  We perform simulations for future Cherenkov Telescope Array (CTA)
observations of RX~J1713.7$-$3946, a young supernova remnant (SNR) and one of
the brightest sources ever discovered in very-high-energy (VHE) gamma rays.
Special attention is paid to explore possible spatial (anti-)correlations of
gamma rays with emission at other wavelengths, in particular X-rays and
CO/H{\sc i} emission. We present a series of simulated images of RX
J1713.7$-$3946 for CTA based on a set of observationally motivated models for
the gamma-ray emission. In these models, VHE gamma rays produced by high-energy
electrons are assumed to trace the non-thermal X-ray emission observed by {\it
XMM-Newton}, whereas those originating from relativistic protons delineate the
local gas distributions. The local atomic and molecular gas distributions are
deduced by the NANTEN team from CO and H{\sc i} observations. Our primary goal
is to show how one can distinguish the emission mechanism(s) of the gamma rays
(i.e., hadronic vs leptonic, or a mixture of the two) through information
provided by their spatial distribution, spectra, and time variation. This work
is the first attempt to quantitatively evaluate the capabilities of CTA to
achieve various proposed scientific goals by observing this important cosmic
particle accelerator.
