A new powerful and highly variable disc wind in an AGN–star-forming galaxy, the case of MCG-03-58-007. Issue 3 (28th June 2018)

• Record Type: Journal Article
• Authors: Braito, V; Reeves, J N; Matzeu, G A; Severgnini, P; Ballo, L; Caccianiga, A; Campana, S; Cicone, C; Della Ceca, R; Turner, T J
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 479:Issue 3(2018)
• Page Start: 3592
• Page End: 3603
• Publication Date: 2018-06-28
• Subjects: galaxies: active -- galaxies: individual: MCG-03-58-007 -- X-rays: galaxies; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/sty1697
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: 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 ∼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 ξ/erg cm s −1 ∼5.5) and high column density ( N H ∼ 5–8 × 10 23 cm −2 ) outflowing absorbers with v out1 ∼ −0.1 c and v out2 ∼ −0.2 c . 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 ∼ −0.35 c ) component of the wind is also seen in this second observation. During this observation we also witnessed an occultation event lasting Δ t ∼ 120 ks, which we ascribe to an increase of the opacity of the disc wind (Δ N H ∼ 1.4 × 10 24 cm −2 ). Our interpretation is that the slow zone ( v out ∼ −0.1 c ) 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.