六个红移1星系团样本的AMI SZ观测和贝叶斯分析
AMI SZ observations and Bayesian analysis of a sample of six redshift-one clusters of galaxies
摘要：
我们使用Arcminute Microkelvin Imager（AMI）和随后的贝叶斯分析，从Culverhouse等人（2010）的X射线和红外选择样本中选择了6个红移星系团（$z \approx 1$），提供16 GHz Sunyaev-Zel'dovich观测。在随后的分析中，我们使用两个集群模型，等温β模型和暗物质GNFW（DM-GNFW）模型，以获得正式的检测概率和集群参数。我们检测到两个集群（CLJ 1415 +3612和XMJ 0830 +5241），并测量它们的总质量，半径为200 $\times$的临界密度在各自的集群的红移。对于CLJ 1415 +3612和XMJ 0830 +5241，我们找到了每个模型的M_{ \mathrm{T}，200}，它们对于每个簇都是一致的。我们还提出了整个样本的源减法之前和之后的地图，并提供1D和2D后验边缘化的概率分布为每个拟合的聚类轮廓参数的检测到的集群。使用考虑到AMI大阵列（LA）测量的源环境，源混淆噪声，CMB原盘，仪器噪声的模拟，我们从Culverhouse等人（2010）的低半径X射线数据中估计样本中每个簇的可探测性，并将其与小阵列（SA）数据的结果进行比较。此外，我们讨论了等温性和恒定气体质量分数的假设的有效性。我们评论的偏见，这些小半径的估计介绍大半径SZ预测。此外，我们还对这两次检测进行了深入的单点LA观察。我们发现，在高分辨率下，CLJ 1415 +3612的3 sigma暂定递减率和XMJ 0830 +5241的5 sigma高分辨率递减率。
英文摘要：
We present 16-GHz Sunyaev-Zel'dovich observations using the Arcminute Microkelvin Imager (AMI) and subsequent Bayesian analysis of six galaxy clusters at redshift ($z \approx 1$) chosen from an X-ray and Infrared selected sample from Culverhouse et al. (2010). In the subsequent analysis we use two cluster models, an isothermal β-model and a Dark Matter GNFW (DM-GNFW) model in order to derive a formal detection probability and the cluster parameters. We detect two clusters (CLJ1415+3612 & XMJ0830+5241) and measure their total masses out to a radius of 200 $\times$ the critical density at the respective cluster's redshift. For CLJ1415+3612 and XMJ0830+5241, we find M_{\mathrm{T},200} for each model, which agree with each other for each cluster. We also present maps before and after source subtraction of the entire sample and provide 1D and 2D posterior marginalised probability distributions for each fitted cluster profile parameter of the detected clusters. Using simulations which take into account the measured source environment from the AMI Large Array (LA), source confusion noise, CMB primordials, instrument noise, we estimate from low-radius X-ray data from Culverhouse et al. (2010), the detectability of each cluster in the sample and compare it with the result from the Small Array (SA) data. Furthermore, we discuss the validity of the assumptions of isothermality and constant gas mass fraction. We comment on the bias that these small-radius estimates introduce to large-radius SZ predictions. In addition, we follow-up the two detections with deep, single-pointed LA observations. We find a 3 sigma tentative decrement toward CLJ1415+3612 at high-resolution and a 5 sigma high-resolution decrement towards XMJ0830+5241.
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