First all-flavor neutrino pointlike source search with the ANTARES neutrino telescope

Albert, A.; André, M.; Anghinolfi, M.; Anton, G.; Ardid, M.; Aubert, Jean-Jacques; Avgitas, T.; Baret, B.; Barrios-Martí, J.; Basa, S.; Belhorma, B.; Bertín, V.; Biagi, S.; Bormuth, R.; Bourret, S.; Bouwhuis, M. C.; Brânzaş, H.; Bruijn, R.; Brünner, J.; Busto, J.; Capone, A.; Caramete, L.; Carr, J.; Celli, S.; Moursli, R. Cherkaoui El; Chiarusi, T.; Circella, M.; Coelho, J. A. B.; Coleiro, A.; Coniglione, R.; Costantini, H.; Coyle, P.; Creusot, A.; Dı́az, A.; Deschamps, A.; Bonis, G. De; Distefano, C.; Palma, I. Di; Domi, Alba; Donzaud, C.; Dornic, D.; Drouhin, D.; Eberl, T.; Bojaddaini, I. El; Khayati, N. El; Elsässer, Dominik; Enzenhöfer, A.; Ettahiri, A.; Fassi, F.; Felis, I.; Fusco, L.; Galatà, S.; Gay, P.; Giordano, V.; Glotin, Hervé; Grégoire, T.; Ruiz, R. Gracia; Graf, Κ.; Hallmann, S.; Haren, Hans van; Heijboer, A.; Hello, Y.; Hernández-Rey, J. J.; Hößl, J.; Hofestädt, J.; Hugon, C.; Illuminati, G.; James, C. W.; Jong, M. de; Jongen, M.; Kadler, M.; Kalekin, O.; Katz, U.; Kießling, D.; Kouchner, A.; Kreter, M.; Kreykenbohm, I.; Kulikovskiy, V.; Lachaud, C.; Lahmann, R.; Lefèvre, D.; Leonora, E.; Lotze, Martín; Loucatos, S.; Marcelin, M.; Margiotta, A.; Marinelli, A.; Martínez-Mora, J. A.; Mele, R.; Melis, K.; Michael, T.; Migliozzi, P.; Moussa, A.; Navas, S.; Nezri, E.; Organokov, M.; Păvălaş, G. E.; Pellegrino, C.; Perrina, C.; Piattelli, P.; Popa, V.; Pradier, T.; Quinn, L.; Racca, C.; Riccobene, G.; Sánchez-Losa, A.; Saldaña, M.; Salvadori, I.; Samtleben, D. F. E.; Sanguineti, M.; Sapienza, P.; Schüßler, F.; Sieger, C.; Spurio, M.; Stolarczyk, Th.; Taiuti, M.; Tayalati, Y.; Trovato, A.; Turpin, D.; Tönnis, Christoph; Vallage, B.; Elewyck, V. Van; Versari, F.; Vivolo, D.; Vizzoca, A.; Wilms, J.; Zornoza, J. D.; Zúñiga, J.

doi:10.1103/physrevd.96.082001

Cited by 81 publications

(104 citation statements)

References 34 publications

(45 reference statements)

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“…No significant clustering of neutrinos above the expected background has been observed so far from any of the current experiments after several years of observations (Aartsen et al 2017a;Albert et al 2017). Active Galactic Nuclei (AGNs) of the blazar category are considered as the main cosmic neutrino source candidates (Mannheim 1995), although it has been suggested, based on the average properties, that they contribute only to a fraction of the observed diffuse flux (Aartsen et al 2017b).…”

Section: Introductionmentioning

confidence: 92%

AGILE Detection of Gamma-Ray Sources Coincident with Cosmic Neutrino Events

Lucarelli

Tavani

Piano

et al. 2019

ApJ

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The origin of cosmic neutrinos is still largely unknown. Using data obtained by the gamma-ray imager on board of the AGILE satellite, we systematically searched for transient gamma-ray sources above 100 MeV that are temporally and spatially coincident with ten recent high-energy neutrino IceCube events. We find three AGILE candidate sources that can be considered possible counterparts to neutrino events. Detecting 3 gamma-ray/neutrino associations out of 10 IceCube events is shown to be unlikely due to a chance coincidence. One of the sources is related to the BL Lac source TXS 2 Lucarelli et al. 0506+056. For the other two AGILE gamma-ray sources there are no obvious known counterparts, and both Galactic and extragalactic origin should be considered.

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Section: Introductionmentioning

confidence: 92%

AGILE Detection of Gamma-Ray Sources Coincident with Cosmic Neutrino Events

Lucarelli

Tavani

Piano

et al. 2019

ApJ

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“…Therefore, the cut value is obtained for each channel by extrapolating the exponential tail of its background distribution and choosing the cut value such that a certain rate of false neutrino candidates from the background distribution is expected. For the ES and DGH (DGL) channels, this rate is one expected false positive event every 50 (20) years of the SD running with design sensitivity. In the DGH (DGL) channel, in order to account for differences in the shower size (shower inclination), a subdivision of events is made based on the number of triggered SD stations (zenith angle).…”

Section: Searches For Ultra-high Energy Neutrinos With Thementioning

confidence: 99%

“…for the flux normalization, assuming flux ∝ E −2 , as a function of the source declination for the different neutrino search channels, for a single flavor assuming a 1:1:1 flavor ratio. Also shown are the limits from IceCube [19] and ANTARES [20]. Note the different energy ranges.…”

Section: Limits On the Diffuse Flux Of Uhe Neutrinos And On Point-likmentioning

confidence: 99%

Ultra-high energy neutrino searches and GW follow-up with the Pierre Auger Observatory

Schimp

2019

Nuclear and Particle Physics Proceedings

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The surface detector array (SD) of the Pierre Auger Observatory is sensitive to neutrinos at energies in the 100 PeV to 100 EeV range. This sensitivity, together with its large acceptance, makes it a complementary detector to other neutrino telescopes, which have their peak sensitivities at lower energies. The neutrino-induced air showers that the SD of the Pierre Auger Observatory is sensitive to can be divided into those induced by interactions of neutrinos of any flavor deep in the atmosphere, and those induced by charged-current interactions of tau neutrinos in the Earth's crust. Both of these types can be efficiently distinguished from cosmic ray-induced air showers, provided that their zenith angles are larger than 60 • . As no neutrino candidates were found in the performed searches, we present limits on the diffuse all-flavor neutrino flux. Using these limits, we obtained constraints on cosmic-ray and neutrino production models. In the light of the recent observations of gravitational waves (GW), we also present the follow-up of LIGO/Virgo GW events. These include binary black hole merger events and also GW170817, the only binary neutron star merger ever observed directly.

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“…upper limits on the total signal flux (sum of the three neutrinos flavours), assuming an E -2 spectrum, are shown (red circles). The dashed red and blue lines are the ANTARES and the IceCube sensitivities [2]. The curves for the sensitivity to neutrino energies under 100 TeV are also included (solid lines).…”

Section: Pos(eps-hep2017)018mentioning

confidence: 99%

Highlights of the ANTARES neutrino telescope results

Margiotta¹

2017

Proceedings of the European Physical Society Conference on High Energy Physics — PoS(EPS-HEP2017)

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The ANTARES neutrino telescope is located in the Mediterranean Sea, at a depth of about 2500 m under the sea level, 40 km off-shore from Toulon. The long attenuation length of the sea water allows for the reconstruction of neutrino direction with an excellent angular resolution. This feature, together with the location of the telescope in the Northern hemisphere, results in competitive sensitivity for neutrino source searches in the Southern Sky at TeV energies. The latest results of the ANTARES analyses for neutrino point sources and for diffuse neutrino emission from the entire sky as well as from several interesting regions such as the Galactic Plane are presented here. An overview of the multi-messenger activities of ANTARES will be given. The results of a search for neutrinos produced in the annihilation of dark matter accumulated in massive objects like the Sun and the Galactic Centre are also presented.

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First all-flavor neutrino pointlike source search with the ANTARES neutrino telescope

Cited by 81 publications

References 34 publications

AGILE Detection of Gamma-Ray Sources Coincident with Cosmic Neutrino Events

AGILE Detection of Gamma-Ray Sources Coincident with Cosmic Neutrino Events

Ultra-high energy neutrino searches and GW follow-up with the Pierre Auger Observatory

Highlights of the ANTARES neutrino telescope results

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