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Fig. 4.

image

Panel a: 1.14 mm flux (scaled to a distance of 140 pc) as a function of the radius for all disks detected in GGD 27 (black squares and triangles), Taurus-Auriga (red circles; Guilloteau et al. 2011; Piétu et al. 2014), Ophiuchus (gray circles; Cieza et al. 2019), and ONC (yellow squares; Eisner et al. 2018). The flux at 1.14 mm was extrapolated from the measurements at 1.3 mm for Taurus and Ophiuchus disks and from 850 μm for ONC disks using an spectral index of α = 3. The dotted line depicts the average mass sensitivity limit (8σ). We show, at the top, the median and its dispersion (1st and 3rd quartiles) for GGD 27 (black), Taurus (red), Ophiuchus (gray), and ONC (yellow) samples. The most massive disks MM1 and MM2(E) were removed from the plot. Panel b: disk masses in GGD 27 (black squares) and ONC (red circles) clusters as a function of their projected distance from the massive star IRAS 18162−2048 and θ1 Ori C (Mann et al. 2014), respectively. The dotted line depicts the average mass sensitivity limit while the dashed line indicates the higher 8σ limit close to MM1. Panel c: disk radii in GGD 27 as a function of their projected distance from the massive star. In all panels upper limits in Rdisk are indicated with triangles.

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