  Recent observations of the Arches cluster located within a projected distance
of 30 pc from the dynamical center of the Galaxy have shown the presence of
diffuse and discrete X-ray continuum emission, diffuse 6.4keV line emission as
well as thermal and nonthermal radio continuum emission. This young and dense
stellar cluster is also recognized to be within the 95% error circle of an
identified steady source of $\gamma$-ray emission associated with the EGRET
source 3EG J1746--2851. Much of the thermal and nonthermal emission can be
explained by shocked gas resulting from colliding winds originating from
massive binaries within the cluster. In particular, we argue that nonthermal
particles could upscatter the radiation field of the cluster by ICS and account
for the $\gamma$-ray emission. We also consider that the fluorescent 6.4 keV
line emission may be the result of the impact of low-energy relativistic
particles on neutral gas distributed in the vicinity of the cluster. Lastly, we
sketch an interpretation in which young stellar clusters and massive young
binary systems are responsible for the origin of nonthermal radio filaments
found throughout the inner 300pc of the Galaxy. The collimation of the
nonthermal filaments may be done in the colliding wind region by the ionized
surface of individual mass-losing stars of massive binary systems. In this
picture, a WR-type phenomenon is expected to power a central star burst in the
Galactic center in order to account for all the observed filaments.
