%0 Generic %1 remyruyer2015linking %A Rémy-Ruyer, A. %A Madden, S. C. %A Galliano, F. %A Lebouteiller, V. %A Baes, M. %A Bendo, G. J. %A Boselli, A. %A Ciesla, L. %A Cormier, D. %A Cooray, A. %A Cortese, L. %A De Looze, I. %A Doublier-Pritchard, V. %A Galametz, M. %A Jones, A. P. %A Karczewski, O. Ł. %A Lu, N. %A Spinoglio, L. %D 2015 %K dust emission metallicity %T Linking dust emission to fundamental properties in galaxies: The low-metallicity picture %U http://arxiv.org/abs/1507.05432 %X In this work, we aim at providing a consistent analysis of the dust properties from metal-poor to metal-rich environments by linking them to fundamental galactic parameters. We consider two samples of galaxies: the Dwarf Galaxy Survey (DGS) and KINGFISH, totalling 109 galaxies, spanning almost 2 dex in metallicity. We collect infrared (IR) to submillimetre (submm) data for both samples and present the complete data set for the DGS sample. We model the observed spectral energy distributions (SED) with a physically-motivated dust model to access the dust properties. Using a different SED model (modified blackbody), dust composition (amorphous carbon), or wavelength coverage at submm wavelengths results in differences in the dust mass estimate of a factor two to three, showing that this parameter is subject to non-negligible systematic modelling uncertainties. For eight galaxies in our sample, we find a rather small excess at 500 microns (< 1.5 sigma). We find that the dust SED of low-metallicity galaxies is broader and peaks at shorter wavelengths compared to more metal-rich systems, a sign of a clumpier medium in dwarf galaxies. The PAH mass fraction and the dust temperature distribution are found to be driven mostly by the specific star-formation rate, SSFR, with secondary effects from metallicity. The correlations between metallicity and dust mass or total-IR luminosity are direct consequences of the stellar mass-metallicity relation. The dust-to-stellar mass ratios of metal-rich sources follow the well-studied trend of decreasing ratio for decreasing SSFR. The relation is more complex for highly star-forming low-metallicity galaxies and depends on the chemical evolutionary stage of the source (i.e., gas-to-dust mass ratio). Dust growth processes in the ISM play a key role in the dust mass build-up with respect to the stellar content at high SSFR and low metallicity. (abridged)

@misc{remyruyer2015linking, abstract = {In this work, we aim at providing a consistent analysis of the dust properties from metal-poor to metal-rich environments by linking them to fundamental galactic parameters. We consider two samples of galaxies: the Dwarf Galaxy Survey (DGS) and KINGFISH, totalling 109 galaxies, spanning almost 2 dex in metallicity. We collect infrared (IR) to submillimetre (submm) data for both samples and present the complete data set for the DGS sample. We model the observed spectral energy distributions (SED) with a physically-motivated dust model to access the dust properties. Using a different SED model (modified blackbody), dust composition (amorphous carbon), or wavelength coverage at submm wavelengths results in differences in the dust mass estimate of a factor two to three, showing that this parameter is subject to non-negligible systematic modelling uncertainties. For eight galaxies in our sample, we find a rather small excess at 500 microns (< 1.5 sigma). We find that the dust SED of low-metallicity galaxies is broader and peaks at shorter wavelengths compared to more metal-rich systems, a sign of a clumpier medium in dwarf galaxies. The PAH mass fraction and the dust temperature distribution are found to be driven mostly by the specific star-formation rate, SSFR, with secondary effects from metallicity. The correlations between metallicity and dust mass or total-IR luminosity are direct consequences of the stellar mass-metallicity relation. The dust-to-stellar mass ratios of metal-rich sources follow the well-studied trend of decreasing ratio for decreasing SSFR. The relation is more complex for highly star-forming low-metallicity galaxies and depends on the chemical evolutionary stage of the source (i.e., gas-to-dust mass ratio). Dust growth processes in the ISM play a key role in the dust mass build-up with respect to the stellar content at high SSFR and low metallicity. (abridged)}, added-at = {2015-07-21T09:50:10.000+0200}, author = {Rémy-Ruyer, A. and Madden, S. C. and Galliano, F. and Lebouteiller, V. and Baes, M. and Bendo, G. J. and Boselli, A. and Ciesla, L. and Cormier, D. and Cooray, A. and Cortese, L. and De Looze, I. and Doublier-Pritchard, V. and Galametz, M. and Jones, A. P. and Karczewski, O. Ł. and Lu, N. and Spinoglio, L.}, biburl = {https://www.bibsonomy.org/bibtex/2b8926cbb11f9faeb90942dc4e15d1645/miki}, description = {[1507.05432] Linking dust emission to fundamental properties in galaxies: The low-metallicity picture}, interhash = {c2150da3f1689085a80ae5bdbd41ce73}, intrahash = {b8926cbb11f9faeb90942dc4e15d1645}, keywords = {dust emission metallicity}, note = {cite arxiv:1507.05432Comment: 44 pages (20 pages main body plus 5 Appendices), 11 figures, 9 tables, accepted for publication in A&A}, timestamp = {2015-07-21T09:50:10.000+0200}, title = {Linking dust emission to fundamental properties in galaxies: The low-metallicity picture}, url = {http://arxiv.org/abs/1507.05432}, year = 2015 }