Astronomy & Astrophysics

Table 1: Sample of protostars surveyed in Taurus. The infrared photometry and the spectral indices are taken from Kenyon & Hartmann (1995), except for IRAS 04191+1523, whose JHK photometry is from the 2MASS database and classification from Motte & André (2001). The bolometric luminosities are from Motte & André (2001). IRAS did not resolve the systems IRAS 04108+2803 AB and IRAS 04181+2654 AB and we assigned the same spectral index, based on unresolved photometry, to both components and split evenly the bolometric luminosity of the later system. The classification of each source is based on the infrared spectral indices (see text); "I'' stands for Class I sources and "FS'' for flat spectrum sources. The last three columns indicate whether the source i) has at least one visual companion within 10 $^{\prime \prime }$ , ii) is surrounded by an extended nebulosity in our images (see also Park & Kenyon 2002), and iii) has an extended (>1000 AU) envelope as seen in millimeter continuum mapping (from Motte & André 2001).
Object J H K $\alpha^{2-12}_{{\rm IR}}$ $\alpha^{2-25}_{{\rm IR}}$ Class $L_{\rm bol} (L_\odot)$ Comp? Opt neb? Mm env?

IRAS 04016+2610 13.62 11.67 9.33 1.06 1.02 I 3.7 N Y N

IRAS 04108+2803 B 16.25 13.25 11.12 0.50 0.62 FS 0.6 N N N

IRAS 04113+2758 11.29 9.15 7.79 -0.01 0.12 FS >1.6 Y N Y

IRAS 04158+2805 13.15 11.92 10.80 1.47 0.72 I >0.4 N Y N

IRAS 04169+2702 16.87 13.83 11.22 0.89 1.10 I 0.8 N Y Y

IRAS 04181+2655 15.46 12.74 10.54 0.60 0.55 I 0.4 N N N

IRAS 04181+2654 A 15.90 12.74 10.58 -0.00 0.10 FS 0.25 N N Y

IRAS 04181+2654 B 18.11 13.64 10.81 -0.00 0.10 FS 0.25 N N Y

IRAS 04191+1523 16.74 14.43 12.26 I 0.5 Y Y Y

IRAS 04239+2436 15.61 12.96 10.58 1.27 1.15 I 1.3 N N Y

IRAS 04248+2612 12.76 11.39 10.65 -0.09 0.48 FS 0.4 Y Y Y

IRAS 04260+2642 14.64 12.96 11.63 0.16 0.25 FS 0.1 N N N

IRAS 04263+2426 10.84 9.06 7.80 1.02 0.74 I 7.0 Y Y Y

IRAS 04264+2433 13.63 12.07 11.09 0.67 0.98 I 0.5 N N N

IRAS 04295+2251 13.62 11.11 9.55 0.11 0.21 FS 0.6 N N N

IRAS 04302+2247 14.20 12.35 11.07 0.15 FS 0.3 N Y N

IRAS 04325+2402 13.02 11.03 0.79 I 0.9 Y Y Y

IRAS 04361+2547 16.07 12.88 10.55 1.27 1.55 I 3.7 N Y Y

IRAS 04365+2535 17.28 13.39 10.62 1.08 1.27 I 2.4 N Y Y

IRAS 04381+2540 16.21 14.32 12.00 1.20 1.31 I 0.7 N Y Y

IRAS 04385+2550 12.61 10.72 9.65 0.14 0.18 FS >0.4 N N N

IRAS 04489+3042 13.74 11.58 10.11 0.18 0.31 FS 0.3 N N N

**Table 1:** Sample of protostars surveyed in Taurus. The infrared photometry and the spectral indices are taken from Kenyon & Hartmann (1995), except for IRAS 04191+1523, whose *JHK* photometry is from the 2MASS database and classification from Motte & André (2001). The bolometric luminosities are from Motte & André (2001). IRAS did not resolve the systems IRAS 04108+2803 AB and IRAS 04181+2654 AB and we assigned the same spectral index, based on unresolved photometry, to both components and split evenly the bolometric luminosity of the later system. The classification of each source is based on the infrared spectral indices (see text); "I'' stands for Class I sources and "FS'' for flat spectrum sources. The last three columns indicate whether the source i) has at least one visual companion within 10 $^{\prime \prime }$ , ii) is surrounded by an extended nebulosity in our images (see also Park & Kenyon 2002), and iii) has an extended (>1000 AU) envelope as seen in millimeter continuum mapping (from Motte & André 2001).
Object	J	H	K	$\alpha^{2-12}_{{\rm IR}}$	$\alpha^{2-25}_{{\rm IR}}$	Class	$L_{\rm bol} (L_\odot)$	Comp?	Opt neb?	Mm env?
IRAS 04016+2610	13.62	11.67	9.33	1.06	1.02	I	3.7	N	Y	N
IRAS 04108+2803 B	16.25	13.25	11.12	0.50	0.62	FS	0.6	N	N	N
IRAS 04113+2758	11.29	9.15	7.79	-0.01	0.12	FS	>1.6	Y	N	Y
IRAS 04158+2805	13.15	11.92	10.80	1.47	0.72	I	>0.4	N	Y	N
IRAS 04169+2702	16.87	13.83	11.22	0.89	1.10	I	0.8	N	Y	Y
IRAS 04181+2655	15.46	12.74	10.54	0.60	0.55	I	0.4	N	N	N
IRAS 04181+2654 A	15.90	12.74	10.58	-0.00	0.10	FS	0.25	N	N	Y
IRAS 04181+2654 B	18.11	13.64	10.81	-0.00	0.10	FS	0.25	N	N	Y
IRAS 04191+1523	16.74	14.43	12.26			I	0.5	Y	Y	Y
IRAS 04239+2436	15.61	12.96	10.58	1.27	1.15	I	1.3	N	N	Y
IRAS 04248+2612	12.76	11.39	10.65	-0.09	0.48	FS	0.4	Y	Y	Y
IRAS 04260+2642	14.64	12.96	11.63	0.16	0.25	FS	0.1	N	N	N
IRAS 04263+2426	10.84	9.06	7.80	1.02	0.74	I	7.0	Y	Y	Y
IRAS 04264+2433	13.63	12.07	11.09	0.67	0.98	I	0.5	N	N	N
IRAS 04295+2251	13.62	11.11	9.55	0.11	0.21	FS	0.6	N	N	N
IRAS 04302+2247	14.20	12.35	11.07		0.15	FS	0.3	N	Y	N
IRAS 04325+2402		13.02	11.03		0.79	I	0.9	Y	Y	Y
IRAS 04361+2547	16.07	12.88	10.55	1.27	1.55	I	3.7	N	Y	Y
IRAS 04365+2535	17.28	13.39	10.62	1.08	1.27	I	2.4	N	Y	Y
IRAS 04381+2540	16.21	14.32	12.00	1.20	1.31	I	0.7	N	Y	Y
IRAS 04385+2550	12.61	10.72	9.65	0.14	0.18	FS	>0.4	N	N	N
IRAS 04489+3042	13.74	11.58	10.11	0.18	0.31	FS	0.3	N	N	N

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