Stellar Iron Abundances at the Galactic Center

Details Stellar Iron Abundances at the Galactic Center Stellar Iron Abundances at the Galactic Center

Dec 1999

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1999aas...195.6205r&link_type=abstract

American Astronomical Society, 195th AAS Meeting, #62.05; Bulletin of the American Astronomical Society, Vol. 31, p.1464

Astronomy and Astrophysics

Astronomy

Scientific paper

Measurements of [Fe/H] for ten M supergiant and giant stars within 30 pc of the Galactic Center (GC) are presented. The results are based on high-resolution (λ / Δ λ = 40,000) K-band spectra, taken with CSHELL at the NASA Infrared Telescope Facility. The iron abundance is determined by detailed abundance analysis, performed with the spectral synthesis program MOOG. The mean [Fe/H] of the GC stars is determined to be near solar, [Fe/H] = +0.09 +/- 0.09. Our analysis is a differential analysis, as we have observed and applied the same analysis technique to eleven nearby stars with similar temperatures and luminosities as the GC stars. The mean [Fe/H] of the nearby comparison stars, [Fe/H] = +0.03 +/- 0.05, is similar to that of the GC stars. The GC width of the [Fe/H] distribution is found to be narrower than the width of the [Fe/H] distribution of Baade's Window in the bulge and consistent with the width of the [Fe/H] distribution of supergiant stars in the solar neighborhood. This work has been supported by NSF grant AST-9619230 and NSF grant # GF-1003-97 from AURA under NSF cooperative agreement AST-8947990 and from Fundación Andes under project C-12984.

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