X射线群中的Galerkin Ⅰ：鲁棒的成员分配和群环境对猝灭的影响
Galaxies in X-ray Groups I: Robust Membership Assignment and the Impact of Group Environments on Quenching
摘要：
了解机制，导致密集的环境，以主机星系更红的颜色，更多的球状形态，和较低的恒星形成率比场人口仍然是一个重要的问题。由于大多数候选过程最终取决于主机晕质量，准确的本地环境的特性，理想地绑定到晕质量估计和跨越范围的晕质量和红移是必要的。在这项工作中，我们提出并测试了一个严格的，probabalistic的方法分配星系组的基础上精确的光度红移和X射线选定的组从宇宙领域。这些星系群的质量范围是10^13 < M_200c/M_sun < 10^14，红移范围是0<z<1。我们通过对光谱子样本的测试，包括在VLT获得的新数据，并通过将我们的方法应用于详细的模拟目录，来表征我们的选择算法。我们发现，我们的集团成员星系样品的纯度为84%，完整性为92%，在0.5 R200 c。我们测量的影响，在红移和组中心的成员选择的质量与模拟的基础上，目前的数据，以及未来的成像和光谱调查的不确定性。作为我们的新的集团成员目录，这将是公开的第一个应用程序，我们表明，成员星系表现出更高的淬火分数相比，在固定的恒星质量到z~1的领域，表明在集团尺度的恒星形成和环境之间的显着关系。我们还解决的建议，尘埃恒星形成星系在这样的群体可能会影响高-l功率谱的宇宙微波背景，并发现这样的人口不能解释低功率在最近的SZ测量。
英文摘要：
Understanding the mechanisms that lead dense environments to host galaxies with redder colors, more spheroidal morphologies, and lower star formation rates than field populations remains an important problem. As most candidate processes ultimately depend on host halo mass, accurate characterizations of the local environment, ideally tied to halo mass estimates and spanning a range in halo mass and redshift are needed. In this work, we present and test a rigorous, probabalistic method for assigning galaxies to groups based on precise photometric redshifts and X-ray selected groups drawn from the COSMOS field. The groups have masses in the range 10^13 < M_200c/M_sun < 10^14 and span redshifts 0<z<1. We characterize our selection algorithm via tests on spectroscopic subsamples, including new data obtained at the VLT, and by applying our method to detailed mock catalogs. We find that our group member galaxy sample has a purity of 84% and completeness of 92% within 0.5 R200c. We measure the impact of uncertainties in redshifts and group centering on the quality of the member selection with simulations based on current data as well as future imaging and spectroscopic surveys. As a first application of our new group member catalog which will be made publicly available, we show that member galaxies exhibit a higher quenched fraction compared to the field at fixed stellar mass out to z~1, indicating a significant relationship between star formation and environment at group scales. We also address the suggestion that dusty star forming galaxies in such groups may impact the high-l power spectrum of the cosmic microwave background and find that such a population cannot explain the low power seen in recent SZ measurements.
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