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

## TL;DR

This study analyzes a deep X-ray observation of the Seyfert 2 galaxy MCG--03--58--007, revealing a clumpy disc-wind structure and variable ionized wind, with implications for understanding AGN obscuration and outflows.

## Contribution

It provides the first detailed evidence for a clumpy disc-wind in a Seyfert 2 galaxy using broadband X-ray data and spectral variability analysis.

## Key findings

- Detection of a variable, highly ionized fast wind.
- Evidence for a clumpy, toroidal obscurer modeled by MYTorus.
- Identification of soft emission lines from star formation and photoionized gas.

## Abstract

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 ($L_{\rm bol}\sim3\times10^{45}\,\rm erg\,s^{-1}$) 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 \texttt{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.