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Galaxy cluster abundance is one of the pillars of modern cosmology, with weak-lensing the gold standard for cluster mass calibration. Despite this achievement in modern cosmology, uncertainties and systematics in cluster observables hamper this probe in cosmological studies. We provide for the first time a model for the intrinsic correlated scatter between weak lensing signal and cluster richness and find a negative correlation between lensing signal and galaxy number count at small scales. We find that the size of the covariance can be explained by the halo formation history. Furthermore, by modeling the cluster richness and weak lensing as multi-(log)-linear equations of secondary halo properties, we provide a quantitative explanation for the physical origin of the negative covariance at small scales. These findings highlight the importance of accounting for the covariance between observables in cluster mass estimation, which is crucial for obtaining accurate constraints on cosmological parameters.
I am a PhD student at the Astronomy & Astrophysics Department at the University of Chicago. I am interested in constraining cluster mass estimates to a precision of 1% in the near future to advance cluster cosmology into a state of the art probe. My current work involves the statistical modeling of cluster observables selected in the weak lensing regime as well as modeling the property covariance of multi-phase profiles of clusters in the multiwavelength regime. In the near future, I am particularly interested in exploring the effects that different galaxy-halo connection models and the correlated scatter of cluster optical and multiwavelength properties have on cluster mass estimation.
Combined video record by Yiwei Bao & Zhuowen Zhang & Haopeng Zhang & Haojie Hu:
https://vshare.sjtu.edu.cn/open/b756cc92a402676e9b6aa4de41c9f9a0a386bd58ef030570b1d75a2a0150ee77