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The Bolometric Quasar Luminosity Function at z = 0-7

, , , , , , and . (2020)cite arxiv:2001.02696Comment: Submitted to MNRAS. The code and data are available at https://bitbucket.org/ShenXuejian/quasarlf/src/master/. Comments are welcomed!.

Abstract

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.

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The Bolometric Quasar Luminosity Function at z = 0-7

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