Characterization Of The Very High Energy Emission From Pulsars With The Magic Telescopes

For several decades, since their discovery in 1967 by Jocelyn Bell Burnell, pulsars have been under intense investigation. Due to their huge magnetic and gravitational elds, pulsars are one of the best laboratories to study matter in extreme conditions. Recently, the detection of emission from the Crab pulsar at Very High Energies (VHE, > 100 GeV) was a breakthrough, as such emission was totally unexpected. Even though pulsars are being deeply studied, their emission location and mechanisms are still poorly understood. Several regions where the VHE gamma rays are expected to be emitted where proposed, each of them exhibiting di erent features in the pulsars emission, such as energy spectrum and light curve properties. The observation of pulsars at VHE is then fundamental in order to understand their emission properties and distinguish between the current models. This thesis deals with the characterization of the VHE emission from pulsars. This study relies on the observations of pulsars with the MAGIC telescopes and the analytic calculation of the pulsar X-ray and gamma-ray emission e ciencies in the framework of the outer-gap model. Two pulsars were selected for the observations with the MAGIC telescopes, namely, the Crab and Geminga pulsars. These pulsars are the two brightest gamma-ray pulsars observable from the Northern Hemisphere. The study of the Crab pulsar revealed the signi cant emission from the interpulse region, also called bridge, located between the two main peaks. This component, already observed at low energies and predicted at VHE, was not previously detected at VHE. Furthermore, the relative emission between the two main peaks and the bridge was computed, including the analysis of 6.5 years of Fermi-LAT data. The behaviors of P2/P1 and bridge/P1 revealed a similar trend, unveiling similar properties in the emission of these distinct components...