  We present a high S/N spectrum for the quasar PG 1138+222. We detect a very
broad HeII$\lambda$4686 emission line component with twice the FWHM of the
conventional broad line region (BLR) as evidenced by the Balmer lines. The
profile shape and centroid redshift also distinguish this HeII component from
the BLR features. The large ratio of HeII\l 4686 to any analogous H$\beta$
emission component is an indicator that it arises in a very high density region
($n_e \simgt 10^{11}-10^{13}$ \cm3). This Helium component is probably emitted
in a Very Broad Line Region (VBLR), where the radiation field is so strong that
the Str\"omgren depth becomes similar to the geometrical thickness of the
emitting clouds. The gas could therefore be optically thin to the Lyman
continuum.
