Table 1
Coordinates, distance, bolometric luminosity, and envelope masses of the low-mass class 0, class I, and intermediate-mass protostars in the sample.
Source | RA | Dec | Class | d | L bol | M env | ||
[h m s] | [° ′ ″] | [pc] | [L⊙] | [M⊙] | ||||
|
||||||||
NGC 1333 IRAS 2A | 03:28:55.6 | +31:14:37.1 | 0 | 235a | 35.7b | 5.1c | ||
NGC 1333 IRAS 4A | 03:29:10.5 | +31:13:30.9 | 0 | 235a | 9.1b | 5.6c | ||
NGC 1333 IRAS 4B | 03:29:12.0 | +31:13:08.1 | 0 | 235a | 4.4b | 3.0c | ||
L 1527 | 04:39:53.9 | +26:03:09.8 | 0 | 140d | 1.9b | 0.9c | ||
Ced110 IRS4 | 11:06:47.0 | −77:22:32.4 | 0 | 125e | 0.8b | 0.2c | ||
IRAS 15398/B228 | 15:43:01.3 | −34:09:15.0 | 0 | 130e | 1.6b | 0.5c | ||
L 483 mm | 18:17:29.9 | −04:39:39.5 | 0 | 200d | 10.2b | 4.4c | ||
Ser SMM1 | 18:29:49.8 | +01:15:20.5 | 0 | 230f | 30.4b | 16.1c | ||
Ser SMM3 | 18:29:59.2 | +01:14:00.3 | 0 | 230f | 5.1b | 3.2c | ||
L 723 mm | 19:17:53.7 | +19:12:20.0 | 0 | 300d | 3.6b | 1.3c | ||
|
||||||||
L 1489 | 04:04:43.0 | +26:18:57.0 | I | 140g | 3.8b | 0.2c | ||
TMR 1 | 04:39:13.7 | +25:53:21.0 | I | 140g | 3.8b | 0.2c | ||
TMC 1A | 04:39:34.9 | +25:41:45.0 | I | 140g | 2.7b | 0.2c | ||
TMC 1 | 04:41:12.4 | +25:46:36.0 | I | 140g | 0.9b | 0.2c | ||
HH 46 | 08:25:43.9 | −51:00:36.0 | I | 450h | 27.9b | 4.4c | ||
IRAS 12496/DK Cha | 12:53:17.2 | −77:07:10.6 | I | 178i | 35.4b | 0.8c | ||
RNO 91 | 16:34:29.3 | −15:47:01.4 | I | 125j | 2.6b | 0.5c | ||
|
||||||||
AFGL 490 | 03:27:38.4 | +58:47:08.0 | IM | 1000k | 2000l | 45m | ||
NGC 2071 | 05:47:04.4 | +00:21:49.0 | IM | 422n | 520o | 30p | ||
Vela IRS 17 | 08:46:34.7 | −43:54:30.5 | IM | 700q | 715r | 6.4s | ||
Vela IRS 19 | 08:48:48.5 | −45:32:29.0 | IM | 700q | 776q | 3.5s | ||
NGC 7129 FIRS 2 | 21:43:01.7 | +66:03:23.6 | IM | 1250t | 430u | 50v | ||
L1641 S3MMS1 | 05:39:55.9 | −07:30:28.0 | IM | 465n | 70w | 20.9x |
Reference. .
Values from Kristensen et al. (2012) using PACS data from the WISH and DIGIT key programs (Karska et al. 2013; Green et al. 2013).
Derived from DUSTY modeling of the sources as described in Kristensen et al. (2012).
Eiroa et al. (2008). Based on VLBA measurements of a star thought to be associated with the Serpens cluster, Dzib et al. (2010) inferred a distance of 415 pc.
Schreyer et al. (2002) derived an envelope mass of 40–50 M⊙.
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