Mayrit 1701117
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Mayrit 1701117 (M1701117) is a proto-brown dwarf launching a large (0.8 light-years, 0.26 parsec) Herbig-Haro object, called HH 1165. Previously only small micro-jets (≤0.03 parsec) were known from young proto-brown dwarfs.
Mayrit 1701117 was discovered in 2008 in the Mayrit catalogue by J. A. Caballero. The Mayrit catalogue is a list of stars and high-mass brown dwarfs in the Sigma Orionis cluster. The catalogue uses DENIS and 2MASS data. Later, the source was detected in H-alpha with the ESO Schmidt telescope at La Silla and catalogued as ESO-HA 1736. The central object has a mass of around 0.04–0.08 M☉ and will most likely evolve into a brown dwarf. The central object is surrounded by a H-alpha halo with a clumpy distribution, which could be due to wind-envelope interactions. The southeastern tail of the H-alpha emission is likely reflecting the light from the nearby star HR 1950. The mass of the central source was later estimated to be around 40 MJ and the system is 30,000-40,000 years old.
The disk and outflow
Observations at the Calar Alto 3.5-m telescope were used to measure an accretion rate of 6.4×10−10 M☉/year and an outflow rate of 10−9 M☉/year, similar to class I protostars. The researchers also obtained observations with the James Clerk Maxwell Telescope and find that the total envelope+disk mass is around 36 MJ. VLT/UVES observations do show signs of strong accretion and outflow and the estimated outflow rate is higher than the previous estimate at (35±17)×10−10 M☉/year. Observations with ALMA detected a pseudo-disk. According to core-collapse models, infalling material will form a flattened disk-like structure, which is called pseudo-disk. This pseudo-disk is rotating and surrounds the Keplerian disk. The pseudo-disk in Mayrit 1701117 has a size of 165–192 AU and a mass of around 0.02 M☉. Emission by H2CO likely traces the Keplerian disk and N2D+ traces a clump close to this disk. Using ALMA the researchers determined the total mass of the circumstellar material as 20.98±1.24 MJ.
In 2017 a large Herbig-Haro object was discovered with SOAR narrow-band imaging. The Herbig-Haro object was named HH 1165 and the jet shows a bent C-shape, multiple knots and fragmented bow shocks at the end of the jets. The jet is mostly detected in sulfur [S II] emission, showing 8 knots in the northwestern direction. A fainter counter-jet in the southeastern direction shows only two knots. The multiple knots can be seen as individual ejection events. The H-alpha image shows a bright scattered emission next to the jet, likely tracing the outflow cavity. The northwest part resembles a classical jet running into a neutral medium, but the southern part resembles an externally irradiated jet.