Ejection–accretion connection in NLS1 AGN 1H 1934-063
Accretion and ejection of matter in active galactic nuclei (AGNs) 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–Newton 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 ∼6 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, ν_(UFO) ~ -0.075 c) with a mild ionization state (log ξ/erg cm s⁻¹) ~ 1.6). 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 ∼ −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.
Additional Information© 2022 The Author(s). Published by Oxford University Press on behalf of Royal Astronomical Society. This article is published and distributed under the terms of the Oxford University Press, Standard Journals Publication Model (https://academic.oup.com/journals/pages/open_access/funder_policies/chorus/standard_publication_model). Accepted 2022 April 12. Received 2022 April 6; in original form 2022 March 4. EK acknowledges support from NASA ADAP grant no. 80NSSC17K0515. JAG acknowledges support from NASA ATP grant no. 80NSSC20K0540 and from the Alexander von Humboldt Foundation. WNA is supported by an ESA research fellowship. DATA AVAILABILITY. The XMM–Newton and NuSTAR data underlying this article are available in ESA's XMM–Newton Science Archive (https://www.cosmos.esa.int/web/xmm-newton/xsa) and HEASARC NuSTAR Archive, respectively.
Published - stac1058.pdf
Accepted Version - 2204.06075.pdf