Empirical temperature- and extinction-dependent extinction coefficients for the GALEX, Pan-STARRS1, Gaia, SDSS, 2MASS, and WISE passbands

Abstract

We have obtained accurate dust reddening from far-ultraviolet (UV) to the mid-infrared (IR) for up to 5 million stars by the star-pair algorithm based on LAMOST stellar parameters along with GALEX, Pan-STARRS 1, Gaia, SDSS, 2MASS, and WISE photometric data. The typical errors are between 0.01-0.03 mag for most colors. We derived the empirical reddening coefficients for 21 colors both in the traditional (single valued) way and as a function of T eff and E(B − V ) by using the largest samples of accurate reddening measurements, together with the extinction values from Schlegel et al. The corresponding extinction coefficients have also been obtained. The results are compared with model predictions and generally in good agreement. Comparisons with measurements in the literature show that the T eff -and E(B − V )-dependent coefficients explain the discrepancies between different measurements naturally, i.e., using sample stars of different temperatures and reddening. Our coefficients are mostly valid in the extinction range of 0-0.5 mag and the temperature range of 4000-10000 K. We recommend that the new T eff -and E(B − V )-dependent reddening and extinction coefficients should be used in the future. A Python package is also provided for the usage of the coefficients a) .

Stellar Loci. VI. An Updated Catalog of the Best and Brightest Metal-poor Stars

“…These stars are dereddened using the Schlegel et al (1998, hereafter SFD) dust reddening map. The reddening coefficients for the K − W1 and W1-W2 colors are empirically determined byZhang & Yuan (2022), which are 0.11 and 0.056, respectively. With the sample above, by considering both the selection efficiency and completeness, we set the new criterion to be (W1-W2) 0 > −0.392 × (K − W1) 0 − 0.017, as shown in Figure1; it yields a success rate of 46% and a completeness of 84% for the sample used.…”