Table 5:

Overview of the envelope properties^a.

Source			N(H2)a	N(C18O)	N(H13CO+)
	('')	()	(1022 cm-2)	(1015 cm-2)	(1015 cm-2)
Chamaeleon
Ced 110 IRS 4	20	0.07	5.0/-	8.3	1.4	181	6.7
Ced 110 IRS 6	20	0.04	3.3/-	5.5	-	90	<13
Cha IRS 6a	-	-	0.26/-	0.43	-	-	-
Cha IRN	20	0.17	4.3/-	7.2	-	400	<5.2
Cha INa 2	-	-	3.8/-	6.3	-	150	-
Corona australisb
CrA IRAS 32	44	0.8	10.5/21.2*	17.5	3.0	257	16
HH100-off	45	1.6	12.4/35.2*	20.7	-	130	<0.9
RCrA IRS 5	43	1.7	20.7/24.5*	35.1	4.8	189	10
RCrA IRS 7A	48	6.3c	21.2/30.5*	35.3	8.9	117	7.7
RCrA IRS 7B	48	6.3c	23.8/30.5*	39.7	12.3	156	10
RCrA TS 3.5	-	-	-/-	-	-	-	-
Isolated
HH 46d	60	5.1	8.1/18.2*	13.5	6.1	103	16
IRAS 07178-4429	-	-	5.5/-	9.2	-	123.9	<8
IRAS 12496-7650	25	0.4	3.0/-	5.0	-	25	<3.1
IRAS 13546-3941	-	-	5.5/-	9.2	-	123	-
IRAS 15398-3359	25	0.5	1.9/-	3.2	-	79	-

The column density of H₂ is derived from that of C¹⁸O assuming H₂/C¹⁸O =  . If 850 m data are available in Di Francesco et al. (2008), column densities based on the dust emission are also computed. These numbers are indicated as the second entry with an asterisk. Both column densities are within the same 18 '' beam; ^b mass estimates in the RCrA region may be severely overestimated due to presence of extended cloud material; ^c RCrA IRS 7A and 7B cannot be distinguished in the sub-millimeter continuum maps; the value refers to the core containing both sources; ^d for a thorough discussion on the mass of HH 46, see van Kempen et al. (2009a).