WISEPC J140518.40+553421.4
Observation data
Epoch MJD 55545.11[1]      Equinox J2000[1]
Constellation Ursa Major
Right ascension 14h 05m 18.27s[1]
Declination 55° 34′ 21.22″[1]
Characteristics
Spectral type Y0 (pec?)[1][2]
Apparent magnitude (J (MKO filter system)) 20.20 ± 0.13[1]
Apparent magnitude (H (MKO filter system)) 21.45 ± 0.41[1]
Astrometry
Proper motion (μ) RA: −2263 ± 47[3] mas/yr
Dec.: 288 ± 41[3] mas/yr
Parallax (π)158.2 ± 2.6 mas[4]
Distance20.6 ± 0.3 ly
(6.3 ± 0.1 pc)
Details
Mass30[5] MJup
Radius0.86[5] RJup
Surface gravity (log g)5.0[5] cgs
Temperature350[5] K
Other designations
WISEPC J140518.40+553421.4[1]
WISEPC J1405+5534[5]
WISE J1405+5534[1]
WISE 1405+5534[1]
Database references
SIMBADdata
WISE 1405+5534 is located in the constellation Ursa Major
WISE 1405+5534 is located in the constellation Ursa Major
WISE 1405+5534
Location of WISE 1405+5534 in the constellation Ursa Major

WISEPC J140518.40+553421.4 (abbreviated WISE 1405+5534) is a brown dwarf of spectral class Y0 (pec?),[1][2] located in constellation Ursa Major at approximately 25.3 light-years from Earth.[3] It is one of the Sun's nearest neighbors.

Discovery

WISE 1405+5534 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). WISE 1405+5534 has two discovery papers: Kirkpatrick et al. (2011) and Cushing et al. (2011), however, basically with the same authors and published nearly simultaneously.[1][5]

  • 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 1405+5534.[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 1405+5534.[5] These seven objects are also the faintest seven of 98 brown dwarfs, presented in Kirkpatrick et al. (2011).[1]

Distance

Currently the most accurate distance estimate of WISE 1405+5534 is a trigonometric parallax, measured using Spitzer Space Telescope and published in 2013 by Trent Dupuy and Adam Kraus: 0.129 ± 0.019 arcsec, corresponding to a distance 7.8+1.3
−1.0 pc, or 25.3+4.4
−3.2 ly.[3]

WISE 1405+5534 distance estimates

SourceParallax, masDistance, pcDistance, lyRef.
Kirkpatrick et al. (2011), Table 6~ 8.6~ 28.0[1]
Cushing et al. (2011), Table 7~ 3.8~ 12.4[5]
Marsh et al. (2013)
(according to Kirkpatrick et al. (2012))		207 ± 394.8+1.1
−0.8		15.8+3.7
−2.5		[2]
Marsh et al. (2013)133 ± 81>3.4[~ 2]>11.1[6]
Dupuy & Kraus (2013)129 ± 19[~ 3]7.8+1.3
−1.0		25.3+4.4
−3.2		[3]

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

Space motion

WISE 1405+5534 has a large proper motion of about 2281 milliarcseconds per year.[3]

WISE 1405+5534 proper motion estimates

Sourceμ,
mas/yr		P. A.,
°		μRA,
mas/yr		μDEC,
mas/yr		Ref.
Kirkpatrick et al. (2011)2693272-2691 ± 29295 ± 271[1]
Marsh et al. (2013)2307275-2297 ± 96212 ± 137[6]
Dupuy & Kraus (2013)2281 ± 48277.3 ± 1.0−2263 ± 47288 ± 41[3]

The most accurate estimates are marked in bold.

Spectral class and temperature

The object's temperature estimate is 350 K [5] (about 77 °C / 170 °F). Its spectrum is similar with spectrum of another Y-dwarf WISE 1738+2732. However, WISE 1405+5534's spectrum has a red shift of H-band flux peak, suggesting that WISE 1405+5534 may be peculiar, therefore it is classified as Y0 (pec?).[2][5]

Variability

WISE 1405+5534 was the first Y-dwarf with a detected variability. The discovery was made with the Spitzer Space Telescope. The Y-dwarf was observed in two epochs. The first epoch was a 24 hour long observation and the second epoch was 149 days later and was also 24 hours long. The first epoch is only variable at 4.5 μm and the second epoch is variable in both 3.6 and 4.5 μm. This means that the variability changes on the timescale of months. The light curve in the second epoch had a semi-amplitude of 3.5% and a rotation period of 8.5 hours. A single bright spot reproduced the observations well. Other models that included clouds and hot spots were not able to reproduce the variability.[7]

See also

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 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.

References

  1. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 15 16 Kirkpatrick, J. Davy; Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, Amy K.; 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, Spencer Adam; 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. S2CID 16850733.
  2. 1 2 3 4 Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Eisenhardt, Peter R.; McLean, Ian S.; Mainzer, Amy K.; Burgasser, Adam J.; Tinney, Chris G.; Parker, Stephen; Salter, Graeme (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. S2CID 119279752.
  3. 1 2 3 4 5 6 7 Dupuy, T. J.; Kraus, A. L. (2013). "Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects". Science. 341 (6153): 1492–5. arXiv:1309.1422. Bibcode:2013Sci...341.1492D. doi:10.1126/science.1241917. PMID 24009359. S2CID 30379513.
  4. ↑ Kirkpatrick, J. Davy; Gelino, Christopher R.; Faherty, Jacqueline K.; Meisner, Aaron M.; Caselden, Dan; Schneider, Adam C.; Marocco, Federico; Cayago, Alfred J.; Smart, R. L.; Eisenhardt, Peter R.; Kuchner, Marc J. (2021). "The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and y Dwarfs". The Astrophysical Journal Supplement Series. 253 (1): 7. arXiv:2011.11616. Bibcode:2021ApJS..253....7K. doi:10.3847/1538-4365/abd107. S2CID 227126954.
  5. 1 2 3 4 5 6 7 8 9 10 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)". The Astrophysical Journal. 743 (1): 50. arXiv:1108.4678. Bibcode:2011ApJ...743...50C. doi:10.1088/0004-637X/743/1/50. S2CID 286881.
  6. 1 2 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. S2CID 42923100.
  7. ↑ Cushing, Michael C.; Hardegree-Ullman, Kevin K.; Trucks, Jesica L.; Morley, Caroline V.; Gizis, John E.; Marley, Mark S.; Fortney, Jonathan J.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Mace, Gregory N.; Carey, Sean J. (2016-06-01). "The First Detection of Photometric Variability in a Y Dwarf: WISE J140518.39+553421.3". The Astrophysical Journal. 823 (2): 152. arXiv:1602.06321. Bibcode:2016ApJ...823..152C. doi:10.3847/0004-637X/823/2/152. ISSN 0004-637X.
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