Heavily Obscured AGN in Star-Forming Galaxies at z 2

• Published in: The Astrophysical journal 2009-11, Vol.706 (1), p.535-552
• Main Authors: Treister, E, Cardamone, Carolin N, Schawinski, Kevin, Urry, C. Megan, Gawiser, Eric, Virani, Shanil, Lira, Paulina, Kartaltepe, Jeyhan, Damen, Maaike, Taylor, Edward N, Le Floc'h, Emeric, Justham, Stephen, Koekemoer, Anton M
• Format: Article
• Language: English
• Subjects: Astronomy; Earth, ocean, space; Exact sciences and technology
• ISSN: 0004-637X; 1538-4357
• DOI: 10.1088/0004-637X/706/1/535

We study the properties of a sample of 211 heavily obscured active galactic nucleus (AGN) candidates in the extended Chandra Deep Field-South selecting objects with f 24 Delta *mm/fR > 1000 and R - K>4.5. Of these, 18 were detected in X-rays and found to be obscured AGNs with neutral hydrogen column densities of ~1023 cm-2. In the X-ray-undetected sample, the following evidence suggests a large fraction of heavily obscured (Compton-thick) AGN: (1) The stacked X-ray signal of the sample is strong, with an observed ratio of soft to hard X-ray counts consistent with a population of ~90% heavily obscured AGNs combined with 10% star-forming galaxies. (2) The X-ray-to-mid-IR ratios for these sources are significantly larger than that of star-forming galaxies and ~2 orders of magnitude smaller than for the general AGN population, suggesting column densities of N H 5 X 1024 cm-2. (3) The Spitzer near- and mid-IR colors of these sources are consistent with those of the X-ray-detected samples if the effects of dust self-absorption are considered. Spectral fitting to the rest-frame UV/optical light (dominated by the host galaxy) returns stellar masses of ~1011 M and E(B - V) = 0.5, and reveals evidence for a significant young stellar population, indicating that these sources are experiencing considerable star formation. This sample of heavily obscured AGN candidates implies a space density at z ~ 2 of ~10-5 Mpc-3, finding a strong evolution in the number of LX >1044 erg s-1 sources from z = 1.5 to 2.5, possibly consistent with a short-lived heavily obscured phase before an unobscured quasar is visible.