RT Journal Article
T1 The host galaxies and black holes of typical z~0.5-1.4 AGNs
A1 Alonso Herrero, Almudena
A1 Pérez González, Pablo Guillermo
A1 Rieke, George H.
A1 Alexander, David M.
A1 Rigby, Jane R.
A1 Papovich, Casey
A1 Donley, Jennifer L.
A1 Rigopoulou, Dimitra
AB We study the stellar and star formation properties of the host galaxies of 58 X-ray-selected AGNs in the GOODS portion of the Chandra Deep Field South (CDF-S) region at z ~ 0.5-1.4. The AGNs are selected such that their rest-frame UV to near-infrared spectral energy distributions (SEDs) are dominated by stellar emission; i.e., they show a prominent 1.6 μm bump, thus minimizing the AGN emission "contamination." This AGN population comprises approximately 50% of the X-ray-selected AGNs at these redshifts. We find that AGNs reside in the most massive galaxies at the redshifts probed here. Their characteristic stellar masses (M_* ~ 7.8 × 10^10 and M_* ~ 1.2 × 10^11 M_☉ at median redshifts of 0.67 and 1.07, respectively) appear to be representative of the X-ray-selected AGN population at these redshifts and are intermediate between those of local type 2 AGNs and high-redshift (z ~ 2) AGNs. The inferred black hole masses (M_BH ~ 2 × 10^8 M_☉) of typical AGNs are similar to those of optically identified quasars at similar redshifts. Since the AGNs in our sample are much less luminous (L_2–10 keV < 10^44 erg s^−1) than quasars, typical AGNs have low Eddington ratios (η ~ 0.01-0.001). This suggests that, at least at intermediate redshifts, the cosmic AGN "downsizing" is due to both a decrease in the characteristic stellar mass of typical host galaxies and less efficient accretion. Finally, there is no strong evidence in AGN host galaxies for either highly suppressed star formation (expected if AGNs played a role in quenching star formation) or elevated star formation when compared to mass-selected (i.e., IRAC-selected) galaxies of similar stellar masses and redshifts.
PB American Astronomical Society
SN 0004-637X
YR 2008
FD 2008-04-10
LK https://hdl.handle.net/20.500.14352/51934
UL https://hdl.handle.net/20.500.14352/51934
LA eng
NO © 2008 The American Astronomical Society. All rights reserved. The authors would like to thank P. Hopkins and M. Kriek for interesting discussions. The authors also thank an anonymous referee for useful suggestions that helped improve the paper. This work was supported by NASA through contract 1255094 issued by the JPL/California Institute of Technology. A. A.-H. acknowledges support from the Spanish Plan Nacional del Espacio under grant ESP2005-01480. P. G. P.-G. acknowledges support from the Ramón y Cajal Fellowship Program financed by the Spanish Government, and from the Spanish Programa Nacional de Astronomía y Astrofísica under grant AYA 2006-02358. This research has made use of the NASA/ IPAC Extragalactic Database (NED), which is operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration.
NO Ministerio de Economía y Competitividad (MINECO)
NO National Aeronautics and Space Administration (NASA)
NO California Institute of Technology (Caltech), NASA
NO Programa Nacional del Espacio (PNE)
NO Programa Nacional de Astronomía y Astrofísica (NAyA)
NO Jet Propulsion Laboratory (JPL), NASA
DS Docta Complutense
RD 20 abr 2025