WISE 0825+2805
 WISE 0825+2805 Credit: JWST/MIRI; Faherty et al. | |
| Observation data Epoch 2000 Equinox 2000 | |
|---|---|
| Constellation | Cancer[1] |
| Right ascension | 08h 25m 07.35720s[2] |
| Declination | +28° 05′ 48.5592″[2] |
| Characteristics | |
| Evolutionary stage | Sub-brown dwarf |
| Spectral type | Y0.5[3] |
| Apparent magnitude (J) | 22.53±0.10 |
| Apparent magnitude (H) | 23.09±0.18 |
| Astrometry | |
| Radial velocity (Rv) | −18.7±3.4[4] km/s |
| Proper motion (μ) | RA: −66.7±0.9 mas/yr[2] Dec.: −235.8±0.9 mas/yr[2] |
| Parallax (π) | 152.6±2 mas[2] |
| Distance | 21.4 ± 0.3 ly (6.55 ± 0.09 pc) |
| Details[4] | |
| Mass | 3.7±0.2 MJup |
| Radius | 1.144±0.002 RJup |
| Surface gravity (log g) | 3.85±0.02 cgs |
| Temperature | 359±3 K |
| Age | 414±23 Myr |
| Other designations | |
| WISEA J082507.37+280548.2, WISE J082507.35+280548.5 | |
| Database references | |
| SIMBAD | data |
WISE 0825+2805 (WISE J082507.35+280548.5) is a planetary mass brown dwarf or rogue planet with a spectral type of Y0.5.[3] It is about 21.4 light-years away from Earth in the Cancer constellation.[5] It is a potential member (93% chance) of the Corona of Ursa Major (CUMA) moving group, a collection of young stars that are 414±23 million years old.[4] If WISE 0825+2805 has the same age as the CUMA moving group, then its spectral energy distribution suggests it has a mass of 3.7±0.2 Jupiter masses, a radius of 1.144±0.002 Jupiter radii, and an effective temperature of 359 ± 3 K (86 ± 3 °C; 187 ± 5 °F).[4]
Discovery
WISE 0825+2805 was discovered in 2015 by Schneider et al. with the Wide-field Infrared Survey Explorer and the Hubble Space Telescope, using WFC3 near-infrared grism spectroscopy. The team also announced the discovery of three T-dwarfs as well as two additional Y-dwarfs (WISE J1206+8401 and WISE J2354+0240) in the same paper.[3]
Physical properties
WISE 0825+2805 has been observed with the James Webb Space Telescope's NIRCam and MIRI instruments. A best-fit model of WISE 0825+2805's spectral energy distribution (SED) indicates that its atmosphere is phosphine-free and diabatic. A good-fitting SED model requires an effective temperature of 350 Kelvin and a surface gravity of log g = 4.0. Alternatively, a lower surface gravity could improve the SED fit. The model parameters correspond to a mass of 5 MJ and an age of 800 Myrs.[6] On the other hand, if WISE 0825+2805 is the same age as the Corona of Ursa Major moving group (414±23 Myr), then the best-fit SED indicates a mass of 3.7±0.2 MJ, a radius of 1.144±0.002 RJ, and an effective temperature of 359 ± 3 K (86 ± 3 °C; 187 ± 5 °F).[4]
See also
References
- ^ Roman, Nancy G. (1987). "Identification of a constellation from a position". Publications of the Astronomical Society of the Pacific. 99 (617): 695. Bibcode:1987PASP...99..695R. doi:10.1086/132034. Constellation record for this object at VizieR.
- ^ a b c d Kirkpatrick, J. Davy; et al. (2021). "The Field Substellar Mass Function Based on the Full-sky 20 pc Census of 525 L, T, and y Dwarfs". The Astrophysical Journal Supplement Series. 253 (1): 7. arXiv:2011.11616. Bibcode:2021ApJS..253....7K. doi:10.3847/1538-4365/abd107.
- ^ a b c Schneider, Adam C.; Cushing, Michael C.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Mace, Gregory N.; Wright, Edward L.; Eisenhardt, Peter R.; Skrutskie, M. F.; Griffith, Roger L.; Marsh, Kenneth A. (2015-05-01). "Hubble Space Telescope Spectroscopy of Brown Dwarfs Discovered with the Wide-field Infrared Survey Explorer". The Astrophysical Journal. 804 (2): 92. arXiv:1502.05365. Bibcode:2015ApJ...804...92S. doi:10.1088/0004-637X/804/2/92. ISSN 0004-637X.
- ^ a b c d e Kiman, Rocio; Beichman, Charles A.; Diaz, Azul Ruiz; Faherty, Jacqueline K.; Lacy, Brianna; Suarez, Genaro; Marocco, Federico; Kirkpatrick, J. Davy; Gagne, Jonathan (January 2026). "The Diversity of Cold Worlds: Age and Characterization of the Exoplanet COCONUTS-2b". The Astronomical Journal. 171 (2): 60. arXiv:2511.20923. doi:10.3847/1538-3881/ae230f.
- ^ Kirkpatrick, J. Davy; et al. (December 2023). "The Initial Mass Function Based on the Full-sky 20-pc Census of ∼3,600 Stars and Brown Dwarfs". The Astrophysical Journal Supplement Series. 271 (2): 55. arXiv:2312.03639. Bibcode:2024ApJS..271...55K. doi:10.3847/1538-4365/ad24e2.
- ^ Leggett, S. K.; Tremblin, Pascal (2024-01-01). "James Webb Space Telescope Spectra of Cold Brown Dwarfs are Well-reproduced by Phosphine-free, Diabatic, ATMO2020++ Models". Research Notes of the American Astronomical Society. 8 (1): 13. Bibcode:2024RNAAS...8...13L. doi:10.3847/2515-5172/ad1b61. ISSN 2515-5172.
