Volume 486, Number 1, July IV 2008
|Page(s)||165 - 176|
|Section||Galactic structure, stellar clusters, and populations|
|Published online||15 May 2008|
Near-infra-red spectroscopic ages of massive star clusters in M 82
Observatoire Astronomique de Strasbourg, Université L. Pasteur & CNRS (UMR 7550), Strasbourg, France e-mail: firstname.lastname@example.org
2 Department of Astronomy, University of Wisconsin-Madison, Madison WI, USA
3 Astrophysics Research Institute, Liverpool John Moores University, Liverpool, UK
4 Space Telescope Science Institute and European Space Agency, Baltimore, MD, USA
5 Department of Physics and Astronomy, University College London, London, UK
6 Institute of Astronomy, Katholieke Universiteit, Leuven, Belgium
7 Department of Physics & Astronomy, The University of Sheffield, Sheffield, UK
8 National Astronomical Observatories, Chinese Academy of Sciences, Beijing, PR China
Accepted: 10 April 2008
Context. Like other starburst galaxies, M 82 hosts compact, massive (>5 105 ) young star clusters that are interesting both in their own right and as benchmarks for population synthesis models.
Aims. In addition to assessing or reassessing the properties of some of the brightest near-IR sources in M 82, this paper addresses the following questions. Can population synthesis models at 750 adequately reproduce the near-IR spectral features and the energy distribution of these clusters between 0.8 and 2.4 μm? How do the derived cluster properties compare with previous results from optical studies?
Methods. We analyse the spectra of 5 massive clusters in M 82, using data acquired with the spectrograph SpeX on the InfraRed Telescope Facility (NASA/IRTF) and a new population synthesis tool with a highly improved near-IR extension, based on a recent collection of empirical and theoretical spectra of red supergiant stars.
Results. We obtain excellent fits across the near-IR with models at quasi-solar metallicity and a solar neighbourhood extinction law. Spectroscopy breaks a strong degeneracy between age and extinction in the near-IR colours in the red supergiant-dominated phase of evolution. The estimated near-IR ages cluster between 9 and 30 Myr, i.e. the ages at which the molecular bands due to luminous red supergiants are strongest in the current models. They do not always agree with optical spectroscopic ages. Adding optical data sometimes leads to the rejection of the solar neighbourhood extinction law. This is not surprising considering small-scale structure around the clusters, but it has no significant effect on the near-IR based spectroscopic ages.
Conclusions. The observed IR-bright clusters are part of the most recent episode of extended star formation in M 82. The near-IR study of clusters that are too faint for optical observation adds important elements to the age distribution of massive clusters in dusty starbursts. Further joint optical and near-IR spectroscopic studies will provide strong constraints on the uncertain physics of massive stars on which population synthesis models rest.
Key words: galaxies: individual: M 82 / galaxies: star clusters / galaxies: stellar content / galaxies: starburst / infrared: galaxies / stars: supergiants
© ESO, 2008
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