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

التفاصيل البيبلوغرافية
العنوان:	A new powerful and highly variable disc wind in an AGN–star-forming galaxy, the case of MCG-03-58-007.
المؤلفون:	Braito, V, Reeves, J N, Matzeu, G A, Severgnini, P, Ballo, L, Caccianiga, A, Campana, S, Cicone, C, Della Ceca, R, Turner, T J
المصدر:	Monthly Notices of the Royal Astronomical Society; 9/21/2018, Vol. 479 Issue 3, p3592-3603, 12p
مصطلحات موضوعية:	SEYFERT galaxies, GALAXIES, ACTIVE galactic nuclei, GALACTIC evolution, ASTRONOMICAL observations
مستخلص:	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 ∼10²³ 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 × 10²³ 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 × 10²⁴ 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. [ABSTRACT FROM AUTHOR]
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قاعدة البيانات:	Complementary Index

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