We introduce a method to obtain self-consistent, axially symmet- ric disklike stellar models in the first post-Newtonian (1PN) approximation. By using in the field equations of the 1PN approximation a distribution function (DF) corresponding to a Newtonian model, two fundamental equa- tions determining the 1PN corrections are obtained. The rotation curves of the corrected models differs from the classical ones and the corrections are clearly appreciable with values of the mass and radius of a typical galaxy. On the other hand, the relativistic mass correction can be ignored for all models.