  We present a numerical code that solves the forward and inverse problem of
the polarized radiative transfer equation in geometrical scale under the Zeeman
regime. The code is fully parallelized, making it able to easily handle large
observational and simulated datasets. We checked the reliability of the forward
and inverse modules through different examples. In particular, we show that
even when properly inferring various physical parameters (temperature, magnetic
field components, and line-of-sight velocity) in optical depth, their
reliability in height-scale depends on the accuracy with which the gas-pressure
or density are known. The code is made publicly available as a tool to solve
the radiative transfer equation and perform the inverse solution treating each
pixel independently. An important feature of this code, that will be exploited
in the future, is that working in geometrical-scale allows for the direct
calculation of spatial derivatives, which are usually required in order to
estimate the gas pressure and/or density via the momentum equation in a
three-dimensional volume, in particular the three-dimensional Lorenz force.

Solar and Stellar Astrophysics