The CALYPSO IRAM-PdBI survey of jets from Class 0 protostars

Aims. As a part of the CALYPSO Large Program, we aim to constrain properties protostellar jets and outflows by searching for corresponding emission in sample 21 Class 0 protostars covering broad range internal luminosities ( L int from 0.035 ? 47 ). Methods. We analyzed high angular (~0.??5–1.??0) resolution IRAM Plateau de Bure Interferometer (PdBI) observations three typical outflow jet tracers, namely: CO (2?1), SO (5 6 ?4 5 ), SiO (5?4). obtained detection rate, spatial distribution, kinematics, collimation lines. Molecular column densities abundances, mass-loss momentum rates, mechanical luminosity are estimated integrated line intensities. Results. Blue- red-shifted which probes outflowing gas, was detected all sources first time cases SerpS-MM22 SerpS-MM18b. Collimated high-velocity (5?4) were 67% (for IRAS4B2, IRAS4B1, L1448-NB, SerpS-MM18a) 77% these also showed or The rate increases with luminosity. In five (that is, 24% sample) ) is elongated reveals velocity gradient perpendicular direction, hence, it inner envelope disk, both. collimated (typical opening angle, ? ~ 10°) surrounded wider angle 15°) 25°) emission. abundance relative H 2 ranges <10 ?7 up 10 ?6 ; whereas SiO, lower limits found >2.4 × >5 , exception IRAS4A1 IRAS4A2, show low (?2?6 ?8 rates ~7 M yr ?1 ~3 1?50 . Conclusions. IRAM-PdBI survey shows that phenomenon ubiquitous our increasing accretion, at least 80% > 1 driving jet. flows exhibit an onion-like structure, where nested into outflow. On scales 300 au less (4°?12°) than atomic II (~3°), possibly dueto projection effects contamination bow-shocks. other hand, asymmetry between two lobes one third sources, similarly jets, suggesting same launching mechanism work. Most rich, indicates very efficient release 1? 10% elemental silicon gas phase likely dust-free winds, launched inside dust sublimation radius. larger orders magnitude what measured indicating ejection decreases as source evolves accretion fades. Similarly 50% mass ? acc correlation holds along star-formation process 4 few Myr.