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Thanks to the huge amount of gamma-ray pulsar photons collected by the FermiLarge Area Telescope since June 2008, it is now possible to constrain gamma-raygeometrical models by comparing simulated and observed light-curvemorphological characteristics. We assumed vacuum-retarded dipole pulsarmagnetic field and tested simulated and observed morphological light-curvecharacteristics in the framework of two pole emission geometries, Polar Cap(PC), radio, and Slot Gap (SG), and Outer Gap (OG)/One Pole Caustic (OPC)emission geometries. We compared simulated and observed/estimated light-curvemorphological parameters as a function of observable and non-observable pulsarparameters. The PC model gives the poorest description of the LAT pulsarlight-curve morphology. The OPC best explains both the observed gamma-ray peakmultiplicity and shape classes. The OPC and SG models describe the observedgamma-ray peak-separation distribution for low- and high-peak separations,respectively. This suggests that the OPC geometry best explains the single-peakstructure but does not manage to describe the widely separated peaks predictedin the framework of the SG model as the emission from the two magnetichemispheres. The OPC radio-lag distribution shows higher agreement withobservations suggesting that assuming polar radio emission, the gamma-rayemission regions are likely to be located in the outer magnetosphere. Thelarger agreement between simulated and LAT estimations in the framework of theOPC suggests that the OPC model best predicts the observed variety of profileshapes. The larger agreement between observations and the OPC model jointlywith the need to explain the abundant 0.5 separated peaks with two-poleemission geometries, calls for thin OPC gaps to explain the single-peakgeometry but highlights the need of two-pole caustic emission geometry toexplain widely separated peaks.

Young and middle age pulsar light-curve morphology: Comparison of Fermi observations with gamma-ray and radio emission geometries