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The UV to X-ray continuum of active galactic nuclei (AGN) is important formaintaining the ionisation and thermal balance of the warm absorbers (WAs).However, the spectra in the sensitive energy range $\sim \,13.6 -300 \ev$ areunobservable due to Galactic extinction. Moreover, many AGN show soft X-rayexcess emission of varying strength in the $0.1-2\kev$ band whose origin isstill highly debated. This soft-excess connects to the UV bump in theunobserved region of $13.6 -300 \ev$. Here we investigate the effect of theassumed physical model for the soft-excess on the flux of the unobserved partof the spectrum and its effect on the WA properties. We perform a case studyusing the \xmm{} observations of the bright Seyfert 1 galaxy IRAS 13349+2438with WA features. The two different physical models for the soft excess:blurred Compton reflection from an ionised disk, and, optically thick thermalComptonisation of the disk photons, predict different fluxes in the unobservedenergy range. However the current X-ray data quality does not allow us todistinguish between them using derived WA parameters. This, in turn, impliesthat it is difficult to determine the origin of the soft-excess emission usingthe warm absorber features.

The effect of UV/Soft X-ray excess emission on the warm absorber properties of Active Galactic Nuclei -- A case study of IRAS 13349+2438