Astronomy and Astrophysics – Astrophysics
Scientific paper
2004-11-19
Mon.Not.Roy.Astron.Soc. 357 (2005) 565-571
Astronomy and Astrophysics
Astrophysics
7 pages, accepted for publication in MNRAS
Scientific paper
10.1111/j.1365-2966.2005.08644.x
Prominent Fe K line emission is detected at around 6.7 keV in the XMM-Newton spectrum of the ultraluminous infrared galaxy Arp220. The continuum emission in the 2.5-10 keV band is flat and a few other spectral features are suggested. The large EW of the Fe K line poses a problem with interpreting the hard X-ray emission as integrated X-ray binary emission. A thermal emission spectrum with a temperature of kT~7 keV modified by some absorption, which would be expected from an internally shocked hot bubble in a starburst region, can describe the spectrum. An ensemble of radio supernovae in a dense environment, as suggested from VLBI imaging, could be another possibility, if frequent occurence of such powerful supernovae is sustained. However, the apparent lack of X-ray binary emission does not match the high supernova rate required by both interpretations. Highly photoionized, low-density gas illuminated by a hidden Compton-thick AGN is a possible alternative, which can be tested by presence/absence of radiative recombination continua in better quality data expected from a forthcoming observation.
Evans Aaron S.
Iwasawa Kashuzi
Miniutti Giovanni
Sanders David B.
Spoon Henrik W. W.
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