Light-curve modelling constraints on the obliquities and aspect angles of the young Fermi pulsars
In more than four years of observation the Large Area Telescope on board the Fermi satellite has identified pulsed $γ$-ray emission from more than 80 young pulsars, providing light curves with high statistics. Fitting the observations with geometrical models can provide estimates of the magnetic obliquity $α$ and aspect angle $ζ$, yielding estimates of the radiation beaming factor and luminosity. Using $γ$-ray emission geometries (Polar Cap, Slot Gap, Outer Gap, One Pole Caustic) and radio emission geometry, we fit $γ$-ray light curves for 76 young pulsars and we jointly fit their $γ$-ray plus radio light curves when possible. We find that a joint radio plus $γ$-ray fit strategy is important to obtain ($α$, $ζ$) estimates that can explain simultaneous radio and $γ$-ray emission. The intermediate-to-high altitude magnetosphere models, Slot Gap, Outer Gap, and One pole Caustic, are favoured in explaining the observations. We find no evolution of $α$ on a time scale of a million years. For all emission geometries our derived $γ$-ray beaming factors are generally less than one and do not significantly evolve with the spin-down power. A more pronounced beaming factor vs. spin-down power correlation is observed for Slot Gap model and radio-quiet pulsars and for the Outer Gap model and radio-loud pulsars. For all models, the correlation between $γ$-ray luminosity and spin-down power is consistent with a square root dependence. The $γ$-ray luminosities obtained by using our beaming factors not exceed the spin-down power. This suggests that assuming a beaming factor of one for all objects, as done in other studies, likely overestimates the real values. The data show a relation between the pulsar spectral characteristics and the width of the accelerator gap that is consistent with the theoretical prediction for the Slot Gap model.