ON THE ORIGIN OF THE SALPETER SLOPE FOR THE INITIAL MASS FUNCTION

We suggest that the intrinsic, stellar initial mass function (IMF) follows a power-law slope γ = 2, inherited from hierarchical fragmentation of molecular clouds into clumps and clumps into stars. The well-known, logarithmic Salpeter slope Γ = 1.35 in clusters is then the aggregate slope for all the star-forming clumps contributing to an individual cluster, and it is steeper than the intrinsic slope within individual clumps because the smallest star-forming clumps contributing to any given cluster are unable to form the highest-mass stars. Our Monte Carlo simulations demonstrate that the Salpeter power-law index is the limiting value obtained for the cluster IMF when the lower-mass limits for allowed stellar masses and star-forming clumps are effectively equal, Mlo = Mlo. This condition indeed is imposed for the high-mass IMF tail by the turnover at the characteristic value mc ∼ 1 Msun. IMF slopes of Γ ∼ 2 are obtained if the stellar and clump upper-mass limits are also equal Mup = Mup ∼ 100 Msun, and so our model explains the observed range of IMF slopes between Γ ∼ 1 and 2. Flatter slopes of Γ = 1 are expected when Mlo > Mup, which is a plausible condition in starbursts, where such slopes are suggested to occur. While this model is a simplistic parameterization of the star formation process, it seems likely to capture the essential elements that generate the Salpeter tail of the IMF for massive stars. These principles also likely explain the integrated galaxy IMF (IGIMF) effect seen in low-density star-forming environments.