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Iron Abundances in AGB Stars and M Supergiant Stars at the Galactic Center

Published online by Cambridge University Press:  25 May 2016

S. V. Ramírez ,
K. Sellgren ,
D. M. Terndrup ,
J. S. Carr ,
S. Balachandran  and
R. D. Blum
S. V. Ramírez
Affiliation:
The Ohio State University, Columbus OH 43210, USA
K. Sellgren
Affiliation:
The Ohio State University, Columbus OH 43210, USA
D. M. Terndrup
Affiliation:
The Ohio State University, Columbus OH 43210, USA
J. S. Carr
Affiliation:
Naval Research Laboratory, Washington, DC 20375, USA
S. Balachandran
Affiliation:
University of Maryland, College Park, MD 20742, USA
R. D. Blum
Affiliation:
CTIO, La Serena, Chile

Abstract

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We are measuring Fe abundances of cool, luminous stars within 30 pc of the center of the Milky Way. Our sample contains both AGB stars and M supergiants. Low-resolution (λ/Δλ = 500) H and K band spectra are used to estimate temperatures and gravities. Stellar Fe abundances are determined from high-resolution (λ/Δλ = 40 000) K band spectra obtained on the IRTF using CSHELL. We find that Fe abundances of stars in the Galactic Center are consistent with the solar Fe abundance.

Type
Part 6. AGB Stars as a Population of Various Galaxies
Information
Symposium - International Astronomical Union , Volume 191: Asymptotic Giant Branch Stars , 1999 , pp. 529 - 534
Copyright
Copyright © Astronomical Society of the Pacific 1999 

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