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Bolocam Sunyaev-Zel'dovich效应与Chandra X射线测量的星系团标度关系

Galaxy Cluster Scaling Relations between Bolocam Sunyaev-Zel'dovich Effect and Chandra X-ray Measurements

N. G. Czakon, J. Sayers, A. Mantz, S. R. Golwala, T. P. Downes, P. M. Koch, K. -Y. Lin, S. M. Molnar, L. A. Moustakas, T. Mroczkowski, E. Pierpaoli, J. A. Shita… 展开作者

N. G. Czakon, J. Sayers, A. Mantz, S. R. Golwala, T. P. Downes, P. M. Koch, K. -Y. Lin, S. M. Molnar, L. A. Moustakas, T. Mroczkowski, E. Pierpaoli, J. A. Shitanishi, S. Siegel, K. Umetsu

备注：
31 pages, 15 figures, accepted by ApJ 04/11/2015. This version is appreciably different from the original submission: it includes an entirely new appendix, extended discussion, and much of the material has been reorganized
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摘要：

我们提出的综合Sunyaev-Zel'dovich效应（SZE）的信号，$Y_{\rm SZ}$，其X射线模拟，$Y_{\rm X}\equiv M_{\rm gas}T_{\rm X}$，和总质量，$M_{\rm tot}$之间的标度关系，为45个星系团的Bolocam X射线-SZ（BOXSZ）样品。所有参数都集成在$r_{2500}$中。$Y_{2500}$值是使用Bolocam收集的SZE数据测量的，Bolocam在加州理工学院亚毫米波天文台（CSO）以140 GHz工作。温度，$T_{\rm X}$，和质量，$M_{\rm gas,2500}$，的集群内的介质是使用X射线数据收集钱德拉，和$M_{\rm tot}$是来自$M_{\rm gas}$假设一个恒定的气体质量分数。我们的分析占了几个潜在的偏差来源，包括：选择效应，从无线电点源的污染，和SZE信号的损失，由于噪声滤波和光束平滑效应。我们测量的$Y_{2500}$ - $Y_{\rm X}$缩放有一个幂律指数为$0.84\pm0.07$，和一个分数的内在分散在$Y_{2500}$的$(21\pm7)\%$在固定的$Y_{\rm X}$，这两者都是与以前的分析一致。我们还测量了$Y_{2500}$和$M_{2500}$之间的缩放，发现$1.06\pm0.12$的幂律指数和在$(25\pm9)\%$的固定质量下$Y_{2500}$中的分数固有散射。虽然最近的SZE标度关系使用X射线质量代理发现幂律指数与自相似预测5/3一致，但我们的测量结果与自相似预测相差约5 $σ$。鉴于测量的$Y_{2500}$ - $Y_{\rm X}$标度之间的良好一致性，这种差异似乎是由每个特定分析所采用的X射线质量代理的校准差异引起的。

英文摘要：

We present scaling relations between the integrated Sunyaev-Zel'dovich Effect (SZE) signal, $Y_{\rm SZ}$, its X-ray analogue, $Y_{\rm X}\equiv M_{\rm gas}T_{\rm X}$, and total mass, $M_{\rm tot}$, for the 45 galaxy clusters in the Bolocam X-ray-SZ (BOXSZ) sample. All parameters are integrated within $r_{2500}$. $Y_{2500}$ values are measured using SZE data collected with Bolocam, operating at 140 GHz at the Caltech Submillimeter Observatory (CSO). The temperature, $T_{\rm X}$, and mass, $M_{\rm gas,2500}$, of the intracluster medium are determined using X-ray data collected with Chandra, and $M_{\rm tot}$ is derived from $M_{\rm gas}$ assuming a constant gas mass fraction. Our analysis accounts for several potential sources of bias, including: selection effects, contamination from radio point sources, and the loss of SZE signal due to noise filtering and beam-smoothing effects. We measure the $Y_{2500}$--$Y_{\rm X}$ scaling to have a power-law index of $0.84\pm0.07$, and a fractional intrinsic scatter in $Y_{2500}$ of $(21\pm7)\%$ at fixed $Y_{\rm X}$, both of which are consistent with previous analyses. We also measure the scaling between $Y_{2500}$ and $M_{2500}$, finding a power-law index of $1.06\pm0.12$ and a fractional intrinsic scatter in $Y_{2500}$ at fixed mass of $(25\pm9)\%$. While recent SZE scaling relations using X-ray mass proxies have found power-law indices consistent with the self-similar prediction of 5/3, our measurement stands apart by differing from the self-similar prediction by approximately 5$σ$. Given the good agreement between the measured $Y_{2500}$--$Y_{\rm X}$ scalings, much of this discrepancy appears to be caused by differences in the calibration of the X-ray mass proxies adopted for each particular analysis.

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