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We investigated the origin and gas properties of a simulated galaxy clusterpair, to connect simulation predictions to the SRG/eROSITA X-ray observationsof the Abell 3391/95 field. The simulated system has been extracted from the(352 cMpc/h)^3 volume of the Magneticum Pathfinder cosmological simulations atz=0.07. We tracked back in time the main progenitors of the pair clusters andsurrounding groups to study the assembly history of the system and itsevolution. Similarly to the observed A3391/95 system, the simulated pair isembedded in a complex network of gas filaments, with structures aligned overmore than 20 projected Mpc and the whole region collapsing towards the centraloverdense node. The spheres of influence (3*R200) of the two main clustersalready overlap at z=0.07, but their virial boundaries are still physicallyseparated. The diffuse gas located in the interconnecting bridge closelyreflects the WHIM, with typical temperature of ~1 keV and overdensity $\sim100$, with respect to the mean baryon density of the Universe, and lowerenrichment level compared to the ICM in clusters. We find that most of thebridge gas collapsed from directions roughly orthogonal to the intra-clustergas accretion directions, and its origin is mostly unrelated to the two clusterprogenitors. We find clear signatures in the surrounding groups of infallmotion towards the pair, such as significant radial velocities and slowdown ofgas compared to dark matter. These findings further support the picture of theNorthern Clump (MCXC J0621.7-5242) cluster infalling along a cosmic gasfilament towards Abell 3391, possibly merging with it. We conclude that, insuch a configuration, the pair clusters of the A3391/95-like system are in apre-merger phase, and did not interact yet. The diffuse gas in theinterconnecting bridge is mostly warm filament gas, rather thantidally-stripped cluster gas.

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