Volume 592, August 2016
|Number of page(s)||12|
|Section||Numerical methods and codes|
|Published online||25 July 2016|
Comparison of black hole growth in galaxy mergers with gasoline and ramses
1 CEA-Saclay, IRFU, SAp, 91191 Gif-sur-Yvette, France
2 Institut d’Astrophysique de Paris, UMR 7095 CNRS, Université Pierre et Marie Curie, 98bis Bd Arago, 75014 Paris, France
3 Center for Theoretical Astrophysics and Cosmology, Institute for Computational Science, University of Zurich, Winterthurerstrasse 190, 8057 Zurich, Switzerland
4 Department of Astrophysics, American Museum of Natural History, Central Park West at 79th Street, New York, NY 10024, USA
5 Astronomy Department, University of Washington, Box 351580, Seattle, WA 98195-1580, USA
Accepted: 22 April 2016
Supermassive black hole dynamics during galaxy mergers is crucial in determining the rate of black hole mergers and cosmic black hole growth. As simulations achieve higher resolution, it becomes important to assess whether the black hole dynamics is influenced by the treatment of the interstellar medium in different simulation codes. We compare simulations of black hole growth in galaxy mergers with two codes: the smoothed particle hydrodynamics code gasoline, and the adaptive mesh refinement code ramses. We seek to identify predictions of these models that are robust despite differences in hydrodynamic methods and implementations of subgrid physics. We find that the general behavior is consistent between codes. Black hole accretion is minimal while the galaxies are well-separated (and even as they fly by within 10 kpc at the first pericenter). At late stages, when the galaxies pass within a few kpc, tidal torques drive nuclear gas inflow that triggers bursts of black hole accretion accompanied by star formation. We also note quantitative discrepancies that are model dependent: our ramses simulations show less star formation and black hole growth, and a smoother gas distribution with larger clumps and filaments than our gasoline simulations. We attribute these differences primarily to the subgrid models for black hole fueling, feedback, and gas thermodynamics. The main conclusion is that differences exist quantitatively between codes, and this should be kept in mind when making comparisons with observations. However, both codes capture the same dynamical behaviors in terms of triggering black hole accretion, star formation, and black hole dynamics, which is reassuring.
Key words: galaxies: active / galaxies: evolution / galaxies: formation / galaxies: interactions / galaxies: star formation
© ESO 2016
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