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We examined variations in the 160/250 and 250/350 micron surface brightnessratios within 24 nearby (<30 Mpc) face-on spiral galaxies observed with theHerschel Space Observatory to identify the heating mechanisms for dust emittingat these wavelengths. The analysis consisted of both qualitative andquantitative comparisons of the 160/250 and 250/350 micron ratios to H alphaand 24 micron surface brightnesses, which trace the light from star formingregions, and 3.6 micron emission, which traces the light from the older stellarpopulations of the galaxies. We find broad variations in the heating mechanismsfor the dust. In one subset of galaxies, we found evidence that emission at<=160 microns (and in rare cases potentially at <=350 microns) originates fromdust heated by star forming regions. In another subset, we found that theemission at >=250 microns (and sometimes at >=160 microns) originates from dustheated by the older stellar population. In the rest of the sample, either theresults are indeterminate or both of these stellar populations may contributeequally to the global dust heating. The observed variations in dust heatingmechanisms does not necessarily match what has been predicted by dust emissionand radiative transfer models, which could lead to overestimated dusttemperatures, underestimated dust masses, false detections of variability indust emissivity, and inaccurate star formation rate measurements.

The identification of dust heating mechanisms in nearby galaxies using Herschel 160/250 and 250/350 micron surface brightness ratios