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Galaxies continuously reprocess their interstellar material. One cantherefore expect changing dust grain properties in galaxies which have followeddifferent evolutionary pathways. Determining the intrinsic dust grain mix of agalaxy helps in reconstructing its evolutionary history. Early-type galaxiesoccasionally display regular dust lanes in their central regions. Due to therelatively simple geometry and composition of their stellar bodies, thesegalaxies are ideal to disentangle dust mix variations from geometric effects.We therefore model the various components of such a galaxy (FCC 167). Wereconstruct its recent history, and investigate the possible fate of the dustlane. MUSE and ALMA observations reveal a nested ISM structure. An ionised-gasdisk pervades the central regions of FCC 167, including those occupied by themain dust lane. Inward of the dust lane, we also find a disk/ring of coldmolecular gas where stars are forming and HII regions contribute to theionised-gas emission. Further in, the gas ionisation points towards an activegalactic nucleus and the fuelling of a central supermassive black hole from itssurrounding ionised and molecular reservoir. Observational constraints andradiative transfer models suggest the dust and gas are distributed in aring-like geometry and the dust mix lacks small grains. The derived dustdestruction timescales from sputtering in hot gas are short and we concludethat the dust must be strongly self-shielding and clumpy, or will quickly beeroded and disappear. Our findings show how detailed analysis of individualsystems can complement statistical studies of dust-lane ETGs.

The Fornax 3D project: dust mix and gas properties in the center of early-type galaxy FCC 167