S Ori 70

S Ori J053810.1-023626

S Ori 70 in the near-infrared
Credit: ESO VLT HAWKI
Observation data
Epoch J2000      Equinox J2000
Constellation Orion
Right ascension 05h 38m 10.10s[1]
Declination −02° 36′ 00.0″[1]
Characteristics
Spectral type T6[2][3]
Apparent magnitude (H) 20.07[4]
Astrometry
Proper motion (μ) RA: 10[1] mas/yr
Dec.: 5[1] mas/yr
Distance1,150[5] ly
(352[4] pc)
Details
Mass3[6] MJup
Surface gravity (log g)3.5[6] cgs
Age3[6] Myr
Other designations
Mayrit 520267
S Ori 70
S Ori J053810.1-023626[7][8]
Database references
SIMBADdata

S Ori 70 or S Ori J053810.1-023626 is a mid-T type astronomical object in the foreground of the σ Orionis cluster, which is approximately 1,150 light-years from Earth. It was discovered on November 24, 2002 by M. R. Zapatero-Osorio and E. L. Martin's team at the Roque de los Muchachos Observatory. It has yet to be determined if it is a field brown dwarf or a 3-million-year-old planet that is part of a cluster. Near-infrared spectroscopy images taken three years after its discovery led to the first motion measurements for the object. Its behavior is significantly different from what may be expected; it was further described as either a low-gravity atmosphere or an atmosphere with metallicity. The object's small proper motion suggests that it is further away than expected if it were a single field T dwarf.

  1. ^ a b c d Faherty, Jacqueline K.; Burgasser, Adam J.; Cruz, Kelle L.; Shara, Michael M.; Walter, Frederick M.; Gelino, Christopher R. (2009). "The Brown Dwarf Kinematics Project I. Proper Motions and Tangential Velocities for a Large Sample of Late-Type M, L, and T Dwarfs". The Astronomical Journal. 137 (1): 1. arXiv:0809.3008. Bibcode:2009AJ....137....1F. doi:10.1088/0004-6256/137/1/1.
  2. ^ Zapatero-Osorio, María Rosa; Béjar, V. J. S.; Bihain, G.; Martín, Eduardo L.; Rebolo, Rafael; Villó-Pérez, I.; Díaz-Sánchez, A.; Pérez Garrido, A.; Caballero, J. A.; Henning, T.; Mundt, R.; Barrado y Navascués, D.; Bailer-Jones, C. A. L. (2008). "New constraints on the membership of the T dwarf S Ori 70 in theσ Orionis cluster". Astronomy & Astrophysics. 477 (3): 895–900. arXiv:0710.2776. Bibcode:2008A&A...477..895Z. doi:10.1051/0004-6361:20078600. S2CID 15928749.
  3. ^ Martín, Eduardo L.; Zapatero-Osorio, María Rosa (2003). "Spectroscopic Estimate of Surface Gravity for a Planetary Member in the σ Orionis Cluster". The Astrophysical Journal. 593 (2): L113. arXiv:astro-ph/0307268. Bibcode:2003ApJ...593L.113M. doi:10.1086/378313.
  4. ^ a b Peña Ramírez, K.; Zapatero-Osorio, María Rosa; Béjar, V. J. S.; Martin, Eduardo L.; Rebolo, Rafael; Villo-Perez, I.; Diaz-Sanchez, A.; Perez-Garrido, A.; Caballero, J. A.; Henning, T.; Mundt, R.; Barrado y Navascues, D.; Bailer-Jones, C. A. L. (2015). "Characterization of the known T-type dwarfs towards the σ Orionis cluster". Astronomy and Astrophysics. 574: A118. arXiv:1411.3370. Bibcode:2015A&A...574A.118P. doi:10.1051/0004-6361/201424816. S2CID 118498007.
  5. ^ "Mysterious Object Might be First Extrasolar Planet Photographed". Silver Star Academy. Archived from the original on 2011-07-16. Retrieved 2010-02-08.
  6. ^ a b c Cite error: The named reference martin was invoked but never defined (see the help page).
  7. ^ Kenyon, M. J.; Jeffries, R. D.; Naylor, Tim; Oliveira, J. M.; Maxted, P. F. L. (2005). "Membership, binarity and accretion among very low-mass stars and brown dwarfs of the σ Orionis cluster". Monthly Notices of the Royal Astronomical Society. 356 (1): 89. arXiv:astro-ph/0409749. Bibcode:2005MNRAS.356...89K. doi:10.1111/j.1365-2966.2004.08455.x.
  8. ^ Burgasser, Adam J.; Geballe, T. R.; Leggett, S. K.; Kirkpatrick, J. Davy; Golimowski, David A. (2006). "A Unified Near-Infrared Spectral Classification Scheme for T Dwarfs". The Astrophysical Journal. 637 (2): 1067–1093. arXiv:astro-ph/0510090. Bibcode:2006ApJ...637.1067B. doi:10.1086/498563.