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arXiv · 2601.06011

Simulations of collision and sloshing in the galaxy group NGC 5098/5096

Richards P. Albuquerque·Gastão B. Lima Neto·Rubens E. G. Machado·Hugo V. Capelato·Florence Durret
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Abstract

The study of galaxy groups is essential to understanding the evolutionary history of large-scale structures in the Universe. These dense environments have a significant impact on galaxy evolution, influencing their gas content, morphology, and star formation activity. In this work we analyse in detail the system NGC~5098$/$5096 composed of two galaxy groups. We performed hydrodynamical $N$-body simulations of a galaxy group collision aimed at reproducing the gas sloshing and surface brightness distribution observed in X-ray data. We conducted a detailed X-ray analysis and generated mock image \textit{Chandra} observations from our simulations. The resulting corrected mock image surface brightness profiles show good agreement with the observed data. The relative line-of-sight velocity between NGC~5098 and NGC~5096 is $v_{\mathrm{los}} = 700$ km s$^{-1}$, with a projected separation of $d_{\mathrm{proj}} = 155$ kpc, suggesting that the collision occurs nearly in the line-of-sight. Our simulations were performed with an inclination angle of $80^\circ$ in order to reproduce the dynamical constraints. We also find a correlation between the dark matter and intragroup light distributions when comparing the residual dark matter map with the intragroup light morphology. Our best-fitting model is consistent with these observational constraints and provides a plausible dynamical scenario for the current state of the NGC~5098 group interaction with NGC 5096.

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Richards P. Albuquerque, Gastão B. Lima Neto, Rubens E. G. Machado, Hugo V. Capelato, Florence Durret. 2026-01-09. Simulations of collision and sloshing in the galaxy group NGC 5098/5096. https://arxiv.org/abs/2601.06011

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