SIMBAD references

As the number of observed brown dwarf outflows is growing it is important to investigate how these outflows compare to the well-studied jets from young stellar objects. A key point of comparison is the relationship between outflow and accretion activity and in particular the ratio between the mass outflow and accretion rates ({dot}(M)_out/{dot}(M)_acc). The brown dwarf candidate ISO-ChaI 217 was discovered by our group, as part of a spectro-astrometric study of brown dwarfs, to be driving an asymmetric outflow with the blue-shifted lobe having a position angle of ∼20°. The aim here is to further investigate the properties of ISO-ChaI 217, the morphology and kinematics of its outflow, and to better constrain {dot}(M)_out/{dot}(M)_acc. The outflow is spatially resolved in the [SII] λλ6716,6731 lines and is detected out to ∼1.6" in the blue-shifted lobe and 1'' in the red-shifted lobe. The asymmetry between the two lobes is confirmed although the velocity asymmetry is less pronounced with respect to our previous study. Using thirteen different accretion tracers we measure log({dot}(M)_acc)[M_☉/yr]=-10.6±0.4. As it was not possible to measure the effect of extinction on the ISO-ChaI 217 outflow {dot}(M)_out was derived for a range of values of A_v, up to a value of A_v=2.5mag estimated for the source extinction. The logarithm of the mass outflow ({dot}(M)_out) was estimated in the range -11.7 to -11.1 for both jets combined. Thus {dot}(M)_out/{dot}(M)_acc[M_☉/yr] lies below the maximum value predicted by magneto-centrifugal jet launching models. Finally, both model fitting of the Balmer decrements and spectro-astrometric analysis of the Hα line show that the bulk of the H I emission comes from the accretion flow.