2022A&A...661A..17B


Query : 2022A&A...661A..17B

2022A&A...661A..17B - Astronomy and Astrophysics, volume 661A, 17-17 (2022/5-1)

The eROSITA view of the Abell 3391/95 field: Case study from the Magneticum cosmological simulation.

BIFFI V., DOLAG K., REIPRICH T.H., VERONICA A., RAMOS-CEJA M.E., BULBUL E., OTA N. and GHIRARDINI V.

Abstract (from CDS):


Context. Clusters of galaxies reside at the nodes of the cosmic web, interconnected by filamentary structures that contain tenuous diffuse gas, especially in the warm-hot phase. Galaxy clusters grow by mergers of smaller objects and gas that are mainly accreted through these large-scale filaments. For the first time, the large-scale cosmic structure and a long gas-emission filament have been captured by eROSITA on board the Spectrum-Roentgen-Gamma mission in a direct X-ray observation of the A3391/95 field.
Aims. We investigate the assembly history of an A3391/95-like system of clusters and the thermo-chemical properties of the diffuse gas in it by connecting simulation predictions to the eROSITA observations with the aim to constrain the origin and nature of the gas in the pair-interconnecting bridge.
Methods. We analysed the properties of a system resembling A3391/95, extracted from the (352 h–1 cMpc)3 volume of the Magneticum Pathfinder cosmological simulations at z = 0.07. We tracked the main progenitors of the pair clusters and of surrounding groups back in time to study the assembly history of the system and its evolution.
Results. Similarly to the observed A3391/95 system, the simulated cluster pair is embedded in a complex network of gas filaments, with structures aligned over more than 20 projected Mpc, and the whole region collapses towards the central overdense node. The spheres of influence (3 x R200) of the two main clusters already overlap at z = 0.07, but their virial boundaries are still physically separated. The diffuse gas located in the interconnecting bridge closely reflects the warm-hot intergalactic medium, with a typical temperature of ∼1 keV and an overdensity δ ∼ 100 with respect to the mean baryon density of the Universe, and a lower enrichment level compared to the intra-cluster medium in clusters. We find that most of the bridge gas collapsed from directions roughly orthogonal to the intra-cluster gas accretion directions, and its origin is mostly unrelated to the two cluster progenitors. We find clear signatures in the surrounding groups of infall motion towards the pair, such as significant radial velocities and a slowdown of gas compared to dark matter. These findings further support the hypothesis that the Northern Clump (MCXC J0621.7-5242) cluster infalls along a cosmic gas filament towards Abell 3391 and might be merging with it.
Conclusions. We conclude that in this configuration, the pair clusters of the A3391/95-like system are in a pre-merger phase and have not yet interacted. The diffuse gas in the interconnecting bridge is mostly warm filament gas and not tidally stripped cluster gas.

Abstract Copyright: © ESO 2022

Journal keyword(s): galaxies: clusters: general - galaxies: clusters: intracluster medium - methods: numerical - X-rays: galaxies: clusters

Simbad objects: 14

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Number of rows : 14
N Identifier Otype ICRS (J2000)
RA
ICRS (J2000)
DEC
Mag U Mag B Mag V Mag R Mag I Sp type #ref
1850 - 2022
#notes
1 ACO 222 ClG 01 37 27.4 -12 58 45           ~ 131 1
2 ACO 223 ClG 01 37 55.9 -12 49 11           ~ 117 1
3 ACO 399 ClG 02 57 56.4 +13 00 59           ~ 373 0
4 ACO 401 ClG 02 58 56.9 +13 34 56           ~ 540 0
5 RXC J0621.7-5242 ClG 06 21 42.0 -52 41 36           ~ 8 0
6 ESO 161-6 IG 06 26 05.3 -54 02 03           ~ 8 0
7 ACO 3391 ClG 06 26 15.4 -53 40 52           ~ 185 1
8 ACO 3395 ClG 06 27 31.1 -54 23 58           ~ 193 0
9 NAME SHAPLEY-CENTAURUS CL SCG 13 06.0 -33 04           ~ 556 0
10 ACO 3556 ClG 13 24 06.2 -31 39 38           ~ 146 0
11 ACO 3558 ClG 13 27 54.8 -31 29 32           ~ 421 2
12 ACO 1758 ClG 13 32 32.1 +50 30 37           ~ 238 2
13 NPM1G +30.0453 ClG 18 24 09.6 +30 29 31           ~ 14 0
14 2MAXI J1825+306 ClG 18 25 22.8 +30 26 32           ~ 37 0

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2022.08.09-16:38:40

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