WISEPA J173835.53+273258.9
Observation data
Epoch MJD 55451.22[1]      Equinox J2000[1]
Constellation Hercules
Right ascension 17h 38m 35.54s[1]
Declination 27° 32′ 58.78″[1]
Characteristics
Spectral type Y0[1][2]
Apparent magnitude (J (MKO filter system)) 19.47 ± 0.08[1]
Apparent magnitude (H (MKO filter system)) 20.66 ± 0.38[1]
Astrometry
Proper motion (μ) RA: 337.1±0.8 mas/yr[3]
Dec.: −343.4±0.8 mas/yr[3]
Parallax (π)130.9 ± 2.1 mas[3]
Distance24.9 ± 0.4 ly
(7.6 ± 0.1 pc)
Details
Mass20 (20–30)[4] MJup
Radius0.93 (0.86–0.94)[4] RJup
Surface gravity (log g)4.75 (4.75–5.0)[4] cgs
Temperature450±88[3] K
Other designations
WISEPA J173835.53+273258.9[1]
WISEP J1738+2732[4]
WISE J1738+2732[1]
WISE 1738+2732[1]
Database references
SIMBADdata

WISEPA J173835.53+273258.9 (abbreviated WISE 1738+2732) is a brown dwarf of spectral class Y0,[1][2] located in the constellation Hercules at 24.9 light-years from Earth.[3]

History of observations

Discovery

WISE 1738+2732 was discovered in 2011 from data, collected by the Wide-field Infrared Survey Explorer (WISE) Earth-orbiting satellite — NASA infrared-wavelength 40 cm (16 in) space telescope, which mission lasted from December 2009 to February 2011. WISE 1738+2732 has two discovery papers: Kirkpatrick et al. (2011) and Cushing et al. (2011), however, basically with the same authors and published nearly simultaneously.[1][4]

  • Kirkpatrick et al. presented discovery of 98 new found by WISE brown dwarf systems with components of spectral types M, L, T and Y, among which also was WISE 1738+2732.[1][~ 1]
  • Cushing et al. presented discovery of seven brown dwarfs — one of T9.5 type, and six of Y-type — first members of the Y spectral class, ever discovered and spectroscopically confirmed, including "archetypal member" of the Y spectral class WISE 1828+2650, and WISE 1738+2732.[4] These seven objects are also the faintest seven of 98 brown dwarfs, presented in Kirkpatrick et al. (2011).[1]

Distance

Currently the most accurate distance estimate of WISE 1738+2732 is a trigonometric parallax, published in 2021 by Kirkpatrick et al.: 130.9±2.1 mas, corresponding to a distance of 7.6±0.1 pc, or 24.9±0.4 ly.[3]

Space motion

WISE 1738+2732 has a proper motion of 481.2±1.1 milliarcseconds per year.[3]

Properties

The object's temperature estimate is 350 (350–400) K.[4] Its spectrum is similar with spectrum of another Y-dwarf WISE 1405+5534.

Disequilibrium chemistry models suggest that this Y-dwarf has a low mass of about 3-9 MJup, making it a possible isolated planetary-mass object, together with WISE 0350-5658.[5] A more recent paper finds a mass of 5-14 MJup.[6]

WISE 1405 is variable in the near- and mid-infrared. The observations were made with the Gemini Observatory and Spitzer. It has a rotation period of 6.0±0.1 hours and the amplitude is 3% for 4.5 μm and may be as high as 5-30% in the near-infrared. This dependence on wavelength can be reproduced with patchy cloud layers made up of potassium chloride (KCl) and sodium sulfide (Na2S).[7]

See also

Notes

  1. ↑ 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. 1 2 3 4 5 6 7 8 9 10 11 12 13 14 Kirkpatrick, J. Davy; Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, Amy K.; Eisenhardt, Peter R.; McLean, Ian S.; Thompson, Maggie A.; Bauer, James M.; Benford, Dominic J.; Bridge, Carrie R.; Lake, Sean E.; Petty, Sara M.; Stanford, Spencer Adam; Tsai, Chao-Wei; Bailey, Vanessa; Beichman, Charles A.; Bloom, Joshua S.; Bochanski, John J.; Burgasser, Adam J.; Capak, Peter L.; Cruz, Kelle L.; Hinz, Philip M.; Kartaltepe, Jeyhan S.; Knox, Russell P.; Manohar, Swarnima; Masters, Daniel; Morales-Calderon, Maria; Prato, Lisa A.; Rodigas, Timothy J.; Salvato, Mara; Schurr, Steven D.; Scoville, Nicholas Z.; Simcoe, Robert A.; Stapelfeldt, Karl R.; Stern, Daniel; Stock, Nathan D.; Vacca, William D. (2011). "The First Hundred Brown Dwarfs Discovered by the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal Supplement. 197 (2): 19. arXiv:1108.4677v1. Bibcode:2011ApJS..197...19K. doi:10.1088/0067-0049/197/2/19. S2CID 16850733.
  2. 1 2 Kirkpatrick, J. Davy; Gelino, Christopher R.; Cushing, Michael C.; Mace, Gregory N.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Eisenhardt, Peter R.; McLean, Ian S.; Mainzer, Amy K.; Burgasser, Adam J.; Tinney, Chris G.; Parker, Stephen; Salter, Graeme (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.
  3. 1 2 3 4 5 6 7 Kirkpatrick, J. Davy; Gelino, Christopher R.; et al. (March 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. S2CID 227126954.
  4. 1 2 3 4 5 6 7 Cushing, Michael C.; Kirkpatrick, J. Davy; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Mainzer, A.; Marsh, Kenneth A.; Beichman, Charles A.; Burgasser, Adam J.; Prato, Lisa A.; Simcoe, Robert A.; Marley, Mark S.; Saumon, D.; Freedman, Richard S.; Eisenhardt, Peter R.; Wright, Edward L. (2011). "The Discovery of Y Dwarfs using Data from the Wide-field Infrared Survey Explorer (WISE)". The Astrophysical Journal. 743 (1): 50. arXiv:1108.4678. Bibcode:2011ApJ...743...50C. doi:10.1088/0004-637X/743/1/50. S2CID 286881.
  5. ↑ Leggett, S. K.; Tremblin, P.; Saumon, D.; Marley, M. S.; Morley, Caroline V.; Amundsen, D. S.; Baraffe, I.; Chabrier, G. (2016-06-01). "Near-infrared Spectroscopy of the Y0 WISEP J173835.52+273258.9 and the Y1 WISE J035000.32-565830.2: The Importance of Non-equilibrium Chemistry". The Astrophysical Journal. 824 (1): 2. arXiv:1603.09400. Bibcode:2016ApJ...824....2L. doi:10.3847/0004-637X/824/1/2. ISSN 0004-637X.
  6. ↑ Leggett, S. K.; Tremblin, P.; Esplin, T. L.; Luhman, K. L.; Morley, Caroline V. (2017-06-01). "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. ISSN 0004-637X.
  7. ↑ Leggett, S. K.; Cushing, Michael C.; Hardegree-Ullman, Kevin K.; Trucks, Jesica L.; Marley, M. S.; Morley, Caroline V.; Saumon, D.; Carey, S. J.; Fortney, J. J.; Gelino, C. R.; Gizis, J. E.; Kirkpatrick, J. D.; Mace, G. N. (2016-10-01). "Observed Variability at 1 and 4 μm in the Y0 Brown Dwarf WISEP J173835.52+273258.9". The Astrophysical Journal. 830 (2): 141. arXiv:1607.07888. Bibcode:2016ApJ...830..141L. doi:10.3847/0004-637X/830/2/141. ISSN 0004-637X.
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