Table 6: Derived parameters from model fits.
IRAS
\begin{sideways}H/L\end{sideways}

\begin{sideways}Comp\end{sideways}
$\xi $   type Sp. $L_{\rm bol}$ $M_{\rm env} ^c$ $R_{\rm env}$ $\theta _{\rm p}$ id
            Cl.
\begin{sideways}({10$^3$ ~$L_{\odot}$ })\end{sideways}
($M_{\odot }$)
\begin{sideways}(10$^4$ ~AU)\end{sideways}
($^{\circ}$) ($^{\circ}$)
05137+3919 L A/1 0.12   IR-P O8 255 2890 25 20 66
    B/2 0.11   IR-S1 B1 5.5 120 10 20 72
05345+3157 L A/3 0.09   IR-S1 B5 0.5 7 6 40 60
    B/1 0.11f   MM-P   1.7 35      
    2     MM-S   0.8 20      
05373+2349 L A/1 0.04   IR-P B5 0.4 26 6 0 60
08211-4158 L A 0.15g   IR-S2 B3 1.0 3 8 20 53
    1   MM-P   1.1 80      
    B 0.01   IR-S1 B5 0.4 8 6 20 53
08470-4243 H A/1 0.22   IR-P B1 4.8 85 8 20 66
08477-4359 L A 0.06   IR-S1 B5 0.45 0.1 1 40 60
    1     MM-P   0.7 85      
08589-4714 H A/1 0.11   IR-P B5 0.3 20 8 40 0
08563-4225 L A/1 0.06   IR-P B3 1.0 23 8 20 60
09131-4723 L A/1 0.15   IR-P B5 0.45 26 8 20 66
    B 0.02   IR-S1 B5 0.3 4.3 8 40 60
    2     MM-S   0.47 25      
    3     MM-S   0.3 21.5      
10019-5712 H A/1 0.13   IR-P B3 0.65 11 6 40 37
    B/2 0.09   IR-S1 B5 0.3 7 6 40 37
10095-5843b L A 0.17l   IR-P B1 4.8 85 8 20 66
10184-5748 H A/1 0.09   IR-P O5 255 2890 30 20 66
    B 0.02   IR-S1 B0 15 54 8 40 37
    C 0.02   IR-S1 B1 4.5 21.6 4 40 60
    G/2 0.14   IR-S1 B1 3.5 62 8 40 45
10501-5556 H A/1 0.07   IR-P B1 3.3 88 8 40 37
10555-6242 H A/1 0.18   IR-P B1 3.3 88 8 40 37
11380-6311a L A/1 0.10   IR-P B5 0.3 20 8 40 37
12063-6259 H A/1 0.04   IR-P O5 373 2890 30 20 78
12127-6244 H A/1 0.13   IR-P O3 888 2050 30 20 72
    2     MM-S   105 1352      
14000-6104 L A 0.31   IR-S2 B0 19 54 8 40 53
    1   MM-P   21 1965      
    B 0.13   IR-S1 B1 3.6 88 10 40 45
    C 0.01   IR-S1 B3 1.0 2.5 8 0 53
    D 0.01   IR-S1 B1 8.6 21.5 4 40 78
    H 0.31h   IR-S1 B1 4.9 132 10 0 0
    I 0.34h   IR-S1 B1 5.0 132 10 0 45
14057-6032a H A/1 0.02   IR-P B5 0.25 6.5 4 40 25
15068-5733b H A 0.21   IR-P O5 176 2145 30 40 37
15454-5335b H A 0.27   IR-P O5 225 2890 30 20 37
    B 0.02   IR-S1 O8 50 720 25 20 53
15519-5430a L A 0.56   IR-S2 B3 1.1 4 8 40 53
    1   MM-P   9.8 485      
    G 0.01   IR-S1 B5 0.5 3 8 20 60
15557-5337a L A/1 0.05   IR-P O8 65.4 721 25 20 73
    B/2 0.06   IR-S1 O8 57 721 25 20 66
    C 0.01   IR-S1 B0 13 4.4 6 40 25
    D 0.05   IR-S1 B1 4.1 1 2 40 53
16148-5011a L A 0.03   IR-S1 O8 71.5 20 10 0 72
    C 0.16   IR-S1 O5 255 2890 30 40 66
    1     MM-Pe   240 2650      
    2     MM-S   43.2 1160      
16232-4917a L A/1 0.06   IR-P B1 4.25 88 10 40 53
16501-4314a L A 0.26i   IR-S2 B1 6.1 26 10 0 78
    1   MM-P   24.7 610      
    2     MM-S   24.7 610      
16535-4300a L A 0.54   IR-S2 B3 2 0.4 1 40 84
    1   MM-P   13.4 750      
    C 0.01   IR-S1 B1 7.5 1.2 2 0 84
17082-4114a L A 0.36   IR-S2 B3 2.1 0.1 1 20 84
    1   MM-P   2.5 282      
    2     MM-S   1.4 166      
    3     MM-S   1.5 185      
17425-3017 L A 0.53   IR-S2 B1 5.1 13 10 40 53
    1   MM-P   23.1 1250      
18024-2119b L G/1 0.53   MM-P   84.2 5850      
18144-1723b L A 0.20   IR-P O5 176 2145 30 40 37
18278-1009 L A 0.13   IR-P B1 9.1 120 10 20 84
18511+0146 L A1 0.17m   IR-S2 B1 6.4 1.2 2 0 72
    1   MM-P   9.2 330      
    A2 0.21   IR-S1 B1 4.5 120 10 20 60
19092+0841a L A 0.43   IR-S2 B3 1.1 8 6 0 66
    1   MM-P   7.8 738      
20062+3550 H A 0.15   IR-P B1 4.8 85 8 20 66
20106+3545b L A 0.11n   IR-P B1 3.6 88 10 40 45
    1     MM-S   1.8 45      
21307+5049 L A/1 0.16   IR-P B1 3.6 88 10 40 45
21519+5613 H A/1 0.18   IR-P B1 5.4 85 8 20 75
22172+5549 L A/1 0.16   IR-P B1 3.6 88 10 40 45
22305+5803 H A/1 0.05   IR-P B1 4.8 86 8 20 66
22506+5944 H A 0.31   IR-S2 B1 7 25 10 20 78
    1   MM-P   8.9 671      
23385+6053 L 1 0.36   MM-P   17.5 222      
a Near distance adopted.
b Far distance adopted.
c A correction factor of 0.4 has been applied to all envelope masses of IR sources to account for different mass opacity assumptions in Whitney et al.'s models and in our greybody mass estimates.
d Between polar axis and plane of the sky.
e Source MM1 is assumed as primary instead of C because source C is not part of the A/MM1/MM2 complex (it's a different IRAS source), although we assume it connected to the same star forming region.
f Model rejected, see Sect. A.2.
g Model rejected, see Sect. A.4.
h Model accepted, see Sect. A.18.
i Model rejected, see Sect. A.26.
l This is not the minimum-$\xi $ model (see Sect. A.11), but it is chosen among the 10 best-$\xi $ models. The minimum $\xi $ model ($\xi=0.14$) provides a better fit to the mid-IR portion, but misses the 100 $\mu $m by slightly more than 50%.
m Model rejected, see Sect. A.33.
n Same as footnote l; see Sect. A.36.


Source LaTeX | All tables | In the text