Notes. Disk mass and 100 K mass around each object are listed. Previous continuum flux density and single-dish measurements are also shown for comparison. ^(a) Elliptical Gaussian is fit to the visibilities to obtain the continuum flux density, phase center, and deconvolved sizes toward TMC1A, L1527, and Elias 29. The flux densities and continuum sizes of GSS30I1 and GSS30I3 are derived in the image plane by fitting a 2D Gaussian to the intensity profile. We list the 10% flux error except for GSS30I1 where the RMS noise around the target is higher than the 10% flux error. ^(b) Flux density at 1.1 mm taken from Jørgensen et al. (2009) or extrapolated from 1.36 mm from Harsono et al. (2014) and Aso et al. (2017) with a flux density frequency dependence of ν^2.5. ^(c) Peak intensity of the 850 μm SCUBA map within a 15″ beam from Di Francesco et al. (2008). Since GSS30I1 and GSS30I3 are within 3 pixels in the SCUBA map, the same peak value is listed. The peak SCUBA 850 μm intensity toward the phase center of GSS30I1 is 440 mJy beam⁻¹. ^(d) Disk mass (gas and dust) derived from ALMA/NOEMA dust continuum fluxes is an average of the masses obtained from varying the dust opacities calculated at 30 K (see text). The derived disk masses from the power-law disk fit to the visibilities by subtracting the envelope’s component (Power-law disk structure) are shown in the parenthesis with their associated 1σ errors. The inner warm disk mass, >100 K, is based on the power-law disk fit to the continuum visibilities with a temperature power-law index q = 0.4 (Persson et al. 2016, see Appendix B).