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 r _ { d } 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 R _ { c } and \gamma .
The obtained distribution of R _ { c } follows a log-normal form , with center and \sigma log \big { ( } \frac { R _ { c } } { pc } \big { ) } 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 \sim 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 R _ { c } 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 .