  We investigate the unusually rich cluster system of NGC4636 with wide-field
Washington photometry. The globular cluster luminosity function can be followed
roughly 1 mag beyond the turn-over magnitude. This corresponds to a distance
modulus of m-M=31.24+-0.17, 0.4 mag larger than the distance determined from
surface brightness fluctuations. The high specific frequency is confirmed, yet
the exact value remains uncertain because of the uncertain distance: it varies
between 5.6+-1.2 and 8.9+-1.2. The globular cluster system has a clearly
bimodal color distribution. The color peak positions show no radial dependence
and are in good agreement with the values found for other galaxies studied in
the same filter system. However, a luminosity dependence is found: brighter
clusters with an ``intermediate'' color exist. The clusters exhibit a shallow
radial distribution within 7'.Within the same radial interval, the galaxy light
has a distinctly steeper profile. Because of the difference in the cluster and
light distribution the specific frequency increases considerably with radius.
At 7' and 9' the density profiles of the red and blue clusters, respectively,
change strongly which indicates that we reach the outer rim of the cluster
system at approximately 11'. This feature is seen for the first time in a
globular cluster system. While the radial distribution of the cluster and field
populations are rather different, this is not true for the ellipticity of the
system: the elongation as well as the position angle of the cluster system
agree well with the galaxy light. We compare the radial distribution of
globular clusters with the light profiles for a sample of elliptical galaxies.
The difference observed in NGC 4636 is typical of an elliptical galaxy of this
luminosity.
