  Broad emission features of abundant chemical elements, such as Iron, are
commonly seen in the X-ray spectra of accreting compact objects and their
studies can provide useful information about the geometry of the accretion
processes. In this work, we focus our attention on GX 3+1, a bright, persistent
accreting low mass X-ray binary, classified as an atoll source. Its spectrum is
well described by an accretion disc plus a stable comptonizing, optically thick
corona which dominates the X-ray emission in the 0.3-20 keV energy band. In
addition, four broad emission lines are found and we associate them with
reflection of hard photons from the inner regions of the accretion disc where
doppler and relativistic effects are important. We used self-consistent
reflection models to fit the spectra of the 2010 XMM-Newton observation and the
stacking of the whole datasets of 2010 INTEGRAL observations. We conclude that
the spectra are consistent with reflection produced at ~10 gravitational radii
by an accretion disc with an ionization parameter of xi~600 erg cm/s and viewed
under an inclination angle of the system of ~35{\deg}. Furthermore, we detected
for the first time for GX 3+1, the presence of a powerlaw component dominant at
energies higher than 20 keV, possibly associated with an optically thin
component of non-thermal electrons.
