3 years ago

# The First APOKASC Catalog of Kepler Dwarf and Subgiant Stars.

Victor Silva Aguirre, Marc Pinsonneault, Warrick H. Ball, D. A. Garcia-Hernandez, Jennifer Johnson, Yvonne Elsworth, Dennis Stello, Aldo Serenelli, Jon Holtzman, Rasmus Handberg, Mikkel N. Lund, Keivan G. Stassun, Savita Mathur, Nicholas Troup, Rafael A. Garcia, Thomas Kallinger, Saskia Hekker, William J. Chaplin, Benoit Mosser, Fred Hearty, Olga Zamora, Patrick Gaulme, Sarbani Basu, Daniel Huber, Guy R. Davies, Jamie Tayar

(Abridged) We present the first APOKASC catalog of spectroscopic and asteroseismic data for 415 dwarfs and subgiants. Asteroseismic data have been obtained by Kepler in short cadence. The spectroscopic parameters are based on spectra taken as part of APOGEE and correspond to DR13 of SDSS. We analyze our data using two Teff scales, the spectroscopic values from DR13 and those derived from SDSS griz photometry. We use the differences in our results arising from these choices as a test of systematic Teff, and find that they can lead to significant differences in the derived stellar properties. Determinations of surface gravity ($\log{g}$), mean density ($\rho$), radius ($R$), mass ($M$), and age ($\tau$) for the whole sample have been carried out with stellar grid-based modeling. We have assessed random and systematic error sources in the spectroscopic and seismic data, as well as in the grid-based modeling determination of the stellar quantities in the catalog. We provide stellar properties for both Teff scales. The median combined (random and systematic) uncertainties are 2% (0.01 dex; $\log{g}$), 3.4% ($\rho$), 2.6% ($R$), 5.1% ($M$), and 19% ($\tau$) for the photometric Teff scale and 2% ($\log{g}$), 3.5% ($\rho$), 2.7% ($R$), 6.3% ($M$), and 23% ($\tau$) for the spectroscopic scale. Comparisons with stellar quantities in the catalog by Chaplin et al.(2014) highlight the importance of metallicity measurements for determining stellar parameters accurately. We compare our results with those from other sources, including stellar radii determined from TGAS parallaxes and asteroseismic analyses based on individual frequencies. We find a very good agreement in all cases. Comparisons give strong support to the determination of stellar quantities based on global seismology, a relevant result for future missions such as TESS and PLATO. Table 5 corrected (wrongly listed SDSS Teff before).

Publisher URL: http://arxiv.org/abs/1710.06858

DOI: arXiv:1710.06858v3

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