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We present the results of studying the accretion disk vs jet power for alarge fraction of all the blazars detected by the Fermi Gamma-Ray SpaceTelescope. The disk power is inferred from the emission line luminositiesobtained from published results. As indicators of jet power, we use lowfrequency radio luminosity from the extended jet, maximum speed of radio knotsobserved in the VLBA monitoring of the pc-scale jets, kinetic energy ofelectrons in the jet deduced from the best-fit theoretical models of theirspectral energy distribution, and gamma-ray luminosity with and without beamingcorrection. We obtain a significant correlation in most of those cases.However, we find that the correlations are often driven by the common redshiftdependence of the compared quantities. In order to remove the redshift bias andprobe the intrinsic correlation between the disk and jet power, we compute thepartial correlation coefficient as well as the correlation in small redshiftbins, and find that the intrinsic disk-jet correlation is still present butweaker. In the cases, in which the common redshift dependence does not affectthe result, we find that blazars do not exhibit high jet power for low diskluminosities while there are both high and low jet power for high diskluminosities. This result indicates that a powerful disk is a necessary but notsufficient condition to produce a powerful jet.

Moderate Correlation between the Accretion Disk and Jet Power in a Large Sample of Fermi Blazars