WISE 1405+5534 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). WISE 1405+5534 has two discovery papers: Kirkpatrick et al. (2011) and Cushing et al. (2011), however, basically with the same authors and published nearly simultaneously.[1][5]
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 1405+5534.[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 1405+5534.[5] These seven objects are also the faintest seven of 98 brown dwarfs, presented in Kirkpatrick et al. (2011).[1]
Distance
An older distance estimate of WISE 1405+5534 is a
trigonometric parallax, measured using
Spitzer Space Telescope and published in 2013 by Trent Dupuy and Adam Kraus: 0.129 ± 0.019
arcsec, corresponding to a distance 7.8+1.3 −1.0pc, or 25.3+4.4 −3.2ly.[3] Later the parallax was refined to 158.2±2.6 mas, showing that it is closer at about 6.3 pc, or 20.6 light years.[4]
The object's temperature estimate is 350
K[5] (about 77 °C / 170 °F). Its spectrum is similar with spectrum of another Y-dwarf
WISE 1738+2732. However, WISE 1405+5534's spectrum has a red shift of H-band flux peak, suggesting that WISE 1405+5534 may be peculiar, therefore it is classified as Y0 (pec?).[2][5] One work has shown that models that include optically thin
sulfides,
KCl and
Cr clouds fit the observed photometry of WISE 1405+5534 better. This is however a tentative result. At this low temperature of WISE 1405+5534 water should condense and form clouds.[7] Another team observed WISE 1405+5534 with the
Very Large Array to search for radio emission coming from an
aurora, but was not able to detect any.[8]
Variability
WISE 1405+5534 was the first Y-dwarf with a detected variability. The discovery was made with the
Spitzer Space Telescope. The Y-dwarf was observed in two epochs. The first epoch was a 24-hour-long observation and the second epoch was 149 days later and was also 24 hours long. The first epoch is only variable at 4.5 μm and the second epoch is variable in both 3.6 and 4.5 μm. This means that the variability changes on the timescale of months. The light curve in the second epoch had a semi-amplitude of 3.5% and a rotation period of 8.5 hours. A single bright spot reproduced the observations well. Other models that included clouds and hot spots were not able to reproduce the variability.[9]
^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).
^
abcdefghijklmnopKirkpatrick, 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.
S2CID16850733.
^
abcdKirkpatrick, 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.
S2CID119279752.
^
abcdefghijCushing, 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.
S2CID286881.