  Full disk vector magnetic fields are used widely for developing better
understanding of large-scale structure, morphology, and patterns of the solar
magnetic field. The data are also important for modeling various solar
phenomena. However, observations of vector magnetic fields have one important
limitation that may affect the determination of the true magnetic field
orientation. This limitation stems from our ability to interpret the differing
character of the Zeeman polarization signals which arise from the photospheric
line-of-sight vs. the transverse components of the solar vector magnetic field,
and is likely exacerbated by unresolved structure (non-unity fill fraction) as
well as the disambiguation of the 180$^\circ$ degeneracy in the
transverse-field azimuth. Here we provide a description of this phenomenon, and
discuss issues, which require additional investigation.
