Аннотация
In this paper, we provide updated constraints on the bolometric quasar
luminosity function (QLF) from $z=0$ to $z=7$. The constraints are based on an
observational compilation that includes observations in the rest-frame IR, B
band, UV, soft and hard X-ray in past decades. Our method follows
Hopkins2007 with an updated quasar SED model and bolometric and
extinction corrections. The new best-fit bolometric quasar luminosity function
behaves qualitatively different from the Hopkins2007 model at high
redshift. The bright-end slope is steeper at $z2$ compared with the old
model. The faint-end slope is steeper at $z3$ and becomes progressively
steeper at higher redshifts. The steep faint-end slope we constrain is
primarily driven by observations in the rest-frame UV and could be affected by
the lack of measurements of the faint-end QLF. Multi-band observations on the
faint-end QLF are needed to confirm this trend. The evolutionary pattern of the
bolometric QLF can be interpreted as an early phase likely dominated by the
hierarchical assembly of structures and a late phase likely dominated by the
quenching of galaxies. We explore the implications of this model on the
ionizing photon production by quasars, the CXB spectrum, the SMBH mass density
and mass functions. The predicted hydrogen ionization rate contributed by
quasars is subdominant during the epoch of reionization and only becomes
important at $z3$. The predicted CXB spectrum, cosmic SMBH mass
density and SMBH mass function are generally consistent with existing
observations.
Пользователи данного ресурса
Пожалуйста,
войдите в систему, чтобы принять участие в дискуссии (добавить собственные рецензию, или комментарий)