. S.},
  year = {2017},
  month = jan,
  volume = {835},
  pages = {83},
  issn = {1538-4357},
  doi = {10.3847/1538-4357/835/1/83},
  abstract = {NASA's K2 mission is observing tens of thousands of stars along the ecliptic, providing data suitable for large scale asteroseismic analyses to inform galactic archaeology studies. Its first campaign covered a field near the north galactic cap, a region never covered before by large asteroseismic-ensemble investigations, and was therefore of particular interest for exploring this part of our Galaxy. Here we report the asteroseismic analysis of all stars selected by the K2 Galactic Archaeology Program during the mission's "North Galactic Cap" campaign 1. Our consolidated analysis uses six independent methods to measure the global seismic properties, in particular the large frequency separation, and the frequency of maximum power. From the full target sample of 8630 stars we find about 1200 oscillating red giants, a number comparable with estimates from galactic synthesis modeling. Thus, as a valuable by-product we find roughly 7500 stars to be dwarfs, which provide a sample well suited for galactic exoplanet occurrence studies because they originate from our simple and easily reproducible selection function. In addition, to facilitate the full potential of the data set for galactic archaeology we assess the detection completeness of our sample of oscillating red giants. We find the sample is at least near complete for stars with 40 {$<$} numax/microHz {$<$} 270, and numax\_detec {$<$} 2.6*1e6 * 2e-Kp microHz. There is a detection bias against helium core burning stars with numax \textasciitilde{} 30 microHz, affecting the number of measurements of DeltaNu and possibly also numax. Although we can detect oscillations down to Kp = 15, our campaign 1 sample lacks enough faint giants to assess the detection completeness for stars fainter than Kp \textasciitilde{} 14.5.},
  archivePrefix = {arXiv},
  eprint = {1611.09852},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/8RIFMKR7/Stello et al. - 2017 - The K2 Galactic Archaeology Program Data Release 1.pdf;/Users/Oliver/Zotero/storage/WF6IPNZ3/1611.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{sullivan+2015,
  title = {The {{Transiting Exoplanet Survey Satellite}}: {{Simulations}} of {{Planet Detections}} and {{Astrophysical False Positives}}},
  shorttitle = {The {{Transiting Exoplanet Survey Satellite}}},
  author = {Sullivan, Peter W. and Winn, Joshua N. and {Berta-Thompson}, Zachory K. and Charbonneau, David and Deming, Drake and Dressing, Courtney D. and Latham, David W. and Levine, Alan M. and McCullough, Peter R. and Morton, Timothy and Ricker, George R. and Vanderspek, Roland and Woods, Deborah},
  year = {2015},
  month = aug,
  volume = {809},
  pages = {77},
  issn = {0004-637X},
  doi = {10.1088/0004-637X/809/1/77},
  abstract = {The Transiting Exoplanet Survey Satellite (TESS) is a NASA-sponsored
Explorer mission that will perform a wide-field survey for planets that
transit bright host stars. Here, we predict the properties of the
transiting planets that TESS will detect along with the EB stars that
produce false-positive photometric signals. The predictions are based on
Monte Carlo simulations of the nearby population of stars, occurrence
rates of planets derived from Kepler, and models for the photometric
performance and sky coverage of the TESS cameras. We expect that TESS
will find approximately 1700 transiting planets from 2\texttimes{}
\{10\}5 pre-selected target stars. This includes 556 planets
smaller than twice the size of Earth, of which 419 are hosted by M dwarf
stars and 137 are hosted by FGK dwarfs. Approximately 130 of the R\textbackslash lt 2
\{R\}\textbackslash oplus planets will have host stars brighter than
\{K\}s=9. Approximately 48 of the planets with R\textbackslash lt 2
\{R\}\textbackslash oplus lie within or near the habitable zone (0.2\textbackslash lt
S/\{S\}\textbackslash oplus \textbackslash lt 2); between 2 and 7 such planets have host
stars brighter than \{K\}s=9. We also expect approximately 1100
detections of planets with radii 2-4 \{R\}\textbackslash oplus , and 67
planets larger than 4 \{R\}\textbackslash oplus . Additional planets larger
than 2 \{R\}\textbackslash oplus can be detected around stars that are not
among the pre-selected target stars, because TESS will also deliver
full-frame images at a 30-minute cadence. The planet detections are
accompanied by over 1000 astrophysical false positives. We discuss how
TESS data and ground-based observations can be used to distinguish the
false positives from genuine planets. We also discuss the prospects for
follow-up observations to measure the masses and atmospheres of the TESS
planets.},
  file = {/Users/Oliver/Zotero/storage/PNWNNRXE/Sullivan et al. - 2015 - The Transiting Exoplanet Survey Satellite Simulat.pdf},
  journal = {The Astrophysical Journal},
  keywords = {planets and satellites: detection,space vehicles: instruments,surveys}
}

@article{tassoul1980,
  title = {Asymptotic Approximations for Stellar Nonradial Pulsations},
  author = {Tassoul, M.},
  year = {1980},
  month = aug,
  volume = {43},
  pages = {469},
  issn = {0067-0049, 1538-4365},
  doi = {10.1086/190678},
  abstract = {The problem of linear nonradial oscillations in stars is reconsidered using sound asymptotic expansions. High-order p- and g-modes are investigated. In the case of g-modes, the possibility of resonance occurs when the model possesses more than one zone in which spatial oscillations may occur.},
  file = {/Users/Oliver/Zotero/storage/4SWUTQMY/Tassoul - 1980 - Asymptotic approximations for stellar nonradial pu.pdf},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en}
}

@article{tayar+2015,
  title = {Rapid {{Rotation}} of {{Low}}-Mass {{Red Giants Using APOKASC}}: {{A Measure}} of {{Interaction Rates}} on the {{Post}}-Main-Sequence},
  shorttitle = {Rapid {{Rotation}} of {{Low}}-Mass {{Red Giants Using APOKASC}}},
  author = {Tayar, Jamie and Ceillier, Tugdual and {Garc{\'i}a-Hern{\'a}ndez}, D. A. and Troup, Nicholas W. and Mathur, Savita and Garc{\'i}a, Rafael A. and Zamora, O. and Johnson, Jennifer A. and Pinsonneault, Marc H. and M{\'e}sz{\'a}ros, Szabolcs and Allende Prieto, Carlos and Chaplin, William J. and Elsworth, Yvonne and Hekker, Saskia and Nidever, David L. and Salabert, David and Schneider, Donald P. and Serenelli, Aldo and Shetrone, Matthew and Stello, Dennis},
  year = {2015},
  month = jul,
  volume = {807},
  pages = {82},
  issn = {0004-637X},
  doi = {10.1088/0004-637X/807/1/82},
  abstract = {We investigate the occurrence rate of rapidly rotating (v\{sin\}i {$>$}10
km s-1), low-mass giant stars in the Apache Point
Observatory Galaxy Evolution Experiment-Kepler (APOKASC) fields with
asteroseismic mass and surface gravity measurements. Such stars are
likely merger products and their frequency places interesting
constraints on stellar population models. We also identify anomalous
rotators, i.e., stars with 5 km s-1 {$<$} v\{sin\}i {$<$}
10 km s-1 that are rotating significantly faster than
both angular momentum evolution predictions and the measured rates of
similar stars. Our data set contains fewer rapid rotators than one would
expect given measurements of the Galactic field star population, which
likely indicates that asteroseismic detections are less common in
rapidly rotating red giants. The number of low-mass moderate (5-10
km s-1) rotators in our sample gives a lower limit of
7\% for the rate at which low-mass stars interact on the upper red giant
branch because single stars in this mass range are expected to rotate
slowly. Finally, we classify the likely origin of the rapid or anomalous
rotation where possible. KIC 10293335 is identified as a merger product
and KIC 6501237 is a possible binary system of two oscillating red
giants.},
  file = {/Users/Oliver/Zotero/storage/84AXP7W9/Tayar et al. - 2015 - Rapid Rotation of Low-mass Red Giants Using APOKAS.pdf},
  journal = {The Astrophysical Journal},
  keywords = {binaries: close,stars: late-type,stars: rotation}
}

@misc{thecheopsstudyteam2013,
  title = {{{CHEOPS Definition Study Report}} ({{Red Book}})},
  author = {{The CHEOPS Study Team}},
  year = {2013},
  file = {/Users/Oliver/Zotero/storage/LHW5RSBK/CHEOPS Definition Study Report (Red Book).pdf}
}

@article{thetheanodevelopmentteam+2016,
  title = {Theano: {{A Python}} Framework for Fast Computation of Mathematical Expressions},
  shorttitle = {Theano},
  author = {{The Theano Development Team} and {Al-Rfou}, Rami and Alain, Guillaume and Almahairi, Amjad and Angermueller, Christof and Bahdanau, Dzmitry and Ballas, Nicolas and Bastien, Fr{\'e}d{\'e}ric and Bayer, Justin and Belikov, Anatoly and Belopolsky, Alexander and Bengio, Yoshua and Bergeron, Arnaud and Bergstra, James and Bisson, Valentin and Snyder, Josh Bleecher and Bouchard, Nicolas and {Boulanger-Lewandowski}, Nicolas and Bouthillier, Xavier and {de Br{\'e}bisson}, Alexandre and Breuleux, Olivier and Carrier, Pierre-Luc and Cho, Kyunghyun and Chorowski, Jan and Christiano, Paul and Cooijmans, Tim and C{\^o}t{\'e}, Marc-Alexandre and C{\^o}t{\'e}, Myriam and Courville, Aaron and Dauphin, Yann N. and Delalleau, Olivier and Demouth, Julien and Desjardins, Guillaume and Dieleman, Sander and Dinh, Laurent and Ducoffe, M{\'e}lanie and Dumoulin, Vincent and Kahou, Samira Ebrahimi and Erhan, Dumitru and Fan, Ziye and Firat, Orhan and Germain, Mathieu and Glorot, Xavier and Goodfellow, Ian and Graham, Matt and Gulcehre, Caglar and Hamel, Philippe and Harlouchet, Iban and Heng, Jean-Philippe and Hidasi, Bal{\'a}zs and Honari, Sina and Jain, Arjun and Jean, S{\'e}bastien and Jia, Kai and Korobov, Mikhail and Kulkarni, Vivek and Lamb, Alex and Lamblin, Pascal and Larsen, Eric and Laurent, C{\'e}sar and Lee, Sean and Lefrancois, Simon and Lemieux, Simon and L{\'e}onard, Nicholas and Lin, Zhouhan and Livezey, Jesse A. and Lorenz, Cory and Lowin, Jeremiah and Ma, Qianli and Manzagol, Pierre-Antoine and Mastropietro, Olivier and McGibbon, Robert T. and Memisevic, Roland and {van Merri{\"e}nboer}, Bart and Michalski, Vincent and Mirza, Mehdi and Orlandi, Alberto and Pal, Christopher and Pascanu, Razvan and Pezeshki, Mohammad and Raffel, Colin and Renshaw, Daniel and Rocklin, Matthew and Romero, Adriana and Roth, Markus and Sadowski, Peter and Salvatier, John and Savard, Fran{\c c}ois and Schl{\"u}ter, Jan and Schulman, John and Schwartz, Gabriel and Serban, Iulian Vlad and Serdyuk, Dmitriy and Shabanian, Samira and Simon, {\'E}tienne and Spieckermann, Sigurd and Subramanyam, S. Ramana and Sygnowski, Jakub and Tanguay, J{\'e}r{\'e}mie and {van Tulder}, Gijs and Turian, Joseph and Urban, Sebastian and Vincent, Pascal and Visin, Francesco and {de Vries}, Harm and {Warde-Farley}, David and Webb, Dustin J. and Willson, Matthew and Xu, Kelvin and Xue, Lijun and Yao, Li and Zhang, Saizheng and Zhang, Ying},
  year = {2016},
  month = may,
  abstract = {Theano is a Python library that allows to define, optimize, and evaluate mathematical expressions involving multi-dimensional arrays efficiently. Since its introduction, it has been one of the most used CPU and GPU mathematical compilers - especially in the machine learning community - and has shown steady performance improvements. Theano is being actively and continuously developed since 2008, multiple frameworks have been built on top of it and it has been used to produce many state-of-the-art machine learning models. The present article is structured as follows. Section I provides an overview of the Theano software and its community. Section II presents the principal features of Theano and how to use them, and compares them with other similar projects. Section III focuses on recently-introduced functionalities and improvements. Section IV compares the performance of Theano against Torch7 and TensorFlow on several machine learning models. Section V discusses current limitations of Theano and potential ways of improving it.},
  archivePrefix = {arXiv},
  eprint = {1605.02688},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/MBJ8ZX6S/The Theano Development Team et al. - 2016 - Theano A Python framework for fast computation of.pdf;/Users/Oliver/Zotero/storage/LCAYNJ3C/1605.html},
  journal = {arXiv:1605.02688 [cs]},
  keywords = {Computer Science - Machine Learning,Computer Science - Mathematical Software,Computer Science - Symbolic Computation},
  primaryClass = {cs}
}

@article{thomas+2016,
  title = {Galactic {{Archaeology}} with {{TESS}}: {{Prospects}} for {{Testing}} the {{Star Formation History}} in the {{Solar Neighbourhood}}},
  shorttitle = {Galactic {{Archaeology}} with {{TESS}}},
  author = {Thomas, Alexandra and Stevenson, Emma and Gittins, Fabian W. R. and Miglio, Andrea and Davies, Guy and Girardi, Leo and Campante, Tiago L. and Schofield, Mathew},
  year = {2016},
  month = oct,
  abstract = {A period of quenching between the formation of the thick and thin disks of the Milky Way has been recently proposed to explain the observed age-[\{\textbackslash alpha\}/Fe] distribution of stars in the solar neighbourhood. However, robust constraints on stellar ages are currently available for only a limited number of stars. The all-sky survey TESS (Transiting Exoplanet Survey Satellite) will observe the brightest stars in the sky and thus can be used to investigate the age distributions of stars in these components of the Galaxy via asteroseismology, where previously this has been difficult using other techniques. The aim of this preliminary study was to determine whether TESS will be able to provide evidence for quenching periods during the star formation history of the Milky Way. Using a population synthesis code, we produced populations based on various stellar formation history models and limited the analysis to red-giant-branch stars. We investigated the mass-Galactic-disk-height distributions, where stellar mass was used as an age proxy, to test for whether periods of quenching can be observed by TESS. We found that even with the addition of 15\% noise to the inferred masses, it will be possible for TESS to find evidence for/against quenching periods suggested in the literature (e.g. between 7 and 9 Gyr ago), therefore providing stringent constraints on the formation and evolution of the Milky Way.},
  archivePrefix = {arXiv},
  eprint = {1610.08862},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/66FHRRTA/Thomas et al. - 2016 - Galactic Archaeology with TESS Prospects for Test.pdf;/Users/Oliver/Zotero/storage/2RHPXHPS/1610.html},
  journal = {arXiv:1610.08862 [astro-ph]},
  keywords = {AR 01/11/16,Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{thomas+2019,
  title = {Asteroseismic Constraints on Active Latitudes of Solar-Type Stars: {{HD}} 173701 Has Active Bands at Higher Latitudes than the {{Sun}}},
  shorttitle = {Asteroseismic Constraints on Active Latitudes of Solar-Type Stars},
  author = {Thomas, Alexandra E. L. and Chaplin, William J. and Davies, Guy R. and Howe, Rachel and Santos, {\'A}ngela R. G. and Elsworth, Yvonne and Miglio, Andrea and Campante, Tiago and Cunha, Margarida S.},
  year = {2019},
  month = may,
  volume = {485},
  pages = {3857--3868},
  issn = {0035-8711},
  doi = {10.1093/mnras/stz672},
  abstract = {We present a new method for determining the location of active bands of
latitude on solar-type stars, which uses stellar-cycle-induced frequency
shifts of detectable solar-like oscillations. When near-surface activity
is distributed in a non-homogeneous manner, oscillation modes of
different angular degree and azimuthal order will have their frequencies
shifted by different amounts. We use this simple concept, coupled to a
model for the spatial distribution of the near-surface activity, to
develop two methods that use the frequency shifts to infer minimum and
maximum latitudes for the active bands. Our methods respond to the range
in latitude over which there is significant magnetic flux present, over
and above weak basal ephemeral flux levels. We verify that we are able
to draw accurate inferences in the solar case, using Sun-as-a-star
helioseismic data and artificial data. We then apply our methods to
Kepler data on the solar analogue HD 173701, and find that its active
bands straddle a much wider range in latitude than do the bands on the
Sun.},
  file = {/Users/Oliver/Zotero/storage/3ACRWTE8/Thomas et al. - 2019 - Asteroseismic constraints on active latitudes of s.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {asteroseismology,stars: activity,stars: individual (HD 173701)}
}

@article{thompson+1996,
  title = {Differential {{Rotation}} and {{Dynamics}} of the {{Solar Interior}}},
  author = {Thompson, M. J. and Toomre, J. and Anderson, E. R. and Antia, H. M. and Berthomieu, G. and Burtonclay, D. and Chitre, S. M. and {Christensen-Dalsgaard}, J. and Corbard, T. and De Rosa, M. and Genovese, C. R. and Gough, D. O. and Haber, D. A. and Harvey, J. W. and Hill, F. and Howe, R. and Korzennik, S. G. and Kosovichev, A. G. and Leibacher, J. W. and Pijpers, F. P. and Provost, J. and Rhodes, Jr., E. J. and Schou, J. and Sekii, T. and Stark, P. B. and Wilson, P. R.},
  year = {1996},
  month = may,
  volume = {272},
  pages = {1300--1305},
  issn = {0036-8075},
  doi = {10.1126/science.272.5266.1300},
  abstract = {Splitting of the sun's global oscillation frequencies by large-scale flows can be used to investigate how rotation varies with radius and latitude within the solar interior. The nearly uninterrupted
observations by the Global Oscillation Network Group (GONG) yield oscillation power spectra with high duty cycles and high signal-to-noise ratios. Frequency splittings derived from GONG observations confirm that the variation of rotation rate with latitude seen at the surface carries through much of the convection zone, at the base of which is an
adjustment layer leading to latitudinally independent rotation at greater depths. A distinctive shear layer just below the surface is discernible at low to mid-latitudes.},
  journal = {Science}
}

@article{ting+2018,
  title = {A {{Large}} and {{Pristine Sample}} of {{Standard Candles}} across the {{Milky Way}}:{\~ }100,000 {{Red Clump Stars}} with 3\% {{Contamination}}},
  shorttitle = {A {{Large}} and {{Pristine Sample}} of {{Standard Candles}} across the {{Milky Way}}},
  author = {Ting, Yuan-Sen and Hawkins, Keith and Rix, Hans-Walter},
  year = {2018},
  month = may,
  volume = {858},
  pages = {L7},
  doi = {10.3847/2041-8213/aabf8e},
  abstract = {Core helium-burning red clump (RC) stars are excellent standard candles in the Milky Way. These stars may have more precise distance estimates from spectrophotometry than from Gaia parallaxes beyond 3 kpc. However, RC stars have values of T \textsubscript{eff} and \{log\}g that are very similar to some red giant branch (RGB) stars. Especially for low-resolution spectroscopic studies where T \textsubscript{eff}, \{log\}g, and [Fe/H] can only be estimated with limited precision, separating RC stars from RGB through established methods can incur{\~ }20\% contamination. Recently, Hawkins et al. demonstrated that the additional information in single-epoch spectra, such as the C/N ratio, can be exploited to cleanly differentiate RC and RGB stars. In this second paper of the series, we establish a data-driven mapping from spectral flux space to independently determined asteroseismic parameters, the frequency and the period spacing. From this, we identify 210,371 RC stars from the publicly available LAMOST DR3 and APOGEE DR14 data, with{\~ }9\% of contamination. We provide an RC sample of 92249 stars with a contamination of only{\~ }3\%, by restricting the combined analysis to LAMOST stars with S/N\textsubscript{pix} {$\geq$} 75. This demonstrates that high-signal-to-noise ratio (S/N), low-resolution spectra covering a broad wavelength range can identify RC samples at least as pristine as their high-resolution counterparts. As coming and ongoing surveys such as TESS, DESI, and LAMOST will continue to improve the overlapping training spectroscopic-asteroseismic sample, the method presented in this study provides an efficient and straightforward way to derive a vast yet pristine sample of RC stars to reveal the three-dimensional (3D) structure of the Milky Way.},
  file = {/Users/Oliver/Zotero/storage/KJMZD6L2/Ting et al. - 2018 - A Large and Pristine Sample of Standard Candles ac.pdf;/Users/Oliver/Zotero/storage/24RQ8BDZ/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en}
}

@article{torres2010,
  title = {On the {{Use}} of {{Empirical Bolometric Corrections}} for {{Stars}}},
  author = {Torres, Guillermo},
  year = {2010},
  month = nov,
  volume = {140},
  pages = {1158},
  doi = {10.1088/0004-6256/140/5/1158},
  abstract = {When making use of tabulations of empirical bolometric corrections for stars (BC\textsubscript{ V }), a commonly overlooked fact is that while the zero point is arbitrary, the bolometric magnitude of the Sun (M \textsubscript{bol,sun}) that is used in combination with such tables cannot be chosen arbitrarily. It must be consistent with the zero point of BC\textsubscript{ V } so that the apparent brightness of the Sun is reproduced. The latter is a measured quantity, for which we adopt the value V \textsubscript{sun} = -26.76 {$\pm$} 0.03. Inconsistent values of M \textsubscript{bol,sun} are listed in many of the most popular sources of BC\textsubscript{ V }. We quantify errors that are introduced by failure to pay attention to this detail. We also take the opportunity to reprint the BC\textsubscript{ V } coefficients of the often used polynomial fits by Flower, which were misprinted in the original publication.},
  file = {/Users/Oliver/Zotero/storage/YM5KB5D2/Torres - 2010 - On the Use of Empirical Bolometric Corrections for.pdf;/Users/Oliver/Zotero/storage/PFJLNCNM/ui.adsabs.harvard.edu.html},
  journal = {The Astronomical Journal},
  language = {en},
  number = {5}
}

@article{toutain+appourchaux1994,
  title = {Maximum Likelihood Estimators: {{An}} Application to the Estimation of the Precision of Helioseismic Measurements},
  shorttitle = {Maximum Likelihood Estimators},
  author = {Toutain, T. and Appourchaux, T.},
  year = {1994},
  month = sep,
  volume = {289},
  pages = {649--658},
  issn = {0004-6361},
  abstract = {In this paper we apply the theory of Maximum Likelihood estimators to
determine the precision of parameters in fitting Lorentzian profiles to
helioseismic power spectra. The precision of frequency, linewidth,
amplitude and noise determination for a single p mode, and of the l = 1
splitting, are derived as a function of the signal-to-noise ratio and
the spectral resolution of the spectrum, Libbrecht's formula (Libbrecht
1992) for frequency precision is derived in a more general case. For
validating the approach, the theoretical precisions are compared with
those obtained with Monte-Carlo simulations and with IPHIR observations.
The robustness of the precisions obtained is ideal for predictive
purposes. The method used to derive the precisions is general enough so
that it can be used for other purposes.},
  file = {/Users/Oliver/Zotero/storage/X2SUK4V7/Toutain and Appourchaux - 1994 - Maximum likelihood estimators An application to t.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {Helioseismology,Hessian Matrices,Maximum Likelihood Estimates,Monte Carlo Method,P Band,Parameter Identification,Power Spectra,Precision,Signal To Noise Ratios,Simulation,Spectral Resolution,Stellar Oscillations}
}

@article{trampedach+2016,
  title = {The Asteroseismic Surface Effect from a Grid of {{3D}} Convection Simulations. {{I}}. {{Frequency}} Shifts from Convective Expansion of Stellar Atmospheres},
  author = {Trampedach, Regner and Aarslev, Magnus J. and Houdek, G{\"u}nter and Collet, Remo and {Christensen-Dalsgaard}, J{\o}rgen and Stein, Robert F. and Asplund, Martin},
  year = {2016},
  month = nov,
  abstract = {We analyse the effect on adiabatic stellar oscillation frequencies of replacing the near-surface layers in 1D stellar structure models with averaged 3D stellar surface convection simulations. The main difference is an expansion of the atmosphere by 3D convection, expected to explain a major part of the asteroseismic surface effect; a systematic overestimation of p-mode frequencies due to inadequate surface physics. We employ pairs of 1D stellar envelope models and 3D simulations from a previous calibration of the mixing-length parameter, alpha. That calibration constitutes the hitherto most consistent matching of 1D models to 3D simulations, ensuring that their differences are not spurious, but entirely due to the 3D nature of convection. The resulting frequency shift is identified as the structural part of the surface effect

license: MIT

license_type: permissive

branch_name: refs/heads/master

extension: bib