Astronomy:WISE 1506+7027
Coordinates: 
15h 06m 49.89s, +70° 27′ 36.23″
  WISE 1506+7027 Location of WISE 1506+7027 in the constellation Ursa Minor | |
| Observation data Equinox J2000.0]] (ICRS) | |
|---|---|
| Constellation | Ursa Minor |
| Right ascension | 15h 06m 52.4406s[1] |
| Declination | +70° 27′ 25.151″[1] |
| Characteristics | |
| Spectral type | T6[2][3] |
| Apparent magnitude (J (2MASS filter system)) | 14.328±0.095[2] |
| Apparent magnitude (J (MKO filter system)) | 13.56±0.05[2] |
| Apparent magnitude (H (2MASS filter system)) | 14.150±0.203[2] |
| Apparent magnitude (H (MKO filter system)) | 13.91±0.04[2] |
| Apparent magnitude (KS (2MASS filter system)) | 14.048±0.136[2] |
| Astrometry | |
| Proper motion (μ) | RA: −1,194.179[1] mas/yr Dec.: +1,042.194[1] mas/yr |
| Parallax (π) | 193.5 ± 0.6[4] mas |
| Distance | 16.86 ± 0.05 ly (5.17 ± 0.02 pc) |
| Details | |
| Temperature | 952[4] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
WISEPC J150649.97+702736.0 (designation abbreviated to WISE 1506+7027, or WISE J1506+7027) is a brown dwarf of spectral class T6,[2][3] located in the constellation Ursa Minor. It is the nearest known star or brown dwarf in this constellation.[5] It is one of the Sun's nearest neighbors, at a distance of 16.85 light-years.[4] Brown dwarfs closer to the Sun include Luhman 16, WISE 0855−0714, ε Indi Ba and ε Indi Bb.
WISE 1506+7027 was discovered in 2011 from data collected by the Wide-field Infrared Survey Explorer (WISE) in the infrared at a wavelength of 40 cm (16 in), whose mission lasted from December 2009 to February 2011. In 2011, Kirkpatrick and colleagues published a paper in The Astrophysical Journal Supplement, where they presented the discovery of 98 new brown dwarf systems found by WISE with components of spectral types M, L, T and Y, among which was WISE 1506+7027.[2][note 1]
The first trigonometric parallax of WISE 1506+7027, which was published in 2013 by Marsh et al., is 0.310″±0.042″, corresponding to a distance of 3.4+0.7
−0.4 pc, or 11.1+2.3
−1.3 ly.[6] The Gaia spacecraft determined an updated parallax of 193.5 milliarcseconds leading to a distance of 16.85 light years.[7] WISE 1506+7027 has a large proper motion of about 1,587 milliarcseconds per year.[4]
A 2024 catalog of stars and brown dwarfs within 20 parsecs lists this object with the name "Thompson's Dwarf",[5] but this name does not appear in any other source and its origin is unclear.
Notes
- ↑ These 98 brown dwarf systems are only among first, not all brown dwarf systems, discovered from data, collected by WISE: six discoveries were published earlier (however, also listed in Kirkpatrick et al. (2011)), in Mainzer et al. (2011), and Burgasser et al. (2011), and the other discoveries were published later.
References
- ↑ 1.0 1.1 1.2 Vallenari, A. et al. (2022). "Gaia Data Release 3. Summary of the content and survey properties". Astronomy & Astrophysics. doi:10.1051/0004-6361/202243940 Gaia DR3 record for this source at VizieR.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 2.6 2.7 2.8 Kirkpatrick, J. Davy; Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, Amy K. et al. (2011). "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal Supplement 197 (2): 19. doi:10.1088/0067-0049/197/2/19. Bibcode: 2011ApJS..197...19K.
- ↑ 3.0 3.1 Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L. 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. doi:10.1088/0004-637X/753/2/156. Bibcode: 2012ApJ...753..156K.
- ↑ 4.0 4.1 4.2 4.3 Kirkpatrick, J. Davy et al. (February 2019). "Preliminary Trigonometric Parallaxes of 184 Late-T and Y Dwarfs and an Analysis of the Field Substellar Mass Function into the "Planetary" Mass Regime". The Astrophysical Journal Supplement Series 240 (2): 69. doi:10.3847/1538-4365/aaf6af. 19. Bibcode: 2019ApJS..240...19K.
- ↑ 5.0 5.1 Kirkpatrick, J. Davy et al. (April 2024). "The Initial Mass Function Based on the Full-sky 20 pc Census of ~3600 Stars and Brown Dwarfs". The Astrophysical Journal Supplement Series 271 (2): 55. doi:10.3847/1538-4365/ad24e2. Bibcode: 2024ApJS..271...55K.
- ↑ 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. doi:10.1088/0004-637X/762/2/119. Bibcode: 2013ApJ...762..119M.
- ↑ Brown, A. G. A. (August 2018). "Gaia Data Release 2: Summary of the contents and survey properties". Astronomy & Astrophysics 616: A1. doi:10.1051/0004-6361/201833051. Bibcode: 2018A&A...616A...1G. Gaia DR2 record for this source at VizieR.
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