Understanding Galaxy Collisions: Simulating the Arrival of a Southern Galaxy Cluster

Exploring the Dynamics and Interactions of Galaxy Clusters Abell 1758N and Abell 1758S

As a dissociative merging cluster, A1758S needs to be taken into account in new simulations. A tangential approach is the most compatible with the observed configuration, while a radial approach is also marginally compatible.

This research was conducted by Rubens E. G. Machado, Ricardo C. Volert, Richards P. Albuquerque from the Departamento Acadêmico de Física, Universidade Tecnológica Federal do Paraná, Curitiba, Brazil; Rogério Monteiro-Oliveira from the Institute of Astronomy and Astrophysics, Academia Sinica, Taipei, Taiwan; and Gastão B. Lima Neto from the Instituto de Astronomia, Geofísica e Ciências Atmosféricas, Universidade de São Paulo, São Paulo, Brazil.

Read more here: https://arxiv.org/pdf/2405.20497

In merging galaxy clusters, the gas between the two clusters compresses, increasing the X-ray emission in the region. Examples of bridges or filaments detected in X-rays between clusters include A3391 and A3395, A222 and A223, and A3556 and A3558.

As giant radio relics, Abell 399/401 and Abell 1758N/1758S are two pairs of pre-merging clusters with extended diffuse emission. In the low-density regions between the clusters, compression and turbulence are thought to cause these radio bridges.