Volume 525, January 2011
|Number of page(s)||15|
|Section||Galactic structure, stellar clusters and populations|
|Published online||07 December 2010|
The evolution of luminosity, colour, and the mass-to-luminosity ratio of Galactic open clusters
Comparison of discrete vs. continuous IMF models
Astrophysikalisches Institut Potsdam,
An der Sternwarte 16,
2 Institute of Astronomy of the Russian Acad. Sci., 48 Pyatnitskaya Str., 109017 Moscow, Russia
3 Astronomisches Rechen-Institut, Mönchhofstraße 12-14, Zentrum für Astronomie der Universität Heidelberg, 69120 Heidelberg, Germany
4 Main Astronomical Observatory, 27 Academica Zabolotnogo Str., 03680 Kiev, Ukraine
Received: 12 July 2010
Accepted: 11 October 2010
Context. We found in previous studies that standard simple stellar population (SSP) models are unable to describe or explain the colours of Galactic open clusters both in the visible and in the near-infrared (NIR) spectral range. The reason for this disagreement is the continuous nature of the stellar initial mass function (IMF) in clusters, which is the underlying assumption in the SSP models. In reality, the Galactic open clusters are sparsely populated with the brightest stars responsible for integrated fluxes.
Aims. In this study, we aim at constructing discrete SSP-models that are able to adequately describe the observed magnitude-, colour-, and mass-to-luminosity-ratio-age relations of open clusters by including a number of seldom considered effects.
Methods. We construct a numerical SSP-model with an underlying Salpeter IMF, which is valid within an upper mu and lower ml stellar mass range, and with the total masses Mc = 102...104 m⊙ typical of open clusters. We assume that the mass loss from a cluster is provided by mass loss from evolved stars and by the dynamical evaporation of low-mass members because of two-body relaxation. The data for the latter process were scaled to the models from high-resolution N-body calculations. We also investigate how a change of the ml-limit influences the magnitudes and colours of clusters of a given mass and derive a necessary condition for a luminosity and colour flash.
Results. The discreteness of the IMF leads to bursts in the magnitude and colour of model clusters at moments when red supergiants or giants appear and then die. The amplitude of the burst depends on the cluster mass and on the spectral range; it is strongly increased in the NIR compared to optical passbands. In the discrete case variations of the parameter ml are able to substantially change the magnitude-age and M/L-age relations. For the colours, the lowering of ml considerably amplifies the discreteness effect. The influence of dynamical mass loss on colour and magnitude is weak, although it provides a change of the slopes of the considered relations, improving their agreement with observations. For the Galactic open clusters we determined luminosity and tidal mass independent of each other. The derived mass-to-luminosity ratio shows, on average, an increase with cluster age in the optical, but gradually declines with age in the NIR. The observed flash statistics can be used to constrain ml in open clusters.
Key words: Galaxy: stellar content / galaxies: fundamental parameters / galaxies: starburst / galaxies: star clusters: general / galaxies: photometry / open clusters and associations: general
© ESO, 2010
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