The initial mass function for massive stars in the Magellanic Clouds. 3: Luminosity and mass functions for 14 OB associations

Details The initial mass function for massive stars in the Magellanic Clouds. 3: Luminosity and mass functions for 14 OB associations The initial mass function for massive stars in the Magellanic Clouds. 3: Luminosity and mass functions for 14 OB associations

Jul 1994

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1994apj...429..204h&link_type=abstract

The Astrophysical Journal, Part 1 (ISSN 0004-637X), vol. 429, no. 1, p. 204-224

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37

Magellanic Clouds, Massive Stars, Open Clusters, Stellar Luminosity, Astronomical Photometry, B Stars, Metallicity, O Stars, Ubv Spectra

Scientific paper

We have used UBV photometry of stars in 14 associations in the Large and Small Magellanic Clouds (LMC/SMS) (Hill, Madore, & Freedman) to derive luminosity and mass functions for the most massive stars. The main-sequence luminosity functions for the associations are quite similar, having an average slope of s = 0.03 +/- 0.06. The mass functions for the associations have slopes that span similar ranges about a common mean for both the LMC and SMC and there is no strong evidence for a significant variation in the slopes from one association to another. Accordingly, metal abundance does not appear to have a strong effect on the initial mass function (IMF), at least for the range in metallicity observed between the Magellanic Clouds. The average slope of the IMF for the Magellanic Cloud associations is Gamma = -2.0 +/- 0.5 for M greater than 9 Solar Masses. The range in the derived slopes is more likely due to the large uncertainties associated with the calculations of the mass functions, rather than to real variations in the IMF. There may be some evidence for a decrease in the slope of the IMF at masses below 9 Solar Masses, but incompleteness and the larger photometric errors associated with the faintest stars make this conclusion tentative.

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