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The emergence of three-dimensional magneto-hydrodynamic (MHD) simulations ofstellar atmospheres has sparked a need for efficient radiative transfer codesto calculate detailed synthetic spectra. We present RH 1.5D, a massivelyparallel code based on the RH code and capable of performing Zeeman polarisedmulti-level non-local thermodynamical equilibrium (NLTE) calculations withpartial frequency redistribution for an arbitrary amount of chemical species.The code calculates spectra from 3D, 2D or 1D atmospheric models on acolumn-by-column basis (or 1.5D). While the 1.5D approximation breaks down inthe cores of very strong lines in an inhomogeneous environment, it isnevertheless suitable for a large range of scenarios and allows for fasterconvergence with finer control over the iteration of each simulation column.The code scales well to at least tens of thousands of CPU cores, and ispublicly available. In the present work we briefly describe its inner workings,strategies for convergence optimisation, its parallelism, and some possibleapplications.

RH 1.5D: a massively parallel code for multi-level radiative transfer with partial frequency redistribution and Zeeman polarisation