WISEPA J041022.71+150248.5

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Coordinates: Sky map 04h 10m 22.79s, +15° 02′ 47.47″

WISEPA J041022.71+150248.5
Observation data
Epoch MJD 55434.04[1]      Equinox J2000[1]
Constellation Taurus
Right ascension 04h 10m 22.79s[1]
Declination 15° 02′ 47.47″[1]
Characteristics
Spectral type Y0[1][2]
Apparent magnitude (J (MKO filter system)) 19.25 ± 0.5[1]
Apparent magnitude (H (MKO filter system)) 19.05 ± 0.09[1]
Astrometry
Proper motion (μ) RA: 966 ± 13[3] mas/yr
Dec.: -2218 ± 13[3] mas/yr
Parallax (π) 160 ± 9[3] mas
Distance 20 ± 1 ly
(6.3 ± 0.4 pc)
Details
Mass 3 (3—9)[4] MJup
Radius 1.22 (1.09—1.22)[4] RJup
Surface gravity (log g) 3.75 (3.75—4.25)[4] cgs
Temperature 450 (400—500)[4] K
Other designations
WISEPA J041022.71+150248.5[1]
WISEP J0410+1502[4]
WISE J0410+1502[1]
WISE 0410+1502[1]

WISE 0410+1502 (full designation WISEPA J041022.71+150248.5) is a brown dwarf[~ 1] of spectral class Y0,[1][2] located in constellation Taurus. Being approximately 20.4 light-years from Earth,[3] it is one of the Sun's nearest neighbors, especially assuming outdated parallax by Marsh et al., corresponding to even closer distance of approximately 14 light-years.[5]

History of observations[edit]

Discovery[edit]

WISE 0410+1502 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 0410+1502 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 0410+1502.[1][~ 2]
  • 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 0410+1502.[4] These seven objects are also the faintest seven of 98 brown dwarfs, presented in Kirkpatrick et al. (2011).[1]

Distance[edit]

Currently the most accurate distance estimate of WISE 0410+1502 is a trigonometric parallax, published in 2014 by Beichman et al.: 0.160 ± 0.009 arcsec, corresponding to a distance 6.3+0.4
−0.3
pc, or 20.4+1.2
−1.1
ly.[3]

WISEPA J041022.71+150248.5 distance estimates

Source Parallax, mas Distance, pc Distance, ly Distance, Pm Ref.
Kirkpatrick et al. (2011), Table 6 9.0 29.4 [1]
Cushing et al. (2011), Table 7 7.1+1.6
−3.8
23.2+5.2
−12.5
[4]
Marsh et al. (2013)
(according Kirkpatrick et al. (2012))
164 ± 24 6.1+1
−0.8
19.9+3.4
−2.5
188.2+32.3
−24
[2]
Marsh et al. (2013) 233 ± 56 4.2+1.2
−0.6
[~ 3]
13.7+3.9
−2.0
[5]
Dupuy & Kraus (2013) 132 ± 15[~ 4] 7.6+1
−0.8
24.7+3.2
−2.5
233.8+30
−23.9
[6]
Beichman et al. (2014) 160 ± 9 6.3+0.4
−0.3
20.4+1.2
−1.1
192.9+11.5
−10.3
[3]

Non-trigonometric distance estimates are marked in italic. The best estimate is marked in bold.

Space motion[edit]

WISE 0410+1502 has a large proper motion of about 2419 milliarcseconds per year.[3]

WISEPA J041022.71+150248.5 proper motion estimates

Source μ,
mas/yr
P. A.,
°
μRA,
mas/yr
μDEC,
mas/yr
Ref.
Kirkpatrick et al. (2011) 2429 155 1044 ± 236 -2193 ± 237 [1]
Marsh et al. (2013) 2355 156 974 ± 79 -2144 ± 72 [5]
Dupuy & Kraus (2013) 2426 ± 30 156.7 ± 0.9 958 ± 37 -2229 ± 29 [6]
Beichman et al. (2014) 2419 156 966 ± 13 -2218 ± 13 [3]

The most accurate estimates are marked in bold.

Temperature[edit]

The object's temperature estimate is 450 (400—500) K.[4]

See also[edit]

The other six discoveries of brown dwarfs, published in Cushing et al. (2011):[4]

Notes[edit]

  1. ^ Since its mass estimate 3 (3—9) MJup is below the lower brown dwarf mass limit ~13 MJup, it may be actually a sub-brown dwarf or a rogue planet.
  2. ^ 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.
  3. ^ 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).
  4. ^ Relative parallax.

References[edit]

  1. ^ a b c d e f g h i j k l m n o p 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.  edit
  2. ^ a b c 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.  edit
  3. ^ a b c d e f g h 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.  edit
  4. ^ a b c d e f g h i j 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. edit
  5. ^ a b c 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.  edit
  6. ^ a b 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.