MACER3D—An Upgrade of MACER2D with Enhanced Subgrid Models and Gas Physics—and Its Application to Simulating AGN Feedback in a Massive Elliptical Galaxy
We present Multiscale AGN-regulated Cosmic Ecosystem Resolver in 3D (MACER3D), a new suite of three-dimensional hydrodynamic simulations that study active galactic nuclei (AGN) feedback on galactic scales over gigayears in duration, with major enhancements in subgrid models and gas physics over its...
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2025-01-01
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| Series: | The Astrophysical Journal |
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| Online Access: | https://doi.org/10.3847/1538-4357/adcaba |
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| author | Haoen Zhang Haojie Xia Suoqing Ji Feng Yuan Minhang Guo Rui Zhang Bocheng Zhu Yihuan Di Aoyun He Tingfang Su Yuxuan Zou |
| author_facet | Haoen Zhang Haojie Xia Suoqing Ji Feng Yuan Minhang Guo Rui Zhang Bocheng Zhu Yihuan Di Aoyun He Tingfang Su Yuxuan Zou |
| author_sort | Haoen Zhang |
| collection | DOAJ |
| description | We present Multiscale AGN-regulated Cosmic Ecosystem Resolver in 3D (MACER3D), a new suite of three-dimensional hydrodynamic simulations that study active galactic nuclei (AGN) feedback on galactic scales over gigayears in duration, with major enhancements in subgrid models and gas physics over its predecessor—Massive AGN Controlled Ellipticals Resolved (MACER), which is in two dimensions (hereafter MACER2D). MACER3D resolves gas dynamics from within the Bondi radius (∼25 pc) to halo scales. Combined with black hole accretion theory, it enables an accurate calculation of AGN outputs and subsequently their large-scale feedback effects. We present results from simulating an isolated elliptical galaxy with different feedback configurations. In the fiducial model with both AGN and supernova (SN) feedback, the temporal evolution of AGN luminosity and star formation rate are strongly correlated, suggesting shared dependence on the availability of gas supply for SMBH accretion and star formation. AGN duty cycles of several percent with a single-cycle timescale of ∼10 ^2 Myr agree with observations, while models with only AGN or SN feedback fail to reproduce observed cycles. While all models maintain a quiescent galaxy state, the fiducial AGN+SN feedback model results in higher star formation than no-SN feedback, suggesting SN feedback, when acting synergistically with AGN feedback, may positively impact star formation. Combined AGN and SN feedback enhances halo-scale metal enrichment compared to single-feedback models. The simulated X-ray properties match observations and predict transient cavities produced by cold-mode AGN winds from past burst events. The differences between the results obtained by MACER2D and MACER3D are also discussed. |
| format | Article |
| id | doaj-art-ce71f2de4b9d44ce92460a451a486de8 |
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| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-ce71f2de4b9d44ce92460a451a486de82025-08-20T01:55:38ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-01985217810.3847/1538-4357/adcabaMACER3D—An Upgrade of MACER2D with Enhanced Subgrid Models and Gas Physics—and Its Application to Simulating AGN Feedback in a Massive Elliptical GalaxyHaoen Zhang0https://orcid.org/0009-0008-0460-8685Haojie Xia1https://orcid.org/0009-0004-3881-674XSuoqing Ji2https://orcid.org/0000-0001-9658-0588Feng Yuan3https://orcid.org/0000-0003-3564-6437Minhang Guo4https://orcid.org/0009-0009-7849-2643Rui Zhang5https://orcid.org/0009-0005-6382-2532Bocheng Zhu6https://orcid.org/0000-0003-0900-4481Yihuan Di7https://orcid.org/0000-0003-1717-6697Aoyun He8https://orcid.org/0000-0002-4882-8953Tingfang Su9https://orcid.org/0009-0003-1442-105XYuxuan Zou10https://orcid.org/0009-0006-4662-3053Astrophysics Division, Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of China; University of Chinese Academy of Sciences , No. 19A Yuquan Road, Beijing 100049, People’s Republic of ChinaAstrophysics Division, Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of China; University of Chinese Academy of Sciences , No. 19A Yuquan Road, Beijing 100049, People’s Republic of ChinaCenter for Astronomy and Astrophysics and Department of Physics, Fudan University , Shanghai 200438, People’s Republic of China ; sqji@fudan.edu.cn, fyuan@fudan.edu.cn; Key Laboratory of Nuclear Physics and Ion-Beam Application (MOE), Fudan University , Shanghai 200433, People’s Republic of ChinaCenter for Astronomy and Astrophysics and Department of Physics, Fudan University , Shanghai 200438, People’s Republic of China ; sqji@fudan.edu.cn, fyuan@fudan.edu.cnAstrophysics Division, Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of China; University of Chinese Academy of Sciences , No. 19A Yuquan Road, Beijing 100049, People’s Republic of China; ShanghaiTech University , 393 Middle Huaxia Road, Shanghai 201210, People’s Republic of ChinaAstrophysics Division, Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of China; University of Chinese Academy of Sciences , No. 19A Yuquan Road, Beijing 100049, People’s Republic of ChinaNational Astronomical Observatories, Chinese Academy of Sciences , 20A Datun Road, Beijing 100101, People’s Republic of ChinaDepartment of Astronomy, Shanghai Jiao Tong University , 800 Dongchuan Road, Shanghai 200240, People’s Republic of ChinaAstrophysics Division, Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of China; University of Chinese Academy of Sciences , No. 19A Yuquan Road, Beijing 100049, People’s Republic of ChinaAstrophysics Division, Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of China; University of Chinese Academy of Sciences , No. 19A Yuquan Road, Beijing 100049, People’s Republic of ChinaAstrophysics Division, Shanghai Astronomical Observatory, Chinese Academy of Sciences , 80 Nandan Road, Shanghai 200030, People’s Republic of China; University of Chinese Academy of Sciences , No. 19A Yuquan Road, Beijing 100049, People’s Republic of ChinaWe present Multiscale AGN-regulated Cosmic Ecosystem Resolver in 3D (MACER3D), a new suite of three-dimensional hydrodynamic simulations that study active galactic nuclei (AGN) feedback on galactic scales over gigayears in duration, with major enhancements in subgrid models and gas physics over its predecessor—Massive AGN Controlled Ellipticals Resolved (MACER), which is in two dimensions (hereafter MACER2D). MACER3D resolves gas dynamics from within the Bondi radius (∼25 pc) to halo scales. Combined with black hole accretion theory, it enables an accurate calculation of AGN outputs and subsequently their large-scale feedback effects. We present results from simulating an isolated elliptical galaxy with different feedback configurations. In the fiducial model with both AGN and supernova (SN) feedback, the temporal evolution of AGN luminosity and star formation rate are strongly correlated, suggesting shared dependence on the availability of gas supply for SMBH accretion and star formation. AGN duty cycles of several percent with a single-cycle timescale of ∼10 ^2 Myr agree with observations, while models with only AGN or SN feedback fail to reproduce observed cycles. While all models maintain a quiescent galaxy state, the fiducial AGN+SN feedback model results in higher star formation than no-SN feedback, suggesting SN feedback, when acting synergistically with AGN feedback, may positively impact star formation. Combined AGN and SN feedback enhances halo-scale metal enrichment compared to single-feedback models. The simulated X-ray properties match observations and predict transient cavities produced by cold-mode AGN winds from past burst events. The differences between the results obtained by MACER2D and MACER3D are also discussed.https://doi.org/10.3847/1538-4357/adcabaGalaxy formationGalaxy evolutionHydrodynamical simulations |
| spellingShingle | Haoen Zhang Haojie Xia Suoqing Ji Feng Yuan Minhang Guo Rui Zhang Bocheng Zhu Yihuan Di Aoyun He Tingfang Su Yuxuan Zou MACER3D—An Upgrade of MACER2D with Enhanced Subgrid Models and Gas Physics—and Its Application to Simulating AGN Feedback in a Massive Elliptical Galaxy The Astrophysical Journal Galaxy formation Galaxy evolution Hydrodynamical simulations |
| title | MACER3D—An Upgrade of MACER2D with Enhanced Subgrid Models and Gas Physics—and Its Application to Simulating AGN Feedback in a Massive Elliptical Galaxy |
| title_full | MACER3D—An Upgrade of MACER2D with Enhanced Subgrid Models and Gas Physics—and Its Application to Simulating AGN Feedback in a Massive Elliptical Galaxy |
| title_fullStr | MACER3D—An Upgrade of MACER2D with Enhanced Subgrid Models and Gas Physics—and Its Application to Simulating AGN Feedback in a Massive Elliptical Galaxy |
| title_full_unstemmed | MACER3D—An Upgrade of MACER2D with Enhanced Subgrid Models and Gas Physics—and Its Application to Simulating AGN Feedback in a Massive Elliptical Galaxy |
| title_short | MACER3D—An Upgrade of MACER2D with Enhanced Subgrid Models and Gas Physics—and Its Application to Simulating AGN Feedback in a Massive Elliptical Galaxy |
| title_sort | macer3d an upgrade of macer2d with enhanced subgrid models and gas physics and its application to simulating agn feedback in a massive elliptical galaxy |
| topic | Galaxy formation Galaxy evolution Hydrodynamical simulations |
| url | https://doi.org/10.3847/1538-4357/adcaba |
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