{"work":{"id":"47fad1d9-8243-4eea-9555-219b56f6aa21","openalex_id":"https://openalex.org/W2766073562","doi":"10.1093/mnras/sty1733","arxiv_id":"1710.04659","raw_key":null,"title":"2018, MNRAS, 479, 4056, doi: 10.1093/mnras/sty1733","authors":[{"given":"Rainer","family":"Weinberger","sequence":"first","affiliation":[{"name":"Heidelberg Institute for Theoretical Studies, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany"}]},{"given":"Volker","family":"Springel","sequence":"additional","affiliation":[{"name":"Heidelberg Institute for Theoretical Studies, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany"},{"name":"Zentrum für Astronomie der Universität Heidelberg, ARI, Mönchhofstrasse 12-14, D-69120 Heidelberg, Germany"},{"name":"Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str 1, D-85748 Garching, Germany"}]},{"given":"Rüdiger","family":"Pakmor","sequence":"additional","affiliation":[{"name":"Heidelberg Institute for Theoretical Studies, Schloss-Wolfsbrunnenweg 35, D-69118 Heidelberg, Germany"}]},{"given":"Dylan","family":"Nelson","sequence":"additional","affiliation":[{"name":"Max-Planck-Institut für Astrophysik, Karl-Schwarzschild-Str 1, D-85748 Garching, Germany"}]},{"ORCID":"https://orcid.org/0000-0002-3185-1540","given":"Shy","family":"Genel","sequence":"additional","affiliation":[{"name":"Center for Computational Astrophysics, Flatiron Institute, 162 Fifth Avenue, New York, NY 10010, USA"},{"name":"Columbia Astrophysics Laboratory, Columbia University, 550 West 120th Street, New York, NY 10027, USA"}],"authenticated-orcid":false},{"given":"Annalisa","family":"Pillepich","sequence":"additional","affiliation":[{"name":"Max-Planck-Institut für Astronomie, Königstuhl 17, D-69117 Heidelberg, Germany"}]},{"given":"Mark","family":"Vogelsberger","sequence":"additional","affiliation":[{"name":"Department of Physics, Kavli Institute for Astrophysics and Space Research, MIT, Cambridge, MA 02139, USA"}]},{"ORCID":"https://orcid.org/0000-0003-3816-7028","given":"Federico","family":"Marinacci","sequence":"additional","affiliation":[{"name":"Department of Physics, Kavli Institute for Astrophysics and Space Research, MIT, Cambridge, MA 02139, USA"}],"authenticated-orcid":false},{"given":"Jill","family":"Naiman","sequence":"additional","affiliation":[{"name":"Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA"}]},{"ORCID":"https://orcid.org/0000-0002-5653-0786","given":"Paul","family":"Torrey","sequence":"additional","affiliation":[{"name":"Department of Physics, Kavli Institute for Astrophysics and Space Research, MIT, Cambridge, MA 02139, USA"}],"authenticated-orcid":false},{"given":"Lars","family":"Hernquist","sequence":"additional","affiliation":[{"name":"Harvard-Smithsonian Center for Astrophysics, 60 Garden Street, Cambridge, MA 02138, USA"}]}],"authors_text":"Weinberger, R","year":2018,"venue":"astro-ph.GA","abstract":"We study the population of supermassive black holes (SMBHs) and their effects on massive central galaxies in the IllustrisTNG cosmological hydrodynamical simulations of galaxy formation. The employed model for SMBH growth and feedback assumes a two-mode scenario in which the feedback from active galactic nuclei occurs through a kinetic, comparatively efficient mode at low accretion rates relative to the Eddington limit, and in the form of a thermal, less efficient mode at high accretion rates. We show that the quenching of massive central galaxies happens coincidently with kinetic-mode feedback, consistent with the notion that active supermassive black cause the low specific star formation rates observed in massive galaxies. However, major galaxy mergers are not responsible for initiating most of the quenching events in our model. Up to black hole masses of about $10^{8.5}\\,{\\rm M}_\\odot$, the dominant growth channel for SMBHs is in the thermal mode. Higher mass black holes stay mainly in the kinetic mode and gas accretion is self-regulated via their feedback, which causes their Eddington ratios to drop, with SMBH mergers becoming the main channel for residual mass growth. As a consequence, the quasar luminosity function is dominated by rapidly accreting, moderately massive black holes in the thermal mode. We show that the associated growth history of SMBHs produces a low-redshift quasar luminosity function and a redshift zero black hole mass-stellar bulge mass relation in good agreement with observations, whereas the simulation tends to over-predict the high-redshift quasar luminosity function.","external_url":"https://doi.org/10.1093/mnras/sty1733","cited_by_count":413,"metadata_source":"doi_reference","metadata_fetched_at":"2026-06-27T07:00:40.202855+00:00","pith_arxiv_id":"1710.04659","created_at":"2026-05-08T17:58:52.825927+00:00","updated_at":"2026-06-27T07:00:40.202855+00:00","title_quality_ok":false,"display_title":"Supermassive black holes and their feedback effects in the IllustrisTNG simulation","render_title":"Supermassive black holes and their feedback effects in the IllustrisTNG simulation"},"hub":{"state":{"work_id":"47fad1d9-8243-4eea-9555-219b56f6aa21","tier":"hub","tier_reason":"10+ Pith inbound or 1,000+ external citations","pith_inbound_count":18,"external_cited_by_count":413,"distinct_field_count":2,"first_pith_cited_at":"2025-09-24T18:00:13+00:00","last_pith_cited_at":"2026-06-24T14:03:23+00:00","author_build_status":"not_needed","summary_status":"needed","contexts_status":"needed","graph_status":"needed","ask_index_status":"not_needed","reader_status":"not_needed","recognition_status":"not_needed","updated_at":"2026-06-27T12:56:07.194349+00:00","tier_text":"hub"},"tier":"hub","role_counts":[{"context_role":"dataset","n":1}],"polarity_counts":[{"context_polarity":"use_dataset","n":1}],"runs":{},"summary":{},"graph":{},"authors":[]}}