This research will examine the role of dark halo merging and interaction in the process of galaxy formation, and will use observational indicators to probe the underlying cosmology. A primary goal is to decipher the underlying dark halo merger and interaction rates, which theoretically guide galaxy interactions and mass growth. The project will carry out high resolution numerical simulations and use the results to refine and test Extended Press-Schechter merger estimates, and will develop models of sub-halo evolution within host halos for direct comparison with observations. Merger rates will be calculated using an Adaptive Refinement Tree method, and existing semi-analytic sub-halo models and simulation techniques will be improved to predict observable indicators of these rates. Modeling the observational consequences of low-mass satellite accretion onto bright galaxies will test the cold dark matter cosmogony precisely where it currently has the most difficulty matching observations.
The research includes working with students and faculty from under-represented groups, and collaboration with a university that does not grant PhDs in astronomy. All results will be publicly available in an easy-to-use format. The research scientist will also be teaching in a program designed to motivate and educate high-school students interested in science and mathematics.
