Supernova feedback efficiency and mass loading in the starburst and
  galactic superwind exemplar M82
  We measure the net energy efficiency of supernova and stellar wind feedback
in the starburst galaxy M82 and the degree of mass-loading of the hot gas
piston driving its superwind by comparing a large suite of 1 and 2-dimensional
hydrodynamical models to a set of observational constraints derived from hard
X-ray observations of the starburst region (the fluxes of the He-alpha and
Ly-alpha-like lines of S, Ar, Ca and Fe, along with the total diffuse E=2--8
keV X-ray luminosity). These are the first direct measurements of the feedback
efficiency and mass-loading of supernova heated and enriched plasma in a
starburst galaxy. All the models that satisfy the existing observational
constraints have medium to high thermalization efficiencies (30% <= epsilon <=
100$%) and the volume-filling wind fluid that flows out of the starburst region
is only mildly centrally mass loaded (1.0 <= beta <= 2.8). These results imply
a temperature of the plasma within the starburst region in the range 30--80
million Kelvin, a mass flow rate of the wind fluid out of the starburst region
of Mdot_tot ~ 1.4--3.6 Msol/yr and a terminal velocity of the wind in the range
v_infinity = 1410--2240 km/s. This velocity is considerably larger than the
escape velocity from M82 (v_esc <~ 460 km/s) and the velocity of the H-alpha
emitting clumps and filaments within M82's wind (v_H-alpha ~ 600 km/s). Drawing
on these results we provide a prescription for implementing starburst-driven
superwinds in cosmological models of galaxy formation and evolution. (Abridged)
