Two merging galaxy clusters with very hot shock fronts observed shortly before pericentric passage
| Autor: | Tatiana F. Laganá, Rubens E. G. Machado, G. S. Souza, R. C. Volert, Paulo A. A. Lopes |
|---|---|
| Rok vydání: | 2019 |
| Předmět: |
Cosmology and Nongalactic Astrophysics (astro-ph.CO)
media_common.quotation_subject FOS: Physical sciences Astrophysics::Cosmology and Extragalactic Astrophysics Astrophysics 01 natural sciences symbols.namesake Intracluster medium 0103 physical sciences Cluster (physics) 010303 astronomy & astrophysics Astrophysics::Galaxy Astrophysics Galaxy cluster media_common Physics Shock (fluid dynamics) 010308 nuclear & particles physics Plane (geometry) Astronomy and Astrophysics Astrophysics - Astrophysics of Galaxies Orbit Mach number Space and Planetary Science Sky Astrophysics of Galaxies (astro-ph.GA) symbols Astrophysics - Cosmology and Nongalactic Astrophysics |
| Zdroj: | Monthly Notices of the Royal Astronomical Society. 487:3922-3934 |
| ISSN: | 1365-2966 0035-8711 |
| Popis: | We present a detailed analysis of two merging clusters, from XMM-\textit{Newton} X-ray archival data: PLCKESZ G036.7+14.9 ($z=0.15$; hereafter G036) and PLCK G292.5+22.0 ($z=0.30$; hereafter G292). We notice that the intracluster medium is heated as a result of the merger, and we find evidence for a merger shock in the region between both subcluster haloes. X-ray observations confirm that the shocks in these systems are among the hottest known in the literature. From the ICM analysis of temperature discontinuity, the Mach numbers were determined to be $M_{\rm G036}=1.3$ and $M_{\rm G292}=1.5$ for G036 and G292, respectively. In this paper, for each cluster, we propose a hydrodynamic model for the merger as a whole, compatible with their diffuse X-ray emission and temperature maps. The simulations suggest that both clusters are observed shortly before pericentric passage. Our simulation results indicate that the merger of the G036 system is seen at an inclination of 50$^{\circ}$ (the angle between the plane of the orbit and the plane of the sky), and merely 50 Myr prior to the pericentric passage. In the case of G292, the subclusters would be merging not far from the plane of the sky ($i=18^{\circ}$) and are observed 150\,Myr before the two cores collide. 13 pages, 11 figures, aceppted for publication in MNRAS |
| Databáze: | OpenAIRE |
| Externí odkaz: |
|