Other
Scientific paper
Jan 2012
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2012aas...21920502s&link_type=abstract
American Astronomical Society, AAS Meeting #219, #205.02
Other
Scientific paper
Using the G and K dwarfs from the SEGUE Survey, we determine the metallicity distributions of cool stars in the Milky Way disk with respect to R and |Z|, which provide important guidance for models of the formation and chemical evolution of the Milky Way thick disk. Benefiting from the well-defined and quantitative target selection algorithm of SEGUE, we weight our spectroscopic sample such that it accurately represents the underlying Milky Way populations. Although we cover a limited range in R, we detect a negative metallicity gradient for both spectral types below |Z| of 1 kpc. Above this height, our samples are consistent with a flat radial metallicity gradient. The two spectral types also show similar behavior to each other in the vertical direction, showing a consistent decrease in [Fe/H] with respect to increasing |Z|. Comparison with the 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|. We compare our distributions to those of two different Galaxy models, from TRILEGAL (Girardi et al. 2004) and Schoenrich & Binney (2009a,b). Both models show little change in [Fe/H] with respect to |Z| and are unable to replicate the low-metallicity structure we observe. Therefore, our metallicity distribution functions challenge the assumptions that go into these models, which must be
modified in light of the observations.
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