  We present a wide field CCD photometric study of Galactic globular cluster
NGC 7492. The derived VR color-magnitude diagram extends down to about 3.5 mag
below the cluster main sequence turn-off. The field covers 42' X 42' about 3
times larger than the known tidal radius of this cluster. The sample of cluster
member candidates obtained by CMD-mask process has been used to construct
luminosity and mass functions and surface density map. NGC 7492 has a very flat
mass function with very little variation in the slope with the distance from
the cluster center. However, there is a clear evidence for the increase of the
slope of the mass function from inner to outer regions, indicating a mass
segregation of the cluster. The surface density map of NGC 7492 shows
extensions toward the Galactic anticenter (northeast) and northwest from the
cluster center. A comparison of luminosity function for stars in the tails with
that for stars within the tidal radius suggests that the extensions shown in
the surface density map could be a real feature. The overall shape of NGC 7492
is significantly flattened. If the flattened shape of the NGC 7492 is caused by
its rotation, Galactic tidal field must have given important influences, since
the initial rotation would have been almost completely removed by dynamical
relaxation.
