| Online-Ressource |
Verfasst von: | Rohr, Eric [VerfasserIn]  |
| Pillepich, Annalisa [VerfasserIn]  |
| Nelson, Dylan [VerfasserIn]  |
| Ayromlou, Mohammadreza [VerfasserIn]  |
| Zinger, Elad [VerfasserIn]  |
Titel: | The hot circumgalactic media of massive cluster satellites in the TNG-Cluster simulation |
Titelzusatz: | existence and detectability |
Verf.angabe: | Eric Rohr, Annalisa Pillepich, Dylan Nelson, Mohammadreza Ayromlou, and Elad Zinger |
E-Jahr: | 2024 |
Jahr: | June 2024 |
Umfang: | 19 S. |
Illustrationen: | Illustrationen |
Fussnoten: | Online veröffentlicht: 31. Mai 2024 ; Gesehen am 27.01.2025 |
Titel Quelle: | Enthalten in: Astronomy and astrophysics |
Ort Quelle: | Les Ulis : EDP Sciences, 1969 |
Jahr Quelle: | 2024 |
Band/Heft Quelle: | 686(2024) vom: Juni, Artikel-ID A86, Seite 1-19 |
ISSN Quelle: | 1432-0746 |
Abstract: | The most massive galaxy clusters in the Universe host tens to hundreds of massive satellite galaxies M⋆ ∼ 1010 − 12.5 M⊙, but it is unclear if these satellites are able to retain their own gaseous atmospheres. We analyze the evolution of ≈90 000 satellites of stellar mass ∼109 − 12.5 M⊙ around 352 galaxy clusters of mass M200c ∼ 1014.3 − 15.4 M⊙ at z = 0 from the new TNG-Cluster suite of cosmological magneto-hydrodynamical galaxy cluster simulations. The number of massive satellites per host increases with host mass, and the mass–richness relation broadly agrees with observations. A halo of mass M200chost ∼ 1014.5(1015) M⊙ hosts ∼100 (300) satellites today. Only a minority of satellites retain some gas, hot or cold, and this fraction increases with stellar mass. lower-mass satellites ∼109 − 10 M⊙ are more likely to retain part of their cold interstellar medium, consistent with ram pressure preferentially removing hot extended gas first. At higher stellar masses ∼1010.5 − 12.5 M⊙, the fraction of gas-rich satellites increases to unity, and nearly all satellites retain a sizeable portion of their hot, spatially extended circumgalactic medium (CGM), despite the ejective activity of their supermassive black holes. According to TNG-Cluster, the CGM of these gaseous satellites can be seen in soft X-ray emission (0.5−2.0 keV) that is, ≳10 times brighter than the local background. This X-ray surface brightness excess around satellites extends to ≈30 − 100 kpc, and is strongest for galaxies with higher stellar masses and larger host-centric distances. Approximately 10% of the soft X-ray emission in cluster outskirts ≈0.75 − 1.5 R200c originates from satellites. The CGM of member galaxies reflects the dynamics of cluster-satellite interactions and contributes to the observationally inferred properties of the intracluster medium. |
DOI: | doi:10.1051/0004-6361/202348583 |
URL: | Bitte beachten Sie: Dies ist ein Bibliographieeintrag. Ein Volltextzugriff für Mitglieder der Universität besteht hier nur, falls für die entsprechende Zeitschrift/den entsprechenden Sammelband ein Abonnement besteht oder es sich um einen OpenAccess-Titel handelt.
kostenfrei: Volltext: https://doi.org/10.1051/0004-6361/202348583 |
| kostenfrei: Volltext: https://www.aanda.org/articles/aa/abs/2024/06/aa48583-23/aa48583-23.html |
| DOI: https://doi.org/10.1051/0004-6361/202348583 |
Datenträger: | Online-Ressource |
Sprache: | eng |
K10plus-PPN: | 1915641500 |
Verknüpfungen: | → Zeitschrift |
¬The¬ hot circumgalactic media of massive cluster satellites in the TNG-Cluster simulation / Rohr, Eric [VerfasserIn]; June 2024 (Online-Ressource)