Other
Scientific paper
Dec 2003
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2003phdt.........5a&link_type=abstract
Thesis (PhD). UNIVERSITY OF MICHIGAN, Source DAI-B 64/06, p. 2713, Dec 2003, 272 pages.
Other
11
Scientific paper
Observations of early-type galaxies from the recently launched Chandra and XMM-Newton Observatories have shown with impressive clarity the structure of the hot ISM and have finally spatially resolved the stellar binary point- source emission. However, the exact origin of the gas in the ISM remains in question. The majority of the ISM is presumed to come from stellar mass loss of old, near- solar metallicity stars with some additional contribution from in-falling matter from the surrounding medium. The problem with this origin model is that the majority of analysis of previous X-ray satellite data (and current X- ray satellite single-object studies) is inconsistent with this interpretation, mostly due to extremely low abundances measured. In order to address the origin and evolution of the ISM in early-type galaxies, we have conducted a multi- wavelength study of three key aspects of the ISM lifecycle. In the infrared, with the Infrared Space Observatory, we determine a stellar population injection rate into the ISM of ˜1.0 solar mass per year for nine early-type galaxies. With optical, ground-based spectroscopy, we measure a near-solar oxygen abundance of the warm phase gas in between the hot and originating, cold phase for seven galaxies. Finally, we analyze over three dozen early-type galaxies from the Chandra archive, representing the first large study of the hot ISM with the newest generation of X-ray telescopes. This study reveals a wealth of new information about the X-ray properties of early-type galaxies. A typical galaxy in the sample can be characterized as having an isothermal profile with a chemical enrichment history dominated by Supernovae type Ia. The metallicity of the gas is seen to be correlated with the stellar metallicity, creating a strong link between these populations. Incorporating the results from all three studies, an updated physical picture is presented for the origin and evolution of the ISM in early-type galaxies which reconciles the long standing inconsistencies between the data and the models.
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