Table 4
Properties of the dust continuum emission from the primary sources in our sample: PdBI data and single-dish observations.
| PdBI | Single dish | Single-dish fluxes | |||||||||||||
|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|---|
| 231 GHz | 94 GHz | extrapolated to 231 GHz | |||||||||||||
| Source | Fint | F20 k λ |  |
 / |
Fint | F20 k λ | α20 k λ | Frequency | Integrated flux | Peak flux | Ref. |  |
 |
||
| (mJy) | (mJy) | (K) | (mJy) | (mJy) | (GHz) | (mJy) | Rint (′′) | (mJy beam−1) | θ (′′) | (mJy) | (mJy beam−1) | ||||
| [1] | [2] | [3] | [4] | [5] | [6] | [7] | [8] | [9] | [10] | [11] | [12] | [13] | [14] | [15] | [16] |
| L1448-2A | 129 ± 18 | 141 ± 14 | 2 | 0.03 | 13 ± 2 | 8 ± 1 | 3.1 ± 0.3 | 268 | 930 | 20 | 730 | 31 | (1) | 580 | 450 |
| L1448-NB1 | 763 ± 50 | 713 ± 40 | 13 | 0.20 | 89 ± 8 | 72 ± 6 | 2.6 ± 0.2 | 243 | 3700 | 20 | 1400 | 12 | (2) | 3240 | 1160 |
| L1448-C | 178 ± 13 | 215 ± 20 | 11 | 0.16 | 20 ± 4 | 21 ± 3 | 2.6 ± 0.3 | 243 | 910 | 14 | 620 | 12 | (2) | 827 | 560 |
| IRAS2A | 386 ± 36 | 420 ± 32 | 12 | 0.13 | 43 ± 6 | 31 ± 5 | 2.9 ± 0.3 | 243 | – | – | 875 | 12 | (2) | 780 | – |
| SVS13B | 318 ± 20 | 269 ± 21 | 12 | 0.23 | 43 ± 4 | 29 ± 4 | 2.5 ± 0.3 | 243 | – | – | 900 | 11 | (3) | 817 | – |
| IRAS4A1 | 2710 ± 110 | 2978 ± 90 | 44 | 0.7 | 314 ± 19 | 253 ± 16 | 2.7 ± 0.2 | 243 | – | – | 4100 | 12 | (2) | 3260 | – |
| IRAS4B1 | 937 ± 90 | 1310 ± 80 | 25 | 0.5 | 127 ± 16 | 128 ± 10 | 2.6 ± 0.2 | 243 | – | – | 1470 | 12 | (2) | 1290 | – |
| IRAM04191 | 4.5 ± 1.3 | 5.2 ± 0.9 | 0.4 | 0.013 | 0.3 ± 0.1 | 0.3 ± 0.1 | 3.0 ± 0.4 | 243 | 650 | 30 | 110 | 11 | (2) | 585 | 99 |
| L1521F | 3.7 ± 1 | 6.4 ± 1 | 0.14 | 0.05 | 0.2 ± 0.08 | 0.45 ± 0.09 | 2.9 ± 0.4 | 243 | – | – | 120 | 14 | (4) | – | 95 |
| L1527 | 220 ± 18 | 262 ± 14 | 12 | 0.20 | 27 ± 3 | 26 ± 3 | 2.6 ± 0.2 | 243 | 1500 | 30 | 375 | 12 | (2) | 1350 | 340 |
| SerpM-S68N | 111 ± 8 | 208 ± 9 | 3 | 0.05 | 10 ± 2 | 10 ± 3 | 3.3 ± 0.3 | 243 | 1030 | 15 | 550 | 11 | (8) | 870 | 465 |
| SerpM-SMM4 | 596 ± 50 | 620 ± 40 | 17 | 0.35 | 60 ± 8 | 60 ± 6 | 2.6 ± 0.2 | 243 | 2550 | 20 | 1000 | 11 | (8) | 2192 | 840 |
| SerpS-MM18 | 453 ± 55 | 483 ± 45 | 13 | 0.17 | 46 ± 6 | 29 ± 3 | 3.1 ± 0.2 | 243 | 2505 | 9 | 1376 | 12 | (5) | 2180 | 1230 |
| SerpS-MM22 | 30 ± 4 | 50 ± 7 | 1.8 | 0.05 | 3.3 ± 0.9 | 3.5 ± 0.8 | 3.0 ± 0.3 | 243 | 261 | 10 | 129 | 12 | (5) | 225 | 111 |
| L1157 | 262 ± 15 | 260 ± 18 | 11 | 0.20 | 34 ± 3 | 24 ± 3 | 2.6 ± 0.3 | 243 | – | – | 630 | 12 | (2) | 569 | – |
| GF9-2 | 13 ± 3 | 13 ± 3 | 1 | 0.02 | 1.7 ± 0.8 | 2.0 ± 0.8 | 2.1 ± 0.3 | 243 | 315 | 35 | 60 | 12 | (7) | 291 | 55 |
Notes. Column 1: primary protostar name. Columns 2 and 6: PdBI integrated fluxes (integrated above the 5σ level in the clean maps) at 231 and 94 GHz, respectively. Columns 3 and 7: visibility fluxes at 20 kλ (shortest common baseline for the 94 and 231 GHz data), averaged in a 20k λ baseline bin centered at 20 kλ that we used to compute thespectral index 
, given in Col. 8. This reflects the properties of dust emission at the largest envelope scales probed by the PdBI observations at 231 GHz (~ 10′′). We note that the 231 GHz visibility fluxes shown here stem from the 231 GHz data alone, before they were merged with the rescaled 219 GHz data (making use of the α20 kλ). Column 4: brightness temperature from the peak flux at 231 GHz. Column 5: ratio TB /Tdust at 0.5′′ scales (using Eq. (2) for Tdust with r the physical radius probed by the synthesized beam) indicative of the optical thickness of the continuum emission at the smallest scales probed in our study. Column 9: frequency of the single-dish observations used to extrapolate the envelope-scale fluxes (zero spacing). Column 10: single-dish integrated flux at the frequency indicated in Col. 9. Column 11: angular radius of the area used to compute the integrated envelope flux in single-dish maps. Column 12: single-dish peak flux at the frequency indicated in Col. 9. Column 13: FWHM of the single-dish beam used to compute the peak flux in single-dish maps. Column 15: envelope-integrated dust continuum flux from the single-dish maps, extrapolated to 231 GHz in order to be used as zero-spacing constraint in our modeling. Column 16: envelope dust continuum flux at the scale that the single-dish beam probes, extrapolated to 231 GHz in order to be used as either zero-spacing constraint in our modeling (if the source is unresolved by single-dish observations) or as an additional point at the equivalent baseline.
References. Reporting the single-dish observations. (1) Enoch et al. (2007) CSO Bolocam 1.1 mm; (2) Motte & André (2001) IRAM-30 m-MPIfR arrays 1.3 mm; (3) Chini et al. (1997) IRAM-30 m MPIfR array 1.3 mm; (4) Crapsi et al. (2004) IRAM-30 m MAMBO II 1.3 mm; (5) Maury et al. (2011) IRAM-30 m MAMBO II 1.3 mm; (6) Wiesemeyer (1997) IRAM-30 m MPIfR array 1.3 mm; (7) Kaas et al. (2004) IRAM-30 m MPIfR array 1.3 mm.
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