Abstract

Contributed Talk - Splinter Multimessenger

Expanding the Quasi-Periodic Multi-Messenger Picture of the Blazar J1048+7143 with the Optical Light Curve

Johannes Just [1,2], Emma Kun [1,2,3,4,5], Ilja Jaroschewski [2,6], Julia Becker Tjus [1,2,7]
[1] Theoretical Physics IV: Plasma-Astroparticle Physics, Faculty for Physics & Astronomy, Ruhr University Bochum, 44780 Bochum, Germany, [2] Ruhr Astroparticle And Plasma Physics Center (RAPP Center), Ruhr University Bochum, 44780 Bochum, Germany, [3] Astronomical Institute, Faculty for Physics & Astronomy, Ruhr University Bochum, 44780 Bochum, Germany, [4] Konkoly Observatory, HUN-REN Research Centre for Astronomy and Earth Sciences, Konkoly Thege Miklós út 15-17, H-1121 Budapest, Hungary, [5] CSFK, MTA Centre of Excellence, Konkoly Thege Miklós út 15-17, H-1121 Budapest, Hungary, [6] IRFU, CEA, Université Paris-Saclay, 91191 Gif-Sur-Yvette, France, [7] Department of Space, Earth and Environment, Chalmers University of Technology, SE-412 96 Gothenburg, Sweden

The gamma-ray and radio light curves of the blazar J1048+7143 reveal a pattern of quasi-periodic oscillations that can be explained by the existence of a supermassive binary black hole (SMBBH) inspiral at its core. In this model, the light curves can be explained via jet precession of the dominant supermassive black hole jet caused by spin-orbit coupling. In this work, we add optical data from different observatories to the multi-messenger picture. We determine the duration and occurrence times of the flares with this new optical data and predict the time of the next flare. Furthermore, we find constrains to the SMBBH parameters that are in agreement with those inferred from the gamma-ray and radio light curves. With the results obtained using these optical data, we build a consistent model across the wavelengths. The gamma-ray and optical light curves of the blazar show a double flare substructure in the main flares, while the radio light curve does not show this feature. In our model, we work out a scenario in which the different wavelengths can be explained consistently and discuss our new findings. Finally, we provide an outlook on how full light curves can be modeled based on Doppler boosting and the evolution of the jet direction over time.