A comprehensive view of PKS 2155-304 from 2008 to 2023 through a multi-epoch modeling of its spectral energy distributions

We investigate the temporal and spectral evolution of the blazar PKS 2155-304 using γ-ray, X-ray, optical/UV, and infrared data from the Markarian Multiwavelength Data Center. We constructed multi-band light curves and time-resolved spectral energy distributions (SEDs) to probe the origin of its emission. The light curves show strong variability, with the largest amplitudes in the soft–medium X-rays and notable variations also in the γ-ray band. Based on the γ-ray light curve we defined 253 epochs and categorized them into quiescent states (QS), multiwavelength flares (MWF), γ-ray flares (γF), X-ray flares (XF), and optical/UV flares (OUF). Each SED is modeled within a one-zone synchrotron self-Compton (SSC) framework using a neural-network surrogate for fast parameter inference. Kolmogorov–Smirnov tests reveal state-dependent parameter variations relative to QS: (i) during MWF, the magnetic field B, electron luminosity Le, maximum electron Lorentz factor γmax, and Doppler factor δ differ significantly; (ii) during γF, a harder electron index p is estimated; (iii) XF shows higher B and γmax with a more compact emitting region; and (IV) during OUF, changes in B, Le, γmax, δ, and p are found while the emitting-zone size remains approximately constant. The jet power is electron-dominated (magnetic-to-electron power ratio ηB ≃ 0.09–0.17, subject to uncertainties introduced by the assumption γmin = 100), with ηB rising during XF. These results suggest that variations in acceleration efficiency and magnetization drive band-dependent flaring in PKS 2155-304.