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We present a physical model that explains the two disparate observationalfacts: 1) the exponential vertical disc structure in the optical and NIR of thenon-obscured part of the stellar disc and 2) the enhanced FIR/submm luminosityby about a factor of four near the obscured mid-plane, which requiresadditional dust and also stellar light to heat the dust component. We usemulti-band photometry in U, B, V, R, and I- band combined with radiativetransfer through a dust component to fit simultaneously the verticalsurface-brightness and colour index profiles in all bands adopting a reasonablestar formation history and dynamical heating function. The final disc modelreproduces the surface-brightness profiles in all bands with a moderatelydeclining star formation rate and a slowly starting heating function for youngstars. The total dust mass is 57 million solar masses as required from theFIR/submm measurements. Without a recent star burst we find in the midplane anexcess of 5.2-, 4.0-, and 3.0-times more stellar light in the U-, B-, andV-band, respectively. The corresponding stellar mass-to-light ratios are 0.91in V- and 1.0 in R-band. The central face-on optical depth in V-band is 0.81and the radial scale length of the dust is 40% larger than that of the stellardisc. Evolutionary disc models are a powerful method to understand the verticalstructure of edge-on galaxies. Insights to the star formation history and thedynamical evolution of stellar discs can be gained. FIR/submm observations arenecessary to restrict the parameter space for the models.Comment: 17 pages, 12 figures (24 files), A&A in pres

An evolutionary disc model of the edge-on galaxy NGC 5907