RT Journal Article
T1 The Blazar TXS 0506+056 Associated with a High-energy Neutrino: Insights into Extragalactic Jets and Cosmic-Ray Acceleration
A1 Barrio Uña, Juan Abel
A1 Contreras González, José Luis
A1 Domínguez Díaz, Alberto
A1 Carreto Fidalgo, David Friedrich
A1 Fonseca González, María Victoria
A1 Hoang, Kim Dinh
A1 López Moya, Marcos
A1 Nievas Rosillo, Mireia
A1 Peñil Del Campo, Pablo
A1 Saha, Lab
AB A neutrino with energy similar to 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 similar to 3 sigma level. We monitored the object in the very-high-energy (VHE) band with the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes for similar to 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 electromagnetic observations with a novel one-zone lepto-hadronic model, based on interactions of electrons and protons co-accelerated in the jet with external photons originating from a slow-moving plasma sheath surrounding the faster jet spine. We can reproduce the multiwavelength spectra of TXS 0506+056 with neutrino rate and energy compatible with IceCube-170922A, and with plausible values for the jet power of similar to 10(45) - 4 x 10(46) erg s(-1). The steep spectrum observed by MAGIC is concordant with internal gamma gamma absorption above similar to 100 GeV entailed by photohadronic production of a similar to 290 TeV neutrino, corroborating a genuine connection between the multi-messenger signals. In contrast to previous predictions of predominantly hadronic emission from neutrino sources, the gamma-rays can be mostly ascribed to inverse Compton upscattering of external photons by accelerated electrons. The X-ray and VHE bands provide crucial constraints on the emission from both accelerated electrons and protons. We infer that the maximum energy of protons in the jet comoving frame can be in the range similar to 10(14) - 10(18) eV.
PB IOP Publishing Ltd
SN 2041-8205
YR 2018
FD 2018-08-10
LK https://hdl.handle.net/20.500.14352/13082
UL https://hdl.handle.net/20.500.14352/13082
LA eng
NO © 2018. The American Astronomical Society. Artículo firmado por 149 autores. We would like to thank the Instituto de Astrofisica de Canarias for the excellent working conditions at the Observatorio del Roque de los Muchachos in La Palma. The financial support of the German BMBF and MPG, the Italian INFN and INAF, the Swiss National Fund SNF, the ERDF under the Spanish MINECO (FPA2015-69818-P, FPA2012-36668, FPA2015-68378-P, FPA2015-69210-C6-2-R, FPA2015-69210-C6-4-R, FPA2015-69210-C6-6-R, AYA2015-71042-P, AYA2016-76012-C3-1-P, ESP2015-71662-C2-2-P, CSD2009-00064), and the Japanese JSPS and MEXT is gratefully acknowledged. This work was also supported by the Spanish Centro de Excelencia "Severo Ochoa" SEV-2012-0234 and SEV-2015-0548, and Unidad de Excelencia "María de Maeztu" MDM-2014-0369, by the Croatian Science Foundation (HrZZ) Project IP-2016-06-9782 and the University of Rijeka Project 13.12.1.3.02, by the DFG Collaborative Research Centers SFB823/C4 and SFB876/C3, the Polish National Research Centre grant UMO-2016/22/M/ST9/00382 and by the Brazilian MCTIC, CNPq and FAPERJ. Part of this work is based on archival data, software or on-line services provided by the Space Science Data Center-ASI.
NO Ministerio de Economía y Competitividad (MINECO)/FEDER
NO Centro de Excelencia "Severo Ochoa"
NO Unidad de Excelencia "María de Maeztu"
NO German BMBF
NO MPG
NO Italian INFN
NO INAF
NO Swiss National Fund SNF
NO Japanese JSPS
NO MEXT
NO Croatian Science Foundation (HrZZ) Project
NO University of Rijeka Project
NO DFG Collaborative Research Centers
NO Polish National Research Centre
NO Brazilian MCTIC
NO Brazilian CNPq
NO Brazilian FAPERJ
DS Docta Complutense
RD 18 abr 2025