Clump mass function at an early stage of molecular cloud evolution - II. Galactic cloud complexes

The statistical approach for derivation of the clump mass function (ClMF) developed by Donkov, Veltchev & Klessen is put to observational test through comparison with mass distributions of clumps from molecular emission and dust continuum maps of Galactic cloud complexes, obtained by various authors. The results indicate gravitational boundedness of the dominant clump population, with or without taking into account the contribution of their thermal and magnetic energy. The ClMF can be presented by combination of two-power-law functions separated by a characteristic mass from about ten to hundreds of solar masses. The slope of the intermediate-mass ClMF is shallow and nearly constant (-0.25 greater than or similar to Gamma(IM) greater than or similar to -0.55) while the high-mass part is fitted by models that imply gravitationally unstable clumps and exhibit slopes in a broader range (-0.9 greater than or similar to Gamma(IM) greater than or similar to -1.6), centred at the value of the stellar initial mass function (Gamma(HM) >/< -1.3).