Stellar Loci. VII. Photometric Metallicities of 5 Million FGK Stars Based on GALEX GR6+7 AIS and Gaia EDR3

Abstract

We combine photometric data from GALEX GR6+7 AIS and Gaia EDR3 with stellar parameters from the SAGA and PASTEL catalogs to construct high-quality training samples for dwarfs ($0.4<\mathrm{BP}-\mathrm{RP}<1.6$) and giants ($0.6<\mathrm{BP}-\mathrm{RP}<1.6$). We apply careful reddening corrections using empirical temperature- and extinction-dependent extinction coefficients. Using the two samples, we establish a relationship between stellar loci (NUV$-$BP vs. BP$-$RP colors), metallicity, and ${\mathrm{M}}_{\mathrm{G}}$. For a given BP$-$RP color, a 1 dex change in [Fe/H] corresponds to an approximately 1 magnitude change in NUV$-$BP color for solar-type stars. These relationships are employed to estimate metallicities based on NUV$-$BP, BP$-$RP, and ${\mathrm{M}}_{\mathrm{G}}$. Thanks to the strong metallicity dependence in the GALEX NUV-band, our models enable a typical photometric-metallicity precision of approximately ${\sigma }_{[Fe/H]}$ = 0.11 dex for dwarfs and ${\sigma }_{[Fe/H]}$ = 0.17 dex for giants, with an effective metallicity range extending down to [Fe/H] $=-3.0$ for dwarfs and [Fe/H] $=-4.0$ for giants. We also find that the NUV-band based photometric-metallicity estimate is not as strongly affected by carbon enhancement as previous photometric techniques. With the Gaia and GALEX data, we have estimated metallicities for about 5 million stars across almost the entire sky, including approximately 4.5 million dwarfs and 0.5 million giants. This work demonstrates the potential of the NUV-band for estimating photometric metallicities, and sets the groundwork for utilizing the NUV data from space telescopes such as the upcoming Chinese Space Station Telescope.

arXiv comment24 pages, 19 figures, accepted by ApJS