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In the BHR71 region, two low-mass protostars drive two distinguishableoutflows. They constitute an ideal laboratory to investigate the effects ofshock chemistry and the mechanisms that led to their formation. We aim todefine the morphology of the warm gas component of the BHR 71 outflow and atmodelling its shocked component. We present the first far infrared Herschelimages of the BHR71 outflow in the CO(14-13), H$_2$O (2$_{21}$-1$_{10}$),H$_2$O (2$_{12}$-1$_{01}$) and [OI] 145 $\mu$m, lines, revealing the presenceof several knots of warm, shocked gas associated with fast outflowing gas. Intwo of these knots we performed a detailed study of the physical conditions bycomparing a large set of transitions from several molecules to a grid of shockmodels. Herschel lines ratios in the outflow knots are quite similar, showingthat the excitation conditions of the fast moving gas do not changesignificantly within the first $\sim$ 0.068 pc of the outflow, apart at theextremity of the southern blue-shifted lobe that is expanding outside themolecular cloud. Rotational diagram, spectral line profile and LVG analysis ofthe CO lines in knot A show the presence of two gas components: one extended,cold ($T\sim$80 K) and dense ($n$(H$_2$) = 3$\times$10$^5$-4$\times$10$^6$cm$^{-3}$) and another compact (18 arcsec), warm ($T$ = 1700-2200 K) withslightly lower density ($n$(H$_2$) = (2-6)$\times$10$^4$ cm$^{-3}$). In the twobrightest knots (where we performed shock modelling) we found that H$_2$ and COare well fitted with non-stationary (young) shocks. These models, however,significantly underestimate the observed fluxes of [OI] and OH lines, but arenot too far off those of H$_2$O, calling for an additional, possiblydissociative, J-type shock component. Our modelling indirectly suggests that anadditional shock component exists, possibly a remnant of the primary jet

The shocked gas of the BHR71 outflow observed by Herschel: indirect evidence for an atomic jet