Volume 430, Number 1, January IV 2005
|Page(s)||L13 - L16|
|Published online||12 January 2005|
Letter to the Editor
UVES observations of the Canis Major overdensity*
ESO - European Southern Observatory, Alonso de Cordova 3107, Vitacura, Santiago de Chile e-mail: firstname.lastname@example.org
2 Universitá di Roma “Tor Vergata”, via Della Ricerca Scientifica 2, Roma, Italy
3 INAF - Osservatorio Astronomico di Trieste, via G. B. Tiepolo, Trieste, Italy
Accepted: 2 December 2004
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 . 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: , , , and . These ratios make it likely that this star was formed in an external galaxy.
Key words: stars: abundances / stars: atmospheres / galaxies: abundances / galaxies: evolution / galaxies: dwarf
© ESO, 2005
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