2018
DOI: 10.3847/2041-8213/aad083
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The Blazar TXS 0506+056 Associated with a High-energy Neutrino: Insights into Extragalactic Jets and Cosmic-Ray Acceleration

Abstract: A neutrino with energy ∼290 TeV, IceCube-170922A, was detected in coincidence with the BL Lac object TXS0506+056 during enhanced gamma-ray activity, with chance coincidence being rejected at ∼3σ level. We monitored the object in the very-high-energy (VHE) band with the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes for ∼41 hr from 1.3 to 40.4 days after the neutrino detection. Day-timescale variability is clearly resolved. We interpret the quasi-simultaneous neutrino and broadband electromag… Show more

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Cited by 192 publications
(164 citation statements)
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“…Britzen et al (2019) use radio data to suggest a possible collision of two jets in TXS 0506+056. However, Ros et al (2019) exclude the presence of a secondary jet core with higher resolution radio data, but find signs of a spine-sheath structure of the jet, which could be relevant for neutrino production see also (see also Ghisellini et al 2005;Tavecchio et al 2014;Ansoldi et al 2018).…”
Section: Multi-wavelength Datamentioning
confidence: 99%
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“…Britzen et al (2019) use radio data to suggest a possible collision of two jets in TXS 0506+056. However, Ros et al (2019) exclude the presence of a secondary jet core with higher resolution radio data, but find signs of a spine-sheath structure of the jet, which could be relevant for neutrino production see also (see also Ghisellini et al 2005;Tavecchio et al 2014;Ansoldi et al 2018).…”
Section: Multi-wavelength Datamentioning
confidence: 99%
“…Software: Fermi-LAT Science Tools (v11r04p00), fermipy (v0.17.4; Wood et al 2018), astropy (Astropy Collaboration et al 2013, 2018, IRAF (Tody 1986(Tody , 1993, ISIS (Alard & Lupton 1998;Alard 2000), XSPEC (Arnaud 1996) The green region in panel 1 marks the quiescent state and vertical red, cyan and black lines mark three flaring states, which are accompanied by X-ray and optical flares, selected for a dedicated gamma-ray spectral analysis (see Tab. 5 and Fig.…”
Section: Source Populationmentioning
confidence: 99%
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“…The modeling of the sources requires the knowledge of their distance, which in the case of BLL, is hard to establish, because by definition of the class the spectral lines are absent or very weak (equivalent width, EW < 5Å). In the past several years some of us have been studying optical spectra of BLL with resolution and signalto-noise ratio (S/N) optimized to detect such weak features (Landoni et al 2014;Paiano et al 2017aPaiano et al ,b,c, 2019a Ansoldi et al 2018;Giommi et al 2020b, and references therein) with BLL, which are a blazar sub-class. These neutrinos permit to shed light on the most energetic processes, which, as mentioned above, are otherwise screened off by the EBL.…”
Section: Introductionmentioning
confidence: 99%
“…The high-energy component is often interpreted as the inverse Compton (IC) upscattering of ambient soft photons by the accelerated electrons (e.g., Böttcher 2007). The soft photons can be either synchrotron photons within the jet( the synchrotron self-Compton, SSC, process, Maraschi et al 1992;Bloom and Marscher 1996), or the photons external to the jet ( the External Compton, EC, process). These external photons may be the UV accretion disk photons (Dermer & Schlickeiser 1993), the accretion disk photons reprocessed by broad-line region clouds (Sikora et al 1994), or infrared photons from the dust torus (Blaźejowski et al 2000).…”
Section: Introductionmentioning
confidence: 99%