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Интеллектуальная Система Тематического Исследования НАукометрических данных |
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Long-term multiwavelength monitoring and reverberation mapping of NGC 2617 during a changing-look eventстатья Электронная публикация
- Авторы: Oknyansky V.L., Brotherton M.S., Tsygankov S.S., Dodin A.V., Tatarnikov A.M., Du P, Bao D.W., Burlak M.A., Ikonnikova N.P., Lipunov V.M., Gorbovskoy E.S., Metlov V.G., Belinski A.A., Shatsky N.I., Zheltouhov S.G., Maslennikova N.A., Huseynov N.A., Wang J.M., Zhai S., Fang F.N., Fu Y.X., Bai H.R., Kasper D., McLane J.N., Maithil J., Zastrocky T.E., Olson K.A., X Chen, Chelouche D., Oknyansky R.S., Buckley D.A.H, Tyurina N.V., Kuznetsov A.S., Rebolo R.L., Zhao B.X.
- Сборник: eprint arXiv:2308.04855
- Год издания: 2023
- Первая страница: 1
- Последняя страница: 14
- Номер статьи: 2308.04855
- Аннотация: We present the results of photometric and spectroscopic monitoring campaigns of the changing look AGN NGC~2617 carried out from 2016 until 2022 and covering the wavelength range from the X-ray to the near-IR. The facilities included the telescopes of the SAI MSU, MASTER Global Robotic Net, the 2.3-m WIRO telescope, Swift, and others. We found significant variability at all wavelengths and, specifically, in the intensities and profiles of the broad Balmer lines. We measured time delays of ~ 6 days (~ 8 days) in the responses of the H-beta (H-alpha) line to continuum variations. We found the X-ray variations to correlate well with the UV and optical (with a small time delay of a few days for longer wavelengths). The K-band lagged the B band by 14 +- 4 days during the last 3 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 HK-band variability is governed primarily by dust. The Balmer decrement of the broad-line components is inversely correlated with the UV flux. The change of the object's type, from Sy1 to Sy1.8, was recorded over a period of ~ 8 years. We interpret these changes as a combination of two factors: changes in the accretion rate and dust recovery along the line of sight. Accepted by the MNRAS.
- Добавил в систему: Окнянский Виктор Львович