The Energetics of the Central Engine in the Powerful Quasar, 3C298
  The compact steep spectrum radio source, 3C 298, (redshift of 1.44) has the
largest 178 MHz luminosity in the 3CR (revised Third Cambridge Catalogue)
catalog; its radio lobes are among the most luminous in the Universe. The
plasma state of the radio lobes is modeled with the aid of interferometric
radio observations (in particular, the new Low Frequency Array observation and
archival MERLIN data) and archival single-station data. It is estimated that
the long-term time-averaged jet power required to fill these lobes with
leptonic plasma is $\overline{Q} \approx 1.28 \pm 0.51 \times 10^{47}
\rm{erg}\,\rm{s}^{-1}$, rivaling the largest time averaged jet powers from any
quasar. Supporting this notion of extraordinary jet power is a 0.5 keV -10 keV
luminosity of $\approx 5.2 \times 10^{46} \rm{erg}\, \rm{s}^{-1}$, comparable
to luminous blazars, yet there is no other indication of strong relativistic
beaming. We combine two new high signal to noise optical spectroscopic
observations from the Hobby-Eberly Telescope with archival Hubble Space
Telescope, Two Micron Survey and Galaxy Evolutionary Explorer data to compute a
bolometric luminosity from the accretion flow of $L_{\rm{bol}} \approx 1.55 \pm
0.15 \times 10^{47} \rm{erg} \,\rm{s}^{-1}$. The ratio,
$\overline{Q}/L_{\rm{bol}}\approx 1$, is the approximate upper limit for
quasars. Characteristic of a large $\overline{Q}/L_{\rm{bol}}$, we find an
extreme ultraviolet (EUV) spectrum that is very steep (the "EUV deficit" of
powerful radio quasars relative to radio quiet quasars) and this weak ionizing
continuum is likely a contributing factor to the relatively small equivalent
widths of the broad emission lines in this quasar.
