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Title:
Deconstructing NGC 7130
Authors:
Levenson, N. A.; Weaver, K. A.; Heckman, T. M.; Awaki, H.; Terashima, Y.
Affiliation:
AA(Department of Physics and Astronomy, University of Kentucky, Lexington, KY 40506; .), AB(NASA Goddard Space Flight Center, Laboratory for High Energy Astrophysics, Code 662, Greenbelt, MD 20771.; Department of Physics and Astronomy, Bloomberg Center, The Johns Hopkins University, Baltimore, MD 21218.), AC(Department of Physics and Astronomy, Bloomberg Center, The Johns Hopkins University, Baltimore, MD 21218.), AD(Department of Physics, Faculty of Science, Ehime University, Bunkyo-cho, Matsuyama, Ehime 790-8577, Japan.), AE(Institute of Space and Astronautical Science, 3-1-1 Yoshinodai, Sagamihara, Kanagawa 229-8510, Japan.)
Publication:
The Astrophysical Journal, Volume 618, Issue 1, pp. 167-177. (ApJ Homepage)
Publication Date:
01/2005
Origin:
UCP
ApJ Keywords:
Galaxies: Individual: NGC Number: NGC 7130, Galaxies: Seyfert, X-Rays: Galaxies
DOI:
10.1086/425913
Bibliographic Code:
2005ApJ...618..167L

Abstract

Observations of the Seyfert 2 and starburst galaxy NGC 7130 with the Chandra X-Ray Observatory illustrate that both of these phenomena contribute significantly to the galaxy's detectable X-ray emission. The active galactic nucleus (AGN) is strongly obscured, buried beneath column density NH>1024cm-2, and it is most evident in a prominent Fe Kα emission line with equivalent width greater than 1 keV. The AGN accounts for most (60%) of the observed X-rays at energy E>2 keV, with the remainder due to spatially extended star formation. The soft X-ray emission is strong and predominantly thermal on both small and large scales. We attribute the thermal emission to stellar processes. In total, the AGN is responsible for only one-third of the observed 0.5-10 keV luminosity of 3×1041ergss-1 of this galaxy and less than half of its bolometric luminosity. Starburst/AGN composite galaxies like NGC 7130 are truly common, and similar examples may contribute significantly to the high-energy cosmic X-ray background while remaining hidden at lower energies, especially if they are distant.
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