WISE 0535−7500

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Coordinates: Sky map 05h 35m 16.8s, −75° 00′ 24.9″

WISE J053516.80−750024.9
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: −127±4[2] mas/yr
Dec.: 13±4[2] mas/yr
Parallax (π)70 ± 5[2] mas
Distance47 ± 3 ly
(14 ± 1 pc)
Details
Mass1.5 - 8[2] MJup
Age300 - 6000[2] Myr
Other designations
WISE J053516.80−750024.9,[1]
WISE 0535−7500[1]
Database references
SIMBADdata
Hertzsprung-Russell diagram of all the nearest stars out to Gliese 1, as well as most brown dwarfs and some planets.
Hertzsprung-Russell diagram of all the nearest stars out to Gliese 1, as well as most brown dwarfs and some planets. WISE 0535−7500 is at bottom right

WISE J053516.80−750024.9 (designation abbreviated to WISE 0535−7500) is either a sub-brown dwarf or a free planet. It has spectral class ≥Y1 and is [1] located in constellation Mensa. It is estimated to be 47 light-years from Earth.[2]

In 2017, more accurate analysis found it to be a binary system made up of two substellar objects of spectral class≥Y1 in orbit less than one astronomical unit from each other.[2]

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 0.070 ± 0.005 arcsec, corresponding to a distance of 14 pc and 47 ly.[2]

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.[3]

References[]

  1. ^ a b c d e f g h i j Kirkpatrick, J. Davy; 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. arXiv:1205.2122. Bibcode:2012ApJ...753..156K. doi:10.1088/0004-637X/753/2/156. S2CID 119279752.
  2. ^ a b c d e f g h Leggett, S. K.; et al. (2017). "The Y-type Brown Dwarfs: Estimates of Mass and Age from New Astrometry, Homogenized Photometry, and Near-infrared Spectroscopy". The Astrophysical Journal. 842 (2). 118. arXiv:1704.03573. Bibcode:2017ApJ...842..118L. doi:10.3847/1538-4357/aa6fb5.
  3. ^ 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.
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