  This paper investigates the off-equatorial plane deflections and
gravitational lensing of both null and timeline signals in Kerr spacetime in
the weak deflection limit, with the finite distance effect of the source and
detector taken into account. The deflection in both the Boyer-Linquidist
coordinates $\phi$ and $\theta$ directions are computed as power series of
$M/r_0$ and $r_0/r_{\mathrm{s,d}}$, where $M,\,r_{\mathrm{s,d}}$ are the
spacetime mass and source and detector radii respectively, and $r_0$ is the
minimal radius of the trajectory. The coefficients of these series are simple
trigonometric functions of $\theta_\mathrm{e}$, the extreme value of $\theta$
coordinate of the trajectory. A set of exact gravitational lensing equations is
used to solve $r_0$ and $\theta_\mathrm{e}$ for given deviation angles
$\delta\theta$ and $\delta\phi$ of the source, and two lensed images are always
obtained. The apparent angles and their magnifications of these images, and the
time delay between them are solved and their dependence on various parameters,
especially spacetime spin $\hat{a}$ are analyzed in great detail. It is found
that generally there exist two critical spacetime spin values that separate the
case of signals reaching the detector from different sides of the $z$ axis and
the cases in which the images appear from the same side in the celestial plane.
Three potential applications of these results are discussed.
