Vertical distributions coupled with their best-fit models of the star samples in different radial action ranges in the outer disk (R_g >  8 kpc), as done in Fig. 4. It should be noted that we increase the size of radial action ranges in the last two lower panels, as the number of stars is relatively small in the outer disk, and the thick disk gives a relatively poor fit in the lower-right panel due to the insufficient number of stars in this radial action range.