NISINI, BrunellaBrunellaNISINISantangelo, G.G.SantangeloGiannini, T.T.GianniniANTONIUCCI, SimoneSimoneANTONIUCCICabrit, S.S.CabritCODELLA, CLAUDIOCLAUDIOCODELLADavis, C. J.C. J.DavisEislöffel, J.J.EislöffelKristensen, L.L.KristensenHerczeg, G.G.HerczegNeufeld, D.D.Neufeldvan Dishoeck, E. F.E. F.van Dishoeck2020-04-212020-04-2120150004-637Xhttp://hdl.handle.net/20.500.12386/24168Financial support from INAF, under PRIN2013 program “Disks, jets and the dawn of planets” is acknowledged.We present Herschel PACS mapping observations of the [O i] 63 μm line toward protostellar outflows in the L1448, NGC 1333-IRAS4, HH 46, BHR 71, and VLA 1623 star-forming regions. We detect emission spatially resolved along the outflow direction, which can be associated with a low-excitation atomic jet. In the L1448-C, HH 46 IRS, and BHR 71 IRS1 outflows this emission is kinematically resolved into blue- and redshifted jet lobes, having radial velocities up to 200 km s<SUP>-1</SUP>. In the L1448-C atomic jet the velocity increases with the distance from the protostar, similarly to what is observed in the SiO jet associated with this source. This suggests that [O i] and molecular gas are kinematically connected and that the latter could represent the colder cocoon of a jet at higher excitation. Mass flux rates ({{\dot{M}}<SUB>jet</SUB>}(O i)) have been measured from the [O i] 63 μm luminosity adopting two independent methods. We find values in the range (1-4) × 10<SUP>-7</SUP> {{M}<SUB>☉ </SUB>} yr<SUP>-1</SUP> for all sources except HH 46, for which an order of magnitude higher value is estimated. {{\dot{M}}<SUB>jet</SUB>}(O i) are compared with mass accretion rates (\dot{M}<SUB>acc</SUB>) onto the protostar and with {{\dot{M}}<SUB>jet</SUB>} derived from ground-based CO observations. {{\dot{M}}<SUB>jet</SUB>}(O i)/\dot{M}<SUB>acc</SUB> ratios are in the range 0.05-0.5, similar to the values for more evolved sources. {{\dot{M}}<SUB>jet</SUB>}(O i) in HH 46 IRS and IRAS4A are comparable to {{\dot{M}}<SUB>jet</SUB>}(CO), while those of the remaining sources are significantly lower than the corresponding {{\dot{M}}<SUB>jet</SUB>}(CO). We speculate that for these three sources most of the mass flux is carried out by a molecular jet, while the warm atomic gas does not significantly contribute to the dynamics of the system.STAMPAenArticle10.1088/0004-637X/801/2/1212-s2.0-84924675237000350965500050https://iopscience.iop.org/article/10.1088/0004-637X/801/2/1212015ApJ...801..121NFIS/05 - ASTRONOMIA E ASTROFISICA