Metal Abundances and Kinematics of Bright Metal-Poor Giants Selected from the LSE Survey: Implications for the Metal-Weak Thick Disk

Details Metal Abundances and Kinematics of Bright Metal-Poor Giants Selected from the LSE Survey: Implications for the Metal-Weak Thick Disk Metal Abundances and Kinematics of Bright Metal-Poor Giants Selected from the LSE Survey: Implications for the Metal-Weak Thick Disk

2002-04-19

arxiv.org/abs/astro-ph/0204339v1

Astronomy and Astrophysics

Astrophysics

41 pages, 9 tables, 6 figures, accepted for publication in The Astronomical Journal

Scientific paper

10.1086/341377

We report medium-resolution (1-2 A) spectroscopy and broadband (UBV) photometry for a sample of 39 bright stars (the majority of which are likely to be giants) selected as metal-deficient candidates from an objective-prism survey concentrating on Galactic latitudes below |b| = 30 deg, the LSE survey of Drilling & Bergeron. Although the primary purpose of the LSE survey was to select OB stars (hence the concentration on low latitudes), the small number of bright metal-deficient giant candidates noted during this survey provide interesting information on the metal-weak thick disk (MWTD) population. The kinematics of the LSE giants indicate the presence of a rapidly rotating population, even at quite low metallicity. We consider the distribution of orbital eccentricity of the LSE giants as a function of [Fe/H], and conclude that the local fraction (i.e., within 1 kpc from the Sun) of metal-poor stars that might be associated with the MWTD is on the order of 30%-40% at abundances below [Fe/H] = -1.0. Contrary to recent analyses of previous (much larger) samples of non-kinematically selected metal-poor stars, we find that this relatively high fraction of local metal-poor stars associated with the MWTD may extend to metallicities below [Fe/H] = -1.6, much lower than had been considered before. We identify a subsample of 11 LSE stars that are very likely to be members of the MWTD, based on their derived kinematics; the lowest metallicity among these stars is [Fe/H] = -2.35. Implications of these results for the origin of the MWTD and for the formation of the Galaxy are considered. (abridged)

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