Astronomy:WISE J0254+0223

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Short description: Star in the constellation Cetus

Coordinates: Sky map 02h 54m 09.62s, +02° 23′ 58.85″

WISEPA J025409.45+022359.1
Observation data
Equinox J2000.0]] (ICRS)
Constellation Cetus
Right ascension  02h 54m 09.62s[1]
Declination 02° 23′ 58.85″[1]
Characteristics
Spectral type T8[1]
Apparent magnitude (Y (MKO filter system)) 16.999±0.014[2]
Apparent magnitude (J (2MASS filter system)) 16.557±0.156[1]
Apparent magnitude (J (MKO filter system)) 15.916±0.008[2]
Apparent magnitude (H (2MASS filter system)) 15.884±0.199[1]
Apparent magnitude (H (MKO filter system)) 16.29±0.02[2]
Apparent magnitude (KS (2MASS filter system)) >16.006[1]
Apparent magnitude (K (MKO filter system)) 16.73±0.05[2]
Astrometry
Proper motion (μ) RA: 2588±27[3] mas/yr
Dec.: 273±27[3] mas/yr
Parallax (π)146.1 ± 1.5[4] mas
Distance22.3 ± 0.2 ly
(6.84 ± 0.07 pc)
Other designations
WISEPC J025409.45+022359.1[5]
WISEPA J025409.45+022359.1[1]
WISE J0254+0223[1]
PSO J043.5395+02.3995[6]
PSO J043.5+02[6]
Database references
SIMBADdata

WISEPA J025409.45+022359.1 (designation is abbreviated to WISE 0254+0223) is a brown dwarf of spectral class T8,[1][7] located in constellation Cetus at approximately 22.3 light-years from Earth.[4]

History of observations

Discovery

WISE 0254+0223 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 0254+0223 has two discovery papers: Scholz et al. (2011) and Kirkpatrick et al. (2011) (the first was published earlier).[5][1]

  • Scholz et al. discovered two late T-type brown dwarfs, including WISE 0254+0223, using preliminary data release from WISE and follow-up near-infrared spectroscopy with LUCIFER1 near-infrared camera/spectrograph at the Large Binocular Telescope (LBT).
  • 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 0254+0223.[1][~ 1]

Distance

Currently the most accurate distance estimate of WISE 0254+0223 is a trigonometric parallax, measured using the Spitzer Space Telescope and published in 2019 by Kirkpatrick et al.: 146.1±1.5 mas, corresponding to a distance 6.84±0.07 pc, or 22.3±0.2 ly.[4]

WISE 0254+0223 distance estimates

Source Parallax, mas Distance, pc Distance, ly Ref.
Scholz et al. (2011) (preprint version 1) 5.5+1.4
−1.1		 17.9+4.6
−3.6		 [8]
Scholz et al. (2011) 5.5+2.3
−1.6		 17.9+7.5
−5.2		 [5]
Kirkpatrick et al. (2011), Table 6 ~ 6.9 ~ 22.5 [1]
Kirkpatrick et al. (2011), Table 7 165±46 6.1+2.3
−1.3		 19.8+7.6
−4.3		 [1]
Liu et al. (2011) 7.2±0.7 23.5±2.3 [6]
Liu et al. (2011) 171±45 5.8+2.1
−1.2		 19.1+7.8
−4.0		 [6]
Scholz et al. (2012) 165±20 6.1+0.8
−0.7		 19.8+2.7
−2.1		 [9]
Marsh et al. (2013)
(according to Kirkpatrick et al. (2012))		 166±26 6.0+1.1
−0.8		 19.6+3.6
−2.7		 [7]
Marsh et al. (2013) 185±42 4.9+1.0
−0.6[~ 2]		 16.0+3.3−2.0 [10]
Dupuy & Kraus (2013) 135 ± 15[~ 3] 7.4+0.9
−0.7		 24.2+3.0
−2.4		 [3]

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

Space motion

WISE 0254+0223 has a large proper motion of about 2602 milliarcseconds per year.[3]

WISE 0254+0223 proper motion estimates

Source μ,
mas/yr		 P. A.,
°		 μRA,
mas/yr		 μDEC,
mas/yr		 Ref.
Scholz et al. (2011) 2511 84 2496±46 276±47 [5]
Kirkpatrick et al. (2011) 2546 85 2534±28 243±37 [1]
Marsh et al. (2013) 2596 83 2578±42 309±50 [10]
Dupuy & Kraus (2013) 2602±27 84.0±0.6 2588±27 273±27 [3]

The most accurate estimates are marked in bold.

See also

Another object, discovered by Scholz et al. (2011):[5]

Notes

  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 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 because 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.

References

  1. ↑ 1.00 1.01 1.02 1.03 1.04 1.05 1.06 1.07 1.08 1.09 1.10 1.11 1.12 1.13 1.14 Kirkpatrick, J. Davy; Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, Amy K. et al. (2011). "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal Supplement 197 (2): 19. doi:10.1088/0067-0049/197/2/19. Bibcode: 2011ApJS..197...19K. 
  2. ↑ 2.0 2.1 2.2 2.3 Liu, Michael C.; Dupuy, Trent J.; Bowler, Brendan P.; Leggett, S. K.; Best, William M. J. (2012). "Two Extraordinary Substellar Binaries at the T/Y Transition and the Y-band Fluxes of the Coolest Brown Dwarfs". The Astrophysical Journal 758 (1): 57. doi:10.1088/0004-637X/758/1/57. Bibcode: 2012ApJ...758...57L. 
  3. ↑ 3.0 3.1 3.2 3.3 3.4 Dupuy, T. J.; Kraus, A. L. (2013). "Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects". Science 341 (6153): 1492–5. doi:10.1126/science.1241917. PMID 24009359. Bibcode: 2013Sci...341.1492D. 
  4. ↑ 4.0 4.1 4.2 Kirkpatrick, J. Davy et al. (February 2019). "Preliminary Trigonometric Parallaxes of 184 Late-T and Y Dwarfs and an Analysis of the Field Substellar Mass Function into the "Planetary" Mass Regime". The Astrophysical Journal Supplement Series 240 (2): 19. doi:10.3847/1538-4365/aaf6af. Bibcode: 2019ApJS..240...19K. 
  5. ↑ 5.0 5.1 5.2 5.3 5.4 Scholz, R.-D.; Bihain, G.; Schnurr, O.; Storm, J. (2011). "Two very nearby (d ~ 5 pc) ultracool brown dwarfs detected by their large proper motions from WISE, 2MASS, and SDSS data". Astronomy & Astrophysics 532: L5. doi:10.1051/0004-6361/201117297. Bibcode: 2011A&A...532L...5S. 
  6. ↑ 6.0 6.1 6.2 6.3 Liu, Michael C.; Deacon, Niall R.; Magnier, Eugene A.; Dupuy, Trent J.; Aller, Kimberly M.; Bowler, Brendan P.; Redstone, Joshua; Goldman, Bertrand et al. (2011). "A Search for High Proper Motion T Dwarfs with PAN-STARRS1 + 2MASS + WISE". The Astrophysical Journal Letters 740 (2): L32. doi:10.1088/2041-8205/740/2/L32. Bibcode: 2011ApJ...740L..32L. 
  7. ↑ 7.0 7.1 Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L. et al. (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. doi:10.1088/0004-637X/753/2/156. Bibcode: 2012ApJ...753..156K. 
  8. ↑ Scholz, R.-D.; Bihain, G.; Schnurr, O.; Storm, J. (2011). "Two very nearby (d~5 pc) ultracool brown dwarfs detected by their large proper motions from WISE, 2MASS, and SDSS data". arXiv:1105.4059v1 [astro-ph.GA].
  9. ↑ Scholz, R.-D.; Bihain, G.; Schnurr, O.; Storm, J. (2012). "UKIDSS detections of cool brown dwarfs. Proper motions of 14 known >T5 dwarfs and discovery of three new T5.5-T6 dwarfs". Astronomy & Astrophysics 541: A163. doi:10.1051/0004-6361/201218947. Bibcode: 2012A&A...541A.163S. 
  10. ↑ 10.0 10.1 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. doi:10.1088/0004-637X/762/2/119. Bibcode: 2013ApJ...762..119M. 

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