and disk fractions as a function of color ($H-K$). We drew the artificial population from a broken power law IMF using the parameters of the one obtained for the IC 348 cluster (2 Myr old) in the paper of @Muench:2003aa. To draw the artificial populations we used the pre-main sequence stellar evolution model by [@DAntona:1997aa], with $[D/H]=2\times 10^{-5}$ to draw the samples for the artificial clusters . We ran the models using a grid of ages in which we varied the mean age of the cluster between 0.5 and 10 Myr, in s.pdf of 0.5 Myr. For each case, we simulated five age spreads between 1.0 to 5.0 Myr. For each case we simulated 500 clusters.

The method could not be applied succesfully for the DR15-N sample, due to the large extinction variations in that cluster, which does not allow us to obtain a sufficient detection rate in the K band at the highest column density regions. In the remaining clusters, we were able to isolate extinction limited samples satisfactorily.

We determined which age/age spread set fits each of the observed KLFs by averaging the KLF over all simulations for each point in the grid and comparing to the observed 