The Galaxy Merger Origin of Hot Gaseous Halos of Ellipticals

Details The Galaxy Merger Origin of Hot Gaseous Halos of Ellipticals The Galaxy Merger Origin of Hot Gaseous Halos of Ellipticals

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..217..412x&link_type=abstract

International Astronomical Union Symposium no. 217, held 14-17 July, 2003 in Sydney, Australia. Edited by P.-A. Duc, J. Braine

Astronomy and Astrophysics

Astronomy

Scientific paper

We report on the properties of the hot gaseous halos of 10 nearby ultraluminous IRAS galaxies from Chandra observations. There exists diffuse soft X-ray emission surrounding the central nucleus within 10 kpc of the nuclear region with a temperature of about 0.7 keV and metallicity about Z˜ 1.0 Z&sun;. Also, emission lines from α elements and ions for are seen in all nearby ULIRGs in our sample. Outside the central region, the Chandra observations reveal a more extended hot gaseous halo with a temperature of about 0.6 keV and low metallicity (Z ˜ 0.1 Z&sun;) for some of the ULIRGs. We discuss the nature and the implications of our results for the origin of X-ray halos in elliptical galaxies and the constraints this places on the feedback process.

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