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1. Search for transient optical counterparts to high-energy IceCube neutrinos with Pan-STARRS1

Author

Kankare, E, Huber, M, Smartt, SJ, Chambers, K, Smith, KW, McBrien, O, Chen, T-W, Flewelling, H, Lowe, T, Magnier, E, Schultz, A, Waters, C, Wainscoat, RJ, Willman, M, Wright, D, Young, D, Aartsen, MG, Ackermann, M, Adams, J, Aguilar, JA, Ahlers, M, Ahrens, M, Alispach, C, Altmann, D, Andeen, K, Anderson, T, Ansseau, I, Anton, G, Argüelles, C, Auffenberg, J, Axani, S, Backes, P, Bagherpour, H, Bai, X, Barbano, A, Barwick, SW, Baum, V, Bay, R, Beatty, JJ, Becker, K-H, Tjus, JB, Benzvi, S, Berley, D, Bernardini, E, Besson, DZ, Binder, G, Bindig, D, Blaufuss, E, Blot, S, Bohm, C, Börner, M, Böser, S, Botner, O, Bourbeau, E, Bourbeau, J, Bradascio, F, Braun, J, Bretz, H-P, Bron, S, Brostean-Kaiser, J, Burgman, A, Busse, RS, Carver, T, Chen, C, Cheung, E, Chirkin, D, Clark, K, Classen, L, Collin, GH, Conrad, JM, Coppin, P, Correa, P, Cowen, DF, Cross, R, Dave, P, André, JPAMD, Clercq, CD, Delaunay, JJ, Dembinski, H, Deoskar, K, Ridder, SD, Desiati, P, Vries, KDD, Wasseige, GD, With, MD, Deyoung, T, Az-Vélez, JCD, Dujmovic, H, Dunkman, M, Dvorak, E, Eberhardt, B, Ehrhardt, T, Eller, P, Evenson, PA, Fahey, S, Fazely, AR, Felde, J, Filimonov, K, Finley, C, Franckowiak, A, Friedman, E, Fritz, A, Gaisser, TK, Gallagher, J, Ganster, E, Garrappa, S, Gerhardt, L, Ghorbani, K, Glauch, T, Glüsenkamp, T, Goldschmidt, A, Gonzalez, JG, Grant, D, Griffith, Z, Günder, M, Gündüz, M, Haack, C, Hallgren, A, Halve, L, Halzen, F, Hanson, K, Hebecker, D, Heereman, D, Helbing, K, Hellauer, R, Henningsen, F, Hickford, S, Hignight, J, Hill, GC, Hoffman, KD, Hoffmann, R, Hoinka, T, Hokanson-Fasig, B, Hoshina, K, Huang, F, Hultqvist, K, Hünnefeld, M, Hussain, R, In, S, Iovine, N, Ishihara, A, Jacobi, E, Japaridze, GS, Jeong, M, Jero, K, Jones, BJP, Kang, W, Kappes, A, Kappesser, D, Karg, T, Karl, M, Karle, A, Katz, U, Kauer, M, Keivani, A, Kelley, JL, Kheirandish, A, Kim, J, Kintscher, T, Kiryluk, J, Kittler, T, Klein, SR, Koirala, R, Kolanoski, H, Köpke, L, Kopper, C, Kopper, S, Koskinen, DJ, Kowalski, M, Krings, K, Krückl, G, Kulacz, N, Kunwar, S, Kurahashi, N, Kyriacou, A, Labare, M, Lanfranchi, JL, Larson, MJ, Lauber, F, Lazar, JP, Leonard, K, Leuermann, M, Liu, QR, Lohfink, E, Mariscal, CJL, Lu, L, Lucarelli, F, Lünemann, J, Luszczak, W, Madsen, J, Maggi, G, Mahn, KBM, Makino, Y, Mallot, K, Mancina, S, Mariş, IC, Maruyama, R, Mase, K, Maunu, R, Meagher, K, Medici, M, Medina, A, Meier, M, Meighen-Berger, S, Menne, T, Merino, G, Meures, T, Miarecki, S, Micallef, J, Momenté, G, Montaruli, T, Moore, RW, Moulai, M, Nagai, R, Nahnhauer, R, Nakarmi, P, Naumann, U, Neer, G, Niederhausen, H, Nowicki, SC, Nygren, DR, Pollmann, AO, Olivas, A, O'Murchadha, A, O'Sullivan, E, Palczewski, T, Pandya, H, Pankova, DV, Park, N, Peiffer, P, Heros, CPDL, Pieloth, D, Pinat, E, Pizzuto, A, Plum, M, Price, PB, Przybylski, GT, Raab, C, Raissi, A, Rameez, M, Rauch, L, Rawlins, K, Rea, IC, Reimann, R, Relethford, B, Renzi, G, Resconi, E, Rhode, W, Richman, M, Robertson, S, Rongen, M, Rott, C, Ruhe, T, Ryckbosch, D, Rysewyk, D, Safa, I, Herrera, SES, Sandrock, A, Sandroos, J, Santander, M, Sarkar, S, Satalecka, K, Schaufel, M, Schlunder, P, Schmidt, T, Schneider, A, Schneider, J, Schumacher, L, Sclafani, S, Seckel, D, Seunarine, S, Silva, M, Snihur, R, Soedingrekso, J, Soldin, D, Song, M, Spiczak, GM, Spiering, C, Stachurska, J, Stamatikos, M, Stanev, T, Stasik, A, Stein, R, Stettner, J, Steuer, A, Stezelberger, T, Stokstad, RG, Stößl, A, Strotjohann, NL, Stuttard, T, Sullivan, GW, Sutherland, M, Taboada, I, Tenholt, F, Ter-Antonyan, S, Terliuk, A, Tilav, S, Tomankova, L, Tönnis, C, Toscano, S, Tosi, D, Tselengidou, M, Tung, CF, Turcati, A, Turcotte, R, Turley, CF, Ty, B, Unger, E, Elorrieta, MAU, Usner, M, Vandenbroucke, J, Driessche, WV, Eijk, DV, Eijndhoven, NV, Vanheule, S, Santen, JV, Vraeghe, M, Walck, C, Wallace, A, Wallraff, M, Wandkowsky, N, Watson, TB, Weaver, C, Weiss, MJ, Weldert, J, Wendt, C, Werthebach, J, Westerhoff, S, Whelan, BJ, Whitehorn, N, Wiebe, K, Wiebusch, CH, Wille, L, Williams, DR, Wills, L, Wolf, M, Wood, J, Wood, TR, Woschnagg, K, Wrede, G, Xu, DL, Xu, XW, Xu, Y, Yanez, JP, Yodh, G, Yoshida, S, Yuan, T, Nordin, J, Physics, Faculty of Sciences and Bioengineering Sciences, Vriendenkring VUB, and Elementary Particle Physics

Subjects
DATA RELEASE, Astrophysics::High Energy Astrophysical Phenomena, media_common.quotation_subject, LIGHT-CURVE, Supernovae: general, FOS: Physical sciences, Flux, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics, 01 natural sciences, Coincidence, SUPERNOVA RATES, 0103 physical sciences, SPECTROGRAPH, Neutrinos, 010306 general physics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, media_common, GAMMA-RAY BURSTS, CALIBRATION, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astroparticle physics, IA, neutrinos, Astronomy and Astrophysics, SUPERNOVAE, Light curve, Redshift, PAN-STARRS, Supernova, Physics and Astronomy, Neutrino detector, astroparticle physics, Space and Planetary Science, Sky, Physique des particules élémentaires, DIGITAL SKY SURVEY, ddc:520, Neutrino, FOLLOW-UP, Astrophysics - High Energy Astrophysical Phenomena, general [supernovae]
Abstract

In order to identify the sources of the observed diffuse high-energy neutrino flux, it is crucial to discover their electromagnetic counterparts. To increase the sensitivity of detecting counterparts of transient or variable sources by telescopes with a limited field of view, IceCube began releasing alerts for single high-energy (Eνâ> â60 TeV) neutrino detections with sky localisation regions of order 1° radius in 2016. We used Pan-STARRS1 to follow-up five of these alerts during 2016-2017 to search for any optical transients that may be related to the neutrinos. Typically 10-20 faint (miP1âââ22.5 mag) extragalactic transients are found within the Pan-STARRS1 footprints and are generally consistent with being unrelated field supernovae (SNe) and AGN. We looked for unusual properties of the detected transients, such as temporal coincidence of explosion epoch with the IceCube timestamp, or other peculiar light curve and physical properties. We found only one transient that had properties worthy of a specific follow-up. In the Pan-STARRS1 imaging for IceCube-160427A (probability to be of astrophysical origin of ∼50%), we found a SN PS16cgx, located at 10.0′ from the nominal IceCube direction. Spectroscopic observations of PS16cgx showed that it was an H-poor SN at redshift zâ=â0.2895â ±â 0.0001. The spectra and light curve resemble some high-energy Type Ic SNe, raising the possibility of a jet driven SN with an explosion epoch temporally coincident with the neutrino detection. However, distinguishing Type Ia and Type Ic SNe at this redshift is notoriously difficult. Based on all available data we conclude that the transient is more likely to be a Type Ia with relatively weak Siâ» II absorption and a fairly normal rest-frame r-band light curve. If, as predicted, there is no high-energy neutrino emission from Type Ia SNe, then PS16cgx must be a random coincidence, and unrelated to the IceCube-160427A. We find no other plausible optical transient for any of the five IceCube events observed down to a 5σ limiting magnitude of miP1â≈â22 mag, between 1 day and 25 days after detection., SCOPUS: ar.j, info:eu-repo/semantics/published

Published
2019

2. The Pandora multi-algorithm approach to automated pattern recognition of cosmic-ray muon and neutrino events in the MicroBooNE detector.

Author

Acciarri R, Adams C, An R, Anthony J, Asaadi J, Auger M, Bagby L, Balasubramanian S, Baller B, Barnes C, Barr G, Bass M, Bay F, Bishai M, Blake A, Bolton T, Camilleri L, Caratelli D, Carls B, Castillo Fernandez R, Cavanna F, Chen H, Church E, Cianci D, Cohen E, Collin GH, Conrad JM, Convery M, Crespo-Anadón JI, Del Tutto M, Devitt A, Dytman S, Eberly B, Ereditato A, Escudero Sanchez L, Esquivel J, Fadeeva AA, Fleming BT, Foreman W, Furmanski AP, Garcia-Gamez D, Garvey GT, Genty V, Goeldi D, Gollapinni S, Graf N, Gramellini E, Greenlee H, Grosso R, Guenette R, Hackenburg A, Hamilton P, Hen O, Hewes J, Hill C, Ho J, Horton-Smith G, Hourlier A, Huang EC, James C, Jan de Vries J, Jen CM, Jiang L, Johnson RA, Joshi J, Jostlein H, Kaleko D, Karagiorgi G, Ketchum W, Kirby B, Kirby M, Kobilarcik T, Kreslo I, Laube A, Li Y, Lister A, Littlejohn BR, Lockwitz S, Lorca D, Louis WC, Luethi M, Lundberg B, Luo X, Marchionni A, Mariani C, Marshall J, Martinez Caicedo DA, Meddage V, Miceli T, Mills GB, Moon J, Mooney M, Moore CD, Mousseau J, Murrells R, Naples D, Nienaber P, Nowak J, Palamara O, Paolone V, Papavassiliou V, Pate SF, Pavlovic Z, Piasetzky E, Porzio D, Pulliam G, Qian X, Raaf JL, Rafique A, Rochester L, Rudolf von Rohr C, Russell B, Schmitz DW, Schukraft A, Seligman W, Shaevitz MH, Sinclair J, Smith A, Snider EL, Soderberg M, Söldner-Rembold S, Soleti SR, Spentzouris P, Spitz J, St John J, Strauss T, Szelc AM, Tagg N, Terao K, Thomson M, Toups M, Tsai YT, Tufanli S, Usher T, Van De Pontseele W, Van de Water RG, Viren B, Weber M, Wickremasinghe DA, Wolbers S, Wongjirad T, Woodruff K, Yang T, Yates L, Zeller GP, Zennamo J, and Zhang C

Abstract

The development and operation of liquid-argon time-projection chambers for neutrino physics has created a need for new approaches to pattern recognition in order to fully exploit the imaging capabilities offered by this technology. Whereas the human brain can excel at identifying features in the recorded events, it is a significant challenge to develop an automated, algorithmic solution. The Pandora Software Development Kit provides functionality to aid the design and implementation of pattern-recognition algorithms. It promotes the use of a multi-algorithm approach to pattern recognition, in which individual algorithms each address a specific task in a particular topology. Many tens of algorithms then carefully build up a picture of the event and, together, provide a robust automated pattern-recognition solution. This paper describes details of the chain of over one hundred Pandora algorithms and tools used to reconstruct cosmic-ray muon and neutrino events in the MicroBooNE detector. Metrics that assess the current pattern-recognition performance are presented for simulated MicroBooNE events, using a selection of final-state event topologies.

Published
2018
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3. Search for neutrinos from decaying dark matter with IceCube: IceCube Collaboration.

Author

Aartsen MG, Ackermann M, Adams J, Aguilar JA, Ahlers M, Ahrens M, Samarai IA, Altmann D, Andeen K, Anderson T, Ansseau I, Anton G, Argüelles C, Auffenberg J, Axani S, Backes P, Bagherpour H, Bai X, Barron JP, Barwick SW, Baum V, Bay R, Beatty JJ, Becker Tjus J, Becker KH, BenZvi S, Berley D, Bernardini E, Besson DZ, Binder G, Bindig D, Blaufuss E, Blot S, Bohm C, Börner M, Bos F, Böser S, Botner O, Bourbeau E, Bourbeau J, Bradascio F, Braun J, Brenzke M, Bretz HP, Bron S, Brostean-Kaiser J, Burgman A, Busse RS, Carver T, Cheung E, Chirkin D, Christov A, Clark K, Classen L, Collin GH, Conrad JM, Coppin P, Correa P, Cowen DF, Cross R, Dave P, Day M, de André JPAM, De Clercq C, DeLaunay JJ, Dembinski H, De Ridder S, Desiati P, de Vries KD, de Wasseige G, de With M, DeYoung T, Díaz-Vélez JC, di Lorenzo V, Dujmovic H, Dumm JP, Dunkman M, Dvorak E, Eberhardt B, Ehrhardt T, Eichmann B, Eller P, Evenson PA, Fahey S, Fazely AR, Felde J, Filimonov K, Finley C, Flis S, Franckowiak A, Friedman E, Fritz A, Gaisser TK, Gallagher J, Ganster E, Gerhardt L, Ghorbani K, Giang W, Glauch T, Glüsenkamp T, Goldschmidt A, Gonzalez JG, Grant D, Griffith Z, Haack C, Hallgren A, Halve L, Halzen F, Hanson K, Hebecker D, Heereman D, Helbing K, Hellauer R, Hickford S, Hignight J, Hill GC, Hoffman KD, Hoffmann R, Hoinka T, Hokanson-Fasig B, Hoshina K, Huang F, Huber M, Hultqvist K, Hünnefeld M, Hussain R, In S, Iovine N, Ishihara A, Jacobi E, Japaridze GS, Jeong M, Jero K, Jones BJP, Kalaczynski P, Kang W, Kappes A, Kappesser D, Karg T, Karle A, Katz U, Kauer M, Keivani A, Kelley JL, Kheirandish A, Kim J, Kim M, Kintscher T, Kiryluk J, Kittler T, Klein SR, Koirala R, Kolanoski H, Köpke L, Kopper C, Kopper S, Koschinsky JP, Koskinen DJ, Kowalski M, Krings K, Kroll M, Krückl G, Kunwar S, Kurahashi N, Kuwabara T, Kyriacou A, Labare M, Lanfranchi JL, Larson MJ, Lauber F, Leonard K, Lesiak-Bzdak M, Leuermann M, Liu QR, Lohfink E, Mariscal CJL, Lu L, Lünemann J, Luszczak W, Madsen J, Maggi G, Mahn KBM, Mancina S, Maruyama R, Mase K, Maunu R, Meagher K, Medici M, Meier M, Menne T, Merino G, Meures T, Miarecki S, Micallef J, Momenté G, Montaruli T, Moore RW, Moulai M, Nahnhauer R, Nakarmi P, Naumann U, Neer G, Niederhausen H, Nowicki SC, Nygren DR, Obertacke Pollmann A, Olivas A, O'Murchadha A, O'Sullivan E, Palczewski T, Pandya H, Pankova DV, Peiffer P, Pepper JA, Pérez de Los Heros C, Pieloth D, Pinat E, Plum M, Price PB, Przybylski GT, Raab C, Rädel L, Rameez M, Rauch L, Rawlins K, Rea IC, Reimann R, Relethford B, Relich M, Resconi E, Rhode W, Richman M, Robertson S, Rongen M, Rott C, Ruhe T, Ryckbosch D, Rysewyk D, Safa I, Sanchez Herrera SE, Sandrock A, Sandroos J, Santander M, Sarkar S, Sarkar S, Satalecka K, Schaufel M, Schlunder P, Schmidt T, Schneider A, Schoenen S, Schöneberg S, Schumacher L, Sclafani S, Seckel D, Seunarine S, Soedingrekso J, Soldin D, Song M, Spiczak GM, Spiering C, Stachurska J, Stamatikos M, Stanev T, Stasik A, Stein R, Stettner J, Steuer A, Stezelberger T, Stokstad RG, Stößl A, Strotjohann NL, Stuttard T, Sullivan GW, Sutherland M, Taboada I, Tatar J, Tenholt F, Ter-Antonyan S, Terliuk A, Tilav S, Toale PA, Tobin MN, Tönnis C, Toscano S, Tosi D, Tselengidou M, Tung CF, Turcati A, Turley CF, Ty B, Unger E, Usner M, Vandenbroucke J, Van Driessche W, van Eijk D, van Eijndhoven N, Vanheule S, van Santen J, Vraeghe M, Walck C, Wallace A, Wallraff M, Wandler FD, Wandkowsky N, Waza A, Weaver C, Weiss MJ, Wendt C, Werthebach J, Westerhoff S, Whelan BJ, Wiebe K, Wiebusch CH, Wille L, Williams DR, Wills L, Wolf M, Wood J, Wood TR, Woolsey E, Woschnagg K, Wrede G, Xu DL, Xu XW, Xu Y, Yanez JP, Yodh G, Yoshida S, and Yuan T

Abstract

With the observation of high-energy astrophysical neutrinos by the IceCube Neutrino Observatory, interest has risen in models of PeV-mass decaying dark matter particles to explain the observed flux. We present two dedicated experimental analyses to test this hypothesis. One analysis uses 6 years of IceCube data focusing on muon neutrino 'track' events from the Northern Hemisphere, while the second analysis uses 2 years of 'cascade' events from the full sky. Known background components and the hypothetical flux from unstable dark matter are fitted to the experimental data. Since no significant excess is observed in either analysis, lower limits on the lifetime of dark matter particles are derived: we obtain the strongest constraint to date, excluding lifetimes shorter than 10 28 s at 90% CL for dark matter masses above 10 TeV .

Published
2018
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4. Measurement of the ν μ energy spectrum with IceCube-79: IceCube Collaboration.

Author

Aartsen MG, Ackermann M, Adams J, Aguilar JA, Ahlers M, Ahrens M, Al Samarai I, Altmann D, Andeen K, Anderson T, Ansseau I, Anton G, Archinger M, Argüelles C, Auffenberg J, Axani S, Bagherpour H, Bai X, Barwick SW, Baum V, Bay R, Beatty JJ, Becker Tjus J, Becker KH, BenZvi S, Berley D, Bernardini E, Besson DZ, Binder G, Bindig D, Blaufuss E, Blot S, Bohm C, Börner M, Bos F, Bose D, Böser S, Botner O, Bradascio F, Braun J, Brayeur L, Bretz HP, Bron S, Burgman A, Carver T, Casier M, Cheung E, Chirkin D, Christov A, Clark K, Classen L, Coenders S, Collin GH, Conrad JM, Cowen DF, Cross R, Day M, de André JPAM, De Clercq C, Del Pino Rosendo E, Dembinski H, De Ridder S, Desiati P, de Vries KD, de Wasseige G, de With M, DeYoung T, Díaz-Vélez JC, di Lorenzo V, Dujmovic H, Dumm JP, Dunkman M, Eberhardt B, Ehrhardt T, Eichmann B, Eller P, Euler S, Evenson PA, Fahey S, Fazely AR, Feintzeig J, Felde J, Filimonov K, Finley C, Flis S, Fösig CC, Franckowiak A, Friedman E, Fuchs T, Gaisser TK, Gallagher J, Gerhardt L, Ghorbani K, Giang W, Gladstone L, Glauch T, Glüsenkamp T, Goldschmidt A, Gonzalez JG, Grant D, Griffith Z, Haack C, Hallgren A, Halzen F, Hansen E, Hansmann T, Hanson K, Hebecker D, Heereman D, Helbing K, Hellauer R, Hickford S, Hignight J, Hill GC, Hoffman KD, Hoffmann R, Hoshina K, Huang F, Huber M, Hultqvist K, In S, Ishihara A, Jacobi E, Japaridze GS, Jeong M, Jero K, Jones BJP, Kang W, Kappes A, Karg T, Karle A, Katz U, Kauer M, Keivani A, Kelley JL, Kheirandish A, Kim J, Kim M, Kintscher T, Kiryluk J, Kittler T, Klein SR, Kohnen G, Koirala R, Kolanoski H, Konietz R, Köpke L, Kopper C, Kopper S, Koskinen DJ, Kowalski M, Krings K, Kroll M, Krückl G, Krüger C, Kunnen J, Kunwar S, Kurahashi N, Kuwabara T, Kyriacou A, Labare M, Lanfranchi JL, Larson MJ, Lauber F, Lennarz D, Lesiak-Bzdak M, Leuermann M, Lu L, Lünemann J, Madsen J, Maggi G, Mahn KBM, Mancina S, Maruyama R, Mase K, Maunu R, McNally F, Meagher K, Medici M, Meier M, Menne T, Merino G, Meures T, Miarecki S, Micallef J, Momenté G, Montaruli T, Moulai M, Nahnhauer R, Naumann U, Neer G, Niederhausen H, Nowicki SC, Nygren DR, Obertacke Pollmann A, Olivas A, O'Murchadha A, Palczewski T, Pandya H, Pankova DV, Peiffer P, Penek Ö, Pepper JA, Pérez de Los Heros C, Pieloth D, Pinat E, Price PB, Przybylski GT, Quinnan M, Raab C, Rädel L, Rameez M, Rawlins K, Reimann R, Relethford B, Relich M, Resconi E, Rhode W, Richman M, Riedel B, Robertson S, Rongen M, Rott C, Ruhe T, Ryckbosch D, Rysewyk D, Sabbatini L, Sanchez Herrera SE, Sandrock A, Sandroos J, Sarkar S, Satalecka K, Schlunder P, Schmidt T, Schoenen S, Schöneberg S, Schumacher L, Seckel D, Seunarine S, Soldin D, Song M, Spiczak GM, Spiering C, Stachurska J, Stanev T, Stasik A, Stettner J, Steuer A, Stezelberger T, Stokstad RG, Stößl A, Ström R, Strotjohann NL, Sullivan GW, Sutherland M, Taavola H, Taboada I, Tatar J, Tenholt F, Ter-Antonyan S, Terliuk A, Tešić G, Tilav S, Toale PA, Tobin MN, Toscano S, Tosi D, Tselengidou M, Tung CF, Turcati A, Unger E, Usner M, Vandenbroucke J, van Eijndhoven N, Vanheule S, van Rossem M, van Santen J, Vehring M, Voge M, Vogel E, Vraeghe M, Walck C, Wallace A, Wallraff M, Wandkowsky N, Waza A, Weaver C, Weiss MJ, Wendt C, Westerhoff S, Whelan BJ, Wickmann S, Wiebe K, Wiebusch CH, Wille L, Williams DR, Wills L, Wolf M, Wood TR, Woolsey E, Woschnagg K, Xu DL, Xu XW, Xu Y, Yanez JP, Yodh G, Yoshida S, and Zoll M

Abstract

IceCube is a neutrino observatory deployed in the glacial ice at the geographic South Pole. The ν μ energy unfolding described in this paper is based on data taken with IceCube in its 79-string configuration. A sample of muon neutrino charged-current interactions with a purity of 99.5% was selected by means of a multivariate classification process based on machine learning. The subsequent unfolding was performed using the software Truee. The resulting spectrum covers an E ν -range of more than four orders of magnitude from 125 GeV to 3.2 PeV. Compared to the Honda atmospheric neutrino flux model, the energy spectrum shows an excess of more than 1.9 σ in four adjacent bins for neutrino energies E ν ≥ 177.8 TeV . The obtained spectrum is fully compatible with previous measurements of the atmospheric neutrino flux and recent IceCube measurements of a flux of high-energy astrophysical neutrinos., (© The Author(s) 2017.)

Published
2017
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