Notes. ^(a) Name of the protostars with the multiple components resolved by the 1.3 mm continuum emission from PdBI observations (Maury et al. 2019). ^(b) Coordinates of the continuum emission peak at 1.3 mm from Maury et al. (2019). ^(c) Distance assumed for the individual sources. We adopt a value of 140 pc for the Taurus distance estimated from a VLBA measurement (Torres et al. 2009). The distances of Perseus and Cepheus are taken following recent Gaia parallax measurements that have determined a distance of (293 ± 20) pc (Ortiz-León et al. 2018)and (352 ± 18) pc (Zucker et al. 2019), respectively. We adopt a value of 200 pc for the GF9-2 cloud distance (Wiesemeyer 1997; Wiesemeyer et al. 1998) but this distance is very uncertain and some studies estimated a higher distance between 440–470 pc (Viotti 1969, C. Zucker, priv. comm.) and 900 pc (Reid et al. 2016). ^(d) Internal luminosities which come from the analysis of Herschel maps from the Gould Belt survey (HGBS, André et al. 2010 and Ladjelate et al., in prep.) and corrected by the assumed distance. ^(e) Envelope mass corrected by the assumed distance. ^(f)Outer radius of the individual protostellar envelope determined from dust continuum emission, corrected by the assumed distance. We adopt the radius from PdBI dust continuum emission (Maury et al. 2019) when we do not have any information on the 30m continuum from Motte & André (2001) and for IRAS4A which is known to be embedded into a compressing cloud (Belloche et al. 2006). ^(g) Position angle of the blue lobe of the outflows estimated from CALYPSO PdBI ¹²CO and SiO emission maps (Podio & CALYPSO, in prep.). PA is defined east from north. Sources indicated with ^(⋆) have an asymmetric outflow and the position angles of both lobes are reported. For IRAS2A, IRAS4A, and L1157, previous works done by Codella et al. (2014b), Santangelo et al. (2015), and Podio et al. (2016), respectively, show a detailed CALYPSO view of the jets. For L1521F, we use the PA estimated by Tokuda et al. (2014, 2016). ^(h) Inclination angle of the equatorial plane with respect to the line of sight. Sources indicated with ^(⋆⋆) have an inclination angle not well constrained, so we assumed a default value of (30 ± 20)°. ⁽ⁱ⁾ References for the protostar discovery paper, the envelope mass, the envelope radius and then the inclination are reported here.

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