  We present high dispersion echelle spectroscopy of the very luminous, young
super star cluster (SSC) `F' in M82, obtained with the 4.2-m William Herschel
Telescope (WHT), for the purpose of deriving its dynamical mass and assessing
whether it will survive to become an old globular cluster. We measure a stellar
velocity dispersion of 13.4 +/- 0.7 km/s, a projected half-light radius of 2.8
+/- 0.3 pc from archival HST/WFPC2 images, and derive a dynamical mass of 1.2
+/- 0.1 x 10^6 solar masses, demonstrating that M82-F is a very massive,
compact cluster. We determine that the current visual luminosity-to-mass ratio
for M82-F is 45 +/- 13. Comparison with spectral synthesis models shows that
the visual luminosity-to-mass ratio is a factor of 5 higher than that predicted
for a standard Kroupa (2001) initial mass function (IMF) at the well-determined
age for M82-F of 60 +/- 20 Myr. This high value of the visual
luminosity-to-mass ratio indicates a deficit of low mass stars in M82-F; the
current mass function (MF) evidently is `top-heavy'. We find that a lower mass
cutoff of 2-3 solar masses is required to match the observations for a MF with
a slope of 2.3. Since the cluster apparently lacks long-lived low mass stars,
it will not become an old globular cluster. We also derive up-dated
luminosity-to-mass ratios for the younger SSCs NGC 1569A and NGC 1705-1. We
discuss the implications of our findings in the context of large scale IMF
variations; with the present data the top-heavy MF could reflect a local mass
segregation effect during the birth of the cluster.
