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Understanding how dust attenuation laws vary between and within galaxies is akey question if we want to reliably measure the physical properties of galaxiesat both global and local scales. To shed new light on this question, we presenta detailed study of the slope and bump strength of the attenuation law in thenearby spiral galaxy NGC628 at the resolved spatial scale of 325 pc. To do so,we have modelled a broad multi-wavelength dataset from the ultraviolet (UV) tothe infrared (IR) with the state-of-the-art SED fitting code CIGALE, includingSWIFT UVOT data for which we have developed a new optimized reduction pipeline.We find that the median dust attenuation curve of NGC628 is fairly steep, butnot as steep as the SMC curve, and has a sub-MW-type UV bump. We observeintriguing variations within the galaxy, with regions of high $A_V$ exhibitinga shallower attenuation curve. We argue that the flattening of the curve is dueto a dominance of absorption-over-scattering events at higher $A_V$. No trendbetween the bump strength and the IRAC 8.0 micron emission was found. However,this does not necessarily rule out PAHs as the main contributors to the UVbump.

Revealing the dust attenuation properties on resolved scales in NGC628 with SWIFT UVOT data