Optimizing high-redshift galaxy surveys for environmental information
Optimizing high-redshift galaxy surveys for environmental information
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DOI：
10.1093/mnras/stab1061
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发表时间：
2021-04
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影响因子：
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通讯作者：
T. Looser;S. Lilly;Larry P. T. Sin;B. Henriques;R. Maiolino;M. Cirasuolo
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文献类型：
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作者：
T. Looser;S. Lilly;Larry P. T. Sin;B. Henriques;R. Maiolino;M. Cirasuolo
我们调查组发现的算法，重建星系群的位置信息的示踪星系，观察到的红移调查进行了多路复用摄谱仪的性能。我们使用模拟光锥产生的L-Galerkin星系演化的半解析模型，其中的基本现实是已知的。我们特别关注在高红移的性能，以及这是如何影响的示踪星系的质量的选择（很大程度上相当于他们共同移动的数密度）和（假设随机）这些示踪剂的采样率。然而，我们首先比较了两种不同的方法，适用于低红移的群体发现，并得出结论，这些是广泛可比的。为了简单起见，我们只采用其中之一，“朋友圈”（FoF）作为我们在高红移研究的基础。我们介绍了12个科学指标，旨在量化的性能组查找相关的广泛的科学调查与组目录。这些指标检查恢复组目录的质量，不同丰富度结构的中间晕质量，暗物质晕质量的分散以及组查找器分类单元素，中心和卫星的成功程度。我们分析了这些指标如何随示踪星系的有限恒星质量和随机采样率而变化，从而可以量化不同调查设计之间的各种权衡。最后，我们看看这些相同的设计参数的影响，在观测时间的调查使用作为一个例子，潜在的MOONRISE调查使用的MOONS仪器的相对“成本”。
We investigate the performance of group finding algorithms that reconstruct galaxy groups from the positional information of tracer galaxies that are observed in redshift surveys carried out with multiplexed spectrographs. We use mock light-cones produced by the L-Galaxies semi-analytic model of galaxy evolution in which the underlying reality is known. We particularly focus on the performance at high redshift, and how this is affected by choices of the mass of the tracer galaxies (largely equivalent to their co-moving number density) and the (assumed random) sampling rate of these tracers. We first however compare two different approaches to group finding as applied at low redshift, and conclude that these are broadly comparable. For simplicity we adopt just one of these, "Friends-of-Friends" (FoF) as the basis for our study at high redshift. We introduce 12 science metrics that are designed to quantify the performance of the group-finder as relevant for a wide range of science investigations with a group catalogue. These metrics examine the quality of the recovered group catalogue, the median halo masses of different richness structures, the scatter in dark matter halo mass and how successful the group-finder classifies singletons, centrals and satellites. We analyze how these metrics vary with the limiting stellar mass and random sampling rate of the tracer galaxies, allowing quantification of the various trade-offs between different possible survey designs. Finally, we look at the impact of these same design parameters on the relative "costs" in observation time of the survey using as an example the potential MOONRISE survey using the MOONS instrument.