Multiwavelength monitoring and reverberation mapping of NGC 2617 at deepest minimum with a sharp upward turn during 2021-2024

V. L. Oknyansky; M. S. Brotherton; S. S. Tsygankov; A. V. Dodin; A. M. Tatarnikov; P. Du; M. A. Burlak; N. P. Ikonnikova; V. G. Metlov; A. A. Belinski; N. I. Shatsky; J. M. Wang; D. W. Bao; F. Fang; S. Zhai; Y. X. Fu; H. R. Bai; T. E. Zastrocky; D. Chelouche; C. Sobrino Figaredo; S. Kaspi; C. M. Gaskell

doi:10.1093/mnras/stae2707

Multiwavelength monitoring and reverberation mapping of NGC 2617 at deepest minimum with a sharp upward turn during 2021-2024

V. L. Oknyansky, M. S. Brotherton, S. S. Tsygankov, A. V. Dodin, A. M. Tatarnikov, P. Du, M. A. Burlak, N. P. Ikonnikova, V. G. Metlov, A. A. Belinski, N. I. Shatsky, J. M. Wang, D. W. Bao, F. Fang, S. Zhai, Y. X. Fu, H. R. Bai, T. E. Zastrocky, D. Chelouche, C. Sobrino FigaredoS. Kaspi, C. M. Gaskell

Department of Physics

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Abstract

We present the results of a new X-ray to near-IR photometric and spectroscopic monitoring of the changing look active galactic nucleus NGC 2617 carried out from March 2022 to March 2024. We found significant variability at all wavelengths and in the intensities and profiles of the broad Balmer lines. Reverberation mapping was carried out for three observing seasons during 2021-2024. We obtained time delays of 4 d for the response of the H line to optical continuum variations. The X-ray variations correlate well with the UV and optical, with a few days lag for longer wavelengths. The K band lagged the B band by 15 d during the last three seasons, which is significantly shorter than the delays reported previously by the 2016 and 2017-2019 campaigns. Near-IR variability arises from two different emission regions: the outer part of the accretion disc and a more distant dust component. The -band variability is governed primarily by dust. The H /H ratio variations (for broad components only) correlate with the X-ray and UV fluxes. The spectral type changed from type 1.8 to type 1.9 during 2023 October-2024 January and then a more rapid change to type 1.5 occurred in 2024 February. We interpret these changes as a combination of two factors: changes in the accretion rate as a dominant cause but also the sublimation or recovery of dust along the line of sight.

Original language	English
Pages (from-to)	2089-2102
Number of pages	14
Journal	Monthly Notices of the Royal Astronomical Society
Volume	536
Issue number	3
DOIs	https://doi.org/10.1093/mnras/stae2707
State	Published - 1 Jan 2025

Bibliographical note

Publisher Copyright:
© 2024 The Author(s).

Keywords

UV
X-rays: galaxies
galaxies: Seyfert
galaxies: active
galaxies: individual: NGC 2617
optical: galaxies

ASJC Scopus subject areas

Astronomy and Astrophysics
Space and Planetary Science

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10.1093/mnras/stae2707

Cite this

Oknyansky, V. L., Brotherton, M. S., Tsygankov, S. S., Dodin, A. V., Tatarnikov, A. M., Du, P., Burlak, M. A., Ikonnikova, N. P., Metlov, V. G., Belinski, A. A., Shatsky, N. I., Wang, J. M., Bao, D. W., Fang, F., Zhai, S., Fu, Y. X., Bai, H. R., Zastrocky, T. E., Chelouche, D., ... Gaskell, C. M. (2025). Multiwavelength monitoring and reverberation mapping of NGC 2617 at deepest minimum with a sharp upward turn during 2021-2024. Monthly Notices of the Royal Astronomical Society, 536(3), 2089-2102. https://doi.org/10.1093/mnras/stae2707

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title = "Multiwavelength monitoring and reverberation mapping of NGC 2617 at deepest minimum with a sharp upward turn during 2021-2024",

abstract = "We present the results of a new X-ray to near-IR photometric and spectroscopic monitoring of the changing look active galactic nucleus NGC 2617 carried out from March 2022 to March 2024. We found significant variability at all wavelengths and in the intensities and profiles of the broad Balmer lines. Reverberation mapping was carried out for three observing seasons during 2021-2024. We obtained time delays of 4 d for the response of the H line to optical continuum variations. The X-ray variations correlate well with the UV and optical, with a few days lag for longer wavelengths. The K band lagged the B band by 15 d during the last three seasons, which is significantly shorter than the delays reported previously by the 2016 and 2017-2019 campaigns. Near-IR variability arises from two different emission regions: the outer part of the accretion disc and a more distant dust component. The -band variability is governed primarily by dust. The H /H ratio variations (for broad components only) correlate with the X-ray and UV fluxes. The spectral type changed from type 1.8 to type 1.9 during 2023 October-2024 January and then a more rapid change to type 1.5 occurred in 2024 February. We interpret these changes as a combination of two factors: changes in the accretion rate as a dominant cause but also the sublimation or recovery of dust along the line of sight.",

keywords = "UV, X-rays: galaxies, galaxies: Seyfert, galaxies: active, galaxies: individual: NGC 2617, optical: galaxies",

author = "Oknyansky, {V. L.} and Brotherton, {M. S.} and Tsygankov, {S. S.} and Dodin, {A. V.} and Tatarnikov, {A. M.} and P. Du and Burlak, {M. A.} and Ikonnikova, {N. P.} and Metlov, {V. G.} and Belinski, {A. A.} and Shatsky, {N. I.} and Wang, {J. M.} and Bao, {D. W.} and F. Fang and S. Zhai and Fu, {Y. X.} and Bai, {H. R.} and Zastrocky, {T. E.} and D. Chelouche and Figaredo, {C. Sobrino} and S. Kaspi and Gaskell, {C. M.}",

note = "Publisher Copyright: {\textcopyright} 2024 The Author(s).",

year = "2025",

month = jan,

day = "1",

doi = "10.1093/mnras/stae2707",

language = "English",

volume = "536",

pages = "2089--2102",

journal = "Monthly Notices of the Royal Astronomical Society",

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Oknyansky, VL, Brotherton, MS, Tsygankov, SS, Dodin, AV, Tatarnikov, AM, Du, P, Burlak, MA, Ikonnikova, NP, Metlov, VG, Belinski, AA, Shatsky, NI, Wang, JM, Bao, DW, Fang, F, Zhai, S, Fu, YX, Bai, HR, Zastrocky, TE, Chelouche, D, Figaredo, CS, Kaspi, S & Gaskell, CM 2025, 'Multiwavelength monitoring and reverberation mapping of NGC 2617 at deepest minimum with a sharp upward turn during 2021-2024', Monthly Notices of the Royal Astronomical Society, vol. 536, no. 3, pp. 2089-2102. https://doi.org/10.1093/mnras/stae2707

TY - JOUR

T1 - Multiwavelength monitoring and reverberation mapping of NGC 2617 at deepest minimum with a sharp upward turn during 2021-2024

AU - Oknyansky, V. L.

AU - Brotherton, M. S.

AU - Tsygankov, S. S.

AU - Dodin, A. V.

AU - Tatarnikov, A. M.

AU - Du, P.

AU - Burlak, M. A.

AU - Ikonnikova, N. P.

AU - Metlov, V. G.

AU - Belinski, A. A.

AU - Shatsky, N. I.

AU - Wang, J. M.

AU - Bao, D. W.

AU - Fang, F.

AU - Zhai, S.

AU - Fu, Y. X.

AU - Bai, H. R.

AU - Zastrocky, T. E.

AU - Chelouche, D.

AU - Figaredo, C. Sobrino

AU - Kaspi, S.

AU - Gaskell, C. M.

PY - 2025/1/1

Y1 - 2025/1/1

N2 - We present the results of a new X-ray to near-IR photometric and spectroscopic monitoring of the changing look active galactic nucleus NGC 2617 carried out from March 2022 to March 2024. We found significant variability at all wavelengths and in the intensities and profiles of the broad Balmer lines. Reverberation mapping was carried out for three observing seasons during 2021-2024. We obtained time delays of 4 d for the response of the H line to optical continuum variations. The X-ray variations correlate well with the UV and optical, with a few days lag for longer wavelengths. The K band lagged the B band by 15 d during the last three seasons, which is significantly shorter than the delays reported previously by the 2016 and 2017-2019 campaigns. Near-IR variability arises from two different emission regions: the outer part of the accretion disc and a more distant dust component. The -band variability is governed primarily by dust. The H /H ratio variations (for broad components only) correlate with the X-ray and UV fluxes. The spectral type changed from type 1.8 to type 1.9 during 2023 October-2024 January and then a more rapid change to type 1.5 occurred in 2024 February. We interpret these changes as a combination of two factors: changes in the accretion rate as a dominant cause but also the sublimation or recovery of dust along the line of sight.

AB - We present the results of a new X-ray to near-IR photometric and spectroscopic monitoring of the changing look active galactic nucleus NGC 2617 carried out from March 2022 to March 2024. We found significant variability at all wavelengths and in the intensities and profiles of the broad Balmer lines. Reverberation mapping was carried out for three observing seasons during 2021-2024. We obtained time delays of 4 d for the response of the H line to optical continuum variations. The X-ray variations correlate well with the UV and optical, with a few days lag for longer wavelengths. The K band lagged the B band by 15 d during the last three seasons, which is significantly shorter than the delays reported previously by the 2016 and 2017-2019 campaigns. Near-IR variability arises from two different emission regions: the outer part of the accretion disc and a more distant dust component. The -band variability is governed primarily by dust. The H /H ratio variations (for broad components only) correlate with the X-ray and UV fluxes. The spectral type changed from type 1.8 to type 1.9 during 2023 October-2024 January and then a more rapid change to type 1.5 occurred in 2024 February. We interpret these changes as a combination of two factors: changes in the accretion rate as a dominant cause but also the sublimation or recovery of dust along the line of sight.

KW - UV

KW - X-rays: galaxies

KW - galaxies: Seyfert

KW - galaxies: active

KW - galaxies: individual: NGC 2617

KW - optical: galaxies

UR - http://www.scopus.com/inward/record.url?scp=85215676464&partnerID=8YFLogxK

U2 - 10.1093/mnras/stae2707

DO - 10.1093/mnras/stae2707

M3 - Article

AN - SCOPUS:85215676464

SN - 0035-8711

VL - 536

SP - 2089

EP - 2102

JO - Monthly Notices of the Royal Astronomical Society

JF - Monthly Notices of the Royal Astronomical Society

IS - 3

ER -

Multiwavelength monitoring and reverberation mapping of NGC 2617 at deepest minimum with a sharp upward turn during 2021-2024

Abstract

Bibliographical note

Keywords

ASJC Scopus subject areas

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