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Title:
Early Reionization by Miniquasars
Authors:
Madau, P.; Rees, M. J.; Volonteri, M.; Haardt, F.; Oh, S. P.
Affiliation:
AA(Department of Astronomy and Astrophysics, University of California, 477 Clark Kerr Hall, Santa Cruz, CA 95064.; Carnegie Observatories, Carnegie Institution of Washington, 813 Santa Barbara Street, Pasadena, CA 91101.), AB(Institute of Astronomy, University of Cambridge, Madingley Road, Cambridge CB3 0HA, UK.), AC(Department of Astronomy and Astrophysics, University of California, 477 Clark Kerr Hall, Santa Cruz, CA 95064.), AD(Dipartimento di Scienze, Università dell'Insubria/Sede di Como, Italy.), AE(Department of Physics, University of California, Santa Barbara, CA 93106.)
Publication:
The Astrophysical Journal, Volume 604, Issue 2, pp. 484-494. (ApJ Homepage)
Publication Date:
04/2004
Origin:
UCP
ApJ Keywords:
Black Hole Physics, Cosmology: Theory, Galaxies: Evolution, Galaxies: Intergalactic Medium, Galaxies: Quasars: General
DOI:
10.1086/381935
Bibliographic Code:
2004ApJ...604..484M

Abstract

Motivated by the recent detection by the Wilkinson Microwave Anisotropy Probe of a large optical depth to Thomson scattering, implying a very early reionization epoch, we assess a scenario where the universe was reionized by ``miniquasars'' powered by intermediate-mass black holes (IMBHs), the remnants of the first generation of massive stars. Pregalactic IMBHs form within minihalos above the cosmological Jeans mass collapsing at z>20, get incorporated through mergers into larger and larger systems, sink to the center as a result of dynamical friction, and accrete cold material. The merger history of dark halos and associated IMBHs is followed by Monte Carlo realizations of the merger hierarchy in a ΛCDM cosmology. Our model is based on the assumptions that quasar activity is driven by major mergers and nuclear IMBHs accrete at the Eddington rate a fraction of the gas in the merger remnant. The long dynamical frictional timescales leave many IMBHs ``wandering'' in galaxy halos after a minor merger. While seed IMBHs that are as rare as the 3.5 σ peaks of the primordial density field evolve largely in isolation, a significant number of BH binary systems will form if IMBHs populate the more numerous 3 σ peaks instead. In the case of rapid binary coalescence a fraction of IMBHs will be displaced from galaxy centers and ejected into the intergalactic medium (IGM) by the ``gravitational rocket'' effect, rather than accrete and shine as miniquasars. We show that, under a number of plausible assumptions for the amount of gas accreted onto IMBHs and their emission spectrum, miniquasars powered by IMBHs, and not their stellar progenitors, may be responsible for cosmological reionization at z~15. Reionization by miniquasars with a hard spectrum may be more ``economical'' than stellar reionization, as soft X-rays escape more easily from the dense sites of star formation and travel farther than EUV radiation. Energetic photons will permeate the universe more uniformly, make the low-density diffuse IGM warm and weakly ionized prior to the epoch of reionization breakthrough, set an entropy floor, and reduce gas clumping. Future 21 cm observations may detect a preheated, weakly ionized IGM in emission against the cosmic microwave background.
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