Properties of low accretion rate magnetic white dwarfs in PCEBs. Stars show objects discovered/recovered with ZTF, dots show known systems from Parsons et al. (2021), Hakala et al. (2022) and Kawka et al. (2021) that we did not recover. The left panel shows the Gaia colour-magnitude diagram with the colours of the symbols by the orbital periods. The right panel shows the magnetic field strength versus the orbital period. For additional context, we also show polars (upward pointing triangles) and intermediate polars (downward pointing triangles) from Ferrario et al. (2015). The cataclysmic variable period gap is shown in grey and the CV period minimum as a dotted line (e.g. Knigge et al. 2011). The short period (≲2 h) systems are likely low-state polars or period bounce polars, while the longer period objects are likely pre-polars, detached polars, or low-state polars.