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WISE J0336−0143

WISE J033605.05−014350.4

WISE J0336−0143 imaged by the James Webb Space Telescope's NIRCam in two different filters
Observation data
Epoch J2000      Equinox J2000
Constellation Eridanus
Right ascension 03h 36m 05.052s[1]
Declination −01° 43′ 50.48″[1]
Characteristics
Spectral type Y + Y
Y0 (effective)
Apparent magnitude (J) 21.26±0.14[2]: 4 
Apparent magnitude (H) 21.59±0.31[2]: 4 
Apparent magnitude (K) 21.8±0.5 (est.)[2]: 5 
Apparent magnitude (W1) 18.164±0.153
Apparent magnitude (W2) 14.664±0.023
Astrometry
Proper motion (μ) RA: −251.5±0.9 mas/yr
Dec.: −1,216.1±0.93 mas/yr
Parallax (π)99.8 ± 2.1 mas[3]
Distance32.7 ± 0.7 ly
(10.0 ± 0.2 pc)
Details[4]: 7 
A
Mass8.5–18 MJup
Temperature415±20 K
B
Mass5–11.5 MJup
Temperature325+15
−10 K
Orbit[4]: 7 
PrimaryA
CompanionB
Period (P)7±2 yr
Semi-major axis (a)0.97+0.05
−0.09 AU (mean separation)
Other designations
WISEA J033605.04–014351.0, CWISE J033604.94−014358.5
Database references
SIMBADdata

WISE J033605.05−014350.4, abbreviated to WISE J0336−0143 or W0336, is a binary system comprising two planetary-mass Y-type brown dwarfs tightly orbiting around their common center of mass. The system is located in the constellation Eridanus, about 33 light-years (10 parsecs) away from the Sun. It was discovered in images taken by the Wide-field Infrared Survey Explorer (WISE) and formally published by Gregory N. Mace and collaborators in March 2013.[5]: 5 [6]: 28  Astronomers suspected the brown dwarf was a binary system upon follow-up observations showing it had an unusual infrared spectrum,[5]: 22  but its binarity was not confirmed until the James Webb Space Telescope resolved the system's components in high-resolution NIRCam imaging in September 2022, with its results published in March 2023.[4]

The two components orbit their system barycenter approximately every 7 years and are separated 0.97 astronomical units from each other, which is slightly less than the distance between the Sun and Earth. The brighter primary component has a temperature of 415 K and a mass within the range of 8.5–18 Jupiter masses, while the fainter secondary component has a temperature of 325 K and a mass range of 5–11.5 Jupiter masses. Because the binary system's age and evolutionary stage have not been determined yet, the individual components' masses are uncertain. Nevertheless, both components appear to have masses near the deuterium fusion threshold of 13 Jupiter masses, which marks the boundary between gas giant planets and brown dwarfs. The study of such low-mass binary systems will provide valuable insight into the formation and evolution of planetary-mass objects.[4]

The secondary component WISE J0336−0143 B (305–340 K) might be one of the coldest objects in interstellar space discovered so far (as of September 2023). Newer models of Y dwarfs produce an even colder temperature of 285–305 K for WISE J0336−0143 B.[7] WISE 0855−0714 remains the coldest object found so far with 225–260 K and WISEA 0830+2837 has a similar temperature with 300–350 K. Models suggest that WISE J0336−0143 B might have water clouds, but it is possible that changes in the pressure–temperature profile might instead explain the color of cold Y dwarfs.[7]

  • Hubble Space Telescope WFC3/near-infrared image of W0336 and the stars and galaxies in the field of view.
    Hubble Space Telescope WFC3/near-infrared image of W0336 and the stars and galaxies in the field of view.
  • Movement of W0336 in the Hubble images between January 2021 and October 2021.
    Movement of W0336 in the Hubble images between January 2021 and October 2021.

See also

References

  1. ^ a b "WISE J033605.05-014350.4 -- Brown Dwarf". SIMBAD. Centre de données astronomiques de Strasbourg. Retrieved 30 March 2023.
  2. ^ a b c Leggett, S. K.; Pascal, Tremblin; Philips, Mark W.; Dupuy, Trent J.; Marley, Mark; Morley, Caroline; et al. (September 2021). "Measuring and Replicating the 1-20 μm Energy Distributions of the Coldest Brown Dwarfs: Rotating, Turbulent, and Nonadiabatic Atmospheres". The Astrophysical Journal. 918 (1): 31. arXiv:2107.00696. Bibcode:2021ApJ...918...11L. doi:10.3847/1538-4357/ac0cfe. 11.
  3. ^ Kirkpatrick, J. Davy; Gelino, Christopher R.; Faherty, Jacqueline K.; Meisner, Aaron M.; Caselden, Dan; Schneider, Adam C.; et al. (March 2021). "The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and Y Dwarfs". The Astrophysical Journal Supplement Series. 253 (1): 85. arXiv:2303.16923. Bibcode:2021ApJS..253....7K. doi:10.3847/1538-4365/abd107. 7.
  4. ^ a b c d Calissendorff, Per; et al. (March 2023). "JWST/NIRCam discovery of the first Y+Y brown dwarf binary: WISE J033605.05−014350.4". The Astrophysical Journal Letters. 947 (2): 8. arXiv:2303.16923. Bibcode:2023ApJ...947L..30C. doi:10.3847/2041-8213/acc86d.
  5. ^ a b Mace, Gregory N.; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; et al. (March 2013). "A Study of the Diverse T Dwarf Population Revealed by WISE". The Astrophysical Journal Supplement. 205 (1): 49. arXiv:1301.3913. Bibcode:2013ApJS..205....6M. doi:10.1088/0067-0049/205/1/6. 6.
  6. ^ Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; et al. (July 2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal. 753 (2): 38. arXiv:1205.2122. Bibcode:2012ApJ...753..156K. doi:10.1088/0004-637X/753/2/156. 156.
  7. ^ a b Leggett, S. K.; Tremblin, Pascal (September 2023). "The First Y Dwarf Data From JWST Show That Dynamic and Diabatic Processes Regulate Cold Brown Dwarf Atmospheres". The Astrophysical Journal. 959 (2): 86. arXiv:2309.14567. Bibcode:2023ApJ...959...86L. doi:10.3847/1538-4357/acfdad.
Quelle: https://en.wikipedia.org/wiki/WISE_J0336%E2%88%920143