@article {21690,
	title = {Multi-epoch Modeling of TXS 0506+056 and Implications for Long-term High-energy Neutrino Emission},
	volume = {891},
	year = {2020},
	month = {2020/03/1},
	pages = {115},
	abstract = {The IceCube report of a \~{} 3.5σ excess of 13 {\textpm} 5 neutrino events in the direction of the blazar TXS 0506+056 in 2014-2015 and the 2017 detection of a high-energy neutrino event, IceCube-170922A, during a gamma-ray flare from the same blazar, have revived the interest in scenarios for neutrino production in blazars. We perform comprehensive analyses on the long-term electromagnetic emission of TXS 0506+056 using optical, X-ray, and gamma-ray data from the All-Sky Automated Survey for Supernovae, the Neil Gehrels Swift Observatory, Monitor of All-sky X-ray Image, and the Fermi Large Area Telescope. We also perform numerical modeling of the spectral energy distributions (SEDs) in four epochs prior to 2017 with contemporaneous gamma-ray and lower-energy (optical and/or X-ray) data. We find that the multi-epoch SEDs are consistent with a hybrid leptonic scenario, where the gamma-rays are produced in the blazar zone via external inverse Compton scattering of accelerated electrons, and high-energy neutrinos are produced via the photomeson production process of co-accelerated protons. The multi-epoch SEDs can be satisfactorily explained with the same jet parameters and variable external photon density and electron luminosity. Using the maximal neutrino flux derived for each epoch, we put an upper limit of \~{}0.4-2 on the muon neutrino number in 10 years of IceCube observations. Our results are consistent with the IceCube-170922A detection, which can be explained as an upper fluctuation from the average neutrino rate expected from the source, but in strong tension with the 2014-2015 neutrino flare.},
	keywords = {1100, 158, 17, 637, 739, Astrophysics - High Energy Astrophysical Phenomena},
	isbn = {0004-637X},
	url = {https://ui.adsabs.harvard.edu/abs/2020ApJ...891..115P},
	author = {Petropoulou, Maria and Murase, Kohta and Santander, Marcos and Buson, Sara and Tohuvavohu, Aaron and Kawamuro, Taiki and Vasilopoulos, Georgios and Negoro, Hiroshi and Ueda, Yoshihiro and Siegel, Michael H. and Keivani, Azadeh and Kawai, Nobuyuki and Mastichiadis, Apostolos and Dimitrakoudis, Stavros}
}
