  Coronal Mass Ejections (CMEs) are highly dynamic events originating in the
solar atmosphere, that show a wide range of kinematic properties and are the
major drivers of the space weather. The angular width of the CMEs is a crucial
parameter in the study of their kinematics. The fact that whether slow and fast
CMEs (as based on their relative speed to the average solar wind speed) are
associated with different processes at the location of their ejection is still
debatable. Thus, in this study, we investigate their angular width to
understand the differences between the slow and fast CMEs. We study the width
distribution of slow and fast CMEs and find that they follow different power
law distributions, with a power law indices ($\alpha$) of -1.1 and -3.7 for
fast and slow CMEs respectively. To reduce the projection effects, we further
restrict our analysis to only limb events as derived from manual catalog and we
find similar results. We then associate the slow and fast CMEs to their source
regions, and classified the sources as Active Regions (ARs) and Prominence
Eruptions (PEs). We find that slow and fast CMEs coming from ARs and PEs, also
follow different power laws in their width distributions. This clearly hints
towards a possibility that different mechanisms might be involved in the width
expansion of slow and fast CMEs coming from different sources.These results are
also crucial from the space weather perspective since the width of the CME is
an important factor in that aspect.
