2012ApJ...755..137C

Traditional pulsar polarization sweep analysis starts from the point dipole rotating vector model (RVM) approximation. If augmented by a measurement of the sweep phase shift, one obtains an estimate of the emission altitude (Blaskiewicz et al.). However, a more realistic treatment of field line sweepback and finite altitude effects shows that this estimate breaks down at modest altitude ∼0.1 R_LC. Such radio emission altitudes turn out to be relevant to the young energetic and millisecond pulsars that dominate the γ-ray population. We quantify the breakdown height as a function of viewing geometry and provide simple fitting formulae that allow observers to correct RVM-based height estimates, preserving reasonable accuracy to R ∼ 0.3 R_LC. We discuss briefly other observables that can check and improve height estimates.