Title: Intracluster light at z~0.5: the MUSE and CFHT view

Abstract:
Within a cluster, gravitational effects can lead to the removal of stars from their parent galaxies 
into the intracluster medium. Gas dynamical effects can additionally strip gas and dust from 
galaxies; both gas and stars contribute to a diffuse emission called the intracluster light 
(herefater ICL). 
The properties of the ICL can therefore constrain the types and frequency of the physical 
processes at work in clusters by serving as a fossil record of the interaction history of the 
cluster.
Through CFHT and MUSE observations, an extraordinary amount of ICL, equivalent to the 
emission from two dominant galaxies, has been detected in this cluster; furthermore emission 
lines were detected in the several diffuse light sources. This emission is likely originating from 
gas similar to what can be found in low excitation parameter objects. The ICL star population is 
of the order of 2.3×10^9 yrs old but is not actively forming stars; on the other hand, the gas is 
dominating the star contribution in the ICL. This speaks in favor of ram pressure stripping, 
turbulent viscous stripping, or supernovae winds to generate the large amount of intracluster 
light.
Since n0308 is not currently undergoing a major merger, we conclude that ram pressure 
stripping is the most plausible process to generate ICL tails similar to what we see in our data.