WISE 0350−5658

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Coordinates: Sky map 03h 50m 00.32s, −56° 58′ 30.2″

WISE J035000.32−565830.2
Observation data
Epoch J2000[1]      Equinox J2000[1]
Constellation Reticulum
Right ascension 03h 50m 00.32s[1]
Declination −56° 58′ 30.2″[1]
Spectral type Y1[1]
Apparent magnitude (J (MKO-NIR filter system)) >22.8[1]
Apparent magnitude (H (MKO-NIR filter system)) >21.5[1]
Proper motion (μ) RA: −125±97[2] mas/yr
Dec.: −865±76[2] mas/yr
Parallax (π) 291 ± 50[2] mas
Distance 12.1+5.2
[2] ly
[2] pc)
Other designations
WISE J035000.32−565830.2,[1]
WISE 0350−5658[1]
Database references

WISE J035000.32−565830.2 (designation abbreviated to WISE 0350−5658) is a brown dwarf of spectral class Y1,[1] located in constellation Reticulum.[note 1] Being approximately 12 light-years from Earth,[2] it is one of the Sun's nearest neighbors.


WISE 0350−5658 was discovered in 2012 by J. Davy Kirkpatrick and colleagues from data collected by the Wide-field Infrared Survey Explorer (WISE) in the infrared at a wavelength of 40 cm (16 in), whose mission lasted from December 2009 to February 2011. In 2012 Kirkpatrick et al. published a paper in The Astrophysical Journal, where they presented the discovery of seven new brown dwarfs of spectral type Y that had been found by WISE, among which was WISE 0350−5658.[1]


WISE 0350−5658 is one of the nearest known brown dwarfs: its trigonometric parallax, published by Marsh et al. (2013), is 0.291 ± 0.050 arcsecond, corresponding to a distance 3.7+1.6
pc (12.1+5.2
ly).[2][note 2]

WISE 0350−5658 distance estimates

Source Parallax, mas Distance, pc Distance, ly Distance, Pm Ref.
Marsh et al. (2013)
(according Kirkpatrick et al. (2012))
238±38 4.2+0.8
Marsh et al. (2013) 291±50 3.7+1.6
[note 2]

Non-trigonometric distance estimates are marked in italic. The most precise estimate is marked in bold.

See also[edit]

The other six discoveries of brown dwarfs, published in Kirkpatrick et al. (2012):[1]


  1. ^ The nearest known star/brown dwarf in this constellation.
  2. ^ a b In this parallax and distance estimates the most probable distance value does not equal to inverse maximum likelihood parallax value, as would be in the case of exact parallax and distance values. This is because Marsh et al. used a more sophisticated method of converting maximum likelihood parallaxes into most probable distances, that uses also some prior information, and not just the calculation of the inverse value. (The method description see in Marsh et al. (2013), Section 4).


  1. ^ a b c d e f g h i j k l m Kirkpatrick, J. D.; Gelino, C. R.; Cushing, M. C.; Mace, G. N.; Griffith, R. L.; Skrutskie, M. F.; Marsh, K. A.; Wright, E. L.; Eisenhardt, P. R.; McLean, I. S.; Mainzer, A. K.; Burgasser, A. J.; Tinney, C. G.; Parker, S.; Salter, G. (2012). "Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function". The Astrophysical Journal 753 (2): 156. arXiv:1205.2122. Bibcode:2012ApJ...753..156K. doi:10.1088/0004-637X/753/2/156. 
  2. ^ a b c d e f g h Marsh, Kenneth A.; Wright, Edward L.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Griffith, Roger L.; Skrutskie, Michael F.; Eisenhardt, Peter R. (2013). "Parallaxes and Proper Motions of Ultracool Brown Dwarfs of Spectral Types Y and Late T". The Astrophysical Journal 762 (2): 119. arXiv:1211.6977. Bibcode:2013ApJ...762..119M. doi:10.1088/0004-637X/762/2/119.