It is located at a distance of 150 light years from the Sun based on parallax, and is drifting further away with a radial velocity of +14.7 km/s.
[5] The primary component is a G-type main-sequence star with a stellar classification of G6V,[3] indicating it is generating energy through core hydrogen fusion.
In 2000, analysis of radial velocity measurements of the star revealed the existence of a brown dwarf companion[8] with at least 17 times the mass of Jupiter around the star in an eccentric orbit with a period of around 256 days.
[7] Even after the brown dwarf was accounted for, the star still showed a drift in the radial velocity measurements, suggesting another companion in a longer-period orbit.
[9] Further observation of this system revised this picture in 2017, showing that the system instead consisted of a pair of co-orbiting stars being viewed nearly face-on, with the pair being orbited in turn by a Super-Jupiter designated HD 202206 c. The secondary stellar companion, now designated component B rather than 'b', is a red dwarf star with 8.9% of the mass of the Sun.