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By
J. P. Fulbright, Department of Physics & Astronomy, The Johns Hopkins University, 3400 N. Charles Street, Baltimore, MD 21218, USA,
R. M. Rich, Division of Astronomy, Department of Physics & Astronomy, UCLA, Los Angeles, CA 90095-1562, USA,
A. McWilliam, Observatories of the Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101, USA
We present the results from optical high-resolution spectroscopic surveys of the Milky Way bulge. The bulge is observed to have stars with [Fe/H] values up to at least +0.5 and [Mg/H] values up to at least +0.8. Age information from color–magnitude diagrams suggests these stars formed at nearly the same time as old metal-rich globular clusters, and the abundance ratios imply that the chemical evolution of the bulge was dominated by Type-ii supernovae, including progenitors at least as metal-rich as those seen in the local disk today.
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