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HandWiki. CFBDSIR 1458+10. Encyclopedia. Available online: https://encyclopedia.pub/entry/28515 (accessed on 15 November 2024).
HandWiki. CFBDSIR 1458+10. Encyclopedia. Available at: https://encyclopedia.pub/entry/28515. Accessed November 15, 2024.
HandWiki. "CFBDSIR 1458+10" Encyclopedia, https://encyclopedia.pub/entry/28515 (accessed November 15, 2024).
HandWiki. (2022, October 09). CFBDSIR 1458+10. In Encyclopedia. https://encyclopedia.pub/entry/28515
HandWiki. "CFBDSIR 1458+10." Encyclopedia. Web. 09 October, 2022.
CFBDSIR 1458+10
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The content is sourced from: https://handwiki.org/wiki/Astronomy:CFBDSIR_1458%2B10

CFBDSIR J145829+101343 (Coordinates: 14h 58m 29.0s, +10° 13′ 43″, designation abbreviated to CFBDSIR 1458+10, or CFBDSIR J1458+1013) is a binary system of two brown dwarfs of spectral classes T9 + Y0 orbiting each other, located in constellation Boötes about 104 light-years away from Earth. The smaller companion, CFBDSIR 1458+10B, has a surface temperature of approx 370 K (≈100 °C) and used to be known as the coolest known brown dwarf until the discovery of WISE 1828+2650 in August 2011.

brown dwarfs 29.0s cfbdsir

1. Discovery

CFBDSIR 1458+10 A was discovered in 2010 by Delorme et al. from the Canada-France Brown Dwarf Survey using the facilities MegaCam and WIRCam mounted on the 3.6 m Canada-France-Hawaii Telescope, located on Mauna Kea Observatory, Hawaii. Image in z` band was taken on 2004 July 15 with MegaCam, and image in J band was taken on 2007 April 1 with WIRCam. In 2009 they made follow-up photometry, using the SOFI near infrared camera at the ESO 3.5 m New Technology Telescope (NTT) at the La Silla Observatory, Chile . In 2010 Delorme et al. published a paper in Astronomy and Astrophysics where they reported the identification of 55 T-dwarfs candidates, six of which were photometrically confirmed as T-dwarfs, including 3 ultracool brown dwarfs (later than T7 dwarfs and possible Y dwarfs), including CFBDSIR 1458+10.[1][2]

1.1. Discovery of B

CFBDSIR 1458+10 B was discovered in 2011 by Liu et al. with laser guide star (LGS) adaptive optics (AO) system of the 10 m Keck II Telescope on Mauna Kea, Hawaii, using infra-red camera NIRC2 (the observations were made on 2010 May 22 and 2010 July 8 (UT)). In 2011 Liu et al. published a paper in The Astrophysical Journal where they presented discovery of CFBDSIR 1458+10 system component B (the only discovery presented in the article). Also they presented a near-infrared (J-band) trigonometric parallax of the system, measured using WIRCam on the Canada-France-Hawaii Telescope (CFHT), Mauna Kea, in seven epochs during the 2009–2010; and spectroscopy with the X-Shooter spectrograph at the European Southern Observatory's Very Large Telescope (VLT) Unit Telescope 2 (UT2) in Chile (the observations have been performed from May 5 to July 9, 2010), that allowed to calculate the temperature (and other physical parameters) of the two brown dwarfs.[3][4]

2. 2012 Keck LGS-AO Imaging

In 2012 CFBDSIR 1458+10 system was observed by Liu et al. with laser guide star (LGS) adaptive optics (AO) system of the 10 m Keck II Telescope on Mauna Kea, Hawaii, using infra-red camera NIRC2 (the observations were made on 2012 April 13 (UT)). In 2012 Liu et al. published a paper in The Astrophysical Journal where they presented results of observations with Keck II LGS-AO of three brown dwarf binary systems, binarity of the two of which was first presented in this paper, and binarity of the other one, CFBDSIR 1458+10, was known before.[5]

3. Distance

Trigonometric parallax of CFBDSIR 1458+10, measured under The Hawaii Infrared Parallax Program by Dupuy & Liu in 2012, is 31.3 ± 2.5 mas, corresponding to a distance 31.9+2.8−2.4 pc, or 104.2+9.0−7.7 ly.[6]

CFBDSIR 1458+10 distance estimates

Source Parallax, mas Distance, pc Distance, ly Ref.
Delorme et al. (2010)   ~23 ~75 [1]
Liu et al. (2011) 43.3 ± 4.5 23.1 ± 2.4 75.3 ± 7.8 [4]
Dupuy & Liu (2012)
(preprint version 1)		 34.0 ± 2.6 29.4+2.4−2.1 95.9+7.9−6.7 [7]
Dupuy & Liu (2012) 31.3 ± 2.5 31.9+2.8−2.4 104.2+9.0−7.7 [6]

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

4. Space Motion

CFBDSIR 1458+10 has proper motion of about 420 milliarcseconds per year.[6]

CFBDSIR 1458+10 proper motion estimates

Source μ,
mas/yr		 P. A.,
°		 μRA,
mas/yr		 μDEC,
mas/yr		 Ref.
Delorme et al. (2010) 444 ± 16 157.5 ± 2.1 170 ± 16 −410 ± 16 [1][4]
Liu et al. (2011) 432 ± 6 154.2 ± 0.7 188 −389 [4]
Dupuy & Liu (2012)
(preprint version 1)		 418.1 ± 3.2 155.4 ± 0.4 174.3 ± 3.0 −380.0 ± 3.2 [7]
Dupuy & Liu (2012) 419.6 ± 2.6 155.50 ± 0.28 174.0 ± 2.0 −381.8 ± 2.7 [6]

The most accurate estimates are marked in bold.

5. Physical Properties

Using three models, Liu et al. calculated physical properties of CFBDSIR 1458+10 components.[4]

From Lyon/COND models and Lbol:

Component and
assumed age		 Mass,
MJup		 Teff,
K		 log g,
cm/s2		 P,
yr
A (for 1 Gyr) 12.1 ± 1.9 556 ± 48 4.45 ± 0.07  
B (for 1 Gyr) 5.8 ± 1.3 360 ± 40 4.10 ± 0.10 35+28−10
A (for 5 Gyr) 31 ± 4 605 ± 55 5.00 ± 0.08  
B (for 5 Gyr) 14 ± 3 380 ± 50 4.58 ± 0.11 22+18−6

From Burrows et al. (1997) models and Lbol):

Component and
assumed age		 Mass,
MJup		 Teff,
K		 log g,
cm/s2		 P,
yr
A (for 1 Gyr) 13 ± 2 550 ± 50 4.47 ± 0.07  
B (for 1 Gyr) 6.8 ± 1.5 350 ± 40 4.14 ± 0.10 33+27−7
A (for 5 Gyr) 36 ± 4 600 ± 60 5.06 ± 0.07  
B (for 5 Gyr) 17 ± 4 380 ± 50 4.65 ± 0.12 20+17−6

From Burrows et al. (2003) models and M(J):

Component and
assumed age		 Mass,
MJup		 Teff,
K		 log g,
cm/s2		 P,
yr
A (for 1 Gyr) 11.1 ± 0.7 479 ± 20 4.37 ± 0.03  
B (for 1 Gyr) 7.6 ± 0.6 386 ± 15 4.19 ± 0.04 34+28−10
A (for 5 Gyr) >25 >483 >4.85  
B (for 5 Gyr) 18.8 ± 1.3 407 ± 15 4.69 ± 0.03 <22

The adopted surface temperature of B is 370 ± 40 K, and adopted mass is 6-15 MJup.[4]

5.1. Luminosity

At the time of its discovery, CFBDSIR 1458+10 B was the least luminous brown dwarf known.[4]

CFBDSIR 1458+10 bolometric luminosity estimates

Source Lbol/L⊙ (A) Lbol/L⊙ (B) Ref.
Liu et al. (2011) 10−6.02 ± 0.14
((1.1 ± 0.4) × 10−6)		 10−6.74 ± 0.19
((2.0 ± 0.9) × 10−7)		 [4]
Liu et al. (2012) 10−5.72 ± 0.13 10−6.53 ± 0.13 [5]

6. B's Spectral Class

In Liu et al. (2011) CFBDSIR 1458+10 B was assigned to the spectral class >T10,[4] it was proposed that CFBDSIR 1458+10 B may be a member of the Y spectral class of brown dwarfs.[1][4][8] In 2012 Liu et al. assigned it a spectral class Y0.[5]

7. Water Clouds

Due to the low surface temperature for a brown dwarf, CFBDSIR 1458+10 B may be able to form water clouds in its upper atmosphere.[9]

References

  1. Delorme, P.; Albert, L.; Forveille, T.; Artigau, E.; Delfosse, X.; Reylé, C.; Willott, C. J.; Bertin, E. et al. (2010). "Extending the Canada-France brown dwarfs survey to the near-infrared: first ultracool brown dwarfs from CFBDSIR". Astronomy and Astrophysics 518: A39. doi:10.1051/0004-6361/201014277. Bibcode: 2010A&A...518A..39D.  https://dx.doi.org/10.1051%2F0004-6361%2F201014277
  2. The other two ultracool brown dwarfs are CFBDSIR221903.07+002417.92 and CFBDSIR221505.06+003053.11. Three earlier type confirmed T dwarfs, as well as 49 unconfirmed candidates, are not listed in the article. (However, it is mentioned, that two of three earlier type confirmed T dwarfs are re-identifications of already spectroscopically confirmed CFBDS brown dwarfs).
  3. European Southern Observatory. "A Very Cool Pair of Brown Dwarfs", 23 March 2011 http://www.eso.org/public/news/eso1110/
  4. T10) Brown Dwarf in a Binary System". The Astrophysical Journal 740 (2): 108. doi:10.1088/0004-637X/740/2/108. Bibcode: 2011ApJ...740..108L.  https://dx.doi.org/10.1088%2F0004-637X%2F740%2F2%2F108" id="ref_4">Liu, Michael C.; Delorme, Philippe; Dupuy, Trent J.; Bowler, Brendan P.; Albert, Loic; Artigau, Etienne; Reylé, Celine; Forveille, Thierry et al. (2011). "CFBDSIR J1458+1013B: A Very Cold (>T10) Brown Dwarf in a Binary System". The Astrophysical Journal 740 (2): 108. doi:10.1088/0004-637X/740/2/108. Bibcode: 2011ApJ...740..108L.  https://dx.doi.org/10.1088%2F0004-637X%2F740%2F2%2F108
  5. Liu, Michael C.; Dupuy, Trent J.; Bowler, Brendan P.; Leggett, S. K.; Best, William M. J. (2012). "Two Extraordinary Substellar Binaries at the T/Y Transition and the Y-band Fluxes of the Coolest Brown Dwarfs". The Astrophysical Journal 758 (1): 57. doi:10.1088/0004-637X/758/1/57. Bibcode: 2012ApJ...758...57L.  https://dx.doi.org/10.1088%2F0004-637X%2F758%2F1%2F57
  6. Dupuy, Trent J.; Liu, Michael C. (2012). "The Hawaii Infrared Parallax Program. I. Ultracool Binaries and the L/T Transition". The Astrophysical Journal Supplement 201 (2): 19. doi:10.1088/0067-0049/201/2/19. Bibcode: 2012ApJS..201...19D.  https://dx.doi.org/10.1088%2F0067-0049%2F201%2F2%2F19
  7. Dupuy, Trent J.; Liu, Michael C. (2012). "The Hawaii Infrared Parallax Program. I. Ultracool Binaries and the L/T Transition". arXiv:1201.2465v1 [astro-ph.SR]. Cite has empty unknown parameter: |bibcode= (help) //arxiv.org/archive/astro-ph.SR
  8. Paul Gilster "Brown Dwarfs and Planets: A Blurry Boundary", Tau Zero Foundation, 23 March 2011 http://www.centauri-dreams.org/?p=17264
  9. Space.com "Coldest Known Star Is a Real Misfit", 23 March 2011 http://www.space.com
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