The Luminosity Function and Initial Mass Function for the Pleiades Cluster

Details The Luminosity Function and Initial Mass Function for the Pleiades Cluster The Luminosity Function and Initial Mass Function for the Pleiades Cluster

Apr 1995

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1995jkas...28...45l&link_type=abstract

Journal of the Korean Astronomical Society, vol. 28, no. 1, p. 45-59

Astronomy and Astrophysics

Astronomy

18

Open Cluster, Cluster:Luminosity Function, Mass Function

Scientific paper

In the best observed Pleiades cluster, the luminosity function(LF) and mass function(MF) for main sequence(MS) stars extended to Mv = 15.5(V=21) are very similar to the initial luminosity function(ILF) and initial mass function(IMF) for field stars in the solar neighborhood showing a bump at log m = -0.05 and a dip at log m = -0.12. This dip is equivalent to the Wielen Dip appearing in the LF for the field stars. The occurence of these bump and dip is independent of adopted mass-luminosity relation(MLR) and their characteristics could be explained by a time-dependent bimodal IMF. The model with this IMF gives a total cluster mass of about 700Mo, about 25 brown dwarfs and about 3 white dwarfs if the upper mass limit of progenitor of white dwarf is greater than 4.5Mo. The cluster age on the basis of LF for brightest stars is given by around 8*10E7 yr and all stars in the cluster lie along the single age sequence in the C-M diagram without showing a large dispersion from the sequence.

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