Clustering of quasars in a wide luminosity range at redshift 4 with Subaru Hyper Suprime-Cam wide field imaging

Abstract

We examine the clustering of quasars over a wide luminosity range, by utilizing 901 quasars at ${\overline{z}}_{\mathrm{phot}}\sim 3.8$ with $-24.73<M_{1450}<-22.23$ photometrically selected from the Hyper Suprime-Cam Subaru Strategic Program (HSC-SSP) S16A Wide2 date release and 342 more luminous quasars at $3.4<z_{\mathrm{spec}}<4.6$ having $-28.0<M_{1450}<-23.95$ from the Sloan Digital Sky Survey (SDSS) that fall in the HSC survey fields. We measure the bias factors of two quasar samples by evaluating the cross-correlation functions (CCFs) between the quasar samples and 25790 bright $z\sim 4$ Lyman Break Galaxies (LBGs) in $M_{1450}<-21.25$ photometrically selected from the HSC dataset. Over an angular scale of \timeform{10.0"} to \timeform{1000.0"}, the bias factors are $5.93_{-1.43}^{+1.34}$ and $2.73_{-2.55}^{+2.44}$ for the low and high luminosity quasars, respectively, indicating no luminosity dependence of quasar clustering at $z\sim 4$. It is noted that the bias factor of the luminous quasars estimated by the CCF is smaller than that estimated by the auto-correlation function (ACF) over a similar redshift range, especially on scales below \timeform{40.0"}. Moreover, the bias factor of the less-luminous quasars implies the minimal mass of their host dark matter halos (DMHs) is $0.3$-$2\times 10^{12}{h}^{-1}{M}_{\odot }$, corresponding to a quasar duty cycle of $0.001$-$0.06$.

20 pages, 10 figures, submitted to PASJ

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