4.7 Article

Which AGN jets quench star formation in massive galaxies?

Journal

MONTHLY NOTICES OF THE ROYAL ASTRONOMICAL SOCIETY
Volume 507, Issue 1, Pages 175-204

Publisher

OXFORD UNIV PRESS
DOI: 10.1093/mnras/stab2021

Keywords

turbulence; methods: numerical; cosmic rays; galaxies: clusters: intracluster medium; galaxies: jets; galaxies: magnetic fields

Funding

  1. Simons Foundation
  2. Alfred P. Sloan Research Fellowship
  3. NSF [1715847, 1455342, AST-1615955, OAC-1835509, AST-2006176, AST-2009687, AST-1715216, AST-1652522, AST-1715101]
  4. NASA [NNX15AT06G, JPL 1589742, 17-ATP17-0214, 17-ATP17-0067, HEC SMD-16-7592]
  5. Scialog Award from the Research Corporation for Science Advancement
  6. Swiss National Science Foundation [194814]
  7. Cottrell Scholar Award from the Research Corporation for Science Advancement
  8. Science and Technology Facilities Council (STFC) astronomy consolidated grant [ST/T000244/1]
  9. Center for Computational Astrophysics at the Flatiron Institute - Simons Foundation

Ask authors/readers for more resources

Research shows that CR-dominated jets are most efficient in quenching galaxies in the halo gas of massive galaxies. Jets with higher specific energy can quench galaxies more effectively, while kinetic jets are less efficient in this process.
Without additional heating, radiative cooling of the halo gas of massive galaxies (Milky Way-mass and above) produces cold gas or stars exceeding that observed. Heating from active galactic nucleus (AGN) jets is likely required, but the jet properties remain unclear. This is particularly challenging for galaxy simulations, where the resolution is orders-of-magnitude insufficient to resolve jet formation and evolution. On such scales, the uncertain parameters include the jet energy form [kinetic, thermal, cosmic ray (CR)]; energy, momentum, and mass flux; magnetic fields; opening angle; precession; and duty cycle. We investigate these parameters in a 10(14)M(circle dot) halo using high-resolution non-cosmological magnetohydrodynamic simulations with the FIRE-2 (Feedback In Realistic Environments) stellar feedback model, conduction, and viscosity. We explorewhich scenarios qualitatively meet observational constraints on the halo gas and show that CR-dominated jets most efficiently quench the galaxy by providing CR pressure support and modifying the thermal instability. Mildly relativistic (similar to MeV or similar to 10(10) K) thermal plasma jets work but require similar to 10 times larger energy input. For fixed energy flux, jets with higher specific energy (longer cooling times) quench more effectively. For this halo mass, kinetic jets are inefficient at quenching unless they have wide opening or precession angles. Magnetic fields also matter less except when the magnetic energy flux reaches greater than or similar to 10(44) erg s(-1) in a kinetic jet model, which significantly widens the jet cocoon. The criteria for a successful jet model are an optimal energy flux and a sufficiently wide jet cocoon with a long enough cooling time at the cooling radius.

Authors

I am an author on this paper
Click your name to claim this paper and add it to your profile.

Reviews

Primary Rating

4.7
Not enough ratings

Secondary Ratings

Novelty
-
Significance
-
Scientific rigor
-
Rate this paper

Recommended

No Data Available
No Data Available