Most, if not all, galaxies contain a supermassive black hole at their center. The accretion of gas onto black holes can drive outflows, jets, and winds that can transform the gas content of galaxies and suppress future star formation. Galaxy formation models rely on this energetic ‘feedback’ from black holes to reproduce key observations of the real universe. However, the exact form of this feedback remains uncertain and recent models vary widely in how they simulate the effect of black holes on galaxies. In this talk, I will describe my journey towards determining the physics of black hole feedback by synthesizing results from observations and simulations. First, I will show how simulated and observed galaxy population demographics reflect how black holes operate to suppress galaxy-wide star formation. Alongside this large-scale statistical approach, further constraining black hole feedback physics will require testing how well models can replicate observed outflows in individual galaxies. To do this, I will share ‘mock’ observations that model the emission of light from simulated galaxies undergoing black hole feedback. By providing a theoretical link between observational data and the physics implemented in simulations, a clearer understanding of how black holes affect galaxy evolution can emerge.
Topic: UIUC Astronomy Colloquium
Time: This is a recurring meeting Meet anytime
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