Supermassive black holes and their feedback effects in the IllustrisTNG simulation
© 2018 The Author(s) Published by Oxford University Press on behalf of The Royal Astronomical Society. 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 employ...
| Main Authors: | , , , , , , , , , , |
|---|---|
| Other Authors: | |
| Format: | Article |
| Language: | English |
| Published: |
Oxford University Press (OUP)
2021
|
| Online Access: | https://hdl.handle.net/1721.1/135836 |
| _version_ | 1826197990105153536 |
|---|---|
| author | Weinberger, Rainer Springel, Volker Pakmor, Rüdiger Nelson, Dylan Genel, Shy Pillepich, Annalisa Vogelsberger, Mark Marinacci, Federico Naiman, Jill Torrey, Paul Hernquist, Lars |
| author2 | Massachusetts Institute of Technology. Department of Physics |
| author_facet | Massachusetts Institute of Technology. Department of Physics Weinberger, Rainer Springel, Volker Pakmor, Rüdiger Nelson, Dylan Genel, Shy Pillepich, Annalisa Vogelsberger, Mark Marinacci, Federico Naiman, Jill Torrey, Paul Hernquist, Lars |
| author_sort | Weinberger, Rainer |
| collection | MIT |
| description | © 2018 The Author(s) Published by Oxford University Press on behalf of The Royal Astronomical Society. 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 holes 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 108.5M⊙, 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 is in good agreement with observations, whereas the simulation tends to overpredict the high-redshift quasar luminosity function. |
| first_indexed | 2024-09-23T10:57:09Z |
| format | Article |
| id | mit-1721.1/135836 |
| institution | Massachusetts Institute of Technology |
| language | English |
| last_indexed | 2024-09-23T10:57:09Z |
| publishDate | 2021 |
| publisher | Oxford University Press (OUP) |
| record_format | dspace |
| spelling | mit-1721.1/1358362023-09-27T17:47:49Z Supermassive black holes and their feedback effects in the IllustrisTNG simulation Weinberger, Rainer Springel, Volker Pakmor, Rüdiger Nelson, Dylan Genel, Shy Pillepich, Annalisa Vogelsberger, Mark Marinacci, Federico Naiman, Jill Torrey, Paul Hernquist, Lars Massachusetts Institute of Technology. Department of Physics MIT Kavli Institute for Astrophysics and Space Research © 2018 The Author(s) Published by Oxford University Press on behalf of The Royal Astronomical Society. 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 holes 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 108.5M⊙, 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 is in good agreement with observations, whereas the simulation tends to overpredict the high-redshift quasar luminosity function. 2021-10-27T20:29:34Z 2021-10-27T20:29:34Z 2018 2019-06-10T10:53:30Z Article http://purl.org/eprint/type/JournalArticle https://hdl.handle.net/1721.1/135836 en 10.1093/MNRAS/STY1733 Monthly Notices of the Royal Astronomical Society Creative Commons Attribution-Noncommercial-Share Alike http://creativecommons.org/licenses/by-nc-sa/4.0/ application/pdf Oxford University Press (OUP) arXiv |
| spellingShingle | Weinberger, Rainer Springel, Volker Pakmor, Rüdiger Nelson, Dylan Genel, Shy Pillepich, Annalisa Vogelsberger, Mark Marinacci, Federico Naiman, Jill Torrey, Paul Hernquist, Lars Supermassive black holes and their feedback effects in the IllustrisTNG simulation |
| title | Supermassive black holes and their feedback effects in the IllustrisTNG simulation |
| title_full | Supermassive black holes and their feedback effects in the IllustrisTNG simulation |
| title_fullStr | Supermassive black holes and their feedback effects in the IllustrisTNG simulation |
| title_full_unstemmed | Supermassive black holes and their feedback effects in the IllustrisTNG simulation |
| title_short | Supermassive black holes and their feedback effects in the IllustrisTNG simulation |
| title_sort | supermassive black holes and their feedback effects in the illustristng simulation |
| url | https://hdl.handle.net/1721.1/135836 |
| work_keys_str_mv | AT weinbergerrainer supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation AT springelvolker supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation AT pakmorrudiger supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation AT nelsondylan supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation AT genelshy supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation AT pillepichannalisa supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation AT vogelsbergermark supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation AT marinaccifederico supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation AT naimanjill supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation AT torreypaul supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation AT hernquistlars supermassiveblackholesandtheirfeedbackeffectsintheillustristngsimulation |