The optically elusive, changing-look active nucleus in NGC 4156

A&A 667, L12 (2022) We report on the changing-look nature of the active galactic nucleus (AGN) in the galaxy NGC 4156, as serendipitously discovered thanks to data acquired in 2019 at the Telescopio Nazionale Galileo (TNG) during a students' observing programme. Previous optical spectra had...

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Bibliographic Details
Main Authors:	Tozzi, Giulia, Lusso, Elisabeta, Casetti, Lapo, Romoli, Marco, Andreuzzi, Gloria, A, Isabel Montoya, Nardini, Emanuele, Cresci, Giovanni, Middei, Riccardo, Bertolini, Silvia, Calabretto, Paolo, Cammelli, Vieri, Cuadra, Francisco, Ragione, Marco Dalla, Marconcini, Cosimo, Miceli, Adriano, Mini, Irene, Palazzini, Martina, Rotellini, Giorgio, Saccardi, Andrea, Samà, Lavinia, Sangalli, Mattia, Serafini, Lorenzo, Spaccino, Fabio
Format:	Journal Article
Language:	English
Published:	17-10-2022
Subjects:	Physics - Astrophysics of Galaxies
Online Access:	Get full text
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Summary:	A&A 667, L12 (2022) We report on the changing-look nature of the active galactic nucleus (AGN) in the galaxy NGC 4156, as serendipitously discovered thanks to data acquired in 2019 at the Telescopio Nazionale Galileo (TNG) during a students' observing programme. Previous optical spectra had never shown any signatures of broad-line emission, and evidence of the AGN had come only from X-ray observations, being the optical narrow-line flux ratios unable to unambiguously denote this galaxy as a Seyfert. Our 2019 TNG data unexpectedly revealed the appearance of broad-line components in both the H$\alpha$ and H$\beta$ profiles, along with a rise of the continuum, thus implying a changing-look AGN transitioning from a type 2 (no broad-line emission) towards a (nearly) type 1. The broad-line emission has then been confirmed by our 2022 follow-up observations, whereas the rising continuum has no longer been detected, which hints at a further evolution backwards to a (nearly) type 2. The presence of broad-line components also allowed us to obtain the first single-epoch estimate of the black hole mass (log(MBH/Msun) $\sim$ 8.1) in this source. The observed spectral variability might be the result of a change in the accretion activity of NGC 4156, although variable absorption cannot be completely excluded.
DOI:	10.48550/arxiv.2210.09341