The eROSITA view of the Abell 3391/95 field: The Northern Clump. The largest infalling structure in the longest known gas filament observed with eROSITA, XMM-Newton, and Chandra

Angie Veronica; Yuanyuan Su; Veronica Biffi; Thomas H. Reiprich; Florian Pacaud; Paul E. J. Nulsen; Ralph P. Kraft; Jeremy S. Sanders; Akos Bogdan; Melih Kara; Klaus Dolag; Jürgen Kerp; Bärbel S. Koribalski; Thomas Erben; Esra Bulbul; Efrain Gatuzz; Vittorio Ghirardini; Andrew M. Hopkins; Ang Liu; Konstantinos Migkas; Tessa Vernstrom

doi:10.1051/0004-6361/202141415

paper

The eROSITA view of the Abell 3391/95 field: The Northern Clump. The largest infalling structure in the longest known gas filament observed with eROSITA, XMM-Newton, and Chandra

arXiv:2106.14543 · doi:10.1051/0004-6361/202141415

Abstract

SRG/eROSITA PV observations revealed the A3391/95 cluster system and the Northern Clump (MCXC J0621.7-5242 galaxy cluster) are aligning along a cosmic filament in soft X-rays, similarly to what has been seen in simulations before. We aim to understand the dynamical state of the Northern Clump as it enters the atmosphere ( $3 \times R_{200}$ ) of A3391. We analyzed joint eROSITA, XMM-Newton, and Chandra observations to probe the morphological, thermal, and chemical properties of the Northern Clump from its center out to a radius of 988 kpc ( $R_{200}$ ). We utilized the ASKAP/EMU radio data, DECam optical image, and Planck y-map to study the influence of the WAT radio source on the Northern Clump central ICM. From the Magneticum simulation, we identified an analog of the A3391/95 system along with an infalling group resembling the Northern Clump. The Northern Clump is a WCC cluster centered on a WAT radio galaxy. The gas temperature over $0.2 - 0.5 R_{500}$ is $k_{B} T_{500} = 1.99 \pm 0.04$ keV. We employed the $M - T$ scaling relation and obtained a mass estimate of $M_{500} = (7.68 \pm 0.43) \times 1 0^{13} M_{⊙}$ and $R_{500} = (636 \pm 12)$ kpc. Its atmosphere has a boxy shape and deviates from spherical symmetry. We identify a southern surface brightness edge, likely caused by subsonic motion relative to the filament gas. At $\sim R_{500}$ , the southern atmosphere appears to be 42% hotter than its northern atmosphere. We detect a downstream tail pointing toward the north with a projected length of $\sim 318$ kpc, plausibly the result of ram pressure stripping. The analog group in the Magneticum simulation is experiencing changes in its gas properties and a shift between the position of the halo center and that of the bound gas while approaching the main cluster pair.

arXiv comment24 pages, 17 figures (main text), 6 figures (appendix). Submitted to A&A for the Special Issue: The Early Data Release of eROSITA and Mikhail Pavlinsky ART-XC on the SRG Mission. For more information, see https://astro.uni-bonn.de/~averonica/NorthernClump/eROSITA_A3391_Northern_Clump_AIfA.html

The eROSITA view of the Abell 3391/95 field: The Northern Clump. The largest infalling structure in the longest known gas filament observed with eROSITA, XMM-Newton, and Chandra

Abstract

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