WISEPA J180435.40+311706.1

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Coordinates: Sky map 18h 04m 35.39s, +31° 17′ 05.98″

WISEPA J180435.40+311706.1
Observation data
Epoch MJD 55459.94[1]      Equinox J2000[1]
Constellation Hercules
Right ascension 18h 04m 35.39s[1]
Declination 31° 17′ 05.98″[1]
Spectral type T9.5:[1][2]
Apparent magnitude (J (2MASS filter system)) >18.88[1]
Apparent magnitude (J (MKO filter system)) 18.70 ± 0.05[1]
Apparent magnitude (H (2MASS filter system)) >18.24[1]
Apparent magnitude (H (MKO filter system)) 19.21 ± 0.11[1]
Apparent magnitude (KS (2MASS filter system)) >16.86[1]
Proper motion (μ) RA: -242 ± 26[3] mas/yr
Dec.: 17 ± 22[3] mas/yr
Parallax (π) 60 ± 11[3] mas
Distance approx. 54 ly
(approx. 17 pc)
Other designations
WISEPA J180435.40+311706.1[1]
WISE J1804+3117[1]
WISE 1804+3117[1]

WISEPA J180435.40+311706.1 (designation abbreviated to WISE 1804+3117, or WISE J1804+3117) is a brown dwarf of spectral class T9.5:,[1][2] located in constellation Hercules at approximately 54 light-years from Earth.[3]

History of observations[edit]


WISE 1804+3117 was discovered in 2011 by J. Davy Kirkpatrick et al. from data, collected by Wide-field Infrared Survey Explorer (WISE) Earth-orbiting satelliteNASA infrared-wavelength 40 cm (16 in) space telescope, which mission lasted from December 2009 to February 2011. In 2011 Kirkpatrick et al. published a paper in The Astrophysical Journal Supplement, where they 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 1804+3117.[1][~ 1]


Currently the most accurate distance estimate of WISE 1804+3117 is a trigonometric parallax, measured using Spitzer Space Telescope and published in 2013 by Trent Dupuy and Adam Kraus: 0.060 ± 0.011 arcsec, corresponding to a distance 16.7+3.7
pc, or 54.4+12.2

WISE 1804+3117 distance estimates

Source Parallax, mas Distance, pc Distance, ly Ref.
Kirkpatrick et al. (2011) ~13.0 ~42.4 [1]
Kirkpatrick et al. (2012) ~9.2 ~30.0 [2]
Dupuy & Kraus (2013) 60 ± 11[~ 2] 16.7+3.7

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

Space motion[edit]

WISE 1804+3117 has proper motion of about 244 milliarcseconds per year.[3]

WISE 1804+3117 proper motion estimates

Source μ,
P. A.,
Kirkpatrick et al. (2011) 1044 316 -719 ± 414 757 ± 475 [1]
Dupuy & Kraus (2013) 244 ± 26 274 ± 5 242 ± 26 17 ± 22 [3]

The most accurate estimates are marked in bold.


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


  1. ^ a b c d e f g h i j k l m n o p q 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.  edit
  2. ^ a b c 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
  3. ^ a b c d e f g h Dupuy, Trent J.; Kraus, Adam L. (2013). "Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects". arXiv:1309.1422v1 [astro-ph.SR]. Bibcode 2013arXiv1309.1422D.