Comparison of observed (left) and modeled (right) morphology of spectral line emission from C¹⁷O, H₂CO, and H¹³CN. In the C¹⁷O model panel, the disk domains are masked (as in Fig. 2). Total intensity from the observed cubes is calculated by integrating over V_lsr range [ + 2, + 4] km s⁻¹. The continuum peak locations are marked by star symbols, the ALMA interferometric beam size is indicated in the bottom left of each “observed” panel. The modeled line intensity maps are convolved with the observational beam size, to aid direct comparison. Line intensity is represented by the color scale and gray contours (identical for observed and modeled panels: lowest level at 0.15 for C¹⁷O, 0.10 Jy beam⁻¹ km s⁻¹ for H₂CO and H¹³CN, and increasing by a factor of 2 each level). Black contours indicate the 0.87 mm dust continuum.