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In this work we present a procedure to infer the mass of progenitors andremnants of Gamma Ray Bursts (GRB), starting from the observed energy$E_{iso}^{GRB}$ emitted isotropically and considering the associated emissionof Gravitational Waves (GW) $ E_{iso}^{GW}$ in the different phases. We assumethat the GW energy of the progenitor $E_{PROG}^{GW}$ is emitted partiallyduring a star collapse, and the residual energy is related to the GW energyemitted by the remnant. We take a sample of $237$ Long GRB, and use an hybridMontecarlo procedure to explore, for each of them, a region of possiblesolutions of $ E_{iso}^{GW}$ as a function of the masses, radii, oblateness,rotation frequencies of progenitor and remnant and the fraction of energy $k$emitted as GW by the GRB. We discriminate between a Neutron Star (NS) or BlackHole (BH) for the remnant and obtain interesting values for the GW emitted bythe remnant NS or BH, for the conversion factor $k$ of and for the masses andradii of GRB progenitor stars. We also obtain remnant populations with meanmasses, mean GW frequencies and GRB frequency of GW emission in agreement withthe most accepted models.

Probing Long Gamma Ray Bursts progenitor mass by Gravitational Waves