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Table 3

Calculated parameters.

No. 1.3 mm flux Dust mass Stellar mass Age LD/L∗
(mJy) (M⊕) (M⊙) (Myr) (× 10-3)
1 <0.436 <0.30 ... ... ≤3.6
2 0.533 0.28 ± 0.09 0.67 2.3
3 <0.426 <0.30 0.35 ≤1.5
4 <0.435 <0.30 ... ... ≤7.1
5 <0.438 <0.30 0.36 ≤3.5
6 <0.431 <0.30 ... ... ≤2.9
7 <0.435 <0.30 ... ... 6.5
8 <0.431 <0.30 0.17 ≤11
9 <0.423 <0.29 0.65 ≤4.6
10 <0.476 <0.14 0.27 ≤1.4
11 <0.472 <0.14 0.31 ≤0.8
12 <0.541 <0.48 0.195 ≤2.3
13 <0.494 <0.44 1.4 ≤2.3∗
14 0.696 0.45 ± 0.13 0.17 80
15 <0.442 <0.37 1.1 ≤0.26
16 <0.453 <0.38 0.70 ≤2.8
17 1.813 2.09 ± 0.44 0.10 140
18 <0.459 <0.21 0.64 ≤3.4
19 <0.483 <0.22 0.34 ≤5.95
20 <0.461 <0.21 0.33 ≤1.96
21 <0.453 <0.20 0.56 ≤2.0
22 <0.442 <0.20 0.77 ≤1.5
23 0.569 0.27 ± 0.05 0.24 28
24 <0.465 <0.26 0.21 ≤5.7

Notes. Four systems have no calculated stellar mass or age as their luminosity does not coincide with any PMS tracks and are therefore probably background main-sequence stars. The final column of LD/L∗ gives the value of fractional disk luminosity, calculated by integration of the system SED.

(∗)

The value of LD/L∗ ≤ 10-3 quoted for system 13 assumes the far-IR emission is due to contamination.

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