Adrian-Martinez, S and Albert, A and Andre, M and Anton, G and Ardid, M and Aubert, J-J and Baret, B and Barrios, J and Basa, S and Bertin, V and Biagi, S and Bogazzi, C and Bormuth, R and Bou-Cabo, M and Bouwhuis, MC and Bruijn, R and Brunner, J and Busto, J and Capone, A and Caramete, L and Carr, J and Chiarusi, T and Circella, M and Coniglione, R and Costantini, H and Coyle, P and Creusot, A and De Rosa, G and Dekeyser, I and Deschamps, A and De Bonis, G and Distefano, C and Donzaud, C and Dornic, D and Dorosti, Q and Drouhin, D and Dumas, A and Eberl, T and Enzenhofer, A and Escoffier, S and Fehn, K and Felis, I and Fermani, P and Folger, F and Fusco, LA and Galata, S and Gay, P and Geisselsoder, S and Geyer, K and Giordano, V and Gleixner, A and Gomez-Gonzalez, JP and Gracia-Ruiz, R and Graf, K and van Haren, H and Heijboer, AJ and Hello, Y and Hernandez-Rey, JJ and Herrero, A and Hossl, J and Hofestadt, J and Hugon, C and James, CW and de Jong, M and Kalekin, O and Katz, U and Kiessling, D and Kooijman, P and Kouchner, A and Kulikovskiy, V and Lahmann, R and Lattuada, D and Lefevre, D and Leonora, E and Loehner, H and Loucatos, S and Mangano, S and Marcelin, M and Margiotta, A and Martinez-Mora, JA and Martini, S and Mathieu, A and Michael, T and Migliozzi, P and Neff, M and Nezri, E and Palioselitis, D and Pavalas, GE and Perrina, C and Piattelli, P and Popa, V and Pradier, T and Racca, C and Riccobene, G and Richter, R and Roensch, K and Rostovtsev, A and Saldana, M and Samtleben, DFE and Sanchez-Losa, A and Sanguineti, M and Sapienza, P and Schmid, J and Schnabel, J and Schulte, S and Schussler, F and Seitz, T and Sieger, C and Spies, A and Spurio, M and Steijger, JJM and Stolarczyk, Th and Taiuti, M and Tamburini, C and Tayalati, Y and Trovato, A and Tselengidou, M and Tonnis, C and Vallage, B and Vallee, C and Van Elewyck, V and Visser, E and Vivolo, D and Wagner, S and de Wolf, E and Yepes, H and Zornoza, JD and Zuniga, J and Krauss, F and Kadler, M and Mannheim, K and Schulz, R and Trustedt, J and Wilms, J and Ojha, R and Ros, E and Baumgartner, W and Beuchert, T and Blanchard, J and Burkel, C and Carpenter, B and Edwards, PG and Eisenacher Glawion, D and Elsasser, D and Fritsch, U and Gehrels, N and Grafe, C and Grossberger, C and Hase, H and Horiuchi, S and Kappes, A and Kreikenbohm, A and Kreykenbohm, I and Langejahn, M and Leiter, K and Litzinger, E and Lovell, JEJ and Muller, C and Phillips, C and Plotz, C and Quick, J and Steinbring, T and Stevens, J and Thompson, DJ and Tzioumis, AK, ANTARES constrains a blazar origin of two IceCube PeV neutrino events, Astronomy and Astrophysics, 576 Article L8. ISSN 0004-6361 (2015) [Refereed Article]
Copyright 2015 ESO
Context: The source(s) of the neutrino excess reported by the IceCube Collaboration is unknown. The TANAMI Collaboration recently reported on the multiwavelength emission of six bright, variable blazars which are positionally coincident with two of the most energetic IceCube events. Objects like these are prime candidates to be the source of the highest-energy cosmic rays, and thus of associated neutrino emission.
Aims: We present an analysis of neutrino emission from the six blazars using observations with the ANTARES neutrino telescope.
Methods. The standard methods of the ANTARES candidate list search are applied to six years of data to search for an excess of muons – and hence their neutrino progenitors – from the directions of the six blazars described by the TANAMI Collaboration, and which are possibly associated with two IceCube events. Monte Carlo simulations of the detector response to both signal and background particle fluxes are used to estimate the sensitivity of this analysis for different possible source neutrino spectra. A maximum-likelihood approach, using the reconstructed energies and arrival directions of through-going muons, is used to identify events with properties consistent with a blazar origin.
Results. Both blazars predicted to be the most neutrino-bright in the TANAMI sample (1653−329 and 1714−336) have a signal flux fitted by the likelihood analysis corresponding to approximately one event. This observation is consistent with the blazar-origin hypothesis of the IceCube event IC 14 for a broad range of blazar spectra, although an atmospheric origin cannot be excluded. No ANTARES events are observed from any of the other four blazars, including the three associated with IceCube event IC20. This excludes at a 90% confidence level the possibility that this event was produced by these blazars unless the neutrino spectrum is flatter than −2.4.
|Item Type:||Refereed Article|
|Keywords:||neutrinos, galaxies: active, quasars: general|
|Research Division:||Physical Sciences|
|Research Group:||Astronomical and Space Sciences|
|Research Field:||Cosmology and Extragalactic Astronomy|
|Objective Division:||Expanding Knowledge|
|Objective Group:||Expanding Knowledge|
|Objective Field:||Expanding Knowledge in the Physical Sciences|
|UTAS Author:||Lovell, JEJ (Dr Jim Lovell)|
|Web of Science® Times Cited:||11|
|Deposited By:||Mathematics and Physics|
|Downloads:||94 View Download Statistics|
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