Polarization properties of changing-look active galactic nuclei: NGC 1365 and NGC 2992^★

¹ Institut d’Astrophysique et de Géophysique, Université de Liège Allée du 6 Août 19c 4000 Liège, Belgium
² Université de Strasbourg, CNRS, Observatoire Astronomique de Strasbourg, UMR 7550 F-67000 Strasbourg, France
³ Institute of Astrophysics, Foundation for Research and Technology-Hellas (FORTH) Heraklion 70013, Greece
⁴ Instituto de Astrofisica de Canarias, Calle Via Lactea s/n E-38205 La Laguna Tenerife, Spain
⁵ Departamento de Astrofisica, Universidad de La Laguna E-38205 La Laguna Tenerife, Spain
⁶ National Astronomical Observatory of Japan 2-21-1 Osawa Mitaka Tokyo 181-8588, Japan

^★★ Corresponding author: This email address is being protected from spambots. You need JavaScript enabled to view it.

Received: 23 September 2025
Accepted: 9 January 2026

Abstract

Changing-look active galactic nuclei (CLAGNs) represent a rare class of AGNs that undergo transitions from type 1 (characterized by the presence of broad emission lines in their spectra) to type 2 (absence of broad emission lines) or vice versa, over timescales ranging from months to years. Such brief periods of variation can significantly constrain the physical processes involved in the accretion of matter onto the AGN central supermassive black hole. Since normal type 1 and type 2 AGNs are known to show different polarization properties, detailed investigations of the CLAGN polarization can shed light on the underlying mechanisms responsible for the changing-look phenomenon. In this paper we present new (spectro)polarimetric observations of two changing-look AGNs located in the core of the inclined spiral galaxies NGC 1365 and NGC 2992. Both AGNs are radio emitters, thereby enabling a comparison of their polarization to the radio jet axis, which defines the accretion disk geometry. In the case of NGC 1365, the AGN shows polarization characteristics consistent with those observed in type 1 Seyferts, in particular polarization parallel to the radio jet. This intrinsic polarization is modified by the wavelength-dependent dichroic extinction that occurs in the galaxy bar and that rotates the polarization angle at the shortest wavelengths. Measuring the polarization of NGC 1365 when the AGN is in a type 2 state would be particularly interesting to see if its polarization becomes perpendicular to the radio axis, as observed in normal type 2 AGNs, or if it remains parallel. NGC 2992, on the other hand, is so inclined that dichroic dust extinction in the disk completely dominates the polarization of the AGN, thus overwhelming any polarization due to scattering. Consequently, the polarization properties remain essentially constant between the different AGN states, and the faint broad lines observed in the polarized flux are most likely not scattered light. Differential dilution between the continuum and the narrow-line polarizations can explain the unusually high polarization measured in the emission lines.