text:
@ARTICLE{halbwachs1986,
	author = {{Halbwachs}, J.~L.},
	title = "{Common proper motion stars in the AGK 3.}",
	journal = {\aaps},
	keywords = {Astronomical Catalogs, Binary Stars, Stellar Motions, Distribution Functions, Astronomy, Binaries:Proper-Motion Stars, Proper-Motion Stars:Binaries, Proper-Motion Stars:Surveys},
	year = 1986,
	month = nov,
	volume = {66},
	pages = {131-148},
	adsurl = {https://ui.adsabs.harvard.edu/abs/1986A&AS...66..131H},
	adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{reinhold+2020,
	author = {{Reinhold}, Timo and {Shapiro}, Alexander I. and {Solanki}, Sami K. and
	{Montet}, Benjamin T. and {Krivova}, Natalie A. and
	{Cameron}, Robert H. and {Amazo-G{\'o}mez}, Eliana M.},
	title = "{The Sun is less active than other solar-like stars}",
	journal = {Science},
	keywords = {ASTRONOMY, Astrophysics - Solar and Stellar Astrophysics},
	year = 2020,
	month = may,
	volume = {368},
	number = {6490},
	pages = {518-521},
	doi = {10.1126/science.aay3821},
	archivePrefix = {arXiv},
	eprint = {2005.01401},
	primaryClass = {astro-ph.SR},
	adsurl = {https://ui.adsabs.harvard.edu/abs/2020Sci...368..518R},
	adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@INPROCEEDINGS{kollmeier+2019,
	author = {{Kollmeier}, Juna and {Anderson}, S.~F. and {Blanc}, G.~A. and
	{Blanton}, M.~R. and {Covey}, K.~R. and {Crane}, J. and {Drory}, N. and
	{Frinchaboy}, P.~M. and {Froning}, C.~S. and {Johnson}, J.~A. and
	{Kneib}, J. -P. and {Kreckel}, K. and {Merloni}, A. and
	{Pellegrini}, E.~W. and {Pogge}, R.~W. and {Ramirez}, S.~V. and
	{Rix}, H.~W. and {Sayres}, C. and {S{\'a}nchez-Gallego}, Jos{\'e} and
	{Shen}, Yue and {Tkachenko}, A. and {Trump}, J.~R. and {Tuttle}, S.~E. and
	{Weijmans}, A. and {Zasowski}, G. and {Barbuy}, B. and {Beaton}, R.~L. and
	{Bergemann}, M. and {Bochanski}, J.~J. and {Brandt}, W.~N. and
	{Casey}, A.~R. and {Cherinka}, B.~A. and {Eracleous}, M. and {Fan}, X. and
	{Garc{\'\i}a}, R.~A. and {Green}, P.~J. and {Hekker}, S. and
	{Lane}, R.~R. and {Longa-Pe{\~n}a}, P. and {Mathur}, S. and {Meza}, A. and
	{Minchev}, I. and {Myers}, A.~D. and {Nidever}, D.~L. and
	{Nitschelm}, C. and {O'Connell}, J.~E. and {Price-Whelan}, A.~M. and
	{Raddick}, M.~J. and {Rossi}, G. and {Sankrit}, R. and {Simon}, J.~D. and
	{Stutz}, A.~M. and {Ting}, Y. -S. and {Trakhtenbrot}, B. and
	{Weaver}, B.~A. and {Willmer}, C.~N.~A. and {Weinberg}, D.~H.},
	title = "{SDSS-V Pioneering Panoptic Spectroscopy}",
	booktitle = {Bulletin of the American Astronomical Society},
	year = 2019,
	volume = {51},
	month = sep,
	eid = {274},
	pages = {274},
	adsurl = {https://ui.adsabs.harvard.edu/abs/2019BAAS...51g.274K},
	adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@INPROCEEDINGS{blanton+2019,
	author = {{Blanton}, Michael and {Anderson}, S.~F. and {Basu}, S. and
	{Beaton}, R.~L. and {Bergemann}, M. and {Bershady}, M.~A. and
	{Bochanski}, J.~J. and {Brandt}, W.~N. and {Brownstein}, J. and
	{Bundy}, K. and {Casey}, A.~R. and {Cherinka}, B.~A. and
	{Covey}, K.~R. and {Eracleous}, M. and {Fan}, X. and {Feuillet}, D.~K. and
	{Frinchaboy}, P.~M. and {Garc{\'\i}a}, R.~A. and {Green}, P.~J. and
	{Johnson}, J.~A. and {Jones}, A. and {Knapp}, G. and {Kneib}, J. -P. and
	{Kollmeier}, J.~A. and {Kreckel}, K. and {Lane}, R.~R. and
	{Longa-Pe{\~n}a}, P. and {Masters}, K. and {Mathur}, S. and
	{Merloni}, A. and {Meza}, A. and {Minchev}, I. and {Nitschelm}, C. and
	{O'Connell}, J.~E. and {Raddick}, M.~J. and {Ramirez}, S.~V. and
	{Rix}, H. -W. and {Rossi}, G. and {Sankrit}, R. and {Shen}, Y. and
	{Simon}, J.~D. and {Stutz}, A.~M. and {Ting}, Y. -S. and
	{Trump}, J.~R. and {Tuttle}, S.~E. and {Weijmans}, A. and
	{Weaver}, B.~A. and {Weinberg}, D.~H. and {Willmer}, C.~N.~A. and
	{Wood-Vasey}, W.~M. and {Zasowski}, G.},
	title = "{The Sloan Digital Sky Survey as an Archetypal Mid-Scale Program}",
	booktitle = {Bulletin of the American Astronomical Society},
	year = 2019,
	volume = {51},
	month = sep,
	eid = {196},
	pages = {196},
	adsurl = {https://ui.adsabs.harvard.edu/abs/2019BAAS...51g.196B},
	adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@ARTICLE{mathur+2019,
	author = {{Mathur}, Savita and {Garc{\'\i}a}, Rafael A. and {Bugnet}, Lisa and
	{Santos}, {\^A}ngela R.~G. and {Santiago}, Netsha and {Beck}, Paul G.},
	title = "{Revisiting the impact of stellar magnetic activity on the detection of solar-like oscillations by Kepler}",
	journal = {Frontiers in Astronomy and Space Sciences},
	keywords = {Asteroseismology-stars, Rotation - Stars, magnetic activity, solar-like oscillations, Solar-like stars: fundamental parameters, spectroscopy, Astrophysics - Solar and Stellar Astrophysics},
	year = 2019,
	month = jul,
	volume = {6},
	eid = {46},
	pages = {46},
	doi = {10.3389/fspas.2019.00046},
	archivePrefix = {arXiv},
	eprint = {1907.01415},
	primaryClass = {astro-ph.SR},
	adsurl = {https://ui.adsabs.harvard.edu/abs/2019FrASS...6...46M},
	adsnote = {Provided by the SAO/NASA Astrophysics Data System}
}

@article{adibekyan+2017,
  title = {Sun-like Stars Unlike the {{Sun}}: {{Clues}} for Chemical Anomalies of Cool Stars},
  shorttitle = {Sun-like Stars Unlike the {{Sun}}},
  author = {Adibekyan, V. and {Delgado-Mena}, E. and Feltzing, S. and Hern{\'a}ndez, J. I. Gonz{\'a}lez and Hinkel, N. R. and Korn, A. J. and Asplund, M. and Beck, P. G. and Deal, M. and Gustafsson, B. and Honda, S. and Lind, K. and Nissen, P. E. and Spina, L.},
  year = {2017},
  month = jan,
  abstract = {We present a summary of the splinter session "Sun-like stars unlike the Sun" that was held on 09 June 2016 as part of the Cool Stars 19 conference (Uppsala, Sweden). We discussed the main limitations (in the theory and observations) in the derivation of very precise stellar parameters and chemical abundances of Sun-like stars. We outlined and discussed the most important and most debated processes that can produce chemical peculiarities in solar-type stars. Finally, in an open discussion between all the participants we tried to identify new pathways and prospects towards future solutions of the currently open questions.},
  archivePrefix = {arXiv},
  eprint = {1701.05737},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/8E9VD3WG/1701.html},
  journal = {arXiv:1701.05737 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{adibekyan+2017a,
  title = {How Alien Can Alien Worlds Be?},
  author = {Adibekyan, V. and Figueira, P. and Santos, N. C.},
  year = {2017},
  month = oct,
  doi = {10.5281/zenodo.1030004},
  abstract = {In an attempt to select stars that can host planets with characteristics similar to our own, we selected seven solar-type stars known to host planets in the habitable zone and for which spectroscopic stellar parameters are available. For these stars we estimated 'empirical' abundances of O, C, Mg and Si, which in turn we used to derive the iron and water mass fraction of the planet building blocks with the use of the model presented in Santos et al. (2015). Our results show that if rocky planets orbit these stars they might have significantly different compositions between themselves and different from that of our Earth. However, for a meaningful comparison between the compositional properties of exoplanets in the habitable zone and our own planet, a far more sophisticated analysis (e.g. Dorn et al., 2017) of a large number of systems with precise mass and radius of planets, and accurate chemical abundances of the host stars. The work presented here is merely the first humble step in this direction.},
  archivePrefix = {arXiv},
  eprint = {1710.07482},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/HBXRXUDH/1710.html},
  journal = {arXiv:1710.07482 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{aerts+2010,
  title = {Asteroseismology},
  author = {Aerts, Conny and {Christensen-Dalsgaard}, J{\o}rgen and Kurtz, Donald W.},
  year = {2010},
  abstract = {The recent research domain of asteroseismology studies the internal structure
of stars, which is not directly observable, through the interpretation of the
frequency spectra of stellar oscillations. The basic principles of
asteroseismology are very similar to those developed by earth seismologists.
Stellar interiors can be probed from oscillations because different
oscillation modes penetrate to different depths inside the star.
Asteroseismology is the only available method to derive the internal structure
of the stars with high precision.

This book - the first on asteroseismology - offers a practical guide for
graduate students and scientists working in stellar astrophysics. It provides
a general introduction to asteroseismology and comprehensive coverage of all
its aspects: fundamental theory, observations and observational techniques,
methodology of data analysis and seismic interpretations of various classes
of multi-periodic pulsating stars.},
  journal = {Asteroseismology, Astronomy and Astrophysics Library. ISBN 978-1-4020-5178-4. Springer Science+Business Media B.V., 2010, p.},
  keywords = {Astronomy,Astrophysics and Cosmology,Physics}
}

@article{aerts+2017,
  title = {Kepler Sheds New and Unprecedented Light on the Variability of a Blue Supergiant: Gravity Waves in the {{O9}}.{{5Iab}} Star {{HD}} 188209},
  shorttitle = {Kepler Sheds New and Unprecedented Light on the Variability of a Blue Supergiant},
  author = {Aerts, C. and {Simon-Diaz}, S. and Bloemen, S. and Debosscher, J. and Papics, P. I. and Bryson, S. and Still, M. and Moravveji, E. and Williamson, M. H. and Grundahl, F. and Andersen, M. Fredslund and Antoci, V. and Palle, P. L. and {Christensen-Dalsgaard}, J. and Rogers, T. M.},
  year = {2017},
  month = mar,
  abstract = {Stellar evolution models are most uncertain for evolved massive stars. Asteroseismology based on high-precision uninterrupted space photometry has become a new way to test the outcome of stellar evolution theory and was recently applied to a multitude of stars, but not yet to massive evolved supergiants.Our aim is to detect, analyse and interpret the photospheric and wind variability of the O9.5Iab star HD 188209 from Kepler space photometry and long-term high-resolution spectroscopy. We used Kepler scattered-light photometry obtained by the nominal mission during 1460d to deduce the photometric variability of this O-type supergiant. In addition, we assembled and analysed high-resolution high signal-to-noise spectroscopy taken with four spectrographs during some 1800d to interpret the temporal spectroscopic variability of the star. The variability of this blue supergiant derived from the scattered-light space photometry is in full in agreement with the one found in the ground-based spectroscopy. We find significant low-frequency variability that is consistently detected in all spectral lines of HD 188209. The photospheric variability propagates into the wind, where it has similar frequencies but slightly higher amplitudes. The morphology of the frequency spectra derived from the long-term photometry and spectroscopy points towards a spectrum of travelling waves with frequency values in the range expected for an evolved O-type star. Convectively-driven internal gravity waves excited in the stellar interior offer the most plausible explanation of the detected variability.},
  archivePrefix = {arXiv},
  eprint = {1703.01514},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/68PTFWWQ/1703.html},
  journal = {arXiv:1703.01514 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{agol+fabrycky2017,
  title = {Transit {{Timing}} and {{Duration Variations}} for the {{Discovery}} and {{Characterization}} of {{Exoplanets}}},
  author = {Agol, Eric and Fabrycky, Dan},
  year = {2017},
  month = jun,
  abstract = {Transiting exoplanets in multi-planet systems have non-Keplerian orbits which can cause the times and durations of transits to vary. The theory and observations of transit timing variations (TTV) and transit duration variations (TDV) are reviewed. A watershed since the last review is that the Kepler spacecraft has detected several hundred perturbed planets. In a few cases, these data have been used to discover additional planets, which has historical resonance with how Neptune was discovered in our own Solar System. However, the more impactful aspect of TTV and TDV studies has been characterization of planetary systems in which multiple planets transit. After addressing the equations of motion and parameter scalings, the main dynamical mechanisms for TTV and TDV are described, with citations to the observational literature for real examples. We describe parameter constraints, particularly how the mass/eccentricity degeneracy comes about and is overcome by the high-frequency component of the signal. On the observational side, derivation of timing precision and introduction to the timing diagram are given. Science results are reviewed, with an emphasis on mass measurements of transiting sub-Neptunes and super-Earths, which allows access to the mass-radius diagram and hence inference of bulk compositions.},
  archivePrefix = {arXiv},
  eprint = {1706.09849},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/3R76WBMR/1706.html},
  journal = {arXiv:1706.09849 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Instrumentation and Methods for Astrophysics,REVIEW},
  primaryClass = {astro-ph}
}

@article{aigrain+2015,
  title = {Precise Time-Series Photometry for the {{Kepler}}-2.0 Mission},
  author = {Aigrain, Suzanne and Hodgkin, Simon T. and Irwin, Michael J. and Lewis, Jim R. and Roberts, Stephen J.},
  year = {2015},
  month = jan,
  volume = {447},
  pages = {2880--2893},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stu2638},
  abstract = {The recently approved NASA K2 mission has the potential to multiply by an order of magnitude the number of short-period transiting planets found by Kepler around bright and low-mass stars, and to revolutionise our understanding of stellar variability in open clusters. However, the data processing is made more challenging by the reduced pointing accuracy of the satellite, which has only two functioning reaction wheels. We present a new method to extract precise light curves from K2 data, combining list-driven, soft-edged aperture photometry with a star-by-star correction of systematic effects associated with the drift in the roll-angle of the satellite about its boresight. The systematics are modelled simultaneously with the stars' intrinsic variability using a semi-parametric Gaussian process model. We test this method on a week of data collected during an engineering test in January 2014, perform checks to verify that our method does not alter intrinsic variability signals, and compute the precision as a function of magnitude on long-cadence (30-min) and planetary transit (2.5-hour) timescales. In both cases, we reach photometric precisions close to the precision reached during the nominal Kepler mission for stars fainter than 12th magnitude, and between 40 and 80 parts per million for brighter stars. These results confirm the bright prospects for planet detection and characterisation, asteroseismology and stellar variability studies with K2. Finally, we perform a basic transit search on the light curves, detecting 2 bona fide transit-like events, 7 detached eclipsing binaries and 13 classical variables.},
  archivePrefix = {arXiv},
  eprint = {1412.6304},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/AN3VFD2N/1412.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {C3,Notes},
  number = {3}
}

@article{allendeprieto2016,
  title = {Learning about Stars from Their Colors},
  author = {Allende Prieto, C.},
  year = {2016},
  month = sep,
  volume = {1609},
  pages = {arXiv:1609.08557},
  abstract = {We pose the question of how much information on the atmospheric parameters of late-type stars can be retrieved purely from colors using standard photometric systems. We carried out numerical experiments using stellar fluxes from model atmospheres, injecting random noise before analyzing them. We examined the presence of degeneracies among
atmospheric parameters, and evaluated how well the parameters are extracted depending on the number and wavelength span of the photometric filters available, from the UV GALEX to the mid-IR WISE passbands. We also considered spectrophotometry from the Gaia mission. We find that stellar effective temperatures can be determined accurately (\$\textbackslash sigma \textbackslash sim\$ 0.01 dex or about 150 K) when reddening is negligible or known, based merely on optical photometry, and the accuracy can be improved twofold by including IR data. On the other hand, stellar metallicities and surface gravities are fairly unconstrained from optical or IR photometryy. However, our ability to retrieve these parameters can improve significantly by adding UV photometry. When reddening is considered a free parameter, assuming it can be modeled perfectly, our experiments suggest that it can be disentangled from the rest of the parameters. This theoretical study indicates that combining broad-band photometry from the UV to the mid-IR allows atmospheric parameters and interstellar extinction to be determined with fair accuracy. The use of UV passbands helps substantially to derive metallicities and surface gravities, as well as to break the degeneracy between effective
temperature and reddening. The Gaia BP/RP data can disentangle all the parameters, provided the stellar SEDs are modeled reasonably well.},
  journal = {ArXiv e-prints},
  keywords = {Astrophysics - Solar and Stellar Astrophysics}
}

@article{alves2000,
  title = {K-{{Band Calibration}} of the {{Red Clump Luminosity}}},
  author = {Alves, David R.},
  year = {2000},
  month = aug,
  volume = {539},
  pages = {732},
  doi = {10.1086/309278},
  abstract = {The average near-infrared (K-band) luminosity of 238 Hipparcos red clump giants is derived and then used to measure the distance to the Galactic center. These Hipparcos red clump giants have been previously employed as I-band standard candles. The advantage of the K-band is a decreased sensitivity to reddening and perhaps a reduced systematic dependence on metallicity. In order to investigate the latter, and also to refer our calibration to a known metallicity zero point, we restrict our sample of red clump calibrators to those with abundances derived from high-resolution spectroscopic data. The mean metallicity of the sample is [Fe/H]=-0.18 dex ({$\sigma$}=0.17 dex). The data are consistent with no correlation between M\textsubscript{K} and [Fe/H] and only weakly constrain the slope of this relation. The luminosity function of the sample peaks at M\textsubscript{K}=-1.61+/-0.03 mag. Next, we assemble published optical and near-infrared photometry for \textasciitilde 20 red clump giants in a Baade's window field with a mean metallicity of [Fe/H]=-0.17+/-0.09 dex, which is nearly identical to that of the Hipparcos red clump. Assuming that the average (V-I)\textsubscript{0} and (V-K)\textsubscript{0} colors of these two red clumps are the same, the extinctions in the Baade's window field are found to be A\textsubscript{V}=1.56, A\textsubscript{I}=0.87, and A\textsubscript{K}=0.15, in agreement with previous estimates. We derive the distance to the Galactic center: (m-M)\textsubscript{0}=14.58+/-0.11 mag, or R=8.24+/-0.42 kpc. The uncertainty in this distance measurement is dominated by the small number of Baade's window red clump giants examined here.},
  file = {/Users/Oliver/Zotero/storage/BN96QLPH/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{amard+matt2020,
  title = {The {{Impact}} of {{Metallicity}} on the {{Evolution}} of {{Rotation}} and {{Magnetic Activity}} of {{Sun}}-{{Like Stars}}},
  author = {Amard, L. and Matt, S. P.},
  year = {2020},
  month = jan,
  abstract = {The rotation rates and magnetic activity of Sun-like and low-mass ( 1.4M ) main-sequence stars are known to decline with time, and there now exist several models for the evolution of rotation and activity. However, the role that chemical composition plays during stellar spin-down has not yet been explored. In this work, we use a structural evolution code to compute the rotational evolution of stars with three different masses (0.7, 1.0, and 1.3 M ) and six different metallicities, ranging from [Fe/H] = -1.0 to [Fe/H] = +0.5. We also implement three different wind-braking formulations from the literature (two modern and one classical) and compare their predictions for rotational evolution. The effect that metallicity has on stellar structural properties, and in particular the convective turnover timescale, leads the two modern wind-braking formulations to predict a strong dependence of the torque on metallicity. Consequently, they predict that metal rich stars spin-down more effectively at late ages ( 1 Gyr) than metal poor stars, and the effect is large enough to be detectable with current observing facilities. For example, the formulations predict that a Sun-like (solar-mass and solar-aged) star with [Fe/H] = -0.3 will have a rotation period of less than 20 days. Even though old, metal poor stars are predicted to rotate more rapidly at a given age, they have larger Rossby numbers and are thus expected to have lower magnetic activity levels. Finally, the different wind-braking formulations predict quantitative differences in the metallicity-dependence of stellar rotation, which may be used to test them.},
  archivePrefix = {arXiv},
  eprint = {2001.10404},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/6DN4UAFL/Amard and Matt - 2020 - The Impact of Metallicity on the Evolution of Rota.pdf},
  journal = {arXiv:2001.10404 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  language = {en},
  primaryClass = {astro-ph}
}

@article{amazo-gomez+2020,
  title = {Rotation Periods from the Inflection Point in the Power Spectrum of Stellar Brightness Variations: {{II}}. {{The Sun}}},
  shorttitle = {Rotation Periods from the Inflection Point in the Power Spectrum of Stellar Brightness Variations},
  author = {{Amazo-G{\'o}mez}, E. M. and Shapiro, A. I. and Solanki, S. K. and Krivova, N. A. and Kopp, G. and Reinhold, T. and Oshagh, M. and Reiners, A.},
  year = {2020},
  month = feb,
  abstract = {Young and active stars generally have regular, almost sinusoidal, patterns of variability attributed to their rotation, while the majority of older and less active stars, including the Sun, have more complex and non-regular light-curves which do not have clear rotational-modulation signals. Consequently, the rotation periods have been successfully determined only for a small fraction of the Sun-like stars observed by transit-based planet-hunting missions, such as CoRoT, Kepler, and TESS. This suggests that only a small fraction of such systems have been properly identified as solar-like analogs. We apply a new method for determining rotation periods of low-activity stars, like the Sun. The method is based on calculating the gradient of the power spectrum (GPS) of stellar brightness variations and identifying a tell-tale inflection point in the spectrum. The rotation frequency is then proportional to the frequency of that inflection point. In this paper test this GPS method against available photometric records of the Sun. We apply GPS, autocorrelation functions, Lomb-Scargle periodograms, and wavelet analyses to the total solar irradiance (TSI) time series obtained from the Total Irradiance Monitor (TIM) on the Solar Radiation and Climate Experiment (SORCE) and the Variability of solar IRradiance and Gravity Oscillations (VIRGO) experiment on the SOlar and Heliospheric Observatory (SoHO) missions. We analyse the performance of all methods at various levels of solar activity. We show that the GPS method returns accurate values of solar rotation independently of the level of solar activity. In particular, it performs well during periods of high solar activity, when TSI variability displays an irregular pattern and other methods fail. Our results suggest that the GPS method can successfully determine the rotational periods of stars with both regular and non-regular light-curves.},
  archivePrefix = {arXiv},
  eprint = {2002.03455},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/88TBVGBX/Amazo-Gómez et al. - 2020 - Rotation periods from the inflection point in the .pdf;/Users/Oliver/Zotero/storage/BY4IXYEA/2002.html},
  journal = {arXiv:2002.03455 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{anders+2017,
  title = {Galactic Archaeology with Asteroseismology and Spectroscopy: {{Red}} Giants Observed by {{CoRoT}} and {{APOGEE}}},
  shorttitle = {Galactic Archaeology with Asteroseismology and Spectroscopy},
  author = {Anders, F. and Chiappini, C. and Rodrigues, T. S. and Miglio, A. and Montalb{\'a}n, J. and Mosser, B. and Girardi, L. and Valentini, M. and Noels, A. and Morel, T. and Johnson, J. A. and Schultheis, M. and Baudin, F. and {de Assis Peralta}, R. and Hekker, S. and Theme{\ss}l, N. and Kallinger, T. and Garc{\'i}a, R. A. and Mathur, S. and Baglin, A. and Santiago, B. X. and Martig, M. and Minchev, I. and Steinmetz, M. and Costa, Da and N, L. and Maia, M. a. G. and Allende Prieto, C. and Cunha, K. and Beers, T. C. and Epstein, C. and P{\'e}rez, Garc{\'i}a and E, A. and {Garc{\'i}a-Hern{\'a}ndez}, D. A. and Harding, P. and Holtzman, J. and Majewski, S. R. and M{\'e}sz{\'a}ros, Sz and Nidever, D. and Pan, K. and Pinsonneault, M. and Schiavon, R. P. and Schneider, D. P. and Shetrone, M. D. and Stassun, K. and Zamora, O. and Zasowski, G.},
  year = {2017},
  month = jan,
  volume = {597},
  pages = {A30},
  doi = {10.1051/0004-6361/201527204},
  abstract = {With the advent of the space missions CoRoT and Kepler, it has recently become feasible to determine precise asteroseismic masses and relative ages for large samples of red giant stars. We present the CoRoGEE dataset, obtained from CoRoT light curves for 606 red giants in two fields of the Galactic disc that have been co-observed by the Apache Point Observatory Galactic Evolution Experiment (APOGEE). We used the Bayesian parameter estimation code PARAM to calculate distances, extinctions, masses, and ages for these stars in a homogeneous analysis, resulting in relative statistical uncertainties of {$\lessequivlnt$}2\% in distance, 4\% in radius, 9\% in mass and 25\% in age. We also assessed systematic age uncertainties stemming from different input physics and mass loss. We discuss the correlation between ages and chemical abundance patterns of field stars over a broad radial range of the Milky Way disc (5 kpc \<R\textsubscript{Gal}\< 14 kpc), focussing on the [{$\alpha$}/Fe]-[Fe/H]-age plane in five radial bins of the Galactic disc. We find an overall agreement with the expectations of pure chemical-evolution models computed before the present data were available, especially for the outer regions. However, our data also indicate that a significant fraction of stars now observed near and beyond the solar neighbourhood migrated from inner regions. Mock CoRoGEE observations of a chemodynamical Milky Way disc model indicate that the number of high-metallicity stars in the outer disc is too high to be accounted for even by the strong radial mixing present in the model. The mock observations also show that the age distribution of the [{$\alpha$}/Fe]-enhanced sequence in the CoRoGEE inner-disc field is much broader than expected from a combination of radial mixing and observational errors. We suggest that a thick-disc/bulge component that formed stars for more than 3 Gyr may account for these discrepancies. Our results are subject to future improvements due to (a) the still low statistics, because our sample had to be sliced into bins of Galactocentric distances and ages; (b) large uncertainties in proper motions (and therefore guiding radii); and (c) corrections to the asteroseismic mass-scaling relation. The situation will improve not only upon the upcoming Gaia data releases, but also with the foreseen increase in the number of stars with both seismic and spectroscopic information. The data described in Table B.1 are only available at the CDS via anonymous ftp to \href{http://cdsarc.u-strasbg.fr}{http://cdsarc.u-strasbg.fr} (\href{http://130.79.128.5}{http://130.79.128.5}) or via \href{http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/597/A30}{http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/597/A30}},
  file = {/Users/Oliver/Zotero/storage/RPMPJN53/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{anderson+1990,
  title = {Modeling of {{Solar Oscillation Power Spectra}}},
  author = {Anderson, Edwin R. and Duvall, Thomas L. and Jefferies, Stuart M.},
  year = {1990},
  month = dec,
  volume = {364},
  pages = {699},
  issn = {0004-637X},
  doi = {10.1086/169452},
  abstract = {To produce accurate estimates of the line-profile parameters of a model used to represent the spectral features in a solar oscillation power spectrum, it is necessary to (1) select the appropriate probability density function when deriving the maximum-likelihood function to be employed for the parameter estimation and (2) allow for the redistribution of spectral power caused by gaps in the data string. This paper describes a maximum-likelihood method for estimating the model parameters (based on the observed power spectrum statistics) that accounts for redistribution of spectral power caused by gaps in the data string, by convolving the model with the power spectrum of the observed window function. The accuracy and reliability of the method were tested using both artificial and authentic solar oscillation power spectrum data. A comparison of this method with various least-squares techniques is also presented.},
  file = {/Users/Oliver/Zotero/storage/D54EIUVF/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en}
}

@article{anderson+2017,
  title = {Improving \textbackslash textsl\{\vphantom\}{{Gaia}}\vphantom\{\} Parallax Precision with a Data-Driven Model of Stars},
  author = {Anderson, Lauren and Hogg, David W. and Leistedt, Boris and {Price-Whelan}, Adrian M. and Bovy, Jo},
  year = {2017},
  month = jun,
  pages = {arXiv:1706.05055},
  abstract = {Converting a noisy parallax measurement into a posterior belief over distance requires inference with a prior. Usually this prior represents beliefs about the stellar density distribution of the Milky Way. However, multi-band photometry exists for a large fraction of the \textbackslash textsl\{\textbackslash small\{Gaia\}\} \textbackslash textsl\{\textbackslash small\{TGAS\}\} Catalog and is incredibly informative about stellar distances. Here we use \textbackslash textsl\{\textbackslash small\{2MASS\}\} colors for 1.4 million \textbackslash textsl\{\textbackslash small\{TGAS\}\} stars to build a noise-deconvolved empirical prior distribution for stars in color--magnitude space. This model contains no knowledge of stellar astrophysics or the Milky Way, but is precise because it accurately generates a large number of noisy parallax measurements under an assumption of stationarity; that is, it is capable of combining the information from many stars. We use the Extreme Deconvolution (\textbackslash textsl\{\textbackslash small\{XD\}\}) algorithm---an Empirical Bayes approximation to a full hierarchical model of the true parallax and photometry of every star---to construct this prior. The prior is combined with a \textbackslash textsl\{\textbackslash small\{TGAS\}\} likelihood to infer a precise photometric parallax estimate and uncertainty (and full posterior) for every star. Our parallax estimates are more precise than the \textbackslash textsl\{\textbackslash small\{TGAS\}\} catalog entries by a median factor of 1.2 (14\% are more precise by a factor {$>$}2) and are more precise than previous Bayesian distance estimates that use spatial priors. We validate our parallax inferences using members of the Milky Way star cluster M67, which is not visible as a cluster in the \textbackslash textsl\{\textbackslash small\{TGAS\}\} parallax estimates, but appears as a cluster in our posterior parallax estimates. Our results, including a parallax posterior pdf for each of 1.4 million \textbackslash textsl\{\textbackslash small\{TGAS\}\} stars, are available in companion electronic tables.},
  file = {/Users/Oliver/Zotero/storage/IIIBFGJX/ui.adsabs.harvard.edu.html},
  journal = {ArXiv e-prints},
  language = {en}
}

@article{andrestriana+2017,
  title = {Internal Rotation of 13 Low-Mass Low-Luminosity Red Giants in the {{Kepler}} Field},
  author = {Andr{\'e}s Triana, Santiago and Corsaro, Enrico and De Ridder, Joris and Bonanno, Alfio and P{\'e}rez Hern{\'a}ndez, Fernando and Garc{\'i}a, Rafael},
  year = {2017},
  month = feb,
  volume = {1702},
  pages = {arXiv:1702.07910},
  abstract = {The Kepler space telescope has provided time series of red giants of such unprecedented quality that a detailed asteroseismic analysis becomes possible. For a limited set of about a dozen red giants, the observed oscillation frequencies obtained by peak-bagging together with the most recent pulsation codes allowed us to reliably determine the core/envelope rotation ratio. The results so far show that the current models are unable to reproduce the rotation ratios, predicting higher values than what is observed and thus indicating that an efficient angular momentum transport mechanism should be at work. Here we provide an asteroseismic analysis of a sample of 13 low-luminosity low-mass red giant stars observed by Kepler during its first nominal mission. These targets form a subsample of the 19 red giants studied previously Corsaro et al. 2015, which not only have a large number of extracted oscillation frequencies, but also unambiguous mode identifications We aim to extend the sample of red giants for which internal rotation ratios obtained by theoretical modeling of peak-bagged frequencies are available. We also derive the rotation ratios using different methods, and compare the results of these methods with each other. We built seismic models using a grid search combined with a Nelder-Mead simplex algorithm and obtained rotation averages employing Bayesian inference and inversion methods. We compared these averages with those obtained using a previously developed model-independent method. We find that the cores of the red giants in this sample are rotating 5 to 10 times faster than their envelopes, which is consistent with earlier results. The rotation rates computed from the different methods show good agreement for some targets, while some discrepancies exist for others.},
  journal = {ArXiv e-prints},
  keywords = {Astrophysics - Solar and Stellar Astrophysics}
}

@article{angus+2015,
  title = {Calibrating Gyrochronology Using {{Kepler}} Asteroseismic Targets},
  author = {Angus, Ruth and Aigrain, Suzanne and {Foreman-Mackey}, Daniel and McQuillan, Amy},
  year = {2015},
  month = jun,
  volume = {450},
  pages = {1787},
  doi = {10.1093/mnras/stv423},
  abstract = {Among the available methods for dating stars, gyrochronology is a powerful one because it requires knowledge of only the star's mass and rotation period. Gyrochronology relations have previously been calibrated using young clusters, with the Sun providing the only age dependence, and are therefore poorly calibrated at late ages. We used rotation period measurements of 310 Kepler stars with asteroseismic ages, 50 stars from the Hyades and Coma Berenices clusters and 6 field stars (including the Sun) with precise age measurements to calibrate the gyrochronology relation, whilst fully accounting for measurement uncertainties in all observable quantities. We calibrated a relation of the form P = A\textsuperscript{n} \texttimes{} (B - V - c)\textsuperscript{b}, where P is rotation period in days, A is age in Myr, B and V are magnitudes and a, b and n are the free parameters of our model. We found a = 0.40\^\{+0.3\}\_\{-0.05\}, b = 0.31\^\{+0.05\}\_\{-0.02\} and n = 0.55\^\{+0.02\}\_\{-0.09\}. Markov Chain Monte Carlo methods were used to explore the posterior probability distribution functions of the gyrochronology parameters and we carefully checked the effects of leaving out parts of our sample, leading us to find that no single relation between rotation period, colour and age can adequately describe all the subsets of our data. The Kepler asteroseismic stars, cluster stars and local field stars cannot all be described by the same gyrochronology relation. The Kepler asteroseismic stars may be subject to observational biases; however, the clusters show unexpected deviations from the predicted behaviour, providing concerns for the overall reliability of gyrochronology as a dating method.},
  file = {/Users/Oliver/Zotero/storage/ZRKW3VS4/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Core Gyrochronology},
  language = {en},
  number = {2}
}

@article{angus+2016,
  title = {Systematics-Insensitive Periodic Signal Search with {{K2}}},
  author = {Angus, Ruth and {Foreman-Mackey}, Daniel and Johnson, John A.},
  year = {2016},
  month = feb,
  volume = {818},
  pages = {109},
  issn = {1538-4357},
  doi = {10.3847/0004-637X/818/2/109},
  abstract = {From pulsating stars to transiting exoplanets, the search for periodic signals in K2 data, Kepler's 2-wheeled extension, is relevant to a long list of scientific goals. Systematics affecting K2 light curves due to the decreased spacecraft pointing precision inhibit the easy extraction of periodic signals from the data. We here develop a method for producing periodograms of K2 light curves that are insensitive to pointing-induced systematics; the Systematics-Insensitive Periodogram (SIP). Traditional sine-fitting periodograms use a generative model to find the frequency of a sinusoid that best describes the data. We extend this principle by including systematic trends, based on a set of 'Eigen light curves', following Foreman-Mackey et al. (2015), in our generative model as well as a sum of sine and cosine functions over a grid of frequencies. Using this method we are able to produce periodograms with vastly reduced systematic features. The quality of the resulting periodograms are such that we can recover acoustic oscillations in giant stars and measure stellar rotation periods without the need for any detrending. The algorithm is also applicable to the detection of other periodic phenomena such as variable stars, eclipsing binaries and short-period exoplanet candidates. The SIP code is available at https://github.com/RuthAngus/SIPK2.},
  archivePrefix = {arXiv},
  eprint = {1505.07105},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/5R7R4JJX/1505.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  number = {2}
}

@article{angus+2016a,
  title = {Stellar Rotation Period Inference with {{Gaussian}} Processes},
  author = {Angus, Ruth and Aigrain, Suzanne and {Foreman-Mackey}, Daniel},
  year = {2016},
  month = oct,
  volume = {29A},
  pages = {191},
  doi = {10.1017/S1743921316002738},
  abstract = {The light curves of spotted, rotating stars are often non-sinusoidal and Quasi-Periodic (QP) and a strictly periodic sinusoid is therefore not a representative generative model. Ideally, a physical model of the stellar surface would be conditioned on the data, however the parameters of such models can be highly degenerate.},
  file = {/Users/Oliver/Zotero/storage/E5YU744A/ui.adsabs.harvard.edu.html},
  journal = {IAU Focus Meeting},
  keywords = {GPs},
  language = {en}
}

@article{angus+2018,
  title = {Inferring Probabilistic Stellar Rotation Periods Using {{Gaussian}} Processes},
  author = {Angus, Ruth and Morton, Timothy and Aigrain, Suzanne and {Foreman-Mackey}, Daniel and Rajpaul, Vinesh},
  year = {2018},
  month = feb,
  volume = {474},
  pages = {2094},
  doi = {10.1093/mnras/stx2109},
  abstract = {Variability in the light curves of spotted, rotating stars is often non-sinusoidal and quasi-periodic - spots move on the stellar surface and have finite lifetimes, causing stellar flux variations to slowly shift in phase. A strictly periodic sinusoid therefore cannot accurately model a rotationally modulated stellar light curve. Physical models of stellar surfaces have many drawbacks preventing effective inference, such as highly degenerate or high-dimensional parameter spaces. In this work, we test an appropriate effective model: a Gaussian Process with a quasi-periodic covariance kernel function. This highly flexible model allows sampling of the posterior probability density function of the periodic parameter, marginalizing over the other kernel hyperparameters using a Markov Chain Monte Carlo approach. To test the effectiveness of this method, we infer rotation periods from 333 simulated stellar light curves, demonstrating that the Gaussian process method produces periods that are more accurate than both a sine-fitting periodogram and an autocorrelation function method. We also demonstrate that it works well on real data, by inferring rotation periods for 275 Kepler stars with previously measured periods. We provide a table of rotation periods for these and many more, altogether 1102 Kepler objects of interest, and their posterior probability density function samples. Because this method delivers posterior probability density functions, it will enable hierarchical studies involving stellar rotation, particularly those involving population modelling, such as inferring stellar ages, obliquities in exoplanet systems, or characterizing star-planet interactions. The code used to implement this method is available online.},
  file = {/Users/Oliver/Zotero/storage/K2NU4AD2/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Core Gyrochronology,GPs},
  language = {en},
  number = {2}
}

@article{angus+2019,
  title = {An Age-Dating Method That Combines Stellar Evolution Models with Gyrochronology},
  author = {Angus, Ruth and Morton, Timothy D. and Brewer, John and Bedell, Megan and {Foreman-Mackey}, Daniel and Curtis, Jason and Hogg, David W.},
  year = {2019},
  month = jan,
  volume = {233},
  pages = {235.09},
  abstract = {By combining two different sets of observable stellar properties and dating methods that are sensitive to two different evolving processes in stars: core hydrogen burning and magnetic braking, it is possible to infer more precise and accurate ages than using either method in isolation. In this investigation, the observables of main sequence stars that trace core hydrogen burning and stellar evolution on the HR diagram are combined with their Kepler rotation periods in a Bayesian framework, to infer stellar ages from both stellar evolution models and gyrochronology. We show that incorporating rotation periods into stellar evolution models significantly improves the precision of inferred ages. Since ages predicted with gyrochronology can, in general, be much more precise than isochronal ages, care must be taken to ensure that the gyrochronology model being used is accurate. We provide open source code that infers stellar ages from spectroscopic parameters, apparent magnitudes, parallaxes and rotation periods.},
  file = {/Users/Oliver/Zotero/storage/XH74NNTY/ui.adsabs.harvard.edu.html},
  journal = {American Astronomical Society Meeting Abstracts \#233},
  keywords = {Core Gyrochronology},
  language = {en}
}

@article{angus+aigrain2015,
  title = {The Future of Gyrochronology: Opportunities from {{K2}} and {{TESS}}},
  shorttitle = {The Future of Gyrochronology},
  author = {Angus, Ruth and Aigrain, Suzanne},
  year = {2015},
  month = aug,
  volume = {29},
  pages = {2258409},
  abstract = {Recent studies of Kepler Solar-like oscillators demonstrate that ages predicted by gyrochronology and asteroseismology are not always compatible. The postulated gyrochronological relation between rotation period, mass and age for F, G and K main-sequence stars may be an over-simplification of the underlying physics. Additional targets with photometric rotation periods and precise ages are needed to resolve the tension between gyrochronology and asteroseismology. K2 and TESS will provide rotation periods and asteroseismic ages for hundreds of stars, some of which will lie in clusters. Both of these surveys will require sophisticated methods for photometry extraction, treatment of systematics and rotation period measurement. A thorough, statistically rigorous approach will be required in order to combine information across surveys and stellar populations. We demonstrate new methods for the extraction of rotation periods from noisy data and discuss the prospects of these missions and the methods required to maximise their impact on the advancement of gyrochronology.},
  file = {/Users/Oliver/Zotero/storage/8F6Q5WKV/ui.adsabs.harvard.edu.html},
  journal = {IAU General Assembly},
  keywords = {Core Gyrochronology},
  language = {en}
}

@article{appourchaux+1998,
  title = {The Art of Fitting P-Mode Spectra. {{I}}. {{Maximum}} Likelihood Estimation},
  author = {Appourchaux, T. and Gizon, L. and {Rabello-Soares}, M.-C.},
  year = {1998},
  month = oct,
  volume = {132},
  pages = {107--119},
  issn = {0365-0138},
  doi = {10.1051/aas:1998441},
  abstract = {In this article we present our state of the art of fitting helioseismic p-mode spectra. We give a step by step recipe for fitting the spectra: statistics of the spectra both for spatially unresolved and resolved data, the use of Maximum Likelihood estimates, the statistics of the p-mode parameters, the use of Monte-Carlo simulation and the
significance of fitted parameters. The recipe is applied to synthetic low-resolution data, similar to those of the LOI, using Monte-Carlo simulations. For such spatially resolved data, the statistics of the Fourier spectrum is assumed to be a multi-normal distribution; the statistics of the power spectrum is not a chi (2) with 2 degrees of freedom. Results for l=1 shows that all parameters describing the p modes can be obtained with negligible bias and with minimum variance provided that the leakage matrix is known. Systematic errors due to an imperfect knowledge of the leakage matrix are derived for all the p-mode parameters.},
  file = {/Users/Oliver/Zotero/storage/JG9NKM37/Appourchaux et al. - 1998 - The art of fitting p-mode spectra. I. Maximum like.pdf},
  journal = {Astronomy and Astrophysics Supplement Series},
  keywords = {DATA ANALYSIS,METHODS: ANALYTICAL,STATISTICAL,SUN: OSCILLATIONS}
}

@article{appourchaux+2010,
  title = {The Quest for the Solar g Modes},
  author = {Appourchaux, T. and Belkacem, K. and Broomhall, A.-M. and Chaplin, W. J. and Gough, D. O. and Houdek, G. and Provost, J. and Baudin, F. and Boumier, P. and Elsworth, Y. and Garc{\'i}a, R. A. and Andersen, B. N. and Finsterle, W. and Fr{\"o}hlich, C. and Gabriel, A. and Grec, G. and Jim{\'e}nez, A. and Kosovichev, A. and Sekii, T. and Toutain, T. and {Turck-Chi{\`e}ze}, S.},
  year = {2010},
  month = feb,
  volume = {18},
  pages = {197--277},
  issn = {0935-4956},
  doi = {10.1007/s00159-009-0027-z},
  abstract = {Solar gravity modes (or g modes)\textemdash oscillations of the solar interior on which buoyancy acts as the restoring force\textemdash have the
potential to provide unprecedented inference on the structure and dynamics of the solar core, inference that is not possible with the well-observed acoustic modes (or p modes). The relative high amplitude of the g-mode eigenfunctions in the core and the evanesence of the modes in the convection zone make the modes particularly sensitive to the physical and dynamical conditions in the core. Owing to the existence of the convection zone, the g modes have very low amplitudes at
photospheric levels, which makes the modes extremely hard to detect. In this article, we review the current state of play regarding attempts to detect g modes. We review the theory of g modes, including theoretical estimation of the g-mode frequencies, amplitudes and damping rates. Then we go on to discuss the techniques that have been used to try to detect g modes. We review results in the literature, and finish by looking to the future, and the potential advances that can be made\textemdash from both data and data-analysis perspectives\textemdash to give unambiguous detections of individual g modes. The review ends by concluding that, at the time of writing, there is indeed a consensus amongst the authors that there is currently no undisputed detection of solar g modes.},
  file = {/Users/Oliver/Zotero/storage/69Z3DYJA/Appourchaux et al. - 2010 - The quest for the solar g modes.pdf},
  journal = {Astronomy and Astrophysics Review},
  keywords = {Data analysis,g modes,Sun,Theory}
}

@article{appourchaux+2012,
  title = {Oscillation Mode Frequencies of 61 Main-Sequence and Subgiant Stars Observed by {{Kepler}}},
  author = {Appourchaux, T. and Chaplin, W. J. and Garc{\'i}a, R. A. and Gruberbauer, M. and Verner, G. A. and Antia, H. M. and Benomar, O. and Campante, T. L. and Davies, G. R. and Deheuvels, S. and Handberg, R. and Hekker, S. and Howe, R. and R{\'e}gulo, C. and Salabert, D. and Bedding, T. R. and White, T. R. and Ballot, J. and Mathur, S. and Silva Aguirre, V. and Elsworth, Y. P. and Basu, S. and Gilliland, R. L. and {Christensen-Dalsgaard}, J. and Kjeldsen, H. and Uddin, K. and Stumpe, M. C. and Barclay, T.},
  year = {2012},
  month = jul,
  volume = {543},
  pages = {A54},
  doi = {10.1051/0004-6361/201218948},
  abstract = {Context. Solar-like oscillations have been observed by Kepler and CoRoT in several solar-type stars, thereby providing a way to probe the stars using asteroseismology \\
 Aims: We provide the mode frequencies of the oscillations of various stars required to perform a comparison with those obtained from stellar modelling. \\
 Methods: We used a time series of nine months of data for each star. The 61 stars observed were categorised in three groups: simple, F-like, and mixed-mode. The simple group includes stars for which the identification of the mode degree is obvious. The F-like group includes stars for which the identification of the degree is ambiguous. The mixed-mode group includes evolved stars for which the modes do not follow the asymptotic relation of low-degree frequencies. Following this categorisation, the power spectra of the 61 main-sequence and subgiant stars were analysed using both maximum likelihood estimators and Bayesian estimators, providing individual mode characteristics such as frequencies, linewidths, and mode heights. We developed and describe a methodology for extracting a single set of mode frequencies from multiple sets derived by different methods and individual scientists. We report on how one can assess the quality of the fitted parameters using the likelihood ratio test and the posterior probabilities. \\
 Results: We provide the mode frequencies of 61 stars (with their 1-{$\sigma$} error bars), as well as their associated \'echelle diagrams. Appendices are available in electronic form at \href{http://www.aanda.org}{http://www.aanda.org}},
  file = {/Users/Oliver/Zotero/storage/49MZCR8I/Appourchaux et al. - 2012 - Oscillation mode frequencies of 61 main-sequence a.pdf;/Users/Oliver/Zotero/storage/P6QB77NC/abstract.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{appourchaux+2016,
  title = {Oscillation Mode Linewidths and Heights of 23 Main-Sequence Stars Observed by {{{\emph{Kepler}}}} {\emph{(}}{{{\emph{Corrigendum}}}}{\emph{)}}},
  author = {Appourchaux, T. and Antia, H. M. and Benomar, O. and Campante, T. L. and Davies, G. R. and Handberg, R. and Howe, R. and R{\'e}gulo, C. and Belkacem, K. and Houdek, G. and Garc{\'i}a, R. A. and Chaplin, W. J.},
  year = {2016},
  month = nov,
  volume = {595},
  pages = {C2},
  issn = {0004-6361, 1432-0746},
  doi = {10.1051/0004-6361/201323317e},
  journal = {Astronomy \& Astrophysics},
  language = {en}
}

@article{appourchaux+2018,
  title = {Searching for g Modes. {{I}}. {{A}} New Calibration of the {{GOLF}} Instrument},
  author = {Appourchaux, T. and Boumier, P. and Leibacher, J. W. and Corbard, T.},
  year = {2018},
  month = sep,
  volume = {617},
  pages = {A108},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201833535},
  abstract = {Context. The recent claims of g-mode detection have restarted the search for these potentially extremely important modes. These claims can be reassessed in view of the different data sets available from the SoHO instruments and ground-based instruments. Aims: We produce a new calibration of the GOLF data with a more consistent p-mode amplitude and a more consistent time shift correction compared to the time series used in the past. Methods: The calibration of 22 yr of GOLF data is done with a simpler approach that uses only the predictive radial velocity of the SoHO spacecraft as a reference. Using p modes, we measure and correct the time shift between ground- and space-based instruments and the GOLF instrument. Results: The p-mode velocity calibration is now consistent to within a few percent with other instruments. The remaining time shifts are within {$\pm$}5 s for 99.8\% of the time series.

The new calibrated series (FITS) are available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr
(ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/617/A108},
  file = {/Users/Oliver/Zotero/storage/SJVIN2PC/Appourchaux et al. - 2018 - Searching for g modes. I. A new calibration of the.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {methods: data analysis,Sun: helioseismology}
}

@article{appourchaux+corbard2019,
  title = {Searching for g Modes. {{II}}. {{Unconfirmed}} g-Mode Detection in the Power Spectrum of the Time Series of Round-Trip Travel Time},
  author = {Appourchaux, T. and Corbard, T.},
  year = {2019},
  month = apr,
  volume = {624},
  pages = {A106},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201935196},
  abstract = {Context. The recent claims of g-mode detection have restarted the search
for these potentially extremely important modes. The claimed detection
of g modes was obtained from the analysis of the power spectrum of the
time series of round-trip travel time of p modes. Aims: The goal
of this paper is to reproduce these results on which the claims are
based for confirming or invalidating the detection of g modes with the
method used to make the claims. Methods: We computed the time
series of round-trip travel time using the procedure given in Fossat et
al. (2017, A\&A, 604, A40), and used different variations of the
times series for comparison. We used the recently calibrated GOLF data
(published in Paper I) with different sampling, different
photomultipliers, different length of data for reproducing the analysis.
We also correlated the power spectrum with an asymptotic model of g-mode
frequencies in a similar manner to Fossat and Schmider (2018, A\&A,
612, L1). We devised a scheme for optimising the correlation both for
pure noise and for the GOLF data. Results: We confirm the
analysis performed in Fossat et al. (2017) but draw different
conclusions. Their claims of detection of g modes cannot be confirmed
when changing parameters such as sampling interval, length of time
series, or photomultipliers. Other instrument such as GONG and BiSON do
not confirm their detection. We also confirm the analysis performed in
Fossat and Schmider (2018), but again draw different conclusions. For
GOLF, the correlation of the power spectrum with the asymptotic model of
g-mode frequencies for l = 1 and l = 2 show a high correlation at lag=0
and at lag corresponding to the rotational splitting {$\nu$}l,
but the same occurs for pure noise due to the large number of peaks
present in the model. In addition, other very different parameters
defining the asymptotic model also provide a high correlation at these
lags. We conclude that the detection performed in Fossat and Schmider
(2018) is an artefact of the methodology.},
  file = {/Users/Oliver/Zotero/storage/DX36VYHA/Appourchaux and Corbard - 2019 - Searching for g modes. II. Unconfirmed g-mode dete.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {Sun: helioseismology,Sun: interior,Sun: oscillations}
}

@article{appourchaux2004,
  title = {On Detecting Short-Lived p Modes in a Stellar Oscillation Spectrum},
  author = {Appourchaux, T.},
  year = {2004},
  month = dec,
  volume = {428},
  pages = {1039--1042},
  issn = {0004-6361, 1432-0746},
  doi = {10.1051/0004-6361:20041682},
  abstract = {The false alarm probability for detecting peaks embedded in a power spectrum of noise was given by Scargle (1982). This test has been used in helioseismology to detect long-lived modes such as g modes (Appourchaux et al. 2000). With the development of asteroseismology, there is now a need to define a similar test but for short-lived p modes. In this article, I define a false alarm test for detecting short-lived p modes, and I give the probability of detecting such modes given their signal-to-noise ratio, their linewidths and the duration of observation.},
  file = {/Users/Oliver/Zotero/storage/6A54JBMC/Appourchaux - 2004 - On detecting short-lived p modes in a stellar osci.pdf},
  journal = {Astronomy \& Astrophysics},
  language = {en},
  number = {3}
}

@article{appourchaux2014,
  title = {A Crash Course on Data Analysis in Asteroseismology},
  author = {Appourchaux, Thierry},
  year = {2014},
  month = feb,
  pages = {123},
  abstract = {In this course, I try to provide a few basics required for performing data analysis in asteroseismology. First, I address how one can properly treat times series: the sampling, the filtering effect, the use of Fourier transform, the associated statistics. Second, I address how one can apply statistics for decision making and for parameter estimation either in a frequentist of a Bayesian framework. Last, I review how these basic principle have been applied (or not) in asteroseismology.},
  file = {/Users/Oliver/Zotero/storage/SY7JFDN2/Appourchaux - 2014 - A crash course on data analysis in asteroseismolog.pdf},
  journal = {Asteroseismology}
}

@article{arenou+2018,
  title = {Gaia {{Data Release}} 2: {{Catalogue}} Validation},
  shorttitle = {Gaia {{Data Release}} 2},
  author = {Arenou, F. and Luri, X. and Babusiaux, C. and Fabricius, C. and Helmi, A. and Muraveva, T. and Robin, A. C. and Spoto, F. and Vallenari, A. and Antoja, T. and {Cantat-Gaudin}, T. and Jordi, C. and Leclerc, N. and Reyl{\'e}, C. and {Romero-G{\'o}mez}, M. and Shih, I.-C. and Soria, S. and Barache, C. and Bossini, D. and Bragaglia, A. and Breddels, M. A. and Fabrizio, M. and Lambert, S. and Marrese, P. M. and Massari, D. and Moitinho, A. and Robichon, N. and {Ruiz-Dern}, L. and Sordo, R. and Veljanoski, J. and Di Matteo, P. and Eyer, L. and Jasniewicz, G. and Pancino, E. and Soubiran, C. and Spagna, A. and Tanga, P. and Turon, C. and Zurbach, C.},
  year = {2018},
  month = apr,
  pages = {arXiv:1804.09375},
  abstract = {The second Gaia data release (DR2), contains very precise astrometric and photometric properties for more than one billion sources, astrophysical parameters for dozens of millions, radial velocities for millions, variability information for half a million of stellar sources and orbits for thousands of solar system objects. Before the Catalogue publication, these data have undergone dedicated validation processes. The goal of this paper is to describe the validation results in terms of completeness, accuracy and precision of the various Gaia DR2 data. The validation processes include a systematic analysis of the Catalogue content to detect anomalies, either individual errors or statistical properties, using statistical analysis, and comparisons to external data or to models. Although the astrometric, photometric and spectroscopic data are of unprecedented quality and quantity, it is shown that the data cannot be used without a dedicated attention to the limitations described here, in the Catalogue documentation and in accompanying papers. A particular emphasis is put on the caveats for the statistical use of the data in scientific exploitation.},
  file = {/Users/Oliver/Zotero/storage/27PMMX5H/Arenou et al. - 2018 - Gaia Data Release 2 Catalogue validation.pdf;/Users/Oliver/Zotero/storage/Z3D3J2BA/ui.adsabs.harvard.edu.html},
  journal = {ArXiv e-prints},
  language = {en}
}

@article{arentoft+2017,
  title = {Convective-Core Overshoot and Suppression of Oscillations: {{Constraints}} from Red Giants in {{NGC6811}}},
  shorttitle = {Convective-Core Overshoot and Suppression of Oscillations},
  author = {Arentoft, T. and Brogaard, K. and {Jessen-Hansen}, J. and Aguirre, V. Silva and Kjeldsen, H. and Mosumgaard, J. R. and Sandquist, E. L.},
  year = {2017},
  month = mar,
  abstract = {Using data from the NASA spacecraft Kepler, we study solar-like oscillations in red-giant stars in the open cluster NGC6811. We determine oscillation frequencies, frequency separations, period spacings of mixed modes and mode visibilities for eight cluster giants. The oscillation parameters show that these stars are helium-core-burning red giants. The eight stars form two groups with very different oscillation power spectra; the four stars with lowest Delta\_nu-values display rich sets of mixed l=1 modes, while this is not the case for the four stars with higher Delta\_nu. For the four stars with lowest Delta\_nu, we determine the asymptotic period spacing of the mixed modes, DeltaP, which together with the masses we derive for all eight stars suggest that they belong to the so-called secondary clump. Based on the global oscillation parameters, we present initial theoretical stellar modeling which indicate that we can constrain convective-core overshoot on the main sequence and in the helium-burning phase for these \textasciitilde 2M\_sun stars. Finally, our results indicate less mode suppression than predicted by recent theories for magnetic suppression of certain oscillation modes in red giants.},
  archivePrefix = {arXiv},
  eprint = {1703.01097},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/2MMJMH9R/Arentoft et al. - 2017 - Convective-core overshoot and suppression of oscil.pdf;/Users/Oliver/Zotero/storage/P4R2WVGZ/1703.html},
  journal = {arXiv:1703.01097 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{armstrong+2015,
  title = {K2 {{Variable Catalogue}}: {{Variable Stars}} and {{Eclipsing Binaries}} in {{K2 Campaigns}} 1 and 0},
  shorttitle = {K2 {{Variable Catalogue}}},
  author = {Armstrong, D. J. and Kirk, J. and Lam, K. W. F. and McCormac, J. and Walker, S. R. and Brown, D. J. A. and Osborn, H. P. and Pollacco, D. L. and Spake, J.},
  year = {2015},
  month = jul,
  volume = {579},
  pages = {A19},
  issn = {0004-6361, 1432-0746},
  doi = {10.1051/0004-6361/201525889},
  abstract = {We have created a catalogue of variable stars found from a search of the publicly available K2 mission data from Campaigns 1 and 0. This catalogue provides the identifiers of 8395 variable stars, including 199 candidate eclipsing binaries with periods up to 60d and 3871 periodic or quasi-periodic objects, with periods up to 20d for Campaign 1 and 15d for Campaign 0. Lightcurves are extracted and detrended from the available data. These are searched using a combination of algorithmic and human classification, leading to a classifier for each object as an eclipsing binary, sinusoidal periodic, quasi periodic, or aperiodic variable. The source of the variability is not identified, but could arise in the non-eclipsing binary cases from pulsation or stellar activity. Each object is cross-matched against variable star related guest observer proposals to the K2 mission, which specifies the variable type in some cases. The detrended lightcurves are also compared to lightcurves currently publicly available. The resulting catalogue is made available online via the MAST archive at https://archive.stsci.edu/prepds/k2varcat/, and gives the ID, type, period, semi-amplitude and range of the variation seen. We also make available the detrended lightcurves for each object.},
  archivePrefix = {arXiv},
  eprint = {1502.04004},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/WUWES985/Armstrong et al. - 2015 - K2 Variable Catalogue Variable Stars and Eclipsin.pdf;/Users/Oliver/Zotero/storage/8BM49DPI/1502.html},
  journal = {Astronomy \& Astrophysics},
  keywords = {C3,Notes}
}

@article{armstrong+2016,
  title = {Transit {{Shapes}} and {{Self Organising Maps}} as a {{Tool}} for {{Ranking Planetary Candidates}}: {{Application}} to {{Kepler}} and {{K2}}},
  shorttitle = {Transit {{Shapes}} and {{Self Organising Maps}} as a {{Tool}} for {{Ranking Planetary Candidates}}},
  author = {Armstrong, David J. and Pollacco, Don and Santerne, Alexandre},
  year = {2016},
  month = nov,
  abstract = {A crucial step in planet hunting surveys is to select the best candidates for follow up observations, given limited telescope resources. This is often performed by human `eyeballing', a time consuming and statistically awkward process. Here we present a new, fast machine learning technique to separate true planet signals from astrophysical false positives. We use Self Organising Maps (SOMs) to study the transit shapes of \textbackslash emph\{Kepler\} and \textbackslash emph\{K2\} known and candidate planets. We find that SOMs are capable of distinguishing known planets from known false positives with a success rate of 87.0\textbackslash\%, using the transit shape alone. Furthermore, they do not require any candidates to be dispositioned prior to use, meaning that they can be used early in a mission's lifetime. A method for classifying candidates using a SOM is developed, and applied to previously unclassified members of the \textbackslash emph\{Kepler\} KOI list as well as candidates from the \textbackslash emph\{K2\} mission. The method is extremely fast, taking minutes to run the entire KOI list on a typical laptop. We make \textbackslash texttt\{Python\} code for performing classifications publicly available, using either new SOMs or those created in this work. The SOM technique represents a novel method for ranking planetary candidate lists, and can be used both alone or as part of a larger autovetting code.},
  archivePrefix = {arXiv},
  eprint = {1611.01968},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/XE5BU8IA/Armstrong et al. - 2016 - Transit Shapes and Self Organising Maps as a Tool .pdf;/Users/Oliver/Zotero/storage/2CCGMFXX/1611.html},
  journal = {arXiv:1611.01968 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Instrumentation and Methods for Astrophysics},
  primaryClass = {astro-ph}
}

@article{armstrong+2016a,
  title = {Variability in the {{Atmosphere}} of the {{Hot Giant Planet HAT}}-{{P}}-7 b},
  author = {Armstrong, David J. and {de Mooij}, Ernst and Barstow, Joanna and Osborn, Hugh P. and Blake, James and Saniee, Nessa Fereshteh},
  year = {2016},
  month = dec,
  volume = {1},
  pages = {0004},
  issn = {2397-3366},
  doi = {10.1038/s41550-016-0004},
  abstract = {As an exoplanet orbits its host star it reflects and emits light, forming a distinctive phase curve. By observing this light, we can study the atmosphere and surface of distant planets. The planets in our Solar System show a wide range of atmospheric phenomena, with stable wind patterns, changing storms, and evolving anomalies. Brown dwarfs also exhibit atmospheric variability. Such temporal variability in the atmosphere of a giant exoplanet has not to date been observed. HAT-P-7 b is an exoplanet with a known offset in the peak of its phase curve. Here we present variations in the peak offset ranging between -0.086+0.033-0.033 to 0.143+0.040-0.037 in phase, implying that the peak brightness repeatedly shifts from one side of the planet's substellar point to the other. The variability occurs on a timescale of tens to hundreds of days. These shifts in brightness are indicative of variability in the planet's atmosphere, and result from a changing balance of thermal emission and reflected flux from the planet's dayside. We suggest that variation in wind speed in the planetary atmosphere, leading to variable cloud coverage on the dayside and a changing energy balance, is capable of explaining the observed variation.},
  archivePrefix = {arXiv},
  eprint = {1612.04225},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/GCJWV9DV/Armstrong et al. - 2016 - Variability in the Atmosphere of the Hot Giant Pla.pdf;/Users/Oliver/Zotero/storage/7DIDRWEE/1612.html},
  journal = {Nature Astronomy},
  keywords = {C3,CHECK},
  number = {1}
}

@article{arnett+moravveji2017,
  title = {Synergies between {{Asteroseismology}} and {{Three}}-Dimensional {{Simulations}} of {{Stellar Turbulence}}},
  author = {Arnett, W. David and Moravveji, E.},
  year = {2017},
  month = jan,
  abstract = {Turbulent mixing of chemical elements by convection has fundamental effects on the evolution of stars. The standard algorithm at present, mixing-length theory (MLT), is intrinsically local, and must be supplemented by extensions with adjustable parameters. As a step toward reducing this arbitrariness, we compare asteroseismically inferred internal structures of two Kepler slowly pulsating B stars (SPB's; \$M\textbackslash sim 3.25 M\_\textbackslash odot\$) to predictions of 321D turbulence theory, based upon well-resolved, truly turbulent three-dimensional simulations (Arnett , et al. 2015, Christini, et al. 2016) which include boundary physics absent from MLT. We find promising agreement between the steepness and shapes of the theoretically-predicted composition profile outside the convective region in 3D simulations and in asteroseismically constrained composition profiles in the best 1D models of the two SPBs. The structure and motion of the boundary layer, and the generation of waves, are discussed.},
  archivePrefix = {arXiv},
  eprint = {1701.07803},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/HEJKV8N6/Arnett and Moravveji - 2017 - Synergies between Asteroseismology and Three-dimen.pdf;/Users/Oliver/Zotero/storage/JESVIGU3/1701.html},
  journal = {arXiv:1701.07803 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{astraatmadja+bailer-jones2016,
  title = {Estimating {{Distances}} from {{Parallaxes}}. {{II}}. {{Performance}} of {{Bayesian Distance Estimators}} on a {{Gaia}}-like {{Catalogue}}},
  author = {Astraatmadja, Tri L. and {Bailer-Jones}, Coryn A. L.},
  year = {2016},
  month = dec,
  volume = {832},
  pages = {137},
  doi = {10.3847/0004-637X/832/2/137},
  abstract = {Estimating a distance by inverting a parallax is only valid in the absence of noise. As most stars in the Gaia catalog will have non-negligible fractional parallax errors, we must treat distance estimation as a constrained inference problem. Here we investigate the performance of various priors for estimating distances, using a simulated Gaia catalog of one billion stars. We use three minimalist, isotropic priors, as well an anisotropic prior derived from the observability of stars in a Milky Way model. The two priors that assume a uniform distribution of stars\textemdash either in distance or in space density\textemdash give poor results: The root mean square fractional distance error, \{f\}\textsubscript{\{rms\vphantom\}}\vphantom\{\}, grows far in excess of 100\% once the fractional parallax error, \{f\}\textsubscript{\{true\vphantom\}}\vphantom\{\}, is larger than 0.1. A prior assuming an exponentially decreasing space density with increasing distance performs well once its single parameter\textemdash the scale length\textemdash{} has been set to an appropriate value: \{f\}\textsubscript{\{rms\vphantom\}}\vphantom\{\} is roughly equal to \{f\}\textsubscript{\{true\vphantom\}}\vphantom\{\} for \{f\}\textsubscript{\{true\vphantom\}}\vphantom\{\}\textbackslash lt 0.4, yet does not increase further as \{f\}\textsubscript{\{true\vphantom\}}\vphantom\{\} increases up to to 1.0. The Milky Way prior performs well except toward the Galactic center, due to a mismatch with the (simulated) data. Such mismatches will be inevitable (and remain unknown) in real applications, and can produce large errors. We therefore suggest adopting the simpler exponentially decreasing space density prior, which is also less time-consuming to compute. Including Gaia photometry improves the distance estimation significantly for both the Milky Way and exponentially decreasing space density prior, yet doing so requires additional assumptions about the physical nature of stars.},
  file = {/Users/Oliver/Zotero/storage/P95BD9AA/Astraatmadja and Bailer-Jones - 2016 - Estimating Distances from Parallaxes. II. Performa.pdf;/Users/Oliver/Zotero/storage/AQ9M7VT9/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{astraatmadja+bailer-jones2016a,
  title = {Estimating {{Distances}} from {{Parallaxes}}. {{III}}. {{Distances}} of {{Two Million Stars}} in the {{Gaia DR1 Catalogue}}},
  author = {Astraatmadja, Tri L. and {Bailer-Jones}, Coryn A. L.},
  year = {2016},
  month = dec,
  volume = {833},
  pages = {119},
  doi = {10.3847/1538-4357/833/1/119},
  abstract = {We infer distances and their asymmetric uncertainties for two million stars using the parallaxes published in the Gaia DR1 (GDR1) catalogue. We do this with two distance priors: A minimalist, isotropic prior assuming an exponentially decreasing space density with increasing distance, and an anisotropic prior derived from the observability of stars in a Milky Way model. We validate our results by comparing our distance estimates for 105 Cepheids which have more precise, independently estimated distances. For this sample we find that the Milky Way prior performs better (the rms of the scaled residuals is 0.40) than the exponentially decreasing space density prior (rms is 0.57), although for distances beyond 2 kpc the Milky Way prior performs worse, with a bias in the scaled residuals of -0.36 (versus -0.07 for the exponentially decreasing space density prior). We do not attempt to include the photometric data in GDR1 due to the lack of reliable color information. Our distance catalog is available at \href{http://www.mpia.de/homes/calj/tgas_distances/main.html}{http://www.mpia.de/homes/calj/tgas\_distances/main.html} as well as at CDS. This should only be used to give individual distances. Combining data or testing models should be done with the original parallaxes, and attention paid to correlated and systematic uncertainties.},
  file = {/Users/Oliver/Zotero/storage/FKGK9NQ9/Astraatmadja and Bailer-Jones - 2016 - Estimating Distances from Parallaxes. III. Distanc.pdf;/Users/Oliver/Zotero/storage/YQR9DH5M/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{astraatmadja+bailer-jones2017,
  title = {Estimating Distances from Parallaxes},
  author = {Astraatmadja, Tri L. and {Bailer-Jones}, Coryn},
  year = {2017},
  month = jan,
  pages = {134.06},
  abstract = {In astrometric surveys such as Gaia and LSST, parallaxes will be measured for about a billion stars, but zero distances will be measured. Distances must be inferred from the parallaxes, and the common inference practice is by inverting the parallax. This, however, is only appropriate when there is no noise present. As noise will always be present and most stars in future surveys will have non-negligible fractional parallax uncertainties, we must treat distance estimation as an inference problem. The usage of prior assumptions become unavoidable. In this talk I will present a method on how to infer distances using Bayesian inference. Three minimalists, isotropic priors are used, as well an anisotropic prior derived from the observability of stars in a Milky Way model. The performance of these priors are investigated using a simulated Gaia-like catalogue. Recent results of distance estimation using the parallaxes of 2 million Gaia DR1 stars will also be discussed.},
  file = {/Users/Oliver/Zotero/storage/9GJFBE85/ui.adsabs.harvard.edu.html},
  journal = {American Astronomical Society Meeting Abstracts},
  language = {en}
}

@article{astropycollaboration+2013,
  title = {Astropy: {{A}} Community {{Python}} Package for Astronomy},
  shorttitle = {Astropy},
  author = {{Astropy Collaboration} and Robitaille, Thomas P. and Tollerud, Erik J. and Greenfield, Perry and Droettboom, Michael and Bray, Erik and Aldcroft, Tom and Davis, Matt and Ginsburg, Adam and {Price-Whelan}, Adrian M. and Kerzendorf, Wolfgang E. and Conley, Alexander and Crighton, Neil and Barbary, Kyle and Muna, Demitri and Ferguson, Henry and Grollier, Fr{\'e}d{\'e}ric and Parikh, Madhura M. and Nair, Prasanth H. and Unther, Hans M. and Deil, Christoph and Woillez, Julien and Conseil, Simon and Kramer, Roban and Turner, James E. H. and Singer, Leo and Fox, Ryan and Weaver, Benjamin A. and Zabalza, Victor and Edwards, Zachary I. and Azalee Bostroem, K. and Burke, D. J. and Casey, Andrew R. and Crawford, Steven M. and Dencheva, Nadia and Ely, Justin and Jenness, Tim and Labrie, Kathleen and Lim, Pey Lian and Pierfederici, Francesco and Pontzen, Andrew and Ptak, Andy and Refsdal, Brian and Servillat, Mathieu and Streicher, Ole},
  year = {2013},
  month = oct,
  volume = {558},
  pages = {A33},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201322068},
  abstract = {We present the first public version (v0.2) of the open-source and community-developed Python package, Astropy. This package provides core astronomy-related functionality to the community, including support for domain-specific file formats such as flexible image transport system (FITS) files, Virtual Observatory (VO) tables, and common ASCII table formats, unit and physical quantity conversions, physical constants specific to astronomy, celestial coordinate and time transformations, world coordinate system (WCS) support, generalized containers for representing gridded as well as tabular data, and a framework for cosmological transformations and conversions. Significant functionality is under activedevelopment, such as a model fitting framework, VO client and server tools, and aperture and point spread function (PSF)
photometry tools. The core development team is actively making additions and enhancements to the current code base, and we encourage anyone interested to participate in the development of future Astropy versions.},
  file = {/Users/Oliver/Zotero/storage/QGLEY4BD/Astropy Collaboration et al. - 2013 - Astropy A community Python package for astronomy.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {methods: data analysis,methods: miscellaneous,virtual observatory tools}
}

@article{astropycollaboration+2018,
  title = {The {{Astropy Project}}: {{Building}} an {{Open}}-Science {{Project}} and {{Status}} of the v2.0 {{Core Package}}},
  shorttitle = {The {{Astropy Project}}},
  author = {{Astropy Collaboration} and {Price-Whelan}, A. M. and Sip{\H o}cz, B. M. and G{\"u}nther, H. M. and Lim, P. L. and Crawford, S. M. and Conseil, S. and Shupe, D. L. and Craig, M. W. and Dencheva, N. and Ginsburg, A. and VanderPlas, J. T. and Bradley, L. D. and {P{\'e}rez-Su{\'a}rez}, D. and {de Val-Borro}, M. and Aldcroft, T. L. and Cruz, K. L. and Robitaille, T. P. and Tollerud, E. J. and Ardelean, C. and Babej, T. and Bach, Y. P. and Bachetti, M. and Bakanov, A. V. and Bamford, S. P. and Barentsen, G. and Barmby, P. and Baumbach, A. and Berry, K. L. and Biscani, F. and Boquien, M. and Bostroem, K. A. and Bouma, L. G. and Brammer, G. B. and Bray, E. M. and Breytenbach, H. and Buddelmeijer, H. and Burke, D. J. and Calderone, G. and Cano Rodr{\'i}guez, J. L. and Cara, M. and Cardoso, J. V. M. and Cheedella, S. and Copin, Y. and Corrales, L. and Crichton, D. and D'Avella, D. and Deil, C. and Depagne, {\'E}. and Dietrich, J. P. and Donath, A. and Droettboom, M. and Earl, N. and Erben, T. and Fabbro, S. and Ferreira, L. A. and Finethy, T. and Fox, R. T. and Garrison, L. H. and Gibbons, S. L. J. and Goldstein, D. A. and Gommers, R. and Greco, J. P. and Greenfield, P. and Groener, A. M. and Grollier, F. and Hagen, A. and Hirst, P. and Homeier, D. and Horton, A. J. and Hosseinzadeh, G. and Hu, L. and Hunkeler, J. S. and Ivezi{\'c}, {\v Z}. and Jain, A. and Jenness, T. and Kanarek, G. and Kendrew, S. and Kern, N. S. and Kerzendorf, W. E. and Khvalko, A. and King, J. and Kirkby, D. and Kulkarni, A. M. and Kumar, A. and Lee, A. and Lenz, D. and Littlefair, S. P. and Ma, Z. and Macleod, D. M. and Mastropietro, M. and McCully, C. and Montagnac, S. and Morris, B. M. and Mueller, M. and Mumford, S. J. and Muna, D. and Murphy, N. A. and Nelson, S. and Nguyen, G. H. and Ninan, J. P. and N{\"o}the, M. and Ogaz, S. and Oh, S. and Parejko, J. K. and Parley, N. and Pascual, S. and Patil, R. and Patil, A. A. and Plunkett, A. L. and Prochaska, J. X. and Rastogi, T. and Reddy Janga, V. and Sabater, J. and Sakurikar, P. and Seifert, M. and Sherbert, L. E. and {Sherwood-Taylor}, H. and Shih, A. Y. and Sick, J. and Silbiger, M. T. and Singanamalla, S. and Singer, L. P. and Sladen, P. H. and Sooley, K. A. and Sornarajah, S. and Streicher, O. and Teuben, P. and Thomas, S. W. and Tremblay, G. R. and Turner, J. E. H. and Terr{\'o}n, V. and {van Kerkwijk}, M. H. and {de la Vega}, A. and Watkins, L. L. and Weaver, B. A. and Whitmore, J. B. and Woillez, J. and Zabalza, V. and {Astropy Contributors}},
  year = {2018},
  month = sep,
  volume = {156},
  pages = {123},
  issn = {0004-6256},
  doi = {10.3847/1538-3881/aabc4f},
  abstract = {The Astropy Project supports and fosters the development of open-source
and openly developed Python packages that provide commonly needed
functionality to the astronomical community. A key element of the
Astropy Project is the core package astropy, which serves as the
foundation for more specialized projects and packages. In this article,
we provide an overview of the organization of the Astropy project and
summarize key features in the core package, as of the recent major
release, version 2.0. We then describe the project infrastructure
designed to facilitate and support development for a broader ecosystem
of interoperable packages. We conclude with a future outlook of planned
new features and directions for the broader Astropy Project.

.},
  file = {/Users/Oliver/Zotero/storage/UMZBPMMS/Astropy Collaboration et al. - 2018 - The Astropy Project Building an Open-science Proj.pdf},
  journal = {The Astronomical Journal},
  keywords = {methods: data analysis,methods: miscellaneous,methods: statistical,reference systems}
}

@article{augustson+2017,
  title = {Dynamo {{Scaling Relationships}}},
  author = {Augustson, Kyle and Mathis, St{\'e}phane and Brun, Allan Sacha and Toomre, Juri},
  year = {2017},
  month = feb,
  abstract = {This paper provides a brief look at dynamo scaling relationships for the degree of equipartition between magnetic and kinetic energies. Two simple models are examined, where one that assumes magnetostrophy and another that includes the effects of inertia. These models are then compared to a suite of convective dynamo simulations of the convective core of a main-sequence B-type star and applied to its later evolutionary stages.},
  archivePrefix = {arXiv},
  eprint = {1702.04227},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/JKEGXWTT/Augustson et al. - 2017 - Dynamo Scaling Relationships.pdf;/Users/Oliver/Zotero/storage/SP6UMN23/1702.html},
  journal = {arXiv:1702.04227 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{augustson+mathis2018,
  title = {Perturbations of {{Stellar Oscillations}}: A {{General Magnetic Field}}},
  shorttitle = {Perturbations of {{Stellar Oscillations}}},
  author = {Augustson, K. C. and Mathis, S.},
  year = {2018},
  month = dec,
  pages = {113--116},
  address = {{eprint: arXiv:1811.04416}},
  abstract = {The purpose of this short paper is to give a summary of the derivation
of a perturbative method to assess the impact of an arbitrary 3D
magnetic field configuration, whose energy is everywhere small relative
to the gravitational binding energy, on the form and value of the
eigenfrequencies and eigenfunctions of stellar oscillations.},
  file = {/Users/Oliver/Zotero/storage/RH2L8RD8/Augustson and Mathis - 2018 - Perturbations of Stellar Oscillations a General M.pdf},
  keywords = {Magnetohydrodynamics (MHD),stars: magnetic fields,stars: oscillations,stars: rotation}
}

@article{baglin+2006,
  title = {The Seismology Programme of the {{CoRoT}} Space Mission},
  author = {Baglin, A. and Michel, E. and Auvergne, M. and Team, Corot},
  year = {2006},
  month = oct,
  volume = {624},
  pages = {34},
  abstract = {A powerful, streamlined new Astrophysics Data System},
  file = {/Users/Oliver/Zotero/storage/5UQNQ9MQ/Baglin et al. - 2006 - The seismology programme of the CoRoT space missio.pdf;/Users/Oliver/Zotero/storage/QDITHA4F/ui.adsabs.harvard.edu.html},
  journal = {Proceedings of SOHO 18/GONG 2006/HELAS I, Beyond the spherical Sun},
  language = {en}
}

@article{bahng+schwarzschild1963,
  title = {Hydrodynamic {{Oscillations}} in the {{Solar Chromosphere}}.},
  author = {Bahng, J. and Schwarzschild, M.},
  year = {1963},
  month = apr,
  volume = {137},
  pages = {901},
  issn = {0004-637X},
  doi = {10.1086/147566},
  abstract = {Abstract image available at:
http://adsabs.harvard.edu/abs/1963ApJ...137..901B},
  file = {/Users/Oliver/Zotero/storage/DABXV9DV/Bahng and Schwarzschild - 1963 - Hydrodynamic Oscillations in the Solar Chromospher.pdf},
  journal = {The Astrophysical Journal}
}

@article{bailer-jones+2018,
  title = {Estimating {{Distance}} from {{Parallaxes}}. {{IV}}. {{Distances}} to 1.33 {{Billion Stars}} in {{Gaia Data Release}} 2},
  author = {{Bailer-Jones}, C. a. L. and Rybizki, J. and Fouesneau, M. and Mantelet, G. and Andrae, R.},
  year = {2018},
  month = aug,
  volume = {156},
  pages = {58},
  doi = {10.3847/1538-3881/aacb21},
  abstract = {For the vast majority of stars in the second Gaia data release, reliable distances cannot be obtained by inverting the parallax. A correct inference procedure must instead be used to account for the nonlinearity of the transformation and the asymmetry of the resulting probability distribution. Here, we infer distances to essentially all 1.33 billion stars with parallaxes published in the second Gaia data release. This is done using a weak distance prior that varies smoothly as a function of Galactic longitude and latitude according to a Galaxy model. The irreducible uncertainty in the distance estimate is characterized by the lower and upper bounds of an asymmetric confidence interval. Although more precise distances can be estimated for a subset of the stars using additional data (such as photometry), our goal is to provide purely geometric distance estimates, independent of assumptions about the physical properties of, or interstellar extinction toward, individual stars. We analyze the characteristics of the catalog and validate it using clusters. The catalog can be queried using ADQL at \href{http://gaia.ari.uni-heidelberg.de/tap.html}{http://gaia.ari.uni-heidelberg.de/tap.html} (which also hosts the Gaia catalog) and downloaded from \href{http://www.mpia.de/~calj/gdr2_distances.html}{http://www.mpia.de/\textasciitilde calj/gdr2\_distances.html}.},
  file = {/Users/Oliver/Zotero/storage/L4QJXISG/Bailer-Jones et al. - 2018 - Estimating Distance from Parallaxes. IV. Distances.pdf;/Users/Oliver/Zotero/storage/PMTSHZUT/ui.adsabs.harvard.edu.html},
  journal = {The Astronomical Journal},
  language = {en},
  number = {2}
}

@article{bailer-jones2015,
  title = {Estimating {{Distances}} from {{Parallaxes}}},
  author = {{Bailer-Jones}, Coryn A. L.},
  year = {2015},
  month = oct,
  volume = {127},
  pages = {994},
  doi = {10.1086/683116},
  abstract = {Astrometric surveys such as Gaia and LSST will measure parallaxes for hundreds of millions of stars. Yet they will not measure a single distance. Rather, a distance must be estimated from a parallax. In this didactic article, I show that doing this is not trivial once the fractional parallax error is larger than about 20\%, which will be the case for about 80\% of stars in the Gaia catalogue. Estimating distances is an inference problem in which the use of prior assumptions is unavoidable. I investigate the properties and performance of various priors and examine their implications. A supposed uninformative uniform prior in distance is shown to give very poor distance estimates (large bias and variance). Any prior with a sharp cut-off at some distance has similar problems. The choice of prior depends on the information one has available - and is willing to use - concerning, for example, the survey and the Galaxy. I demonstrate that a simple prior which decreases asymptotically to zero at infinite distance has good performance, accommodates non-positive parallaxes, and does not require a bias correction.},
  file = {/Users/Oliver/Zotero/storage/RB59DX54/Bailer-Jones - 2015 - Estimating Distances from Parallaxes.pdf;/Users/Oliver/Zotero/storage/FBD66RUW/ui.adsabs.harvard.edu.html},
  journal = {Publications of the Astronomical Society of the Pacific},
  language = {en},
  number = {956}
}

@article{bailey+2016,
  title = {Solar {{Obliquity Induced}} by {{Planet Nine}}},
  author = {Bailey, Elizabeth and Batygin, Konstantin and Brown, Michael E.},
  year = {2016},
  month = nov,
  volume = {152},
  pages = {126},
  issn = {0004-6256},
  doi = {10.3847/0004-6256/152/5/126},
  abstract = {The six-degree obliquity of the Sun suggests that either an asymmetry was present in the solar system's formation environment, or an
external torque has misaligned the angular momentum vectors of the Sun and the planets. However, the exact origin of this obliquity remains an open question. Batygin \& Brown have recently shown that the physical alignment of distant Kuiper Belt orbits can be explained by a 5\{--\}20 \{m\}\textbackslash oplus planet on a distant, eccentric, and inclined orbit, with an approximate perihelion distance of {$\sim$}250 au. Using an analytic model for secular interactions between Planet Nine and the remaining giant planets, here, we show that a planet with similar parameters can naturally generate the observed obliquity as well as the specific pole position of the Sun's spin axis, from a nearly
aligned initial state. Thus, Planet Nine offers a testable explanation for the otherwise mysterious spin\textendash orbit misalignment of the solar system.},
  file = {/Users/Oliver/Zotero/storage/FUR8H6VQ/Bailey et al. - 2016 - Solar Obliquity Induced by Planet Nine.pdf},
  journal = {The Astronomical Journal},
  keywords = {AR 01/11/16,planets and satellites: dynamical evolution and stability}
}

@article{ball+gizon2017,
  title = {Surface-Effect Corrections for Oscillation Frequencies of Evolved Stars},
  author = {Ball, W. H. and Gizon, L.},
  year = {2017},
  month = feb,
  abstract = {Accurate modelling of solar-like oscillators requires that modelled mode frequencies are corrected for the systematic shift caused by improper modelling of the near-surface layers, known as the surface effect. ... We investigate how much additional uncertainty is introduced to stellar model parameters by our uncertainty about the functional form of the surface effect. At the same time, we test whether any of the parametrizations is significantly better or worse at modelling observed subgiants and low-luminosity red giants. We model six stars observed by Kepler that show clear mixed modes. We fix the input physics of the stellar models and vary the choice of surface correction ... Models using a solar-calibrated power law correction consistently fit the observations more poorly than the other four corrections. Models with the remaining four corrections generally fit ... about equally well, with the combined surface correction by Ball \& Gizon perhaps being marginally superior. The fits broadly agree on the model parameters within about the \$2\textbackslash sigma\$ uncertainties, with discrepancies between the modified Lorentzian and free power law corrections occasionally exceeding the \$3\textbackslash sigma\$ level. Relative to the best-fitting values, the total uncertainties on the masses, radii and ages of the stars are all less than 2, 1 and 6 per cent, respectively. A solar-calibrated power law ... appears unsuitable for use with more evolved solar-like oscillators. Among the remaining surface corrections, the uncertainty in the model parameters introduced by the surface effects is about twice as large as the uncertainty in the individual fits for these six stars. Though the fits are thus somewhat less certain because of our uncertainty of how to manage the surface effect, these results also demonstrate that it is feasible to model the individual mode frequencies of subgiants and low-luminosity red giants. ...},
  archivePrefix = {arXiv},
  eprint = {1702.02570},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/687BPS5T/Ball and Gizon - 2017 - Surface-effect corrections for oscillation frequen.pdf;/Users/Oliver/Zotero/storage/HFFAWDTN/1702.html},
  journal = {arXiv:1702.02570 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{ballot+2004,
  title = {Seismic Extraction of the Convective Extent in Solar-like Stars. {{The}} Observational Point of View},
  author = {Ballot, J. and {Turck-Chi{\`e}ze}, S. and Garc{\'i}a, R. A.},
  year = {2004},
  month = sep,
  volume = {423},
  pages = {1051--1061},
  issn = {0004-6361},
  doi = {10.1051/0004-6361:20035898},
  abstract = {Convection is the first manifestation of macroscopic motions in stars.
In the next decade, the extent of the external convective zone of
solar-like stars will have to be derived from the eigenfrequencies of
their low-degree ({$\mathscr{l}$}=0,1 and 2) acoustic modes. In this paper, we
compare different tracers of the base of the convective zone (BCZ) and
show that the second difference {$\delta$}2{$\nu$} stays simple and
well suited for analyzing real data. We suggest the use of
\textbackslash tilde\{t\}BCZ=(2{$<\Delta\nu>$})-1 -
\textbackslash tilde\{{$\tau\rbrace$}BCZ as a quasi-non-biased indicator of the BCZ
acoustic radius. The method is first checked on a long-time solar
observation with GOLF, then on shorter real observations by VIRGO and 10
000 simulated observations of solar-like stars. We present results for
different observational duration and stellar masses. The intrinsic error
due to the method on the convective extent is smaller than 1.5\% (in
units of stellar acoustic radius) for stars with masses between 0.9 and
1.3 M{$\odot$}. The limited observational interval adds a
supplementary uncertainty of about 1.6\% for a 150-day long simulated
observation. In this study, we have also analyzed the effects of
stochastic excitation and of non-continuous runs of shorter lengths. We
discuss how to take into account the variations in activity.

Appendix B is only available in electronic form at
http://www.edpsciences.org\vphantom\}},
  file = {/Users/Oliver/Zotero/storage/3FBFZNG8/Ballot et al. - 2004 - Seismic extraction of the convective extent in sol.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {convection,methods: data analysis,stars: interiors,stars: oscillations,Sun: helioseismology}
}

@article{ballot+2006,
  title = {Rotation Speed and Stellar Axis Inclination from p Modes: How {{CoRoT}} Would See Other Suns},
  shorttitle = {Rotation Speed and Stellar Axis Inclination from p Modes},
  author = {Ballot, J. and Garcia, R. A. and Lambert, P.},
  year = {2006},
  month = jul,
  volume = {369},
  pages = {1281--1286},
  issn = {0035-8711, 1365-2966},
  doi = {10.1111/j.1365-2966.2006.10375.x},
  abstract = {In the context of future space-based asteroseismic missions, we have studied the problem of extracting the rotation speed and the rotation-axis inclination of solar-like stars from the expected data. We have focused on slow rotators (at most twice solar rotation speed), first, because they constitute the most difficult case and, secondly, because some of the Convection Rotation and planetary Transits (CoRoT) main targets are expected to have slow rotation rates. Our study of the likelihood function has shown a correlation between the estimates of inclination of the rotation axis i and the rotational splitting {$\delta\nu$} of the star. By using the parameters, i and {$\delta\nu$} = {$\delta\nu$} sin i, we propose and discuss new fitting strategies. Monte Carlo simulations have shown that we can extract a mean splitting and the rotation-axis inclination down to solar rotation rates. However, at the solar rotation rate we are not able to correctly recover the angle i, although we are still able to measure a correct {$\delta\nu$} with a dispersion less than 40 nHz.},
  file = {/Users/Oliver/Zotero/storage/HAA56NJK/Ballot et al. - 2006 - Rotation speed and stellar axis inclination from p.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {3}
}

@article{ballot+2008,
  title = {Effect of the Stellar Inclination Angle upon Theoretical Errors of L=1 P-Mode Parameters},
  author = {Ballot, J. and Appourchaux, T. and Toutain, T.},
  year = {2008},
  month = jun,
  volume = {329},
  pages = {558},
  doi = {10.1002/asna.200710996},
  abstract = {The asteroseismic observations provided by current and future missions like CoRoT or Kepler will have a quality closer to those obtained for the Sun. In this context, tools and methods developed for helioseismology can be applied to other stars. In this paper, we focus on solar-like oscillations of stars with an unknown rotation axis inclination and study, by means of maximum-likelihood estimation, the errors on the determination of l=1 p-mode parameters.},
  file = {/Users/Oliver/Zotero/storage/E2RA3MTC/Ballot et al. - 2008 - Effect of the stellar inclination angle upon theor.pdf;/Users/Oliver/Zotero/storage/RNMKVPBE/ui.adsabs.harvard.edu.html},
  journal = {Astronomische Nachrichten},
  language = {en},
  number = {5}
}

@article{ballot+2008a,
  title = {On Deriving P-Mode Parameters for Inclined Solar-like Stars},
  author = {Ballot, J. and Appourchaux, T. and Toutain, T. and Guittet, M.},
  year = {2008},
  month = aug,
  volume = {486},
  pages = {867--875},
  issn = {0004-6361, 1432-0746},
  doi = {10.1051/0004-6361:20079343},
  abstract = {Thanks to their high quality, new and upcoming asteroseismic observations - with CoRoT, Kepler, and from the ground... - can benefit from the experience gained with helioseismology. We focus in this paper on solar-like oscillations, for which the inclination of the rotation axis is unknown. We present a theoretical study of the errors of p-mode parameters determined by means of a maximum-likelihood estimator, and we also analyze correlations and biases. We have used different, complementary approaches: we have performed either semi-analytical computation of the Hessian matrix, fitting of single mean profiles, or Monte Carlo simulations. We give first analytical approximations for the errors of frequency, inclination and rotational splitting. The determination of the inclination is very challenging for the common case of slow rotators (like the Sun), making difficult the determination of a reliable rotational splitting. Moreover, due to the numerous correlations, biases - more or less significant - can appear in the determination of various parameters in the case of bad inclination fittings, especially when a locking at 90 degrees occurs. This issue concerning inclination locking is also discussed. Nevertheless, the central frequency and some derived parameters such as the total power of the mode are free of such biases.},
  archivePrefix = {arXiv},
  eprint = {0803.0885},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/JIDJ75A2/Ballot et al. - 2008 - On deriving p-mode parameters for inclined solar-l.pdf;/Users/Oliver/Zotero/storage/CV4JJAIC/0803.html},
  journal = {Astronomy \& Astrophysics},
  keywords = {Astrophysics},
  number = {3}
}

@article{banyai+2013,
  title = {Variability of {{M}} Giant Stars Based on {{Kepler}} Photometry: General Characteristics},
  shorttitle = {Variability of {{M}} Giant Stars Based on {{Kepler}} Photometry},
  author = {Banyai, E. and Kiss, L. L. and Bedding, T. R. and Bellamy, B. and Benko, J. M. and Bodi, A. and Callingham, J. R. and Compton, D. and Csanyi, I. and Derekas, A. and Dorval, J. and Huber, D. and Shrier, O. and Simon, A. E. and Stello, D. and Szabo, G. M. and Szabo, R. and Szatmary, K.},
  year = {2013},
  month = dec,
  volume = {436},
  pages = {1576--1587},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stt1685},
  file = {/Users/Oliver/Zotero/storage/PUN29GWC/stt1685.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {2}
}

@article{barnabe+2017,
  title = {Confinement of the Solar Tachocline by a Cyclic Dynamo Magnetic Field},
  author = {Barnab{\'e}, R. and Strugarek, A. and Charbonneau, P. and Brun, A. S. and Zahn, J.-P.},
  year = {2017},
  month = mar,
  abstract = {The surprising thinness of the solar tachocline is still not understood with certainty today. Among the numerous possible scenarios suggested to explain its radial confinement, one hypothesis is based on Maxwell stresses that are exerted by the cyclic dynamo magnetic field of the Sun penetrating over a skin depth below the turbulent convection zone. Our goal is to assess under which conditions (turbulence level in the tachocline, strength of the dynamo-generated field, spreading mechanism) this scenario can be realized in the solar tachocline. We develop a simplified 1D model of the upper tachocline under the influence of an oscillating magnetic field imposed from above. The turbulent transport is parametrized with enhanced turbulent diffusion (or anti-diffusion) coefficients. Two main processes that thicken the tachocline are considered; either turbulent viscous spreading or radiative spreading. An extensive parameter study is carried out to establish the physical parameter regimes under which magnetic confinement of the tachocline that is due to a surface dynamo field can be realized. We have explored a large range of magnetic field amplitudes, viscosities, ohmic diffusivities and thermal diffusivities. We find that, for large but still realistic magnetic field strengths, the differential rotation can be suppressed in the upper radiative zone (and hence the tachocline confined) if weak turbulence is present (with an enhanced ohmic diffusivity of \$\textbackslash eta {$>$} 10\^\{7-8\} \textbackslash, cm\^2/s\$), even in the presence of radiative spreading. Our results show that a dynamo magnetic field can, in the presence of weak turbulence, prevent the inward burrowing of a tachocline subject to viscous diffusion or radiative spreading.},
  archivePrefix = {arXiv},
  eprint = {1703.02374},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/JS4ZSQV9/Barnabé et al. - 2017 - Confinement of the solar tachocline by a cyclic dy.pdf;/Users/Oliver/Zotero/storage/8TCGFCN8/1703.html},
  journal = {arXiv:1703.02374 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{barnes+2015,
  title = {A Color-Period Diagram for the Open Cluster {{M}} 48 ({{NGC}} 2548), and Its Rotational Age},
  author = {Barnes, Sydney A. and Weingrill, Joerg and Granzer, Thomas and Spada, Federico and Strassmeier, Klaus G.},
  year = {2015},
  month = nov,
  volume = {583},
  pages = {A73},
  doi = {10.1051/0004-6361/201526129},
  abstract = {Rotation periods are increasingly being used to derive ages for cool single field stars. Such ages are based on an empirical understanding of how cool stars spin down, acquired by constructing color-period diagrams (CPDs) for a series of open clusters. Our main aims here are to construct a CPD for M 48, to compare this with other clusters of similar age to check for consistency, and to derive a rotational age for M 48 using gyrochronology. We monitored M 48 photometrically for over 2 months with AIP's STELLA I 1.2 m telescope and the WiFSIP 4K imager in Tenerife. Light curves with 3 mmag precision for bright (V \textasciitilde{} 14 mag) stars were produced and then analysed to provide rotation periods. A cluster CPD has then been constructed. We report 62 rotation periods for cool stars in M 48. The CPD displays a clear slow/I-sequence of rotating stars, similar to those seen in the 625 Myr-old Hyades and 590 Myr-old Praesepe clusters, and below both, confirming that M 48 is younger. A similar comparison with the 250 Myr-old M 34 cluster shows that M 48 is older and does not possess any fast/C-sequence G or early K stars like those in M 34, although relatively fast rotators do seem to be present among the late-K and M stars. A more detailed comparison of the CPD with rotational evolution models shows that the cluster stars have a mean age of 450 Myr, and its (rotating) stars can be individually dated to {$\pm$} 117 Myr (26\%). Much of this uncertainty stems from intrinsic astrophysical spread in initial periods, and almost all stars are consistent with a single age of 450 Myr. The gyro-age of M 48 as a whole is 450 {$\pm$} 50 Myr, in agreement with the previously determined isochrone age of 400 {$\pm$} 100 Myr. Based on data obtained with the STELLA robotic telescopes in Tenerife, an AIP facility jointly operated by AIP and IAC; this paper presents results for the STELLA Open Cluster Survey (SOCS).Appendices A and B are available in electronic form at \href{http://www.aanda.org/10.1051/0004-6361/201526129/olm}{http://www.aanda.org}The cluster photometry table is only available at the CDS via anonymous ftp to \href{http://cdsarc.u-strasbg.fr}{http://cdsarc.u-strasbg.fr} (ftp://130.79.128.5) or via \href{http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/583/A73}{http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/583/A73}},
  file = {/Users/Oliver/Zotero/storage/WH87NLXG/Barnes et al. - 2015 - A color-period diagram for the open cluster M 48 (.pdf;/Users/Oliver/Zotero/storage/GXE3GFYH/abstract.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{barnes+2016,
  title = {Rotation {{Periods}} for {{Cool Stars}} in the 4 {{Gyr}} Old {{Open Cluster M67}}, {{The Solar}}-{{Stellar Connection}}, and the {{Applicability}} of {{Gyrochronology}} to at Least {{Solar Age}}},
  author = {Barnes, Sydney A. and Weingrill, Joerg and Fritzewski, Dario and Strassmeier, Klaus G. and Platais, Imants},
  year = {2016},
  month = may,
  volume = {823},
  pages = {16},
  doi = {10.3847/0004-637X/823/1/16},
  abstract = {We report rotation periods for 20 cool (FGK) main sequence member stars of the 4 Gyr-old open cluster M67 (=NGC 2682), obtained by analyzing data from Campaign 5 of the K2 mission with the Kepler Space Telescope. The rotation periods delineate a sequence in the color-period diagram (CPD) of increasing period with redder color. This sequence represents a cross-section at the cluster age of the surface P = P(t, M), suggested in prior work to extend to at least solar age. The current Sun is located marginally (approximately 1{$\sigma$}) above M67 in the CPD, as its relative age leads us to expect, and lies on the P = P(t, M) surface to within measurement precision. We therefore conclude that the solar rotation rate is normal as compared with cluster stars, a fact that strengthens the solar-stellar connection. The agreement between the M67 rotation period measurements and prior predictions further implies that rotation periods, especially when coupled with appropriate supporting work such as spectroscopy, can provide reliable ages via gyrochronology for other similar FGK dwarfs from the early main sequence to solar age and likely until the main sequence turnoff. The M67 rotators have a rotational age of 4.2 Gyr with a standard deviation of 0.7 Gyr, implying that similar field stars can be age-dated to precisions of{\~ }17\%. The rotational age of the M67 cluster as a whole is therefore 4.2 Gyr, but with a lower (averaged) uncertainty of 0.2 Gyr.},
  file = {/Users/Oliver/Zotero/storage/UL3J2K6C/Barnes et al. - 2016 - Rotation Periods for Cool Stars in the 4 Gyr old O.pdf;/Users/Oliver/Zotero/storage/99BNSW7W/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{barnes+2016a,
  title = {Some Aspects of Cool Main Sequence Star Ages Derived from Stellar Rotation (Gyrochronology)},
  author = {Barnes, S. A. and Spada, F. and Weingrill, J.},
  year = {2016},
  month = sep,
  volume = {337},
  pages = {810},
  doi = {10.1002/asna.201612377},
  abstract = {Rotation periods for cool stars can be measured with good precision by monitoring starspot light modulation. Observations have shown that the rotation periods of dwarf stars of roughly solar metallicity have such systematic dependencies on stellar age and mass that they can be used to derive reliable ages, a procedure called gyrochronology. We review the method and show illustrative cases, including recent ground- and space-based data. The age uncertainties approach 10 \% in the best cases, making them a valuable complement to, and constraint on, asteroseismic or other ages. Edited, updated, and refereed version of a presentation at the WE-Heraeus-Seminar in Bad Honnef, Germany: Reconstructing the Milky Way's History: Spectroscopic Surveys, Asteroseismology and Chemodynamical Models},
  file = {/Users/Oliver/Zotero/storage/WIBLE3ER/Barnes et al. - 2016 - Some aspects of cool main sequence star ages deriv.pdf;/Users/Oliver/Zotero/storage/2XZQAN7Q/abstract.html},
  journal = {Astronomische Nachrichten},
  language = {en},
  number = {8-9}
}

@article{barnes2003,
  title = {On the {{Rotational Evolution}} of {{Solar}}- and {{Late}}-{{Type Stars}}, {{Its Magnetic Origins}}, and the {{Possibility}} of {{Stellar Gyrochronology}}},
  author = {Barnes, Sydney A.},
  year = {2003},
  month = mar,
  volume = {586},
  pages = {464--479},
  issn = {0004-637X},
  doi = {10.1086/367639},
  abstract = {We propose a simple interpretation of the rotation period data for
solar- and late-type stars. The open cluster and Mount Wilson star
observations suggest that rotating stars lie primarily on two sequences,
initially called I and C. Some stars lie in the intervening gap. These
sequences, and the fractional numbers of stars on each sequence, evolve
systematically with cluster age, enabling us to construct crude
rotational isochrones allowing ``stellar gyrochronology,'' a procedure,
on improvement, likely to yield ages for individual field stars. The age
and color dependences of the sequences allow the identification of the
underlying mechanism, which appears to be primarily magnetic. The
majority of solar- and late-type stars possess a dominant Sun-like, or
interface, magnetic field, which connects the convective envelope to
both the radiative interior of the star and the exterior, where winds
can drain off angular momentum. These stars spin down Skumanich style.
An age-decreasing fraction of young G, K, and M stars, which are rapid
rotators, possess only a convective field, which is not only inefficient
in depleting angular momentum but also incapable of coupling the surface
convection zone to the inner radiative zone, so that only the outer zone
is spun down, and on an exponential timescale. These stars do not yet
possess large-scale dynamos. The large-scale magnetic field associated
with the dynamo, apparently created by the shear between the decoupled
radiative and convective zones, (re)couples the convective and radiative
zones and drives a star from the convective to the interface sequence
through the gap on a timescale that increases as stellar mass decreases.
Fully convective stars do not possess such an interface, cannot generate
an interface dynamo, and hence can never make such a transition.
Helioseismic results for the present-day Sun agree with this scheme,
which also explains the rotational bimodality observed by Herbst and
collaborators among pre-main-sequence stars and the termination of this
bimodality when stars become fully convective. This paradigm also
provides a new basis for understanding stellar X-ray and chromospheric
activity, light-element abundances, and perhaps other stellar phenomena
that depend on rotation.

This is Paper 13 of the WIYN Open Cluster Study (WOCS).},
  file = {/Users/Oliver/Zotero/storage/3JWPLF93/Barnes - 2003 - On the Rotational Evolution of Solar- and Late-Typ.pdf},
  journal = {The Astrophysical Journal},
  keywords = {Galaxy: Open Clusters and Associations: General,Stars: Evolution,Stars: Interiors,Stars: Late-Type,Stars: Magnetic Fields,Stars: Rotation}
}

@article{barnes2007,
  title = {Ages for {{Illustrative Field Stars Using Gyrochronology}}: {{Viability}}, {{Limitations}}, and {{Errors}}},
  shorttitle = {Ages for {{Illustrative Field Stars Using Gyrochronology}}},
  author = {Barnes, Sydney A.},
  year = {2007},
  month = nov,
  volume = {669},
  pages = {1167},
  doi = {10.1086/519295},
  abstract = {We here develop an improved way of using a rotating star as a clock, set it using the Sun,

repository: sandorkruk/malatium

repo_name: sandorkruk/malatium