Not yet reviewed by Pith; the record is open.

We present three-dimensional Monte Carlo radiative transfer models of a very young (<10^5 years old) low mass (50 Msun) stellar cluster containing 23 stars and 27 brown dwarfs. The models use the density and the stellar mass distributions from the large-scale smoothed particle hydrodynamics (SPH) simulation of the formation of a low-mass stellar cluster by Bate, Bonnell and Bromm. We compute the spectral energy distributions of the whole cluster and the individual objects, simulated far-infrared Spitzer Space Telescope (SST) images and construct colour-colour diagrams (near-infrared HKL and SST mid-infrared bands). The presence of accretion discs around the light sources influences the morphology of the dust temperature structure on a large scale (up to a several 10^4 au). A considerable fraction of the interstellar dust is underheated compared to a model without the accretion discs because the radiation from the light sources is blocked/shadowed by the discs. The spectral energy distribution (SED) of the model cluster with accretion discs shows excess emission at lambda = 3-30 micron and lambda > 500 micron compared to that without accretion discs. Our model with accretion discs around each object shows a similar distribution of spectral index (2.2-20 micron) values (i.e. Class 0--III sources) as seen in the Rho Ophiuchus cloud. We confirm that the best diagnostics for identifying objects with accretion discs are mid-infrared (lambda = 3-10 micron) colours (e.g. SST IRAC bands) rather than HKL colours.