  We present wide field CCD photometry of a galactic globular cluster M92
obtained in the V and I bands with the CFH12K mosaic CCD at the
Canada-France-Hawaii Telescope. A well-defined color-magnitude diagram is
derived down to 5 magnitudes fainter than the cluster main sequence turn-off.
After removing the background contribution, we obtain luminosity and mass
functions, surface density profiles, and the surface number density maps of the
stars belonging to the cluster. The surface density profile of all stars shows
that the cluster's halo extends at least out to ~30' from the cluster center in
agreement with previous study, but the profile of faint stars at the very outer
region of the cluster shows a different gradient compared with that of bright
stars. For a mass function of the cluster, we find that the inner region of the
cluster has x = 1.2+-0.2, whereas the outer region has x = 1.8 +-0.3, clearly
indicating a mass segregation of the cluster. An estimate of the photometric
mass of the cluster implies that the remnant populations (white dwarfs and
neutron stars) contribute at least 25% of the total cluster mass. The surface
density map of M92 shows some evidence that the tidal tail of M92 may be
oriented perpendicular to the direction toward the Galactic center.
