1988 claims

The first indications of γ Cephei Ab were reported in July 1988. The planet was tentatively identified by a Canadian team of astronomers, which was led by Bruce Campbell, Gordon Walker and Stephenson Yang,^[8] while its existence was also announced by Anthony Lawton and P. Wright in 1989. Though not confirmed, this would have been the first true discovery of an extrasolar planet, and it was hypothesized based on the same radial velocity technique later used successfully by others. However, the claim was retracted in 1992 due to the quality of the data not being good enough to make a solid discovery.^[9]

2003 confirmation

On 7 May 2003, γ Cephei Ab was finally confirmed. The team of astronomers (including William D. Cochran, Artie P. Hatzes, et al.) at the Planetary Systems and their Formation Workshop announced the preliminary confirmation of a long-suspected planet γ Cephei Ab with a minimum mass of 1.59 M_J (1.59 times that of Jupiter).^[10] The parameters were later recalculated when direct detection of the secondary star γ Cephei B allowed astronomers to better constrain the properties of the system.^[11] γ Cephei Ab moves in an elliptical orbit with a semimajor axis of 2.044 AU which takes almost two-and-a-half years to complete. The eccentricity is 0.115, which means it moves between 1.81 and 2.28 AU in orbital distance around γ Cephei A, which would place it from slightly beyond the orbit of Mars, to the inner asteroid belt in the Solar System.

Astrometric observations

Hipparcos data taken in 2006 constrains its mass below "13.3 M_J at the 95% confidence level, and 16.9 M_J at the 99.73% (3 σ) confidence level". This is not much to go on, but it is enough to verify that it is not another unseen brown or red dwarf.^[12]

In 2018, Hubble astrometric observations revealed the true mass of γ Cephei Ab to be 9.4 M_J.^[3]