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Dust has long been identified as a barrier to measuring inherent galaxyproperties. However, the link between dust and attenuation is notstraightforward and depends on both the amount of dust and its distribution.Herschel imaging of nearby galaxies undertaken as part of the KINGFISH projectallows us to map the dust as seen in emission with unprecedented sensitivityand ~1 kpc resolution. We present here new optical integral field unitspectroscopy for eight of these galaxies that provides complementary 100-200 pcscale maps of the dust attenuation through observation of the reddening in boththe Balmer decrement and the stellar continuum. The stellar continuumreddening, which is systematically less than that observed in the Balmerdecrement, shows no clear correlation with the dust, suggesting that thedistribution of stellar reddening acts as a poor tracer of the overall dustcontent. The brightest HII regions are observed to be preferentially located industy regions, and we do find a correlation between the Balmer line reddeningand the dust mass surface density for which we provide an empirical relation.Some of the high-inclination systems in our sample exhibit high extinction, butwe also find evidence that unresolved variations in the dust distribution onscales smaller than 500 pc may contribute to the scatter in this relation. Wecaution against the use of integrated A_V measures to infer global dustproperties.

Mapping dust through emission and absorption in nearby galaxies