Soft excess in AGN with relativistic X-ray reflection

The soft X-ray excess, emission below & SIM;$$ \sim $$2 keV over the X-ray power-law, is a marked spectral component in the X-ray spectra of many Seyfert 1 galaxies. We investigate if the observed soft X-ray excess in a sample of Seyfert 1s is in accordance with the prediction of the relativistic reflection model by analyzing the XMM-Newton and NuSTAR spectra. The fractional difference in the soft excess (SE) obtained from the blurred reflection emission predicted (from NuSTAR) and the observed (from XMM-Newton) luminosities show that the reflection model underestimates the SE emission in our sample. The results point to alternative models (for example, warm Comptonization) to explain the soft X-ray excess in AGN.