To invert vector magnetic fields from an emitting coronal plasma pixel at an apparent height h above the photosphere, we require two inputs: Stokes IQU observations (see A. R. Paraschiv & P. G. Judge 2022) and Alfvénic-waves-derived B_POS (as demonstrated by Z. Yang et al. 2020a, 2024). The inputs are then ingested by the IQUD CLEDB inversion (described and validated by A. R. Paraschiv 2026) to infer vector magnetic field components. Our Earth-observing geometric system is defined along y- (horizontal) and z- (vertical) directions in the POS, while x goes along the LOS.