The distribution in the difference between spectropolarimetrically predicted disk PA and observed disk PA for the sample presented in Table 3 (blue dashed). This is compared to a random distribution (black short dotted). On the left we show a distribution where polarisation signatures are always orientated perpendicularly to circumstellar disks and on the right we present the distribution for a scenario where the spectropolarimetric signatures can be either perpendicular or parallel to disks (see the text for more detail). Both model distributions have a maximum error of 15°. In both cases, a random orientation of disk and polarisation position angles can be discarded at the 3σ level.