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S Ori 70

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Object in the Orionis cluster in the constellation Orion
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J. |last2=Jeffries |first2=R. D. |last3=Naylor |first3=Tim |last4=Oliveira |first4=J. M. |last5=Maxted |first5=P. F. L. |year=2005 |doi=10.1111/j.1365-2966.2004.08455.x |doi-access=free |arxiv=astro-ph/0409749 }}</ref><ref>{{Cite journal |bibcode=2006ApJ...637.1067B |title=A Unified Near-Infrared Spectral Classification Scheme for T Dwarfs |journal=The Astrophysical Journal |volume=637 |issue=2 |pages=1067–1093 |last1=Burgasser |first1=Adam J. |last2=Geballe |first2=T. R. |last3=Leggett |first3=S. K. |last4=Kirkpatrick |first4=J. Davy |last5=Golimowski |first5=David A. |year=2006 |doi=10.1086/498563| arxiv=astro-ph/0510090 |doi-access=free }}</ref>"}},"i":6}},"\n",{"template":{"target":{"wt":"Starbox reference\n","href":"./Template:Starbox_reference"},"params":{"Simbad":{"wt":"Mayrit+520267"}},"i":7}},"\n",{"template":{"target":{"wt":"Starbox end","href":"./Template:Starbox_end"},"params":{},"i":8}}]}'>
S Ori J053810.1-023626

S Ori 70 in the near-infrared
Credit: ESO VLT HAWKI
Observation data
Epoch J2000Equinox ICRS
Constellation Orion [1]
Right ascension 05h 38m 10.10s[2]
Declination −02°36′00.0′′[2]
Characteristics
Spectraltype T6[3] [4]
Apparent magnitude(H) 20.07[5]
Astrometry
Proper motion (μ) RA:10[2] mas/yr
Dec.:5[2] mas/yr
Distance 1,150[6] ly
(352[5] pc)
Details
Mass 3[7] MJup
Surface gravity (logg)3.5[7] cgs
Age 3[7] Myr
Other designations
Mayrit 520267, S Ori 70, S Ori J053810.1-023626[8] [9]
Database references
SIMBAD data

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 rogue 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.

Discovery

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The σ Orionis open cluster has been the focus of Osorio's team observations due to the age of the cluster (approximately 3 to 8 million years). The cluster also has low extinction, its distance is convenient, and it is observed to be rich and dense. Using the 4.2-meter (170-inch) William Herschel Telescope in a pencil-beam deep mini-survey measuring 55 square minutes of arc at a sensitivity of 21 magnitudes in the J and H Bands [7] allowed the team to find S Ori 70. The raw data collected was reduced to the Image Reduction and Analysis Facility (IRAF), a standard technique used with near-infrared images; after subtracting the sky background and dark current, an extracted object spectrum was derived. It was the faintest and coolest member found in the cluster and was named S Ori 70.

Argument of the initial study

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Adam J. Burgasser[10] [11] examined the claims of Osorio's T-type brown dwarf discovery and its spectroscopically verified low-mass. A comparison of the J band spectrum between S Ori 70 and other field objects was done. The J band spectrum revealed a distinct triangular-shaped spectral morphology which was previously explained by Zapatero-Osorio and Martín was due to the surface's low gravity. In order to see if similar discrepancies occurred in the T dwarf's behavior, Burgasser's team compared data from the claims of Osorio to that of standard COND models. Identical wavelength scales interpolated through both empirical and model spectra were Gaussian smoothed; this showed that best-fit spectral models can yield skewed gravities for late-type field T dwarfs which resulted in the underestimation of age and mass. Burgasser concluded that S Ori 70 is not a member of the Sigma Ori cluster but is rather a foreground field brown dwarf. Further study of the object suggest that the low gravity was not from the field T dwarf but rather a nearby background star.[10] As of 2009 no direct scientific data have dispelled nor confirmed either conclusion.

It could be the first "free floating" non-stellar planet discovered[6] with a mass of 3 MJ, but needs confirmation.

See also

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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. 1 2 3 4 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 .
  3. ↑ 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.
  4. ↑ 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 .
  5. 1 2 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.
  6. 1 2 "Mysterious Object Might be First Extrasolar Planet Photographed". Silver Star Academy. Archived from the original on 2011年07月16日. Retrieved 2010年02月08日.
  7. 1 2 3 4 Martín, Eduardo L. (2004). "S Ori 70: Still a strong cluster planet candidate". arXiv:astro-ph/0410678 .
  8. ↑ 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 .
  9. ↑ 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 .
  10. 1 2 Burgasser, Adam J.; Kirkpatrick, J. Davy; McGovern, Mark R.; McLean, Ian S.; Prato, L.; Reid, I. Neill (2004). "S Orionis 70: Just a Foreground Field Brown Dwarf?". The Astrophysical Journal. 604 (2): 827–831. arXiv:astro-ph/0312285 . Bibcode:2004ApJ...604..827B. doi:10.1086/382129. S2CID 14102676.
  11. ↑ "T dwarfs". MIT.edu. Retrieved 2010年02月08日.

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