2017
DOI: 10.1051/0004-6361/201731726
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Unveiling the physics behind the spectral variations of changing-look quasars with optical polarimetry

Abstract: A handful of active galactic nuclei (AGN) have shown strong spectral variations in the optical band between epochs that are years apart. The appearance or disappearance of broad emission lines in their spectra completely changes their classification. Since their nucleus orientation cannot change in such short timescales another physical interpretation has to be found. Several scenarios are competing to explain their changing-look nature and, for the first time, we conduct polarized radiative transfer Monte Car… Show more

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Cited by 17 publications
(18 citation statements)
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“…This result supports the variable accretion rate scenario as suggested by [21]. Afterwards, [35] reinforced the use of polarimetry as a diagnostic tool by modeling the optical continuum polarization expected from CL AGN in a transition from type 1 to type 2. The author carried out simulations for the two described scenarios, variable accretion rate and variable obscuration, using the Monte Carlo radiative transfer code STOKES [36,37].…”
Section: Changing-look Scenario and Optical Polarimetry As A Diagnostsupporting
confidence: 83%
“…This result supports the variable accretion rate scenario as suggested by [21]. Afterwards, [35] reinforced the use of polarimetry as a diagnostic tool by modeling the optical continuum polarization expected from CL AGN in a transition from type 1 to type 2. The author carried out simulations for the two described scenarios, variable accretion rate and variable obscuration, using the Monte Carlo radiative transfer code STOKES [36,37].…”
Section: Changing-look Scenario and Optical Polarimetry As A Diagnostsupporting
confidence: 83%
“…In this phase, the intensity in the broad component of a spectral line is too weak that probably the AP15 method could not be used. Another technique must be used to explore the geometry of the object, such as proved by Hutsemékers et al (2017) and Marin (2017).…”
Section: Observationsmentioning
confidence: 99%
“…LaMassa et al 2015;Ruan et al (2016); MacLeod et al 2016;Runnoe et al 2016;McElroy et al 2016;Gezari et al 2017). Possible explanations for this phenomenon include changes in accretion rate (e.g., Marin 2017). On longer timescales, >10 4 yr, AGN variability is probed through extended AGN photoionised emission line regions (EELR) such as the Voorwerpjes (VP, e.g., Lintott et al 2009;Gagne et al 2011;Keel et al 2012;Keel et al 2017;Sartori et al 2016;Sartori et al 2018) or ionisation and radio structures in our own Milky Way (e.g., Su et al look quasars" are used inconsistently throughout the literature, and can refer to changes both in emission line width or obscuration, as well as in luminosity.…”
Section: Introductionmentioning
confidence: 98%