The failure of stellar feedback, magnetic fields, conduction, and morphological quenching in maintaining red galaxies

Kung Yi Su*, Philip F. Hopkins, Christopher C. Hayward, Xiangcheng Ma, Claude André Faucher-Giguère, Dusan Keres, Matthew E. Orr, T. K. Chan, Victor H. Robles

*Corresponding author for this work

Research output: Contribution to journalArticle

1 Citation (Scopus)

Abstract

The quenching 'maintenance' and related 'cooling flow' problems are important in galaxies from Milky Way mass through clusters. We investigate this in haloes with masses ∼1012-1014M0, using non-cosmological high-resolution hydrodynamic simulations with the FIRE-2 (Feedback In Realistic Environments) stellar feedback model. We specifically focus on physics present without AGN, and show that various proposed 'non-AGN' solution mechanisms in the literature, including Type Ia supernovae, shocked AGB winds, other forms of stellar feedback (e.g. cosmic rays), magnetic fields, Spitzer-Braginskii conduction, or 'morphological quenching' do not halt or substantially reduce cooling flows nor maintain 'quenched' galaxies in this mass range. We show that stellar feedback (including cosmic rays from SNe) alters the balance of cold/warm gas and the rate at which the cooled gas within the galaxy turns into stars, but not the net baryonic inflow. If anything, outflowing metals and dense gas promote additional cooling. Conduction is important only in the most massive haloes, as expected, but even at ∼1014M0 reduces inflow only by a factor ∼2 (owing to saturation effects and anisotropic suppression). Changing the morphology of the galaxies only slightly alters their Toomre-Q parameter, and has no effect on cooling (as expected), so has essentially no effect on cooling flows or maintaining quenching. This all supports the idea that additional physics, e.g. AGN feedback, must be important in massive galaxies.

Original languageEnglish (US)
Pages (from-to)4393-4408
Number of pages16
JournalMonthly Notices of the Royal Astronomical Society
Volume487
Issue number3
DOIs
StatePublished - Jan 1 2019

Fingerprint

quenching
galaxies
magnetic field
cooling
conduction
magnetic fields
cosmic ray
cosmic rays
halos
inflow
physics
FIRE (climatology)
gases
gas
maintenance
supernovae
hydrodynamics
retarding
saturation
stars

Keywords

  • Clusters
  • Clusters
  • Evolution-galaxies
  • Galaxies
  • Intracluster medium-X-rays
  • MHD-methods
  • Numerical - cosmic rays-Galaxy

ASJC Scopus subject areas

  • Astronomy and Astrophysics
  • Space and Planetary Science

Cite this

Su, Kung Yi ; Hopkins, Philip F. ; Hayward, Christopher C. ; Ma, Xiangcheng ; Faucher-Giguère, Claude André ; Keres, Dusan ; Orr, Matthew E. ; Chan, T. K. ; Robles, Victor H. / The failure of stellar feedback, magnetic fields, conduction, and morphological quenching in maintaining red galaxies. In: Monthly Notices of the Royal Astronomical Society. 2019 ; Vol. 487, No. 3. pp. 4393-4408.
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The failure of stellar feedback, magnetic fields, conduction, and morphological quenching in maintaining red galaxies. / Su, Kung Yi; Hopkins, Philip F.; Hayward, Christopher C.; Ma, Xiangcheng; Faucher-Giguère, Claude André; Keres, Dusan; Orr, Matthew E.; Chan, T. K.; Robles, Victor H.

In: Monthly Notices of the Royal Astronomical Society, Vol. 487, No. 3, 01.01.2019, p. 4393-4408.

Research output: Contribution to journalArticle

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T1 - The failure of stellar feedback, magnetic fields, conduction, and morphological quenching in maintaining red galaxies

AU - Su, Kung Yi

AU - Hopkins, Philip F.

AU - Hayward, Christopher C.

AU - Ma, Xiangcheng

AU - Faucher-Giguère, Claude André

AU - Keres, Dusan

AU - Orr, Matthew E.

AU - Chan, T. K.

AU - Robles, Victor H.

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AB - The quenching 'maintenance' and related 'cooling flow' problems are important in galaxies from Milky Way mass through clusters. We investigate this in haloes with masses ∼1012-1014M0, using non-cosmological high-resolution hydrodynamic simulations with the FIRE-2 (Feedback In Realistic Environments) stellar feedback model. We specifically focus on physics present without AGN, and show that various proposed 'non-AGN' solution mechanisms in the literature, including Type Ia supernovae, shocked AGB winds, other forms of stellar feedback (e.g. cosmic rays), magnetic fields, Spitzer-Braginskii conduction, or 'morphological quenching' do not halt or substantially reduce cooling flows nor maintain 'quenched' galaxies in this mass range. We show that stellar feedback (including cosmic rays from SNe) alters the balance of cold/warm gas and the rate at which the cooled gas within the galaxy turns into stars, but not the net baryonic inflow. If anything, outflowing metals and dense gas promote additional cooling. Conduction is important only in the most massive haloes, as expected, but even at ∼1014M0 reduces inflow only by a factor ∼2 (owing to saturation effects and anisotropic suppression). Changing the morphology of the galaxies only slightly alters their Toomre-Q parameter, and has no effect on cooling (as expected), so has essentially no effect on cooling flows or maintaining quenching. This all supports the idea that additional physics, e.g. AGN feedback, must be important in massive galaxies.

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KW - MHD-methods

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