A combined Gaia-astrometry and color-color method yields a more complete catalog of red supergiant candidates in the metal-poor galaxy NGC 6822, with a metallicity-dependent empirical calibration for the stellar locus.
The AGB population of NGC 6822
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abstract
The metallicity gradient and the stellar distribution within the Local Group dwarf galaxy NGC 6822 has been studied photometrically using asymptotic branch stars (AGB). In order to study the stellar and metallicity distribution, the carbon- and oxygen-rich AGB stars have been isolated using deep high-quality near-infrared UKIRT photometry. The ratio between them, the C/M ratio, has been used to derive the [Fe/H] abundance within the galaxy. The [Fe/H] abundance and stellar distribution were analysed as a function of galactic radius. A mean C/M ratio of 0.288 +/- 0.014 has been found which corresponds to an iron abundance of [Fe/H] =-1.14 +/-0.08 dex, with variations in the north and south, as well as at larger galactocentric distances. Variations in the magnitude of the tip of the red giant branch has also been detected.
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A New Approach to Identifying Red Supergiant Stars in Metal-poor Galaxies: A Case Study of NGC 6822
A combined Gaia-astrometry and color-color method yields a more complete catalog of red supergiant candidates in the metal-poor galaxy NGC 6822, with a metallicity-dependent empirical calibration for the stellar locus.