Comparison between the photometric and kinematic decomposition of the Sombrero-like galaxy in face-on views. The top panels show, from left to right, the relationship between the distributions of f_bulge,p vs. f_bulge and f_disk,p vs. f_disk. The different symbols represent the visual classification of each Sombrero-like galaxy. The bottom panels show the accumulative distribution profiles of their relative differences. The galaxies are color-coded by mass, with red indicating high-mass galaxies and blue indicating low-mass galaxies. The blue solid line represents y=x, while the dashed blue lines represent the ±0.1 deviation range from y=x. Galaxies with a fit stellar halo ellipticity of less than 0.3 are considered thick disks and are highlighted with black rectangles. The galaxies are divided into three mass bins: log(M_★/M_⊙) = 10−10.5 (blue), 10.5−11 (light blue), and 11−11.5 (red). Additionally, instances where f_bulge = 0 suggest that no bulge is sufficiently prominent to be detected by the kinematic decomposition method, as noted by Du et al. (2021). The gap appearing around f_bulge∼0.03 lacks physical significance. Furthermore, the morphological decomposition method inherently identifies any excess luminous structure as a bulge, regardless of whether it exhibits significant rotation or not.