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arXiv 0907.3753astro-ph.CO
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SDSS中的NoSOCS。II。利用光学和X射线特性对低红移星系团的质量刻度

NoSOCS in SDSS. II. Mass Calibration of Low Redshift Galaxy Clusters with Optical and X-ray Properties

P. A. A. Lopes, R. R. de Carvalho, J. L. Kohl-Moreira, C. Jones

备注：
27 pages, 22 figures, 12 tables, Accepted to MNRAS
发表信息：
MNRAS, 399:2201-2220, 2009
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摘要：

利用SDSS数据研究了127个NoSOCS和56个CIRS星系团在低红移（$z \le 0.10$）下的标度关系。我们表明，丰富度和光学和X射线光度是可靠的质量代理。在固定的可观察的质量散射是$\sim$ 40%，这取决于所考虑的孔径、样品和可观察。例如，对于大规模CIRS系统，$σ_{lnM500|N500}$ = 0.33 $\pm$ 0.05和$σ_{lnM500|Lx}$ = 0.48 $\pm$ 0.06。对于全样品，$σ_{lnM500|N500}$ = 0.43 $\pm$ 0.03和$σ_{lnM500|Lx}$ = 0.56 $\pm$ 0.06。我们估计使用二维和三维光学数据的子结构，验证子结构没有显着的影响集群的缩放关系（截距和斜率），独立的子结构测试，我们使用。对于一个子集的21个集群，我们估计质量的M-T $_X$关系使用温度测量BAX。从光学质量和X射线质量导出的标度关系确实非常相似，这表明我们的方法一致地估计团簇质量，并且无论我们测量质量的波长如何，都产生等效的结果。对于大质量系统，我们用一个形式为${\rm ln (M_{200}) = A + B \times ln(N_{200}/60)}$的函数来表示质量丰度关系，其中M $_{200}$以10 $^{14}$ M $_{\odot}$为单位来表示。使用维里质量，对于CIRS簇，我们发现A =（1.39 $\pm$ 0.07）和B =（1.00 $\pm$ 0.11）。基于维里质量的关系式的离散度为$σ_{lnM200|N200}$ = 0.37 $\pm$ 0.05，而对于苛性质量，$σ_{lnM200|N200}$ = 0.77 $\pm$ 0.22，对于基于温度的质量，$σ_{lnM200|N200}$ = 0.34 $\pm$ 0.08（简化）。

英文摘要：

We use SDSS data to investigate the scaling relations of 127 NoSOCS and 56 CIRS galaxy clusters at low redshift ($z \le 0.10$). We show that richness and both optical and X-ray luminosities are reliable mass proxies. The scatter in mass at fixed observable is $\sim$ 40%, depending on the aperture, sample and observable considered. For example, for the massive CIRS systems $σ_{lnM500|N500}$ = 0.33 $\pm$ 0.05 and $σ_{lnM500|Lx}$ = 0.48 $\pm$ 0.06. For the full sample $σ_{lnM500|N500}$ = 0.43 $\pm$ 0.03 and $σ_{lnM500|Lx}$ = 0.56 $\pm$ 0.06. We estimate substructure using two and three dimensional optical data, verifying that substructure has no significant effect on the cluster scaling relations (intercepts and slopes), independent of which substructure test we use. For a subset of twenty-one clusters, we estimate masses from the M-T$_X$ relation using temperature measures from BAX. The scaling relations derived from the optical and X-ray masses are indeed very similar, indicating that our method consistently estimates the cluster mass and yields equivalent results regardless of the wavelength from which we measure mass. For massive systems, we represent the mass-richness relation by a function with the form ${\rm ln (M_{200}) = A + B \times ln(N_{200}/60)}$, with M$_{200}$ being expressed in units of 10$^{14}$ M$_{\odot}$. Using the virial mass, for CIRS clusters, we find A = (1.39 $\pm$ 0.07) and B = (1.00 $\pm$ 0.11). The relations based on the virial mass have a scatter of $σ_{lnM200|N200}$ = 0.37 $\pm$ 0.05, while $σ_{lnM200|N200}$ = 0.77 $\pm$ 0.22 for the caustic mass and $σ_{lnM200|N200}$ = 0.34 $\pm$ 0.08 for the temperature based mass (abridged).

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