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We analyse the spectra of the archival XMM-Newton data of the Seyfert 1 AGNZw 229.015 in the energy range $0.3 - 10.0$ keV. When fitted with a simplepower-law, the spectrum shows signatures of weak soft excess below 1.0 keV. Wefind that both thermal comptonisation and relativistically blurred reflectionmodels provide the most acceptable spectral fits with plausible physicalexplanations to the origin of the soft excess than do multicolour discblackbody and smeared wind absorption models. This motivated us to study thevariability properties of the soft and the hard X-ray emissions from the sourceand the relationship between them to put further constraints on the abovemodels. Our analysis reveals that the variation in the $3.0 - 10.0$ keV bandlags that in the $0.3 - 1.0$ keV by $600^{+290}_{-280}$ s, while the lagbetween the $1.0 - 10.0$ keV and $0.3 - 1.0$ keV is $980^{+500}_{-500}$ s. Thisimplies that the X-ray emissions are possibly emanating from different regionswithin the system. From these values, we estimate the X-ray emission region tobe within $20R_g$ of the central supermassive black hole (where $R_g=GM/c^2$,$M$ is the mass of black hole, $G$ the Newton gravitational constant and $c$the speed of light). Furthermore, we use XMM-Newton and Kepler photometriclightcurves of the source to search for possible nonlinear signature in theflux variability. We find evidence that the variability in the system may bedominated by stochasticity rather than deterministic chaos which hasimplications for the dynamics of the accretion system.

Spectral and Time Series Analyses of the Seyfert 1 AGN: Zw 229.015