W3 OH             The 2MASS source is 3.5" away from the coordinates adopted here.
L1448 I2          Fluxes from O'Linger et al. (1999ApJ...515..696O) taken in the whole observed field are not used L1448NW is situated about 20" NNW of the binary L1448N(A/B). The flux measurements are strongly influenced by the extended envelope of this nearby source. Fluxes from Chandler and Richer (2000ApJ...530..851C) are given in Jy/beam and hence not used. The two 2.7mm fluxes measured in small (<5") apertures by Looney et al. (2000ApJ...529..477L) are not used either.
L1448 N           This source is actually a protostellar binary consisting of L1448 IRAS3A and IRAS3B. Since IRAS3A is about one order of magnitude brighter in the FIR as well as in the millimeter range, all the unresolved observations are attributed to IRAS3A. Sub-mm fluxes taken in 40" apertures (Shirley et al. 2000ApJS..131..249S) are not used due to the vicinity of L1448NW.
L1448 C           We chose the values measured in boxes larger than 30", in order not to miss emission from the outer regions of the extended envelope.
RNO 15 FIR        In the vicinity (about 1' south-east) of RNO15FIR the somewhat older source RNO15 can be found. Both objects possess about the same brightness and hence flux measurements in large boxes might be influenced by RNO15. This applies especially for the IRAS data. At 60 and 100{mu}m there are discrepancies between the IRAS and ISO data. We used the ISO data since they are measured in a slightly smaller aperture.
RNO 15            The data at short wavelengths and arround the maximum show a large scatter. This might partly be due to the nearby source RNO15FIR and also due to the fact that most of these measurements are taken before 1990 and suffer from large uncertainties.
NGC 1333 I1       Here the fluxes given by Sandell et al. (2001ApJ...546L..49S) are excluded. They are unreliable because the source is at the edge of their observed field.
IRAS 03256+3055   This source seems to consist of three objects (Young et al. 2003ApJS..145..111Y). The IRAS position coincides with the weakest of the sub-mm sources. We excluded the fluxes measured in the 120" apertures. There is a discrepancy between the 800 and 850{mu}m point. We did not use the 800{mu}m data from Anglada and Rodriguez (2002RMxAA..38...13A) since an unusual {beta}>3 would be obtained.
NGC 1333 I2       NGC1333I2 is a double source consisting of IRAS2A and 2B with a separation of about 30". IRAS2A is much brighter than IRAS2B in the sub-mm and hence the fluxes given for both objects are attributed to IRAS2A.
SVS 13 B          Here it is particular important to have the aperture sizes in which the photometry was obtained, since SVS13B is a triple protostellar system. It consists of MMS1, 2, and 3. While MMS1 and 2 have about the same brightness, MMS3 is weaker. There are no data for the single sources at wavelengths shorter than 350{mu}m.
NGC 1333 I4 A     This is a double source I4A1 and I4A2. I4A1 is the brighter of the two sources and all the photometric data was attributed to this object.
NGC 1333 I4 B     NGC1333I4B is situated about 30" south-east of NGC1333I4A and hence the fluxes measured in large areas might be influenced. The data from Sandell et al. (2001ApJ...546L..49S) were taken in a relatively small aperture and might not include all the emission from the envelope. It was therefore not used. The flux from Rengel et al. (2004BaltA..13..449R) is also excluded since the object is at the border of their map. The large fluxes given from Rebull et al. (2003AJ....125.2568R) are not used since they might be influenced by surrounding emission.
IRAS 03282+3035   Even though this source seems to be isolated, the fluxes measured in the 120" box by Sandell et al. (2000) are excluded.
HH 211 MM         The data from Dent et al. (1998MNRAS.301.1049D) are taken in an unknown aperture and hence not used.
B213              We did not use the fluxes measured in a 120" aperture by Young et al. (2003ApJS..145..111Y) since they might by influenced by other surrounding sources. The IRAS 100{mu}m limit was used as flux.
L1551 IRS 5       Mesurements taken in very small apertures (<10") were exluded. Also the data taken in the 270" apertures are not used.
L1551 NE          This object is a double source consisting of L1551 NE A and B. All fluxes are attributed to L1551 NE A.
IRAS 04325+2402   The measurements arround 800{mu}m and 1.3mm do not correspond to each other. We did not use the low values given by Moriarty-Schieven et al. (1994ApJ...436..800M), since very high values of {beta} (>3) are needed to explain these data.  Also the upper limits given by Barsony and Kenyon (1992ApJ...384L..53B) seem to be too low in this context. The 2MASS source is 6" away from the coordinates adopted here.
L1527             There is a large scatter in the fluxes taken between 350{mu}m and 1.3mm even if they are taken with the same aperture size. We do not use data taken in the 120" apertures.
HH 114 MMS        Difficulties occur since the IRAS points are only upper limits at all wavelengths. The 1.3mm flux given by Chini et al. (1997ApJ...474L.135C) for the whole observed field was excluded.
IRAS 05173-0555   There is a large scatter in the data at all wavelengths. We did not use the flux of the whole field given by Chini et al. (1997ApJ...474L.135C). There are two sets of fluxes in the sub-mm data; low and high values. We chose the lower fluxes since they seem to present the better the central source and its envelope.
L1634 IRS 7       The 2MASS source is 3" away from the coordinates adopted here.
RNO 43 MM         The measurement from Chini et al. (1997ApJ...474L.135C) at 1.3mm for the whole field was excluded.
OMC 3 MM 6        No data shortward of 100{mu}m are available. The 185{mu}m point taken in a 3' aperture was not used. All the fluxes below 200{mu}m seem to be anomolous due to the large apertures.
OMC 3 MM 9        There is no IRAS detection. The 2MASS source is 6.6" away from the coordinates adopted here.
OMC 3 MM 7        The upper limit at 100{mu}m in the IRAS catalogue seems to be too small compared to the other data. The 2MASS source is 3.5" away from the coordinates adopted here.
L1641 N           The 2MASS source is 7" away from the coordinates adopted here.
HH 1-2 MMS 2      There is a large scatter in the 1.3mm data. We used only the flux measured in the 8.5" aperture.
L1641 VLA 1       The scatter in the measurements is very large. We did not use the huge 1.3mm flux. The 2MASS source is 4.3" away from the coordinates adopted here.
L1641 SMS III     The 2MASS source is 6.5" away from the coordinates adopted here.
HH 147 MMS        Measurements taken in large apertures (>30") are excluded. The 2MASS source is 2.5" away from the coordinates adopted here.
NGC 2023 MM 1     The 450{mu}m point from Sandell et al. (1999ApJ...519..236S) in the small aperture was excluded, as well as the data taken in the 180" apertures.
NGC 2024 FIR 5    The huge 1.3mm flux in the 30" aperture was excluded.
HH 212 MM         The 1.3mm flux from Chini et al. (1997ApJ...474L.135C), measured in the whole observed field, was excluded.
HH 25 MMS         The two fluxes from Gibb and Davis (1998MNRAS.298..644G) measured in large apertures at 60 and 100{mu}m are excluded. The 1.3mm point is not used.
HH 24 MMS         All the IRAS points are just upper limits. The 1.3mm flux from Launhard et al. (1996A&A...312..569L) measured in a 30" aperture was excluded.
NGC 2068 LBS 17   All data shortward of 100{mu}m are upper limits.
HH 111 MMS        The data obtained in large apertures ({>=}30") were excluded as well as the high flux at 1.3mm. The 2MASS source is 4" away from the coordinates adopted here.
Mon OB1 IRAS12 S1 The 2MASS source is 4" away from the coordinates adopted here.
IRAS 08076-3556   The 2MASS source is 4.7" away from the coordinates adopted here.
BHR 71 MM         The 2MASS source is 4" away from the coordinates adopted here.
IRAS 12553-7651   The 2MASS source is 7" away from the coordinates adopted here.
IRAS 15398-3359   The measurements in the 120" apertures are excluded. The 2MASS source is 3" away from the coordinates adopted here.
IRAS 16017-3936   The 2MASS source is 9" away from the coordinates adopted here.
VLA 1623          This source is a double object consisting of the two sources VLA1623A and B, which are comparably bright in the millimeter range. The measurements from Pudritz et al. (1996ApJ...470L.123P) were excluded.
IRAS 16293-2422   IRAS 16293-2422 consits of two sources, IRAS16293A and B, seperated by about 4" (Looney et al. 2000ApJ...529..477L). We used only the data given for both objects together.
IRAS 16493-4242   The 2MASS source is 3.5" away from the coordinates adopted here.
IRAS 18148-0440   The data taken in the 19 and 120" apertures are excluded. The 2MASS source is 6" away from the coordinates adopted here.
Serp SMM 5        The 2MASS source is 4" away from the coordinates adopted here.
Serp-SMM 3        The flux at 3.4mm measured in the small aperture was not used.
Serp-SMM 2        The upper limits at long wavelengths are taken within small apertures and hence do not contradict the fluxes.
IRAS 18331-0035   The 1.3mm flux taken in a 11" aperture was excluded. The 2MASS source is 3" away from the coordinates adopted here.
HH 108 MMS        The 1.3mm flux taken in a 11" aperture was excluded.
G34.24+0.13MM     The 2MASS source is 5" away from the coordinates adopted here.
IRAS 19156+1906   The large flux at 1.3mm given by Cabrit and Andre (1991ApJ...379L..25C) was excluded. Also all data taken in apertures larger than 100", as well as the other large flux taken at 1.3mm were not used.
IRAS 19180+1114   The 2MASS source is 3" away from the coordinates adopted here.
R CrA R1          The 2MASS source is 5" away from the coordinates adopted here.
IRAS 19345+0727   IRAS 19345+0727 shows a large scatter in the sub-mm fluxes. We did not use the data taken in apertures larger than 120".
IRAS 20050+2720   The 2MASS source is 2.5" away from the coordinates adopted here.
IRAS 20386+6751   The sub-mm data taken in apertures larger than 60" were excluded. There is large scatter in the sub-mm data.
IRAS 21017+6742   Sub-mm fluxes measured in the 120" apertures are excluded. There is a large scatter in the sub-mm data.
CB 230            The 2MASS source is 2" away from the coordinates adopted here.
L944 SMM 1        The sub-mm fluxes measured in the 50" apertures by Visser et al. (2002AJ....124.2756V) are used.
IC 1396 W         The IRAS data might be confused by other cold dust in the vicinity.
CB 232            This is a double source consisting of CB232SMM1 and SMM2. SMM1 is much brighter in the sub-mm. Hence, all data are attributed to this object. The 2MASS source is 6" away from the coordinates adopted here.
NGC 7129 FIRS 2   From the 1.3mm points we chose the 1.49Jy, since all the others contradict significantly with the data taken at nearby wavelengths.
L1251 B           Data taken in the 120" apertures are excluded.
L1211             These are several (at least four) sources. Also there are no sub-mm data. The ISO data represent the object MMS4, while the IRAS source might include all objects (MMS1, 2, 3, and 4). The ISO data were used and the IRAS points are excluded. The 2MASS source is 6" away from the coordinates adopted here.
Cep E-MM          This is a double source with a separation of 1.4". The flux of Moro-Martin et al. (2001ApJ...555..146M) at 1.3mm is not used due to the small aperture.
NGC 7538 S        The 2MASS source is 3" away from the coordinates adopted here.
L1246 SMM 1       The sub-mm fluxes taken in the 50" apertures by Visser et al. (2002AJ....124.2756V) are used.
IRAS 23238+7401   The 120" aperture measurments are excluded.