The [CII]--SFR correlation in dwarf galaxies across cosmic time
  Current galaxy observations suggest that a roughly linear correlation exists
between the [CII] emission and the star formation rate, either as
spatially-resolved or integrated quantities. Observationally, this correlation
seems to be independent of metallicity, but the very large scatter does not
allow to properly assess whether this is true. On the other hand, theoretical
models tend to suggest a metallicity dependence of the correlation. In this
study, we investigate the metallicity evolution of the correlation via a
high-resolution zoom-in cosmological simulation of a dwarf galaxy employing
state-of-the-art sub-grid modelling for gas cooling, star formation, and
stellar feedback, and that self-consistently evolves the abundances of metal
elements out of equilibrium. Our results suggest that the correlation should
evolve with metallicity, in agreement with theoretical predictions, but also
that this evolution can be hardly detected in observations, because of the
large scatter. We also find that most of the [CII] emission is associated with
neutral gas at low-intermediate densities, whereas the highest emissivity is
produced by the densest regions around star-forming regions.
