Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Taurus |
Right ascension | 04h 07m 07.527s [1] |
Declination | +15° 46′ 45.540″ [1] |
Characteristics | |
Spectral type | L3.5 [2] |
Apparent magnitude (G) | 20.704 ± 0.014 [1] |
Apparent magnitude (J) | 15.478 ± 0.058 [1] |
Apparent magnitude (H) | 14.354 ± 0.057 [1] |
Apparent magnitude (K) | 13.559 ± 0.038 [1] |
Astrometry | |
Radial velocity (Rv) | 43.4 ± 2.1 [2] km/s |
Proper motion (μ) |
RA: 61.250 ± 3.490
[1]
mas/
yr Dec.: –53.130 ± 2.712 [1] mas/ yr |
Parallax (π) | 27.4408 ± 1.7735 mas [1] |
Distance | 119 ± 8
ly (36 ± 2 pc) |
Details [2] | |
Mass | 0.064+0.009 −0.027 M☉ |
Radius | 0.100+0.024 −0.008 R☉ |
Surface gravity (log g) | 5.2 ± 0.4 cgs |
Temperature | 1840 ± 210 K |
Rotation | 1.23±0.01 h |
Rotational velocity (v sin i) | 82.6 ± 0.2 km/s |
Age | 0.8+11.2 −0.65 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
2MASS J04070752+1546457 (abbreviated to 2MASS J0407+1546) is a rapidly-rotating brown dwarf of spectral class L3.5, located in the constellation Taurus about 119 light-years from Earth. With a photometrically measured rotation period of 1.23 hours, it is one of the fastest-rotating known brown dwarfs announced by a team of astronomers led by Megan E. Tannock in March 2021. With a rotational velocity of over 80 km/s (50 mi/s), it is approaching the predicted rotational speed limit beyond which it would break apart due to centripetal forces. As a consequence of its rapid rotation, the brown dwarf is slightly flattened at its poles to a similar degree as Saturn, the most oblate planet in the Solar System. [3] Its rapid rotation may enable strong auroral radio emissions via particle interactions in its magnetic field, as observed in other known rapidly-rotating brown dwarfs. [2]
2MASS J0407+1546 was first catalogued as a point source in June 2003 by the Two Micron All-Sky Survey (2MASS) organized by the University of Massachusetts Amherst and the Infrared Processing and Analysis Center under the California Institute of Technology. [4] It was discovered to be a brown dwarf of the spectral class L3.5 by I. Neill Reid and collaborators, based on near-infrared spectra obtained in October 2005 with the Gemini North at the Mauna Kea Observatory, Hawaii. Their discovery and spectroscopic characterization of 430 ultracool dwarfs including 2MASS J0407+1546 was published in The Astronomical Journal in September 2008. [5]
The trigonometric parallax of 2MASS 1114−2618 was measured to be 27.4408±1.7735 milliarcseconds by the Gaia spacecraft in 2018, corresponding to a distance of 36.4 ± 2.4 parsecs (118.7 ± 7.8 ly). [1] This is in close agreement with Reid et al.'s spectrophotometric estimate of 33.1 ± 3.3 parsecs (108 ± 11 ly) in 2008, calculated from the object's spectral type and near-infrared absolute magnitude. [5]
From Gaia DR2, 2MASS J0407+1546 has a measured net proper motion of 81.0 mas/ yr with position angle 139.06 degrees, [a] [b] indicating motion in south-east direction on the sky. [1]
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Taurus |
Right ascension | 04h 07m 07.527s [1] |
Declination | +15° 46′ 45.540″ [1] |
Characteristics | |
Spectral type | L3.5 [2] |
Apparent magnitude (G) | 20.704 ± 0.014 [1] |
Apparent magnitude (J) | 15.478 ± 0.058 [1] |
Apparent magnitude (H) | 14.354 ± 0.057 [1] |
Apparent magnitude (K) | 13.559 ± 0.038 [1] |
Astrometry | |
Radial velocity (Rv) | 43.4 ± 2.1 [2] km/s |
Proper motion (μ) |
RA: 61.250 ± 3.490
[1]
mas/
yr Dec.: –53.130 ± 2.712 [1] mas/ yr |
Parallax (π) | 27.4408 ± 1.7735 mas [1] |
Distance | 119 ± 8
ly (36 ± 2 pc) |
Details [2] | |
Mass | 0.064+0.009 −0.027 M☉ |
Radius | 0.100+0.024 −0.008 R☉ |
Surface gravity (log g) | 5.2 ± 0.4 cgs |
Temperature | 1840 ± 210 K |
Rotation | 1.23±0.01 h |
Rotational velocity (v sin i) | 82.6 ± 0.2 km/s |
Age | 0.8+11.2 −0.65 Gyr |
Other designations | |
Database references | |
SIMBAD | data |
2MASS J04070752+1546457 (abbreviated to 2MASS J0407+1546) is a rapidly-rotating brown dwarf of spectral class L3.5, located in the constellation Taurus about 119 light-years from Earth. With a photometrically measured rotation period of 1.23 hours, it is one of the fastest-rotating known brown dwarfs announced by a team of astronomers led by Megan E. Tannock in March 2021. With a rotational velocity of over 80 km/s (50 mi/s), it is approaching the predicted rotational speed limit beyond which it would break apart due to centripetal forces. As a consequence of its rapid rotation, the brown dwarf is slightly flattened at its poles to a similar degree as Saturn, the most oblate planet in the Solar System. [3] Its rapid rotation may enable strong auroral radio emissions via particle interactions in its magnetic field, as observed in other known rapidly-rotating brown dwarfs. [2]
2MASS J0407+1546 was first catalogued as a point source in June 2003 by the Two Micron All-Sky Survey (2MASS) organized by the University of Massachusetts Amherst and the Infrared Processing and Analysis Center under the California Institute of Technology. [4] It was discovered to be a brown dwarf of the spectral class L3.5 by I. Neill Reid and collaborators, based on near-infrared spectra obtained in October 2005 with the Gemini North at the Mauna Kea Observatory, Hawaii. Their discovery and spectroscopic characterization of 430 ultracool dwarfs including 2MASS J0407+1546 was published in The Astronomical Journal in September 2008. [5]
The trigonometric parallax of 2MASS 1114−2618 was measured to be 27.4408±1.7735 milliarcseconds by the Gaia spacecraft in 2018, corresponding to a distance of 36.4 ± 2.4 parsecs (118.7 ± 7.8 ly). [1] This is in close agreement with Reid et al.'s spectrophotometric estimate of 33.1 ± 3.3 parsecs (108 ± 11 ly) in 2008, calculated from the object's spectral type and near-infrared absolute magnitude. [5]
From Gaia DR2, 2MASS J0407+1546 has a measured net proper motion of 81.0 mas/ yr with position angle 139.06 degrees, [a] [b] indicating motion in south-east direction on the sky. [1]