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.
American Astronomical Society Meeting Abstracts
- Pub Date:
- December 1995