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Table 4:

Spectral slopes at mm wavelengths, dust disc masses, and properties of the 10-$\mu $m silicate feature.

Source
$\alpha_{1-3}$ $\alpha_{3-7}$ Dust disc massa Strength (Furlan et al. 2006) Strength $F^{10\mu m}_{\rm peak}$ Shape
      ( $10^{-4}~M_\odot$) ( $F_{10}-F_{\rm cont}$)/ $F_{\rm cont}$ max( $1+\frac{(F_\nu - F_{\rm\nu, c})}{(F_{\rm\nu, c})}$) F11.3/F9.8

HBC 553
... ... ... 0.22 1.43 0.86
HBC 556 ... ... <5.1 0.40 1.64 0.99
HBC 557 ... ... <4.4 0.21 1.37 0.95
HBC 559 ... ... <4.0 0.39 1.60 0.85
HBC 560 ... ... ... 0.29 1.44 1.03
HBC 561 ... ... ... 0.43 1.67 0.90

SZ Cha
$3.8 \pm 0.4$b ... 0.6 0.71 2.30 0.85
Sz 32 >3.7b <1.8 <0.8 0.14 1.24 1.11

IK Lup
$2.7 \pm 0.3$b ... 0.7 0.36 1.51 0.93
Sz 66 $1.9 \pm 0.2$b ... 0.4 0.40 1.62 0.92
HM Lup ... ... ... 0.50 1.81 0.85
Sz 73 ... ... ... 0.26 1.38 0.95
HN Lup ... ... ... 0.18 1.29 1.03
Sz 76 ... ... ... 0.45 1.77 0.77
Sz 77 ... ... ... 0.43 1.63 0.94
IM Lup $3.6 \pm 0.4$b $1.8 \pm 0.3$ 1.7 0.52 1.81 0.85
RY Lup $3.8 \pm 0.5$ >2.0 0.5 1.10 3.16 0.66
MY Lup $2.1 \pm 0.5$ >3.5 1.7 0.54 1.87 0.79
EX Lup ... ... ... 0.54 2.01 0.73
Sz 96 ... ... ... 0.78 2.30 0.82
Sz 102 ... ... ... 0.80 2.36 0.82
Sz 111 $2.5 \pm 0.4$ >2.9 1.1 ... ... ...
SSTc2d J161029.57-392214.7h ... ... <0.3 0.29 1.52 0.89
SSTc2d J161159.81-382338.5 ... ... <0.3 0.92 2.48 0.84
RX J1615.3-3255 $3.4 \pm 0.5$ >3.4 1.3 1.25 3.04 0.96
VV Ser ... ... <1.0 0.33 1.45 0.97
SSTc2d J182850.20+000949.7 ... ... <1.1 0.36 1.57 0.88
SSTc2d J182900.88+002931.5 $2.4 \pm 0.4$ ... 2.0 0.15 1.27 0.96
CoKu Ser-G3 ... ... <1.0 -0.09 0.82 1.17
IRAS 18268-0025 ... ... <0.7 0.48 1.67 1.14
SSTc2d J182944.10+003356.1i ... ... <0.7 0.30 1.53 0.96
EC 82 aka CK 3 ... ... <1.7 1.41 3.55 0.67
EC 90 aka CK 1 $2.5 \pm 0.5$ ... 6.7 0.26 1.40 1.12
EC 97 aka CK 4 ... ... ... 0.34 1.56 0.90
GSC 00446-00153 $3.0 \pm 0.5$ ... 4.0 ... ... ...

S CrA
$2.9 \pm 0.7$e $2.5 \pm 0.4$ 3.6 0.34 1.51 0.97
DG CrA ... ... <0.4 1.04 2.94 0.67
VV CrA $2.5 \pm 0.5$ d,e,f,g $2.4 \pm 0.5$g 3.9 ... ... ...

Notes. (a) Dust disc masses estimated from ATCA and CARMA fluxes, assuming a dust opacity $\kappa_\nu = 0.9$ cm2 g-1 (cf. Beckwith et al. 1990), and a dust temperature $T_{\rm dust} = 25$ K.
(b) Using the SEST 1.27 mm (single-dish) flux from Nürnberger et al. (1997).
(c) Using the SEST 1.27 mm (single-dish) flux from Henning et al. (1993).
(d) Using the SEST 1.20 mm (single-dish) flux from Chini et al. (2003).
(e) Using the SEST 1.27 mm (single-dish) flux from Henning et al. (1994).
(f) Taking a combined flux of 50.2 mJy at 3.17 mm.
(g) Using the PSF extraction method for the Spitzer IRS spectrum.
(h) Observed with Spitzer IRS for Program ID 30843 (B. Merín PI). The full IRS spectrum will be presented in Merín et al. (2010, in prep.).
(i) Observed with Spitzer IRS for Program ID 30223 (K.M. Pontoppidan PI). The full IRS spectrum will be presented in Oliveira et al. (2010, in prep.).


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