SCYON Abstract

Received on June 5 2007

A new method to derive star formation histories of galaxies from their star cluster distributions

Authors	Thomas Maschberger and Pavel Kroupa
Affiliation	Argelander-Institut fuer Astronomie, Bonn Rhine Stellar Dynamics Network
Accepted by	Monthly Notices of the Royal Astronomical Society
Contact	tmasch@astro.uni-bonn.de
URL	http://arxiv.org/abs/0705.0988
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Abstract

Star formation happens in a clustered way which is why the star cluster population of a particular galaxy is closely related to the star formation history of this galaxy. From the probabilistic nature of a mass function follows that the mass of the most-massive cluster of a complete population, M_max, has a distribution with the total mass of the population as a parameter. The total mass of the population is connected to the star formation rate (SFR) by the length of a formation epoch. Since due to evolutionary effects only massive star clusters are observable up to high ages it is convenient to use this M_max (SFR) relation for the reconstruction of a star formation history. The age-distribution of the most-massive clusters can therefore be used to constrain the star formation history of a galaxy. The method, including an assessment of the inherent uncertainties, is introduced with this contribution, while following papers will apply this method to a number of galaxies.