Lacy, M. and Sajina, A. and Gates, E. (2006) Radio galaxies and type-2 quasars in the Spitzer Extragalactic First Look Survey. Astronomische Nachrichten, 327 (2-3). pp. 258-261. ISSN 0004-6337 http://resolver.caltech.edu/CaltechAUTHORS:20110602-135032880
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We use mid-infrared colour-colour plots made with data from the Spitzer First Look Survey to explore the emission mechanisms of faint radio sources in that field. Using mid-infrared colours alone, we are able to see the transition from a starburst-dominated radio source population at sub-mJy levels to the radiogalaxy/quasar population at mJy levels. Both FR I and some FR II galaxies show little or no mid-infrared excess, suggesting they either lack dusty tori, or a strong continuum source to heat them, or both. Objects with hot, dusty tori, most likely radio-intermediate and radio-quiet AGN, make up a significant fraction of the faint radio source population. We also discuss the use of mid-infrared colour-colour plots to select radio quiet obscured AGN. Early results from imaging the host galaxies of these type-2 quasars at high spatial resolution with adaptive optics indicates that they, like type-1 quasars and radio galaxies, are often found to be hosted by giant elliptical galaxies.
|Additional Information:||© 2006 Wiley-VCH Verlag GmbH & Co. KGaA, Weinheim. Received 8 October 2005; accepted 15 November 2005; published online 20 February 2006. We would like to thank Gabriela Canalizo, Steve Rawlings and Alejo Martinez-Sansigre for helping with obtaining redshifts for some of the type-2 quasars.|
|Subject Keywords:||galaxies : active; quasars : general; infrared : general|
|Official Citation:||Lacy, M., Sajina, A., Gates, E. and the XFLS Team (2006), Radio galaxies and type-2 quasars in the Spitzer Extragalactic First Look Survey. Astronomische Nachrichten, 327: 258–261. doi: 10.1002/asna.200510518|
|Usage Policy:||No commercial reproduction, distribution, display or performance rights in this work are provided.|
|Deposited By:||Tony Diaz|
|Deposited On:||14 Jun 2011 19:54|
|Last Modified:||14 Jun 2011 19:54|
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