2MASSI J0937347+293142

2MASS J09373487+2931409, or 2MASSI J0937347+293142 (abbreviated to 2MASS 0937+2931) is a brown dwarf of spectral class T6,[3][4] located in the constellation Leo about 19.96 light-years from Earth.[1]

2MASS J09373487+2931409
Observation data
Epoch J2000      Equinox J2000
Constellation Leo
Right ascension  09h 37m 34.9s
Declination 29° 31′ 41″
Characteristics
Spectral type T6p
Astrometry
Proper motion (μ) RA: 944.15 ± 1.24 mas/yr
Dec.: −1319.78 ± 1.21 mas/yr
Parallax (π)163.39 ± 1.76[1] mas
Distance20.0 ± 0.2 ly
(6.12 ± 0.07 pc)
Details
Mass0.03[2] M☉
Temperature780–840 K
Other designations
2MASS J09373487+2931409
2MASSI J0937347+293142
2MASS 0937+2931
Database references
SIMBADdata

Discovery

2MASS 0937+2931 was discovered in 2002 by Adam J. Burgasser et al. from Two Micron All-Sky Survey (2MASS), conducted from 1997 to 2001. Follow-up observations were made in 1998–2001 using the Near-Infrared Camera, mounted on the Palomar 60 inch (1.5 m) Telescope; CTIO Infrared Imager (CIRIM) and Ohio State Infrared Imager/Spectrometer (OSIRIS), mounted on the Cerro Tololo Inter-American Observatory (CTIO) 1.5 m Telescope; and some additional observations were made using the Near Infrared Camera (NIRC), mounted on the Keck I 10 m telescope, and nearinfrared camera D78, mounted on the Palomar 5 m Hale Telescope. In 2002 Burgasser et al. published a paper, where they defined new spectral subtypes T1—T8, and presented discovery of 11 new T-type brown dwarfs, among which also was 2MASS 0937+2931. This 11 objects were among the earliest T-type brown dwarfs ever discovered: before this, the total number of known T-type objects was 13, and this discoveries increased it up to 24 (apart from additional T-type dwarfs, identified by Geballe et al. 2001 in SDSS data).[3]

Distance

Currently the most precise distance estimate of 2MASS 0937+2931 is trigonometric parallax, published in 2009 by Schilbach et al.: 163.39 ± 1.76 mas, corresponding to a distance 6.12 ± 0.07 pc, or 19.96 ± 0.22 ly.[1] A less precise parallax of this object, measured under U.S. Naval Observatory Infrared Astrometry Program, was published in 2004 by Vrba et al.[5]

Properties

2MASS 0937+2931 has an unusual spectrum, indicating a metal-poor atmosphere and/or a high surface gravity (high pressure at the surface).[3] Its effective temperature is estimated at about 800 Kelvin. The Research Consortium On Nearby Stars (RECONS) estimates the brown dwarf to be 0.03 solar masses.[2]

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gollark: Link to this `ccrunx`?
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gollark: I need to test in game a lot.
gollark: So I can edit in VSCode and run a command to copy it to CC directly.

See also

The other 10 brown dwarfs, presented in Burgasser et al. (2002):[3]

  • 2MASS 0243-2453 (T6)
  • 2MASS 0415-0935 (T8)
  • 2MASS 0727+1710 (T7)

References
  1. Schilbach, E.; Röser, S.; Scholz, R.-D. (2009). "Trigonometric parallaxes of ten ultracool subdwarfs". Astronomy and Astrophysics. 493 (2): L27–L30. arXiv:0811.4136. Bibcode:2009A&A...493L..27S. doi:10.1051/0004-6361:200811281.
  2. Research Consortium on Nearby Stars, Georgia State University (January 1, 2012). "The 100 nearest star systems". RECONS. Retrieved 2012-06-11.
  3. Burgasser, A. J.; Kirkpatrick, J. D.; Brown, M. E.; Reid, I. N.; Burrows, A.; Liebert, J.; Matthews, K.; Gizis, J. E.; Dahn, C. C.; Monet, D. G.; Cutri, R. M.; Skrutskie, M. F. (2002). "The Spectra of T Dwarfs. I. Near-Infrared Data and Spectral Classification". The Astrophysical Journal. 564 (1): 421–451. arXiv:astro-ph/0108452. Bibcode:2002ApJ...564..421B. doi:10.1086/324033.
  4. "2MASS J09373487+2931409 -- Brown Dwarf (M<0.08solMass)". SIMBAD. Centre de Données astronomiques de Strasbourg. Retrieved 2012-11-26.
  5. Vrba, F. J.; Henden, A. A.; Luginbuhl, C. B.; Guetter, H. H.; Munn, J. A.; Canzian, B.; Burgasser, A. J.; Kirkpatrick, J. Davy; Fan, X.; Geballe, T. R.; Golimowski, D. A.; Knapp, G. R.; Leggett, S. K.; Schneider, D. P.; Brinkmann, J. (2004). "Preliminary Parallaxes of 40 L and T Dwarfs from the US Naval Observatory Infrared Astrometry Program". The Astronomical Journal. 127 (5): 2948–2968. arXiv:astro-ph/0402272. Bibcode:2004AJ....127.2948V. doi:10.1086/383554.
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