Table 1:

Sample of embedded protostars.

Source	RA [J2000]	Dec [J2000]	[K]	[]	d [pc]
Class 0
L1448-mm	03 25 38.9	+30 44 05.4	77	5.3	220
NGC 1333:
-IRAS2A	03 28 55.6	+31 14 37.1	57	20a	220
-IRAS4A-SE	03 29 10.5	+31 13 31.0	43	5.8	220
-IRAS4A-NW	03 29 10.4	+31 13 32.3	-	-	220
-IRAS4B	03 29 12.0	+31 13 08.1	55	3.8b	220
-IRAS4B'	03 29 12.8	+31 13 07.0	-	-	220
L1527	04 39 53.9	+26 03 09.8	59	2.0	140
L483	18 17 29.9	-04 39 39.6	60	9.0	200
B335	19 37 00.9	+07 34 09.7	60	3.0	250
L1157	20 39 06.3	+68 02 16.0	42	6.0	325
Class I
L1489-IRS	04 04 42.9	+26 18 56.3	238	3.7	140
TMR1	04 39 13.9	+25 53 20.6	144	3.7	140
TMC1A	04 39 35.2	+25 41 44.4	172	2.2	140
GSS30-IRS3	16 26 21.7	-24 22 50.6	300	14c	125
GSS30-IRS1	16 26 22.2	-24 23 01.9	-	-	125
WL 12	16 26 44.2	-24 34 48.7	440	2.6	125
Elias 29	16 27 09.4	-24 37 20.0	350	41	125
IRS 43	16 27 26.9	-24 40 50.6	310	6.0	125
IRS 54	16 27 51.8	-24 31 45.4	740	2.5	125
IRS 63	16 31 35.7	-24 01 29.6	530	3.3	125

^aFor NGC 1333-IRAS2A Evans et al. (2009) quote a luminosity of 76 . Estimating the luminosity from scaling the 70 m flux using the approach of Dunham et al. (2008) gives a luminosity of 19.6 , which agrees well with previous estimates from modeling the SED in the range 16-20 . The higher luminosity in the c2d compilation is a result of the SED of IRAS2A being unconstrained at 24 m (Dunham, priv. comm) - and we therefore adopt a luminosity of 20  for this source. ^b The Spitzer maps of NGC 1333-IRAS4B shows significant emission from a nearby outflow shock within the typical single-dish beam. As total luminosity for this source, we adopt the sum of the two components, SSTc2d J032912.06+311305.4 and SSTc2d J032912.06+311301.7, from Evans et al. (2009). ^c The emission from GSS30-IRS3 (LFAM1) and GSS30-IRS1 are not separated in the Spitzer catalog (the latter dominates the emission and its luminosity is quoted here).