2018/12/07 by Javier A. Garcia, Javier A. García, Erin Kara +25 · 99 citations
Physics and Astronomy · #Absorption edge #Accretion (finance) #Active galactic nucleus #Astrophysical Phenomena and Observations #Astrophysics #Astrophysics and Cosmic Phenomena #Black hole (networking) #Corona (planetary geology) #Electron #Galaxies: Formation, Evolution, Phenomena #Galaxy #Ion #Ionization #Nuclear physics #Photoionization #Physics #Quantum mechanics #Reflection (computer programming) #astro-ph.HE
paper · pdf · doi:10.3847/1538-4357/aaf739
published in The Astrophysical Journal 871(1), 88 (IOP Publishing) · Accepted for publication in ApJ, 18 pages, 7 figures
arxiv created 2018/12/07 · openalex publication_date 2019/01/20 · arxiv updated 2019/03/13 · openalex created_date 2020/11/23 · openalex updated_date 2026/07/22
Abstract We present the analysis of the first Nuclear Spectroscopic Telescope Array observations (∼220 ks), simultaneous with the last Suzaku observations (∼50 ks), of the active galactic nucleus of the bright Seyfert 1 galaxy Mrk 509. The time-averaged spectrum in the 1–79 keV X-ray band is dominated by a power-law continuum (Γ ∼ 1.8–1.9), a strong soft excess around 1 keV, and signatures of X-ray reflection in the form of Fe K emission (∼6.4 keV), an Fe K absorption edge (∼7.1 keV), and a Compton hump due to electron scattering (∼20–30 keV). We show that these data can be described by two very different prescriptions for the soft excess: a warm ( kT ∼ 0.5–1 keV) and optically thick ( τ ∼ 10–20) Comptonizing corona or a relativistically blurred ionized reflection spectrum from the inner regions of the accretion disk. While these two scenarios cannot be distinguished based on their fit statistics, we argue that the parameters required by the warm corona model are physically incompatible with the conditions of standard coronae. Detailed photoionization calculations show that even in the most favorable conditions, the warm corona should produce strong absorption in the observed spectrum. On the other hand, while the relativistic reflection model provides a satisfactory description of the data, it also requires extreme parameters, such as maximum black hole spin, a very low and compact hot corona, and a very high density for the inner accretion disk. Deeper observations of this source are thus necessary to confirm the presence of relativistic reflection and further understand the nature of its soft excess.