OH far-infrared emission from low- and intermediate-mass protostars surveyed with Herschel-PACS

S. F. Wampfler; S. Bruderer; A. Karska; G. J. Herczeg; E. F. van Dishoeck; L. E. Kristensen; J. R. Goicoechea; A. O. Benz; S. D. Doty; C. McCoey; A. Baudry; T. Giannini; B. Larsson

doi:10.1051/0004-6361/201219929

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A&A, 552 (2013) A56

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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	235^a	35.7^b	5.1^c
NGC 1333 IRAS 4A	03:29:10.5	+31:13:30.9	0	235^a	9.1^b	5.6^c
NGC 1333 IRAS 4B	03:29:12.0	+31:13:08.1	0	235^a	4.4^b	3.0^c
L 1527	04:39:53.9	+26:03:09.8	0	140^d	1.9^b	0.9^c
Ced110 IRS4	11:06:47.0	−77:22:32.4	0	125^e	0.8^b	0.2^c
IRAS 15398/B228	15:43:01.3	−34:09:15.0	0	130^e	1.6^b	0.5^c
L 483 mm	18:17:29.9	−04:39:39.5	0	200^d	10.2^b	4.4^c
Ser SMM1	18:29:49.8	+01:15:20.5	0	230^f	30.4^b	16.1^c
Ser SMM3	18:29:59.2	+01:14:00.3	0	230^f	5.1^b	3.2^c
L 723 mm	19:17:53.7	+19:12:20.0	0	300^d	3.6^b	1.3^c


L 1489	04:04:43.0	+26:18:57.0	I	140^g	3.8^b	0.2^c
TMR 1	04:39:13.7	+25:53:21.0	I	140^g	3.8^b	0.2^c
TMC 1A	04:39:34.9	+25:41:45.0	I	140^g	2.7^b	0.2^c
TMC 1	04:41:12.4	+25:46:36.0	I	140^g	0.9^b	0.2^c
HH 46	08:25:43.9	−51:00:36.0	I	450^h	27.9^b	4.4^c
IRAS 12496/DK Cha	12:53:17.2	−77:07:10.6	I	178ⁱ	35.4^b	0.8^c
RNO 91	16:34:29.3	−15:47:01.4	I	125^j	2.6^b	0.5^c


AFGL 490	03:27:38.4	+58:47:08.0	IM	1000^k	2000^l	45^m
NGC 2071	05:47:04.4	+00:21:49.0	IM	422ⁿ	520^o	30^p
Vela IRS 17	08:46:34.7	−43:54:30.5	IM	700^q	715^r	6.4^s
Vela IRS 19	08:48:48.5	−45:32:29.0	IM	700^q	776^q	3.5^s
NGC 7129 FIRS 2	21:43:01.7	+66:03:23.6	IM	1250^t	430^u	50^v
L1641 S3MMS1	05:39:55.9	−07:30:28.0	IM	465ⁿ	70^w	20.9^x

Reference. .

^(a)

Hirota et al. (2008),

^(b)

Values from Kristensen et al. (2012) using PACS data from the WISH and DIGIT key programs (Karska et al. 2013; Green et al. 2013).

^(c)

Derived from DUSTY modeling of the sources as described in Kristensen et al. (2012).

^(d)

André et al. (2000),

^(e)

Knude & Hog (1998),

^(f)

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.

^(g)

Kenyon et al. (2008),

^(h)

Heathcote et al. (1996),

⁽ⁱ⁾

Whittet et al. (1997),

^(j)

de Geus et al. (1989),

^(k)

Snell et al. (1984),

^(l)

Mozurkewich et al. (1986),

^(m)

Schreyer et al. (2002) derived an envelope mass of 40–50 M_⊙.

⁽ⁿ⁾

Wilson et al. (2005),

^(o)

Butner et al. (1990),

^(p)

Johnstone et al. (2001),

^(q)

Liseau et al. (1992),

^(r)

Giannini et al. (2005),

^(s)

Massi et al. (1999),

^(t)

Shevchenko & Yakubov (1989),

^(u)

Johnstone et al. (2010),

^(v)

Crimier et al. (2010),

^(w)

Stanke et al. (2000),

^(x)

van Kempen et al. (2012)

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