  We characterize the radii and masses of the star and planets in the Kepler-59
system, as well as their orbital parameters. The star parameters are determined
through a standard spectroscopic analysis, resulting in a mass of $1.359\pm
0.155\,M_\odot$ and a radius of $1.367\pm 0.078\,R_\odot$. The planetary radii
obtained are $1.5\pm 0.1\,R_\oplus$ for the inner and $2.2\pm 0.1\,R_\oplus$
for the outer planet. The orbital parameters and the planetary masses are
determined by the inversion of Transit Timing Variations (TTV) signals. For
this, we consider two different data sets, one provided by Holczer et al. 2016,
with TTVs only for the planet Kepler-59c, and the other provided by Rowe et al.
2015, with TTVs signals for both planets. The inversion method is carried out
by applying an algorithm of Bayesian inference (MultiNest) combined with an
efficient N-body integrator (Swift). For each of the data sets, two possible
solutions are found, both having the same probability according to their
corresponding Bayesian evidences. All four solutions appear to be
indistinguishable within their 2-$\sigma$ uncertainties. Nevertheless,
statistical analyses show that the solutions from Rowe et al. 2015 data better
characterize the data. The first and second solutions identify masses of
$5_{-2}^{+4}~M_{\mathrm{\oplus}}$ and $4.6_{-2.0}^{+3.6}~M_{\mathrm{\oplus}}$,
and $3.0^{+0.8}_{-0.8}~M_{\mathrm{\oplus}}$ and
$2.6^{+1.9}_{-0.8}~M_{\mathrm{\oplus}}$ for the inner and outer planet,
respectively. This points to a system with an inner super-Earth and an outer
mini-Neptune. Dynamical studies show the planets have almost co-planar orbits
with small eccentricities ($e<0.1$), close but not into the 3:2 mean motion
resonance. Stability analysis indicates that this configuration is stable over
million years of evolution.
