Metallicity and Kinematics of M31's Outer Stellar Halo from a Keck Spectrocscopic Survey

Details Metallicity and Kinematics of M31's Outer Stellar Halo from a Keck Spectrocscopic Survey Metallicity and Kinematics of M31's Outer Stellar Halo from a Keck Spectrocscopic Survey

2002-03-21

arxiv.org/abs/astro-ph/0203389v3

Astronomy and Astrophysics

Astrophysics

98 pages, including 4 tables and 24 figures; Accepted for publication in the July, 2002 edition of the Astronomical Journal

Scientific paper

10.1086/341175

We present multislit CaII near-infrared triplet spectroscopy with the Keck 10-m telescope/LRIS of 99 M31 halo red giant candidates in the apparent mag range 200.6 dex, spans the full 2dex range over which [Fe/H] measurement methods are calibrated, and has a mean/median value around <[Fe/H]>=-1.9 to -1.1dex and possibly higher since the high-[Fe/H] end of the distribution is not well constrained by our sample. Our data on M31 field halo giants suggest that they are more metal-rich than their Milky Way counterparts, similar to M31 and Milky Way globular clusters, consistent with a scenario in which the halo is built from accretion of small stellar subsystems. There are 4 stars in the secure M31 sample with unusually strong Ca lines (>~solar [Fe/H]) at a common velocity of -340km/s close to M31's systemic velocity, similar to what might be expected for M31 disk giants on the minor axis. The M31 disk would have to be large and/or warped to account for these stars. More likely, these stars are metal-rich debris from a past accretion event in M31's halo.

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