Extreme relativistic reflection in the active galaxy ESO 033-G002. Issue 2 (19th July 2021)

• Record Type: Journal Article
• Authors: Walton, D J; Baloković, M; Fabian, A C; Gallo, L C; Koss, M; Nardini, E; Reynolds, C S; Ricci, C; Stern, D; Alston, W N; Dauser, T; García, J A; Kosec, P; Reynolds, M T; Harrison, F A; Miller, J M
• Is Part Of: Monthly notices of the Royal Astronomical Society. Volume 506:Issue 2(2021)
• Page Start: 1557
• Page End: 1572
• Publication Date: 2021-07-19
• Subjects: black hole physics -- galaxies: active -- X-rays: individual: ESO 033-G002; Astronomy -- Periodicals; Periodicals; 520.5
• DOI: 10.1093/mnras/stab1290
• Languages: English
• ISSNs: 0035-8711

Abstract

ABSTRACT: We present the first high signal-to-noise broad-band X-ray spectrum of the radio-quiet type-2 Seyfert ESO 033-G002, combining data from XMM–Newton and NuSTAR . The nuclear X-ray spectrum is complex, showing evidence for both neutral and ionized absorption, as well as reflection from both the accretion disc and more distant material, but our broad-band coverage allows us to disentangle all of these different components. The total neutral column during this epoch is N H ∼ (5−6) × 10 22 $\rm \, cm^{-2}$, consistent with the optical classification of ESO 033-G002 as a type-2 Seyfert but not so large as to prevent us from robustly determining the properties of the innermost accretion flow. The ionized absorption – dominated by lines from Fe xxv and Fe xxvi – reveals a moderately rapid outflow ( v out ∼ 5400 $\rm \, km~s^{-1}$ ) which has a column comparable to the neutral absorption. We find the disc reflection from the innermost regions to be extreme, with a reflection fraction of R frac ∼ 5. This requires strong gravitational lightbending and, in turn, both an extremely compact corona (within ∼2 R G of the black hole) and a rapidly rotating black hole ( a * > 0.96). Despite this tight size constraint, with a temperature of kT e = 40–70 keV the X-ray corona in ESO 033-G002 appears similar to other active galactic nucle in terms of its placement in the compactness–temperature plane, consistent with sitting close to the limit determined by runaway pair production. Finally, combining X-ray spectroscopy, timing, and updated optical spectroscopy, we also estimate the mass of the black hole to be log[ M BH /M⊙ ] ∼ 7.0–7.5.