[12] In 2003 and 2004, an object (now catalogued as AB Pictoris b) was observed close to the star by a team of astronomers at the European Southern Observatory.

Since it had common proper motion with AB Pictoris, it was concluded that it was physically close to the star.

This confirmed this object as an L-dwarf with low surface gravity, matching a spectral type of L0-L1.

The planetary orbit is significantly misaligned with its spin axis orientation (obliquity), possibly due to gravitational interactions with the additional inner planet.

[18] This result was later corroborated with a re-analysis of the Gaia excess noise and the proper motion anomaly.