Submitted Successfully!
To reward your contribution, here is a gift for you: A free trial for our video production service.
Thank you for your contribution! You can also upload a video entry or images related to this topic.
Version Summary Created by Modification Content Size Created at Operation
1 handwiki
Sirius Huang
 -- 779 2022-10-09 01:35:08 |
2 table format
Sirius Huang
 Meta information modification 779 2022-10-09 05:34:15 |

Video Upload Options

Do you have a full video?
Send video materials Upload full video

Confirm

Are you sure to Delete?
Yes No
Cite
If you have any further questions, please contact Encyclopedia Editorial Office.
HandWiki. CFBDSIR 1458+10. Encyclopedia. Available online: https://encyclopedia.pub/entry/28515 (accessed on 02 July 2024).
HandWiki. CFBDSIR 1458+10. Encyclopedia. Available at: https://encyclopedia.pub/entry/28515. Accessed July 02, 2024.
HandWiki. "CFBDSIR 1458+10" Encyclopedia, https://encyclopedia.pub/entry/28515 (accessed July 02, 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
Edit
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
More
©Text is available under the terms and conditions of the Creative Commons-Attribution ShareAlike (CC BY-SA) license; additional terms may apply. By using this site, you agree to the Terms and Conditions and Privacy Policy.
Upload a video for this entry
Information
Subjects: Astronomy & Astrophysics
Contributor MDPI registered users' name will be linked to their SciProfiles pages. To register with us, please refer to https://encyclopedia.pub/register :
HandWiki
View Times: 758
Entry Collection: HandWiki
Revisions: 2 times (View History)
Update Date: 09 Oct 2022
Table of Contents
    1000/1000
    Hot Most Recent
    Video Production Service
    Feedback