The BIG X-ray tail
Chong Ge, Ming Sun, Masafumi Yagi, Matteo Fossati, William Forman,, Pavel J\'achym, Eugene Churazov, Irina Zhuravleva, Alessandro Boselli,, Christine Jones, Li Ji, and Rongxin Luo

TL;DR
This paper reports the discovery of a 250 kpc X-ray tail behind the Blue Infalling Group (BIG) in cluster A1367, revealing insights into galaxy preprocessing and the multiphase nature of stripped gas in cluster environments.
Contribution
The study presents the first detection of a large X-ray tail associated with the BIG, highlighting the multiphase gas and suppressed instabilities that allow long-lived stripped ISM in galaxy clusters.
Findings
The X-ray tail contains about 7×10^10 solar masses of hot gas.
The tail's temperature is approximately 1 keV with low apparent metallicity.
Surface brightness correlations suggest mixing of ISM and ICM in the tail.
Abstract
Galaxy clusters grow primarily through the continuous accretion of group-scale haloes. Group galaxies experience preprocessing during their journey into clusters. A star-bursting compact group, the Blue Infalling Group (BIG), is plunging into the nearby cluster A1367. Previous optical observations reveal rich tidal features in the BIG members, and a long H trail behind. Here we report the discovery of a projected kpc X-ray tail behind the BIG using Chandra and XMM-Newton observations. The total hot gas mass in the tail is with an X-ray bolometric luminosity of erg s. The temperature along the tail is keV, but the apparent metallicity is very low, an indication of the multi- nature of the gas. The X-ray and H surface brightnesses in the front part of the BIG tail follow the tight…
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