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Title:
Discovery of Hot Gas in Outflow in NGC 3379
Authors:
Trinchieri, G.; Pellegrini, S.; Fabbiano, G.; Fu, R.; Brassington, N. J.; Zezas, A.; Kim, D.-W.; Gallagher, J.; Angelini, L.; Davies, R. L.; Kalogera, V.; King, A. R.; Zepf, S.
Affiliation:
AA(INAF-Osservatorio Astronomico di Brera, Via Brera 28, 20212 Milano, Italy; ), AB(Dipartimento di Astronomia, Universita di Bologna, Via Ranzani 1, 40127 Bologna, Italy), AC(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138), AD(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138), AE(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138), AF(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138), AG(Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138), AH(Department of Astronomy, University of Wisconsin, Madison, WI 53706-1582), AI(Laboratory for X-Ray Astrophysics, NASA Goddard Space Flight Center, Greenbelt, MD 20771), AJ(Sub-Department of Astrophysics, University of Oxford, Oxford OX1 3RH, UK), AK(Northwestern University, Department of Physics and Astronomy, Evanston, IL 60208), AL(Theoretical Astrophysics Group, University of Leicester, Leicester LE1 7RH, UK), AM(Department of Physics and Astronomy, Michigan State University, East Lansing, MI 48824-2320)
Publication:
The Astrophysical Journal, Volume 688, Issue 2, pp. 1000-1008. (ApJ Homepage)
Publication Date:
12/2008
Origin:
UCP
ApJ Keywords:
Galaxies: Elliptical and Lenticular, cD, Galaxies: Individual: NGC Number: NGC 3379, X-Rays: Galaxies, X-Rays: ISM
Abstract Copyright:
(c) 2008: Discovery of Hot Gas in Outflow in NGC 3379
DOI:
10.1086/592287
Bibliographic Code:
2008ApJ...688.1000T

Abstract

We report the discovery of a faint (LX~4+/-1.5×1037 ergs s-1, 0.5-2 keV), outflowing gaseous hot interstellar medium (ISM) in NGC 3379. This represents the lowest X-ray luminosity ever measured from a hot phase of the ISM in a nearby early-type galaxy. The discovery of the hot ISM in a very deep Chandra observation was possible thanks to its unique spectral and spatial signatures, which distinguish it from the integrated stellar X-ray emission, responsible for most of the unresolved emission in the Chandra data. This hot component is found in a region of ~800 pc in radius at the center of the galaxy and has a total mass M~3+/-1×105 Msolar. Independent theoretical prediction of the characteristics of an ISM in this galaxy, based on the intrinsic properties of NGC 3379, reproduce well the observed luminosity, temperature, and radial distribution and mass of the hot gas, and indicate that the gas is in an outflowing phase, predicted by models but not observed in any system so far.
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