  X-CIGALE, built upon the spectral energy distribution (SED) code of CIGALE,
implements important new features: The code accounts for obscuring material in
the polars of the AGN and has the ability to fit X-ray fluxes. In this work, we
use ~2500 spectroscopic, X-ray AGN from the XMM-XXL-North field and examine the
improvements the new features bring in the SED modelling analysis. Based on our
results, X-CIGALE successfully connects the X-ray with the UV luminosity in the
whole range spanned by our sample (log Lx(2-10 keV) = (42 - 46) erg/s). The
addition of the new features globally improves the efficiency of X-CIGALE in
the estimation and characterization of the AGN component. The classification
into type 1 and type 2 based on their inclination angle is improved, especially
at redshifts lower than 1. The statistical significance of the AGN fraction,
fracAGN, measurements is increased, in particular for luminous X-ray sources
(log LX > 45 erg/s). These conclusions hold under the condition that (mid-) IR
photometry is available in the SED fitting process. The addition of polar dust
increases the AGN fraction and the efficiency of the SED decomposition to
detect AGN among X-ray selected sources. X-CIGALE estimates a strong AGN
(fracAGN > 0.3) in more than 90% of the infrared selected AGN and 75% of X-ray
detected AGN not selected by IR colour criteria. The latter drops to ~50% when
polar dust is not included. The ability of X-CIGALE to include X-ray
information in the SED fitting process can be instrumental in the optimal
exploitation of the wealth of data that current (eROSITA) and future (ATHENA)
missions will provide us.

High Energy Astrophysical Phenomena;Cosmology and Nongalactic Astrophysics