Dr. Jennifer Piscionere
Dark matter outnumbers baryons by more than a factor of five. Our current theories of galaxy clustering assume that the density distribution of dark matter drives the distribution of galaxies in the universe. However, what if there are scales at which galaxy clustering is determined not by just the dark matter, but by some intrinsic property of the galaxy-such as luminosity, or the observed epoch? The answer to these questions can be found by studying galaxy clustering within an individual dark matter halo. Measuring and modeling galaxy clustering on these scales less than about 200 kpc requires careful analysis of large data sets, in particular the Sloan Digital Sky Survey (SDSS) (York et al., 2000). It also requires comparing this data set to a large suite of cosmological N-body simulations of different volumes using a sophisticated massively parallel MCMC fitting engine powered by Kraken petascale computing cluster, part of the XSEDE network.
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