Ejection-accretion connection in NLS1 AGN 1H 1934-063

TL;DR

This study analyzes high-resolution X-ray spectra of NLS1 AGN 1H 1934-063, revealing a stable ultra-fast outflow and variable warm absorber, and suggests a possible connection between accretion disk reprocessing and ejection mechanisms.

Contribution

It provides the first detailed spectral analysis linking outflows and reprocessing features in NLS1 AGN, proposing a new scenario for the origin of certain emission lines.

Findings

Detection of a stable ultra-fast outflow at ~0.075c

Identification of a potentially variable warm absorber

Proposed model of blueshifted reflection explaining emission lines

Abstract

Accretion and ejection of matter in active galactic nuclei (AGN) are tightly connected phenomena and represent fundamental mechanisms regulating the growth of the central supermassive black hole and the evolution of the host galaxy. However, the exact physical processes involved are not yet fully understood. We present a high-resolution spectral analysis of a simultaneous \xmm\ and \nustar\ observation of the narrow line Seyfert 1 (NLS1) AGN 1H 1934-063, during which the X-ray flux dropped by a factor of $\sim6$ and subsequently recovered within 140 kiloseconds. By means of the time-resolved and flux-resolved X-ray spectroscopy, we discover a potentially variable warm absorber and a relatively stable ultra-fast outflow (UFO, $v_\mathrm{UFO}\sim-0.075\,c$) with a mild ionization state ($\log(\xi/\mathrm{erg\,cm\,s^{-1})}\sim1.6$). The detected emission lines (especially a strong and broad feature around 1\,keV) are of unknown origin and cannot be explained with emission from plasmas in photo- or collisional-ionization equilibrium. Such emission lines could be well described by a strongly blueshifted ($z\sim-0.3$) secondary reflection off the base of the equatorial outflows, which may reveal the link between the reprocessing of the inner accretion flow photons and the ejection. However, this scenario although being very promising is only tentative and will be tested with future observations.