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The data for "Accurate, Precise, and Physically Self-consistent Ages andMetallicities for 400,000 Solar Neighborhood Subgiant Branch Stars"
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The data for "Accurate, Precise, and Physically Self-consistent Ages andMetallicities for 400,000 Solar Neighborhood Subgiant Branch Stars"

David Nataf, Kevin Schlaufman, Henrique Reggiani and Isabel Hahn
Zenodo
2024
DOI: 10.5281/zenodo.13750876
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https://doi.org/10.5281/zenodo.13750876View
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Abstract

These files and scripts relate to the development and derivation of the results by Nataf, Schlaufman, Reggiani, & Hahn (2024), titled "ccurate, Precise, and Physically Self-consistent Ages and Metallicities for 400,000 Solar Neighborhood Subgiant Branch Stars". The input for the primary sample is "PlatinumSGB.fits", a 380 MB file. The input for the metal-poor annex is "MPannexSGB.fits". These two files have the same columns, but different rows corresponding to different selection functions. These files include a lot of data from Gaia DR3, 2MASS, WISE, Skymapper DR2, SDSS, GALEX, as well as that of any identified matches from ASAS-SN, GALAH, LAMOST LRS, APOGEE, and GALAH. The Jupyter Notebook "IsochronesSubgiants.ipynb" can be found at the associated github repository for this project. It is a sample of the code used to convert these input data, along with our priors, into derived posteriors for the stars using the Isochrones package (Morton 2015), which evaluates observations relative to the MIST v1.2 isochrones using pyMultinest. The putfut file which includes our derived stellar parameters from pyMultiNest, as well as derived orbital parameters using galPy, is "TotalSample.fits", a 76 MB fits file, and equivalently, "TotalSample.csv", a 275 MB file in the comma-separated-variables format. The file "TopOfMRT.txt" is located in this repository, and includes a description of the output columns in "TotalSample", both csv and fits versions. The file "StarFormationHistoryKinematicsMovie.mp4" is an animation, whereby each frame shows 2 percentiles of the stars of our full sample in order of increasing ages, and at each age we see the kinematics of the stars color-coded by metallicity, and the metallicity distribution function of the stars.  

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