  We have simulated a population of young spin-powered pulsars and computed the
beaming pattern and lightcurves for the three main geometrical models: polar
cap emission, two-pole caustic ("slot gap") emission and outer magnetosphere
emission. The light curve shapes depend sensitively on the magnetic inclination
alpha and viewing angle zeta. We present the results as maps of observables
such as peak multiplicity and gamma-ray peak separation in the (alpha, zeta)
plane. These diagrams can be used to locate allowed regions for radio-loud and
radio-quiet pulsars and to convert observed fluxes to true all-sky emission.
