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Todays Colloquium: Understanding and observing simulated universes.

Submitter: Marcel Haas (STScI)
Description: Understanding the physics that drives the evolution of galaxies is often approached from either the observational side, or using numerical simulations. Comparison of the two constrains physical ingredients like star formation efficiencies and feedback by supernovae and AGN.

I will present a large suite of numerical cosmological simulations of the OverWhelmingly Large Simulations project and will discuss how self-regulation of the star formation by accretion, cooling and feedback sets most of the basic physical parameters of the simulated galaxies.

I will compare to observed properties of the galaxy population and then move that comparison into the observational domain by creating mock images from the simulations. I will show that basic observable properties of the mock galaxies are very well recovered using standard techniques used on Hubble data like the HUDF or CANDELS.

I will also present a method to reliably classify observed galaxies as centrals in their dark matter halos or satellites, based on simple imaging data only. This method works very well out to high redshift and also allows one to estimate the dark matter halo mass of the observed galaxies.
Copyright: M. Haas
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