Probing the Dust Properties of Galaxies at Submillimetre Wavelengths II.
  Dust-to-gas mass ratio trends with metallicity and the submm excess in dwarf
  galaxies
  We are studying the effects of submm observations on the total dust mass and
thus dust-to-gas mass ratio measurements. We gather a wide sample of galaxies
that have been observed at submm wavelengths to model their Spectral Energy
Distributions using submm observations and then without submm observational
constraints in order to quantify the error on the dust mass when submm data are
not available. Our model does not make strong assumptions on the dust
temperature distribution to precisely avoid submm biaises in the study. Our
sample includes 52 galaxies observed at submm wavelengths. Out of these, 9
galaxies show an excess in submm which is not accounted for in our fiducial
model, most of these galaxies being low- metallicity dwarfs. We chose to add an
independant very cold dust component (T=10K) to account for this excess. We
find that metal-rich galaxies modelled with submm data often show lower dust
masses than when modelled without submm data. Indeed, these galaxies usually
have dust SEDs that peaks at longer wavelengths and require constraints above
160 um to correctly position the peak and sample the submillimeter slope of
their SEDs and thus correctly cover the dust temperature distribution. On the
other hand, some metal-poor dwarf galaxies modelled with submm data show higher
dust masses than when modelled without submm data. Using submm constraints for
the dust mass estimates, we find a tightened correlation of the dust-to-gas
mass ratio with the metallicity of the galaxies. We also often find that when
there is a submm excess present, it occurs preferentially in low-metallicity
galaxies. We analyse the conditions for the presence of this excess and find a
relation between the 160/850 um ratio and the submm excess.
