  3C 82 at a redshift of 2.87 is the most distant 3C (Third Cambridge
Catalogue) quasar. Thus, it is a strong candidate to have the most luminous
radio lobes in the Universe. 3C 82 belongs to the class of compact steep
spectrum radio sources. We use single dish and interferometric radio
observations in order to model the plasma state of these powerful radio lobes.
It is estimated that the long-term time-averaged jet power required to fill
these lobes with leptonic plasma is $\overline{Q} \approx 2.66 \pm 1.33 \times
10^{47} \rm{ergs/sec}$, among the largest time averaged jet powers from a
quasar. Positing protonic lobes is not tenable since they would require two
orders of magnitude more mass transport to the lobes than was accreted to the
central black hole during their formation. The first high signal to noise
optical spectroscopic observation obtained of this object indicates that there
is a powerful high ionization broad line wind with a kinetic power $\sim
10^{45} \rm{ergs/sec}$ and a velocity $\sim 0.01$c. We also estimate from the
broad lines in 2018 and the UV continuum in three epochs spread out over three
decades that the accretion flow bolometric luminosity is $L_{\rm{bol}} \approx
3.2-5.8 \times 10^{46} \rm{ergs/sec}$. The ratio of
$\overline{Q}/L_{\rm{bol}}\approx 6.91 \pm 3.41$, is perhaps the largest of any
known quasar. Extremely powerful jets tend to strongly suppress powerful winds
of ionized baryonic matter. Consequently, 3C 82 provides a unique laboratory
for studying the dynamical limits of the central engine of outflow initiation
in quasars.
