Evidence for a clumpy disc-wind in the star forming Seyfert\,2 galaxy MCG--03--58--007

We report the results of a detailed analysis of a deep simultaneous $130,\rm ks\textit{XMM-Newton & NuSTAR} observation of the nearby (z=0.0315$) and bright ($L_{\mathrm{b}\mathrm{o}\mathrm{l}}\sim 3\times {10}^{45}\mathrm{e}\mathrm{r}\mathrm{g}{\mathrm{s}}^{-1}$) starburst-AGN Seyfert,2 system: MCG–03–58–007. From the broadband fitting we show that most of the obscuration needs to be modeled with a toroidal type reprocessor such as $\mathtt{\text{MYTorus}}$ \citep{MurphyYaqoob09}. Nonetheless the signature of a powerful disc-wind is still apparent at higher energies and the observed rapid short-term X-ray spectral variability is more likely caused by a variable zone of highly ionized fast wind rather than by a neutral clumpy medium. We also detect X-ray emission from larger scale gas as seen from the presence of several soft narrow emission lines in the RGS, originating from a contribution of a weak star forming activity together with a dominant photoionized component from the AGN.