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Table 3

Sources detected in the CALYPSO millimeter continuum maps.

Source α2000 δ2000 Source a Other
nature names
(h:m:s) (°:′:′′) (mJy beam−1) [au]
[1] [2] [3] [4] [5] [6] [7] [8]
L1448-2A 03:25:22.405 30:45:13.26 23 ± 2 5.8 ± 1 Primary protostar Per-emb-22A
L1448-2Ab 03:25:22.360 30:45:13.20 11 ± 1 4.5 ± 2a CE protostar ? 130 Per-emb-22B
               
L1448-NA 03:25:36.498 30:45:21.85 46 ± 4 6.7 ± 0.3 CE Class I 1700 L1448-IRS3A
L1448-NB1 03:25:36.378 30:45:14.77 146 ± 6 69 ± 2 primary protostar L1448-IRS3B
L1448-NB2 03:25:36.315 30:45:15.15 69 ± 3 <25 ± 5a CE protostar ? 210 L1448-IRS3B-a
L1448-NW 03:25:35.670 30:45:33.86 6.4 SE protostar 4900 L1448-IRS3C
               
L1448-C 03:25:38.875 30:44:05.33 123 ± 5 19 ± 1 Primary protostar L1448-mm
L1448-CS 03:25:39.132 30:43:58.04 8 ± 2 1.6 ± 0.1 CE Class I 1900
               
IRAS2A1 03:28:55.570 31:14:37.07 132 ± 5 20 ± 1 Primary protostarb Per-emb-27
               
SVS13B 03:29:03.078 31:15:51.74 127 ± 7 22 ± 1 Primary protostar
SVS13A 03:29:03.756 31:16:03.80 120 ± 7 21 ± 1 SE Class I 2330
SVS13C 03:29:01.980 31:15:38.14 5.8 ± 2 SE protostar 3550
VLA3 03:29:03.378 31:16:03.33 9 ± 1 2.6 ± 0.5 unknown 1390 A2
               
IRAS4A1 03:29:10.537 31:13:30.98 481 ± 10 148 ± 6 Primary protostarb Per-emb-12
IRAS4A2 03:29:10.432 31:13:32.12 186 ± 8 <34 ± 10a CE protostar 420
               
IRAS4B 03:29:12.016 31:13:08.02 278 ± 6 75 ± 3 Primary protostar Per-emb-13
IRAS4B2 03:29:12.841 31:13:06.84 114 ± 4 31 ± 1 SE protostar ? 2500 IRAS 4BII
               
IRAM04191 04:21:56.899 15:29:46.11 4.7 ± 0.8 0.31 ± 0.09 Primary protostar
               
L1521F 04:28:38.941 26:51:35.14 1.6 ± 0.2 0.27 ± 0.05 Primary protostar MC27
               
L1527 04:39:53.875 26:03:09.66 129 ± 8 23 ± 1 Primary protostar
               
SerpM-S68N 18:29:48.091 01:16:43.41 35 ± 3 5.3 ± 0.5 Primary protostar Ser-emb8
SerpM-S68Nb 18:29:48.707 01:16:55.53 2.9 ± 0.4 SE protostar 6400 Ser-emb8(N)
SerpM-S68Nc 18:29:48.811 01:17:04.24 2.7 ± 0.5 SE Class I ? 9700
               
SerpM-SMM4a 18:29:56.716 01:13:15.65 184 ± 11 48 ± 2 Primary protostar
SerpM-SMM4b 18:29:56.525 01:13:11.58 27 ± 4 9 ± 1 CE protostar ? 2000
               
SerpS-MM18a 18:30:04.118 −02:03:02.55 148 ± 9 20 ± 1 Primary protostar CARMA-7
SerpS-MM18b 18:30:03.541 −02:03:08.33 62 ± 4 7.8 ± 0.8 CE protostar ? 2600 CARMA-6
               
SerpS-MM22 18:30:12.310 −02:06:53.56 20 ± 2 2.8 ± 0.7 Primary protostar
               
L1157 20:39:06.269 68:02:15.70 117 ± 9 18 ± 1 Primary protostar
               
GF9-2 20:51:29.823 60:18:38.44 9.9 ± 1 1.6 ± 0.4 Primary protostar L1082 C

Notes. Column 1: name of the primary protostar and its individual mm components. Columns 2 and 3: equatorial coordinates of the dust continuum peak position in the CALYPSO 231 GHz maps. Columns 4 and 5: 231 and 94 GHz dust continuum peak flux densities in the PdBI synthesized beams reported in Table 2. Column 6: putative nature of the source (see Sect. 5.3 and comments on individual sources in Appendix C). SE is used for a candidate protostellar companion with a separate envelope, and CE is used when the (candidate) protostellar companion is within a common envelope with the primary protostar. We use the sizes computed from single-dish observations (see “Single-dish constraints” in Appendix C) as envelope radii. Column 7: projected separation (in the plane of the sky) between the secondary and the primary protostar, translated into physical units using the distances reported in Table 1. Column 8: other names used in the literature for the associated object (when previously reported). (a)Unresolved from the primary source because of the larger 94 GHz synthesized beam: the measured peak flux is largely contaminated by the flux belonging to the primary source. (b)IRAS4A3 (Santangelo et al. 2015), as well as IRAS2A2 and IRAS2A3 (Maury et al. 2014; Codella et al. 2014b), are not reported here as individual sources (see Sect. 5.3 for further details). A secondary source 0.4′′ south of IRAS2A is detected with VLA (Tobin et al. 2015a) and ALMA (Maury et al., in prep.) but is not detected with our CALYPSO data because the high-resolution data for IRAS2A was obtained prior to the CALYPSO program (see Appendix C.4).

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