text:
, a new data-driven approach for determining stellar labels from spectroscopic data. The Cannon learns from the ``known'' labels of reference stars how the continuum-normalized spectra depend on these labels by fitting a flexible model at each wavelength; then, The Cannon uses this model to derive labels for the remaining survey stars. We illustrate The Cannon by training the model on only 542 stars in 19 clusters as reference objects, with \{T\}\textsubscript{\{eff\vphantom\}}\vphantom\{\}, \{log\} g, and [\{Fe\}/\{\{H\}\}] as the labels, and then applying it to the spectra of 55,000 stars from APOGEE DR10. The Cannon is very accurate. Its stellar labels compare well to the stars for which APOGEE pipeline (ASPCAP) labels are provided in DR10, with rms differences that are basically identical to the stated ASPCAP uncertainties. Beyond the reference labels, The Cannon makes no use of stellar models nor any line-list, but needs a set of reference objects that span label-space. The Cannon performs well at lower signal-to-noise, as it delivers comparably good labels even at one-ninth the APOGEE observing time. We discuss the limitations of The Cannon and its future potential, particularly, to bring different spectroscopic surveys onto a consistent scale of stellar labels.},
  file = {/Users/Oliver/Zotero/storage/6BMINX6W/Ness et al. - 2015 - The Cannon A data-driven approach to Stellar Labe.pdf;/Users/Oliver/Zotero/storage/NSW86P48/abstract.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {1}
}

@article{ness+2017,
  title = {Galactic {{Doppelganger}}: {{The}} Chemical Similarity among Field Stars and among Stars with a Common Birth Origin},
  shorttitle = {Galactic {{Doppelganger}}},
  author = {Ness, M. and Rix, H.-W. and Hogg, David W. and Casey, A. R. and Holtzman, J. and Fouesneau, M. and Zasowski, G. and Geisler, D. and Shetrone, M. and Minniti, D. and Frinchaboy, Peter M. and {Roman-Lopes}, Alexandre},
  year = {2017},
  month = jan,
  abstract = {We explore to which extent stars within Galactic disk open clusters resemble each other in the high-dimensional space of their photospheric element abundances, and contrast this with pairs of field stars. Our analysis is based on abundances for 20 elements, homogeneously derived from APOGEE spectra (with carefully quantified uncertainties, with a median value of \$\textbackslash sim 0.03\$ dex). We consider 90 red giant stars in seven open clusters and find that most stars within a cluster have abundances in most elements that are indistinguishable (in a \$\textbackslash chi\^2\$-sense) from those of the other members, as expected for stellar birth siblings. An analogous analysis among pairs of \${$>$}1000\$ field stars shows that highly significant abundance differences in the 20-dimensional space can be established for the vast majority of these pairs, and that the APOGEE-based abundance measurements have high discriminating power. However, pairs of field stars whose abundances are indistinguishable even at 0.03\textasciitilde dex precision exist: \$\textbackslash sim 0.3\$ percent of all field star pairs, and \$\textbackslash sim 1.0\$ percent of field star pairs at the same (solar) metallicity [Fe/H] = \$0 \textbackslash pm 0.02\$. Most of these pairs are presumably not birth siblings from the same cluster, but rather doppelganger. Our analysis implies that 'chemical tagging' in the strict sense, identifying birth siblings for typical disk stars through their abundance similarity alone, will not work with such data. However, our approach shows that abundances have extremely valuable information for probabilistic chemo-orbital modeling and combined with velocities, we have identified new cluster members from the field.},
  archivePrefix = {arXiv},
  eprint = {1701.07829},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/C2ZDS898/Ness et al. - 2017 - Galactic Doppelganger The chemical similarity amo.pdf;/Users/Oliver/Zotero/storage/2HWWVITZ/1701.html},
  journal = {arXiv:1701.07829 [astro-ph]},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{nielsen+2013,
  title = {Rotation Periods of 12 000 Main-Sequence {{Kepler}} Stars: {{Dependence}} on Stellar Spectral Type and Comparison with v Sin i Observations},
  shorttitle = {Rotation Periods of 12 000 Main-Sequence {{Kepler}} Stars},
  author = {Nielsen, M. B. and Gizon, L. and Schunker, H. and Karoff, C.},
  year = {2013},
  month = sep,
  volume = {557},
  pages = {L10},
  issn = {0004-6361},
  doi = {10.1051/0004-6361/201321912},
  abstract = {Aims: We aim to measure the starspot rotation periods of active
stars in the Kepler field as a function of spectral type and to extend
reliable rotation measurements from F-, G-, and K-type to M-type stars.
 Methods: Using the Lomb-Scargle periodogram we searched more than
150 000 stellar light curves for periodic brightness variations. We
analyzed periods between 1 and 30 days in eight consecutive Kepler
quarters, where 30 days is an estimated maximum for the validity of the
PDC\_MAP data correction pipeline. We selected stable rotation periods,
i.e., periods that do not vary from the median by more than one day in
at least six of the eight quarters. We averaged the periods for each
stellar spectral class according to B - V color and compared the results
to archival vsini data, using stellar radii estimates from the Kepler
Input Catalog. Results: We report on the stable starspot rotation
periods of 12 151 Kepler stars. We find good agreement between starspot
velocities and vsini data for all F-, G- and early K-type stars. The 795
M-type stars in our sample have a median rotation period of 15.4 days.
We find an excess of M-type stars with periods less than 7.5 days that
are potentially fast-rotating and fully convective. Measuring
photometric variability in multiple Kepler quarters appears to be a
straightforward and reliable way to determine the rotation periods of a
large sample of active stars, including late-type stars.

Table 1 is only available at the CDS via anonymous ftp to http://cdsarc.u-strasbg.fr
(ftp://130.79.128.5) or via http://cdsarc.u-strasbg.fr/viz-bin/qcat?J/A+A/557/L10},
  file = {/Users/Oliver/Zotero/storage/XBJCNPN3/Nielsen et al. - 2013 - Rotation periods of 12 000 main-sequence Kepler st.pdf},
  journal = {Astronomy and Astrophysics},
  keywords = {stars: late-type,stars: rotation,starspots}
}

@article{nielsen+2015,
  title = {Constraining Differential Rotation of {{Sun}}-like Stars from Asteroseismic and Starspot Rotation Periods},
  author = {Nielsen, M. B. and Schunker, H. and Gizon, L. and Ball, W. H.},
  year = {2015},
  month = oct,
  volume = {582},
  pages = {A10},
  doi = {10.1051/0004-6361/201526615},
  abstract = {In previous work, we identified six Sun-like stars observed by Kepler with exceptionally clear asteroseismic signatures of rotation. Here, we show that five of these stars exhibit surface variability suitable for measuring rotation. We compare the rotation periods obtained from light-curve variability with those from asteroseismology in order to further constrain differential rotation. The two rotation measurement methods are found to agree within uncertainties, suggesting that radial differential rotation is weak, as is the case for the Sun. Furthermore, we find significant discrepancies between ages from asteroseismology and from three different gyrochronology relations, implying that stellar age estimation is problematic even for Sun-like stars.},
  file = {/Users/Oliver/Zotero/storage/UD4N7J2L/Nielsen et al. - 2015 - Constraining differential rotation of Sun-like sta.pdf;/Users/Oliver/Zotero/storage/F6Y6MWWV/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  keywords = {Seismic rotation},
  language = {en}
}

@article{nielsen+2017,
  title = {Limits on Radial Differential Rotation in {{Sun}}-like Stars from Parametric Fits to Oscillation Power Spectra},
  author = {Nielsen, M. B. and Schunker, H. and Gizon, L. and Schou, J. and Ball, W. H.},
  year = {2017},
  month = jun,
  volume = {603},
  pages = {A6},
  doi = {10.1051/0004-6361/201730896},
  abstract = {Context. Rotational shear in Sun-like stars is thought to be an important ingredient in models of stellar dynamos. Thanks to helioseismology, rotation in the Sun is characterized well, but the interior rotation profiles of other Sun-like stars are not so well constrained. Until recently, measurements of rotation in Sun-like stars have focused on the mean rotation, but little progress has been made on measuring or even placing limits on differential rotation. \\
 Aims: Using asteroseismic measurements of rotation we aim to constrain the radial shear in five Sun-like stars observed by the NASA Kepler mission: KIC 004914923, KIC 005184732, KIC 006116048, KIC 006933899, and KIC 010963065. \\
 Methods: We used stellar structure models for these five stars from previous works. These models provide the mass density, mode eigenfunctions, and the convection zone depth, which we used to compute the sensitivity kernels for the rotational frequency splitting of the modes. We used these kernels as weights in a parametric model of the stellar rotation profile of each star, where we allowed different rotation rates for the radiative interior and the convective envelope. This parametric model was incorporated into a fit to the oscillation power spectrum of each of the five Kepler stars. This fit included a prior on the rotation of the envelope, estimated from the rotation of surface magnetic activity measured from the photometric variability. \\
 Results: The asteroseismic measurements without the application of priors are unable to place meaningful limits on the radial shear. Using a prior on the envelope rotation enables us to constrain the interior rotation rate and thus the radial shear. In the five cases that we studied, the interior rotation rate does not differ from the envelope by more than approximately {$\pm$} 30\%. Uncertainties in the rotational splittings are too large to unambiguously determine the sign of the radial shear.},
  file = {/Users/Oliver/Zotero/storage/2YV7ZHIE/Nielsen et al. - 2017 - Limits on radial differential rotation in Sun-like.pdf;/Users/Oliver/Zotero/storage/F2IPFW3M/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  keywords = {Seismic rotation},
  language = {en}
}

@article{nielsen+2019,
  title = {Starspot Rotation Rates vs. Activity Cycle Phase: {{Butterfly}} Diagrams of {{Kepler}} Stars Are Unlike the {{Sun}}'s},
  shorttitle = {Starspot Rotation Rates vs. Activity Cycle Phase},
  author = {Nielsen, M. B. and Gizon, L. and Cameron, R. H. and Miesch, M.},
  year = {2019},
  month = feb,
  volume = {622},
  pages = {A85},
  issn = {0004-6361, 1432-0746},
  doi = {10.1051/0004-6361/201834373},
  abstract = {During the solar magnetic activity cycle the emergence latitudes of sunspots change, leading to the well-known butterfly diagram. This phenomenon is poorly understood for other stars as starspot latitudes are generally unknown. The related changes in starspot rotation rates caused by latitudinal differential rotation can however be measured. Using the set of 3093 Kepler stars with activity cycles identified by Reinhold et al. (2017), we aim to study the temporal change in starspot rotation rates over magnetic activity cycles, and how this relates to the activity level, mean rotation rate, and effective temperature of the star. We measure the photometric variability as a proxy for the magnetic activity and the spot rotation rate in each quarter over the duration of the Kepler mission. We phase-fold these measurements with the cycle period. We perform averages over stars with comparable mean rotation rates and effective temperature at fixed activity-cycle phases. We detect a clear correlation between the variation of activity level and the variation of the starspot rotation rate. The sign and amplitude of this correlation depends on the mean stellar rotation and, to a lesser extent, on the effective temperature. For slowly rotating stars (with periods between 15-28 days) the starspot rotation rates are clearly anti-correlated with the level of activity during the activity cycles. A transition is seen at periods of 10-15 days, where stars with effective temperature above 4200K instead show positive correlation. Our results can be interpreted in terms of a stellar "butterfly diagram", but these appear different from the Sun's as the starspot rotation rates are either in phase or anti-phase with the activity level. Alternatively, the activity cycles seen by Kepler are short (around 2.5 years) and may therefore be secondary cycles, perhaps analogous to the solar quasi-biennial oscillations.},
  archivePrefix = {arXiv},
  eprint = {1812.06414},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/BQUP5IP8/Nielsen et al. - 2019 - Starspot rotation rates vs. activity cycle phase .pdf;/Users/Oliver/Zotero/storage/8RZSN7LZ/1812.html},
  journal = {Astronomy \& Astrophysics},
  keywords = {Astrophysics - Solar and Stellar Astrophysics}
}

@article{north+2016,
  title = {A Simple Model to Describe Intrinsic Stellar Noise for Exoplanet Detection around Red Giants},
  author = {North, Thomas S. H. and Chaplin, William J. and Gilliland, Ronald L. and Huber, Daniel and Campante, Tiago L. and Handberg, Rasmus and Lund, Mikkel N. and Veras, Dimitri and Kuszlewicz, James S. and Farr, Will M.},
  year = {2016},
  month = oct,
  abstract = {In spite of the huge advances in exoplanet research provided by the NASA Kepler Mission, there remain only a small number of transit detections around evolved stars. Here we present a reformulation of the noise properties of red-giant stars, where the intrinsic stellar granulation, and the stellar oscillations described by asteroseismology play a key role. The new noise model is a significant improvement on the current Kepler results for evolved stars. Our noise model may be used to help understand planet detection thresholds for the ongoing K2 and upcoming TESS missions, and serve as a predictor of stellar noise for these missions. As an application of our noise model, we explore the minimum detectable planet radii for red giant stars, and find that Neptune sized planets should be detectable around low luminosity red giant branch stars.},
  archivePrefix = {arXiv},
  eprint = {1610.08688},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/RMZNVMUQ/North et al. - 2016 - A simple model to describe intrinsic stellar noise.pdf;/Users/Oliver/Zotero/storage/56NX8GHN/1610.html},
  journal = {arXiv:1610.08688 [astro-ph]},
  keywords = {AR 01/11/16,Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{nsamba+2016,
  title = {Asteroseismic Modelling of the {{Binary HD}} 176465},
  author = {Nsamba, B. and Monteiro, M. J. P. F. G. and Campante, T. L. and Reese, D. R. and White, T. R. and Hern{\'a}ndez, A. Garc{\'i}a and Jiang, C.},
  year = {2016},
  month = nov,
  abstract = {The detection and analysis of oscillations in binary star systems is critical in understanding stellar structure and evolution. This is partly because such systems have the same initial chemical composition and age. Solar-like oscillations have been detected by Kepler in both components of the asteroseismic binary HD 176465. We present an independent modelling of each star in this binary system. Stellar models generated using MESA (Modules for Experiments in Stellar Astrophysics) were fitted to both the observed individual frequencies and complementary spectroscopic parameters. The individual theoretical oscillation frequencies for the corresponding stellar models were obtained using GYRE as the pulsation code. A Bayesian approach was applied to find the probability distribution functions of the stellar parameters using AIMS (Asteroseismic Inference on a Massive Scale) as the optimisation code. The ages of HD 176465 A and HD 176465 B were found to be 2.81 \$\textbackslash pm\$ 0.48 Gyr and 2.52 \$\textbackslash pm\$ 0.80 Gyr, respectively. These results are in agreement when compared to previous studies carried out using other asteroseismic modelling techniques and gyrochronology.},
  archivePrefix = {arXiv},
  eprint = {1611.05698},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/FJW25S4G/Nsamba et al. - 2016 - Asteroseismic modelling of the Binary HD 176465.pdf;/Users/Oliver/Zotero/storage/8RUTVT63/1611.html},
  journal = {arXiv:1611.05698 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{opatrny+2017,
  title = {Life under a Black Sun},
  author = {Opatrn{\'y}, Tom{\'a}{\v s} and Richterek, Luk{\'a}{\v s} and Bakala, Pavel},
  year = {2017},
  month = jan,
  volume = {85},
  pages = {14--22},
  issn = {0002-9505, 1943-2909},
  doi = {10.1119/1.4966905},
  abstract = {Life is dependent on the income of energy with low entropy and the disposal of energy with high entropy. On Earth, the low-entropy energy is provided by solar radiation and the high-entropy energy is disposed as infrared radiation emitted into the cold space. Here we turn the situation around and assume cosmic background radiation as the low-entropy source of energy for a planet orbiting a black hole into which the high-entropy energy is disposed. We estimate the power that can be produced by thermodynamic processes on such a planet, with a particular interest in planets orbiting a fast rotating Kerr black hole as in the science fiction movie \{\textbackslash em Interstellar\}. We also briefly discuss a reverse Dyson sphere absorbing cosmic background radiation from the outside and dumping waste energy to a black hole inside.},
  archivePrefix = {arXiv},
  eprint = {1601.02897},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/9NU6G3VI/Opatrný et al. - 2017 - Life under a black sun.pdf;/Users/Oliver/Zotero/storage/AEN9FV54/1601.html},
  journal = {American Journal of Physics},
  keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics,General Relativity and Quantum Cosmology,Physics - Optics,Physics - Popular Physics},
  number = {1}
}

@article{ouazzani+2016,
  title = {A New Asteroseismic Diagnostic for Internal Rotation in \$\$\textbackslash backslash\$ Gamma \$ {{Doradus}} Stars},
  author = {Ouazzani, Rhita-Maria and Salmon, SJAJ and Antoci, V. L. and Bedding, T. R. and Murphy, S. J. and Roxburgh, I. W.},
  year = {2016},
  file = {/Users/Oliver/Zotero/storage/EGKUCUEU/1610.06184v2.pdf},
  journal = {arXiv preprint arXiv:1610.06184},
  keywords = {AR 01/11/16}
}

@article{pablo+2017,
  title = {The Most Massive Heartbeat: An in-Depth Analysis of {$\iota$} {{Orionis}}},
  shorttitle = {The Most Massive Heartbeat},
  author = {Pablo, Herbert and Richardson, N. D. and Fuller, J. and Rowe, J. and Moffat, A. F. J. and Kuschnig, R. and Popowicz, A. and Handler, G. and Neiner, C. and Pigulski, A. and Wade, G. A. and Weiss, W. and Buysschaert, B. and Ramiaramanantsoa, T. and Bratcher, A. D. and Gerhartz, C. J. and Greco, J. J. and {Hardegree-Ullman}, K. and Lembryk, L. and Oswald, W. L.},
  year = {2017},
  month = may,
  volume = {467},
  pages = {2494--2503},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stx207},
  file = {/Users/Oliver/Zotero/storage/TNPDM6BX/stx207.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {2}
}

@article{paczynski+stanek1998,
  title = {Galactocentric {{Distance}} with the {{Optical Gravitational Lensing Experiment}} and {{HIPPARCOS Red Clump Stars}}},
  author = {Paczy{\'n}ski, Bohdan and Stanek, Krzysztof Z.},
  year = {1998},
  month = feb,
  volume = {494},
  pages = {L219},
  doi = {10.1086/311181},
  abstract = {We compare red clump stars with parallaxes known to better than 10\% in the Hipparcos catalog and corrected for interstellar extinction with the OGLE red clump stars in Baade's Window, also corrected for interstellar extinction. There are \textasciitilde 600 and \textasciitilde 10,000 such stars in the two data sets, respectively. We find empirically that the average I-band magnitude of red clump stars does not depend on their intrinsic color in the range 0.8\<(V-I)\textsubscript{0}\<1.4. The red clump luminosity function is well represented by a Gaussian with the peak at M\textsubscript{I\textsubscript{0},m}=-0.28 and the dispersion {$\sigma$}\textsubscript{RC}\textasciitilde 0.2 mag. This allows a single-step determination of the distance to the Galactic center and gives R\textsubscript{0}=8.4+/-0.4 kpc. The number of red clump stars is so large that the formal statistical error is only \textasciitilde 1\%. The local stars are relatively blue and have a small color dispersion: \<(V-I)\>=1.01 and {$\sigma$}\textsubscript{(V-I)}=0.08, while for the bulge stars \<(V-I)\textsubscript{0}\>=1.22 and {$\sigma$}\textsubscript{(V-I)\textsubscript{0}}=0.14. Presumably, the bulge population has a broader range and a higher average metallicity than the local disk population.},
  file = {/Users/Oliver/Zotero/storage/TQ4CEHEP/Paczyński and Stanek - 1998 - Galactocentric Distance with the Optical Gravitati.pdf;/Users/Oliver/Zotero/storage/RXLIDSNM/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{pancino+others2016,
  title = {The {{Gaia}}-{{ESO Survey}}: Calibration Strategy},
  shorttitle = {The {{Gaia}}-{{ESO Survey}}},
  author = {Pancino, E. and others},
  year = {2016},
  file = {/Users/Oliver/Zotero/storage/UGT32GDN/1610.06480v1.pdf},
  journal = {arXiv preprint arXiv:1610.06480},
  keywords = {AR 01/11/16}
}

@article{paxton+2011,
  title = {Modules for {{Experiments}} in {{Stellar Astrophysics}} ({{MESA}})},
  author = {Paxton, Bill and Bildsten, Lars and Dotter, Aaron and Herwig, Falk and Lesaffre, Pierre and Timmes, Frank},
  year = {2011},
  month = jan,
  volume = {192},
  pages = {3},
  doi = {10.1088/0067-0049/192/1/3},
  abstract = {Stellar physics and evolution calculations enable a broad range of research in astrophysics. Modules for Experiments in Stellar Astrophysics (MESA) is a suite of open source, robust, efficient, thread-safe libraries for a wide range of applications in computational stellar astrophysics. A one-dimensional stellar evolution module, MESAstar, combines many of the numerical and physics modules for simulations of a wide range of stellar evolution scenarios ranging from very low mass to massive stars, including advanced evolutionary phases. MESAstar solves the fully coupled structure and composition equations simultaneously. It uses adaptive mesh refinement and sophisticated timestep controls, and supports shared memory parallelism based on OpenMP. State-of-the-art modules provide equation of state, opacity, nuclear reaction rates, element diffusion data, and atmosphere boundary conditions. Each module is constructed as a separate Fortran 95 library with its own explicitly defined public interface to facilitate independent development. Several detailed examples indicate the extensive verification and testing that is continuously performed and demonstrate the wide range of capabilities that MESA possesses. These examples include evolutionary tracks of very low mass stars, brown dwarfs, and gas giant planets to very old ages; the complete evolutionary track of a 1 M \textsubscript{sun} star from the pre-main sequence (PMS) to a cooling white dwarf; the solar sound speed profile; the evolution of intermediate-mass stars through the He-core burning phase and thermal pulses on the He-shell burning asymptotic giant branch phase; the interior structure of slowly pulsating B Stars and Beta Cepheids; the complete evolutionary tracks of massive stars from the PMS to the onset of core collapse; mass transfer from stars undergoing Roche lobe overflow; and the evolution of helium accretion onto a neutron star. MESA can be downloaded from the project Web site (\href{http://mesa.sourceforge.net/}{http://mesa.sourceforge.net/}).},
  file = {/Users/Oliver/Zotero/storage/AN2S55VI/Paxton et al. - 2011 - Modules for Experiments in Stellar Astrophysics (M.pdf;/Users/Oliver/Zotero/storage/GPC9R7V8/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en},
  number = {1}
}

@article{paxton+2013,
  title = {Modules for {{Experiments}} in {{Stellar Astrophysics}} ({{MESA}}): {{Planets}}, {{Oscillations}}, {{Rotation}}, and {{Massive Stars}}},
  shorttitle = {Modules for {{Experiments}} in {{Stellar Astrophysics}} ({{MESA}})},
  author = {Paxton, Bill and Cantiello, Matteo and Arras, Phil and Bildsten, Lars and Brown, Edward F. and Dotter, Aaron and Mankovich, Christopher and Montgomery, M. H. and Stello, Dennis and Timmes, F. X. and Townsend, Richard},
  year = {2013},
  month = sep,
  volume = {208},
  pages = {4},
  doi = {10.1088/0067-0049/208/1/4},
  abstract = {We substantially update the capabilities of the open source software package Modules for Experiments in Stellar Astrophysics (MESA), and its one-dimensional stellar evolution module, MESA star. Improvements in MESA star's ability to model the evolution of giant planets now extends its applicability down to masses as low as one-tenth that of Jupiter. The dramatic improvement in asteroseismology enabled by the space-based Kepler and CoRoT missions motivates our full coupling of the ADIPLS adiabatic pulsation code with MESA star. This also motivates a numerical recasting of the Ledoux criterion that is more easily implemented when many nuclei are present at non-negligible abundances. This impacts the way in which MESA star calculates semi-convective and thermohaline mixing. We exhibit the evolution of 3-8 M \textsubscript{{$\Sun$}} stars through the end of core He burning, the onset of He thermal pulses, and arrival on the white dwarf cooling sequence. We implement diffusion of angular momentum and chemical abundances that enable calculations of rotating-star models, which we compare thoroughly with earlier work. We introduce a new treatment of radiation-dominated envelopes that allows the uninterrupted evolution of massive stars to core collapse. This enables the generation of new sets of supernovae, long gamma-ray burst, and pair-instability progenitor models. We substantially modify the way in which MESA star solves the fully coupled stellar structure and composition equations, and we show how this has improved the scaling of MESA's calculational speed on multi-core processors. Updates to the modules for equation of state, opacity, nuclear reaction rates, and atmospheric boundary conditions are also provided. We describe the MESA Software Development Kit that packages all the required components needed to form a unified, maintained, and well-validated build environment for MESA. We also highlight a few tools developed by the community for rapid visualization of MESA star results.},
  file = {/Users/Oliver/Zotero/storage/AL52E8JW/Paxton et al. - 2013 - Modules for Experiments in Stellar Astrophysics (M.pdf;/Users/Oliver/Zotero/storage/8H4T84Q6/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en},
  number = {1}
}

@article{paxton+2015,
  title = {Modules for {{Experiments}} in {{Stellar Astrophysics}} ({{MESA}}): {{Binaries}}, {{Pulsations}}, and {{Explosions}}},
  shorttitle = {Modules for {{Experiments}} in {{Stellar Astrophysics}} ({{MESA}})},
  author = {Paxton, Bill and Marchant, Pablo and Schwab, Josiah and Bauer, Evan B. and Bildsten, Lars and Cantiello, Matteo and Dessart, Luc and Farmer, R. and Hu, H. and Langer, N. and Townsend, R. H. D. and Townsley, Dean M. and Timmes, F. X.},
  year = {2015},
  month = sep,
  volume = {220},
  pages = {15},
  doi = {10.1088/0067-0049/220/1/15},
  abstract = {We substantially update the capabilities of the open-source software instrument Modules for Experiments in Stellar Astrophysics (MESA). MESA can now simultaneously evolve an interacting pair of differentially rotating stars undergoing transfer and loss of mass and angular momentum, greatly enhancing the prior ability to model binary evolution. New MESA capabilities in fully coupled calculation of nuclear networks with hundreds of isotopes now allow MESA to accurately simulate the advanced burning stages needed to construct supernova progenitor models. Implicit hydrodynamics with shocks can now be treated with MESA, enabling modeling of the entire massive star lifecycle, from pre-main-sequence evolution to the onset of core collapse and nucleosynthesis from the resulting explosion. Coupling of the GYRE non-adiabatic pulsation instrument with MESA allows for new explorations of the instability strips for massive stars while also accelerating the astrophysical use of asteroseismology data. We improve the treatment of mass accretion, giving more accurate and robust near-surface profiles. A new MESA capability to calculate weak reaction rates ``on-the-fly'' from input nuclear data allows better simulation of accretion induced collapse of massive white dwarfs and the fate of some massive stars. We discuss the ongoing challenge of chemical diffusion in the strongly coupled plasma regime, and exhibit improvements in MESA that now allow for the simulation of radiative levitation of heavy elements in hot stars. We close by noting that the MESA software infrastructure provides bit-for-bit consistency for all results across all the supported platforms, a profound enabling capability for accelerating MESA's development.},
  file = {/Users/Oliver/Zotero/storage/UFUN2VYI/Paxton et al. - 2015 - Modules for Experiments in Stellar Astrophysics (M.pdf;/Users/Oliver/Zotero/storage/ZHI2ELHJ/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en},
  number = {1}
}

@article{paxton+2017,
  title = {Modules for {{Experiments}} in {{Stellar Astrophysics}} ({{MESA}}): {{Convective Boundaries}}, {{Element Diffusion}}, and {{Massive Star Explosions}}},
  shorttitle = {Modules for {{Experiments}} in {{Stellar Astrophysics}} ({{MESA}})},
  author = {Paxton, Bill and Schwab, Josiah and Bauer, Evan B. and Bildsten, Lars and Blinnikov, Sergei and Duffell, Paul and Farmer, R. and Goldberg, Jared A. and Marchant, Pablo and Sorokina, Elena and Thoul, Anne and Townsend, Richard H. D. and Timmes, F. X.},
  year = {2017},
  month = oct,
  abstract = {We update the capabilities of the software instrument Modules for Experiments in Stellar Astrophysics (MESA) and enhance its ease of use and availability. Our new approach to locating convective boundaries is consistent with the physics of convection, and yields reliable values of the convective core mass during both hydrogen and helium burning phases. Stars with \$M{$<$}8\textbackslash,\{\textbackslash rm M\_\textbackslash odot\}\$ become white dwarfs and cool to the point where the electrons are degenerate and the ions are strongly coupled, a realm now available to study with MESA due to improved treatments of element diffusion, latent heat release, and blending of equations of state. Studies of the final fates of massive stars are extended in MESA by our addition of an approximate Riemann solver that captures shocks and conserves energy to high accuracy during dynamic epochs. We also introduce a 1D capability for modeling the effects of Rayleigh-Taylor instabilities that, in combination with the coupling to a public version of the STELLA radiation transfer instrument, creates new avenues for exploring Type II supernovae properties. These capabilities are exhibited with exploratory models of pair-instability supernova, pulsational pair-instability supernova, and the formation of stellar mass black holes. The applicability of MESA is now widened by the capability of importing multi-dimensional hydrodynamic models into MESA. We close by introducing software modules for handling floating point exceptions and stellar model optimization, and four new software tools -- MESAWeb, MESA-Docker, pyMESA, and mesastar.org -- to enhance MESA's education and research impact.},
  archivePrefix = {arXiv},
  eprint = {1710.08424},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/BRRJ328Q/Paxton et al. - 2017 - Modules for Experiments in Stellar Astrophysics (M.pdf;/Users/Oliver/Zotero/storage/GNXHHVFJ/1710.html},
  journal = {arXiv:1710.08424 [astro-ph]},
  keywords = {Astrophysics - High Energy Astrophysical Phenomena,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{pereira+2017,
  title = {{{SIGS}} - {{Seismic Inferences}} for {{Glitches}} in {{Stars}}},
  author = {Pereira, L. F. R. and Faria, J. P. and Monteiro, M. J. P. F. G.},
  year = {2017},
  month = mar,
  abstract = {The increased amount of high precision seismic data for solar-like stars calls for the existence of tools that can extract information from such data. In the case of the study of acoustic glitches there are no publicly available tools and most existing ones require a deep knowledge of their implementation. In this work a tool is presented that aims to both simplify the interaction with the user and also be capable of working automatically to determine properties of acoustic glitches from seismic data of solar-like stars. This tool is shown to work with both the Sun and other solar analogs but also shows that are still severe limitations to the methods used, when considering smaller datasets.},
  archivePrefix = {arXiv},
  eprint = {1703.04828},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/FAI8HJG5/Pereira et al. - 2017 - SIGS - Seismic Inferences for Glitches in Stars.pdf;/Users/Oliver/Zotero/storage/NJCN28NI/1703.html},
  journal = {arXiv:1703.04828 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{pereira+2019,
  title = {Gaussian Process Modelling of Granulation and Oscillations in Red Giant Stars},
  author = {Pereira, Filipe and Campante, Tiago L. and Cunha, Margarida S. and Faria, Jo{\~a}o P. and Santos, Nuno C. and Barros, Susana C. C. and Demangeon, Olivier and Kuszlewicz, James S. and Corsaro, Enrico},
  year = {2019},
  month = nov,
  volume = {489},
  pages = {5764--5774},
  issn = {0035-8711},
  doi = {10.1093/mnras/stz2405},
  abstract = {The analysis of photometric time series in the context of transiting planet surveys suffers from the presence of stellar signals, often dubbed `stellar noise'. These signals, caused by stellar oscillations and granulation, can usually be disregarded for main-sequence stars, as the stellar contributions average out when phase-folding the light curve. For evolved stars, however, the amplitudes of such signals are larger and the timescales similar to the transit duration of
short-period planets, requiring that they be modelled alongside the transit. With the promise of TESS delivering of the order of
{$\sim$}105 light curves for stars along the red giant branch, there is a need for a method capable of describing the `stellar noise' while simultaneously modelling an exoplanet's transit. In this work, a Gaussian process regression framework is used to model stellar light curves and the method validated by applying it to TESS-like artificial data. Furthermore, the method is used to characterize the stellar oscillations and granulation of a sample of well-studied Kepler
low-luminosity red giant branch stars. The parameters determined are compared to equivalent ones obtained by modelling the power spectrum of the light curve. Results show that the method presented is capable of describing the stellar signals in the time domain and can also return an accurate and precise measurement of {$\nu$}max, i.e. the
frequency of maximum oscillation amplitude. Preliminary results show that using the method in transit modelling improves the precision and accuracy of the ratio between the planetary and stellar radius,
Rp/R{$\star$}. The method's implementation is
publicly available.1},
  file = {/Users/Oliver/Zotero/storage/6JI4KTNX/Pereira et al. - 2019 - Gaussian process modelling of granulation and osci.pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {asteroseismology,methods: data analysis,planets and satellites: fundamental parameters,stars: oscillations,techniques: photometric}
}

@article{perez+granger2007,
  title = {{{IPython}}: {{A System}} for {{Interactive Scientific Computing}}},
  shorttitle = {{{IPython}}},
  author = {Perez, Fernando and Granger, Brian E.},
  year = {2007},
  volume = {9},
  pages = {21--29},
  doi = {10.1109/MCSE.2007.53},
  abstract = {Not Available},
  journal = {Computing in Science and Engineering}
}

@article{pietrukowicz+2017,
  title = {Blue Large-Amplitude Pulsators as a New Class of Variable Stars},
  author = {Pietrukowicz, P. and Dziembowski, W. A. and Latour, M. and Angeloni, R. and Poleski, R. and {di Mille}, F. and Soszynski, I. and Udalski, A. and Szymanski, M. K. and Wyrzykowski, L. and Kozlowski, S. and Skowron, J. and Skowron, D. and Mroz, P. and Pawlak, M. and Ulaczyk, K.},
  year = {2017},
  month = jun,
  volume = {1},
  pages = {0166},
  issn = {2397-3366},
  doi = {10.1038/s41550-017-0166},
  abstract = {Regular intrinsic brightness variations observed in many stars are caused by pulsations. These pulsations provide information on the global and structural parameters of the star. The pulsation periods range from seconds to years, depending on the compactness of the star and properties of the matter that forms its outer layers. Here, we report the discovery of more than a dozen of previously unknown short-period variable stars: blue large-amplitude pulsators. These objects show very regular brightness variations with periods in the range of 20-40 min and amplitudes of 0.2-0.4 mag in the optical passbands. The phased light curves have a characteristic sawtooth shape, similar to the shape of classical Cepheids and RR Lyrae-type stars pulsating in the fundamental mode. The objects are significantly bluer than main sequence stars observed in the same fields, which indicates that all of them are hot stars. Follow-up spectroscopy confirms a high surface temperature of about 30,000 K. Temperature and colour changes over the cycle prove the pulsational nature of the variables. However, large-amplitude pulsations at such short periods are not observed in any known type of stars, including hot objects. Long-term photometric observations show that the variable stars are very stable over time. Derived rates of period change are of the order of 10\^-7 per year and, in most cases, they are positive. According to pulsation theory, such large-amplitude oscillations may occur in evolved low-mass stars that have inflated helium-enriched envelopes. The evolutionary path that could lead to such stellar configurations remains unknown.},
  archivePrefix = {arXiv},
  eprint = {1706.07802},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/VR9H5495/Pietrukowicz et al. - 2017 - Blue large-amplitude pulsators as a new class of v.pdf;/Users/Oliver/Zotero/storage/BQ2VDI7K/1706.html},
  journal = {Nature Astronomy},
  keywords = {Astrophysics - Solar and Stellar Astrophysics}
}

@article{pinsonneault+2014,
  title = {The {{APOKASC Catalog}}: {{An Asteroseismic}} and {{Spectroscopic Joint Survey}} of {{Targets}} in the {{Kepler Fields}}},
  shorttitle = {The {{APOKASC Catalog}}},
  author = {Pinsonneault, Marc H. and Elsworth, Yvonne and Epstein, Courtney and Hekker, Saskia and M{\'e}sz{\'a}ros, Sz and Chaplin, William J. and Johnson, Jennifer A. and Garc{\'i}a, Rafael A. and Holtzman, Jon and Mathur, Savita and Garc{\'i}a P{\'e}rez, Ana and Silva Aguirre, Victor and Girardi, L{\'e}o and Basu, Sarbani and Shetrone, Matthew and Stello, Dennis and Allende Prieto, Carlos and An, Deokkeun and Beck, Paul and Beers, Timothy C. and Bizyaev, Dmitry and Bloemen, Steven and Bovy, Jo and Cunha, Katia and De Ridder, Joris and Frinchaboy, Peter M. and {Garc{\'i}a-Hern{\'a}ndez}, D. A. and Gilliland, Ronald and Harding, Paul and Hearty, Fred R. and Huber, Daniel and Ivans, Inese and Kallinger, Thomas and Majewski, Steven R. and Metcalfe, Travis S. and Miglio, Andrea and Mosser, Benoit and Muna, Demitri and Nidever, David L. and Schneider, Donald P. and Serenelli, Aldo and Smith, Verne V. and Tayar, Jamie and Zamora, Olga and Zasowski, Gail},
  year = {2014},
  month = dec,
  volume = {215},
  pages = {19},
  doi = {10.1088/0067-0049/215/2/19},
  abstract = {We present the first APOKASC catalog of spectroscopic and asteroseismic properties of 1916 red giants observed in the Kepler fields. The spectroscopic parameters provided from the Apache Point Observatory Galactic Evolution Experiment project are complemented with asteroseismic surface gravities, masses, radii, and mean densities determined by members of the Kepler Asteroseismology Science Consortium. We assess both random and systematic sources of error and include a discussion of sample selection for giants in the Kepler fields. Total uncertainties in the main catalog properties are of the order of 80 K in T \textsubscript{eff}, 0.06 dex in [M/H], 0.014 dex in log g, and 12\% and 5\% in mass and radius, respectively; these reflect a combination of systematic and random errors. Asteroseismic surface gravities are substantially more precise and accurate than spectroscopic ones, and we find good agreement between their mean values and the calibrated spectroscopic surface gravities. There are, however, systematic underlying trends with T \textsubscript{eff} and log g. Our effective temperature scale is between 0 and 200 K cooler than that expected from the infrared flux method, depending on the adopted extinction map, which provides evidence for a lower value on average than that inferred for the Kepler Input Catalog (KIC). We find a reasonable correspondence between the photometric KIC and spectroscopic APOKASC metallicity scales, with increased dispersion in KIC metallicities as the absolute metal abundance decreases, and offsets in T \textsubscript{eff} and log g consistent with those derived in the literature. We present mean fitting relations between APOKASC and KIC observables and discuss future prospects, strengths, and limitations of the catalog data.},
  file = {/Users/Oliver/Zotero/storage/SNQVJ2YC/Pinsonneault et al. - 2014 - The APOKASC Catalog An Asteroseismic and Spectros.pdf;/Users/Oliver/Zotero/storage/TXTZGSHZ/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal Supplement Series},
  language = {en},
  number = {2}
}

@article{pinsonneault+2018,
  title = {The {{Second APOKASC Catalog}}: {{The Empirical Approach}}},
  shorttitle = {The {{Second APOKASC Catalog}}},
  author = {Pinsonneault, Marc H. and Elsworth, Yvonne P. and Tayar, Jamie and Serenelli, Aldo and Stello, Dennis and Zinn, Joel and Mathur, Savita and Garc{\'i}a, Rafael A. and Johnson, Jennifer A. and Hekker, Saskia and Huber, Daniel and Kallinger, Thomas and M{\'e}sz{\'a}ros, Szabolcs and Mosser, Benoit and Stassun, Keivan and Girardi, L{\'e}o and Rodrigues, Tha{\'i}se S. and Silva Aguirre, Victor and An, Deokkeun and Basu, Sarbani and Chaplin, William J. and Corsaro, Enrico and Cunha, Katia and {Garc{\'i}a-Hern{\'a}ndez}, D. A. and Holtzman, Jon and J{\"o}nsson, Henrik and Shetrone, Matthew and Smith, Verne V. and Sobeck, Jennifer S. and Stringfellow, Guy S. and Zamora, Olga and Beers, Timothy C. and {Fern{\'a}ndez-Trincado}, J. G. and Frinchaboy, Peter M. and Hearty, Fred R. and Nitschelm, Christian},
  year = {2018},
  month = apr,
  pages = {arXiv:1804.09983},
  abstract = {We present a catalog of stellar properties for a large sample of 6676 evolved stars with APOGEE spectroscopic parameters and \textbackslash textit\{Kepler\} asteroseismic data analyzed using five independent techniques. Our data includes evolutionary state, surface gravity, mean density, mass, radius, age, and the spectroscopic and asteroseismic measurements used to derive them. We employ a new empirical approach for combining asteroseismic measurements from different methods, calibrating the inferred stellar parameters, and estimating uncertainties. With high statistical significance, we find that asteroseismic parameters inferred from the different pipelines have systematic offsets that are not removed by accounting for differences in their solar reference values. We include theoretically motivated corrections to the large frequency spacing (\$\textbackslash Delta \textbackslash nu\$) scaling relation, and we calibrate the zero point of the frequency of maximum power (\$\textbackslash nu\_\{\textbackslash rm max\}\$) relation to be consistent with masses and radii for members of star clusters. For most targets, the parameters returned by different pipelines are in much better agreement than would be expected from the pipeline-predicted random errors, but 22\textbackslash\% of them had at least one method not return a result and a much larger measurement dispersion. This supports the usage of multiple analysis techniques for asteroseismic stellar population studies. The measured dispersion in mass estimates for fundamental calibrators is consistent with our error model, which yields median random and systematic mass uncertainties for RGB stars of order 4\textbackslash\%. Median random and systematic mass uncertainties are at the 9\textbackslash\% and 8\textbackslash\% level respectively for RC stars.},
  file = {/Users/Oliver/Zotero/storage/RCSNPNZU/Pinsonneault et al. - 2018 - The Second APOKASC Catalog The Empirical Approach.pdf;/Users/Oliver/Zotero/storage/ZKZ7MKF6/ui.adsabs.harvard.edu.html},
  journal = {ArXiv e-prints},
  language = {en}
}

@article{planckcollaboration+2019,
  title = {Planck 2018 Results. {{VI}}. {{Cosmological}} Parameters},
  author = {{Planck Collaboration} and Aghanim, N. and Akrami, Y. and Ashdown, M. and Aumont, J. and Baccigalupi, C. and Ballardini, M. and Banday, A. J. and Barreiro, R. B. and Bartolo, N. and Basak, S. and Battye, R. and Benabed, K. and Bernard, J.-P. and Bersanelli, M. and Bielewicz, P. and Bock, J. J. and Bond, J. R. and Borrill, J. and Bouchet, F. R. and Boulanger, F. and Bucher, M. and Burigana, C. and Butler, R. C. and Calabrese, E. and Cardoso, J.-F. and Carron, J. and Challinor, A. and Chiang, H. C. and Chluba, J. and Colombo, L. P. L. and Combet, C. and Contreras, D. and Crill, B. P. and Cuttaia, F. and {de Bernardis}, P. and {de Zotti}, G. and Delabrouille, J. and Delouis, J.-M. and Di Valentino, E. and Diego, J. M. and Dor{\'e}, O. and Douspis, M. and Ducout, A. and Dupac, X. and Dusini, S. and Efstathiou, G. and Elsner, F. and En{\ss}lin, T. A. and Eriksen, H. K. and Fantaye, Y. and Farhang, M. and Fergusson, J. and {Fernandez-Cobos}, R. and Finelli, F. and Forastieri, F. and Frailis, M. and Fraisse, A. A. and Franceschi, E. and Frolov, A. and Galeotta, S. and Galli, S. and Ganga, K. and {G{\'e}nova-Santos}, R. T. and Gerbino, M. and Ghosh, T. and {Gonz{\'a}lez-Nuevo}, J. and G{\'o}rski, K. M. and Gratton, S. and Gruppuso, A. and Gudmundsson, J. E. and Hamann, J. and Handley, W. and Hansen, F. K. and Herranz, D. and Hildebrandt, S. R. and Hivon, E. and Huang, Z. and Jaffe, A. H. and Jones, W. C. and Karakci, A. and Keih{\"a}nen, E. and Keskitalo, R. and Kiiveri, K. and Kim, J. and Kisner, T. S. and Knox, L. and Krachmalnicoff, N. and Kunz, M. and {Kurki-Suonio}, H. and Lagache, G. and Lamarre, J.-M. and Lasenby, A. and Lattanzi, M. and Lawrence, C. R. and Jeune, M. Le and Lemos, P. and Lesgourgues, J. and Levrier, F. and Lewis, A. and Liguori, M. and Lilje, P. B. and Lilley, M. and Lindholm, V. and {L{\'o}pez-Caniego}, M. and Lubin, P. M. and Ma, Y.-Z. and {Mac{\'i}as-P{\'e}rez}, J. F. and Maggio, G. and Maino, D. and Mandolesi, N. and Mangilli, A. and {Marcos-Caballero}, A. and Maris, M. and Martin, P. G. and Martinelli, M. and {Mart{\'i}nez-Gonz{\'a}lez}, E. and Matarrese, S. and Mauri, N. and McEwen, J. D. and Meinhold, P. R. and Melchiorri, A. and Mennella, A. and Migliaccio, M. and Millea, M. and Mitra, S. and {Miville-Desch{\^e}nes}, M.-A. and Molinari, D. and Montier, L. and Morgante, G. and Moss, A. and Natoli, P. and {N{\o}rgaard-Nielsen}, H. U. and Pagano, L. and Paoletti, D. and Partridge, B. and Patanchon, G. and Peiris, H. V. and Perrotta, F. and Pettorino, V. and Piacentini, F. and Polastri, L. and Polenta, G. and Puget, J.-L. and Rachen, J. P. and Reinecke, M. and Remazeilles, M. and Renzi, A. and Rocha, G. and Rosset, C. and Roudier, G. and {Rubi{\~n}o-Mart{\'i}n}, J. A. and {Ruiz-Granados}, B. and Salvati, L. and Sandri, M. and Savelainen, M. and Scott, D. and Shellard, E. P. S. and Sirignano, C. and Sirri, G. and Spencer, L. D. and Sunyaev, R. and {Suur-Uski}, A.-S. and Tauber, J. A. and Tavagnacco, D. and Tenti, M. and Toffolatti, L. and Tomasi, M. and Trombetti, T. and Valenziano, L. and Valiviita, J. and Van Tent, B. and Vibert, L. and Vielva, P. and Villa, F. and Vittorio, N. and Wandelt, B. D. and Wehus, I. K. and White, M. and White, S. D. M. and Zacchei, A. and Zonca, A.},
  year = {2019},
  month = sep,
  abstract = {We present cosmological parameter results from the final full-mission Planck measurements of the CMB anisotropies. We find good consistency with the standard spatially-flat 6-parameter \$\textbackslash Lambda\$CDM cosmology having a power-law spectrum of adiabatic scalar perturbations (denoted "base \$\textbackslash Lambda\$CDM" in this paper), from polarization, temperature, and lensing, separately and in combination. A combined analysis gives dark matter density \$\textbackslash Omega\_c h\^2 = 0.120\textbackslash pm 0.001\$, baryon density \$\textbackslash Omega\_b h\^2 = 0.0224\textbackslash pm 0.0001\$, scalar spectral index \$n\_s = 0.965\textbackslash pm 0.004\$, and optical depth \$\textbackslash tau = 0.054\textbackslash pm 0.007\$ (in this abstract we quote \$68\textbackslash,\textbackslash\%\$ confidence regions on measured parameters and \$95\textbackslash,\textbackslash\%\$ on upper limits). The angular acoustic scale is measured to \$0.03\textbackslash,\textbackslash\%\$ precision, with \$100\textbackslash theta\_*=1.0411\textbackslash pm 0.0003\$. These results are only weakly dependent on the cosmological model and remain stable, with somewhat increased errors, in many commonly considered extensions. Assuming the base-\$\textbackslash Lambda\$CDM cosmology, the inferred late-Universe parameters are: Hubble constant \$H\_0 = (67.4\textbackslash pm 0.5)\$km/s/Mpc; matter density parameter \$\textbackslash Omega\_m = 0.315\textbackslash pm 0.007\$; and matter fluctuation amplitude \$\textbackslash sigma\_8 = 0.811\textbackslash pm 0.006\$. We find no compelling evidence for extensions to the base-\$\textbackslash Lambda\$CDM model. Combining with BAO we constrain the effective extra relativistic degrees of freedom to be \$N\_\{\textbackslash rm eff\} = 2.99\textbackslash pm 0.17\$, and the neutrino mass is tightly constrained to \$\textbackslash sum m\_\textbackslash nu{$<$} 0.12\$eV. The CMB spectra continue to prefer higher lensing amplitudes than predicted in base -\$\textbackslash Lambda\$CDM at over \$2\textbackslash,\textbackslash sigma\$, which pulls some parameters that affect the lensing amplitude away from the base-\$\textbackslash Lambda\$CDM model; however, this is not supported by the lensing reconstruction or (in models that also change the background geometry) BAO data. (Abridged)},
  archivePrefix = {arXiv},
  eprint = {1807.06209},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/AC6NCHGC/Planck Collaboration et al. - 2019 - Planck 2018 results. VI. Cosmological parameters.pdf;/Users/Oliver/Zotero/storage/2K9KT33Q/1807.html},
  journal = {arXiv:1807.06209 [astro-ph]},
  keywords = {Astrophysics - Cosmology and Nongalactic Astrophysics},
  primaryClass = {astro-ph}
}

@article{plaskett1916,
  title = {A {{Variation}} in the {{Solar Rotation}}},
  author = {Plaskett, H. H.},
  year = {1916},
  month = mar,
  volume = {43},
  pages = {145},
  issn = {0004-637X},
  doi = {10.1086/142239},
  abstract = {Not Available},
  file = {/Users/Oliver/Zotero/storage/AP5HDKD2/Plaskett - 1916 - A Variation in the Solar Rotation.pdf},
  journal = {The Astrophysical Journal}
}

@book{poisson1821,
  title = {{M\'emoire sur l'integration des \'equations lin\'eaires aux diff\'erences partielles; par M. Poisson. Lu \`a l'Acad\'emie des Sciences, le 31 D\'ecembre 1821}},
  author = {Poisson, Simeon Denis},
  year = {1821},
  googlebooks = {TzdANIuLeFcC},
  language = {fr}
}

@article{prat+2016,
  title = {Seismic Diagnosis from Gravity Modes Strongly Affected by Rotation},
  author = {Prat, Vincent and Mathis, St{\'e}phane and Ligni{\`e}res, Fran{\c c}ois and Ballot, J{\'e}r{\^o}me and Culpin, Pierre-Marie},
  year = {2016},
  month = oct,
  abstract = {Most of the information we have about the internal rotation of stars comes from modes that are weakly affected by rotation, for example by using rotational splittings. In contrast, we present here a method, based on the asymptotic theory of Prat et al. (2016), which allows us to analyse the signature of rotation where its effect is the most important, that is in low-frequency gravity modes that are strongly affected by rotation. For such modes, we predict two spectral patterns that could be confronted to observed spectra and those computed using fully two-dimensional oscillation codes.},
  archivePrefix = {arXiv},
  eprint = {1610.08674},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/5GJZFEKK/Prat et al. - 2016 - Seismic diagnosis from gravity modes strongly affe.pdf;/Users/Oliver/Zotero/storage/M3AACCSP/1610.html},
  journal = {arXiv:1610.08674 [astro-ph]},
  keywords = {AR 01/11/16,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{prieto2016,
  title = {Learning about Stars from Their Colors},
  author = {Prieto, C. Allende},
  year = {2016},
  file = {/Users/Oliver/Zotero/storage/S7BN9WE9/1609.08557v2.pdf},
  journal = {arXiv preprint arXiv:1609.08557}
}

@article{prsa+2016,
  title = {Nominal {{Values}} for {{Selected Solar}} and {{Planetary Quantities}}: {{IAU}} 2015 {{Resolution B3}}},
  shorttitle = {Nominal {{Values}} for {{Selected Solar}} and {{Planetary Quantities}}},
  author = {Pr{\v s}a, Andrej and Harmanec, Petr and Torres, Guillermo and Mamajek, Eric and Asplund, Martin and Capitaine, Nicole and {Christensen-Dalsgaard}, J{\o}rgen and Depagne, {\'E}ric and Haberreiter, Margit and Hekker, Saskia and Hilton, James and Kopp, Greg and Kostov, Veselin and Kurtz, Donald W. and Laskar, Jacques and Mason, Brian D. and Milone, Eugene F. and Montgomery, Michele and Richards, Mercedes and Schmutz, Werner and Schou, Jesper and Stewart, Susan G.},
  year = {2016},
  month = aug,
  volume = {152},
  pages = {41},
  doi = {10.3847/0004-6256/152/2/41},
  abstract = {In this brief communication we provide the rationale for and the outcome of the International Astronomical Union (IAU) resolution vote at the XXIXth General Assembly in Honolulu, Hawaii, in 2015, on recommended nominal conversion constants for selected solar and planetary properties. The problem addressed by the resolution is a lack of established conversion constants between solar and planetary values and SI units: a missing standard has caused a proliferation of solar values (e.g., solar radius, solar irradiance, solar luminosity, solar effective temperature, and solar mass parameter) in the literature, with cited solar values typically based on best estimates at the time of paper writing. As precision of observations increases, a set of consistent values becomes increasingly important. To address this, an IAU Working Group on Nominal Units for Stellar and Planetary Astronomy formed in 2011, uniting experts from the solar, stellar, planetary, exoplanetary, and fundamental astronomy, as well as from general standards fields to converge on optimal values for nominal conversion constants. The effort resulted in the IAU 2015 Resolution B3, passed at the IAU General Assembly by a large majority. The resolution recommends the use of nominal solar and planetary values, which are by definition exact and are expressed in SI units. These nominal values should be understood as conversion factors only, not as the true solar/planetary properties or current best estimates. Authors and journal editors are urged to join in using the standard values set forth by this resolution in future work and publications to help minimize further confusion.},
  file = {/Users/Oliver/Zotero/storage/K46LH3YS/Prša et al. - 2016 - Nominal Values for Selected Solar and Planetary Qu.pdf;/Users/Oliver/Zotero/storage/HIBBX3GP/abstract.html},
  journal = {The Astronomical Journal},
  language = {en},
  number = {2}
}

@article{raghavan+2010,
  title = {A {{Survey}} of {{Stellar Families}}: {{Multiplicity}} of {{Solar}}-Type {{Stars}}},
  shorttitle = {A {{Survey}} of {{Stellar Families}}},
  author = {Raghavan, Deepak and McAlister, Harold A. and Henry, Todd J. and Latham, David W. and Marcy, Geoffrey W. and Mason, Brian D. and Gies, Douglas R. and White, Russel J. and {ten Brummelaar}, Theo A.},
  year = {2010},
  month = sep,
  volume = {190},
  pages = {1--42},
  issn = {0067-0049},
  doi = {10.1088/0067-0049/190/1/1},
  abstract = {We present the results of a comprehensive assessment of companions to solar-type stars. A sample of 454 stars, including the Sun, was selected from the Hipparcos catalog with {$\pi>$}40 mas,
{$\sigma\pi$}/{$\pi$} {$<$} 0.05, 0.5 {$<$}= B - V {$<$}= 1.0
(\textasciitilde F6-K3), and constrained by absolute magnitude and color to exclude evolved stars. These criteria are equivalent to selecting all dwarf and subdwarf stars within 25 pc with V-band flux between 0.1 and 10 times that of the Sun, giving us a physical basis for the term "solar-type." New observational aspects of this work include surveys for (1) very close companions with long-baseline interferometry at the Center for High Angular Resolution Astronomy Array, (2) close companions with speckle interferometry, and (3) wide proper-motion companions identified by blinking multi-epoch archival images. In addition, we include the results from extensive radial-velocity monitoring programs and evaluate companion information from various catalogs covering many different techniques. The results presented here include four new common
proper-motion companions discovered by blinking archival images. Additionally, the spectroscopic data searched reveal five new stellar companions. Our synthesis of results from many methods and sources results in a thorough evaluation of stellar and brown dwarf companions to nearby Sun-like stars. The overall observed fractions of single, double, triple, and higher-order systems are 56\% {$\pm$} 2\%, 33\%
{$\pm$} 2\%, 8\% {$\pm$} 1\%, and 3\% {$\pm$} 1\%, respectively, counting
all confirmed stellar and brown dwarf companions. If all candidate, i.e., unconfirmed, companions identified are found to be real, the percentages would change to 54\% {$\pm$} 2\%, 34\% {$\pm$} 2\%, 9\%
{$\pm$} 2\%, and 3\% {$\pm$} 1\%, respectively. Our completeness analysis
indicates that only a few undiscovered companions remain in this well-studied sample, implying that the majority (54\% {$\pm$} 2\%) of
solar-type stars are single, in contrast to the results of prior multiplicity studies. Our sample is large enough to enable a check of the multiplicity dependence on various physical parameters by analyzing appropriate subsamples. Bluer, more massive stars are seen as more likely to have companions than redder, less massive ones, consistent with the trend seen over the entire spectral range. Systems with larger interaction cross sections, i.e., those with more than two components or long orbital periods, are preferentially younger, suggesting that companions may be stripped over time by dynamical interactions. We confirm the planet-metallicity correlation (i.e., higher metallicity stars are more likely to host planets), but are unable to check it for brown dwarfs due to the paucity of such companions, implying that the brown dwarf desert extends over all separation regimes. We find no correlation between stellar companions and metallicity for B - V {$<$} 0.625, but among the redder subset, metal-poor stars ([Fe/H] {$<$}-0.3) are more likely to have companions with a 2.4{$\sigma$} significance. The orbital-period distribution of companions is unimodal and roughly log normal with a peak and median of about 300 years. The
period-eccentricity relation shows the expected circularization for periods below 12 days, caused by tidal forces over the age of the Galaxy, followed by a roughly flat distribution. The mass-ratio
distribution shows a preference for like-mass pairs, which occur more frequently in relatively close pairs. The fraction of planet hosts among single, binary, and multiple systems are statistically
indistinguishable, suggesting that planets are as likely to form around single stars as they are around components of binary or multiple systems with sufficiently wide separations. This, along with the preference of long orbital periods among stellar systems, increases the space around stars conducive for planet formation, and perhaps life.},
  file = {/Users/Oliver/Zotero/storage/2TZ6ZYXR/Raghavan et al. - 2010 - A Survey of Stellar Families Multiplicity of Sola.pdf},
  journal = {The Astrophysical Journal Supplement Series},
  keywords = {binaries: general,planetary systems,stars: solar-type,stars: statistics,surveys}
}

@book{rasmussen+williams2006,
  title = {Gaussian Processes for Machine Learning},
  author = {Rasmussen, Carl Edward and Williams, Christopher K. I.},
  year = {2006},
  publisher = {{MIT Press}},
  address = {{Cambridge, Mass}},
  file = {/Users/Oliver/Zotero/storage/8NZFZ87G/Rasmussen and Williams - 2006 - Gaussian processes for machine learning.pdf},
  isbn = {978-0-262-18253-9},
  keywords = {Data processing,Gaussian processes,Machine learning,Mathematical models},
  language = {en},
  lccn = {QA274.4 .R37 2006},
  series = {Adaptive Computation and Machine Learning}
}

@article{rauer+2014,
  title = {The {{PLATO}} 2.0 Mission},
  author = {Rauer, H. and Catala, C. and Aerts, C. and Appourchaux, T. and Benz, W. and Brandeker, A. and {Christensen-Dalsgaard}, J. and Deleuil, M. and Gizon, L. and Goupil, M.-J. and G{\"u}del, M. and {Janot-Pacheco}, E. and {Mas-Hesse}, M. and Pagano, I. and Piotto, G. and Pollacco, D. and Santos, {\.C}. and Smith, A. and Su{\'a}rez, J.-C. and Szab{\'o}, R. and Udry, S. and Adibekyan, V. and Alibert, Y. and Almenara, J.-M. and {Amaro-Seoane}, P. and Eiff, M. Ammler-von and Asplund, M. and Antonello, E. and Barnes, S. and Baudin, F. and Belkacem, K. and Bergemann, M. and Bihain, G. and Birch, A. C. and Bonfils, X. and Boisse, I. and Bonomo, A. S. and Borsa, F. and Brand{\~a}o, I. M. and Brocato, E. and Brun, S. and Burleigh, M. and Burston, R. and Cabrera, J. and Cassisi, S. and Chaplin, W. and Charpinet, S. and Chiappini, C. and Church, R. P. and Csizmadia, Sz. and Cunha, M. and Damasso, M. and Davies, M. B. and Deeg, H. J. and D{\'i}az, R. F. and Dreizler, S. and Dreyer, C. and Eggenberger, P. and Ehrenreich, D. and Eigm{\"u}ller, P. and Erikson, A. and Farmer, R. and Feltzing, S. and {de Oliveira Fialho}, F. and Figueira, P. and Forveille, T. and Fridlund, M. and Garc{\'i}a, R. A. and Giommi, P. and Giuffrida, G. and Godolt, M. and {Gomes da Silva}, J. and Granzer, T. and Grenfell, J. L. and {Grotsch-Noels}, A. and G{\"u}nther, E. and Haswell, C. A. and Hatzes, A. P. and H{\'e}brard, G. and Hekker, S. and Helled, R. and Heng, K. and Jenkins, J. M. and Johansen, A. and Khodachenko, M. L. and Kislyakova, K. G. and Kley, W. and Kolb, U. and Krivova, N. and Kupka, F. and Lammer, H. and Lanza, A. F. and Lebreton, Y. and Magrin, D. and {Marcos-Arenal}, P. and Marrese, P. M. and Marques, J. P. and Martins, J. and Mathis, S. and Mathur, S. and Messina, S. and Miglio, A. and Montalban, J. and Montalto, M. and Monteiro, M. J. P. F. G. and Moradi, H. and Moravveji, E. and Mordasini, C. and Morel, T. and Mortier, A. and Nascimbeni, V. and Nelson, R. P. and Nielsen, M. B. and Noack, L. and Norton, A. J. and Ofir, A. and Oshagh, M. and Ouazzani, R.-M. and P{\'a}pics, P. and Parro, V. C. and Petit, P. and Plez, B. and Poretti, E. and Quirrenbach, A. and Ragazzoni, R. and Raimondo, G. and Rainer, M. and Reese, D. R. and Redmer, R. and Reffert, S. and {Rojas-Ayala}, B. and Roxburgh, I. W. and Salmon, S. and Santerne, A. and Schneider, J. and Schou, J. and Schuh, S. and Schunker, H. and {Silva-Valio}, A. and Silvotti, R. and Skillen, I. and Snellen, I. and Sohl, F. and Sousa, S. G. and Sozzetti, A. and Stello, D. and Strassmeier, K. G. and {\v S}vanda, M. and Szab{\'o}, Gy. M. and Tkachenko, A. and Valencia, D. and Van Grootel, V. and Vauclair, S. D. and Ventura, P. and Wagner, F. W. and Walton, N. A. and Weingrill, J. and Werner, S. C. and Wheatley, P. J. and Zwintz, K.},
  year = {2014},
  month = nov,
  volume = {38},
  pages = {249--330},
  issn = {0922-6435},
  doi = {10.1007/s10686-014-9383-4},
  abstract = {PLATO 2.0 has recently been selected for ESA's M3 launch opportunity (2022/24). Providing accurate key planet parameters (radius, mass, density and age) in statistical numbers, it addresses fundamental questions such as: How do planetary systems form and evolve? Are there other systems with planets like ours, including potentially habitable planets? The PLATO 2.0 instrument consists of 34 small aperture
telescopes (32 with 25 s readout cadence and 2 with 2.5 s candence) providing a wide field-of-view (2232 deg 2) and a large photometric magnitude range (4-16 mag). It focusses on bright (4-11 mag) stars in wide fields to detect and characterize planets down to
Earth-size by photometric transits, whose masses can then be determined by ground-based radial-velocity follow-up measurements. Asteroseismology will be performed for these bright stars to obtain highly accurate stellar parameters, including masses and ages. The combination of bright targets and asteroseismology results in high accuracy for the bulk planet parameters: 2 \%, 4-10 \% and 10 \% for planet radii, masses and ages, respectively. The planned baseline observing strategy includes two long pointings (2-3 years) to detect and bulk characterize planets reaching into the habitable zone (HZ) of solar-like stars and an additional step-and-stare phase to cover in total about 50 \% of the sky. PLATO 2.0 will observe up to 1,000,000 stars and detect and characterize hundreds of small planets, and thousands of planets in the Neptune to gas giant regime out to the HZ. It will therefore provide the first large-scale catalogue of bulk characterized planets with accurate radii, masses, mean densities and ages. This catalogue will include terrestrial planets at intermediate orbital distances, where surface temperatures are moderate. Coverage of this parameter range with statistical numbers of bulk characterized planets is unique to PLATO 2.0. The PLATO 2.0 catalogue allows us to e.g.: - complete our knowledge of planet
diversity for low-mass objects, - correlate the planet mean
density-orbital distance distribution with predictions from planet formation theories,- constrain the influence of planet migration and scattering on the architecture of multiple systems, and - specify how planet and system parameters change with host star characteristics, such as type, metallicity and age. The catalogue will allow us to study planets and planetary systems at different evolutionary phases. It will further provide a census for small, low-mass planets. This will serve to identify objects which retained their primordial hydrogen atmosphere and in general the typical characteristics of planets in such low-mass, low-density range. Planets detected by PLATO 2.0 will orbit bright stars and many of them will be targets for future atmosphere spectroscopy exploring their atmosphere. Furthermore, the mission has the potential to detect exomoons, planetary rings, binary and Trojan planets. The planetary science possible with PLATO 2.0 is complemented by its impact on stellar and galactic science via asteroseismology as well as light curves of all kinds of variable stars, together with observations of stellar clusters of different ages. This will allow us to improve stellar models and study stellar activity. A large number of well-known ages from red giant stars will probe the structure and evolution of our Galaxy. Asteroseismic ages of bright stars for different phases of stellar evolution allow calibrating stellar age-rotation relationships. Together with the results of ESA's Gaia mission, the results of PLATO 2.0 will provide a huge legacy to planetary, stellar and galactic science.},
  file = {/Users/Oliver/Zotero/storage/5LVC3AWC/Rauer et al. - 2014 - The PLATO 2.0 mission.pdf},
  journal = {Experimental Astronomy},
  keywords = {Asteroseismology,Exoplanetary science,Exoplanets,Stellar science,Transit survey}
}

@article{rebull+2016,
  title = {Rotation in the {{Pleiades}} with {{K2}}. {{I}}. {{Data}} and {{First Results}}},
  author = {Rebull, L. M. and Stauffer, J. R. and Bouvier, J. and Cody, A. M. and Hillenbrand, L. A. and Soderblom, D. R. and Valenti, J. and Barrado, D. and Bouy, H. and Ciardi, D. and Pinsonneault, M. and Stassun, K. and Micela, G. and Aigrain, S. and Vrba, F. and Somers, G. and Christiansen, J. and Gillen, E. and Collier Cameron, A.},
  year = {2016},
  month = nov,
  volume = {152},
  pages = {113},
  issn = {0004-6256},
  doi = {10.3847/0004-6256/152/5/113},
  abstract = {Young (125 Myr), populous ({$>$}1000 members), and relatively nearby, the Pleiades has provided an anchor for stellar angular momentum models for both younger and older stars. We used K2 to explore the distribution of rotation periods in the Pleiades. With more than 500 new periods for Pleiades members, we are vastly expanding the number of Pleiades with periods, particularly at the low-mass end. About 92\% of the members in our sample have at least one measured spot-modulated rotation period. For the {$\sim$}8\% of the members without periods, non-astrophysical
effects often dominate (saturation, etc.), such that periodic signals might have been detectable, all other things being equal. We now have an unusually complete view of the rotation distribution in the Pleiades. The relationship between P and \{(V-\{K\}\{\{s\}\})\}0 follows the overall trends found in other Pleiades studies. There is a slowly rotating sequence for 1.1 {$\lessequivlnt$}
\{(V-\{K\}\{\{s\}\})\}0 {$\lessequivlnt$} 3.7 and a primarily rapidly rotating population for \{(V-\{K\}\{\{s\}\})\}0 {$\greaterequivlnt$}
5.0. There is a region in which there seems to be a disorganized relationship between P and \{(V-\{K\}\{\{s\}\})\}0 for 3.7 {$\lessequivlnt$} \{(V-\{K\}\{\{s\}\})\}0 {$\lessequivlnt$} 5.0. Paper II
continues the discussion, focusing on multiperiod structures, and Paper III speculates about the origin and evolution of the period distribution in the Pleiades.},
  file = {/Users/Oliver/Zotero/storage/WEXX586P/Rebull et al. - 2016 - Rotation in the Pleiades with K2. I. Data and Firs.pdf},
  journal = {The Astronomical Journal},
  keywords = {globular clusters: individual: Pleiades,stars: rotation}
}

@article{rebull+2017,
  title = {Rotation of {{Late}}-Type {{Stars}} in {{Praesepe}} with {{K2}}},
  author = {Rebull, L. M. and Stauffer, J. R. and Hillenbrand, L. A. and Cody, A. M. and Bouvier, J. and Soderblom, D. R. and Pinsonneault, M. and Hebb, L.},
  year = {2017},
  month = apr,
  volume = {839},
  pages = {92},
  issn = {0004-637X},
  doi = {10.3847/1538-4357/aa6aa4},
  abstract = {We have Fourier-analyzed 941 K2 light curves (LCs) of likely members of Praesepe, measuring periods for 86\% and increasing the number of rotation periods (P) by nearly a factor of four. The distribution of P versus (V-\{K\}\{\{s\}\}), a mass proxy, has three different regimes: (V-\{K\}\{\{s\}\}) {$<$} 1.3, where the rotation rate
rapidly slows as mass decreases; 1.3 {$<$} (V-\{K\}\{\{s\}\}) {$<$} 4.5, where the rotation rate slows more gradually as mass decreases; and (V-\{K\}\{\{s\}\}) {$>$} 4.5, where the rotation rate rapidly
increases as mass decreases. In this last regime, there is a bimodal distribution of periods, with few between {$\sim$}2 and {$\sim$}10 days. We
interpret this to mean that once M stars start to slow down, they do so rapidly. The K2 period-color distribution in Praesepe ({$\sim$}790 Myr) is much different than that in the Pleiades ({$\sim$}125 Myr) for late F, G, K, and early-M stars; the overall distribution moves to longer periods and is better described by two line segments. For mid-M stars, the relationship has a similarly broad scatter and is steeper in Praesepe. The diversity of LCs and of periodogram types is similar in the two clusters; about a quarter of the periodic stars in both clusters have multiple significant periods. Multi-periodic stars dominate among the higher masses, starting at a bluer color in Praesepe
((V-\{K\}\{\{s\}\}) {$\sim$} 1.5) than in the Pleiades
((V-\{K\}\{\{s\}\}) {$\sim$} 2.6). In Praesepe, there are relatively more LCs that have two widely separated periods, \{\{{$\Delta$} \}\}P{$>$} 6
\{days\}. Some of these could be examples of M star binaries where one star has spun down but the other has not.},
  file = {/Users/Oliver/Zotero/storage/SV6BFQYB/Rebull et al. - 2017 - Rotation of Late-type Stars in Praesepe with K2.pdf},
  journal = {The Astrophysical Journal},
  keywords = {stars: rotation,stars: variables: general}
}

@article{rendle+2019,
  title = {{{AIMS}} - a New Tool for Stellar Parameter Determinations Using Asteroseismic Constraints},
  author = {Rendle, Ben M. and Buldgen, Ga{\"e}l and Miglio, Andrea and Reese, Daniel and Noels, Arlette and Davies, Guy R. and Campante, Tiago L. and Chaplin, William J. and Lund, Mikkel N. and Kuszlewicz, James S. and Scott, Laura J. A. and Scuflaire, Richard and Ball, Warrick H. and Smetana, Jiri and Nsamba, Benard},
  year = {2019},
  month = mar,
  volume = {484},
  pages = {771},
  doi = {10.1093/mnras/stz031},
  abstract = {A key aspect in the determination of stellar properties is the comparison of observational constraints with predictions from stellar models. Asteroseismic Inference on a Massive Scale (AIMS) is an open source code that uses Bayesian statistics and a Markov Chain Monte Carlo approach to find a representative set of models that reproduce a given set of classical and asteroseismic constraints. These models are obtained by interpolation on a pre-calculated grid, thereby increasing computational efficiency. We test the accuracy of the different operational modes within AIMS for grids of stellar models computed with the Li\`ege stellar evolution code (main sequence and red giants) and compare the results to those from another asteroseismic analysis pipeline, PARAM. Moreover, using artificial inputs generated from models within the grid (assuming the models to be correct), we focus on the impact on the precision of the code when considering different combinations of observational constraints (individual mode frequencies, period spacings, parallaxes, photospheric constraints,...). Our tests show the absolute limitations of precision on parameter inferences using synthetic data with AIMS, and the consistency of the code with expected parameter uncertainty distributions. Interpolation testing highlights the significance of the underlying physics to the analysis performance of AIMS and provides caution as to the upper limits in parameter step size. All tests demonstrate the flexibility and capability of AIMS as an analysis tool and its potential to perform accurate ensemble analysis with current and future asteroseismic data yields.},
  file = {/Users/Oliver/Zotero/storage/RCE2BKLR/Rendle et al. - 2019 - AIMS - a new tool for stellar parameter determinat.pdf;/Users/Oliver/Zotero/storage/T4U7UAKZ/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@article{rendle+2019a,
  title = {The {{K2 Galactic Caps Project}} -- {{Going Beyond}} the \textbackslash textit\{\vphantom\}{{Kepler}}\vphantom\{\} {{Field}} and {{Ageing}} the {{Galactic Disc}}},
  author = {Rendle, B. M. and Miglio, A. and Chiappini, C. and Valentini, M. and Davies, G. R. and Mosser, B. and Elsworth, Y. and Garc{\'i}a, R. A. and Mathur, S. and Jofr{\'e}, P. and Worley, C. C. and Casagrande, L. and Girardi, L. and Lund, M. N. and Feuillet, D. K. and Gavel, A. and Magrini, L. and Khan, S. and Rodrigues, T. S. and Johnson, J. A. and Cunha, K. and Lane, R. L. and Nitschelm, C. and Chaplin, W. J.},
  year = {2019},
  month = dec,
  volume = {490},
  pages = {4465--4480},
  issn = {0035-8711, 1365-2966},
  doi = {10.1093/mnras/stz2454},
  abstract = {Analyses of data from spectroscopic and astrometric surveys have led to conflicting results concerning the vertical characteristics of the Milky Way. Ages are often used to provide clarity, but typical uncertainties of {$>$} 40 \% from photometry restrict the validity of the inferences made. Using the Kepler APOKASC sample for context, we explore the global population trends of two K2 campaign fields (3 and 6), which extend further vertically out of the Galactic plane than APOKASC. We analyse the properties of red giant stars utilising three asteroseismic data analysis methods to cross-check and validate detections. The Bayesian inference tool PARAM is used to determine the stellar masses, radii and ages. Evidence of a pronounced red giant branch bump and an [{$\alpha$}/Fe] dependence on the position of the red clump is observed from the K2 fields radii distribution. Two peaks in the age distribution centred at {$\sim$}5 and and {$\sim$}12 Gyr are found using a sample with {$\sigma$}age {$<$} 35 \%. In comparison with Kepler, we find the older peak to be more prominent for K2. This age bimodality is also observed based on a chemical selection of low- ({$\leq$} 0.1) and high- ({$>$} 0.1) [{$\alpha$}/Fe] stars. As a function of vertical distance from the Galactic mid-plane (|Z |), the age distribution shows a transition from a young to old stellar population with increasing |Z | for the K2 fields. Further coverage of campaign targets with high resolution spectroscopy is required to increase the yield of precise ages achievable with asteroseismology.},
  archivePrefix = {arXiv},
  eprint = {1906.07489},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/TQXEYBDV/Rendle et al. - 2019 - The K2 Galactic Caps Project -- Going Beyond the .pdf},
  journal = {Monthly Notices of the Royal Astronomical Society},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  language = {en},
  number = {4}
}

@article{reville+2015,
  title = {The Effect of Magnetic Topology on Thermally-Driven Winds: Towards a General Formulation of the Braking Law},
  shorttitle = {The Effect of Magnetic Topology on Thermally-Driven Winds},
  author = {R{\'e}ville, Victor and Brun, Allan Sacha and Matt, Sean and Strugarek, Antoine and Pinto, Rui},
  year = {2015},
  month = jan,
  volume = {798},
  pages = {116},
  issn = {1538-4357},
  doi = {10.1088/0004-637X/798/2/116},
  abstract = {Stellar winds are thought to be the main process responsible for the spin down of main-sequence stars. The extraction of angular momentum by a magnetized wind has been studied for decades, leading to several formulations for the resulting torque. However, previous studies generally consider simple dipole or split monopole stellar magnetic topologies. Here we consider in addition to a dipolar stellar magnetic field, both quadrupolar and octupolar configurations, while also varying the rotation rate and the magnetic field strength. 60 simulations made with a 2.5D, cylindrical and axisymmetric set-up and computed with the PLUTO code were used to find torque formulations for each topology. We further succeed to give a unique law that fits the data for every topology by formulating the torque in terms of the amount of open magnetic flux in the wind. We also show that our formulation can be applied to even more realistic magnetic topologies, with examples of the Sun in its minimum and maximum phase as observed at the Wilcox Solar Observatory, and of a young K-star (TYC-0486- 4943-1) whose topology has been obtained by Zeeman-Doppler Imaging (ZDI).},
  archivePrefix = {arXiv},
  eprint = {1410.8746},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/HHQ9PNEF/Réville et al. - 2015 - The effect of magnetic topology on thermally-drive.pdf;/Users/Oliver/Zotero/storage/VHXVIGLV/1410.html},
  journal = {The Astrophysical Journal},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  number = {2}
}

@article{ricker+2015,
  title = {Transiting {{Exoplanet Survey Satellite}} ({{TESS}})},
  author = {Ricker, George R. and Winn, Joshua N. and Vanderspek, Roland and Latham, David W. and Bakos, G{\'a}sp{\'a}r {\'A} and Bean, Jacob L. and {Berta-Thompson}, Zachory K. and Brown, Timothy M. and Buchhave, Lars and Butler, Nathaniel R. and Butler, R. Paul and Chaplin, William J. and Charbonneau, David and {Christensen-Dalsgaard}, J{\o}rgen and Clampin, Mark and Deming, Drake and Doty, John and De Lee, Nathan and Dressing, Courtney and Dunham, Edward W. and Endl, Michael and Fressin, Francois and Ge, Jian and Henning, Thomas and Holman, Matthew J. and Howard, Andrew W. and Ida, Shigeru and Jenkins, Jon M. and Jernigan, Garrett and Johnson, John Asher and Kaltenegger, Lisa and Kawai, Nobuyuki and Kjeldsen, Hans and Laughlin, Gregory and Levine, Alan M. and Lin, Douglas and Lissauer, Jack J. and MacQueen, Phillip and Marcy, Geoffrey and McCullough, Peter R. and Morton, Timothy D. and Narita, Norio and Paegert, Martin and Palle, Enric and Pepe, Francesco and Pepper, Joshua and Quirrenbach, Andreas and Rinehart, Stephen A. and Sasselov, Dimitar and Sato, Bun'ei and Seager, Sara and Sozzetti, Alessandro and Stassun, Keivan G. and Sullivan, Peter and Szentgyorgyi, Andrew and Torres, Guillermo and Udry, Stephane and Villasenor, Joel},
  year = {2015},
  month = jan,
  volume = {1},
  pages = {014003},
  doi = {10.1117/1.JATIS.1.1.014003},
  abstract = {The Transiting Exoplanet Survey Satellite (TESS) will search for planets transiting bright and nearby stars. TESS has been selected by NASA for launch in 2017 as an Astrophysics Explorer mission. The spacecraft will be placed into a highly elliptical 13.7-day orbit around the Earth. During its 2-year mission, TESS will employ four wide-field optical charge-coupled device cameras to monitor at least 200,000 main-sequence dwarf stars with I\textsubscript{C}{$\approx$}4-13 for temporary drops in brightness caused by planetary transits. Each star will be observed for an interval ranging from 1 month to 1 year, depending mainly on the star's ecliptic latitude. The longest observing intervals will be for stars near the ecliptic poles, which are the optimal locations for follow-up observations with the James Webb Space Telescope. Brightness measurements of preselected target stars will be recorded every 2 min, and full frame images will be recorded every 30 min. TESS stars will be 10 to 100 times brighter than those surveyed by the pioneering Kepler mission. This will make TESS planets easier to characterize with follow-up observations. TESS is expected to find more than a thousand planets smaller than Neptune, including dozens that are comparable in size to the Earth. Public data releases will occur every 4 months, inviting immediate community-wide efforts to study the new planets. The TESS legacy will be a catalog of the nearest and brightest stars hosting transiting planets, which will endure as highly favorable targets for detailed investigations.},
  file = {/Users/Oliver/Zotero/storage/6UKZMZT8/Ricker et al. - 2015 - Transiting Exoplanet Survey Satellite (TESS).pdf;/Users/Oliver/Zotero/storage/WPZGTJ3M/abstract.html},
  journal = {Journal of Astronomical Telescopes, Instruments, and Systems},
  language = {en}
}

@article{riess+2018,
  title = {Milky {{Way Cepheid Standards}} for {{Measuring Cosmic Distances}} and {{Application}} to {{Gaia DR2}}: {{Implications}} for the {{Hubble Constant}}},
  shorttitle = {Milky {{Way Cepheid Standards}} for {{Measuring Cosmic Distances}} and {{Application}} to {{Gaia DR2}}},
  author = {Riess, Adam G. and Casertano, Stefano and Yuan, Wenlong and Macri, Lucas and Bucciarelli, Beatrice and Lattanzi, Mario G. and MacKenty, John W. and Bowers, J. Bradley and Zheng, WeiKang and Filippenko, Alexei V. and Huang, Caroline and Anderson, Richard I.},
  year = {2018},
  month = jul,
  volume = {861},
  pages = {126},
  doi = {10.3847/1538-4357/aac82e},
  abstract = {We present Hubble Space Telescope (HST) photometry of a selected sample of 50 long-period, low-extinction Milky Way Cepheids measured on the same WFC3 F555W-, F814W-, and F160W-band photometric system as extragalactic Cepheids in Type Ia supernova host galaxies. These bright Cepheids were observed with the WFC3 spatial scanning mode in the optical and near-infrared to mitigate saturation and reduce pixel-to-pixel calibration errors to reach a mean photometric error of 5 mmag per observation. We use the new Gaia DR2 parallaxes and HST photometry to simultaneously constrain the cosmic distance scale and to measure the DR2 parallax zeropoint offset appropriate for Cepheids. We find the latter to be -46 {$\pm$} 13 {$\mu$}as or {$\pm$}6 {$\mu$}as for a fixed distance scale, higher than found from quasars, as expected for these brighter and redder sources. The precision of the distance scale from DR2 has been reduced by a factor of 2.5 because of the need to independently determine the parallax offset. The best-fit distance scale is 1.006 {$\pm$} 0.033, relative to the scale from Riess et al. with H \textsubscript{0} = 73.24 km s\textsuperscript{-1} Mpc\textsuperscript{-1} used to predict the parallaxes photometrically, and is inconsistent with the scale needed to match the Planck 2016 cosmic microwave background data combined with {$\Lambda$}CDM at the 2.9{$\sigma$} confidence level (99.6\%). At 96.5\% confidence we find that the formal DR2 errors may be underestimated as indicated. We identify additional errors associated with the use of augmented Cepheid samples utilizing ground-based photometry and discuss their likely origins. Including the DR2 parallaxes with all prior distance-ladder data raises the current tension between the late and early universe route to the Hubble constant to 3.8{$\sigma$} (99.99\%). With the final expected precision from Gaia, the sample of 50 Cepheids with HST photometry will limit to 0.5\% the contribution of the first rung of the distance ladder to the uncertainty in H \textsubscript{0}.},
  file = {/Users/Oliver/Zotero/storage/CY8U8XYN/Riess et al. - 2018 - Milky Way Cepheid Standards for Measuring Cosmic D.pdf;/Users/Oliver/Zotero/storage/YUA43W3M/ui.adsabs.harvard.edu.html},
  journal = {The Astrophysical Journal},
  language = {en},
  number = {2}
}

@article{rodrigues+2014,
  title = {Bayesian Distances and Extinctions for Giants Observed by {{Kepler}} and {{APOGEE}}},
  author = {Rodrigues, Tha{\'i}se S. and Girardi, L{\'e}o and Miglio, Andrea and Bossini, Diego and Bovy, Jo and Epstein, Courtney and Pinsonneault, Marc H. and Stello, Dennis and Zasowski, Gail and Allende Prieto, Carlos and Chaplin, William J. and Hekker, Saskia and Johnson, Jennifer A. and M{\'e}sz{\'a}ros, Szabolcs and Mosser, Beno{\^i}t and Anders, Friedrich and Basu, Sarbani and Beers, Timothy C. and Chiappini, Cristina and Costa, Da and N, Luiz A. and Elsworth, Yvonne and Garc{\'i}a, Rafael A. and P{\'e}rez, Garc{\'i}a and E, Ana and Hearty, Fred R. and Maia, Marcio A. G. and Majewski, Steven R. and Mathur, Savita and Montalb{\'a}n, Josefina and Nidever, David L. and Santiago, Basilio and Schultheis, Mathias and Serenelli, Aldo and Shetrone, Matthew},
  year = {2014},
  month = dec,
  volume = {445},
  pages = {2758},
  doi = {10.1093/mnras/stu1907},
  abstract = {We present a first determination of distances and extinctions for individual stars in the first release of the APOKASC catalogue, built from the joint efforts of the Apache Point Observatory Galactic Evolution Experiment (APOGEE) and the Kepler Asteroseismic Science Consortium (KASC). Our method takes into account the spectroscopic constraints derived from the APOGEE Stellar Parameters and Chemical Abundances Pipeline, together with the asteroseismic parameters from KASC. These parameters are then employed to estimate intrinsic stellar properties, including absolute magnitudes, using the Bayesian tool PARAM. We then find the distance and extinction that best fit the observed photometry in Sloan Digital Sky Survey (SDSS), 2MASS, and WISE passbands. The first 1989 giants targetted by APOKASC are found at typical distances between 0.5 and 5 kpc, with individual uncertainties of just{\~ }1.8 per cent. Our extinction estimates are systematically smaller than provided in the Kepler Input Catalogue and by the Schlegel et al. maps. Distances to individual stars in the NGC 6791 and NGC 6819 star clusters agree to within their credible intervals. Comparison with the APOGEE red clump and SAGA catalogues provide another useful check, exhibiting agreement with our measurements to within a few per cent. Overall, present methods seem to provide excellent distance and extinction determinations for the bulk of the APOKASC sample. Approximately one third of the stars present broad or multiple-peaked probability density functions and hence increased uncertainties. Uncertainties are expected to be reduced in future releases of the catalogue, when a larger fraction of the stars will have seismically determined evolutionary status classifications.},
  file = {/Users/Oliver/Zotero/storage/NQWYT978/Rodrigues et al. - 2014 - Bayesian distances and extinctions for giants obse.pdf;/Users/Oliver/Zotero/storage/H4Y3MTM5/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {3}
}

@article{rodrigues+2017,
  title = {Determining Stellar Parameters of Asteroseismic Targets: Going beyond the Use of Scaling Relations},
  shorttitle = {Determining Stellar Parameters of Asteroseismic Targets},
  author = {Rodrigues, Tha{\'i}se S. and Bossini, Diego and Miglio, Andrea and Girardi, L{\'e}o and Montalb{\'a}n, Josefina and Noels, Arlette and Trabucchi, Michele and Coelho, Hugo Rodrigues and Marigo, Paola},
  year = {2017},
  month = may,
  volume = {467},
  pages = {1433},
  doi = {10.1093/mnras/stx120},
  abstract = {Asteroseismic parameters allow us to measure the basic stellar properties of field giants observed far across the Galaxy. Most of such determinations are, up to now, based on simple scaling relations involving the large-frequency separation, {$\increment\nu$}, and the frequency of maximum power, {$\nu$}\textsubscript{max}. In this work, we implement {$\increment\nu$} and the period spacing, {$\increment$}P, computed along detailed grids of stellar evolutionary tracks, into stellar isochrones and hence in a Bayesian method of parameter estimation. Tests with synthetic data reveal that masses and ages can be determined with typical precision of 5 and 19 per cent, respectively, provided precise seismic parameters are available. Adding independent on the stellar luminosity, these values can decrease down to 3 and 10 per cent, respectively. The application of these methods to NGC 6819 giants produces a mean age in agreement with those derived from isochrone fitting, and no evidence of systematic differences between RGB and RC stars. The age dispersion of NGC 6819 stars, however, is larger than expected, with at least part of the spread ascribable to stars that underwent mass-transfer events.},
  file = {/Users/Oliver/Zotero/storage/TVGMEETP/Rodrigues et al. - 2017 - Determining stellar parameters of asteroseismic ta.pdf;/Users/Oliver/Zotero/storage/RBVUQBHY/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {2}
}

@article{rowe+2017,
  title = {Time-{{Series Analysis}} of {{Broadband Photometry}} of {{Neptune}} from {{K2}}},
  author = {Rowe, Jason F. and Gaulme, Patrick and Lissauer, Jack J. and Marley, Mark S. and Simon, Amy A. and Hammel, Heidi B. and Aguirre, Victor Silva and Barclay, Thomas and Benomar, Othman and Boumier, Patrick and Caldwell, Douglas A. and Casewell, Sarah L. and Chaplin, William J. and Colon, Knicole D. and Corsaro, Enrico and Davies, G. R. and Fortney, Jonathan J. and Garcia, Rafael A. and Gizis, John E. and Haas, Michael R. and Mosser, Benoit and Schmider, Francois-Xavier},
  year = {2017},
  month = feb,
  abstract = {We report here on our search for excess power in photometry of Neptune collected by the K2 mission that may be due to intrinsic global oscillations of the planet Neptune. To conduct this search, we developed new methods to correct for instrumental effects such as intrapixel variability and gain variations. We then extracted and analyzed the time-series photometry of Neptune from 49 days of nearly continuous broadband photometry of the planet. We find no evidence of global oscillations and place an upper limit of \$\textbackslash sim\$5 ppm at 1000 \textbackslash uhz\textbackslash{} for the detection of a coherent signal. With an observed cadence of 1-minute and point-to-point scatter less than 0.01\textbackslash\%, the photometric signal is dominated by reflected light from the Sun, which is in turn modulated by atmospheric variability of Neptune at the 2\textbackslash\% level. A change in flux is also observed due to the increasing distance between Neptune and the K2 spacecraft, and solar variability with convection-driven solar p modes present.},
  archivePrefix = {arXiv},
  eprint = {1702.02943},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/D9FGJ4FJ/Rowe et al. - 2017 - Time-Series Analysis of Broadband Photometry of Ne.pdf;/Users/Oliver/Zotero/storage/7WKXW95T/1702.html},
  journal = {arXiv:1702.02943 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Instrumentation and Methods for Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{roxburgh+vorontsov2006,
  title = {The Autocorrelation Function of Stellar P-Mode Measurements and Its Diagnostic Properties},
  author = {Roxburgh, I. W. and Vorontsov, S. V.},
  year = {2006},
  month = jul,
  volume = {369},
  pages = {1491},
  doi = {10.1111/j.1365-2966.2006.10396.x},
  abstract = {The basic properties of acoustic wave propagation in stellar interiors can be analysed from the autocorrelation function (ACF) of intensity (or velocity) observations without measuring the resonant p-mode frequencies. We show how the strength of acoustic wave refraction in the stellar core, or forward acoustic amplitude, can be measured from a modulation in the ACF. This is the basic physical quantity which governs the so-called `small frequency separations', and its measurement from the ACF can be used for determining the small frequency separations when the data is of insufficient quality for a reliable identification of the stellar p-mode frequencies.},
  file = {/Users/Oliver/Zotero/storage/W65FCL92/Roxburgh and Vorontsov - 2006 - The autocorrelation function of stellar p-mode mea.pdf;/Users/Oliver/Zotero/storage/7BM2US3P/abstract.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {3}
}

@article{roxburgh2009,
  title = {Narrow Frequency-Windowed Autocorrelations as a Diagnostic of Solar-like Stars},
  author = {Roxburgh, I. W.},
  year = {2009},
  month = oct,
  volume = {506},
  pages = {435},
  doi = {10.1051/0004-6361/200911906},
  abstract = {Aims: This paper investigates the diagnostic potential of narrow, frequency-windowed autocorrelation as a tool for probing the properties of solar-like oscillating stars when the determination of individual frequencies is impossible or is subject to large uncertainties, and when mode identification is difficult. \\
Methods: I use theoretical analysis including phase-shifts, modelling, and data analysis. \\
Results: Narrow-windowed autocorrelation of a time series can reveal the variation with frequency of the large separations {$\increment$}({$\nu$}) and the half large separations {$\increment$}\textsubscript{01}, {$\increment$}\textsubscript{10}, thus helping with mode identification. This technique is applied to the CoRoT p-mode oscillators HD 49933, HD 175726, HD 181420, and HD 181906. Theoretical analysis and modelling are presented to illustrate the technique.},
  file = {/Users/Oliver/Zotero/storage/SWA4PQ4Z/Roxburgh - 2009 - Narrow frequency-windowed autocorrelations as a di.pdf;/Users/Oliver/Zotero/storage/L9RPGPP4/abstract.html},
  journal = {Astronomy and Astrophysics},
  language = {en},
  number = {1}
}

@article{ruiz-dern+2017,
  title = {Empirical Photometric Calibration of the {{Gaia Red Clump}}: Colours, Effective Temperature and Absolute Magnitude},
  shorttitle = {Empirical Photometric Calibration of the {{Gaia Red Clump}}},
  author = {{Ruiz-Dern}, L. and Babusiaux, C. and Arenou, F. and Turon, C. and Lallement, R.},
  year = {2017},
  month = oct,
  abstract = {Gaia Data Release 1 allows to recalibrate standard candles such as the Red Clump stars. To use those, they first need to be accurately characterised. In particular, colours are needed to derive the interstellar extinction. As no filter is available for the first Gaia data release and to avoid the atmosphere model mismatch, an empirical calibration is unavoidable. The purpose of this work is to provide the first complete and robust photometric empirical calibration of the Gaia Red Clump stars of the solar neighbourhood, through colour-colour, effective temperature-colour and absolute magnitude-colour relations, from the Gaia, Johnson, 2MASS, Hipparcos, Tycho-2, APASS-SLOAN and WISE photometric systems, and the APOGEE DR13 spectroscopic temperatures. We used a 3D extinction map to select low reddening red giants. To calibrate the colour-colour and the effective temperature-colour relations, we developed a MCMC method which accounts for all variable uncertainties and selects the best model for each photometric relation. We estimate the Red Clump absolute magnitude through the mode of a kernel-based distribution function. We provide 20 colour vs G-Ks relations and the first Teff vs G-Ks calibration. We obtained the Red Clump absolute magnitudes for 15 photometric bands with, in particular, M\_Ks = -1.606 +/- 0.009 and M\_G = (0.495 +/- 0.009) + (1.121 +/- 0.128) (G-Ks-2.1). We present an unreddened Gaia-TGAS HR diagram and use the calibrations to compare its Red Clump and its Red Giant Branch Bump with the Padova isochrones.},
  archivePrefix = {arXiv},
  eprint = {1710.05803},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/9BBUBWUX/Ruiz-Dern et al. - 2017 - Empirical photometric calibration of the Gaia Red .pdf;/Users/Oliver/Zotero/storage/K65FCTCD/1710.html},
  journal = {arXiv:1710.05803 [astro-ph]},
  keywords = {Astrophysics - Astrophysics of Galaxies,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{sahlholdt+2018,
  title = {Testing Asteroseismic Radii of Dwarfs and Subgiants with {{Kepler}} and {{Gaia}}},
  author = {Sahlholdt, C. L. and Silva Aguirre, V. and Casagrande, L. and Mosumgaard, J. R. and {Bojsen-Hansen}, M.},
  year = {2018},
  month = may,
  volume = {476},
  pages = {1931},
  doi = {10.1093/mnras/sty319},
  abstract = {We test asteroseismic radii of Kepler main-sequence and subgiant stars by deriving their parallaxes which are compared with those of the first Gaia data release. We compute radii based on the asteroseismic scaling relations as well as by fitting observed oscillation frequencies to stellar models for a subset of the sample, and test the impact of using effective temperatures from either spectroscopy or the infrared flux method. An offset of 3 per cent, showing no dependency on any stellar parameters, is found between seismic parallaxes derived from frequency modelling and those from Gaia. For parallaxes based on radii from the scaling relations, a smaller offset is found on average; however, the offset becomes temperature dependent which we interpret as problems with the scaling relations at high stellar temperatures. Using the hotter infrared flux method temperature scale, there is no indication that radii from the scaling relations are inaccurate by more than about 5 per cent. Taking the radii and masses from the modelling of individual frequencies as reference values, we seek to correct the scaling relations for the observed temperature trend. This analysis indicates that the scaling relations systematically overestimate radii and masses at high temperatures, and that they are accurate to within 5 per cent in radius and 13 per cent in mass for main-sequence stars with temperatures below 6400 K. However, further analysis is required to test the validity of the corrections on a star-by-star basis and for more evolved stars.},
  file = {/Users/Oliver/Zotero/storage/JRZ7DSGS/Sahlholdt et al. - 2018 - Testing asteroseismic radii of dwarfs and subgiant.pdf;/Users/Oliver/Zotero/storage/DC5RHDGL/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {2}
}

@article{sahlholdt+silvaaguirre2018,
  title = {Asteroseismic Radii of Dwarfs: {{New}} Accuracy Constraints from {{Gaia DR2}} Parallaxes},
  shorttitle = {Asteroseismic Radii of Dwarfs},
  author = {Sahlholdt, Christian L. and Silva Aguirre, Victor},
  year = {2018},
  month = sep,
  pages = {arXiv:1809.05112},
  abstract = {Precise stellar masses and radii can be determined using asteroseismology, but their accuracy must be tested against independent estimates. Using radii derived from Gaia DR2 parallaxes, we test the accuracy of asteroseismic radii for a sample of 93 dwarfs based on both individual frequency fitting and the seismic scaling relations. Radii from frequency fitting are about 1 per cent smaller than Gaia radii on average; however, this difference may be explained by a negative bias of 30 \$\textbackslash mu\$as in the Gaia parallaxes. This indicates that the radii derived from frequency fitting are accurate to within 1 per cent. The scaling relations are found to overestimate radii by more than 5 per cent, compared to the Gaia radii, at the highest temperatures. We demonstrate that this offset is reduced to 3 per cent after applying corrections based on model frequencies to the scaling relation for \$\textbackslash Delta\textbackslash nu\$, but only when the model frequencies are corrected for the surface effect. With corrections to \$\textbackslash Delta\textbackslash nu\$, the scaling relation gives radii accurate to about 2--3 per cent for dwarfs in the temperature range \$5400\$--\$6700\$ K. The remaining offset at the highest temperatures may indicate the need for a correction to the scaling relation for \$\textbackslash nu\_\{\textbackslash mathrm\{max\}\}\$.},
  file = {/Users/Oliver/Zotero/storage/ZPQLQE6L/Sahlholdt and Silva Aguirre - 2018 - Asteroseismic radii of dwarfs New accuracy constr.pdf;/Users/Oliver/Zotero/storage/DCELKZXK/ui.adsabs.harvard.edu.html},
  journal = {ArXiv e-prints},
  language = {en}
}

@article{salabert+2016,
  title = {Effect of {{Kepler}} Calibration on Global Seismic and Background Parameters},
  author = {Salabert, D. and Garcia, R. A. and Mathur, S. and Ballot, J.},
  year = {2016},
  month = nov,
  volume = {1611},
  pages = {arXiv:1611.05184},
  abstract = {Calibration issues associated to scrambled collateral smear affecting the Kepler short-cadence data were discovered in the Data Release 24 and were found to be present in all the previous data releases since launch. In consequence, a new Data Release 25 was reprocessed to correct for these problems. We perform here a preliminary study to evaluate the impact on the extracted global seismic and background parameters between data releases. We analyze the sample of seismic solar analogs observed by Kepler in short cadence between Q5 and Q17. We start with this set of stars as it constitutes the best sample to put the Sun into context along its evolution, and any significant differences on the seismic and background parameters need to be investigated before any further studies of this sample can take place. We use the A2Z pipeline to derive both global seismic parameters and background parameters from the Data Release 25 and previous data releases and report on the measured differences.},
  journal = {ArXiv e-prints},
  keywords = {Astrophysics - Solar and Stellar Astrophysics}
}

@article{salaris+2018,
  title = {Effective Temperatures of Red Giants in the {{APOKASC}} Catalogue and the Mixing Length Calibration in Stellar Models},
  author = {Salaris, M. and Cassisi, S. and Schiavon, R. P. and Pietrinferni, A.},
  year = {2018},
  month = apr,
  volume = {612},
  pages = {A68},
  doi = {10.1051/0004-6361/201732340},
  abstract = {Red giants in the updated APOGEE-Kepler catalogue, with estimates of mass, chemical composition, surface gravity and effective temperature, have recently challenged stellar models computed under the standard assumption of solar calibrated mixing length. In this work, we critically reanalyse this sample of red giants, adopting our own stellar model calculations. Contrary to previous results, we find that the disagreement between the T\textsubscript{eff} scale of red giants and models with solar calibrated mixing length disappears when considering our models and the APOGEE-Kepler stars with scaled solar metal distribution. However, a discrepancy shows up when {$\alpha$}-enhanced stars are included in the sample. We have found that assuming mass, chemical composition and effective temperature scale of the APOGEE-Kepler catalogue, stellar models generally underpredict the change of temperature of red giants caused by {$\alpha$}-element enhancements at fixed [Fe/H]. A second important conclusion is that the choice of the outer boundary conditions employed in model calculations is critical. Effective temperature differences (metallicity dependent) between models with solar calibrated mixing length and observations appear for some choices of the boundary conditions, but this is not a general result.},
  file = {/Users/Oliver/Zotero/storage/DCN29LJA/Salaris et al. - 2018 - Effective temperatures of red giants in the APOKAS.pdf;/Users/Oliver/Zotero/storage/IQWVV4IJ/ui.adsabs.harvard.edu.html},
  journal = {Astronomy and Astrophysics},
  language = {en}
}

@article{salaris+girardi2002,
  title = {Population Effects on the Red Giant Clump Absolute Magnitude: The {{K}} Band},
  shorttitle = {Population Effects on the Red Giant Clump Absolute Magnitude},
  author = {Salaris, Maurizio and Girardi, L{\'e}o},
  year = {2002},
  month = nov,
  volume = {337},
  pages = {332},
  doi = {10.1046/j.1365-8711.2002.05917.x},
  abstract = {We present a detailed analysis of the behaviour of the red clump K-band absolute magnitude (M\textsuperscript{RC}\textsubscript{K}) in simple and composite stellar populations, in light of its use as a standard candle for distance determinations. The advantage of using M\textsuperscript{RC}\textsubscript{K}, following recent empirical calibrations of its value for the solar neighbourhood, arises from its very low sensitivity to extinction by interstellar dust. We show that, as in the case of the V- and I-band results, M\textsuperscript{RC}\textsubscript{K} is a complicated function of the stellar metallicity Z and age t. In general, M\textsuperscript{RC}\textsubscript{K} is more sensitive to t and Z than M\textsuperscript{RC}\textsubscript{I}, for high t and low Z. Moreover, for ages above \textasciitilde 1.5 Gyr, M\textsuperscript{RC}\textsubscript{K} decreases with increasing Z, i.e. the opposite behaviour with respect to M\textsuperscript{RC}\textsubscript{V} and M\textsuperscript{RC}\textsubscript{I}. We provide data and equations that allow the determination of the K-band population correction {$\increment$}M\textsuperscript{RC}\textsubscript{K} (the difference between the red clump brightness in the solar neighbourhood and in the population under scrutiny) for any generic stellar population. These data complement the results presented by Girardi \& Salaris for the V- and I-band. We show how data from galactic open clusters consistently support our predicted {$\increment$}M\textsuperscript{RC}\textsubscript{V} , {$\increment$}M\textsuperscript{RC}\textsubscript{I} and {$\increment$}M\textsuperscript{RC}\textsubscript{K} values. Multiband VIK population corrections for various galaxy systems are provided. They can be used in conjunction with the method devised by Alves et al., in order to derive simultaneously reddening and distance from the use of VIK observations of red clump stars. We have positively tested this technique on the Galactic globular cluster 47 Tuc, for which both an empirical parallax-based main-sequence-fitting distance and reddening estimates exist. We have also studied the case of using only V and I photometry, recovering consistent results for both reddening and distance. Application of this method to an OGLE-II field, and the results by Alves et al., confirm a Large Magellanic Cloud distance modulus of about 18.50, in agreement with the Hubble Space Telescope extragalactic distance scale zero-point.},
  file = {/Users/Oliver/Zotero/storage/WHWJVCYN/Salaris and Girardi - 2002 - Population effects on the red giant clump absolute.pdf;/Users/Oliver/Zotero/storage/KY84CLWN/ui.adsabs.harvard.edu.html},
  journal = {Monthly Notices of the Royal Astronomical Society},
  language = {en},
  number = {1}
}

@article{salvatier+2016,
  title = {Probabilistic Programming in {{Python}} Using {{PyMC3}}},
  author = {Salvatier, John and Wiecki, Thomas V. and Fonnesbeck, Christopher},
  year = {2016},
  month = apr,
  volume = {2},
  pages = {e55},
  issn = {2376-5992},
  doi = {10.7717/peerj-cs.55},
  abstract = {Probabilistic programming allows for automatic Bayesian inference on user-defined probabilistic models. Recent advances in Markov chain Monte Carlo (MCMC) sampling allow inference on increasingly complex models. This class of MCMC, known as Hamiltonian Monte Carlo, requires gradient information which is often not readily available. PyMC3 is a new open source probabilistic programming framework written in Python that uses Theano to compute gradients via automatic differentiation as well as compile probabilistic programs on-the-fly to C for increased speed. Contrary to other probabilistic programming languages, PyMC3 allows model specification directly in Python code. The lack of a domain specific language allows for great flexibility and direct interaction with the model. This paper is a tutorial-style introduction to this software package.},
  file = {/Users/Oliver/Zotero/storage/VCB9DSVE/Salvatier et al. - 2016 - Probabilistic programming in Python using PyMC3.pdf},
  journal = {PeerJ Computer Science},
  language = {en}
}

@article{sandford+kipping2017,
  title = {Know the {{Planet}}, {{Know}} the {{Star}}: {{Precise Stellar Densities}} from {{Kepler Transit Light Curves}}},
  shorttitle = {Know the {{Planet}}, {{Know}} the {{Star}}},
  author = {Sandford, Emily and Kipping, David},
  year = {2017},
  month = oct,
  abstract = {The properties of a transiting planet's host star are written in its transit light curve. The light curve can reveal the stellar density and the limb darkening profile in addition to the characteristics of the planet and its orbit. For planets with strong prior constraints on orbital eccentricity, we may measure these stellar properties directly from the light curve; this method promises to aid greatly in the characterization of transiting planet host stars targeted by the upcoming NASA TESS mission and any long-period, singly-transiting planets discovered in the same systems. Using Bayesian inference, we fit a transit model, including a nonlinear limb darkening law, to 66 Kepler transiting planet hosts to measure their stellar properties. We present posterior distributions of stellar density, limb-darkening coefficients, and other system parameters for these stars. We measure densities to within 5\% for the majority of our target stars, with the dominant precision-limiting factor being the signal-to-noise ratio of the transits. 95 \% of our measured stellar densities are in 3-sigma or better agreement with previously published literature values. We make posterior distributions for all of our target KOIs available for online download.},
  archivePrefix = {arXiv},
  eprint = {1710.07293},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/HVQZQCHU/Sandford and Kipping - 2017 - Know the Planet, Know the Star Precise Stellar De.pdf;/Users/Oliver/Zotero/storage/Q8JGRWZT/1710.html},
  journal = {arXiv:1710.07293 [astro-ph]},
  keywords = {Astrophysics - Earth and Planetary Astrophysics,Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{santos+2016,
  title = {On the Relation between Activity-Related Frequency Shifts and the Sunspot Distribution over the Solar Cycle 23},
  author = {Santos, A. R. G. and Cunha, M. S. and Avelino, P. P. and Chaplin, W. J. and Campante, T. L.},
  year = {2016},
  month = nov,
  abstract = {The activity-related variations in the solar acoustic frequencies have been known for 30 years. However, the importance of the different contributions is still not well established. With this in mind, we developed an empirical model to estimate the spot-induced frequency shifts, which takes into account the sunspot properties, such as area and latitude. The comparison between the model frequency shifts obtained from the daily sunspot records and those observed suggests that the contribution from a stochastic component to the total frequency shifts is about 30\%. The remaining 70\% is related to a global, long-term variation. We also propose a new observable to investigate the short- and mid-term variations of the frequency shifts, which is insensitive to the long-term variations contained in the data. On the shortest time scales the variations in the frequency shifts are strongly correlated with the variations in the total area covered by sunspots. However, a significant loss of correlation is still found, which cannot be fully explained by ignoring the invisible side of the Sun when accounting for the total sunspot area. We also verify that the times when the frequency shifts and the sunspot areas do not vary in a similar way tend to coincide with the times of the maximum amplitude of the quasi-biennial variations found in the seismic data.},
  archivePrefix = {arXiv},
  eprint = {1611.07475},
  eprinttype = {arxiv},
  file = {/Users/Oliver/Zotero/storage/CPCA2VD2/Santos et al. - 2016 - On the relation between activity-related frequency.pdf;/Users/Oliver/Zotero/storage/XBVDV85U/1611.html},
  journal = {arXiv:1611.07475 [astro-ph]},
  keywords = {Astrophysics - Solar and Stellar Astrophysics},
  primaryClass = {astro-ph}
}

@article{santos+2016a,
  title = {Starspot Signature on the Light Curve: {{Learning}} about the Latitudinal Distribution of Spots},
  shorttitle = {Starspot Signature on the Light Curve},

repository: sandorkruk/malatium

repo_name: sandorkruk/malatium