Left: beam-averaged water (HO) column densities within 50 AU radius as a function of accretion rates. The different colors indicate the disk mass dependence for R_disk = 200 AU models: M_d = 0.05 M_⊙ (red triangles), 0.2 (blue circles), and 0.5 (green squares). The different lines show the luminosity dependence: L_⋆ = 1 L_⊙ (solid) and 5 L_⊙ (dashed). Center: integrated line flux densities arising from the disk as defined by the yellow line in Fig. 7. The observed integrated HO line is indicated by the gray lines for the three different embedded YSOs in Persson et al. (2014). Right: integrated line flux densities accounting for the entire water vapor mass assuming a Gaussian line width of 1 km s^-1, which is appropriate for NGC 1333-IRAS 4B.