text:
$, \$mode(M\_\{W4\})=-1.73\^m\textbackslash pm0.03\^m\$, as well as the corresponding estimates of their de-reddened colors.},
  archivePrefix = {arXiv},
  eprint = {1706.09725},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/R2KMHEBV/Gontcharov - 2017 - Systematic Error of the Gaia DR1 TGAS Parallaxes f.pdf;/Users/Oliver/Zotero/storage/K9HC62Z5/1706.html},
  journal = {arXiv:1706.09725 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{gonzalez2016,
  title = {A {{Revised Gyro}}-{{Age}} for {{M}} 67 from {{Kepler}}/{{K2}}-{{Campaign}}-5 {{Light Curves}}},
  author = {Gonzalez, Guillermo},
  year = {2016},
  month = dec,
  volume = {463},
  pages = {3513--3519},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stw2237},
  abstract = {We revisit the photometric variability of stars in the M 67 field using Kepler/K2-Campaign-5 light curves. In our previous work, we limited the search area around M\textbackslash,67 to that of a recent ground-based study. In the present work, we expand the search area and apply a more rigorous period-finding algorithm to determine the rotation periods of 98 main sequence cluster members from the same data. In addition, we derive periods of 40 stars from the K2SC detrended light curves. We determine the mean period of single sun-like main sequence cluster members to be \$29.6 \textbackslash pm 0.6\$ d. Assuming the periods correspond to stellar rotation, the corresponding mean gyro-age is \$5.4 \textbackslash pm 0.2\$ Gyr.},
  archivePrefix = {arXiv},
  eprint = {1609.00601},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/748MDEEJ/Gonzalez - 2016 - A Revised Gyro-Age for M 67 from KeplerK2-Campaig.pdf;/Users/Oliver/Zotero/storage/LGWND9C8/1609.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {4}
}

@article{goode+thompson1992,
  title = {The Effect of an Inclined Magnetic Field on Solar Oscillation Frequencies},
  author = {Goode, Philip R. and Thompson, Michael J.},
  year = {1992},
  month = aug,
  volume = {395},
  pages = {307--315},
  issn = {0004-637X},
  doi = {10.1086/171653},
  abstract = {The radiative interior of the sun could be hiding a large-scale magnetic field, which might not be axisymmetric about the observed rotation axis. Using helioseismic data, we estimate that the strength of any such relic field must be less than about 30 MG, if the field is axisymmetric about the rotation axis. The shape oblateness caused by a field at this limiting strength is about 5-10 x 10 exp -6. Stronger fields can be accommodated by the helioseismic data if they are inclined to the rotation axis. We further conclude that the convention zone and at least the outer part of the radiative interior rotate on the same axis.},
  file = {/Users/Oliver/Zotero/storage/FTCPM7QF/Goode and Thompson - 1992 - The effect of an inclined magnetic field on solar .pdf},
  journal = {The Astrophysical Journal},
  keywords = {Axes Of Rotation,Fine Structure,Magnetic Field Configurations,Pre-Main Sequence Stars,Solar Interior,Solar Magnetic Field,Solar Oscillations,Solar Rotation,Solar Spectra}
}

@article{goodman+weare2010,
  title = {Ensemble Samplers with Affine Invariance},
  author = {Goodman, Jonathan and Weare, Jonathan},
  year = {2010},
  volume = {5},
  pages = {65--80},
  doi = {10.2140/camcos.2010.5.65},
  abstract = {We propose a family of Markov chain Monte Carlo methods whose
performance is unaffected by affine tranformations of space. These
algorithms are easy to construct and require little or no additional
computational overhead. They should be particularly useful for sampling
badly scaled distributions. Computational tests show that the affine
invariant methods can be significantly faster than standard MCMC methods
on highly skewed distributions.},
  journal = {Communications in Applied Mathematics and Computational Science, Vol. 5, No. 1, p. 65-80, 2010},
  keywords = {affine invariance,ensemble samplers,Markov chain Monte Carlo}
}

@article{gough+thompson1990,
  title = {The Effect of Rotation and a Buried Magnetic Field on Stellar Oscillations},
  author = {Gough, D. O. and Thompson, M. J.},
  year = {1990},
  month = jan,
  volume = {242},
  pages = {25--55},
  issn = {0035-8711},
  doi = {10.1093/mnras/242.1.25},
  abstract = {A perturbation method is presented for calculating the frequency modification of stellar oscillations caused by rotation and internal magnetic field. A short-wavelength asymptotic analysis derived from ray theory is also presented. The effects on high-order solar acoustic modes of various hypothetical angular velocity and magnetic field
configurations are investigated using both methods of calculation. The asymptotic formulas provide a good estimate for the frequency splitting of five-minute modes when the field and the rotation vary sufficiently smoothly. On the other hand, a localized magnetic field, for example at the base of the convection zone, produces a characteristic oscillatory perturbation to the eigenfrequencies.},
  file = {/Users/Oliver/Zotero/storage/GJQH3SEU/Gough and Thompson - 1990 - The effect of rotation and a buried magnetic field.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Angular Velocity,Broken Symmetry,Gravitational Effects,Perturbation Theory,Resonant Frequencies,Stellar Interiors,Stellar Magnetic Fields,Stellar Oscillations,Stellar Rotation}
}

@article{gough1983,
  title = {The Protosolar Helium Abundance},
  author = {Gough, D. O.},
  year = {1983},
  month = feb,
  pages = {117--136},
  abstract = {The theory of stellar evolution applied to the sun cannot alone determine the solar helium abundance. Only if the neutrino flux is taken into account can a formal calibration be carried out. But that procedure appears to give the wrong result. An astronomical argument for
calibrating mixing-length theory, using a measure of chromospheric activity in lower main-sequence stars, suggests that the protosolar abundance by mass is about 0.25. More direct measurements, using five-minute high-degree oscillation frequencies to measure conditions in the upper regions of the convection zone, and five-minute low-degree oscillations to probe the radiative interior, corroborate this finding. A recent unpublished report of quadrupole g-mode frequencies is also consistent. It is difficult to assess the uncertainty in the estimated abundance, because there are systematic unexplained discrepancies between theory and observation. However, the spread in the various determinations, excluding that involving the neutrino flux, is less than 10 percent of the mean value.},
  file = {/Users/Oliver/Zotero/storage/5MPHUZZJ/Gough - 1983 - The protosolar helium abundance.pdf},
  keywords = {Abundance,Calibrating,Flux (Rate),Helium,Protostars,Solar Neutrinos,Solar Oscillations,Stellar Evolution,Stellar Models}
}

@article{green+2018,
  title = {Galactic Reddening in {{3D}} from Stellar Photometry - an Improved Map},
  author = {Green, Gregory M. and Schlafly, Edward F. and Finkbeiner, Douglas and Rix, Hans-Walter and Martin, Nicolas and Burgett, William and Draper, Peter W. and Flewelling, Heather and Hodapp, Klaus and Kaiser, Nicholas and Kudritzki, Rolf-Peter and Magnier, Eugene A. and Metcalfe, Nigel and Tonry, John L. and Wainscoat, Richard and Waters, Christopher},
  year = {2018},
  month = jul,
  volume = {478},
  pages = {651},
  doi = {10.1093/mnras/sty1008},
  abstract = {We present a new 3D map of interstellar dust reddening, covering three quarters of the sky (declinations of {$\delta$} {$\greaterequivlnt$} -30\textdegree ) out to a distance of several kiloparsecs. The map is based on high-quality stellar photometry of 800 million stars from Pan-STARRS 1 and 2MASS. We divide the sky into sightlines containing a few hundred stars each, and then infer stellar distances and types, along with the line-of-sight dust distribution. Our new map incorporates a more accurate average extinction law and an additional 1.5 yr of Pan-STARRS 1 data, tracing dust to greater extinctions and at higher angular resolutions than our previous map. Out of the plane of the Galaxy, our map agrees well with 2D reddening maps derived from far-infrared dust emission. After accounting for a 25 per cent difference in scale, we find a mean scatter of{\~ }10 per cent between our map and the Planck far-infrared emission-based dust map, out to a depth of 0.8 mag in E(g\textsubscript{P1} - r\textsubscript{P1}), with the level of agreement varying over the sky. Our map can be downloaded at http://argonaut.skymaps.info, or from the Harvard Dataverse (Green 2017).},
  file = {/Users/Oliver/Zotero/storage/GDJCKDHU/Green et al. - 2018 - Galactic reddening in 3D from stellar photometry -.pdf;/Users/Oliver/Zotero/storage/6DMXXZKZ/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@book{grenander1959,
  title = {Probability and {{Statistics}}: {{The Harald Cram鈋r Volume}}},
  shorttitle = {Probability and {{Statistics}}},
  author = {Grenander, Ulf},
  year = {1959},
  publisher = {{Alqvist \& Wiksell}},
  googlebooks = {UPc0AAAAMAAJ},
  language = {en}
}

@article{groenewegen2008,
  title = {The Red Clump Absolute Magnitude Based on Revised {{Hipparcos}} Parallaxes},
  author = {Groenewegen, M. a. T.},
  year = {2008},
  month = sep,
  volume = {488},
  pages = {935},
  doi = {10.1051/0004-6361:200810201},
  abstract = {Context: Over the past decade the use of the red clump (RC) as distance indicator has increased in importance as this evolutionary phase is well populated and a good local calibration exists. \\
Aims: The absolute calibration of the RC in the I and K band is investigated again based on the recently published revised Hipparcos parallaxes. \\
Methods: A numerical model is developed that takes the various selection criteria and the properties of the Hipparcos catalogue into account. The biases involved in applying certain selections are estimated with this model. \\
Results: The absolute magnitudes that are found are M\textsubscript{I} = -0.22 {$\pm$} 0.03 and M\textsubscript{K} = -1.54 {$\pm$} 0.04 (on the 2MASS system). The I-band value is in good agreement with previous determinations, the K-band value is fainter than previously quoted, and this seems to be related to a selection bias whereby accurate K-magnitudes are only available for relatively few bright stars. Applying population corrections to the absolute K magnitude of RC stars in clusters supports the fainter magnitude scale.},
  file = {/Users/Oliver/Zotero/storage/9F4QNFE5/Groenewegen - 2008 - The red clump absolute magnitude based on revised .pdf;/Users/Oliver/Zotero/storage/DC7UWZD5/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en},
  number = {3}
}

@article{grunblatt+2017,
  title = {Seeing {{Double}} with {{K2}}: {{Testing Re}}-Inflation with {{Two Remarkably Similar Planets}} around {{Red Giant Branch Stars}}},
  shorttitle = {Seeing {{Double}} with {{K2}}},
  author = {Grunblatt, Samuel K. and Huber, Daniel and Gaidos, Eric and Lopez, Eric D. and Howard, Andrew W. and Isaacson, Howard T. and Sinukoff, Evan and Vanderburg, Andrew and Nofi, Larissa and Yu, Jie and North, Thomas S. H. and Chaplin, William and {Foreman-Mackey}, Daniel and Petigura, Erik and Ansdell, Megan and Weiss, Lauren and Fulton, Benjamin and Lin, Douglas N. C.},
  year = {2017},
  month = dec,
  volume = {154},
  pages = {254},
  doi = {10.3847/1538-3881/aa932d},
  abstract = {Despite more than 20 years since the discovery of the first gas giant planet with an anomalously large radius, the mechanism for planet inflation remains unknown. Here, we report the discovery of K2-132b, an inflated gas giant planet found with the NASA K2 Mission, and a revised mass for another inflated planet, K2-97b. These planets orbit on {$\approx$}9 day orbits around host stars that recently evolved into red giants. We constrain the irradiation history of these planets using models constrained by asteroseismology and Keck/High Resolution Echelle Spectrometer spectroscopy and radial velocity measurements. We measure planet radii of 1.31 {$\pm$} 0.11 R \textsubscript{J} and 1.30 {$\pm$} 0.07 R \textsubscript{J}, respectively. These radii are typical for planets receiving the current irradiation, but not the former, zero age main-sequence irradiation of these planets. This suggests that the current sizes of these planets are directly correlated to their current irradiation. Our precise constraints of the masses and radii of the stars and planets in these systems allow us to constrain the planetary heating efficiency of both systems as 0.03\{ \% \}\textsubscript{-0.02 \% }\textsuperscript{+0.03 \% }. These results are consistent with a planet re-inflation scenario, but suggest that the efficiency of planet re-inflation may be lower than previously theorized. Finally, we discuss the agreement within 10\% of the stellar masses and radii, and the planet masses, radii, and orbital periods of both systems, and speculate that this may be due to selection bias in searching for planets around evolved stars.},
  file = {/Users/Oliver/Zotero/storage/TITCD2RP/Grunblatt et al. - 2017 - Seeing Double with K2 Testing Re-inflation with T.pdf;/Users/Oliver/Zotero/storage/D3BQQ6J4/ui.adsabs.harvard.edu.html},
  journal = {The Astronomical Journal},
  language = {en},
  number = {6}
}

@article{guo+2016,
  title = {The Metallicity Distribution and Hot {{Jupiter}} Rate of the {{Kepler}} Field: {{Hectochelle High}}-Resolution Spectroscopy for 776 {{Kepler}} Target Stars},
  shorttitle = {The Metallicity Distribution and Hot {{Jupiter}} Rate of the {{Kepler}} Field},
  author = {Guo, Xueying and Johnson, John A. and Mann, Andrew W. and Kraus, Adam L. and Curtis, Jason L. and Latham, David W.},
  year = {2016},
  month = dec,
  volume = {1612},
  pages = {arXiv:1612.01616},
  abstract = {The occurrence rate of hot Jupiters from the Kepler transit survey is
roughly half that of radial velocity surveys targeting solar
neighborhood stars. One hypothesis to explain this difference is that
the two surveys target stars with different stellar metallicity
distributions. To test this hypothesis, we measure the metallicity
distribution of the Kepler targets using the Hectochelle multi-fiber,
high-resolution spectrograph. Limiting our spectroscopic analysis to 610
dwarf stars in our sample with log(g){$>$}3.5, we measure a metallicity
distribution characterized by a mean of [M/H]\_\{mean\} = -0.045 +/- 0.00,
in agreement with previous studies of the Kepler field target stars. In
comparison, the metallicity distribution of the California Planet Search
radial velocity sample has a mean of [M/H]\_\{CPS, mean\} = -0.005 +/-
0.006, and the samples come from different parent populations according
to a Kolmogorov-Smirnov test. We refit the exponential relation between
the fraction of stars hosting a close-in giant planet and the host star
metallicity using a sample of dwarf stars from the California Planet
Search with updated metallicities. The best-fit relation tells us that
the difference in metallicity between the two samples is insufficient to
explain the discrepant Hot Jupiter occurrence rates; the metallicity
difference would need to be \$\textbackslash simeq\$0.2-0.3 dex for perfect agreement.
We also show that (sub)giant contamination in the Kepler sample cannot
reconcile the two occurrence calculations. We conclude that other
factors, such as binary contamination and imperfect stellar properties,
must also be at play.},
  journal = {ArXiv e-prints},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics}
}

@article{guzman-ramirez2016,
  title = {\$\^3\${{He Abundances}} in {{Planetary Nebulae}}},
  author = {{Guzman-Ramirez}, Lizette},
  year = {2016},
  month = dec,
  volume = {1612},
  pages = {arXiv:1612.02599},
  abstract = {The \$\^3\$He isotope is important to many fields of astrophysics, including stellar evolution, chemical evolution, and cosmology. The isotope is produced in stars which evolve through the planetary nebula phase. Planetary nebulae are the final evolutionary phase of low- and intermediate-mass stars, where the extensive mass lost by the star on the asymptotic giant branch is ionised by the emerging white dwarf. This ejecta quickly disperses and merges with the surrounding ISM. The abundance of \$\^3\$He can only be derived from the hyperfine transition of the ionised \$\^3\$He, which is represented as \$\^3\$He\$\^+\$, these transition can be observed in the radio at the rest frequency of 8.665 GHz. \$\^3\$He abundances in PNe can help test models of the chemical evolution of the Galaxy. Many hours have been put into trying to detect this line, using telescopes like Effelsberg a 100m dish from the Max Planck Institute for Radio Astronomy, the National Radio Astronomy Observatory (NRAO) 140-foot telescope, the NRAO Very Large Array, the Arecibo antenna, the Green Bank Telescope, and only just recently, the Deep Space Station 63 antenna from the Madrid Deep Space Communications Complex.},
  journal = {ArXiv e-prints},
  keywords = {Astrophysics - Solar and Stellar Astrophysics}
}

@article{hacking+1999,
  title = {The {{Wide}}-{{Field Infrared Explore}} ({{WIRE}}) {{Mission}}},
  author = {Hacking, P. and Lonsdale, C. and Gautier, T. and Herter, T. and Shupe, D. and Stacey, G. and Fang, F. and Xu, C. and Graf, P. and Werner, M. and Soifer, B. and Moseley, H. and Houck, J.},
  year = {1999},
  volume = {177},
  pages = {409},
  abstract = {Not Available},
  file = {/Users/Oliver/Zotero/storage/JE4YD6RN/Hacking et al. - 1999 - The Wide-Field Infrared Explore (WIRE) Mission.pdf}
}

@article{hadden+lithwick2016,
  title = {Kepler {{Planet Masses}} and {{Eccentricities}} from {{TTV Analysis}}},
  author = {Hadden, Sam and Lithwick, Yoram},
  year = {2016},
  month = nov,
  abstract = {We conduct a uniform analysis of the transit timing variations (TTVs) of 145 planets from 55 Kepler multiplanet systems to infer planet masses and eccentricities. Eighty of these planets do not have previously reported mass and eccentricity measurements. We employ two complementary methods to fit TTVs: Markov chain Monte Carlo simulations based on N-body integration and an analytic fitting approach. Mass measurements of 49 planets, including 12 without previously reported masses, meet our criterion for classification as robust. Using mass and radius measurements, we infer the masses of planets' gaseous envelopes for both our TTV sample as well as transiting planets with radial velocity observations. Insight from analytic TTV formulae allows us to partially circumvent degeneracies inherent to inferring eccentricities from TTV observations. We find that planet eccentricities are generally small, typically a few percent, but in many instances are non-zero.},
  archivePrefix = {arXiv},
  eprint = {1611.03516},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/HJK57XK5/Hadden and Lithwick - 2016 - Kepler Planet Masses and Eccentricities from TTV A.pdf;/Users/Oliver/Zotero/storage/56XI7VIH/1611.html},
  journal = {arXiv:1611.03516 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics},
  primaryClass = {astro-ph}
}

@article{hale+2016,
  title = {Performance of the {{Birmingham Solar}}-{{Oscillations Network}} ({{BiSON}})},
  author = {Hale, S. J. and Howe, R. and Chaplin, W. J. and Davies, G. R. and Elsworth, Y. P.},
  year = {2016},
  month = jan,
  volume = {291},
  pages = {1--28},
  issn = {1573-093X},
  doi = {10.1007/s11207-015-0810-0},
  abstract = {The Birmingham Solar-Oscillations Network (BiSON) has been operating with a full complement of six stations since 1992. Over 20 years later, we look back on the network history. The meta-data from the sites have been analysed to assess performance in terms of site insolation, with a brief look at the challenges that have been encountered over the years. We explain how the international community can gain easy access to the ever-growing dataset produced by the network, and finally look to the future of the network and the potential impact of nearly 25 years of technology miniaturisation.},
  file = {/Users/Oliver/Zotero/storage/47L9KUHH/Hale et al. - 2016 - Performance of the Birmingham Solar-Oscillations N.pdf},
  journal = {Solar Physics},
  language = {en},
  number = {1}
}

@article{hall+2019,
  title = {Testing Asteroseismology with {{Gaia DR2}}: {{Hierarchical}} Models of the {{Red Clump}}},
  shorttitle = {Testing Asteroseismology with {{Gaia DR2}}},
  author = {Hall, Oliver J. and Davies, Guy R. and Elsworth, Yvonne P. and Miglio, Andrea and Bedding, Timothy R. and Brown, Anthony G. A. and Khan, Saniya and Hawkins, Keith and Garc{\'i}a, Rafael A. and Chaplin, William J. and North, Thomas S. H.},
  year = {2019},
  month = jul,
  volume = {486},
  pages = {3569--3585},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stz1092},
  abstract = {Asteroseismology provides fundamental stellar parameters independent of distance, but subject to systematics under calibration. Gaia DR2 has provided parallaxes for a billion stars, which are offset by a parallax zero-point. Red Clump (RC) stars have a narrow spread in luminosity, thus functioning as standard candles to calibrate these systematics. This work measures how the magnitude and spread of the RC in the Kepler field are affected by changes to temperature and scaling relations for seismology, and changes to the parallax zero-point for Gaia. We use a sample of 5576 RC stars classified through asteroseismology. We apply hierarchical Bayesian latent variable models, finding the population level properties of the RC with seismology, and use those as priors on Gaia parallaxes to find the parallax zero-point offset. We then find the position of the RC using published values for the zero-point. We find a seismic temperature insensitive spread of the RC of \textasciitilde 0.03 mag in the 2MASS K band and a larger and slightly temperature-dependent spread of \textasciitilde 0.13 mag in the Gaia G band. This intrinsic dispersion in the K band provides a distance precision of \textasciitilde 1\% for RC stars. Using Gaia data alone, we find a mean zero-point of -41 \$\textbackslash pm\$ 10 \$\textbackslash mu\$as. This offset yields RC absolute magnitudes of -1.634 \$\textbackslash pm\$ 0.018 in K and 0.546 \$\textbackslash pm\$ 0.016 in G. Obtaining these same values through seismology would require a global temperature shift of \textasciitilde -70 K, which is compatible with known systematics in spectroscopy.},
  archivePrefix = {arXiv},
  eprint = {1904.07919},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/TM3FW7TC/Hall et al. - 2019 - Testing asteroseismology with Gaia DR2 Hierarchic.pdf;/Users/Oliver/Zotero/storage/UGMWMDVZ/1904.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {3}
}

@article{handberg+2017,
  title = {{{NGC}} 6819: Testing the Asteroseismic Mass Scale, Mass Loss and Evidence for Products of Non-Standard Evolution},
  shorttitle = {{{NGC}} 6819},
  author = {Handberg, R. and Brogaard, K. and Miglio, A. and Bossini, D. and Elsworth, Y. and Slumstrup, D. and Davies, G. R. and Chaplin, W. J.},
  year = {2017},
  month = nov,
  volume = {472},
  pages = {979},
  doi = {10.1093/mnras/stx1929},
  abstract = {We present an extensive peakbagging effort on Kepler data of {$\sim$}50 red giant stars in the open star cluster NGC 6819. By employing sophisticated pre-processing of the time series and Markov chain Monte Carlo techniques we extracted individual frequencies, heights and line widths for hundreds of oscillation modes. We show that the 'average' asteroseismic parameter {$\delta\nu$}\textsubscript{02}, derived from these, can be used to distinguish the stellar evolutionary state between the red giant branch (RGB) stars and red clump (RC) stars. Masses and radii are estimated using asteroseismic scaling relations, both empirically corrected to obtain self-consistency and agreement with independent measures of distance, and using updated theoretical corrections. Remarkable agreement is found, allowing the evolutionary state of the giants to be determined exclusively from the empirical correction to the scaling relations. We find a mean mass of the RGB stars and RC stars in NGC 6819 to be 1.61 {$\pm$} 0.02 and 1.64 {$\pm$} 0.02 M\textsubscript{{$\Sun$}}, respectively. The difference {$\increment$}M = -0.03 {$\pm$} 0.01 M\textsubscript{{$\Sun$}} is almost insensitive to systematics, suggesting very little RGB mass loss, if any. Stars that are outliers relative to the ensemble reveal overmassive members that likely evolved via mass transfer in a blue straggler phase. We suggest that KIC 4937011, a low-mass Li-rich giant, is a cluster member in the RC phase that experienced very high mass loss during its evolution. Such over- and undermassive stars need to be considered when studying field giants, since the true age of such stars cannot be known and there is currently no way to distinguish them from normal stars.},
  file = {/Users/Oliver/Zotero/storage/954DLCH6/Handberg et al. - 2017 - NGC 6819 testing the asteroseismic mass scale, ma.pdf;/Users/Oliver/Zotero/storage/UIW7Z6PS/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@article{handberg+campante2011,
  title = {Bayesian Peak-Bagging of Solar-like Oscillators Using {{MCMC}}: A Comprehensive Guide},
  shorttitle = {Bayesian Peak-Bagging of Solar-like Oscillators Using {{MCMC}}},
  author = {Handberg, R. and Campante, T. L.},
  year = {2011},
  month = mar,
  volume = {527},
  pages = {A56},
  doi = {10.1051/0004-6361/201015451},
  abstract = {Context. Asteroseismology has entered a new era with the advent of the NASA Kepler mission. Long and continuous photometric observations of unprecedented quality are now available which have stimulated the development of a number of suites of innovative analysis tools. \\
 Aims: The power spectra of solar-like oscillations are an inexhaustible source of information on stellar structure and evolution. Robust methods are hence needed in order to infer both individual oscillation mode parameters and parameters describing non-resonant features, thus making a seismic interpretation possible. \\
 Methods: We present a comprehensive guide to the implementation of a Bayesian peak-bagging tool that employs a Markov chain Monte Carlo (MCMC). Besides making it possible to incorporate relevant prior information through Bayes' theorem, this tool also allows one to obtain the marginal probability density function for each of the fitted parameters. We apply this tool to a couple of recent asteroseismic data sets, namely, to CoRoT observations of HD 49933 and to ground-based observations made during a campaign devoted to Procyon. \\
 Results: The developed method performs remarkably well at constraining not only in the traditional case of extracting oscillation frequencies, but also when pushing the limit where traditional methods have difficulties. Moreover it provides an rigorous way of comparing competing models, such as the ridge identifications, against the asteroseismic data.},
  file = {/Users/Oliver/Zotero/storage/QIUX7D9S/Handberg and Campante - 2011 - Bayesian peak-bagging of solar-like oscillators us.pdf;/Users/Oliver/Zotero/storage/XDURZMY2/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  keywords = {Core Seismology},
  language = {en}
}

@article{handberg+lund2014,
  title = {Automated Preparation of {{Kepler}} Time Series of Planet Hosts for Asteroseismic Analysis},
  author = {Handberg, R. and Lund, M. N.},
  year = {2014},
  month = dec,
  volume = {445},
  pages = {2698--2709},
  issn = {0035-8711},
  doi = {10.1093/mnras/stu1823},
  abstract = {One of the tasks of the Kepler Asteroseismic Science Operations Center
(KASOC) is to provide asteroseismic analyses on Kepler Objects of
Interest. However, asteroseismic analysis of planetary host stars
presents some unique complications with respect to data pre-processing,
compared to pure asteroseismic targets. If not accounted for, the
presence of planetary transits in the photometric time series often
greatly complicates or even hinders these asteroseismic analyses. This
drives the need for specialized methods of pre-processing data to make
them suitable for asteroseismic analysis. In this paper, we present the
KASOC filter, which is used to automatically prepare data from the
Kepler/K2 mission for asteroseismic analyses of solar-like planet host
stars. The methods are very effective at removing unwanted signals of
both instrumental and planetary origins and produce significantly
cleaner photometric time series than the original data. The methods are
automated and can therefore easily be applied to a large number of
stars. The application of the filter is not restricted to planetary
hosts, but can be applied to any solar-like or red giant stars observed
by Kepler/K2.},
  file = {/Users/Oliver/Zotero/storage/QMMIUBJD/Handberg and Lund - 2014 - Automated preparation of Kepler time series of pla.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {methods: data analysis,planetary systems,stars: oscillations}
}

@article{handler2009,
  title = {Confirmation of Simultaneous p and g Mode Excitation in {{HD}} 8801 and {$\gamma$} {{Peg}} from Time-Resolved Multicolour Photometry of Six Candidate `hybrid' Pulsators},
  author = {Handler, G.},
  year = {2009},
  month = sep,
  volume = {398},
  pages = {1339--1351},
  issn = {0035-8711},
  doi = {10.1111/j.1365-2966.2009.15005.x},
  abstract = {We carried out a multicolour time-series photometric study of six stars
claimed as `hybrid' p and g mode pulsators in the literature. {$\gamma$}
Peg was confirmed to show short-period oscillations of the {$\beta$} Cep
type and simultaneous long-period pulsations typical of Slowly Pulsating
B (SPB) stars. From the measured amplitude ratios in the Str\"omgren
uvy passbands, the stronger of the two short period pulsation modes was
identified as radial; the second is l = 1. Three of the four SPB-type
modes are most likely l = 1 or 2. Comparison with theoretical model
calculations suggests that {$\gamma$} Peg is either a \textasciitilde 8.5
Msolar radial fundamental mode pulsator or a \textasciitilde 9.6
Msolar first radial overtone pulsator. HD 8801 was
corroborated as a `hybrid' {$\delta$} Sct/{$\gamma$} Dor star; four pulsation
modes of the {$\gamma$} Dor type were detected, and two modes of the
{$\delta$} Sct type were confirmed. Two pulsational signals between the
frequency domains of these two known classes of variables were confirmed
and another was newly detected. These are either previously unknown
types of pulsation or do not originate from HD 8801. The O-type star HD
13745 showed small-amplitude slow variability on a time-scale of 3.2 d.
This object may be related to the suspected new type of supergiant SPB
stars, but a rotational origin of its light variations cannot be ruled
out at this point. 53 Psc is an SPB star for which two pulsation
frequencies were determined and identified with low spherical degree.
Small-amplitude variability was formally detected for 53 Ari but is
suspected not to be intrinsic. The behaviour of {$\iota$} Her is consistent
with non-variability during our observations, and we could not confirm
light variations of the comparison star 34 Psc previously suspected. The
use of signal-to-noise criteria in the analysis of data sets with strong
aliasing is critically discussed.},
  file = {/Users/Oliver/Zotero/storage/JPBYS6I8/Handler - 2009 - Confirmation of simultaneous p and g mode excitati.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {stars: chemically peculiar,stars: early-type,stars: individual: γ Peg,stars: oscillations,stars: variables: other,δ Scuti}
}

@article{handler2013,
  title = {Asteroseismology},
  author = {Handler, Gerald},
  year = {2013},
  pages = {207},
  doi = {10.1007/978-94-007-5615-1_4},
  abstract = {Asteroseismology is the determination of the interior structures of stars by using their oscillations as seismic waves. Simple explanations of the astrophysical background and some basic theoretical
considerations needed in this rapidly evolving field are followed by introductions to the most important concepts and methods on the basis of example. Previous and potential applications of asteroseismology are reviewed and future trends are attempted to be foreseen.},
  file = {/Users/Oliver/Zotero/storage/NA3QRPHP/Handler - 2013 - Asteroseismology.pdf},
  journal = {Planets, Stars and Stellar Systems. Volume 4: Stellar Structure and Evolution},
  keywords = {Physics}
}

@article{hansen+1977,
  title = {The Effects of Differential Rotation on the Splitting of Nonradial Modes of Stellar Oscillation},
  author = {Hansen, C. J. and Cox, J. P. and {van Horn}, H. M.},
  year = {1977},
  month = oct,
  volume = {217},
  pages = {151--159},
  issn = {0004-637X},
  doi = {10.1086/155564},
  abstract = {The problem of the splitting of adiabatic nonradial modes of stellar
oscillation owing to slow differential rotation is examined. Integral
expressions for the frequency splitting are derived for the case of
cylindrically symmetric rotation, and, for a particular rotation 'law',
the results are applied to cooling white dwarfs and upper-main-sequence
stars.},
  file = {/Users/Oliver/Zotero/storage/PQ5LM9FS/Hansen et al. - 1977 - The effects of differential rotation on the splitt.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Adiabatic Conditions,Astrophysics,Oscillations,Relativistic Effects,Stellar Models,Stellar Rotation,Stellar Structure,Variable Stars,White Dwarf Stars}
}

@article{hart1954,
  title = {Motions in the {{Sun}} at the Photospheric Level. {{IV}}. {{The}} Equatorial Rotation and Possible Velocity Fields in the Photosphere},
  author = {Hart, A. B.},
  year = {1954},
  volume = {114},
  pages = {17},
  issn = {0035-8711},
  doi = {10.1093/mnras/114.1.17},
  abstract = {Abstract image available at:
http://adsabs.harvard.edu/abs/1954MNRAS.114...17H},
  file = {/Users/Oliver/Zotero/storage/RSIEAN6I/Hart - 1954 - Motions in the Sun at the photospheric level. IV. .pdf},
  journal = {Monthly Notices of the Royal Astronomical Society}
}

@article{hart1956,
  title = {Motions in the {{Sun}} at the Photospheric Level. {{VI}}. {{Large}}-Scale Motions in the Equatorial Region},
  author = {Hart, A. B.},
  year = {1956},
  volume = {116},
  pages = {38},
  issn = {0035-8711},
  doi = {10.1093/mnras/116.1.38},
  abstract = {Abstract image available at:
http://adsabs.harvard.edu/abs/1956MNRAS.116...38H},
  file = {/Users/Oliver/Zotero/storage/VGK9J6RR/Hart - 1956 - Motions in the Sun at the photospheric level. VI. .pdf},
  journal = {Monthly Notices of the Royal Astronomical Society}
}

@article{harvey1985,
  title = {High-{{Resolution Helioseismology}}},
  author = {Harvey, J.},
  year = {1985},
  month = jun,
  volume = {235},
  pages = {199},
  issn = {0379-6566,1609-042X},
  abstract = {The author considers the basic method of helioseismology, some of the considerations that are important in designing an instrument to obtain the required observations, the present status of observational techniques and results and some of the advantages of space observations.},
  file = {/Users/Oliver/Zotero/storage/4RBN64B5/Harvey - 1985 - High-Resolution Helioseismology.pdf;/Users/Oliver/Zotero/storage/DW8DB85L/abstract.html},
  journal = {Future Missions in Solar, Heliospheric \& Space Plasma Physics},
  language = {en}
}

@article{hawkins+2017,
  title = {Red Clump Stars and {{Gaia}}: Calibration of the Standard Candle Using a Hierarchical Probabilistic Model},
  shorttitle = {Red Clump Stars and {{Gaia}}},
  author = {Hawkins, Keith and Leistedt, Boris and Bovy, Jo and Hogg, David W.},
  year = {2017},
  month = oct,
  volume = {471},
  pages = {722},
  doi = {10.1093/mnras/stx1655},
  abstract = {Distances to individual stars in our own Galaxy are critical in order to piece together the nature of its velocity and spatial structure. Core helium burning red clump (RC) stars have similar luminosities, are abundant throughout the Galaxy and thus constitute good standard candles. We build a hierarchical probabilistic model to quantify the quality of RC stars as standard candles using parallax measurements from the first Gaia data release. A unique aspect of our methodology is to fully account for (and marginalize over) parallax, photometry and dust correction uncertainties, which lead to more robust results than standard approaches. We determine the absolute magnitude and intrinsic dispersion of the RC in 2MASS bands J, H, K\textsubscript{s}, Gaia G band and WISE bands W1, W2, W3 and W4. We find that the absolute magnitude of the RC is -1.61 {$\pm$} 0.01 (in K\textsubscript{s}), +0.44 {$\pm$} 0.01 (in G), -0.93 {$\pm$} 0.01 (in J), -1.46 {$\pm$} 0.01 (in H), -1.68 {$\pm$} 0.02 (in W1), -1.69 {$\pm$} 0.02 (in W2), -1.67 {$\pm$} 0.02 (in W3) and -1.76 {$\pm$} 0.01 mag (in W4). The mean intrinsic dispersion is{\~ }0.17 {$\pm$} 0.03 mag across all bands (yielding a typical distance precision of{\~ }8 per cent). Thus RC stars are reliable and precise standard candles. In addition, we have also re-calibrated the zero-point of the absolute magnitude of the RC in each band, which provides a benchmark for future studies to estimate distances to RC stars. Finally, the parallax error shrinkage in the hierarchical model outlined in this work can be used to obtain more precise parallaxes than Gaia for the most distant RC stars across the Galaxy.},
  file = {/Users/Oliver/Zotero/storage/U4J9T5QF/Hawkins et al. - 2017 - Red clump stars and Gaia calibration of the stand.pdf;/Users/Oliver/Zotero/storage/9RL5TWHG/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@article{hawkins+2018,
  title = {Photospheric {{Diagnostics}} of {{Core Helium Burning}} in {{Giant Stars}}},
  author = {Hawkins, Keith and Ting, Yuan-Sen and {Walter-Rix}, Hans},
  year = {2018},
  month = jan,
  volume = {853},
  pages = {20},
  doi = {10.3847/1538-4357/aaa08a},
  abstract = {Core helium burning primary red clump (RC) stars are evolved red giant stars that are excellent standard candles. As such, these stars are routinely used to map the Milky Way or determine the distance to other galaxies, among other things. However, distinguishing RC stars from their less evolved precursors, namely red giant branch (RGB) stars, is still a difficult challenge and has been deemed the domain of asteroseismology. In this paper, we use a sample of 1676 RGB and RC stars that have both single epoch infrared spectra from the APOGEE survey and asteroseismic parameters and classification to show that the spectra alone can be used to (1) predict asteroseismic parameters with precision high enough to (2) distinguish core helium burning RC from other giant stars with less than 2\% contamination. This will not only allow for a clean selection of a large number of standard candles across our own and other galaxies from spectroscopic surveys, but also will remove one of the primary roadblocks for stellar evolution studies of mixing and mass loss in red giant stars.},
  file = {/Users/Oliver/Zotero/storage/YZPJIIRL/Hawkins et al. - 2018 - Photospheric Diagnostics of Core Helium Burning in.pdf;/Users/Oliver/Zotero/storage/8JMSES2E/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en}
}

@article{hayakawa+2017,
  title = {Records of {{Sunspots}} and {{Aurora Candidates}} in the {{Chinese Official Histories}} of the {{Yu}}\textbackslash 'an and {{M}}\textbackslash 'ing {{Dynasties}} during 1261-1644},
  author = {Hayakawa, Hisashi and Tamazawa, Harufumi and Ebihara, Yusuke and Miyahara, Hiroko and Kawamura, Akito Davis and Aoyama, Tadanobu and Isobe, Hiroaki},
  year = {2017},
  month = may,
  abstract = {Records of observations of sunspots and auroras in pre-telescopic historical documents provide useful information about past solar activity both in long-term trends and short-term space weather events. In this study, we present the results of a comprehensive survey of the records of sunspots and aurora candidates in the Yu\textbackslash 'ansh\textbackslash v\{i\} and M\textbackslash 'ingsh\textbackslash v\{i\}, Chinese Official Histories spanning 1261-1368 and 1368-1644, based on continuous observations with well-formatted reportds conducted by contemporary professional astronomers. We then provide a brief comparison of these data with Total Solar Irradiance (TSI) as an indicator of the solar activity during the corresponding periods to show significant active phases between 1350s-80s and 1610s-30s. We then compared the former with contemporary Russian reports for naked-eye sunspots and the latter with contemporary sunspot drawings based on Western telescopic observations. Especially some of the latter are consistent with nitrate signals preserved in ice cores. These results show us some insights on not only minima and maxima of solar activity during 13th - 17th century.},
  archivePrefix = {arXiv},
  eprint = {1705.02238},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/NEJHZJCB/Hayakawa et al. - 2017 - Records of Sunspots and Aurora Candidates in the C.pdf;/Users/Oliver/Zotero/storage/J2K85UJD/1705.html},
  journal = {arXiv:1705.02238 [astro-ph, physics:physics]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics,Physics - History and Philosophy of Physics,Physics - Space Physics},
  primaryClass = {astro-ph, physics:physics}
}

@article{hekker+2011,
  title = {Characterization of Red Giant Stars in the Public {{Kepler}} Data},
  author = {Hekker, S. and Gilliland, R. L. and Elsworth, Y. and Chaplin, W. J. and De Ridder, J. and Stello, D. and Kallinger, T. and Ibrahim, K. A. and Klaus, T. C. and Li, J.},
  year = {2011},
  month = jul,
  volume = {414},
  pages = {2594},
  doi = {10.1111/j.1365-2966.2011.18574.x},
  abstract = {The first public release of long-cadence stellar photometric data collected by the NASA Kepler mission has now been made available. In this paper, we characterize the red giant (G-K) stars in this large sample in terms of their solar-like oscillations. We use published methods and well-known scaling relations in the analysis. Just over 70 per cent of the red giants in the sample show detectable solar-like oscillations, and from these oscillations we are able to estimate the fundamental properties of the stars. This asteroseismic analysis reveals different populations: low-luminosity H-shell burning red giant branch stars, cool high-luminosity red giants on the red giant branch and He-core burning clump and secondary-clump giants.},
  file = {/Users/Oliver/Zotero/storage/2GS86676/Hekker et al. - 2011 - Characterization of red giant stars in the public .pdf;/Users/Oliver/Zotero/storage/BHM3BZ55/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {3}
}

@article{hekker+christensen-dalsgaard2016,
  title = {Giant Star Seismology},
  author = {Hekker, S. and {Christensen-Dalsgaard}, J.},
  year = {2016},
  month = sep,
  abstract = {The internal properties of stars in the red-giant phase undergo significant changes on relatively short timescales. Long near-interrupted high-precision photometric timeseries observations from dedicated space missions such as CoRoT and Kepler have provided seismic inferences of the global and internal properties of a large number of evolved stars, including red giants. These inferences are confronted with predictions from theoretical models to improve our understanding of stellar structure and evolution. Our knowledge and understanding of red giants have indeed increased tremendously using these seismic inferences, and we anticipate that more information is still hidden in the data. Unraveling this will further improve our understanding of stellar evolution. This will also have significant impact on our knowledge of the Milky Way Galaxy as well as on exo-planet host stars. The latter is important for our understanding of the formation and structure of planetary systems.},
  archivePrefix = {arXiv},
  eprint = {1609.07487},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/J79RM4XJ/Hekker and Christensen-Dalsgaard - 2016 - Giant star seismology.pdf;/Users/Oliver/Zotero/storage/5XTVFMQ9/1609.html},
  journal = {arXiv:1609.07487 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{heller2017,
  title = {On the {{Detection}} of {{Extrasolar Moons}} and {{Rings}}},
  author = {Heller, Ren{\'e}},
  year = {2017},
  month = jan,
  abstract = {Since the discovery of a planet transiting its host star in the year 2000, thousands of additional exoplanets and exoplanet candidates have been detected, mostly by NASA's Kepler space telescope. Some of them are almost as small as the Earth's moon. As the solar system is teeming with moons, more than a hundred of which are in orbit around the eight local planets, and with all of the local giant planets showing complex ring systems, astronomers have naturally started to search for moons and rings around exoplanets in the past few years. We here discuss the principles of the observational methods that have been proposed to find moons and rings beyond the solar system and we review the first searches. Though no exomoon or exoring has been unequivocally validated so far, theoretical and technological requirements are now on the verge of being mature for such discoveries.},
  archivePrefix = {arXiv},
  eprint = {1701.04706},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/2S6MMZKS/Heller - 2017 - On the Detection of Extrasolar Moons and Rings.pdf;/Users/Oliver/Zotero/storage/5D54WA8E/1701.html},
  journal = {arXiv:1701.04706 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics},
  primaryClass = {astro-ph}
}

@article{hermes+2017,
  title = {Evidence from {{K2}} for Rapid Rotation in the Descendant of an Intermediate-Mass Star},
  author = {Hermes, J. J. and Kawaler, Steven D. and Romero, A. D. and Kepler, S. O. and Tremblay, P.-E. and Bell, Keaton J. and Dunlap, B. H. and Montgomery, M. H. and Gaensicke, B. T. and Clemens, J. C. and Dennihy, E. and Redfield, S.},
  year = {2017},
  month = apr,
  abstract = {Using patterns in the oscillation frequencies of a white dwarf observed by K2, we have measured the fastest rotation rate, 1.13(02) hr, of any isolated pulsating white dwarf known to date. Balmer-line fits to follow-up spectroscopy from the SOAR telescope show that the star (SDSSJ0837+1856, EPIC 211914185) is a 13,590(340) K, 0.87(03) solar-mass white dwarf. This is the highest mass measured for any pulsating white dwarf with known rotation, suggesting a possible link between high mass and fast rotation. If it is the product of single-star evolution, its progenitor was a roughly 4.0 solar-mass main-sequence B star; we know very little about the angular momentum evolution of such intermediate-mass stars. We explore the possibility that this rapidly rotating white dwarf is the byproduct of a binary merger, which we conclude is unlikely given the pulsation periods observed.},
  archivePrefix = {arXiv},
  eprint = {1704.08690},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/4TRF54VJ/Hermes et al. - 2017 - Evidence from K2 for rapid rotation in the descend.pdf;/Users/Oliver/Zotero/storage/SKXUP6A3/1704.html},
  journal = {arXiv:1704.08690 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{hirsch+2017,
  title = {Assessing the {{Effect}} of {{Stellar Companions}} from {{High}}-{{Resolution Imaging}} of {{Kepler Objects}} of {{Interest}}},
  author = {Hirsch, Lea A. and Ciardi, David R. and Howard, Andrew W. and Everett, Mark E. and Furlan, Elise and Saylors, Mindy and Horch, Elliott P. and Howell, Steve B. and Teske, Johanna and Marcy, Geoffrey W.},
  year = {2017},
  file = {/Users/Oliver/Zotero/storage/PFNUHFA6/1701.06577.pdf},
  journal = {arXiv preprint arXiv:1701.06577}
}

@article{hjorringgaard+2016,
  title = {Testing Stellar Evolution Models with the Retired {{A}} Star {{HD}} 185351},
  author = {Hj{\o}rringgaard, Jakob G. and Aguirre, V. Silva and White, Tim R. and Huber, Daniel and Pope, Benjamin JS and Casagrande, Luca and Justesen, Anders B. and {Christensen-Dalsgaard}, J{\o}rgen},
  year = {2016},
  pages = {stw2559},
  file = {/Users/Oliver/Zotero/storage/4Q7VVJA3/1610.05990v1.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {AR 01/11/16}
}

@article{ho+2016,
  title = {Label {{Transfer}} from {{APOGEE}} to {{LAMOST}}: {{Precise Stellar Parameters}} for 450,000 {{LAMOST Giants}}},
  shorttitle = {Label {{Transfer}} from {{APOGEE}} to {{LAMOST}}},
  author = {Ho, Anna Y. Q. and Ness, Melissa K. and Hogg, David W. and Rix, Hans-Walter and Liu, Chao and Yang, Fan and Zhang, Yong and Hou, Yonghui and Wang, Yuefei},
  year = {2016},
  month = jan,
  volume = {1602},
  pages = {arXiv:1602.00303},
  abstract = {In this era of large-scale stellar spectroscopic surveys, measurements
of stellar attributes ("labels," i.e. parameters and abundances) must be
made precise and consistent across surveys. Here, we demonstrate that
this can be achieved by a data-driven approach to spectral modeling.
With The Cannon, we transfer information from the APOGEE survey to
determine precise Teff, log g, [Fe/H], and [\$\textbackslash alpha\$/M] from the spectra
of 450,000 LAMOST giants. The Cannon fits a predictive model for LAMOST
spectra using 9952 stars observed in common between the two surveys,
taking five labels from APOGEE DR12 as ground truth: Teff, log g,
[Fe/H], [\textbackslash alpha/M], and K-band extinction \$A\_k\$. The model is then used
to infer Teff, log g, [Fe/H], and [\$\textbackslash alpha\$/M] for 454,180 giants, 20\%
of the LAMOST DR2 stellar sample. These are the first [\$\textbackslash alpha\$/M]
values for the full set of LAMOST giants, and the largest catalog of
[\$\textbackslash alpha\$/M] for giant stars to date. Furthermore, these labels are by
construction on the APOGEE label scale; for spectra with S/N {$>$} 50,
cross-validation of the model yields typical uncertainties of 70K in
Teff, 0.1 in log g, 0.1 in [Fe/H], and 0.04 in [\$\textbackslash alpha\$/M], values
comparable to the broadly stated, conservative APOGEE DR12
uncertainties. Thus, by using "label transfer" to tie low-resolution
(LAMOST R \$\textbackslash sim\$ 1800) spectra to the label scale of a much
higher-resolution (APOGEE R \$\textbackslash sim\$ 22,500) survey, we substantially
reduce the inconsistencies between labels measured by the individual
survey pipelines. This demonstrates that label transfer with The Cannon
can successfully bring different surveys onto the same physical scale.},
  journal = {ArXiv e-prints},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics}
}

@article{hoffman+gelman2014,
  title = {The {{No}}-{{U}}-{{Turn Sampler}}: {{Adaptively Setting Path Lengths}} in {{Hamiltonian Monte Carlo}}},
  shorttitle = {The {{No}}-{{U}}-{{Turn Sampler}}},
  author = {Hoffman, Matthew D. and Gelman, Andrew},
  year = {2014},
  volume = {15},
  pages = {1593--1623},
  issn = {1533-7928},
  file = {/Users/Oliver/Zotero/storage/G9CAXMAK/Hoffman and Gelman - 2014 - The No-U-Turn Sampler Adaptively Setting Path Len.pdf;/Users/Oliver/Zotero/storage/G8HUJXGI/hoffman14a.html},
  journal = {Journal of Machine Learning Research},
  number = {47}
}

@article{hog+2000,
  title = {The {{Tycho}}-2 Catalogue of the 2.5 Million Brightest Stars},
  author = {H{\o}g, E. and Fabricius, C. and Makarov, V. V. and Urban, S. and Corbin, T. and Wycoff, G. and Bastian, U. and Schwekendiek, P. and Wicenec, A.},
  year = {2000},
  month = mar,
  volume = {355},
  pages = {L27-L30},
  issn = {0004-6361},
  abstract = {The Tycho-2 Catalogue presented here is an astrometric reference catalogue containing positions and proper motions as well as two-colour photometric data for the 2.5 million brightest stars in the sky. The Tycho-2 positions and magnitudes are based on precisely the same observations as the original Tycho Catalogue (hereafter Tycho-1) collected by the star mapper of the ESA Hipparcos satellite, but Tycho-2 is much bigger and slightly more precise, owing to a more advanced reduction technique. Components of double stars with separations down to 0.8 arcsec are included. Proper motions precise to about 2.5 mas/yr are given as derived from a comparison with the Astrographic Catalogue and 143 other ground-based astrometric catalogues, all reduced to the Hipparcos celestial coordinate system. Tycho-2 supersedes in most applications Tycho-1, as well as the ACT and TRC catalogues based on Tycho-1. Based on observations made with the ESA Hipparcos astrometry satellite. The catalogue is distributed on CD-ROM and through the astronomical data centres, and further information is given on the website http://www.astro.ku.dk/\textasciitilde erik/Tycho-2.},
  file = {/Users/Oliver/Zotero/storage/VGL4M7WN/Høg et al. - 2000 - The Tycho-2 catalogue of the 2.5 million brightest.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {ASTROMETRY,CATALOGS,STARS: FUNDAMENTAL PARAMETERS}
}

@article{hogg+2010,
  title = {Data Analysis Recipes: {{Fitting}} a Model to Data},
  shorttitle = {Data Analysis Recipes},
  author = {Hogg, David W. and Bovy, Jo and Lang, Dustin},
  year = {2010},
  month = aug,
  pages = {arXiv:1008.4686},
  abstract = {We go through the many considerations involved in fitting a model to data, using as an example the fit of a straight line to a set of points in a two-dimensional plane. Standard weighted least-squares fitting is only appropriate when there is a dimension along which the data points have negligible uncertainties, and another along which all the uncertainties can be described by Gaussians of known variance; these conditions are rarely met in practice. We consider cases of general, heterogeneous, and arbitrarily covariant two-dimensional uncertainties, and situations in which there are bad data (large outliers), unknown uncertainties, and unknown but expected intrinsic scatter in the linear relationship being fit. Above all we emphasize the importance of having a "generative model" for the data, even an approximate one. Once there is a generative model, the subsequent fitting is non-arbitrary because the model permits direct computation of the likelihood of the parameters or the posterior probability distribution. Construction of a posterior probability distribution is indispensible if there are "nuisance parameters" to marginalize away.},
  file = {/Users/Oliver/Zotero/storage/8XUUFTIN/Hogg et al. - 2010 - Data analysis recipes Fitting a model to data.pdf;/Users/Oliver/Zotero/storage/PQE48L9Y/ui.adsabs.harvard.edu.html},
  journal = {ArXiv e-prints},
  language = {en}
}

@article{hogg2012,
  title = {Data Analysis Recipes: {{Probability}} Calculus for Inference},
  shorttitle = {Data Analysis Recipes},
  author = {Hogg, David W.},
  year = {2012},
  month = may,
  pages = {arXiv:1205.4446},
  abstract = {In this pedagogical text aimed at those wanting to start thinking about or brush up on probabilistic inference, I review the rules by which probability distribution functions can (and cannot) be combined. I connect these rules to the operations performed in probabilistic data analysis. Dimensional analysis is emphasized as a valuable tool for helping to construct non-wrong probabilistic statements. The applications of probability calculus in constructing likelihoods, marginalized likelihoods, posterior probabilities, and posterior predictions are all discussed.},
  file = {/Users/Oliver/Zotero/storage/9AFMTB33/Hogg - 2012 - Data analysis recipes Probability calculus for in.pdf;/Users/Oliver/Zotero/storage/UBI46Y85/abstract.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{hogg2018,
  title = {A Likelihood Function for the {{Gaia Data}}},
  author = {Hogg, David W.},
  year = {2018},
  month = apr,
  pages = {arXiv:1804.07766},
  abstract = {When we perform probabilistic inferences with the Gaia Mission data, we technically require a likelihood function, or a probability of the (raw-ish) data as a function of stellar (astrometric and photometric) properties. Unfortunately, we aren't (at present) given access to the Gaia data directly; we are only given a Catalog of derived astrometric properties for the stars. How do we perform probabilistic inferences in this context? The answer - implicit in many publications - is that we should look at the Gaia Catalog as containing the parameters of a likelihood function, or a probability of the Gaia data, conditioned on stellar properties, evaluated at the location of the data. Concretely, my recommendation is to assume (for, say, the parallax) that the Catalog-reported value and uncertainty are the mean and root-variance of a Gaussian function that can stand in for the true likelihood function. This is the implicit assumption in most Gaia literature to date; my only goal here is to make the assumption explicit. Certain technical choices by the Mission team slightly invalidate this assumption for DR1 (TGAS), but not seriously. Generalizing beyond Gaia, it is important to downstream users of any Catalog products that they deliver likelihood information about the fundamental data; this is a challenge for the probabilistic catalogs of the future.},
  file = {/Users/Oliver/Zotero/storage/9TTY8RNE/Hogg - 2018 - A likelihood function for the Gaia Data.pdf;/Users/Oliver/Zotero/storage/JFVCIYDJ/ui.adsabs.harvard.edu.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{holczer+2016,
  title = {Transit {{Timing Observations}} from {{Kepler}}. {{IX}}. {{Catalog}} of the {{Full Long}}-{{Cadence Data Set}}},
  author = {Holczer, Tomer and Mazeh, Tsevi and Nachmani, Gil and {Jontof-Hutter}, Daniel and Ford, Eric B. and Fabrycky, Daniel and Ragozzine, Darin and Kane, Mackenzie and Steffen, Jason H.},
  year = {2016},
  month = jul,
  volume = {225},
  pages = {9},
  issn = {1538-4365},
  doi = {10.3847/0067-0049/225/1/9},
  abstract = {We present a new transit timing catalog of 2599 Kepler Objects of Interest (=KOIs), using the PDC-MAP long-cadence light curves that include the full seventeen quarters of the mission (ftp://wise- ftp.tau.ac.il/pub/tauttv/TTV/ver\_112). The goal is to produce an easy-to-use catalog that can stimulate further analyses of interesting systems. For 779 KOIs with high enough SNRs, we derived the timing, duration and depth of 69,914 transits. For 1820 KOIs with lower SNR, we derived only the timing of 225,273 transits. After removal of outlier timings, we derived various statistics for each KOI that were used to indicate significant variations. Including systems found by previous works, we have detected 260 KOIs which showed significant TTVs with long-term variations ({$>$}100 day), and another fourteen KOIs with periodic modulations shorter than 100 day and small amplitudes. For five of those, the periodicity is probably due to the crossing of rotating stellar spots by the transiting planets.},
  archivePrefix = {arXiv},
  eprint = {1606.01744},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/F224B53Z/Holczer et al. - 2016 - Transit Timing Observations from Kepler. IX. Catal.pdf;/Users/Oliver/Zotero/storage/IMSJSR6H/1606.html},
  journal = {The Astrophysical Journal Supplement Series},
  keywords = {C3},
  number = {1}
}

@article{hon+2017,
  title = {Deep Learning Classification in Asteroseismology},
  author = {Hon, Marc and Stello, Dennis and Yu, Jie},
  year = {2017},
  month = aug,
  volume = {469},
  pages = {4578},
  doi = {10.1093/mnras/stx1174},
  abstract = {In the power spectra of oscillating red giants, there are visually distinct features defining stars ascending the red giant branch from those that have commenced helium core burning. We train a 1D convolutional neural network by supervised learning to automatically learn these visual features from images of folded oscillation spectra. By training and testing on Kepler red giants, we achieve an accuracy of up to 99 per cent in separating helium-burning red giants from those ascending the red giant branch. The convolutional neural network additionally shows capability in accurately predicting the evolutionary states of 5379 previously unclassified Kepler red giants, by which we now have greatly increased the number of classified stars.},
  file = {/Users/Oliver/Zotero/storage/J4Z2XM7G/Hon et al. - 2017 - Deep learning classification in asteroseismology.pdf;/Users/Oliver/Zotero/storage/Y2AS7G4U/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {4}
}

@article{houdek+1999,
  title = {Amplitudes of Stochastically Excited Oscillations in Main-Sequence Stars},
  author = {Houdek, G. and Balmforth, N. J. and {Christensen-Dalsgaard}, J. and Gough, D. O.},
  year = {1999},
  month = nov,
  volume = {351},
  pages = {582--596},
  issn = {0004-6361},
  abstract = {We present estimates of the amplitudes of intrinsically stable stochastically excited radial oscillations in stars near the main sequence. The amplitudes are determined by the balance between
acoustical energy generation by turbulent convection (the Lighthill mechanism) and linear damping. Convection is treated with a
time-dependent, nonlocal, mixing-length model, which includes both convective heat flux and turbulent pressure in both the equilibrium model and the pulsations. Velocity and luminosity amplitudes are computed for stars with masses between 0.9 M\_sun and 2.0 M\_sun in the vicinity of the main sequence, for various metallicities and convection parameters. As in previous studies, the amplitudes are found to increase with stellar mass, and therefore with luminosity. Amongst those stars that are pulsationally stable, the largest amplitudes are predicted for a 1.6 M\_sun model of spectral type F2; the values are approximately 15 times larger than those measured in the Sun.},
  file = {/Users/Oliver/Zotero/storage/8JNN2UFE/Houdek et al. - 1999 - Amplitudes of stochastically excited oscillations .pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {CONVECTION,STARS: OSCILLATIONS,TURBULENCE}
}

@article{houdek2017,
  title = {Calibrating Damping Rates with {{LEGACY}} Linewidths},
  author = {Houdek, G{\"u}nter},
  year = {2017},
  month = feb,
  abstract = {Linear damping rates of radial oscillation modes in selected \$Kepler\$ stars are estimated with the help of a nonadiabatic stability analysis. The convective fluxes are obtained from a nonlocal, time-dependent convection model. The mixing-length parameter is calibrated to the surface-convection-zone depth of a stellar model obtained from fitting adiabatic frequencies to the LEGACY observations, and two of the three nonlocal convection parameters are calibrated to the corresponding LEGACY linewidth measurements. The atmospheric structure in the 1D stability analysis adopts a temperature-optical-depth relation derived from 3D hydrodynamical simulations. Results from 3D simulations are also used to calibrate the turbulent pressure and to guide the functional form of the depth-dependence of the anisotropy of the turbulent velocity field in the 1D stability computations.},
  archivePrefix = {arXiv},
  eprint = {1702.04251},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/VN6T569X/Houdek - 2017 - Calibrating damping rates with LEGACY linewidths.pdf;/Users/Oliver/Zotero/storage/JI6XPTSZ/1702.html},
  journal = {arXiv:1702.04251 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{howe+2017,
  title = {Parametrizing the Time Variation of the `Surface Term' of Stellar p-Mode Frequencies: Application to Helioseismic Data},
  shorttitle = {Parametrizing the Time Variation of the `Surface Term' of Stellar p-Mode Frequencies},
  author = {Howe, R. and Basu, S. and Davies, G. R. and Ball, W. H. and Chaplin, W. J. and Elsworth, Y. and Komm, R.},
  year = {2017},
  month = feb,
  volume = {464},
  pages = {4777--4788},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stw2668},
  file = {/Users/Oliver/Zotero/storage/TBW7EIIC/4777.full.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {4}
}

@article{howell+2014,
  title = {The {{K2 Mission}}: {{Characterization}} and {{Early Results}}},
  shorttitle = {The {{K2 Mission}}},
  author = {Howell, Steve B. and Sobeck, Charlie and Haas, Michael and Still, Martin and Barclay, Thomas and Mullally, Fergal and Troeltzsch, John and Aigrain, Suzanne and Bryson, Stephen T. and Caldwell, Doug and Chaplin, William J. and Cochran, William D. and Huber, Daniel and Marcy, Geoffrey W. and Miglio, Andrea and Najita, Joan R. and Smith, Marcie and Twicken, J. D. and Fortney, Jonathan J.},
  year = {2014},
  month = apr,
  volume = {126},
  pages = {398},
  issn = {0004-6280},
  doi = {10.1086/676406},
  abstract = {The K2 mission will make use of the Kepler spacecraft and its assets to expand upon Kepler's groundbreaking discoveries in the fields of exoplanets and astrophysics through new and exciting observations. K2 will use an innovative way of operating the spacecraft to observe target fields along the ecliptic for the next 2-3 years. Early science
commissioning observations have shown an estimated photometric precision near 400 ppm in a single 30 minute observation, and a 6-hour photometric precision of 80 ppm (both at V=12). The K2 mission offers long-term, simultaneous optical observation of thousands of objects at a precision far better than is achievable from ground-based telescopes. Ecliptic fields will be observed for approximately 75-days enabling a unique exoplanet survey which fills the gaps in duration and sensitivity between the Kepler and TESS missions, and offers pre-launch exoplanet target identification for JWST transit spectroscopy. Astrophysics observations with K2 will include studies of young open clusters, bright stars, galaxies, supernovae, and asteroseismology.},
  file = {/Users/Oliver/Zotero/storage/UDRD59IJ/Howell et al. - 2014 - The K2 Mission Characterization and Early Results.pdf},
  journal = {Publications of the Astronomical Society of the Pacific}
}

@article{huber+2009,
  title = {Automated Extraction of Oscillation Parameters for {{Kepler}} Observations of Solar-Type Stars},
  author = {Huber, D. and Stello, D. and Bedding, T. R. and Chaplin, W. J. and Arentoft, T. and Quirion, P.-O. and Kjeldsen, H.},
  year = {2009},
  month = oct,
  volume = {160},
  pages = {74},
  abstract = {The recent launch of the Kepler space telescope brings the opportunity to study oscillations systematically in large numbers of solar-like stars. In the framework of the asteroFLAG project, we have developed an automated pipeline to estimate global oscillation parameters, such as the frequency of maximum power ({$\nu$}max ) and the large frequency spacing ({$\increment\nu$}), for a large number of time series. We present an effective method based on the autocorrelation function to find excess power and use a scaling relation to estimate granulation timescales as initial conditions for background modelling. We derive reliable uncertainties for {$\nu$}max and {$\increment\nu$} through extensive simulations. We have tested the pipeline on about 2000 simulated Kepler stars with magnitudes of V{\~ } 7-12 and were able to correctly determine {$\nu$}max and {$\increment\nu$} for about half of the sample. For about 20\%, the returned large frequency spacing is accurate enough to determine stellar radii to a 1\% precision. We conclude that the methods presented here are a promising approach to process the large amount of data expected from Kepler.},
  file = {/Users/Oliver/Zotero/storage/GVHE9WB6/Huber et al. - 2009 - Automated extraction of oscillation parameters for.pdf;/Users/Oliver/Zotero/storage/53KUIED6/abstract.html},
  journal = {Communications in Asteroseismology},
  language = {en}
}

@article{huber+2009a,
  title = {Automated Extraction of Oscillation Parameters for {{Kepler}} Observations of Solar-Type Stars},
  author = {Huber, Daniel and Stello, Dennis and Bedding, Timothy R. and Chaplin, William J. and Arentoft, Torben and Quirion, Pierre-Olivier and Kjeldsen, Hans},
  year = {2009},
  month = oct,
  abstract = {The recent launch of the Kepler space telescope brings the opportunity to study oscillations systematically in large numbers of solar-like stars. In the framework of the asteroFLAG project, we have developed an automated pipeline to estimate global oscillation parameters, such as the frequency of maximum power (nu\_max) and the large frequency spacing (Delta\_nu), for a large number of time series. We present an effective method based on the autocorrelation function to find excess power and use a scaling relation to estimate granulation timescales as initial conditions for background modelling. We derive reliable uncertainties for nu\_max and Delta\_nu through extensive simulations. We have tested the pipeline on about 2000 simulated Kepler stars with magnitudes of V\textasciitilde 7-12 and were able to correctly determine nu\_max and Delta\_nu for about half of the sample. For about 20\%, the returned large frequency spacing is accurate enough to determine stellar radii to a 1\% precision. We conclude that the methods presented here are a promising approach to process the large amount of data expected from Kepler.},
  archivePrefix = {arXiv},
  eprint = {0910.2764},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/RE2C6M7Z/Huber et al. - 2009 - Automated extraction of oscillation parameters for.pdf;/Users/Oliver/Zotero/storage/MIUGSN77/0910.html},
  journal = {arXiv:0910.2764 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{huber+2011,
  title = {Testing {{Scaling Relations}} for {{Solar}}-like {{Oscillations}} from the {{Main Sequence}} to {{Red Giants Using Kepler Data}}},
  author = {Huber, D. and Bedding, T. R. and Stello, D. and Hekker, S. and Mathur, S. and Mosser, B. and Verner, G. A. and Bonanno, A. and Buzasi, D. L. and Campante, T. L. and Elsworth, Y. P. and Hale, S. J. and Kallinger, T. and Silva Aguirre, V. and Chaplin, W. J. and De Ridder, J. and Garc{\'i}a, R. A. and Appourchaux, T. and Frandsen, S. and Houdek, G. and {Molenda-{\.Z}akowicz}, J. and Monteiro, M. J. P. F. G. and {Christensen-Dalsgaard}, J. and Gilliland, R. L. and Kawaler, S. D. and Kjeldsen, H. and Broomhall, A. M. and Corsaro, E. and Salabert, D. and Sanderfer, D. T. and Seader, S. E. and Smith, J. C.},
  year = {2011},
  month = dec,
  volume = {743},
  pages = {143},
  doi = {10.1088/0004-637X/743/2/143},
  abstract = {We have analyzed solar-like oscillations in \textasciitilde 1700 stars observed by the Kepler Mission, spanning from the main sequence to the red clump. Using evolutionary models, we test asteroseismic scaling relations for the frequency of maximum power ({$\nu$}\textsubscript{max}), the large frequency separation ({$\increment\nu$}), and oscillation amplitudes. We show that the difference of the {$\increment\nu$}-{$\nu$}\textsubscript{max} relation for unevolved and evolved stars can be explained by different distributions in effective temperature and stellar mass, in agreement with what is expected from scaling relations. For oscillation amplitudes, we show that neither (L/M)\textsuperscript{ s } scaling nor the revised scaling relation by Kjeldsen \& Bedding is accurate for red-giant stars, and demonstrate that a revised scaling relation with a separate luminosity-mass dependence can be used to calculate amplitudes from the main sequence to red giants to a precision of \textasciitilde 25\%. The residuals show an offset particularly for unevolved stars, suggesting that an additional physical dependency is necessary to fully reproduce the observed amplitudes. We investigate correlations between amplitudes and stellar activity, and find evidence that the effect of amplitude suppression is most pronounced for subgiant stars. Finally, we test the location of the cool edge of the instability strip in the Hertzsprung-Russell diagram using solar-like oscillations and find the detections in the hottest stars compatible with a domain of hybrid stochastically excited and opacity driven pulsation.},
  file = {/Users/Oliver/Zotero/storage/LXCQLGWD/Huber et al. - 2011 - Testing Scaling Relations for Solar-like Oscillati.pdf;/Users/Oliver/Zotero/storage/7I9G8SGJ/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{huber+2011a,
  title = {Solar-like {{Oscillations}} and {{Activity}} in {{Procyon}}: {{A Comparison}} of the 2007 {{MOST}} and {{Ground}}-Based {{Radial Velocity Campaigns}}},
  shorttitle = {Solar-like {{Oscillations}} and {{Activity}} in {{Procyon}}},
  author = {Huber, Daniel and Bedding, Timothy R. and Arentoft, Torben and Gruberbauer, Michael and Guenther, David B. and Houdek, G{\"u}nter and Kallinger, Thomas and Kjeldsen, Hans and Matthews, Jaymie M. and Stello, Dennis and Weiss, Werner W.},
  year = {2011},
  month = apr,
  volume = {731},
  pages = {94},
  doi = {10.1088/0004-637X/731/2/94},
  abstract = {We compare the simultaneous 2007 space-based MOST photometry and ground-based radial velocity (RV) observations of the F5 star Procyon. We identify slow variations in the MOST data that are similar to those reported in the RV time series and confirm by comparison with the Sun that these variations are likely the signature of stellar activity. The MOST power spectrum yields clear evidence for individual oscillation frequencies that match those found in the RV data by Bedding et al. We identify the same ridges due to modes of different spherical degree in both data sets, but are not able to confirm a definite ridge identification using the MOST data. We measure the luminosity amplitude per radial mode A \textsubscript{ l=0,phot} = 9.1 {$\pm$} 0.5 ppm. Combined with the estimate for the RV data by Arentoft et al., this gives a mean amplitude ratio of A \textsubscript{ l=0,phot}/A \textsubscript{ l=0,RV} = 0.24 {$\pm$} 0.02 ppm cm\textsuperscript{-1} s, considerably higher than expected from scaling relations but in reasonable agreement with theoretical models by Houdek. We also compare the amplitude ratio as a function of frequency and find that the maximum of the oscillation envelope is shifted to higher frequencies in photometry than in velocity. Based on data from the MOST satellite, a Canadian Space Agency mission, jointly operated by Dynacon Inc., the University of Toronto Institute for Aerospace Studies and the University of British Columbia, with the assistance of the University of Vienna.},
  file = {/Users/Oliver/Zotero/storage/C9M2BMHZ/Huber et al. - 2011 - Solar-like Oscillations and Activity in Procyon A.pdf;/Users/Oliver/Zotero/storage/QCIJDJZI/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{huber+2012,
  title = {Validation of the Exoplanet {{Kepler}}-21b Using {{PAVO}}/{{CHARA}} Long-Baseline Interferometry},
  author = {Huber, Daniel and Ireland, Michael J. and Bedding, Timothy R. and Howell, Steve B. and Maestro, Vicente and M{\'e}rand, Antoine and Tuthill, Peter G. and White, Timothy R. and Farrington, Christopher D. and Goldfinger, P. J. and McAlister, Harold A. and Schaefer, Gail H. and Sturmann, Judit and Sturmann, Laszlo and Brummelaar, Ten and A, Theo and Turner, Nils H.},
  year = {2012},
  month = jun,
  volume = {423},
  pages = {L16},
  doi = {10.1111/j.1745-3933.2012.01242.x},
  abstract = {We present long-baseline interferometry of the Kepler exoplanet host star HD 179070 (Kepler-21) using the Precision Astronomical Visible Observations (PAVO) beam combiner at the Center for High Angular Resolution Astronomy (CHARA) Array. The visibility data are consistent with a single star and exclude stellar companions at separations{\~ }1-1000 mas {\~(}0.1-113 au) and contrasts \<3.5 mag. This result supports the validation of the 1.6 R \textsubscript{{$\oplus$}} exoplanet Kepler-21b by Howell et al. and complements the constraints set by adaptive optics imaging, speckle interferometry and radial-velocity observations to rule out false positives due to stellar companions. We conclude that long-baseline interferometry has strong potential to validate transiting extrasolar planets, particularly for future projects aimed at brighter stars and for host stars where radial-velocity follow-up is not available.},
  file = {/Users/Oliver/Zotero/storage/I9KLLB52/Huber et al. - 2012 - Validation of the exoplanet Kepler-21b using PAVO.pdf;/Users/Oliver/Zotero/storage/WP3Z3K7U/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@article{huber+2013,
  title = {Fundamental {{Properties}} of {{Kepler Planet}}-Candidate {{Host Stars}} Using {{Asteroseismology}}},
  author = {Huber, Daniel and Chaplin, William J. and {Christensen-Dalsgaard}, J{\o}rgen and Gilliland, Ronald L. and Kjeldsen, Hans and Buchhave, Lars A. and Fischer, Debra A. and Lissauer, Jack J. and Rowe, Jason F. and {Sanchis-Ojeda}, Roberto and Basu, Sarbani and Handberg, Rasmus and Hekker, Saskia and Howard, Andrew W. and Isaacson, Howard and Karoff, Christoffer and Latham, David W. and Lund, Mikkel N. and Lundkvist, Mia and Marcy, Geoffrey W. and Miglio, Andrea and Silva Aguirre, Victor and Stello, Dennis and Arentoft, Torben and Barclay, Thomas and Bedding, Timothy R. and Burke, Christopher J. and Christiansen, Jessie L. and Elsworth, Yvonne P. and Haas, Michael R. and Kawaler, Steven D. and Metcalfe, Travis S. and Mullally, Fergal and Thompson, Susan E.},
  year = {2013},
  month = apr,
  volume = {767},
  pages = {127},
  doi = {10.1088/0004-637X/767/2/127},
  abstract = {We have used asteroseismology to determine fundamental properties for 66 Kepler planet-candidate host stars, with typical uncertainties of 3\% and 7\% in radius and mass, respectively. The results include new asteroseismic solutions for four host stars with confirmed planets (Kepler-4, Kepler-14, Kepler-23 and Kepler-25) and increase the total number of Kepler host stars with asteroseismic solutions to 77. A comparison with stellar properties in the planet-candidate catalog by Batalha et al. shows that radii for subgiants and giants obtained from spectroscopic follow-up are systematically too low by up to a factor of 1.5, while the properties for unevolved stars are in good agreement. We furthermore apply asteroseismology to confirm that a large majority of cool main-sequence hosts are indeed dwarfs and not misclassified giants. Using the revised stellar properties, we recalculate the radii for 107 planet candidates in our sample, and comment on candidates for which the radii change from a previously giant-planet/brown-dwarf/stellar regime to a sub-Jupiter size or vice versa. A comparison of stellar densities from asteroseismology with densities derived from transit models in Batalha et al. assuming circular orbits shows significant disagreement for more than half of the sample due to systematics in the modeled impact parameters or due to planet candidates that may be in eccentric orbits. Finally, we investigate tentative correlations between host-star masses and planet-candidate radii, orbital periods, and multiplicity, but caution that these results may be influenced by the small sample size and detection biases.},
  file = {/Users/Oliver/Zotero/storage/8PMGPRPQ/Huber et al. - 2013 - Fundamental Properties of Kepler Planet-candidate .pdf;/Users/Oliver/Zotero/storage/MCZESDNN/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{huber+2013a,
  title = {Stellar {{Spin}}-{{Orbit Misalignment}} in a {{Multiplanet System}}},
  author = {Huber, Daniel and Carter, Joshua A. and Barbieri, Mauro and Miglio, Andrea and Deck, Katherine M. and Fabrycky, Daniel C. and Montet, Benjamin T. and Buchhave, Lars A. and Chaplin, William J. and Hekker, Saskia and Montalb{\'a}n, Josefina and {Sanchis-Ojeda}, Roberto and Basu, Sarbani and Bedding, Timothy R. and Campante, Tiago L. and {Christensen-Dalsgaard}, J{\o}rgen and Elsworth, Yvonne P. and Stello, Dennis and Arentoft, Torben and Ford, Eric B. and Gilliland, Ronald L. and Handberg, Rasmus and Howard, Andrew W. and Isaacson, Howard and Johnson, John Asher and Karoff, Christoffer and Kawaler, Steven D. and Kjeldsen, Hans and Latham, David W. and Lund, Mikkel N. and Lundkvist, Mia and Marcy, Geoffrey W. and Metcalfe, Travis S. and Silva Aguirre, Victor and Winn, Joshua N.},
  year = {2013},
  month = oct,
  volume = {342},
  pages = {331},
  doi = {10.1126/science.1242066},
  abstract = {Stars hosting hot Jupiters are often observed to have high obliquities, whereas stars with multiple coplanar planets have been seen to have low obliquities. This has been interpreted as evidence that hot-Jupiter formation is linked to dynamical disruption, as opposed to planet migration through a protoplanetary disk. We used asteroseismology to measure a large obliquity for Kepler-56, a red giant star hosting two transiting coplanar planets. These observations show that spin-orbit misalignments are not confined to hot-Jupiter systems. Misalignments in a broader class of systems had been predicted as a consequence of torques from wide-orbiting companions, and indeed radial velocity measurements revealed a third companion in a wide orbit in the Kepler-56 system.},
  file = {/Users/Oliver/Zotero/storage/L5IL69TP/Huber et al. - 2013 - Stellar Spin-Orbit Misalignment in a Multiplanet S.pdf;/Users/Oliver/Zotero/storage/WBG2NQ4Y/ui.adsabs.harvard.edu.html},
  journal = {Science},
  language = {en},
  number = {6156}
}

@article{huber+2013b,
  title = {Fundamental {{Properties}} of {{Kepler Planet}}-Candidate {{Host Stars}} Using {{Asteroseismology}}},
  author = {Huber, Daniel and Chaplin, William J. and {Christensen-Dalsgaard}, J{\o}rgen and Gilliland, Ronald L. and Kjeldsen, Hans and Buchhave, Lars A. and Fischer, Debra A. and Lissauer, Jack J. and Rowe, Jason F. and {Sanchis-Ojeda}, Roberto and Basu, Sarbani and Handberg, Rasmus and Hekker, Saskia and Howard, Andrew W. and Isaacson, Howard and Karoff, Christoffer and Latham, David W. and Lund, Mikkel N. and Lundkvist, Mia and Marcy, Geoffrey W. and Miglio, Andrea and Silva Aguirre, Victor and Stello, Dennis and Arentoft, Torben and Barclay, Thomas and Bedding, Timothy R. and Burke, Christopher J. and Christiansen, Jessie L. and Elsworth, Yvonne P. and Haas, Michael R. and Kawaler, Steven D. and Metcalfe, Travis S. and Mullally, Fergal and Thompson, Susan E.},
  year = {2013},
  month = apr,
  volume = {767},
  pages = {127},
  issn = {0004-637X},
  doi = {10.1088/0004-637X/767/2/127},
  abstract = {We have used asteroseismology to determine fundamental properties for 66
Kepler planet-candidate host stars, with typical uncertainties of 3\% and
7\% in radius and mass, respectively. The results include new
asteroseismic solutions for four host stars with confirmed planets
(Kepler-4, Kepler-14, Kepler-23 and Kepler-25) and increase the total
number of Kepler host stars with asteroseismic solutions to 77. A
comparison with stellar properties in the planet-candidate catalog by
Batalha et al. shows that radii for subgiants and giants obtained from
spectroscopic follow-up are systematically too low by up to a factor of
1.5, while the properties for unevolved stars are in good agreement. We
furthermore apply asteroseismology to confirm that a large majority of
cool main-sequence hosts are indeed dwarfs and not misclassified giants.
Using the revised stellar properties, we recalculate the radii for 107
planet candidates in our sample, and comment on candidates for which the
radii change from a previously giant-planet/brown-dwarf/stellar regime
to a sub-Jupiter size or vice versa. A comparison of stellar densities
from asteroseismology with densities derived from transit models in
Batalha et al. assuming circular orbits shows significant disagreement
for more than half of the sample due to systematics in the modeled
impact parameters or due to planet candidates that may be in eccentric
orbits. Finally, we investigate tentative correlations between host-star
masses and planet-candidate radii, orbital periods, and multiplicity,
but caution that these results may be influenced by the small sample
size and detection biases.},
  file = {/Users/Oliver/Zotero/storage/QPEXTLWW/Huber et al. - 2013 - Fundamental Properties of Kepler Planet-candidate .pdf},
  journal = {The Astrophysical Journal},
  keywords = {planetary systems,stars: late-type,stars: oscillations,techniques: photometric,techniques: spectroscopic}
}

@article{huber+2014,
  title = {Revised {{Stellar Properties}} of {{Kepler Targets}} for the {{Quarter}} 1-16 {{Transit Detection Run}}},
  author = {Huber, Daniel and Silva Aguirre, Victor and Matthews, Jaymie M. and Pinsonneault, Marc H. and Gaidos, Eric and Garc{\'i}a, Rafael A. and Hekker, Saskia and Mathur, Savita and Mosser, Benoit and Torres, Guillermo and Bastien, Fabienne A. and Basu, Sarbani and Bedding, Timothy R. and Chaplin, William J. and Demory, Brice-Olivier and Fleming, Scott W. and Guo, Zhao and Mann, Andrew W. and Rowe, Jason F. and Serenelli, Aldo M. and Smith, Myron A. and Stello, Dennis},
  year = {2014},
  month = mar,
  volume = {211},
  pages = {2},
  doi = {10.1088/0067-0049/211/1/2},
  abstract = {We present revised properties for 196,468 stars observed by the NASA Kepler mission and used in the analysis of Quarter 1-16 (Q1-Q16) data to detect and characterize transiting planets. The catalog is based on a compilation of literature values for atmospheric properties (temperature, surface gravity, and metallicity) derived from different observational techniques (photometry, spectroscopy, asteroseismology, and exoplanet transits), which were then homogeneously fitted to a grid of Dartmouth stellar isochrones. We use broadband photometry and asteroseismology to characterize 11,532 Kepler targets which were previously unclassified in the Kepler Input Catalog (KIC). We report the detection of oscillations in 2762 of these targets, classifying them as giant stars and increasing the number of known oscillating giant stars observed by Kepler by \textasciitilde 20\% to a total of \textasciitilde 15,500 stars. Typical uncertainties in derived radii and masses are \textasciitilde 40\% and \textasciitilde 20\%, respectively, for stars with photometric constraints only, and 5\%-15\% and \textasciitilde 10\% for stars based on spectroscopy and/or asteroseismology, although these uncertainties vary strongly with spectral type and luminosity class. A comparison with the Q1-Q12 catalog shows a systematic decrease in radii of M dwarfs, while radii for K dwarfs decrease or increase depending on the Q1-Q12 provenance (KIC or Yonsei-Yale isochrones). Radii of F-G dwarfs are on average unchanged, with the exception of newly identified giants. The Q1-Q16 star properties catalog is a first step toward an improved characterization of all Kepler targets to support planet-occurrence studies.},
  file = {/Users/Oliver/Zotero/storage/6UQDAXEM/Huber et al. - 2014 - Revised Stellar Properties of Kepler Targets for t.pdf;/Users/Oliver/Zotero/storage/85RN2555/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en},
  number = {1}
}

@article{huber+2017,
  title = {Asteroseismology and {{Gaia}}: {{Testing Scaling Relations Using}} 2200 {{Kepler Stars}} with {{TGAS Parallaxes}}},
  shorttitle = {Asteroseismology and {{Gaia}}},
  author = {Huber, Daniel and Zinn, Joel and {Bojsen-Hansen}, Mathias and Pinsonneault, Marc and Sahlholdt, Christian and Serenelli, Aldo and Silva Aguirre, Victor and Stassun, Keivan and Stello, Dennis and Tayar, Jamie and Bastien, Fabienne and Bedding, Timothy R. and Buchhave, Lars A. and Chaplin, William J. and Davies, Guy R. and Garc{\'i}a, Rafael A. and Latham, David W. and Mathur, Savita and Mosser, Benoit and Sharma, Sanjib},
  year = {2017},
  month = aug,
  volume = {844},
  pages = {102},
  doi = {10.3847/1538-4357/aa75ca},
  abstract = {We present a comparison of parallaxes and radii from asteroseismology and Gaia DR1 (TGAS) for 2200 Kepler stars spanning from the main sequence to the red-giant branch. We show that previously identified offsets between TGAS parallaxes and distances derived from asteroseismology and eclipsing binaries have likely been overestimated for parallaxes {$\lessequivlnt$} 5\{--\}10 mas ({$\approx$}90\%-98\% of the TGAS sample). The observed differences in our sample can furthermore be partially compensated by adopting a hotter \{T\}\textsubscript{\{eff\vphantom\}}\vphantom\{\} scale (such as the infrared flux method) instead of spectroscopic temperatures for dwarfs and subgiants. Residual systematic differences are at the {$\approx$}2\% level in parallax across three orders of magnitude. We use TGAS parallaxes to empirically demonstrate that asteroseismic radii are accurate to {$\approx$}5\% or better for stars between {$\approx$} 0.8\{--\}8 \{R\}\textsubscript{{$\Sun$} }. We find no significant offset for main-sequence ({$\lessequivlnt$} 1.5 \{R\}\textsubscript{{$\Sun$} }) and low-luminosity RGB stars ({$\approx$}3-8 \{R\}\textsubscript{{$\Sun$} }), but seismic radii appear to be systematically underestimated by {$\approx$}5\% for subgiants ({$\approx$}1.5-3 \{R\}\textsubscript{{$\Sun$} }). We find no systematic errors as a function of metallicity between [\{Fe\}/\{\{H\}\}]{$\approx$} -0.8 to +0.4 dex, and show tentative evidence that corrections to the scaling relation for the large frequency separation (\{\{{$\increment$} \}\}{$\nu$} ) improve the agreement with TGAS for RGB stars. Finally, we demonstrate that beyond {$\approx$} 3 \{kpc\} asteroseismology will provide more precise distances than end-of-mission Gaia data, highlighting the synergy and complementary nature of Gaia and asteroseismology for studying galactic stellar populations.},
  file = {/Users/Oliver/Zotero/storage/HASXSDI7/Huber et al. - 2017 - Asteroseismology and Gaia Testing Scaling Relatio.pdf;/Users/Oliver/Zotero/storage/Q2HYJDTG/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{huber+2019,
  title = {A {{Hot Saturn Orbiting}} an {{Oscillating Late Subgiant Discovered}} by {{TESS}}},
  author = {Huber, Daniel and Chaplin, William J. and Chontos, Ashley and Kjeldsen, Hans and {Christensen-Dalsgaard}, J{\o}rgen and Bedding, Timothy R. and Ball, Warrick and Brahm, Rafael and Espinoza, Nestor and Henning, Thomas and Jord{\'a}n, Andr{\'e}s and Sarkis, Paula and Knudstrup, Emil and Albrecht, Simon and Grundahl, Frank and Andersen, Mads Fredslund and Pall{\'e}, Pere L. and Crossfield, Ian and Fulton, Benjamin and Howard, Andrew W. and Isaacson, Howard T. and Weiss, Lauren M. and Handberg, Rasmus and Lund, Mikkel N. and Serenelli, Aldo M. and Mosumgaard, Jakob R{\o}rsted and Stokholm, Amalie and Bieryla, Allyson and Buchhave, Lars A. and Latham, David W. and Quinn, Samuel N. and Gaidos, Eric and Hirano, Teruyuki and Ricker, George R. and Vanderspek, Roland K. and Seager, Sara and Jenkins, Jon M. and Winn, Joshua N. and Antia, H. M. and Appourchaux, Thierry and Basu, Sarbani and Bell, Keaton J. and Benomar, Othman and Bonanno, Alfio and Buzasi, Derek L. and Campante, Tiago L. and Orhan, Z. {\c C}elik and Corsaro, Enrico and Cunha, Margarida S. and Davies, Guy R. and Deheuvels, Sebastien and Grunblatt, Samuel K. and Hasanzadeh, Amir and Mauro, Maria Pia Di and Garc{\'i}a, Rafael A. and Gaulme, Patrick and Girardi, L{\'e}o and Guzik, Joyce A. and Hon, Marc and Jiang, Chen and Kallinger, Thomas and Kawaler, Steven D. and Kuszlewicz, James S. and Lebreton, Yveline and Li, Tanda and Lucas, Miles and Lundkvist, Mia S. and Mann, Andrew W. and Mathis, St{\'e}phane and Mathur, Savita and Mazumdar, Anwesh and Metcalfe, Travis S. and Miglio, Andrea and Monteiro, M{\'a}rio J. P. F. G. and Mosser, Benoit and Noll, Anthony and Nsamba, Benard and Ong, Jia Mian Joel and {\"O}rtel, S. and Pereira, Filipe and Ranadive, Pritesh and R{\'e}gulo, Clara and Rodrigues, Tha{\'i}se S. and Roxburgh, Ian W. and Aguirre, Victor Silva and Smalley, Barry and Schofield, Mathew and Sousa, S{\'e}rgio G. and Stassun, Keivan G. and Stello, Dennis and Tayar, Jamie and White, Timothy R. and Verma, Kuldeep and Vrard, Mathieu and Y{\i}ld{\i}z, M. and Baker, David and Bazot, Micha{\"e}l and Beichmann, Charles and Bergmann, Christoph and Bugnet, Lisa and Cale, Bryson and Carlino, Roberto and Cartwright, Scott M. and Christiansen, Jessie L. and Ciardi, David R. and Creevey, Orlagh and Dittmann, Jason A. and Jr, Jose-Dias Do Nascimento and Eylen, Vincent Van and F{\"u}r{\'e}sz, Gabor and Gagn{\'e}, Jonathan and Gao, Peter and Gazeas, Kosmas and Giddens, Frank and Hall, Oliver J. and Hekker, Saskia and Ireland, Michael J. and Latouf, Natasha and LeBrun, Danny and Levine, Alan M. and Matzko, William and Natinsky, Eva and Page, Emma and Plavchan, Peter and {Mansouri-Samani}, Masoud and McCauliff, Sean and Mullally, Susan E. and Orenstein, Brendan and Soto, Aylin Garcia and Paegert, Martin and van Saders, Jennifer L. and Schnaible, Chloe and Soderblom, David R. and Szab{\'o}, R{\'o}bert and Tanner, Angelle and Tinney, C. G. and Teske, Johanna and Thomas, Alexandra and Trampedach, Regner and Wright, Duncan and Yuan, Thomas T. and Zohrabi, Farzaneh},
  year = {2019},
  month = may,
  volume = {157},
  pages = {245},
  issn = {1538-3881},
  doi = {10.3847/1538-3881/ab1488},
  file = {/Users/Oliver/Zotero/storage/54YKC3YP/Huber et al. - 2019 - A Hot Saturn Orbiting an Oscillating Late Subgiant.pdf;/Users/Oliver/Zotero/storage/U6WPLN2X/ab1488.html},
  journal = {The Astronomical Journal},
  language = {en},
  number = {6}
}

@article{huber2015,
  title = {Asteroseismology of {{Eclipsing Binary Stars}}},
  author = {Huber, Daniel},
  year = {2015},
  volume = {408},
  pages = {169},
  doi = {10.1007/978-3-319-09198-3_7},
  abstract = {Eclipsing binaries have long served as benchmark systems to measure fundamental properties of stars. In recent decades, asteroseismology\textemdash the study of stellar pulsations\textemdash has emerged as a powerful new tool to study the structure and evolution of stars across the H-R diagram. Pulsating stars in eclipsing binary systems are particularly valuable since fundamental properties such as radii and masses can then be determined using two independent techniques. Furthermore, independently measured properties from binary orbits can be used to improve asteroseismic modelling for pulsating stars in which mode identifications are not straightforward. This chapter provides a review of asteroseismic detections in eclipsing binary stars, with a focus on space-based missions such as CoRoT and Kepler and empirical tests of asteroseismic scaling relations for stochastic (`solar-like') oscillations.},
  file = {/Users/Oliver/Zotero/storage/AHQE3SEC/Huber - 2015 - Asteroseismology of Eclipsing Binary Stars.pdf;/Users/Oliver/Zotero/storage/GJCHF4ZJ/ui.adsabs.harvard.edu.html},
  journal = {Giants of Eclipse: The \ζ Aurigae Stars and Other Binary Systems},
  language = {en}
}

@article{hubrig+2017,
  title = {A Pulsating Early-{{B}} Type Star with an Extremely Strong Magnetic Field: {{Characterizing CPD}} -62 2124},
  shorttitle = {A Pulsating Early-{{B}} Type Star with an Extremely Strong Magnetic Field},
  author = {Hubrig, S. and Kholtygin, A. F. and Ilyin, I. and Sch{\"o}ller, M. and Jarvinen, S. P.},
  year = {2017},
  month = feb,
  abstract = {A strong longitudinal magnetic field of the order of 5.2kG was recently detected in CPD-62 2124 in the framework of the BOB collaboration. Our spectropolarimetric monitoring of this star with FORS2 at the VLT revealed the presence of a huge magnetic field dominated by a dipolar component with a polar strength between 32.5 and 35.7kG. Such an extraordinary strong magnetic field strength was not previously detected in any massive early-B type star. Although being in an advanced evolutionary state, CPD-62 2124 rotates fast with v\_eq {$>$}= 176 km/s over the period P\_rot = 1.45031+-0.00002d. An analysis of the spectral variability of CPD-62 2124 on different time scales shows, apart from the rotational modulation of the line profiles, also distinct changes in shape and position of line profiles taking place on time-scales corresponding to the duration of the sub-exposure sequences. This short-term variability can probably be attributed to betaCep like pulsations. The rotational variability pattern of hydrogen and metal lines exhibits a similar behaviour while the He lines vary opposite to all other elements studied, indicating a different elemental surface distribution.},
  archivePrefix = {arXiv},
  eprint = {1702.01063},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/G9AR8ZM4/Hubrig et al. - 2017 - A pulsating early-B type star with an extremely st.pdf;/Users/Oliver/Zotero/storage/NUJ3CJWI/1702.html},
  journal = {arXiv:1702.01063 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{hunter2007,
  title = {Matplotlib: {{A 2D Graphics Environment}}},
  shorttitle = {Matplotlib},
  author = {Hunter, John D.},
  year = {2007},
  month = may,
  volume = {9},
  pages = {90--95},
  doi = {10.1109/MCSE.2007.55},
  abstract = {Matplotlib is a 2D graphics package for Python for application development, interactive scripting, and publication-quality image generation across user interfaces and operating systems.},
  journal = {Computing in Science and Engineering},
  keywords = {Application development,Python,Scientific programming,Scripting languages}
}

@article{hwang+2010,
  title = {N-{{Terminal Acetylation}} of {{Cellular Proteins Creates Specific Degradation Signals}}},
  author = {Hwang, C.-S. and Shemorry, A. and Varshavsky, A.},
  year = {2010},
  month = feb,
  volume = {327},
  pages = {973--977},
  issn = {0036-8075, 1095-9203},
  doi = {10.1126/science.1183147},
  file = {/Users/Oliver/Zotero/storage/FJB97SU2/977.full.pdf},
  journal = {Science},
  language = {en},
  number = {5968}
}

@article{jao+2016,
  title = {Distance-Dependent {{Offsets}} between {{Parallaxes}} for {{Nearby Stars}} and {{Gaia DR1 Parallaxes}}},
  author = {Jao, Wei-Chun and Henry, Todd J. and Riedel, Adric R. and Winters, Jennifer G. and Slatten, Kenneth J. and Gies, Douglas R.},
  year = {2016},
  month = nov,
  volume = {832},
  pages = {L18},
  doi = {10.3847/2041-8205/832/1/L18},
  abstract = {We use 612 single stars with previously published trigonometric parallaxes placing them within 25 pc to evaluate parallaxes released in Gaia's first data release (DR1). We find that the Gaia parallaxes are, on average, 0.24 {$\pm$} 0.02 mas smaller than the weighted mean trigonometric parallax values for these stars in the solar neighborhood. We also find that the offset changes with distance out to 100 pc, in the sense that the closer the star, the larger the offset. We find no systematic trends in the parallax offsets with stellar V magnitude, V - K color, or proper motion. We do find that the offset is roughly twice as large for stars south of the ecliptic compared to those that are north.},
  file = {/Users/Oliver/Zotero/storage/Z39JDWFT/Jao et al. - 2016 - Distance-dependent Offsets between Parallaxes for .pdf;/Users/Oliver/Zotero/storage/I3AFI5ZZ/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{jenkins+2010,
  title = {{{OVERVIEW OF THE}} {{{\emph{KEPLER}}}} {{SCIENCE PROCESSING PIPELINE}}},
  author = {Jenkins, Jon M. and Caldwell, Douglas A. and Chandrasekaran, Hema and Twicken, Joseph D. and Bryson, Stephen T. and Quintana, Elisa V. and Clarke, Bruce D. and Li, Jie and Allen, Christopher and Tenenbaum, Peter and Wu, Hayley and Klaus, Todd C. and Middour, Christopher K. and Cote, Miles T. and McCauliff, Sean and Girouard, Forrest R. and Gunter, Jay P. and Wohler, Bill and Sommers, Jeneen and Hall, Jennifer R. and Uddin, Akm K. and Wu, Michael S. and Bhavsar, Paresh A. and Van Cleve, Jeffrey and Pletcher, David L. and Dotson, Jessie A. and Haas, Michael R. and Gilliland, Ronald L. and Koch, David G. and Borucki, William J.},
  year = {2010},
  month = apr,
  volume = {713},
  pages = {L87-L91},
  issn = {2041-8205, 2041-8213},
  doi = {10.1088/2041-8205/713/2/L87},
  file = {/Users/Oliver/Zotero/storage/CWM6GPQ5/pdf.pdf},
  journal = {The Astrophysical Journal},
  keywords = {C3,Notes},
  number = {2}
}

@article{jermyn+2020,
  title = {Differential Rotation in Convective Envelopes: Constraints from Eclipsing Binaries},
  shorttitle = {Differential Rotation in Convective Envelopes},
  author = {Jermyn, Adam S. and Tayar, Jamie and Fuller, Jim},
  year = {2020},
  month = jan,
  volume = {491},
  pages = {690--707},
  issn = {0035-8711},
  doi = {10.1093/mnras/stz2983},
  abstract = {Over time, tides synchronize the rotation periods of stars in a binary
system to the orbital period. However, if the star exhibits differential
rotation, then only a portion of it can rotate at the orbital period, so
the rotation period at the surface may not match the orbital period. The
difference between the rotation and orbital periods can therefore be
used to infer the extent of the differential rotation. We use a simple
parametrization of differential rotation in stars with convective
envelopes in circular orbits to predict the difference between the
surface rotation period and the orbital period. Comparing this
parametrization to observed eclipsing binary systems, we find that in
the surface convection zones of stars in short-period binaries there is
very little radial differential rotation, with |r{$\partial$}rln
{$\Omega$}| {$<$} 0.02. This holds even for longer orbital periods, though
it is harder to say which systems are synchronized at long periods, and
larger differential rotation is degenerate with asynchronous rotation.},
  file = {/Users/Oliver/Zotero/storage/UUBXPU4I/Jermyn et al. - 2020 - Differential rotation in convective envelopes con.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {binaries: eclipsing,convection,stars: rotation}
}

@article{jimenez+2011,
  title = {The Acoustic Cut-off Frequency of the {{Sun}} and the Solar Magnetic Activity Cycle},
  author = {Jimenez, A. and Garcia, R. A. and Palle, P. L.},
  year = {2011},
  month = dec,
  volume = {743},
  pages = {99},
  issn = {0004-637X, 1538-4357},
  doi = {10.1088/0004-637X/743/2/99},
  abstract = {The acoustic cut-off frequency -the highest frequency for acoustic solar eigenmodes- is an important parameter of the solar atmosphere as it determines the upper boundary of the p-mode resonant cavities. At frequencies beyond this value, acoustic disturbances are no longer trapped but traveling waves. Interference amongst them give rise to higher-frequency peaks -the pseudomodes- in the solar acoustic spectrum. The pseudomodes are shifted slightly in frequency with respect to p modes making possible the use of pseudomodes to determine the acoustic cut-off frequency. Using data from GOLF and VIRGO instruments on board the SOHO spacecraft, we calculate the acoustic cut-off frequency using the coherence function between both the velocity and intensity sets of data. By using data gathered by these instruments during the entire lifetime of the mission (1996 till the present), a variation in the acoustic cut-off frequency with the solar magnetic activity cycle is found.},
  archivePrefix = {arXiv},
  eprint = {1109.3326},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/VZTBNAPZ/Jimenez et al. - 2011 - The acoustic cut-off frequency of the Sun and the .pdf;/Users/Oliver/Zotero/storage/J4W62V82/1109.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {2}
}

@article{jofre+2015,
  title = {Stellar Parameters and Chemical Abundances of 223 Evolved Stars with and without Planets},
  author = {Jofr{\'e}, E. and Petrucci, R. and Saffe, C. and Saker, L. and {de la Villarmois}, E. Artur and Chavero, C. and G{\'o}mez, M. and Mauas, P. J. D.},
  year = {2015},
  month = feb,
  volume = {574},
  pages = {A50},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201424474},
  abstract = {Aims: We present fundamental stellar parameters, chemical
abundances, and rotational velocities for a sample of 86 evolved stars
with planets (56 giants; 30 subgiants), and for a control sample of 137
stars (101 giants; 36 subgiants) without planets. The analysis was based
on both high signal-to-noise and resolution echelle spectra. The main
goals of this work are i) to investigate chemical differences between
evolved stars that host planets and those of the control sample without
planets; ii) to explore potential differences between the properties of
the planets around giants and subgiants; and iii) to search for possible
correlations between these properties and the chemical abundances of
their host stars. Implications for the scenarios of planet formation and
evolution are also discussed. Methods: The fundamental stellar
parameters (Teff, log g, [Fe/H], {$\xi$}t) were
computed homogeneously using the FUNDPAR code. The chemical abundances
of 14 elements (Na, Mg, Al, Si, Ca, Sc, Ti, V, Cr, Mn, Co, Ni, Zn, and
Ba) were obtained using the MOOG code. Rotational velocities were
derived from the full width at half maximum of iron isolated lines. Results: In agreement with previous studies, we find that subgiants
with planets are, on average, more metal-rich than subgiants without
planets by \textasciitilde 0.16 dex. The [Fe/H] distribution of giants with planets is
centered at slightly subsolar metallicities and there is no metallicity
enhancement relative to the [Fe/H] distribution of giants without
planets. Furthermore, contrary to recent results, we do not find any
clear difference between the metallicity distributions of stars with and
without planets for giants with M{$\star>$} 1.5
M{$\odot$}. With regard to the other chemical elements, the
analysis of the [X/Fe] distributions shows differences between giants
with and without planets for some elements, particularly V, Co, and Ba.
Subgiants with and without planets exhibit similar behavior for most of
the elements. On the other hand, we find no evidence of rapid rotation
among the giants with planets or among the giants without planets.
Finally, analyzing the planet properties, some interesting trends might
be emerging: i) multi-planet systems around evolved stars show a slight
metallicity enhancement compared with single-planet systems; ii) planets
with a {$\lessequivlnt$} 0.5 AU orbit subgiants with [Fe/H] {$>$} 0 and giants
hosting planets with a {$\lessequivlnt$} 1 AU have [Fe/H] {$<$} 0; iii) higher-mass
planets tend to orbit more metal-poor giants with M{$\star$}
{$\leq$} 1.5 M{$\odot$}, whereas planets around subgiants seem to
follow the planet-mass metallicity trend observed on dwarf hosts; iv)
[X/Fe] ratios for Na, Si, and Al seem to increase with the mass of
planets around giants; v) planets orbiting giants show lower orbital
eccentricities than those orbiting subgiants and dwarfs, suggesting a
more efficient tidal circularization or the result of the engulfment of
close-in planets with larger eccentricities.

Based on spectral data retrieved from the ELODIE and SOPHIE archives at
Observatoire de Haute-Provence (Moultaka et al. 2004).Based on data
obtained from the ESO Science Archive Facility collected at the La Silla
Paranal Observatory, ESO (Chile) with the HARPS and FEROS spectrographs.},
  file = {/Users/Oliver/Zotero/storage/4YU583TQ/Jofré et al. - 2015 - Stellar parameters and chemical abundances of 223 .pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {planetary systems,stars: abundances,stars: fundamental parameters,techniques: spectroscopic}
}

@inproceedings{johnson+2017,
  title = {Overview of {{Galactic Archaelogy}} with {{Kepler}} and {{K2}}},
  booktitle = {American {{Astronomical Society Meeting Abstracts}}},
  author = {Johnson, Jennifer and {APOKASC Team} and {APO-K2 Team}},
  year = {2017},
  month = jan,
  volume = {229},
  pages = {305.01},
  abstract = {The exquisite lightcurves of the Kepler and K2 missions have been an unexpected boon to the field of near-field cosmology. Ages and
evolutionary states can now be derived for field red giants, by
combining seismic and granulation signatures with spectroscopic data. Red giants, far more luminous than the main-sequence turnoff stars usually used, allow us to probe the evolution of the whole Galaxy. Originally these investigations were restricted to a single line of sight in the direction of Cygnus. With the failure of the reaction wheels and the start of the K2 program, we now probe distinctly
different Galactic populations, including the inner and outer disks, the bulge-halo interface, and far more ofthe Galactic halo. I will present an overview of some of the Galactic archaeology efforts underway with Kepler and K2 data, focusing on our calibration of absolute ages. I will also present results on Galactic chemical evolution and the timescales for the formation of the elements.}
}

@article{johnson+apokasccollaboration2016,
  title = {Galactic Stellar Populations with {{APOGEE}} and {{Kepler}}},
  author = {Johnson, J. A. and {APOKASC Collaboration}},
  year = {2016},
  month = sep,
  volume = {337},
  pages = {917},
  issn = {0004-6337},
  doi = {10.1002/asna.201612410},
  abstract = {Understanding the history of baryons is key to understanding galaxy formation, as galaxies with very similar stellar mass and/or dark matter halo mass can have markedly different morphologies in their stellar light. Stars are a useful way to study this history, because properties such as their composition, age, and orbital motion can map galaxy formation and evolution. Lightcurves from the Kepler mission, both original and extended, provide asteroseismic parameters, such as {$\Delta$} {$\nu$} and {$\nu\_$}max, and rotation periods. The high-resolution near-infrared APOGEE spectroscopic survey is observing an extensive sample of red giants and cool dwarfs in both the Kepler and K2 fields to provide composition and effective temperature measurements. These spectroscopic and seismic parameters can be combined to yield ages, important for dissecting the history of the Milky Way. Results based on this
combination have already been published in the first APOKASC catalog. Among the interesting results about stellar populations so far are the presence of a large metallicity spread in the young secondary red clump population at the solar circle, the identification of young, yet {$\alpha$}-rich stars, and the detection of a field blue straggler
descendant. The K2 fields along the ecliptic will extend the
possibilities of these techniques to new lines of sight in the Galaxy and provide a much more representative sample of Galactic populations with seismic and spectroscopic information.},
  journal = {Astronomische Nachrichten},
  keywords = {Galaxy: abundances,Galaxy: evolution,Galaxy: stellar content,stars: oscillations,stars: rotation}
}

@article{judge+2017,
  title = {The Magnetic Future of the {{Sun}}},
  author = {Judge, Philip and Egeland, RIcky and Metcalfe, Travis and Guinan, Edward and Engel, Scott},
  year = {2017},
  month = oct,
  abstract = {We analyze space- and ground-based data for the old (\$7.0\textbackslash pm0.3\$\textasciitilde Gyr) solar analogs 16 Cyg A and B. The stars were observed with the Cosmic Origins UV Spectrographs on the Hubble Space Telescope (HST) on 23 October 2015 and 3 February 2016 respectively, and with the Chandra X-ray Observatory on 7 February 2016. Time-series data in \textbackslash ion\{Ca\}\{2\} data are used to place the UV data in context. The UV spectra of 18 Sco (3.7\$\textbackslash pm0.5\$ Gyr), the Sun (4.6\$\textbackslash pm0.04\$ Gyr) and \$

license: MIT

license_type: permissive

branch_name: refs/heads/master

extension: bib