标题： z ~ 1 的大星系团 XMMU J1230.3+1339：颜色-星等关系，Butcher-Oemler 效应，X 射线和弱引力透镜质量估计 显示英文标题

标题： The Massive Galaxy Cluster XMMU J1230.3+1339 at z ~ 1: Colour-magnitude relation, Butcher-Oemler effect, X-ray and weak lensing mass estimates

摘要： 我们展示了对红移 z ~ 1 的 XMMU J1230.3+1339 的多波长研究结果。我们分析了大型双筒望远镜的深度多波段广域图像、来自甚大望远镜的多目标光谱观测，以及来自 GALEX 和钱德拉 X 射线天文台的空间观测数据。我们应用了一种贝叶斯光度红移代码，使用 FUV、NUV 和深度 U、B、V、r、i、z 数据推导出红移。当使用所有（可靠）光谱数据时，我们达到了$\triangle z/(1+z)$= 0.07（0.04）的精度，灾难性异常值的比例为$\eta$= 13（0）%。光度红移成员的 i - z 对比 z 色-星等关系显示出一个紧密的红色序列，零点为 0.935 星等，斜率为 -0.027。我们观察到在红色团星系序列的暗端存在截断以及 Butcher-Oemler 效应，发现蓝色星系的比例为$f_b \approx$0.5。进一步地，我们对深度 26'$\times$26' r 波段 LBC 图像进行了弱引力透镜分析。观测到的剪切用单等温球模型和 Navarro-Frenk-White 模型进行拟合，分别获得速度弥散和模型参数。 我们最佳拟合值为，速度弥散$\sigma_{SIS}$= 1308$\pm$284，浓度参数 c = 4.0$^{+14}_{-2}$和尺度半径 r$_{s}$= 345$^{+50}_{-57}$kpc。 结合我们的动力学、X射线和弱引力透镜分析的质量估计，我们得到一个总星系团质量为$M^{tot}_{200}$ = (4.56 $\pm$ 2.3) $\times$ 10$^{14}$ M$_{\sun}$。 这项研究证明了在z ~ 1范围内基于地面的星系团弱引力透镜测量的可行性。 显示英文摘要

摘要： We present results from the multi-wavelength study of XMMU J1230.3+1339 at z ~ 1. We analyze deep multi-band wide-field images from the Large Binocular Telescope, multi-object spectroscopy observations from VLT, as well as space-based serendipitous observations, from the GALEX and Chandra X-ray observatories. We apply a Bayesian photometric redshift code to derive the redshifts using the FUV, NUV and the deep U, B, V, r, i, z data. We achieve an accuracy of $\triangle z/(1+z)$ = 0.07 (0.04) and the fraction of catastrophic outliers is $\eta$ = 13 (0)%, when using all (secure) spectroscopic data, respectively. The i - z against z colour-magnitude relation of the photo-z members shows a tight red-sequence with a zero point of 0.935 mag, and slope equal to -0.027. We observe evidence for a truncation at the faint end of the red-cluster-sequence and the Butcher-Oemler effect, finding a fraction of blue galaxies $f_b \approx$ 0.5. Further we conduct a weak lensing analysis of the deep 26' $\times$ 26' r-band LBC image. The observed shear is fitted with a Single-Isothermal-Sphere and a Navarro-Frenk-White model to obtain the velocity dispersion and the model parameters, respectively. Our best fit values are, for the velocity dispersion $\sigma_{SIS}$ = 1308 $\pm$ 284, concentration parameter c = 4.0$^{+14}_{-2}$ and scale radius r$_{s}$ = 345$^{+50}_{-57}$ kpc. Combining our mass estimates from the kinematic, X-ray and weak lensing analyses we obtain a total cluster mass of $M^{tot}_{200}$ = (4.56 $\pm$ 2.3) $\times$ 10$^{14}$ M$_{\sun}$. This study demonstrates the feasibility of ground based weak lensing measurements of galaxy clusters up to z ~ 1.