%0 Generic %1 niida2020faint %A Niida, Mana %A Nagao, Tohru %A Ikeda, Hiroyuki %A Akiyama, Masayuki %A Matsuoka, Yoshiki %A He, Wanqiu %A Matsuoka, Kenta %A Toba, Yoshiki %A Onoue, Masafusa %A Kobayashi, Masakazu A. R. %A Taniguchi, Yoshiaki %A Furusawa, Hisanori %A Harikane, Yuichi %A Imanishi, Masatoshi %A Kashikawa, Nobunari %A Kawaguchi, Toshihiro %A Komiyama, Yutaka %A Shirakata, Hikari %A Terashima, Yuichi %A Ueda, Yoshihiro %D 2020 %K library %T The Faint End of the Quasar Luminosity Function at $z 5$ from the Subaru Hyper Suprime-Cam Survey %U http://arxiv.org/abs/2010.00481 %X We present the quasar luminosity function at $z 5$ derived from the optical wide-field survey data obtained as a part of the Subaru strategic program (SSP) with Hyper Suprime-Cam (HSC). From $\sim$81.8 deg$^2$ area in the Wide layer of the HSC-SSP survey, we selected 224 candidates of low-luminosity quasars at $z 5$ by adopting the Lyman-break method down to $i = 24.1$ mag. Based on our candidates and spectroscopically-confirmed quasars from the Sloan Digital Sky Survey (SDSS), we derived the quasar luminosity function at $z 5$ covering a wide luminosity range of $-28.76 < M_1450 < -22.32$ mag. We found that the quasar luminosity function is fitted by a double power-law model with a break magnitude of $M^*_1450 = -25.05^+0.10_-0.24$ mag. The inferred number density of low-luminosity quasars is lower, and the derived faint-end slope, $-1.22^+0.03_-0.10$, is flatter than those of previous studies at $z 5$. A compilation of the quasar luminosity function at $4 z 6$ from the HSC-SSP suggests that there is little redshift evolution in the break magnitude and in the faint-end slope within this redshift range, although previous studies suggest that the faint-end slope becomes steeper at higher redshifts. The number density of low-luminosity quasars decreases more rapidly from $z 5$ to $z 6$ than from $z 4$ to $z 5$.

@misc{niida2020faint, abstract = {We present the quasar luminosity function at $z \sim 5$ derived from the optical wide-field survey data obtained as a part of the Subaru strategic program (SSP) with Hyper Suprime-Cam (HSC). From $\sim$81.8 deg$^2$ area in the Wide layer of the HSC-SSP survey, we selected 224 candidates of low-luminosity quasars at $z \sim 5$ by adopting the Lyman-break method down to $i = 24.1$ mag. Based on our candidates and spectroscopically-confirmed quasars from the Sloan Digital Sky Survey (SDSS), we derived the quasar luminosity function at $z \sim 5$ covering a wide luminosity range of $-28.76 < M_{\rm 1450} < -22.32$ mag. We found that the quasar luminosity function is fitted by a double power-law model with a break magnitude of $M^{*}_{1450} = -25.05^{+0.10}_{-0.24}$ mag. The inferred number density of low-luminosity quasars is lower, and the derived faint-end slope, $-1.22^{+0.03}_{-0.10}$, is flatter than those of previous studies at $z \sim 5$. A compilation of the quasar luminosity function at $4 \leq z \leq 6$ from the HSC-SSP suggests that there is little redshift evolution in the break magnitude and in the faint-end slope within this redshift range, although previous studies suggest that the faint-end slope becomes steeper at higher redshifts. The number density of low-luminosity quasars decreases more rapidly from $z \sim 5$ to $z \sim 6$ than from $z \sim 4$ to $z \sim 5$.}, added-at = {2020-10-02T04:59:12.000+0200}, author = {Niida, Mana and Nagao, Tohru and Ikeda, Hiroyuki and Akiyama, Masayuki and Matsuoka, Yoshiki and He, Wanqiu and Matsuoka, Kenta and Toba, Yoshiki and Onoue, Masafusa and Kobayashi, Masakazu A. R. and Taniguchi, Yoshiaki and Furusawa, Hisanori and Harikane, Yuichi and Imanishi, Masatoshi and Kashikawa, Nobunari and Kawaguchi, Toshihiro and Komiyama, Yutaka and Shirakata, Hikari and Terashima, Yuichi and Ueda, Yoshihiro}, biburl = {https://www.bibsonomy.org/bibtex/28364643036051c9397943a65ae9038f7/gpkulkarni}, description = {The Faint End of the Quasar Luminosity Function at $z \sim 5$ from the Subaru Hyper Suprime-Cam Survey}, interhash = {c4b6a1879ee2bc837d960ef1ee52aeab}, intrahash = {8364643036051c9397943a65ae9038f7}, keywords = {library}, note = {cite arxiv:2010.00481Comment: 18 pages, 11 figures, accepted for publication in ApJ}, timestamp = {2020-10-02T04:59:12.000+0200}, title = {The Faint End of the Quasar Luminosity Function at $z \sim 5$ from the Subaru Hyper Suprime-Cam Survey}, url = {http://arxiv.org/abs/2010.00481}, year = 2020 }