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arXiv 0810.4144astro-ph
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SDSS DR5的类星体成团：物理性质的依赖性

Quasar Clustering from SDSS DR5: Dependences on Physical Properties

Yue Shen, Michael A. Strauss, Nicholas P. Ross, Patrick B. Hall, Yen-Ting Lin, Gordon T. Richards, Donald P. Schneider, David H. Weinberg, Andrew J. Connolly, X… 展开作者

Yue Shen, Michael A. Strauss, Nicholas P. Ross, Patrick B. Hall, Yen-Ting Lin, Gordon T. Richards, Donald P. Schneider, David H. Weinberg, Andrew J. Connolly, Xiaohui Fan, Joseph F. Hennawi, Francesco Shankar, Daniel E. Vanden Berk, Neta A. Bahcall, Robert J. Brunner

备注：
Updated version; accepted for publication in ApJ
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摘要：

利用从SDSS数据发布5类星体目录中抽取的天空覆盖率为$4000 {\rm deg^2}$的38，208个类星体的均匀样本，我们研究了类星体聚集对光度、维里黑洞质量、类星体颜色和射电响度的依赖性。在$z<2.5$，类星体集群弱依赖于光度和维里黑洞质量，与典型的不确定性水平$\sim 10%$的测量相关长度。这些弱的依赖性是一致的模型，其中类星体的光度，维里黑洞质量和主机暗物质晕质量之间的大量散射稀释了任何集群的差异，其中晕质量被假定为最相关的集群强度的相关量。然而，最明亮和最大质量的类星体更强烈的集群（在$\sim 2σ$水平）比样本的其余部分，我们归因于在主机晕的高质量端的偏置因子的快速增加。在我们的样本中，我们没有观察到聚类强度对类星体颜色的强烈依赖。另一方面，射电强的类星体比射电静的类星体在红移和光学光度（或维里黑洞质量）上更强烈地聚集在一起，这与射电星系和射电强的2型活动星系核的局部观测结果一致。因此，在有偏差的晕簇图中，射电噪声类星体存在于更大质量和更密集的环境中。使用Sheth et al.（2001）的线性晕偏差公式，射电强类星体的主晕质量估计为$\sim 10^{13} h^{-1}M_\odot$，而射电静类星体主晕质量估计为$\sim 2\times 10^{12} h^{-1}M_\odot$，在$z\sim 1.5$。

英文摘要：

Using a homogenous sample of 38,208 quasars with a sky coverage of $4000 {\rm deg^2}$ drawn from the SDSS Data Release Five quasar catalog, we study the dependence of quasar clustering on luminosity, virial black hole mass, quasar color, and radio loudness. At $z<2.5$, quasar clustering depends weakly on luminosity and virial black hole mass, with typical uncertainty levels $\sim 10%$ for the measured correlation lengths. These weak dependences are consistent with models in which substantial scatter between quasar luminosity, virial black hole mass and the host dark matter halo mass has diluted any clustering difference, where halo mass is assumed to be the relevant quantity that best correlates with clustering strength. However, the most luminous and most massive quasars are more strongly clustered (at the $\sim 2σ$ level) than the remainder of the sample, which we attribute to the rapid increase of the bias factor at the high-mass end of host halos. We do not observe a strong dependence of clustering strength on quasar colors within our sample. On the other hand, radio-loud quasars are more strongly clustered than are radio-quiet quasars matched in redshift and optical luminosity (or virial black hole mass), consistent with local observations of radio galaxies and radio-loud type 2 AGN. Thus radio-loud quasars reside in more massive and denser environments in the biased halo clustering picture. Using the Sheth et al.(2001) formula for the linear halo bias, the estimated host halo mass for radio-loud quasars is $\sim 10^{13} h^{-1}M_\odot$, compared to $\sim 2\times 10^{12} h^{-1}M_\odot$ for radio-quiet quasar hosts at $z\sim 1.5$.

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