  In this Letter, the properties of the extended radio emission form SDSS DR7
quasars with $0.4<z<0.8$ is studied. This low redshift sample is useful since
any corresponding FIRST radio observations are sensitive enough to detect
extended flux in even the weakest FR II radio sources. In the sample, 2.7% of
the sources have detectable extended emission on larger than galactic scales
($>$ 20 - 30 kpc). The frequency of quasars with FR II level extended radio
emission is $\approx 2.3%$ and $>0.4%$ of quasars have FR I level extended
radio emission. The lower limit simply reflects the flux density limit of the
survey. The distribution of the long term time averaged jet powers of these
quasars, $\bar{Q}$, has a broad peak $\sim 3\times 10^{44}$ ergs/sec that turns
over below below $10^{44}$ ergs/sec and sources above $10^{45}$ ergs/sec are
extremely rare. It is found that the correlation between the bolometric (total
thermal) luminosity of the accretion flow, $L_{bol}$, and $\bar{Q}$ is not
strong. The correlation of $\bar{Q}$ with narrow line luminosity is stronger
than the correlation with broad line luminosity and the continuum luminosity.
It is therefore concluded that previous interpretations of correlations of
$\bar{Q}$ with narrow line strengths in radio galaxies as a direct correlation
of jet power and accretion power have been overstated. It is explained why this
interpretation mistakenly overlooks the sizeable fraction of sources with weak
accretion luminosity and powerful jets discovered by Ogle et al (2006).
