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Mining the Kepler Field: Atmospheric Parameters, Bolometric Corrections, and Luminosities

Diego Godoy-Rivera, Desmond H. Grossmann, Tyler Richey-Yowell, Angela R. G. Santos, Savita Mathur, Rafael A. Garcia

Abstract

The ~ 200,000 stars observed by the Kepler mission have provided unprecedented constraints across astrophysics. With the advent of modern spectroscopic and photometric surveys, new limits in stellar characterizations are within reach. In this work, we report a compilation of atmospheric parameters (Teff, logg, and [M/H]) for the Kepler stars by crossmatching with several spectroscopic and spectro-photometric surveys. We use these to calculate bolometric corrections, which combined with color-magnitude diagram (CMD) information from Gaia yield self-consistent luminosities on a survey-by-survey basis. These properties will aid in future explorations of Kepler data towards new astrophysical insights. We make our catalog publicly available online in Zenodo (doi:10.5281/zenodo.18620911).

Mining the Kepler Field: Atmospheric Parameters, Bolometric Corrections, and Luminosities

Abstract

The ~ 200,000 stars observed by the Kepler mission have provided unprecedented constraints across astrophysics. With the advent of modern spectroscopic and photometric surveys, new limits in stellar characterizations are within reach. In this work, we report a compilation of atmospheric parameters (Teff, logg, and [M/H]) for the Kepler stars by crossmatching with several spectroscopic and spectro-photometric surveys. We use these to calculate bolometric corrections, which combined with color-magnitude diagram (CMD) information from Gaia yield self-consistent luminosities on a survey-by-survey basis. These properties will aid in future explorations of Kepler data towards new astrophysical insights. We make our catalog publicly available online in Zenodo (doi:10.5281/zenodo.18620911).
Paper Structure (5 sections, 2 equations, 1 figure)

This paper contains 5 sections, 2 equations, 1 figure.

Table of Contents

  1. Introduction
  2. Method
  3. Spectroscopic Compilation
  4. Bolometric Corrections
  5. Luminosities

Figures (1)

  • Figure 1: Kiel (top) and Hertzsprung-Russell (bottom) diagram for the Kepler stars. Each panel indicates a survey, with the number of stars found in each indicated in the legend.