Faint AGN and the Ionizing Background

Abstract

We determine the evolution of the faint, high-redshift, optical luminosity function (LF) of AGN implied by several observationally-motivated models of the ionizing background. Our results depend crucially on whether we use the total ionizing rate measured by the proximity effect technique or the lower determination from the flux decrement distribution of Ly alpha forest lines. Assuming a faint-end LF slope of 1.58 and the SDSS estimates of the bright-end slope and normalization, we find that the LF must break at M_B*=-24.2,-22.3, -20.8 at z=3,4, 5 if we adopt the lower ionization rate and assume no stellar contribution to the background. The break must occur at M_B*=-20.6,-18.7, -18.7 for the proximity effect background estimate. These values brighten by as much as ~2 mag if high-z galaxies contribute to the background with an escape fraction of ionizing photons consistent with recent estimates: f_e=0.16. By comparing to faint AGN searches, we find that the typically-quoted proximity effect estimates of the background imply an over-abundance of faint AGN (even with f_e=1). Even adopting the lower bound on proximity effect measurements, the stellar escape fraction must be high: f_e>0.2. Conversely, the lower flux- decrement-derived background requires a limited stellar contribution: f_e<0.05. Our derived LFs together with the locally-estimated black hole density suggest that the efficiency of converting mass to light in optically-unobscured AGN is somewhat lower than expected, <0.05. Comparison with similar estimates based on X-ray counts suggests that more than half of all AGN are obscured in the UV/optical. We also derive lower limits on typical AGN lifetimes and obtain >10^7 yrs for favored cases.