WISE 1405+5534

WISE 1405+5534 (full designation WISEPC J140518.40+553421.4) 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.

WISEPC J140518.40+553421.4

Observation data Epoch MJD 55545.11[1]      Equinox J2000[1]
Constellation	Ursa Major
Right ascension	14^h 05^m 18.27^s[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)	129 ± 19[3] mas
Distance	approx. 25 ly (approx. 8 pc)
Details
Mass	30[4] MJup
Radius	0.86[4] RJup
Surface gravity (log g)	5.0[4] cgs
Temperature	350[4] K
Other designations
WISEPC J140518.40+553421.4[1] WISEPC J1405+5534[4] WISE J1405+5534[1] WISE 1405+5534[1]
Database references
SIMBAD	data

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][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 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.[4] 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

Source	Parallax, mas	Distance, pc	Distance, ly	Ref.
Kirkpatrick et al. (2011), Table 6		~ 8.6	~ 28.0	[1]
Cushing et al. (2011), Table 7		~ 3.8	~ 12.4	[4]
Marsh et al. (2013) (according to Kirkpatrick et al. (2012))	207 ± 39	4.8^+1.1 −0.8	15.8^+3.7 −2.5	[2]
Marsh et al. (2013)	133 ± 81	>3.4[~ 2]	>11.1	[5]
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

Source	μ, mas/yr	P. A., °	μRA, mas/yr	μDEC, mas/yr	Ref.
Kirkpatrick et al. (2011)	2693	272	-2691 ± 292	95 ± 271	[1]
Marsh et al. (2013)	2307	275	-2297 ± 96	212 ± 137	[5]
Dupuy & Kraus (2013)	2281 ± 48	277.3 ± 1.0	−2263 ± 47	288 ± 41	[3]

The most accurate estimates are marked in bold.

Spectral class and temperature

The object's temperature estimate is 350 K [4] (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][4]

See also

• List of star systems within 25–30 light-years
• WISE 0148-7202 (T9.5)
• WISE 0410+1502 (Y0)
• WISE 1541-2250 (Y0.5)
• WISE 1738+2732 (Y0)
• WISE 1828+2650 (≥Y2)
• WISE 2056+1459 (Y0)

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. 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. 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.
3. 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.
4. 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.
5. 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.