Speaker
Description
The splashback radius is a physically motivated boundary of galaxy clusters, offering a unique window into the cluster's mass accretion rate and the interplay between dark matter and baryonic processes. Consequently, accurate measurements of the splashback radius are crucial for testing cosmological models and advancing our understanding of structure formation. With the advent of large-scale surveys like Euclid and LSST, there is a growing need to develop robust and innovative methods to measure the splashback radius, as these data sets will offer unprecedented precision and depth.
In this presentation, I will provide an overview of our analyses based on galaxy clusters detected in the Kilo Degree Survey (KiDS) using the AMICO (Adaptive Matched Identifier of Clustered Objects) cluster finder. First, I will discuss the splashback radius constraints obtained from stacked cluster weak-lensing measurements based on KiDS-DR3 data, covering an effective area of 377 square degrees and extending up to redshift z = 0.6. Then, I will delve into the weak-lensing mass calibration of AMICO KiDS-1000 clusters, covering more than double the area of KiDS-DR3 and extending up to z = 0.8. Using this data set, we determine the splashback radius through both weak-lensing profiles and cluster-galaxy projected correlation function. We propose an innovative method for measuring the cluster-galaxy correlation function and modelling the profiles, incorporating corrections for photometric selection effects.
