Which AGN jets quench star formation in massive galaxies?

Author:

Su Kung-Yi123,Hopkins Philip F3ORCID,Bryan Greg L1ORCID,Somerville Rachel S2,Hayward Christopher C2ORCID,Anglés-Alcázar Daniel24,Faucher-Giguère Claude-André5ORCID,Wellons Sarah5ORCID,Stern Jonathan56ORCID,Terrazas Bryan A7ORCID,Chan T K89ORCID,Orr Matthew E310ORCID,Hummels Cameron3,Feldmann Robert11ORCID,Kereš Dušan9

Affiliation:

1. Department of Astronomy, Columbia University, 550 West 120th Street, New York, NY 10027, USA

2. Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USA

3. TAPIR 350-17, California Institute of Technology, 1200 E. California Boulevard, Pasadena, CA 91125, USA

4. Department of Physics, University of Connecticut, 196 Auditorium Road, U-3046, Storrs, CT 06269-3046, USA

5. Department of Physics & Astronomy and CIERA, Northwestern University, 1800 Sherman Ave, Evanston, IL 60201, USA

6. School of Physics & Astronomy, Tel Aviv University, Tel Aviv 69978, Israel

7. Harvard-Smithsonian Center for Astrophysics, Cambridge, MA 02138, USA

8. Institute for Computational Cosmology, Durham University, South Road, Durham DH1 3LE, UK

9. Department of Physics and Center for Astrophysics and Space Science, University of California at San Diego, 9500 Gilman Drive, La Jolla, CA 92093, USA

10. Department of Physics and Astronomy, Rutgers, The State University of New Jersey, 136 Frelinghuysen Rd, Piscataway, NJ 08854, USA

11. Institute for Computational Science, University of Zurich, Winterthurerstrasse 190, CH-8057 Zurich, Switzerland

Abstract

ABSTRACT 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 $10^{14}\, {\rm M}_{\odot }$ halo using high-resolution non-cosmological magnetohydrodynamic simulations with the FIRE-2 (Feedback In Realistic Environments) stellar feedback model, conduction, and viscosity. We explore which 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 (∼MeV or ∼1010K) thermal plasma jets work but require ∼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 ≳ 1044 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.

Funder

Simons Foundation

NSF

NASA

RSS

CCH

Research Corporation for Science Advancement

Swiss National Science Foundation

Science and Technology Facilities Council

Caltech

Publisher

Oxford University Press (OUP)

Subject

Space and Planetary Science,Astronomy and Astrophysics

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