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).