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Table 1

Summary of 2D Gaussian model fitting of the Stokes I in the image plane.

Source Data Peak position [04h19m.., +27◦..] Major axisa(mas) Minor axisa(mas) PAa (deg) Flux (mJy) Peak flux (mJy beam−1) Reference freq. (GHz) Inc.b (deg)
K04166 3 mm ..42s.504, .13′35″.89 729 ± 13 554 ± 13 127 12.50 ± 0.03 10.96 ± 0.02 100.748 41
K04166 1 mm-combine ..42s.509, ..13′35″.84 402.0 ± 5.6 353.0 ± 6.0 119 84.19 ± 0.17 73.27 ± 0.09 231.796 45
K04166 1 mm-high ..42s.509, ..13′35″.84 136.6 ± 0.5 96.0 ± 0.4 125 68.93 ± 0.07 50.76 ± 0.03 225.601 45

K04169 3 mm ..58s.474, ..09′56″.82 Unresolved Unresolved 13.13 ± 0.03 13.15 ± 0.02 100.748
K04169 1 mm-combine ..58s.478, ..09′56″.80 169 ± 11 136 ± 14 128 98.30 ± 0.21 95.97 ± 0.12 231.796 36
K04169 1 mm-high ..58s.477, ..09′56″.83 195.0 ± 0.3 143.0 ± 0.2 139 93.65 ± 0.08 54.132 ± 0.030 225.601 43

Notes. Parameters obtained by minimizing an elliptical Gaussian model to the dust continuum emission maps, using the CASA task imfit. aProjected extent of the deconvolved size on the plane of the sky. bThe inclination angles on the line-of-sight were estimated from the aspect ratio of major axis and minor axis best parameters, by assumption of a circular geometry for the disk. 0 ◦means face-on, whereas 90 ◦means edge-on.

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