QUASAR CLUSTERING FROM SDSS DR5: DEPENDENCES ON PHYSICAL PROPERTIES
QUASAR CLUSTERING FROM SDSS DR5: DEPENDENCES ON PHYSICAL PROPERTIES
复制标题
DOI：
10.1088/0004-637x/697/2/1656
复制
发表时间：
2008-10
期刊：
影响因子：
--
通讯作者：
Yue Shen;M. Strauss;N. Ross;P. Hall;Yen-Ting Lin;G. Richards;D. Schneider;D. Weinberg;A. Connolly;Xiaohui Fan;J. Hennawi;F. Shankar;D. V. vanden Berk;N. Bahcall;R. Brunner
中科院分区：
文献类型：
--
作者：
Yue Shen;M. Strauss;N. Ross;P. Hall;Yen-Ting Lin;G. Richards;D. Schneider;D. Weinberg;A. Connolly;Xiaohui Fan;J. Hennawi;F. Shankar;D. V. vanden Berk;N. Bahcall;R. Brunner
使用一个均匀的样本38,208类星体的天空覆盖范围为104000 deg 2绘制从斯隆数字巡天数据发布五类星体目录，我们研究了类星体集群的依赖光度，维里黑洞（BH）的质量，类星体的颜色，和射电响度。在z < 2.5时，类星体的成团与光度和维里黑洞质量的关系很弱，测量的相关长度的不确定度一般在10%左右。这些弱的依赖性是一致的模型中，类星体的光度，维里BH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，晕质量被假定为相关的数量，最好的集群强度。然而，最明亮和最大质量的类星体比样本的其余部分更强烈地聚集在一起（在102 σ水平上），我们将其归因于宿主晕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，射电大声类星体比射电安静类星体在红移和光学光度（或维里BH质量）方面匹配的类星体聚集得更强烈，这与射电星系和射电大声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，射电强的类星体存在于更大质量和更密集的环境中。使用Sheth等人（2001）的线性晕偏差公式，射电强的类星体的主晕质量估计为1013 h−1 M，而射电静的类星体主晕质量为102 × 1012 h−1 M。
Using a homogenous sample of 38,208 quasars with a sky coverage of ∼4000 deg2 drawn from the Sloan Digital Sky Survey Data Release Five quasar catalog, we study the dependence of quasar clustering on luminosity, virial black hole (BH) mass, quasar color, and radio loudness. At z < 2.5, quasar clustering depends weakly on luminosity and virial BH mass, with typical uncertainty levels ∼10% for the measured correlation lengths. These weak dependences are consistent with models in which substantial scatter between quasar luminosity, virial BH 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 ∼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 BH mass), consistent with local observations of radio galaxies and radio-loud type 2 active galactic nuclei. 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 ∼1013 h−1 M☉, compared to ∼2 × 1012 h−1 M☉ for radio-quiet quasar hosts at z ∼ 1.5.