2014/06/30 by Tiago Costa, Debora Sijacki, Martin G. Haehnelt
Physics and Astronomy · #Astrophysics and Star Formation Studies #Cosmology and Gravitation Theories #Galaxies: Formation, Evolution, Phenomena #astro-ph.CO #astro-ph.GA
paper · pdf · doi:10.1093/mnras/stu1632
25 pages, 17 figures, 1 table, MNRAS (accepted in August 2014 after minor revisions)
openalex publication_date 2014/09/10 · arxiv created 2015/02/12 · arxiv updated 2015/06/19 · openalex created_date 2025/10/10 · openalex updated_date 2026/07/28
We employ hydrodynamical simulations using the moving-mesh code arepo to investigate the role of energy and momentum input from active galactic nuclei (AGN) in driving large-scale galactic outflows. We start by reproducing analytic solutions for both energy- and momentum-driven outflowing shells in simulations of a spherical isolated dark matter potential with gas in hydrostatic equilibrium and with no radiative cooling. We confirm that for this simplified setup, galactic outflows driven by a momentum input rate of order LEdd/c can establish an MBH–σ relation with slope and normalization similar to that observed. We show that momentum input at a rate of LEdd/c is however insufficient to drive efficient outflows once cooling and gas inflows as predicted by cosmological simulations at resolved scales are taken into account. We argue that observed large-scale AGN-driven outflows are instead likely to be energy-driven and show that such outflows can reach momentum fluxes exceeding 10LEdd/c within the innermost 10 kpc of the galaxy. The outflows are highly anisotropic, with outflow rates and a velocity structure found to be inadequately described by spherical outflow models. We verify that the hot energy-driven outflowing gas is expected to be strongly affected by metal-line cooling, leading to significant amounts ( ≳ 109 M⊙) of entrained cold gas.