WISE 1405+5534

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Coordinates: Sky map 14h 05m 18.27s, +55° 34′ 21.22″

WISEPC J140518.40+553421.4
Observation data
Epoch MJD 55545.11[1]      Equinox J2000[1]
Constellation Ursa Major
Right ascension  14h 05m 18.27s[1]
Declination 55° 34′ 21.22″[1]
Spectral type Y0 (pec?)[1][2]
Apparent magnitude (J (MKO filter system)) 20.20 ± 0.13[1]
Apparent magnitude (H (MKO filter system)) 21.45 ± 0.41[1]
Proper motion (μ) RA: −2263 ± 47[3] mas/yr
Dec.: 288 ± 41[3] mas/yr
Parallax (π)129 ± 19[3] mas
Distanceapprox. 25 ly
(approx. 8 pc)
Mass30[4] MJup
Radius0.86[4] RJup
Surface gravity (log g)5.0[4] cgs
Temperature350[4] K
Other designations
WISEPC J140518.40+553421.4[1]
WISEPC J1405+5534[4]
WISE J1405+5534[1]
WISE 1405+5534[1]
Database references

WISE 1405+5534 (full designation WISEPC J140518.40+553421.4) is a brown dwarf of spectral class Y0 (pec?),[1][2] located in constellation Ursa Major at approximately 25.3 light-years from Earth.[3] It is one of the Sun's nearest neighbors.


WISE 1405+5534 was discovered in 2011 from data collected by the Wide-field Infrared Survey Explorer (WISE) in the infrared at a wavelength of 40 cm (16 in). WISE 1405+5534 has two discovery papers: Kirkpatrick et al. (2011) and Cushing et al. (2011), however, basically with the same authors and published nearly simultaneously.[1][4]

  • Kirkpatrick et al. presented discovery of 98 new found by WISE brown dwarf systems with components of spectral types M, L, T and Y, among which also was WISE 1405+5534.[1][~ 1]
  • Cushing et al. presented discovery of seven brown dwarfs—one of T9.5 type, and six of Y-type—first members of the Y spectral class, ever discovered and spectroscopically confirmed, including "archetypal member" of the Y spectral class WISE 1828+2650, and WISE 1405+5534.[4] These seven objects are also the faintest seven of 98 brown dwarfs, presented in Kirkpatrick et al. (2011).[1]


Currently the most accurate distance estimate of WISE 1405+5534 is a trigonometric parallax, measured using Spitzer Space Telescope and published in 2013 by Trent Dupuy and Adam Kraus: 0.129 ± 0.019 arcsec, corresponding to a distance 7.8+1.3
pc, or 25.3+4.4

WISE 1405+5534 distance estimates

Source Parallax, mas Distance, pc Distance, ly Ref.
Kirkpatrick et al. (2011), Table 6 ~ 8.6 ~ 28.0 [1]
Cushing et al. (2011), Table 7 ~ 3.8 ~ 12.4 [4]
Marsh et al. (2013)
(according to Kirkpatrick et al. (2012))
207 ± 39 4.8+1.1
Marsh et al. (2013) 133 ± 81 >3.4[~ 2] >11.1 [5]
Dupuy & Kraus (2013) 129 ± 19[~ 3] 7.8+1.3

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

Space motion[edit]

WISE 1405+5534 has a large proper motion of about 2281 milliarcseconds per year.[3]

WISE 1405+5534 proper motion estimates

Source μ,
P. A.,
Kirkpatrick et al. (2011) 2693 272 -2691 ± 292 95 ± 271 [1]
Marsh et al. (2013) 2307 275 -2297 ± 96 212 ± 137 [5]
Dupuy & Kraus (2013) 2281 ± 48 277.3 ± 1.0 −2263 ± 47 288 ± 41 [3]

The most accurate estimates are marked in bold.

Spectral class and temperature[edit]

The object's temperature estimate is 350 K [4] (about 77 °C / 170 °F). Its spectrum is similar with spectrum of another Y-dwarf WISE 1738+2732. However, WISE 1405+5534's spectrum has a red shift of H-band flux peak, suggesting that WISE 1405+5534 may be peculiar, therefore it is classified as Y0 (pec?).[2][4]

See also[edit]


  1. ^ These 98 brown dwarf systems are only among first, not all brown dwarf systems, discovered from data, collected by WISE: six discoveries were published earlier (however, also listed in Kirkpatrick et al. (2011)) in Mainzer et al. (2011) and Burgasser et al. (2011), and the other discoveries were published later.
  2. ^ In this parallax and distance estimates the 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).
  3. ^ Relative parallax.


  1. ^ a b c d e f g h i j k l m n o p Kirkpatrick, J. Davy; Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, A.; Eisenhardt, Peter R.; McLean, Ian S.; Thompson, Maggie A.; Bauer, James M.; Benford, Dominic J.; Bridge, Carrie R.; Lake, Sean E.; Petty, Sara M.; Stanford, S. A.; Tsai, Chao-Wei; Bailey, Vanessa; Beichman, Charles A.; Bloom, Joshua S.; Bochanski, John J.; Burgasser, Adam J.; Capak, Peter L.; Cruz, Kelle L.; Hinz, Philip M.; Kartaltepe, Jeyhan S.; Knox, Russell P.; Manohar, Swarnima; Masters, Daniel; Morales-Calderon, Maria; Prato, Lisa A.; Rodigas, Timothy J.; Salvato, Mara; Schurr, Steven D.; Scoville, Nicholas Z.; Simcoe, Robert A.; Stapelfeldt, Karl R.; Stern, Daniel; Stock, Nathan D.; Vacca, William D. (2011). "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal Supplement. 197 (2): 19. arXiv:1108.4677v1. Bibcode:2011ApJS..197...19K. doi:10.1088/0067-0049/197/2/19.
  2. ^ a b c d 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.
  3. ^ a b c d e f g h Dupuy, T. J.; Kraus, A. L. (2013). "Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects". Science. 341 (6153): 1492–5. arXiv:1309.1422. Bibcode:2013Sci...341.1492D. doi:10.1126/science.1241917. PMID 24009359.
  4. ^ a b c d e f g h i j Cushing, Michael C.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Mainzer, A.; Marsh, Kenneth A.; Beichman, Charles A.; Burgasser, Adam J.; Prato, Lisa A.; Simcoe, Robert A.; Marley, Mark S.; Saumon, D.; Freedman, Richard S.; Eisenhardt, Peter R.; Wright, Edward L. (2011). "The Discovery of Y Dwarfs using Data from the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal. 743 (1): 50. arXiv:1108.4678. Bibcode:2011ApJ...743...50C. doi:10.1088/0004-637X/743/1/50.
  5. ^ a b 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.