X-ray emission signatures of galactic feedback in the hot circumgalactic medium: predictions from cosmological hydrodynamical simulations
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| Format: | Preprint |
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2025
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| _version_ | 1866908415120375808 |
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| author | Silich, Emily M. ZuHone, John Bellomi, Elena Hummels, Cameron Oppenheimer, Benjamin Hopkins, Philip F. Lochhaas, Cassandra Ponnada, Sam B. Vikhlinin, Alexey |
| author_facet | Silich, Emily M. ZuHone, John Bellomi, Elena Hummels, Cameron Oppenheimer, Benjamin Hopkins, Philip F. Lochhaas, Cassandra Ponnada, Sam B. Vikhlinin, Alexey |
| contents | Little is currently known about the physical properties of the hot circumgalactic medium (CGM) surrounding massive galaxies. Next-generation X-ray observatories will enable detailed studies of the hot CGM in emission. To support these future efforts, we make predictions of the X-ray emission from the hot CGM using a sample of 28 $\sim$Milky Way-mass disk galaxies at $z=0$ from seven cosmological hydrodynamical simulation suites incorporating a wide range of galactic feedback prescriptions. The X-ray surface brightness (XSB) morphology of the hot CGM varies significantly across simulations. XSB-enhanced outflows and bubble-like structures are predicted in many galaxies simulated with AGN feedback and in some stellar-feedback-only galaxies, while other galaxies exhibit more isotropic XSB distributions at varying brightnesses. Galaxies simulated without cosmic ray physics exhibit radial XSB profiles with similar shapes ($\propto r^{-3}$ within $20-200$ kpc), with scatter about this slope likely due to underlying feedback physics. The hot CGM kinematics also differ substantially: velocity maps reveal signatures of bulk CGM rotation and high-velocity biconical outflows, particularly in simulations incorporating AGN feedback. Some stellar-feedback-only models also generate similar AGN-like outflows, which we postulate is due to centrally-concentrated star formation. Simulations featuring AGN feedback frequently produce extended temperature enhancements in large-scale galactic outflows, while simulations incorporating cosmic ray physics predict the coolest CGM due to pressure support being provided by cosmic rays rather than hot CGM. Individually-resolved X-ray emission lines further distinguish hot CGM phases, with lower-energy lines (e.g., O VII) largely tracing volume-filling gas, and higher-energy lines (e.g., Fe XVII) highlighting high-velocity feedback-driven outflows. |
| format | Preprint |
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arxiv_https___arxiv_org_abs_2506_17440 |
| institution | arXiv |
| publishDate | 2025 |
| record_format | arxiv |
| spellingShingle | X-ray emission signatures of galactic feedback in the hot circumgalactic medium: predictions from cosmological hydrodynamical simulations Silich, Emily M. ZuHone, John Bellomi, Elena Hummels, Cameron Oppenheimer, Benjamin Hopkins, Philip F. Lochhaas, Cassandra Ponnada, Sam B. Vikhlinin, Alexey Astrophysics of Galaxies High Energy Astrophysical Phenomena Little is currently known about the physical properties of the hot circumgalactic medium (CGM) surrounding massive galaxies. Next-generation X-ray observatories will enable detailed studies of the hot CGM in emission. To support these future efforts, we make predictions of the X-ray emission from the hot CGM using a sample of 28 $\sim$Milky Way-mass disk galaxies at $z=0$ from seven cosmological hydrodynamical simulation suites incorporating a wide range of galactic feedback prescriptions. The X-ray surface brightness (XSB) morphology of the hot CGM varies significantly across simulations. XSB-enhanced outflows and bubble-like structures are predicted in many galaxies simulated with AGN feedback and in some stellar-feedback-only galaxies, while other galaxies exhibit more isotropic XSB distributions at varying brightnesses. Galaxies simulated without cosmic ray physics exhibit radial XSB profiles with similar shapes ($\propto r^{-3}$ within $20-200$ kpc), with scatter about this slope likely due to underlying feedback physics. The hot CGM kinematics also differ substantially: velocity maps reveal signatures of bulk CGM rotation and high-velocity biconical outflows, particularly in simulations incorporating AGN feedback. Some stellar-feedback-only models also generate similar AGN-like outflows, which we postulate is due to centrally-concentrated star formation. Simulations featuring AGN feedback frequently produce extended temperature enhancements in large-scale galactic outflows, while simulations incorporating cosmic ray physics predict the coolest CGM due to pressure support being provided by cosmic rays rather than hot CGM. Individually-resolved X-ray emission lines further distinguish hot CGM phases, with lower-energy lines (e.g., O VII) largely tracing volume-filling gas, and higher-energy lines (e.g., Fe XVII) highlighting high-velocity feedback-driven outflows. |
| title | X-ray emission signatures of galactic feedback in the hot circumgalactic medium: predictions from cosmological hydrodynamical simulations |
| topic | Astrophysics of Galaxies High Energy Astrophysical Phenomena |
| url | https://arxiv.org/abs/2506.17440 |