Quantifying Baryonic Feedback on the Warm–Hot Circumgalactic Medium in CAMELS Simulations
The baryonic physics shaping galaxy formation and evolution are complex, spanning a vast range of scales and making them challenging to model. Cosmological simulations rely on subgrid models that produce significantly different predictions. Understanding how models of stellar and active galactic nuc...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/ada442 |
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| author | Isabel Medlock Chloe Neufeld Daisuke Nagai Daniel Anglés-Alcázar Shy Genel Benjamin D. Oppenheimer Xavier Sims Priyanka Singh Francisco Villaescusa-Navarro |
| author_facet | Isabel Medlock Chloe Neufeld Daisuke Nagai Daniel Anglés-Alcázar Shy Genel Benjamin D. Oppenheimer Xavier Sims Priyanka Singh Francisco Villaescusa-Navarro |
| author_sort | Isabel Medlock |
| collection | DOAJ |
| description | The baryonic physics shaping galaxy formation and evolution are complex, spanning a vast range of scales and making them challenging to model. Cosmological simulations rely on subgrid models that produce significantly different predictions. Understanding how models of stellar and active galactic nucleus (AGN) feedback affect baryon behavior across different halo masses and redshifts is essential. Using the SIMBA and IllustrisTNG suites from the Cosmology and Astrophysics with MachinE Learning Simulations (CAMELS) project, we explore the effect of parameters governing the subgrid implementation of stellar and AGN feedback. We find that while IllustrisTNG shows higher cumulative feedback energy across all halos, SIMBA demonstrates a greater spread of baryons, quantified by the closure radius and circumgalactic medium (CGM) gas fraction. This suggests that feedback in SIMBA couples more effectively to baryons and drives them more efficiently within the host halo. There is evidence that the different feedback modes are highly interrelated in these subgrid models. The parameters controlling the stellar feedback efficiency significantly impact AGN feedback, as seen in the suppression of black hole mass growth and delayed activation of AGN feedback to higher-mass halos with increasing stellar feedback efficiency in both simulations. Additionally, the AGN feedback efficiency parameters affect the CGM gas fraction at low halo masses in SIMBA, hinting at complex, nonlinear interactions between the AGN and supernova feedback modes. Overall, we demonstrate that stellar and AGN feedback are intimately interwoven, especially at low redshift, due to subgrid implementation, resulting in halo property effects that might initially seem counterintuitive. |
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| institution | Kabale University |
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| language | English |
| publishDate | 2025-01-01 |
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| series | The Astrophysical Journal |
| spelling | doaj-art-8d1ee53991b74ef78f85444c115027ce2025-02-04T11:45:29ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0198016110.3847/1538-4357/ada442Quantifying Baryonic Feedback on the Warm–Hot Circumgalactic Medium in CAMELS SimulationsIsabel Medlock0Chloe Neufeld1https://orcid.org/0000-0002-6558-9894Daisuke Nagai2https://orcid.org/0000-0002-6766-5942Daniel Anglés-Alcázar3Shy Genel4https://orcid.org/0000-0002-3185-1540Benjamin D. Oppenheimer5https://orcid.org/0000-0002-3391-2116Xavier Sims6Priyanka Singh7Francisco Villaescusa-Navarro8Department of Astronomy, Yale University , New Haven, CT 06520, USADepartment of Astronomy, Yale University , New Haven, CT 06520, USADepartment of Astronomy, Yale University , New Haven, CT 06520, USA; Department of Physics, Yale University , New Haven, CT 06520, USADepartment of Physics, University of Connecticut , 196 Auditorium Road, U-3046, Storrs, CT 06269, USACenter for Computational Astrophysics, Flatiron Institute , 162 5th Avenue, New York, NY 10010, USA; Columbia Astrophysics Laboratory, Columbia University , 550 West 120th Street, New York, NY 10027, USACASA, Department of Astrophysical and Planetary Sciences, University of Colorado , Boulder, CO 80309, USADepartment of Physics, University of Connecticut , 196 Auditorium Road, U-3046, Storrs, CT 06269, USADepartment of Physics, Yale University , New Haven, CT 06520, USA; Department of Astronomy, Astrophysics & Space Engineering, Indian Institute of Technology Indore , IndiaCenter for Computational Astrophysics, Flatiron Institute , 162 5th Avenue, New York, NY 10010, USA; Department of Astrophysical Sciences, Princeton University , Peyton Hall, Princeton, NJ 08544, USAThe baryonic physics shaping galaxy formation and evolution are complex, spanning a vast range of scales and making them challenging to model. Cosmological simulations rely on subgrid models that produce significantly different predictions. Understanding how models of stellar and active galactic nucleus (AGN) feedback affect baryon behavior across different halo masses and redshifts is essential. Using the SIMBA and IllustrisTNG suites from the Cosmology and Astrophysics with MachinE Learning Simulations (CAMELS) project, we explore the effect of parameters governing the subgrid implementation of stellar and AGN feedback. We find that while IllustrisTNG shows higher cumulative feedback energy across all halos, SIMBA demonstrates a greater spread of baryons, quantified by the closure radius and circumgalactic medium (CGM) gas fraction. This suggests that feedback in SIMBA couples more effectively to baryons and drives them more efficiently within the host halo. There is evidence that the different feedback modes are highly interrelated in these subgrid models. The parameters controlling the stellar feedback efficiency significantly impact AGN feedback, as seen in the suppression of black hole mass growth and delayed activation of AGN feedback to higher-mass halos with increasing stellar feedback efficiency in both simulations. Additionally, the AGN feedback efficiency parameters affect the CGM gas fraction at low halo masses in SIMBA, hinting at complex, nonlinear interactions between the AGN and supernova feedback modes. Overall, we demonstrate that stellar and AGN feedback are intimately interwoven, especially at low redshift, due to subgrid implementation, resulting in halo property effects that might initially seem counterintuitive.https://doi.org/10.3847/1538-4357/ada442Stellar feedbackCircumgalactic mediumHydrodynamical simulationsActive galactic nuclei |
| spellingShingle | Isabel Medlock Chloe Neufeld Daisuke Nagai Daniel Anglés-Alcázar Shy Genel Benjamin D. Oppenheimer Xavier Sims Priyanka Singh Francisco Villaescusa-Navarro Quantifying Baryonic Feedback on the Warm–Hot Circumgalactic Medium in CAMELS Simulations The Astrophysical Journal Stellar feedback Circumgalactic medium Hydrodynamical simulations Active galactic nuclei |
| title | Quantifying Baryonic Feedback on the Warm–Hot Circumgalactic Medium in CAMELS Simulations |
| title_full | Quantifying Baryonic Feedback on the Warm–Hot Circumgalactic Medium in CAMELS Simulations |
| title_fullStr | Quantifying Baryonic Feedback on the Warm–Hot Circumgalactic Medium in CAMELS Simulations |
| title_full_unstemmed | Quantifying Baryonic Feedback on the Warm–Hot Circumgalactic Medium in CAMELS Simulations |
| title_short | Quantifying Baryonic Feedback on the Warm–Hot Circumgalactic Medium in CAMELS Simulations |
| title_sort | quantifying baryonic feedback on the warm hot circumgalactic medium in camels simulations |
| topic | Stellar feedback Circumgalactic medium Hydrodynamical simulations Active galactic nuclei |
| url | https://doi.org/10.3847/1538-4357/ada442 |
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