Baryon fraction as a function of M_* given on the left. The baryon fraction is the sum of the stellar and the hot CGM within R_vir divided by the virial mass (f_{b, hot CGM + star, < Rvir} = (M_{hot CGM, < Rvir} + M_*)/M_vir). We assume that the metallicity abundance of the hot CGM is 0.1 Z_⊙, 0.3 Z_⊙ and Z_⊙, and the temperature of the hot CGM is at virial temperature (T_vir) or half (0.5T_vir). The baryon fractions predicted with different metallicity abundances and temperatures are summarised in purple square. The dashed line (f_b = 0.16) is the cosmological baryon fraction (Planck Collaboration VI 2020). The gray points are taken from tSZ measurements (Bregman et al. 2022; Das et al. 2023), and X-ray measurements (Li et al. 2018; Das et al. 2020; Nicastro et al. 2023). Right panel shows the baryon fraction as a function of M_500c under assumptions of metallicity abundances and temperatures. The baryon fraction is the hot CGM within R_500c divided by the M_500c (f_{b, hot CGM, < R500c} = (M_{hot CGM, < R500c})/M_500c).The gray points are gas fractions estimated from detected clusters and groups in X-ray (Sun et al. 2009; Sanderson et al. 2013; Lovisari et al. 2015; Eckert et al. 2016; Nugent et al. 2020; Akino et al. 2022).