Photometric Study of Kepler Asteroseismic Targets

TL;DR

This study presents photometric observations of Kepler asteroseismic targets, analyzing their stellar parameters and comparing photometric and spectroscopic temperatures and gravities, revealing systematic differences.

Contribution

It provides a detailed photometric analysis of Kepler targets and compares photometric and spectroscopic stellar parameters, highlighting systematic discrepancies.

Findings

Photometric temperatures are higher than spectroscopic ones for T_eff > 6400 K.

Good agreement between photometric and spectroscopic temperatures for T_eff < 6250 K.

Photometric surface gravities are about twice as large as spectroscopic values.

Abstract

Reported are UBV and uvbybeta observations of 15 candidates for Kepler primary astero- seismic targets and 14 other stars in the Kepler field, carried out at the M.G. Fracastoro station of the Catania Astrophysical Observatory. These data serve to plot the 29 stars in two-parameter diagrams with the photometric indices (such as B-V or delta m1 and the atmospheric parameters (such as the MK type or [Fe/H]) as coordinates. The two-parameter diagrams show no evidence of interstellar reddening. The photometric indices B-V and beta are then used to derive photometric effective temperatures, Teff(B-V) and Teff(beta). For Teff(B-V) > 6400 K, the photometric effective temperatures turn out to be systematically higher than spectroscopic effective temperatures by 311 +/- 34 K and 346 +/- 91 K for Teff(B-V) and Teff(beta), respectively. For T_eff(B-V) < 6250 K, the agreement between Teff(B-V) and the spectroscopic effective temperatures is very good. The photometric surface gravities, derived from c_1 and beta, show a range of about a factor of two greater than their spectroscopic counterparts do.