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Table 3:

Disk properties.

Object name
$R_{\rm {out}}$ (AW07) $R_{\rm {out}}$-interval $\alpha $ $\beta $ $M_{\rm {dust}}\times\kappa_{\rm {1~mm}}$ $M_{\rm {dust}}^{q=2.5}$ $M_{\rm {dust}}^{q=3}$ $M_{\rm {dust}}^{q=3.5}$
  (AU) (AU)     ( $M_{\odot} \times$ cm2 g-1) ($M_\odot$) ($M_\odot$) ($M_\odot$)
(1) (2) (3) (4) (5) (6) (7) (8) (9)

SR 4
... 100-300 2.5 0.7 $1.3\times10^{-4}$ $2.1\times10^{-5}$ $2.4\times10^{-5}$ ...
GSS 26 ... 100-300 1.9 0.0 $3.5\times10^{-4}$ $2.3\times10^{-3}$ ... ...
EL 20 ... 100-300 2.5 0.8 $3.2\times10^{-4}$ $4.3\times10^{-5}$ $4.5\times10^{-5}$ $1.9\times10^{-4}$
DoAr 25 200 100-300 2.3 0.5 $8.0\times10^{-4}$ $1.8\times10^{-4}$ $2.6\times10^{-4}$ ...
EL 24 175 75-275 2.2 0.4 $9.9\times10^{-4}$ $2.9\times10^{-4}$ $6.3\times10^{-4}$ ...
EL 27 275 175-375 2.2 0.5 $1.5\times10^{-3}$ $3.5\times10^{-4}$ $5.6\times10^{-4}$ ...
SR 21 600 500-700 2.9 1.1 $5.3\times10^{-4}$ $4.9\times10^{-5}$ $4.5\times10^{-5}$ $ 5.5\times10^{-5}$
IRS 41 ... 100-300 2.1 0.3 $1.3\times10^{-4}$ $6.6\times10^{-5}$ $6.8\times10^{-4}$ ...
YLW 16c ... 100-300 2.4 0.0 $2.3\times10^{-4}$ $4.3\times10^{-5}$ $5.6\times10^{-5}$ ...
IRS 49 ... 100-300 1.8 0.0 $3.9\times10^{-5}$ $2.2\times10^{-3}$ ... ...
DoAr 33 ... 100-300 2.2 0.4 $1.2\times10^{-4}$ $3.4\times10^{-5}$ $9.9\times10^{-5}$ ...
WSB 52 ... 100-300 1.8 0.0 $1.4\times10^{-5}$ $2.6\times10^{-3}$ ... ...
WSB 60 350 250-450 1.9 0.3 $5.6\times10^{-4}$ $2.9\times10^{-4}$ $3.0\times10^{-3}$ ...
DoAr 44 ... 100-300 2.2 0.4 $3.0\times10^{-4}$ $8.8\times10^{-5}$ $1.9\times10^{-4}$ ...
RNO 90 ... 100-300 2.3 0.4 $1.1\times10^{-4}$ $3.1\times10^{-5}$ $7.1\times10^{-5}$ ...
Wa Oph 6 275 175-375 2.4 0.7 $4.9\times10^{-4}$ $8.0\times10^{-5}$ $9.8\times10^{-5}$ ...
AS 209 200 100-300 2.4 0.7 $7.9\times10^{-4}$ $1.2\times10^{-4}$ $1.4\times10^{-4}$ ...

Notes. (1) Underlined objects are those which have not been mapped to date through high-angular resolution imaging. The objects which have been mapped but do not have an estimate for the outer disk radius as reported in Col. (2) have been spatially resolve by Andrews et al. (2009). Contrary to Andrews & Williams (2007a), they modeled the disk surface brightness by using a self-similar profile instead of a truncated power-law. For this reason no estimate for $R_{\rm {out}}$ could be extracted for these sources (see footnote in Sect. 4.1). (2) Best-fit estimate of the disk outer radius by fitting the observed visibilities at sub-millimeter wavelengths using a truncated power-law for the surface density profile. AW07: Andrews & Williams (2007a). (3) Interval of the disk outer radius adopted for our analysis. (4) Best-fit estimate of the spectral index of the SED $\alpha $ between 1 and 3 mm derived by considering for the outer disk radius the central value of the interval reported in Col. 3, and for the power-law index of the surface density profile p=1. (5) Best-fit estimate of the spectral index of the dust opacity $\beta $ between 1 and 3 mm. (6) Product between the dust mass and the dust opacity at 1 mm from the best-fit two-layer disk model. (7) Dust mass obtained with a power-law index for the grain size distribution q=2.5. (8) Like Col. (7) but with q=3. The sources without an estimate of the dust mass have a $\beta $-value (reported in Col. (6)) which cannot be reproduced with q=3. (9) Like Col. (8) but with q=3.5.


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