Hostname: page-component-cd9895bd7-gxg78 Total loading time: 0 Render date: 2024-12-27T06:51:09.502Z Has data issue: false hasContentIssue false
  • English
  • Français

Abundance patterns in the galactic bulge: cluster vs field populations

Published online by Cambridge University Press:  23 December 2005

Livia Origlia ,
R. Michael Rich  and
Elena Valenti
Livia Origlia
Affiliation:
INAF-Osservatorio Astronomico di Bologna, Via Ranzani 1, I-40127 Bologna, Italy email: [email protected]
R. Michael Rich
Affiliation:
Department of Physics and Astronomy, University of California at Los Angeles, Los Angeles, CA 90095-1562 email: [email protected]
Elena Valenti
Affiliation:
Dipartimento di Astronomia, Università di Bologna, Via Ranzani 1, 40127 Bologna, Italy, email: [email protected]
Rights & Permissions [Opens in a new window]

Abstract

Core share and HTML view are not available for this content. However, as you have access to this content, a full PDF is available via the ‘Save PDF’ action button.

Despite its importance, the Galactic Bulge and its globular cluster (GC) system in particular, remain relatively unexplored due to high foreground extinction and severely crowded field populations. The new generation of high resolution IR spectrographs opens new and unique perspectives to obtain detailed abundances in the Bulge field and GCs. Using the NIRSPEC spectrograph at Keck II, high resolution, echelle spectra in the range 1.5–1.8 micron of bright giants in the Baade's window and other fields closer to the Galactic center as well as in a sample of 10 Bulge GCs have been obtained. We present the results of our abundance analysis of Fe, Al, 12C, 13C, O, and other α-elements, by using full spectral synthesis techniques.

Keywords

Galaxy: bulgeGalaxy: globular clustersstars: abundancesinfrared:stars
Type
Contributed Papers
Information
Proceedings of the International Astronomical Union , Volume 1 , Symposium S228: From Lithium to Uranium: Elemental Tracers of Early Cosmic Evolution , May 2005 , pp. 385 - 388
Copyright
© 2005 International Astronomical Union