We compare population synthesis results for inner and outer magnetosphereemission models with the various characteristics measured in the first LATpulsar catalogue for both the radio-loud and radio-weak or radio-quietgamma-ray pulsars. We show that all models fail to reproduce the observations:for each model there is a lack of luminous and energetic objects that suggest anon dipolar magnetic field structure or spin-down evolution. The largedispersion that we find in the simulated gamma-ray luminosity versus spin-downpower relation does not allow to use the present trend seen in the Fermi datato distinguish among models. For each model and each Fermi detected pulsar, wehave generated light curves as a function of obliquity and inclination angles.The theoretical curves were fitted to the observed one, using amaximum-likelihood approach, to derive the best-fit orientations and to comparehow well each model can reproduce the data. Including the radio light-curvegives an additional key constraint to restrict the orientation space
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