Top-left: total dust-to-stellar mass ratios vs. local galaxy densities ρ₁₀ (Cappellari et al. 2011b). The symbols are as in Fig. 2. Top-right: as in the top-left panel, but for the global gas-to-stellar mass ratios. Solid circles show galaxies detected in at least one of H₂ and H I (but observed in both). Downward open triangles show global cold gas mass upper limits (i.e. the sums of the 3σ upper limits on the global H I and H₂ masses). Upward triangles show H₂ masses only and are formally all global gas-to-stellar mass ratio lower limits. Middle-left: global dust-to-gas mass ratios vs. ρ₁₀. Solid circles show galaxies robustly detected in at least one AKARI FIR band and in at least one of H₂ and H I (but observed in both). Downward open triangles show 3σ total dust mass upper limits for galaxies not robustly detected in any AKARI FIR band. Galaxies observed and detected in H₂ only are also shown as downward triangles and are formally all global dust-to-gas mass ratio upper limits and global cold gas mass lower limits. Upward triangles show global cold gas mass upper limits and are formally all global dust-to-gas mass ratio lower limits. Middle-right: as in the middle-left panel, but for the central dust-to-gas mass ratios. Bottom-left: X-ray luminosity-to-dust mass ratios vs. ρ₁₀. Solid circles show galaxies robustly detected in at least one AKARI FIR band. Upward open triangles show 3σ total dust mass upper limits for galaxies not robustly detected in any AKARI FIR band and are formally all X-ray luminosity-to-dust mass ratio lower limits. Bottom-right: as in the bottom-left panel, but for the X-ray luminosity-to-stellar mass ratios. In all panels, the solid line at log(ρ₁₀/Mpc³) = − 0.4 divides Virgo Cluster galaxies from group and field galaxies. The horizontal lines and grey-shaded regions in the middle panels are as in Fig. 3.