학술논문
The eROSITA view of the Abell 3391/95 field: Cluster Outskirts and Filaments
Document Type
Working Paper
Author
Veronica, Angie; Reiprich, Thomas H.; Pacaud, Florian; Ota, Naomi; Aschersleben, Jann; Biffi, Veronica; Bulbul, Esra; Clerc, Nicolas; Dolag, Klaus; Erben, Thomas; Gatuzz, Efrain; Ghirardini, Vittorio; Kerp, Jürgen; Klein, Matthias; Liu, Ang; Liu, Teng; Migkas, Konstantinos; Ramos-Ceja, Miriam E.; Sanders, Jeremy; Spinelli, Claudia
Source
Subject
Language
Abstract
Aims. We aim to characterize the gas properties in the cluster outskirts ($R_{500}R_{200}$) of the A3391/95 system and to compare them to predictions. Methods. We performed X-ray image and spectral analyses using the eROSITA PV data to assess the gas morphology and properties in the outskirts and the filaments in the directions of the previously detected Northern and Southern Filament of the A3391/95 system. We took particular care of the foreground. Results. In the filament-facing outskirts of A3391 and the Northern Clump, we find higher temperatures than typical cluster outskirts profiles, with a significance of $1.6-2.8\sigma$, suggesting heating due to their connections with the filaments. We confirm SB excess in the profiles of the Northern, Eastern, and Southern Filaments. From spectral analysis, we detect hot gas of ~1 keV for the Northern and Southern Filaments. The filament metallicities are below 10% solar metallicity and the $n_e$ range between 2.6 and $6.3\times10^{-5}~\mathrm{cm^{-3}}$. The characteristic properties of the Little Southern Clump (~1.5$R_{200}$ from A3395S in the Southern Filament) suggest that it is a small galaxy group. Excluding the LSC from the analysis of the Southern Filament decreases the gas density by 30%. This shows the importance of taking into account any clumps to avoid overestimation of the gas measurement in the outskirts and filament regions. Conclusions. The $n_e$ of the filaments are consistent with the WHIM properties as predicted by cosmological simulations, but the temperatures are higher, close to the upper WHIM temperature limit. As both filaments are short and located in a denser environment, stronger gravitational heating may be responsible for this temperature enhancement. The metallicities are low, but still within the expected range from the simulations.
Comment: Accepted for publication in Astronomy & Astrophysics: 17 pages, 6 figures (main text), 1 figure (appendix)
Comment: Accepted for publication in Astronomy & Astrophysics: 17 pages, 6 figures (main text), 1 figure (appendix)