Table 1
Summary of analyzed ALMA observations.
| Name | θres (a) | σI (b) | σP (b) |  (c) |
λ | Pfrac,max (d) | MRS (e) | Reference (f) |
|---|---|---|---|---|---|---|---|---|
| (au) |  |
 |
(1023 cm−2) | (mm) | (103au) | |||
| Serpens Emb 6 | 161 | 0.05 | 0.060 | 0.46–67 | 0.87 | 19% ± 4 | 2.5 | Hull et al. (2017b) |
| Serpens Emb 8 | 161 | 0.07 | 0.025 | 0.11–9.7 | 0.87 | 42% ± 9 | 2.5 | Hull et al. (2017a) |
| Serpens Emb 8(N) | 161 | 0.08 | 0.035 | 0.28–8.7 | 39% ± 11 | Le Gouellec et al. (2019) | ||
| BHR71 IRS1 | 200 | 0.30 | 0.025 | 0.13–14 | 1.3 | 24% ± 5 | 4.3 | Hull et al. (2020) |
| BHR71 IRS2 | 200 | 0.15 | 0.025 | 0.071–14 | 19% ± 4 | |||
| 101 | 0.06 | 0.002 | 0.063–3.7 | 1.3 | 26% ± 6 | 2.2 | Maury et al. (2018), | |
| B335 | 48 | 0.04 | 0.010 | 0.15–5.7 | 1.5 | 25% ± 7 | 0.7 | Maury et al. (in prep.) |
| 122 | 0.03 | 0.005 | 0.17–3.1 | 3.0 | 30% ± 7 | 3.0 | ||
| IRAS 16293A/B | 36 | 0.28 | 0.025 | 0.73–61 | 1.3 | 35% ± 7 | 0.59 | Sadavoy et al. (2018b) |
| VLA 1623A/B | 34 | 0.09 | 0.027 | 0.84–59 | 1.3 | 21% ± 7 | 0.62 | Sadavoy et al. (2018a) |
| L1448 IRS2 | 134 | 0.85 | 0.020 | 0.21–4.8 | 1.3 | 32% ± 6 | 1.5 | Kwon et al. (2019) |
| OMC3 MMS6(g) | 56 | 0.23 | 0.022 | 3.7–145 | 1.3 | 24% ± 5 | 0.43 | Takahashi et al. (2019) |
| 12 | 0.08 | 0.020 | 43–167 | 24% ± 4 | 0.095 | |||
| IRAS4A | 112 | 0.4 | 0.045 | 0.87–62 | 1.3 | 41% ± 8 | 1.2 | Ko et al. (2020) |
| 47 | 0.50 | 0.046 | 1.7–65 | 0.87 | 36% ± 7 | 0.8 | ||
Notes. This table presents the details of the ALMA observations. For further information about the individual sources, see Table B.1. (a) Angular resolution in au. We took the effective synthesized beam size (where the beam is the resolution elements) of the ALMA maps. (b) rms noise in the maps of total intensity I and polarized intensity P. (c) Typical H2 column densities probed in the protostellar envelope by the ALMA observations, selecting the pixels with total intensity values greater than 5 times the rms noise in the Stokes I map. The column density of each pixel was derived following the method described in Sect. 2.2. Each pointing in BHR 71 contains both of the components of the wide binary. Thus, the corresponding ranges in column density include all emission from both BHR 71 IRS1 and IRS2. (d)The maximum value of polarization fraction in the core, selecting the pixels with total intensity values greater than 5 times the rms noise in the Stokes I map. (e) Maximum recoverable scale. (f) Reference of the publication(s) presenting the corresponding ALMA polarization dataset(s). (g) Takahashi et al. (2019) presented the ALMA observations of OMC3 MMS6 in two separate datasets, as the angular resolutions of the two datasets were very different, and thus probe distinct regions of the envelope.
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