WISEPC J205628.90+145953.3

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Coordinates: Sky map 20h 56m 28.88s, +14° 59′ 53.68″

WISEPC J205628.90+145953.3
Observation data
Epoch MJD 55511.01[1]      Equinox J2000[1]
Constellation Delphinus
Right ascension 20h 56m 28.88s[1]
Declination 14° 59′ 53.68″[1]
Characteristics
Spectral type Y0[1][2]
Apparent magnitude (J (2MASS filter system)) >17.6[1]
Apparent magnitude (J (MKO filter system)) 19.21 ± 0.07[1]
Apparent magnitude (H (2MASS filter system)) >17.1[1]
Apparent magnitude (H (MKO filter system)) 19.56 ± 0.18[1]
Astrometry
Proper motion (μ) RA: 812 ± 9[3] mas/yr
Dec.: 534 ± 8[3] mas/yr
Parallax (π) 140 ± 9[3] mas
Distance 23 ± 1 ly
(7.1 ± 0.5 pc)
Details
Mass 20 (12—30)[4] MJup
Radius 0.93 (0.86—1.01)[4] RJup
Surface gravity (log g) 4.75 (4.5—5.0)[4] cgs
Temperature 350 (350—400)[4] K
Other designations
WISEPC J205628.90+145953.3[1]
WISEPC J2056+1459[4]
WISE J2056+1459[1]
WISE 2056+1459[1]

WISEPC J205628.90+145953.3 (designation is abbreviated to WISE 2056+1459) is a brown dwarf of spectral class Y0,[1][2] located in constellation Delphinus at approximately 23.3 light-years from Earth.[3]

History of observations[edit]

Discovery[edit]

WISE 2056+1459 was discovered in 2011 from data, collected by Wide-field Infrared Survey Explorer (WISE) Earth-orbiting satellite — NASA infrared-wavelength 40 cm (16 in) space telescope, which mission lasted from December 2009 to February 2011. WISE 2056+1459 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 2056+1459.[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 2056+1459.[4] These seven objects are also the faintest seven of 98 brown dwarfs, presented in Kirkpatrick et al. (2011).[1]

Distance[edit]

Currently the most accurate distance estimate of WISE 2056+1459 is a trigonometric parallax, published in 2014 by Beichman et al.: 0.140 ± 0.009 arcsec, corresponding to a distance 7.1+0.5
−0.4
pc, or 23.3+1.6
−1.4
ly.[3]

WISEPC J205628.90+145953.3 distance estimates

Source Parallax, mas Distance, pc Distance, ly Ref.
Kirkpatrick et al. (2011), Table 6 7.7 25.1 [1]
Cushing et al. (2011), Table 7 3.0+3.4
−0.6
9.8+11.1
−2.0
[4]
Kirkpatrick et al. (2012), Tables 4 & 8 ~ 192 ~ 5.2 ~ 17 [2]
Marsh et al. (2013)
(according Kirkpatrick et al. (2012))
?[~ 2] ? ? [2]
Marsh et al. (2013) 144 ± 44 7.5+4.3
−1.8
[~ 3]
24.5+14.0
−5.9
[5]
Dupuy & Kraus (2013) 144 ± 23[~ 4] 6.9+1.3
−1
22.6+4.3
−3.1
[6]
Beichman et al. (2014) 140 ± 9 7.1+0.5
−0.4
23.3+1.6
−1.4
[3]

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

Space motion[edit]

WISE 2056+1459 has proper motion of about 972 milliarcseconds per year.[3]

WISEPC J205628.90+145953.3 proper motion estimates

Source μ,
mas/yr
P. A.,
°
μRA,
mas/yr
μDEC,
mas/yr
Ref.
Kirkpatrick et al. (2011) 872 44 604 ± 393 629 ± 378 [1]
Marsh et al. (2013) 1035 58 881 ± 57 544 ± 42 [5]
Dupuy & Kraus (2013) 911 ± 41 56.7 ± 1.9 761 ± 46 500 ± 21 [6]
Beichman et al. (2014) 972 57 812 ± 9 534 ± 8 [3]

The most accurate estimates are marked in bold.

Temperature[edit]

The object's temperature estimate is 350 (350—400) K.[4]

See also[edit]

The other six discoveries of brown dwarfs, published in Cushing et al. (2011):[4]

Notes[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. ^ The paper does not give the parallax value, but it is mentioned that it is roughly the size of the error itself.
  3. ^ 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).
  4. ^ Relative parallax.

References[edit]

  1. ^ a b c d e f g h i j k l m n o p q r 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 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 Beichman, C.; Gelino, Christopher R.; Kirkpatrick, J. Davy; Cushing, Michael C.; Dodson-Robinson, Sally; Marley, Mark S.; Morley, Caroline V.; Wright, E. L. (2014). "WISE Y Dwarfs As Probes of the Brown Dwarf-Exoplanet Connection". The Astrophysical Journal 783 (2): 68. arXiv:1401.1194v2. Bibcode:2014ApJ...783...68B. doi:10.1088/0004-637X/783/2/68.  edit
  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)". arXiv:1108.4678v1 [astro-ph.SR]. Bibcode 2011ApJ...743...50C. doi:10.1088/0004-637X/743/1/50. edit
  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.  edit
  6. ^ a b 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.