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Here we explore the disk-jet connection in the broad-line radio quasar4C+74.26, utilizing the results of the multiwavelength monitoring of thesource. The target is unique in that its radiative output at radio wavelengthsis dominated by a moderately-beamed nuclear jet, at optical frequencies by theaccretion disk, and in the hard X-ray range by the disk corona. Our analysisreveals a correlation (local and global significance of 96\% and 98\%,respectively) between the optical and radio bands, with the disk lagging behindthe jet by $250 \pm 42$ days. We discuss the possible explanation for this,speculating that the observed disk and the jet flux changes are generated bymagnetic fluctuations originating within the innermost parts of a truncateddisk, and that the lag is related to a delayed radiative response of the diskwhen compared with the propagation timescale of magnetic perturbations alongrelativistic outflow. This scenario is supported by the re-analysis of theNuSTAR data, modelled in terms of a relativistic reflection from the diskilluminated by the coronal emission, which returns the inner disk radius$R_{\rm in}/R_{\rm ISCO} =35^{+40}_{-16}$. We discuss the global energetics inthe system, arguing that while the accretion proceeds at the Eddington rate,with the accretion-related bolometric luminosity $L_{\rm bol} \sim 9 \times10^{46}$ erg s$^{-1}$ $\sim 0.2 L_{\rm Edd}$, the jet total kinetic energy$L_\textrm{j} \sim 4 \times 10^{44}$ erg s$^{-1}$, inferred from the dynamicalmodelling of the giant radio lobes in the source, constitutes only a smallfraction of the available accretion power.

Signatures of the disk-jet coupling in the Broad-line Radio Quasar 4C+74.26