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The known population of pulsars contains objects with four and five componentprofiles, for which the peak-to-peak separations between the inner and outercomponents can be measured. These Q and M type profiles can be interpreted as aresult of sightline cut through a nested cone beam, or through a set ofazimuthal fan beams. We show that the ratio R_W of the components' separationsprovides a useful measure of the beam shape, which is mostly independent ofparameters that determine the beam scale and complicate interpretation ofsimpler profiles. In particular, the method does not depend on the emissionaltitude and the dipole tilt distribution. The different structures of theradio beam imply manifestly different statistical distributions of R_W, withthe conal model being several orders of magnitude less consistent with datathan the fan beam model. To bring the conal model into consistency with data,strong effects of observational selection need to be called for, with 80% of Qand M profiles assumed to be undetected because of intrinsic blending effects.It is concluded that the statistical properties of Q and M profiles are moreconsistent with the fan-shaped beams, than with the traditional nested conegeometry.

The ratio of profile peak separations as a probe of pulsar radio-beam structure