Статья

Cosmic evolution of stellar quenching by AGN feedback: clues from the Horizon-AGN simulation

Ricarda S. Beckmann1Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UKJulien Devriendt1Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UKAdrianne Slyz1Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UKSébastien Peirani3Sorbonne Universites, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75005 Paris, FranceMark L. A. Richardson1Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UKYohan Dubois3Sorbonne Universites, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75005 Paris, FranceChristophe Pichon3Sorbonne Universites, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75005 Paris, FranceNora Elisa Chisari1Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UKSugata Kaviraj6Centre for Astrophysics Research, University of Hertfordshire, College Lane, Hatfield, Herts AL10 9AB, UKC. Laigle1Sub-department of Astrophysics, University of Oxford, Keble Road, Oxford OX1 3RH, UKMarta Volonteri3Sorbonne Universites, UPMC Univ Paris 06, UMR 7095, Institut d'Astrophysique de Paris, F-75005 Paris, France

2017en

ABI

Аннотация

Abstract The observed massive end of the galaxy stellar mass function is steeper than its predicted dark matter halo counterpart in the standard Λ cold dark matter paradigm. In this paper, we investigate the impact of active galactic nuclei (AGN) feedback on star formation in massive galaxies. We isolate the impact of AGN by comparing two simulations from the HORIZON suite, which are identical except that one also includes supermassive black holes (SMBHs) and related feedback models. This allows us to cross-identify individual galaxies between simulations and quantify the effect of AGN feedback on their properties, including stellar mass and gas outflows. We find that massive galaxies (M* ≥ 1011 M⊙) are quenched by AGN feedback to the extent that their stellar masses decrease by up to 80 per cent at z = 0. SMBHs affect their host halo through a combination of outflows that reduce their baryonic mass, particularly for galaxies in the mass range 109 M⊙ ≤ M* ≤ 1011 M⊙, and a disruption of central gas inflows, which limits in situ star formation. As a result, net gas inflows on to massive galaxies, M* ≥ 1011 M⊙, drop by up to 70 per cent. We measure a redshift evolution in the stellar mass ratio of twin galaxies with and without AGN feedback, with galaxies of a given stellar mass showing stronger signs of quenching earlier on. This evolution is driven by a progressive flattening of the MSMBH–M* relation with redshift, particularly for galaxies with M* ≤ 1010 M⊙. MSMBH/M* ratios decrease over time, as falling average gas densities in galaxies curb SMBH growth.

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Идентификаторы

DOI: 10.1093/mnras/stx1831

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Цитирований: 1Использованных источников: 0

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