WISE 1541−2250
Coordinates: 
15h 41m 51.57s, −22° 50′ 25.03″
| Observation data Epoch MJD 55424.68[1] Equinox J2000[1] | |
|---|---|
| Constellation | Libra |
| Right ascension | 15h 41m 51.57s[1] |
| Declination | −22° 50′ 25.03″[1] |
| Characteristics | |
| Spectral type | Y0.5[2] |
| Apparent magnitude (J (MKO filter system)) | 21.16 ± 0.36[1] |
| Apparent magnitude (H (MKO filter system)) | 20.99 ± 0.52[1] |
| Astrometry | |
| Proper motion (μ) | RA: −895 ± 5[3] mas/yr Dec.: −88 ± 5[3] mas/yr |
| Parallax (π) | 175.1 ± 4.4[3] mas |
| Distance | 18.6 ± 0.5 ly (5.7 ± 0.1 pc) |
| Details | |
| Mass | 12 (8–12)[4] MJup |
| Radius | 1.01 (1.01–1.07)[4] RJup |
| Surface gravity (log g) | 4.50 (4.25–4.5)[4] cgs |
| Temperature | 350[4] K |
| Other designations | |
| Database references | |
| SIMBAD | data |
WISE 1541−2250 (full designation WISEPA J154151.66−225025.2) is a sub-brown or brown dwarf of spectral class Y0.5,[2] located in the constellation Libra at approximately 18.6 light-years from Earth.[3] This object received popular attention when its discovery was announced in 2011 at a distance estimated to be only about 9 light-years, which would have made it the closest brown dwarf known.[5] (For really close brown dwarfs see, for example, Luhman 16, WISE 1506+7027, Epsilon Indi Ba, Bb, or UGPS 0722-05). It is not the farthest known Y-type brown dwarf to Earth.
History of observations
Discovery
WISE 1541−2250 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. WISE 1541−2250 has two discovery papers: Kirkpatrick et al. (2011) and Cushing et al. (2011) with mostly the same authors and published nearly simultaneously.[1][4]
- Kirkpatrick et al. presented the discovery of 98 brown dwarf systems with components of spectral types M, L, T and Y, among which was WISE 1541−2250.[1][~ 1]
- Cushing et al. presented the discovery of seven brown dwarfs, one of the T9.5 type and six of the Y-type, the first members of the Y spectral class discovered and spectroscopically confirmed, including an "archetypal member" of the Y spectral class, WISE 1828+2650, and WISE 1541−2250.[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 1541−2250 is a trigonometric parallax, published in 2014 by Tinney et al.: 0.1751 ± 0.0044 arcsec, corresponding to a distance 5.71+0.15
−0.14 pc, or 18.6 ± 0.5 ly.[3]
For several months after its discovery, before the publication of its parallax by Kirkpatrick et al. in 2012,[2] WISE 1541−2250 was considered to be the nearest known brown dwarf at approximately 9 light-years from the Sun, and the seventh-nearest of all star systems, at slightly more than twice the distance of the nearest known star system Alpha Centauri. This view existed because of a very rough preliminary parallax with a baseline of 1.2 years, published in the discovery paper: 0.351 ± 0.108 arcsec, corresponding to a distance 2.8+1.3
−0.6 pc, or 9.3+4.1
−2.2 ly.[1] Also, there were other estimates: spectrophotometric distance estimate 8.2 pc (26.7 ly),[1] and photometric distance estimate 1.8+0.2
−0 pc (5.9+0.6
−0 ly).[4]
WISE 1541−2250 distance estimates
| Source | Parallax, mas | Distance, pc | Distance, ly | Distance, Pm | Ref. |
|---|---|---|---|---|---|
| Kirkpatrick et al. (2011) (Table 6) | ~ 8.2 | ~ 26.7 | ~ 253 | [1] | |
| Kirkpatrick et al. (2011) (Table 7) | 351±108 | 2.8+1.3 −0.7 |
9.3+4.1 −2.2 |
87.9+39.1 −20.7 |
|
| Cushing et al. (2011) | 1.8+0.2 −0 |
5.9+0.7 −0 |
55.5+6.2 −0 |
[4] | |
| Kirkpatrick et al. (2012) (Tables 4; 8) | ~ 238 | ~ 4.2 | ~ 13.7 | ~ 129.7 | [2] |
| Marsh et al. (2013) (according Kirkpatrick et al. (2012)) |
87±54 | 11.5+18.8 −4.4 |
37.5+61.3 −14.4 |
354.7+580.4 −135.8 |
[2] |
| Marsh et al. (2013) | −21±94 | >6.0[~ 2] | >19.6 | >185.1 | [6] |
| Dupuy & Kraus (2013) | 74±31[~ 3] | 13.5+9.7 −4 |
44.1+31.8 −13 |
417+300.6 −123.1 |
[7] |
| Beichman et al. (2014) | 176±9 | 5.68+0.31 −0.28 |
18.5+1 −0.9 |
175.3+9.4 −8.5 |
[8] |
| Tinney et al. (2014) | 175.1±4.4 | 5.71+0.15 −0.14 |
18.6±0.5 | 176.2+4.5 −4.3 |
[3] |
Non-trigonometric distance estimates are marked in italic. The most precise estimate is marked in bold.
Space motion
WISE 1541−2250 has proper motion of about 899 milliarcseconds per year.[3]
WISE 1541−2250 proper motion estimates
| Source | μ, mas/yr | P. A., ° | μRA, mas/yr | μDEC, mas/yr | Ref. |
|---|---|---|---|---|---|
| Kirkpatrick et al. (2011) | 810 ± 292 | 254.4 ± 21.4 | −780 ± 234 | −218 ± 249 | [1] |
| Marsh et al. (2013) | 1021 ± 138 | 254.3 ± 8 | −983 ± 111 | −276 ± 116 | [6] |
| Dupuy & Kraus (2013) | 870 ± 130 | 269 ± 4 | −870 ± 130 | −13 ± 58 | [7] |
| Beichman et al. (2014) | 861 ± 13 | 264.2 ± 0.9 | −857 ± 12 | −87 ± 13 | [8] |
| Tinney et al. (2014) | 899.0 ± 4.2 | 264.4 ± 0.3 | −895 ± 5 | −88 ± 5 | [3] |
The most accurate estimates are marked in bold. Italic are computed values, not italic are values, given in the sources.
Spectral class and temperature
WISE 1541−2250 is among the first known examples of a Y-class brown dwarf, the coldest spectral class of stars, and has temperature about 350 K[4] (about 77 °C / 170 °F). Its spectral class is Y0.5[2] (initially was estimated as Y0).[1][4]
See also
The other six discoveries of brown dwarfs, published in Cushing et al. (2011):[4]
- WISE 0148−7202 (T9.5)
- WISE 0410+1502 (Y0)
- WISE 1405+5534 (Y0 (pec?))
- WISE 1738+2732 (Y0)
- WISE 1828+2650 (≥Y2)
- WISE 2056+1459 (Y0)
Lists:
- List of brown dwarfs
- List of nearest stars
Notes
- ↑ These 98 brown-dwarf systems are among the first brown-dwarf systems discovered in data collected by WISE and 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 most probable 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
- ↑ 1.0 1.1 1.2 1.3 1.4 1.5 1.6 1.7 1.8 1.9 1.10 1.11 1.12 1.13 1.14 1.15 1.16 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.
- ↑ 2.0 2.1 2.2 2.3 2.4 2.5 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.
- ↑ 3.0 3.1 3.2 3.3 3.4 3.5 3.6 3.7 Tinney, C. G.; Faherty, Jacqueline K.; Kirkpatrick, J. Davy; Cushing, Mike; Morley, Caroline V.; Wright, Edward L. (2014). "The Luminosities of the Coldest Brown Dwarfs". The Astrophysical Journal 796 (1): 39. arXiv:1410.0746. Bibcode:2014ApJ...796...39T. doi:10.1088/0004-637X/796/1/39.
- ↑ 4.0 4.1 4.2 4.3 4.4 4.5 4.6 4.7 4.8 4.9 4.10 4.11 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. Bibcode:2011ApJ...743...50C. doi:10.1088/0004-637X/743/1/50.
- ↑ "NASA'S Wise Mission Discovers Coolest Class of Stars". WISE Mission News (2011-263). 2011-08-23.
- ↑ 6.0 6.1 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.
- ↑ 7.0 7.1 Dupuy, T. J.; Kraus, A. L. (2013). "Distances, Luminosities, and Temperatures of the Coldest Known Substellar Objects". Science 341 (6153): 1492. doi:10.1126/science.1241917.
- ↑ 8.0 8.1 Beichman, C.; Gelino, Christopher R.; Kirkpatrick, J. Davy; Cushing, Michael C.; Dodson-Robinson, Sally; Marley, Mark S.; Morley, Caroline V.; Wright, E. L. (2014). "WISE Y Dwarfs As Probes of the Brown Dwarf-Exoplanet Connection". The Astrophysical Journal 783 (2): 68. arXiv:1401.1194v2. Bibcode:2014ApJ...783...68B. doi:10.1088/0004-637X/783/2/68.
External links
- Choi, C. Q. (August 26, 2011). "Y dwarf star? Because they're cool, that's Y!". Space.com. Retrieved August 31, 2011.
- NASA news release
- Science news
- Solstation.com (New Objects within 20 light-years)
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