Detection of Metal-poor Stars in the Direction of the North Galactic Pole

Details Detection of Metal-poor Stars in the Direction of the North Galactic Pole Detection of Metal-poor Stars in the Direction of the North Galactic Pole

Jan 2001

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2001aj....121..458y&link_type=abstract

The Astronomical Journal, Volume 121, Issue 1, pp. 458-475.

Astronomy and Astrophysics

Astronomy

2

Galaxy: Halo, Galaxy: Stellar Content, Stars: Population Ii

Scientific paper

A simple approach to detecting metal-poor stars is to measure a magnesium index, which depends on the Mg H band plus the three nearby Mg b lines and is derived through intermediate-band interference filters. An empirically established line of demarcation in the Mg index versus B-V diagram separates metal-poor stars from solar-abundance stars. A further separation between metal-poor dwarfs and giants depends on B-V primarily dwarfs for B-V<0.55, giants for B-V>0.7, with both dwarfs and giants falling in the transition region. For the metal-poor giants the distance from the demarcation line correlates well with [Fe/H], permitting estimates of stellar abundances. Stars in two regions on the sky in the vicinity of the north Galactic pole have been observed with such a set of filters. Eighteen stars (6% of the population of 299) in the sample covering the V range 8.7 to 15.6 and 48 stars (31% of the population of 163) in a deeper probe to V=19.9 found through this process are suspected metal-poor stars according to their Mg indices. Twenty-three are specifically deemed giants, with <[Fe/H]><=-1.5.

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