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Fig. 6

image

Disk mass, derived from (sub)-mm fluxes, in units of solar masses (top panel) and stellar mass (bottom panel) as a function of the mass of the parent body for all targets in this paper. Binaries are highlighted with diamonds. A conservative estimate of disk mass uncertainty arising from unknown individual distances is shown in the bottom left of the top panel, assuming a conservative Δdist = ±10% (cf. Torres et al. 2007, who estimate a “depth” of Taurus of 20 pc). Dotted lines show the typical sensitivity limits derived from Eq. (3) for targets in Taurus (F1300,lim ≈ 1 mJy, dist = 140 pc) and TW Hya (F1300,lim ≈ 0.05 mJy, dist = 50 pc), using BCAH98 isochrones to convert mass to luminosity.

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