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Simulating galaxy formation with black hole driven thermal and kinetic feedback
Name
1607.03486.pdf
Description
Accepted version
Size
2.21 MB
Format
Adobe PDF
Checksum (MD5)
15663a55e1d0ef6864e65ef1f472ccd5
Author(s)
Weinberger, Rainer
Springel, Volker
Hernquist, Lars
Pillepich, Annalisa
Marinacci, Federico
Pakmor, Rüdiger
Nelson, Dylan
Genel, Shy
Vogelsberger, Mark
Naiman, Jill
Journal
Monthly Notices of the Royal Astronomical Society
Publisher
Oxford University Press (OUP)
Citation
Weinberger, Rainer, et al. "Simulating Galaxy Formation with Black Hole Driven Thermal and Kinetic Feedback." Monthly Notices of the Royal Astronomical Society 465 3 (2017): 3291-308.
Version
Final published version
Abstract
© 2016 The Authors. The inefficiency of star formation in massive elliptical galaxies is widely believed to be caused by the interactions of an active galactic nucleus (AGN) with the surrounding gas. Achieving a sufficiently rapid reddening of moderately massive galaxies without expelling too many baryons has however proven difficult for hydrodynamical simulations of galaxy formation, prompting us to explore a new model for the accretion and feedback effects of supermassive black holes. For high-accretion rates relative to the Eddington limit, we assume that a fraction of the accreted rest mass energy heats the surrounding gas thermally, similar to the 'quasar mode' in previouswork. For low-accretion rates, we invoke a new, pure kinetic feedback model that imparts momentum to the surrounding gas in a stochastic manner. These two modes of feedback are motivated both by theoretical conjectures for the existence of different types of accretion flows as well as recent observational evidence for the importance of kinetic AGN winds in quenching galaxies.We find that a large fraction of the injected kinetic energy in this mode thermalizes via shocks in the surrounding gas, thereby providing a distributed heating channel. In cosmological simulations, the resulting model produces red, non-star-forming massive elliptical galaxies, and achieves realistic gas fractions, black hole growth histories and thermodynamic profiles in large haloes.
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DOI of Published Version
10.1093/MNRAS/STW2944
