AGN-driven quenching of satellite galaxies. (arXiv:1906.07431v1 [astro-ph.GA])
<a href="http://arxiv.org/find/astro-ph/1/au:+Dashyan_G/0/1/0/all/0/1">Gohar Dashyan</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Choi_E/0/1/0/all/0/1">Ena Choi</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Somerville_R/0/1/0/all/0/1">Rachel S. Somerville</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Naab_T/0/1/0/all/0/1">Thorsten Naab</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Quirk_A/0/1/0/all/0/1">Amanda C. N. Quirk</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Hirschmann_M/0/1/0/all/0/1">Michaela Hirschmann</a>, <a href="http://arxiv.org/find/astro-ph/1/au:+Ostriker_J/0/1/0/all/0/1">Jeremiah P. Ostriker</a>
We explore the effect of active galactic nucleus (AGN) feedback from central
galaxies on their satellites by comparing two sets of cosmological zoom-in runs
of 27 halos with masses ranging from $10^{12}$ to $10^{13.4}$ solar masses at
z=0, with (wAGN) and without (noAGN) AGN feedback. Both simulations include
stellar feedback from multiple processes, including powerful winds from
supernovae, stellar winds from young massive stars, AGB stars, radiative
heating within Str”omgren spheres and photoelectric heating. Our wAGN model is
identical to the noAGN model except that it also includes a model for black
hole seeding and accretion, as well as AGN feedback via high-velocity broad
absorption line winds and Compton/photoionization heating. We show that the
inclusion of AGN feedback from the central galaxy significantly affects the
star formation history and the gas content of the satellite galaxies. AGN
feedback starts to affect the gas content and the star formation of the
satellites as early as z=2. The mean gas rich fraction of satellites at z=0
decreases from 15% in the noAGN simulation to 5% in the wAGN simulation. The
difference between the two sets extends as far out as five times the virial
radius of the central galaxy at z=1. We investigate the quenching mechanism by
studying the physical conditions in the surroundings of pairs of satellites
matched across the wAGN and noAGN simulations and find an increase in the
temperature and relative velocity of the intergalactic gas.
We explore the effect of active galactic nucleus (AGN) feedback from central
galaxies on their satellites by comparing two sets of cosmological zoom-in runs
of 27 halos with masses ranging from $10^{12}$ to $10^{13.4}$ solar masses at
z=0, with (wAGN) and without (noAGN) AGN feedback. Both simulations include
stellar feedback from multiple processes, including powerful winds from
supernovae, stellar winds from young massive stars, AGB stars, radiative
heating within Str”omgren spheres and photoelectric heating. Our wAGN model is
identical to the noAGN model except that it also includes a model for black
hole seeding and accretion, as well as AGN feedback via high-velocity broad
absorption line winds and Compton/photoionization heating. We show that the
inclusion of AGN feedback from the central galaxy significantly affects the
star formation history and the gas content of the satellite galaxies. AGN
feedback starts to affect the gas content and the star formation of the
satellites as early as z=2. The mean gas rich fraction of satellites at z=0
decreases from 15% in the noAGN simulation to 5% in the wAGN simulation. The
difference between the two sets extends as far out as five times the virial
radius of the central galaxy at z=1. We investigate the quenching mechanism by
studying the physical conditions in the surroundings of pairs of satellites
matched across the wAGN and noAGN simulations and find an increase in the
temperature and relative velocity of the intergalactic gas.
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