2025ApJS..276....2C

We present resolved 3.6-250 μm dust spectral energy distribution (SED) fitting for ∼800 nearby galaxies. We measure the distribution of radiation field intensities heating the dust, the dust mass surface density (Σ_d), and the fraction of dust in the form of polycyclic aromatic hydrocarbons (PAHs; q_PAH). We find that the average interstellar radiation field ($\overline{U}$) is correlated both with stellar mass surface density (Σ_⋆) and star formation rate surface density (Σ_SFR), while more intense radiation fields are only correlated with Σ_SFR. We show that q_PAH is a steeply decreasing function of Σ_SFR, likely reflecting PAH destruction in H II regions. Galaxy-integrated q_PAH is strongly, negatively correlated with specific star formation rate (sSFR) and offset from the star-forming “main sequence” (ΔMS), suggesting that both metallicity and star formation intensity play a role in setting the global q_PAH. We also find a nearly constant M_d/M_* ratio for galaxies on the main sequence, with a lower ratio for more quiescent galaxies, likely due to their lower gas fractions. From these results, we construct prescriptions to estimate the radiation field distribution in both integrated and resolved galaxies. We test these prescriptions by comparing our predicted $\overline{U}$ to results of SED fitting for stacked “main-sequence” galaxies at 0 < z < 4 from M. Béthermin et al. and find sSFR is an accurate predictor of $\overline{U}$ even at these high redshifts. Finally, we describe the public delivery of matched-resolution Wide-field Infrared Survey Explorer and Herschel maps along with the resolved dust SED-fitting results through the Infrared Science Archive.