Using SEGUE Cool Stars to Examine the Metallicity Structure of the Milky Way Disk

Details Using SEGUE Cool Stars to Examine the Metallicity Structure of the Milky Way Disk Using SEGUE Cool Stars to Examine the Metallicity Structure of the Milky Way Disk

Jan 2012

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21911405s&link_type=abstract

American Astronomical Society, AAS Meeting #219, #114.05

Astronomy and Astrophysics

Astronomy

Scientific paper

We utilize the spectroscopically observed stars from the SEGUE Survey to examine the metallicity structure of the Galactic disk. Previous analyses of the metallicity distribution function of cool stars in the disk relied on local samples consisting of hundreds of stars (Rocha-Pinto & Maciel 1998, Kotoneva et al. 2002). Utilizing SDSS, we can greatly increase the sample size and extent of the disk probed. We benefit from the quantitative and systematic target selection algorithm of SEGUE, which allows us to use our spectroscopic sample of 60,000 stars to reflect the properties of the underlying stellar populations. This is by far the largest analysis of the disk utilizing spectroscopic metallicities and will be particularly critical for understanding the chemical evolution of the Milky Way. Throughout the disk, we find good agreement between G and K dwarfs, indicating similar star formation histories. In addition, both are deficient in metal-poor stars when compared with a simple closed box model, the classic "G dwarf problem." The two spectral types also show a consistent decrease in [Fe/H] with respect to increasing |Z|. Comparison with thin and thick disk samples, defined by [α/Fe], from Lee et al. (2011) indicates that the vertical metallicity gradient reflects the transition in G and K dwarfs from a thin-disk-dominated sample at small |Z| to a sample consisting primarily of thick-disk stars at high |Z|.

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