Stellar Iron Abundances at the Galactic Center
OHIO STATE UNIV COLUMBUS DEPT OF ASTRONOMY
Pagination or Media Count:
We present measurements of FeH for six M supergiant stars and three giant stars within 2.5 pc of the Galactic center GC and one M supergiant star within 30 pc of the GC. The results are based on high-resolution K-band spectra, taken with CSHELL at the NASA Infrared Telescope Facility. We determine the iron abundance by detailed abundance analysis, performed with the spectral synthesis program MOOG. The mean FeH of the GC stars is determined to be near solar, FeH0.12 - 0.22. Our analysis is a differential analysis, as we have observed and applied the same analysis technique to 11 cool, luminous stars in the solar neighborhood with similar temperatures and luminosities as the GC stars. The mean FeH of the solar neighborhood comparison stars, FeH 0.03 - 0.16, is similar to that of the GC stars. The width of the GC FeH distribution is found to be narrower than the width of the FeH distribution of Baades window in the bulge but consistent with the width of the FeH distribution of giant and supergiant stars in the solar neighborhood.
- Atomic and Molecular Physics and Spectroscopy