  We consider a Kerr black hole acting as a gravitational deflector within the
geometrical optics, and point source approximations. The Kerr black hole
gravitational lens geometry consisting of an observer and a source located far
away and placed at arbitrary inclinations with respect to the black hole's
equatorial plane is studied in the strong field regime. For this geometry the
null geodesics equations of our interest can go around the black hole several
times before reaching the observer. Such photon trajectories are written in
terms of the angular positions in the observer's sky and therefore become "lens
equations". As a consequence, we found for any image a simple classification
scheme based in two integers numbers: the number of turning points in the polar
coordinate $\theta$, and the number of windings around the black hole's
rotation axis. As an application, and to make contact with the literature, we
consider a supermassive Kerr black hole at the Galactic center as a
gravitational deflector. In this case, we show that our proposed computational
scheme works successfully by computing the positions and magnifications of the
relativistic images for different source-observer geometries. In fact, it is
shown that our general procedure and results for the positions and
magnifications of the images off the black hole's equatorial plane, reduce and
agree with well known cases found in the literature.
