Infalling particles form a sharp physical boundary around their first apocenters around the parent halo, which is called "splashback radius". The previous measurements of splashback radius using optical clusters reported a ~20% discrepancy against the theory prediction. Here, using galaxy clusters detected by SZ surveys (ACT, SPT), we present the detection of the splashback radius and its consistency with respect to N-body simulations, by cross-correlating the galaxy clusters to the DES galaxies. On the other hand, it is known that the infalling galaxies around galaxy clusters experience enhanced star formation quenching. Using galaxy samples split on their colors, we also present the possibility of constraining the quenching parameters in quenching models we adopt (e.g. quenching timescale), making use of N-body simulations.
Speaker: Tae-Hyeon Shin, Pennsylvania State
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