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We analyzed the regions of star formation in the spiral galaxies NGC 3184 andNGC 3938 from archive images at multiple wavelengths (NUV from GALEX, H-alphafrom JKT and KPNO, 8 and 24 um from Spitzer, and CO from BIMA). We used theClump Find Algorithm to extract the properties of the star forming tracersshown as emission regions at each wavelength. We obtained a power-law relationbetween the luminosity and the emission region volume that scales as expected,$L proportional to V, for the H-alpha and NUV emission; but much faster for thedust (8 and 24 um) and molecular gas emitting regions in CO. This isinterpreted as a change on the emissivity with the size of the cloud, either byan augmentation of the overall density or due to the presence of high densityclumps, with high local emissivity coefficients. Although the clumpy nature ofmolecular gas may not be surprising, the clumpy nature of mid-infrared emissionregions, that could be explained by newly formed high to intermediate massstars embedded into the dust and heating it, is clearly revealed in bothgalaxies.

Density effect on multi-wavelength luminosities on star formation regions in NGC 3184 and NGC 3938