  I present a method to deproject the observed intensity profile of an
axisymmetric bulge with arbitrary flattening to derive the 3D luminosity
density profile and to calculate the contribution of the bulge to the rotation
curve. I show the rotation curves for a family of fiducial bulges with Sersic
surface brightness profiles and with various concentrations and intrinsic axis
ratios. Both parameters have a profound impact on the shape of the rotation
curve. In particular, I show how the peak rotation velocity, as well as the
radius where it is reached, depend on both parameters.
  I also discuss the implications of the flattening of a bulge for the
decomposition of a rotation curve and use the case of NGC 5533 to show the
errors that result from neglecting it. For NGC 5533, neglecting the flattening
of the bulge leads to an overestimate of its mass-to-light ratio by
approximately 30% and an underestimate of the contributions from the stellar
disc and dark matter halo in the regions outside the bulge-dominated area.
