Massive black hole remnants of the first stars II: optical and X-ray signatures in present-day galactic haloes

Details Massive black hole remnants of the first stars II: optical and X-ray signatures in present-day galactic haloes Massive black hole remnants of the first stars II: optical and X-ray signatures in present-day galactic haloes

2003-09-20

arxiv.org/abs/astro-ph/0309558v2

Mon.Not.Roy.Astron.Soc.354:443,2004

Astronomy and Astrophysics

Astrophysics

14 pages, 10 figures; updated to match published version

Scientific paper

10.1111/j.1365-2966.2004.08202.x

The first stars forming in minihaloes at redshifts greater than 20 may have been very massive and could have left behind massive black hole (MBH) remnants. In a previous paper we investigated the hierarchical merging of these MBHs and their associated haloes, using a semi-analytical approach consisting of a hierarchical merger tree algorithm and explicit prescriptions for the dynamics of merged substructure inside a larger host halo following a merger. One of the results was the prediction of a number of MBHs orbiting throughout present-day galactic haloes. In addition we determined the mass accretion rate of these MBHs assuming that they could in principle remain embedded in a gaseous core that is a remnant of the haloes with which the MBHs were associated before merging with the host system. On this basis we determine in this paper the bolometric, optical and X-ray luminosity functions for the accreting MBHs using thin disk and advection dominated accretion flow models. Our predicted MBH X-ray emissions are then compared with observations of ultra-luminous X-ray sources in galaxies. We find that the slope and normalisation of the predicted X-ray luminosity function are consistent with the observations.

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