Table 2
Parameters of the sources detected with the SMA at 1.3 mm dust continuum emission.
| Positiona | Deconv. ang. sizea | PAa |  a |
Sνb | Massc | |||
|---|---|---|---|---|---|---|---|---|
| Source | α(J2000) | δ(J2000) |  |
(°) | (mJy beam−1) | (mJy) | (M⊙) | Associationd |
| SMA1 | 00:36:47.366 | 63:29:02.237 | 1.6 ± 0.3 × 0.9 ± 0.2 | 8 ± 15 | 13.84 ± 1.72 | 41.4 ± 8.3 | 0.69 | CM:VLA 3/IR:IRAS |
| SMA3a | 00:36:46.860 | 63:28:59.414 | 1.2 ± 0.2 × 0.6 ± 0.1 | − 44 ± 8 | 4.71 ± 0.28 | 9.2 ± 1.9 | 0.15 | – |
| SMA3b | 00:36:46.562 | 63:28:58.040 | 0.9 ± 0.3 × 0.6 ± 0.2 | − 69 ± 31 | 6.45 ± 0.66 | 11.1 ± 2.3 | 0.19 | IR:RNO1C |
| SMA3c | 00:36:46.761 | 63:28:57.583 | 1.9 ± 0.4 × 0.6 ± 0.1 | − 9 ± 6 | 8.72 ± 0.85 | 24.7 ± 5.0 | 0.41 | CM:VLA 1 |
| SMA3d | 00:36:46.387 | 63:28:57.326 | Point source | – | 5.93 ± 0.24 | 11.0 ± 2.2 | 0.18 | – |
| SMA3e | 00:36:46.198 | 63:28:56.829 | 0.6 ± 0.1 × 0.5 ± 0.1 | − 77 ± 29 | 6.24 ± 0.35 | 8.6 ± 1.8 | 0.14 | – |
| SMA3f | 00:36:46.348 | 63:28:55.930 | 1.0 ± 0.3 × 0.6 ± 0.1 | − 25 ± 11 | 4.74 ± 0.10 | 8.6 ± 1.8 | 0.14 | – |
| SMA3g | 00:36:46.450 | 63:28:54.966 | 1.5 ± 0.3 × 0.4 ± 0.2 | − 70 ± 10 | 5.72 ± 0.36 | 13.0 ± 2.7 | 0.22 | – |
| SMA3h | 00:36:46.330 | 63:28:54.583 | Point source | – | 5.41 ± 0.39 | 7.3 ± 1.5 | 0.12 | – |
| SMA3i | 00:36:46.606 | 63:28:54.248 | 2.0 ± 0.6 × 0.6 ± 0.2 | − 13 ± 8 | 6.22 ± 0.58 | 18.4 ± 3.8 | 0.31 | – |
| SMA5a | 00:36:46.000 | 63:28:52.704 | 1.1 ± 0.3 × 0.5 ± 0.2 | − 64 ± 17 | 4.50 ± 0.42 | 8.3 ± 1.7 | 0.14 | IR:RNO1B |
| SMA5b | 00:36:46.255 | 63:28:52.307 | 0.9 ± 0.2 × 0.1 ± 0.1 | − 16 ± 8 | 5.63 ± 0.46 | 7.6 ± 1.6 | 0.13 | – |
| SMA6a | 00:36:46.584 | 63:28:49.613 | 1.5 ± 0.3 × 0.9 ± 0.2 | − 82 ± 22 | 8.50 ± 0.11 | 25.7 ± 5.2 | 0.43 | – |
| SMA6b | 00:36:46.936 | 63:28:47.078 | 0.7 ± 0.1 × 0.2 ± 0.1 | − 28 ± 8 | 4.96 ± 0.24 | 6.5 ± 1.3 | 0.11 | – |
Notes. (a) Position, deconvolvedsize, position angle (PA), peak intensity, flux density and the respective uncertainties derived from fitting a 2D Gaussian to each source using IMFIT task from MIRIAD. (b) Error in flux density has been calculated as 
(Beltrán et al. 2001; Palau et al. 2013), where σ is the rms of the map, θsource and θbeam are the size of the source and the beam, respectively, and σflux-scale is the error in the flux scale, which takes into account the uncertainty on the calibration applied to the flux density of the source (Sν × %uncertainty) which we assumed to be 20%. (c)Masses derived assuming a dust temperature of 22 K, and a dust (+gas) mass opacity coefficient at 1.3 mm of 0.9 cm2 g−1 (for thin ice mantles after 105 yr of coagulation at a gas density of 106 cm−3, Ossenkopf & Henning 1994). The uncertainty in the masses due to the opacity law and temperature is estimated to be a factor of 4. (d) Association with signposts of stellar activity: IR = infrared source; CM = Centimeter radio source. IRAS refers to IRAS 0038 + 6312.
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