March 13 - 18, 2016
Clustering of large-scale structure is a sensitive probe of cosmology,
which independently tests both the cosmic expansion history and the structure growth rate. On comoving scales larger than tens of Mpc, linear theory accurately describes the growth of cosmic structure. Large spectroscopic, imaging, and CMB surveys will cover volumes sufficient to probe this growth and constrain cosmological models. However, a complete understanding of observational systematics is required to map observed clustering into fundamental cosmological parameters. On scales of several Mpc, the development of non-linear perturbation theory and halo occupation models for clustering have begun to provide insight to how dark matter halos assemble and to test models of modified gravity and the neutrino mass. On yet smaller scales, the non-linear growth of dark matter fluctuations couples with baryonic physics to cloud our understanding of galaxy properties, galaxies in clusters, and the formation of quasars, thus requiring sophisticated numerical simulations to interpret observations.
This conference will provide the opportunity for researchers in observation, theory, and numerical simulation to discuss the implications of clustering across all scales. The conference will provide a venue to compare the results of the latest simulations to analytic models and to the observed clustering of matter. Finally, the conference will provide direction for future efforts in the field of galaxy evolution and cosmology from the clustering of large-scale structure.
We therefore invite you to join us March 13-18, 2016, at the SnowPAC conference. The conference will be held at Snowbird Ski Resort in the spectacular Little Cottonwood Canyon outside of Salt Lake City, Utah. Over the course of the week, conference attendees will engage in discussion that draws the connection between galaxy evolution on the smallest scales and implications for constraints on cosmology on the largest scales.
• Imaging and spectroscopic surveys
• Environmental effect on galaxy evolution
• Galaxy populations in galaxy clusters
• Stellar and gas content in galaxy clusters
• Halo and abundance matching models
• Assembly bias
• Clustering at small scales
• Gas accretion, star formation, and stellar feedback in numerical simulations
• Hydrodynamical simulation of cosmological volumes
• Perturbation theory and structure formation
• Tests of primordial non-gaussianity and modifications of gravity