WISEPA J174124.26+255319.5

Coordinates: 17h 41m 24.22s, +25° 53′ 18.96″

WISEPA J174124.26+255319.5
Observation data
Epoch MJD 55451.80[1]      Equinox J2000[1]
Constellation Hercules
Right ascension 17h 41m 24.22s[1]
Declination 25° 53′ 18.96″[1]
Characteristics
Spectral type T9[1]
Apparent magnitude (J (2MASS filter system)) 16.53±0.02[1]
Apparent magnitude (H (2MASS filter system)) 16.63±0.03[1]
Apparent magnitude (KS (2MASS filter system)) 16.89±0.20[1]
Astrometry
Proper motion (μ) RA: −495±11[2] mas/yr
Dec.: −1472±13[2] mas/yr
Parallax (π)180 ± 15[3] mas
Distance18 ± 2 ly
(5.6 ± 0.5 pc)
Other designations
WISEPC J174124.25+255319.5[4]
WISEPA J174124.26+255319.5[1]
WISE J1741+2553[1]
Database references
SIMBADdata

WISEPA J174124.26+255319.5 (designation is abbreviated to WISE 1741+2553) is a brown dwarf of spectral class T9,[1][5] located in constellation Hercules at approximately 18 light-years from Earth.[3]

History of observations

Discovery

WISE 1741+2553 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 1741+2553 has three discovery papers: Scholz et al. (2011), Gelino et al. (2011) and Kirkpatrick et al. (2011).[4][6][1]

Distance

Currently the most accurate distance estimate of WISE 1741+2553 is a trigonometric parallax, measured using Spitzer Space Telescope and published in 2013 by Trent Dupuy and Adam Kraus: 0.180±0.015 arcsec, corresponding to a distance 5.6+0.5
−0.4 pc, or 18.1+1.6
−1.4 ly.[3]

WISEPA J174124.26+255319.5 distance estimates

Source Parallax, mas Distance, pc Distance, ly Distance, Pm Ref.
Scholz et al. (2011), see Section 5 4.6+1.2
−1.0		 15+3.9
−3.3		 141.9+37
−30.9		 [4]
Scholz et al. (2011), Section 4 4.6+1.9
−1.4		 15+6.2
−4.6		 141.9+58.6
−43.2		 [4]
Kirkpatrick et al. (2011), Table 6 ~ 4.7 ~ 15.3 ~ 145 [1]
Kirkpatrick et al. (2011), Table 7 182±38 5.5+1.4
−0.9		 17.9+4.7
−3.1		 169.5+44.7
−29.3		 [1]
Marsh et al. (2013)
(according Kirkpatrick et al. (2012))		 176±22 5.7+0.8
−0.6		 18.5+2.6
−2.1		 175.3+25
−19.5		 [5]
Smart et al. (2013) 4±1 13±3.3 123.4±30.9 [7]
Marsh et al. (2013) 176±26[~ 2] 5.7+1
−0.7		 18.5+3.2
−2.4		 175.3+30.4
−22.6		 [2]
Dupuy & Kraus (2013) 180±15[~ 3] 5.6+0.5
−0.4		 18.1+1.6
−1.4		 171.4+15.6
−13.2		 [3]

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

Space motion

WISE 1741+2553 has proper motion of about 1553 milliarcseconds per year.[2]

WISEPA J174124.26+255319.5 proper motion estimates

Source μ, mas/yr P. A., ° μRA, mas/yr μDEC, mas/yr Ref.
Scholz et al. (2011)1579 ± 24198.2 ± 1.6−492 ± 43−1500 ± 11[4]
Kirkpatrick et al. (2011)1555 ± 20198.3 ± 0.7−488 ± 16−1476 ± 16[1]
Marsh et al. (2013)1553 ± 16198.6 ± 0.5−495 ± 11−1472 ± 13[2]
Dupuy & Kraus (2013)1550 ± 33199.2 ± 1.3−509 ± 35−1463 ± 32[3]

The most accurate estimates are marked in bold. Italic are computed values, not italic are values, given in the sources.

See also

Another object, discovered by Scholz et al. (2011):[4]

The other eight objects, checked for binarity by Gelino et al. (2011) on Keck II:[6]

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 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).
  3. ↑ Relative parallax.
  4. ↑ Presented in Gelino et al. (2011), but this is not mentioned in Kirkpatrick et al. (2011) and Kirkpatrick et al. (2012) — according these two articles, the only discovery paper of WISE 0750+2725 is Kirkpatrick et al. (2011).

References

  1. ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 1.10 1.11 1.12 1.13 1.14 1.15 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.
  2. ↑ 2.0 2.1 2.2 2.3 2.4 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.
  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. doi:10.1126/science.1241917.
  4. ↑ 4.0 4.1 4.2 4.3 4.4 4.5 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. arXiv:1105.4059. Bibcode:2011A&A...532L...5S. doi:10.1051/0004-6361/201117297.
  5. ↑ 5.0 5.1 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.
  6. ↑ 6.0 6.1 Gelino, Christopher R.; Kirkpatrick, J. Davy; Cushing, Michael C.; Eisenhardt, Peter R.; Griffith, Roger L.; Mainzer, Amanda K.; Marsh, Kenneth A.; Skrutskie, Michael F.; Wright, Edward L. (2011). "WISE Brown Dwarf Binaries: The Discovery of a T5+T5 and a T8.5+T9 System". The Astronomical Journal 142 (2): 57. arXiv:1106.3142. Bibcode:2011AJ....142...57G. doi:10.1088/0004-6256/142/2/57.
  7. ↑ Smart, R. L.; Tinney, C. G.; Bucciarelli, B.; Marocco, F.; Abbas, U.; Andrei, A.; Bernardi, G.; Burningham, B.; Cardoso, C.; Costa, E.; Crosta, M. T.; Daprá, M.; Day-Jones, A.; Goldman, B.; Jones, H. R. A.; Lattanzi, M. G.; Leggett, S. K.; Lucas, P.; Mendez, R.; Penna, J. L.; Pinfield, D.; Smith, L.; Sozzetti, A.; Vecchiato, A. (2013). "NPARSEC: NTT Parallaxes of Southern Extremely Cool objects. Goals, targets, procedures and first results". Monthly Notices of the Royal Astronomical Society 433 (3): 2054–2063. arXiv:1306.4527. Bibcode:2013MNRAS.433.2054S. doi:10.1093/mnras/stt876.
  8. ↑ Mainzer, A.; Cushing, Michael C.; Skrutskie, M.; Gelino, C. R.; Kirkpatrick, J. Davy; Jarrett, T.; Masci, F.; Marley, Mark S.; Saumon, D.; Wright, E.; Beaton, R.; Dietrich, M.; Eisenhardt, P.; Garnavich, P.; Kuhn, O.; Leisawitz, D.; Marsh, K.; McLean, I.; Padgett, D.; Rueff, K. (2011). "The First Ultra-cool Brown Dwarf Discovered by the Wide-field Infrared Survey Explorer". The Astrophysical Journal 726 (1): 30. arXiv:1011.2279. Bibcode:2011ApJ...726...30M. doi:10.1088/0004-637X/726/1/30.
  9. ↑ Burgasser, Adam J.; Cushing, Michael C.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, Roger L.; Looper, Dagny L.; Tinney, Christopher; Simcoe, Robert A.; Bochanski, John J.; Skrutskie, Michael F.; Mainzer, A.; Thompson, Maggie A.; Marsh, Kenneth A.; Bauer, James M.; Wright, Edward L. (2011). "Fire Spectroscopy of Five Late-type T Dwarfs Discovered with the Wide-field Infrared Survey Explorer". The Astrophysical Journal 735 (2): 116. arXiv:1104.2537. Bibcode:2011ApJ...735..116B. doi:10.1088/0004-637X/735/2/116.

External links