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Subaru High-z Exploration of Low-Luminosity Quasars (SHELLQs). V. Quasar Luminosity Function and Contribution to Cosmic Reionization at z = 6 | | Yoshiki Matsuoka
; Michael A. Strauss
; Nobunari Kashikawa
; Masafusa Onoue
; Kazushi Iwasawa
; Ji-Jia Tang
; Chien-Hsiu Lee
; Masatoshi Imanishi
; Tohru Nagao
; Masayuki Akiyama
; Naoko Asami
; James Bosch
; Hisanori Furusawa
; Tomotsugu Goto
; James E. Gunn
; Yuichi Harikane
; Hiroyuki Ikeda
; Takuma Izumi
; Toshihiro Kawaguchi
; Nanako Kato
; Satoshi Kikuta
; Kotaro Kohno
; Yutaka Komiyama
; Robert H. Lupton
; Takeo Minezaki
; Satoshi Miyazaki
; Hitoshi Murayama
; Mana Niida
; Atsushi J. Nishizawa
; Akatoki Noboriguchi
; Masamune Oguri
; Yoshiaki Ono
; Masami Ouchi
; Paul A. Price
; Hiroaki Sameshima
; Andreas Schulze
; Hikari Shirakata
; John D. Silverman
; Naoshi Sugiyama
; Philip J. Tait
; Masahiro Takada
; Tadafumi Takata
; Masayuki Tanaka
; Yoshiki Toba
; Yousuke Utsumi
; Shiang-Yu Wang
; Takuji Yamashita
; | | Date: |
5 Nov 2018 | | Abstract: | We present new measurements of the quasar luminosity function (LF) at $z sim
6$, over an unprecedentedly wide range of the rest-frame ultraviolet luminosity
$M_{1450}$ from $-30$ to $-22$ mag. This is the fifth in a series of
publications from the Subaru High-$z$ Exploration of Low-Luminosity Quasars
(SHELLQs) project, which exploits the deep multi-band imaging data produced by
the Hyper Suprime-Cam (HSC) Subaru Strategic Program survey. The LF was
calculated with a complete sample of 110 quasars at $5.7 le z le 6.5$, which
includes 48 SHELLQs quasars discovered over 650 deg$^2$, and 63 brighter
quasars discovered by the Sloan Digital Sky Survey and the Canada-France-Hawaii
Quasar Survey (including one overlapping object). This is the largest sample of
$z sim 6$ quasars with a well-defined selection function constructed to date,
and has allowed us to detect significant flattening of the LF at its faint end.
A double power-law function fit to the sample yields a faint-end slope $alpha
= -1.23^{+0.44}_{-0.34}$, a bright-end slope $eta = -2.73^{+0.23}_{-0.31}$, a
break magnitude $M_{1450}^* = -24.90^{+0.75}_{-0.90}$, and a characteristic
space density $Phi^* = 10.9^{+10.0}_{-6.8}$ Gpc$^{-3}$ mag$^{-1}$. Integrating
this best-fit model over the range $-18 < M_{1450} < -30$ mag, quasars emit
ionizing photons at the rate of $dot{n}_{
m ion} = 10^{48.8 pm 0.1}$
s$^{-1}$ Mpc$^{-3}$ at $z = 6.0$. This is less than 10 % of the critical rate
necessary to keep the intergalactic medium ionized, which indicates that
quasars are not a major contributor to cosmic reionization. | | Source: | arXiv, 1811.1963 | | Services: | Forum | Review | PDF | Favorites | |
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