X-Ray Emission from Expanding Shells in NGC 3077

Details X-Ray Emission from Expanding Shells in NGC 3077 X-Ray Emission from Expanding Shells in NGC 3077

Jun 2004

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=2004iaus..217..310o&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

Deep Chandra observations of NGC 3077, a starburst dwarf galaxy in the M 81 triplet, resolve the X-ray emission from several supershells. The emission is brightest in the cavities defined by expanding shells detected previously in Hα emission. Thermal emission models fitted to the data imply temperatures ranging from 1.3 to 4.9× 106 K. The total 0.3-6.0 keV X-ray luminosity is 2-5× 1039 erg s-1 (depending on the selected thermal plasma model). Most (85%) of the X-ray luminosity in NGC 3077 comes from the hot interstellar gas; the remainder comes from six X-ray point sources. The radial density profile of the hot gas is not as steep as that expected in a freely expanding wind (e.g., as seen in the neighboring starburst galaxy M 82) implying that the hot gas is still confined by the Hα shells.

Affiliated with

Also associated with

No associations

Rating

X-Ray Emission from Expanding Shells in NGC 3077 does not yet have a rating. At this time, there are no reviews or comments for this scientific paper.

If you have personal experience with X-Ray Emission from Expanding Shells in NGC 3077, we encourage you to share that experience with our LandOfFree.com community. Your opinion is very important and X-Ray Emission from Expanding Shells in NGC 3077 will most certainly appreciate the feedback.

Rate now

Comments { 0 }

Profile ID: LFWR-SCP-O-853050