Cookies

We use cookies to ensure that we give you the best experience on our website. By continuing to browse this repository, you give consent for essential cookies to be used. You can read more about our Privacy and Cookie Policy.


Durham Research Online
You are in:

The weak Fe fluorescence line and long-term X-ray evolution of the Compton-thick active galactic nucleus in NGC 7674.

Gandhi, P. and Annuar, A. and Lansbury, G. B. and Stern, D. and Alexander, D. M. and Bauer, F. E. and Bianchi, S. and Boggs, S. E. and Boorman, P. G. and Brandt, W. N. and Brightman, M. and Christensen, F. E. and Comastri, A. and Craig, W. W. and Del Moro, A. and Elvis, M. and Guainazzi, M. and Hailey, C. J. and Harrison, F. A. and Koss, M. and Lamperti, I. and Malaguti, G. and Masini, A. and Matt, G. and Puccetti, S. and Ricci, C. and Rivers, E. and Walton, D. J. and Zhang, W. W. (2017) 'The weak Fe fluorescence line and long-term X-ray evolution of the Compton-thick active galactic nucleus in NGC 7674.', Monthly notices of the Royal Astronomical Society., 467 (4). pp. 4606-4621.

Abstract

We present NuSTAR X-ray observations of the active galactic nucleus (AGN) in NGC 7674. The source shows a flat X-ray spectrum, suggesting that it is obscured by Compton-thick gas columns. Based upon long-term flux dimming, previous work suggested the alternate possibility that the source is a recently switched-off AGN with the observed X-rays being the lagged echo from the torus. Our high-quality data show the source to be reflection-dominated in hard X-rays, but with a relatively weak neutral Fe Kα emission line (equivalent width [EW] of ≈ 0.4 keV) and a strong Fe xxvi ionized line (EW ≈ 0.2 keV). We construct an updated long-term X-ray light curve of NGC 7674 and find that the observed 2–10 keV flux has remained constant for the past ≈ 20 yr, following a high-flux state probed by Ginga. Light travel time arguments constrain the minimum radius of the reflector to be ∼ 3.2 pc under the switched-off AGN scenario, ≈ 30 times larger than the expected dust sublimation radius, rendering this possibility unlikely. A patchy Compton-thick AGN (CTAGN) solution is plausible, requiring a minimum line-of-sight column density (NH) of 3 × 1024 cm−2 at present, and yields an intrinsic 2–10 keV luminosity of (3–5) × 1043 erg s−1. Realistic uncertainties span the range of ≈ (1–13) × 1043 erg s−1. The source has one of the weakest fluorescence lines amongst bona fide CTAGN, and is potentially a local analogue of bolometrically luminous systems showing complex neutral and ionized Fe emission. It exemplifies the difficulty of identification and proper characterization of distant CTAGN based on the strength of the neutral Fe Kα line.

Item Type:Article
Full text:(VoR) Version of Record
First Live Deposit - 22 June 2017
Download PDF
(1265Kb)
Status:Peer-reviewed
Publisher Web site:https://doi.org/10.1093/mnras/stx357
Publisher statement:This article has been accepted for publication in Monthly Notices of the Royal Astronomical Society ©: 2017 The Authors Published by Oxford University Press on behalf of the Royal Astronomical Society. All rights reserved.
Record Created:22 Jun 2017 10:13
Last Modified:29 Aug 2018 16:29

Social bookmarking: del.icio.usConnoteaBibSonomyCiteULikeFacebookTwitterExport: EndNote, Zotero | BibTex
Look up in GoogleScholar | Find in a UK Library