In this letter a near-infrared integral field study of a proto-brown dwarf candidate is presented .
A \sim 0 \aas@@fstack { \prime \prime } 5 blue-shifted outflow is detected in both H _ { 2 } and [ Fe II ] lines at V _ { sys } = ( -35 \pm 2 )  km s ^ { -1 } and V _ { sys } = ( -51 \pm 5 )  km s ^ { -1 } respectively .
In addition , slower ( \sim \pm  10 km s ^ { -1 } ) H _ { 2 } emission is detected out to < 5 \aas@@fstack { \prime \prime } 4 , in the direction of both the blue and red-shifted outflow lobes but along a different position angle to the more compact faster emission .
It is argued that the more compact emission is a jet and the extended H _ { 2 } emission is tracing a cavity .
The source extinction is estimated at A _ { v } = 18 mag \pm 1 mag and the outflow extinction at Av = 9 mag \pm 0.4 mag .
The H _ { 2 } outflow temperature is calculated to be 1422 K \pm  255 K and the electron density of the [ Fe II ] outflow is measured at \sim 10000 cm ^ { -3 } .
Furthermore , the mass outflow rate is estimated at \dot { M } _ { out [ H 2 ] } = 3.8 \times 10 ^ { -10 } Â M _ { \odot } Â yr ^ { -1 } and \dot { M } _ { out [ FeII ] } = 1 \times 10 ^ { -8 } Â M _ { \odot } Â yr ^ { -1 } . \dot { M } _ { out [ FeII ] } takes a Fe depletion of \sim 88 \% into account .
The depletion is investigated using the ratio of the [ FeII ] Â 1.257Â \mu m and [ PII ] Â 1.188Â \mu m lines .
Using the Pa \beta and Br \gamma lines and a range in stellar mass and radius \dot { M } _ { acc } is calculated to be ( 3 - 10 ) \times 10 ^ { -8 } Â M _ { \odot } Â yr ^ { -1 } .
Comparing these rates puts the jet efficiency in line with predictions of magneto-centrifugal models of jet launching in low mass protostars .
This is a further case of a brown dwarf outflow exhibiting analogous properties to protostellar jets .