  Positron annihilation radiation from the Galaxy has been observed by the
OSSE, SMM and TGRS instruments. Improved spectral modeling of OSSE observations
has allowed studies of the distribution of both positron annihilation radiation
components, the narrow line emission at 511 keV and the positronium continuum
emission. The results derived for each individual annihilation component are
then compared with each other. These comparisons reveal approximate agreement
between the distribution of these two emissions. In certain regions of the sky
(notably in the vicinity of the previously reported positive latitude
enhancement), the distribution of the emissions differ. We discuss these
differences and the methods currently being employed to understand whether the
differences are physical or a systematic error in the present analysis.
