  We report the Australia Telescope Compact Array 16 cm observation of CIZA
J1358.9-4750. Recent X-ray studies imply that this galaxy cluster is composed
of merging, binary clusters. Using the EW367 configuration, we found no
significant diffuse radio emission in and around the cluster. An upper limit of
the total radio power at 1.4 GHz is $\sim 1.1 \times 10^{22}$ Watt/Hz in $30$
square arcminutes which is a typical size of radio relics. It is known that an
empirical relation holds between the total radio power and X-ray luminosity of
the host cluster. The upper limit is about one order of magnitude lower than
the power expected from the relation. Very young ($\sim 70$ Myr) shocks with
low Mach numbers ($\sim 1.3$), which are often seen at an early stage of merger
simulations, are suggested by the previous X-ray observation. The shocks may
generate cosmic-ray electrons with a steep energy spectrum, which is consistent
with non-detection of bright ($>10^{23}$ Watt/Hz) relic in this 16 cm band
observation. Based on the assumption of energy equipartition, the upper limit
gives the magnetic-field strength below $0.68f(D_{\rm los}/{\rm
1~Mpc})^{-1}(\gamma_{\rm min}/200)^{-1}$ $\mu$G, where $f$ is the cosmic-ray
total energy density over the cosmic-ray electron energy density, $D_{\rm los}$
is the depth of the shock wave along the sightline and $\gamma_{\rm min}$ is
the lower cutoff Lorentz factor of the cosmic-ray electron energy spectrum.
