Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2011
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2011aas...21715237d&link_type=abstract
American Astronomical Society, AAS Meeting #217, #152.37; Bulletin of the American Astronomical Society, Vol. 43, 2011
Astronomy and Astrophysics
Astronomy
Scientific paper
Our current understanding of chemical evolution, nucleosynthesis and galaxy assembly is based largely on stellar abundance studies of old stars in only one galaxy: the Milky Way (MW). Unfortunately, beyond the MW and it's nearest neighbors, old (red giant branch) stars are too faint to observe at the high spectral resolutions(>= 20,000) and high signal-to-noise ratios (SNR >= 60)required for the analysis of individual absorption lines. While young stars can be studied at larger distances, they only record the recent gas-phase abundances. To enable chemical abundance studies of old stars at larger distances, we have developed a method to analyze high resolution (R 20,000) integrated light (IL) spectra of extragalactic Globular Clusters (GCs).
GCs are unique tracers of the formation histories of galaxies; they form throughout the lifetimes of galaxies in episodes of rapid star formation (SF) and their properties are known to correlate strongly with the properties of the host galaxy (see Brodie & Strader 2006). We have demonstrated that our GC analysis provides abundances that are as accurate as standard abundance analysis of individual RBG stars, as well as accurate ages for clusters between 0.1 and 13 Gyrs. Here, we present the first detailed chemical abundances (alpha, Fe-peak, and neutron capture elements) and ages for a sample of 5 GCs in NGC 5128, the nearest E/S0 galaxy.
Bernstein Rebecca
Duran Maria
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