**Table 1:** Characteristics of the sources.
		(1)	(2)	(3)	(4)	(5)	(6)	(7)	(8)
Source		$L_{{\rm NIR}}$	$L_{{\rm MIR}}$	$L_{{\rm IRAS}}$	$L_{{\rm submm}}$	$L_{\rm bol}$	$M_{{\rm env}}$	$A_{{\rm V}}$	N_*
		(%)	(%)	(%)	(%)	( $L_{\odot}$ )	( $M_{\odot}$ )	(Mag)	(pc^-2)
LLN 8	IRAS 08211-4158	5.3	10.5	53.3	31.0	141^a	...	...	...
LLN 13	IRAS 08375-4109	5.3	6.8	72.8	17.7	960^b	2.6^b	$\geq$ 40^a	800^b
LLN 17	IRAS 08448-4343	1.3	4.0	60.8	33.9	3100^b	6.4^b	$\sim$ 40^a	3400^b
LLN 19	IRAS 08470-4321	4.8	20.3	65.8	9.1	1600^b	3.5^b	$\sim$ 40^a	2400^b
LLN 41	IRAS 09017-4716	...	...	80.7	19.3	470	...	...
LLN 20^c	IRAS 08476-4306	0.5	3.1	66.8	29.7	1600 ^b	2.2^b		3900^b
LLN 33^c	IRAS 08576-4314	2.6	12.6	80.6	4.2	91^a	...	...	...
LLN 39^c	IRAS 09014-4736	1.3	5.7	71.1	22.0	807^a	...	...	...
LLN 47^c	IRAS 09094-4522	3.4	13.3	74.4	8.9	21^a	...	...	...

Notes: The dots refer to values which are not available in the literature.
Columns 1-4: The fractional luminosities are computed by Liseau et al. (1992). The indices refer to the wavelength range 1-5 $\mu$ m (Col. 1); 5-12 $\mu$ m (Col. 2), 12-100 $\mu$ m (Col. 3) and 0.1-1 mm (Col. 4) for NIR, MIR, IRAS and submm, respectively. $L_{{\rm submm}}$ are estimated by Liseau et al. (1992) when the millimeter observations do not exist. Column 5: bolometric luminosity. Column 6: the envelope masses ( $M_{{\rm env}}$ ) are derived from 1 mm continuum flux by Massi et al. (1999) for four of our sources. Envelope masses are only given for those sources for which millimeter observations have been carried out. Column 7: extinction estimated by Liseau et al. (1992). Column 8: N_* refers to the maximum stellar surface densities measured.
Reference: ^a Liseau et al. (1992); ^b Massi et al. (1999); ^c VLT-ISAAC data analyzed by Pontoppidan et al. (2003b).

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