Table 1
Characteristics of the full sample.
| Name | α (J2000) | δ (J2000) | Cloud | Distance | Menv | References |
|---|---|---|---|---|---|---|
| (pc) | ||||||
| Per B1-bS (a) | 03:33:21.35 | +31:07:26.4 | Perseus/Barnard | 230 | 3.0 | [2, 12] |
| Per B1-c (a) | 03:33:17.88 | +31:09:32.0 | Perseus/Barnard | 230 | 2.1 | [2, 11] |
| B335 | 19:37:00.90 | +07:34:09.6 | isolated | 100 | 1.3 (b) | [3, 15] |
| BHR7-MMS (a) | 08:14:23.33 | −34:31:03.7 | Gum/Vela | 400 | 1.0 | [5, 13] |
| CB230 | 21:17:40.00 | +68:17:32.0 | Cepheus | 352 | 3.4 | [4, 14] |
| HH25-MMS (a) | 05:46:07.40 | −00:13:43.4 | Orion/L1630 | 400 | 0.5 | [6, 16] |
| HH211-mm (a) | 03:43:56.52 | +32:00:52.8 | Perseus/IC348 | 320 | 1.5 | [1, 16] |
| HH212* | 05:43:51.40 | −01:02:53.0 | Orion/L1630 | 400 | 0.2 | [6, 17] |
| HH797 | 03:43:57.10 | +32:03:05.6 | Perseus/IC348 | 320 | 1.1 | [1, 19] |
| IRAS03282 | 03:31:20.40 | +30:45:24.7 | Perseus | 293 | 2.2 | [1, 18] |
| IRAS16293-A | 16:32:22.9 | −24:28:36.0 | Ophiuchus | 150 | 2.3 | [8, 16] |
| L1157 | 20:39:06.3 | +68:02:15.8 | Cepheus | 352 | 3.0 | [4, 10] |
| L1448C | 03:25:38.9 | +30:44:05.4 | Perseus | 293 | 2.0 | [1, 10] |
| L1448N-B | 03:25:36.3 | +30:45:14.9 | Perseus | 293 | 4.8 | [1, 10] |
| L1448-2A | 03:25:22.4 | +30:45:13.0 | Perseus | 293 | 1.9 | [1, 10] |
| L483-mm (a) | 18:17:29.94 | −04:39:39.3 | Serpens Cirrus | 250 | 1.8 | [7, 18] |
| NGC 1333 IRAS4A | 03:29:10.5 | +31:13:31.0 | Perseus | 293 | 12.3 | [1, 10] |
| NGC 1333 IRAS4B | 03:29:12.0 | +31:13:08.0 | Perseus | 293 | 4.7 | [1, 10] |
| Serpens South MM18 (a) | 18:30:04.12 | −02:03:02.55 | Serpens South | 350 | 5 | [9, 10] |
| SVS13-B | 03:29:03.1 | +31:15:52:0 | Perseus | 293 | 2.8 | [1, 10] |
Notes. (a) These are the sources whose SMA polarization observations are described in this paper. The polarization results for the rest of the sources are described in Galametz et al. (2018), Girart et al. (2014) and Rao et al. (2009). (b) The total globule mass is probably a factor of 3–5 larger (Stutz et al. 2008).
References. References for the distances and Menv : [1] Ortiz-León et al. (2018a), [2] Černis & Straižys (2003), [3] Olofsson & Olofsson (2009), [4] Zucker et al. (2019), [5] Woermann et al. (2001), [6] Anthony-Twarog (1982) [7] Herczeg et al. (2019) [8] Ortiz-León et al. (2018b), [9] on-going work re-analyzing the Gaia data toward Serpens South suggests a large extinction layer up to distances of 350 pc (Palmeirim, André et al., in prep.). We use this re-evaluated distance. [10] Maret et al. (2020), [11] Matthews et al. (2006), [12] Andersen et al. (2019), [13] Tobin et al. (2018), [14] Massi et al. (2008), [15] Launhardt et al. (2013), [16] André et al. (2000), [17] Wiseman et al. (2001), [18] Tobin et al. (2011), [19] Sadavoy et al. (2014).
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