2021MNRAS.502.4723Z

We combine observations from Atacama Large Millimeter/submillimeter Array (ALMA), Australia Telescope Compact Array, Multi Unit Spectroscopic Explorer (MUSE), and Herschel 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. The sample spans a stellar mass range of 8.3 <= log(M_*/M_☉) <= 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 H I deficiencies, but H₂-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 H I-to-dust ratios, while H₂-to-dust ratios are increased. Resolved observations of NGC 1436 show a radial increase in H₂-to-dust ratio, and show that low ratios are present throughout the disc. We propose various explanations for the low H₂-to-dust ratios in the Fornax cluster, including the more efficient stripping of H₂ compared to dust, more efficient enrichment of dust in the star formation process, and altered interstellar medium physics in the cluster environment.