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Can AGN (Active Galactic Nuclei) Alone Make the Cosmic X-ray Background?

Published online by Cambridge University Press:  19 July 2016

Darryl Leiter  and
Elihu Boldt
Darryl Leiter
Affiliation:
Laboratory for High Energy Astrophysics, NASA/Goddard Space Flight Center, Greenbelt, MD 20771
Elihu Boldt
Affiliation:
Laboratory for High Energy Astrophysics, NASA/Goddard Space Flight Center, Greenbelt, MD 20771

Extract

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Recent ROSAT X-ray observations of AGN have yielded important new information about the analytic structure of the AGN X-ray luminosity function and its evolution out to z = 3. Using the luminosity evolution obtained within the cosmological context of Ω=0, we find[ that AGN could readily make up the CXB (cosmic X-ray background). However, in this case we find that accounting for the CXB with accretion-powered AGN emission is incompatible with the observed mass function for present-epoch black hole galactic nuclei (both active and dormant). On the other hand, we find that the luminosity evolution obtained with ROSAT for such AGN within the cosmological context of Ω=1 is indeed compatible with the present-epoch black hole galactic nuclei mass function. This apparently acceptable solution, though, definitely falls short of accounting for all the CXB, even when considering unified models for AGN. This difficulty can be resolved by noting that the underlying supermassive black holes which already exist at the onset of the canonical AGN phenomenon of supply-limited accretion must have undergone a previous growth phase where the accretion would be expected to be Eddington-limited. In this likely scenario (i.e., for Ω=1) the residual CXB, that over and above the foreground of canonical AGN, can be naturally explained by the characteristic X-ray emission from highly compact PAG (precursor active galaxy) sources associated with these numerous black holes, at redshifts just beyond the earliest AGN.

Type
Poster Contributions: X-Rays and Higher Energies
Information
Symposium - International Astronomical Union , Volume 159: Multi-Wavelength Continuum Emission of AGN , 1994 , pp. 378
Copyright
Copyright © Kluwer 1994 

References

1. Boyle, et al. 1993, MNRAS, 260, 49.Google Scholar
2. Madau, P., Ghisellini, G., & Fabian, A., 1993, ApJ., 410, L7.Google Scholar
3. Zdziarski, A., Zycki, P., & Krolik, J., 1993, ApJ., 414, L81.Google Scholar
4. Comastri, A. Setti, G., Zamoriani, G., & Hasinger, G., 1993, First Stromlo Symposium, Canberra, Australia.Google Scholar
5. Boldt, E., & Leiter, D., 1993, First Stromlo Symposium, Canberra, Australia.Google Scholar
6. Leiter, D., & Boldt, E., 1993, submitted to ApJ. Letters.Google Scholar