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The spatial distribution of dust in galaxies affects the global attenuation,and hence inferred properties, of galaxies. We trace the spatial distributionof dust in five fields (at 0.6-0.9 kpc scale) of M31 by comparing opticalattenuation with the total dust mass distribution. We measure the attenuationfrom the Balmer decrement using Integral Field Spectroscopy and the dust massfrom Herschel far-IR observations. Our results show that M31's dust attenuationclosely follows a foreground screen model, contrary to what was previouslyfound in other nearby galaxies. By smoothing the M31 data we find that spatialresolution is not the cause for this difference. Based on the emission lineratios and two simple models, we conclude that previous models of dust/gasgeometry need to include a weakly or non-attenuated diffuse ionized gas (DIG)component. Due to the variation of dust and DIG scale heights with galacticradius, we conclude that different locations in galaxies will have differentvertical distributions of gas and dust and therefore different measuredattenuation. The difference between our result in M31 with that found in othernearby galaxies can be explained by our fields in M31 lying at larger galacticradii than the previous studies that focused on the centres of galaxies.

Attenuation modified by DIG and dust as seen in M31