SCYON Abstract

Received on August 30 2010

The galaxy-wide IMF - from star clusters to galaxies

AuthorsC. Weidner (1,2), J. Pflamm-Altenburg (2), and P. Kroupa (2)
Affiliation(1) Scottish Universities Physics Alliance (SUPA), School of Physics and Astronomy, University of St. Andrews, North Haugh, St. Andrews, Fife KY16 9SS, UK
(2) Argelander-Institut für Astronomie (Sternwarte), Auf dem Hügel 71, D-53121 Bonn, Germany
To appear inproceedings of the conference/workshop, UP: Have Observations Revealed a Variable Upper End of the Initial Mass Function?, held in Sedona, USA 20/06 -- 25/06/2010, ASP conference series
Contactcw60@st-andrews.ac.uk
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Abstract

Over the past years observations of young and populous star clusters have shown that the stellar initial mass function (IMF) can be conveniently described by a two-part power-law with an exponent α2 = 2.3 for stars more massive than about 0.5 M(sun) and an exponent of α1 = 1.3 for less massive stars. A consensus has also emerged that most, if not all, stars form in stellar groups and star clusters, and that the mass function of these can be described as a power-law (the embedded cluster mass function, ECMF) with an exponent β ≈ 2. These two results imply that the integrated galactic IMF (IGIMF) for early-type stars cannot be a Salpeter power-law, but that they must have a steeper exponent. An application to star-burst galaxies shows that the IGIMF can become top-heavy. This has important consequences for the distribution of stellar remnants and for the chemo-dynamical and photometric evolution of galaxies. In this contribution the IGIMF theory is described, and the accompanying contribution by Pflamm-Altenburg, Weidner & Kroupa (this volume) documents the applications of the IGIMF theory to galactic astrophysics.