Recently, the exploitation of spectropolarimetric data has allowed to improve our knowledge of the dynamical and magnetic response of the photospheric and chromospheric layers to the rapid release of energy occurring during solar flares. In this framework, we have used high-resolution observations acquired on 22nd October 2014 during an X1.6 confined flare by the Interferometric Bidimensional Spectropolarimeter (IBIS) instrument, observing the full Stokes parameters for the Fe I 6173 Å and Ca II 8542 Å transitions. We employed the newly developed Departure Coefficient Aided Stokes Inversion based on Response Functions (DeSIRe) code to infer the spatial distribution and the vertical stratification of the atmospheric parameters at photospheric and chromospheric layers. Our results indicate significant temperature increases and pronounced upflows within the chromospheric flare ribbon, suggesting that the flaring event is producing hot material that is moving upwards. Conversely, the photosphere shows no discernible temperature rise or strong velocities, implying that the impact of the flaring event mainly occurs at the middle and upper layers. The information about the magnetic field vector reveals relatively smooth stratifications with height for both magnetic field strength and inclination. We also find that the spatial locations belonging to the flare ribbon present a significant depression in the height of formation (or sensitivity) for the chromospheric line, whereas we find no clear indication that the same occurs for the Fe I transition. These results confirm that, in the low atmospheric layers, the main impact of the flaring activity takes place at chromospheric levels.