Structural analysis of disk super star clusters of M82: size and profile
  shape at intermediate ages
  We present the structural parameters of 99 Super Star Clusters (SSCs) in the
Disk of M82. Moffat-EFF, King and Wilson models were fitted using a chi^2
minimisation method to background-subtracted Surface Brightness Profiles (SBPs)
in F435W (B), F555W (V), and F814W (I) bands of the Advanced Camera for Surveys
(ACS) of the Hubble Space Telescope (HST). The majority of the SSC profiles is
best-fitted by the Moffat-EFF profile. The scale parameter rd and the shape
parameter gamma in the three filters are identical within the measurement
errors. The analysed sample is big enough to allow characterisation of the
distributions of core radii Rc and gamma. The obtained distribution of Rc
follows a log-normal form, with center and sigma(log(Rc/pc)) being 1.73 pc and
0.25, respectively. The gamma distribution is also log-normal with center and
sigma(log(gamma)) being 2.88 and 0.08, respectively. M82 is well-known for the
absence of current star formation in its disk, with all disk SSCs older than 50
Myr and hardly any cluster older than ~300 Myr. The derived distributions
compare very well with the distributions for intermediate-age clusters in the
Large Magellanic Cloud (LMC), which is also a low-mass late-type galaxy similar
to M82. On the other hand, the distributions of Rc in both these galaxies are
shifted towards larger values as compared to SSCs of similar age in the giant
spiral galaxy M83. M82 and LMC also span a narrower range of gamma values as
compared to that in M83.
