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Table 1

CALYPSO sample of target protostars.

Protostar Distance Lint Menv Outflow PA References
(pc) (L) (M) (°)
[1] [2] [3] [4] [5] [6]
L1448-2A 235 3.0 1.2 −63 O’Linger et al. (1999)/Enoch et al. (2009)
L1448-NB 235 2.5 3.1 −80 Curiel et al. (1990)/Sadavoy et al. (2014)
L1448-C 235 7.0 1.3 −17 Anglada et al. (1989)/Sadavoy et al. (2014)
IRAS2A 235 30 5.1 +205 Jennings et al. (1987)/Karska et al. (2013)
SVS13B 235 2.0 1.8 +167 Grossman et al. (1987)/Chini et al. (1997)
IRAS4A 235 3.0 7.9 +180 Jennings et al. (1987)/Sadavoy et al. (2014)
IRAS4B 235 1.5 3.0 +167 Jennings et al. (1987)/Sadavoy et al. (2014)
IRAM04191 140 0.05 0.5 +200 André et al. (1999)/André et al. (2000)
L1521F 140 0.035 0.7–2 +240 Mizuno et al. (1994)/Tokuda et al. (2016)
L1527 140 0.9 1.2 +60 Ladd et al. (1991)/Motte & André (2001)
SerpM-S68N 415 10 10 −45 Casali et al. (1993)/Kaas et al. (2004)
SerpM-SMM4 415 2 7 +30 Casali et al. (1993)/Kaas et al. (2004)
SerpS-MM18 260 16 3 +188 Maury et al. (2011)/Maury et al. (2011)
SerpS-MM22 260 0.2 0.5 +230 Maury et al. (2011)/Maury et al. (2011)
L1157 250 2.0 1.5 163 Umemoto et al. (1992)/Motte & André (2001)
GF9-2 200 0.3 0.5 0 Schneider & Elmegreen (1979)/Wiesemeyer (1997)

Notes. The sources are ordered by increasing right ascension of the targeted core (see phase centers of our observations in Table A.1). Column 1: name of the protostar. Column 2: distance of the cloud where the protostar lies. The Taurus distance is taken from a VLBA measurement estimating distances from 130 to 160 pc (Torres et al. 2009) depending on the location in the cloud: we adopt a mean value of 140 pc. The distance of Perseus is taken following recent VLBI parallax measurements that have determined a distance to the NGC 1333 region 235 ± 18 pc (Hirota et al. 2008) and a distance to the L1448 cloud of 232 ± 18 pc (Hirota et al. 2011). The distance of the Serpens Main cloud (SerpM sources) follows VLBI measurements in Dzib et al. (2010), who have determined a distance of 415 pc for the Serpens Main core, while a distance 230–260 pc was widely used before. Therefore, both Lint and Menv reported here are larger by a factor of 2.8 than those listed in the Bolocam and Spitzer literature before 2011. The distance of Serpens South (SerpS sources) is still subject of debate, since no VLBI measurements toward the Serpens South filament exist: for consistency, we use here the distance of 260 pc adopted in Maury et al. (2011) and in Herschel studies of Könyves et al. (2010, 2015). Column 3: internal luminosity of the protostar. The internal luminosities come from the analysis of Herschel maps obtained in the framework of the Gould Belt survey (HGBS, see, e.g., André et al. 2010 and Ladjelate et al., in prep.). Column 4: protostellar envelope mass from the literature (associated references in Col. 6). Column 5: position angle (PA of the blue lobe counted east of north) of the high-velocity emission from 12CO or SiO tracing the protostellar jet component, from our CALYPSO molecular line emission maps when detected. For some protostars, the blue and red lobes are not well aligned, and/or several jets are detected in our CALYPSO maps: in these cases, we report the PA of the blue lobe, originating from the primary protostar position (see Table 3). Information on individual sources is reported in Appendix C, and the global jet properties in the CALYPSO sample will be provided in Podio & CALYPSO (in prep.). Column 6: references for values reported here: protostar discovery paper, then the reference for the envelope mass.

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