  Despite considerations of mass loss from stellar evolution suggesting
otherwise, the content of gas in globular clusters seems poor and hence its
measurement very elusive. One way of constraining the presence of ionized gas
in a globular cluster is through its dispersive effects on the radiation of the
millisecond pulsars included in the cluster. This effect led Freire et al. in
2001 to the first detection of any kind of gas in a globular cluster in the
case of 47 Tucanae. By exploiting the results of 12 additional years of timing,
as well as the observation of new millisecond pulsars in 47 Tucanae, we
revisited this measurement: we first used the entire set of available timing
parameters in order to measure the dynamical properties of the cluster and the
three-dimensional position of the pulsars. Then we applied and tested various
gas distribution models: assuming a constant gas density, we confirmed the
detection of ionized gas with a number density of $n= 0.23\pm 0.05$ cm$^{-3}$,
larger than the previous determination (at 2$\sigma$ uncertainty). Models
predicting a decreasing density or following the stellar distribution density
are highly disfavoured. We are also able to investigate the presence of an
intermediate mass black hole in the centre of the cluster, showing that is not
required by the available data, with an upper limit for the mass at $\sim 4000$
M$_{\odot}$.
