Notes. ^(a) Peak position of CALYPSO 1.3 mm continuum emission as derived by Maury et al. (2019). ^(b) Distance to the hosting cloud. ^(c)Position angle of the outflow derived from the CALYPSO molecular line emission maps. ^(d) Bolometric temperature. ^(e)Internal luminosity. The L_int were calculated from the analysis of the Herschel maps from the Herschel Gould Belt survey (André et al. 2010; Ladjelate, in prep.) and rescaled to the distances used in this analysis. ^(f) Envelope mass. The M_env were rescaled to the distances used in this analysis. ^(g)A mean distance of 436 pc for the Serpens Cloud has been determined by Ortiz-León et al. (2018b) using the Gaia-DR2 results and seems to correspond to the average distance determined from the Main cloud or the star-forming region W40. Ongoing work reanalyzing the Gaia data toward Serpens South seems, however, to suggest a first layer of extinction around 300–350 pc while its associated young stellar objects could be distributed in a larger extinction layer up to distances of 350 pc (Palmeirim et al., in prep.). We use this new distance for the paper. As we are working on flux ratios, this does not affect the slope we present for SerpS-MM18. This, however, has an impact on the envelope mass discussed in Sect. 6, which would be higher by a factor of 1.6 if the distance is 436 pc.

References. ⁽¹⁾ Ortiz-León et al. (2018a), ⁽²⁾ Ortiz-León et al. (2018b), ⁽³⁾ Torres et al. (2009), ⁽⁴⁾ Zucker et al. (2019). ⁽⁵⁾ Podio & CALYPSO (in prep.) and Maury et al. (2019). ⁽⁶⁾Motte & André (2001), ⁽⁷⁾Enoch et al. (2011), ⁽⁸⁾Kristensen et al. (2012), ⁽⁹⁾Maury et al. (2011), ⁽¹⁰⁾Tobin et al. (2016), ⁽¹¹⁾Sadavoy et al. (2014), ⁽¹²⁾Enoch et al. (2009), ⁽¹³⁾Chini et al. (1997), ⁽¹⁴⁾Karska et al. (2013), ⁽¹⁵⁾Motte & André (2001), ⁽¹⁶⁾Kaas et al. (2004), ⁽¹⁷⁾Maury et al. (2011), and ⁽¹⁸⁾Sadavoy et al. (2014).