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Mayrit 1701117

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Mayrit 1701117

Large outflow around Mayrit 1701117 with ESO VLT MUSE, showing sulfur in red, nitrogen in blue and H-alpha in green
Observation data
Epoch J2000      Equinox J2000
Constellation Orion[1]
Right ascension 05h 40m 25.8041s[2]
Declination −02° 48′ 55.501″[2]
Characteristics
Evolutionary stage proto-brown dwarf
Apparent magnitude (G) 17.842±0.031[2]
Apparent magnitude (I) 16.538±0.07[3]
Apparent magnitude (J) 15.146±0.039[3]
Apparent magnitude (H) 14.101±0.030[3]
Apparent magnitude (K) 13.074±0.036[3]
Astrometry
Proper motion (μ) RA: 0.429±0.315 mas/yr[2]
Dec.: 1.834±0.298 mas/yr[2]
Parallax (π)3.3546±0.3747 mas[2]
Distanceapprox. 1,000 ly
(approx. 300 pc)
Details
Mass~40[4] MJup
Luminosity0.012[4] L☉
Age30,000-40,000[4] years
Other designations
ESO-HA 1736, 2MASS J05402580-0248553, Gaia DR2 3216418342740867840, TIC 11359910
Database references
SIMBADdata

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.[5]

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.[3] Later, the source was detected in H-alpha with the ESO Schmidt telescope at La Silla and catalogued as ESO-HA 1736.[6] 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.[5] The mass of the central source was later estimated to be around 40 MJ and the system is 30,000-40,000 years old.[4]

The disk and outflow

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Discovery image of the jet with SOAR

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.[7] 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.[5] 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.[4]

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.[5]

References

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  1. ^ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
  2. ^ a b c d e Vallenari, A.; et al. (Gaia collaboration) (2023). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy and Astrophysics. 674: A1. arXiv:2208.00211. Bibcode:2023A&A...674A...1G. doi:10.1051/0004-6361/202243940. S2CID 244398875. Gaia DR3 record for this source at VizieR.
  3. ^ a b c d e Caballero, J. A. (2007-12-04). "Stars and brown dwarfs in theσOrionis cluster: the Mayrit catalogue". Astronomy & Astrophysics. 478 (2): 667–674. arXiv:0710.5882. Bibcode:2008A&A...478..667C. doi:10.1051/0004-6361:20077885. ISSN 0004-6361.
  4. ^ a b c d e B., Riaz; Machida, M. N.; D., Stamatellos (July 2019). "ALMA reveals a pseudo-disc in a proto-brown dwarf". Monthly Notices of the Royal Astronomical Society. 486 (3): 4114. arXiv:1904.06418. Bibcode:2019MNRAS.486.4114R. doi:10.1093/mnras/stz1032. ISSN 0035-8711.
  5. ^ a b c d Riaz, B.; Briceño, C.; Whelan, E. T.; Heathcote, S. (2017-07-20). "First Large-scale Herbig–Haro Jet Driven by a Proto-brown Dwarf". The Astrophysical Journal. 844 (1): 47. arXiv:1705.01170. Bibcode:2017ApJ...844...47R. doi:10.3847/1538-4357/aa70e8. ISSN 0004-637X.
  6. ^ Pettersson, Bertil; Armond, Tina; Reipurth, Bo (October 2014). "Hαemission-line stars in molecular clouds". Astronomy & Astrophysics. 570: A30. arXiv:1406.7037. Bibcode:2014A&A...570A..30P. doi:10.1051/0004-6361/201423594. ISSN 0004-6361.
  7. ^ Riaz, B.; Thompson, M. A.; Whelan, E. T.; Lodieu, N. (2014-10-13). "Very low-luminosity Class I/Flat outflow sources in sigma Orionis". MNRAS. 446 (3): 2550–2559. arXiv:1410.3377. Bibcode:2015MNRAS.446.2550R. doi:10.1093/mnras/stu2139.
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