ZABEL , NIKKI JOHANNANIKKI JOHANNAZABELDavis, Timothy A.Timothy A.DavisSmith, Matthew W.~L.Matthew W.~L.SmithSarzi, MarcMarcSarziLONI, AlessandroAlessandroLONISERRA, PaoloPaoloSERRALara-López, Maritza A.Maritza A.Lara-LópezCigan, PhilPhilCiganBaes, MaartenMaartenBaesBendo, George J.George J.BendoDe Looze, IlseIlseDe LoozeIODICE, ENRICHETTAENRICHETTAIODICEKLEINER, DANEDANEKLEINERKoribalski, Bärbel S.Bärbel S.KoribalskiPeletier, ReynierReynierPeletierPinna, FrancescaFrancescaPinnade Zeeuw, P. TimP. Timde Zeeuw2025-03-272025-03-2720210035-8711http://hdl.handle.net/20.500.12386/36959We combine observations from ALMA, ATCA, MUSE, andHerschel to study gas-to-dust ratios in 15 Fornax cluster galaxies detected in the FIR/sub-mm by Herschel 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-phase metallicities derived from MUSE observations (from the Fornax3D survey) to study these ratios as a function of metallicity, and to study dust-to-metal ratios, in a sub-sample of nine galaxies. We find that gas-to-dust ratios in Fornax galaxies are systematically lower than those in field galaxies at fixed stellar mass/metallicity. This implies that a relatively large fraction of the metals in these Fornax systems is locked up in dust, which is possibly due to altered chemical evolution as a result of the dense environment. The low ratios are not only driven by HI deficiencies, but H$_2$-to-dust ratios are also significantly decreased. This is different in the Virgo cluster, where low gas-to-dust ratios inside the virial radius are driven by low HI-to-dust ratios, while H$_2$-to-dust ratios are increased. Resolved observations of NGC1436 show a radial increase in H$_2$-to-dust ratio, and show that low ratios are present throughout the disc. We propose various explanations for the low H$_2$-to-dust ratios in the Fornax cluster, including the more efficient stripping of H$_2$ compared to dust, more efficient enrichment of dust in the star formation process, and altered ISM physics in the cluster environment.STAMPAenArticle10.1093/mnras/stab3422-s2.0-85105226997https://academic.oup.com/mnras/article/502/4/4723/6129797http://arxiv.org/abs/2102.02148v1FIS/05 - ASTRONOMIA E ASTROFISICA