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A fraction of the early-type galaxy population hosts a prominent dust lane.Methods to quantify the dust content of these systems based on optical imagingdata usually yield dust masses which are an order of magnitude lower than dustmasses derived from the observed FIR emission. High-quality optical data fromthe Next Generation Virgo cluster Survey (NGVS) and FIR/submm observations fromthe Herschel Virgo Cluster Survey (HeViCS) allow us to revisit previous methodsto determine the dust content in galaxies and explore new ones. We aim toderive the dust mass in NGC 4370 from both optical and FIR data, andinvestigate the need to invoke a putative diffuse dust component. We createcolor and attenuation maps, which are converted to approximate dust mass mapsbased on simple dust geometries. Dust masses are also derived from SED fits toFIR/submm observations. Finally, inverse radiative transfer fitting isperformed to investigate more complex dust geometries. The empirical methodsapplied to the optical data yield lower limits of 3.4e5 solar masses, an orderof magnitude below the total dust masses derived from SED fitting. In contrast,radiative transfer models yield dust masses which are slightly lower, but fullyconsistent with the FIR-derived mass. Dust is more likely to be distributed ina ring around the centre of NGC 4370 as opposed to an exponential disc or asimple foreground screen. Moreover, using inverse radiative transfer fitting,we are able to constrain most of the parameters describing these geometries.The resulting dust masses are high enough to account for the dust observed atFIR/submm wavelengths, so that no diffuse dust component needs to be invoked.We furthermore caution for the interpretation of dust masses and optical depthsbased on optical data alone, using overly simplistic star-dust geometries andthe neglect of scattering effects. [ABRIDGED]

NGC4370: a case study for testing our ability to infer dust distribution and mass in nearby galaxies