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X-Ray Emission from Expanding Shells in NGC 3077

Published online by Cambridge University Press:  26 May 2016

Jürgen Ott ,
Crystal L. Martin  and
Fabian Walter
Jürgen Ott
Affiliation:
CSIRO Australia Telescope National Facility, Cnr Vimiera & Pembroke Rds, Marsfield NSW 2122, Australia
Crystal L. Martin
Affiliation:
University of California, Santa Barbara, Department of Physics, Santa Barbara, CA 93106, USA
Fabian Walter
Affiliation:
National Radio Astronomy Observatory, P. O. Box O, Socorro, NM 87801, USA

Abstract

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Deep Chandra observations of NGC 3077, a starburst dwarf galaxy in the M81 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 × 1039ergs−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.

Type
Part 3. Ejection and Outflow
Information
Symposium - International Astronomical Union , Volume 217: Recycling Intergalactic and Interslettar Matter , 2004 , pp. 310 - 311
Copyright
Copyright © Astronomical Society of the Pacific 2004 

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