Astronomy and Astrophysics – Astronomy
Scientific paper
Jan 2009
adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2009aas...21341702k&link_type=abstract
American Astronomical Society, AAS Meeting #213, #417.02; Bulletin of the American Astronomical Society, Vol. 41, p.229
Astronomy and Astrophysics
Astronomy
Scientific paper
The unresolved (diffuse and pseudo-diffuse) X-ray emission in late-type galaxy disks is dominated by star-formation. Comparison of the late-type galaxy disks with the best Chandra data reveals strong differences in the character of the unresolved emission: flocculent galaxies like M101 show little variation in the spectrum of the emission with location, while galaxies with strong m=2 spiral structure (M83 and M33) have harder emission in regions with higher X-ray surface brightness. The depth of the ChaseM33 data and the closeness of M33 make it an excellent laboratory for understanding the origin and the structure of the unresolved emission, as the bulk of the X-ray binaries and identifiable SNR can be removed. We correlate the X-ray surface brightness with multi-wavelength tracers of star-formation to demonstrate the extent to which the X-ray surface brightness tracks the density of star-formation. The global spectrum of the unresolved emission can be fit with two thermal component with (kT_S,kT_H) (0.2,0.75) keV. We will show the change of the X-ray spectrum with hardness ratio in order to determine whether the variation in hardness ratio is due to a change in the ratio of the hard and soft components, or to an increase in the temperature of the gas or to a systematic increase of absorption. From this variation we hope to gain an understanding of the sources of the emission and the physical mechanism producing the variation in the hardness ratio.
ChASeM33 Team
Ghavamian Parviz
Kuntz Kip D.
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