tokens: to the Jet Power for Multiple-Zone Modeling of the Multiwavelength Data of Quiescent-State Emission from AP Librae The contributions of disk, broadline region (BLR), and torus radiation to the IC emission by the blob and pc-scale jet of AP Librae are considered in earlier papers. The energy of the BLR photons is blueshifted in the rest frame of the blob. The reprocessed BLR emission has been parameterized in Equation (12) of Hervet et al. ( 2015 ). The parameter values presented in Table 3 of Hervet et al. ( 2015 ) have been chosen such that at HE, the EC emission of blob-BLR origin is significant. A similar discussion is given in Zacharias Wagner ( 2016 ). Direct emissions from the disk, BLR, and torus are low as they are not detected, however, EC emission from the blob due to the reprocessed emission could be significant (depending on the parameter values chosen and the distances of the blob and jet from the black hole) after Doppler boosting. Moreover, it is discussed that, due to the outward relativistic motion of the blob and its distance from the accretion disk, the EC emission of blob electrons due to disk radiation is negligible. From Equation (A.6) of Zacharias Wagner ( 2016 ), the energy density of reprocessed emission from the dusty torus in the reference frame of the blob is . Assuming the radius of the region within which the emission is confined to be r DT = 1 pc, luminosity L DT = 10 42 erg s −1 , the Lorentz factor of the blob Γ = 7, the efficiency of reprocessing τ DT = 0.001, and the energy density in radiation u DT = 2 × 10 −8 erg cm −3 , which is much lower than the synchrotron photon energy density inside the blob, 1.28 × 10 −5 erg cm −3 . By adjusting the parameter values suitably, the energy density in reprocessed external radiation could be made even lower. Moreover, the pc jet is assumed to be located beyond the BLR and torus region, which makes EC emission insignificant. 3. Results and Discussions As shown in Figures 2 – 4 , the observed quiescent-state SED of AP Librae has been fitted by the three-zone model adopted in the present work. The optical–UV frequency data in the SED are accounted for partially by the synchrotron emission of electrons from the blob and partially by the blackbody radiation from the accretion disk. The thermal emission from the accretion disk is reproduced by assuming a Shakura–Sunyaev type disk (Shakura Sunyaev 1973 ) with a luminosity of L D = 1.3 × 10 44 erg s −1 . Incidentally, Zacharias Wagner ( 2016 ) used the same estimate for disk luminosity,The jet power requirements from each region are calculated from the expression of P jet presented in Equation ( 11 ). For the parameters used in our model, we find that the required jet power in Zone-1 is 5.7 × 10 47 erg s −1 and in Zone-2 is 3.75 × 10 47 erg s −1 . The jet power requirement in Zone-3 is 4.86 × 10 48 erg s −1 . Assuming a simple power-law proton spectrum of spectral index 2 in the energy range of 10 15 –10 18 eV, we have
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