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First results on new helium based eco-gas mixtures for the Extreme Energy Events Project
M. Abbrescia, C. Avanzini, L. Baldini, R. Baldini Ferroli, G. Batignani, M. Battaglieri, S. Boi, E. Bossini, F. Carnesecchi, F. Cavazza, C. Cicalò, L. Cifarelli, F. Coccetti, E. Coccia, A. Corvaglia, D. De Gruttola, S. De Pasquale, L. Galante, M. Garbini, I. Gnesi, et al (41)
Aug 06 2024 hep-ex physics.ins-det arXiv:2408.01802v2

@misc{2408.01802, author = {M.~Abbrescia and C.~Avanzini and L.~Baldini and R.~Baldini Ferroli and G.~Batignani and M.~Battaglieri and S.~Boi and E.~Bossini and F.~Carnesecchi and F.~Cavazza and C.~Cicalò and L.~Cifarelli and F.~Coccetti and E.~Coccia and A.~Corvaglia and D.~De Gruttola and S.~De Pasquale and L.~Galante and M.~Garbini and I.~Gnesi and F.~Gramegna and S.~Grazzi and D.~Hatzifotiadou and P.~La Rocca and Z.~Liu and G.~Mandaglio and A.~Margotti and G.~Maron and M.~N.~Mazziotta and A.~Mulliri and R.~Nania and F.~Noferini and F.~Nozzoli and F.~Palmonari and M.~Panareo and M.~P.~Panetta and R.~Paoletti and C.~Pellegrino and L.~Perasso and O.~Pinazza and C.~Pinto and S.~Pisano and F.~Riggi and G.~Righini and C.~Ripoli and M.~Rizzi and G.~Sartorelli and E.~Scapparone and M.~Schioppa and G.~Scioli and A.~Scribano and M.~Selvi and M.~Taiuti and G.~Terreni and A.~Trifirò and M.~Trimarchi and C.~Vistoli and L.~Votano and M.~C.~S.~Williams and A.~Zichichi and R.~Zuyeuski}, title = {{F}irst results on new helium based eco-gas mixtures for the {E}xtreme {E}nergy {E}vents {P}roject}, year = {2024}, eprint = {2408.01802}, note = {arXiv:2408.01802v2} }
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The Extreme Energy Events (EEE) Project, a joint project of the Centro Fermi (Museo Storico della Fisica e Centro Studi e Ricerche "E.Fermi") and INFN, has a dual purpose: a scientific research program on cosmic rays at ground level and an intense outreach and educational program. The project consists in a network of about 60 tracking detectors, called telescopes, mostly hosted in Italian High Schools. Each telescope is made by three Multigap Resistive Plate Chambers, operated so far with a gas mixture composed by 98% C$_2$H$_2$F$_4$ and 2% SF$_6$. Due to its high Global Warming Potential, a few years ago the EEE collaboration has started an extensive R&D on alternative mixtures environmentally sustainable and compatible with the current experimental setup and operational environment. Among other gas mixtures, the one with helium and hydrofluoroolefin R1234ze gave the best result during the preliminary tests performed with two of the network telescopes. The detector has proved to reach performance levels comparable to those obtained with previous mixtures, without any modification of the hardware. We will discuss the first results obtained with the new mixture, tested with different percentages of the two components.
Acoustic Positioning for Deep Sea Neutrino Telescopes with a System of Piezo Sensors Integrated into Glass Spheres
A. Albert, S. Alves, M. André, M. Ardid, S. Ardid, J.-J. Aubert, J. Aublin, B. Baret, S. Basa, Y. Becherini, B. Belhorma, M. Bendahman, F. Benfenati, V. Bertin, S. Biagi, J. Boumaaza, M. Bouta, M.C. Bouwhuis, H. Brânzaş, R. Bruijn, et al (120)
May 14 2024 astro-ph.IM physics.ins-det arXiv:2405.07230v1

@misc{2405.07230, author = {A.~Albert and S.~Alves and M.~André and M.~Ardid and S.~Ardid and J.-J.~Aubert and J.~Aublin and B.~Baret and S.~Basa and Y.~Becherini and B.~Belhorma and M.~Bendahman and F.~Benfenati and V.~Bertin and S.~Biagi and J.~Boumaaza and M.~Bouta and M.C.~Bouwhuis and H.~Brânzaş and R.~Bruijn and J.~Brunner and J.~Busto and B.~Caiffi and D.~Calvo and S.~Campion and A.~Capone and F.~Carenini and J.~Carr and V.~Carretero and S.~Celli and L.~Cerisy and M.~Chabab and R.~Cherkaoui El Moursli and T.~Chiarusi and M.~Circella and J.A.B.~Coelho and A.~Coleiro and R.~Coniglione and P.~Coyle and A.~Creusot and A.~F.~Díaz and B.~De Martino and C.~Distefano and I.~Di Palma and C.~Donzaud and D.~Dornic and D.~Drouhin and T.~Eberl and A.~Eddymaoui and T.~van Eeden and D.~van Eijk and S.~El Hedri and N.~El Khayati and A.~Enzenhöfer and P.~Fermani and G.~Ferrara and F.~Filippini and L.~Fusco and S.~Gagliardini and J.~García and C.~Gatius Oliver and P.~Gay and N.~Geißelbrecht and H.~Glotin and R.~Gozzini and R.~Gracia Ruiz and K.~Graf and C.~Guidi and L.~Haegel and H.~van Haren and A.J.~Heijboer and Y.~Hello and L.~Hennig and J.J.~Hernández-Rey and J.~Hößl and F.~Huang and G.~Illuminati and B.~Jisse-Jung and M.~de Jong and P.~de Jong and M.~Kadler and O.~Kalekin and U.~Katz and A.~Kouchner and I.~Kreykenbohm and V.~Kulikovskiy and R.~Lahmann and M.~Lamoureux and A.~Lazo and D.~Lefèvre and E.~Leonora and G.~Levi and S.~Le Stum and S.~Loucatos and J.~Manczak and M.~Marcelin and A.~Margiotta and A.~Marinelli and J.A.~Martínez-Mora and P.~Migliozzi and A.~Moussa and R.~Muller and S.~Navas and E.~Nezri and B.~Ó Fearraigh and E.~Oukacha and A.~Păun and G.E.~Păvălaş and S.~Peña-Martínez and M.~Perrin-Terrin and P.~Piattelli and C.~Poirè and V.~Popa and T.~Pradier and N.~Randazzo and D.~Real and G.~Riccobene and A.~Romanov and A.~Sánchez-Losa and A.~Saina and F.~Salesa Greus and D.~F.~E.~Samtleben and M.~Sanguineti and P.~Sapienza and F.~Schüssler and J.~Seneca and M.~Spurio and Th.~Stolarczyk and M.~Taiuti and Y.~Tayalati and B.~Vallage and G.~Vannoye and V.~Van Elewyck and S.~Viola and D.~Vivolo and J.~Wilms and S.~Zavatarelli and A.~Zegarelli and J.D.~Zornoza and J.~Zúñiga}, title = {{A}coustic {P}ositioning for {D}eep {S}ea {N}eutrino {T}elescopes with a {S}ystem of {P}iezo {S}ensors {I}ntegrated into {G}lass {S}pheres}, year = {2024}, eprint = {2405.07230}, note = {arXiv:2405.07230v1} }
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Position calibration in the deep sea is typically done by means of acoustic multilateration using three or more acoustic emitters installed at known positions. Rather than using hydrophones as receivers that are exposed to the ambient pressure, the sound signals can be coupled to piezo ceramics glued to the inside of existing containers for electronics or measuring instruments of a deep sea infrastructure. The ANTARES neutrino telescope operated from 2006 until 2022 in the Mediterranean Sea at a depth exceeding 2000m. It comprised nearly 900 glass spheres with 432mm diameter and 15mm thickness, equipped with photomultiplier tubes to detect Cherenkov light from tracks of charged elementary particles. In an experimental setup within ANTARES, piezo sensors have been glued to the inside of such - otherwise empty - glass spheres. These sensors recorded signals from acoustic emitters with frequencies from 46545 to 60235Hz. Two waves propagating through the glass sphere are found as a result of the excitation by the waves in the water. These can be qualitatively associated with symmetric and asymmetric Lamb-like waves of zeroth order: a fast (early) one with $v_e \approx 5$mm/$\mu$s and a slow (late) one with $v_\ell \approx 2$mm/$\mu$s. Taking these findings into account improves the accuracy of the position calibration. The results can be transferred to the KM3NeT neutrino telescope, currently under construction at multiple sites in the Mediterranean Sea, for which the concept of piezo sensors glued to the inside of glass spheres has been adapted for monitoring the positions of the photomultiplier tubes.
The Power Board of the KM3NeT Digital Optical Module: design, upgrade, and production
S. Aiello, A. Albert, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, E. Androutsou, M. Anguita, L. Aphecetche, M. Ardid, S. Ardid, H. Atmani, J. Aublin, F. Badaracco, L. Bailly-Salins, Z. Bardacova, B. Baret, A. Bariego Quintana, S. Basegmez du Pree, et al (264)
Nov 28 2023 astro-ph.IM physics.ins-det arXiv:2311.14872v1

@misc{2311.14872, author = {S.~Aiello and A.~Albert and S.~Alves Garre and Z.~Aly and A.~Ambrosone and F.~Ameli and M.~Andre and E.~Androutsou and M.~Anguita and L.~Aphecetche and M.~Ardid and S.~Ardid and H.~Atmani and J.~Aublin and F.~Badaracco and L.~Bailly-Salins and Z.~Bardacova and B.~Baret and A.~Bariego Quintana and S.~Basegmez du Pree and Y.~Becherini and M.~Bendahman and F.~Benfenati and M.~Benhassi and D.~M.~Benoit and E.~Berbee and V.~Bertin and V.~van Beveren and S.~Biagi and M.~Boettcher and D.~Bonanno and J.~Boumaaza and M.~Bouta and M.~Bouwhuis and C.~Bozza and R.~M.~Bozza and H.Branzas and F.~Bretaudeau and R.~Bruijn and J.~Brunner and R.~Bruno and E.~Buis and R.~Buompane and J.~Busto and B.~Caiffi and D.~Calvo and S.~Campion and A.~Capone and F.~Careniniu and V.~Carretero and T.~Cartraud and P.~Castaldi and V.~Cecchini and S.~Celli and L.~Cerisy and M.~Chabab and M.~Chadolias and C.~Champion and A.~Chena and S.~Cherubini and T.~Chiarusi and M.~Circella and R.~Cocimano and J.~A.~B.~Coelho and A.~Coleiro and S.~Colonges and R.~Coniglione and P.~Coyle and A.~Creusot and G.~Cuttone and R.~Dallier and Y.~Darras and A.~De Benedittis and B.~De Martino and V.~Decoene and R.~Del Burgo and I.~Del Rosso and U.~M.~Di Cerbo and L.~S.~Di Mauro and I.~Di Palma and A.~F.~Díaz and C.~Diaz and D.~Diego-Tortosa and C.~Distefano and A.~Domia and C.~Donzaud and D.~Dornic and M.~Dorra and E.~Drakopoulou and D.~Drouhin and R.~Dvornicky and T.~Eberla and E.~Eckerova and A.~Eddymaoui and T.~van Eeden and M.~Eff and D.~van Eijk and I.~El Bojaddaini and S.~El Hedri and A.~Enzenhofer and G.~Ferrara and M.~D.~Filipovica and F.~Filippini and D.~Franciotti and L.~A.~Fusco and O.~Gabellaa and J.~Gabriela and S.~Gagliardini and T.~Gal and J.~Garcıa Mendez and A.~Garcia Soto and C.~Gatius Oliver and N.~Geißelbrecht and H.~Ghaddari and L.~Gialanella and B.~K.~Gibson and E.~Giorgio and I.~Goos and P.~Goswami and D.~Goupilliere and S.~R.~Gozzini and R.~Gracia and K.~Grafa and C.~Guidi and B.~Guillon and M.~Gutierrez and H.~van Haren and A.~Heijboer and A.~Hekalo and L.~Henniga and J.~J.~Hernandez-Rey and W.~Idrissi Ibnsalih and G.~Illuminati and P.~Jansweijer and M.~de Jonga and P.~de Jonga and B.~J.~Jung and P.~Kalaczynski and O.~Kalekin and U.~F.~Katz and A.~Khatun and G.~Kistauri and C.~Kopper and A.~Kouchner and V.~Kueviakoe and V.~Kulikovskiy and R.~Kvatadze and M.~Labalme and R.~Lahmann and G.~Larosa and C.~Lastoria and A.~Lazo and S.~Le Stum and G.~Lehaut and E.~Leonora and N.~Lessing and G.~Levi and M.~Lindsey Clark and P.~Litrico and F.~Longhitano and J.~Majumdar and L.~Malerba and F.~Mamedov and J.~Manczak and A.~Manfredae and M.~Marconi and A.~Margiotta and A.~Marinelli and C.~Markou and L.~Martin and J.~A.~Martınez-Mora and F.~Marzaioli and M.~Mastrodicasa and S.~Mastroianni and S.~Miccich and G.~Miele and P.~Migliozzi and E.~Migneco and S.~Minutoli and M.~L.~Mitsou and C.~M.~Mollo and L.~Morales-Gallegos and M.~Morga and A.~Moussa and I.~Mozun Mateo and R.~Muller and P.~Musico and M.~R.~Musone and M.~Musumeci and S.~Navas and A.~Nayerhoda and C.~A.~Nicolau and B.~Nkosi and B.~O.~Fearraigh and V.~Oliviero and A.~Orlando and E.~Oukacha and D.~Paesani and J.~Palacios Gonzalez and G.~Papalashvili and V.~Parisi and E.J.~Pastor Gomez and A.~M.~Pauna and G.~E.~Pavalas and G.~Pellegrini and S.~Peñaa Martinez and M.~Perrin-Terrin and J.~Perronnel and V.~Pestel and R.~Pestes and P.~Piattelli and C.~Poirre and V.~Popa and T.~Pradier and J.~Prado and S.~Pulvirenti and G.~Quemener and C.A.~Quiroz-Rangel and U.~Rahaman and N.~Randazzo and R.~Randriatoamana and S.~Razzaque and I.~C.~Rea and D.~Real and G.~Riccobene and J.~Robinson and A.~Romanov and A.~Saina and F.~Salesa Greus and D.~F.~E.~Samtleben and A.~Sanchez Losa and S.~Sanfilippo and M.~Sanguineti and C.~Santonastaso and D.~Santonocito and P.~Sapienza and J.~Schmelling and J.~Schnabel and J.~Schumann and H.~M.~Schutt and J.~Seneca and N.~Sennan and B.~Setter and I.~Sgura and R.~Shanidze and A.~Sharma and Y.~Shitov and F.~Simkovic and A.~Simonelli and A.~Sinopoulou and M.V.~Smirnov and B.~Spisso and M.~Spurio and D.~Stavropoulos and I.~Stekl and M.~Taiuti and Y.~Tayalati and H.~Thiersen and I.~Tosta e Melo and E.~Tragi and B.~Trocme and V.~Tsourapis and E.~Tzamariudaki and A.~Vacheret and A.~Valer Melchor and V.~Valsecchi and V.~Van Elewyck and G.~Vannoye and G.~Vasileiadis and F.~Vazquez de Sola and C.~Verilhac and A.~Veutro and S.~Viola and D.~Vivolo and J.~Wilms and E.~de Wolf and H.~Yepes Ramirez and G.~Zarpapis and S.~Zavatarelli and A.~Zegarelli and D.~Zito and J.~D.~Zornoza and J.~Zuniga and N.~Zywuck}, title = {{T}he {P}ower {B}oard of the {KM}3{N}e{T} {D}igital {O}ptical {M}odule: design, upgrade, and production}, year = {2023}, eprint = {2311.14872}, note = {arXiv:2311.14872v1} }
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The KM3NeT Collaboration is building an underwater neutrino observatory at the bottom of the Mediterranean Sea consisting of two neutrino telescopes, both composed of a three-dimensional array of light detectors, known as digital optical modules. Each digital optical module contains a set of 31 three inch photomultiplier tubes distributed over the surface of a 0.44 m diameter pressure-resistant glass sphere. The module includes also calibration instruments and electronics for power, readout and data acquisition. The power board was developed to supply power to all the elements of the digital optical module. The design of the power board began in 2013, and several prototypes were produced and tested. After an exhaustive validation process in various laboratories within the KM3NeT Collaboration, a mass production batch began, resulting in the construction of over 1200 power boards so far. These boards were integrated in the digital optical modules that have already been produced and deployed, 828 until October 2023. In 2017, an upgrade of the power board, to increase reliability and efficiency, was initiated. After the validation of a pre-production series, a production batch of 800 upgraded boards is currently underway. This paper describes the design, architecture, upgrade, validation, and production of the power board, including the reliability studies and tests conducted to ensure the safe operation at the bottom of the Mediterranean Sea throughout the observatory's lifespan
Ecological transition for the gas mixtures of the MRPC cosmic ray telescopes of the EEE Project
C. Ripoli, M. Abbrescia, C. Avanzini, L. Baldini, R. Baldini Ferroli, G. Batignani, M. Battaglieri, S. Boi, E. Bossini, F. Carnesecchi, D. Cavazza, C. Cicalò, L. Cifarelli, F. Coccetti, E. Coccia, A. Corvaglia, D. De Gruttola, S. De Pasquale, L. Galante, M. Garbini, et al (45)
Oct 02 2023 hep-ex physics.ins-det arXiv:2309.17375v1

@misc{2309.17375, author = {C.~Ripoli and M.~Abbrescia and C.~Avanzini and L.~Baldini and R.~Baldini Ferroli and G.~Batignani and M.~Battaglieri and S.~Boi and E.~Bossini and F.~Carnesecchi and D.~Cavazza and C.~Cicalò and L.~Cifarelli and F.~Coccetti and E.~Coccia and A.~Corvaglia and D.~De Gruttola and S.~De Pasquale and L.~Galante and M.~Garbini and I.~Gnesi and E.~Gramstad and S.~Grazzi and E.S.~Håland and D.~Hatzifotiadou and P.~La Rocca and Z.~Liu and L.~Lombardo and G.~Mandaglio and A.~Margotti and G.~Maron and M.~N.~Mazziotta and A.~Mulliri and R.~Nania and F.~Noferini and F.~Nozzoli and F.~Ould-Saada and F.~Palmonari and M.~Panareo and M.~P.~Panetta and R.~Paoletti and M.~Parvis and C.~Pellegrino and L.~Perasso and O.~Pinazza and C.~Pinto and S.~Pisano and F.~Riggi and G.~Righini and M.~Rizzi and G.~Sartorelli and E.~Scapparone and M.~Schioppa and G.~Scioli and A.~Scribano and M.~Selvi and M.~Taiuti and G.~Terreni and A.~Trifirò and M.~Trimarchi and C.~Vistoli and L.~Votano and M.~C.~S.~Williams and A.~Zichichil and R.~Zuyeuskiv}, title = {{E}cological transition for the gas mixtures of the {MRPC} cosmic ray telescopes of the {EEE} {P}roject}, year = {2023}, eprint = {2309.17375}, note = {arXiv:2309.17375v1} }
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The Extreme Energy Events (EEE) Collaboration is fully involved in an ecological transition. The use of the standard gas mixture, \ceC_2H_2F_4+ \ceSF_6, has stopped in favor of an alternative green mixture based on \ceC_3H_2F_4 with the addition of He or \ceCO_2. The choise of these new mixtures is motivated by the significant lower Global Warming Potential (GWP) to reduce the emission of gases potentially contributing to the greenhouse effect. The EEE experiment consists of 61 muon telescopes based on Multigap Resistive Plate Chambers (MRPCs), each telescope composed of 3 chambers filled with gas. Several EEE detectors are today completely fluxed with the new ecological mixture. This contribution will report recent results about the telescope performance obtained from studies with the eco-friendly alternative mixture carried out in the last years.
Studying Bioluminescence Flashes with the ANTARES Deep Sea Neutrino Telescope
N. Reeb, S. Hutschenreuter, P. Zehetner, T. Ensslin, S. Alves, M. André, M. Anghinolfi, G. Anton, M. Ardid, J.-J. Aubert, J. Aublin, B. Baret, S. Basa, B. Belhorma, M. Bendahman, V. Bertin, S. Biagi, M. Bissinger, J. Boumaaza, M. Bouta, et al (124)
Jul 20 2021 physics.ao-ph astro-ph.IM q-bio.PE arXiv:2107.08063v1

@misc{2107.08063, author = {N.~Reeb and S.~Hutschenreuter and P.~Zehetner and T.~Ensslin and S.~Alves and M.~André and M.~Anghinolfi and G.~Anton and M.~Ardid and J.-J.~Aubert and J.~Aublin and B.~Baret and S.~Basa and B.~Belhorma and M.~Bendahman and V.~Bertin and S.~Biagi and M.~Bissinger and J.~Boumaaza and M.~Bouta and M.C.~Bouwhuis and H.~Brânzaş and R.~Bruijn and J.~Brunner and J.~Busto and B.~Caiffi and A.~Capone and L.~Caramete and J.~Carr and V.~Carretero and S.~Celli and M.~Chabab and T.~N.~Chau and R.~Cherkaoui El Moursli and T.~Chiarusi and M.~Circella and A.~Coleiro and M.~Colomer-Molla and R.~Coniglione and P.~Coyle and A.~Creusot and A.~F.~Díaz and G.~de Wasseige and A.~Deschamps and C.~Distefano and I.~Di Palma and A.~Domi and C.~Donzaud and D.~Dornic and D.~Drouhin and T.~Eberl and T.~van Eeden and N.~El Khayati and A.~Enzenhöfer and P.~Fermani and G.~Ferrara and F.~Filippini and L.~Fusco and Y.~Gatelet and P.~Gay and H.~Glotin and R.~Gozzini and R.~Gracia Ruiz and K.~Graf and C.~Guidi and S.~Hallmann and H.~van Haren and A.J.~Heijboer and Y.~Hello and J.J.~Hernández-Rey and J.~Hößl and J.~Hofestädt and F.~Huang and G.~Illuminati and C.~W.~James and B.~Jisse-Jung and M.~d.~Jong and P.~d.~Jong and M.~Jongen and M.~Kadler and O.~Kalekin and U.~Katz and N.R.~Khan-Chowdhury and A.~Kouchner and I.~Kreykenbohm and V.~Kulikovskiy and R.~Lahmann and R.~Le Breton and D.~Lefèvre and E.~Leonora and G.~Levi and M.~Lincetto and D.~Lopez-Coto and S.~Loucatos and L.~Maderer and J.~Manczak and M.~Marcelin and A.~Margiotta and A.~Marinelli and J.A.~Martínez-Mora and K.~Melis and P.~Migliozzi and A.~Moussa and R.~Muller and L.~Nauta and S.~Navas and E.~Nezri and B.~Ó Fearraigh and M.~Organokov and G.E.~Păvălaş and C.~Pellegrino and M.~Perrin-Terrin and P.~Piattelli and C.~Pieterse and C.~Poirè and V.~Popa and T.~Pradier and N.~Randazzo and S.~Reck and G.~Riccobene and A.~Romanov and A.~Sánchez-Losa and F.~Salesa Greus and D.~F.~E.~Samtleben and M.~Sanguineti and P.~Sapienza and J.~Schnabel and J.~Schumann and F.~Schüssler and M.~Spurio and Th.~Stolarczyk and M.~Taiuti and Y.~Tayalati and S.J.~Tingay and B.~Vallage and V.~Van Elewyck and F.~Versari and S.~Viola and D.~Vivolo and J.~Wilms and S.~Zavatarelli and A.~Zegarelli and J.D.~Zornoza and J.~Zúñiga}, title = {{S}tudying {B}ioluminescence {F}lashes with the {ANTARES} {D}eep {S}ea {N}eutrino {T}elescope}, year = {2021}, eprint = {2107.08063}, note = {arXiv:2107.08063v1} }
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We develop a novel technique to exploit the extensive data sets provided by underwater neutrino telescopes to gain information on bioluminescence in the deep sea. The passive nature of the telescopes gives us the unique opportunity to infer information on bioluminescent organisms without actively interfering with them. We propose a statistical method that allows us to reconstruct the light emission of individual organisms, as well as their location and movement. A mathematical model is built to describe the measurement process of underwater neutrino telescopes and the signal generation of the biological organisms. The Metric Gaussian Variational Inference algorithm is used to reconstruct the model parameters using photon counts recorded by the neutrino detectors. We apply this method to synthetic data sets and data collected by the ANTARES neutrino telescope. The telescope is located 40 km off the French coast and fixed to the sea floor at a depth of 2475 m. The runs with synthetic data reveal that we can reliably model the emitted bioluminescent flashes of the organisms. Furthermore, we find that the spatial resolution of the localization of light sources highly depends on the configuration of the telescope. Precise measurements of the efficiencies of the detectors and the attenuation length of the water are crucial to reconstruct the light emission. Finally, the application to ANTARES data reveals the first precise localizations of bioluminescent organisms using neutrino telescope data.
The cosmic muon and detector simulation framework of the Extreme Energy Events (EEE) experiment
M. Abbrescia, C. Avanzini, L. Baldini, R. Baldini Ferroli, G. Batignani, M. Battaglieri, S. Boi, E. Bossin, F. Carnesecchi, C. Cicalò, L. Cifarelli, F. Coccetti, E. Coccia, A. Corvaglia, D. De Gruttola, S. De Pasquale, F. Fabbri, A. Fulci, L. Galante, M. Garbini, et al (43)
Apr 14 2021 physics.ins-det arXiv:2104.06012v1

@misc{2104.06012, author = {M.~Abbrescia and C.~Avanzini and L.~Baldini and R.~Baldini Ferroli and G.~Batignani and M.~Battaglieri and S.~Boi and E.~Bossin and F.~Carnesecchi and C.~Cicalò and L.~Cifarelli and F.~Coccetti and E.~Coccia and A.~Corvaglia and D.~De Gruttola and S.~De Pasquale and F.~Fabbri and A.~Fulci and L.~Galante and M.~Garbini and G.~Gemme and I.~Gnesi and S.~Grazzi and D.~Hatzifotiadou and P.~La Rocca and Z.~Liu and G.~Mandaglio and G.~Maron and M.~N.~Mazziotta and A.~Mulliri and R.~Nania and F.~Noferini and F.~Nozzoli and F.~Palmonari and M.~Panareo and M.~P.~Panetta and R.~Paoletti and C.~Pellegrino and O.~Pinazza and C.~Pinto and S.~Pisano and F.~Riggi and G.~Righini and C.~Ripoli and M.~Rizzi and G.~Sartorelli and E.~Scapparone and M.~Schioppa and A.~Scribano and M.~Selvi and G.~Serri and S Squarcia and M.~Taiuti and G.~Terreni and A.~Trifirò and M.~Trimarchi and A.S.~Triolo and C.~Vistoli and L.~Votano and M.~Ungaro and M.~C.~S.~Williams and A.~Zichichi and R.~Zuyeuski}, title = {{T}he cosmic muon and detector simulation framework of the {E}xtreme {E}nergy {E}vents ({EEE}) experiment}, year = {2021}, eprint = {2104.06012}, note = {arXiv:2104.06012v1} }
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This paper describes the simulation framework of the Extreme Energy Events (EEE) experiment. EEE is a network of cosmic muon trackers, each made of three Multi-gap Resistive Plate Chambers (MRPC), able to precisely measure the absolute muon crossing time and the muon integrated angular flux at the ground level. The response of a single MRPC and the combination of three chambers have been implemented in a GEANT4-based framework (GEMC) to study the telescope response. The detector geometry, as well as details about the surrounding materials and the location of the telescopes have been included in the simulations in order to realistically reproduce the experimental set-up of each telescope. A model based on the latest parametrization of the cosmic muon flux has been used to generate single muon events. After validating the framework by comparing simulations to selected EEE telescope data, it has been used to determine detector parameters not accessible by analysing experimental data only, such as detection efficiency, angular and spatial resolution.
Strategies to reduce the environmental impact in the MRPC array of the EEE experiment
M.P. Panetta, M. Abbrescia, C. Avanzini, L. Baldini, R. Baldini Ferroli, G. Batignani, M. Battaglieri, S. Boi, E. Bossini, F. Carnesecchi, C. Cicalò, L. Cifarelli, F. Coccetti, E. Coccia, A. Corvaglia, D. De Gruttola, S. De Pasquale, F. Fabbri, D. Falchieri, L. Galante, et al (44)
Jul 01 2020 physics.ins-det astro-ph.IM hep-ex arXiv:2006.16773v2

@misc{2006.16773, author = {M.P.~Panetta and M.~Abbrescia and C.~Avanzini and L.~Baldini and R.~Baldini Ferroli and G.~Batignani and M.~Battaglieri and S.~Boi and E.~Bossini and F.~Carnesecchi and C.~Cicalò and L.~Cifarelli and F.~Coccetti and E.~Coccia and A.~Corvaglia and D.~De Gruttola and S.~De Pasquale and F.~Fabbri and D.~Falchieri and L.~Galante and M.~Garbini and G.~Gemme and I.~Gnesi and S.~Grazzi and D.~Hatzifotiadou and P.~La Rocca and Z.~Liu and L.~Lombardo and G.~Mandaglio and G.~Maron and M.~N.~Mazziotta and A.~Mulliri and R.~Nania and F.~Noferini and F.~Nozzoli and F.~Palmonari and M.~Panareo and R.~Paoletti and M.~Parvis and C.~Pellegrino and L.~Perasso and O.~Pinazza and C.~Pinto and S.~Pisano and F.~Riggi and G.~Righini and C.~Ripoli and M.~Rizzi and G.~Sartorelli and E.~Scapparone and M.~Schioppa and A.~Scribano and M.~Selvi and G.~Serri and S.~Squarcia and M.~Taiuti and G.~Terreni and A.~Trifirò and M.~Trimarchi and C.~Vistoli and L.~Votano and M.~C.~S.~Williams and A.~Zichichi and R.~Zuyeuski}, title = {{S}trategies to reduce the environmental impact in the {MRPC} array of the {EEE} experiment}, year = {2020}, eprint = {2006.16773}, note = {arXiv:2006.16773v2} }
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The Extreme Energy Events (EEE) Project employs Multi-gap Resistive Plate Chamber (MRPC) for studying the secondary cosmic ray muons in Extensive Air Showers. The array consists of about 60 tracking detectors, sparse on Italian territory and at CERN. The MRPCs are flowed with a gas mixture based on $C_2H_2F_4$ and $SF_6$, both of which are fluorinated greenhouse gases with a high environmental impact on the atmosphere. Due to the restrictions imposed by the European Union, these gases are being phased out of production and their cost is largely increasing. The EEE Collaboration started a campaign to reduce the gas emission from its array with the aim of containing costs and decreasing the experiment global warming impact. One method is to reduce the gas rate in each EEE detector. Another is to develop a gas recirculation system, whose a first prototype has been installed at one of the EEE stations located at CERN. Jointly a parallel strategy is focused on searching for environmental friendly gas mixtures which are able to substitute the standard mixture without affecting the MRPC performance. An overview and first results are presented here.
Characteristics and performance of the Multigap Resistive Plate Chambers of the EEE experiment
F. Coccetti, M. Abbrescia, C. Avanzini, L. Baldini, R. Baldini Ferroli, G. Batignani, M. Battaglieri, S. Boi, E. Bossini, F. Carnesecchi, C. Cicalò, L. Cifarelli, E. Coccia, A. Corvaglia, D. De Gruttola, S. De Pasquale, F. Fabbri, D. Falchieri, L. Galante, M. Garbini, et al (44)
Jun 04 2020 physics.ins-det arXiv:2006.02002v2

@misc{2006.02002, author = {F.~Coccetti and M.~Abbrescia and C.~Avanzini and L.~Baldini and R.~Baldini Ferroli and G.~Batignani and M.~Battaglieri and S.~Boi and E.~Bossini and F.~Carnesecchi and C.~Cicalò and L.~Cifarelli and E.~Coccia and A.~Corvaglia and D.~De Gruttola and S.~De Pasquale and F.~Fabbri and D.~Falchieri and L.~Galante and M.~Garbini and G.~Gemme and I.~Gnesi and S.~Grazzi and D.~Hatzifotiadou and P.~La Rocca and Z.~Liu and L.~Lombardo and G.~Mandaglio and G.~Maron and M.~N.~Mazziotta and A.~Mulliri and R.~Nania and F.~Noferini and F.~Nozzoli and F.~Palmonari and M.~Panareo and M.~P.~Panetta and R.~Paoletti and M.~Parvis and C.~Pellegrino and L.~Perasso and O.~Pinazza and C.~Pinto and S.~Pisano and F.~Riggi and G.~Righini and C.~Ripoli and M.~Rizzi and G.~Sartorelli and E.~Scapparone and M.~Schioppa and A.~Scribano and M.~Selvi and G.~Serri and S Squarcia and M.~Taiuti and G.~Terreni and A.~Trifirò and M.~Trimarchi and C.~Vistoli and L.~Votano and M.~C.~S.~Williams and A.~Zichichi and R.~Zuyeuski}, title = {{C}haracteristics and performance of the {M}ultigap {R}esistive {P}late {C}hambers of the {EEE} experiment}, year = {2020}, eprint = {2006.02002}, note = {arXiv:2006.02002v2} }
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The Extreme Energy Events (EEE) experiment, dedicated to the study of secondary cosmic rays, is arguably the largest detector system in the world implemented by Multigap Resistive Plate Chambers. The EEE network consists of 60 telescopes distributed over all the Italian territory; each telescope is made of three MRPCs and allows to reconstruct the trajectory of cosmic muons with high efficiency and optimal angular resolution. A distinctive feature of the EEE network is that almost all telescopes are housed in High Schools and managed by groups of students and teachers, who previously took care of their construction at CERN. This peculiarity is a big plus for the experiment, which combines the scientific relevance of its objectives with effective outreach activities. The unconventional location of the detectors, mainly in standard classrooms of school buildings, with heterogeneous maintenance conditions and without controlled temperature and dedicated power lines, is a unique test field to verify the robustness, the low aging characteristics and the long-lasting performance of MRPC technology for particle monitoring and timing. Finally, it is reported how the spatial resolution, efficiency, tracking capability and stability of these chambers behave in time.
A simulation tool for MRPC telescopes of the EEE project
G. Mandaglio, M. Abbrescia, C. Avanzini, L. Baldini, R. Baldini Ferroli, G. Batignani, M. Battaglieri, S. Boi, E. Bossin, F. Carnesecchi, C. Cicalò, L. Cifarelli, F. Coccetti, E. Coccia, A. Corvaglia, D. De Gruttola, S. De Pasquale, F. Fabbri, A. Fulci, D. Falchieri, et al (46)
Jun 01 2020 physics.ins-det arXiv:2005.14644v2

@misc{2005.14644, author = {G.~Mandaglio and M.~Abbrescia and C.~Avanzini and L.~Baldini and R.~Baldini Ferroli and G.~Batignani and M.~Battaglieri and S.~Boi and E.~Bossin and F.~Carnesecchi and C.~Cicalò and L.~Cifarelli and F.~Coccetti and E.~Coccia and A.~Corvaglia and D.~De Gruttola and S.~De Pasquale and F.~Fabbri and A.~Fulci and D.~Falchieri and L.~Galante and M.~Garbini and G.~Gemme and I.~Gnesi and S.~Grazzi and D.~Hatzifotiadou and P.~La Rocca and Z.~Liu and L.~Lombardo and G.~Maron and M.~N.~Mazziotta and A.~Mulliri and R.~Nania and F.~Noferini and F.~Nozzoli and F.~Palmonari and M.~Panareo and M.~P.~Panetta and R.~Paoletti and M.~Parvis and C.~Pellegrino and L.~Perasso and O.~Pinazza and C.~Pinto and S.~Pisano and F.~Riggi and G.~Righini and C.~Ripoli and M.~Rizzi and G.~Sartorelli and E.~Scapparone and M.~Schioppa and A.~Scribano and M.~Selvi and G.~Serri and S Squarcia and M.~Taiuti and G.~Terreni and A.~Trifirò and M.~Trimarchi and A.S.~Triolo and C.~Vistoli and L.~Votano and M.~C.~S.~Williams and A.~Zichichi and R.~Zuyeuski}, title = {{A} simulation tool for {MRPC} telescopes of the {EEE} project}, year = {2020}, eprint = {2005.14644}, note = {arXiv:2005.14644v2} }
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The Extreme Energy Events (EEE) Project is mainly devoted to the study of the secondary cosmic ray radiation by using muon tracker telescopes made of three Multigap Resistive Plate Chambers (MRPC) each. The experiment consists of a telescope network mainly distributed across Italy, hosted in different building structures pertaining to high schools, universities and research centers. Therefore, the possibility to take into account the effects of these structures on collected data is important for the large physics programme of the project. A simulation tool, based on GEANT4 and using GEMC framework, has been implemented to take into account the muon interaction with EEE telescopes and to estimate the effects on data of the structures surrounding the experimental apparata.A dedicated event generator producing realistic muon distributions, detailed geometry and microscopic behavior of MRPCs have been included to produce experimental-like data. The comparison between simulated and experimental data, and the estimation of detector resolutions is here presented and discussed.
MRPC Telescope Simulation for the Extreme Energy Events Experiment
G. Mandaglio, M. Abbrescia, C. Avanzini, L. Baldini, R. Baldini Ferroli, G. Batignani, M. Battaglieri, S. Boi, E. Bossini, F. Carnesecchi, C. Cicalò, L. Cifarelli, F. Coccetti, E. Coccia, A. Corvaglia, D. De Gruttola, S. De Pasquale, F. Fabbri, A. Fulci, L. Galante, et al (44)
Apr 21 2020 physics.ins-det arXiv:2004.08651v2

@misc{2004.08651, author = {G.~Mandaglio and M.~Abbrescia and C.~Avanzini and L.~Baldini and R.~Baldini Ferroli and G.~Batignani and M.~Battaglieri and S.~Boi and E.~Bossini and F.~Carnesecchi and C.~Cicalò and L.~Cifarelli and F.~Coccetti and E.~Coccia and A.~Corvaglia and D.~De Gruttola and S.~De Pasquale and F.~Fabbri and A.~Fulci and L.~Galante and P.~Galeotti and M.~Garbini and G.~Gemme and I.~Gnesi and S.~Grazzi and D.~Hatzifotiadou and P.~La Rocca and Z.~Liu and G.~Maron and M.~N.~Mazziotta and A.~Mulliri and R.~Nania and F.~Noferini and F.~Nozzoli and F.~Palmonari and M.~Panareo and M.~P.~Panetta and R.~Paoletti and C.~Pellegrino and L.~Perasso and C.~Pinto and G.~Piragino and S.~Pisano and F.~Riggi and G.~Righini and C.~Ripoli and M.~Rizzi and G.~Sartorelli and E.~Scapparone and M.~Schioppa and A.~Scribano and M.~Selvi and G.~Serri and S Squarcia and M.~Taiuti and G.~Terreni and A.~Trifirò and M.~Trimarchi and A.S.~Triolo and C.~Vistoli and L.~Votano and M.~C.~S.~Williams and A.~Zichichi and R.~Zuyeuski}, title = {{MRPC} {T}elescope {S}imulation for the {E}xtreme {E}nergy {E}vents {E}xperiment}, year = {2020}, eprint = {2004.08651}, note = {arXiv:2004.08651v2} }
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A simulation tool based on GEMC framework to describe the MRPC telescope of the Extreme Energy Events (EEE) Project is presented. The EEE experiment is mainly devoted to the study of the secondary cosmic muons by using MRPC telescope distributed in high schools and research centres in Italy and at CERN. This takes into account the muon interactions with EEE telescopes and the structures surrounding the experimental apparata; it consists of a dedicated event generator producing realistic muon distribution and a detailed geometry description of the detector. Microscopic behaviour of MRPCs has been included to produce experimental-like data. A method to estimate the chamber effciency directly from data has been implemented and tested by comparing the experimental and simulated polar angle distribution of muons.
Event reconstruction for KM3NeT/ORCA using convolutional neural networks
Sebastiano Aiello, Arnauld Albert, Sergio Alves Garre, Zineb Aly, Fabrizio Ameli, Michel Andre, Giorgos Androulakis, Marco Anghinolfi, Mancia Anguita, Gisela Anton, Miquel Ardid, Julien Aublin, Christos Bagatelas, Giancarlo Barbarino, Bruny Baret, Suzan Basegmez du Pree, Meriem Bendahman, Edward Berbee, Vincent Bertin, Simone Biagi, et al (212)
Apr 20 2020 astro-ph.IM physics.ins-det arXiv:2004.08254v1

@misc{2004.08254, author = {Sebastiano Aiello and Arnauld Albert and Sergio Alves Garre and Zineb Aly and Fabrizio Ameli and Michel Andre and Giorgos Androulakis and Marco Anghinolfi and Mancia Anguita and Gisela Anton and Miquel Ardid and Julien Aublin and Christos Bagatelas and Giancarlo Barbarino and Bruny Baret and Suzan Basegmez du Pree and Meriem Bendahman and Edward Berbee and Vincent Bertin and Simone Biagi and Andrea Biagioni and Matthias Bissinger and Markus Boettcher and Jihad Boumaaza and Mohammed Bouta and Mieke Bouwhuis and Cristiano Bozza and Horea Branzas and Ronald Bruijn and Jürgen Brunner and Ernst-Jan Buis and Raffaele Buompane and Jose Busto and Barbara Caiffi and David Calvo and Antonio Capone and Víctor Carretero and Paolo Castaldi and Silvia Celli and Mohamed Chabab and Nhan Chau and Andrew Chen and Silvio Cherubini and Vitaliano Chiarella and Tommaso Chiarusi and Marco Circella and Rosanna Cocimano and Joao Coelho and Alexis Coleiro and Marta Colomer Molla and Rosa Coniglione and Paschal Coyle and Alexandre Creusot and Giacomo Cuttone and Antonio D'Onofrio and Richard Dallier and Maarten de Jong and Paul de Jong and Mauro De Palma and Gwenhaël de Wasseige and Els de Wolf and Irene Di Palma and Antonio Diaz and Dídac Diego-Tortosa and Carla Distefano and Alba Domi and Roberto Donà and Corinne Donzaud and Damien Dornic and Manuel Dörr and Doriane Drouhin and Thomas Eberl and Imad El Bojaddaini and Dominik Elsaesser and Alexander Enzenhöfer and Paolo Fermani and Giovanna Ferrara and Miroslav Filipovic and Francesco Filippini and Luigi Antonio Fusco and Omar Gabella and Tamas Gal and Alfonso Andres Garcia Soto and Fabio Garufi and Yoann Gatelet and Nicole Geißelbrecht and Lucio Gialanella and Emidio Giorgio and Sara Rebecca Gozzini and Rodrigo Gracia and Kay Graf and Dario Grasso and Giuseppe Grella and Carlo Guidi and Steffen Hallmann and Hassane Hamdaoui and Aart Heijboer and Amar Hekalo and Juan-Jose Hernandez-Rey and Jannik Hofestädt and Feifei Huang and Walid Idrissi Ibnsalih and Giulia Illuminati and Clancy James and Bouke Jisse Jung and Matthias Kadler and Piotr Kalaczyński and Oleg Kalekin and Uli Katz and Nafis Rezwan Khan Chowdhury and Giorgi Kistauri and Els Koffeman and Paul Kooijman and Antoine Kouchner and Michael Kreter and Vladimir Kulikovskiy and Robert Lahmann and Giuseppina Larosa and Remy Le Breton and Ornella Leonardi and Francesco Leone and Emanuele Leonora and Giuseppe Levi and Massimiliano Lincetto and Miles Lindsey Clark and Thomas Lipreau and Alessandro Lonardo and Fabio Longhitano and Daniel Lopez Coto and Lukas Maderer and Jerzy Mańczak and Karl Mannheim and Annarita Margiotta and Antonio Marinelli and Christos Markou and Lilian Martin and Juan Antonio Martínez-Mora and Agnese Martini and Fabio Marzaioli and Stefano Mastroianni and Safaa Mazzou and Karel Melis and Gennaro Miele and Pasquale Migliozzi and Emilio Migneco and Piotr Mijakowski and Luis Salvador Miranda Palacios and Carlos Maximiliano Mollo and Mauro Morganti and Michael Moser and Abdelilah Moussa and Rasa Muller and Mario Musumeci and Lodewijk Nauta and Sergio Navas and Carlo Alessandro Nicolau and Brían Ó Fearraigh and Mukharbek Organokov and Angelo Orlando and Gogita Papalashvili and Riccardo Papaleo and Cosimo Pastore and Alice Paun and Gabriela Emilia Pavalas and Carmelo Pellegrino and Mathieu Perrin-Terrin and Paolo Piattelli and Camiel Pieterse and Konstantinos Pikounis and Ofelia Pisanti and Chiara Poirè and Vlad Popa and Maarten Post and Thierry Pradier and Gerd Pühlhofer and Sara Pulvirenti and Omphile Rabyang and Fabrizio Raffaelli and Nunzio Randazzo and Antonio Rapicavoli and Soebur Razzaque and Diego Real and Stefan Reck and Giorgio Riccobene and Marc Richer and Stephane Rivoire and Alberto Rovelli and Francisco Salesa Greus and Dorothea Franziska Elisabeth Samtleben and Agustín Sánchez Losa and Matteo Sanguineti and Andrea Santangelo and Domenico Santonocito and Piera Sapienza and Jutta Schnabel and Jordan Seneca and Irene Sgura and Rezo Shanidze and Ankur Sharma and Francesco Simeone and Anna Sinopoulou and Bernardino Spisso and Maurizio Spurio and Dimitris Stavropoulos and Jos Steijger and Simona Maria Stellacci and Mauro Taiuti and Yahya Tayalati and Enrique Tenllado and Tarak Thakore and Steven Tingay and Ekaterini Tzamariudaki and Dimitrios Tzanetatos and Ad van den Berg and Frits van der Knaap and Daan van Eijk and Véronique Van Elewyck and Hans van Haren and Godefroy Vannoye and George Vasileiadis and Federico Versari and Salvatore Viola and Daniele Vivolo and Joern Wilms and Rafał Wojaczyński and Dmitry Zaborov and Sandra Zavatarelli and Angela Zegarelli and Daniele Zito and Juan-de-Dios Zornoza and Juan Zúñiga and Natalia Zywucka}, title = {{E}vent reconstruction for {KM}3{N}e{T}/{ORCA} using convolutional neural networks}, year = {2020}, eprint = {2004.08254}, note = {arXiv:2004.08254v1} }
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The KM3NeT research infrastructure is currently under construction at two locations in the Mediterranean Sea. The KM3NeT/ORCA water-Cherenkov neutrino detector off the French coast will instrument several megatons of seawater with photosensors. Its main objective is the determination of the neutrino mass ordering. This work aims at demonstrating the general applicability of deep convolutional neural networks to neutrino telescopes, using simulated datasets for the KM3NeT/ORCA detector as an example. To this end, the networks are employed to achieve reconstruction and classification tasks that constitute an alternative to the analysis pipeline presented for KM3NeT/ORCA in the KM3NeT Letter of Intent. They are used to infer event reconstruction estimates for the energy, the direction, and the interaction point of incident neutrinos. The spatial distribution of Cherenkov light generated by charged particles induced in neutrino interactions is classified as shower- or track-like, and the main background processes associated with the detection of atmospheric neutrinos are recognized. Performance comparisons to machine-learning classification and maximum-likelihood reconstruction algorithms previously developed for KM3NeT/ORCA are provided. It is shown that this application of deep convolutional neural networks to simulated datasets for a large-volume neutrino telescope yields competitive reconstruction results and performance improvements with respect to classical approaches.
Dark matter search in a Beam-Dump eXperiment (BDX) at Jefferson Lab -- 2018 update to PR12-16-001
M. Battaglieri, A. Bersani, G. Bracco, B. Caiffi, A. Celentano, R. De Vita, L. Marsicano, P. Musico, F. Panza, M. Ripani, E. Santopinto, M. Taiuti, V. Bellini, M. Bondi', P. Castorina, M. De Napoli, A. Italiano, V. Kuznetzov, E. Leonora, F. Mammoliti, et al (105)
Oct 09 2019 physics.ins-det hep-ex arXiv:1910.03532v1

@misc{1910.03532, author = {M.~Battaglieri and A.~Bersani and G.~Bracco and B.~Caiffi and A.~Celentano and R.~De Vita and L.~Marsicano and P.~Musico and F.~Panza and M.~Ripani and E.~Santopinto and M.~Taiuti and V.~Bellini and M.~Bondi' and P.~Castorina and M.~De Napoli and A.~Italiano and V.~Kuznetzov and E.~Leonora and F.~Mammoliti and N.~Randazzo and L.~Re and G.~Russo and M.~Russo and A.~Shahinyan and M.~Sperduto and S.~Spinali and C.~Sutera and F.~Tortorici and N.Baltzell and M.~Dalton and A.~Freyberger and F.-X.~Girod and G.~Kharashvili and V.~Kubarovsky and E.~Pasyuk and E.S.~Smith and S.~Stepanyan and H.~Szumilla-Vance and M.~Ungaro and T.~Whitlatch and E.~Izaguirre and G.~Krnjaic and I.~Ehle and D.~Snowden-Ifft and D.~Loomba and M.~Carpinelli and D.~D'Urso and A.~Gabrieli and G.~Maccioni and M.~Sant and V.~Sipala and F.~Ameli and E.~Cisbani and F.~De Persio and A.~Del Dotto and F.~Garibaldi and F.~Meddi and C.~A.~Nicolau and G.~M.~Urciuoli and T.~Chiarusi and M.~Manzali and C.~Pellegrino and P.~Schuster and N.~Toro and R.~Essig and M.H.~Wood and M.~Holtrop.~and R.~Paremuzyan and G.~De Cataldo and R.~De Leo and D.~Di Bari and L.~Lagamba and E.~Nappi and R.~Perrino and I.~Balossino and L.~Barion and G.~Ciullo and M.~Contalbrigo and A.~Drago and P.~Lenisa and A.~Movsisyan and L.~Pappalardo and F.~Spizzo and M.~Turisini and D.~Hasch and V.~Lucherini and M.~Mirazita and S.~Pisano and P.~Rossi and S.~Tomassini and G.~Simi and A.~D'Angelo and L.~Lanza and A.~Rizzo and A.~Filippi and M.~Genovese and M.~Kunkel and M.~Bashkanov and A.~Murphy and G.~Smith and D.~Watts and N.~Zachariou and L.~Zana and D.~Glazier and D.~Ireland and B.~McKinnon and D.~Sokhan and L.~Colaneri and S.~Anefalos Pereira and A.~Afanasev and B.~Briscoe and I.~Strakovsky and N.~Kalantarians and L.~Weinstein and K.~P.~Adhikari and J.~A.~Dunne and D.~Dutta and L.~El Fassi and L.~Ye and K.~Hicks and P.~Cole and S.~Dobbs and C.~Fanelli and P.~Mohanmurthy}, title = {{D}ark matter search in a {B}eam-{D}ump e{X}periment ({BDX}) at {J}efferson {L}ab -- 2018 update to {PR}12-16-001}, year = {2019}, eprint = {1910.03532}, note = {arXiv:1910.03532v1} }
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This document complements and completes what was submitted last year to PAC45 as an update to the proposal PR12-16-001 "Dark matter search in a Beam-Dump eXperiment (BDX)" at Jefferson Lab submitted to JLab-PAC44 in 2016. Following the suggestions contained in the PAC45 report, in coordination with the lab, we ran a test to assess the beam-related backgrounds and validate the simulation framework used to design the BDX experiment. Using a common Monte Carlo framework for the test and the proposed experiment, we optimized the selection cuts to maximize the reach considering simultaneously the signal, cosmic-ray background (assessed in Catania test with BDX-Proto) and beam-related backgrounds (irreducible NC and CC neutrino interactions as determined by simulation). Our results confirmed what was presented in the original proposal: with 285 days of a parasitic run at 65 $\mu$A (corresponding to $10^{22}$ EOT) the BDX experiment will lower the exclusion limits in the case of no signal by one to two orders of magnitude in the parameter space of dark-matter coupling versus mass.
Dependence of atmospheric muon flux on seawater depth measured with the first KM3NeT detection units
KM3NeT Collaboration, M. Ageron, S. Aiello, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, G. Anton, M. Ardid, J. Aublin, C. Bagatelas, G. Barbarino, B. Baret, S. Basegmez du Pree, A. Belias, E. Berbee, A. M. van den Berg, V. Bertin, V. van Beveren, S. Biagi, et al (245)
Jun 07 2019 physics.ins-det hep-ex arXiv:1906.02704v3

@misc{1906.02704, author = {KM3NeT Collaboration and M.~Ageron and S.~Aiello and F.~Ameli and M.~Andre and G.~Androulakis and M.~Anghinolfi and G.~Anton and M.~Ardid and J.~Aublin and C.~Bagatelas and G.~Barbarino and B.~Baret and S.~Basegmez du Pree and A.~Belias and E.~Berbee and A.~M.~van den Berg and V.~Bertin and V.~van Beveren and S.~Biagi and A.~Biagioni and S.~Bianucci and M.~Billault and M.~Bissinger and R.~de Boer and J.~Boumaaza and S.~Bourret and M.~Bouta and M.~Bouwhuis and C.~Bozza and H.Brânzaş and M.~Briel and M.~Bruchner and R.~Bruijn and J.~Brunner and E.~Buis and R.~Buompane and J.~Busto and G.~Cacopardo and L.~Caillat and C.~Calì and D.~Calvo and A.~Capone and S.~Celli and M.~Chabab and N.~Chau and S.~Cherubini and V.~Chiarella and T.~Chiarusi and M.~Circella and R.~Cocimano and J.~A.~B.~Coelho and A.~Coleiro and M.~Colomer Molla and S.~Colonges and R.~Coniglione and A.~Cosquer and P.~Coyle and A.~Creusot and G.~Cuttone and C.~D'Amato and A.~D'Amico and A.~D'Onofrio and R.~Dallier and M.~De Palma and C.~De Sio and I.~Di Palma and A.~F.~Díaz and D.~Diego-Tortosa and C.~Distefano and A.~Domi and R.~Donà and C.~Donzaud and L.~van Dooren and D.~Dornic and M.~Dörr and M.~Durocher and T.~Eberl and T.~van Eeden and I.~El Bojaddaini and H.~Eljarrari and D.~Elsaesser and A.~Enzenhöfer and P.~Fermani and G.~Ferrara and M.~D.~Filipović and L.~A.~Fusco and D.~Gajanana and T.~Gal and A.~Garcia Soto and F.~Garufi and L.~Gialanella and E.~Giorgio and A.~Giuliante and S.~R.~Gozzini and R.~Gracia and K.~Graf and D.~Grasso and T.~Grégoire and G.~Grella and A.~Grimaldi and A.~Grmek and D.~Guderian and M.~Guerzoni and C.~Guidi and S.~Hallmann and H.~Hamdaoui and H.~van Haren and A.~Heijboer and A.~Hekalo and S.~Henry and J.~J.~Hernández-Rey and J.~Hofestädt and F.~Huang and E.~Huesca Santiago and G.~Illuminati and C.~W.~James and P.~Jansweijer and M.~Jongen and M.~de Jong and P.~de Jong and M.~Kadler and P.~Kalaczyński and O.~Kalekin and U.~F.~Katz and F.~Kayzel and P.~Keller and N.~R.~Khan Chowdhury and F.~van der Knaap and E.~N.~Koffeman and P.~Kooijman and J.~Koopstra and A.~Kouchner and M.~Kreter and V.~Kulikovskiy and Meghna K.~K.~and R.~Lahmann and P.~Lamare and G.~Larosa and J.~Laurence and R.~Le Breton and F.~Leone and E.~Leonora and G.~Levi and F.~Librizzi and M.~Lincetto and P.~Litrico and C.~D.~Llorens Alvarez and A.~Lonardo and F.~Longhitano and D.~Lopez-Coto and G.~Maggi and J.~Mańczak and K.~Mannheim and A.~Margiotta and A.~Marinelli and C.~Markou and L.~Martin and J.~A.~Martínez-Mora and A.~Martini and F.~Marzaioli and R.~Mele and K.~W.~Melis and P.~Migliozzi and E.~Migneco and P.~Mijakowski and L.~S.~Miranda and C.~M.~Mollo and M.~Mongelli and M.~Morganti and M.~Moser and A.~Moussa and R.~Muller and P.~Musico and M.~Musumeci and L.~Nauta and S.~Navas and C.~A.~Nicolau and C.~Nielsen and B.~Ó Fearraigh and M.~Organokov and A.~Orlando and V.~Panagopoulos and G.~Pancaldi and G.~Papalashvili and R.~Papaleo and C.~Pastore and G.~E.~Păvălaş and G.~Pellegrini and C.~Pellegrino and M.~Perrin-Terrin and P.~Piattelli and K.~Pikounis and O.~Pisanti and C.~Poirè and G.~Polydefki and V.~Popa and M.~Post and T.~Pradier and G.~Pühlhofer and S.~Pulvirenti and L.~Quinn and F.~Raffaelli and N.~Randazzo and A.~Rapicavoli and S.~Razzaque and D.~Real and S.~Reck and J.~Reubelt and G.~Riccobene and L.~Rigalleau and G.~Rizza and R.~Rocco and A.~Rovelli and J.~Royon and M.~Salemi and I.~Salvadori and D.~F.~E.~Samtleben and A.~Sánchez Losa and M.~Sanguineti and A.~Santangelo and D.~Santonocito and P.~Sapienza and J.~Schmelling and V.~Sciacca and D.~Sciliberto and J.~Seneca and I.~Sgura and R.~Shanidze and A.~Sharma and F.~Simeone and A.Sinopoulou and B.~Spisso and M.~Spurio and D.~Stavropoulos and J.~Steijger and S.~M.~Stellacci and B.~Strandberg and D.~Stransky and T.~Stüven and M.~Taiuti and Y.~Tayalati and E.~Tenllado and D.~Tézier and T.~Thakore and S.~Theraube and P.~Timmer and S.~Tingay and A.~Trovato and S.~Tsagkli and E.~Tzamariudaki and D.~Tzanetatos and C.~Valieri and V.~Van Elewyck and F.~Versari and S.~Viola and D.~Vivolo and G.~de Wasseige and J.~Wilms and R.~Wojaczyński and E.~de Wolf and D.~Zaborov and A.~Zegarelli and J.~D.~Zornoza and J.~Zúñiga}, title = {{D}ependence of atmospheric muon flux on seawater depth measured with the first {KM}3{N}e{T} detection units}, year = {2019}, eprint = {1906.02704}, doi = {10.1140/epjc/s10052-020-7629-z}, note = {arXiv:1906.02704v3} }
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KM3NeT is a research infrastructure located in the Mediterranean Sea, that will consist of two deep-sea Cherenkov neutrino detectors. With one detector (ARCA), the KM3NeT Collaboration aims at identifying and studying TeV-PeV astrophysical neutrino sources. With the other detector (ORCA), the neutrino mass ordering will be determined by studying GeV-scale atmospheric neutrino oscillations. The first KM3NeT detection units were deployed at the Italian and French sites between 2015 and 2017. In this paper, a description of the detector is presented, together with a summary of the procedures used to calibrate the detector in-situ. Finally, the measurement of the atmospheric muon flux between 2232-3386 m seawater depth is obtained.
Letter of Interest for a Neutrino Beam from Protvino to KM3NeT/ORCA
A. V. Akindinov, E. G. Anassontzis, G. Anton, M. Ardid, J. Aublin, B. Baret, V. Bertin, S. Bourret, C. Bozza, M. Bruchner, R. Bruijn, J. Brunner, M. Chabab, N. Chau, A. S. Chepurnov, M. Colomer Molla, P. Coyle, A. Creusot, G. de Wasseige, A. Domi, et al (71)
Feb 19 2019 physics.ins-det hep-ex arXiv:1902.06083v3

@misc{1902.06083, author = {A.~V.~Akindinov and E.~G.~Anassontzis and G.~Anton and M.~Ardid and J.~Aublin and B.~Baret and V.~Bertin and S.~Bourret and C.~Bozza and M.~Bruchner and R.~Bruijn and J.~Brunner and M.~Chabab and N.~Chau and A.~S.~Chepurnov and M.~Colomer Molla and P.~Coyle and A.~Creusot and G.~de Wasseige and A.~Domi and C.~Donzaud and T.~Eberl and A.~Enzenhöfer and M.~Faifman and M.~D.~Filipović and L.~Fusco and V.~I.~Garkusha and T.~Gal and S.~R.~Gozzini and K.~Graf and T.~Grégoire and G.~Grella and S.~Hallmann and A.~Heijboer and J.~J.~Hernández-Rey and J.~Hofestädt and S.~V.~Ivanov and C.~W.~James and M.~de Jong and P.~de Jong and P.~Kalaczyński and I.~D.~Kakorin and U.~F.~Katz and N.~R.~Khan Chowdhury and M.~M.~Kirsanov and A.~Kouchner and V.~Kulikovskiy and K.~S.~Kuzmin and R.~Le Breton and O.~P.~Lebedev and M.~Lincetto and E.~Litvinovich and D.~Lopez-Coto and C.~Markou and A.~V.~Maximov and K.~W.~Melis and R.~Muller and V.~A.~Naumov and S.~Navas and L.~Nauta and C.~Nielsen and F.~N.~Novoskoltsev and B.~Ó Fearraigh and M.~Organokov and G.~Papalashvili and M.~Perrin-Terrin and C.~Poirè and T.~Pradier and L.~Quinn and D.~F.~E.~Samtleben and M.~Sanguineti and J.~Seneca and R.~Shanidze and E.~V.~Shirokov and A.~Sinopoulou and R.~Yu.~Sinyukov and M.~D.~Skorokhvatov and I.~Sokalski and A.~A.~Sokolov and B.~Spisso and S.~M.~Stellacci and B.~Strandberg and M.~Taiuti and T.~Thakore and E.~Tzamariudaki and V.~Van Elewyck and E.~de Wolf and D.~Zaborov and A.~M.~Zaitsev and J.~D.~Zornoza and J.~Zúñiga}, title = {{L}etter of {I}nterest for a {N}eutrino {B}eam from {P}rotvino to {KM}3{N}e{T}/{ORCA}}, year = {2019}, eprint = {1902.06083}, note = {arXiv:1902.06083v3} }
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The Protvino accelerator facility located in the Moscow region, Russia, is in a good position to offer a rich experimental research program in the field of neutrino physics. Of particular interest is the possibility to direct a neutrino beam from Protvino towards the KM3NeT/ORCA detector, which is currently under construction in the Mediterranean Sea 40 km offshore Toulon, France. This proposal is known as P2O. Thanks to its baseline of 2595 km, this experiment would yield an unparalleled sensitivity to matter effects in the Earth, allowing for the determination of the neutrino mass ordering with a high level of certainty after only a few years of running at a modest beam intensity of $\approx$ 90 kW. With a prolonged exposure ($\approx$ 1500 kW*yr), a 2$\sigma$ sensitivity to the leptonic CP-violating Dirac phase can be achieved. A second stage of the experiment, comprising a further intensity upgrade of the accelerator complex and a densified version of the ORCA detector (Super-ORCA), would allow for up to a 6$\sigma$ sensitivity to CP violation and a 10$^\circ$-17$^\circ$ resolution on the CP phase after 10 years of running with a 450 kW beam, competitive with other planned experiments. The initial composition and energy spectrum of the neutrino beam would need to be monitored by a near detector, to be constructed several hundred meters downstream from the proton beam target. The same neutrino beam and near detector set-up would also allow for neutrino-nucleus cross section measurements to be performed. A short-baseline sterile neutrino search experiment would also be possible.
New Eco-gas mixtures for the Extreme Energy Events MRPCs: results and plans
S. Pisano, M. Abbrescia, C. Avanzini, L. Baldini Ferroli, L. Baldini, G. Batignani, M. Battaglieri, S. Boi, E. Bossini, F. Carnesecchi, A. Chiavassa, C. Cicalo, L. Cifarelli, F. Coccetti, E. Coccia, A. Corvaglia, D. De Gruttola, S. De Pasquale, F. L. Fabbri, V. Frolov, et al (47)
Jun 12 2018 physics.ins-det arXiv:1806.03918v2

@misc{1806.03918, author = {S.~Pisano and M.~Abbrescia and C.~Avanzini and L.~Baldini Ferroli and L.~Baldini and G.~Batignani and M.~Battaglieri and S.~Boi and E.~Bossini and F.~Carnesecchi and A.~Chiavassa and C.~Cicalo and L.~Cifarelli and F.~Coccetti and E.~Coccia and A.~Corvaglia and D.~De Gruttola and S.~De Pasquale and F.~L.~Fabbri and V.~Frolov and L.~Galante and P.~Galeotti and M.~Garbini and G.~Gemme and I.~Gnesi and S.~Grazzi and C.~Gustavino and D.~Hatzifotiadou and P.~La Rocca and G.~Mandaglio and O.~Maragoto Rodriguez and G.~Maron and M.~N.~Mazziotta and S.~Miozzi and R.~Nania and F.~Noferini and F.~Nozzoli and F.~Palmonari and M.~Panareo and M.~P.~Panetta and R.~Paoletti and W.~Park and C.~Pellegrino and L.~Perasso and F.~Pilo and G.~Piragino and F.~Riggi and G.~C.~Righini and C.~Ripoli and M.~Rizzi and G.~Sartorelli and E.~Scapparone and M.~Schioppa and A.~Scribano and M.~Selvi and S.~Serci and S.~Squarcia and M.~Taiuti and G.~Terreni and A.~Trifirò and M.~Trimarchi and M.~C.~Vistoli and L.~Votano and M.~C.~S.~Williams and L.~Zheng and A.~Zichichi and R.~Zuyeuski}, title = {{N}ew {E}co-gas mixtures for the {E}xtreme {E}nergy {E}vents {MRPC}s: results and plans}, year = {2018}, eprint = {1806.03918}, note = {arXiv:1806.03918v2} }
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The Extreme Energy Events observatory is an extended muon telescope array, covering more than 10 degrees both in latitude and longitude. Its 59 muon telescopes are equipped with tracking detectors based on Multigap Resistive Plate Chamber technology with time resolution of the order of a few hundred picoseconds. The recent restrictions on greenhouse gases demand studies for new gas mixtures in compliance with the relative requirements. Tetrafluoropropene is one of the candidates for tetrafluoroethane substitution, since it is characterized by a Global Warming Power around 300 times lower than the gas mixtures used up to now. Several mixtures have been tested, measuring efficiency curves, charge distributions, streamer fractions and time resolutions. Results are presented for the whole set of mixtures and operating conditions, %. A set of tests on a real EEE telescope, with cosmic muons, are being performed at the CERN-01 EEE telescope. The tests are focusing on identifying a mixture with good performance at the low rates typical of an EEE telescope.
Performance of the Multigap Resistive Plate Chambers of the Extreme Energy Events Project
D.De Gruttola, M.Abbrescia, C.Avanzini, L.Baldini, R.Baldini Ferroli, G.Batignani, M.Battaglieri, S.Boi, E.Bossini, F.Carnesecchi, A.Chiavassa, C.Cicalo, L.Cifarelli, F.Coccetti, E.Coccia, A.Corvaglia, S.De Pasquale, F.L.Fabbri, V.Frolov, L.Galante, et al (47)
Jun 12 2018 physics.ins-det arXiv:1806.03879v1

@misc{1806.03879, author = {D.De Gruttola and M.Abbrescia and C.Avanzini and L.Baldini and R.Baldini Ferroli and G.Batignani and M.Battaglieri and S.Boi and E.Bossini and F.Carnesecchi and A.Chiavassa and C.Cicalo and L.Cifarelli and F.Coccetti and E.Coccia and A.Corvaglia and S.De Pasquale and F.L.Fabbri and V.Frolov and L.Galante and P.Galeotti and M.Garbini and G.Gemme and I.Gnesi and S.Grazzi and C.Gustavino and D.Hatzifotiadou and P.La Rocca and G.Mandaglio and O.Maragoto Rodriguez and G.Maron and M.N.Mazziotta and S.Miozzi and R.Nania and F.Noferini and F.Nozzoli and F.Palmonari and M.Panareo and M.P.Panetta and R.Paoletti and W.Park and C.Pellegrino and L.Perasso and F.Pilo and G.Piragino and S.Pisano and F.Riggi and G.C.Righini and C.Ripoli and M.Rizzi and G.Sartorelli and E.Scapparone and M.Schioppa and A.Scribano and M.Selvi and S.Serci and S.Squarcia and M.Taiuti and G.Terreni and A.Trifirò and M.Trimarchi and M.C.Vistoli and L.Votan and M.C.S.Williams and L.Zheng and A.Zichichi and R.Zuyeuski}, title = {{P}erformance of the {M}ultigap {R}esistive {P}late {C}hambers of the {E}xtreme {E}nergy {E}vents {P}roject}, year = {2018}, eprint = {1806.03879}, note = {arXiv:1806.03879v1} }
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The muon telescopes of the Extreme Energy Events (EEE) Project are made of three Multigap Resistive Plate Chambers (MRPC). The EEE array is composed, so far, of 59 telescopes and is organized in clusters and single telescope stations distributed all over the Italian territory. They are installed in High Schools with the aim to join research and teaching activities, by involving researchers, teachers and students in the construction, maintenance, data taking and data analysis. The unconventional working sites, mainly school buildings with non-controlled environmental parameters and heterogeneous maintenance conditions, are a unique test field for checking the robustness, the low-ageing features and the long-lasting performance of the MRPC technology for particle tracking and timing purposes. The measurements performed with the EEE array require excellent performance in terms of time and spatial resolution, efficiency, tracking capability and stability. The data from two recent coordinated data taking periods, named Run 2 and Run 3, have been used to measure these quantities and the results are described, together with a comparison with expectations and with the results from a beam test performed in 2006 at CERN.
First results from the upgrade of the Extreme Energy Events experiment
M. Abbrescia, C. Avanzini, L. Baldini, R. Baldini Ferroli, G. Batignani, M. Battaglieri, S. Boi, E. Bossini, F. Carnesecchi, A. Chiavassa, C. Cicalo, L. Cifarelli, F. Coccetti, E. Coccia, A. Corvaglia, D. De Gruttola, S. De Pasquale, L. Fabbri, V. Frolov, L. Galante, et al (46)
Jun 12 2018 physics.ins-det arXiv:1806.03913v1

@misc{1806.03913, author = {M.~Abbrescia and C.~Avanzini and L.~Baldini and R.~Baldini Ferroli and G.~Batignani and M.~Battaglieri and S.~Boi and E.~Bossini and F.~Carnesecchi and A.~Chiavassa and C.~Cicalo and L.~Cifarelli and F.~Coccetti and E.~Coccia and A.~Corvaglia and D.~De Gruttola and S.~De Pasquale and L.~Fabbri and V.~Frolov and L.~Galante and P.~Galeotti and M.~Garbini and G.~Gemme and I.~Gnesi and S.~Grazzi and C.~Gustavino and D.~Hatzifotiadou and P.~La Rocca and G.~Mandaglio and O.~Maragoto Rodriguez and G.~Maron and M.~N.~Mazziotta and S.~Miozzi and R.~Nania and F.~Noferini and F.~Nozzoli and F.~Palmonari and M.~Panareo and M.~P.~Panetta and R.~Paoletti and W.~Park and C.~Pellegrino and L.~Perasso and F.~Pilo and G.~Piragino and S.~Pisano and F.~Riggi and G.~C.~Righini and C.~Ripoli and M.~Rizzi and G.~Sartorelli and E.~Scapparone and M.~Schioppa and A.~Scribano and M.~Selvi and S.~Serci and S.~Squarcia and M.~Taiuti and G.~Terreni and A.~Trifirò and M.~Trimarchi and M.~C.~Vistoli.~L.~Votano and M.~C.~S.~Williams and L.~Zheng and A.~Zichichi and R.~Zuyeuski}, title = {{F}irst results from the upgrade of the {E}xtreme {E}nergy {E}vents experiment}, year = {2018}, eprint = {1806.03913}, note = {arXiv:1806.03913v1} }
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The Extreme Energy Events (EEE) experiment is the largest system in the world completely implemented with Multigap Resistive Plate Chambers (MRPCs). Presently, it consists of a network of 59 muon telescopes, each made of 3 MRPCs, devoted to the study of secondary cosmic rays. Its stations, sometimes hundreds of kilometers apart, are synchronized at a few nanoseconds level via a clock signal delivered by the Global Positioning System. The data collected during centrally coordinated runs are sent to INFN CNAF, the largest center for scientific computing in Italy, where they are reconstructed and made available for analysis. Thanks to the on-line monitoring and data transmission, EEE operates as a single coordinated system spread over an area of about $3 \times 10^5$ km$^2$. In 2017, the EEE collaboration started an important upgrade program, aiming to extend the network with 20 additional stations, with the option to have more in the future. This implies the construction, testing and commissioning of 60 chambers, for a total detector surface of around 80 m$^2$. In this paper, aspects related to this challenging endeavor are covered, starting from the technological solutions chosen to build these state-of-the-art detectors, to the quality controls and the performance tests carried on.
The Extreme Energy Events experiment: an overview of the telescopes performance
M.Abbrescia, C.Avanzini, L.Baldini Ferroli, L.Baldini, G.Batignani, M.Battaglieri, S.Boi, E.Bossini, F.Carnesecchi, A.Chiavassa, C.Cicalo, L.Cifarelli, F.Coccetti, E.Coccia, A.Corvaglia, D.De Gruttola, S.De Pasquale, F.L.Fabbri, V.Frolov, L.Galante, et al (47)
May 14 2018 physics.ins-det arXiv:1805.04177v1

@misc{1805.04177, author = {M.Abbrescia and C.Avanzini and L.Baldini Ferroli and L.Baldini and G.Batignani and M.Battaglieri and S.Boi and E.Bossini and F.Carnesecchi and A.Chiavassa and C.Cicalo and L.Cifarelli and F.Coccetti and E.Coccia and A.Corvaglia and D.De Gruttola and S.De Pasquale and F.L.Fabbri and V.Frolov and L.Galante and P.Galeotti and M.Garbini and G.Gemme and I.Gnesi and S.Grazzi and C.Gustavino and D.Hatzifotiadou and P.La Rocca and G.Mandaglio and O.Maragoto Rodriguez and G.Maron and M.N.Mazziotta and S.Miozzi and R.Nania and F.Noferini and F.Nozzoli and F.Palmonari and M.Panareo and M.P.Panetta and R.Paoletti and W.Park and C.Pellegrino and L.Perasso and F.Pilo and G.Piragino and S.Pisano and F.Riggi and G.C.Righini and C.Ripoli and M.Rizzi and G.Sartorelli and E.Scapparone and M.Schioppa and A.Scribano and M.Selvi and S.Serci and S.Squarcia and M.Taiuti and G.Terreni and A.Trifirò and M.Trimarchi and M.C.Vistoli and L.Votan and M.C.S.Williams and L.Zheng and A.Zichichi and R.Zuyeuski}, title = {{T}he {E}xtreme {E}nergy {E}vents experiment: an overview of the telescopes performance}, year = {2018}, eprint = {1805.04177}, note = {arXiv:1805.04177v1} }
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Multigap Resistive Plate Chambers (MRPC). The EEE network is composed, so far, of 53 telescopes, each made of three MRPC detectors; it is organized in clusters and single telescope stations distributed all over the Italian territory and installed in High Schools, covering an area larger than $3\times10^{5}$ km$^{2}$. The study of Extensive Air Showers (EAS), that is one of the goal of the project, requires excellent performance in terms of time and spatial resolution, efficiency, tracking capability and long term stability. The data from two recent coordinated data taking periods, named Run 2 and Run 3, have been used to measure these quantities and the results are here reported, together with a comparison with expectations and with the results from a beam test performed in 2006 at CERN.
Dark matter search in a Beam-Dump eXperiment (BDX) at Jefferson Lab: an update on PR12-16-001
M. Battaglieri, A. Bersani, G. Bracco, B. Caiffi, A. Celentano, R. De Vita, L. Marsicano, P. Musico, M. Osipenko, F. Panza, M. Ripani, E. Santopinto, M. Taiuti, V. Bellini, M. Bondi', P. Castorina, M. De Napoli, A. Italiano, V. Kuznetzov, E. Leonora, et al (106)
Dec 06 2017 physics.ins-det hep-ex arXiv:1712.01518v2

@misc{1712.01518, author = {M.~Battaglieri and A.~Bersani and G.~Bracco and B.~Caiffi and A.~Celentano and R.~De Vita and L.~Marsicano and P.~Musico and M.~Osipenko and F.~Panza and M.~Ripani and E.~Santopinto and M.~Taiuti and V.~Bellini and M.~Bondi' and P.~Castorina and M.~De Napoli and A.~Italiano and V.~Kuznetzov and E.~Leonora and F.~Mammoliti and N.~Randazzo and L.~Re and G.~Russo and M.~Russo and A.~Shahinyan and M.~Sperduto and S.~Spinali and C.~Sutera and F.~Tortorici and N.Baltzell and M.~Dalton and A.~Freyberger and F.-X.~Girod and G.~Kharashvili and V.~Kubarovsky and E.~Pasyuk and E.S.~Smith and S.~Stepanyan and M.~Ungaro and T.~Whitlatch and E.~Izaguirre and G.~Krnjaic and D.~Snowden-Ifft and D.~Loomba and M.~Carpinelli and D.~D'Urso and A.~Gabrieli and G.~Maccioni and M.~Sant and V.~Sipala and F.~Ameli and E.~Cisbani and F.~De Persio and A.~Del Dotto and F.~Garibaldi and F.~Meddi and C.~A.~Nicolau and G.~M.~Urciuoli and T.~Chiarusi and M.~Manzali and C.~Pellegrino and P.~Schuster and N.~Toro and R.~Essig and M.H.~Wood and M.~Holtrop.~R.~Paremuzyan and G.~De Cataldo and R.~De Leo and D.~Di Bari and L.~Lagamba and E.~Nappi and R.~Perrino and I.~Balossino and L.~Barion and G.~Ciullo and M.~Contalbrigo and A.~Drago and P.~Lenisa and A.~Movsisyan and L.~Pappalardo and F.~Spizzo and M.~Turisini and D.~Hasch and V.~Lucherini and M.~Mirazita and S.~Pisano and P.~Rossi and S.~Tomassini and G.~Simi and A.~D'Angelo and L.~Lanza and A.~Rizzo and C.~Schaerf and I.~Zonta and A.~Filippi and M.~Genovese and S.~Fegan and M.~Kunkel and M.~Bashkanov and A.~Murphy and G.~Smith and D.~Watts and N.~Zachariou and L.~Zana and D.~Glazier and D.~Ireland and B.~McKinnon and D.~Sokhan and L.~Colaneri and S.~Anefalos Pereira and A.~Afanasev and B.~Briscoe and I.~Strakovsky and N.~Kalantarians and L.~Weinstein and K.~P.~Adhikari and J.~A.~Dunne and D.~Dutta and L.~El Fassi and L.~Ye and K.~Hicks and P.~Cole and S.~Dobbs and C.~Fanelli and P.~T.~M.~Murthy}, title = {{D}ark matter search in a {B}eam-{D}ump e{X}periment ({BDX}) at {J}efferson {L}ab: an update on {PR}12-16-001}, year = {2017}, eprint = {1712.01518}, note = {arXiv:1712.01518v2} }
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This document is an update to the proposal PR12-16-001 Dark matter search in a Beam-Dump eXperiment (BDX) at Jefferson Lab submitted to JLab-PAC44 in 2016 reporting progress in addressing questions raised regarding the beam-on backgrounds. The concerns are addressed by adopting a new simulation tool, FLUKA, and planning measurements of muon fluxes from the dump with its existing shielding around the dump. First, we have implemented the detailed BDX experimental geometry into a FLUKA simulation, in consultation with experts from the JLab Radiation Control Group. The FLUKA simulation has been compared directly to our GEANT4 simulations and shown to agree in regions of validity. The FLUKA interaction package, with a tuned set of biasing weights, is naturally able to generate reliable particle distributions with very small probabilities and therefore predict rates at the detector location beyond the planned shielding around the beam dump. Second, we have developed a plan to conduct measurements of the muon ux from the Hall-A dump in its current configuration to validate our simulations.
An algorithm for the reconstruction of neutrino-induced showers in the ANTARES neutrino telescope
A. Albert, M. André, M. Anghinolfi, G. Anton, M. Ardid, J.-J. Aubert, T. Avgitas, B. Baret, J. Barrios-Martí, S. Basa, B. Belhorma, V. Bertin, S. Biagi, R. Bormuth, S. Bourret, M.C. Bouwhuis, H. Brânzaş, R. Bruijn, J. Brunner, J. Busto, et al (107)
Aug 15 2017 astro-ph.IM physics.ins-det arXiv:1708.03649v2

@misc{1708.03649, author = {A.~Albert and M.~André and M.~Anghinolfi and G.~Anton and M.~Ardid and J.-J.~Aubert and T.~Avgitas and B.~Baret and J.~Barrios-Martí and S.~Basa and B.~Belhorma and V.~Bertin and S.~Biagi and R.~Bormuth and S.~Bourret and M.C.~Bouwhuis and H.~Brânzaş and R.~Bruijn and J.~Brunner and J.~Busto and A.~Capone and L.~Caramete and J.~Carr and S.~Celli and R.~Cherkaoui El Moursli and T.~Chiarusi and M.~Circella and J.A.B.~Coelho and A.~Coleiro and R.~Coniglione and H.~Costantini and P.~Coyle and A.~Creusot and A.~F.~Díaz and A.~Deschamps and G.~De Bonis and C.~Distefano and I.~Di Palma and A.~Domi and C.~Donzaud and D.~Dornic and D.~Drouhin and T.~Eberl and I.~El Bojaddaini and N.~El Khayati and D.~Elsässer and A.~Enzenhöfer and A.~Ettahiri and F.~Fassi and I.~Felis and L.A.~Fusco and P.~Gay and V.~Giordano and H.~Glotin and T.~Grégoire and R.~Gracia Ruiz and K.~Graf and S.~Hallmann and H.~van Haren and A.J.~Heijboer and Y.~Hello and J.J.~Hernández-Rey and J.~Hößl and J.~Hofestädt and C.~Hugon and G.~Illuminati and C.W.~James and M.~de Jong and M.~Jongen and M.~Kadler and O.~Kalekin and U.~Katz and D.~Kießling and A.~Kouchner and M.~Kreter and I.~Kreykenbohm and V.~Kulikovskiy and C.~Lachaud and R.~Lahmann and D.~Lefèvre and E.~Leonora and M.~Lotze and S.~Loucatos and M.~Marcelin and A.~Margiotta and A.~Marinelli and J.A.~Martínez-Mora and R.~Mele and K.~Melis and T.~Michael and P.~Migliozzi and A.~Moussa and S.~Navas and E.~Nezri and M.~Organokov and G.E.~Păvălaş and C.~Pellegrino and C.~Perrina and P.~Piattelli and V.~Popa and T.~Pradier and L.~Quinn and C.~Racca and G.~Riccobene and A.~Sánchez-Losa and M.~Saldaña and I.~Salvadori and D.~F.~E.~Samtleben and M.~Sanguineti and P.~Sapienza and F.~Schüssler and C.~Sieger and M.~Spurio and Th.~Stolarczyk and M.~Taiuti and Y.~Tayalati and A.~Trovato and D.~Turpin and C.~Tönnis and B.~Vallage and V.~Van Elewyck and F.~Versari and D.~Vivolo and A.~Vizzoca and J.~Wilms and J.D.~Zornoza and J.~Zúñiga}, title = {{A}n algorithm for the reconstruction of neutrino-induced showers in the {ANTARES} neutrino telescope}, year = {2017}, eprint = {1708.03649}, note = {arXiv:1708.03649v2} }
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Muons created by $\nu_\mu$ charged current (CC) interactions in the water surrounding the ANTARES neutrino telescope have been almost exclusively used so far in searches for cosmic neutrino sources. Due to their long range, highly energetic muons inducing Cherenkov radiation in the water are reconstructed with dedicated algorithms that allow the determination of the parent neutrino direction with a median angular resolution of about \unit0.4\degree for an $E^{-2}$ neutrino spectrum. In this paper, an algorithm optimised for accurate reconstruction of energy and direction of shower events in the ANTARES detector is presented. Hadronic showers of electrically charged particles are produced by the disintegration of the nucleus both in CC and neutral current (NC) interactions of neutrinos in water. In addition, electromagnetic showers result from the CC interactions of electron neutrinos while the decay of a tau lepton produced in $\nu_\tau$ CC interactions will in most cases lead to either a hadronic or an electromagnetic shower. A shower can be approximated as a point source of photons. With the presented method, the shower position is reconstructed with a precision of about \unit1\metre, the neutrino direction is reconstructed with a median angular resolution between \unit2\degree and \unit3\degree in the energy range of \SIrange11000TeV. In this energy interval, the uncertainty on the reconstructed neutrino energy is about \SIrange510\%. The increase in the detector sensitivity due to the use of additional information from shower events in the searches for a cosmic neutrino flux is also presented.
Intrinsic limits on resolutions in muon- and electron-neutrino charged-current events in the KM3NeT/ORCA detector
S. Adrián-Martínez, M. Ageron, S. Aiello, A. Albert, F. Ameli, E. G. Anassontzis, M. Andre, G. Androulakis, M. Anghinolfi, G. Anton, M. Ardid, T. Avgitas, G. Barbarino, E. Barbarito, B. Baret, J. Barrios-Martí, A. Belias, E. Berbee, A. van den Berg, V. Bertin, et al (233)
Dec 19 2016 physics.ins-det hep-ex hep-ph arXiv:1612.05621v2

@misc{1612.05621, author = {S.~Adrián-Martínez and M.~Ageron and S.~Aiello and A.~Albert and F.~Ameli and E.~G.~Anassontzis and M.~Andre and G.~Androulakis and M.~Anghinolfi and G.~Anton and M.~Ardid and T.~Avgitas and G.~Barbarino and E.~Barbarito and B.~Baret and J.~Barrios-Martí and A.~Belias and E.~Berbee and A.~van den Berg and V.~Bertin and S.~Beurthey and V.~van Beveren and N.~Beverini and S.~Biagi and A.~Biagioni and M.~Billault and M.~Bondì and R.~Bormuth and B.~Bouhadef and G.~Bourlis and S.~Bourret and C.~Boutonnet and M.~Bouwhuis and C.~Bozza and R.~Bruijn and J.~Brunner and E.~Buis and R.~Buompane and J.~Busto and G.~Cacopardo and L.~Caillat and M.~Calamai and D.~Calvo and A.~Capone and L.~Caramete and S.~Cecchini and S.~Celli and C.~Champion and S.~Cherubini and V.~Chiarella and T.~Chiarusi and M.~Circella and L.~Classen and D.~Cobas and R.~Cocimano and J.~A.~B.~Coelho and A.~Coleiro and S.~Colonges and R.~Coniglione and M.~Cordelli and A.~Cosquer and P.~Coyle and A.~Creusot and G.~Cuttone and C.~D'Amato and A.~D'Amico and A.~D'Onofrio and G.~De Bonis and C.~De Sio and I.~Di Palma and A.~F.~Díaz and C.~Distefano and C.~Donzaud and D.~Dornic and Q.~Dorosti-Hasankiadeh and E.~Drakopoulou and D.~Drouhin and M.~Durocher and T.~Eberl and S.~Eichie and D.~van Eijk and I.~El Bojaddaini and D.~Elsaesser and A.~Enzenhöfer and M.~Favaro and P.~Fermani and G.~Ferrara and G.~Frascadore and L.~A.~Fusco and T.~Gal and S.~Galatà and F.~Garufi and P.~Gay and M.~Gebyehu and F.~Giacomini and L.~Gialanella and V.~Giordano and N.~Gizani and R.~Gracia and K.~Graf and T.~Grégoire and G.~Grella and A.~Grmek and R.~Habel and S.~Hallmann and H.~van Haren and S.~Harissopulos and T.~Heid and A.~Heijboer and E.~Heine and S.~Henry and J.~J.~Hernández-Rey and M.~Hevinga and J.~Hofestädt and C.~M.~F.~Hugon and G.~Illuminati and C.~W.~James and P.~Jansweijer and M.~Jongen and M.~de Jong and M.~Kadler and O.~Kalekin and A.~Kappes and U.~F.~Katz and P.~Keller and G.~Kieft and D.~Kießling and E.~N.~Koffeman and P.~Kooijman and A.~Kouchner and M.~Kreter and V.~Kulikovskiy and R.~Lahmann and P.~Lamare and G.~Larosa and A.~Leisos and F.~Leone and E.~Leonora and M.~Lindsey Clark and A.~Liolios and C.~D.~Llorens Alvarez and D.~Lo Presti and H.~Löhner and A.~Lonardo and M.~Lotze and S.~Loucatos and E.~Maccioni and K.~Mannheim and M.~Manzali and A.~Margiotta and A.~Marinelli and O.~Mariş and C.~Markou and J.~A.~Martínez-Mora and A.~Martini and F.~Marzaioli and R.~Mele and K.~W.~Melis and T.~Michael and P.~Migliozzi and E.~Migneco and P.~Mijakowski and A.~Miraglia and C.~M.~Mollo and M.~Mongelli and M.~Morganti and A.~Moussa and P.~Musico and M.~Musumeci and S.~Navas and C.~A.~Nicolau and I.~Olcina and C.~Olivetto and A.~Orlando and A.~Orzelli and A.~Papaikonomou and R.~Papaleo and G.~E.~Păvălaş and H.~Peek and G.~Pellegrini and C.~Pellegrino and C.~Perrina and M.~Pfutzner and P.~Piattelli and K.~Pikounis and M.-O.~Pleinert and G.~E.~Poma and V.~Popa and T.~Pradier and F.~Pratolongo and G.~Pühlhofer and S.~Pulvirenti and L.~Quinn and C.~Racca and F.~Raffaelli and N.~Randazzo and T.~Rauch and D.~Real and L.~Resvanis and J.~Reubelt and G.~Riccobene and C.~Rossi and A.~Rovelli and M.~Saldaña and I.~Salvadori and D.~F.~E.~Samtleben and A.~Sánchez García and A.~Sánchez Losa and M.~Sanguineti and A.~Santangelo and D.~Santonocito and P.~Sapienza and F.~Schimmel and J.~Schmelling and J.~Schnabel and V.~Sciacca and M.~Sedita and T.~Seitz and I.~Sgura and F.~Simeone and V.~Sipala and B.~Spisso and M.~Spurio and G.~Stavropoulos and J.~Steijger and S.~M.~Stellacci and D.~Stransky and M.~Taiuti and Y.~Tayalati and F.~Terrasi and D.~Tézier and S.~Theraube and P.~Timmer and C.~Tönnis and L.~Trasatti and R.~Travaglini and A.~Trovato and A.~Tsirigotis and S.~Tzamarias and E.~Tzamariudaki and B.~Vallage and V.~Van Elewyck and J.~Vermeulen and P.~Vicini and S.~Viola and D.~Vivolo and M.~Volkert and L.~Wiggers and J.~Wilms and E.~de Wolf and K.~Zachariadou and J.~D.~Zornoza and J.~Zúñiga}, title = {{I}ntrinsic limits on resolutions in muon- and electron-neutrino charged-current events in the {KM}3{N}e{T}/{ORCA} detector}, year = {2016}, eprint = {1612.05621}, howpublished = {The KM3NeT collaboration, Adri{\'a}n-Mart{\'\i}nez, S., Ageron, M. et al. J. High Energ. Phys. (2017) 2017: 8}, doi = {10.1007/JHEP05(2017)008}, note = {arXiv:1612.05621v2} }
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Studying atmospheric neutrino oscillations in the few-GeV range with a multimegaton detector promises to determine the neutrino mass hierarchy. This is the main science goal pursued by the future KM3NeT/ORCA water Cherenkov detector in the Mediterranean Sea. In this paper, the processes that limit the obtainable resolution in both energy and direction in charged-current neutrino events in the ORCA detector are investigated. These processes include the composition of the hadronic fragmentation products, the subsequent particle propagation and the photon-sampling fraction of the detector. GEANT simulations of neutrino interactions in seawater produced by GENIE are used to study the effects in the 1 - 20 GeV range. It is found that fluctuations in the hadronic cascade in conjunction with the variation of the inelasticity y are most detrimental to the resolutions. The effect of limited photon sampling in the detector is of significantly less importance. These results will therefore also be applicable to similar detectors/media, such as those in ice.
Letter of Intent for KM3NeT 2.0
S. Adrián-Martínez, M. Ageron, F. Aharonian, S. Aiello, A. Albert, F. Ameli, E. Anassontzis, M. Andre, G. Androulakis, M. Anghinolfi, G. Anton, M. Ardid, T. Avgitas, G. Barbarino, E. Barbarito, B. Baret, J. Barrios-Martí, B. Belhorma, A. Belias, E. Berbee, et al (227)
Jan 28 2016 astro-ph.IM astro-ph.HE hep-ex physics.ins-det arXiv:1601.07459v2

@misc{1601.07459, author = {S.~Adrián-Martínez and M.~Ageron and F.~Aharonian and S.~Aiello and A.~Albert and F.~Ameli and E.~Anassontzis and M.~Andre and G.~Androulakis and M.~Anghinolfi and G.~Anton and M.~Ardid and T.~Avgitas and G.~Barbarino and E.~Barbarito and B.~Baret and J.~Barrios-Martí and B.~Belhorma and A.~Belias and E.~Berbee and A.~van den Berg and V.~Bertin and S.~Beurthey and V.~van Beveren and N.~Beverini and S.~Biagi and A.~Biagioni and M.~Billault and M.~Bond and R.~Bormuth and B.~Bouhadef and G.~Bourlis and S.~Bourret and C.~Boutonnet and M.~Bouwhuis and C.~Bozza and R.~Bruijn and J.~Brunner and E.~Buis and J.~Busto and G.~Cacopardo and L.~Caillat and M.~Calamai and D.~Calvo and A.~Capone and L.~Caramete and S.~Cecchini and S.~Celli and C.~Champion and R.~Cherkaoui El Moursli and S.~Cherubini and T.~Chiarusi and M.~Circella and L.~Classen and R.~Cocimano and J.~A.~B.~Coelho and A.~Coleiro and S.~Colonges and R.~Coniglione and M.~Cordelli and A.~Cosquer and P.~Coyle and A.~Creusot and G.~Cuttone and A.~D'Amico and G.~De Bonis and G.~De Rosa and C.~De Sio and F.~Di Capua and I.~Di Palma and A.~F.~Díaz García and C.~Distefano and C.~Donzaud and D.~Dornic and Q.~Dorosti-Hasankiadeh and E.~Drakopoulou and D.~Drouhin and L.~Drury and M.~Durocher and T.~Eberl and S.~Eichie and D.~van Eijk and I.~El Bojaddaini and N.~El Khayati and D.~Elsaesser and A.~Enzenhöfer and F.~Fassi and P.~Favali and P.~Fermani and G.~Ferrara and G.~Frascadore and C.~Filippidis and L.~A.~Fusco and T.~Gal and S.~Galatà and F.~Garufi and P.~Gay and M.~Gebyehu and V.~Giordano and N.~Gizani and R.~Gracia and K.~Graf and T.~Grégoire and G.~Grella and R.~Habel and S.~Hallmann and H.~van Haren and S.~Harissopulos and T.~Heid and A.~Heijboer and E.~Heine and S.~Henry and J.~J.~Hernández-Rey and M.~Hevinga and J.~Hofestädt and C.~M.~F.~Hugon and G.~Illuminati and C.~W.~James and P.~Jansweijer and M.~Jongen and M.~de Jong and M.~Kadler and O.~Kalekin and A.~Kappes and U.~F.~Katz and P.~Keller and G.~Kieft and D.~Kießling and E.~N.~Koffeman and P.~Kooijman and A.~Kouchner and V.~Kulikovskiy and R.~Lahmann and P.~Lamare and A.~Leisos and E.~Leonora and M.~Lindsey Clark and A.~Liolios and C.~D.~Llorens Alvarez and D.~Lo Presti and H.~Löhner and A.~Lonardo and M.~Lotze and S.~Loucatos and E.~Maccioni and K.~Mannheim and A.~Margiotta and A.~Marinelli and O.~Mariş and C.~Markou and J.~A.~Martínez-Mora and A.~Martini and R.~Mele and K.~W.~Melis and T.~Michael and P.~Migliozzi and E.~Migneco and P.~Mijakowski and A.~Miraglia and C.~M.~Mollo and M.~Mongelli and M.~Morganti and A.~Moussa and P.~Musico and M.~Musumeci and S.~Navas and C.~A.~Nicolau and I.~Olcina and C.~Olivetto and A.~Orlando and A.~Papaikonomou and R.~Papaleo and G.~E.~Păvălaş and H.~Peek and C.~Pellegrino and C.~Perrina and M.~Pfutzner and P.~Piattelli and K.~Pikounis and G.~E.~Poma and V.~Popa and T.~Pradier and F.~Pratolongo and G.~Pühlhofer and S.~Pulvirenti and L.~Quinn and C.~Racca and F.~Raffaelli and N.~Randazzo and P.~Rapidis and P.~Razis and D.~Real and L.~Resvanis and J.~Reubelt and G.~Riccobene and C.~Rossi and A.~Rovelli and M.~Saldaña and I.~Salvadori and D.~F.~E.~Samtleben and A.~Sánchez García and A.~Sánchez Losa and M.~Sanguineti and A.~Santangelo and D.~Santonocito and P.~Sapienza and F.~Schimmel and J.~Schmelling and V.~Sciacca and M.~Sedita and T.~Seitz and I.~Sgura and F.~Simeone and I.~Siotis and V.~Sipala and B.~Spisso and M.~Spurio and G.~Stavropoulos and J.~Steijger and S.~M.~Stellacci and D.~Stransky and M.~Taiuti and Y.~Tayalati and D.~Tézier and S.~Theraube and L.~Thompson and P.~Timmer and C.~Tönnis and L.~Trasatti and A.~Trovato and A.~Tsirigotis and S.~Tzamarias and E.~Tzamariudaki and B.~Vallage and V.~Van Elewyck and J.~Vermeulen and P.~Vicini and S.~Viola and D.~Vivolo and M.~Volkert and G.~Voulgaris and L.~Wiggers and J.~Wilms and E.~de Wolf and K.~Zachariadou and J.~D.~Zornoza and J.~Zúñiga}, title = {{L}etter of {I}ntent for {KM}3{N}e{T} 2.0}, year = {2016}, eprint = {1601.07459}, howpublished = {Journal of Physics G: Nuclear and Particle Physics, 43 (8), 084001, 2016}, doi = {10.1088/0954-3899/43/8/084001}, note = {arXiv:1601.07459v2} }
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The main objectives of the KM3NeT Collaboration are i) the discovery and subsequent observation of high-energy neutrino sources in the Universe and ii) the determination of the mass hierarchy of neutrinos. These objectives are strongly motivated by two recent important discoveries, namely: 1) The high-energy astrophysical neutrino signal reported by IceCube and 2) the sizable contribution of electron neutrinos to the third neutrino mass eigenstate as reported by Daya Bay, Reno and others. To meet these objectives, the KM3NeT Collaboration plans to build a new Research Infrastructure consisting of a network of deep-sea neutrino telescopes in the Mediterranean Sea. A phased and distributed implementation is pursued which maximises the access to regional funds, the availability of human resources and the synergetic opportunities for the earth and sea sciences community. Three suitable deep-sea sites are identified, namely off-shore Toulon (France), Capo Passero (Italy) and Pylos (Greece). The infrastructure will consist of three so-called building blocks. A building block comprises 115 strings, each string comprises 18 optical modules and each optical module comprises 31 photo-multiplier tubes. Each building block thus constitutes a 3-dimensional array of photo sensors that can be used to detect the Cherenkov light produced by relativistic particles emerging from neutrino interactions. Two building blocks will be configured to fully explore the IceCube signal with different methodology, improved resolution and complementary field of view, including the Galactic plane. One building block will be configured to precisely measure atmospheric neutrino oscillations.
The prototype detection unit of the KM3NeT detector
KM3NeT Collaboration, S. Adrián-Martínez, M. Ageron, F. Aharonian, S. Aiello, A. Albert, F. Ameli, E.G. Anassontzis, G.C. Androulakis, M. Anghinolfi, G. Anton, S. Anvar, M. Ardid, T. Avgitas, K. Balasi, H. Band, G. Barbarino, E. Barbarito, F. Barbato, B. Baret, et al (229)
Oct 07 2015 astro-ph.IM hep-ex physics.ins-det arXiv:1510.01561v2

@misc{1510.01561, author = {KM3NeT Collaboration and S.~Adrián-Martínez and M.~Ageron and F.~Aharonian and S.~Aiello and A.~Albert and F.~Ameli and E.G.~Anassontzis and G.C.~Androulakis and M.~Anghinolfi and G.~Anton and S.~Anvar and M.~Ardid and T.~Avgitas and K.~Balasi and H.~Band and G.~Barbarino and E.~Barbarito and F.~Barbato and B.~Baret and S.~Baron and J.~Barrios and A.~Belias and E.~Berbee and A.M.~van den Berg and A.~Berkien and V.~Bertin and S.~Beurthey and V.~van Beveren and N.~Beverini and S.~Biagi and A.~Biagioni and S.~Bianucci and M.~Billault and A.~Birbas and H.~Boer Rookhuizen and R.~Bormuth and V.~Bouché and B.~Bouhadef and G.~Bourlis and C.~Boutonnet and M.~Bouwhuis and C.~Bozza and R.~Bruijn and J.~Brunner and G.~Cacopardo and L.~Caillat and M.~Calamai and D.~Calvo and A.~Capone and L.~Caramete and F.~Caruso and S.~Cecchini and A.~Ceres and R.~Cereseto and C.~Champion and F.~Château and T.~Chiarusi and B.~Christopoulou and M.~Circella and L.~Classen and R.~Cocimano and A.~Coleiro and S.~Colonges and R.~Coniglione and A.~Cosquer and M.~Costa and P.~Coyle and A.~Creusot and G.~Cuttone and C.~D'Amato and A.~D'Amico and G.~De Bonis and G.~De Rosa and N.~Deniskina and J.-J.~Destelle and C.~Distefano and F.~Di Capua and C.~Donzaud and D.~Dornic and Q.~Dorosti-Hasankiadeh and E.~Drakopoulou and D.~Drouhin and L.~Drury and D.~Durand and T.~Eberl and D.~Elsaesser and A.~Enzenhöfer and P.~Fermani and L.A.~Fusco and D.~Gajanana and T.~Gal and S.~Galatà and F.~Garufi and M.~Gebyehu and V.~Giordano and N.~Gizani and R.~GraciaRuiz and K.~Graf and R.~Grasso and G.~Grella and A.~Grmek and R.~Habel and H.~van Haren and T.~Heid and A.~Heijboer and E.~Heine and S.~Henry and J.J.~Hernández-Rey and B.~Herold and M.A.~Hevinga and M.~van der Hoek and J.~Hofestädt and J.~Hogenbirk and C.~Hugon and J.~Hößl and M.~Imbesi and C.W.~James and P.~Jansweijer and J.~Jochum and M.~de Jong and M.~Jongen and M.~Kadler and O.~Kalekin and A.~Kappes and E.~Kappos and U.~Katz and O.~Kavatsyuk and P.~Keller and G.~Kieft and E.~Koffeman and H.~Kok and P.~Kooijman and J.~Koopstra and A.~Korporaal and A.~Kouchner and I.~Kreykenbohm and V.~Kulikovskiy and R.~Lahmann and P.~Lamare and G.~Larosa and D.~Lattuada and H.~Le Provost and K.P.~Leismüller and A.~Leisos and D.~Lenis and E.~Leonora and M.~LindseyClark and C.D.~Llorens Alvarez and H.~Löhner and A.~Lonardo and S.~Loucatos and F.~Louis and E.~Maccioni and K.~Mannheim and K.~Manolopoulos and A.~Margiotta and O.~Mariş and C.~Markou and J.A.~Martínez-Mora and A.~Martini and R.~Masullo and K.W.~Melis and T.~Michael and P.~Migliozzi and E.~Migneco and A.~Miraglia and C.M.~Mollo and M.~Mongelli and M.~Morganti and S.~Mos and Y.~Moudden and P.~Musico and M.~Musumeci and C.~Nicolaou and C.A.~Nicolau and A.~Orlando and A.~Orzelli and A.~Papaikonomou and R.~Papaleo and G.E.~Păvălaş and H.~Peek and C.~Pellegrino and M.G.~Pellegriti and C.~Perrina and P.~Piattelli and K.~Pikounis and V.~Popa and Th.~Pradier and M.~Priede and G.~Pühlhofer and S.~Pulvirenti and C.~Racca and F.~Raffaelli and N.~Randazzo and P.A.~Rapidis and P.~Razis and D.~Real and L.~Resvanis and J.~Reubelt and G.~Riccobene and A.~Rovelli and M.~Saldaña and D.F.E.~Samtleben and M.~Sanguineti and A.~Santangelo and P.~Sapienza and J.~Schmelling and J.~Schnabel and V.~Sciacca and M.~Sedita and T.~Seitz and I.~Sgura and F.~Simeone and V.~Sipala and A.~Spitaleri and M.~Spurio and G.~Stavropoulos and J.~Steijger and T.~Stolarczyk and D.~Stransky and M.~Taiuti and G.~Terreni and D.~Tézier and S.~Théraube and L.F.~Thompson and P.~Timmer and L.~Trasatti and A.~Trovato and M.~Tselengidou and A.~Tsirigotis and S.~Tzamarias and E.~Tzamariudaki and B.~Vallage and V.~Van Elewyck and J.~Vermeulen and P.~Vernin and P.~Vicini and S.~Viola and D.~Vivolo and P.~Werneke and L.~Wiggers and J.~Wilms and E.~de Wolf and R.H.L.~van Wooning and E.~Zonca and J.D.~Zornoza and J.~Zúñiga and A.~Zwart}, title = {{T}he prototype detection unit of the {KM}3{N}e{T} detector}, year = {2015}, eprint = {1510.01561}, note = {arXiv:1510.01561v2} }
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A prototype detection unit of the KM3NeT deep-sea neutrino telescope has been installed at 3500m depth 80km offshore the Italian coast. KM3NeT in its final configuration will contain several hundreds of detection units. Each detection unit is a mechanical structure anchored to the sea floor, held vertical by a submerged buoy and supporting optical modules for the detection of Cherenkov light emitted by charged secondary particles emerging from neutrino interactions. This prototype string implements three optical modules with 31 photomultiplier tubes each. These optical modules were developed by the KM3NeT Collaboration to enhance the detection capability of neutrino interactions. The prototype detection unit was operated since its deployment in May 2014 until its decommissioning in July 2015. Reconstruction of the particle trajectories from the data requires a nanosecond accuracy in the time calibration. A procedure for relative time calibration of the photomultiplier tubes contained in each optical module is described. This procedure is based on the measured coincidences produced in the sea by the 40K background light and can easily be expanded to a detector with several thousands of optical modules. The time offsets between the different optical modules are obtained using LED nanobeacons mounted inside them. A set of data corresponding to 600 hours of livetime was analysed. The results show good agreement with Monte Carlo simulations of the expected optical background and the signal from atmospheric muons. An almost background-free sample of muons was selected by filtering the time correlated signals on all the three optical modules. The zenith angle of the selected muons was reconstructed with a precision of about 3\deg.
Long term monitoring of the optical background in the Capo Passero deep-sea site with the NEMO tower prototype
S. Adrián-Martínez, S. Aiello, F. Ameli, M. Anghinolfi, M. Ardid, G. Barbarino, E. Barbarito, F.C.T. Barbato, N. Beverini, S. Biagi, A. Biagioni, B. Bouhadef, C. Bozza, G. Cacopardo, M. Calamai, C. Calí, D. Calvo, A. Capone, F. Caruso, A. Ceres, et al (84)
Jul 20 2015 physics.ins-det arXiv:1507.05024v2

@misc{1507.05024, author = {S.~Adrián-Martínez and S.~Aiello and F.~Ameli and M.~Anghinolfi and M.~Ardid and G.~Barbarino and E.~Barbarito and F.C.T.~Barbato and N.~Beverini and S.~Biagi and A.~Biagioni and B.~Bouhadef and C.~Bozza and G.~Cacopardo and M.~Calamai and C.~Calí and D.~Calvo and A.~Capone and F.~Caruso and A.~Ceres and T.~Chiarusi and M.~Circella and R.~Cocimano and R.~Coniglione and M.~Costa and G.~Cuttone and C.~D'Amato and A.~D'Amico and G.~De Bonis and V.~De Luca and N.~Deniskina and G.~De Rosa and F.~di Capua and C.~Distefano and A.~Enzenhöfer and P.~Fermani and G.~Ferrara and V.~Flaminio and L.A.~Fusco and F.~Garufi and V.~Giordano and A.~Gmerk and R.~Grasso and G.~Grella and C.~Hugon and M.~Imbesi and V.~Kulikovskiy and R.~Lahmann and G.~Larosa and D.~Lattuada and K.P.~Leismüller and E.~Leonora and P.~Litrico and C.~D.~Llorens Alvarez and A.~Lonardo and F.~Longhitano and D.~Lo Presti and E.~Maccioni and A.~Margiotta and A.~Marinelli and A.~Martini and R.~Masullo and P.~Migliozzi and E.~Migneco and A.~Miraglia and C.M.~Mollo and M.~Mongelli and M.~Morganti and P.~Musico and M.~Musumeci and C.A.~Nicolau and A.~Orlando and A.~Orzelli and R.~Papaleo and C.~Pellegrino and M.G.~Pellegriti and C.~Perrina and P.~Piattelli and C.~Pugliatti and S.~Pulvirenti and F.~Raffaelli and N.~Randazzo and D.~Real and G.~Riccobene and A.~Rovelli and M.~Saldaña and M.~Sanguineti and P.~Sapienza and V.~Sciacca and I.~Sgura and F.~Simeone and V.~Sipala and F.~Speziale and A.~Spitaleri and M.~Spurio and S.M.~Stellacci and M.~Taiuti and G.~Terreni and L.~Trasatti and A.~Trovato and C.~Ventura and P.~Vicini and S.~Viola and D.~Vivolo}, title = {{L}ong term monitoring of the optical background in the {C}apo {P}assero deep-sea site with the {NEMO} tower prototype}, year = {2015}, eprint = {1507.05024}, note = {arXiv:1507.05024v2} }
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The NEMO Phase-2 tower is the first detector which was operated underwater for more than one year at the "record" depth of 3500 m. It was designed and built within the framework of the NEMO (NEutrino Mediterranean Observatory) project. The 380 m high tower was successfully installed in March 2013 80 km offshore Capo Passero (Italy). This is the first prototype operated on the site where the italian node of the KM3NeT neutrino telescope will be built. The installation and operation of the NEMO Phase-2 tower has proven the functionality of the infrastructure and the operability at 3500 m depth. A more than one year long monitoring of the deep water characteristics of the site has been also provided. In this paper the infrastructure and the tower structure and instrumentation are described. The results of long term optical background measurements are presented. The rates show stable and low baseline values, compatible with the contribution of 40K light emission, with a small percentage of light bursts due to bioluminescence. All these features confirm the stability and good optical properties of the site.
Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope
S. Adrián-Martínez, A. Albert, M. André, G. Anton, M. Ardid, J.-J. Aubert, B. Baret, J. Barrios-Martí, S. Basa, V. Bertin, S. Biagi, C. Bogazzi, R. Bormuth, M. Bou-Cabo, M.C. Bouwhuis, R. Bruijn, J. Brunner, J. Busto, A. Capone, L. Caramete, et al (110)
Jul 16 2015 physics.ins-det astro-ph.IM hep-ex arXiv:1507.04182v1

@misc{1507.04182, author = {S.~Adrián-Martínez and A.~Albert and M.~André and G.~Anton and M.~Ardid and J.-J.~Aubert and B.~Baret and J.~Barrios-Martí and S.~Basa and V.~Bertin and S.~Biagi and C.~Bogazzi and R.~Bormuth and M.~Bou-Cabo and M.C.~Bouwhuis and R.~Bruijn and J.~Brunner and J.~Busto and A.~Capone and L.~Caramete and J.~Carr and T.~Chiarusi and M.~Circella and R.~Coniglione and H.~Costantini and P.~Coyle and A.~Creusot and I.~Dekeyser and A.~Deschamps and G.~De Bonis and C.~Distefano and C.~Donzaud and D.~Dornic and D.~Drouhin and A.~Dumas and T.~Eberl and D.~Elsässer and A.~Enzenhöfer and K.~Fehn and I.~Felis and P.~Fermani and V.~Flaminio and F.~Folger and L.A.~Fusco and S.~Galatà and P.~Gay and S.~Geißelsöder and K.~Geyer and V.~Giordano and A.~Gleixner and R.~Gracia-Ruiz and J.P.~Gómez-González and K.~Graf and H.~van Haren and A.J.~Heijboer and Y.~Hello and J.J.~Hernández-Rey and A.~Herrero and J.~Hößl and J.~Hofestädt and C.~Hugon and C.W James and M.~de Jong and M.~Kadler and O.~Kalekin and U.~Katz and D.~Kießling and P.~Kooijman and A.~Kouchner and I.~Kreykenbohm and V.~Kulikovskiy and R Lahmann and G.~Lambard and D.~Lattuada and D.~Lefèvre and E.~Leonora and S.~Loucatos and S.~Mangano and M.~Marcelin and A.~Margiotta and A.~Marinelli and J.A.~Martínez-Mora and S.~Martini and A.~Mathieu and T.~Michael and P.~Migliozzi and A.~Moussa and C.~Mueller and M.~Neff and E.~Nezri and G.E.~Păvălaş and C.~Pellegrino and C.~Perrina and P.~Piattelli and V.~Popa and T.~Pradier and C.~Racca and G.~Riccobene and R.~Richter and K.~Roensch and A.~Rostovtsev and M.~Saldaña and D.~F.~E.~Samtleben and A.~Sánchez-Losa and M.~Sanguineti and P.~Sapienza and J.~Schmid and J.~Schnabel and S.~Schulte and F.~Schüssler and T.~Seitz and C.~Sieger and M.~Spurio and J.J.M.~Steijger and Th.~Stolarczyk and M.~Taiuti and C.~Tamburini and A.~Trovato and M.~Tselengidou and C.~Tönnis and D.~Turpin and B.~Vallage and C.~Vallée and V.~Van Elewyck and E.~Visser and D.~Vivolo and S.~Wagner and J.~Wilms and J.D.~Zornoza and J.~Zúñiga}, title = {{T}ime calibration with atmospheric muon tracks in the {ANTARES} neutrino telescope}, year = {2015}, eprint = {1507.04182}, note = {arXiv:1507.04182v1} }
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The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of $\sim$10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices.
Proton recoil telescope based on diamond detectors for measurement of fusion neutrons
B. Caiffi, M. Osipenko, M. Ripani, M. Pillon, M. Taiuti
May 26 2015 physics.ins-det nucl-ex arXiv:1505.06316v1

@misc{1505.06316, author = {B.~Caiffi and M.~Osipenko and M.~Ripani and M.~Pillon and M.~Taiuti}, title = {{P}roton recoil telescope based on diamond detectors for measurement of fusion neutrons}, year = {2015}, eprint = {1505.06316}, note = {arXiv:1505.06316v1} }
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Diamonds are very promising candidates for the neutron diagnostics in harsh environments such as fusion reactor. In the first place this is because of their radiation hardness, exceeding that of Silicon by an order of magnitude. Also, in comparison to the standard on-line neutron diagnostics (fission chambers, silicon based detectors, scintillators), diamonds are less sensitive to $\gamma$ rays, which represent a huge background in fusion devices. Finally, their low leakage current at high temperature suppresses the detector intrinsic noise. In this talk a CVD diamond based detector has been proposed for the measurement of the 14 MeV neutrons from D-T fusion reaction. The detector was arranged in a proton recoil telescope configuration, featuring a plastic converter in front of the sensitive volume in order to induce the (n,p) reaction. The segmentation of the sensitive volume, achieved by using two crystals, allowed to perform measurements in coincidence, which suppressed the neutron elastic scattering background. A preliminary prototype was assembled and tested at FNG (Frascati Neutron Generator, ENEA), showing promising results regarding efficiency and energy resolution.
Measurement of the atmospheric muon depth intensity relation with the NEMO Phase-2 tower
S. Aiello, F. Ameli, M. Anghinolfi, G. Barbarino, E. Barbarito, F. Barbato, N. Beverini, S. Biagi, B. Bouhadef, C. Bozza, G. Cacopardo, M. Calamai, C. Calì, A. Capone, F. Caruso, A. Ceres, T. Chiarusi, M. Circella, R. Cocimano, R. Coniglione, et al (73)
Dec 03 2014 physics.ins-det astro-ph.IM hep-ex arXiv:1412.0849v2

@misc{1412.0849, author = {S.~Aiello and F.~Ameli and M.~Anghinolfi and G.~Barbarino and E.~Barbarito and F.~Barbato and N.~Beverini and S.~Biagi and B.~Bouhadef and C.~Bozza and G.~Cacopardo and M.~Calamai and C.~Calì and A.~Capone and F.~Caruso and A.~Ceres and T.~Chiarusi and M.~Circella and R.~Cocimano and R.~Coniglione and M.~Costa and G.~Cuttone and C.~D'Amato and A.~D'Amico and G.~De Bonis and V.~De Luca and N.~Deniskina and G.~De Rosa and F.~Di Capua and C.~Distefano and P.~Fermani and L.A.~Fusco and F.~Garufi and V.~Giordano and A.~Gmerk and R.~Grasso and G.~Grella and C.~Hugon and M.~Imbesi and V.~Kulikovskiy and G.~Larosa and D.~Lattuada and K.P.~Leismueller and E.~Leonora and P.~Litrico and A.~Lonardo and F.~Longhitano and D.~Lo Presti and E.~Maccioni and A.~Margiotta and A.~Martini and R.~Masullo and P.~Migliozzi and E.~Migneco and A.~Miraglia and C.M.~Mollo and M.~Mongelli and M.~Morganti and P.~Musico and M.~Musumeci and C.A.~Nicolau and A.~Orlando and R.~Papaleo and C.~Pellegrino and M.G.~Pellegriti and C.~Perrina and P.~Piattelli and C.~Pugliatti and S.~Pulvirenti and A.~Orselli and F.~Raffaelli and N.~Randazzo and G.~Riccobene and A.~Rovelli and M.~Sanguineti and P.~Sapienza and V.~Sciacca and I.~Sgura and F.~Simeone and V.~Sipala and F.~Speziale and M.~Spina and A.~Spitaleri and M.~Spurio and S.M.~Stellacci and M.~Taiuti and G.~Terreni and L.~Trasatti and A.~Trovato and C.~Ventura and P.~Vicini and S.~Viola and D.~Vivolo}, title = {{M}easurement of the atmospheric muon depth intensity relation with the {NEMO} {P}hase-2 tower}, year = {2014}, eprint = {1412.0849}, note = {arXiv:1412.0849v2} }
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The results of the analysis of the data collected with the NEMO Phase-2 tower, deployed at 3500 m depth about 80 km off-shore Capo Passero (Italy), are presented. Cherenkov photons detected with the photomultipliers tubes were used to reconstruct the tracks of atmospheric muons. Their zenith-angle distribution was measured and the results compared with Monte Carlo simulations. An evaluation of the systematic effects due to uncertainties on environmental and detector parameters is also included. The associated depth intensity relation was evaluated and compared with previous measurements and theoretical predictions. With the present analysis, the muon depth intensity relation has been measured up to 13 km of water equivalent.
Dark matter search in a Beam-Dump eXperiment (BDX) at Jefferson Lab
BDX Collaboration, M. Battaglieri, A. Celentano, R. De Vita, E. Izaguirre, G. Krnjaic, E. Smith, S. Stepanyan, A. Bersani, E. Fanchini, S. Fegan, P. Musico, M. Osipenko, M. Ripani, E. Santopinto, M. Taiuti, P. Schuster, N. Toro, M. Dalton, A. Freyberger, et al (66)
Jun 13 2014 physics.ins-det astro-ph.IM hep-ex hep-ph nucl-ex arXiv:1406.3028v1

@misc{1406.3028, author = {BDX Collaboration and M.~Battaglieri and A.~Celentano and R.~De Vita and E.~Izaguirre and G.~Krnjaic and E.~Smith and S.~Stepanyan and A.~Bersani and E.~Fanchini and S.~Fegan and P.~Musico and M.~Osipenko and M.~Ripani and E.~Santopinto and M.~Taiuti and P.~Schuster and N.~Toro and M.~Dalton and A.~Freyberger and F.-X.~Girod and V.~Kubarovsky and M.~Ungaro and G.~De Cataldo and R.~De Leo and D.~Di Bari and L.~Lagamba and E.~Nappi and R.~Perrino and M.~Carpinelli and V.~Sipala and S.~Aiello and V.~Bellini and M.~De Napoli and A.~Giusa and F.~Mammoliti and E.~Leonora and F.~Noto and N.~Randazzo and G.~Russo and M.~Sperduto and C.~Sutera and C.~Ventura and L.~Barion and G.~Ciullo and M.~Contalbrigo and P.~Lenisa and A.~Movsisyan and F.~Spizzo and M.~Turisini and F.~De Persio and E.~Cisbani and C.~Fanelli and F.~Garibaldi and F.~Meddi and G.~M.~Urciuoli and S.~Anefalos Pereira and E.~De Sanctis and D.~Hasch and V.~Lucherini and M.~Mirazita and R.~Montgomery and S.~Pisano and G.~Simi and A.~D'Angelo and L.~Colaneri L.~Lanza and A.~Rizzo and C.~Schaerf and I.~Zonta and D.~Calvo and A.~Filippi and M.Holtrop and R.~Peremuzyan and D.~Glazier and D.~Ireland and B.~McKinnon and D.~Sokhan A.~Afanasev and B.~Briscoe and N.~Kalantarians and L.El Fassi and L.Weinstein and P.~Beltrame and A.~Murphy and D.~Watts and L.~Zana and K.~Hicks}, title = {{D}ark matter search in a {B}eam-{D}ump e{X}periment ({BDX}) at {J}efferson {L}ab}, year = {2014}, eprint = {1406.3028}, note = {arXiv:1406.3028v1} }
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MeV-GeV dark matter (DM) is theoretically well motivated but remarkably unexplored. This Letter of Intent presents the MeV-GeV DM discovery potential for a 1 m$^3$ segmented plastic scintillator detector placed downstream of the beam-dump at one of the high intensity JLab experimental Halls, receiving up to 10$^{22}$ electrons-on-target (EOT) in a one-year period. This experiment (Beam-Dump eXperiment or BDX) is sensitive to DM-nucleon elastic scattering at the level of a thousand counts per year, with very low threshold recoil energies ($\sim$1 MeV), and limited only by reducible cosmogenic backgrounds. Sensitivity to DM-electron elastic scattering and/or inelastic DM would be below 10 counts per year after requiring all electromagnetic showers in the detector to exceed a few-hundred MeV, which dramatically reduces or altogether eliminates all backgrounds. Detailed Monte Carlo simulations are in progress to finalize the detector design and experimental set up. An existing 0.036 m$^3$ prototype based on the same technology will be used to validate simulations with background rate estimates, driving the necessary R$\&$D towards an optimized detector. The final detector design and experimental set up will be presented in a full proposal to be submitted to the next JLab PAC. A fully realized experiment would be sensitive to large regions of DM parameter space, exceeding the discovery potential of existing and planned experiments by two orders of magnitude in the MeV-GeV DM mass range.
Deep sea tests of a prototype of the KM3NeT digital optical module
S. Adrián-Martínez, M. Ageron, F. Aharonian, S. Aiello, A. Albert, F. Ameli, E.G. Anassontzis, M. Anghinolfi, G. Anton, S. Anvar, M. Ardid, R. de Asmundis, K. Balasi, H. Band, G. Barbarino, E. Barbarito, F. Barbato, B. Baret, S. Baron, A. Belias, et al (230)
May 06 2014 astro-ph.IM physics.ins-det arXiv:1405.0839v2

@misc{1405.0839, author = {S.~Adrián-Martínez and M.~Ageron and F.~Aharonian and S.~Aiello and A.~Albert and F.~Ameli and E.G.~Anassontzis and M.~Anghinolfi and G.~Anton and S.~Anvar and M.~Ardid and R.~de Asmundis and K.~Balasi and H.~Band and G.~Barbarino and E.~Barbarito and F.~Barbato and B.~Baret and S.~Baron and A.~Belias and E.~Berbee and A.M.~van den Berg and A.~Berkien and V.~Bertin and S.~Beurthey and V.~van Beveren and N.~Beverini and S.~Biagi and S.~Bianucci and M.~Billault and A.~Birbas and H.~Boer Rookhuizen and R.~Bormuth and V.~Bouche and B.~Bouhadef and G.~Bourlis and M.~Bouwhuis and C.~Bozza and R.~Bruijn and J.~Brunner and G.~Cacopardo and L.~Caillat and M.~Calamai and D.~Calvo and A.~Capone and L.~Caramete and F.~Caruso and S.~Cecchini and A.~Ceres and R.~Cereseto and C.~Champion and F.~Chateau and T.~Chiarusi and B.~Christopoulou and M.~Circella and L.~Classen and R.~Cocimano and S.~Colonges and R.~Coniglione and A.~Cosquer and M.~Costa and P.~Coyle and A.~Creusot and C.~Curtil and G.~Cuttone and C.~D'Amato and A.~D'Amico and G.~De Bonis and G.~De Rosa and N.~Deniskina and J.-J.~Destelle and C.~Distefano and C.~Donzaud and D.~Dornic and Q.~Dorosti-Hasankiadeh and E.~Drakopoulou7 and D.~Drouhin and L.~Drury and D.~Durand and T.~Eberl and C.~Eleftheriadis and D.~Elsaesser and A.~Enzenhofer and P.~Fermani and L.~A.~Fusco and D.~Gajana and T.~Gal and S.~Galata and F.~Gallo and F.~Garufi and M.~Gebyehu and V.~Giordano and N.~Gizani and R.~Gracia Ruiz and K.~Graf and R.~Grasso and G.~Grella and A.~Grmek and R.~Habel and H.~van Haren and T.~Heid and A.~Heijboer and E.~Heine and S.~Henry and J.J.~Hernandez-Rey and B.~Herold and M.A.~Hevinga and M.~van der Hoek and J.~Hofestadt and J.~Hogenbirk and C.~Hugon and J.~Hosl and M.~Imbesi and C.~James and P.~Jansweijer and J.~Jochum and M.~de Jong and M.~Kadler and O.~Kalekin and A.~Kappes and E.~Kappos and U.~Katz and O.~Kavatsyuk and P.~Keller and G.~Kieft and E.~Koffeman and H.~Kok and P.~Kooijman and J.~Koopstra and A.~Korporaal and A.~Kouchner and S.~Koutsoukos and I.~Kreykenbohm and V.~Kulikovskiy and R.~Lahmann and P.~Lamare and G.~Larosa and D.~Lattuada and H.~Le Provost and A.~Leisos and D.~Lenis and E.~Leonora and M.~Lindsey Clark and A.~Liolios and C.~D.~Llorens Alvarez and H.~Lohner and D.~Lo Presti and F.~Louis and E.~Maccioni and K.~Mannheim and K.~Manolopoulos and A.~Margiotta and O.~Maris and C.~Markou and J.~A.~Martinez-Mora and A.~Martini and R.~Masullo and T.~Michael and P.~Migliozzi and E.~Migneco and A.~Miraglia and C.~Mollo and M.~Mongelli and M.~Morganti and S.~Mos and Y.~Moudden and P.~Musico and M.~Musumeci and C.~Nicolaou and C.~A.~Nicolau and A.~Orlando and A.~Orzelli and K.~Papageorgiou and A.~Papaikonomou and R.~Papaleo and G.E.~Pavalas and H.~Peek and C.~Pellegrino and M.~G.~Pellegriti and C.~Perrina and C.~Petridou and P.~Piattelli and K.~Pikounis and V.~Popa and Th.~Pradier and M.~Priede and G.~Puhlhofer and S.~Pulvirenti and C.~Racca and F.~Raffaelli and N.~Randazzo and P.A.~Rapidis and P.~Razis and D.~Real and L.~Resvanis and J.~Reubelt and G.~Riccobene and A.~Rovelli and J.~Royon and M.~Saldana and D.F.E.~Samtleben and M.~Sanguineti and A.~Santangelo and P.~Sapienza and I.~Savvidis and J.~Schmelling and J.~Schnabel and M.~Sedita and T.~Seitz and I.~Sgura and F.~Simeone and I.~Siotis and V.~Sipala and M.~Solazzo and A.~Spitaleri and M.~Spurio and G.~Stavropoulos and J.~Steijger and T.~Stolarczyk and D.~Stransky and M.~Taiuti and G.~Terreni and D.~Tezier and S.~Theraube and L.F.~Thompson and P.~Timmer and H.I.~Trapierakis and L.~Trasatti and A.~Trovato and M.~Tselengidou and A.~Tsirigotis and S.~Tzamarias and E.~Tzamariudaki and B.~Vallage and V.~Van Elewyck and J.~Vermeulen and P.~Vernin and S.~Viola and D.~Vivolo and P.~Werneke and L.~Wiggers and J.~Wilms and E.~de Wolf and R.H.L.~van Wooning and K.~Yatkin and K.~Zachariadou and E.~Zonca and J.D.~Zornoza and J.~Zúñiga and A.~Zwart}, title = {{D}eep sea tests of a prototype of the {KM}3{N}e{T} digital optical module}, year = {2014}, eprint = {1405.0839}, note = {arXiv:1405.0839v2} }
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The first prototype of a photo-detection unit of the future KM3NeT neutrino telescope has been deployed in the deep waters of the Mediterranean Sea. This digital optical module has a novel design with a very large photocathode area segmented by the use of 31 three inch photomultiplier tubes. It has been integrated in the ANTARES detector for in-situ testing and validation. This paper reports on the first months of data taking and rate measurements. The analysis results highlight the capabilities of the new module design in terms of background suppression and signal recognition. The directionality of the optical module enables the recognition of multiple Cherenkov photons from the same $^{40}$K decay and the localization bioluminescent activity in the neighbourhood. The single unit can cleanly identify atmospheric muons and provide sensitivity to the muon arrival directions.
A Fast Algorithm for Muon Track Reconstruction and its Application to the ANTARES Neutrino Telescope
ANTARES collaboration, J.A. Aguilar, I. Al Samarai, A. Albert, M. Andre, M. Anghinolfi, G. Anton, S. Anvar, M. Ardid, A.C. Assis Jesus, T. Astraatmadja, J-J. Aubert, R. Auer, B. Baret, S. Basa, M. Bazzotti, V. Bertin, S. Biagi, C. Bigongiari, C. Bogazzi, et al (123)
May 23 2011 astro-ph.IM astro-ph.HE hep-ex physics.data-an arXiv:1105.4116v1

@misc{1105.4116, author = {ANTARES collaboration and J.A.~Aguilar and I.~Al Samarai and A.~Albert and M.~Andre and M.~Anghinolfi and G.~Anton and S.~Anvar and M.~Ardid and A.C.~Assis Jesus and T.~Astraatmadja and J-J.~Aubert and R.~Auer and B.~Baret and S.~Basa and M.~Bazzotti and V.~Bertin and S.~Biagi and C.~Bigongiari and C.~Bogazzi and M.~Bou-Cabo and M.C.~Bouwhuis and A.M.~Brown and J.~Brunner and J.~Busto and F.~Camarena and A.~Capone and C.Carloganu and G.~Carminati and J.~Carr and S.~Cecchini and Ph.~Charvis and T.~Chiarusi and M.~Circella and R.~Coniglione and H.~Costantini and N.~Cottini and P.~Coyle and C.~Curtil and M.P.~Decowski and I.~Dekeyser and A.~Deschamps and C.~Distefano and C.~Donzaud and D.~Dornic and Q.~Dorosti and D.~Drouhin and T.~Eberl and U.~Emanuele and J-P.~Ernenwein and S.~Escoffier and F.~Fehr and V.~Flaminio and U.~Fritsch and J-L.~Fuda and S.~Galata and P.~Gay and G.~Giacomelli and J.P.~Gomez-Gonzalez and K.~Graf and G.~Guillard and G.~Halladjian and G.~Hallewell and H.~van Haren and A.J.~Heijboer and Y.~Hello and J.J.~Hernandez-Rey and B.~Herold and J.~Hößl and C.C.~Hsu and M.~de Jong and M.~Kadler and N.~Kalantar-Nayestanaki and O.~Kalekin and A.~Kappes and U.~Katz and P.~Kooijman and C.~Kopper and A.~Kouchner and V.~Kulikovskiy and R.~Lahmann and P.~Lamare and G.~Larosa and D.~Lefevre and G.~Lim and D.~Lo Presti and H.~Loehner and S.~Loucatos and F.~Lucarelli and S.~Mangano and M.~Marcelin and A.~Margiotta and J.A.~Martinez-Mora and A.~Mazure and A.~Meli and T.~Montaruli and M.~Morganti and L.~Moscoso and H.~Motz and C.~Naumann and M.~Neff and D.~Palioselitis and G.E.Pavalas and P.~Payre and J.~Petrovic and N.~Picot-Clemente and C.~Picq and V.~Popa and T.~Pradier and E.~Presani and C.~Racca and C.~Reed and G.~Riccobene and C.~Richardt and R.~Richter and A.~Rostovtsev and M.~Rujoiu and G.V.~Russo and F.~Salesa and P.~Sapienza and F.~Schöck and J-P.~Schuller and R.~Shanidze and F.~Simeone and A.~Spiess and M.~Spurio and J.J.M.~Steijger and Th.~Stolarczyk and M.~Taiuti and C.~Tamburini and L.~Tasca and S.~Toscano and B.~Vallage and V.~Van Elewyck and G.~Vannoni and M.~Vecchi and P.~Vernin and G.~Wijnker and E.~de Wolf and H.~Yepes and D.~Zaborov and J.D.~Zornoza and J.~Zuniga}, title = {{A} {F}ast {A}lgorithm for {M}uon {T}rack {R}econstruction and its {A}pplication to the {ANTARES} {N}eutrino {T}elescope}, year = {2011}, eprint = {1105.4116}, howpublished = {Astropart.Phys.34:652-662,2011}, doi = {10.1016/j.astropartphys.2011.01.003}, note = {arXiv:1105.4116v1} }
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An algorithm is presented, that provides a fast and robust reconstruction of neutrino induced upward-going muons and a discrimination of these events from downward-going atmospheric muon background in data collected by the ANTARES neutrino telescope. The algorithm consists of a hit merging and hit selection procedure followed by fitting steps for a track hypothesis and a point-like light source. It is particularly well-suited for real time applications such as online monitoring and fast triggering of optical follow-up observations for multi-messenger studies. The performance of the algorithm is evaluated with Monte Carlo simulations and various distributions are compared with that obtained in ANTARES data.
Time Calibration of the ANTARES Neutrino Telescope
ANTARES Collaboration, J.A. Aguilar, I. Al Samarai, A. Albert, M. André, M. Anghinolfi, G. Anton, S. Anvar, M. Ardid, A.C. Assis Jesus, T. Astraatmadja, J.J. Aubert, R. Auer, B. Baret, S. Basa, M. Bazzotti, V. Bertin, S. Biagi, C. Bigongiari, M. Bou-Cabo, et al (118)
Dec 13 2010 astro-ph.IM hep-ex physics.ins-det arXiv:1012.2204v1

@misc{1012.2204, author = {ANTARES Collaboration and J.A.~Aguilar and I.~Al Samarai and A.~Albert and M.~André and M.~Anghinolfi and G.~Anton and S.~Anvar and M.~Ardid and A.C.~Assis Jesus and T.~Astraatmadja and J.J.~Aubert and R.~Auer and B.~Baret and S.~Basa and M.~Bazzotti and V.~Bertin and S.~Biagi and C.~Bigongiari and M.~Bou-Cabo and M.C.~Bouwhuis and A.~M.~Brown and J.~Brunner and J.~Busto and F.~Camarena and A.~Capone and C.Carloganu and G.~Carminati and J.~Carr and S.~Cecchini and Ph.~Charvis and T.~Chiarusi and M.~Circella and H.~Costantini and N.~Cottini and P.~Coyle and C.~Curtil and M.P.~Decowski and I.~Dekeyser and A.~Deschamps and C.~Distefano and C.~Donzaud and D.~Dornic and D.~Drouhin and T.~Eberl and U.~Emanuele and J.P.~Ernenwein and S.~Escoffier and F.~Fehr and V.~Flaminio and U.~Fritsch and J.L.~Fuda and S.~Galata and P.~Gay and G.~Giacomelli and J.P.~Gómez-González and K.~Graf and G.~Guillard and G.~Halladjian and G.~Hallewell and H.~van Haren and A.J.~Heijboer and Y.~Hello and J.J.~Hernández-Rey and B.~Herold and J.~Hössl and C.C.~Hsu and M.~de Jong and M.~Kadler and N.~Kalantar-Nayestanaki and O.~Kalekin and A.~Kappes and U.~Katz and P.~Kooijman and C.~Kopper and A.~Kouchner and V.~Kulikovskiy and R.~Lahmann and P.~Lamare and G.~Larosa and D.~Lefèvre and G.~Lim and D.~Lo Presti and H.~Loehner and S.~Loucatos and F.~Lucarelli and S.~Mangano and M.~Marcelin and A.~Margiotta and J.A.~Martinez-Mora and A.~Mazure and T.~Montaruli and M.~Morganti and L.~Moscoso and H.~Motz and C.~Naumann and M.~Neff and D.~Palioselitis and G.E.Pavalas and P.~Payre and J.~Petrovic and P.~Piattelli and N.~Picot-Clemente and C.~Picq and V.~Popa and T.~Pradier and E.~Presani and C.~Racca and C.~Reed and G.~Riccobene and C.~Richardt and M.~Rujoiu and G.V.~Russo and F.~Salesa and P.~Sapienza and F.~Schöck and J.P.~Schuller and R.~Shanidze and F.~Simeone and A.~Spies and M.~Spurio and J.J.M.~Steijger and Th.~Stolarczyk and M.~Taiuti and C.~Tamburini and L.~Tasca and S.~Toscano and B.~Vallage and V.~Van Elewyck and G.~Vannoni and M.~Vecchi and P.~Vernin and G.~Wijnker and E.~de Wolf and H.~Yepes and D.~Zaborov and J.D.~Zornoza and J.~Zúñiga}, title = {{T}ime {C}alibration of the {ANTARES} {N}eutrino {T}elescope}, year = {2010}, eprint = {1012.2204}, howpublished = {Astropart.Phys.34:539-549,2011}, doi = {10.1016/j.astropartphys.2010.12.004}, note = {arXiv:1012.2204v1} }
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The ANTARES deep-sea neutrino telescope comprises a three-dimensional array of photomultipliers to detect the Cherenkov light induced by upgoing relativistic charged particles originating from neutrino interactions in the vicinity of the detector. The large scattering length of light in the deep sea facilitates an angular resolution of a few tenths of a degree for neutrino energies exceeding 10 TeV. In order to achieve this optimal performance, the time calibration procedures should ensure a relative time calibration between the photomultipliers at the level of about 1ns. The methods developed to attain this level of precision are described.