The ANTARES Neutrino Telescope : Contributions to the 34th International Cosmic Ray Conference (ICRC 2015, The Hague)

The ANTARES detector, completed in 2008, is the largest neutrino telescope in the Northern hemisphere. Located at a depth of 2.5 km in the Mediterranean Sea, 40 km off the Toulon shore, its main goal is the search for astrophysical high energy neutrinos. In this paper we collect 22 contributions of the ANTARES collaboration to the 34th International Cosmic Ray Conference (ICRC 2015). The scientific output is very rich and the contributions included in these proceedings cover the main physics results, ranging from steady point sources, diffuse searches, multi-messenger analyses to exotic physics

Searches for point-like and extended neutrino sources close to the galactic center using the antares neutrino telescope

A search for cosmic neutrino sources using six years of data collected by the ANTARES neutrino telescope has been performed. Clusters of muon neutrinos over the expected atmospheric background have been looked for. No clear signal has been found. The most signal-like accumulation of events is located at equatorial coordinates R.A. =-46.°8 and decl. =-64.°9 and corresponds to a 2.2σ background fluctuation. In addition, upper limits on the flux normalization of an E -2 muon neutrino energy spectrum have been set for 50 pre-selected astrophysical objects. Finally, motivated by an accumulation of seven events relatively close to the Galactic Center in the recently reported neutrino sample of the IceCube telescope, a search for point sources in a broad region around this accumulation has been carried out. No indication of a neutrino signal has been found in the ANTARES data and upper limits on the flux normalization of an E -2 energy spectrum of neutrinos from point sources in that region have been set. The 90% confidence level upper limits on the muon neutrino flux normalization vary between 3.5 and 5.1 × 10 -8 GeV cm-2 s-1, depending on the exact location of the source. © 2014. The American Astronomical Society. All rights reserved

Searches for clustering in the time integrated skymap of the ANTARES neutrino telescope

This paper reports a search for spatial clustering of the arrival directions of high energy muon neutrinos detected by the ANTARES neutrino telescope. An improved two-point correlation method is used to study the autocorrelation of 3058 neutrino candidate events as well as cross-correlations with other classes of astrophysical objects: sources of high energy gamma rays, massive black holes and nearby galaxies. No significant deviations from the isotropic distribution of arrival directions expected from atmospheric backgrounds are observed. © 2014 IOP Publishing Ltd and Sissa Medialab srl

A search for neutrino emission from the Fermi bubbles with the ANTARES telescope

Analysis of the Fermi-LAT data has revealed two extended structures above and below the Galactic Centre emitting gamma rays with a hard spectrum, the so-called Fermi bubbles. Hadronic models attempting to explain the origin of the Fermi bubbles predict the emission of high-energy neutrinos and gamma rays with similar fluxes. The ANTARES detector, a neutrino telescope located in the Mediterranean Sea, has a good visibility to the Fermi bubble regions. Using data collected from 2008 to 2011 no statistically significant excess of events is observed and therefore upper limits on the neutrino flux in TeV range from the Fermi bubbles are derived for various assumed energy cutoffs of the source. © 2014 The Author(s)

Measurement of the atmospheric nu (mu) energy spectrum from 100 GeV to 200 TeV with the ANTARES telescope

151Atmospheric neutrinos are produced during cascades initiated by the interaction of primary cosmic rays with air nuclei. In this paper, a measurement of the atmospheric energy spectrum in the energy range 0.1-200 TeV is presented, using data collected by the ANTARES underwater neutrino telescope from 2008 to 2011. Overall, the measured flux is similar to 25 % higher than predicted by the conventional neutrino flux, and compatible with the measurements reported in ice. The flux is compatible with a single power-law dependence with spectral index gamma (meas)=3.58 +/- 0.12. With the present statistics the contribution of prompt neutrinos cannot be established.nonemixedAdrian-Martinez S; Albert A; Al Samarai I; Andre M; Anghinolfi M; Anton G; Anvar S; Ardid M; Astraatmadja T; Aubert JJ; Baret B; Barrios-Marti J; Basa S; Bertin V; Biagi S; Bigongiari C; Bogazzi C; Bouhou B; Bouwhuis MC; Bruijn R; Brunner J; Busto J; Capone A; Caramete L; Carloganu C; Carr J; Cecchini S; Charif Z; Charvis P; Chiarusi T; Circella M; Classen F; Core L; Costantini H; Coyle P; Creusot A; Curtil C; Dekeyser I; Deschamps A; De Bonis G; Decowski MP; Distefano C; Donzaud C; Dornic D; Dorosti Q; Drouhin D; Dumas A; Eberl T; Emanuele U; Enzenhofer A; Ernenwein JP; Escoffier S; Fehn K; Fermani P; Flaminio V; Folger F; Fritsch U; Fusco LA; Galata S; Gay P; Geisselsoder S; Geyer K; Giacomelli G; Giordano V; Gleixner A; Gomez-Gonzalez JP; Graf K; Guillard G; van Haren H; Heijboer AJ; Hello Y; Hernandez-Rey JJ; Herold B; Hossl J; James CW; de Jong M; Kadler M; Kalekin O; Kappes A; Katz U; Kooijman P; Kouchner A; Kreykenbohm I; Kulikovskiy V; Lahmann R; Lambard E; Lambard G; Larosa G; Lattuada D; Lefevre D; Leonora E; Lo Presti D; Loehner H; Loucatos S; Louis F; Mangano S; Marcelin M; Margiotta A; Martinez-Mora JA; Martini S; Michael T; Montaruli T; Morganti M; Motz H; Mueller C; Neff M; Nezri E; Palioselitis D; Pavalas GE; Perrina C; Piattelli P; Popa V; Pradier T; Racca C; Richter R; Riviere C; Robert A; Roensch K; Rostovtsev A; Samtleben DFE; Sanguineti M; Sapienza P; Schmid J; Schnabel J; Schulte S; Schussler F; Seitz T; Shanidze R; Sieger C; Simeone F; Spies A; Spurio M; Steijger JJM; Stolarczyk T; Sanchez-Losa A; Taiuti M; Tamburini C; Tayalati Y; Trovato A; Vallage B; Vallee C; Van Elewyck V; Vernin P; Visser E; Wagner S; Wilms J; de Wolf E; Yatkin K; Yepes H; Zornoza JD; Zuniga JAdrian-Martinez, S; Albert, A; Al Samarai, I; Andre, M; Anghinolfi, M; Anton, G; Anvar, S; Ardid, M; Astraatmadja, T; Aubert, Jj; Baret, B; Barrios-Marti, J; Basa, S; Bertin, V; Biagi, S; Bigongiari, C; Bogazzi, C; Bouhou, B; Bouwhuis, Mc; Bruijn, R; Brunner, J; Busto, J; Capone, A; Caramete, L; Carloganu, C; Carr, J; Cecchini, S; Charif, Z; Charvis, P; Chiarusi, T; Circella, M; Classen, F; Core, L; Costantini, H; Coyle, P; Creusot, A; Curtil, C; Dekeyser, I; Deschamps, A; De Bonis, G; Decowski, Mp; Distefano, C; Donzaud, C; Dornic, D; Dorosti, Q; Drouhin, D; Dumas, A; Eberl, T; Emanuele, U; Enzenhofer, A; Ernenwein, Jp; Escoffier, S; Fehn, K; Fermani, P; Flaminio, V; Folger, F; Fritsch, U; Fusco, La; Galata, S; Gay, P; Geisselsoder, S; Geyer, K; Giacomelli, G; Giordano, V; Gleixner, A; Gomez-Gonzalez, Jp; Graf, K; Guillard, G; van Haren, H; Heijboer, Aj; Hello, Y; Hernandez-Rey, Jj; Herold, B; Hossl, J; James, Cw; de Jong, M; Kadler, M; Kalekin, O; Kappes, A; Katz, U; Kooijman, P; Kouchner, A; Kreykenbohm, I; Kulikovskiy, V; Lahmann, R; Lambard, E; Lambard, G; Larosa, G; Lattuada, D; Lefevre, D; Leonora, E; Lo Presti, D; Loehner, H; Loucatos, S; Louis, F; Mangano, S; Marcelin, M; Margiotta, A; Martinez-Mora, Ja; Martini, S; Michael, T; Montaruli, T; Morganti, M; Motz, H; Mueller, C; Neff, M; Nezri, E; Palioselitis, D; Pavalas, Ge; Perrina, C; Piattelli, P; Popa, V; Pradier, T; Racca, C; Richter, R; Riviere, C; Robert, A; Roensch, K; Rostovtsev, A; Samtleben, Dfe; Sanguineti, M; Sapienza, P; Schmid, J; Schnabel, J; Schulte, S; Schussler, F; Seitz, T; Shanidze, R; Sieger, C; Simeone, F; Spies, A; Spurio, M; Steijger, Jjm; Stolarczyk, T; Sanchez-Losa, A; Taiuti, M; Tamburini, C; Tayalati, Y; Trovato, A; Vallage, B; Vallee, C; Van Elewyck, V; Vernin, P; Visser, E; Wagner, S; Wilms, J; de Wolf, E; Yatkin, K; Yepes, H; Zornoza, Jd; Zuniga,

The Antares Collaboration : Contributions to the 33st International Cosmic Ray Conference (ICRC 2013, Rio de Janeiro)

The ANTARES detector, completed in 2008, is the largest neutrino telescope in the Northern hemisphere. Located at a depth of 2.5 km in the Mediterranean Sea, 40 km off the Toulon shore, its main goal is the search for astrophysical high energy neutrinos. In this paper we collect the 14 contributions of the ANTARES collaboration to the 33rd International Cosmic Ray Conference (ICRC 2013). The scientific output is very rich and the contributions included in these proceedings cover the main physics results, ranging from steady point sources to exotic physics and multi-messenger analyses

Measurement of the atmospheric νμ energy spectrum from 100 GeV to 200 TeV with the ANTARES telescope

Atmospheric neutrinos are produced during cascades initiated by the interaction of primary cosmic rays with air nuclei. In this paper, a measurement of the atmospheric νμ + ν̄μ energy spectrum in the energy range 0.1-200 TeV is presented, using data collected by the ANTARES underwater neutrino telescope from 2008 to 2011. Overall, the measured flux is ~25 % higher than predicted by the conventional neutrino flux, and compatible with the measurements reported in ice. The flux is compatible with a single power-law dependence with spectral index γmeas=3.58±0.12. With the present statistics the contribution of prompt neutrinos cannot be established. © 2013 The Author(s)

Performance of novel VUV-sensitive Silicon Photo-Multipliers for nEXO

Liquid xenon time projection chambers are promising detectors to search for neutrinoless double beta decay (0$\nu \beta \beta$), due to their response uniformity, monolithic sensitive volume, scalability to large target masses, and suitability for extremely low background operations. The nEXO collaboration has designed a tonne-scale time projection chamber that aims to search for 0$\nu \beta \beta$ of \ce{^{136}Xe} with projected half-life sensitivity of $1.35\times 10^{28}$~yr. To reach this sensitivity, the design goal for nEXO is $\leq$1% energy resolution at the decay $Q$-value ($2458.07\pm 0.31$~keV). Reaching this resolution requires the efficient collection of both the ionization and scintillation produced in the detector. The nEXO design employs Silicon Photo-Multipliers (SiPMs) to detect the vacuum ultra-violet, 175 nm scintillation light of liquid xenon. This paper reports on the characterization of the newest vacuum ultra-violet sensitive Fondazione Bruno Kessler VUVHD3 SiPMs specifically designed for nEXO, as well as new measurements on new test samples of previously characterised Hamamatsu VUV4 Multi Pixel Photon Counters (MPPCs). Various SiPM and MPPC parameters, such as dark noise, gain, direct crosstalk, correlated avalanches and photon detection efficiency were measured as a function of the applied over voltage and wavelength at liquid xenon temperature (163~K). The results from this study are used to provide updated estimates of the achievable energy resolution at the decay $Q$-value for the nEXO design

Performance of novel VUV-sensitive Silicon Photo-Multipliers for nEXO

Liquid xenon time projection chambers are promising detectors to search for neutrinoless double beta decay (0$\nu \beta \beta$), due to their response uniformity, monolithic sensitive volume, scalability to large target masses, and suitability for extremely low background operations. The nEXO collaboration has designed a tonne-scale time projection chamber that aims to search for 0$\nu \beta \beta$ of \ce{^{136}Xe} with projected half-life sensitivity of $1.35\times 10^{28}$~yr. To reach this sensitivity, the design goal for nEXO is $\leq$1% energy resolution at the decay $Q$-value ($2458.07\pm 0.31$~keV). Reaching this resolution requires the efficient collection of both the ionization and scintillation produced in the detector. The nEXO design employs Silicon Photo-Multipliers (SiPMs) to detect the vacuum ultra-violet, 175 nm scintillation light of liquid xenon. This paper reports on the characterization of the newest vacuum ultra-violet sensitive Fondazione Bruno Kessler VUVHD3 SiPMs specifically designed for nEXO, as well as new measurements on new test samples of previously characterised Hamamatsu VUV4 Multi Pixel Photon Counters (MPPCs). Various SiPM and MPPC parameters, such as dark noise, gain, direct crosstalk, correlated avalanches and photon detection efficiency were measured as a function of the applied over voltage and wavelength at liquid xenon temperature (163~K). The results from this study are used to provide updated estimates of the achievable energy resolution at the decay $Q$-value for the nEXO design

Search for Gamma-Ray and Neutrino Coincidences Using HAWC and ANTARES Data

In the quest for high-energy neutrino sources, the Astrophysical Multimessenger Observatory Net- work (AMON) has implemented a new search by combining data from the High Altitude Water Cherenkov (HAWC) observatory and the Astronomy with a Neutrino Telescope and Abyss environ- mental RESearch (ANTARES) neutrino telescope. Using the same analysis strategy as in a previous detector combination of HAWC and IceCube data, we perform a search for coincidences in HAWC and ANTARES events that are below the threshold for sending public alerts in each individual detector. Data were collected between July 2015 and February 2020 with a livetime of 4.39 years. Over this time period, 3 coincident events with an estimated false-alarm rate of $< 1$ coincidence per year were found. This number is consistent with background expectations