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We utilize archival far-infrared maps from the Herschel Space Observatory infour Local Group galaxies (Small and Large Magellanic Clouds, M31, and M33). Wemodel their Spectral Energy Distribution (SED) from 100 to 500 $\mu$m using asingle-temperature modified blackbody emission with a fixed emissivity index of$\beta = 1.8$. From the best-fit model, we derive the dust temperature, $T_{\rmd}$, and the dust mass surface density, $\Sigma_{\rm d}$, at 13 parsecresolution for SMC and LMC, and at 167 parsec resolution for all targets. Thismeasurement allows us to build the distribution of dust mass and luminosity asfunctions of dust temperature and mass surface density. We compare thosedistribution functions among galaxies and between regions in a galaxy. We findthat LMC has the highest mass-weighted average $T_{\rm d}$, while M31 and M33have the lowest mass-weighted average $T_{\rm d}$. Within a galaxy, starforming regions have higher $T_{\rm d}$ and $\Sigma_{\rm d}$ relative to theoverall distribution function, due to more intense heating by young stars andhigher gas mass surface density. When we degrade the resolutions to mimicdistant galaxies, the mass-weighted mean temperature gets warmer as theresolution gets coarser, meaning the temperature derived from unresolvedobservation is systematically higher than that in highly resolved observation.As an implication, the total dust mass is lower (underestimated) in coarserresolutions. This resolution-dependent effect is more prominent in clumpystar-forming galaxies (SMC, LMC, and M33), and less prominent in more quiescentmassive spiral (M31).

The Resolved Distributions of Dust Mass and Temperature in Local Group Galaxies