Metal-poor stars don't blush: Broadband colors of confirmed cool subdwarfs in the SDSS.

Details Metal-poor stars don't blush: Broadband colors of confirmed cool subdwarfs in the SDSS. Metal-poor stars don't blush: Broadband colors of confirmed cool subdwarfs in the SDSS.

Feb 2009

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aipc.1094..545l&link_type=abstract

COOL STARS, STELLAR SYSTEMS AND THE SUN: Proceedings of the 15th Cambridge Workshop on Cool Stars, Stellar Systems and the Sun.

Physics

2

Low Luminosity Stars, Subdwarfs, And Brown Dwarfs, Stellar Characteristics And Properties, Luminosities, Magnitudes, Effective Temperatures, Colors, And Spectral Classification

Scientific paper

The colors of low-mass, metal-poor stars are determined using an unprecedented sample of 3,000 spectroscopically confirmed cool and ultra-cool subdwarfs of spectral subtype M0-M8, a sample which increases the census of spectroscopically confirmed M subdwarfs by almost an order of magnitude. Color-color diagrams in the Sloan Digital Sky Survey ugriz system and the Two Micron All Sky Survey JHK system indicates that M subdwarfs do not ``blush'' as much as their Solar-metallicity analogs (the M dwarf), as they are significantly bluer in r-i, i-z, and J-K. Further, it appears that these color terms are a function of metallicity, the more metal-poor the star, the bluer. In (g-r)/(r-i) color-color-space, the M dwarfs/subdwarfs extend on a grid which separates the stars along spectral subclass (i.e. metallicity) and spectral subtype. This not only makes it straightforward to identify M subdwarfs in deep photometric surveys, but suggests that faint, low-mass subdwarfs could be classified, and their metallicities estimated from broadband photometry alone.

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