OTS 44

OTS 44

OTS 44 (orange crosshair) and surrounding nebulae
Observation data
Epoch J2000.0      Equinox J2000.0
Constellation Chamaeleon
Right ascension 11h 10m 11.5s
Declination −76° 32′ 13″
Characteristics
Spectral type M9.5[1]
Astrometry
Distance530 ly
(162.5 pc)[2]
Details
Mass12[2] MJup
Radius3.2 or 3.6[3] RJup
Luminosity0.00126[3] – 0.0024[2] L☉
Temperature1,700[3][2]–2,300[1] K
Age1 – 6[3] Myr
Database references
SIMBADdata
An artist's concept of OTS 44's dust disk

OTS 44 is a free-floating planetary-mass object or brown dwarf located at 530 light-years (160 pc) in the constellation Chamaeleon near the reflection nebula IC 2631. It is among the lowest-mass free-floating substellar objects, with approximately 11.5 times the mass of Jupiter, or approximately 1.1% that of the Sun.[3][4] Its radius is estimated to be 3.2 or 3.6 times that of Jupiter.[3]

OTS 44 was discovered in 1998 by Oasa, Tamura, and Sugitani as a member of the star-forming region Chamaeleon I.[5][6] Based upon infrared observations with the Spitzer Space Telescope and the Herschel Space Observatory, OTS 44 emits an excess of infrared radiation for an object of its type, suggesting it has a circumstellar disk of dust and particles of rock and ice.[1][2][7] This disk (gas+dust) has a SED-fitted mass of at about 30 Earth masses.[2] Observations with the SINFONI spectrograph at the Very Large Telescope show that the disk is accreting matter at the rate of approximately 10−11 of the mass of the Sun per year.[2] It could eventually develop into a planetary system. Observations with ALMA detected the disk in millimeter wavelengths. The observations constrained the dust mass of the disk between 0.07 and 0.63 ME, but these mass estimates are limited by assumptions on poorly constrained parameters.[8] Another work estimates the dust mass to 0.064 ME (5.2 ML) for dust particles of 1 mm in size and 0.295 ME (24 ML) for dust particles of 1 μm in size.[9]

  1. ^ a b c Cite error: The named reference apj620_1_L51 was invoked but never defined (see the help page).
  2. ^ a b c d e f g Cite error: The named reference Joergens2013 was invoked but never defined (see the help page).
  3. ^ a b c d e f Cite error: The named reference Bonnefoy2014 was invoked but never defined (see the help page).
  4. ^ Luhmann, K. L.; Peterson, D. E.; Megeath, S. T. (2004). "Spectroscopic Confirmation of the Least Massive Known Brown Dwarf in Chamaeleon". The Astrophysical Journal. 617 (1): 565–568. arXiv:astro-ph/0411445. Bibcode:2004ApJ...617..565L. doi:10.1086/425228. S2CID 18157277.
  5. ^ Tamura, M.; Itoh, Y.; Oasa, Y.; Nakajima, T. (1998). "Isolated and Companion Young Brown Dwarfs in the Taurus and Chamaeleon Molecular Clouds". Science. 282 (5391): 1095–7. Bibcode:1998Sci...282.1095T. doi:10.1126/science.282.5391.1095. PMID 9804541.
  6. ^ Oasa, Y.; Tamura, M.; Sugitani, K. (1999). "A Deep Near-Infrared Survey of the Chamaeleon I Dark Cloud Core". The Astrophysical Journal. 526 (1): 336–343. Bibcode:1999ApJ...526..336O. doi:10.1086/307964.
  7. ^ "Blurring the lines between stars and planets: Lonely planets offer clues to star formation". MPIA Science Release 2013-09. Retrieved 1 September 2014.
  8. ^ Bayo, Amelia; Joergens, Viki; Liu, Yao; Brauer, Robert; Olofsson, Johan; Arancibia, Javier; Pinilla, Paola; Wolf, Sebastian; Ruge, Jan Philipp; Henning, Thomas; Natta, Antonella (May 2017). "First Millimeter Detection of the Disk around a Young, Isolated, Planetary-mass Object". Astrophysical Journal Letters. 841 (1): L11. arXiv:1705.06378. Bibcode:2017ApJ...841L..11B. doi:10.3847/2041-8213/aa7046. hdl:10150/624481. ISSN 0004-637X. S2CID 73605838.
  9. ^ Wu, Ya-Lin; Bowler, Brendan P.; Sheehan, Patrick D.; Close, Laird M.; Eisner, Joshua A.; Best, William M. J.; Ward-Duong, Kimberly; Zhu, Zhaohuan; Kraus, Adam L. (2022-05-01). "ALMA Discovery of a Disk around the Planetary-mass Companion SR 12 c". The Astrophysical Journal. 930 (1): L3. arXiv:2204.06013. Bibcode:2022ApJ...930L...3W. doi:10.3847/2041-8213/ac6420. ISSN 0004-637X.