Mass segregation represented by the cumulative mean mass profile of stars above the completeness limit at 708 Myr: from the BFSR (solid blue), from the observation (solid black), the average of 15 different simulations with different random seeds for the coordinate and velocity distribution or IMF (dashed red), and their 1 σ range (grey area). The lighter shades of grey represent the lower number (only ~4–5) of simulations, which had stars inside that radius from the cluster centre.