Structure formation theory provides very effective predictions of the properties of dark matter halos, including their mass function, clustering, and internal structure. Observations of structure, however, rely on luminous galaxies as tracers. A detailed understanding of the way galaxies occupy dark matter halos is essential for connecting structure formation theory to observation. We describe some of the observables available for contraining the halo occupancy, illustrating each using data from the Sloan Digital Sky Survey. Many of these observables can now be measured with great statistical precision. Comparison of these observables to theory is now limited by systematic uncertainty in the relationship between observable quantities (like velocity dispersion vs. cluster richness) and theoretically favored quantities (like M_(200)). We argue for the use of carefully crafted simulations in making this connection, and illustrate their use in some example analyses.
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机译：结构形成理论对暗物质晕的性质，包括其质量函数，聚类和内部结构，提供了非常有效的预测。但是，对结构的观察依赖于发光星系作为示踪剂。对星系占据暗物质光环的方式的详细了解对于将结构形成理论与观测联系起来至关重要。我们描述了一些可用于限制光环占用的可观测数据，并举例说明了使用Sloan Digital Sky Survey的数据。现在，这些可观测值中的许多都可以以很高的统计精度进行测量。这些可观察物与理论的比较现在受到可观察量（例如速度分散与簇富度）与理论上有利量（例如M_（200））之间系统不确定性的限制。我们主张在建立这种连接时使用精心设计的仿真，并在一些示例分析中说明它们的使用。
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