Star Formation in Extreme Starburst Environments - Super Star Clusters.pdf

Star Formation in Extreme Starburst Environments - Super Star Clusters.pdf

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Star Formation in Extreme Starburst Environments - Super Star Clusters

a r X i v : a s t r o - p h / 0 3 0 8 2 3 2 v 1 1 3 A u g 2 0 0 3 **TITLE** ASP Conference Series, Vol. **VOLUME***, **YEAR OF PUBLICATION** **NAMES OF EDITORS** Star Cluster Formation in Extreme Starburst Environments Richard de Grijs Department of Physics Astronomy, The University of Sheffield, Hicks Building, Hounsfield Road, Sheffield S3 7RH, UK Abstract. The currently available empirical evidence on the star for- mation processes in the extreme, high-pressure environments induced by galaxy encounters, mostly based on high-resolution Hubble Space Tele- scope imaging observations, strongly suggests that star cluster formation is an important and perhaps even the dominant mode of star formation in the starburst events associated with galaxy interactions. 1. Gravitational Interaction Induced Star (Cluster) Formation Close encounters between gas-rich galaxies often have devastating effects on the state of their interstellar medium (ISM), in particular of the ISM of either the smaller or of the most gas-rich of the interacting galaxies (e.g., de Grijs et al. 2001, 2003). The ram pressure caused by the time-varying gravitational poten- tial induced by the interaction causes free-floating giant molecular clouds in the affected galaxy’s ISM to collapse and enter a phase of violent star formation. This process is particularly well illustrated by the ongoing interaction between NGC 6745 and its small northern companion galaxy, “NGC 6745c” (cf. de Grijs et al. 2003), where dynamical and kinematic evidence from Hi observations obtained with the Very Large Array support the scenario that the small com- panion galaxy has traveled from the south east across the eastern edge of the main galaxy to its current location north of the main galaxy, in its wake leaving a frenzy of very violent and active star, and in particular star cluster, formation. In de Grijs et al. (2003b) we used the ages, masses and metallicities of the rich young star cluster system in NGC 6745, based o

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