3 years ago

# The Near-Infrared Outflow and Cavity of the proto-Brown Dwarf Candidate ISO-Oph 200.

Emma Whelan, Bastien Rouze, Basmah Riaz

In this letter a near-infrared integral field study of a proto-brown dwarf candidate is presented. A $\sim$ 0\farcs5 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 %CONTENT%lt;$5\farcs4, in the direction of both the blue and red-shifted outflow lobes but along a different position angle to the more compact faster emission. It is argued that the more compact emission is a jet and the extended H$_{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[H2]}$= 3.8$\times$10$^{-10}$~\Msun~yr$^{-1}$and$\dot{M}_{out[FeII]}$= 1$\times$10$^{-8}$~\Msun~yr$^{-1}$.$\dot{M}_{out[FeII]}$takes a Fe depletion of$\sim$88$\%$into account. The depletion is investigated using the ratio of the [FeII]~1.257~$\mu$m and [PII]~1.188~$\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}$~\Msun~yr$^{-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.

Publisher URL: http://arxiv.org/abs/1801.08749

DOI: arXiv:1801.08749v1

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