Table 2
Properties of the protostellar objects found within the N2H+ and HC3N maps.
| Source | RA | Dec | Other names | Class(a) | Multiple? (b) | υLSR (C) | Outflow PA (d) | Disk i(e) |
|---|---|---|---|---|---|---|---|---|
| (J2000) | (J2000) | (km s−1) | (º) | (º) | ||||
| IRAS4A | 03:29:10.54 | +31:13:30.93 | Per-emb 12 | 0 | Y | 6.9 ± 0.005(1) | 19(6) | 35 |
| IRAS4B | 03:29:12.02 | +31:13:08.03 | Per-emb 13 | 0 | Y | 7.1 ± 0.009(1) | 176(6) | 49 |
| Per-emb-14 | 03:29:13.55 | +31:13:58.15 | NGC 1333 IRAS4C | 0 | N | 7.9 ± 0.03(1) | 96(7) | 64 |
| Per-emb-15 | 03:29:04.06 | +31:14:46.24 | RNO15-FIR, SK 14 | 0 | N | 6.8 ± 0.01(1) | −35(5) | |
| Per-emb-27 | 03:28:55.57 | +31:14:37.03 | NGC 1333 IRAS2A | 0/I | Y | 8.1 ± 0.02(1) | 105(5,ƒ) | |
| Per-emb-36 | 03:28:57.37 | +31:14:15.77 | NGC 1333 IRAS2B | I | Y | 6.9 ± 0.02(1) | 24(5) | |
| Per-emb-44 | 03:29:03.76 | +31:16:03.81 | SVS13A | 0/I | Y | 8.7 ± 0.02(1) | 140(8) | |
| SVS13C | 03:29:01.97 | +31:15:38.05 | 0 | Y | 8.9 ± 0.02(1) | 8(8) | 75 | |
| SVS13B | 03:29:03.08 | +31:15:51.74 | 0 | Y | 8.5 ± 0.01(1) | 170(6) | 61 | |
| IRAS4B2 | 03:29:12.84 | +31:13:06.89 | NGC 1333 IRAS4B' | 0 | Y | −99(9) | ||
| EDJ2009-183 | 03:28:59.30 | +31:15:48.41 | ASR 106 | Flat | Y | 8.69(2) | ||
| EDJ2009-173 | 03:28:56.96 | +31:16:22.20 | ASR 118, SVS15 | II | N | 9.08(2) | ||
| VLA3 | 03:29:03.00 | +31:16:02.00 | 0 | |||||
| SK 15 | 03:29:06.50 | +31:15:38.60 | ASR 6, HRF 50 | I | 7.95(3) | |||
| ASR 3 | 03:29:02.16 | +31:16:11.40 | [GMM2008] 76 | II | ||||
| ASR 53 | 03:29:02.16 | +31:16:11.40 | [GMM2008] 89 | II | 13.5 ± 3.4(4) | |||
| ASR 54 | 03:29:09.41 | +31:14:14.10 | [GMM2008] 135 | II |
Notes. We only describe the properties of protostars in regions with HC3N emission or in which the outflow lobe is within the HC3N emission map.(a)SED classification from the literature (Enoch et al. 2009; Evans et al. 2009). We also indicate when a source is Class 0/I according to the classification in the VANDAM sample (Tobin et al. 2018). (b)Y if the source contains more than one protostar, N if it is single (Tobin et al. 2018). (c)Obtained from available molecular tracer observations of cores or from spectroscopic surveys. (d)Angle of the red lobe from north to east. (e)Disk inclination with respect to the plane of the sky from Segura-Cox et al. (2018). (ƒ)IRAS 2A contains two outflows that are perpendicular to each other. We list the most strongly collimated outflow, where the red lobe is included in the footprint of our HC3N data.
References. (1) Stephens et al. (2019), (2) Foster et al. (2015), (3) Imai et al. (2018), (4) Kounkel et al. (2019), (5) Stephens et al. (2017), (6) Lee et al. (2016), (7) Zhang et al. (2018), (8) Plunkett et al. (2013), (9) Podio et al. (2021)
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