Clustering of High Redshift ($z\ge 2.9$) Quasars from the Sloan Digital Sky Survey

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dc.creatorShen, Yue
dc.creatorStrauss, Michael A.
dc.creatorOguri, Masamune
dc.creatorHennawi, Joseph F.
dc.creatorFan, Xiaohui
dc.creatorRichards, Gordon T.
dc.creatorHall, Patrick B.
dc.creatorGunn, James E.
dc.creatorSchneider, Donald P.
dc.creatorSzalay, Alexander S.
dc.creatorThakar, Anirudda R.
dc.creatorBerk, Daniel E. Vanden
dc.creatorAnderson, Scott F.
dc.creatorBahcall, Neta A.
dc.creatorConnolly, Andrew J.
dc.creatorKnapp, Gillian R.
dc.date2007-02-07
dc.date.accessioned2026-07-07T11:21:07Z
dc.date.available2026-07-07T11:21:07Z
dc.description(Abridged) We study the two-point correlation function of a uniformly selected sample of 4,426 luminous optical quasars with redshift $2.9 \le z\le 5.4$ selected over 4041 deg$^2$ from the Fifth Data Release of the Sloan Digital Sky Survey. For a real-space correlation function of the form $ξ(r)=(r/r_0)^{-γ}$, the fitted parameters in comoving coordinates are $r_0 = 15.2 \pm 2.7 h^{-1}$ Mpc and $γ= 2.0 \pm 0.3$, over a scale range $4\le r_p\le 150 h^{-1}$ Mpc. Thus high-redshift quasars are appreciably more strongly clustered than their $z \approx 1.5$ counterparts, which have a comoving clustering length $r_0 \approx 6.5 h^{-1}$ Mpc. Dividing our sample into two redshift bins: $2.9\le z\le 3.5$ and $z\ge 3.5$, and assuming a power-law index $γ=2.0$, we find a correlation length of $r_0 = 16.9 \pm 1.7 h^{-1}$ Mpc for the former, and $r_0 = 24.3 \pm 2.4 h^{-1}$ Mpc for the latter. Following Martini & Weinberg, we relate the clustering strength and quasar number density to the quasar lifetimes and duty cycle. Using the Sheth & Tormen halo mass function, the quasar lifetime is estimated to lie in the range $4\sim 50$ Myr for quasars with $2.9\le z\le 3.5$; and $30\sim 600$ Myr for quasars with $z\ge 3.5$. The corresponding duty cycles are $0.004\sim 0.05$ for the lower redshift bin and $0.03\sim 0.6$ for the higher redshift bin. The minimum mass of halos in which these quasars reside is $2-3\times 10^{12}\ h^{-1}M_\odot$ for quasars with $2.9\le z\le 3.5$ and $4-6\times 10^{12}\ h^{-1}M_\odot$ for quasars with $z\ge 3.5$.
dc.descriptionTo appear in AJ; 20 emulateapj pages; supplemental materials can be found at http://www.astro.princeton.edu/~yshen/highz_qso_clustering/qso_clustering.htm
dc.identifierhttps://arxiv.org/abs/astro-ph/0702214
dc.identifierhttp://arxiv.org/abs/astro-ph/0702214
dc.identifierAstron.J.133:2222-2241,2007
dc.identifierdoi:10.1086/513517
dc.identifier.urihttp://salesiana.dossiersoluciones.com/handle/123456789/194170
dc.subjectAstrophysics
dc.titleClustering of High Redshift ($z\ge 2.9$) Quasars from the Sloan Digital Sky Survey
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