The Emergence of X-Ray Emission Lines during Relativistic Radio-jet Formation in the Changing-look Active Galactic Nucleus 1ES 1927+654

Abstract We present results from a comprehensive multiwavelength monitoring campaign of the changing-look active galactic nucleus 1ES 1927+654 during the onset and evolution of a relativistic radio jet ∼(2022 May–2025 August), using observations from XMM-Newton, Swift, Telescopio Nazionale Galileo (TNG), the Zwicky Transient Facility (ZTF), Very Large Array (VLA), and Very Long Baseline Array (VLBA). The soft X-ray emission lines at ∼0.56 keV and ∼1 keV have appeared with variable strength and width during the formation of the nascent jet. We note that the ∼1 keV feature has been persisting since the post-2017 flare phase. We also report the detection of a broad (∼800 eV) FeK emission feature at (6–7) keV in the ∼70 ks stacked EPIC-pn spectra, marking the first such detection, which historically was lacking in this source. The joint spectral fitting of XMM-Newton EPIC-pn and Reflection Grating Spectrometer (RGS) data reveals the presence of ionized absorbers in 2022 ( log ξ / erg cm s − 1 ∼ 1.5 ± 0.3 , N H ∼ 2.5 ± 0.9 × 10 20 cm −2 ), but weaker than that detected during the high accretion state in 2018 (Eddington ratio, λ Edd > 1). The absorption features further weakened in 2023–2025 and were marginally detectable ( N H ≤ 10 20 cm −2 ). The entire scenario is suggestive of a real-time transition of the accretion flow (from λ Edd > 1 to λ Edd ∼ 0.3) during which the winds become weaker and the jet starts to form and evolve. Furthermore, both the soft X-ray (0.3–2) keV and 5 GHz radio fluxes, which increased by factors of ∼10 and ∼60, respectively, since 2022, have recently plateaued at elevated levels, indicating a stabilized accretion disk, corona, and jet configuration.

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Journal
The Astrophysical Journal
Published
2026-10-29
DOI
https://doi.org/10.3847/1538-4357/ae96b4
Primary Topic
Astrophysical Phenomena and Observations
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article
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article

The Emergence of X-Ray Emission Lines during Relativistic Radio-jet Formation in the Changing-look Active Galactic Nucleus 1ES 1927+654

Ehud Behar, Erin Kara, F. Panessa, Luigi Gallo et al.
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The Astrophysical Journal
Astrophysical Phenomena and Observations
article

The Emergence of X-Ray Emission Lines during Relativistic Radio-jet Formation in the Changing-look Active Galactic Nucleus 1ES 1927+654

Ehud Behar, Erin Kara, F. Panessa, Luigi Gallo, Eileen T. Meyer, Cláudio Ricci, Amelia Hankla, Fabio Pacucci, Missagh Mehdipour, T. R. Kallman, Fabio La Franca, Onic I. Shuvo, James N. Reeves, Mitchell C. Begelman, Main Pal, M. Guainazzi, Megan Masterson, Ralf Ballhausen, Dev R. Sadaula, Suvendu Rakshit, S. Bianchi, Rostom Mbarek, S. B. Cenko, Tahir Yaqoob, Ilaria Villani, Federica Ricci, Ritesh Ghosh, Sibasish Laha, Alexander Philippov, Javier A Garcia
article en

Abstract

Abstract We present results from a comprehensive multiwavelength monitoring campaign of the changing-look active galactic nucleus 1ES 1927+654 during the onset and evolution of a relativistic radio jet ∼(2022 May–2025 August), using observations from XMM-Newton, Swift, Telescopio Nazionale Galileo (TNG), the Zwicky Transient Facility (ZTF), Very Large Array (VLA), and Very Long Baseline Array (VLBA). The soft X-ray emission lines at ∼0.56 keV and ∼1 keV have appeared with variable strength and width during the formation of the nascent jet. We note that the ∼1 keV feature has been persisting since the post-2017 flare phase. We also report the detection of a broad (∼800 eV) FeK emission feature at (6–7) keV in the ∼70 ks stacked EPIC-pn spectra, marking the first such detection, which historically was lacking in this source. The joint spectral fitting of XMM-Newton EPIC-pn and Reflection Grating Spectrometer (RGS) data reveals the presence of ionized absorbers in 2022 ( log ξ / erg cm s − 1 ∼ 1.5 ± 0.3 , N H ∼ 2.5 ± 0.9 × 10 20 cm −2 ), but weaker than that detected during the high accretion state in 2018 (Eddington ratio, λ Edd > 1). The absorption features further weakened in 2023–2025 and were marginally detectable ( N H ≤ 10 20 cm −2 ). The entire scenario is suggestive of a real-time transition of the accretion flow (from λ Edd > 1 to λ Edd ∼ 0.3) during which the winds become weaker and the jet starts to form and evolve. Furthermore, both the soft X-ray (0.3–2) keV and 5 GHz radio fluxes, which increased by factors of ∼10 and ∼60, respectively, since 2022, have recently plateaued at elevated levels, indicating a stabilized accretion disk, corona, and jet configuration.

The Astrophysical JournalVol. 1011(1)
University of Delhi (IN), Roma Tre University (IT), Space Telescope Science Institute (US), National Institute of Standards and Technology (US), Harvard University (US), Princeton University (US), Peking University (CN), University of Michigan (US), Astronomical Observatory of Rome (IT), European Space Agency (FR), Aryabhatta Research Institute of Observational Sciences (IN), Institute for Space Astrophysics and Planetology (IT), Center for Astrophysics Harvard & Smithsonian (US), Massachusetts Institute of Technology (US), Saint Mary's University (CA), University of Maryland, College Park (US), University of Maryland, Baltimore County (US), Catholic University of America (US), National Institute for Astrophysics (IT)
National Science Foundation, National Aeronautics and Space Administration, United States-Israel Binational Science Foundation, Goddard Space Flight Center
Openalex Percentile: Top 49%
Astrophysical Phenomena and Observations
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