Epoch MJD 55518.52 Equinox J2000
|Right ascension||15h 06m 49.89s|
|Declination||70° 27′ 36.23″|
|Apparent magnitude (J (2MASS filter system))||14.328±0.095|
|Apparent magnitude (J (MKO filter system))||13.56±0.05|
|Apparent magnitude (H (2MASS filter system))||14.150±0.203|
|Apparent magnitude (H (MKO filter system))||13.91±0.04|
|Apparent magnitude (KS (2MASS filter system))||14.048±0.136|
|Proper motion (μ)||RA: 1241±85− mas/yr
Dec.: 1046±64 mas/yr
|Parallax (π)||310 ± 42 mas|
WISEPC J150649.97+702736.0 (designation abbreviated to WISE 1506+7027, or WISE J1506+7027) is a brown dwarf of spectral class T6, located in constellation Ursa Minor.[note 1] Being 11.1+2.3
−1.3 light-years from Earth, it is one of the Sun's nearest neighbors. Brown dwarfs closer to the Sun include Luhman 16 and WISE 0855−0714. Other brown dwarfs that may be closer to the Sun include ε Indi Ba and ε Indi Bb at 11.8 light-years and WISE 0350-5658 at 12.1+5.2
WISE 1506+7027 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), whose mission lasted from December 2009 to February 2011. In 2011, Kirkpatrick and colleagues 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 1506+7027.[note 2]
Photometric distance estimate of WISE 1506+7027, published in its discovery paper in 2011, is 4.9 pc (16 ly).
WISE 1506+7027 distance estimates
|Source||Parallax, mas||Distance, pc||Distance, ly||Distance, Pm||Ref.|
|Kirkpatrick et al. (2011) (Table 6)||~ 4.9||~ 16||~ 151.2|||
|Marsh et al. (2013)
(according Kirkpatrick et al. (2012))
|Marsh et al. (2013)||310±42||3.4+0.7
Non-trigonometric distance estimates are marked in italic. The most precise estimate is marked in bold.
WISE 1506+7027 has a large proper motion of about 1623 milliarcseconds per year.
WISE 1506+7027 proper motion estimates
|Source||μ, mas/yr||P. A., °||μRA, mas/yr||μDEC, mas/yr||Ref.|
|Kirkpatrick et al. (2011)||1388 ± 128||314.1 ± 5.3||−996 ± 75||966 ± 107|||
|Marsh et al. (2013)||1623 ± 106||310.1 ± 3.7||−1241 ± 85||1046 ± 64|||
The most accurate estimates are marked in bold. Italic are computed values, not italic are values, given in the sources.
- The nearest known star/brown dwarf in this constellation.
- 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.
- 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).
- 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.
- 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.
- 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.