  We present the results of studying the accretion disk vs jet power for a
large fraction of all the blazars detected by the Fermi Gamma-Ray Space
Telescope. The disk power is inferred from the emission line luminosities
obtained from published results. As indicators of jet power, we use low
frequency radio luminosity from the extended jet, maximum speed of radio knots
observed in the VLBA monitoring of the pc-scale jets, kinetic energy of
electrons in the jet deduced from the best-fit theoretical models of their
spectral energy distribution, and gamma-ray luminosity with and without beaming
correction. We obtain a significant correlation in most of those cases.
However, we find that the correlations are often driven by the common redshift
dependence of the compared quantities. In order to remove the redshift bias and
probe the intrinsic correlation between the disk and jet power, we compute the
partial correlation coefficient as well as the correlation in small redshift
bins, and find that the intrinsic disk-jet correlation is still present but
weaker. In the cases, in which the common redshift dependence does not affect
the result, we find that blazars do not exhibit high jet power for low disk
luminosities while there are both high and low jet power for high disk
luminosities. This result indicates that a powerful disk is a necessary but not
sufficient condition to produce a powerful jet.
