  We present high-resolution seeing limited and AO NIR imaging observations of
the stellar cluster within about one parsec of Sgr A*, the massive black hole
at the centre of the Milky Way. Stellar number counts and the diffuse
background light density were extracted from these observations in order to
examine the structure of the nuclear stellar cluster.Our findings are as
follows: (a) A broken-power law provides an excellent fit to the overall
structure of the GC nuclear cluster. The power-law slope of the cusp is
$\Gamma=0.19\pm0.05$, the break radius is $R_{\rm break} = 6.0'' \pm 1.0''$ or
$0.22\pm0.04$ pc, and the cluster density decreases with a power-law index of
$\Gamma=0.75\pm0.1$ outside of $R_{\rm break}$. (b) Using the best velocity
dispersion measurements from the literature, we derive higher mass estimates
for the central parsec than assumed until now. The inferred density of the
cluster at the break radius is $2.8\pm1.3\times 10^{6} {\rm M_{\odot}
pc^{-3}}$. This high density agrees well with the small extent and flat slope
of the cusp. Possibly, the mass of the stars makes up only about 50% of the
total cluster mass. (c) Possible indications of mass segregation in the cusp
are found (d) The cluster appears not entirely homogeneous. Several density
clumps are detected that are concentrated at projected distances of $R=3''$ and
$R=7''$ from Sgr A*.(e) There appears to exist an under-density of horizontal
branch/red clump stars near $R=5''$, or an over-density of stars of similar
brightness at $R=3''$ and $R=7''$. (f) The extinction map in combination with
cometary-like features in an L'-band image may provide support for the
assumption of an outflow from Sgr A*.
