text:
. The important, typically non-adiabatic, modal components of the surface effect are not included in the present analysis, but relegated to future papers. Evaluating the structural surface effect at the frequency of maximum mode amplitude, \$\textbackslash nu\_\{\textbackslash rm max\}\$, we find shifts from \$\textbackslash delta\textbackslash nu\$=-0.8 microHz for giants at \$\textbackslash log g\$=2.2 to -35 microHz for a (\$T\_\{\textbackslash rm eff\}=6901\$ K, \$\textbackslash log g\$=4.29) dwarf. The fractional effect \$\textbackslash delta\textbackslash nu(\textbackslash nu\_\{\textbackslash rm max\})/\textbackslash nu\_\{\textbackslash rm max\}\$, ranges from -0.1\% for a cool dwarf (4185 K, 4.74) to -6\% for a warm giant (4962 K, 2.20).},
  archivePrefix = {arXiv},
  eprint = {1611.02638},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/HSZASHJ2/Trampedach et al. - 2016 - The asteroseismic surface effect from a grid of 3D.pdf;/Users/Oliver/Zotero/storage/8QU9MS52/1611.html},
  journal = {arXiv:1611.02638 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{triana+2017,
  title = {Internal Rotation of 13 Low-Mass Low-Luminosity Red Giants in the {{Kepler}} Field},
  author = {Triana, Santiago Andr{\'e}s and Corsaro, Enrico and De Ridder, Joris and Bonanno, Alfio and Hern{\'a}ndez, Fernando P{\'e}rez and Garc{\'i}a, Rafael},
  year = {2017},
  month = feb,
  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.},
  archivePrefix = {arXiv},
  eprint = {1702.07910},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/UVXMBCQN/Triana et al. - 2017 - Internal rotation of 13 low-mass low-luminosity re.pdf;/Users/Oliver/Zotero/storage/KQRBVG63/1702.html},
  journal = {arXiv:1702.07910 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{turck-chieze+1997,
  title = {First {{View}} of the {{Solar Core}} from {{GOLF Acoustic Modes}}},
  author = {{Turck-Chi{\`e}ze}, S. and Basu, S. and Brun, A. S. and {Christensen-Dalsgaard}, J. and {Eff-Darwich}, A. and Lopes, I. and P{\'e}rez Hern{\'a}ndez, F. and Berthomieu, G. and Provost, J. and Ulrich, R. K. and Baudin, F. and Boumier, P. and Charra, J. and Gabriel, A. H. and Garcia, R. A. and Grec, G. and Renaud, C. and Robillot, J. M. and Roca Cort{\'e}s, T.},
  year = {1997},
  month = oct,
  volume = {175},
  pages = {247--265},
  issn = {0038-0938},
  doi = {10.1023/A:1004992727541},
  abstract = {After 8 months of nearly continuous measurements the GOLF instrument, aboard SOHO, has detected acoustic mode frequencies of more than 100 modes, extending from 1.4 mHz to 4.9 mHz. In this paper, we compare these results with the best available predictions coming from solar models. To verify the quality of the data, we examine the asymptotic seismic parameters; this confirms the improvements achieved in solar models during the last decade.},
  journal = {Solar Physics}
}

@article{turck-chieze+2001,
  title = {Solar {{Neutrino Emission Deduced}} from a {{Seismic Model}}},
  author = {{Turck-Chi{\`e}ze}, S. and Couvidat, S. and Kosovichev, A. G. and Gabriel, A. H. and Berthomieu, G. and Brun, A. S. and {Christensen-Dalsgaard}, J. and Garc{\'i}a, R. A. and Gough, D. O. and Provost, J. and {Roca-Cortes}, T. and Roxburgh, I. W. and Ulrich, R. K.},
  year = {2001},
  month = jul,
  volume = {555},
  pages = {L69-L73},
  issn = {0004-637X},
  doi = {10.1086/321726},
  abstract = {Three helioseismic instruments on the Solar and Heliospheric Observatory have observed the Sun almost continuously since early 1996. This has led to detailed study of the biases induced by the instruments that measure intensity or Doppler velocity variation. Photospheric turbulence hardly influences the tiny signature of conditions in the energy-generating core in the low-order modes, which are therefore very informative. We use sound-speed and density profiles inferred from GOLF and MDI data including these modes, together with recent improvements to stellar model computations, to build a spherically symmetric seismically adjusted model in agreement with the observations. The model is in hydrostatic and thermal balance and produces the present observed luminosity. In constructing the model, we adopt the best physics available, although we adjust some fundamental ingredients, well within the commonly estimated errors, such as the p-p reaction rate (+1\%) and the heavy-element abundance (+3.5\%); we also examine the sensitivity of the density profile to the nuclear reaction rates. Then, we deduce the corresponding emitted neutrino fluxes and consequently demonstrate that it is unlikely that the deficit of the neutrino fluxes measured on Earth can be explained by a spherically symmetric classical model without neutrino flavor transitions. Finally, we discuss the limitations of our results and future developments.},
  file = {/Users/Oliver/Zotero/storage/TLZLHF82/Turck-Chièze et al. - 2001 - Solar Neutrino Emission Deduced from a Seismic Mod.pdf},
  journal = {The Astrophysical Journal Letters},
  keywords = {Neutrinos,Sun: Interior,Sun: Oscillations}
}

@article{turck-chieze+2004,
  title = {Looking for {{Gravity}}-{{Mode Multiplets}} with the {{GOLF Experiment}} Aboard {{SOHO}}},
  author = {{Turck-Chi{\`e}ze}, S. and Garc{\'i}a, R. A. and Couvidat, S. and Ulrich, R. K. and Bertello, L. and Varadi, F. and Kosovichev, A. G. and Gabriel, A. H. and Berthomieu, G. and Brun, A. S. and Lopes, I. and Pall{\'e}, P. and Provost, J. and Robillot, J. M. and Roca Cort{\'e}s, T.},
  year = {2004},
  month = mar,
  volume = {604},
  pages = {455--468},
  issn = {0004-637X},
  doi = {10.1086/381743},
  abstract = {This paper is focused on the search for low-amplitude solar gravity modes between 150 and 400 {$\mu$}Hz, corresponding to low-degree, low-order modes. It presents results based on an original strategy that looks for multiplets instead of single peaks, taking into consideration our knowledge of the solar interior from acoustic modes. Five years of quasi-continuous measurements collected with the helioseismic GOLF experiment aboard the SOHO spacecraft are analyzed. We use different power spectrum estimators and calculate confidence levels for the most significant peaks. This approach allows us to look for signals with velocities down to 2 mm s-1, not far from the limit of existing instruments aboard SOHO, amplitudes that have never been investigated up to now. We apply the method to series of 1290 days, beginning in 1996 April, near the solar cycle minimum. An automatic detection algorithm lists those peaks and multiplets that have a probability of more than 90\% of not being pure noise. The detected patterns are then followed in time, considering also series of 1768 and 2034 days, partly covering the solar cycle maximum. In the analyzed frequency range, the probability of detection of the multiplets does not increase with time as for very long lifetime modes. This is partly due to the observational conditions after 1998 October and the degradation of these observational conditions near the solar maximum, since these modes have a ``mixed'' character and probably behave as acoustic modes. Several structures retain our attention because of the presence of persistent peaks along the whole time span. These features may support the idea of an increase of the rotation in the inner core. There are good arguments for thinking that complementary observations up to the solar activity minimum in 2007 will be decisive for drawing conclusions on the presence or absence of gravity modes detected aboard the SOHO satellite.},
  file = {/Users/Oliver/Zotero/storage/98L8AC68/Turck-Chièze et al. - 2004 - Looking for Gravity-Mode Multiplets with the GOLF .pdf},
  journal = {The Astrophysical Journal},
  keywords = {Sun: Helioseismology,Sun: Interior,Sun: Oscillations}
}

@article{udalski2000,
  title = {The {{Optical Gravitational Lensing Experiment}}: {{Red Clump Stars}} as a {{Distance Indicator}}},
  shorttitle = {The {{Optical Gravitational Lensing Experiment}}},
  author = {Udalski, A.},
  year = {2000},
  month = mar,
  volume = {531},
  pages = {L25},
  doi = {10.1086/312513},
  abstract = {We present relation of the mean I-band brightness of red clump stars on metallicity. Red clump stars were proposed to be a very attractive standard candle for distance determination. The calibration is based on 284 nearby red giant stars whose high-quality spectra made it possible to determine accurate individual metal abundances. High-quality parallaxes ({$\sigma$}\textsubscript{{$\pi$}}/{$\pi\&$}lt;10\%) and photometry of these very bright stars come from Hipparcos measurements. Metallicity of the sample covers a large range: -0.6 dex\<[Fe/H]\<+0.2 dex. We find a weak dependence of the mean I-band brightness on metallicity (\textasciitilde 0.13 mag dex\textsuperscript{-1}). What is more important, the range of metallicity of the Hipparcos sample partially overlaps with metallicity of field giants in the LMC, thus making it possible to determine the distance to the LMC by almost direct comparison of brightness of the local Hipparcos red clump giants with that of LMC stars. Photometry of field red clump giants in nine low-extinction fields of the LMC halo collected during the OGLE II microlensing survey compared with the Hipparcos red clump stars data yields the distance modulus to the LMC: (m-M)\textsubscript{LMC}=18.24+/-0.08 mag. Based on observations obtained with the 1.3 m Warsaw telescope at the Las Campanas Observatory of the Carnegie Institution of Washington.},
  file = {/Users/Oliver/Zotero/storage/ZR56URQY/Udalski - 2000 - The Optical Gravitational Lensing Experiment Red .pdf;/Users/Oliver/Zotero/storage/8WDFK8HY/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{ulrich1970,
  title = {The {{Five}}-{{Minute Oscillations}} on the {{Solar Surface}}},
  author = {Ulrich, Roger K.},
  year = {1970},
  month = dec,
  volume = {162},
  pages = {993},
  issn = {0004-637X},
  doi = {10.1086/150731},
  abstract = {Abstract image available at:
http://adsabs.harvard.edu/abs/1970ApJ...162..993U},
  file = {/Users/Oliver/Zotero/storage/3P5J84FL/Ulrich - 1970 - The Five-Minute Oscillations on the Solar Surface.pdf},
  journal = {The Astrophysical Journal}
}

@article{ulrich1986,
  title = {Determination of {{Stellar Ages}} from {{Asteroseismology}}},
  author = {Ulrich, Roger K.},
  year = {1986},
  month = jul,
  volume = {306},
  pages = {L37},
  issn = {0004-637X},
  doi = {10.1086/184700},
  abstract = {This Letter shows that measurements of the stellar analog of the solar 5 minute oscillations can permit the determination of the radius and age of isolated stars. The key frequencies of oscillation correspond to pairs of modes differing by two in the degree of the spherical harmonic describing the angular dependence of the motion and by one in the overtone order of the modes. The frequency pairs are very nearly degenerate, and adequate frequency resolution will require a nearly unbroken time sequence extending over 15 days.},
  file = {/Users/Oliver/Zotero/storage/TTBMER59/Ulrich - 1986 - Determination of Stellar Ages from Asteroseismolog.pdf;/Users/Oliver/Zotero/storage/RPAQWAKM/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en}
}

@article{unno+1989,
  title = {Nonradial Oscillations of Stars},
  author = {Unno, Wasaburo and Osaki, Yoji and Ando, Hiroyasu and Saio, H. and Shibahashi, H.},
  year = {1989},
  abstract = {Not Available},
  journal = {Nonradial oscillations of stars, Tokyo: University of Tokyo Press, 1989, 2nd ed.}
}

@article{vandakurov1967,
  title = {The {{Frequency Distribution}} of {{Stellar Oscillations}}.},
  author = {Vandakurov, Yu. V.},
  year = {1967},
  volume = {44},
  pages = {786},
  issn = {0004-6299},
  abstract = {Not Available},
  journal = {Astronomicheskii Zhurnal}
}

@article{vanderburg+johnson2014,
  title = {A {{Technique}} for {{Extracting Highly Precise Photometry}} for the {{Two}}-{{Wheeled Kepler Mission}}},
  author = {Vanderburg, Andrew and Johnson, John Asher},
  year = {2014},
  month = oct,
  volume = {126},
  pages = {948--958},
  issn = {0004-6280},
  doi = {10.1086/678764},
  abstract = {The original Kepler mission achieved high photometric precision thanks
to ultrastable pointing enabled by use of four reaction wheels. The loss
of two of these reaction wheels reduced the telescope's ability to point
precisely for extended periods of time, and as a result, the photometric
precision has suffered. We present a technique for generating
photometric light curves from pixel-level data obtained with the
two-wheeled extended Kepler mission, K2. Our photometric technique
accounts for the nonuniform pixel response function of the Kepler
detectors by correlating flux measurements with the spacecraft's
pointing and removing the dependence. When we apply our technique to the
ensemble of stars observed during the Kepler Two-Wheel Concept
Engineering Test, we find improvements over raw K2 photometry by factors
of 2-5, with noise properties qualitatively similar to Kepler targets at
the same magnitudes. We find evidence that the improvement in
photometric precision depends on each target's position in the Kepler
field of view, with worst precision near the edges of the field.
Overall, this technique restores the median-attainable photometric
precision within a factor of two of the original Kepler photometric
precision for targets ranging from 10th to 15th magnitude in the Kepler
bandpass, peaking with a median precision within 35\% to that of Kepler
for stars between 12th and 13th magnitude in the Kepler bandpass.},
  file = {/Users/Oliver/Zotero/storage/ZJU5CW22/Vanderburg and Johnson - 2014 - A Technique for Extracting Highly Precise Photomet.pdf},
  journal = {Publications of the Astronomical Society of the Pacific},
  keywords = {C3,Notes}
}

@article{vanderplas+2012,
  title = {Introduction to {{astroML}}: {{Machine}} Learning for Astrophysics},
  shorttitle = {Introduction to {{astroML}}},
  author = {VanderPlas, J. and Connolly, A. J. and Ivezic, Z. and Gray, A.},
  year = {2012},
  month = oct,
  pages = {47--54},
  address = {{eprint: arXiv:1411.5039}},
  doi = {10.1109/CIDU.2012.6382200},
  abstract = {Astronomy and astrophysics are witnessing dramatic increases in data
volume as detectors, telescopes and computers become ever more powerful.
During the last decade, sky surveys across the electromagnetic spectrum
have collected hundreds of terabytes of astronomical data for hundreds
of millions of sources. Over the next decade, the data volume will enter
the petabyte domain, and provide accurate measurements for billions of
sources. Astronomy and physics students are not traditionally trained to
handle such voluminous and complex data sets. In this paper we describe
astroML; an initiative, based on Python and scikit-learn, to develop a
compendium of machine learning tools designed to address the statistical
needs of the next generation of students and astronomical surveys. We
introduce astroML and present a number of example applications that are
enabled by this package.},
  file = {/Users/Oliver/Zotero/storage/NQ26HGB8/VanderPlas et al. - 2012 - Introduction to astroML Machine learning for astr.pdf}
}

@article{vanderplas+ivezic2015,
  title = {Periodograms for {{Multiband Astronomical Time Series}}},
  author = {VanderPlas, Jacob T. and Ivezi{\'c}, {\v Z}eljko},
  year = {2015},
  month = oct,
  volume = {812},
  pages = {18},
  issn = {0004-637X},
  doi = {10.1088/0004-637X/812/1/18},
  abstract = {This paper introduces the multiband periodogram, a general extension of the well-known Lomb-Scargle approach for detecting periodic
signals in time-domain data. In addition to advantages of the
Lomb-Scargle method such as treatment of non-uniform sampling and heteroscedastic errors, the multiband periodogram significantly improves period finding for randomly sampled multiband light curves (e.g., Pan-STARRS, DES, and LSST). The light curves in each band are modeled as arbitrary truncated Fourier series, with the period and phase shared across all bands. The key aspect is the use of Tikhonov regularization which drives most of the variability into the so-called base model common to all bands, while fits for individual bands describe residuals relative to the base model and typically require lower-order Fourier series. This decrease in the effective model complexity is the main reason for improved performance. After a pedagogical development of the formalism of least-squares spectral analysis, which motivates the essential features of the multiband model, we use simulated light curves and randomly subsampled SDSS Stripe 82 data to demonstrate the
superiority of this method compared to other methods from the literature and find that this method will be able to efficiently determine the correct period in the majority of LSST's bright RR Lyrae stars
with as little as six months of LSST data, a vast improvement over the years of data reported to be required by previous studies. A Python implementation of this method, along with code to fully reproduce the results reported here, is available on GitHub.},
  file = {/Users/Oliver/Zotero/storage/ELFSHVMX/VanderPlas and Ivezić - 2015 - Periodograms for Multiband Astronomical Time Serie.pdf},
  journal = {The Astrophysical Journal},
  keywords = {methods: data analysis,methods: statistical,surveys}
}

@article{vanderplas2018,
  title = {Understanding the {{Lomb}}-{{Scargle Periodogram}}},
  author = {VanderPlas, Jacob T.},
  year = {2018},
  month = may,
  volume = {236},
  pages = {16},
  issn = {1538-4365},
  doi = {10.3847/1538-4365/aab766},
  abstract = {The Lomb-Scargle periodogram is a well-known algorithm for detecting and characterizing periodic signals in unevenly-sampled data. This paper presents a conceptual introduction to the Lomb-Scargle periodogram and important practical considerations for its use. Rather than a rigorous mathematical treatment, the goal of this paper is to build intuition about what assumptions are implicit in the use of the Lomb-Scargle periodogram and related estimators of periodicity, so as to motivate important practical considerations required in its proper application and interpretation.},
  archivePrefix = {arXiv},
  eprint = {1703.09824},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/L6HGANIC/VanderPlas - 2018 - Understanding the Lomb-Scargle Periodogram.pdf;/Users/Oliver/Zotero/storage/L6QRX9EY/1703.html},
  journal = {The Astrophysical Journal Supplement Series},
  keywords = {Astrophysics - Instrumentation and Methods for Astrophysics},
  number = {1}
}

@article{vanderwalt+2011,
  title = {The {{NumPy Array}}: {{A Structure}} for {{Efficient Numerical Computation}}},
  shorttitle = {The {{NumPy Array}}},
  author = {{van der Walt}, St{\'e}fan and Colbert, S. Chris and Varoquaux, Ga{\"e}l},
  year = {2011},
  month = mar,
  volume = {13},
  pages = {22--30},
  doi = {10.1109/MCSE.2011.37},
  abstract = {In the Python world, NumPy arrays are the standard representation for numerical data. Here, we show how these arrays enable efficient
implementation of numerical computations in a high-level language. Overall, three techniques are applied to improve performance:
vectorizing calculations, avoiding copying data in memory, and
minimizing operation counts. We first present the NumPy array structure, then show how to use it for efficient computation, and finally how to share array data with other libraries.},
  file = {/Users/Oliver/Zotero/storage/SBN8XU27/van der Walt et al. - 2011 - The NumPy Array A Structure for Efficient Numeric.pdf},
  journal = {Computing in Science and Engineering}
}

@article{vaneylen+2013,
  title = {Investigation of {{Systematic Effects}} in {{Kepler Data}}: {{Seasonal Variations}} in the {{Light Curve}} of {{HAT}}-{{P}}-7b},
  shorttitle = {Investigation of {{Systematic Effects}} in {{Kepler Data}}},
  author = {Van Eylen, V. and Lindholm Nielsen, M. and Hinrup, B. and Tingley, B. and Kjeldsen, H.},
  year = {2013},
  month = sep,
  volume = {774},
  pages = {L19},
  issn = {0004-637X},
  doi = {10.1088/2041-8205/774/2/L19},
  abstract = {With years of Kepler data currently available, the measurement of
variations in planetary transit depths over time can now be attempted.
To do so, it is of primary importance to understand which systematic
effects may affect the measurement of transits. We aim to measure the
stability of Kepler measurements over years of observations. We present
a study of the depth of about 500 transit events of the Hot Jupiter
HAT-P-7b, using 14 quarters (Q0-Q13) of data from the Kepler satellite.
We find a systematic variation in the depth of the primary transit,
related to quarters of data and recurring yearly. These seasonal
variations are about 1\%. Within seasons, we find no evidence for trends.
We speculate that the cause of the seasonal variations could be unknown
field crowding or instrumental artifacts. Our results show that care
must be taken when combining transits throughout different quarters of
Kepler data. Measuring the relative planetary radius of HAT-P-7b without
taking these systematic effects into account leads to unrealistically
low error estimates. This effect could be present in all Kepler targets.
If so, relative radius measurements of all Hot Jupiters to a precision
much better than 1\% are unrealistic.},
  file = {/Users/Oliver/Zotero/storage/KUH7ZD96/Van Eylen et al. - 2013 - Investigation of Systematic Effects in Kepler Data.pdf},
  journal = {The Astrophysical Journal Letters},
  keywords = {C3,Notes}
}

@article{vaneylen+2014,
  title = {What Asteroseismology Can Do for Exoplanets: {{Kepler}}-{{410A}} b Is a {{Small Neptune}} around a Bright Star, in an Eccentric Orbit Consistent with Low Obliquity},
  shorttitle = {What Asteroseismology Can Do for Exoplanets},
  author = {Van Eylen, Vincent and Lund, Mikkel N. and Aguirre, Victor Silva and Arentoft, Torben and Kjeldsen, Hans and Albrecht, Simon and Chaplin, William J. and Isaacson, Howard and Pedersen, May G. and {Jessen-Hansen}, Jens and Tingley, Brandon W. and {Christensen-Dalsgaard}, Joergen and Aerts, Conny and Campante, Tiago L. and Bryson, Stephen T.},
  year = {2014},
  month = jan,
  volume = {782},
  pages = {14},
  issn = {0004-637X, 1538-4357},
  doi = {10.1088/0004-637X/782/1/14},
  abstract = {We confirm the Kepler planet candidate Kepler-410b (KOI-42b) as a Neptune sized exoplanet on a 17.8 day, eccentric orbit around the bright (Kp = 9.4) star Kepler-410A. This is the third brightest confirmed planet host star in the Kepler field and one of the brightest hosts of all currently known transiting exoplanets. Kepler-410 consists of a blend between the fast rotating planet host star (Kepler-410A) and a fainter star (Kepler-410B), which has complicated the confirmation of the planetary candidate. Employing asteroseismology, using constraints from the transit light curve, adaptive optics and speckle images, and Spitzer transit observations, we demonstrate that the candidate can only be an exoplanet orbiting Kepler-410A. Via asteroseismology we determine the following stellar and planetary parameters with high precision; M\$\_\textbackslash star = 1.214 \textbackslash pm 0.033\$ M\$\_\textbackslash odot\$, R\$\_\textbackslash star = 1.352 \textbackslash pm 0.010\$ R\$\_\textbackslash odot\$, Age = \$2.76 \textbackslash pm 0.54\$ Gyr, planetary radius (\$2.838 \textbackslash pm 0.054\$ R\$\_\textbackslash oplus\$), and orbital eccentricity (\$0.17\^\{+0.07\}\_\{-0.06\}\$). In addition, rotational splitting of the pulsation modes allows for a measurement of Kepler-410A's inclination and rotation rate. Our measurement of an inclination of \$82.5\^\{+7.5\}\_\{-2.5\}\$ [\$\^\textbackslash circ\$] indicates a low obliquity in this system. Transit timing variations indicate the presence of at least one additional (non-transiting) planet in the system.},
  archivePrefix = {arXiv},
  eprint = {1312.4938},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/QN2RYLCU/Van Eylen et al. - 2014 - What asteroseismology can do for exoplanets Keple.pdf;/Users/Oliver/Zotero/storage/FY6S754W/1312.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  number = {1}
}

@article{vaneylen+2015,
  title = {What Asteroseismology Can Do for Exoplanets},
  author = {Van Eylen, Vincent and Lund, Mikkel N. and Aguirre, Victor Silva and Arentoft, Torben and Kjeldsen, Hans and Albrecht, Simon and Chaplin, William J. and Isaacson, Howard and Pedersen, May G. and {Jessen-Hansen}, Jens and Tingley, Brandon and {Christensen-Dalsgaard}, Joergen and Aerts, Conny and Campante, Tiago L. and Bryson, Steve T.},
  year = {2015},
  volume = {101},
  pages = {02005},
  issn = {2100-014X},
  doi = {10.1051/epjconf/201510102005},
  abstract = {We describe three useful applications of asteroseismology in the context of exoplanet science: (1) the detailed characterisation of exoplanet host stars; (2) the measurement of stellar inclinations; and (3) the determination of orbital eccentricity from transit duration making use of asteroseismic stellar densities. We do so using the example system Kepler-410 (Van Eylen et al. 2014). This is one of the brightest (V = 9.4) Kepler exoplanet host stars, containing a small (2.8 Rearth) transiting planet in a long orbit (17.8 days), and one or more additional non-transiting planets as indicated by transit timing variations. The validation of Kepler-410 (KOI-42) was complicated due to the presence of a companion star, and the planetary nature of the system was confirmed after analyzing a Spitzer transit observation as well as ground-based follow-up observations.},
  archivePrefix = {arXiv},
  eprint = {1412.4848},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/WRN73922/Van Eylen et al. - 2015 - What asteroseismology can do for exoplanets.pdf;/Users/Oliver/Zotero/storage/53XNICUN/1412.html},
  journal = {EPJ Web of Conferences},
  keywords = {C1}
}

@article{vaneylen+2017,
  title = {An Asteroseismic View of the Radius Valley: Stripped Cores, Not Born Rocky},
  shorttitle = {An Asteroseismic View of the Radius Valley},
  author = {Van Eylen, Vincent and Agentoft, Camilla and Lundkvist, Mia S. and Kjeldsen, Hans and Owen, James E. and Fulton, Benjamin J. and Petigura, Erik and Snellen, Ignas},
  year = {2017},
  month = oct,
  abstract = {Various theoretical models treating the effect of stellar irradiation on planetary envelopes predict the presence of a radius valley: i.e. a bimodal distribution of planet radii, with super-Earths and sub-Neptune planets separated by a valley at around \$\textbackslash approx 2\textasciitilde R\_\textbackslash oplus\$. Such a valley was observed recently, owing to an improvement in the precision of stellar, and therefore planetary radii. Here we investigate the presence, location and shape of such a valley using a small sample with highly accurate stellar parameters determined from asteroseismology, which includes 117 planets with a median uncertainty on the radius of 3.3\%. We detect a clear bimodal distribution, with super-Earths (\$\textbackslash approx 1.5\textasciitilde R\_\textbackslash oplus\$) and sub-Neptunes (\$\textbackslash approx 2.5\textasciitilde R\_\textbackslash oplus\$) separated by a deficiency around \$2\textasciitilde R\_\textbackslash oplus\$. We furthermore characterize the slope of the valley as a power law \$R \textbackslash propto P\^\textbackslash gamma\$ with \$\textbackslash gamma = \{-0.09\^\{+0.02\}\_\{-0.04\}\}\$. A negative slope is consistent with models of photo-evaporation, but not with the late formation of rocky planets in a gas-poor environment, which would lead to a slope of opposite sign. The exact location of the gap further points to planet cores consisting of a significant fraction of rocky material.},
  archivePrefix = {arXiv},
  eprint = {1710.05398},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/43GTMP5Q/Van Eylen et al. - 2017 - An asteroseismic view of the radius valley stripp.pdf;/Users/Oliver/Zotero/storage/J5ZDDJ9T/1710.html},
  journal = {arXiv:1710.05398 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics},
  primaryClass = {astro-ph}
}

@article{vaneylen+2018,
  title = {An Asteroseismic View of the Radius Valley: Stripped Cores, Not Born Rocky},
  shorttitle = {An Asteroseismic View of the Radius Valley},
  author = {Van Eylen, V. and Agentoft, Camilla and Lundkvist, M. S. and Kjeldsen, H. and Owen, J. E. and Fulton, B. J. and Petigura, E. and Snellen, I.},
  year = {2018},
  month = oct,
  volume = {479},
  pages = {4786},
  doi = {10.1093/mnras/sty1783},
  abstract = {Various theoretical models treating the effect of stellar irradiation on planetary envelopes predict the presence of a radius valley, i.e. a bimodal distribution of planet radii, with super-Earths and sub-Neptune planets separated by a valley at around \{{$\approx$} \} 2 R\_\textbackslash oplus. Such a valley has been observed recently, owing to an improvement in the precision of stellar and therefore planetary radii. Here, we investigate the presence, location, and shape of such a valley using a small sample with highly accurate stellar parameters determined from asteroseismology, which includes 117 planets with a median uncertainty on the radius of 3.3 per cent. We detect a clear bimodal distribution, with super-Earths (\{{$\approx$} \} 1.5 R\_\textbackslash oplus) and sub-Neptunes ({$\approx$}2.5 R\textsubscript{{$\oplus$}}) separated by a deficiency around 2 R\_\textbackslash oplus. We furthermore characterize the slope of the valley as a power law R{$\propto$}P\textsuperscript{{$\gamma$}} with {$\gamma$} = \{-0.09\^\{+0.02\}\_\{-0.04\}\}. A negative slope is consistent with models of photoevaporation, but not with the late formation of rocky planets in a gas-poor environment, which would lead to a slope of opposite sign. The exact location of the gap further points to planet cores consisting of a significant fraction of rocky material.},
  file = {/Users/Oliver/Zotero/storage/9LY4WHXW/Van Eylen et al. - 2018 - An asteroseismic view of the radius valley stripp.pdf;/Users/Oliver/Zotero/storage/GR8ILQRL/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {4}
}

@article{vaneylen+albrecht2015,
  title = {Eccentricity from Transit Photometry: Small Planets in {{Kepler}} Multi-Planet Systems Have Low Eccentricities},
  shorttitle = {Eccentricity from Transit Photometry},
  author = {Van Eylen, Vincent and Albrecht, Simon},
  year = {2015},
  month = jul,
  volume = {808},
  pages = {126},
  issn = {1538-4357},
  doi = {10.1088/0004-637X/808/2/126},
  abstract = {Solar system planets move on almost circular orbits. In strong contrast, many massive gas giant exoplanets travel on highly elliptical orbits, whereas the shape of the orbits of smaller, more terrestrial, exoplanets remained largely elusive. Knowing the eccentricity distribution in systems of small planets would be important as it holds information about the planet's formation and evolution, and influences its habitability. We make these measurements using photometry from the Kepler satellite and utilizing a method relying on Kepler's second law, which relates the duration of a planetary transit to its orbital eccentricity, if the stellar density is known. Our sample consists of 28 bright stars with precise asteroseismic density measurements. These stars host 74 planets with an average radius of 2.6 \$R\_\textbackslash oplus\$. We find that the eccentricity of planets in Kepler multi-planet systems is low and can be described by a Rayleigh distribution with \$\textbackslash sigma\$ = 0.049 \$\textbackslash pm\$ 0.013. This is in full agreement with solar system eccentricities, but in contrast to the eccentricity distributions previously derived for exoplanets from radial velocity studies. Our findings are helpful in identifying which planets are habitable because the location of the habitable zone depends on eccentricity, and to determine occurrence rates inferred for these planets because planets on circular orbits are less likely to transit. For measuring eccentricity it is crucial to detect and remove Transit Timing Variations (TTVs), and we present some previously unreported TTVs. Finally transit durations help distinguish between false positives and true planets and we use our measurements to confirm six new exoplanets.},
  archivePrefix = {arXiv},
  eprint = {1505.02814},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/RFHBV6ZQ/Van Eylen and Albrecht - 2015 - Eccentricity from transit photometry small planet.pdf;/Users/Oliver/Zotero/storage/ZZFDHVIV/1505.html},
  journal = {The Astrophysical Journal},
  keywords = {C3,CHECK},
  number = {2}
}

@article{vanhelshoecht+groenewegen2007,
  title = {K-Band Magnitude of the Red Clump as a Distance Indicator},
  author = {{van Helshoecht}, V. and Groenewegen, M. a. T.},
  year = {2007},
  month = feb,
  volume = {463},
  pages = {559},
  doi = {10.1051/0004-6361:20052721},
  abstract = {We have investigated how the K-band magnitude of the red clump [M\_K(RC)] depends on age and metallicity, using 2MASS infrared data for a sample of 24 open clusters with known distances. We show that a constant value of M\_K(RC)=-1.57 {$\pm$} 0.05 is a reasonable assumption to use in distance determinations for clusters with metallicity between -0.5 and +0.4 dex and age between 10\textsuperscript{8.5} and 10\textsuperscript{9.9} years. Figures 8 and 9 are available in electronic form at http://www.aanda.org},
  file = {/Users/Oliver/Zotero/storage/TKSUW9EY/van Helshoecht and Groenewegen - 2007 - K-band magnitude of the red clump as a distance in.pdf;/Users/Oliver/Zotero/storage/GC8W6JVG/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en},
  number = {2}
}

@article{vanhoey+2013,
  title = {Python Package for Model {{STructure ANalysis}} ({{pySTAN}})},
  author = {Van Hoey, Stijn and {van der Kwast}, Johannes and Nopens, Ingmar and Seuntjens, Piet},
  year = {2013},
  month = apr,
  volume = {15},
  pages = {EGU2013-10059},
  abstract = {The selection and identification of a suitable hydrological model structure is more than fitting parameters of a model structure to reproduce a measured hydrograph. The procedure is highly dependent on various criteria, i.e. the modelling objective, the characteristics and the scale of the system under investigation as well as the available data. Rigorous analysis of the candidate model structures is needed to support and objectify the selection of the most appropriate structure for a specific case (or eventually justify the use of a proposed ensemble of structures). This holds both in the situation of choosing between a limited set of different structures as well as in the framework of flexible model structures with interchangeable components. Many different methods to evaluate and analyse model structures exist. This leads to a sprawl of available methods, all characterized by different assumptions, changing conditions of application and various code implementations. Methods typically focus on optimization, sensitivity analysis or uncertainty analysis, with backgrounds from optimization, machine-learning or statistics amongst others. These methods also need an evaluation metric (objective function) to compare the model outcome with some observed data. However, for current methods described in literature, implementations are not always transparent and reproducible (if available at all). No standard procedures exist to share code and the popularity (and amount of applications) of the methods is sometimes more dependent on the availability than the merits of the method. Moreover, new implementations of existing methods are difficult to verify and the different theoretical backgrounds make it difficult for environmental scientists to decide about the usefulness of a specific method. A common and open framework with a large set of methods can support users in deciding about the most appropriate method. Hence, it enables to simultaneously apply and compare different methods on a fair basis. We developed and present pySTAN (python framework for STructure Analysis), a python package containing a set of functions for model structure evaluation to provide the analysis of (hydrological) model structures. A selected set of algorithms for optimization, uncertainty and sensitivity analysis is currently available, together with a set of evaluation (objective) functions and input distributions to sample from. The methods are implemented model-independent and the python language provides the wrapper functions to apply administer external model codes. Different objective functions can be considered simultaneously with both statistical metrics and more hydrology specific metrics. By using so-called reStructuredText (sphinx documentation generator) and Python documentation strings (docstrings), the generation of manual pages is semi-automated and a specific environment is available to enhance both the readability and transparency of the code. It thereby enables a larger group of users to apply and compare these methods and to extend the functionalities.},
  file = {/Users/Oliver/Zotero/storage/VSSJNGE2/Van Hoey et al. - 2013 - Python package for model STructure ANalysis (pySTA.pdf;/Users/Oliver/Zotero/storage/4JE5569C/ui.adsabs.harvard.edu.html},
  journal = {EGU General Assembly Conference Abstracts},
  language = {en}
}

@article{vanleeuwen2007,
  title = {Validation of the New {{Hipparcos}} Reduction},
  author = {{van Leeuwen}, F.},
  year = {2007},
  month = nov,
  volume = {474},
  pages = {653--664},
  issn = {0004-6361},
  doi = {10.1051/0004-6361:20078357},
  abstract = {Context: A new reduction of the astrometric data as produced by the Hipparcos mission has been published, claiming accuracies for nearly all stars brighter than magnitude Hp=8 to be better, by up to a factor 4, than in the original catalogue. \\
Aims: The new Hipparcos astrometric catalogue is checked for the quality of the data and the consistency of the formal errors as well as the possible presence of error correlations. The differences with the earlier publication are explained. \\
Methods: The internal errors are followed through the reduction process, and the external errors are investigated on the basis of a comparison with radio observations of a small selection of stars, and the distribution of negative parallaxes. Error correlation levels are investigated and the reduction by more than a factor 10 as obtained in the new catalogue is explained. \\
Results: The formal errors on the parallaxes for the new catalogue are confirmed. The presence of a small amount of additional noise, though unlikely, cannot be ruled out. \\
Conclusions: The new reduction of the Hipparcos astrometric data provides an improvement by a factor 2.2 in the total weight compared to the catalogue published in 1997, and provides much improved data for a wide range of studies on stellar luminosities and local galactic kinematics.},
  file = {/Users/Oliver/Zotero/storage/H3EWNB9D/van Leeuwen - 2007 - Validation of the new Hipparcos reduction.pdf;/Users/Oliver/Zotero/storage/R27J4VJ8/abstract.html},
  journal = {A\&A},
  language = {en},
  number = {2}
}

@article{vanon+ogilvie2016,
  title = {Zonal Flow Evolution and Overstability in Accretion Discs},
  author = {Vanon, Riccardo and Ogilvie, Gordon},
  year = {2016},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stw3232},
  abstract = {This work presents a linear analytical calculation on the stability and evolution of a compressible, viscous self-gravitating (SG) Keplerian disc with both horizontal thermal diffusion and a constant cooling timescale when an axisymmetric structure is present and freely evolving. The calculation makes use of the shearing sheet model and is carried out for a range of cooling times. Although the solutions to the inviscid problem with no cooling or diffusion are well known, it is non-trivial to predict the effect caused by the introduction of cooling and of small diffusivities; this work focuses on perturbations of intermediate wavelengths, therefore representing an extension to the classical stability analysis on thermal and viscous instabilities. For density wave modes the analysis can be simplified by means of a regular perturbation analysis; considering both shear and thermal diffusivities, the system is found to be overstable for intermediate and long wavelengths for values of the Toomre parameter \$Q \textbackslash lesssim 2\$; a non-SG instability is also detected for wavelengths \$\textbackslash gtrsim 18H\$, where \$H\$ is the disc scale height, as long as \$\textbackslash gamma \textbackslash lesssim 1.305\$. The regular perturbation analysis does not however hold for the entropy and potential vorticity slow modes as their ideal growth rates are degenerate. To understand their evolution, equations for the axisymmetric structure's amplitudes in these two quantities are analytically derived and their instability regions obtained. The instability appears boosted by increasing the value of the adiabatic index and of the Prandtl number, while it is quenched by efficient cooling.},
  archivePrefix = {arXiv},
  eprint = {1612.04326},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/RCBG8W25/Vanon and Ogilvie - 2016 - Zonal flow evolution and overstability in accretio.pdf;/Users/Oliver/Zotero/storage/7EB2K9Q9/1612.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics,Physics - Fluid Dynamics}
}

@article{vansaders+2016,
  title = {Weakened Magnetic Braking as the Origin of Anomalously Rapid Rotation in Old Field Stars},
  author = {{van Saders}, Jennifer L. and Ceillier, Tugdual and Metcalfe, Travis S. and Silva Aguirre, Victor and Pinsonneault, Marc H. and Garc{\'i}a, Rafael A. and Mathur, Savita and Davies, Guy R.},
  year = {2016},
  month = jan,
  volume = {529},
  pages = {181},
  doi = {10.1038/nature16168},
  abstract = {A knowledge of stellar ages is crucial for our understanding of many astrophysical phenomena, and yet ages can be difficult to determine. As they become older, stars lose mass and angular momentum, resulting in an observed slowdown in surface rotation. The technique of `gyrochronology' uses the rotation period of a star to calculate its age. However, stars of known age must be used for calibration, and, until recently, the approach was untested for old stars (older than 1\,gigayear, Gyr). Rotation periods are now known for stars in an open cluster of intermediate age (NGC 6819; 2.5\,Gyr old), and for old field stars whose ages have been determined with asteroseismology. The data for the cluster agree with previous period-age relations, but these relations fail to describe the asteroseismic sample. Here we report stellar evolutionary modelling, and confirm the presence of unexpectedly rapid rotation in stars that are more evolved than the Sun. We demonstrate that models that incorporate dramatically weakened magnetic braking for old stars can\textemdash unlike existing models\textemdash reproduce both the asteroseismic and the cluster data. Our findings might suggest a fundamental change in the nature of ageing stellar dynamos, with the Sun being close to the critical transition to much weaker magnetized winds. This weakened braking limits the diagnostic power of gyrochronology for those stars that are more than halfway through their main-sequence lifetimes.},
  file = {/Users/Oliver/Zotero/storage/IT867Q68/van Saders et al. - 2016 - Weakened magnetic braking as the origin of anomalo.pdf;/Users/Oliver/Zotero/storage/YT7NEI3Q/ui.adsabs.harvard.edu.html},
  journal = {Nature},
  keywords = {Core Gyrochronology},
  language = {en},
  number = {7585}
}

@article{vansaders+2019,
  title = {Forward {{Modeling}} of the {{Kepler Stellar Rotation Period Distribution}}: {{Interpreting Periods}} from {{Mixed}} and {{Biased Stellar Populations}}},
  shorttitle = {Forward {{Modeling}} of the {{Kepler Stellar Rotation Period Distribution}}},
  author = {{van Saders}, Jennifer L. and Pinsonneault, Marc H. and Barbieri, Mauro},
  year = {2019},
  month = feb,
  volume = {872},
  pages = {128},
  doi = {10.3847/1538-4357/aafafe},
  abstract = {Stellar surface rotation carries information about stellar parameters\textemdash particularly ages\textemdash and thus the large rotational data sets extracted from Kepler time series represent powerful probes of stellar populations. In this article, we address the challenge of interpreting such data sets with a forward-modeling exercise. We combine theoretical models of stellar rotation, a stellar population model for the galaxy, and prescriptions for observational bias to predict the rotation distribution in the Kepler field under standard ``vanilla'' assumptions. We arrive at two central conclusions: first, that standard braking models fail to reproduce the observed distribution at long periods, and second, that the interpretation of the period distribution is complicated by a mixture of evolutionary states and observational uncertainties. If we assume that the detectability of rotational signatures scales with the Rossby number, we can show that the observed period distribution contains an apparent ``Rossby edge'' at \{\{\{Ro\}\}\}\textsubscript{thresh}\vphantom\{\}=2.08, above which long-period, high Rossby number stars are either absent or undetected. This threshold suggests either that weakened magnetic braking is in operation in the full Kepler population or that stars undergo a transition in spottedness and activity. We discuss the observations necessary to disentangle these competing scenarios. Regardless of the physical origin of the edge, it biases the inferred age distributions, affecting stars older than {$\sim$}9 Gyr at \{T\}\textsubscript{eff}\vphantom\{\}=5100 \{\{K\}\}, older than {$\sim$} 4.2 \{Gyr\} at solar temperatures, and 1.5 \{Gyr\} at 6500 K. Below 5100 \{\{K\}\}, rotation periods should be viable age diagnostics in even the oldest stars in the population.},
  file = {/Users/Oliver/Zotero/storage/QKJBPPYG/van Saders et al. - 2019 - Forward Modeling of the Kepler Stellar Rotation Pe.pdf;/Users/Oliver/Zotero/storage/HUTEQTMA/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{vansaders+pinsonneault2013,
  title = {Fast {{Star}}, {{Slow Star}}; {{Old Star}}, {{Young Star}}: {{Subgiant Rotation}} as a {{Population}} and {{Stellar Physics Diagnostic}}},
  shorttitle = {Fast {{Star}}, {{Slow Star}}; {{Old Star}}, {{Young Star}}},
  author = {{van Saders}, Jennifer L. and Pinsonneault, Marc H.},
  year = {2013},
  month = oct,
  volume = {776},
  pages = {67},
  doi = {10.1088/0004-637X/776/2/67},
  abstract = {Stellar rotation is a strong function of both mass and evolutionary state. Missions such as Kepler and CoRoT provide tens of thousands of rotation periods, drawn from stellar populations that contain objects at a range of masses, ages, and evolutionary states. Given a set of reasonable starting conditions and a prescription for angular momentum loss, we address the expected range of rotation periods for cool field stellar populations (\textasciitilde 0.4-2.0 M \textsubscript{{$\Sun$}}). We find that cool stars fall into three distinct regimes in rotation. Rapid rotators with surface periods less than 10 days are either young low-mass main sequence (MS) stars, or higher mass subgiants which leave the MS with high rotation rates. Intermediate rotators (10-40 days) can be either cool MS dwarfs, suitable for gyrochronology, or crossing subgiants at a range of masses. Gyrochronology relations must therefore be applied cautiously, since there is an abundant population of subgiant contaminants. The slowest rotators, at periods greater than 40 days, are lower mass subgiants undergoing envelope expansion. We identify additional diagnostic uses of rotation periods. There exists a period-age relation for subgiants distinct from the MS period-age relations. There is also a period-radius relation that can be used as a constraint on the stellar radius, particularly in the interesting case of planet host stars. The high-mass/low-mass break in the rotation distribution on the MS persists onto the subgiant branch, and has potential as a diagnostic of stellar mass. Finally, this set of theoretical predictions can be compared to extensive datasets to motivate improved modeling.},
  file = {/Users/Oliver/Zotero/storage/Y2HAU6TY/van Saders and Pinsonneault - 2013 - Fast Star, Slow Star\; Old Star, Young Star Subgia.pdf;/Users/Oliver/Zotero/storage/VZ9I62LX/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  keywords = {Core Gyrochronology,Seismic rotation},
  language = {en},
  number = {2}
}

@article{verma+2017,
  title = {Seismic Measurement of the Locations of the Base of Convection Zone and Helium Ionization Zone for Stars in the \{\textbackslash it \vphantom\}{{Kepler}}\vphantom\{\} Seismic {{LEGACY}} Sample},
  author = {Verma, Kuldeep and Raodeo, Keyuri and Antia, H. M. and Mazumdar, Anwesh and Basu, Sarbani and Lund, Mikkel N. and Aguirre, V{\'i}ctor Silva},
  year = {2017},
  month = jan,
  abstract = {Acoustic glitches are regions inside a star where the sound speed or its derivatives change abruptly. These leave a small characteristic oscillatory signature in the stellar oscillation frequencies. With the precision achieved by \{\textbackslash it Kepler\} seismic data, it is now possible to extract these small amplitude oscillatory signatures, and infer the locations of the glitches. We perform glitch analysis for all the 66 stars in the \{\textbackslash it Kepler\} seismic LEGACY sample to derive the locations of the base of the envelope convection zone and the helium ionization zone. The signature from helium ionization zone is found to be robust for all stars in the sample, whereas the convection zone signature is found to be weak and problematic, particularly for relatively massive stars with large errorbars on the oscillation frequencies. We demonstrate that the helium glitch signature can be used to constrain the properties of the helium ionization layers and the helium abundance.},
  archivePrefix = {arXiv},
  eprint = {1701.08987},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/H8XMJV6E/Verma et al. - 2017 - Seismic measurement of the locations of the base o.pdf;/Users/Oliver/Zotero/storage/UAPMW9PH/1701.html},
  journal = {arXiv:1701.08987 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{verner+2006,
  title = {The Detectability of Signatures of Rapid Variation in Low-Degree Stellar p-Mode Oscillation Frequencies},
  author = {Verner, G. A. and Chaplin, W. J. and Elsworth, Y.},
  year = {2006},
  volume = {638},
  pages = {440},
  file = {/Users/Oliver/Zotero/storage/DSFXNUC6/pdf.pdf},
  journal = {The Astrophysical Journal},
  number = {1}
}

@article{verner+2011,
  title = {Global Asteroseismic Properties of Solar-like Oscillations Observed by {{Kepler}}: A Comparison of Complementary Analysis Methods},
  shorttitle = {Global Asteroseismic Properties of Solar-like Oscillations Observed by {{Kepler}}},
  author = {Verner, G. A. and Elsworth, Y. and Chaplin, W. J. and Campante, T. L. and Corsaro, E. and Gaulme, P. and Hekker, S. and Huber, D. and Karoff, C. and Mathur, S. and Mosser, B. and Appourchaux, T. and Ballot, J. and Bedding, T. R. and Bonanno, A. and Broomhall, A.-M. and Garc{\'i}a, R. A. and Handberg, R. and New, R. and Stello, D. and R{\'e}gulo, C. and Roxburgh, I. W. and Salabert, D. and White, T. R. and Caldwell, D. A. and Christiansen, J. L. and Fanelli, M. N.},
  year = {2011},
  month = aug,
  volume = {415},
  pages = {3539},
  doi = {10.1111/j.1365-2966.2011.18968.x},
  abstract = {We present the asteroseismic analysis of 1948 F-, G- and K-type main-sequence and subgiant stars observed by the National Aeronautics and Space Administration Kepler mission. We detect and characterize solar-like oscillations in 642 of these stars. This represents the largest cohort of main-sequence and subgiant solar-like oscillators observed to date. The photometric observations are analysed using the methods developed by nine independent research teams. The results are combined to validate the determined global asteroseismic parameters and calculate the relative precision by which the parameters can be obtained. We correlate the relative number of detected solar-like oscillators with stellar parameters from the Kepler Input Catalogue and find a deficiency for stars with effective temperatures in the range 5300 {$\lessequivlnt$}T\textsubscript{eff}{$\lessequivlnt$} 5700 K and a drop-off in detected oscillations in stars approaching the red edge of the classical instability strip. We compare the power-law relationships between the frequency of peak power, {$\nu$}\textsubscript{max}, the mean large frequency separation, {$\increment\nu$}, and the maximum mode amplitude, A\textsubscript{max}, and show that there are significant method-dependent differences in the results obtained. This illustrates the need for multiple complementary analysis methods to be used to assess the robustness and reproducibility of results derived from global asteroseismic parameters.},
  file = {/Users/Oliver/Zotero/storage/999HKP84/Verner et al. - 2011 - Global asteroseismic properties of solar-like osci.pdf;/Users/Oliver/Zotero/storage/XDYV92RF/abstract.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {4}
}

@article{verner+roxburgh2011,
  title = {A Power-Spectrum Autocorrelation Technique to Detect Global Asteroseismic Parameters},
  author = {Verner, G. A. and Roxburgh, I. W.},
  year = {2011},
  month = apr,
  pages = {arXiv:1104.0631},
  abstract = {This article describes a moving-windowed autocorrelation technique which, when applied to an asteroseismic Fourier power spectrum, can be used to automatically detect the frequency of maximum p-mode power, large and small separations, mean p-mode linewidth, and constrain the stellar inclination angle and rotational splitting. The technique is illustrated using data from the CoRoT and Kepler space telescopes and tested using artificial data.},
  file = {/Users/Oliver/Zotero/storage/4J4LN38P/Verner and Roxburgh - 2011 - A power-spectrum autocorrelation technique to dete.pdf;/Users/Oliver/Zotero/storage/6TPAX9UE/abstract.html},
  journal = {arXiv e-prints},
  language = {en}
}

@article{viani+2017,
  title = {Changing the {$\nu$} Max {{Scaling Relation}}: {{The Need}} for a {{Mean Molecular Weight Term}}},
  shorttitle = {Changing the {$\nu$} Max {{Scaling Relation}}},
  author = {Viani, Lucas S. and Basu, Sarbani and Chaplin, William J. and Davies, Guy R. and Elsworth, Yvonne},
  year = {2017},
  month = jul,
  volume = {843},
  pages = {11},
  issn = {0004-637X},
  doi = {10.3847/1538-4357/aa729c},
  abstract = {The scaling relations that relate the average asteroseismic parameters \{\{{$\Delta$} \}\}{$\nu$} and \{{$\nu$} \}\textbackslash max to the global properties
of stars are used quite extensively to determine stellar properties. While the \{\{{$\Delta$} \}\}{$\nu$} scaling relation has been examined carefully
and the deviations from the relation have been well documented, the \{{$\nu$} \}\textbackslash max scaling relation has not been examined as
extensively. In this paper, we examine the \{{$\nu$} \}\textbackslash max
scaling relation using a set of stellar models constructed to have a wide range of mass, metallicity, and age. We find that as with \{\{{$\Delta$} \}\}{$\nu$} , \{{$\nu$} \}\textbackslash max does not follow the simple scaling
relation. The most visible deviation is because of a mean molecular weight term and a \{\{\{{$\Gamma$} \}\}\}1 term that are commonly
ignored. The remaining deviation is more difficult to address. We find that the influence of the scaling relation errors on asteroseismically derived values of \{log\}g are well within uncertainties. The influence of the errors on mass and radius estimates is small for main sequence and subgiants, but can be quite large for red giants.},
  file = {/Users/Oliver/Zotero/storage/CYP5TAF9/Viani et al. - 2017 - Changing the ν max Scaling Relation The Need for .pdf},
  journal = {The Astrophysical Journal},
  keywords = {stars: fundamental parameters,stars: interiors,stars: oscillations}
}

@article{viani+2019,
  title = {Determining the {{Best Method}} of {{Calculating}} the {{Large Frequency Separation For Stellar Models}}},
  author = {Viani, Lucas S. and Basu, Sarbani and Corsaro, Enrico and Ball, Warrick H. and Chaplin, William J.},
  year = {2019},
  month = jul,
  volume = {879},
  pages = {33},
  doi = {10.3847/1538-4357/ab232e},
  abstract = {Asteroseismology of solar-like oscillators often relies on the comparisons between stellar models and stellar observations in order to determine the properties of stars. The values of the global seismic parameters, {$\nu$} \textsubscript{max} (the frequency where the smoothed amplitude of the oscillations peak) and {$\increment\nu$} (the large frequency separation), are frequently used in grid-based modeling searches. However, the methods by which {$\increment\nu$} is calculated from observed data and how {$\increment\nu$} is calculated from stellar models are not the same. Typically for observed stars, especially for those with low signal-to-noise data, {$\increment\nu$} is calculated by taking the power spectrum of a power spectrum, or with autocorrelation techniques. However, for stellar models, the actual individual mode frequencies are calculated and the average spacing between them directly determined. In this work we try to determine the best way to combine model frequencies in order to obtain {$\increment\nu$} that can be compared with observations. For this we use stars with high signal-to-noise observations from Kepler as well as simulated Transiting Exoplanet Survey Satellite data of Ball et al. We find that when determining {$\increment\nu$} from individual mode frequencies the best method is to use the {$\mathscr{l}$} = 0 modes with either no weighting or with a Gaussian weighting around {$\nu$} \textsubscript{max}.},
  file = {/Users/Oliver/Zotero/storage/UPAQJWE8/Viani et al. - 2019 - Determining the Best Method of Calculating the Lar.pdf;/Users/Oliver/Zotero/storage/FID7VEAN/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{vogt+2017,
  title = {A {{Six}}-{{Planet System Around}} the {{Star HD}} 34445},
  author = {Vogt, Steven S. and Butler, R. Paul and Burt, Jennifer and Tuomi, Mikko and Laughlin, Gregory and Holden, Brad and Teske, Johanna K. and Shectman, Stephen A. and Crane, Jeffrey D. and Diaz, Matias and Thompson, Ian B. and Arriagada, Pamela and Keiser, Sandy},
  year = {2017},
  month = oct,
  volume = {154},
  pages = {181},
  issn = {1538-3881},
  doi = {10.3847/1538-3881/aa8b61},
  abstract = {We present a new precision radial velocity dataset that reveals a multi-planet system orbiting the G0V star HD 34445. Our 18-year span consists of 333 precision radial velocity observations, 56 of which were previously published, and 277 which are new data from Keck Observatory, Magellan at Las Campanas Observatory, and the Automated Planet Finder at Lick Observatory. These data indicate the presence of six planet candidates in Keplerian motion about the host star with periods of 1057, 215, 118, 49, 677, and 5700 days, and minimum masses of 0.63, 0.17, 0.1, 0.05, 0.12 and 0.38 Jupiter masses respectively. The HD 34445 planetary system, with its high degree of multiplicity, its long orbital periods, and its induced stellar radial velocity half-amplitudes in the range \$2 \textbackslash,\{\textbackslash rm m\textbackslash, s\^\{-1\}\} \textbackslash lesssim K \textbackslash lesssim 5\textbackslash,\{\textbackslash rm m\textbackslash, s\^\{-1\}\}\$ is fundamentally unlike either our own solar system (in which only Jupiter and Saturn induce significant reflex velocities for the Sun), or the Kepler multiple-transiting systems (which tend to have much more compact orbital configurations)},
  archivePrefix = {arXiv},
  eprint = {1710.07337},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/24BMTHTZ/Vogt et al. - 2017 - A Six-Planet System Around the Star HD 34445.pdf;/Users/Oliver/Zotero/storage/BWATZUBG/1710.html},
  journal = {The Astronomical Journal},
  keywords = {Astrophysics - Earth and Planetary Astrophysics},
  number = {5}
}

@article{vorontsov+1991,
  title = {Seismological Measurement of Solar Helium Abundance},
  author = {Vorontsov, S. V. and Baturin, V. A. and Pamiatnykh, A. A.},
  year = {1991},
  month = jan,
  volume = {349},
  pages = {49--51},
  issn = {0028-0836},
  doi = {10.1038/349049a0},
  abstract = {A new approach to the helioseismological determination of the solar helium abundance is described which is based on an analysis of the phase shift of acoustic waves of intermediate-degree modes. From accurate intermediate-mode data a helium mass fraction of 0.25 + or - 0.01 in the solar convection zone is obtained, significantly smaller than the value of 0.27-0.29 predicted by recent solar evolutionary models. The
discrepancy indicates either that initial helium abundance was reduced in the envelope by downward diffusion or that the protosolar value was lower than currently accepted.},
  journal = {Nature},
  keywords = {Abundance,Acoustic Frequencies,Helioseismology,Helium,Signal To Noise Ratios,Solar Interior,Solar Oscillations}
}

@article{vrard+2016,
  title = {Period Spacings in Red Giants. {{II}}. {{Automated}} Measurement},
  author = {Vrard, M. and Mosser, B. and Samadi, R.},
  year = {2016},
  month = apr,
  volume = {588},
  pages = {A87},
  doi = {10.1051/0004-6361/201527259},
  abstract = {Context. The space missions CoRoT and Kepler have provided photometric data of unprecedented quality for asteroseismology. A very rich oscillation pattern has been discovered for red giants, including mixed modes that are used to decipher the red giants' interiors. They carry information on the radiative core of red giant stars and bring strong constraints on stellar evolution. \\
 Aims: Since more than 15 000 red giant light curves have been observed by Kepler, we have developed a simple and efficient method for automatically characterizing the mixed-mode pattern and measuring the asymptotic period spacing. \\
 Methods: With the asymptotic expansion of the mixed modes, we have revealed the regularity of the gravity-mode pattern. The stretched periods were used to study the evenly space periods with a Fourier analysis and to measure the gravity period spacing, even when rotation severely complicates the oscillation spectra. \\
 Results: We automatically measured gravity period spacing for more than 6100 Kepler red giants. The results confirm and extend previous measurements made by semi-automated methods. We also unveil the mass and metallicity dependence of the relation between the frequency spacings and the period spacings for stars on the red giant branch. \\
 Conclusions: The delivery of thousands of period spacings combined with all other seismic and non-seismic information provides a new basis for detailed ensemble asteroseismology. Full Table 2 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/588/A87}{http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/588/A87}},
  file = {/Users/Oliver/Zotero/storage/K743K4NX/Vrard et al. - 2016 - Period spacings in red giants. II. Automated measu.pdf;/Users/Oliver/Zotero/storage/4NBU2I3A/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{wang+2016,
  title = {Calibration of {{LAMOST Stellar Surface Gravities}} Using the {{Kepler Asteroseismic Data}}},
  author = {Wang, Liang and Wang, Wei and Wu, Yue and Zhao, Gang and Li, Yinbi and Luo, Ali and Liu, Chao and Zhang, Yong and Hou, Yonghui and Wang, Yuefei and Cao, Zihuang},
  year = {2016},
  month = jul,
  volume = {152},
  pages = {6},
  doi = {10.3847/0004-6256/152/1/6},
  abstract = {Asteroseismology is a powerful tool to precisely determine the evolutionary status and fundamental properties of stars. With the unprecedented precision and nearly continuous photometric data acquired by the NASA Kepler mission, parameters of more than 10\textsuperscript{4} stars have been determined nearly consistently. However, most studies still use photometric effective temperatures (T \textsubscript{eff}) and metallicities ([Fe/H]) as inputs, which are not sufficiently accurate as suggested by previous studies. We adopted the spectroscopic T \textsubscript{eff} and [Fe/H] values based on the Large sky Area Multi-Object fiber Spectroscopic Telescope (LAMOST) low-resolution spectra (R {$\simeq$} 1800), and combined them with the global oscillation parameters to derive the physical parameters of a large sample of stars. Clear trends were found between \{\{{$\increment$} \}\}\{log\}g(\{\{LAMOST\}\}-\{\{seismic\}\}) and spectroscopic T \textsubscript{eff} as well as log g, which may result in an overestimation of up to 0.5 dex for the log g values of giants in the LAMOST catalog. We established empirical calibration relations for the log g values of dwarfs and giants. These results can be used for determining the precise distances to these stars based on their spectroscopic parameters.},
  file = {/Users/Oliver/Zotero/storage/XWEBR34Y/Wang et al. - 2016 - Calibration of LAMOST Stellar Surface Gravities us.pdf;/Users/Oliver/Zotero/storage/HQ6TS295/ui.adsabs.harvard.edu.html},
  journal = {The Astronomical Journal},
  language = {en},
  number = {1}
}

@misc{waskom+2018,
  title = {Mwaskom/Seaborn: V0.9.0 ({{July}} 2018)},
  shorttitle = {Mwaskom/Seaborn},
  author = {Waskom, Michael and Olga Botvinnik and Drew O'Kane and Paul Hobson and Joel Ostblom and Saulius Lukauskas and David C Gemperline and Tom Augspurger and Yaroslav Halchenko and John B. Cole and Jordi Warmenhoven and {Julian de Ruiter} and Cameron Pye and Stephan Hoyer and Jake Vanderplas and Santi Villalba and Gero Kunter and Eric Quintero and Pete Bachant and Marcel Martin and Kyle Meyer and Alistair Miles and Yoav Ram and Thomas Brunner and Tal Yarkoni and Mike Lee Williams and Constantine Evans and Clark Fitzgerald and Brian and Adel Qalieh},
  year = {2018},
  month = jul,
  doi = {10.5281/zenodo.1313201},
  abstract = {v0.9.0 (July 2018) Note: a version of these release notes with working links appears in the online documentation. This is a major release with several substantial and long-desired new features. There are also updates/modifications to the themes and color palettes that give better consistency with matplotlib 2.0 and some notable API changes. New relational plots Three completely new plotting functions have been added: catplot, scatterplot, and lineplot. The first is a figure-level interface to the latter two that combines them with a FacetGrid. The functions bring the high-level, dataset-oriented API of the seaborn categorical plotting functions to more general plots (scatter plots and line plots). These functions can visualize a relationship between two numeric variables while mapping up to three additional variables by modifying hue, size, and/or style semantics. The common high-level API is implemented differently in the two functions. For example, the size semantic in scatterplot scales the area of scatter plot points, but in lineplot it scales width of the line plot lines. The API is dataset-oriented, meaning that in both cases you pass the variable in your dataset rather than directly specifying the matplotlib parameters to use for point area or line width. Another way the relational functions differ from existing seaborn functionality is that they have better support for using numeric variables for hue and size semantics. This functionality may be propagated to other functions that can add a hue semantic in future versions; it has not been in this release. The lineplot function also has support for statistical estimation and is replacing the older tsplot function, which still exists but is marked for removal in a future release. lineplot is better aligned with the API of the rest of the library and more flexible in showing relationships across additional variables by modifying the size and style semantics independently. It also has substantially improved support for date and time data, a major pain factor in tsplot. The cost is that some of the more esoteric options in tsplot for representing uncertainty (e.g. a colormapped KDE of the bootstrap distribution) have not been implemented in the new function. There is quite a bit of new documentation that explains these new functions in more detail, including detailed examples of the various options in the API reference and a more verbose tutorial. These functions should be considered in a "stable beta" state. They have been thoroughly tested, but some unknown corner cases may remain to be found. The main features are in place, but not all planned functionality has been implemented. There are planned improvements to some elements, particularly the default legend, that are a little rough around the edges in this release. Finally, some of the default behavior (e.g. the default range of point/line sizes) may change somewhat in future releases. Updates to themes and palettes Several changes have been made to the seaborn style themes, context scaling, and color palettes. In general the aim of these changes was to make the seaborn styles more consistent with the style updates in matplotlib 2.0 and to leverage some of the new style parameters for better implementation of some aspects of the seaborn styles. Here is a list of the changes: Reorganized and updated some axes\_style/plotting\_context parameters to take advantage of improvements in the matplotlib 2.0 update. The biggest change involves using several new parameterss in the "style" spec while moving parameters that used to implement the corresponding aesthetics to the "context" spec. For example, axes spines and ticks are now off instead of having their width/length zeroed out for the darkgrid style. That means the width/length of these elements can now be scaled in different contexts. The effect is a more cohesive appearance of the plots, especially in larger contexts. These changes include only minimal support for the 1.x matplotlib series. Users who are stuck on matplotlib 1.5 but wish to use seaborn styling may want to use the seaborn parameters that can be accessed through the matplotlib stylesheet interface. Updated the seaborn palettes ("deep", "muted", "colorblind", etc.) to correspond with the new 10-color matplotlib default. The legacy palettes are now available at "deep6", "muted6", "colorblind6", etc. Additionally, a few individual colors were tweaked for better consistency, aesthetics, and accessibility. Calling color\_palette (or set\_palette) with a named qualitative palettes (i.e. one of the seaborn palettes, the colorbrewer qualitative palettes, or the matplotlib matplotlib tableau-derived palettes) and no specified number of colors will return all of the colors in the palette. This means that for some palettes, the returned list will have a different length than it did in previous versions. Enhanced color\_palette to accept a parameterized specification of a cubehelix palette in in a string, prefixed with "ch:" (e.g. "ch:-.1,.2,l=.7"). Note that keyword arguments can be spelled out or referenced using only their first letter. Reversing the palette is accomplished by appending "\_r", as with other matplotlib colormaps. This specification will be accepted by any seaborn function with a palette= parameter. Slightly increased the base font sizes in plotting\_context and increased the scaling factors for "talk" and "poster" contexts. Calling set will now call set\_color\_codes to re-assign the single letter color codes by default API changes A few functions have been renamed or have had changes to their default parameters. The factorplot function has been renamed to catplot. The new name ditches the original R-inflected terminology to use a name that is more consistent with terminology in pandas and in seaborn itself. This change should hopefully make catplot easier to discover, and it should make more clear what its role is. factorplot still exists and will pass its arguments through to catplot with a warning. It may be removed eventually, but the transition will be as gradual as possible. The other reason that the factorplot name was changed was to ease another alteration which is that the default kind in catplot is now "strip" (corresponding to stripplot). This plots a categorical scatter plot which is usually a much better place to start and is more consistent with the default in relplot. The old default style in factorplot ("point", corresponding to pointplot) remains available if you want to show a statistical estimation. The lvplot function has been renamed to boxenplot. The "letter-value" terminology that was used to name the original kind of plot is obscure, and the abbreviation to lv did not help anything. The new name should make the plot more discoverable by describing its format (it plots multiple boxes, also known as "boxen"). As with factorplot, the lvplot function still exists to provide a relatively smooth transition. Renamed the size parameter to height in multi-plot grid objects (FacetGrid, PairGrid, and JointGrid) along with functions that use them (factorplot, lmplot, pairplot, and jointplot) to avoid conflicts with the size parameter that is used in scatterplot and lineplot (necessary to make relplot work) and also makes the meaning of the parameter a bit more clear. Changed the default diagonal plots in pairplot to use `func`:kdeplot` when a "hue" dimension is used. Deprecated the statistical annotation component of JointGrid. The method is still available but will be removed in a future version. Two older functions that were deprecated in earlier versions, coefplot and interactplot, have undergone final removal from the code base. Documentation improvements There has been some effort put into improving the documentation. The biggest change is that the introduction to the library has been completely rewritten to provide much more information and, critically, examples. In addition to the high-level motivation, the introduction also covers some important topics that are often sources of confusion, like the distinction between figure-level and axes-level functions, how datasets should be formatted for use in seaborn, and how to customize the appearance of the plots. Other improvements have been made throughout, most notably a thorough re-write of the categorical tutorial categorical\_tutorial. Other small enhancements and bug fixes Changed rugplot to plot a matplotlib LineCollection instead of many Line2D objects, providing a big speedup for large arrays. Changed the default off-diagonal plots to use scatterplot. (Note that the "hue" currently draws three separate scatterplots instead of using the hue semantic of the scatterplot function). Changed color handling when using kdeplot with two variables. The default colormap for the 2D density now follows the color cycle, and the function can use color and label kwargs, adding more flexibility and avoiding a warning when using with multi-plot grids. Added the subplot\_kws parameter to PairGrid for more flexibility. Removed a special case in PairGrid that defaulted to drawing stacked histograms on the diagonal axes. Fixed jointplot/JointGrid and regplot so that they now accept list inputs. Fixed a bug in FacetGrid when using a single row/column level or using col\_wrap=1. Fixed functions that set axis limits so that they preserve auto-scaling state on matplotlib 2.0. Avoided an error when using matplotlib backends that cannot render a canvas (e.g. PDF). Changed the install infrastructure to explicitly declare dependencies in a way that pip is aware of. This means that pip install seaborn will now work in an empty environment. Additionally, the dependencies are specified with strict minimal versions. Updated the testing infrastructure to execute tests with pytest (although many individual tests still use nose assertion).},
  file = {/Users/Oliver/Zotero/storage/HQGU7UIM/1313201.html},
  howpublished = {Zenodo}
}

@misc{waskom+2020,
  title = {Mwaskom/Seaborn: V0.10.0 ({{January}} 2020)},
  shorttitle = {Mwaskom/Seaborn},
  author = {{Waskom} and Olga Botvinnik and Joel Ostblom and Saulius Lukauskas and Paul Hobson and MaozGelbart and David C Gemperline and Tom Augspurger and Yaroslav Halchenko and John B. Cole and Jordi Warmenhoven and {Julian de Ruiter} and Cameron Pye and Stephan Hoyer and Jake Vanderplas and Santi Villalba and Gero Kunter and Eric Quintero and Pete Bachant and Marcel Martin and Kyle Meyer and Corban Swain and Alistair Miles and Thomas Brunner and Drew O'Kane and Tal Yarkoni and Mike Lee Williams and Constantine Evans},
  year = {2020},
  month = jan,
  doi = {10.5281/zenodo.3629446},
  abstract = {This is a major update that is being released simultaneously with version 0.9.1. It has all of the same features (and bugs!) as 0.9.1, but there are important changes to the dependencies. Most notably, all support for Python 2 has now been dropped. Support for Python 3.5 has also been dropped. Seaborn is now strictly compatible with Python 3.6+. Minimally supported versions of the dependent PyData libraries have also been increased, in some cases substantially. While seaborn has tended to be very conservative about maintaining compatibility with older dependencies, this was causing increasing pain during development. At the same time, these libraries are now much easier to install. Going forward, seaborn will likely stay close to the Numpy community guidelines for version support. This release also removes a few previously-deprecated features: The tsplot function and seaborn.timeseries module have been removed. Recall that tsplot was replaced with lineplot. The seaborn.apionly entry-point has been removed. The seaborn.linearmodels module (previously renamed to seaborn.regression) has been removed. Looking forward Now that seaborn is a Python 3 library, it can take advantage of keyword-only arguments. It is likely that future versions will introduce this syntax, potentially in a breaking way. For guidance, most seaborn functions have a signature that looks like func(x, y, ..., data=None, **kwargs) where the **kwargs are specified in the function. Going forward it will likely be necessary to specify data and all subsequent arguments with an explicit key=value mapping. This style has long been used throughout the documentation, and the formal requirement will not be introduced until at least the next major release. Adding this feature will make it possible to enhance some older functions with more modern capabilities (e.g., adding a native hue semantic within functions like jointplot and regplot).},
  file = {/Users/Oliver/Zotero/storage/PFWJ2PAR/3629446.html},
  howpublished = {Zenodo}
}

@article{watkins+vandermarel2016,
  title = {Tycho-{{Gaia Astrometric Solution}} Parallaxes and Proper Motions for 5 {{Galactic}} Globular Clusters},
  author = {Watkins, Laura L. and {van der Marel}, Roeland P.},
  year = {2016},
  month = nov,
  abstract = {We perform a systematic search for Galactic globular cluster (GC) stars in the Tycho-Gaia Astrometric Solution (TGAS) catalogue that formed part of Gaia Data Release 1 (DR1), and identify 5 members of NGC104 (47 Tucanae), 1 member of NGC5272 (M3), 5 members of NGC6121 (M4), 7 members of NGC6397, and 2 members of NGC6656 (M22). By taking a weighted average of the member stars, fully accounting for the correlations between parameter estimates, we estimate the parallax (and, hence, distance) and proper motion (PM) of the GCs. This provides a homogeneous PM study of multiple GCs based on an astrometric catalog with small and well-controlled systematic errors, and yields random PM errors that are similar to existing measurements. Detailed comparison to the available Hubble Space Telescope (HST) measurements generally shows excellent agreement, validating the astrometric quality of both TGAS and HST. By contrast, comparison to ground-based measurements shows that some of those must have systematic errors exceeding the random errors. Our parallax estimates have uncertainties an order of magnitude larger than previous studies, but nevertheless imply distances consistent with previous estimates. By combining our PM measurements with literature positions, distances and radial velocities, we measure Galactocentric space motions for the clusters and find that these are also in good agreement with previous orbital analyses. Our results highlight the future promise of Gaia for the determining accurate distances and PMs of Galactic GCs, which will provide crucial constraints on the near end of the cosmic distance ladder, and provide accurate GC orbital histories.},
  archivePrefix = {arXiv},
  eprint = {1611.03170},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/J3B5IJBR/1611.html},
  journal = {arXiv:1611.03170 [astro-ph]},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{wevers+2017,
  title = {The Fast Transient Sky with {{Gaia}}},
  author = {Wevers, Thomas and Jonker, Peter G. and Hodgkin, Simon T. and {Kostrzewa-Rutkowska}, Zuzanna and Harrison, Diana L. and Rixon, Guy and Nelemans, Gijs and Roelens, Maroussia and Eyer, Laurent and {van Leeuwen}, Floor and Yoldas, Abdullah},
  year = {2017},
  month = oct,
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stx2625},
  abstract = {The ESA Gaia satellite scans the whole sky with a temporal sampling ranging from seconds and hours to months. Each time a source passes within the Gaia field of view, it moves over 10 CCDs in 45 s and a lightcurve with 4.5 s sampling (the crossing time per CCD) is registered. Given that the 4.5 s sampling represents a virtually unexplored parameter space in optical time domain astronomy, this data set potentially provides a unique opportunity to open up the fast transient sky. We present a method to start mining the wealth of information in the per CCD Gaia data. We perform extensive data filtering to eliminate known on-board and data processing artefacts, and present a statistical method to identify sources that show transient brightness variations on \textasciitilde 2 hours timescales. We illustrate that by using the Gaia photometric CCD measurements, we can detect transient brightness variations down to an amplitude of 0.3 mag on timescales ranging from 15 seconds to several hours. We search an area of \textasciitilde 23.5 square degrees on the sky, and find four strong candidate fast transients. Two candidates are tentatively classified as flares on M-dwarf stars, while one is probably a flare on a giant star and one potentially a flare on a solar type star. These classifications are based on archival data and the timescales involved. We argue that the method presented here can be added to the existing Gaia Science Alerts infrastructure for the near real-time public dissemination of fast transient events.},
  archivePrefix = {arXiv},
  eprint = {1710.08924},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/HMGUSAN7/Wevers et al. - 2017 - The fast transient sky with Gaia.pdf;/Users/Oliver/Zotero/storage/PDB6VMDF/1710.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Astrophysics - High Energy Astrophysical Phenomena,Astrophysics - Instrumentation and Methods for Astrophysics,Astrophysics - Solar and Stellar Astrophysics}
}

@article{white+2011,
  title = {Calculating {{Asteroseismic Diagrams}} for {{Solar}}-like {{Oscillations}}},
  author = {White, Timothy R. and Bedding, Timothy R. and Stello, Dennis and {Christensen-Dalsgaard}, J{\o}rgen and Huber, Daniel and Kjeldsen, Hans},
  year = {2011},
  month = dec,
  volume = {743},
  pages = {161},
  doi = {10.1088/0004-637X/743/2/161},
  abstract = {With the success of the Kepler and CoRoT missions, the number of stars with detected solar-like oscillations has increased by several orders of magnitude; for the first time we are able to perform large-scale ensemble asteroseismology of these stars. In preparation for this golden age of asteroseismology we have computed expected values of various asteroseismic observables from models of varying mass and metallicity. The relationships between these asteroseismic observables, such as the separations between mode frequencies, are able to significantly constrain estimates of the ages and masses of these stars. We investigate the scaling relation between the large frequency separation, {$\increment\nu$}, and mean stellar density. Furthermore we present model evolutionary tracks for several asteroseismic diagrams. We have extended the so-called C-D diagram beyond the main sequence to the subgiants and the red giant branch. We also consider another asteroseismic diagram, the epsilon diagram, which is more sensitive to variations in stellar properties at the subgiant stages and can aid in determining the correct mode identification. The recent discovery of gravity-mode period spacings in red giants forms the basis for a third asteroseismic diagram. We compare the evolutionary model tracks in these asteroseismic diagrams with results from pre-Kepler studies of solar-like oscillations and early results from Kepler.},
  file = {/Users/Oliver/Zotero/storage/56Z2B77Y/White et al. - 2011 - Calculating Asteroseismic Diagrams for Solar-like .pdf;/Users/Oliver/Zotero/storage/PQ8TV4JG/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{white+2013,
  title = {Interferometric Radii of Bright {{Kepler}} Stars with the {{CHARA Array}}: \texttheta{} {{Cygni}} and 16 {{Cygni A}} and {{B}}},
  shorttitle = {Interferometric Radii of Bright {{Kepler}} Stars with the {{CHARA Array}}},
  author = {White, T. R. and Huber, D. and Maestro, V. and Bedding, T. R. and Ireland, M. J. and Baron, F. and Boyajian, T. S. and Che, X. and Monnier, J. D. and Pope, B. J. S. and Roettenbacher, R. M. and Stello, D. and Tuthill, P. G. and Farrington, C. D. and Goldfinger, P. J. and McAlister, H. A. and Schaefer, G. H. and Sturmann, J. and Sturmann, L. and Brummelaar, Ten and A, T. and Turner, N. H.},
  year = {2013},
  month = aug,
  volume = {433},
  pages = {1262},
  doi = {10.1093/mnras/stt802},
  abstract = {We present the results of long-baseline optical interferometry observations using the Precision Astronomical Visual Observations (PAVO) beam combiner at the Center for High Angular Resolution Astronomy (CHARA) Array to measure the angular sizes of three bright Kepler stars: \texttheta{} Cygni, and both components of the binary system 16 Cygni. Supporting infrared observations were made with the Michigan Infrared Combiner (MIRC) and Classic beam combiner, also at the CHARA Array. We find limb-darkened angular diameters of 0.753 {$\pm$} 0.009 mas for \texttheta{} Cyg, 0.539 {$\pm$} 0.007 mas for 16 Cyg A and 0.490 {$\pm$} 0.006 mas for 16 Cyg B. The Kepler Mission has observed these stars with outstanding photometric precision, revealing the presence of solar-like oscillations. Due to the brightness of these stars the oscillations have exceptional signal-to-noise, allowing for detailed study through asteroseismology, and are well constrained by other observations. We have combined our interferometric diameters with Hipparcos parallaxes, spectrophotometric bolometric fluxes and the asteroseismic large frequency separation to measure linear radii (\texttheta{} Cyg: 1.48 {$\pm$} 0.02 R\textsubscript{{$\Sun$}}, 16 Cyg A: 1.22 {$\pm$} 0.02 R\textsubscript{{$\Sun$}}, 16 Cyg B: 1.12 {$\pm$} 0.02 R\textsubscript{{$\Sun$}}), effective temperatures (\texttheta{} Cyg: 6749 {$\pm$} 44 K, 16 Cyg A: 5839 {$\pm$} 42 K, 16 Cyg B: 5809 {$\pm$} 39 K) and masses (\texttheta{} Cyg: 1.37 {$\pm$} 0.04 M\textsubscript{{$\Sun$}}, 16 Cyg A: 1.07 {$\pm$} 0.05 M\textsubscript{{$\Sun$}}, 16 Cyg B: 1.05 {$\pm$} 0.04 M\textsubscript{{$\Sun$}}) for each star with very little model dependence. The measurements presented here will provide strong constraints for future stellar modelling efforts.},
  file = {/Users/Oliver/Zotero/storage/HV9WQ5GF/White et al. - 2013 - Interferometric radii of bright Kepler stars with .pdf;/Users/Oliver/Zotero/storage/CGKI79SN/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {2}
}

@article{white+2017,
  title = {Beyond the {{Kepler}}/{{K2}} Bright Limit: Variability in the Seven Brightest Members of the {{Pleiades}}},
  shorttitle = {Beyond the {{Kepler}}/{{K2}} Bright Limit},
  author = {White, T. R. and Pope, B. J. S. and Antoci, V. and P{\'a}pics, P. I. and Aerts, C. and Gies, D. R. and Gordon, K. and Huber, D. and Schaefer, G. H. and Aigrain, S. and Albrecht, S. and Barclay, T. and Barentsen, G. and Beck, P. G. and Bedding, T. R. and Fredslund Andersen, M. and Grundahl, F. and Howell, S. B. and Ireland, M. J. and Murphy, S. J. and Nielsen, M. B. and Silva Aguirre, V. and Tuthill, P. G.},
  year = {2017},
  month = nov,
  volume = {471},
  pages = {2882--2901},
  issn = {0035-8711},
  doi = {10.1093/mnras/stx1050},
  abstract = {The most powerful tests of stellar models come from the brightest stars
in the sky, for which complementary techniques, such as astrometry,
asteroseismology, spectroscopy and interferometry, can be combined. The
K2 mission is providing a unique opportunity to obtain high-precision
photometric time series for bright stars along the ecliptic. However,
bright targets require a large number of pixels to capture the entirety
of the stellar flux, and CCD saturation, as well as restrictions on data
storage and bandwidth, limit the number and brightness of stars that can
be observed. To overcome this, we have developed a new photometric
technique, which we call halo photometry, to observe very bright stars
using a limited number of pixels. Halo photometry is simple, fast and
does not require extensive pixel allocation, and will allow us to use K2
and other photometric missions, such as TESS, to observe very bright
stars for asteroseismology and to search for transiting exoplanets. We
apply this method to the seven brightest stars in the Pleiades open
cluster. Each star exhibits variability; six of the stars show what are
most likely slowly pulsating B-star pulsations, with amplitudes ranging
from 20 to 2000 ppm. For the star Maia, we demonstrate the utility of
combining K2 photometry with spectroscopy and interferometry to show
that it is not a `Maia variable', and to establish that its variability
is caused by rotational modulation of a large chemical spot on a 10 d
time-scale.},
  file = {/Users/Oliver/Zotero/storage/9GZYBT33/White et al. - 2017 - Beyond the KeplerK2 bright limit variability in .pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {asteroseismology,open clusters and associations: individual: Pleiades,stars: early type,stars: variables: general,techniques: photometric}
}

@phdthesis{woodard1984,
  title = {Short-{{Period Oscillations}} in the {{Total Solar Irradiance}}.},
  author = {Woodard, Martin Frederic},
  year = {1984},
  abstract = {This dissertation deals with normal-mode vibrations of the Sun, as measured by their effect on the solar total irradiance. I have studied "5-minute" p-mode oscillations of radial order n (TURNEQ) 16 - 26 and degree l = 0 - 2 in the 1980 data from the Active Cavity Radiometer Irradiance Monitor (ACRIM) on the Solar Maximum Mission satellite (SMM). The frequencies of separate (n,l) peaks in the spectrum of ACRIM data agree with those of previous observers to within ('(TURN))3 parts in 10('4). For the oscillatory peaks of highest signal quality the
frequency error is estimated to be less than one part in 10('4). Discrepancies between observed and theoretical frequencies are already much greater than discrepancies among observed frequencies. Quasi -degenerate m states, of which the (n,l) peaks are in principle
comprised, cannot be distinguished in the ACRIM power spectrum, contrary to previous claims. The mean amplitudes of individual (n,l) peaks have been established with 10 - 20\% accuracy; r.m.s. fractional irradiance variations of up to 3 parts per million occur. The observed amplitude ratio of 5-min modes in velocity and intensity agrees roughly with preliminary theoretical estimates, but more theory and observation are required. The 5-min oscillation data from the ACRIM have been
interpreted in terms of a theoretically motivated picture in which the modes behave like independently and randomly excited harmonic
oscillators. The relative frequency width of the most prominent l = 0 modes is about one part in 2000, implying an oscillator time constant (e-folding time for energy decay) of 1 to 2 days. This lifetime is approximately confirmed by direct observations of amplitude variations in these modes. The lifetime of these modes was previously a matter of controversy. Solar rotation will split the m states belonging to a given (n,l) multiplet, making the l {$>$} 1 peaks broader than they would
otherwise be. From the widths of the l = 1 peaks I deduce an upper limit on the separation of adjacent m states of 1.0 (mu)Hz with ('(TURN))99\% confidence. This is 2.2 times the splitting that solid-body rotation at the observed ('(TURN))1/25-day sidereal equatorial surface rate would imply. . . . (Author's abstract exceeds stipulated maximum length. Discontinued here with permission of author.) UMI.},
  journal = {Ph.D. Thesis}
}

@article{yang+tian2017,
  title = {The Effects of the Overshooting of the Convective Core on Main-Sequence Turnoffs of Young- and Intermediate-Age Star Clusters},
  author = {Yang, Wuming and Tian, Zhijia},
  year = {2017},
  month = jan,
  abstract = {Recent investigations have shown that the extended main-sequence turnoffs (eMSTOs) are a common feature of intermediate-age star clusters in the Magellanic Clouds. The eMSTOs are also found in the color-magnitude diagram (CMD) of young-age star clusters. The origin of the eMSTOs is still an open question. Moreover, asteroseismology shows that the value of the overshooting parameter \$\textbackslash delta\_\{\textbackslash rm ov\}\$ of the convective core is not fixed for the stars with an approximatelly equal mass. Thus the MSTO of star clusters may be affected by the overshooting of the convective core (OVCC). We calculated the effects of the OVCC with different \$\textbackslash delta\_\{\textbackslash rm ov\}\$ on the MSTO of young- and intermediate-age star clusters. \textbackslash textbf\{If \$\textbackslash delta\_\{\textbackslash rm ov\}\$ varies between stars in a cluster,\} the observed eMSTOs of young- and intermediate-age star clusters can be explained well by the effects. The equivalent age spreads of MSTO caused by the OVCC are related to the age of star clusters and are in good agreement with observed results of many clusters. Moreover, the observed eMSTOs of NGC 1856 are reproduced by the coeval populations with different \$\textbackslash delta\_\{\textbackslash rm ov\}\$. The eMSTOs of star clusters may be relevant to the effects of the OVCC. The effects of the OVCC \textbackslash textbf\{are similar to that of rotation in some respects. But the effects cannot result in a significant split of main sequence of young star clusters at \$m\_\{U\}\textbackslash lesssim 21\$.\} The presence of a rapid rotation can make the split of main sequence of young star clusters more significant.},
  archivePrefix = {arXiv},
  eprint = {1701.05963},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/V96R8S52/Yang and Tian - 2017 - The effects of the overshooting of the convective .pdf;/Users/Oliver/Zotero/storage/9XWDCIQW/1701.html},
  journal = {arXiv:1701.05963 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{yu+2018,
  title = {Asteroseismology of 16,000 {{Kepler Red Giants}}: {{Global Oscillation Parameters}}, {{Masses}}, and {{Radii}}},
  shorttitle = {Asteroseismology of 16,000 {{Kepler Red Giants}}},
  author = {Yu, Jie and Huber, Daniel and Bedding, Timothy R. and Stello, Dennis and Hon, Marc and Murphy, Simon J. and Khanna, Shourya},
  year = {2018},
  month = jun,
  volume = {236},
  pages = {42},
  doi = {10.3847/1538-4365/aaaf74},
  abstract = {The Kepler mission has provided exquisite data to perform an ensemble asteroseismic analysis on evolved stars. In this work we systematically characterize solar-like oscillations and granulation for 16,094 oscillating red giants, using end-of-mission long-cadence data. We produced a homogeneous catalog of the frequency of maximum power (typical uncertainty \{{$\sigma$} \}\textsubscript{\{{$\nu$} \vphantom\}}\textsubscript{\textbackslash max }\vphantom\{\}=1.6 \% ), the mean large frequency separation (\{{$\sigma$} \}\textsubscript{\{\{{$\increment$} \vphantom{\}\}}}\vphantom\{\}{$\nu$} \vphantom\{\}=0.6 \% ), oscillation amplitude (\{{$\sigma$} \}\textsubscript{\{\{A\vphantom{\}\}}}\vphantom\{\}\vphantom\{\}=4.7 \% ), granulation power (\{{$\sigma$} \}\textsubscript{gran}\vphantom\{\}=8.6 \% ), power excess width (\{{$\sigma$} \}\textsubscript{width}\vphantom\{\}=8.8 \% ), seismically derived stellar mass (\{{$\sigma$} \}\textsubscript{\{\{M\vphantom{\}\}}}\vphantom\{\}\vphantom\{\}=7.8 \% ), radius (\{{$\sigma$} \}\textsubscript{\{\{R\vphantom{\}\}}}\vphantom\{\}\vphantom\{\}=2.9 \% ), and thus surface gravity (\{{$\sigma$} \}\textsubscript{log}g\vphantom\{\}=0.01 dex). Thanks to the large red giant sample, we confirm that red-giant-branch (RGB) and helium-core-burning (HeB) stars collectively differ in the distribution of oscillation amplitude, granulation power, and width of power excess, which is mainly due to the mass difference. The distribution of oscillation amplitudes shows an extremely sharp upper edge at fixed \{{$\nu$} \}\textsubscript{\textbackslash max }, which might hold clues for understanding the excitation and damping mechanisms of the oscillation modes. We find that both oscillation amplitude and granulation power depend on metallicity, causing a spread of 15\% in oscillation amplitudes and a spread of 25\% in granulation power from [Fe/H] = -0.7 to 0.5 dex. Our asteroseismic stellar properties can be used as reliable distance indicators and age proxies for mapping and dating galactic stellar populations observed by Kepler. They will also provide an excellent opportunity to test asteroseismology using Gaia parallaxes, and lift degeneracies in deriving atmospheric parameters in large spectroscopic surveys such as APOGEE and LAMOST.},
  file = {/Users/Oliver/Zotero/storage/R27ESZ7J/Yu et al. - 2018 - Asteroseismology of 16,000 Kepler Red Giants Glob.pdf;/Users/Oliver/Zotero/storage/QXQUW7PS/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en},
  number = {2}
}

@article{yu+2020,
  title = {Asteroseismology of Luminous Red Giants with {{Kepler I}}: {{Long Period Variables}} with Radial and Non-Radial Modes},
  shorttitle = {Asteroseismology of Luminous Red Giants with {{Kepler I}}},
  author = {Yu, Jie and Bedding, Timothy R. and Stello, Dennis and Huber, Daniel and Compton, Douglas L. and Gizon, Laurent and Hekker, Saskia},
  year = {2020},
  month = mar,
  volume = {493},
  pages = {1388--1403},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/staa300},
  abstract = {While long period variables (LPVs) have been extensively investigated, especially with MACHO and OGLE data for the Magellanic Clouds, there still exist open questions in their pulsations regarding the excitation mechanisms, radial order and angular degree assignment. Here, we perform asteroseismic analyses on LPVs observed by the 4-year Kepler mission. Using a cross-correlation method, we detect unambiguous pulsation ridges associated with radial fundamental modes (n = 1) and overtones (n 2), where the radial order assignment is made by using theoretical frequencies and observed frequencies. Our results confirm that the amplitude variability seen in semiregulars is consistent with oscillations being solar-like. We identify that the dipole modes, l = 1, are dominant in the radial orders of 3 {$\leq$} n {$\leq$} 6, and that quadrupole modes, l = 2, are dominant in the first overtone n = 2. A test of seismic scaling relations using Gaia DR2 parallaxes reveals the possibility that the relations break down when {$\nu$}max 3 \textmu Hz (R 40 R , or log L/L 2.6). Our homogeneous measurements of pulsation amplitude and period for 3213 LPVs will be very valuable for probing effects of pulsation on mass loss, in particular in those stars with periods around 60 days, which has been argued as a threshold of substantial pulsation-triggered mass loss.},
  archivePrefix = {arXiv},
  eprint = {2001.10878},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/W5SDEGE2/Yu et al. - 2020 - Asteroseismology of luminous red giants with Keple.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  language = {en},
  number = {1}
}

@article{yuan+2013,
  title = {Empirical Extinction Coefficients for the {{GALEX}}, {{SDSS}}, {{2MASS}} and {{WISE}} Passbands},
  author = {Yuan, H. B. and Liu, X. W. and Xiang, M. S.},
  year = {2013},
  month = apr,
  volume = {430},
  pages = {2188},
  doi = {10.1093/mnras/stt039},
  abstract = {By using the `standard pair' technique of pairing stars of almost nil and high extinction but otherwise with almost identical stellar parameters from the Sloan Digital Sky Survey (SDSS), and combining this information with photometry from the SDSS, Galaxy Evolution Explorer (GALEX), Two Micron All Sky Survey (2MASS) and Wide-field Infrared Survey Explorer (WISE) photometry ranging from the far ultraviolet (UV) to the mid-infrared (mid-IR), we measure dust reddening in the FUV - NUV, NUV - u, u - g, g - r, r - i, i - z, z - J, J - H, H - Ks, Ks - W1 and W1 - W2 colours for thousands of Galactic stars. The measurements, together with the E(B - V) values given by Schlegel et al., allow us to derive the observed, model-free reddening coefficients for these colours. The results are compared with previous measurements and with the predictions of various Galactic reddening laws. We find that (i) the dust reddening map of Schlegel et al. overestimates E(B - V) by about 14 per cent, consistent with the recent work of Schlafly et al. and Schlafly \& Finkbeiner; (ii) after accounting for the differences in reddening normalization, the newly deduced reddening coefficients for colours FUV - NUV, NUV - u, u - g, g - r, r - i, i - z, z - J, J - H and H - Ks differ by respectively -1640, 15.5, 12.6, -0.8, 3.4, -0.7, 3.5, 2.5 and 1.4 per cent from the predictions of the Fitzpatrick reddening law for an assumed total-to-selective extinction ratio R(V) = 3.1, and by respectively -1730, 13.0 , 8.1, 10.0, 8.0, -13.5, -1.7, -6.7 and -17.1 per cent from the predictions of the CCM reddening law; and (iii) all the new reddening coefficients, except those for NUV - u and u - g, favour the R(V) = 3.1 Fitzpatrick reddening law over the R(V) = 3.1 CCM and O'Donnell reddening laws. Using the Ks-band extinction coefficient predicted by the R(V) = 3.1 Fitzpatrick law and the observed reddening coefficients, we deduce new extinction coefficients for the FUV, NUV, u, g, r, i, z, J, H, W1 and W2 passbands. We recommend that the new reddening and extinction coefficients should be used in the future and that the Fitzpatrick reddening law in the UV should probably be updated. We stress, however, that the FUV- and NUV-band coefficients should be used with caution, given their relatively large measurement uncertainties. Finally, potential applications of the `standard pair' technique with the upcoming LAMOST Galactic surveys are discussed.},
  file = {/Users/Oliver/Zotero/storage/F833W3I5/Yuan et al. - 2013 - Empirical extinction coefficients for the GALEX, S.pdf;/Users/Oliver/Zotero/storage/TC2M6YPW/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {3}
}

@article{zhao+2012,
  title = {{{LAMOST}} Spectral Survey \textemdash{} {{An}} Overview},
  author = {Zhao, Gang and Zhao, Yong-Heng and Chu, Yao-Quan and Jing, Yi-Peng and Deng, Li-Cai},
  year = {2012},
  month = jul,
  volume = {12},
  pages = {723--734},
  issn = {1674-4527},
  doi = {10.1088/1674-4527/12/7/002},
  abstract = {LAMOST (Large sky Area Multi-Object fiber Spectroscopic Telescope) is a Chinese national scientific research facility operated by National Astronomical Observatories, Chinese Academy of Sciences (NAOC). After two years of commissioning beginning in 2009, the telescope,
instruments, software systems and operations are nearly ready to begin the main science survey. Through a spectral survey of millions of objects in much of the northern sky, LAMOST will enable research in a number of contemporary cutting edge topics in astrophysics, such as discovery of the first generation stars in the Galaxy, pinning down the formation and evolution history of galaxies \textemdash{} especially the Milky Way and its central massive black hole, and looking for signatures of the distribution of dark matter and possible sub-structures in the Milky Way halo. To maximize the scientific potential of the facility, wide national participation and international collaboration have been emphasized. The survey has two major components: the LAMOST
ExtraGAlactic Survey (LEGAS) and the LAMOST Experiment for Galactic Understanding and Exploration (LEGUE). Until LAMOST reaches its full capability, the LEGUE portion of the survey will use the available observing time, starting in 2012. An overview of the LAMOST project and the survey that will be carried out in the next five to six years is presented in this paper. The science plan for the whole LEGUE survey, instrumental specifications, site conditions, and the descriptions of the current on-going pilot survey, including its footprints and target selection algorithm, will be presented as separate papers in this volume.},
  file = {/Users/Oliver/Zotero/storage/TVE7LVFL/Zhao et al. - 2012 - LAMOST spectral survey — An overview.pdf},
  journal = {Research in Astronomy and Astrophysics}
}

@article{zinn+2017,
  title = {Evidence for {{Spatially Correlated Gaia Parallax Errors}} in the {{Kepler Field}}},
  author = {Zinn, Joel C. and Huber, Daniel and Pinsonneault, Marc H. and Stello, Dennis},
  year = {2017},
  month = aug,
  volume = {844},
  pages = {166},
  doi = {10.3847/1538-4357/aa7c1c},
  abstract = {We present evidence for a spatially dependent systematic error in the first data release of Gaia parallaxes based on comparisons to asteroseismic parallaxes in the Kepler field and provide a parameterized model of the angular dependence of these systematics. We report an error of \{0.059\}\textsubscript{-0.004}\textsuperscript{+0.004} mas on scales of 0.\textdegree 3, which decreases for larger scales to become \{0.011\}\textsubscript{-0.004}\textsuperscript{+0.006} mas at 8\textdegree. This is consistent with the{\~ }2\% zero-point offset for the whole sample discussed by Huber et al. and is compatible with the effect predicted by the Gaia team. Our results are robust to dust prescriptions and choices in temperature scales used to calculate asteroseismic parallaxes. We also do not find evidence for significant differences in the signal when using red clump versus red giant stars. Our approach allows us to quantify and map the correlations in an astrophysically interesting field, resulting in a parameterized model of the spatial systematics that can be used to construct a covariance matrix for any work that relies on TGAS parallaxes.},
  file = {/Users/Oliver/Zotero/storage/32NNMH3S/Zinn et al. - 2017 - Evidence for Spatially Correlated Gaia Parallax Er.pdf;/Users/Oliver/Zotero/storage/R3AABSAP/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{zinn+2019,
  title = {Confirmation of the {{Gaia DR2 Parallax Zero}}-Point {{Offset Using Asteroseismology}} and {{Spectroscopy}} in the {{Kepler Field}}},
  author = {Zinn, Joel C. and Pinsonneault, Marc H. and Huber, Daniel and Stello, Dennis},
  year = {2019},
  month = jun,
  volume = {878},
  pages = {136},
  issn = {0004-637X},
  doi = {10.3847/1538-4357/ab1f66},
  abstract = {We present an independent confirmation of the zero-point offset of Gaia Data Release 2 parallaxes using asteroseismic data of evolved stars in the Kepler field. Using well-characterized red giant branch stars from the APOKASC-2 catalog, we identify a Gaia astrometric pseudocolor (\{{$\nu$} \}\textsubscript{eff}\vphantom\{\})- and Gaia G-band magnitude-dependent zero-point offset of \{\textbackslash varpi \}\textsubscript{seis}\vphantom\{\} - \{\textbackslash varpi \}\textsubscript{\{Gaia\vphantom\}}\vphantom\{\} = 52.8 {$\pm$} 2.4 (rand.) {$\pm$} 8.6 (syst.) - (150.7 {$\pm$} 22.7)(\{{$\nu$} \}\textsubscript{eff}\vphantom\{\} - 1.5) - (4.21 {$\pm$} 0.77)(G - 12.2) {$\mu$}as, in the sense that Gaia parallaxes are too small. The offset is found in high- and low-extinction samples, as well as among both shell H-burning red giant stars and core He-burning red clump stars. We show that errors in the asteroseismic radius and temperature scales may be distinguished from errors in the Gaia parallax scale. We estimate systematic effects on the inferred global Gaia parallax offset, c, due to radius and temperature systematics, as well as choices in bolometric correction and the adopted form for Gaia parallax spatial correlations. Because of possible spatially correlated parallax errors, as discussed by the Gaia team, our Gaia parallax offset model is specific to the Kepler field, but broadly compatible with the magnitude- and color-dependent offset inferred by the Gaia team and several subsequent investigations using independent methods.},
  file = {/Users/Oliver/Zotero/storage/NQLA5S2J/Zinn et al. - 2019 - Confirmation of the Gaia DR2 Parallax Zero-point O.pdf;/Users/Oliver/Zotero/storage/CGMIB2XB/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{zinn+2019a,
  title = {Testing the Radius Scaling Relation with \$\{\textbackslash it \vphantom\}{{Gaia}}\vphantom\{\}\$ {{DR2}} in the \$\{\textbackslash it \vphantom\}{{Kepler}}\vphantom\{\}\$ Field},
  author = {Zinn, Joel C. and Pinsonneault, Marc H. and Huber, Daniel and Stello, Dennis and Stassun, Keivan and Serenelli, Aldo},
  year = {2019},
  month = oct,
  pages = {arXiv:1910.00719},
  abstract = {We compare radii based on \$\{\textbackslash it Gaia\}\$ parallaxes to asteroseismic scaling relation-based radii of \$\textbackslash sim 300\$ dwarfs \$\textbackslash\&\$ subgiants and \$\textbackslash sim 3600\$ first-ascent giants from the \$\{\textbackslash it Kepler\}\$ mission. Systematics due to temperature, bolometric correction, extinction, asteroseismic radius, and the spatially-correlated \$\{\textbackslash it Gaia\}\$ parallax zero-point, contribute to a \$2\textbackslash\%\$ systematic uncertainty on the \$\{\textbackslash it Gaia\}\$-asteroseismic radius agreement. We find that dwarf and giant scaling radii are on a parallactic scale at the \$-2.1 \textbackslash\% \textbackslash pm 0.5 \textbackslash\% \{\textbackslash rm \textbackslash{} (rand.)\} \textbackslash pm 2.0\textbackslash\% \{\textbackslash rm \textbackslash{} (syst.)\}\$ level (dwarfs) and \$+1.7\textbackslash\% \textbackslash pm 0.3\textbackslash\% \{\textbackslash rm \textbackslash{} (rand.)\} \textbackslash pm 2.0\textbackslash\% \{\textbackslash rm (syst.)\}\$ level (giants), supporting the accuracy and precision of scaling relations in this domain. In total, the \$2\textbackslash\%\$ agreement that we find holds for stars spanning radii between \$0.8R\_\{\textbackslash odot\}\$ and \$30 R\_\{\textbackslash odot\}\$. We do, however, see evidence for \$\textbackslash textit\{relative\}\$ errors in scaling radii between dwarfs and giants at the \$4\textbackslash\% \textbackslash pm 0.6\textbackslash\%\$ level, and find evidence of departures from simple scaling relations for radii above \$30 R\_\{\textbackslash odot\}\$. Asteroseismic masses for very metal-poor stars are still overestimated relative to astrophysical priors, but at a reduced level. We see no trend with metallicity in radius agreement for stars with \$-0.5 \<\$ [Fe/H] \$\< +0.5\$. We quantify the spatially-correlated parallax errors in the \$\{\textbackslash it Kepler\}\$ field, which globally agree with the \$\{\textbackslash it Gaia\}\$ team's published covariance model. We provide \$\{\textbackslash it Gaia\}\$ radii, corrected for extinction and the \$\{\textbackslash it Gaia\}\$ parallax zero-point for our full sample of \$\textbackslash sim 3900\$ stars, including dwarfs, subgiants, and first-ascent giants.},
  file = {/Users/Oliver/Zotero/storage/DEBWLB7Z/Zinn et al. - 2019 - Testing the radius scaling relation with $ it Gai.pdf;/Users/Oliver/Zotero/storage/ND8IGKAS/abstract.html},
  journal = {arXiv e-prints},
  language = {en}
}

@misc{zotero-3001,
  title = {Bayesian Evidence and Model Selection | {{Elsevier Enhanced Reader}}},
  doi = {10.1016/j.dsp.2015.06.012},
  file = {/Users/Oliver/Zotero/storage/NY3WPN4R/Bayesian evidence and model selection  Elsevier E.pdf;/Users/Oliver/Zotero/storage/XUYLAU6B/S1051200415001980.html},
  howpublished = {https://reader.elsevier.com/reader/sd/pii/S1051200415001980?token=70470AE39CDBAC8C6A3F4D85108D322C630BE1581CF5BF0B23395AD70C8FDD7FCA81964EFA1C7A189D76D4B7EDEC2F27},
  language = {en}
}

@misc{zotero-3004,
  title = {Home / {{Twitter}}},
  file = {/Users/Oliver/Zotero/storage/76TPCT8N/1262764694294507528.html},
  howpublished = {https://twitter.com/hbs\_eric/status/1262764694294507528/photo/1},
  journal = {Twitter},
  language = {en}
}

@article{zwintz+2017,
  title = {Constraining the Near-Core Rotation of the Gamma {{Doradus}} Star 43 {{Cygni}} Using {{BRITE}}-{{Constellation}} Data},
  author = {Zwintz, Konstanze and Van Reeth, Timothy and Tkachenko, Andrew and Goessl, Stefan and Pigulski, Andrzej and Kuschnig, Rainer and Handler, Gerald and Moffat, Anthony F. J. and Popowicz, Adam and Wade, Gregg and Weiss, Werner W.},
  year = {2017},
  month = oct,
  abstract = {Photometric time series of the \$\textbackslash gamma\$ Dor star 43 Cyg obtained with the BRITE-Constellation nano-satellites allow us to study its pulsational properties in detail and to constrain its interior structure. We aim to find a g-mode period spacing pattern that allows us to determine the near-core rotation rate of 43 Cyg and redetermine the star's fundamental atmospheric parameters and chemical composition. We conducted a frequency analysis using the 156-days long data set obtained with the BRITE-Toronto satellite and employed a suite of MESA/GYRE models to derive the mode identification, asymptotic period spacing and near-core rotation rate. We also used high-resolution, high signal-to-noise ratio spectroscopic data obtained at the 1.2m Mercator telescope with the HERMES spectrograph to redetermine the fundamental atmospheric parameters and chemical composition of 43 Cyg using the software Spectroscopy Made Easy (SME). We detected 43 intrinsic pulsation frequencies and identified 18 of them to be part of a period spacing pattern consisting of prograde dipole modes with an asymptotic period spacing \$\textbackslash Delta \textbackslash Pi\_\{l=1\}\$ of \$2970\^\{+700\}\_\{-570\} \textbackslash rm s\$. The near-core rotation rate was determined to be \$f\_\{\textbackslash rm rot\} = 0.56\^\{+0.12\}\_\{-0.14\}\textbackslash,\textbackslash rm d\^\{-1\}\$. The atmosphere of 43 Cyg shows solar chemical composition at an effective temperature of 7150 \$\textbackslash pm\$ 150 K, a log g of 4.2 \$\textbackslash pm\$ 0.6 dex and

repository: sandorkruk/malatium

repo_name: sandorkruk/malatium