  We present results from a Mopra 7mm-wavelength survey that targeted the dense
gas-tracing CS(1-0) transition towards the young gamma-ray-bright supernova
remnant, RXJ1713.7-3946 (SNR G347.3-0.5). In a hadronic gamma-ray emission
scenario, where cosmic ray protons interact with gas to produce the observed
gamma-ray emission, the mass of potential cosmic ray target material is an
important factor. We summarise newly-discovered dense gas components, towards
Cores G and L, and Clumps N1, N2, N3 and T1, which have masses of 1-10^4 solar
masses. We argue that these components are not likely to contribute
significantly to gamma-ray emission in a hadronic gamma-ray emission scenario.
This would be the case if RXJ1713.7-3946 were at either the currently favoured
distance of ~1kpc or an alternate distance (as suggested in some previous
studies) of ~6kpc.
  This survey also targeted the shock-tracing SiO molecule. Although no SiO
emission corresponding to the RXJ1713.7-3946 shock was observed,
vibrationally-excited SiO(1-0) maser emission was discovered towards what may
be an evolved star. Observations taken one year apart confirmed a transient
nature, since the intensity, line-width and central velocity of
SiO(J=1-0,v=1,2) emission varied significantly.
