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Persistent URL http://purl.org/net/epubs/work/10918564
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Record Id 10918564
Title Infrared power-law galaxies in the chandra deep field-south: Active galactic nuclei and ultraluminous infrared galaxies
Abstract We investigate the nature of a sample of 92 Spitzer MIPS 24 ?m-selected galaxies in the CDF-S, showing power-law-like emission in the Spitzer IRAC 3.6-8 ?m bands. The main goal is to determine whether the galaxies not detected in X-rays (47% of the sample) are part of the hypothetical population of obscured AGNs not detected even in deep X-ray surveys. The majority of the IR power-law galaxies are ULIRGs at z > 1, and those with LIRG-like IR luminosities are usually detected in X-rays. The optical-to-IR SEDs of the X-ray-detected galaxies are almost equally divided between a BLAGN SED class (similar to an optically selected QSO) and an NLAGN SED (similar to the BLAGN SED but with an obscured UV/optical continuum). A small fraction of SEDs resemble warm ULIRGs (e.g., Mrk 231). Most galaxies not detected in X-rays have SEDs in the NLAGN+ULIRG class as they tend to be optically fainter and possibly more obscured. Moreover, the IR power-law galaxies have SEDs significantly different from those of high-z (z > 1) IR (24 ?m) selected and optically bright (WDS I ? 24) star-forming galaxies whose SEDs show a very prominent stellar bump at 1.6 ?m. The galaxies detected in X-rays have 2-8 keV rest-frame luminosities typical of AGNs. The galaxies not detected in X-rays have global X-ray-to-mid-IR SED properties that make them good candidates to contain IR-bright X-ray-absorbed AGNs. If all these sources are actually obscured AGNs, we would observe a ratio of obscured to unobscured 24 ?m-detected AGNs of 2:1, whereas models predict a ratio of up to 3:1. Additional studies using Spitzer to detect X-ray-quiet AGNs are likely to find more such obscured sources. © 2006. The American Astronomical Society. All rights reserved.
Organisation CCLRC , SSTD , SSTD-SP
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Language English (EN)
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Journal Article Astrophys J Lett Ed 640 (2006): 167-184. doi:10.1086/499800 2006
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