Abstract
Abstract Low-mass galaxy cluster systems and groups will play an essential role in upcoming cosmological studies, such as those to be carried out with eROSITA. Though the effects of active galactic nuclei (AGNs) and merging processes are of special importance to quantify biases like selection effects or deviations from hydrostatic equilibrium, they are poorly understood on the galaxy-group scale. We present an analysis of recent deep Chandra and XMM-Newton integrations of NGC 741 that provides an excellent example of a group with multiple concurrent phenomena: both an old central radio galaxy and a spectacular infalling head-tail source, strongly bent jets, a 100-kpc radio trail, intriguing narrow X-ray filaments, and gas-sloshing features. Supported principally by X-ray and radio continuum data, we address the merging history of the group, the nature of the X-ray filaments, the extent of gas-stripping from NGC 742, the character of cavities in the group, and the roles of the central AGN and infalling galaxy in heating the intra-group medium.
Highlights
Galaxy clusters, as the most massive gravitationally relaxed systems in the Universe, are excellent tools to study cosmology, especially the phenomena of dark matter and dark energy
Low-mass objects like galaxy groups are ideal for tracing baryons, since about 50% of galaxies reside in galaxy groups, while galaxy clusters host only a few percent (Eke et al 1998)
In the hierarchical formation process, high mass galaxy clusters are the final stage of evolution, while galaxy groups are the predominant site of merging processes
Summary
As the most massive gravitationally relaxed systems in the Universe, are excellent tools to study cosmology, especially the phenomena of dark matter and dark energy. X-ray emission from the hot intracluster medium (ICM) traces the most massive visible component of clusters and enables derivation of both the total gravitational mass and that of the radiating baryonic component. A deep understanding of the evolution of the baryon distribution in the Universe is essential for modeling the structure formation process, especially for low-mass objects where non-gravitational effects become progressively more dominant. Low-mass objects like galaxy groups are ideal for tracing baryons, since about 50% of galaxies reside in galaxy groups, while galaxy clusters host only a few percent (Eke et al 1998). Extended emission observed in galaxy groups can be approximated as a scaled-down version of typical cluster emission, the gas properties in groups show differences in both the scaling relations (Eckmiller et al 2011; Lovisari et al 2015) and AGN feedback properties (Sun et al 2009; Bharadwaj et al 2014); these differences contribute to the justification of the study of groups independently of clusters
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