TY - JOUR
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.
N1 - Funding Information:
We thank Eliot Quataert for useful discussion. The Flatiron Institute is supported by the Simons Foundation. Support for PFH was provided by an Alfred P. Sloan Research Fellowship, NASA ATP Grant NNX14AH35G, and NSF Collaborative Research Grant #1411920 and CAREER grant #1455342. CAFG was supported by NSF through grants AST-1412836, AST-1517491, AST-1715216, and CAREER award AST-1652522, by NASA through grant NNX15AB22G, by CXO through grant TM7-18007, and by a Cottrell Scholar Award from the Research Corporation for Science Advancement. DK was supported by NSF grant AST-1715101 and the Cottrell Scholar Award from the Research Corporation for Science Advancement. VHR acknowledges support from UC-MEXUS and CONACyT through the postdoctoral fellowship. Numerical calculations were run on the Caltech compute cluster 'Wheeler,' allocations from XSEDE TG-AST130039 and PRAC NSF.1713353 supported by the NSF, and NASA HEC SMD-16-7592.
Funding Information:
We thank Eliot Quataert for useful discussion. The Flatiron Institute is supported by the Simons Foundation. Support for PFH was provided by an Alfred P. Sloan Research Fellowship, NASA ATP Grant NNX14AH35G, and NSF Collaborative Research Grant #1411920 and CAREER grant #1455342. CAFG was supported by NSF through grants AST-1412836, AST-1517491, AST-1715216, and CAREER award AST-1652522, by NASA through grant NNX15AB22G, by CXO through grant TM7-18007, and by a Cottrell Scholar Award from the Research Corporation for Science Advancement. DK was supported by NSF grant AST-1715101 and the Cottrell Scholar Award from the Research Corporation for Science Advancement. VHR acknowledges support from UC-MEXUS and CONACyT through the postdoctoral fellowship. Numerical calculations were run on the Caltech compute cluster ‘Wheeler,’ allocations from XSEDE TG-AST130039 and PRAC NSF.1713353 supported by the NSF, and NASA HEC SMD-16-7592.
Publisher Copyright:
© 2019 The Author(s) Published by Oxford University Press on behalf of the Royal Astronomical Society.
PY - 2019/8/11
Y1 - 2019/8/11
N2 - 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.
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.
KW - Clusters
KW - Clusters
KW - Evolution-galaxies
KW - Galaxies
KW - Intracluster medium-X-rays
KW - MHD-methods
KW - Numerical - cosmic rays-Galaxy
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U2 - 10.1093/mnras/stz1494
DO - 10.1093/mnras/stz1494
M3 - Article
AN - SCOPUS:85072371471
SN - 0035-8711
VL - 487
SP - 4393
EP - 4408
JO - Monthly Notices of the Royal Astronomical Society
JF - Monthly Notices of the Royal Astronomical Society
IS - 3
ER -