Neutrino emission from the direction of the blazar TXS 0506+056 prior to the IceCube-170922A alert

Aartsen, M. G.; Ackermann, M.; Adams, J.; Aguilar, J. A.; Ahlers, M.; Ahrens, M.; Samarai, I. Al; Altmann, D.; Andeen, K.; Anderson, Tyler; Ansseau, I.; Anton, Gisela; Argüelles, C.; Arsioli, B.; Auffenberg, J.; Axani, Spencer; Bagherpour, H.; Bai, X.; Barron, J. P.; Barwick, S. W.; Baum, V.; Bay, R.; Beatty, J. J.; Becker, K. H.; Tjus, J. Becker; BenZvi, S.; Berley, D.; Bernardini, E.; Besson, D.; Binder, G.; Bindig, D.; Blaufuss, E.; Blot, Summer; Böhm, C.; Boerner, Mathis; Bos, F.; Boeser, S.; Botner, O.; Bourbeau, Etienne; Bourbeau, J.; Bradascio, Federica; Braun, J.; Brenzke, M.; Bretz, H.-P.; Bron, S.; Brostean-Kaiser, Jannes; Burgman, A.; Busse, Raffaela; Carver, T.; Cheung, E.; Chirkin, D.; Christov, A.; Clark, K.; Classen, L.; Coenders, S.; Collin, Gabriel; Conrad, J. M.; Coppin, Paul; Correa, Pablo; Cowen, D. F.; Cross, R.; Dave, Pranav; Day, M.; André, J. P. A. M. de; Clercq, C. De; DeLaunay, James; Dembinski, H.-P.; DeRidder, Sam; Desiati, P.; Vries, Krijn de; Wasseige, G. de; DeWith, Meike; DeYoung, T.; Díaz–Vélez, Juan Carlos; Lorenzo, V. di; Dujmović, Hrvoje; Dumm, J.; Dunkman, M.; Dvorak, Emily; Eberhardt, B.; Ehrhardt, Thomas; Eichmann, B.; Eller, P.; Evenson, P. A.; Fahey, S.; Fazely, A. R.; Felde, J.; Filimonov, K.; Finley, C.; Flis, S.; Franckowiak, A.; Friedman, E.; Fritz, A.; Gaisser, T. K.; Gallagher, J.; Gerhardt, L.; Ghorbani, K.; Giommi, P.; Glauch, Theo; Gluesenkamp, T.; Goldschmidt, A.; González, J. G.; Grant, D.; Griffith, Z.; Haack, Christian; Hallgren, A.; Halzen, F.; Hanson, K.; Hebecker, D.; Heereman, D.; Helbing, K.; Hellauer, R.; Hickford, S.; Hignight, J.; Hill, G. C.; Hoffman, K. D.; Hoffmann, R.; Hoinka, Tobias; Hokanson-Fasig, B.; Hoshina, K.; Huang, F.; Huber, Matthías; Hultqvist, K.; Huennefeld, Mirco; Hussain, Raamis; In, Seongjin; Iovine, N.; Ishihara, A.; Jacobi, E.; Japaridze, G. S.; Jeong, Minjin; Jero, K.; Jones, B. J. P.; Kalaczyński, P.; Kang, Woosik; Kappes, A.; Kappesser, David; Karg, T.; Karle, A.; Katz, U.; Kauer, M.; Keivani, A.; Kelley, J. L.; Kheirandish, Ali; Kim, Jong-Hyun; Kim, Myoungchul; Kintscher, T.; Kiryluk, J.; Kittler, T.; Klein, S. R.; Koirala, R.; Kolanoski, H.; Koepke, L.; Kopper, C.; Kopper, S.; Koschinsky, J. P.; Koskinen, D. J.; Kowalski, M.; Krammer, Benedikt; Krings, K.; Kroll, M.; Krueckl, Gerald; Kunwar, S.; Neilson, Naoko Kurahashi; Kuwabara, T.; Kyriacou, A.; Labare, M.; Lanfranchi, J. L.; Larson, M. J.; Lauber, Frederik Hermann; Leonard, K.; Lesiak-Bzdak, M.; Leuermann, M.; Liu, Qinrui; Mariscal, Cristian Jesús Lozano; Lu, Lu; Luenemann, J.; Luszczak, William; Madsen, J.; Maggi, G.; Mahn, Kendall; Mancina, Sarah; Maruyama, R.; Mase, K.; Maunu, R.; Meagher, K.; Medici, M.; Meier, Maximilian; Menne, T.; Merino, G.; Meures, T.; Miarecki, S.; Micallef, Jessie; Momenté, G.; Montaruli, T.; Moore, R. W.; Morse, R.; Moulai, Marjon; Nahnhauer, R.; Nakarmi, P.; Naumann, Uwe; Neer, G.; Niederhausen, H.; Nowicki, S. C.; Nygren, D. R.; Pollmann, A. Obertacke; Olivas, A.; Murchadha, Aongus Ó; O’Sullivan, Erin; Padovani, P.; Palczewski, T.; Pandya, Hershal; Pankova, D. V.; Peiffer, P.; Pepper, J. A.; Heros, C. Pérez de los; Pieloth, D.; Pinat, E.; Plum, M.; Price, Buford; Przybylski, G. T.; Raab, Christoph; Raedel, L.; Rameez, M.; Rawlins, K.; Rea, Immacolata Carmen; Reimann, R.; Relethford, B.; Relich, M.; Resconi, E.; Rhode, W.; Richman, M.; Robertson, Sally; Rongen, Martin; Rott, C.; Ruhe, T.; Ryckbosch, D.; Rysewyk, D.; Safa, Ibrahim; Saelzer, Tobias; Sahakyan, N.; Herrera, Sebastian Sanchez; Sandrock, A.; Sandroos, J.; Santander, M.; Sarkar, Sourav; Sarkar, Subir; Satalecka, K.; Schlunder, P.; Schmidt, T.; Schneider, A.; Schoenen, S.; Schoeneberg, S.; Schumacher, Lisa Johanna; Sclanfani, Stephen; Seckel, D.; Seunarine, S.; Soedingrekso, Jan; Soldin, D.; Song, M.; Spiczak, G. M.; Spiering, Christian; Stachurska, J.; Stamatikos, M.; Stanev, T.; Stasik, A.; Stettner, J.; Steuer, A.; Stezelberger, T.; Stokstad, R. G.; Stoeßl, A.; Strotjohann, N. L.; Stuttard, T.; Sullivan, G. W.; Sutherland, M.; Taboada, I.; Tatar, J.; Tenholt, F.; Ter–Antonyan, S.; Terliuk, A.; Tilav, S.; Toale, P. A.; Tobin, M. N.; Toennis, Christoph; Toscano, S.; Tosi, D.; Tselengidou, M.; Tung, Chunfai; Turcati, A.; Turley, C. F.; Ty, Bunheng; Unger, L.; Usner, M.; Driessche, W. Van; Eijk, D. van; Eijndhoven, N. van; Vandenbroucke, J.; Vanheule, S.; Santen, J. V.; Vogel, E.; Vraeghe, M.; Walck, C.; Wallace, A.; Wallraff, M.; Wandler, F. D.; Wandkowsky, N.; Waza, A.; Weaver, Chris; Weiss, Matthew J.; Wendt, Chris; Werthebach, Johannes; Westerhoff, S.; Whelan, B. J.; Whitehorn, N.; Wiebe, K.; Wiebusch, C. H.; Wille, L.; Williams, D. R.; Wills, L.; Wolf, M.; Wood, J.; Wood, T. R.; Woschnagg, K.; Xu, D. L.; Xu, X. W.; Xu, Y.; Yañez, J. P.; Yodh, G.; Yoshida, Shigeru; Yuan, Tianlu

doi:10.1126/science.aat2890

Cited by 758 publications

(525 citation statements)

References 33 publications

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“…14]. The recent detection of a ∼ 290-TeV neutrino (IceCube-170922A) by the IceCube observatory in the direction of blazar TXS 0506+056 [23,24], spatially and temporally coincident with its flaring MW activity provided the first clear evidence in favor of hadronic emission. Further investigation of data revealed neutrinos detection in the same direction during a quiescent state of the source [23].…”

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confidence: 99%

A Multi-Wavelength View of OJ 287 Activity in 2015–2017: Implications of Spectral Changes on Central-Engine Models and MeV-GeV Emission Mechanism

Kushwaha

2020

Galaxies

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A diverse range of observational results and peculiar properties across the domains of observation have made OJ 287 one of the best-explored BL Lac objects on the issues of relativistic jets and accretion physics as well as the strong theory of gravity. We here present a brief compilation of observational results from the literature and inferences/insights from the extensive studies but focus on the interpretation of its ∼ 12-yr quasi-periodic optical outbursts (QPOOs) and high energy emission mechanisms. The QPOOs in one model are attributed to the disk-impact related to dynamics of the binary SMBHs while alternative models attribute it to the geometrical effect related to the precession of a single jet or double jets. We discuss implications of the new spectral features reported during the 2015-2017 multi-wavelength high activity of the source -a break in the NIR-optical spectrum and hardening of the MeV-GeV emission accompanied by a shift in the location of its peak, in the context of the two. The reported NIR-optical break nicely fits the description of a standard accretion disk emission from an SMBH of mass ∼ 10 10 M while the time of its first appearance in end-May 2013 (MJD 56439) is in close coincidence with the time of impact predicted by the disk-impact binary SMBH model. This spectral and temporal coincidence with the model parameters of the disk-impact binary SMBH model provides independent evidence in favor of the model over the geometrical models which argue a total central-engine mass in the range of 10 7−9 M . On the other hand, the MeV-GeV spectral change is naturally reproduced by the inverse Compton scattering of photons from the broad-line region and is consistent with the detection of broad emission lines during the previous cycles of quasi-periodic outbursts. Combining this with previous SED studies suggests that in OJ 287, MeV-GeV emission results from external Comptonization. 2 of 21 minutes and even less to decades 1 [∼ 6-7 orders of magnitude; e.g. 2]. Their radio and optical emission is highly polarized and have been observed to vary often with the source flux, all the way from 0 to > 50%. Imaging in radio, infra-red (IR), optical, and X-ray, on the other hand, show an extremely well collimated jet extending up to Mpc scales [∼ 9-13 orders of magnitude; e.g. 3,4] with frequent sighting of superluminal features in high-resolution imaging of the core. Taken together with the observational and theoretical understanding of other astrophysical objects combined with their high and rarely repeating observational behavior indicates that they are the site of complex, multi-level, multi-scale physics and thus, are normally called extreme sources among non-catastrophic events.Though studies in different energy bands finally culminated into a unified scheme for radio-loud AGNs [5], it also revealed that AGNs need well-coordinated multi-wavelength (MW) observations to go beyond the limits associated with individual bands. The launch of the gamma-ray survey observatory Fermi-LAT (Large Area Telescope...

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confidence: 99%

A Multi-Wavelength View of OJ 287 Activity in 2015–2017: Implications of Spectral Changes on Central-Engine Models and MeV-GeV Emission Mechanism

Kushwaha

2020

Galaxies

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“…The hadronic models for compact non-thermal astrophysical sources, such as Gamma Ray Bursts (GRBs), are a viable alternative to the more popular leptonic ones [1], [2]. Apart from having implications for the sites of Cosmic Ray acceleration and for high energy neutrino astronomy [3], which start becoming testable by ongoing observations [4], hadronic models have an intriguing property, coined as supercriticality [5]. Relativistic protons become supercritical when their energy density inside a source exceeds a certain threshold [6].…”

Section: Hadronic Supercriticalities In Grbsmentioning

confidence: 99%

The Onset of Hadronic Supercriticality in ExpandingSources

Florou¹,

Mastichiadis²

2020

Proceedings of High Energy Phenomena in Relativistic Outflows VII — PoS(HEPRO VII)

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An overlooked property of hadronic models is that they can become supercritical by abruptly transforming the energy stored in the relativistic protons into radiation. Supercriticality manifests itself when the proton density exceeds a critical value. We seek to map the complete parameter space of this behaviour in cases where a source, consisting of relativistic protons, is expanding so adiabatic losses become important. We search those critical values that lead the system to the supercritical regime and are closely related to Gamma Ray Bursts. For this reason we adopt the Relativistic Blast Wave (RBW) model which is thought to describe the production of a GRB after the initial explosion High Energy Phenomena in Relativistic Outflows VII -HEPRO VII

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“…The latest constraints on the neutrino mass square differences are [49] We first consider the time delay of SNN signals from the same side of the lens. In this work, we focus on the SNNs because their properties are better understood comparing to neutrinos of other astrophysical origin [7,8,51]. Because neutrinos have three mass eigenstates, for any given SNN spectrum that usually last a few seconds the three mass eigenstates will decouple from each other during propagation from supernova to observer which costs long time.…”

Section: A Snn Time Delaymentioning

confidence: 99%

“…With the discovery of supernova neutrino (SNN) from SN1987A [1,2], the recent observation of gravitational wave (GW) signal [3][4][5][6] and more recent confirmation of neutrino emission from blazer TXS 0506+056 [7,8], astronomy has certainly entered the multi-messenger era. In particular, the observation of the binary neutron star merger GW170817 and GRB 170817A [6,9,10] is a simultaneous observation of the Gamma-ray burst (GRB) and GW signals.…”

Section: Introductionmentioning

confidence: 99%

Time delay of timelike particles in gravitational lensing of the Schwarzschild spacetime

Jia

Liu

2019

Phys. Rev. D

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Time delay in Schwarzschild spacetime for null and timelike signals with arbitrary velocity v is studied. The total travel time t if is evaluated both exactly and approximately in the weak field limit, with the result given as functions of signal velocity, source-lens and lens-observer distances, angular position of the source and lens mass. Two time delays, ∆t v between signals with different velocities but coming from same side of the lens and ∆t p between signals from different sides of the lens, as well as the difference ∆t pv between two ∆t p 's are calculated. These time delays are applied to the gravitational-lensed supernova neutrinos and gravitational waves (GW). It is shown that the ∆t v between different mass eigenstates of supernova neutrinos can be related to the mass square difference of these eigenstates and therefore could potentially be used to discriminate neutrino mass orderings, while the difference ∆t pv between neutrino and optical signals can be correlated with the absolute mass of neutrinos. The formula for time delay in a general lens mass profile is derived and the result is applied to the singular isothermal sphere case. For GWs, it is found that the difference ∆t pv between GW and GRB can only reach 1.45 × 10 −5 second for very large source distance (2 × 10 4 [Mpc]) and source angle (10 [as]) if v GM = (1 − 3 × 10 −15 )c. This time difference is at least three order smaller than uncertainties in time measurement of the recently observed GW/GRB signals and thus calls for improvement if ∆t pv is to be used to further constrain the GW velocity.

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Neutrino emission from the direction of the blazar TXS 0506+056 prior to the IceCube-170922A alert

Cited by 758 publications

References 33 publications

A Multi-Wavelength View of OJ 287 Activity in 2015–2017: Implications of Spectral Changes on Central-Engine Models and MeV-GeV Emission Mechanism

A Multi-Wavelength View of OJ 287 Activity in 2015–2017: Implications of Spectral Changes on Central-Engine Models and MeV-GeV Emission Mechanism

The Onset of Hadronic Supercriticality in ExpandingSources

Time delay of timelike particles in gravitational lensing of the Schwarzschild spacetime

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