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2MASS J11193254−1137466

Coordinates: Sky map 11h 19m 32.543s, −11° 37′ 46.70″
From Wikipedia, the free encyclopedia
2MASS J11193254–1137466 A

2MASS J1119−1137A (upper left) and 2MASS J1119−1137B (lower right)
Credit: Keck Observatory; Best et al. Processing: Melina Thévenot
Observation data
Epoch J2000      Equinox J2000
Constellation Crater
Right ascension 11h 19m 32.543s[1]
Declination −11° 37′ 46.70″[1]
Characteristics
Evolutionary stage Sub-brown dwarf
Spectral type L7red[1]
Apparent magnitude (H) 15.61±0.14[1]
Apparent magnitude (K) 14.62±0.11[1]
Details
Mass~5-10 MJup
Luminosity (bolometric)0.00004 (total luminosity) L☉
Other designations
WISE J111932.43-113747.7, TWA 42, TIC 453454626
Database references
SIMBADdata
2MASS J11193254–1137466 B
Discovery
Discovery date2016
Imaging
Designations
WISE J111932.43-113747.7, 2MASS J11193254-1137466
Orbital characteristics
3.6 ± 0.9 AU
90+80
−50 years
Physical characteristics
Mass~5–10 MJ
Spectral type
L7red

2MASS J11193254–1137466 AB[2] (often shortened to 2MASS J1119–1137 AB) is a planetary mass binary[3][4] located 86±23 light-years from the Earth[3] in the constellation Crater. The components of 2MASS J1119–1137 are each roughly four Jupiter masses. The planetary-mass objects are probably a part of the TW Hydrae association which has an age of approximately 10 million years.[3][5] The planetary-mass objects are candidate rogue planets.

Overview

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The object was found by a team of scientists from Canada, the United States and Chile during a search for unusually red brown dwarfs (such color indicates some notable properties of their atmospheres, e.g. dustiness). The search used data of 3 surveys: SDSS (visible light data), 2MASS (near-infrared) and WISE (mid-wave infrared). 2MASS J1119–1137 was one of the reddest and, according to the authors, the most interesting object found. Results of the work were published in December 2015.[6]

In April 2016, the first detailed study of the object was published. The investigators conducted its infrared spectroscopy on the telescope Gemini South. Radial velocity and proper motion were also calculated. The astronomers determined low surface gravity and moderate age of 2MASS J1119–1137.[5][7]

In November 2016 and March 2017, 2MASS J1119–1137 was imaged by the telescope Keck II with adaptive optics technique, which revealed its binarity. The angular separation of components is 0.13788 ± 0.00034 arcseconds (which corresponds to linear projected separation 3.6 ± 0.9 AU). Their stellar magnitudes are roughly equal. Total mass of the system is estimated as 7.4+2.5
−1.9 Jupiter masses. Their total bolometric luminosity is approximately 0.00004 solar units. The estimated orbital period is 90+80
−50 years.[3]

One of the components[which?] of the binary is rotating rapidly, having a period of 3.02+0.04
−0.03 hours while the typical rotation period for young brown dwarfs is 10 hours.[8]

Candidate exomoon

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In August 2021, researchers reported signs of a habitable zone 1.7 R🜨 exomoon (a moon orbiting a planetary-mass object outside our solar system) transiting one of the components in 2MASS J1119–1137. A possible single transit of the moon candidate was detected in archival Spitzer Space Telescope data. The study determined that the detected event might have been caused by variability (clouds/weather) in the host planet's atmosphere, but that an exomoon was a better fit to the observed data suggesting that the detection was most likely caused by an exomoon transit.[9]

See also

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References

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  1. ^ a b c d e "2MASS J11193254-1137466". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 3 Jun 2017.
  2. ^ "Free-Floating Giant Planet Analog Found 95 Light-Years Away". 14 April 2016. Retrieved 2016-04-22.
  3. ^ a b c d Best, William M. J.; Liu, Michael C.; Dupuy, Trent J.; Magnier, Eugene A. (2017). "The Young L Dwarf 2MASS J11193254-1137466 is a Planetary-Mass Binary". The Astrophysical Journal Letters. 843 (1): L4. arXiv:1706.01883. Bibcode:2017ApJ...843L...4B. doi:10.3847/2041-8213/aa76df. S2CID 119081444.
  4. ^ Schilling, Govert. "Mistaken brown dwarf is actually two planets orbiting each other". New Scientist. Retrieved 23 June 2017.
  5. ^ a b "YOUNG, UNATTACHED JUPITER ANALOG FOUND IN SOLAR NEIGHBORHOOD". Western University. 6 April 2016. Retrieved 2016-04-22.
  6. ^ Kellogg, Kendra; Metchev, Stanimir; Geißler, Kerstin; Hicks, Shannon; Kirkpatrick, J. Davy; Kurtev, Radostin (2015). "A Targeted Search for Peculiarly Red L and T Dwarfs in SDSS, 2MASS, and WISE: Discovery of a Possible L7 Member of the TW Hydrae Association". The Astronomical Journal. 150 (6): 182. arXiv:1510.08464. Bibcode:2015AJ....150..182K. doi:10.1088/0004-6256/150/6/182. S2CID 28912543.
  7. ^ Kellogg, Kendra; Metchev, Stanimir; Gagné, Jonathan; Faherty, Jacqueline (2016). "The Nearest Isolated Member of the TW Hydrae Association is a Giant Planet Analog". The Astrophysical Journal Letters. 821 (1): L15. arXiv:1603.08529. Bibcode:2016ApJ...821L..15K. doi:10.3847/2041-8205/821/1/L15. S2CID 119289711.
  8. ^ Schneider, Adam C.; Hardegree-Ullman, Kevin K.; Cushing, Michael C.; Davy Kirkpatrick, J.; Shkolnik, Evgenya L. (2018), "Spitzer Light Curves of the Young, Planetary-Mass TW Hya Members 2MASS J11193254−1137466AB and WISEA J114724.10−204021.3", The Astronomical Journal, 155 (6): 238, arXiv:1804.06917, Bibcode:2018AJ....155..238S, doi:10.3847/1538-3881/aabfc2, S2CID 54664068
  9. ^ Limbach, Mary Anne; Vos, Johanna M.; Winn, Joshua N.; Heller, Rene; Mason, Jeffrey C.; Schneider, Adam C.; Dai, Fei (2021-08-18). "On the Detection of Exomoons Transiting Isolated Planetary-mass Objects". The Astrophysical Journal Letters. 918 (2): L25. arXiv:2108.08323. Bibcode:2021ApJ...918L..25L. doi:10.3847/2041-8213/ac1e2d. S2CID 237213523.
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External videos
video icon Western-led astronomy team discovers Jupiter analogue among young stars, 2016, from YouTube posted by Western University YouTube channel.
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