  The gas that is present in the interstellar medium is usually very far
removed from (local) thermodynamic equilibrium, and in some cases may also not
be in a steady-state equilibrium with its surroundings. The physics of this
material is complex and one needs a sophisticated numerical code to study it.
For this purpose the open-source photoionization code Cloudy was created. It
models the physical state of the gas and predicts the spectrum that it emits.
  Cloudy is continually being developed to improve the treatment of the
microphysical processes and the database of fundamental data that it uses. In
this paper we will discuss how we are developing the code to improve our
high-density predictions by implementing better collisional-radiative models
for all ions. We will also briefly discuss the experimental mode in Cloudy to
model gas that is not in steady-state equilibrium and present a preliminary
model of recombining gas in a planetary nebula that is on the cooling track. We
finish with a short discussion of how we are speeding up the code by using
parallelization.
