Radiative cooling rates, ion fractions, molecule abundances and line
  emissivities including self-shielding and both local and metagalactic
  radiation fields
  We use the spectral synthesis code Cloudy to tabulate the properties of gas
for an extensive range in redshift (z=0 to 9), temperature (log T [K] = 1 to
9.5), metallicity (log Z/$\mathrm{Z}_{\odot}$ = -4 to +0.5, Z=0), and density
(log $n_{\mathrm{H}}$ [$\mathrm{cm}^{-3}$] = -8 to +6). This therefore includes
gas with properties characteristic of the interstellar, circumgalactic and
intergalactic media. The gas is exposed to a redshift-dependent UV/X-ray
background, while for the self-shielded lower-temperature gas (i.e. ISM gas) an
interstellar radiation field and cosmic rays are added. The radiation field is
attenuated by a density- and temperature-dependent column of gas and dust.
Motivated by the observed star formation law, this gas column density also
determines the intensity of the interstellar radiation field and the cosmic ray
density. The ionization balance, molecule fractions, cooling rates, line
emissivities, and equilibrium temperatures are calculated self-consistently. We
include dust, cosmic rays, and the interstellar radiation field step-by-step to
study their relative impact. These publicly available tables are ideal for
hydrodynamical simulations. They can be used stand alone or coupled to a
non-equilibrium network for a subset of elements. The release includes a C
routine to read in and interpolate the tables, as well as an easy to use python
graphical user interface to explore the tables.
