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WISE 0535−7500

Coordinates: Sky map 05h 35m 16.8s, −75° 00′ 24.9″
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WISE J053516.80−750024.9

WISE 0535-7500
Credit: NASA/ESA/CSA JWST MIRI
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[2]
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[3] mas/yr
Dec.: 13±4[3] mas/yr
Parallax (π)70 ± 5 mas[3]
Distance47 ± 3 ly
(14 ± 1 pc)
Details
Mass8 - 20[3] MJup
Temperature526+16
−26[2] K
Age3 - 8[3] Gyr
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[2] and is located in constellation Mensa. It is estimated to be 47 light-years from Earth.[3]

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.[3]

Discovery

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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

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Trigonometric parallax of WISE 0535−7500 is 0.070 ± 0.005 arcsec, corresponding to a distance of 14 pc and 47 ly.[3]

Y dwarf

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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 M dwarfs, 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]

JWST observation

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WISE 0535−7500 was studied with JWST by Beiler et al. in 2024 together with 22 other late-T and Y-dwarfs. WISE 0535−7500 stands out due to it having no discernable CO2 band and an almost undetectable CO band. This could be due a low metallicity or high surface gravity. These features make this object extremely red in Spitzer colors. This object also showed stronger NH3 absorption when compared to objects of the same temperature. Other common prominent features like H2O and CH4 are present in its spectrum. But like other late-T and Y-dwarfs it is missing PH3, which is predicted to occur for these objects.[2]

See also

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References

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  1. ^ a b c d e f g h 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 Beiler, Samuel A.; Cushing, Michael C.; Kirkpatrick, J. Davy; Schneider, Adam C.; Mukherjee, Sagnick; Marley, Mark S.; Marocco, Federico; Smart, Richard L. (11 Jul 2024). "Precise Bolometric Luminosities and Effective Temperatures of 23 late-T and Y dwarfs Obtained with JWST". arXiv:2407.08518 [astro-ph.SR].
  3. ^ 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. S2CID 119249195.
  4. ^ 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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