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X-CIGALE, built upon the spectral energy distribution (SED) code of CIGALE,implements important new features: The code accounts for obscuring material inthe polars of the AGN and has the ability to fit X-ray fluxes. In this work, weuse ~2500 spectroscopic, X-ray AGN from the XMM-XXL-North field and examine theimprovements the new features bring in the SED modelling analysis. Based on ourresults, X-CIGALE successfully connects the X-ray with the UV luminosity in thewhole range spanned by our sample (log Lx(2-10 keV) = (42 - 46) erg/s). Theaddition of the new features globally improves the efficiency of X-CIGALE inthe estimation and characterization of the AGN component. The classificationinto type 1 and type 2 based on their inclination angle is improved, especiallyat 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-) IRphotometry is available in the SED fitting process. The addition of polar dustincreases the AGN fraction and the efficiency of the SED decomposition todetect 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-raydetected AGN not selected by IR colour criteria. The latter drops to ~50% whenpolar dust is not included. The ability of X-CIGALE to include X-rayinformation in the SED fitting process can be instrumental in the optimalexploitation of the wealth of data that current (eROSITA) and future (ATHENA)missions will provide us.

X-ray flux in the SED modelling: An application of X-CIGALE in the XMM-XXL field