WISE 0359−5401

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Coordinates: Sky map 03h 59m 34.06s, −54° 01′ 54.6″

WISE J035934.06−540154.6
Observation data
Epoch J2000[1]      Equinox J2000[1]
Constellation Reticulum
Right ascension 03h 59m 34.06s[1]
Declination −54° 01′ 54.6″[1]
Spectral type Y0[1]
Apparent magnitude (J (MKO-NIR filter system)) 21.56±0.24[1]
Apparent magnitude (H (MKO-NIR filter system)) 22.20±0.43[1]
Proper motion (μ) RA: 177±53[2] mas/yr
Dec.: 930±62[2] mas/yr
Parallax (π) 145 ± 39[2] mas
Distance 19.2+4.2
[2] ly
[2] pc)
Other designations
WISE J035934.06−540154.6,[1]
WISE 0359−5401[1]
Database references

WISE J035934.06−540154.6 (designation abbreviated to WISE 0359−5401) is a brown dwarf of spectral class Y0,[1] located in constellation Reticulum. Estimated to be approximately 19 light-years from Earth,[2] it is one of the Sun's nearest neighbors.


WISE 0359−5401 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 discovery of seven new found by WISE brown dwarfs of spectral type Y, among which also was WISE 0359−5401.[1]


Trigonometric parallax of WISE 0359−5401, published in 2013 by Marsh et al., is 0.145±0.039 arcsec, corresponding to a distance 5.9+1.3
, or 19.2+4.2
.[2][note 1]

WISE 0359−5401 distance estimates

Source Parallax, mas Distance, pc Distance, ly Distance, Pm Ref.
Kirkpatrick et al. (2012), Table 8 ~ 13.5 ~ 44 ~ 416.6 [1]
Marsh et al. (2013)
(according Kirkpatrick et al. (2012))
?[note 2] [1]
Marsh et al. (2013) 145±39[note 1] 5.9+1.3

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. ^ 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 due to the fact that 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).
  2. ^ The parallax value is not shown in Kirkpatrick et al. (2012), but it is mentioned that it is roughly the size of the error itself.


  1. ^ a b c d e f g h i j k l m n 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.  edit
  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.  edit