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G 196-3 is a young low-mass M dwarf type star which is about 100 million years old. The star is located within the Ursa Major constellation about 71.1 light years away[1] from the Earth. During observations by Instituto de Astrofísica de Canarias in Tenerife, Spain in 1998, a substellar-mass object was discovered to orbit approximately 300 astronomical units (AU) from the star. It was detected using direct imaging.[2][3][4][5]
| Observation data Epoch J2000 Equinox J2000 | |
|---|---|
| Constellation | Ursa Major |
| Right ascension | 10h 04m 21.4629s[1] |
| Declination | 50° 23′ 13.3872″[1] |
| Apparent magnitude (V) | 13.3 |
| Characteristics | |
| Spectral type | M3V |
| U−B color index | +1.67 |
| B−V color index | +1.16 |
| Astrometry | |
| Radial velocity (Rv) | 11.7 km/s |
| Proper motion (μ) | RA: −141.177±0.055[1] mas/yr Dec.: −202.394±0.053[1] mas/yr |
| Parallax (π) | 45.8611 ± 0.0388 mas[1] |
| Distance | 71.12 ± 0.06 ly (21.80 ± 0.02 pc) |
| Absolute magnitude (MV) | 13.33 |
| Other designations | |
| Database references | |
| SIMBAD | data |
Observations of the substellar object were performed on January 25, 1998 where a faint red companion was present 16.2 arc seconds southwest of the star. A comparison of images taken at different wavelengths was done using low-intermediate-resolution spectroscopy confirmed the presence of a substellar object which was named G 196-3B. The Further observations confirmed the discovery when the team of Rafael Rebolo obtained R & I broadband photometry on March 19, 1998. The TCS Telescope showed its very cool nature in near-infrared (K Band). The comparison of the optical and infrared magnitudes including dust condensation has allowed astronomers to conclude that the substellar object was 25–10+15 Jupiter masses or simply 25 masses that of the Jovian-planet Jupiter. This was the second[6][7] discovery of a brown dwarf that was found around a low-mass star whose age[8] was relatively young. The separation of the star and the substellar object has suggested that both were parts of a fragment from a collapsing cloud although another possible scenario suggests that it originated from a dissipated protoplanetary disk.[9][2][10][11][12][13]
| Companion (in order from star) |
Mass | Semimajor axis (AU) |
Orbital period (days) |
Eccentricity | Inclination | Radius |
|---|---|---|---|---|---|---|
| B | 26±1 MJ | 350±1 | — | — | — | 1.36±0.23 RJ |
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