The Close AGN Reference Survey (CARS). Long-term spectral variability study of the changing look AGN Mrk 1018

TL;DR

This study investigates the long-term spectral variability of the changing-look AGN Mrk 1018, revealing how its accretion flow and circumnuclear gas evolve during a transition from a bright to a faint state, with multi-wavelength analysis and physical modeling.

Contribution

It provides a detailed multi-wavelength spectral variability analysis of Mrk 1018, modeling its accretion flow transition and circumnuclear gas evolution during a changing-look event.

Findings

UV and hard X-ray flux decreased by factors of 24 and 8 respectively.

Soft X-ray excess faded and was not detected by 2021.

Fe Kalpha line flux dropped by half the continuum's decline.

Abstract

Changing-look AGNs (CLAGN) are accreting supermassive black hole systems that undergo variations in optical spectral type, driven by major changes in accretion rate. Mrk 1018 has undergone two transitions, a brightening event in the 1980s and a transition back to a faint state over the course of 2-3 years in the early 2010s. We characterize the evolving physical properties of the source's inner accretion flow, particularly during the bright-to-faint transition, as well as the morphological properties of its parsec-scale circumnuclear gas. We model archival X-ray spectra from XMM-Newton, Chandra, Suzaku, and Swift, using physically-motivated models to characterize X-ray spectral variations and track Fe Kalpha line flux. We also quantify Mrk 1018's long-term multi-wavelength spectral variability from optical/UV to the X-rays. Over the duration of the bright-to-faint transition, the UV and hard X-ray flux fell by differing factors, roughly 24 and 8, respectively. The soft X-ray excess faded, and was not detected by 2021. In the faint state, when the Eddington ratio drops to log Lbol/LEdd < -1.7, the hot X-ray corona photon index shows a 'softer-when-fainter' trend, similar to that seen in some black hole X-ray binaries and samples of low-luminosity AGNs. Finally, the Fe Kalpha line flux has dropped by only half the factor of the drop in the X-ray continuum. The transition from the bright state to the faint state is consistent with the inner accretion flow transitioning from a geometrically-thin disk to an ADAF-dominated state, with the warm corona disintegrating or becoming energetically negligible, while the X-ray-emitting hot flow becoming energetically dominant. Meanwhile, narrow Fe Kalpha emission has not yet fully responded to the drop in its driving continuum, likely because its emitter extends up to roughly 10 pc.