WISEPA J173835.53+273258.9
From Wikipedia, the free encyclopedia
Coordinates: 
17h 38m 35.54s, +27° 32′ 58.78″
| 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][ 1] |
| 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: 292 ± 63[ 1] mas/yr Dec.: −396 ± 22[ 1] mas/yr |
| Parallax (π) | 102 ± 18[ 1] mas |
| Distance | approx. 32 ly (approx. 10 pc) |
| Details | |
| Mass | 20 (20—30)[ 1] MJup |
| Radius | 0.93 (0.86—0.94)[ 1] RJup |
| Surface gravity (log g) | 4.75 (4.75—5.0)[ 1] cgs |
| Temperature | 350 (350—400)[ 1] K |
| Other designations | |
WISEPA J173835.53+273258.9 (designation is abbreviated to WISE 1738+2732) is a brown dwarf of spectral class Y0,[ 1][ 1] located in constellation Hercules at 32.0 light-years from Earth.[ 1]
History of observations
Discovery
WISE 1738+2732 was discovered in 2011 from data, collected by 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][ 1]
- 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.[ 1] 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, measured using Spitzer Space Telescope and published in 2013 by Trent Dupuy and Adam Kraus: 0.102 ± 0.018 arcsec, corresponding to a distance 9.8+2.1
−1.5 pc, or 32.0+6.9
−4.8 ly.[ 1]
WISE 1738+2732 distance estimates
| Source | Parallax, mas | Distance, pc | Distance, ly | Ref. |
|---|---|---|---|---|
| Kirkpatrick et al. (2011), Table 6 | 10.5 | 34.2 | [ 1] | |
| Cushing et al. (2011), Table 7 | 3.4+3.9 −0 | 11.1+12.7 −0 | [ 1] | |
| Marsh et al. (2013) (according Kirkpatrick et al. (2012)) | 111 ± 36 | 9.0+4.3 −2.2 | 29.4+14.1 −7.2 | [ 1] |
| Marsh et al. (2013) | 66 ± 50 | >6.0[~ 2] | >19.6 | [ 1] |
| Dupuy & Kraus (2013) | 102 ± 18[~ 3] | 9.8+2.1 −1.5 | 32.0+6.9 −4.8 | [ 1] |
Non-trigonometric distance estimates are marked in italic. The most precise estimate is marked in bold.
Space motion
WISE 1738+2732 has proper motion of about 493 milliarcseconds per year.[ 1]
WISE 1738+2732 proper motion estimates
| Source | μ, mas/yr | P. A., ° | μRA, mas/yr | μDEC, mas/yr | Ref. |
|---|---|---|---|---|---|
| Kirkpatrick et al. (2011) | 1141 | 148 | 602 ± 398 | -969 ± 456 | [ 1] |
| Marsh et al. (2013) | 496 | 135 | 348 ± 71 | -354 ± 55 | [ 1] |
| Dupuy & Kraus (2013) | 493 ± 40 | 144 ± 6 | 292 ± 63 | -396 ± 22 | [ 1] |
The most accurate estimates are marked in bold.
Properties
The object's temperature estimate is 350 (350—400) K.[ 1] Its spectrum is similar with spectrum of another Y-dwarf WISE 1405+5534.
See also
The other six discoveries of brown dwarfs, published in Cushing et al. (2011):[ 1]
- WISE 0148-7202 (T9.5)
- WISE 0410+1502 (Y0)
- WISE 1405+5534 (Y0 (pec?))
- WISE 1541-2250 (Y0.5)
- WISE 1828+2650 (≥Y2)
- WISE 2056+1459 (Y0)
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.
- ↑ In this parallax and distance estimates the distance value does not equal to inverse maximum likelihood parallax value, as would be in the case of exact parallax and distance values. This is due to the fact that Marsh et al. used a more sophisticated method of converting maximum likelihood parallaxes into most probable distances, that uses also some prior information, and not just the calculation of the inverse value. (The method description see in Marsh et al. (2013), Section 4).
- ↑ Relative parallax.
References
- ↑ 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)". arXiv:1108.4678v1 [astro-ph.SR]. Bibcode 2011ApJ...743...50C. doi:10.1088/0004-637X/743/1/50.
- ↑ Kirkpatrick, J. Davy; Cushing, Michael C.; Gelino, Christopher R.; Griffith, Roger L.; Skrutskie, Michael F.; Marsh, Kenneth A.; Wright, Edward L.; Mainzer, A.; 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, S. A.; 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.
- ↑ Kirkpatrick, J. D.; Gelino, C. R.; Cushing, M. C.; Mace, G. N.; Griffith, R. L.; Skrutskie, M. F.; Marsh, K. A.; Wright, E. L.; Eisenhardt, P. R.; McLean, I. S.; Mainzer, A. K.; Burgasser, A. J.; Tinney, C. G.; Parker, S.; Salter, G. (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.
- ↑ 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. arXiv:1211.6977. Bibcode:2013ApJ...762..119M. doi:10.1088/0004-637X/762/2/119.
- ↑ Dupuy, Trent J.; Kraus, Adam L. (2013). "Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects". arXiv:1309.1422v1 [astro-ph.SR]. Bibcode 2013arXiv1309.1422D.
| ||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||||
| ||||||||||||||||||||||||||
This article is issued from Wikipedia. The text is available under the Creative Commons Attribution/Share Alike; additional terms may apply for the media files.