Notes. Column [2]: dissipation radius in units of 10¹⁵ cm and (in parenthesis) in units of Schwarzschild radii; Col. [3]: power injected in the blob calculated in the comoving frame, in units of 10⁴⁵ erg s^-1; Col. [4]: magnetic field in Gauss; Col. [5]: bulk Lorentz factor at R_diss; Cols. [6] and [7]: break and maximum random Lorentz factors of the injected electrons; Cols. [8], [9]: slopes of the injected electron distribution [Q(γ)] below and above γ_b. Cols. [10]–[13]: logarithm of the jet power in the form of radiation (P_r), Poynting flux (P_B, bulk motion of electrons (P_e and protons (P_p, assuming one proton per emitting electron). Powers are in erg s^-1. The black hole mass is assumed to be M = 3 × 10⁸M_⊙. The disk luminosity is assumed to be always the same and equal to L_d = 5.9 × 10⁴⁵ erg s^-1 (equivalent to 0.13 L_Edd. The radius of the broad line region is assumed to be R_BLR = 2.4 × 10¹⁷ cm. The total X-ray corona luminosity is assumed to be 30 per cent of L_d. Its spectral shape is assumed to be always ∝ν^-1exp(−hν/ 150 keV). The viewing angle θ_v is 3° for all states. The Doppler factor δ varies from 17.8 (when Γ = 13) to 18.81 (Γ = 16). The first four lines show the parameters for the Synchrotron – inverse Compton blazar model adopted (Ghisellini & Tavecchio 2009) to reproduce the radio-to-gamma-ray SEDs of Fig. 7. The last line shows the parameters used to reproduce the VHE emission of Mar 2009, quasi-simultaneous with lower frequency data (see Fig. 7c).