Table A.1
Upper limits on the contribution to the 1.3 and 3.2 mm emission not coming from thermal dust emission.
| Name | αff+s (a) | Flux at 200 kλ | Contribution | Flux at 200 kλ | Contribution | References |
|---|---|---|---|---|---|---|
| at 1.3 mm | at 1.3 mm | at 3.2 mm | at 3.2 mm | |||
| (mJy) | (%) | (mJy) | (%) | |||
| NGC 1333-IRAS 2A1 | 1.1 | 85 | 4.5 | 13 | 11 | 1 |
| NGC 1333-IRAS 4A1 | 1.1 | 310 | 3.8 | 47 | 9.1 | 3 |
| NGC 1333-IRAS 4B | 0.5 | 196 | 0.2 | 20 | 1.4 | 3 |
| L1448-2A | 0.5 | 28 | 4.0 | 3.9 | 18 | 3 |
| L1448-C | 1.0 | 102 | 2.9 | 18 | 6.7 | 3 |
| L1448-NB1 | 0.3 | 82 | 3.6 | 13 | 14 | 2, 4 |
| SVS13B | 0.8 | 72 | 6.9 | 12 | 19 | 5 |
| L1527 | 0.3 | 136 | 1.7 | 19 | 9.3 | 6 |
| SerpM-S68N | 0.6 | 45 | 0.9 | 3.4 | 6.8 | 7, 8 |
| SerpM-SMM4 | 1.1 (f) | 46 | 9.6 | 8.7 | 19 | 8 |
| SerpS-MM18 | 1.1 (f) | 97 | 3.6 | 8.2 | 16 | 9 |
| L1157 | 0.3 | 103 | 0.5 | 12.6 | 3.2 | 10 |
Notes. (a) As in Tobin et al. (2015), the spectral slopes αff+s are defined by Fν = 
, with λ0 = 1 mm. (f) indicates when αff+s has been fixed to 1.1.
References. For the centimeter fluxes used to estimate the free–free+synchrotron contribution: [1] Tobin et al. (2015), [2] Reipurth et al. (2002), [3] Tychoniec et al. (2018b), [4] Curiel et al. (1990), [5] Rodríguez et al. (1997), [6] Melis et al. (2011), [7] McMullin et al. (1994), [8] Eiroa et al. (2005), [9] Kern et al. (2016), [10] Meehan et al. (1998).
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