WISEPA J031325.96+780744.2

From Wikipedia, the free encyclopedia
Jump to: navigation, search

Coordinates: Sky map 03h 13m 26.02s, +78° 07′ 44.4″

WISEPA J031325.96+780744.2
Observation data
Epoch MJD 55448.07[1]      Equinox J2000[1]
Constellation Cepheus
Right ascension 03h 13m 26.02s[1]
Declination 78° 07′ 44.4″[1]
Characteristics
Spectral type T8.5[1][2]
Apparent magnitude (J (2MASS filter system)) 17.65 ± 0.07[1]
Apparent magnitude (H (2MASS filter system)) 17.63 ± 0.06[1]
Astrometry
Proper motion (μ) RA: 147 ± 151[1] mas/yr
Dec.: -4 ± 148[1] mas/yr
Distance ~ 28.0[2] ly
(~ 8.6[2] pc)
Other designations
WISEPA J031325.96+780744.2[1]
WISE J0313+7807[1]
WISE 0313+7807[1]

WISEPA J031325.96+780744.2 (designation abbreviated to WISE 0313+7807, or WISE J0313+7807) is a brown dwarf of spectral class T8.5,[1][2] located in constellation Cepheus at approximately 28 light-years from Earth.[2]

Discovery[edit]

WISE 0313+7807 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 0313+7807.[1][note 1]

Distance[edit]

Trigonometric parallax of WISE 0313+7807 is not yet measured. Therefore, there are only distance estimates of this object, obtained by indirect — spectrofotometric — means (see table).

WISE 0313+7807 distance estimates

Source Parallax, mas Distance, pc Distance, ly Ref.
Kirkpatrick et al. (2011) ~8.1 ~26.4 [1]
Kirkpatrick et al. (2012) ~8.6 ~28.0 [2]

Non-trigonometric distance estimates are marked in italic.

Notes[edit]

  1. ^ This 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.

References[edit]

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