The Composition of the Old, Metal-Rich Open Cluster, NGC 6791

Details The Composition of the Old, Metal-Rich Open Cluster, NGC 6791 The Composition of the Old, Metal-Rich Open Cluster, NGC 6791

Dec 2006

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2006aas...20916511j&link_type=abstract

2007 AAS/AAPT Joint Meeting, American Astronomical Society Meeting 209, #165.11; Bulletin of the American Astronomical Society,

Astronomy and Astrophysics

Astronomy

1

Scientific paper

The populous open cluster, NGC 6791, has presented an anomaly as it appears to be very old (8-10 Gyr), yet metal-rich. We have made high resolution (45,000) spectroscopic observations of two turn-off stars (V = 17.4) with HIRES on the Keck I telescope on Mauna Kea. We have determined the stellar parameters for these two stars spectroscopically. The high metallicity of NGC 6791 is confirmed by our results, [Fe/H] = +0.40. In addition we have found elemental abundances for Na, Si, Ca, Ti, Ni, Cr and Y. We compare our results with those of field star samples that are both old and metal-rich: a) six dwarf stars with [Fe/H] > +0.01 and age > 8.5 Gyr from Edvardsson et al. (1993), b) nine old dwarf stars with [Fe/H] from +0.05 to +0.39 from Chen et al. (2003), and c) four old dwarf stars with [Fe/H] from +0.15 to +0.47 from Feltzing & Gonzalez (2001). The abundances of these elements are in agreement in the field and in the cluster with the possible exception of Ti which appears higher in the cluster stars; it is not clear why Ti would be enhanced when Si and Ca are not. We discuss the possible interpretations of the cluster peculiarities.
This research was supported by NSF through the REU program to the Institute for Astronomy, AST04-53395, and by a grant to AMB, AST05-05899.

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