2012MNRAS.427..637P

We determine the distribution of stellar surface densities, Σ, from models of static and dynamically evolving star clusters with different morphologies, including both radially smooth and substructured clusters. We find that the Σ distribution is degenerate, in the sense that many different cluster morphologies (smooth or substructured) produce similar cumulative distributions. However, when used in tandem with a measure of structure, such as the \mi Q-parameter, the current spatial and dynamical state of a star cluster can be inferred. The effect of cluster dynamics on the Σ distribution and the \mi Q-parameter is investigated using N-body simulations and we find that, depending on the assumed initial conditions, the Σ distribution can rapidly evolve from high to low densities in less than 5Myr. This suggests that the Σ distribution can only be used to assess the current density of a star-forming region, and provides little information on its initial density. However, if the Σ distribution is used together with the \mi Q-parameter, then information on the amount of substructure can be used as a proxy to infer the amount of dynamical evolution that has taken place. Substructure is erased quickly through dynamics, which can disrupt binary star systems and planets, as well as facilitate dynamical mass segregation. Therefore, dynamical processing in young star-forming regions could still be significant, even without currently observed high densities.