XRISM Constrains Atmospheric Motion and Turbulent Dissipation in the Archetypal Radio-mode Feedback System Hydra-A
We present XRISM Resolve observations centered on Hydra-A, a redshift z = 0.054 brightest cluster galaxy, which hosts one of the largest and most powerful FR-I radio sources in the nearby Universe. We examine the effects of its high jet power on the velocity structure of the cluster’s hot atmosphere...
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2025-01-01
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| Online Access: | https://doi.org/10.3847/1538-4357/adf32d |
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| author | Tom Rose B. R. McNamara Julian Meunier A. C. Fabian Helen Russell Paul Nulsen Neo Dizdar Timothy M. Heckman Michael McDonald Maxim Markevitch Frits Paerels Aurora Simionescu Norbert Werner Alison L. Coil Edmund Hodges-Kluck Eric D. Miller Michael Wise |
| author_facet | Tom Rose B. R. McNamara Julian Meunier A. C. Fabian Helen Russell Paul Nulsen Neo Dizdar Timothy M. Heckman Michael McDonald Maxim Markevitch Frits Paerels Aurora Simionescu Norbert Werner Alison L. Coil Edmund Hodges-Kluck Eric D. Miller Michael Wise |
| author_sort | Tom Rose |
| collection | DOAJ |
| description | We present XRISM Resolve observations centered on Hydra-A, a redshift z = 0.054 brightest cluster galaxy, which hosts one of the largest and most powerful FR-I radio sources in the nearby Universe. We examine the effects of its high jet power on the velocity structure of the cluster’s hot atmosphere. Hydra-A’s central radio jets have inflated X-ray cavities with energies upward of 10 ^61 erg. They reach altitudes of 225 kpc from the cluster center, well beyond the atmosphere’s central cooling region. Resolve’s 3′× 3′ field of view covers 190 × 190 kpc, which encompasses most of the cooling volume. We find a one-dimensional atmospheric velocity dispersion across the volume of 164 ± 10 km s ^−1 . The fraction in isotropic turbulence or unresolved bulk velocity is unknown. Assuming pure isotropic turbulence, the turbulent kinetic energy is 2.5% of the thermal energy radiated away over the cooling timescale, implying that kinetic energy must be supplied continually to offset cooling. While Hydra-A’s radio jets are powerful enough to supply kinetic energy to the atmosphere at the observed level, turbulent dissipation alone would struggle to offset cooling throughout the cooling volume. The central galaxy’s radial velocity is similar to the atmospheric velocity, with an offset of −37 ± 23 km s ^−1 . |
| format | Article |
| id | doaj-art-a5f3ceb5e3134960b2c1280b6e6ec36f |
| institution | Kabale University |
| issn | 1538-4357 |
| language | English |
| publishDate | 2025-01-01 |
| publisher | IOP Publishing |
| record_format | Article |
| series | The Astrophysical Journal |
| spelling | doaj-art-a5f3ceb5e3134960b2c1280b6e6ec36f2025-08-25T05:51:04ZengIOP PublishingThe Astrophysical Journal1538-43572025-01-0199014210.3847/1538-4357/adf32dXRISM Constrains Atmospheric Motion and Turbulent Dissipation in the Archetypal Radio-mode Feedback System Hydra-ATom Rose0https://orcid.org/0000-0002-8310-2218B. R. McNamara1https://orcid.org/0000-0002-2622-2627Julian Meunier2A. C. Fabian3https://orcid.org/0000-0002-9378-4072Helen Russell4https://orcid.org/0000-0001-5208-649XPaul Nulsen5https://orcid.org/0000-0003-0297-4493Neo Dizdar6Timothy M. Heckman7Michael McDonald8https://orcid.org/0000-0001-5226-8349Maxim Markevitch9https://orcid.org/0000-0003-0144-4052Frits Paerels10https://orcid.org/0000-0001-9225-6481Aurora Simionescu11https://orcid.org/0000-0002-9714-3862Norbert Werner12https://orcid.org/0000-0003-0392-0120Alison L. Coil13https://orcid.org/0000-0002-2583-5894Edmund Hodges-Kluck14https://orcid.org/0000-0002-2397-206XEric D. Miller15https://orcid.org/0000-0002-3031-2326Michael Wise16https://orcid.org/0000-0002-6470-2285Waterloo Centre for Astrophysics, University of Waterloo , ON N2L 3G1, CanadaWaterloo Centre for Astrophysics, University of Waterloo , ON N2L 3G1, CanadaWaterloo Centre for Astrophysics, University of Waterloo , ON N2L 3G1, CanadaInstitute of Astronomy, Cambridge University , Madingley Rd., Cambridge, CB3 0HA, UKSchool of Physics & Astronomy, University of Nottingham , Nottingham, NG7 2RD, UKCenter for Astrophysics ∣ Harvard & Smithsonian , 60 Garden St., Cambridge, MA 02138, USA; ICRAR, University of Western Australia , 35 Stirling Hwy., Crawley, WA 6009, AustraliaWaterloo Centre for Astrophysics, University of Waterloo , ON N2L 3G1, CanadaThe William H. Miller III Department of Physics and Astronomy, The Johns Hopkins University , Baltimore, MD 21218, USAMIT Kavli Institute for Astrophysics and Space Research , Massachusetts Institute of Technology, Cambridge, MA 02139, USANASA Goddard Space Flight Center , Code 662, Greenbelt, MD 20771, USAColumbia Astrophysics Laboratory, Columbia University , 538 W. 120th St., New York, NY 10027, USASRON Space Research Organisation Netherlands , Niels Bohrweg 4, 2333 CA Leiden, The NetherlandsDepartment of Theoretical Physics and Astrophysics, Faculty of Science, Masaryk University , Kotlářská, Brno, 61137, Czech RepublicDepartment of Astronomy and Astrophysics, University of California , 9500 Gilman Dr., La Jolla, CA 92093, USAUniversity of Michigan NASA Goddard Space Flight Center: Greenbelt , MD, USAKavli Institute for Astrophysics and Space Research , Massachusetts Institute of Technology, MA 02139, USASRON , Netherlands Institute for Space Research, Niels Bohrweg 4, 2333 CA Leiden, The NetherlandsWe present XRISM Resolve observations centered on Hydra-A, a redshift z = 0.054 brightest cluster galaxy, which hosts one of the largest and most powerful FR-I radio sources in the nearby Universe. We examine the effects of its high jet power on the velocity structure of the cluster’s hot atmosphere. Hydra-A’s central radio jets have inflated X-ray cavities with energies upward of 10 ^61 erg. They reach altitudes of 225 kpc from the cluster center, well beyond the atmosphere’s central cooling region. Resolve’s 3′× 3′ field of view covers 190 × 190 kpc, which encompasses most of the cooling volume. We find a one-dimensional atmospheric velocity dispersion across the volume of 164 ± 10 km s ^−1 . The fraction in isotropic turbulence or unresolved bulk velocity is unknown. Assuming pure isotropic turbulence, the turbulent kinetic energy is 2.5% of the thermal energy radiated away over the cooling timescale, implying that kinetic energy must be supplied continually to offset cooling. While Hydra-A’s radio jets are powerful enough to supply kinetic energy to the atmosphere at the observed level, turbulent dissipation alone would struggle to offset cooling throughout the cooling volume. The central galaxy’s radial velocity is similar to the atmospheric velocity, with an offset of −37 ± 23 km s ^−1 .https://doi.org/10.3847/1538-4357/adf32dGalaxy clustersIntracluster mediumX-ray astronomy |
| spellingShingle | Tom Rose B. R. McNamara Julian Meunier A. C. Fabian Helen Russell Paul Nulsen Neo Dizdar Timothy M. Heckman Michael McDonald Maxim Markevitch Frits Paerels Aurora Simionescu Norbert Werner Alison L. Coil Edmund Hodges-Kluck Eric D. Miller Michael Wise XRISM Constrains Atmospheric Motion and Turbulent Dissipation in the Archetypal Radio-mode Feedback System Hydra-A The Astrophysical Journal Galaxy clusters Intracluster medium X-ray astronomy |
| title | XRISM Constrains Atmospheric Motion and Turbulent Dissipation in the Archetypal Radio-mode Feedback System Hydra-A |
| title_full | XRISM Constrains Atmospheric Motion and Turbulent Dissipation in the Archetypal Radio-mode Feedback System Hydra-A |
| title_fullStr | XRISM Constrains Atmospheric Motion and Turbulent Dissipation in the Archetypal Radio-mode Feedback System Hydra-A |
| title_full_unstemmed | XRISM Constrains Atmospheric Motion and Turbulent Dissipation in the Archetypal Radio-mode Feedback System Hydra-A |
| title_short | XRISM Constrains Atmospheric Motion and Turbulent Dissipation in the Archetypal Radio-mode Feedback System Hydra-A |
| title_sort | xrism constrains atmospheric motion and turbulent dissipation in the archetypal radio mode feedback system hydra a |
| topic | Galaxy clusters Intracluster medium X-ray astronomy |
| url | https://doi.org/10.3847/1538-4357/adf32d |
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