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We are studying the effects of submm observations on the total dust mass andthus dust-to-gas mass ratio measurements. We gather a wide sample of galaxiesthat have been observed at submm wavelengths to model their Spectral EnergyDistributions using submm observations and then without submm observationalconstraints in order to quantify the error on the dust mass when submm data arenot available. Our model does not make strong assumptions on the dusttemperature distribution to precisely avoid submm biaises in the study. Oursample includes 52 galaxies observed at submm wavelengths. Out of these, 9galaxies show an excess in submm which is not accounted for in our fiducialmodel, most of these galaxies being low- metallicity dwarfs. We chose to add anindependant very cold dust component (T=10K) to account for this excess. Wefind that metal-rich galaxies modelled with submm data often show lower dustmasses than when modelled without submm data. Indeed, these galaxies usuallyhave dust SEDs that peaks at longer wavelengths and require constraints above160 um to correctly position the peak and sample the submillimeter slope oftheir SEDs and thus correctly cover the dust temperature distribution. On theother hand, some metal-poor dwarf galaxies modelled with submm data show higherdust masses than when modelled without submm data. Using submm constraints forthe dust mass estimates, we find a tightened correlation of the dust-to-gasmass ratio with the metallicity of the galaxies. We also often find that whenthere is a submm excess present, it occurs preferentially in low-metallicitygalaxies. We analyse the conditions for the presence of this excess and find arelation between the 160/850 um ratio and the submm excess.

astronomy and astrophysics

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