A new powerful and highly variable disc wind in an AGN-star-forming galaxy, the case of MCG-03-58-007

We present the discovery of a new candidate for a fast disc wind, in the nearby Seyfert 2 galaxy MCG-03-58-007. This wind is discovered in a deep Suzaku observation that was performed in 2010. Overall the X-ray spectrum of MCG-03-58-007 is highly absorbed by a neutral column density of N-H similar to 10(23) cm(-2), in agreement with the optical classification as a type 2 active galactic nucleus. In addition, this observation unveiled the presence of two deep absorption troughs at E = 7.4 +/- 0.1 and 8.5 +/- 0.2 keV. If associated with blueshifted Fe XXVI, these features can be explained with the presence of two highly ionized (log xi/erg cm s(-1) similar to 5.5) and high column density (N-H similar to 5-8 x 10(23) cm(-2)) outflowing absorbers with v(out1) similar to -0.1c and v(out2) similar to -0.2c. The disc wind detected during this observation is most likely launched from within a few hundreds gravitational radii from the central black and has a kinetic output that matches the prescription for significant feedback. The presence of the lower velocity component of the disc wind is independently confirmed by the analysis of a follow-up XMM-Newton and NuSTAR observation. A faster (v(out) similar to-0.35c) component of the wind is also seen in this second observation. During this observation we also witnessed an occultation event lasting Delta t similar to 120 ks, which we ascribe to an increase of the opacity of the disc wind (Delta N-H similar to 1.4 x 10(24) cm(-2)). Our interpretation is that the slow zone (v(out) similar to -0.1c) of the wind is the most stable but inhomogeneous component, while the faster zones could be associated with two different inner streamlines of the wind.