On the faint end of the high redshift AGN luminosity function

Using the results of recent optical surveys we conclude that the non-detection of quasars down to faint magnitudes implies a significant flattening of the high redshift (z ∼ 6) optical active galactic nuclei (AGN) luminosity function for M1450 > −26.7. We find that all the data are consistent with a faint-end slope for the optical AGN luminosity function of β = −2.2 and β = −2.8, at the 90% and 99% confidence level respectively, flatter than the bright-end slope of β ∼ −3.2. We also show that X-ray deep surveys have probed even fainter magnitudes than the optical ones yielding more significant constraints on the shallow faint-end slope of the optical luminosity function. The inclusion of Type II AGN candidates, detected in the Chandra deep fields, hints towards an higher normalization for the total AGN luminosity function, if these sources lie at 5 . z . 6.5. We then discuss simple theoretical models of AGN formation and evolution in the context of cold dark matter cosmology. The comparison with the total AGN luminosity function favors a redshift-dependent relation between black hole and dark matter halo masses of the type M• ∝ M α halo, with 1.3 . α . 1.7, compatible with independent studies from statistical analysis and rotation curve measurements. Finally we compute the quasar contribution to reionization to be . 9% at z ∼ 6, up to ∼ 30% when integrated within 5.5 . z . 6.5, significantly smaller than that from galaxies. Subject headings: galaxies: active quasars:general