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1. Recent Developments within The Cosmic Ray Extremely Distributed Observatory (CREDO)

Author: Alvarez-Castillo, David, Homola, Piotr, Sushchov, Oleksandr, Stasielak, Jarosław, Stuglik, Sławomir, Góra, Dariusz, Nazari, Vahab, Oancea, Cristina, Granja, Carlos, Beznosko, Dmitriy, Zabari, Noemi, Gupta, Alok C., Hnatyk, Bohdan, Mozgova, Alona, Kasztelan, Marcin, Bielewicz, Marcin, Kovacs, Peter, Łozowski, Bartosz, Medvedev, Mikhail V., Miszczyk, Justyna, Bibrzycki, Łukasz, Niedźwiecki, Michał, Smelcerz, Katarzyna, Piekarczyk, Tomasz Hachaj Marcin, Pawlik, Maciej, Rzecki, Krzysztof, Rosas, Matías, Smolek, Karel, Svanidze, Manana, Beradze, Revaz, Tursunov, Arman, Wibig, Tadeusz, Zamora-Saa, Jilberto, Poncyljusz, Bożena, Mędrala, Justyna, Opiła, Gabriela, Pryga, Jerzy, Ruimi, Ophir, and Cahuantzi, Mario Rodriguez
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: This contribution presents the recent research developments within the Cosmic Ray Extremely Distributed Observatory (CREDO) in the search for resolution of various scientific puzzles, ranging from fundamental physical questions to applications like the determination of earthquake precursors. The state-of-the art theoretical, numerical and computational aspects of these phenomena are addressed, as well as recent experimental developments for detection., Comment: 9 pages, 7 figures. Based on the contribution to the XVIII Mexican Workshop on Particles and Fields in Puebla, Mexico, November 2022. M\'exico
Published: 2024
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2. Simulation of the isotropic ultra-high energy photons flux in the solar magnetic field and a comparison with observations made by the HAWC and Fermi-LAT observatories

Author: Alvarez-Castillo, David, Homola, Piotr, Poncyljusz, Bożena, Gora, Dariusz, Dhital, Niraj, Sushchov, Oleksandr, Stasielak, Jarosław, Stuglik, Sławomir, Nazari, Vahab, Oancea, Cristina, Beznosko, Dmitriy, Zabari, Noemi, Gupta, Alok C., Hnatyk, Bohdan, Mozgova, Alona, Kasztelan, Marcin, Bielewicz, Marcin, Kovacs, Peter, Łozowski, Bartosz, Medvedev, Mikhail V., Miszczyk, Justyna, Bibrzycki, Łukasz, Niedźwiecki, Michał, Smelcerz, Katarzyna, Hachaj, Tomasz, Piekarczyk, Marcin, Pawlik, Maciej, Rzecki, Krzysztof, Rosas, Matías, Smolek, Karel, Svanidze, Manana, Beradze, Revaz, Tursunov, Arman, Wibig, Tadeusz, Zamora-Saa, Jilberto, Mędrala, Justyna, Opiła, Gabriela, Pryga, Jerzy, Ruimi, Ophir, and Cahuantzi, Mario Rodriguez
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: In this contribution we study the possibility of the formation of cosmic ray ensembles (CRE) created by the interaction of ultra-high energy (UHE) photons with the magnetic field of the Sun. The lack of observation of those UHE and the difficulties for their identification given the current methodologies motivates this study. We performed simulations using the PRESHOWER program in order to simulate the expected extensive air showers which might be spatially correlated generated upon entering the Earth's atmosphere. We found characteristic features like very thing and extremely elongates cascades of secondary photons with their corresponding energies spanning the entire cosmic range spectrum. Shower footprints are as large as hundreds of kilometres. An application of this study is the scenario of gamma-ray emission from the vicinity of the Sun as a result of ultra-high energy photon cascading in the solar magnetic field in order to understand recent observations made by the HAWC and Fermi-LAT observatories., Comment: 8 pages, 4 figures, 38th International Cosmic Ray Conference (ICRC2023) 26 July - 3 August, 2023 Nagoya, Japan
Published: 2023
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3. Constraining X-ray variability of the blazar 3C 273 using XMM-Newton observations over two decades

Author: Dinesh, Adithiya, Bhatta, Gopal, Adhikari, Tek P., Mohorian, Maksym, Dhital, Niraj, Chaudhary, Suvas C., Panis, Radim, and Gora, Dariusz
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Blazars exhibit relentless variability across diverse spatial and temporal frequencies. The study of long- and short-term variability properties observed in the X-ray band provides insights into the inner workings of the central engine. In this work, we present timing and spectral analyses of the blazar 3C 273 using the X-ray observations from the $\textit{XMM-Newton}$ telescope covering the period from 2000 to 2020. The methods of timing analyses include estimation of fractional variability, long- and short-term flux distribution, rms-flux relation, and power spectral density analysis. The spectral analysis include estimating a model independent flux hardness ratio and fitting the observations with multiplicative and additive spectral models such as \textit{power-law}, \textit{log-parabola}, \textit{broken power-law}, and \textit{black body}. The \textit{black body} represents the thermal emission from the accretion disk, while the other models represent the possible energy distributions of the particles emitting synchrotron radiation in the jet. During the past two decades, the source flux changed by of a factor of three, with a considerable fractional variability of 27\%. However, the intraday variation was found to be moderate. Flux distributions of the individual observations were consistent with a normal or log-normal distribution, while the overall flux distribution including entire observations appear to be rather multi-modal and of a complex shape. The spectral analyses indicate that \textit{log-parabola} added with a \textit{black body} gives the best fit for most of the observations. The results indicate a complex scenario in which the variability can be attributed to the intricate interaction between the disk/corona system and the jet., Comment: 18 pages, 8 figures, ApJ accepted
Published: 2023

4. Method for calculation of the beta exponent from the Heitler-Matthews model of hadronic air showers

Author: Cheminant, Kevin Almeida, Gora, Dariusz, Borodai, Nataliia, Engel, Ralph, Pierog, Tanguy, Pekala, Jan, Roth, Markus, Stasielak, Jarosław, Unger, Michael, Veberic, Darko, and Wilczynski, Henryk
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The number of muons in an air shower is a strong indicator of the mass of the primary particle and increases with a small power of the cosmic ray mass by the $\beta$-exponent, $N_{\mu} \sim A^{(1-\beta)}$. This behaviour can be explained in terms of the Heitler-Matthews model of hadronic air showers. In this paper, we present a method for calculating $\beta$ from the Heitler-Matthews model. The method has been successfully verified with a series of simulated events observed by the Pierre Auger Observatory at $10^{19}$ eV. To follow real measurements of the mass composition at this energy, the generated sample consists of a certain fraction of events produced with p, He, N and Fe primary energies. Since hadronic interactions at the highest energies can differ from those observed at energies reached by terrestrial accelerators, we generate a mock data set with $\beta =0.92$ (the canonical value) and $\beta =0.96$ (a more exotic scenario). The method can be applied to measured events to determine the muon signal for each primary particle as well as the muon scaling factor and the $\beta$-exponent. Determining the $\beta$-exponent can effectively constrain the parameters that govern hadronic interactions and help solve the so-called muon problem, where hadronic interaction models predict too few muons relative to observed events. In this paper, we lay the foundation for the future analysis of measured data from the Pierre Auger Observatory with a simulation study., Comment: Proccedings of 38th International Cosmic Ray Conference (ICRC2023)
Published: 2023
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5. Profound optical flares from the relativistic jets of active galactic nuclei

Author: Bhatta, Gopal, Zola, Staszek, Drozdz, M., Reichart, Daniel, Haislip, Joshua, Kouprianov, Vladimir, Matsumoto, Katsura, Sonbas, Eda, Caton, D., Pajdosz-Śmierciak, Urszula, Simon, A., Provencal, J., Góra, Dariusz, and Stachowski, Grzegorz
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Intense outbursts in blazars are among the most extreme phenomena seen in extragalactic objects. Studying these events can offer important information about the energetic physical processes taking place within the innermost regions of blazars, which are beyond the resolution of current instruments. This work presents some of the largest and most rapid flares detected in the optical band from the sources 3C 279, OJ 49, S4 0954+658, Ton 599, and PG 1553+113, which are mostly TeV blazars. The source flux increased by nearly ten times within a few weeks, indicating the violent nature of these events. Such energetic events might originate from magnetohydrodynamical instabilities near the base of the jets, triggered by processes modulated by the magnetic field of the accretion disc. We explain the emergence of flares owing to the injection of high-energy particles by the shock wave passing along the relativistic jets. Alternatively, the flares may have also arisen due to geometrical effects related to the jets. We discuss both source-intrinsic and source-extrinsic scenarios as possible explanations for the observed large amplitude flux changes., Comment: 8 pages, 2 figures, 38th International Cosmic Ray Conference (ICRC2023) proceedings
Published: 2023

6. The muon deficit problem: a new method to calculate the muon rescaling factors and the Heitler-Matthews beta exponent

Author: Cheminant, Kevin Almeida, Góra, Dariusz, Borodai, Nataliia, Engel, Ralph, Pierog, Tanguy, Pękala, Jan, Roth, Markus, Stasielak, Jarosław, Unger, Michael, Veberič, Darko, and Wilczyński, Henryk
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Simulations of extensive air showers using current hadronic interaction models predict too small numbers of muons compared to events observed in the air-shower experiments, which is known as the muon-deficit problem. In this work, we present a new method to calculate the factor by which the muon signal obtained via Monte-Carlo simulations must be rescaled to match the data, as well as the beta exponent from the Heitler-Matthews model which governs the number of muons found in an extensive air shower as a function of the mass and the energy of the primary cosmic ray. This method uses the so-called z variable (difference between the total reconstructed and the simulated signals), which is connected to the muon signal and is roughly independent of the zenith angle, but depends on the mass of the primary cosmic ray. Using a mock dataset built from QGSJetII-04, we show that such a method allows us to reproduce the average muon signal from this dataset using Monte-Carlo events generated with the EPOS-LHC hadronic model, with accuracy better than 6%. As a consequence of the good recovery of the muon signal for each primary included in the analysis, also the beta exponent can be obtained with accuracy of less than 1% for the studied system. Detailed simulations show a dependence of the beta exponent on hadronic interaction properties, thus the determination of this parameter is important for understanding the muon deficit problem., Comment: 8 pages, 5 figures, 2 tables, accepted for publication in the proceedings of the 27th European Cosmic Ray Symposium
Published: 2023

7. Catching profound optical flares in blazars

Author: Bhatta, Gopal, Zola, Staszek, Drozdz, M., Reichart, Daniel, Haislip, Joshua, Kouprianov, Vladimir, Matsumoto, Katsura, Sonbas, Eda, Caton, D., Pajdosz-Śmierciak, Urszula, Simon, A., Provencal, J., Góra, Dariusz, and Stachowski, Grzegorz
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Flaring episodes in blazars represent one of the most violent processes observed in extra-galactic objects. Studies of such events shed light on the energetics of the physical processes occurring in the innermost regions of blazars, which cannot otherwise be resolved by any current instruments. In this work, we present some of the largest and most rapid flares captured in the optical band in the blazars 3C 279, OJ 49, S4 0954+658, TXS 1156+295 and PG 1553+113. The source flux was observed to increase by nearly ten times within a timescale of a few weeks. We applied several methods of time series analysis and symmetry analysis. Moreover, we also performed searches for periodicity in the light curves of 3C 279, OJ 49 and PG 1553+113 using the Lomb-Scargle method and found plausible indications of quasi-periodic oscillations (QPOs). In particular, the 33- and 22-day periods found in 3C 279, i.e. a 3:2 ratio, are intriguing. These violent events might originate from magnetohydrodynamical instabilities near the base of the jets, triggered by processes modulated by the magnetic field of the accretion disc. We present a qualitative treatment as the possible explanation for the observed large amplitude flux changes in both the source-intrinsic and source-extrinsic scenarios., Comment: 11 pages, 6 figures, MNRAS accepted
Published: 2023
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8. Calculation of rescaling factors and nuclear multiplication of muons in extensive air showers

Author: Cheminant, Kevin Almeida, Góra, Dariusz, Borodai, Nataliia, Engel, Ralph, Pierog, Tanguy, Pȩkala, Jan, Roth, Markus, Unger, Michael, Veberič, Darko, and Wilczyński, Henryk
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Recent results obtained from leading cosmic ray experiments indicate that simulations using LHC-tuned hadronic interaction models underestimate the number of muons in extensive air showers compared to experimental data. This is the so-called muon deficit problem. Determination of the muon component in the air shower is crucial for inferring the mass of the primary particle, which is a key ingredient in the efforts to pinpoint the sources of ultra-high energy cosmic rays.In this paper, we present a new method to derive the muon signal in detectors, which uses the difference between the total reconstructed (data) and simulated signals is roughly independent of the zenith angle, but depends on the mass of the primary cosmic ray. Such a method offers an opportunity not only to test/calibrate the hadronic interaction models, but also to derive the $\beta$ exponent, which describes an increase of the number of muons in a shower as a function of the energy and mass of the primary cosmic ray. Detailed simulations show a dependence of the $\beta$ exponent on hadronic interaction properties, thus the determination of this parameter is important for understanding the muon deficit problem. We validate the method by using Monte Carlo simulations for the EPOS-LHC and QGSJetII-04 hadronic interaction models, and showing that this method allows us to recover the ratio of the muon signal between EPOS-LHC and QGSJetII-04 and the average $\beta$ exponent for the studied system, within less than a few percent. This is a consequence of the good recovery of the muon signal for each primary included in the analysis., Comment: This work corresponds to the presentation at the ICNFP 2022 at Kolymbari, Crete, in September 2022. The proceedings will be published in Physica Scripta. arXiv admin note: text overlap with arXiv:2108.07527
Published: 2022
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9. Muon measurements at the Pierre Auger Observatory

Author: Góra, Dariusz
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Pierre Auger Observatory is the world's largest detector for observation of ultra-high-energy cosmic rays (UHECRs) (above the energy of $10^{17}$ eV). It consists of a Fluorescence Detector (FD) and an array of particle detectors known as the Surface Detector (SD). Observations of extensive air showers by the Observatory can be used to probe hadronic interactions at high energy, in a kinematic and energy region inaccessible to experiments at man-made accelerators and to measure the muon component of the shower. Air showers induced by different primaries have different muon contents. With increasing mass of the primary cosmic ray particle, it is expected that the muon content in the corresponding air showers should also increase. Recent results obtained from the Pierre Auger Observatory and other experiments indicate that all the shower simulations underestimate the number of muons in the showers compared to the data. This is the so-called muon deficit. In this paper we briefly review the muon measurements, and present in more detail recent results on fluctuations in the muon number. These results provide new insights into the origin of the muon deficit in air shower simulations and constrain the models of hadronic interactions at ultrahigh energies. With the current design of the surface detectors it is also difficult to reliably separate the contributions of muons to the SD signal from the contributions of photons, electrons, and positrons. Therefore, we also present a new method to extract the muon component of the signal time traces recorded by each SD station using recurrent neural networks. The combination of such algorithms, with the future data collected by the upgraded Pierre Auger Observatory, will be a major step forward, as we are likely to achieve an unprecedented resolution in mass estimation on an event-by-event basis., Comment: Proceedings of the ISMD-2022 conference, accepted for publication SciPost Proceedings
Published: 2022

10. Shore Shadow Effect in Baikal

Author: Bhatta, Apoorva, Malecki, Paweł, and Góra, Dariusz
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The measurement of the individual charged particles especially muons in an extended air shower (EAS) resulting from primary cosmic rays provides important distinguishing parameters to identify the chemical composition of the cosmic primary particles. For Neutrino Telescope experiments like Baikal-GVD, the estimation of underwater muon flux is of importance to study atmospheric muons. In this paper, a GEANT4-based simulation is presented to estimate the atmospheric muon flux underwater taking Baikal-GVD as an example. The location of the Baikal-GVD experiment at Lake Baikal provides a unique opportunity to study the passage of muons through its northern shore and the water. The muons arriving from the north direction will lose more energy as compared to those arriving from the south. An approximation for the northern shore is also simulated in the GEANT4 geometry and the results of the simulation are compared with the measurements from the NT-96 detector. The results of the simulations are consistent with the shore shadow observed in the measurements in the NT-96. This approach can also be used to propagate the muons from generators like CORSIKA through long distances in matter like water, ice, earth, etc. for simulations in such experiments.
Published: 2022
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11. Simulations of Cosmic Ray Ensembles originated nearby the Sun

Author: Alvarez-Castillo, David E., Sushchov, Oleksandr, Homola, Piotr, Beznosko, Dmitriy, Budnev, Nikolai, Góra, Dariusz, Gupta, Alok C., Hnatyk, Bohdan, Kasztelan, Marcin, Kovacs, Peter, Łozowski, Bartosz, Medvedev, Mikhail V., Miszczyk, Justyna, Mozgova, Alona, Nazari, Vahab, Niedźwiecki, Michał, Pawlik, Maciej, Rosas, Matías, Rzecki, Krzysztof, Smelcerz, Katarzyna, Smolek, Karel, Stasielak, Jarosław, Stuglik, Sławomir, Svanidze, Manana, Tursunov, Arman, Verbetsky, Yuri, Wibig, Tadeusz, Zamora-Saa, Jilberto, Poncyljusz, Bożena, Mędrala, Justyna, Opiła, Gabriela, Bibrzyck, Łukasz, and Piekarczyk, Marcin
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Cosmic Ray Ensembles (CRE) are yet not observed groups of cosmic rays with a common primary interaction vertex or the same parent particle. One of the processes capable of initiating identifiable CRE is an interaction of an ultra-high energy (UHE) photon with the solar magnetic field which results in an electron pair production and the subsequent synchrotron radiation. The resultant electromagnetic cascade forms a very characteristic line-like front of a very small width ($\sim$ meters), stretching from tens of thousands to even many millions of kilometers. In this contribution we present the results of applying a toy model to simulate detections of such CRE at the ground level with an array of ideal detectors of different dimensions. The adopted approach allows us to assess the CRE detection feasibility for a specific configuration of a detector array. The process of initiation and propagation of an electromagnetic cascade originated from an UHE photon passing near the Sun, as well as the resultant particle distribution on ground, were simulated using the CORSIKA program with the PRESHOWER option, both modified accordingly. The studied scenario results in photons forming a cascade that extends even over tens of millions of kilometers when it arrives at the top of the Earth's atmosphere, and the photon energies span practically the whole cosmic ray energy spectrum. The topology of the signal consists of very extended CRE shapes, and the characteristic, very much elongated disk-shape of the particle distribution on ground illustrates the potential for identification of CRE of this type., Comment: 8 pages, 3 figures. Proceedings of the International Cosmic Rays Conference 2021, 12-23 July, Berlin, Germany
Published: 2021
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12. Particle physics in cosmic rays

Author: Gora, Dariusz
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Pierre Auger Observatory is the world's largest detector of ultra--high energy cosmic rays (UHECRs). It uses an array of fluorescence telescopes and particle detectors at the ground to obtain detailed measurements of the energy spectrum, mass composition and arrival directions of primary cosmic rays (above the energy of $10^{17}$ eV) with accuracy not attainable until now.Observations of extensive air showers performed by the Pierre Auger Observatory can also be used to probe hadronic interactions at high energy, in a kinematic and energy region not accessible by man-made accelerators. Indeed, exploiting Auger data, we reach center-of-mass energies up to 400 TeV, i.e. more than 30 times of those attainable at the LHC, and explore interactions in the very forward region of phase space on targets of atomic mass of 14. In addition, a precise measurement of the muon component of air showers at the ground is more sensitive to the details of the hadronic interactions along many steps of the cascade development, such as the multiplicity of the secondaries and the fraction of electromagnetic component with respect to the total signal. On the other hand, the intrinsic muon fluctuations mostly depend on the first interaction. In this paper we overview the new Auger studies exploring the connection between the dynamics of the air shower and the multi-particle production, and how this knowledge can be translated into constraints of the high energy hadronic models as well as direct measurements, complementary to, and beyond the reach of, accelerator experiments., Comment: Proceedings of 9th International Conference on New Frontiers in Physics (ICNFP 2020), paper submitted to IJMPA
Published: 2021
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13. Machine learning aided noise filtration and signal classification for CREDO experiment

Author: Bibrzycki, Łukasz, Alvarez-Castillo, David, Bar, Olaf, Gora, Dariusz, Homola, Piotr, Kovács, Péter, Niedźwiecki, Michał, Piekarczyk, Marcin, Rzecki, Krzysztof, Stasielak, Jaroslaw, Stuglik, Sławomir, Sushchov, Oleksandr, and Tursunov, Arman
Subjects: Physics - Instrumentation and Detectors, Electrical Engineering and Systems Science - Signal Processing
Abstract: The wealth of smartphone data collected by the Cosmic Ray Extremely Distributed Observatory(CREDO) greatly surpasses the capabilities of manual analysis. So, efficient means of rejectingthe non-cosmic-ray noise and identification of signals attributable to extensive air showers arenecessary. To address these problems we discuss a Convolutional Neural Network-based method ofartefact rejection and complementary method of particle identification based on common statisticalclassifiers as well as their ensemble extensions. These approaches are based on supervised learning,so we need to provide a representative subset of the CREDO dataset for training and validation.According to this approach over 2300 images were chosen and manually labeled by 5 judges.The images were split into spot, track, worm (collectively named signals) and artefact classes.Then the preprocessing consisting of luminance summation of RGB channels (grayscaling) andbackground removal by adaptive thresholding was performed. For purposes of artefact rejectionthe binary CNN-based classifier was proposed which is able to distinguish between artefacts andsignals. The classifier was fed with input data in the form of Daubechies wavelet transformedimages. In the case of cosmic ray signal classification, the well-known feature-based classifierswere considered. As feature descriptors, we used Zernike moments with additional feature relatedto total image luminance. For the problem of artefact rejection, we obtained an accuracy of 99%. For the 4-class signal classification, the best performing classifiers achieved a recognition rate of 88%., Comment: 9 pages,4 figurek, ICRC 2021 contribution
Published: 2021

14. Muon number rescaling in simulations of air showers

Author: Góra, Dariusz, Borodai, Nataliia, Engel, Ralph, Pierog, Tanguy, Pękala, Jan, Roth, Markus, Stasielak, Jaroslaw, Unger, Michael, Veberic, Darko, and Wilczyński, Henryk
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, High Energy Physics - Experiment
Abstract: The number of muons in extensive air showers predicted using LHC-tuned hadronic interaction models, such as EPOS-LHC and QGSJetII-04, is smaller than observed in showers recorded by leading cosmic ray experiments. In this paper, we present a new method to derive muon rescaling factors by analyzing reconstructions of simulated showers. The z-variable used (difference of initially simulated and reconstructed total signal in detectors) is connected to the muon signal and is roughly independent of the zenith angle but depends on the mass of primary cosmic ray. The performance of the method is tested using Monte Carlo shower simulations for the hybrid detector of the Pierre Auger Observatory. Having an individual z-value from each simulated hybrid event, the corresponding signal at 1000 m from the shower axis, and using a parametrization of the muon fraction in simulated showers, we can calculate the multiplicative rescaling parameters of the muon signals in the ground detector even for an individual event. We can also study its dependence as a function of zenith angle and the mass of primary cosmic ray. This gives a possibility not only to test/calibrate the hadronic interaction models, but also to derive the $\beta$-exponent, describing an increase of the number of muons as a function of primary energy and mass of the cosmic ray. Detailed simulations show dependence of the $\beta$-exponent on hadronic interaction properties, thus the determination of this parameter is important for understanding the muon deficit problem., Comment: Proceedings of 37th International Cosmic Ray Conference (ICRC 2021), July 12th -- 23rd, 2021
Published: 2021

15. Cosmic Ray Extremely Distributed Observatory

Author: Homola, Piotr, Beznosko, Dmitriy, Bhatta, Gopal, Bibrzycki, Lukasz, Borczynska, Michalina, Bratek, Lukasz, Budnev, Nikolai, Burakowski, Dariusz, Alvarez-Castillo, David E., Cheminant, Kevin Almeida, Cwikla, Aleksander, Dam-o, Punsiri, Dhital, Niraj, Duffy, Alan R., Glownia, Piotr, Gorzkiewicz, Krzysztof, Gora, Dariusz, Gupta, Alok C., Hlavkova, Zuzana, Homola, Martin, Jalocha, Joanna, Kaminski, Robert, Karbowiak, Michal, Kasztelan, Marcin, Kierepko, Renata, Knap, Marek, Kovacs, Peter, Kulinski, Szymon, Lozowski, Bartosz, Magrys, Marek, Medvedev, Mikhail V., Medrala, Justyna, Mietelski, Jerzy W., Miszczyk, Justyna, Mozgova, Alona, Napolitano, Antonio, Nazari, Vahab, Ng, Y. Jack, Niedzwiecki, Michal, Oancea, Cristina, Ogan, Boguslaw, Opila, Gabriela, Oziomek, Krzysztof, Pawlik, Maciej, Piekarczyk, Marcin, Poncyliusz, Bozena, Pryga, Jerzy, Rosas, Matias, Rzecki, Krzysztof, Zamora-Saa, Jilberto, Smelcerz, Katarzyna, Smolek, Karel, Stanek, Weronika, Stasielak, Jaroslaw, Stuglik, Slawomir, Sulma, Jolanta, Sushchov, Oleksandr, Svanidze, Manana, Tam, Kyle, Tursunov, Arman, Vaquero, Jose M., Wibig, Tadeusz, and Wozniak, Krzysztof W.
Subjects: Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Cosmic Ray Extremely Distributed Observatory (CREDO) is a newly formed, global collaboration dedicated to observing and studying cosmic rays (CR) and cosmic ray ensembles (CRE): groups of a minimum of two CR with a common primary interaction vertex or the same parent particle. The CREDO program embraces testing known CR and CRE scenarios, and preparing to observe unexpected physics, it is also suitable for multi-messenger and multi-mission applications. Perfectly matched to CREDO capabilities, CRE could be formed both within classical models (e.g. as products of photon-photon interactions), and exotic scenarios (e.g. as results of decay of Super Heavy Dark Matter particles). Their fronts might be significantly extended in space and time, and they might include cosmic rays of energies spanning the whole cosmic ray energy spectrum, with a footprint composed of at least two extensive air showers with correlated arrival directions and arrival times. Since CRE are mostly expected to be spread over large areas and, because of the expected wide energy range of the contributing particles, CRE detection might only be feasible when using available cosmic ray infrastructure collectively, i.e. as a globally extended network of detectors. Thus, with this review article, the CREDO Collaboration invites the astroparticle physics community to actively join or to contribute to the research dedicated to CRE, and in particular to share any cosmic ray data useful for the specific CRE detection strategies., Comment: 59 pages, 23 figures
Published: 2020
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16. CREDO project

Author: Kamiński, Robert, Wibig, Tadeusz, Castillo, David Alvarez, Cheminant, Kevin Almeida, Ćwikła, Aleksander, Duffy, Alan R., Góra, Dariusz, Homola, Piotr, Jagoda, Paweł, Kasztelan, Marcin, Knap, Marek, Kopański, Konrad, Kovacs, Peter, Krupiński, Michał, Magryś, Marek, Nazari, Vahabeddin, Niedźwiecki, Michał, Noga, Wojciech, Rosas, Matias, Ryszkowski, Szymon, Smelcerz, Katarzyna, Smolek, Karel, Stasielak, Jarosław, Stuglik, Sławomir, Sułek, Mateusz, Sushchov, Oleksandr, and Woźniak, Krzysztof
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Cosmic-Ray Extremely Distributed Observatory (CREDO) is a project created a few years ago in the Institute of Nuclear Physics PAS in Krak\'ow and dedicated is to global studies of extremely extended cosmic-ray phenomena. The main reason for creating such a project was that the cosmic-ray ensembles (CRE) are beyond the capabilities of existing detectors and observatories. Until now, cosmic ray studies, even in major observatories, have been limited to the recording and analysis of individual air showers therefore ensembles of cosmic-rays, which may spread over a significant fraction of the Earth were neither recorded nor analyzed. In this paper the status and perspectives of the CREDO project are presented., Comment: 8 pages, 5 figures
Published: 2020
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17. Search for ultra-high energy photons through preshower effect with gamma-ray telescopes: Study of CTA-North efficiency

Author: Cheminant, Kévin Almeida, Góra, Dariusz, Castillo, David E. Alvarez, Ćwikła, Aleksander, Dhital, Niraj, Duffy, Alan R., Homola, Piotr, Kopański, Konrad, Kasztelan, Marcin, Kovacs, Peter, Marek, Marta, Mozgova, Alona, Nazari, Vahab, Niedzźwiecki, Michał, Ostrogórski, Dominik, Smolek, Karel, Stasielak, Jarosław, Sushchov, Oleksandr, and Zamora-Saa, Jilberto
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: We study the feasibility of detecting preshower initiated by ultra-high energy photons using Monte-Carlo simulations of nearly horizontal air showers for the example of the La Palma site of the Cherenkov Telescope Array. We investigate the efficiency of multivariate analysis in correctly identifying preshower events initiated by 40 EeV photons and cosmic-ray dominated background simulated in the energy range 10 TeV -- 10 EeV. The effective areas for such kind of events are also investigated and event rate predictions related to different ultra-high energy photons production models are presented. While the expected number of preshowers from diffuse emission of UHE photon for 30 hours of observation is estimated around $3.3\times10^{-5}$ based on the upper limits put by the Pierre Auger Observatory, this value is at the level of $2.7\times10^{-4}$ ($5.7\times 10^{-5}$) when considering the upper limits of the Pierre Auger Observatory (Telescope Array) on UHE photon point sources. However, UHE photon emission may undergo possible "boosting" due to gamma-ray burst, increasing the expected number of preshower events up to 0.17 and yielding a minimum required flux of $\sim 0.2$ $\mathrm{km^{-2}yr^{-1}}$ to obtain one preshower event, which is about a factor 10 higher than upper limits put by the Pierre Auger Observatory and Telescope Array (0.034 and 0.019 $\mathrm{km^{-2}yr^{-1}}$, respectively)., Comment: 16 pages, 16 figures, 4 tables
Published: 2020
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18. Recognition and classification of the cosmic-ray events in images captured by CMOS/CCD cameras

Author: Niedzwiecki, Michal, Rzecki, Krzysztof, Marek, Marta, Homola, Piotr, Smelcerz, Katarzyna, Castillo, David Alvarez, Smolek, Karel, Hnatyk, Bohdan, Zamora-Saa, Jilberto, Mozgova, Alona, Nazaric, Vahab, Gora, Dariusz, Kopanski, Konrad, Wibig, Tadeusz, Duffy, Alan R., Stasielak, Jaroslaw, Zimboras, Zoltan, and Kasztelan, Marcin
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Muons and other ionizing radiation produced by cosmic rays and radiative decays affect CMOS/CCD sensor. When particles colliding with sensors atoms cause specific kind of noise on images recorded by cameras. We present a concept and preliminary implementation of method for recognizing those events and algorithms for image processing and their classification by machine learning. Our method consists of analyzing the shape of traces present in images recorded by a camera sensor and metadata related to an image like camera model, GPS location of camera, vertical and horizontal orientation of a camera sensor, timestamp of image acquisition, and other events recognized near-by sensors. The so created feature vectors are classified as either a muon-like event, an electron-like event or the other event, possibly noise. For muon-like events our method estimates azimuth of a muon track. Source of the data is database of CREDO (Cosmic-Ray Extremely Distributed Observatory) project and ESO (European Southern Observatory) archives. The telescope dark frames from ESO are analysed. CREDO project collected so far over 2 millions images of events from many kinds of cameralike: smartphones camera, laptop webcams and Internet of Things cameras localised around the globe., Comment: 36th International Cosmic Ray Conference (ICRC2019)
Published: 2019

19. MAGIC as a high-energy $\nu_\tau$ detector: performance study to follow-up IceCube transient events

Author: Mallamaci, Manuela, Gora, Dariusz, and Bernardini, Elisa
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: MAGIC is a system of two Imaging Atmospheric Cherenkov Telescopes located on the Canary Island of La Palma and dedicated to the study of very high energy gamma rays above 30 GeV. MAGIC has recently demonstrated its capability as a neutrino detector, by exploiting the Earth-skimming technique. The neutrino-event selection has been studied by pointing the telescopes towards the sea a few degrees below the horizon, with no pre-defined source direction. An upper limit to the $\nu_\tau$ flux was set. In this work, a follow-up strategy of given source directions is presented. This new approach is characterised by pointing to targets passing through the sea window observable with MAGIC and for which a trigger from dedicated neutrino observatories is issued with large significance. Above a few tens of PeV, the acceptance of MAGIC to $\nu_\tau$ is considerably large and compelling results can be obtained for transient events of short duration. The performance of this new method is tested on a sample of data collected by pointing MAGIC for a few days from March to May 2016 towards the direction of a multi-PeV neutrino that IceCube detected on June 11th 2014 (reconstructed direction (J2000.0) RA: 110.34$^\circ$ and Dec.: 11.48$^\circ$). A selection cut is studied in order to discriminate $\tau$-lepton-induced air showers from the background of very inclined cosmic-ray-induced air showers. An upper limit on the neutrino flux from the above given neutrino direction is presented., Comment: Proceedings of the ICRC 2019
Published: 2019

20. A communication solution for portable detectors of the Cosmic Ray Extremely Distributed Observatory

Author: Smelcerz, Katarzyna, Kopański, Konrad, Noga, Wojciech, Sułek, Mateusz, Cheminant, Kevin Almeida, Dhital, Niraj, Gora, Dariusz, Homola, Piotr, Sushchov, Oleksandr, Beznosko, Dmitriy, Zamora-Saa, Jilberto, Duffy, Alan R., Kasztelan, Marcin, Kovacs, Peter, Nazari, Vahab, Niedźwiecki, Michał, Rzecki, Krzysztof, Smolek, Karel, Stasielak, Jaroslaw, and Zimborás, Zoltán
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The search for Cosmic-Ray Ensembles (CRE), groups of correlated cosmic rays that might be distributed over very large areas, even of the size of the planet, requires a globally spread and dense network of detectors, as proposed by the Cosmic-Ray Extremely Distributed Observatory (CREDO) Collaboration. This proposal motivates an effort towards exploring the potential of using even very much diversified detection technologies within one system, with detection units located even in hard-to-reach places, where, nevertheless, the sensors could work independently - without human intervention. For these reasons we have developed a dedicated communication solution enabling the connection of many different types of detectors, in a range of environments. The proposed data transmission system uses radio waves as an information carrier on the 169MHz frequency band in a contrast to the typical commercially used frequencies in a IoT systems (868MHz). The connectivity within the system is based on the star topology, which ensures the least energy consumption. The solution is now being prepared to being implemented using the prototype detection system based on the CosmicWatch open hardware design: a portable, pocket size, and economy particle detector using the scintillation technique. Our prototype detector is equipped with a dedicated software that integrates it with the already operational CREDO server system., Comment: ICRC2019
Published: 2019

21. Public engagement as a scientific tool to implement multi-messenger strategies with the Cosmic-Ray Extremely Distributed Observatory

Author: Homola, Piotr, Castillo, David E. Alvarez, Góra, Dariusz, Duffy, Alan R., Hnatyk, Bohdan, Jagoda, Paweł, Kasztelan, Marcin, Kopański, Konrad, Kovacs, Peter, Krupiński, Michał, Mozgova, Alona, Nazari, Vahab, Niedźwiecki, Michal, Noga, Wojciech, Ostrogórski, Dominik, Smolek, Karel, Stasielak, Jaroslaw, Sushchov, Oleksandr, Wibig, Tadeusz, Woźniak, Krzysztof W., and Zamora-Saa, Jilberto
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Cosmic-Ray Extremely Distributed Observatory (CREDO) uses the hunt for particle cascades from deep space as a vehicle for a unique "bottom-up" approach to scientific research. By engaging the non-specialist public of all ages as "citizen scientists" we create opportunities for lifelong learning for individuals as well as for cooperation and the sharing of common educational tools amongst institutions. The discoveries of these citizen scientists will feed directly into a pioneering new area of scientific research oriented on Cosmic Ray Ensembles (CRE). The detection (or non-detection) of such particle groups promises to open up a new method for exploring our universe, and a new channel on the multi-messenger stage, oriented on both astro- and geo-investigations. The opportunities this would create for cross-disciplinary research are significant and beneficial for individuals, networks of institutions and the global communities of both professional scientists and science enthusiasts., Comment: 4 pages, 3 figures, Proceedings The New Era of Multi-Messenger Astrophysics - Asterics2019, 25 - 29 March, 2019 Groningen, The Netherlands
Published: 2019

22. Search for ultra-high energy photons: observing the preshower effect with gamma-ray telescopes

Author: Cheminant, Kevin Almeida, Gora, Dariusz, Castillo, David E. Alvarez, Dhital, Niraj, Homola, Piotr, Jagoda, Pawel, Kopanski, Konrad, Kasztelan, Marcin, Kovacs, Peter, Marek, Marta, Nazari, Vahab, Niedzwiecki, Michal, Smelcerz, Katarzyna, Smolek, Karel, Stasielak, Jaroslaw, Sushchov, Oleksandr, Rzecki, Krzysztof, Wibig, Tadeusz, and Zamora-Saa, Jilberto
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: Ultra-high energy photons constitute one of the most important pieces of the astroparticle physics problems. Their observation may provide new insight on several phenomena such as supermassive particle annihilation or the GZK effect. Because of the absence of any significant photon identification by a leading experiments such as the Pierre Auger Observatory, we consider a screening phenomenon called preshower effect which could efficiently affect ultra-high energy photon propagation. This effect is a consequence of photon interactions with the geomagnetic field and results in large electromagnetic cascade of particles several thousands kilometers above the atmosphere. This collection of particles, called cosmic-ray ensembles (CRE), may reach the atmosphere and produce the well-known air showers. In this paper we propose to use gamma-ray telescopes to look for air showers induced by CRE. Possible sources of ultra-high energy photons include the GZK effect and Super Heavy Dark Matter particles. Simulations involving the preshower effect and detectors response are performed and properties of these peculiar air showers are investigated. The use of boosted decision trees to obtain the best cosmic-ray ensemble/hadron separation, the aperture and event rate predictions for a few models of photon production are also presented., Comment: 8 pages, 3 figures, International Cosmic Ray Conference 2019
Published: 2019

23. Cosmic ray ensembles from ultra-high energy photons propagating in the galactic and intergalactic space

Author: Dhital, Niraj, Sushchov, Oleksandr, Pekala, Jan, Cheminant, Kevin Almeida, Góra, Dariusz, Homola, Piotr, Duffy, Alan R., Jagoda, Paweł, Kaminski, Robert, Kasztelan, Marcin, Kovacs, Peter, Nazari, Vahab, Niedźwiecki, Michał, Smelcerz, Katarzyna, Smolek, Karel, Rzecki, Krzysztof, Zamora-Saa, Jilberto, and Zimborás, Zoltán
Subjects: Astrophysics - High Energy Astrophysical Phenomena
Abstract: Propagation of ultra-high energy photons in the galactic and intergalactic space gives rise to cascades comprising thousands of photons. Using Monte Carlo simulations, we investigate the development of such cascades in the solar magnetosphere, and find that the photons in the cascades are distributed over hundreds of kilometers as they arrive at the top of the Earth's atmosphere. We also perform similar study for cascades starting as far as 10 Mpc away from us using relevant magnetic field models. A few photons correlated in time are expected to arrive at the Earth from the latter type of cascade. We present our simulation results and discuss the prospects for detection of these cascades with the Cosmic-Ray Extremely Distributed Observatory.
Published: 2019

24. Cosmic Ray Extremely Distributed Observatory: Status and perspectives of a global cosmic ray detection framework

Author: Gora, Dariusz, Cheminant, Kevin Almeida, Castillo, David E. Alvarez, Beznosko, Dmitriy, Dhital, Niraj, Duffy, Alan R., Homola, Piotr, Kopanski, Konrad, Kovacs, Peter, Marek, Marta, Mozgova, Alona, Nazari, Vahab, Niedzwiecki, Michal, Noga, Wojciech, Smelcerz, Katarzyna, Smolek, Karel, Stasielak, Jaroslaw, Sushchov, Oleksandr, Ostrogorski, Dominik, Rzecki, Krzysztof, Wozniak, Krzysztof W., and Zamora-Saa, Jilberto
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: The Cosmic-Ray Extremely Distributed Observatory (CREDO) is a project dedicated to global studies of extremely extended cosmic-ray phenomena, the cosmic-ray ensembles (CRE), beyond the capabilities of existing detectors and observatories. Up to date cosmic-ray research has been focused on detecting single air showers, while the search for ensembles of cosmic-rays, which may spread over a significant fraction of the Earth, is a scientific terra incognita. The key idea of CREDO is to combine existing cosmic-ray detectors (large professional arrays, educational instruments, individual detectors, such as smartphones, etc.) into a worldwide network, thus enabling a global analysis. The second goal of CREDO involves a large number of participants (citizen science!), assuring the geographical spread of the detectors and managing manpower necessary to deal with vast amount of data to search for evidence for cosmic-ray ensembles. In this paper the status and perspectives of the project are presented., Comment: Proceedings of 36th International Cosmic Ray Conference - ICRC2019 - July 24th - August 1st, 2019 Madison, WI, U.S.A
Published: 2019

25. Detection of Cosmic-Ray Ensembles with CREDO

Author: Woźniak, Krzysztof W., Almeida-Cheminant, Kevin, Bratek, Łukasz, Castillo, David Edwin Alvarez, Dhital, Niraj, Duffy, Alan R., Góra, Dariusz, Hnatyk, Bohdan, Homola, Piotr, Jagoda, Paweł, Jałocha-Bratek, Joanna, Kasztelan, Marcin, Lemański, Dawid, Kovács, Peter, Nazari, Vahab, Niedźwiecki, Michał, Smelcerz, Katarzyna, Smolek, Karel, Stasielak, Jarosław, Stuglik, Sławomir, Sushchov, Oleksandr, and Zamora-Saá, Jilberto
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: One of the main objectives of cosmic-ray studies are precise measurements of energy and chemical composition of particles with extreme energies. Large and sophisticated detectors are used to find events seen as showers starting in the Earth's atmosphere with recorded energies larger than 100 EeV. However, a Cosmic-Ray Ensemble (CRE) developing before reaching the Earth as a bunch of correlated particles may spread over larger areas and requires an extended set of detectors to be discovered. The Cosmic-Ray Extremely Distributed Observatory (CREDO) is a solution to find such phenomena. Even simple detectors measuring the particle arrival time only are useful in this approach, as they are sufficient both to provide candidate CRE events and to determine the direction from which they are arriving., Comment: 20th International Symposium on Very High Energy Cosmic Ray Interactions, May 21-15, 2018, Nagoya, Japan
Published: 2018
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26. The Pierre Auger Observatory: review of latest results and perspectives

Author: Gora, Dariusz
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: The Pierre Auger Observatory is the world's largest operating detection system for the observation of ultra high energy cosmic rays (UHECRs). The detector allows detailed measurements of their energy spectrum, mass composition and arrival directions of primary cosmic rays in the energy range above $10^{17}$ eV. The data collected at the Observatory over the last decade show the suppression of the cosmic ray flux at energies above $4\times10^{19}$ eV. However, it is still unclear if this suppression is caused by the propagation of cosmic rays or rather by energy limitation of their sources. The other puzzle is the origin of UHECRs. Some clues can be drawn from studying the distribution of their arrival directions. The recently observed dipole anisotropy has an orientation which indicates an extragalactic origin of UHECRs. The Auger surface detector array is also sensitive to showers due to ultra high energy neutrinos of all flavours and photons, and recent neutrino and photon limits provided by the Observatory can constrain models of the cosmogenic neutrino production and exotic scenarios of the UHECRs origin, such as the decays of super heavy particles. In this paper the recent results on measurements of the energy spectrum, mass composition and arrival directions of cosmic rays, and future prospects are presented., Comment: This article belongs to the Special Issue Selected Papers from the 7th International Conference on New Frontiers in Physics (ICNFP 2018)
Published: 2018
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27. Detection of tau neutrinos by Imaging Air Cherenkov Telescopes

Author: Gora, Dariusz and Bernardini, Elisa
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: This paper investigates the potential to detect tau neutrinos in the energy range of 1-1000 PeV searching for very inclined showers with imaging Cherenkov telescopes. A neutrino induced tau lepton escaping from the Earth may decay and initiate an air shower which can be detected by a fluorescence or Cherenkov telescope. We present here a study of the detection potential of Earth-skimming neutrinos taking into account neutrino interactions in the Earth crust, local matter distributions at various detector sites, the development of tau-induced showers in air and the detection of Cherenkov photons with IACTs. We analyzed simulated shower images on the camera focal plane and implemented generic reconstruction chains based on Hillas parameters. We find that present IACTs can distinguish air showers induced by tau neutrinos from the background of hadronic showers in the PeV-EeV energy range. We present the neutrino trigger efficiency obtained for a few configurations being considered for the next-generation Cherenkov telescopes, i.e. the Cherenkov Telescope Array. Finally, for a few representative neutrino spectra expected from astrophysical sources, we compare the expected event rates at running IACTs to what is expected for the dedicated IceCube neutrino telescope., Comment: Paper accepted for publication in Astroparticle Physics
Published: 2016
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28. Detection of tau neutrinos by Imaging Air Cherenkov Telescopes

Author: Gora, Dariusz and Bernardini, Elisa
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics
Abstract: This paper investigates the potential to detect tau neutrinos in the energy range of 1-1000 PeV searching for very inclined showers with imaging Cherenkov telescopes. A neutrino induced tau lepton escaping from the Earth may decay and initiate an air shower which can be detected by a fluorescence or Cherenkov telescope. We present here a study of the detection potential of Earth-skimming neutrinos taking into account neutrino interactions in the Earth crust, local matter distributions at various detector sites, the development of tau-induced showers in air and the detection of Cherenkov photons with IACTs. We analysed simulated shower images on the camera focal plane and implemented generic reconstruction chains based on Hillas parameters. We find that present IACTs can distinguish air showers induced by tau neutrinos from the background of hadronic showers in the PeV-EeV energy range. We present the neutrino trigger efficiency obtained for a few configurations being considered for the next-generation Cherenkov telescopes, i.e. the Cherenkov Telescope Array. Finally, for a few representative neutrino spectra expected from astrophysical sources, we compare the expected event rates at running IACTs to what expected for the dedicated IceCube neutrino telescope., Comment: Proceedings of the 34th International Cosmic Ray Conference, 30 July- 6 August, 2015, The Hague, The Netherlands
Published: 2015

29. Search for ultra-high energy photons through preshower effect with gamma-ray telescopes: Study of CTA-North efficiency

Author: Almeida Cheminant, Kévin, Góra, Dariusz, Alvarez Castillo, David E., Ćwikła, Aleksander, Dhital, Niraj, Duffy, Alan R., Homola, Piotr, Kopański, Konrad, Kasztelan, Marcin, Kovacs, Peter, Marek, Marta, Mozgova, Alona, Nazari, Vahab, Niedźwiecki, Michał, Ostrogórski, Dominik, Smolek, Karel, Stasielak, Jarosław, Sushchov, Oleksandr, and Zamora-Saa, Jilberto
Published: 2020
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30. Tau neutrino search with Cherenkov telescopes

Author: Gora, Dariusz and Bernardini, Elisa
Subjects: Astrophysics - Instrumentation and Methods for Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract: Cherenkov telescopes could have the capability of detecting high energy tau neutrinos by searching for very inclined showers. If a tau lepton, produced by a tau neutrino, escapes from the Earth crust, it will decay and initiate an air shower which can be detected by a fluorescence/Cherenkov telescope. Here we present a detailed Monte Carlo simulation of event rates induced by tau neutrinos in the energy range from 1 PeV to 1 EeV. Topographic conditions are taken into account for a set of example locations. As expected, we find a neutrino sensitivity which depends on the shape of the energy spectrum from astrophysical sources. We compare our findings with the sensitivity of the dedicated IceCube neutrino telescope under different conditions. We also find that a difference of several factors can be observed depending on the topographic conditions of the sites sampled., Comment: Proceedings of 33nd International Cosmic Ray Conference - 2013 - Rio de Janeiro, Brazil
Published: 2013

31. Using cosmic neutrinos to search for non-perturbative physics at the Pierre Auger Observatory

Author: Anchordoqui, Luis A., Goldberg, Haim, Gora, Dariusz, Paul, Thomas, Roth, Markus, Sarkar, Subir, and Winders, Lisa Lee
Subjects: High Energy Physics - Phenomenology
Abstract: The Pierre Auger (cosmic ray) Observatory provides a laboratory for studying fundamental physics at energies far beyond those available at colliders. The Observatory is sensitive not only to hadrons and photons, but can in principle detect ultrahigh energy neutrinos in the cosmic radiation. Interestingly, it may be possible to uncover new physics by analyzing characteristics of the neutrino flux at the Earth. By comparing the rate for quasi-horizontal, deeply penetrating air showers triggered by all types of neutrinos, with the rate for slightly upgoing showers generated by Earth-skimming tau neutrinos, we determine the ratio of events which would need to be detected in order to signal the existence of new non-perturbative interactions beyond the TeV-scale in which the final state energy is dominated by the hadronic component. We use detailed Monte Carlo simulations to calculate the effects of interactions in the Earth and in the atmosphere. We find that observation of 1 Earth-skimming and 10 quasi-horizontal events would exclude the standard model at the 99% confidence level. If new non-perturbative physics exists, a decade or so would be required to find it in the most optimistic case of a neutrino flux at the Waxman-Bahcall level and a neutrino-nucleon cross-section an order of magnitude above the standard model prediction., Comment: 8 pages revtex, 4 eps figures
Published: 2010
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32. Simulation of up- and down-going neutrino induced showers at the site of the Pierre Auger Observatory

Author: Gora, Dariusz, Roth, Markus, and Tamburro, Alessio
Subjects: Astrophysics
Abstract: We present a study about the possibility to detect neutrino induced extensive air showers at the Pierre Auger Observatory. The Monte Carlo simulations performed take into account the details of the neutrino propagation inside the Earth, the air as well as the surrounding mountains which are modelled by a digital elevation map. Details on the sensitivity with respect to the incoming direction as well as the aperture and the total observable event rates are calculated on the basis of various assumptions of the incoming neutrino flux., Comment: Based on a talk presented at European Cosmic Ray Symposium, Lisbon, September 2006
Published: 2006
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33. Simulation of the isotropic ultra-high energy photons flux in the solar magnetic field and a comparison with observations made by the HAWC and Fermi-LAT observatories

Author: Alvarez-Castillo, David, primary, Homola, Piotr, additional, Sushchov, Oleksandr, additional, Stasielak, Jaroslaw, additional, Stuglik, Slawomir, additional, Gora, Dariusz, additional, Nazari, Vahab, additional, Oancea, Cristina, additional, Beznosko, Dmitriy, additional, Zabari, Noemi, additional, Hnatyk, Bohdan, additional, Mozgova, Alona, additional, Kasztelan, Marcin, additional, Bielewicz, Marcin Michal, additional, Kovacs, Peter, additional, Lozowski, Bartosz, additional, Medvedev, Mikhail V., additional, Miszczyk, Justyna, additional, Bibrzycki, Lukasz, additional, Niedzwiecki, Michal, additional, Smelcerz, Katarzyna, additional, Hachaj, Tomasz, additional, Piekarczyk, Marcin, additional, Pawlik, Maciej, additional, Rzecki, Krzysztof, additional, Rosas, Matias, additional, Smolek, Karel, additional, Svanidze, Manana, additional, Beradze, Revaz, additional, Tursunov, Arman, additional, Wibig, Tadeusz, additional, Zamora-Saa, Jilberto, additional, Poncyljusz, Bozena, additional, Medrala, Justyna, additional, Opila, Gabriela, additional, Pryga, Jerzy Seweryn, additional, Ruimi, Ophir, additional, and Gupta, Alok C., additional
Published: 2023
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34. Method for calculation of the beta exponent from the Heitler-Matthews model of hadronic air showers

Author: Gora, Dariusz, primary
Published: 2023
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35. The muon deficit problem: a new method to calculate the muon rescaling factors and the Heitler-Matthew’s β-exponent

Author: Pękala, Jan, primary, Almeida Cheminant, Kévin, additional, Gora, Dariusz, additional, Borodai, Nataliia, additional, Engel, Ralph, additional, Pierog, Tanguy, additional, Roth, Markus, additional, Stasielak, Jarosław, additional, Unger, Michael, additional, Veberic, Darko, additional, and Wilczyński, Henryk, additional
Published: 2023
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36. Search for tau neutrinos with the MAGIC telescopes: improving selection criteria

Author: Manganaro Marina, Kardum Leonora, Bernardini Elisa, Doro Michele, Gora Dariusz, Micanović Saša, Terzić Tomislav, and Will Martin
Subjects: Physics, QC1-999
Abstract: MAGIC, a system of two Cherenkov telescopes located at the Roque de los Muchachos Observatory (2200 a.s.l.) in the Canary Island of La Palma, has lately been engaged in an unconventional task: the search for a signature of particle showers induced by earth-skimming cosmic tau neutrinos arising from the ocean, in the PeV to EeV energy range. When pointing at the sea, the MAGIC telescopes can collect data in a range of about 5 deg in zenith and 80 deg in azimuth: the analysis of the shower images from ~30 hours of data, together with the simulations of upward-going tau neutrino showers, shows that the air showers induced by tau neutrinos can be discriminated from the hadronic background coming from a similar direction. We have calculated the point source acceptance and the expected event rates, assuming an incoming v flux consistent with IceCube measurements, and for a sample of generic neutrino fluxes from photohadronic interactions in AGNs and GRBs. A 90% C.L. upper limit on the tau-neutrino point source flux of 2.0 × 10–4 GeV cm–2 s–1 has been obtained. The presented results can also be important for future Cherenkov experiments such as the Cherenkov Telescope Array. This next generation ground-based observatory can have a much better possibility to detect v, given its larger FOV and much larger effective area.
Published: 2019
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37. The upgrade of the Pierre Auger Observatory with the Scintillator Surface Detector

Author: Pierre Auger Collaboration, Cataldi, G., Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, boncioli, denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agustín, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Conceição, Rúben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. de, Jesús, Joaquín de, Jong, Sijbrand J. de, De Mauro, Giuseppe, Mello Neto, João de, De Mitri, Ivan, Oliveira, Jaime de, Oliveira Franco, Danelise de, Palma, Francesco de, Souza, Vitor de, De Vito, Emanuele, Río, Mariano del, Deligny, Olivier, Deval, Luca, Matteo, Armando di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita dos, Santos, Diego dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tomáš, Freire, Martín Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, García Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia María, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, Hörandel, Jörg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Juryšek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Köpke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafa, Miguel, Müller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotný, Vladimír, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, Pękala, Jan, Pelayo, Rodrigo, Peña-Rodríguez, Jesús, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perlin, Matías, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico Andrés, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schröder, Frank G., Schröder, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczyński, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Pierre Auger Observatory, Photomultiplier, business.industry, Physics, Astronomy, Detector, Electrical engineering, Scintillator, Data acquisition, Upgrade, Observatory, Experimental High Energy Physics, ddc:530, Electronics, High Energy Physics, business
Abstract: Since its full commissioning in 2008, the Pierre Auger Observatory has consistently demonstrated its scientific productivity. A major upgrade of the Surface Detector array (SD) improves the capabilities of measuring the different components of extensive air showers. One of the elements of the upgrade consists of new Scintillator Surface Detectors (SSD) placed on top of the Water-Cherenkov stations of the SD. At the Observatory, the integration of the SSD components and their deployment in the array is well advanced. In this paper, the main challenges and characteristics of the construction and installation will be reviewed. Started in 2016, an Engineering Array of twelve upgraded stations has been taking data in the field. In March 2019, a preproduction array of 77 SSDs started data acquisition with an adapted version of non-upgraded electronics. It is collecting events and proving the goodness of SSD design. Since December 2020, the upgraded electronics boards are being deployed in the field together with the photomultiplier tubes, increasing the number of SSD detectors, which are taking data continuosly with good stability. In this paper, the-long term performance of a subset of stations acquiring data for more than two years will be discussed. The data collected so far demonstrate the quality of the new detectors and the physics potential of the upgrade project
Published: 2022

38. Indication of a mass-dependent anisotropy above 10 18.7 eV in the hybrid data of the Pierre Auger Observatory

Author: Pierre Auger Collaboration, Mayotte, Eric, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, boncioli, denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agustín, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Conceição, Rúben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. de, Jesús, Joaquín de, Jong, Sijbrand J. de, De Mauro, Giuseppe, Mello Neto, João de, De Mitri, Ivan, Oliveira, Jaime de, Oliveira Franco, Danelise de, Palma, Francesco de, Souza, Vitor de, De Vito, Emanuele, Río, Mariano del, Deligny, Olivier, Deval, Luca, Matteo, Armando di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita dos, Santos, Diego dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tomáš, Freire, Martín Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, García Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia María, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, Hörandel, Jörg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Juryšek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Köpke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafa, Miguel, Müller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotný, Vladimír, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, Pękala, Jan, Pelayo, Rodrigo, Peña-Rodríguez, Jesús, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perlin, Matías, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico Andrés, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schröder, Frank G., Schröder, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczyński, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Physics, Pierre Auger Observatory, Astronomy, Astrophysics, Galactic plane, Mass composition, Threshold energy, Distribution (mathematics), Experimental High Energy Physics, Sensitivity (control systems), High Energy Physics, ddc:620, Anisotropy, Hybrid data, Engineering & allied operations
Abstract: We test the hypothesis of an anisotropy laying along the galactic plane which depends on the mass of primary cosmic-rays. The sensitivity to primary mass is provided by the depth of shower maximum, $X_\text{max}$, from hybrid events measured at the Pierre Auger Observatory. The 14 years of available data are split into on- and off-plane regions using the galactic latitude of each event to form two distributions in $X_\text{max}$, which are compared using the Anderson-Darling 2-samples test. A scan over a subset of the data is used to select an optimal threshold energy of $10^{18.7}$ eV and a galactic latitude splitting at $|b| = 30^\circ$, which are then set as a prescription for the remaining data. With these thresholds, the distribution of $X_\text{max}$ from the on-plane region is found to have a $9.1 \pm 1.6^{+2.1}_{-2.2}$ g/cm$^{2}$ shallower mean and a $5.9\pm2.1^{+3.5}_{-2.5}$ g/cm$^{2}$ narrower width than that of the off-plane region. These differences are as such to indicate that the mean mass of primary particles arriving from the on-plane region is greater than that of those coming from the off-plane region. Monte-Carlo studies yield a $4.4\,\sigma$ post-penalization statistical significance for the independent data. Including the scanned data results in a $4.9^{+1.4}_{-1.5}\,\sigma$ post-penalization statistical significance, where the uncertainties are of systematic origin. Accounting for systematic uncertainties leads to an indication for anisotropy in mass composition above $10^{18.7}$ eV at a confidence level of $3.3\,\sigma$. The anisotropy is observed independently at each of the four fluorescence telescope sites. Interpretations of possible causes of the observed effect are discussed.
Published: 2022
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39. A tau scenario application to a search for upward-going showers with the Fluorescence Detector of the Pierre Auger Observatory

Author: Pierre Auger Collaboration, Caracas, Ioana Alexandra, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, boncioli, denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agustín, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Conceição, Rúben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. de, Jesús, Joaquín de, Jong, Sijbrand J. de, De Mauro, Giuseppe, Mello Neto, João de, De Mitri, Ivan, Oliveira, Jaime de, Oliveira Franco, Danelise de, Palma, Francesco de, Souza, Vitor de, De Vito, Emanuele, Río, Mariano del, Deligny, Olivier, Deval, Luca, Matteo, Armando di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita dos, Santos, Diego dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tomáš, Freire, Martín Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, García Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia María, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, Hörandel, Jörg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Juryšek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Köpke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafa, Miguel, Müller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotný, Vladimír, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, Pękala, Jan, Pelayo, Rodrigo, Peña-Rodríguez, Jesús, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perlin, Matías, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico Andrés, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schröder, Frank G., Schröder, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczyński, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Pierre Auger Observatory, Physics, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Flux, Astrophysics, Spectral line, Path length, Experimental High Energy Physics, High Energy Physics::Experiment, High Energy Physics, ddc:620, Engineering & allied operations, Energy (signal processing), Intensity (heat transfer), Zenith
Abstract: Recent observations of two coherent radio pulses with the ANITA detector can be interpreted as steeply upward-going cosmic-ray showers with energies of a few tenths of an EeV and remain unexplained. The Pierre Auger Observatory has a large exposure to such upward propagating shower-like events, and has used 14 years of its Fluorescence Detector (FD) data to perform a generic search for such events with elevation angles greater than 20$^\circ$ from the horizon. Here this search is recast to constrain models generating high energy $\tau$-leptons. For maximal flexibility, only the propagation, decay, and interactions of $\tau$-leptons are treated in this analysis, meaning that the results are independent of the $\tau$-production scenario. This treatment allows for the application of these results to the wide range of models producing $\tau$-leptons that have been proposed to describe the "anomalous" ANITA events. The goal of this study is accomplished by generating $\tau$-leptons within the Earth and its atmosphere with an intensity dependent on the media density. The zenith angle, location and calorimetric energy of any resulting $\tau$-induced air showers are then used to calculate the exposure of the FD of the Pierre Auger Observatory to $\tau$ primaries. Differential limits as low as $10^{-9}$GeV s$^{-1}$cm$^{-2}$sr$^{-1}$ to the flux of $\tau$-leptons produced with less than a 50 km path length below the Earth's surface are reported for several zenith angle ranges and primary energy spectra. Full exposure and sensitivity information is provided, facilitating the application of these results to different $\tau$-lepton production models.
Published: 2022
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40. Study on multi-ELVES in the Pierre Auger Observatory

Author: Collaboration, Pierre Auger, V��squez Ram��rez, Adriana, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Bel��n, Andringa, Sofia, Aramo, Carla, Ara��jo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hern��n Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Teresa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, Boncioli, Denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, B��sken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agust��n, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Concei��o, R��ben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia Dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. De, Jes��s, Joaqu��n De, Jong, Sijbrand J. De, De Mauro, Giuseppe, Mello Neto, Jo��o De, De Mitri, Ivan, Oliveira, Jaime De, Oliveira Franco, Danelise De, Palma, Francesco De, Souza, Vitor De, De Vito, Emanuele, R��o, Mariano Del, Deligny, Olivier, Deval, Luca, Matteo, Armando Di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita Dos, Santos, Diego Dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tom��, Freire, Mart��n Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, Garc��a, Beatriz, Garc��a Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, GIACCARI, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, G��mez Berisso, Mariano, G��mez Vitale, Primo F., Gongora, Juan Pablo, Gonz��lez, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Mat��as Rolf, Hansen, Patricia Mar��a, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, H��randel, J��rg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Jury��ek, Jakub, K��p��, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, K��pke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui De Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, L��pez, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Mart��nez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, Fran��ois, Morello, Carlo, Mostafa, Miguel, M��ller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotn��, Vladim��r, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, P��kala, Jan, Pelayo, Rodrigo, Pe��a-Rodr��guez, Jes��s, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, P��rez Bertolli, Carmina, Perlin, Mat��as, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, M��rio, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues De Carvalho, Washington, Rodriguez Rojo, Jorge Rub��n, Roncoroni, Mat��as J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, S��nchez, Federico Andr��s, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Sch��fer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schl��ter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schr��der, Frank G., Schr��der, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Silli, Gaia, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stani��, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Su��rez-Dur��n, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tom��, Bernardo, Torr��s, Zo��, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Luk��, Vacula, Martin, Vald��s Galicia, Jose F., Valore, Laura, Varela, Enrique, V��squez-Ram��rez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe, Clara Keiko Oliveira, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczy��ski, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Physics, Pierre Auger Observatory, Polarity (physics), Astronomy, Astrophysics, Lightning, Lightning strike, Altitude, Experimental High Energy Physics, Light emission, Satellite, High Energy Physics, ddc:620, Ionosphere, Engineering & allied operations
Abstract: Since 2013, the four sites of the Fluorescence Detector (FD) of the Pierre Auger Observatory record ELVES with a dedicated trigger. These UV light emissions are correlated to distant lightning strikes. The length of recorded traces has been increased from 100 $\mu$s (2013), to 300 $\mu$s (2014-16), to 900 $\mu$s (2017-present), to progressively extend the observation of the light emission towards the vertical of the causative lightning and beyond. A large fraction of the observed events shows double ELVES within the time window, and, in some cases, even more complex structures are observed. The nature of the multi-ELVES is not completely understood but may be related to the different types of lightning in which they are originated. For example, it is known that Narrow Bipolar Events can produce double ELVES, and Energetic In-cloud Pulses, occurring between the main negative and upper positive charge layer of clouds, can induce double and even quadruple ELVES in the ionosphere. This report shows the seasonal and daily dependence of the time gap, amplitude ratio, and correlation between the pulse widths of the peaks in a sample of 1000+ multi-ELVES events recorded during the period 2014-20. The events have been compared with data from other satellite and ground-based sensing devices to study the correlation of their properties with lightning observables such as altitude and polarity.
Published: 2022
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41. Machine learning aided noise filtration and signal classification for CREDO experiment

Author: Bibrzycki, ��ukasz, Alvarez-Castillo, David, Bar, Olaf, Gora, Dariusz, Homola, Piotr, Kov��cs, P��ter, Nied��wiecki, Micha��, Piekarczyk, Marcin, Rzecki, Krzysztof, Stasielak, Jaroslaw, Stuglik, S��awomir, Sushchov, Oleksandr, and Tursunov, Arman
Subjects: Signal Processing (eess.SP), Physics - Instrumentation and Detectors, FOS: Electrical engineering, electronic engineering, information engineering, FOS: Physical sciences, Instrumentation and Detectors (physics.ins-det), Electrical Engineering and Systems Science - Signal Processing
Abstract: The wealth of smartphone data collected by the Cosmic Ray Extremely Distributed Observatory(CREDO) greatly surpasses the capabilities of manual analysis. So, efficient means of rejectingthe non-cosmic-ray noise and identification of signals attributable to extensive air showers arenecessary. To address these problems we discuss a Convolutional Neural Network-based method ofartefact rejection and complementary method of particle identification based on common statisticalclassifiers as well as their ensemble extensions. These approaches are based on supervised learning,so we need to provide a representative subset of the CREDO dataset for training and validation.According to this approach over 2300 images were chosen and manually labeled by 5 judges.The images were split into spot, track, worm (collectively named signals) and artefact classes.Then the preprocessing consisting of luminance summation of RGB channels (grayscaling) andbackground removal by adaptive thresholding was performed. For purposes of artefact rejectionthe binary CNN-based classifier was proposed which is able to distinguish between artefacts andsignals. The classifier was fed with input data in the form of Daubechies wavelet transformedimages. In the case of cosmic ray signal classification, the well-known feature-based classifierswere considered. As feature descriptors, we used Zernike moments with additional feature relatedto total image luminance. For the problem of artefact rejection, we obtained an accuracy of 99%. For the 4-class signal classification, the best performing classifiers achieved a recognition rate of 88%., 9 pages,4 figurek, ICRC 2021 contribution
Published: 2021

42. UHECR arrival directions in the latest data from the original Auger and TA surface detectors and nearby galaxies

Author: di Matteo, Armando, primary, Anchordoqui, Luis A., additional, Bister, Teresa, additional, Biteau, Jonathan, additional, Caccianiga, Lorenzo, additional, de Almeida, Rogerio M., additional, Deligny, Olivier, additional, GIACCARI, Ugo, additional, Harari, Diego, additional, Kim, Jihyun, additional, Kuznetsov, Mikhail, additional, Maris, Ioana Codrina, additional, Rubtsov, Grigory, additional, Tinyakov, Petr, additional, Troitsky, Sergey, additional, Urban, Federico, additional, Abreu, Pedro, additional, Aglietta, Marco, additional, Albury, Justin M., additional, Allekotte, Ingomar, additional, Almela, Alejandro, additional, Alvarez-Muniz, Jaime, additional, Alves Batista, Rafael, additional, Anastasi, Gioacchino Alex, additional, Andrada, Belén, additional, Andringa, Sofia, additional, Aramo, Carla, additional, Araújo Ferreira, Paulo Ricardo, additional, Arteaga Velazquez, Juan Carlos, additional, Asorey, Hernán Gonzalo, additional, Assis, Pedro, additional, Avila, Gualberto, additional, Badescu, Alina Mihaela, additional, Bakalova, Alena, additional, Balaceanu, Alexandru, additional, Barbato, Felicia, additional, Barreira Luz, Ricardo Jorge, additional, Becker, Karl-Heinz, additional, Bellido, Jose A., additional, Berat, Corinne, additional, Bertaina, Mario Edoardo, additional, Bertou, Xavier, additional, Biermann, Peter L., additional, Binet, Virginia, additional, Bismark, Kathrin, additional, Blazek, Jiri, additional, Bleve, Carla, additional, Bohacova, Martina, additional, Boncioli, Denise, additional, Bonifazi, Carla, additional, Bonneau Arbeletche, Luan, additional, Borodai, Nataliia, additional, Botti, Ana Martina, additional, Brack, Jeffrey, additional, Bretz, Thomas, additional, Brichetto Orchera, P. Gabriel, additional, Briechle, Florian Lukas, additional, Buchholz, Peter, additional, Bueno, Antonio, additional, Buitink, Stijn, additional, Buscemi, Mario, additional, Büsken, Max, additional, Caballero-Mora, Karen S., additional, Canfora, Fabrizia, additional, Caracas, Ioana, additional, Carceller, Juan Miguel, additional, Caruso, Rossella, additional, Castellina, Antonella, additional, Catalani, Fernando, additional, Cataldi, Gabriella, additional, Cazon, Lorenzo, additional, Cerda, Marcos, additional, Chinellato, Jose Augusto, additional, Chudoba, Jiří, additional, Chytka, Ladislav, additional, Clay, Roger W, additional, Cobos Cerutti, Agustín, additional, Colalillo, Roberta, additional, Coleman, Alan, additional, Coluccia, Maria Rita, additional, Conceição, Rúben, additional, Condorelli, Antonio, additional, Consolati, Giovanni, additional, Contreras, Fernando, additional, Convenga, Fabio, additional, Correia dos Santos, Diego, additional, Covault, Corbin, additional, Dasso, Sergio, additional, Daumiller, Kai, additional, Dawson, Bruce R., additional, Day, Jarryd A., additional, de Jesús, Joaquín, additional, de Jong, Sijbrand J., additional, De Mauro, Giuseppe, additional, de Mello Neto, João, additional, De Mitri, Ivan, additional, de Oliveira, Jaime, additional, de Oliveira Franco, Danelise, additional, de Palma, Francesco, additional, de Souza, Vitor, additional, De Vito, Emanuele, additional, del Río, Mariano, additional, Deval, Luca, additional, Dobrigkeit, Carola, additional, D'Olivo, Juan Carlos, additional, Domingues Mendes, Luis Miguel, additional, dos Anjos, Rita Cassia, additional, dos Santos, Diego, additional, Dova, Maria Teresa, additional, Ebr, Jan, additional, Engel, Ralph, additional, Epicoco, Italo, additional, Erdmann, Martin, additional, Escobar, Carlos O., additional, Etchegoyen, Alberto, additional, Falcke, Heino, additional, Farmer, John, additional, Farrar, Glennys R., additional, Fauth, Anderson, additional, Fazzini, Norberto, additional, Feldbusch, Fridtjof, additional, Fenu, Francesco, additional, Fick, Brian, additional, Figueira, Juan Manuel, additional, Filipcic, Andrej, additional, Fitoussi, Thomas, additional, Fodran, Tomáš, additional, Freire, Martín Miguel, additional, Fuster, Alan, additional, Galea, Cristina, additional, Galelli, Claudio, additional, García, Beatriz, additional, García Vegas, Adrianna Luz, additional, Gemmeke, Hartmut, additional, Gesualdi, Flavia, additional, Gherghel-Lascu, Alexandru, additional, Ghia, Piera Luisa, additional, Giammarchi, Marco, additional, Glombitza, Jonas, additional, Gobbi, Fabian, additional, Gollan, Fernando, additional, Golup, Geraldina, additional, Gómez Berisso, Mariano, additional, Gómez Vitale, Primo F., additional, Gongora, Juan Pablo, additional, González, Juan Manuel, additional, Gonzalez, Nicolas Martin, additional, Goos, Isabel, additional, Gora, Dariusz, additional, Gorgi, Alessio, additional, Gottowik, Marvin, additional, Grubb, Trent D., additional, Guarino, Fausto, additional, Guedes, Germano, additional, Guido, Eleonora, additional, Hahn, Steffen, additional, Hamal, Petr, additional, Hampel, Matías Rolf, additional, Hansen, Patricia María, additional, Harvey, Violet M., additional, Haungs, Andreas, additional, Hebbeker, Thomas, additional, Heck, Dieter, additional, Hill, Gary C., additional, Hojvat, Carlos, additional, Hörandel, Jörg R., additional, Horvath, Pavel, additional, Hrabovsky, Miroslav, additional, Huege, Tim, additional, Insolia, Antonio, additional, Isar, Paula Gina, additional, Janecek, Petr, additional, Johnsen, Jeffrey A., additional, Jurysek, Jakub, additional, Kääpä, Alex, additional, Kampert, Karl-Heinz, additional, Karastathis, Nikolaos, additional, Keilhauer, Bianca, additional, Kemp, Julian, additional, Khakurdikar, Abha, additional, Kizakke Covilakam, Varada Varma, additional, Klages, Hans, additional, Kleifges, Matthias, additional, Kleinfeller, Jonny, additional, Köpke, Marcel, additional, Kunka, Norbert, additional, Lago, Bruno L., additional, Lang, Rodrigo Guedes, additional, Langner, Niklas, additional, Leigui de Oliveira, Marcelo Augusto, additional, Lenok, Vladimir, additional, Letessier-Selvon, Antoine, additional, Lhenry-Yvon, Isabelle, additional, Lo Presti, Domenico, additional, LOPES, Luis, additional, López, Rebeca, additional, Lu, Lu, additional, Luce, Quentin, additional, Machado Payeras, Allan, additional, Mancarella, Giovanni, additional, Mandat, Dusan, additional, Manning, Bradley C., additional, Manshanden, Julien, additional, Mantsch, Paul, additional, Marafico, Sullivan, additional, Mariazzi, Analisa, additional, Marsella, Giovanni, additional, Martello, Daniele, additional, Martinelli, Sara, additional, Martínez Bravo, Oscar, additional, Mastrodicasa, Massimo, additional, Mathes, Hermann-Josef, additional, Matthews, James, additional, Matthiae, Giorgio, additional, Mayotte, Eric, additional, Mazur, Peter, additional, Medina-Tanco, Gustavo, additional, Melo, Diego, additional, Menshikov, Alexander, additional, Merenda, Kevin-Druis, additional, Michal, Stanislav, additional, Micheletti, Maria Isabel, additional, Miramonti, Lino, additional, Mollerach, Silvia, additional, Montanet, François, additional, Morello, Carlo, additional, Mostafa, Miguel, additional, Müller, Ana L., additional, Muller, Marcio Aparecido, additional, Mulrey, Katharine, additional, Mussa, Roberto, additional, Muzio, Marco Stein, additional, Namasaka, Wilson M., additional, Nasr-Esfahani, Alina, additional, Nellen, Lukas, additional, Niculescu-Oglinzanu, Mihai, additional, Niechciol, Marcus, additional, Nitz, Dave, additional, Nosek, Dalibor, additional, Novotný, Vladimír, additional, Nozka, Libor, additional, Nucita, Achille, additional, Nunez, Luis A., additional, Palatka, Miroslav, additional, Pallotta, Juan, additional, Papenbreer, Philipp, additional, Parente, Gonzalo, additional, Parra, Alejandra, additional, Pawlowsky, Jannis, additional, Pech, Miroslav, additional, Pedreira, Francisco, additional, Pękala, Jan, additional, Pelayo, Rodrigo, additional, Peña-Rodríguez, Jesús, additional, Pereira Martins, Edyvania Emily, additional, Perez Armand, Johnnier, additional, Pérez Bertolli, Carmina, additional, Perlin, Matías, additional, Perrone, Lorenzo, additional, Petrera, Sergio, additional, Pierog, Tanguy, additional, Pimenta, Mário, additional, Pirronello, Valerio, additional, Platino, Manuel, additional, Pont, Bjarni, additional, Pothast, Mart, additional, Privitera, Paolo, additional, Prouza, Michael, additional, Puyleart, Andrew, additional, Querchfeld, Sven, additional, Rautenberg, Julian, additional, Ravignani, Diego, additional, Reininghaus, Maximilian, additional, Ridky, Jan, additional, Riehn, Felix, additional, Risse, Markus, additional, Rizi, Vincenzo, additional, Rodrigues de Carvalho, Washington, additional, Rodriguez Rojo, Jorge Rubén, additional, Roncoroni, Matías J., additional, Rossoni, Simone, additional, Roth, Markus, additional, Roulet, Esteban, additional, Rovero, Adrian, additional, Ruehl, Philip, additional, Saftoiu, Alexandra, additional, Salamida, Francesco, additional, Salazar, Humberto Ibarguen, additional, Salina, Gaetano, additional, Sanabria Gomez, Jose, additional, Sánchez, Federico Andrés, additional, Santos, Edivaldo Moura, additional, Santos, Eva, additional, Sarazin, Fred, additional, Sarmento, Raul, additional, Sarmiento-Cano, Christian, additional, Sato, Ricardo, additional, Savina, Pierpaolo, additional, Schäfer, Christoph M., additional, Scherini, Viviana, additional, Schieler, Harald, additional, Schimassek, Martin, additional, Schimp, Michael, additional, Schlüter, Felix, additional, Schmidt, David, additional, Scholten, Olaf, additional, Schovanek, Petr, additional, Schröder, Frank G., additional, Schröder, Sonja, additional, Schulte, Josina, additional, Sciutto, Sergio, additional, Scornavacche, Marina, additional, Segreto, Alberto, additional, Sehgal, Srijan, additional, Shellard, Ronald C., additional, Sigl, Guenter, additional, Silli, Gaia, additional, Sima, Octavian, additional, Smida, Radomir, additional, Sommers, Paul, additional, Soriano, Jorge F., additional, Souchard, Julien, additional, Squartini, Ruben, additional, Stadelmaier, Maximilian, additional, Stanca, Denis, additional, Stanič, Samo, additional, Stasielak, Jaroslaw, additional, Stassi, Patrick, additional, Streich, Alexander, additional, Suárez-Durán, Mauricio, additional, Sudholz, Tristan, additional, Suomijarvi, Tiina, additional, Supanitsky, A. Daniel, additional, Szadkowski, Zbigniew, additional, Tapia, Alex, additional, Taricco, Carla, additional, Timmermans, Charles, additional, Tkachenko, Olena, additional, Tobiska, Petr, additional, Todero Peixoto, Carlos J., additional, Tomé, Bernardo, additional, Torrès, Zoé, additional, Travaini, Andres, additional, Travnicek, Petr, additional, Trimarelli, Caterina, additional, Tueros, Matías, additional, Ulrich, Ralf, additional, Unger, Michael, additional, Vaclavek, Lukáš, additional, Vacula, Martin, additional, Valdés Galicia, Jose F., additional, Valore, Laura, additional, Varela, Enrique, additional, Vásquez-Ramírez, Adriana, additional, Veberic, Darko, additional, Ventura, Cynthia, additional, Vergara Quispe, Indira D., additional, Verzi, Valerio, additional, Vicha, Jakub, additional, Vink, Jacco, additional, Vorobiov, Serguei, additional, Wahlberg, Hernan, additional, Watanabe, Clara Keiko Oliveira, additional, Watson, Alan, additional, Weber, Marc, additional, Weindl, Andreas, additional, Wiencke, Lawrence, additional, Wilczyński, Henryk, additional, Wirtz, Marcus, additional, Wittkowski, David, additional, Wundheiler, Brian, additional, Yushkov, Alexey, additional, Zapparrata, Orazio, additional, Zas, Enrique, additional, Zavrtanik, Danilo, additional, Zavrtanik, Marko, additional, Zehrer, Lukas, additional, Abbasi, Rasha, additional, Abu-Zayyad, Tareq, additional, Allen, Monica, additional, Arai, Yuto, additional, Arimura, Ryuhei, additional, Barcikowski, Elliott, additional, Belz, John, additional, Bergman, Douglas, additional, Blake, Samuel, additional, Cady, Robert, additional, Cheon, ByongGu, additional, Chiba, Jyunsei, additional, Chikawa, Michiyuki, additional, Fujii, Toshihiro, additional, Fujisue, Kozo, additional, Fujita, Keitaro, additional, Fujiwara, Ryota, additional, Fukushima, Masaki, additional, Fukushima, Ryota, additional, Furlich, Greg, additional, Gonzalez, Ricardo, additional, Hanlon, William, additional, Hayashi, Motoki, additional, Hayashida, Naoaki, additional, Hibino, Kinya, additional, Higuchi, Ryo, additional, Honda, Ken, additional, Ikeda, Daisuke, additional, Inadomi, Taichi, additional, Inoue, Naoya, additional, Ishii, Takaaki, additional, Ito, Hirotaka, additional, Ivanov, Dmitri, additional, Iwakura, Hirokazu, additional, Iwasaki, Aoi, additional, Jeong, Hyoming, additional, Jeong, Soomin, additional, Jui, Charlie, additional, Kadota, Kenichi, additional, Kakimoto, Fumio, additional, Kalashev, Oleg, additional, Kasahara, Katsuaki, additional, Kasami, Saori, additional, Kawai, Hideyuki, additional, Kawakami, Saburo, additional, Kawana, Shingo, additional, Kawata, Katsumasa, additional, Kharuk, Ivan, additional, Kido, Eiji, additional, Kim, HangBae, additional, Kim, Jihee, additional, Kim, Min Hyo, additional, Kim, Sang Woo, additional, Kimura, Yusuke, additional, Kishigami, Shoichi, additional, Kubota, Yuto, additional, Kurisu, Shinnosuke, additional, Kuzmin, Vladim, additional, Kwon, Youngjoon, additional, Lee, Kwangho, additional, Lubsandorzhiev, BayarJon Paul, additional, Lundquist, Jon Paul, additional, Machida, Kazuhiro, additional, Matsumiya, Hiroyuki, additional, Matsuyama, Toshio, additional, Matthews, John, additional, Mayta, Rosa, additional, Minamino, Mayuko, additional, Mukai, Keijiro, additional, Myers, Isaac, additional, Nagataki, Shigehiro, additional, Nakai, Kei, additional, Nakamura, Ryo, additional, Nakamura, Toru, additional, Nakamura, Tomoyuki, additional, Nakamura, Yuya, additional, Nakazawa, Arata, additional, Nishio, Eiji, additional, Nonaka, Toshiyuki, additional, Oda, Hiroyuki, additional, Ogio, Shoichi, additional, Ohnishi, Munehiro, additional, Ohoka, Hideyuki, additional, Oku, Yuya, additional, Okuda, Takeshi, additional, Omura, Yugo, additional, Ono, Masaomi, additional, Onogi, Ryota, additional, Oshima, Akitoshi, additional, OZAWA, Shunsuke, additional, Park, Il Hung, additional, Potts, Matt, additional, Pshirkov, Maxim, additional, Remington, Jackson, additional, Rodriguez, Doug, additional, Ryu, Dongsu, additional, Sagawa, Hiroyuki, additional, Sahara, Ryosuke, additional, Saito, Yasunori, additional, Sakaki, Naoto, additional, Sako, Takashi, additional, Sakurai, Nobuyuki, additional, Sano, Kengo, additional, Sato, Koki, additional, Seki, Terutsugu, additional, Sekino, Koichi, additional, Shah, Priti, additional, Shibasaki, Yuma, additional, Shibata, Fumiya, additional, Shibata, Norimichi, additional, Shibata, Tatsunobu, additional, Shimodaira, Hideaki, additional, Shin, Bokkyun, additional, Shin, Heungsu, additional, Shinto, Daiki, additional, Smith, Jeremy, additional, Sokolsky, Pierre, additional, Sone, Naohiro, additional, Stokes, Ben, additional, Stroman, Tom, additional, Takagi, Yoshinori, additional, Takahashi, Yuichi, additional, Takamura, Mai, additional, Takeda, Masahiro, additional, Takeishi, Ryuji, additional, Taketa, Akimichi, additional, Takita, Masato, additional, Tameda, Yuichiro, additional, Tanaka, Hideki, additional, Tanaka, Koichi, additional, Tanaka, Manobu, additional, Tanoue, Yuta, additional, Thomas, Stanton, additional, Thomson, Gordon, additional, Tkachev, Igor, additional, Tokuno, Hisono, additional, Tomida, Taka, additional, Tsuda, Ryosuke, additional, Tsunesada, Yoshiki, additional, Uchihori, Yukio, additional, Udo, Shigeharu, additional, Uehama, Takafumi, additional, Wong, Tiffany, additional, Yada, Kohei, additional, Yamamoto, Mashu, additional, Yamazaki, Katsuya, additional, Yang, Jongmann, additional, Yashiro, Kenta, additional, Yoshida, Fugo, additional, Yoshioka, Tsubasa, additional, Zhezher, Yana, additional, and Zundel, Zach, additional
Published: 2021
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43. Simulations of Cosmic Ray Ensembles originated nearby the Sun

Author: Alvarez-Castillo, David, primary, Sushchov, Oleksandr, additional, Homola, Piotr, additional, Beznosko, Dmitriy, additional, Budnev, Nikolai, additional, Gora, Dariusz, additional, Gupta, Alok, additional, Hnatyk, Bohdan, additional, Kasztelan, Marcin, additional, Kovacs, Peter, additional, Lozowski, Bartosz, additional, Medvedev, Mikhail, additional, Miszczyk, Justyna, additional, Mozgova, Alona, additional, Nazari, Vahab, additional, Niedzwiecki, Michal, additional, Pawlik, Maciej, additional, Rosas, Matias, additional, Rzecki, Krzysztof, additional, Smelcerz, Katarzyna, additional, Smolek, Karel, additional, Stasielak, Jaroslaw, additional, Stuglik, Slawomir, additional, Svanidze, Manana, additional, Tursunov, Arman, additional, Verbetsky, Yuri, additional, Wibig, Tadeusz, additional, Zamora-Saa, Jilberto, additional, Poncyljusz, Bozena, additional, Medrala, Justyna, additional, Opila, Gabriela, additional, Bibrzyck, Lukasz, additional, and Piekarczyk., Marcin, additional
Published: 2021
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44. Determination of Zenith Angle Dependence of Incoherent Cosmic Ray Muon Flux Using Smartphones of the CREDO Project

Author: Wibig, Tadeusz, primary, Karbowiak, Michał, additional, Alvarez-Castillo, David, additional, Bar, Olaf, additional, Bibrzycki, Łukasz, additional, Gora, Dariusz, additional, Homola, Piotr, additional, Kovacs, Peter, additional, Piekarczyk, Marcin, additional, Stasielak, Jaroslaw, additional, Stuglik, Sławomir, additional, Sushchov, Oleksandr, additional, and Tursunov, Arman, additional
Published: 2021
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45. Invitation to the Cosmic Ray Extremely Distributed Observatory

Author: Homola, Piotr, primary, Alvarez Castillo, David E, additional, Almeida Cheminant, Kévin, additional, Beznosko, Dmitriy, additional, Budnev, Nikolai, additional, Gora, Dariusz, additional, Gupta, Alok C., additional, Hnatyk, Bohdan, additional, Kasztelan, Marcin, additional, Kovacs, Peter, additional, Lozowski, Bartosz, additional, Medvedev, Mikhail V., additional, Miszczyk, Justyna, additional, Mozgova, Alona, additional, Nazari, Vahab, additional, Niedzwiecki, Michal, additional, Pawlik, Maciej, additional, Rosas, Matias, additional, Rzecki, Krzysztof, additional, Smelcerz, Katarzyna, additional, Smolek, Karel, additional, Stasielak, Jaroslaw, additional, Stuglik, Slawomir, additional, Sushchov, Oleksandr, additional, Svanidze, Manana, additional, Tursunov, Arman, additional, Vaquero, Jose Manuel, additional, Verbetsky, Yuri, additional, Wibig, Tadeusz, additional, WOZNIAK, Krzysztof, additional, and Zamora-Saa, Jilberto, additional
Published: 2021
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46. Event rates of UHE photons cascading in the geomagnetic field at CTA-North

Author: Almeida Cheminant, Kévin, primary, Gora, Dariusz, additional, Alvarez Castillo, David E, additional, Budnev, Nikolay, additional, Gupta, Alok C., additional, Homola, Piotr, additional, Łozowski, Bartosz, additional, Medvedev, Mikhail V., additional, Mozgova, Alona, additional, Pawlik, Maciej, additional, Rzecki, Krzysztof, additional, Smolek, Karel, additional, Stasielak, Jaroslaw, additional, Sushchov, Oleksandr, additional, Tursunov, Arman, additional, Wibig, Tadeusz, additional, and Zamora-Saa, Jilberto, additional
Published: 2021
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47. Performance of the 433 m surface array of the Pierre Auger Observatory

Author: Pierre Auger Collaboration, Silli, Gaia, Abreu, Pedro, Aglietta, Marco, Albury, Justin M., Allekotte, Ingomar, Almela, Alejandro, Alvarez-Muniz, Jaime, Alves Batista, Rafael, Anastasi, Gioacchino Alex, Anchordoqui, Luis A., Andrada, Belén, Andringa, Sofia, Aramo, Carla, Araújo Ferreira, Paulo Ricardo, Arteaga Velazquez, Juan Carlos, Asorey, Hernán Gonzalo, Assis, Pedro, Avila, Gualberto, Badescu, Alina Mihaela, Bakalova, Alena, Balaceanu, Alexandru, Barbato, Felicia, Barreira Luz, Ricardo Jorge, Becker, Karl-Heinz, Bellido, Jose A., Berat, Corinne, Bertaina, Mario Edoardo, Bertou, Xavier, Biermann, Peter L., Binet, Virginia, Bismark, Kathrin, Bister, Terasa, Biteau, Jonathan, Blazek, Jiri, Bleve, Carla, Bohacova, Martina, Boncioli, Denise, Bonifazi, Carla, Bonneau Arbeletche, Luan, Borodai, Nataliia, Botti, Ana Martina, Brack, Jeffrey, Bretz, Thomas, Brichetto Orchera, P. Gabriel, Briechle, Florian Lukas, Buchholz, Peter, Bueno, Antonio, Buitink, Stijn, Buscemi, Mario, Büsken, Max, Caballero-Mora, Karen S., Caccianiga, Lorenzo, Canfora, Fabrizia, Caracas, Ioana, Carceller, Juan Miguel, Caruso, Rossella, Castellina, Antonella, Catalani, Fernando, Cataldi, Gabriella, Cazon, Lorenzo, Cerda, Marcos, Chinellato, Jose Augusto, Chudoba, Jiri, Chytka, Ladislav, Clay, Roger W., Cobos Cerutti, Agustín, Colalillo, Roberta, Coleman, Alan, Coluccia, Maria Rita, Conceição, Rúben, Condorelli, Antonio, Consolati, Giovanni, Contreras, Fernando, Convenga, Fabio, Correia dos Santos, Diego, Covault, Corbin, Dasso, Sergio, Daumiller, Kai, Dawson, Bruce R., Day, Jarryd A., Almeida, Rogerio M. de, Jesús, Joaquín de, Jong, Sijbrand J. de, De Mauro, Giuseppe, Mello Neto, João de, De Mitri, Ivan, Oliveira, Jaime de, Oliveira Franco, Danelise de, Palma, Francesco de, Souza, Vitor de, De Vito, Emanuele, Río, Mariano del, Deligny, Olivier, Deval, Luca, Matteo, Armando di, Dobrigkeit, Carola, D'Olivo, Juan Carlos, Domingues Mendes, Luis Miguel, Anjos, Rita dos, Santos, Diego dos, Dova, Maria Teresa, Ebr, Jan, Engel, Ralph, Epicoco, Italo, Erdmann, Martin, Escobar, Carlos O., Etchegoyen, Alberto, Falcke, Heino, Farmer, John, Farrar, Glennys R., Fauth, Anderson, Fazzini, Norberto, Feldbusch, Fridtjof, Fenu, Francesco, Fick, Brian, Figueira, Juan Manuel, Filipcic, Andrej, Fitoussi, Thomas, Fodran, Tomáš, Freire, Martín Miguel, Fujii, Toshihiro, Fuster, Alan, Galea, Cristina, Galelli, Claudio, García, Beatriz, García Vegas, Adrianna Luz, Gemmeke, Hartmut, Gesualdi, Flavia, Gherghel-Lascu, Alexandru, Ghia, Piera Luisa, Giaccari, Ugo, Giammarchi, Marco, Glombitza, Jonas, Gobbi, Fabian, Gollan, Fernando, Golup, Geraldina, Gómez Berisso, Mariano, Gómez Vitale, Primo F., Gongora, Juan Pablo, González, Juan Manuel, Gonzalez, Nicolas Martin, Goos, Isabel, Gora, Dariusz, Gorgi, Alessio, Gottowik, Marvin, Grubb, Trent D., Guarino, Fausto, Guedes, Germano, Guido, Eleonora, Hahn, Steffen, Hamal, Petr, Hampel, Matías Rolf, Hansen, Patricia María, Harari, Diego, Harvey, Violet M., Haungs, Andreas, Hebbeker, Thomas, Heck, Dieter, Hill, Gary C., Hojvat, Carlos, Hörandel, Jörg, Horvath, Pavel, Hrabovsky, Miroslav, Huege, Tim, Insolia, Antonio, Isar, Paula Gina, Janecek, Petr, Johnsen, Jeffrey A., Juryšek, Jakub, Kääpä, Alex, Kampert, Karl-Heinz, Karastathis, Nikolaos, Keilhauer, Bianca, Kemp, Julian, Khakurdikar, Abha, Kizakke Covilakam, Varada Varma, Klages, Hans, Kleifges, Matthias, Kleinfeller, Jonny, Köpke, Marcel, Kunka, Norbert, Lago, Bruno L., Lang, Rodrigo Guedes, Langner, Niklas, Leigui de Oliveira, Marcelo Augusto, Lenok, Vladimir, Letessier-Selvon, Antoine, Lhenry-Yvon, Isabelle, Lo Presti, Domenico, LOPES, Luis, López, Rebeca, Lu, Lu, Luce, Quentin, Lundquist, Jon Paul, Machado Payeras, Allan, Mancarella, Giovanni, Mandat, Dusan, Manning, Bradley C., Manshanden, Julien, Mantsch, Paul, Marafico, Sullivan, Mariazzi, Analisa, Maris, Ioana Codrina, Marsella, Giovanni, Martello, Daniele, Martinelli, Sara, Martínez Bravo, Oscar, Mastrodicasa, Massimo, Mathes, Hermann-Josef, Matthews, James, Matthiae, Giorgio, Mayotte, Eric, Mazur, Peter, Medina-Tanco, Gustavo, Melo, Diego, Menshikov, Alexander, Merenda, Kevin-Druis, Michal, Stanislav, Micheletti, Maria Isabel, Miramonti, Lino, Mollerach, Silvia, Montanet, François, Morello, Carlo, Mostafa, Miguel, Müller, Ana L., Muller, Marcio Aparecido, Mulrey, Katharine, Mussa, Roberto, Muzio, Marco Stein, Namasaka, Wilson M., Nasr-Esfahani, Alina, Nellen, Lukas, Niculescu-Oglinzanu, Mihai, Niechciol, Marcus, Nitz, Dave, Nosek, Dalibor, Novotný, Vladimír, Nozka, Libor, Nucita, Achille, Nunez, Luis A., Palatka, Miroslav, Pallotta, Juan, Papenbreer, Philipp, Parente, Gonzalo, Parra, Alejandra, Pawlowsky, Jannis, Pech, Miroslav, Pedreira, Francisco, Pękala, Jan, Pelayo, Rodrigo, Peña-Rodríguez, Jesús, Pereira Martins, Edyvania Emily, Perez Armand, Johnnier, Pérez Bertolli, Carmina, Perlin, Matías, Perrone, Lorenzo, Petrera, Sergio, Pierog, Tanguy, Pimenta, Mário, Pirronello, Valerio, Platino, Manuel, Pont, Bjarni, Pothast, Mart, Privitera, Paolo, Prouza, Michael, Puyleart, Andrew, Querchfeld, Sven, Rautenberg, Julian, Ravignani, Diego, Reininghaus, Maximilian, Ridky, Jan, Riehn, Felix, Risse, Markus, Rizi, Vincenzo, Rodrigues de Carvalho, Washington, Rodriguez Rojo, Jorge Rubén, Roncoroni, Matías J., Rossoni, Simone, Roth, Markus, Roulet, Esteban, Rovero, Adrian, Ruehl, Philip, Saffi, Steven J., Saftoiu, Alexandra, Salamida, Francesco, Salazar, Humberto Ibarguen, Salina, Gaetano, Sanabria Gomez, Jose, Sánchez, Federico Andrés, Santos, Edivaldo Moura, Santos, Eva, Sarazin, Fred, Sarmento, Raul, Sarmiento-Cano, Christian, Sato, Ricardo, Savina, Pierpaolo, Schäfer, Christoph M., Scherini, Viviana, Schieler, Harald, Schimassek, Martin, Schimp, Michael, Schlüter, Felix, Schmidt, David, Scholten, Olaf, Schovanek, Petr, Schröder, Frank G., Schröder, Sonja, Schulte, Josina, Sciutto, Sergio, Scornavacche, Marina, Segreto, Alberto, Sehgal, Srijan, Shellard, Ronald C., Sigl, Guenter, Sima, Octavian, Smida, Radomir, Sommers, Paul, Soriano, Jorge F., Souchard, Julien, Squartini, Ruben, Stadelmaier, Maximilian, Stanca, Denis, Stanič, Samo, Stasielak, Jaroslaw, Stassi, Patrick, Streich, Alexander, Suárez-Durán, Mauricio, Sudholz, Tristan, Suomijarvi, Tiina, Supanitsky, A. Daniel, Szadkowski, Zbigniew, Tapia, Alex, Taricco, Carla, Timmermans, Charles, Tkachenko, Olena, Tobiska, Petr, Todero Peixoto, Carlos J., Tomé, Bernardo, Torrès, Zoé, Travaini, Andres, Travnicek, Petr, Trimarelli, Caterina, Tueros, Matias, Ulrich, Ralf, Unger, Michael, Vaclavek, Lukáš, Vacula, Martin, Valdés Galicia, Jose F., Valore, Laura, Varela, Enrique, Vásquez-Ramírez, Adriana, Veberic, Darko, Ventura, Cynthia, Vergara Quispe, Indira D., Verzi, Valerio, Vicha, Jakub, Vink, Jacco, Vorobiov, Serguei, Wahlberg, Hernan, Watanabe Oliveira, Clara Keiko, Watson, Alan, Weber, Marc, Weindl, Andreas, Wiencke, Lawrence, Wilczyński, Henryk, Wirtz, Marcus, Wittkowski, David, Wundheiler, Brian, Yushkov, Alexey, Zapparrata, Orazio, Zas, Enrique, Zavrtanik, Danilo, Zavrtanik, Marko, and Zehrer, Lukas
Subjects: Physics, Pierre Auger Observatory, Photon, Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Galactic Center, Astrophysics::Instrumentation and Methods for Astrophysics, Flux, Computational physics, Auger, Distribution function, Observatory, Experimental High Energy Physics, ddc:530, High Energy Physics, Energy (signal processing)
Abstract: The Pierre Auger Observatory, located in western Argentina, is the world's largest cosmic-ray observatory. While it was originally built to study the cosmic-ray flux above $10^{18.5}~$eV, several enhancements have reduced this energy threshold. One such enhancement is a surface array composed of a triangular grid of $19$ water-Cherenkov detectors separated by $433~$m (SD-433) to explore the energies down to about $10^{16}~$eV. We are developing two research lines employing the SD-433. Firstly, we will measure the energy spectrum in a region where previous experiments have shown evidence of the second knee. Secondly, we will search for ultra-high energy photons to study PeV cosmic-ray sources residing in the Galactic center. In this work, we introduce the SD-433 and we show that it is fully efficient above $5\times 10^{16}~$eV for hadronic primaries with $\theta < 45^\circ$. Using seven years of data, we present the parametrization of the lateral distribution function of measured signals. Finally, we show that an angular resolution of $1.8^\circ$ ($0.5^\circ$) can be attained at the lowest (highest) primary energies. Our study lays the goundmark for measurements in the energy range above $10^{16}~$eV by utilizing the SD-433 and thus expanding the scientific output of the Auger surface detector.
Published: 2021

48. Simulation of up- and down-going neutrino induced showers at the site of the Pierre Auger Observatory

Author: Góra, Dariusz, Roth, Markus, and Tamburro, Alessio
Published: 2008
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49. Muon number rescaling in simulations of air showers

Author: Gora, Dariusz, primary, Borodai, Nataliia, additional, Engel, Ralph, additional, Pierog, Tanguy, additional, Pękala, Jan, additional, Roth, Markus, additional, Stasielak, Jarosław, additional, Unger, Michael, additional, Veberic, Darko, additional, and Wilczyński, Henryk, additional
Published: 2021
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50. The blazar TXS 0506+056 associated with a high-energy neutrino: insights into extragalactic jets and cosmic ray acceleration

Author: Ansoldi, S., Antonelli, L. A., Antonelli, Lucio Angelo, Arcaro, Cornelia, Baack, Dominik, Babić, Ana, Banerjee, Biswajit, Bangale, Priyadarshini, Barres De Almeida, Ulisses, Barrio, Juan Abel, Becerra González, Josefa, Bednarek, Wlodek, Bernardini, Elisa, Berti, Alessio, Bhattacharyya, Wrijupan, Biland, Adrian, Blanch, Oscar, Bonnoli, Giacomo, Carosi, Roberto, Carosi, Alessandro, Ceribella, Giovanni, Chatterjee, Anshu, Colak, Sidika Merve, Colin, Pierre, Colombo, Eduardo, Contreras, Jose Luis, Cortina, Juan, Covino, Stefano, Cumani, Paolo, Da Vela, Paolo, Dazzi, Francesco, De Angelis, Alessandro, De Lotto, Barbara, Delfino, Manuel, Delgado, Jordi, Di Pierro, Federico, Domínguez, Alberto, Dominis Prester, Dijana, Dorner, Daniela, Doro, Michele, Einecke, Sabrina, Elsaesser, Dominik, Fallah Ramazani, Vandad, Fernández-Barral, Alba, Fidalgo, David, Foffano, Luca, Pfrang, Konstantin, Fonseca, Maria Victoria, Font, Lluis, Fruck, Christian, Galindo, Daniel, Gallozzi, Stefano, López, Ramon J. García, Garczarczyk, Markus, Gaug, Markus, Giammaria, Paola, Godinović, Nikola, Gora, Dariusz, Guberman, Daniel, Hadasch, Daniela, Hahn, Alexander, Hassan, Tarek, Hayashida, Masaaki, Herrera, Javier, Hose, Juergen, Hrupec, Dario, Inoue, Susumu, Ishio, Kazuma, Iwamura, Yuki, Konno, Yusuke, Kubo, Hidetoshi, Kushida, Junko, Lelas, Damir, Lindfors, Elina, Lombardi, Saverio, Longo, Francesco, López, Marcos, Maggio, Camilla, Majumdar, Pratik, Makariev, Martin, Maneva, Galina, Manganaro, Marina, Mannheim, Karl, Maraschi, Laura, Mariotti, Mosé, Martínez, Manel, Masuda, Shu, Mazin, Daniel, Minev, Milen, Miranda, Jose Miguel, Mirzoyan, Razmik, Moralejo, Abelardo, Moreno, Victoria, Moretti, Elena, Nagayoshi, Tsutomu, Neustroev, Vitaly, Niedzwiecki, Andrzej, Nievas Rosillo, Mireia, Nigro, Cosimo, Nilsson, Kari, Ninci, Daniele, Nishijima, Kyoshi, Noda, Koji, Nogués, Leyre, Paiano, Simona, Palacio, Joaquim, Paneque, David, Paoletti, Riccardo, Paredes, Josep M., Pedaletti, Giovanna, Peresano, Michele, Persic, Massimo, Prada Moroni, Pier Giorgio, Prandini, Elisa, Puljak, Ivica, Rodriguez Garcia, Jezabel, Reichardt, Ignasi, Rhode, Wolfgang, Ribó, Marc, Rico, Javier, Righi, Chiara, Rugliancich, Andrea, Saito, Takayuki, Satalecka, Konstancja, Schweizer, Thomas, Sitarek, Julian, Snidarić, Iva, Sobczynska, Dorota, Stamerra, Antonio, Strzys, Marcel, Surić, Tihomir, Takahashi, Mitsunari, Tavecchio, Fabrizio, Temnikov, Petar, Terzić, Tomislav, Teshima, Masahiro, Torres-Albà, Nuria, Treves, Aldo, Tsujimoto, Shimpei, Vanzo, Gaia, Vazquez Acosta, Monica, Vovk, Ievgen, Ward, John E., Will, Martin, Zarić, Darko, and Cerruti, Matteo
Subjects: neutrino: energy: high, photon, MAGIC, VHE, blazar, X-ray, messenger, electromagnetic, p: energy, Compton scattering: inverse, gamma ray, electron: interaction, cosmic radiation: acceleration, absorption, plasma
Abstract: The astrophysical journal 863(1), L10 (2018). doi:10.3847/2041-8213/aad083, A neutrino with energy ∼290 TeV, IceCube-170922A, was detected in coincidence with the BL Lac object TXS 0506+056 during enhanced gamma-ray activity, with chance coincidence being rejected at ∼3σ level. We monitored the object in the very-high-energy (VHE) band with the Major Atmospheric Gamma-ray Imaging Cherenkov (MAGIC) telescopes for ∼41 hr from 1.3 to 40.4 days after the neutrino detection. Day-timescale variability is clearly resolved. We interpret the quasi-simultaneous neutrino and broadband electromagnetic observations with a novel one-zone lepto-hadronic model, based on interactions of electrons and protons co-accelerated in the jet with external photons originating from a slow-moving plasma sheath surrounding the faster jet spine. We can reproduce the multiwavelength spectra of TXS 0506+056 with neutrino rate and energy compatible with IceCube-170922A, and with plausible values for the jet power of $\sim 10^{45} - 4 \times 10^{46} erg s^{-1}$. The steep spectrum observed by MAGIC is concordant with internal γγ absorption above ∼100 GeV entailed by photohadronic production of a ∼290 TeV neutrino, corroborating a genuine connection between the multi-messenger signals. In contrast to previous predictions of predominantly hadronic emission from neutrino sources, the gamma-rays can be mostly ascribed to inverse Compton upscattering of external photons by accelerated electrons. The X-ray and VHE bands provide crucial constraints on the emission from both accelerated electrons and protons. We infer that the maximum energy of protons in the jet comoving frame can be in the range $∼10^{14} – 10^{18}$ eV., Published by IOP, Chicago, Ill. [u.a.]
Published: 2018
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