On the Contribution of Active Galactic Nuclei to the Cosmic Background Radiation
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We present the results of calculations of the cosmic AGN background spectrum from 3 keV (4 × 10-4 μm)to 1000 μm. These computations make use of the measured X-ray luminosity function and its evolution, as well as fits from synthesis models of the cosmic X-ray background (CXB), to predict the AGN contribution to the cosmic infrared background (CIRB) for different models of the location and distribution of the absorbing material. By comparing our results to observational constraints, we conclude that the current deep Spitzer surveys can account for the entire AGN contribution to the CIRB at 24 μm, but these AGNs are almost all Compton-thin. In fact, the calculations show that Compton-thick AGNs are a small fraction of the CIRB for λ < 100 μm. For this reason, the most efficient method of identifying the Compton-thick AGN population is through hard X-ray imaging at energies ≳40 keV. Selection of AGNs based on their rest-frame near-IR colors will miss low-luminosity type 2 AGNs, due to contamination from the host galaxy. Finally, the AGNs that dominate the CXB must have star formation rates < 100 M⊙ yr-1, consistent with them having properties similar to the sources that dominate the CIRB at Z ∼ 1. Including the estimated reradiated emission from star formation, AGNs and their host galaxies may contribute ∼30% of the CIRB at 70 μm, dropping to ∼10% at 24 μm and ∼1% at 1-10 μm. © 2007. The American Astronomical Society. All rights reserved.
author list (cited authors)
Ballantyne, D. R., & Papovich, C.