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We combine observations from ALMA, ATCA, MUSE, andHerschel to studygas-to-dust ratios in 15 Fornax cluster galaxies detected in the FIR/sub-mm byHerschel and observed by ALMA as part of the ALMA Fornax Cluster Survey(AlFoCS). The sample spans a stellar mass range of 8.3 $\leq$ log (M$_*$ /M$_\odot$) $\leq$ 11.16, and a variety of morphological types. We use gas-phasemetallicities derived from MUSE observations (from the Fornax3D survey) tostudy these ratios as a function of metallicity, and to study dust-to-metalratios, in a sub-sample of nine galaxies. We find that gas-to-dust ratios inFornax galaxies are systematically lower than those in field galaxies at fixedstellar mass/metallicity. This implies that a relatively large fraction of themetals in these Fornax systems is locked up in dust, which is possibly due toaltered chemical evolution as a result of the dense environment. The low ratiosare not only driven by HI deficiencies, but H$_2$-to-dust ratios are alsosignificantly decreased. This is different in the Virgo cluster, where lowgas-to-dust ratios inside the virial radius are driven by low HI-to-dustratios, while H$_2$-to-dust ratios are increased. Resolved observations ofNGC1436 show a radial increase in H$_2$-to-dust ratio, and show that low ratiosare present throughout the disc. We propose various explanations for the lowH$_2$-to-dust ratios in the Fornax cluster, including the more efficientstripping of H$_2$ compared to dust, more efficient enrichment of dust in thestar formation process, and altered ISM physics in the cluster environment.

AlFoCS + F3D II: unexpectedly low gas-to-dust ratios in the Fornax galaxy cluster