Surface brightness profiles for five rich star clusters in the Large Magellanic Cloud

I present surface brightness profiles for five rich star clusters in the Large Magellanic Cloud (NGC 1783, 1856, 1987, 2107 and 2108), with ages between 108 and 109 yr. The profiles are well represented by King-like models, and the core radii follow the trend, of increasing core radius with age, found in a previous study (Paper I). If this trend reveals expansion due to mass loss through stellar evolution, as proposed in Paper I, then the new data reinforce the suggestion in Paper I that the slope of the initial mass function, which determines the rate of expansion, is consistent with the Salpeter value (⁠|$x=1.35$|⁠), and is not in general as steep as |$x=2.5$|⁠.