Long-term optical spectral monitoring of a changing-look active galactic nucleus NGC 3516 -- II. Broad-line profile variability

A&A 675, A178 (2023) We analyze the broad H$\beta$ line profile variability of the "changing look" active galactic nucleus (CL-AGN) NGC 3516 over a long period of 25 years. The observed change in the broad line profile may indicate a change in the geometry of the broad line region (BLR...

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Bibliographic Details
Main Authors:	Popović, Luka C, Ilić, Dragana, Burenkov, Alexander, Álvarez, Victor Manuel Patiño, Marceta-Mandić, Sladjana, Dojcinović, Jelena Kovacević, Shablovinskaya, Elena, Kovacević, Andjelka B, Marziani, Paola, Chavushyan, Vahram, Wang, Jian-Min, Li, Yan-Rong, Mediavilla, Evencio G
Format:	Journal Article
Language:	English
Published:	01-06-2023
Subjects:	Physics - Astrophysics of Galaxies Physics - Cosmology and Nongalactic Astrophysics
Online Access:	Get full text
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Summary:	A&A 675, A178 (2023) We analyze the broad H$\beta$ line profile variability of the "changing look" active galactic nucleus (CL-AGN) NGC 3516 over a long period of 25 years. The observed change in the broad line profile may indicate a change in the geometry of the broad line region (BLR). Using spectral line profiles, we aim to explore changes in the kinematics and dimensions of the BLR in NGC 3516. We consider two possible scenarios, i.e. changes in the broad-line emission are caused by a decrease of ionization continuum emission or by the BLR obscuration by outer dusty regions. With this investigation we aim to clarify the CL mechanism of this AGN. We analyze the spectral band around the H$\beta$ line as well as the broad H$\beta$ line parameters, and how they change in time. We model the broad-line profiles assuming that there is an emission from the accretion disc superposed with an emission from a surrounding region that is outside the disc. We find that in the Type 1 activity phase, the BLR is very complex. There is a clear disc-like BLR that contributes to the broad line wings and an additional intermediate line region (ILR) that contributes to the line core. In the high activity phase, the ILR emission is close to the center of the line (in some cases slightly shifted to the red), whereas in the low activity phase (i.e., Type 2 phase), the ILR component has a significant shift to the blue, indicating an outflow. We propose that the changing look mechanism in NGC 3516 is rather connected with the intrinsic effects than with an outer obscuring region. It may still be possible that the dust has an important role in the low activity phase when it is coming inside of the BLR, making a dusty BLR. In this way, it causes a decrease in the ionization and recombination rates.
DOI:	10.48550/arxiv.2306.00669