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A grid of 20 millions 3-1100$\mu$m SED models is presented for syntheticyoung clusters embedded in dense clumps. The models depend on four primaryparameters: the clump mass M$_{clump}$ and dust temperature T$_{dust}$, thefraction of mass f$_{core}$ locked in dense cores, and the age of the clumpt$_{SF}$. We populate the YSO clusters using the IMF from Kroupa(2001) and theYSOs SED models grid of Robitaille et al. (2006). We conduct extensive testingof SED fitting using a simulated dataset and we find that M$_{clump}$essentially depends on the submillimeter portion of the SED, while T$_{dust}$is mostly determined from the shape of the SED in the 70-350$\mu$m range.Thanks to the large number of models computed we verify that the combinedanalysis of L/M, [8-24] and [24-70] colours removes much of the SEDsf$_{core}$-t$_{SF}$ degeneracy. The L/M values are particularly useful todiagnose f$_{core}$. L/M$\leq$1 identifies protoclusters with f$_{core}\leq$0.1and t$_{SF} \leq 10^5$ years, while L/M$\geq$10 excludes f$_{core}\leq$0.1. Wecharacterize lower limits of L/M where ZAMS stars are not found in models, andwe also find models with L/M $\geq$10 and no ZAMS stars, in which[8-24]$\geq0.8\pm 0.1$ independently from M$_{clump}$, temperature andluminosity. This is the first set of synthesis SED models suited to model forembedded and unresolved clusters of YSOs. A set of new evolutionary tracks inthe L/M diagram is also presented.

monthly notices of the royal astronomical society

Evolution of young protoclusters embedded in dense massive clumps. A new  grid of population synthesis SED models and a new set of L/M evolutionary  tracks