UVES observations of the Canis Major overdensity

Details UVES observations of the Canis Major overdensity UVES observations of the Canis Major overdensity

2004-12-04

arxiv.org/abs/astro-ph/0412098v1

Astronomy and Astrophysics

Astrophysics

4 pages, 4 figures, accepted for publication in A&A letters

Scientific paper

10.1051/0004-6361:200400118

We present the first detailed chemical abundances for three giant stars which are candidate members of the Canis Major overdensity, obtained by using FLAMES-UVES at VLT. The stars, in the background of the open cluster NGC 2477, have radial velocities compatible with a membership to this structure. However, due to Galactic disc contamination, radial velocity by itself is unable to firmly establish membership. The metallicities span the range -0.5 < [Fe/H] < +0.1. Assuming that at least one of the three stars is indeed a member of CMa implies that this structure has undergone a high level of chemical processing, comparable to that of the Galactic disc. The most metal-rich star of the sample, EIS 6631, displays several abundance ratios which are remarkably different from those of Galactic stars: [alpha/Fe] ~-0.2, [Cu/Fe] ~+0.25, [La/Fe]~+0.6, [Ce/Fe]~+0.8 and [Nd/Fe]~+0.6. These ratios make it likely that this star was formed in an external galaxy.

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