| Description |
The clustering of galaxies, or the dark matter halos they reside in, is a key tool in building an understanding of how the large scale structure in the late Universe came to be. Although broad properties of the 2- and higher-point correlation functions of galaxies have been well understood for a long time, finer questions such as how this clustering behaves as a function of length scale, or how well it can be described using simple linear and deterministic models, are still open. And in the era of precision cosmology, these questions are important even if the effects they address are small. The current state-of-the-art in answering these relies on using large, high resolution N-body simulations for calibration. I will discuss some recent analytical progress which gives insights into the origin of these effects, and the results of some first tests of these analytical ideas.
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