Left: averaged H I mass at different radii for the low-mass bin (blue), medium-mass bin (green), and high-mass bin (red). The shaded regions represent the uncertainties of the stacking results. We use shaded regions with hatching for the low-mass bins to emphasize the stellar mass incompleteness (Figure 2). The vertical dashed line shows the splashback radius of clusters at ∼1.5 R₂₀₀ (T. Shin et al. 2019). Right: averaged H I mass fraction as a function of radius and stellar mass bins. The dashed lines show the M_HI/M_* ratios for low- (blue), intermediate- (green), and high-stellar-mass (red) bins from H. Guo et al. (2021), which are the stacking results from ALFALFA. The values of M_HI/M_* are taken at the average stellar masses of the three bins, ﹩\mathrm{log}({M}_{* }/{M}_{\odot })=9.2﹩, 10.0, and 11.2, and are treated as representative of field galaxies. The M_HI/M_* ratios in our sample are lower than those of field galaxies even at 5R₂₀₀, implying that a similar preprocessing effect may occur in the cluster outskirts.