[en] 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⁻¹. 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 (${\stackrel{\dot{}<!--\; ??\; -->}{M}}_{\mathrm{j}\mathrm{e}\mathrm{t}}$(O i)) have been measured from the [O i] 63 μm luminosity adopting two independent methods. We find values in the range (1–4) × 10⁻⁷ $M_{\odot <!--\; ???\; -->}$ yr⁻¹ for all sources except HH 46, for which an order of magnitude higher value is estimated. ${\stackrel{\dot{}<!--\; ??\; -->}{M}}_{\mathrm{j}\mathrm{e}\mathrm{t}}$(O i) are compared with mass accretion rates ($\stackrel{\dot{}<!--\; ??\; -->}{M}$_acc) onto the protostar and with ${\stackrel{\dot{}<!--\; ??\; -->}{M}}_{\mathrm{j}\mathrm{e}\mathrm{t}}$ derived from ground-based CO observations. ${\stackrel{\dot{}<!--\; ??\; -->}{M}}_{\mathrm{j}\mathrm{e}\mathrm{t}}$(O i)/$\stackrel{\dot{}<!--\; ??\; -->}{M}$_acc ratios are in the range 0.05–0.5, similar to the values for more evolved sources. ${\stackrel{\dot{}<!--\; ??\; -->}{M}}_{\mathrm{j}\mathrm{e}\mathrm{t}}$(O i) in HH 46 IRS and IRAS4A are comparable to ${\stackrel{\dot{}<!--\; ??\; -->}{M}}_{\mathrm{j}\mathrm{e}\mathrm{t}}$(CO), while those of the remaining sources are significantly lower than the corresponding ${\stackrel{\dot{}<!--\; ??\; -->}{M}}_{\mathrm{j}\mathrm{e}\mathrm{t}}$(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.