DustPedia - the relationships between stars, gas and dust for galaxies
  residing in different environments
  We use a sub-set of the DustPedia galaxy sample (461 galaxies) to investigate
the effect the environment has had on galaxies. We consider Virgo cluster and
field samples and also assign a density contrast parameter to each galaxy, as
defined by the local density of SDSS galaxies. We consider their chemical
evolution (using M_{Dust}/M_{Baryon} and M_{Gas}/M_{Baryon}), their specific
star formation rate (SFR/M_{Stars}), star formation efficiency (SFR/M_{Gas}),
stars-to-dust mass ratio (M_{Stars}/M_{Dust}), gas-to-dust mass ratio
(M_{Gas}/M_{Dust}) and the relationship between star formation rate per unit
mass of dust and dust temperature (SFR/M_{Dust} and T_{Dust}). Late type
galaxies (later than Sc) in all of the environments can be modelled using
simple closed box chemical evolution and a simple star formation history
(SFR(t) \propto t\exp{-t/\tau}). For earlier type galaxies the physical
mechanisms that give rise to their properties are clearly much more varied and
require a more complicated model (mergers, gas in or outflow). However, we find
little or no difference in the properties of galaxies of the same morphological
type within the cluster, field or with different density contrasts. It appears
that it is morphology, how and whenever this is laid down, and consistent
internal physical processes that primarily determine the derived properties of
galaxies in the DustPedia sample and not processes related to differences in
the local environment.
