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Table 1

Source parameters.

Source νLSR Lbol d Menv References
(km s-1) (L) (kpc) (M)

Low-mass: Class 0
L 1448-MM + 5.2 9.0 0.235 3.9 1
NGC 1333 IRAS 2A + 7.7 35.7 0.235 5.1 1
NGC 1333 IRAS 4A + 7.0 9.1 0.235 5.6 1
NGC 1333 IRAS 4B + 7.4 4.4 0.235 3.0 1
L 1527 + 5.9 1.9 0.140 0.9 1
Ced110 IRS4 + 4.2 0.8 0.125 0.2 1
BHR 71 −4.4 14.8 0.200 2.7 1
IRAS 15398 + 5.1 1.6 0.130 0.5 1
L 483-MM + 5.2 10.2 0.200 4.4 1
Ser SMM 1 + 8.5 30.4 0.230 16.1 1
Ser SMM 4 + 8.0 1.9 0.230 2.1 1
Ser SMM 3 + 7.6 5.1 0.230 3.2 1
L 723-MM + 11.2 3.6 0.300 1.3 1
B 335 + 8.4 3.3 0.250 1.2 1
L 1157 + 2.6 4.7 0.325 1.5 1

Low-mass: Class I
L 1489 + 7.2 3.8 0.140 0.2 1
L 1551 IRS 5 + 6.2 22.1 0.140 2.3 1
TMR 1 + 6.3 3.8 0.140 0.2 1
TMC 1A + 6.6 2.7 0.140 0.2 1
TMC 1 + 5.2 0.9 0.140 0.2 1
HH 46 + 5.2 27.9 0.450 4.4 1
IRAS 12496 + 3.1 35.4 0.178 0.8 1
Elias 29 + 4.3 14.1 0.125 0.3 1
Oph IRS 63 + 2.8 1.0 0.125 0.3 1
GSS 30 IRS1 + 3.5 13.9 0.125 0.6 1
RNO 91 + 0.5 2.6 0.125 0.5 1

Intermediate-mass
NGC 7129 FIRS 2 −9.8 430 1.25 50.0 2
L1641 S3 MMS1 5.3 70 0.50 20.9 2
NGC 2071 9.6 520 0.45 30.0 2
Vela IRS 17 3.9 715 0.70 6.4 2
Vela IRS 19 12.2 776 0.70 3.5 2
AFGL 490 −13.5 2000 1.00 45.0 2

High-mass
IRAS 05358+3543 −17.6 6.3 × 103 1.8 142 3
IRAS 16272−4837 −46.2 2.4 × 104 3.4 2170 3
NGC 6334-I(N) −3.3 1.9 × 103 1.7 3826 3
W43-MM1 +98.8 2.3 × 104 5.5 7550 3
DR21(OH) −3.1 1.3 × 104 1.5 472 3
W3-IRS5 −38.4 1.7 × 105 2.0 424 3
IRAS 18089−1732 +33.8 1.3 × 104 2.3 172 3
W33A +37.5 1.1 × 105 3.8 1220 3
IRAS 18151−1208 +32.8 2.0 × 104 3.0 153 3
AFGL2591 −5.5 2.2 × 105 3.3 320 3
G327−0.6 −45.3 5.0 × 104 3.3 2044 3
NGC 6334-I −7.4 2.6 × 105 1.7 500 3
G29.96−0.02 +97.6 3.5 × 105 6.0 768 3
G31.41+0.31 +97.4 2.3 × 105 7.9 2968 3
G5.89−0.39 +10.0 5.1 × 104 1.3 140 3
G10.47+0.03 +67.3 3.7 × 105 5.8 1168 3
G34.26+0.15 +58.0 3.2 × 105 3.3 1792 3
W51N-e1 +59.5 1.0 × 105 5.1 4530 3
NGC 7538-IRS1 −56.2 1.3 × 105 2.7 433 3

Notes.See van Dishoeck et al. (2011) for the source coordinates.

Reference. (1) Bolometric luminosities and envelope masses obtained from Kristensen et al. (2012). (2) Envelope masses collected in Wampfler et al. (2013). (3) Bolometric luminosities (obtained from observations) and envelope masses calculated in van der Tak et al. (2013).

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