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Dust emission at submm to cm wavelengths is often simply the Rayleigh-Jeanstail of dust particles at thermal equilibrium and is used as a cold mass tracerin various environments including nearby galaxies. However, well-sampledspectral energy distributions of the nearby, star-forming Magellanic Cloudshave a pronounced (sub-)millimeter excess (Israel et al., 2010). This studyattempts to confirm the existence of such a millimeter excess above expecteddust, free-free and synchrotron emission and to explore different possibilitiesfor its origin. We model NIR to radio spectral energy distributions of theMagellanic Clouds with dust, free-free and synchrotron emission. A millimeterexcess emission is confirmed above these components and its spectral shape andintensity are analysed in light of different scenarios: very cold dust, CosmicMicrowave Background (CMB) fluctuations, a change of the dust spectral indexand spinning dust emission. We show that very cold dust or CMB fluctuations arevery unlikely explanations for the observed excess in these two galaxies. Theexcess in the LMC can be satisfactorily explained either by a change of thespectral index due to intrinsic properties of amorphous grains, or by spinningdust emission. In the SMC however, due to the importance of the excess, thedust grain model including TLS/DCD effects cannot reproduce the observedemission in a simple way. A possible solution was achieved with spinning dustemission, but many assumptions on the physical state of the interstellar mediumhad to be made. Further studies, using higher resolution data from Planck andHerschel, are needed to probe the origin of this observed submm-cm excess moredefinitely. Our study shows that the different possible origins will be bestdistinguished where the excess is the highest, as is the case in the SMC.

Submillimeter to centimeter excess emission from the Magellanic Clouds. II. On the nature of the excess