The CALYPSO IRAM-PdBI survey of jets from Class 0 protostars: Exploring whether jets are ubiquitous in young stars

Aims. As a part of the CALYPSO Large Program, we aim to constrain the properties of protostellar jets and outflows by searching for corresponding emission in a sample of 21 Class 0 protostars covering a broad range of internal luminosities ( L int from 0.035 L ⊙ to 47 L ⊙ ). Methods. We analyzed high angular (~0.′′5–1.′′0) resolution IRAM Plateau de Bure Interferometer (PdBI) observations in three typical outflow and jet tracers, namely: CO (2−1), SO (5 6 −4 5 ), and SiO (5−4). We obtained the detection rate, spatial distribution, kinematics, and collimation of the outflow and jet emission in the three lines. Molecular column densities and abundances, the jet mass-loss and momentum rates, and mechanical luminosity are estimated from the integrated line intensities. Results. Blue- and red-shifted emission in CO (2−1), which probes outflowing gas, was detected in all the sources in the sample and detected for the first time in the cases of SerpS-MM22 and SerpS-MM18b. Collimated high-velocity jets in SiO (5−4) were detected in 67% of the sources (for the first time in IRAS4B2, IRAS4B1, L1448-NB, SerpS-MM18a) and 77% of these also showed jet or outflow emission in SO (5 6 −4 5 ). The detection rate of jets in SiO and SO increases with internal luminosity. In five sources (that is, 24% of the sample) SO (5 6 −4 5 ) is elongated and reveals a velocity gradient perpendicular to the jet direction, hence, it probes the inner envelope or the disk, or both. The detected SiO jets are collimated (typical opening angle, α ~ 10°) and surrounded by wider angle SO ( α ~ 15°) and CO ( α ~ 25°) emission. The abundance of SO relative to H 2 ranges from 2.4 × 10 −7 to >5 × 10 −6 , with the exception of the jets from IRAS4A1 and IRAS4A2, which show low SiO abundance (≤2−6 × 10 −8 ). The mass-loss rates range from ~7 × 10 −8 M ⊙ yr −1 up to ~3 × 10 −6 M ⊙ yr −1 for L int ~ 1−50 L ⊙ . Conclusions. The CALYPSO IRAM-PdBI survey shows that the outflow phenomenon is ubiquitous in our sample of protostars and that the detection rate of high-velocity collimated jets increases for increasing protostellar accretion, with at least 80% of the sources with L int > 1 L ⊙ driving a jet. The detected protostellar flows exhibit an onion-like structure, where the SiO jet is nested into a wider angle SO and CO outflow. On scales > 300 au the SiO jets are less collimated (4°−12°) than atomic jets from Class II sources