Toward understanding the formation of multiple systems - A pilot IRAM-PdBI survey of Class 0 objects

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Table 1:

Class 0 source sample.
Source	$\alpha$ (J2000)	$\delta$ (J2000)	SFR¹	Distance²	$M_{\rm {env}}$	$L_{\rm {bol}}$	Ref.³
				(pc)	( $M_{\odot}$ )	( $L_{\odot}$ )
L1448-C	03:25:38.87	+30:44:05.4	Perseus	250	1.6	5	(a)
NGC 1333-IRS2A	03:28:55.58	+31:14:37.1	Perseus	250	1.7	10	(b)
IRAM 04191	04:21:56.91	+15:29:46.1	Taurus	140	0.5-1.5	0.1	(c)
L1527	04:39:53.90	+26:03:10.0	Taurus	140	0.8-1.7	1.6	(a), (d)
L1521-F	04:28:38.99	+26:51:35.6	Taurus	140	0.7-4	0.1	(e), (f)

Notes. ⁽¹⁾ Star Forming Region with which the Class 0 object is associated. ⁽²⁾ Recent estimates of the distance to Perseus range from 220 to 350 pc. Throughout this paper, we adopt a distance of 250 pc for the Perseus molecular cloud (Enoch et al. 2006). ⁽³⁾ References for the adopted values of $M_{\rm {env}}$ and $L_{\rm {bol}}$ : (a) Motte & André (2001); (b) Jørgensen et al. (2007); (c) André et al. (1999); (d) Ohashi et al. (1997); (e) Bourke et al. (2006); (f) Crapsi et al. (2004).

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