A Method for Determining the Relative Metal Abundances of M Stars Using Multi-Color Photometry

Details A Method for Determining the Relative Metal Abundances of M Stars Using Multi-Color Photometry A Method for Determining the Relative Metal Abundances of M Stars Using Multi-Color Photometry

Dec 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995aas...187.1401b&link_type=abstract

American Astronomical Society, 187th AAS Meeting, #14.01; Bulletin of the American Astronomical Society, Vol. 27, p.1301

Astronomy and Astrophysics

Astronomy

Scientific paper

Presented is a scheme using broad band filters for determining the relative metal abundances of M stars. The "Lindblad depression" makes a filter centered at 425nm dimmer for metal poor stars than for normal stars. A temperature dependent color is made from filters centered at 535nm and 900nm. This is plotted against 425nm-535nm to determine metallicity. Typical metal poor stars separate from disk stars by a about tenth of a magnitude in 425nm-535nm, and the extreme subdwarf LHS453 separates from disk stars by .8mag. This is useful in surveys, where one wants to find a lot of metal poor stars quickly.

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