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We obtained an axi-symmetric model for the large-scale distribution of starsand dust in the Milky Way (MW) using a radiative transfer code that can accountfor the existing near-infrared (NIR)/mid-infrared/submm all-sky emission mapsof our Galaxy. We find that the MW has a star-formation rate of ${SFR}=1.25\pm0.2\,{ M}_{\odot}$/yr, a stellar mass $M_{*}=(4.9\pm0.3)\times10^{10}\,{ M}_{\odot}$, and a specific SFR that is relativelyconstant with radius (except for the inner 1 kpc). We identified an innerradius $R_{ in}= 4.5$\,kpc beyond which the stellar emissivity and dustdistribution fall exponentially. For $R<R_{ in}$ the emissivities fall linearlytowards the centre. The old stellar populations in the disk have an exponentialscalelength that increases monotonically from $h_{ s}^{ disk}(K)=2.2\pm0.6$\,kpc in the NIR, to $h_{ s}^{ disk}(B)=3.2\pm 0.9$\,kpc at the shorteroptical bands, and a scaleheight that varies with radial distance, from $z_{s}^{ disk}(0)=140\pm 20$\,pc in the centre to $z_{ s}^{ disk}(R_{\odot})=300\pm20$\,pc at the solar radius. The young stellar populations have a scalelengthof $h_{ s}^{ tdisk}=3.2\pm 0.9$\,kpc and a scaleheight that varies from $z_{s}^{ tdisk}(0)=50\pm 10$\,pc in the centre to $z_{ s}^{ tdisk}(R_{\odot})=90\pm10$\,pc at the solar radius. We discovered an inner stellar disk within thecentral 4.5 kpc, which we associate with the extended long bar of the MW. Mostof the obscured star formation happens within this inner thin disk. The diffusedust is mainly distributed in a disk with scalelength $h_{ d}^{ disk}=5.2\pm0.8$\,kpc and scaleheight $z_{ d}^{ disk}=0.14\pm 0.02$\,kpc. We give the firstderivation of the MW attenuation curve and present it as a functional fit tothe model data. We find the MW to lie in the Green Valley of the main sequencerelation for spiral galaxies.

A radiation transfer model for the Milky Way. II The global properties and large scale structure