WISE 0535−7500
Coordinates: 
05h 35m 16.8s, −75° 00′ 24.9″
| Observation data Epoch J2000[1] Equinox J2000[1] | |
|---|---|
| Constellation | Mensa |
| Right ascension | 05h 35m 16.8s[1] |
| Declination | −75° 00′ 24.9″[1] |
| Characteristics | |
| Spectral type | ≥Y1[1] |
| Apparent magnitude (J (MKO-NIR filter system)) | >21.1[1] |
| Apparent magnitude (H (MKO-NIR filter system)) | >21.6[1] |
| Astrometry | |
| Proper motion (μ) | RA: -310 ± 128[2] mas/yr Dec.: 159 ± 92[2] mas/yr |
| Parallax (π) | 250 ± 79[2] mas |
| Distance | 13.0+6.0 −3.1[3] ly (4.0+1.9 −-0.9[3] pc) |
| Other designations | |
| Database references | |
| SIMBAD | data |
WISE J053516.80−750024.9 (designation abbreviated to WISE 0535−7500) is either a brown dwarf or a free planet. It has spectral class ≥Y1 and is [1] located in constellation Mensa. It is estimated to be 13 light-years from Earth.[3] As of October 2015, that makes it the third-nearest Y dwarf, after WISE 0855−0714 and WISE 0350−5658. It is nearer than all but four naked eye stars, and the 31st-nearest star system to the Solar System. If a free planet, it is the second-nearest, the nearest being WISE 0855−0714. If a brown dwarf, then it is the ninth-nearest brown dwarf.
Discovery
WISE 0535−7500 was discovered in 2012 by J. Davy Kirkpatrick et al. from data, collected by Wide-field Infrared Survey Explorer (WISE) Earth-orbiting satellite — NASA infrared-wavelength 40-centimetre (16 in) space telescope, which mission lasted from December 2009 to February 2011. In 2012 Kirkpatrick et al. published a paper in The Astrophysical Journal, where they presented the discovery of seven new found by WISE brown dwarfs of spectral type Y, among which also was WISE 0535−7500.[1]
Distance
Trigonometric parallax of WISE 0535−7500 is 0.250 ± 0.079 arcsec, corresponding to a distance[3] of 4.0+1.9
−-0.9 pc and 13.0+6.1
−3.1 ly.
WISE 0535−7500 distance estimates
| Source | Parallax, mas | Distance, pc | Distance, ly | Ref. |
|---|---|---|---|---|
| Marsh et al. (2013) (according to Kirkpatrick et al. (2012)) | 170 ± 44 | 5.9+2.1 −1.2 | 19.2+6.7 −3.9 | [1] |
| Marsh et al. (2013) | 250 ± 79 | 21+13 −11 | 68.5+42.4 −35.9 | [2] |
| Paterson (2015) | 250 ± 79 | 4.0+1.9 −-0.9 | 13.0+6.1 −3.1 | [3] |
Non-trigonometric distance estimates are marked in italic. The best estimate is marked in bold.
Y dwarf
Brown dwarfs are defined as substellar objects that have at some time in their lives burnt deuterium in their interior. The borderline between a brown dwarf and a planet is conventionally taken to be 13 times the mass of Jupiter. All brown dwarfs are either L dwarfs, T dwarfs or Y dwarfs, in order of decreasing temperature. An increasing number after the letter in the spectral type also means decreasing temperature, a Y2 dwarf is cooler than a Y1 dwarf is cooler than a Y0 dwarf. Planets can also be L dwarfs, T dwarfs or Y dwarfs.[4]
If planets are L dwarfs or T dwarfs then they must be both young (younger than 350 million years) and heavy.[4] The cooler a Y dwarf, the higher the likelihood that it is a planet. WISE 0535-7500 is the second-nearest Y dwarf that could be of a type cooler than Y1, so could easily be the second-nearest free planet to Earth. Of the two nearer Y dwarfs, WISE 0855−0714 has an effective temperature below the freezing point of water, and WISE 0350−5658 has an effective temperature above the boiling point of water. WISE 0535−7500 is of a spectral type between that of WISE 0855−0714 and WISE 0350−5658 so the possibility exists that it may in the correct temperature range for liquid water to exist on its surface.
References
- 1 2 3 4 5 6 7 8 9 10 11 12 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. Bibcode:2012ApJ...753..156K. arXiv:1205.2122
. doi:10.1088/0004-637X/753/2/156. - 1 2 3 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. Bibcode:2013ApJ...762..119M. arXiv:1211.6977 . doi:10.1088/0004-637X/762/2/119.
- 1 2 3 4 5 Paterson, David.A. "Topics in Astronomy: Topic 8. Inappropriateness of the Lutz-Kelker equation for brown dwarfs".
- 1 2 I. Neill Reid and Stanimir A. Metchev, Chapter 5: The Brown Dwarf – Exoplanet Connection, in John W. Mason (ed.) Exoplanets: Detection, Formation, Properties, Habitability; Springer, Berlin, 2008.