  In this work we present a procedure to infer the mass of progenitors and
remnants of Gamma Ray Bursts (GRB), starting from the observed energy
$E_{iso}^{GRB}$ emitted isotropically and considering the associated emission
of Gravitational Waves (GW) $ E_{iso}^{GW}$ in the different phases. We assume
that the GW energy of the progenitor $E_{PROG}^{GW}$ is emitted partially
during a star collapse, and the residual energy is related to the GW energy
emitted by the remnant. We take a sample of $237$ Long GRB, and use an hybrid
Montecarlo procedure to explore, for each of them, a region of possible
solutions 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 Black
Hole (BH) for the remnant and obtain interesting values for the GW emitted by
the remnant NS or BH, for the conversion factor $k$ of and for the masses and
radii of GRB progenitor stars. We also obtain remnant populations with mean
masses, mean GW frequencies and GRB frequency of GW emission in agreement with
the most accepted models.
