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arXiv 1804.06409astro-ph.GA
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XXL调查XXXII。XXL-S AGN的空间聚类

The XXL Survey XXXII. Spatial clustering of the XXL-S AGN

M. Plionis, L. Koutoulidis, E. Koulouridis, L. Moscardini, C. Lidman, M. Pierre, C. Adami, L. Chiappetti, L. Faccioli, S. Fotopoulou, F. Pacaud, S. Paltani

备注：
accepted in A&A
发表信息：
A&A 620, A17 (2018)
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摘要：

XMM-XXL巡天跨越两个$\rm 25$ deg $^2$场，每个场用XMM观测超过6 M，提供了数万个点源的样本，通量极限分别为$\sim 2.2 \times 10^{-15}$和$\sim 1.4 \times 10^{-14}$ erg s $^{-1}$ cm $^{2}$，分别对应于软带和硬带面积曲线的50%。本文介绍了用AAOmega装置观测到的$\sim 3100$和$\sim 1900$ X射线活动星系核（AGN）在0.5-2和2-10 keV波段的空间成团性质。这个样品是90%的红移完成下降到$r\lesssim 21.8$的光学幅度限制。源跨越红移区间$0<z<5.2$，尽管在当前的分析中，我们将样本限制为$z\le 3$，软带和硬带的相应样本中值分别为$\bar{z}\simeq 0.96$和0.79。我们采用投影的两点相关函数来推断空间聚类，并找到一个相关长度$r_0=7.0 (\pm 0.34)$和6.42 $(\pm 0.42)$ $h^{-1}$ Mpc，分别为软，硬带检测源与斜率为$γ=1.44 (\pm 0.1)$的情况下。在1和$\sim$ 25 $h^{-1}$ Mpc的共动分离内检测到幂律聚类。这些结果，以及在两个单独的红移范围内得出的结果，提供了相应的活动星系核宿主暗物质晕的偏置因子，与$\log_{10} [M_h/(h^{-1} M_{\odot})]=13.04\pm 0.06$的晕质量一致，证实了最近基于较小的X射线活动星系核样品的研究结果。

英文摘要：

The XMM-XXL Survey spans two fields of $\rm 25$ deg$^2$ each observed for more than 6Ms with XMM, which provided a sample of tens of thousands of point sources with a flux limit of $\sim 2.2 \times 10^{-15}$ and $\sim 1.4 \times 10^{-14}$ erg s$^{-1}$ cm$^{2}$, corresponding to 50% of the area curve, in the soft band and hard band, respectively. In this paper we present the spatial clustering properties of $\sim 3100$ and $\sim 1900$ X-ray active galactic nuclei (AGNs) in the 0.5-2 and 2-10 keV bands, respectively, which have been spectroscopically observed with the AAOmega facility. This sample is 90% redshift complete down to an optical magnitude limit of $r\lesssim 21.8$. The sources span the redshift interval $0<z<5.2$, although in the current analysis we limit our samples to $z\le 3$, with corresponding sample median values of $\bar{z}\simeq 0.96$ and 0.79 for the soft band and hard band, respectively. We employ the projected two-point correlation function to infer the spatial clustering and find a correlation length $r_0=7.0 (\pm 0.34)$ and 6.42$(\pm 0.42)$ $h^{-1}$ Mpc, respectively, for the soft- and hard-band detected sources with a slope for both cases of $γ=1.44 (\pm 0.1)$. The power-law clustering was detected within comoving separations of 1 and $\sim$25 $h^{-1}$ Mpc. These results, as well as those derived in two separate redshift ranges, provide bias factors of the corresponding AGN host dark matter halos that are consistent with a halo mass of $\log_{10} [M_h/(h^{-1} M_{\odot})]=13.04\pm 0.06$, confirming the results of most recent studies based on smaller X-ray AGN samples.

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