![]() DENIS-P J020529.0−115925 system with Hubble, the primary A is on the upper left Credit: Hubble Space Telescope | |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Cetus |
Right ascension | 02h 05m 29.401s [1] |
Declination | −11° 59′ 29.67″ [1] |
Characteristics | |
Spectral type | L5.5 + L8 + T0 [2] |
Apparent magnitude (J) | 14.587 [1] |
Astrometry | |
Proper motion (μ) |
RA: 427
[3]
mas/
yr Dec.: 52 [3] mas/ yr |
Parallax (π) | 50.60 ± 1.50 mas [4] |
Distance | 64 ± 2
ly (19.8 ± 0.6 pc) |
Other designations | |
Database references | |
SIMBAD | data |
DENIS-P J020529.0−115925 is a brown dwarf system in the constellation of Cetus. It is located 64 light-years (19.8 parsecs) away, based on the system's parallax. [4] It was first found in the Deep Near Infrared Survey of the Southern Sky.
This is a triple brown dwarf system: objects that do not have enough mass to fuse hydrogen like stars. The two brightest components, designated A and B respectively, are both L-type objects. As of 2003, the two were separated 0.287° along a position angle of 246°. [2]
Component B was observed as elongated, suggesting a third component. This third component, named C, is a T-type object. [2] It is separated about 1.9 astronomical units (au) from B, and based on a total mass of 0.1 M☉, the two may orbit each other every 8 years. [2]
![]() DENIS-P J020529.0−115925 system with Hubble, the primary A is on the upper left Credit: Hubble Space Telescope | |
Observation data Epoch J2000 Equinox J2000 | |
---|---|
Constellation | Cetus |
Right ascension | 02h 05m 29.401s [1] |
Declination | −11° 59′ 29.67″ [1] |
Characteristics | |
Spectral type | L5.5 + L8 + T0 [2] |
Apparent magnitude (J) | 14.587 [1] |
Astrometry | |
Proper motion (μ) |
RA: 427
[3]
mas/
yr Dec.: 52 [3] mas/ yr |
Parallax (π) | 50.60 ± 1.50 mas [4] |
Distance | 64 ± 2
ly (19.8 ± 0.6 pc) |
Other designations | |
Database references | |
SIMBAD | data |
DENIS-P J020529.0−115925 is a brown dwarf system in the constellation of Cetus. It is located 64 light-years (19.8 parsecs) away, based on the system's parallax. [4] It was first found in the Deep Near Infrared Survey of the Southern Sky.
This is a triple brown dwarf system: objects that do not have enough mass to fuse hydrogen like stars. The two brightest components, designated A and B respectively, are both L-type objects. As of 2003, the two were separated 0.287° along a position angle of 246°. [2]
Component B was observed as elongated, suggesting a third component. This third component, named C, is a T-type object. [2] It is separated about 1.9 astronomical units (au) from B, and based on a total mass of 0.1 M☉, the two may orbit each other every 8 years. [2]