WISE 0350-5658
Brown dwarf WISE J035000.32−565830.2 |
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Observation dates equinox : J2000.0 , epoch : J2000.0 |
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Constellation | network | ||
Right ascension | 03 h 50 m 0.32 s | ||
declination | -56 ° 58 ′ 30.2 ″ | ||
Apparent brightness | J-band:> 22.8 mag H-band:> 21.5 mag |
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parallax | 291 ± 50 mas | ||
distance | 12.1 +5.2−1.3 Lj (3.7 +1.6−0.4 pc ) |
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Proper movement | |||
Rec. Share: | −125 ± 97 mas / a | ||
Dec. portion: | −865 ± 76 mas / a | ||
Typing | |||
Spectral class | Y1 | ||
Physical Properties | |||
Other names and catalog entries |
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WISE J035000.32-565830.2 (abbreviated name: WISE 0350-5658 ) is a brown dwarf of the spectral class Y1 in the constellation Netz . At a distance of about 12 light years , it is one of the Sun's closest neighbors .
discovery
WISE 0350-5658 was in 2012 by the American astronomer J. Davy Kirkpatrick and his colleagues of the data based on the Space Telescope Wide-field Infrared Survey Explorer (WISE) discovered that, between December 2009 and February 2011, a survey in the infrared at a wavelength of 40 cm performed. In 2012, Kirkpatrick et al. in the Astrophysical Journal the discovery of seven brown dwarfs of spectral class Y newly found by WISE, among which WISE 0350-5658 was.
The other brown dwarfs discovered by the research group in 2012 are WISE 0146 + 4234 (Y0), WISE 0359−5401 (Y0), WISE 0535−7500 (≥Y1), WISE 0713−2917 (Y0), WISE 0734−7157 (Y0) , WISE 2220-3628 (Y0).
distance
WISE 0350-5658 is one of the closest known brown dwarfs. His Trigonometric Parallax , published by Marsh et al. (2013), is 0.291 ± 0.050 arc seconds , corresponding to a distance of 3.7 +1.6−0.4 Parsec (12.1 +5.2−1.3 Light years).
Determination of the distance for WISE 0350-5658
source | Parallax (mas) | Distance (pc) | Distance (Lj) | Distance ( Pm ) |
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Marsh et al. (2013) (according to Kirkpatrick et al. (2012)) |
238 ± 38 | 4.2 + 0.8−0.6 | 13.7 +2.6−1.9 | 129.7 +24.6−17.9 |
Marsh et al. (2013) | 291 ± 50 | 3.7 +1.6−0.4 | 12.1 +5.2−1.3 |
Non-trigonometric distance determinations are marked in italics . The most precise determination is marked in bold .
Individual evidence
- ↑ a b c d e f g Kirkpatrick, JD; Gelino, CR; Cushing, MC; Mace, GN; Griffith, RL; Skrutskie, MF; Marsh, KA; Wright, EL; Eisenhardt, PR; McLean, IS; Mainzer, AK; Burgasser, AJ; Tinney, CG; Parker, S .; Salter, G .: Further Defining Spectral Type "Y" and Exploring the Low-mass End of the Field Brown Dwarf Mass Function . arxiv : 1205.2122 .
- ^ A b c d e Marsh, Kenneth A .; Wright, Edward L .; Kirkpatrick, J. Davy; Gelino, Christopher R .; Cushing, Michael C .; Griffith, Roger L .; Skrutskie, Michael F .; Eisenhardt, Peter R .: Parallax and Proper Motions of Ultra Cool Brown Dwarfs of spectral type Y and Late T . arxiv : 1211.6977 .