HD 4113
HD 4113 is a double star system in the southern constellation of Sculptor. It is too faint to be viewed with the naked eye, having an apparent visual magnitude of 7.88. The distance to this star, as estimated by parallax measurements, is 137 light years. It is receding away from the Sun with a radial velocity of +5 km/s.
System components
The primary member of this system, component A, is a Sun-like G-type main-sequence star with a stellar classification of G5V. Estimates of its age are five to seven billion years old, and it is spinning with a leisurely projected rotational velocity of 2.3 km/s. The star is metal rich, with nearly the same mass, radius, and luminosity as the Sun.Orbiting this star is a giant planet and a brown dwarf ; the latter has been directly imaged. It also has a co-moving stellar companion, designated component B, which is a red dwarf with a class of M0–1V at an angular separation of. This angle is equivalent to a projected separation of.
The most recent parameters for HD 4113 C as of 2022 come from a combination of data from radial velocity, astrometry, and imaging, showing that it is about 52 times the mass of Jupiter, and on an eccentric orbit with a semi-major axis of about 50.4 AU and an orbital period of about 348 years.
Observations with SPHERE found a lack of a detection of HD 4113 C in H3, likely due to methane absorption in the H-band. Using the extracted spectrum the team estimated a spectral type of T9. Observation with GRAVITY+ showed strong methane absorption in the K-band spectrum of HD 4113 C. The inconsistency between temperature and isochronal mass estimate is seen as potential evidence for a binary brown dwarf.