I track the history of star count estimates of the Milky Way field star and open cluster IMFs, concentrating on the neglected mass range from 1 to 15 M⊙. The prevalent belief that the IMF is universal appears to be without basis for this mass range. Two recent estimates of the field star IMF using different methods and samples give values of the average logarithmic slope Γ between -1.7 and -2.1...

High spatial resolution, near-infrared imaging and spectroscopy of the nuclear star cluster have given key new insights about the dynamics, evolution and mass distribution in the Milky Way Center. The central parsec is powered by a cluster of hot, massive stars which must have formed a few million years ago. Either star formation was triggered in the central parsec by the infall of a very dense...

Tidal tails of star clusters are not homogeneous but show well defined clumps in observations as well as in numerical simulations. Recently an epicyclic theory for the formation of these clumps was presented. A quantitative analysis was still missing. We present a quantitative derivation of the angular momentum and energy distribution of escaping stars from a star cluster in the tidal field of ...

We examine various physical processes associated with the formation of globular clusters by using the three-dimensional Smoothed Particle Hydrodynamics (SPH) code. Our code includes radiative cooling of gases, star formation, energy feedback from stars including stellar winds and supernovae, and chemical enrichment by stars. We assume that, in the collapsing galaxy, isothermal cold clouds form ...

The formation of star clusters involves the growth smaller, gas-rich subclusters through accretion gas from giant molecular cloud within which are embedded. two main mechanisms responsible for this dense filaments, and ambient background cloud. We perform simulations both these processes onto using coupled smoothed particle hydrodynamics to model gas, N-body dynamics stars. find that, processes...

We employ panoramic, multicolour (BRz) and narrow-band Hα imaging of the cluster Cl 0024.0+1652 (z = 0.39) from Subaru covering a ∼ 30 arcmin field, to determine cluster membership and star formation rates for a large sample of galaxies across a wide field in the cluster, ∼ 10Mpc. We use photometric redshifts to identify cluster members, and statistically correct for the residual field contamin...