Observation of the Suppression of the Flux of Cosmic Rays above<mml:math xmlns:mml="http://www.w3.org/1998/Math/MathML" display="inline"><mml:mn>4</mml:mn><mml:mo>×</mml:mo><mml:msup><mml:mn>10</mml:mn><mml:mn>19</mml:mn></mml:msup><mml:mtext> </mml:mtext><mml:mtext> </mml:mtext><mml:mi>eV</mml:mi></mml:math>

Abraham, J.; Abreu, P.; Aglietta, M.; Aguirre, C.; Allard, Denis; Allekotte, I.; Allen, J.; Allison, P.; Álvarez-Muñiz, J.; Ambrosio, M.; Anchordoqui, Luis A.; Andringa, S.; Anzalone, A.; Aramo, C.; Argirò, S.; Arisaka, K.; Armengaud, E.; Arneodo, F.; Arqueros, F.; Asch, T.; Asorey, H.; Assis, P.; Atulugama, B. S.; Aublin, J.; Ave, M.; Ávila, G.; Bäcker, T.; Badagnani, D.; Barbosa, A. F.; Barnhill, D.; Barroso, S. L. C.; Baughman, B. M.; Bauleo, P.; Beatty, J. J.; Beau, T.; Becker, B. R.; Becker, Karl‐Heinz; Bellido, J. A.; BenZvi, S.; Bérat, C.; Bergmann, T.; Bernardini, P.; Bertou, X.; Biermann, P. L.; Billoir, P.; Blanch-Bigas, O.; Blanco, F.; Blasi, Pasquale; Bleve, C.; Blümer, H.; Bohã̌cov́a, M.; Bonifazi, C.; Bonino, R.; Brack, J.; Brogueira, P.; Brown, W. C.; Buchholz, P.; Bueno, A.; Burton, R. E.; Busca, N. G.; Caballero-Mora, K. S.; Cai, B.; Camin, D.V.; Caramete, L.; Caruso, R.; Carvalho, W. 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C.; Fazzini, N.; Ferrer, Francesc; Ferrero, A.; Fick, B.; Filevich, A.; Filipčić, A.; Fleck, I.; Fracchiolla, C. E.; Fulgione, W.; García, Beatriz; Gámez, D. García; Garcia-Pinto, D.; Garrido, X.; Geenen, H.; Gelmini, Graciela B.; Gemmeke, H.; Ghia, P. L.; Giller, M.; Glass, H.; Gold, M.; Golup, G.; Albarracin, F. Gómez; Berisso, M. Gómez; Gonçalves, P.; Amaral, Marcelo; Gonzalez, D.; González, J. G.; González, M. M.; Góra, D.; Gorgi, A.; Gouffon, P.; Grassi, V.; Grillo, A. F.; Grunfeld, C.; Guardincerri, Y.; Guarino, F.; Guedes, G. P.; Gutiérrez, J.; Hague, J. D.; Halenka, V.; Hamilton, J. C.; Hansen, P.; Harari, D.; Harmsma, S.; Harton, J. L.; Haungs, A.; Hauschildt, T.; Healy, M. D.; Hebbeker, T.; Hebrero, G.; Heck, D.; Hojvat, C.; Holmes, V. C.; Homola, P.; Hörandel, J. R.; Horneffer, A.; Hrabovský, M.; Huege, T.; Hussain, M.; Iarlori, M.; Insolia, A.; Ionita, F.; Italiano, A.; Kaducak, M.; Kampert, K.‐H.; Karova, T.; Kasper, P. A.; Kégl, Balázs; Keilhauer, B.; Kemp, E.; Kieckhafer, R. M.; Klages, H. O.; Kleifges, M.; Kleinfeller, J.; Knapik, R.; Knapp, J.; Koang, D. H.; Krieger, A. S.; Krömer, O.; Kuempel, D.; Kunka, N.; Kusenko, Alexander; Rosa, G. La; Lachaud, C.; Lago, Bruno L.; Lebrun, D.; Lebrun, P.; Lee, J.; Oliveira, M. A. Leigui de; Letessier‐Selvon, A.; Leuthold, M.; Lhenry-Yvon, I.; López, R.; Agúera, A. López; Bahilo, J. J. Lozano; Lucero, A.; García, R. Luna; Maccarone, M. C.; Macolino, C.; Maldera, S.; Mancarella, G.; Manceñido, Mónica E.; Mandat, D.; Mantsch, P.; Mariazzi, A. G.; Maris, Ioana Codrina; Falcon, H. R. Marquez; Martello, D.; Martínez, J.; Bravo, O. Martínez; Mathes, H. J.; Matthews, J. N.; Matthews, John; Matthiae, G.; Maurizio, D.; Mazur, Péter; McCauley, T.; McEwen, M.; McNeil, R. R.; Medina, M. C.; Medina‐Tanco, G.; Melo, D.; Menichetti, E.; Menschikov, A.; Meurer, C.; Meyhandan, R.; Micheletti, M. I.; Miele, Gennaro; Miller, William H.; Mollerach, Silvia; Monasor, M.; Ragaigne, D. Monnier; Montanet, F.; Morales, B.; Morello, C.; Moreno, J. C.; Morris, C.; Mostafá, M.; Müller, M. A.; Mussa, R.; Navarra, G.; Navarro, J. L. La Rosa; Navas, S.; Nečesal, P.; Nellen, L.; Newman-Holmes, C.; Newton, D.; Nhung, P. T.; Nierstenhoefer, N.; Nitz, D.; Nosek, D.; Nožka, L.; Oehlschläger, J.; Ohnuki, T.; Olinto, Angela V.; Olmos-Gilbaja, V. M.; Ortiz, María J.; Ortolani, Fabrizio; Ostapchenko, S.; Otero, Lidia Ana; Pacheco, N.; Selmi-Dei, D. Pakk; Palatka, M.; Pallotta, J.; Parente, G.; Parizot, E.; Parlati, S.; Pastor, S.; Patel, M.; Paul, T.; Pavlidou, V.; Payet, K.; Pech, M.; Pękala, Jan; Pelayo, R.; Pepe, I. M.; Perrone, L.; Pesce, R.; Petrera, S.; Petrinca, P.; Petrov, Y.; Pichel, A.; Piegaia, R.; Pierog, T.; Pimenta, M.; Pinto, T.; Pirronello, V.; Pisanti, O.; Platino, M.; Pochon, J.; Privitera, P.; Prouza, M.; Quel, E. 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doi:10.1103/physrevlett.101.061101

Cited by 564 publications

(183 citation statements)

References 17 publications

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“…The efforts to improve sensitivity to the UHE neutrino flux may test the existence of the Berezinsky-Zatsepin (BZ) neutrinos [2]. Those neutrinos are generated through the same process that predicts the Greisen-Zatsepin-Kuzmin (GZK) cutoff [3] of Cosmic Ray (CR) flux, which has been observed by HiRes [4] and the Auger Observatory [5]. The most energetic CRs, most probably composed by protons and nuclei, may have an origin at relatively close sources, of the order of 100 Mpc for protons and even less for nuclei [6].…”

Section: Introductionmentioning

confidence: 99%

Confusing the extragalactic neutrino flux limit with a neutrino propagation limit

Barranco

Miranda

Moura

et al. 2011

J. Cosmol. Astropart. Phys.

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ABSTRACT:We study the possible suppression of the extragalactic neutrino flux due to a nonstandard interaction during its propagation. In particular, we study neutrino interaction with an ultra-light scalar field dark matter. It is shown that the extragalactic neutrino flux may be suppressed by such an interaction, leading to a new mechanism to reduce the ultra-high energy neutrino flux. We study both the cases of non-self-conjugate as well as self-conjugate dark matter. In the first case, the suppression is independent of the neutrino and dark matter masses. We conclude that care must be taken when explaining limits on the neutrino flux through source acceleration mechanisms only, since there could be other mechanisms for the reduction of the neutrino flux.

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Section: Introductionmentioning

confidence: 99%

Confusing the extragalactic neutrino flux limit with a neutrino propagation limit

Barranco

Miranda

Moura

et al. 2011

J. Cosmol. Astropart. Phys.

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“…The sources of ultra-high energy cosmic rays (UHECR) still remain in veil, but the recent observation of the suppression in the energy spectrum of UHECR above the so-called Greisen-Zatsepin-Kuzmin (GZK) cutoff (E GZK ∼ 4 × 10 19 GeV) [1,2] indicates that at least the UHECR with energies above the GZK cutoff come from relatively close (within the GZK radius ∼ 100 Mpc) extragalactic sources. The magnitude and extension of the intergalactic magnetic fields are supposed not to be large enough to significantly alter the arrival directions of UHECR with these energies.…”

Section: Introductionmentioning

confidence: 99%

Statistical analysis of the correlation between active galactic nuclei and ultra-high energy cosmic rays

Kim

2011

J. Cosmol. Astropart. Phys.

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We develop the statistical methods for comparing two sets of arrival directions of cosmic rays in which the two-dimensional distribution of arrival directions is reduced to the one-dimensional distributions so that the standard one-dimensional Kolmogorov-Smirnov test can be applied. Then we apply them to the analysis of correlation between the ultra-high energy cosmic rays (UHECR) with energies above 5.7 × 10 19 eV, observed by Pierre Auger Observatory (PAO) and Akeno Giant Air Shower Array (AGASA), and the active galactic nuclei (AGN) within the distance 100 Mpc. For statistical test, we set up the simple AGN model for UHECR sources in which a certain fraction of observed UHECR are originated from AGN within a chosen distance, assuming that all AGN have equal UHECR luminosity and smearing angle, and the remaining fraction are from the isotropic background contribution. For the PAO data, our methods exclude not only a hypothesis that the observed UHECR are simply isotropically distributed but also a hypothesis that they are completely originated from the selected AGN. But, the addition of appropriate amount of isotropic component either through the background contribution or through the large smearing effect improves the correlation greatly and makes the AGN hypothesis for UHECR sources a viable one. We also point out that restricting AGN within the distance bin of 40 − 60 Mpc happens to yield a good correlation without appreciable isotropic component and large smearing effect. For the AGASA data, we don't find any significant correlation with AGN.

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“…Since the magnitude of the interstellar magnetic fields are insufficient to confine these particles to within the galaxy, the sources of highest energy particles are expected to be of extra-galactic in nature. The recent results from the PAO indicate that the hypothesis of a single power law beyond the ankle in the cosmic ray spectrum is not valid and their data are consistent with the existence of the so called Greisen-ZatsepinKuzmin (GZK) cutoff [18,19] beyond the energy of 4 x 10 19 eV [20]. An important corollary of this result is the large reduction in the flux of the highest energy cosmic rays.…”

Section: Diffuse γ γ γ γ γ-Ray Flux ~ 100 Tevmentioning

confidence: 64%

High Energy Astroparticle Physics at Ooty and the GRAPES-3 Experiment

Gupta¹

2014

Proceedings of the Indian National Science Academy

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The astroparticle studies at Ooty have their roots going way back into the fifties, when studies using cosmic rays were initiated with cloud chambers of progressively larger sizes as the primary detector and measuring device to obtain properties of hadrons at high energies. This study was subsequently strengthened with the installation of a total absorption calorimeter and a modest extensive air shower array to probe the composition of the primary cosmic rays to very high energies. The discovery of pulsars provided a thrust for the exploration of these compact objects as the sources of γ-rays at TeV energies with the aid of atmospheric Cerenkov detectors in the seventies. With the rapid technological advances occurring during the subsequent years in detectors, electronics and computers, physicists world-wide were able to set up very large and remarkably sensitive experiments that were hard to imagine a decade earlier. With the increasing sophistication and complexity the modern experiments require participation of very large teams of scientists. This development has made the formation of collaboration of large number of physicists both experimental and theoretical, engineers, technicians etc., from a number of institutions and universities, a prerequisite for setting up any major experimental facility. The GRAPES-3 experiment is a collaboration of 34 scientists from 13 institutions, including 8 from India and 5 from Japan. The GRAPES-3 experiment contains a dense extensive air shower array operating with ~ 400 scintillator detectors and a 560 m 2 tracking muon detector (Em > 1 GeV), at Ooty in India. 25 % of scintillator detectors are instrumented with two fast photomultiplier tubes (PMTs) for extending the dynamic range to ~ 5x10 3 particles m -2. The scintillators, signal processing electronics and data recording systems were fabricated in-house to cut costs and optimize performance. The muon multiplicity distribution of the EAS is used to probe the composition of primary cosmic rays below the 'knee', with an overlap with direct measurements. Search for multi-TeV γ-rays from point sources is done with the aid of the muon detector. A good angular resolution of 0.7 o at 30 TeV, is measured from shadow of the Moon on the isotropic flux of cosmic rays. Sensitive limit on the diffuse flux of 100 TeV γ-rays is placed by using muon detector to filter out the charged cosmic ray background. The tracking muon detector allows sensitive measurements on the coronal mass ejections and solar flares through Forbush decrease events. We have major expansion plans to enhance the sensitivity of the GRAPES-3 experiment in the areas listed above. PACS

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Observation of the Suppression of the Flux of Cosmic Rays above4×1019 eV

Cited by 564 publications

References 17 publications

Confusing the extragalactic neutrino flux limit with a neutrino propagation limit

Confusing the extragalactic neutrino flux limit with a neutrino propagation limit

Statistical analysis of the correlation between active galactic nuclei and ultra-high energy cosmic rays

High Energy Astroparticle Physics at Ooty and the GRAPES-3 Experiment

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