The Initial Mass Function for Massive Stars in the Magellanic Clouds.

Details The Initial Mass Function for Massive Stars in the Magellanic Clouds. The Initial Mass Function for Massive Stars in the Magellanic Clouds.

Feb 1991

adsabs.harvard.edu/cgi-bin/nph-data_query?bibcode=1991phdt........75h&link_type=abstract

Thesis (PH.D.)--UNIVERSITY OF TORONTO (CANADA), 1991.Source: Dissertation Abstracts International, Volume: 53-02, Section: B, pa

Physics

1

Scientific paper

UBV CCD photometry has been obtained using the University of Toronto's 0.6m and the Carnegie Institution of Washington's 1.0m telescopes at Las Campanas, Chile, for 14 OB associations in the Magellanic Clouds. The data have been used to construct colour-magnitude diagrams for the purposes of investigating the massive-star content of the associations. The colour excesses range from E(B - V) = 0.01 to 0.26 mag for the LMC associations and from E(B - V) = 0.06 to 0.25 mag for the SMC objects. A detailed analysis of the effects of systematic and random errors demonstrates that the observed scatter in the colour excesses of individual stars within an association can only be explained by the existence of differential reddening in many of the associations. The main sequence luminosity functions of the associations are remarkably similar over the magnitude range -4 < Mv < -1 mag. The slope of the luminosity function (s = 0.30) is flatter than published luminosity of functions for brighter stars (Mv < -5 mag) in the Galaxy and Local Group galaxies, where s ~ 0.7. The reason for this difference is probably due to the fact that the brighter star samples consist primarily of a mixed and more highly evolved population. The slope of the initial mass function (IMF) is Gamma = -2.0 +/- 0.5 for masses 9 <= M <= 60M_odot. There is no evidence for any significant variation of the IMF among the associations or for any strong dependence on metallicity. There is, however, some evidence that the slope of the IMF is flatter for masses M < 10M_ odot.

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