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This article reports the first observation of the Moon and the Sun shadows in the sky distribution of cosmicray induced muons measured by the KM3NeT/ORCA detector. The analysed data-taking period spans from February 2020 to November 2021, when the detector had 6 Detection Units deployed at the bottom of the Mediterranean Sea, each composed of 18 Digital Optical Modules. The shadows induced by the Moon and the Sun were detected at their nominal position with a statistical significance of 4.2s and 6.2s, and an angular resolution of sres = 0.49¿ and sres = 0.66¿, respectively, consistent with the prediction of 0.53¿ from simulations. This early result confirms the effectiveness of the detector calibration, in time, position and orientation and the accuracy of the event direction reconstruction. This also demonstrates the performance and the competitiveness of the detector in terms of pointing accuracy and angular resolution, Article signat per 254 autors i autores: S. Aiello, A. Albert, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, M. Anghinolfi, M. Anguita, M. Ardid, S. Ardid, J. Aublin, C. Bagatelas, L. Bailly-Salins, B. Baret, S. Basegmez du Pree, Y. Becherini, M. Bendahman, F. Benfenati, E. Berbee, V. Bertin, S. Biagi, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, M. Bouwhuis, C. Bozza, H.Brânzaş, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, D. Calvo, S. Campion, A. Capone, F. Carenini, V. Carretero, P. Castaldi, S. Celli, L. Cerisy, M. Chabab, N. Chau, A. Chen, R. Cherkaoui El Moursli, S. Cherubini, V. Chiarella, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, R. Coniglione, P. Coyle, A. Creusot, A. Cruz, G. Cuttone, R. Dallier, Y. Darras, A. De Benedittis, B. De Martino, V. Decoene, R. Del Burgo, I. Di Palma, A. F. Díaz, D. Diego-Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, E. Drakopoulou, D. Drouhin, T. Eberl, A. Eddyamoui, T. van Eeden, M. Eff, D. van Eijk, I. El Bojaddaini, S. El Hedri, A. Enzenhöfer, V. Espinosa, G. Ferrara, M. D. Filipović, F. Filippini, L. A. Fusco, J. Gabriel, T. Gal, J. García Méndez, A. Garcia Soto, F. Garufi, C. Gatius Oliver, N. Geißelbrecht, L. Gialanella, E. Giorgio, A. Girardi , I. Goos, S. R. Gozzini, R. Gracia, K. Graf, D. Guderian, C. Guidi, B. Guillon, M. Gutiérrez, L. Haegel, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, J. J. Hernández-Rey, F. Huang, W. Idrissi Ibnsalih, G. Illuminati, C. W. James, D. Janezashvili, M. de Jong, P. de Jong, B. J. Jung, P. Kalaczyński, O. Kalekin, U. F. Katz, N. R. Khan Chowdhury, G. Kistauri, F. van der Knaap, P. Kooijman, A. Kouchner, V. Kulikovskiy, M. Labalme, R. Lahmann, A. Lakhal, M. Lamoureux, G. Larosa, C. Lastoria, A. Lazo, R. Le Breton, S. Le Stum, G. Lehaut, E. Leonora, N. Lessing, G. Levi, S. Liang, M. Lindsey Clark, F. Longhitano, L. Maderer, J. Majumdar, J. Mańczak, A. Margiotta, A. Marinelli, C. Markou, L. Marti, Postprint (published version)

A causality preserving interpretation of the electromagnetic (EM) leaky-wave (LW) propagation in space and time is proposed for the first time. The Cagniard-deHoop (CdH) joint transform technique is applied for elucidating the relation between time-domain (TD) head waves (HWs), body waves (BWs), Cherenkov wave effects, and LWs. It is conjectured that the LW phenomenon in the TD is associated with a local maximum in the observed signal that occurs between the arrivals of the HW and BW constituents. A quantitative analysis that enables the space-time localization of the LW effect is performed theoretically and, then, illustrated via representative examples including the pulsed EM radiation from both a line source above a dielectric half-space, and narrow-slot antennas., Green Open Access added to TU Delft Institutional Repository ‘You share, we take care!’ – Taverne project https://www.openaccess.nl/en/you-share-we-take-care Otherwise as indicated in the copyright section: the publisher is the copyright holder of this work and the author uses the Dutch legislation to make this work public., Electrical Engineering Education

Unter dem geografischen Südpol liegt das IceCube Neutrino Observatorium. Es nutzt einen Kubikkilometer Gletschereis, um Sekundärteilchen aus Neutrinointerkationen zu detektieren. Der Detektor besteht aus insgesamt 5160 optischen Sensoren, die das Cherenkov Licht der relativistischen, geladenen Teilchen messen. Um die Sensitivität und das Detektionsvermögen zu erhöhen sind Vergrößerungen des Detektors mit neuentwickelten optischen Sensoren geplant. Mindestens einer dieser neuen Sensoren soll den Messbereich aus dem optischen Bereich in den UV Bereich erweitern, wobei eine neu entwickelte wellenlängenschiebende Technologie verwendet wird. Um die Verbesserungen dieser neuen Module zu verstehen, wurde ein Kalibrierungsgerät gebaut, getestet und zweimal bei einer in-situ Messung am geografischen Südpol verwendet. Die Messung wurde in dem offenen SPICEcore borehole durchgeführt. In dem Kalibrierungsgerät waren sowohl Lichtquelle, als auch Detektor verbaut. Um die Eiseigenschaften zu vermessen, wurde Licht in möglichst kurzen Pulsen in das Eis gestrahlt. Der Detektor hat nun die Zeitverteilung gemessen, mit der die Photonen wieder zu dem Detektor zurückgestreut werden. Zur Detektion nutzt das Kalibrierungsgerät die gleiche wellenlängenschiebende Technologie, wie die neuentwickelten optischen Module. Die Messung wurde für Wellenlängen zwischen 245 nm und 400 nm an mehreren Tiefen in einem Bereich, in dem auch IceCube liegt durchgeführt. Diese in-situ Messungen sind der erste erfolgreiche Einsatz der neuen wellenlängenschiebenden Technologie. Mit einem likelihood fit wurde die Messung mit einer Simulation verglichen, welche die Absorption und Streuung der Photonen im Eis als Parameter variiert. Mit dieser Analyse konnte für jede Wellenlänge und Tiefe am besten passende Parameter mit Unsicherheiten, bestehend aus statistischen und systematischen Fehlern gefunden werden. Der größte Einfluss auf die Unsicherheiten ist die schlechte Zeitauflösung des Detektors. Die Ergebnisse le, The IceCube Neutrino Observatory lies under the South Pole. It instruments one cubic kilometer of glacial ice to detect secondary particles originating from neutrino interactions. The detector consists of 5160 optical sensors, which measure the Cherenkov light of these relativistic, charged particles. In order to increase the sensitivity and detection range, new extensions with newly developed optical sensors are planned. At least one of these new sensors is supposed to expand the detection range from the optical into the UV range, using a new wavelength shifting technology. To understand the improvements of these new modules, the UV calibration device was built, tested, and deployed twice in in-situ measurements at the geographic South Pole. The measurement was carried out in the open SPICEcore borehole. A light source and a detector were included in the design of the UV calibration device. To measure the ice properties, the light was pulsed in the ice as short as possible. The detector measured the timing distribution of the light getting scattered back. For the detection, the wavelength shifting technology developed for the new optical sensors is used. The measurement was carried out with four wavelengths between 245 nm and 400 nm at several depths, some within the IceCube range. These in-situ measurements successfully applied the new wavelength shifting technology for the first time. Using a likelihood fit, the measurements were compared to a simulation, which varied the absorption and scattering coefficients of the photons in the ice as parameters. With this analysis, a best-fitting set of parameters could be found for each wavelength and depth. The uncertainties are very conservative, consisting of statistical and systematic errors. The most significant influence on the uncertainties is caused by the insufficient time resolution of the detection system. The results suggest a high transparency for the deep UV range and provide a deeper insight into the scatteri

KM3NeT/ORCA is a water-Cherenkov neutrino detector, currently under construction in the Mediterranean Sea at a depth of 2450 meters. The project’s main goal is the determination of the neutrino mass hierarchy by measuring the energy- and zenith-angle-resolved oscillation probabilities of atmospheric neutrinos traversing the Earth. Additionally, the detector observes a large amount of atmospheric muons, which can be used to study extensive air showers generated by cosmic ray particles. This work describes a deep-learning based reconstruction of atmospheric muons using graph convolutional networks. They are used to reconstruct the zenith angle, the muon multiplicity and the diameter of atmospheric muon bundles. Simulations and measured data from an early four line stage of the detector are used to evaluate the performance. Furthermore, the reconstructions are compared to the ones of classical approaches, and use cases for the indirect study of cosmic ray particles are shown., Article signat per 297 autors/es: M.Ageron, S. Aiello, A. Albert, M. Alshamsi, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, G. Anton, M. Ardid, S. Ardid, W. Assal, J. Aublin, C. Bagatelas, B. Baret, S. Basegmez du Pree, M. Bendahman, F. Benfenati, E. Berbee, A. M. van den Berg, V. Bertin, S. Beurthey, V. van Beveren, S. Biagi, M. Billault, M. Bissinger, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, C. Boutonnet, G. Bouvet, M. Bouwhuis, C. Bozza, H.Brânzas, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, L. Caillat, D. Calvo, S. Campion, A. Capone, H. Carduner, V. Carretero, P. Castaldi, S. Celli;, R. Cereseto, M. Chabab, C. Champion, N. Chau, A. Chen, S. Cherubini, V. Chiarella, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, M. Colomer Molla, S. Colonges, R. Coniglione, A. Cosquer, P. Coyle, M. Cresta, A. Creuso, A. Cruz, G. Cuttone, A. D’Amico, R. Dallier, B. De Martino, M. De Palma, I. Di Palma, A. F. Díaz, D. Diego- Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, D. Drouhin, T. Eberl, A. Eddyamoui, T. van Eeden, D. van Eijk, I. El Bojaddaini, H. Eljarrari, D. Elsaesser, A. Enzenhöfer, V. Espinosa, P. Fermani, G. Ferrara, M. D. Filipovic, F. Filippini, J. Fransen, L. A. Fusco, D. Gajanana, T. Gal, J. García Méndez, A. Garcia Soto, E. Garçon, F. Garufi, C. Gatius, N. Geißelbrecht, L. Gialanella, E. Giorgio, S. R. Gozzini, R. Gracia, K. Graf, G. Grella, D. Guderian, C. Guidi, B. Guillon, M. Gutiérrez, J. Haefner, S. Hallmann, H. Hamdaoui, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, S. Henry, J. J. Hernández-Rey, J. Hofestädt, F. Huang,W. Idrissi Ibnsalih, A. Ilioni, G. Illuminati, C.W. James, D. Janezashvili, P. Jansweijer, M. de Jong, P. de Jong, B. J. Jung, M. Kadler, P. Kalaczynski, O. Kalekin,U. F. Katz, F. Kayzel, P.Keller, N. R. Khan Chowdhury, G. Kistauri, F. van der Knaap, P. Kooijman, A. Kouchner, M. Kreter, V. Kulikovskiy, M. La, Postprint (published version)

The discovery of a high-energy cosmic neutrino flux has paved the way for the field of neutrino astronomy. For a large part of the flux, the sources remain unidentified. The KM3NeT detector, which is under construction in the Mediterranean sea, is designed to determine their origin. KM3NeT will instrument a cubic kilometre of seawater with photomultiplier tubes that detect Cherenkov radiation from neutrino interaction products with nanosecond precision. For single cascade event signatures, KM3NeT already showed that it can reach degree-level resolutions, greatly increasing the use of these neutrinos for astronomy. In this contribution, we further refine the cascade reconstruction by making a more detailed model of the neutrinos events and including additional information on the hit times. The arrival time of light can be used to improve the identification of double cascade signatures from tau neutrinos, and the angular resolution of both single and double cascade signatures. Sub-degree resolution is achieved in both cases. © Copyright owned by the author(s)., Article signat per 297 autors/es: M.Ageron, S. Aiello, A. Albert, M. Alshamsi, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, G. Anton, M. Ardid, S. Ardid, W. Assal, J. Aublin, C. Bagatelas, B. Baret, S. Basegmez du Pree, M. Bendahman, F. Benfenati, E. Berbee, A. M. van den Berg, V. Bertin, S. Beurthey, V. van Beveren, S. Biagi, M. Billault, M. Bissinger, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, C. Boutonnet, G. Bouvet, M. Bouwhuis, C. Bozza, H.Brânzas, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, L. Caillat, D. Calvo, S. Campion, A. Capone, H. Carduner, V. Carretero, P. Castaldi, S. Celli;, R. Cereseto, M. Chabab, C. Champion, N. Chau, A. Chen, S. Cherubini, V. Chiarella, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, M. Colomer Molla, S. Colonges, R. Coniglione, A. Cosquer, P. Coyle, M. Cresta, A. Creuso, A. Cruz, G. Cuttone, A. D’Amico, R. Dallier, B. De Martino, M. De Palma, I. Di Palma, A. F. Díaz, D. Diego- Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, D. Drouhin, T. Eberl, A. Eddyamoui, T. van Eeden, D. van Eijk, I. El Bojaddaini, H. Eljarrari, D. Elsaesser, A. Enzenhöfer, V. Espinosa, P. Fermani, G. Ferrara, M. D. Filipovic, F. Filippini, J. Fransen, L. A. Fusco, D. Gajanana, T. Gal, J. García Méndez, A. Garcia Soto, E. Garçon, F. Garufi, C. Gatius, N. Geißelbrecht, L. Gialanella, E. Giorgio, S. R. Gozzini, R. Gracia, K. Graf, G. Grella, D. Guderian, C. Guidi, B. Guillon, M. Gutiérrez, J. Haefner, S. Hallmann, H. Hamdaoui, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, S. Henry, J. J. Hernández-Rey, J. Hofestädt, F. Huang,W. Idrissi Ibnsalih, A. Ilioni, G. Illuminati, C.W. James, D. Janezashvili, P. Jansweijer, M. de Jong, P. de Jong, B. J. Jung, M. Kadler, P. Kalaczynski, O. Kalekin,U. F. Katz, F. Kayzel, P.Keller, N. R. Khan Chowdhury, G. Kistauri, F. van der Knaap, P. Kooijman, A. Kouchner, M. Kreter, V. Kulikovskiy, M. La, Postprint (published version)

The KM3NeT collaboration is currently building a new generation of large-volume waterCherenkov neutrino telescopes in the Mediterranean sea. Two detectors, ARCA and ORCA, are under construction. They feature different neutrino energy thresholds: TeV range for ARCA and GeV range for ORCA. The main research goal of ORCA is the measurement of the neutrino mass ordering and atmospheric neutrino oscillation parameters, while the detector is also sensitive to a wide variety of other physics topics, including non-standard interactions, sterile neutrinos and Earth tomography, as well as low-energy neutrino astronomy. This contribution will present an overview of the updated ORCA sensitivity projection to its main science objectives, including - but not limited to - the measurement of the neutrino mass ordering and oscillation parameters Future perspectives for ORCA to serve as far detector for a long baseline neutrino experiment with a neutrino beam from the U70 accelerator complex at Protvino in Russia will also be discussed., Article signat per 297 autors/es: M.Ageron, S. Aiello, A. Albert, M. Alshamsi, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, G. Anton, M. Ardid, S. Ardid, W. Assal, J. Aublin, C. Bagatelas, B. Baret, S. Basegmez du Pree, M. Bendahman, F. Benfenati, E. Berbee, A. M. van den Berg, V. Bertin, S. Beurthey, V. van Beveren, S. Biagi, M. Billault, M. Bissinger, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, C. Boutonnet, G. Bouvet, M. Bouwhuis, C. Bozza, H.Brânzas, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, L. Caillat, D. Calvo, S. Campion, A. Capone, H. Carduner, V. Carretero, P. Castaldi, S. Celli;, R. Cereseto, M. Chabab, C. Champion, N. Chau, A. Chen, S. Cherubini, V. Chiarella, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, M. Colomer Molla, S. Colonges, R. Coniglione, A. Cosquer, P. Coyle, M. Cresta, A. Creuso, A. Cruz, G. Cuttone, A. D’Amico, R. Dallier, B. De Martino, M. De Palma, I. Di Palma, A. F. Díaz, D. Diego- Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, D. Drouhin, T. Eberl, A. Eddyamoui, T. van Eeden, D. van Eijk, I. El Bojaddaini, H. Eljarrari, D. Elsaesser, A. Enzenhöfer, V. Espinosa, P. Fermani, G. Ferrara, M. D. Filipovic, F. Filippini, J. Fransen, L. A. Fusco, D. Gajanana, T. Gal, J. García Méndez, A. Garcia Soto, E. Garçon, F. Garufi, C. Gatius, N. Geißelbrecht, L. Gialanella, E. Giorgio, S. R. Gozzini, R. Gracia, K. Graf, G. Grella, D. Guderian, C. Guidi, B. Guillon, M. Gutiérrez, J. Haefner, S. Hallmann, H. Hamdaoui, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, S. Henry, J. J. Hernández-Rey, J. Hofestädt, F. Huang,W. Idrissi Ibnsalih, A. Ilioni, G. Illuminati, C.W. James, D. Janezashvili, P. Jansweijer, M. de Jong, P. de Jong, B. J. Jung, M. Kadler, P. Kalaczynski, O. Kalekin,U. F. Katz, F. Kayzel, P.Keller, N. R. Khan Chowdhury, G. Kistauri, F. van der Knaap, P. Kooijman, A. Kouchner, M. Kreter, V. Kulikovskiy, M. La, Postprint (published version)

The muons produced by cosmic ray interactions in the upper atmosphere constitute the most abundant signal for underwater neutrino detectors such as KM3NeT (the Cubic Kilometre Neutrino Telescope), which is currently being deployed in the Mediterranean Sea at two distinct locations. Situated at different depths, the KM3NeT/ARCA and KM3NeT/ORCA detectors experience a different flux of muons, and thus are uniquely positioned to study their evolution and propagation from cosmic ray showers. It is imperative to the main physics goals of the experiment that the atmospheric muon background is modelled correctly, which aids in benchmarking and understanding the detector response to the constant flux of these particles. In this study, the data from the KM3NeT/ORCA detector is used and compared with the Monte Carlo (MC) prediction from the MUPAGE (MUons from PArametric formulas: a fast GEnerator for neutrino telescopes) software package, which generates the energy spectrum, lateral distribution, and muon multiplicity of muon bundles according to a specific parametrisation at different depths below sea level. This parametrisation consists of many free parameters which can be tuned such that simulated physical observables in the detector agree with those measured in data. In this way, improvements to the data-MC agreement are achieved by quantitatively comparing the level of agreement between simulated and measured observables in the KM3NeT detector., Article signat per 297 autors/es: M.Ageron, S. Aiello, A. Albert, M. Alshamsi, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, G. Anton, M. Ardid, S. Ardid, W. Assal, J. Aublin, C. Bagatelas, B. Baret, S. Basegmez du Pree, M. Bendahman, F. Benfenati, E. Berbee, A. M. van den Berg, V. Bertin, S. Beurthey, V. van Beveren, S. Biagi, M. Billault, M. Bissinger, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, C. Boutonnet, G. Bouvet, M. Bouwhuis, C. Bozza, H.Brânzas, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, L. Caillat, D. Calvo, S. Campion, A. Capone, H. Carduner, V. Carretero, P. Castaldi, S. Celli;, R. Cereseto, M. Chabab, C. Champion, N. Chau, A. Chen, S. Cherubini, V. Chiarella, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, M. Colomer Molla, S. Colonges, R. Coniglione, A. Cosquer, P. Coyle, M. Cresta, A. Creuso, A. Cruz, G. Cuttone, A. D’Amico, R. Dallier, B. De Martino, M. De Palma, I. Di Palma, A. F. Díaz, D. Diego- Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, D. Drouhin, T. Eberl, A. Eddyamoui, T. van Eeden, D. van Eijk, I. El Bojaddaini, H. Eljarrari, D. Elsaesser, A. Enzenhöfer, V. Espinosa, P. Fermani, G. Ferrara, M. D. Filipovic, F. Filippini, J. Fransen, L. A. Fusco, D. Gajanana, T. Gal, J. García Méndez, A. Garcia Soto, E. Garçon, F. Garufi, C. Gatius, N. Geißelbrecht, L. Gialanella, E. Giorgio, S. R. Gozzini, R. Gracia, K. Graf, G. Grella, D. Guderian, C. Guidi, B. Guillon, M. Gutiérrez, J. Haefner, S. Hallmann, H. Hamdaoui, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, S. Henry, J. J. Hernández-Rey, J. Hofestädt, F. Huang,W. Idrissi Ibnsalih, A. Ilioni, G. Illuminati, C.W. James, D. Janezashvili, P. Jansweijer, M. de Jong, P. de Jong, B. J. Jung, M. Kadler, P. Kalaczynski, O. Kalekin,U. F. Katz, F. Kayzel, P.Keller, N. R. Khan Chowdhury, G. Kistauri, F. van der Knaap, P. Kooijman, A. Kouchner, M. Kreter, V. Kulikovskiy, M. La, Postprint (published version)

The KM3NeT Collaboration has successfully deployed the first detection units of the next generation undersea neutrino telescopes in the Mediterranean Sea at the two sites in Italy and in France. The data sample collected between December 2016 and January 2020 has been used to measure the atmospheric muon rate at two different depths under the sea level: 3.5 km with KM3NeTARCA and 2.5 km with KM3NeT-ORCA. Atmospheric muons represent an abundant signal in a neutrino telescope and can be used to test the reliability of the Monte Carlo simulation chain and to study the physics of extensive air showers caused by highly-energetic primary nuclei impinging the Earth’s atmosphere. At energies above PeV the contribution from prompt muons, created right after the first interaction in the shower, is expected to become dominant, however its existence has not yet been experimentally confirmed. In this talk, data collected with the first detection units of KM3NeT are compared to Monte Carlo simulations based on MUPAGE and CORSIKA codes. The main features of the simulation and reconstruction chains are presented. Additionally, the first results of the simulated signal from the prompt muon component for KM3NeT-ARCA and KM3NeT-ORCA obtained with CORSIKA are discussed., Article signat per 297 autors/es: M.Ageron, S. Aiello, A. Albert, M. Alshamsi, S. Alves Garre, Z. Aly, A. Ambrosone, F. Ameli, M. Andre, G. Androulakis, M. Anghinolfi, M. Anguita, G. Anton, M. Ardid, S. Ardid, W. Assal, J. Aublin, C. Bagatelas, B. Baret, S. Basegmez du Pree, M. Bendahman, F. Benfenati, E. Berbee, A. M. van den Berg, V. Bertin, S. Beurthey, V. van Beveren, S. Biagi, M. Billault, M. Bissinger, M. Boettcher, M. Bou Cabo, J. Boumaaza, M. Bouta, C. Boutonnet, G. Bouvet, M. Bouwhuis, C. Bozza, H.Brânzas, R. Bruijn, J. Brunner, R. Bruno, E. Buis, R. Buompane, J. Busto, B. Caiffi, L. Caillat, D. Calvo, S. Campion, A. Capone, H. Carduner, V. Carretero, P. Castaldi, S. Celli;, R. Cereseto, M. Chabab, C. Champion, N. Chau, A. Chen, S. Cherubini, V. Chiarella, T. Chiarusi, M. Circella, R. Cocimano, J. A. B. Coelho, A. Coleiro, M. Colomer Molla, S. Colonges, R. Coniglione, A. Cosquer, P. Coyle, M. Cresta, A. Creuso, A. Cruz, G. Cuttone, A. D’Amico, R. Dallier, B. De Martino, M. De Palma, I. Di Palma, A. F. Díaz, D. Diego- Tortosa, C. Distefano, A. Domi, C. Donzaud, D. Dornic, M. Dörr, D. Drouhin, T. Eberl, A. Eddyamoui, T. van Eeden, D. van Eijk, I. El Bojaddaini, H. Eljarrari, D. Elsaesser, A. Enzenhöfer, V. Espinosa, P. Fermani, G. Ferrara, M. D. Filipovic, F. Filippini, J. Fransen, L. A. Fusco, D. Gajanana, T. Gal, J. García Méndez, A. Garcia Soto, E. Garçon, F. Garufi, C. Gatius, N. Geißelbrecht, L. Gialanella, E. Giorgio, S. R. Gozzini, R. Gracia, K. Graf, G. Grella, D. Guderian, C. Guidi, B. Guillon, M. Gutiérrez, J. Haefner, S. Hallmann, H. Hamdaoui, H. van Haren, A. Heijboer, A. Hekalo, L. Hennig, S. Henry, J. J. Hernández-Rey, J. Hofestädt, F. Huang,W. Idrissi Ibnsalih, A. Ilioni, G. Illuminati, C.W. James, D. Janezashvili, P. Jansweijer, M. de Jong, P. de Jong, B. J. Jung, M. Kadler, P. Kalaczynski, O. Kalekin,U. F. Katz, F. Kayzel, P.Keller, N. R. Khan Chowdhury, G. Kistauri, F. van der Knaap, P. Kooijman, A. Kouchner, M. Kreter, V. Kulikovskiy, M. La, Postprint (published version)

The 8-channel Multiple Use Silicon Photo-multiplier (SiPM) Integrated Circuit (MUSIC) Application specific integrated circuit (ASIC) for SiPM anode readout has been designed for applications where large photo-detection areas are required. MUSIC offers three main features: (1) Sum of the eight input channels using a differential output driver, (2) eight individual single ended (SE) analog outputs, and (3) eight individual SE binary outputs using a time over threshold technique. Each functionality, summation and individual readout includes a selectable dual-gain configuration. Moreover, the signal sum implements a dual-gain output providing a 15-bit dynamic range. The circuit contains a tunable pole zero cancellation of the SiPM recovery time constant to deal with most of the available SiPM devices in the market. Experimental tests show how MUSIC can linearly sum signals from different SiPMs and distinguish even a few photons. Additionally, it provides a single photon output pulse width at half maximum (FWHM) between 5–10 ns for the analog output and a single-photon time resolution (SPTR) around 118 ps sigma using a Hamamatsu SiPM S13360-3075CS for the binary output. Lastly, the summation mode has a power consumption of ≈200 mW, whereas the individual readout consumes ≈30 mW/ch.

Polaritons in two-dimensional (2D) materials have shown their unique capabilities to concentrate light into deep subwavelength scales. Precise control of the excitation and propagation of 2D polaritons has remained a central challenge for future on-chip nanophotonic devices and circuits. To solve this issue, we exploit Cherenkov radiation, a classic physical phenomenon that occurs when a charged particle moves at a velocity greater than the phase velocity of light in that medium, in low-dimensional material heterostructures. Here, we report an experimental observation of Cherenkov phonon polariton wakes emitted by superluminal one-dimensional plasmon polaritons in a silver nanowire and hexagonal boron nitride heterostructure using near-field infrared nanoscopy. The observed Cherenkov radiation direction and radiation rate exhibit large tunability through varying the excitation frequency. Such tunable Cherenkov phonon polaritons provide opportunities for novel deep subwavelength-scale manipulation of light and nanoscale control of energy flow in low-dimensional material heterostructures.

External beam radiation therapy (EBRT) is one of the most common forms of therapy used to treat cancers worldwide. New EBRT modalities are being developed across a range of therapies to improve patient outcomes. With these new therapies comes unique challenges for dosimetry and quality assurance which is vital for safe and effective treatments. Microbeam radiation therapy (MRT) is a novel form of EBRT that uses spatially fractionated synchrotron sourced kilovoltage x-rays to deliver highly-targeted planes of x-rays to the target volume. These microbeams are typically 25 – 50 µm in thickness, with a peak-to-peak separation of 200 – 400 µm . MRT is currently limited to synchrotron sources, and is therefore only being studied at a small number of facilities worldwide, but the emergence of compact synchrotron technology has the potential to make MRT much more accessible. Due to the extreme dose rates of MRT (in excess of 5000 Gy/s in some configurations) and high spatial fractionation of the microbeams, MRT dosimetry is an ongoing challenge that must be solved if it is to be used in human clinical trials. In this thesis scintillator fibre-optic dosimeters (FODs) with the highest spatial res- olution found in the literature are developed and tested at the Australian Synchrotron on the Imaging and Medical BeamLine, where MRT cell and animal studies are being conducted. These scintillator FODs use plastic scintillator due to its water-equivalence, energy and temperature independence and radiation hardness. The scintillator is fab- ricated to have a thickness equal to the desired one-dimensional spatial resolution for microbeam dosimetry. In this thesis scintillator probes with thicknesses 50 µm , 20 µm , and 10 µm are presented. The scintillator is coupled to an optical fibre with core diameter 1.0 mm. When oriented with the thin edge of the scintillator towards the beam, a microbeam array can be scanned with this high resolution. The FODs were able to resolve microbeams w

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 similar to 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. (C) 2016 Elsevier B.V. All rights reserved., Postprint (author's final draft)

We analyze the full relativistic force experienced by swift electrons moving close to planar films for the experimental conditions commonly used in electron energy loss spectroscopy in STEM. In metals the main effects derive from the dispersion of the surface plasmons, which are clearly observed in the EEL spectra. In insulators we explore the role played by the Cherenkov radiation (CR) emitted in the energy gap window. The focus is placed on the transverse force and different factors which may turn this force into repulsive, as reported in recent experimental and theoretical works.

The full retarded electromagnetic force experienced by swift electrons moving parallel to planar boundaries is revisited, for both metallic and dielectric targets, with special emphasis on the consequences in electron microscopy experiments. The focus is placed on the sign of the transverse force experienced by the electron beam as a function of the impact parameter. For point probes, the force is found to be always attractive. The contribution of the induced magnetic field and the causality requirements of the target dielectric response, given by the Kramers-Kronig (K-K) relations, prove to be crucial issues at small impact parameters. For spatially extended probes, repulsive forces are predicted for close trajectories, in agreement with previous works. The force experienced by the target is also explored, with the finding that in insulators, the momentum associated to Cherenkov radiation (CR) is relevant at large impact parameters.

The characterization of the new Hamamatsu R11265-103-M64 multi-anode photomultiplier tube is presented. The sample available in our laboratory was tested and in particular the response to single photon was extensively studied. The gain, the anode uniformity and the dark current were measured. The tube behaviour in a longitudinal magnetic field up to 100 G was studied and the gain loss due to the ageing was quantified. The characteristics and performance of the photomultiplier tube make the R11265-103-M64 particularly tailored for an application in high energy physics experiments, such as in the LHCb Ring Imaging Cherenkov (RICH) detector at LHC.

The full retarded electromagnetic force experienced by swift electrons moving parallel to planar boundaries is revisited, for both metallic and dielectric targets, with special emphasis on the consequences in electron microscopy experiments. The focus is placed on the sign of the transverse force experienced by the electron beam as a function of the impact parameter. For point probes, the force is found to be always attractive. The contribution of the induced magnetic field and the causality requirements of the target dielectric response, given by the Kramers-Kronig (K-K) relations, prove to be crucial issues at small impact parameters. For spatially extended probes, repulsive forces are predicted for close trajectories, in agreement with previous works. The force experienced by the target is also explored, with the finding that in insulators, the momentum associated to Cherenkov radiation (CR) is relevant at large impact parameters. © 2014 IOP Publishing Ltd and Deutsche Physikalische Gesellschaft.

This study investigates the effects of different charge density rise times upon the magnitude of the Cerenkov radiation produced by a semi-infinite electron beam. The magnetic field pulses were generated for different rise times and relationships between the maximum magnitudes and their associated rise times were obtained. These were compared with theoretical relationships derived from a power series approximation. The generated results were close to those predicted by theory for short rise times at short radial distances. For longer rise times, the departure from theory was caused by the magnitude of the decay portion of the magnetic pulse. This effect could be mitigated at longer rise times by increasing the radial distance from the electron beam., http://archive.org/details/effectsofcharged1094537535, Lieutenant, United States Navy, Approved for public release; distribution is unlimited.

We study theoretically the Čerenkov-type second-harmonic generation by a Gaussian beam in quadratic nonlinear media with periodically reverted ferroelectric domains. In particular, we consider the role of fundamental beam width on the harmonic emission process. We show that varying the beam width of the fundamental wave not only affects the strength of the emitted Čerenkov harmonic signal but also changes the sensitivity of the emission process to wavelength tuning., Postprint (published version)

The radiation from a relativistic electron uniformly moving along the axis of cylindrical waveguide filled with laminated material of finite length is investigated. Expressions for the spectral distribution of radiation passing throw the transverse section of waveguide at large distances from the laminated material are derived with no limitations on the amplitude and variation profile of the layered medium permittivity and permeability. Numerical results for layered material consisting of dielectric plates alternated with vacuum gaps are given. It is shown that at a special choice of problem parameters, Cherenkov radiation generated by the relativistic electron inside the plates is self-amplified. The visual explanation of this effect is given and a possible application is discussed.

We calculate the rate at which a free tachyon (faster than light particle) would emit gravitational radiation. It is very small.

The muon and anti-muon neutrino energy spectrum is determined from 2000-2003 AMANDA telescope data using regularised unfolding. This is the first measurement of atmospheric neutrinos in the energy range 2-200 TeV. The result is compared to different atmospheric neutrino models and it is compatible with the atmospheric neutrinos from pion and kaon decays. No significant contribution from charm had-ron decays or extraterrestrial neutrinos is detected. The capabilities to improve the measurement of the neutrino spectrum with the successor experiment IceCube are discussed.

The muon and anti-muon neutrino energy spectrum is determined from 2000-2003 AMANDA telescope data using regularised unfolding. This is the first measurement of atmospheric neutrinos in the energy range 2-200 TeV. The result is compared to different atmospheric neutrino models and it is compatible with the atmospheric neutrinos from pion and kaon decays. No significant contribution from charm hadron decays or extraterrestrial neutrinos is detected. The capabilities to improve the measurement of the neutrino spectrum with the successor experiment IceCube are discussed., 0, SCOPUS: ar.j, info:eu-repo/semantics/published

Cherenkov radiation in the soft x-ray region is generated in narrowband regions at inner-shell absorption edges. Mainly low-Z elements are suitable Cherenkov sources, which emit in a photon energy range from 30 eV to 1 keV and require moderate electron energies up to 25 MeV. Generally, in the soft x-ray region materials are highly absorbing and therefore the Cherenkov radiation theory is discussed for absorbing media. A detailed description includes transition radiation that is generated at the interface when the relativistic electron exits the material. We show that the transition radiation yield equation, when it is adopted for an absorbing medium, includes Cherenkov radiation. Based on this approach it is shown that the spectral intensity of Cherenkov radiation in the soft x-ray region is large compared to transition radiation for moderate electron energies. First measurements of soft x-ray Cherenkov radiation in the water-window spectral region, generated in titanium and vanadium foils, are discussed in detail. The measured spectral and angular distribution of the radiation, and the measured total yield (≈ 10 -4 photon per electron) are in agreement with theoretical predictions based on the refractive index data. We show that the brightness that can be achieved using a small electron accelerator is sufficient for practical x-ray microscopy in the water window.

Plasma modes in stacked Josephson junctions are easily understood analytically from a linearization of the coupled sine-Gordon equation describing the system. We demonstrate here by numerical methods that the analytically derived symmetries of the plasma modes are carried over to the fluxon modes. Using this fact we are, with a few exceptions, able to predict and construct a full family of Josephson fluxon modes without using numerical methods. The nature of the locking mechanism needed to create the technologically important in-phase fluxon modes is discussed.

Fluxon dynamics in a system of three coupled driven damped sine-Gordon equations is investigated. Bunching of fluxons is observed. It is shown that fluxon-fluxon-fluxon bound states exist in a certain interval of the fluxon velocity. Attraction between fluxons occurs as a result of indirect fluxon-fluxon interaction mediated by Swihart waves. To tackle the problem analytically a piece-wise linear approach is developed. The analytical approximations show good agreement with the results obtained by direct numerical simulations.

The purpose of this thesis is to examine the properties of NaBi(WO4)2 and determine its usefulness as a Cherenkov radiator. An implicit requirement in this process is to determine the best configuration of a counter using NaBi(WO4)2 to detect the Cherenkov photons using a photomultiplier tube.

by Lui Bong Chun, Richard., Thesis (M.Phil.)--Chinese University of Hong Kong, 1995., Includes bibliographical references., Acknowledgment, Chapter Chapter 1 --- Introduction --- p.1, Chapter 1.1 --- Background for the Project --- p.1, Chapter 1.1.1 --- Interests in Blue-Green Laser --- p.1, Chapter 1.1.2 --- Progress of Blue-Green Laser --- p.2, Chapter 1.2 --- The Aim of the Project --- p.3, Chapter 1.3 --- Overview the Remaining Parts of this Thesis --- p.4, Chapter 1.4 --- References --- p.6, Chapter Chapter 2 --- Sum Frequency Generation --- p.8, Chapter 2.1 --- Introduction --- p.8, Chapter 2.2 --- Sum Frequency Generation --- p.8, Chapter 2.2.1 --- Theoretical Background for Sum Frequency Generation --- p.9, Chapter 2.2.2 --- The Coupled Wave Equations for SFG --- p.13, Chapter 2.2.3 --- Phase Matching Considerations --- p.16, Chapter 2.3 --- References --- p.18, Chapter Chapter 3 --- Cerenkov Radiation --- p.19, Chapter 3.1 --- Introduction --- p.19, Chapter 3.2 --- The Properties of Cerenkov Radiation by Using TM Mode --- p.21, Chapter 3.2.1 --- Refractive Index Notation --- p.23, Chapter 3.2.2 --- Fundamental Wave TM Guides Mode --- p.23, Chapter 3.2.3 --- Second Harmonic TM Radiation Mode --- p.24, Chapter 3.2.4 --- Efficiency of SHG --- p.25, Chapter 3.3 --- Simplified Model Analysis of Cerenkov Radiation in TE Mode --- p.29, Chapter 3.4 --- Simulation --- p.33, Chapter 3.4.1 --- Modeling the LiNb03 --- p.33, Chapter 3.4.2 --- Modeling an Asymmetric Slab Waveguide ´ؤPMMA doped with MNA on Fused Quartz --- p.37, Chapter 3.4.3 --- Modeling a Symmetric Slab Waveguide ´ؤPMMA doped with MNA on Fused Quartz --- p.42, Chapter 3.5 --- References --- p.47, Chapter Chapter 4 --- Ellipsometry --- p.49, Chapter 4.1 --- Introduction --- p.49, Chapter 4.2 --- General Principles --- p.49, Chapter 4.3 --- Basic Operation --- p.50, Chapter 4.4 --- The Optical Constants of the Bulk Materials --- p.51, Chapter 4.5 --- Calculation the Refractive Index of the Substrates --- p.53, Chapter 4.6 --- Ellipsometric Theory for the Thin Film --- p.57, Chapter 4.7 --- Measurement the Refractive Index and the Thickness of the Thin Film --- p.59, Chapter 4.7.1 --- Data --- p.62, Chapter 4.7.2 --- Discussions --- p.73, Chapter 4.8 --- Calculation the Refractive Index of the thin Film by Considering as a Bulk Material --- p.78, Chapter 4.9 --- References --- p.80, Chapter Chapter 5 --- Prism Coupling --- p.81, Chapter 5.1 --- Introduction --- p.81, Chapter 5.2 --- Coupling of a Plane Wave --- p.82, Chapter 5.3 --- Numerical Approach for the Calculation of the Coupling Efficiency --- p.85, Chapter 5.4 --- Experiment --- p.88, Chapter 5.4.1 --- Experimental Setup --- p.88, Chapter 5.4.2 --- Experimental Result and Discussions --- p.90, Chapter 5.5 --- References --- p.92, Chapter Chapter 6 --- Conclusion --- p.93, Chapter Chapter 7 --- Future Plans --- p.96, Chapter 7.1 --- Simplified Model of Corona Poling --- p.96, Chapter 7.2 --- Advanced Models of Poling --- p.98, Chapter 7.2.1 --- Slab Waveguide --- p.98, Chapter 7.2.2 --- Channel Waveguide --- p.99, Chapter 7.3 --- References --- p.100, Chapter Appendix 1 --- Materials' Descriptions --- p.A-l, Chapter A.1.1 --- 2-Methyl-4-Nitoaniline --- p.A-1, Chapter A.1.2 --- Poly ( Methyl Methacrylate ) --- p.A-3, Chapter A.1.3 --- References --- p.A-4, Chapter Appendix 2 --- Fabrication Procedures --- p.A-5, Chapter A.2.1 --- Cleaning the Apparatus --- p.A-5, Chapter A.2.2 --- Cleaning the Substrate --- p.A-5, Chapter A.2.3 --- Thin film Fabrication --- p.A-5, Chapter A.2.4 --- Thin Film Removal --- p.A-6, Chapter A.2.5 --- References --- p.A-6, Chapter Appendix 3 --- Alpha Step --- p.A-7, Chapter A.3.1 --- Introduction --- p.A-7, Chapter A.3.2 --- Experimental Setup --- p.A-8, Chapter A.3.3 --- Experimental Results --- p.A-9, Chapter A.3.3.1 --- Thin Film of PMMA without Dopant --- p.A-9, Chapter A.3.3.2 --- Thin Film of PMMA doped with MNA --- p.A-19, Chapter A.3.4 --- Discussions --- p.A-27, Chapter A.3.5 --- References --- p.A-28, Chapter Appendix 4 --- Scanning Electron Microscope --- p.A-29, Chapter A.4.1 --- Scanning Electron Microscope --- p.A-29, Chapter A.4.2 --- Reference --- p.A-30, Chapter Appendix 5 --- Gaussian Beam & Coordinate System Transformation --- p.A-31, Chapter A.5.1 --- Gaussian Beam in a Homogeneous Medium --- p.A-31, Chapter A.5.2 --- Transformation of the Coordinate Systems --- p.A-32, Chapter A.5.3 --- Reference --- p.A-32, Chapter Appendix 6 --- Waist Size Measurement of Gaussian Beam --- p.A-33, Chapter A.6.1 --- Waist Size Measurement of Gaussian Beam --- p.A-33, Chapter A.6.2 --- References --- p.A-34, Chapter Appendix 7 --- Quasi Phase Matching --- p.A-35, Chapter A. 7.1 --- Introduction --- p.A-35, Chapter A.7.2 --- Basic Concept of QPM --- p.A-36, Chapter A.7.3 --- References --- p.A-38, Chapter Appendix 8 --- Program Listing --- p.A-41, Chapter A.8.1 --- Program Listing ( Chapter 3 ) --- p.A-41, Chapter A.8.1.1 --- Program 3.1 (transcendental.m ) --- p.A-41, Chapter A.8.1.2 --- Program 3.2 (linbo3.m) --- p.A-42, Chapter A.8.2 --- Program Listing ( Chapter 4 ) --- p.A-45, Chapter A.8.2.1 --- Program 4.1 ( ellipsometry.m ) --- p.A-45, Chapter A.8.3 --- Program Listing ( Chapter 5 ) --- p.A-47, Chapter A.8.3.1 --- Program 5.1 ( parameter.m ) --- p.A-47, Chapter A.8.3.2 --- Program 5.2 ( coupling.m ) --- p.A-49, Chapter A.8.3.3 --- Program 5.3 ( v_3_amp.m ) --- p.A-50, Chapter A.8.3.4 --- Program 5.4 ( input_profile.m ) --- p.A-51, http://library.cuhk.edu.hk/record=b5895596, Use of this resource is governed by the terms and conditions of the Creative Commons “Attribution-NonCommercial-NoDerivatives 4.0 International” License (http://creativecommons.org/licenses/by-nc-nd/4.0/)

This publication provides a simplified technical description of the TRIGA research reactor at AFRRI. Topics covered include general principles of reactor operation and a description of the TRIGA reactor and its unique features., Revision Rept. no. AFFRI-TR-86-1, ADA168238.

Cerenkov radiation is calculated for electron beams which exceed the velocity of radiation in a non dispersive dielectric medium. The electron beam is assumed to be bunched as emitted from a travelling wave accelerator, and the emission region is assumed to be finite. Predictions include: emission at harmonics of the bunch rate; coherence of radiation at low frequencies; smearing of the emission angle for finite emission regions; and explicit evaluation of power spectrum in terms of bunch dimensions. The results apply to microwave emission from fast electrons in air or other dielectrics. (Author), Chief of Naval Research, http://archive.org/details/cerenkovradiatio00busk, 62763N;RF68-342-800 N0001482WR20195, NA

The electron beam in a free electron laser (FEL) becomes axially modulated at the optical wave length of the FEL radiation. This electron beam passed through a gas may produce intense Cerenkov radiation. The effects of the radial and axial dimension of the electron bunches on the radiation are explored, Prepared for: Defense Advanced Research Projects Agency, Arlington, VA 2209-2309., http://archive.org/details/radiationproduce00busk, Approved for public release; distribution is unlimited.

Measurement of microwave Cerenkov radiation in air exhibits the diffraction pattern predicted in earlier work. The radiation appears only at harmonics of the frequency of periodic electron bunches. Angular distribution power measurements are presented for frequencies of 2.86, 5.71, 8.57, and 11.42 GHz corresponding to the fundamental and the first three harmonics of an S-band rf linac.

X-ray Çerenkov radiation can be generated by electrons incident on thin foils. For grazing incidence the Çerenkov radiation intensity can be more than a decade greater than for perpendicular incidence. Experimental results are discussed in terms of a simple formalism. 17 refs., 3 figs.

Degree granted: Thesis (M.S.)--Florida Atlantic University, 1982., Summary: The dispersion relation for a dielectrically loaded cylindrical waveguide, both with and without a beam of electrons, is found. It is shown that in the limit of Cerenkov threshold, the frequency goes to infinity. Also, using the fields derived, the Poynting vector is computed. It is shown that the Poynting vector increases and the operating frequency decreases with the thickness of the liner., Charles E. Schmidt College of Science, Collection: FAU Electronic Theses and Dissertations Collection

Self-diffracted Cherenkov X-rays emitted from relativistic electrons penetrating into the periodic multilayer nanostructure are consid-ered in this work, Belgorod State University

X-ray Cherenkov radiation in the vicinity of the photoabsorption edge of a target is considered in this work, Belgorod State University

Nuclear recoil events produced by neutron scatters form one of the most important classes of background in WIMP direct detection experiments, as they may produce nuclear recoils that look exactly like WIMP interactions. In DarkSide-50, we both actively suppress and measure the rate of neutron-induced background events using our neutron veto, composed of a boron-loaded liquid scintillator detector within a water Cherenkov detector

An experiment was conducted which measured the Radio Frequency (RF) radiation from the PHERMEX accelerator, capable of 30 MeV and 600 A. This was accomplished by placing TEM horn antennae at varying angles from the path of the electron beam. The signals received by the antennae were then recorded by using a Digitizing Camera System (DCS). Measurements were taken of the radiation from propagating and non-propagating beams, beams with energy above and below Cherenkov threshold, and beams with varied currents. The captured RF signals and their corresponding frequency spectra were then analyzed. This analysis showed that the radio frequency radiation from the beams below the cherenkov threshold contained primarily transition radiation; when above, diffracted Cherenkov radiation was observed. Non-propagating beams produced larger-angle radiation and had less definition in their spectrum. All electric fields measured were proportional to the beam current. Lastly, the electron beam pulse width and separation were determined by both the received signals and their spectrum., http://archive.org/details/analysisofradiof1094537527, Captain, United States Army, Approved for public release; distribution is unlimited.

Tato práce řeší vztah mezi jasem Čerenkovova záření v jaderném reaktoru a výkonem jaderného reaktoru. Čerenkovovo záření vzniká při průchodu nabitých částic hmotným prostředím, pokud je jejich rychlost vyšší než fázová rychlost světla v daném prostředí. V jaderných reaktorech moderovaných vodou vzniká díky vytržení elektronů z obalů působením gama záření. Měření je provedeno pomocí fotoaparátu a softwaru na fotometrické měření jasu. Dále je zde řešeno využití detekce Čerenkovova záření pro měření vyhoření použitého jaderného paliva. Jsou zde uvedeny příklady využití detekce Čerenkovova záření pro měření výkonu jaderných reaktorů, včetně analýzy naměřených výsledků na školním jaderném reaktoru VR-1. Naměřené výsledky ukazují, že při rostoucím výkonu roste i intenzita Čerenkovova záření, ovšem při prudkém snížení se objevuje zbytkové záření způsobené zpožděným gama zářením. Možné využití detekce jasu Čerenkovova záření je při monitorování nepředvídatelného zvýšení výkonu reaktoru či při kontrole použitého paliva., This work deals with the connection between the luminance of Cherenkov radiation in a nuclear reactor and his power. Cherenkov radiation arises when charged particle passing through the medium if their speed is higher than the phase velocity of light in that medium. In water moderated reactors, it is caused by secondary electrons produced by absorption of gamma rays. The measurement is done using the camera and software for photometric luminance measurements. Furthermore, there is mentioned the use of Cerenkov radiation detection to measure burnout of spent nuclear fuel. There are examples of usage of Cherenkov radiation detection to measure of nuclear reactors power, including an analysis of the measured results on research nuclear reactor VR -1. The measured results show increasing intensity of Cherenkov radiation with increasing reactor power, but residual detection response caused by delayed gamma radiation was observed after the rapid decrease of the reactor power. Possible use of detection luminance of Cherenkov radiation is in monitoring unforeseen increase in reactor power or in the control of used fuel.

Tato práce řeší vztah mezi jasem Čerenkovova záření v jaderném reaktoru a výkonem jaderného reaktoru. Čerenkovovo záření vzniká při průchodu nabitých částic hmotným prostředím, pokud je jejich rychlost vyšší než fázová rychlost světla v daném prostředí. V jaderných reaktorech moderovaných vodou vzniká díky vytržení elektronů z obalů působením gama záření. Měření je provedeno pomocí fotoaparátu a softwaru na fotometrické měření jasu. Dále je zde řešeno využití detekce Čerenkovova záření pro měření vyhoření použitého jaderného paliva. Jsou zde uvedeny příklady využití detekce Čerenkovova záření pro měření výkonu jaderných reaktorů, včetně analýzy naměřených výsledků na školním jaderném reaktoru VR-1. Naměřené výsledky ukazují, že při rostoucím výkonu roste i intenzita Čerenkovova záření, ovšem při prudkém snížení se objevuje zbytkové záření způsobené zpožděným gama zářením. Možné využití detekce jasu Čerenkovova záření je při monitorování nepředvídatelného zvýšení výkonu reaktoru či při kontrole použitého paliva., This work deals with the connection between the luminance of Cherenkov radiation in a nuclear reactor and his power. Cherenkov radiation arises when charged particle passing through the medium if their speed is higher than the phase velocity of light in that medium. In water moderated reactors, it is caused by secondary electrons produced by absorption of gamma rays. The measurement is done using the camera and software for photometric luminance measurements. Furthermore, there is mentioned the use of Cerenkov radiation detection to measure burnout of spent nuclear fuel. There are examples of usage of Cherenkov radiation detection to measure of nuclear reactors power, including an analysis of the measured results on research nuclear reactor VR -1. The measured results show increasing intensity of Cherenkov radiation with increasing reactor power, but residual detection response caused by delayed gamma radiation was observed after the rapid decrease of the reactor power. Possible use of detection luminance of Cherenkov radiation is in monitoring unforeseen increase in reactor power or in the control of used fuel.

Tato práce řeší vztah mezi jasem Čerenkovova záření v jaderném reaktoru a výkonem jaderného reaktoru. Čerenkovovo záření vzniká při průchodu nabitých částic hmotným prostředím, pokud je jejich rychlost vyšší než fázová rychlost světla v daném prostředí. V jaderných reaktorech moderovaných vodou vzniká díky vytržení elektronů z obalů působením gama záření. Měření je provedeno pomocí fotoaparátu a softwaru na fotometrické měření jasu. Dále je zde řešeno využití detekce Čerenkovova záření pro měření vyhoření použitého jaderného paliva. Jsou zde uvedeny příklady využití detekce Čerenkovova záření pro měření výkonu jaderných reaktorů, včetně analýzy naměřených výsledků na školním jaderném reaktoru VR-1. Naměřené výsledky ukazují, že při rostoucím výkonu roste i intenzita Čerenkovova záření, ovšem při prudkém snížení se objevuje zbytkové záření způsobené zpožděným gama zářením. Možné využití detekce jasu Čerenkovova záření je při monitorování nepředvídatelného zvýšení výkonu reaktoru či při kontrole použitého paliva., This work deals with the connection between the luminance of Cherenkov radiation in a nuclear reactor and his power. Cherenkov radiation arises when charged particle passing through the medium if their speed is higher than the phase velocity of light in that medium. In water moderated reactors, it is caused by secondary electrons produced by absorption of gamma rays. The measurement is done using the camera and software for photometric luminance measurements. Furthermore, there is mentioned the use of Cerenkov radiation detection to measure burnout of spent nuclear fuel. There are examples of usage of Cherenkov radiation detection to measure of nuclear reactors power, including an analysis of the measured results on research nuclear reactor VR -1. The measured results show increasing intensity of Cherenkov radiation with increasing reactor power, but residual detection response caused by delayed gamma radiation was observed after the rapid decrease of the reactor power. Possible use of detection luminance of Cherenkov radiation is in monitoring unforeseen increase in reactor power or in the control of used fuel.

Tato práce řeší vztah mezi jasem Čerenkovova záření v jaderném reaktoru a výkonem jaderného reaktoru. Čerenkovovo záření vzniká při průchodu nabitých částic hmotným prostředím, pokud je jejich rychlost vyšší než fázová rychlost světla v daném prostředí. V jaderných reaktorech moderovaných vodou vzniká díky vytržení elektronů z obalů působením gama záření. Měření je provedeno pomocí fotoaparátu a softwaru na fotometrické měření jasu. Dále je zde řešeno využití detekce Čerenkovova záření pro měření vyhoření použitého jaderného paliva. Jsou zde uvedeny příklady využití detekce Čerenkovova záření pro měření výkonu jaderných reaktorů, včetně analýzy naměřených výsledků na školním jaderném reaktoru VR-1. Naměřené výsledky ukazují, že při rostoucím výkonu roste i intenzita Čerenkovova záření, ovšem při prudkém snížení se objevuje zbytkové záření způsobené zpožděným gama zářením. Možné využití detekce jasu Čerenkovova záření je při monitorování nepředvídatelného zvýšení výkonu reaktoru či při kontrole použitého paliva., This work deals with the connection between the luminance of Cherenkov radiation in a nuclear reactor and his power. Cherenkov radiation arises when charged particle passing through the medium if their speed is higher than the phase velocity of light in that medium. In water moderated reactors, it is caused by secondary electrons produced by absorption of gamma rays. The measurement is done using the camera and software for photometric luminance measurements. Furthermore, there is mentioned the use of Cerenkov radiation detection to measure burnout of spent nuclear fuel. There are examples of usage of Cherenkov radiation detection to measure of nuclear reactors power, including an analysis of the measured results on research nuclear reactor VR -1. The measured results show increasing intensity of Cherenkov radiation with increasing reactor power, but residual detection response caused by delayed gamma radiation was observed after the rapid decrease of the reactor power. Possible use of detection luminance of Cherenkov radiation is in monitoring unforeseen increase in reactor power or in the control of used fuel.

Tato práce řeší vztah mezi jasem Čerenkovova záření v jaderném reaktoru a výkonem jaderného reaktoru. Čerenkovovo záření vzniká při průchodu nabitých částic hmotným prostředím, pokud je jejich rychlost vyšší než fázová rychlost světla v daném prostředí. V jaderných reaktorech moderovaných vodou vzniká díky vytržení elektronů z obalů působením gama záření. Měření je provedeno pomocí fotoaparátu a softwaru na fotometrické měření jasu. Dále je zde řešeno využití detekce Čerenkovova záření pro měření vyhoření použitého jaderného paliva. Jsou zde uvedeny příklady využití detekce Čerenkovova záření pro měření výkonu jaderných reaktorů, včetně analýzy naměřených výsledků na školním jaderném reaktoru VR-1. Naměřené výsledky ukazují, že při rostoucím výkonu roste i intenzita Čerenkovova záření, ovšem při prudkém snížení se objevuje zbytkové záření způsobené zpožděným gama zářením. Možné využití detekce jasu Čerenkovova záření je při monitorování nepředvídatelného zvýšení výkonu reaktoru či při kontrole použitého paliva., This work deals with the connection between the luminance of Cherenkov radiation in a nuclear reactor and his power. Cherenkov radiation arises when charged particle passing through the medium if their speed is higher than the phase velocity of light in that medium. In water moderated reactors, it is caused by secondary electrons produced by absorption of gamma rays. The measurement is done using the camera and software for photometric luminance measurements. Furthermore, there is mentioned the use of Cerenkov radiation detection to measure burnout of spent nuclear fuel. There are examples of usage of Cherenkov radiation detection to measure of nuclear reactors power, including an analysis of the measured results on research nuclear reactor VR -1. The measured results show increasing intensity of Cherenkov radiation with increasing reactor power, but residual detection response caused by delayed gamma radiation was observed after the rapid decrease of the reactor power. Possible use of detection luminance of Cherenkov radiation is in monitoring unforeseen increase in reactor power or in the control of used fuel.

Tato práce řeší vztah mezi jasem Čerenkovova záření v jaderném reaktoru a výkonem jaderného reaktoru. Čerenkovovo záření vzniká při průchodu nabitých částic hmotným prostředím, pokud je jejich rychlost vyšší než fázová rychlost světla v daném prostředí. V jaderných reaktorech moderovaných vodou vzniká díky vytržení elektronů z obalů působením gama záření. Měření je provedeno pomocí fotoaparátu a softwaru na fotometrické měření jasu. Dále je zde řešeno využití detekce Čerenkovova záření pro měření vyhoření použitého jaderného paliva. Jsou zde uvedeny příklady využití detekce Čerenkovova záření pro měření výkonu jaderných reaktorů, včetně analýzy naměřených výsledků na školním jaderném reaktoru VR-1. Naměřené výsledky ukazují, že při rostoucím výkonu roste i intenzita Čerenkovova záření, ovšem při prudkém snížení se objevuje zbytkové záření způsobené zpožděným gama zářením. Možné využití detekce jasu Čerenkovova záření je při monitorování nepředvídatelného zvýšení výkonu reaktoru či při kontrole použitého paliva., This work deals with the connection between the luminance of Cherenkov radiation in a nuclear reactor and his power. Cherenkov radiation arises when charged particle passing through the medium if their speed is higher than the phase velocity of light in that medium. In water moderated reactors, it is caused by secondary electrons produced by absorption of gamma rays. The measurement is done using the camera and software for photometric luminance measurements. Furthermore, there is mentioned the use of Cerenkov radiation detection to measure burnout of spent nuclear fuel. There are examples of usage of Cherenkov radiation detection to measure of nuclear reactors power, including an analysis of the measured results on research nuclear reactor VR -1. The measured results show increasing intensity of Cherenkov radiation with increasing reactor power, but residual detection response caused by delayed gamma radiation was observed after the rapid decrease of the reactor power. Possible use of detection luminance of Cherenkov radiation is in monitoring unforeseen increase in reactor power or in the control of used fuel.