Table 1: The observed sample. IRAS16293-2422, which has been studied elsewhere (see text) is included for comparison.
Source $\alpha (2000)$ $\delta (2000)$ Cloud Dist.a $L_{\rm bol}$b $M_{\rm env}$b $L_{\rm smm}/L_{\rm bol}$c $T_{\rm bol}$b
        (pc) ( $L_{\hbox{$\odot$ }}$ ) ( $M_{\hbox {$\odot $ }}$ ) (%) (K)
NGC 1333-IRAS 4A 03:29:10.3 +31:13:31 Perseus 220 6 2.3 5 34
NGC 1333-IRAS 4B 03:29:12.0 +31:13:09 Perseus 220 6 2.0 3 36
NGC 1333-IRAS 2 03:28:55.4 +31:14:35 Perseus 220 16 1.7 $\la$1 50
L1448-MM 03:25:38.8 +30:44:05 Perseus 220 5 0.9 2 60
L1448-N 03:25:36.3 +30:45:15 Perseus 220 6 3.5 3 55
L1157-MM 20:39:06.2 +68:02:22 Isolated 325 11 1.6 5 60
L1527 04:39:53.9 +26:03:10 Taurus 140 2 0.9 0.7 60
VLA1623 16:26:26.4 -24:24:30 $\rho$-Ophiuchus 160 1 0.2 10 <35
IRAS 16293-2422d 16:32:22.7 -24:38:32 $\rho$-Ophiuchus 160 27 5.4 2 43
a From André et al. (2000), except for Perseus sources (Cernis 1990).
b From Jørgensen et al. (2002).
c From André et al. (2000).
d Included for comparison.


Source LaTeX | All tables | In the text