Contours: mass fraction of gas with temperatures <8 K as a function of total core mass, and density power-index p for a low-mass star formation (1-1-1) ISRF (left) and a high-mass star formation (4-4-4) ISRF (right), respectively. Color-coded background: for each p, the core mass functions of Aquila (left) and Orion A North (right) are shown as a function of the core mass. Since the actual p dependence is unknown, we assume that all cores have the same p. The dashed line indicates the mass limit below which 95% of all cores are located.