Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Boötes |
Right ascension | 14h 58m 29.0s |
Declination | 10° 13′ 43″ |
Characteristics | |
Whole system ( MKO filter system) | |
Apparent magnitude (Y) | 20.58 ± 0.21 [1] |
Apparent magnitude (J) | 19.67 ± 0.02 [2] [1] |
Apparent magnitude (H) | 20.06 ± 0.10 [2] [1] |
Apparent magnitude (K) | 20.50 ± 0.24 [1] |
Component A ( MKO filter system) | |
Spectral type | T9 [1] |
Apparent magnitude (Y) | 20.81 ± 0.21 [1] |
Apparent magnitude (J) | 19.83 ± 0.02 [1] |
Apparent magnitude (H) | 20.18 ± 0.10 [1] |
Apparent magnitude (K) | 20.63 ± 0.24 [1] |
Component B ( MKO filter system) | |
Spectral type | Y0V [1] |
Apparent magnitude (Y) | 22.36 ± 0.24 [1] |
Apparent magnitude (J) | 21.85 ± 0.06 [1] |
Apparent magnitude (H) | 22.51 ± 0.16 [1] |
Apparent magnitude (K) | 22.83 ± 0.30 [1] |
Astrometry | |
Proper motion (μ) |
RA: 174.0 ± 2.0
[3]
mas/
yr Dec.: −381.8 ± 2.7 [3] mas/ yr |
Parallax (π) | 31.3 ± 2.5 mas [3] |
Distance | 104 ± 8
ly (32 ± 3 pc) |
Orbit [4] | |
Primary | A |
Companion | B |
Period (P) | 20+17 −6—35+28 −10 yr |
Details | |
Component A | |
Mass | (11.1 ± 0.7)—(36 ± 4) [4] MJup |
Radius | 0.15 R☉ |
Luminosity (bolometric) | 10−5.72 ± 0.13 [1] L☉ |
Surface gravity (log g) | (4.37 ± 0.03)—(5.06 ± 0.07) [4] cgs |
Temperature | (479 ± 20)—(605 ± 55) [4] K |
Component B | |
Mass | 6–15 [4] MJup |
Radius | 0.13 R☉ |
Luminosity (bolometric) | 10−6.53 ± 0.13 [1] L☉ |
Surface gravity (log g) | (4.10 ± 0.10)—(4.69 ± 0.03) [4] cgs |
Temperature | 370 ± 40 [4] K |
Position (relative to A) | |
Component | B |
Epoch of observation | UT 2012 April 13 |
Angular distance | 127.2 ± 1.4 mas [1] |
Position angle | 318.1 ± 1.1° [1] |
Projected separation | 4.06 AU [1] [3] |
Other designations | |
Database references | |
SIMBAD | data |
CFBDSIR J145829+101343 (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, [1] located in constellation Boötes about 104 light-years away from Earth. [3]
The smaller companion, CFBDSIR 1458+10B, has a surface temperature of approx 370 K (≈100 °C) [6] [7]. It used to be known as the coolest known brown dwarf until the discovery of WISE 1828+2650 in August 2011. [8]
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. [9] [note 1]
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. [6] [4]
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. [1]
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.
[3]
CFBDSIR 1458+10 distance estimates
Source | Parallax, mas | Distance, pc | Distance, ly | Ref. |
---|---|---|---|---|
Delorme et al. (2010) | ~23 | ~75 | [9] | |
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 |
[10] |
Dupuy & Liu (2012) | 31.3 ± 2.5 | 31.9+2.8 −2.4 |
104.2+9.0 −7.7 |
[3] |
Non-trigonometric distance estimates are marked in italic. The best estimate is marked in bold.
CFBDSIR 1458+10 has proper motion of about 420 milliarcseconds per year. [3]
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 | [9] [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 | [10] |
Dupuy & Liu (2012) | 419.6 ± 2.6 | 155.50 ± 0.28 | 174.0 ± 2.0 | −381.8 ± 2.7 | [3] |
The most accurate estimates are marked in bold.
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]
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 | [1] |
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. [9] [4] [11] In 2012 Liu et al. assigned it a spectral class Y0. [1]
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. [7]
The other two brown dwarf binary systems, observed by Liu et al. with Keck II LGS- AO in 2012: [1]