Publication: Characterization of active galactic nuclei and their hosts in the extended groth strip: a multiwavelength analysis
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2009-01
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IOP Publishing ltd
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Abstract
We have employed a reliable technique of classification of active galactic nuclei (AGNs) based on the fit of well sampled spectral energy distributions (SEDs) with a complete set of AGN and starburst galaxy templates. We have compiled UV, optical, and IR data for a sample of 116 AGNs originally selected for their X-ray and mid-IR emissions (96 with single detections and 20 with double optical counterparts). This is the most complete compilation of multiwavelength data for such a large sample of AGN in the Extended Groth Strip. Through these SEDs, we are able to obtain highly reliable photometric redshifts and to distinguish between pure and host-dominated AGNs. For the objects with unique detection we find that they can be separated into five main groups, namely: Starburst-dominated AGNs (24% of the sample), Starburst-contaminated AGNs (7%), Type-1 AGNs (21%), Type-2 AGNs (24%), and Normal galaxy hosting AGN (24%). We find these groups concentrated at different redshifts: Type-2 AGNs and Normal galaxy hosting AGNs are concentrated at low redshifts, whereas Starburst-dominated AGNs and Type-1 AGNs show a larger span. Correlations between hard/soft X-ray and UV, optical and IR luminosities are reported for the first time for such a sample of AGNs spanning a wide range of redshifts. For the 20 objects with double detection, the percentage of Starburst-dominated AGNs increases up to 48%.
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© 2009. The American Astronomical Society.
NASA’s Chandra X-Ray Observatory was launched in July 1999. The Chandra Data Archive (CDA) is part of the Chandra X-Ray Center (CXC) which is operated for NASA by the Smithsonian Astrophysical Observatory. This work is based on observations obtained with XMMNewton, an ESA Science Mission with instruments and contributions directly funded by ESA Member States and NASA. GALEX (Galaxy Evolution Explorer) is a NASA Small Explorer, launched in 2003 April. We gratefully acknowledge NASA’s support for construction, operation, and science analysis of the GALEX Mission, developed in cooperation with the Centre National d’Etudes Spatiales of France and the Korean Ministry of Science and Technology. This work is based in part on observations made with the Spitzer Space Telescope, which is operated by the Jet Propulsion Laboratory, California, Institute of Technology under a contract with NASA. This work is based on observations obtained with MegaPrime/ MegaCam, a joint project of CFHT and CEA/DAPNIA, at the Canada–France–Hawaii Telescope (CFHT) which is operated by the National Research Council (NRC) of Canada, the Institut National des Science de l’Univers of the Centre National de la Reserche Scientifique (CNRS) of France, and the University of Hawaii. This work is based in part on data products produced at TERAPIX and the Canadian Astronomy data Centre as part of the CFHT Legacy Survey, a collaborative project of NRC and CNRS. This work is based on observations obtained at the Hale Telescope, Palomar Observatory, as part of a collaborative agreement between the California Institute of Technology, its divisions Caltech Optical Observatories and the Jet Propulsion Laboratory (operated for NASA), and Cornell University. Many images of this article are based on observations made with the NASA/ESA Hubble Space Telescope, obtained from the data archive at the Space Telescope Science Institute (STScI). STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS5- 26555.
This work uses data obtained with support of the National Science Foundation grants AST 95-29028 and AST 00-71198.This work is partially funded by PN AYA2007-67965-C0301, PN AYA2006-02358, and by the Spanish MEC under the Consolider-Ingenio 2010 Program grant CSD2006-00070: First Science with the GTC (http://www.iac.es/consolider-ingeniogtc/). P. G. P.-G. acknowledges support from the Ramón y Cajal Program financed by the Spanish Government and the European Union. C. R. A., J. R. E., G. B., J. G., and P. G. P.-G. acknowledge Roser Pelló, Antonio Cabrera Lavers, and Casiana Muñoz Tuñon for their valuable help. We finally appreciate the very useful report of the anonymous referee.
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