Speaker
Description
I will present a comprehensive analysis of weak gravitational lensing data to assess mass biases in galaxy clusters and characterize their splashback radius, with implications for precision cluster cosmology.
Systematic assessments using state-of-the-art hydrodynamical simulations reveal that weak lensing mass biases depend on cluster mass, redshift, and orientation, with biases as high as 30% for specific projections but reducing to <10% through stacking.
I will discuss that the mass bias decreases for clusters more massive than 1015𝑀sun, with relaxed systems being less biased than unrelaxed ones. In refining the richness-mass relation, I will show that the zero-point parameter is redshift-independent but sensitive to the stellar mass threshold, with the slope evolving quadratically -- relatively constant up to z=0.55 -- and scatter increasing linearly with redshift. By modeling the projected matter density profiles, I will illustrate that splashback radius marking sharp transitions in cluster profile slopes, align closely with theoretical predictions but suggest a bias in optically selected clusters. These findings will provide a framework for improving mass-observable relations, essential for achieving the percent-level accuracy required in upcoming wide-field surveys.
