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A large fraction of Gamma Ray Bursts (GRBs) displays an X-ray plateau phasewithin <10^{5} s from the prompt emission, proposed to be powered by thespin-down energy of a rapidly spinning newly born magnetar. In this work we usethe properties of the Galactic neutron star population to constrain theGRB-magnetar scenario. We re-analyze the X-ray plateaus of all Swift GRBs withknown redshift, between January 2005 and August 2014. From the derived initialmagnetic field distribution for the possible magnetars left behind by the GRBs,we study the evolution and properties of a simulated GRB-magnetar populationusing numerical simulations of magnetic field evolution, coupled with MonteCarlo simulations of Pulsar Population Synthesis in our Galaxy. We find that ifthe GRB X-ray plateaus are powered by the rotational energy of a newly formedmagnetar, the current observational properties of the Galactic magnetarpopulation are not compatible with being formed within the GRB scenario(regardless of the GRB type or rate at z=0). Direct consequences would be thatwe should allow the existence of magnetars and "super-magnetars" havingdifferent progenitors, and that Type Ib/c SNe related to Long GRBs formsystematically neutron stars with higher initial magnetic fields. We put anupper limit of <16 "super-magnetars" formed by a GRB in our Galaxy in the pastMyr (at 99% c.l.). This limit is somewhat smaller than what roughly expectedfrom Long GRB rates, although the very large uncertainties do not allow us todraw strong conclusion in this respect.

Constraining the GRB-magnetar model by means of the Galactic pulsar population