  We present the results of numerically solving the rate equations for the
first 31 rotational states of CS in the ground vibrational state to determine
the conditions under which the J=1-0, J=2-1 and J=3-2 transitions are inverted
to produce maser emission. The essence of our results is that the CS($v=0$)
masers are collisionally pumped and that, depending on the spectral energy
distribution, dust emission can suppress the masers. Apart from the J=1-0 and
J=2-1 masers the calculations also show that the J=3-2 transition can be
inverted to produce maser emission. It is found that beaming is necessary to
explain the observed brightness temperatures of the recently discovered CS
masers in W51 e2e. The model calculations suggest that a CS abundance of a few
times $10^{-5}$ and CS($v=0$) column densities of the order
$10^{16}\,\mathrm{cm^{-2}}$ are required for these masers. The rarity of the CS
masers in high mass star forming regions might be the result of a required high
CS abundance as well as due to attenuation of the maser emission inside as well
as outside of the hot core.
