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1. Advances in Understanding High-Mass X-ray Binaries with INTEGRAL and Future Directions

Author

Peter Kretschmar, Felix Furst, Lara Sidoli, Enrico Bozzo, Julia Alfonso-Garzon, Arash Bodaghee, Sylvain Chaty, Masha Chernyakova, Carlo Ferrigno, Antonios Manousakis, Ignacio Negueruela, Konstantin Postnov, Adamantia Paizis, Pablo Reig, Jose Joaquın Rodes-Roca, Sergey Tsygankov, Antony J. Bird, Matthias Bissinger ne’ Kuhnel, Pere Blay, Isabel Caballero, Malcolm J. Coe, Albert Domingo, Victor Doroshenko, Lorenzo Ducci, Maurizio Falanga, Sergei A. Grebenev, Victoria Grinberg, Paul Hemphill, Ingo Kreykenbohm, Sonja Kreykenbohm ne’ Fritz, Jian Li, Alexander A. Lutovinov, Silvia Martınez-Nunez, J. Miguel Mas-Hesse, Nicola Masetti, Vanessa A. McBride, Andrii Neronov, Katja Pottschmidt, Jerome Rodriguez, Patrizia Romano, Richard E. Rothschild, Andrea Santangelo, Vito Sguera, Rudiger Staubert, John A. Tomsick, Jose Miguel Torrejon, Diego F. Torres, Roland Walter, Jorn Wilms, Colleen A. Wilson-Hodge, and Shu Zhang

Subjects
Astronomy
Abstract

High mass X-ray binaries are among the brightest X-ray sources in the Milky Way, as well as in nearby Galaxies. Thanks to their highly variable emissions and complex phenomenology, they have attracted the interest of the high energy astrophysical community since the dawn of X-ray Astronomy. In more recent years, they have challenged our comprehension of physical processes in many more energy bands, ranging from the infrared to very high energies. In this review, we provide a broad but concise summary of the physical processes dominating the emission from high mass X-ray binaries across virtually the whole electromagnetic spectrum. These comprise the interaction of stellar winds with the high gravitational and magnetic fields of compact objects, the behaviour of matter under extreme magnetic and gravity conditions, and the perturbation of the massive star evolutionary processes. We highlight the role of the INTEGRAL mission in the discovery of many of the most interesting objects in the high mass X-ray binary class and its contribution in reviving the interest for these sources over the past two decades. We show how the INTEGRAL discoveries have not only contributed to significantly increase the number of high mass X-ray binaries known, thus advancing our understanding of the population as a whole, but also have opened new windows of investigation that stimulated the multi-wavelength approach nowadays common in most astrophysical research fields. We conclude the review by providing an overview of future facilities being planned from the X-ray to the very high energy domain that will hopefully help us in finding an answer to the many questions left open after more than 18 years of INTEGRAL scientific observations.

Published
2020
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2. Quantitative determination of minimum spanning tree structures: Using the pulsar tree for analyzing the appearance of new classes of pulsars

Author

C R García and Diego F Torres

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

In this work, we introduce a quantitative methodology to define what is the main trunk and what are the significant branches of a minimum spanning tree (MST). We apply it to the pulsar tree, i.e. the MST of the pulsar population constructed upon a Euclidean distance over the pulsar's intrinsic properties. Our method makes use of the betweenness centrality estimator, as well as of non-parametric tests to establish the distinct character of the defined branches. Armed with these concepts, we study how the pulsar population has evolved throughout history, and analyze how to judge whether a new class of pulsars appears in new data, future surveys, or new incarnations of pulsar catalogs., An updated app of the web application we develop for visualizing the pulsar tree can be found at http://www.pulsartree.ice.csic.es

Published
2023

4. AGUTER a platform for automated generation of user acceptance tests from requirements specifications

Author

Leandro Antonelli, Pascale Zaraté, Diego F. Torres, and Guy Camilleri

Subjects
Control and Systems Engineering, business.industry, Computer science, Acceptance testing, Computer Science (miscellaneous), Software engineering, business, Engineering (miscellaneous), Social Sciences (miscellaneous), Theoretical Computer Science
Abstract

PurposeThis article proposes a strategy to make the testing step easier, generating user acceptance tests (UATs) in an automatic way from requirements artifacts.Design/methodology/approachThis strategy is based on two modeling frameworks: scenarios and task/method paradigm. Scenarios are a requirement artifact used to describe business processes and requirements, and task/method paradigm is a modeling paradigm coming from the artificial intelligence field. The proposed strategy is composed of four steps. In the first step, scenarios are described through a semantic wiki website. Then scenarios are automatically translated into a task/method model (step two). In the third step, the task/method model obtained in step two is executed in order to produce and store all possible achievements of tasks and thus scenarios. The stored achievements are saved in a data structure called execution tree (ET). Finally, from this ET (step four), the UATs are generated.FindingsThe feasibility of this strategy is shown through a case study coming from the agriculture production systems field.Originality/valueGenerally, test design approaches deal with a small number of variables describing one specific situation where a decision table or workflow is used to design tests. The proposed approach can deal with many variables because the authors rely on scenarios that can be composed in order to obtain a tree with all the testing paths that can arise from their description.

Published
2021
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5. LHAASO J2226+6057 as a pulsar wind nebula

Author

Agnibha De Sarkar, Wei Zhang, Jonatan Martín, Diego F. Torres, Jian Li, Xian Hou, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), CSIC - Instituto de Ciencias del Espacio (ICE), University of Science and Technology of China, and Chinese Academy of Sciences

Subjects
Radiation mechanisms: non-therma, High Energy Astrophysical Phenomena (astro-ph.HE), Pulsars: general, Space and Planetary Science, Gamma rays: general, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

[Context] The Large High Altitude Air Shower Observatory has reported the detection of cosmic-ray sources in the Milky Way that can accelerate particles up to PeV (=1015 eV) energies. These sources, so-called “PeVatrons”, are mostly unidentified. Several classes of sources, such as supernova remnants, pulsar wind nebula, or young stellar clusters can potentially be the counterparts of these PeVatrons., [Aims] The aim of this work is to study a pulsar wind nebula interpretation of one of these PeVatrons, LHAASO J2226+6057, which has a relatively well covered multifrequency spectrum., [Methods] We have performed a leptonic, time-dependent modeling of the pulsar wind nebula (PWN) associated with PSR J2229+6114 considering a time-energy-dependent diffusion-loss equation. Injection, energy losses, as well as the escape of particles were considered to balance the time-dependent lepton population. We have also included the dynamics of the PWN and the associated supernova remnant and their interaction via the reverse shock to study the reverberation phase of the system., [Results] We have considered different values of the braking index (n) and true age (tage) for the fitting of the MultiWaveLength (MWL) spectral energy distribution (SED) of LHAASO J2226+6057. The best-fit PWN model parameters and their 1σ confidence intervals have been evaluated. We have also demonstrated the impact of reverberation on the MWL SED with increasing time. Additionally, we have discussed the resultant large radius and low magnetic field associated with the PWN in question, as caveats for the possible physical connection of the pulsar as the origin of this high energy source., This work has been supported by grant PID2021-124581OB-I00. D.F.T. acknowledges as well USTC and the Chinese Academy of Sciences Presidential International Fellowship Initiative 2021VMA0001. This work was also supported by the Spanish program Unidad de Excelencia María de Maeztu CEX2020-001058-M.

Published
2022

7. Inferring pulsar periods from synchro-curvature spectra

Author

Daniel Íñiguez-Pascual, Diego F. Torres, Daniele Viganò, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Consejo Superior de Investigaciones Científicas (España), European Research Council, European Commission, and Chinese Academy of Sciences

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

The period and the period derivative of a pulsar are critical magnitudes for defining the properties of the magnetospheric size and plasma dynamics. The pulsar light cylinder, the magnetic field intensity nearby it, and the curvature radius all depend on these timing properties, and shape the observed high-energy synchro-curvature emission. Therefore, the radiative properties of pulsars are inextricably linked to them. This fact poses the question of how well does a given pulsar's spectral energy distribution embed information of the timing parameters, and if so, whether we can deduce them if they have not been measured directly. This is relevant to possibly constrain the timing properties of potential pulsar candidates among unidentified γ-ray sources. We consider well-measured pulsar spectra blinding us from the knowledge of their timing properties, and address this question by using our radiative synchro-curvature model that was proven able to fit the observed spectra of the pulsar population. We find that in the majority of the cases studied (8 out of 13), the spin period is constrained within a range of about 1 order of magnitude, within which the real period lies. In the other cases, there is degeneracy and no period range can be constrained. This can be used to facilitate the blind search of pulsed signals., This work has been supported by the grants PID2021-124581OB-I00, PGC2018-095512-B-I00 as well as the Spanish program Unidad de Excelencia "Mara de Maeztu" CEX2020-001058-M. D.I.P. has been supported by CSIC program JAE-ICU. D.F.T. also acknowledges USTC and the Chinese Academy of Sciences Presidential Fellowship Initiative 2021VMA0001. D.V. is funded by the European Research Council (ERC) under the European Unions Horizon 2020 research and innovation program (ERC Starting Grant IMAGINE, No. 948582).

Published
2022

8. Visualizing the pulsar population using graph theory

Author

C R García, Diego F Torres, Alessandro Patruno, Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Chinese Academy of Sciences, and Universidad Autónoma de Barcelona

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Pulsars: general, Methods: data analysis, Space and Planetary Science, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, Stars: neutron
Abstract

The PP˙ diagram is a cornerstone of pulsar research. It is used in multiple ways for classifying the population, understanding evolutionary tracks, identifying issues in our theoretical reach, and more. However, we have been looking at the same plot for more than five decades. A fresh appraisal may be healthy. Is the PP˙ -diagram the most useful or complete way to visualize the pulsars we know? Here we pose a fresh look at the information we have on the pulsar population. First, we use principal component analysis over magnitudes depending on the intrinsic pulsar’s timing properties (proxies to relevant physical pulsar features), to analyse whether the information contained by the pulsar’s period and period derivative is enough to describe the variety of the pulsar population. Even when the variables of interest depend on P and P˙⁠, we show that PP˙ are not principal components. Thus, any distance ranking or visualization based only on P and P˙ is potentially misleading. Next, we define and compute a properly normalized distance to measure pulsar nearness, calculate the minimum spanning tree of the population, and discuss possible applications. The pulsar tree hosts information about pulsar similarities that go beyond P and P˙⁠, and are thus naturally difficult to read from the PP˙-diagram. We use this work to introduce the pulsar tree website containing visualization tools and data to allow users to gather information in terms of MST and distance ranking., This work has been supported by the grants PID2021-124581OB-I00 and PGC2018-095512-B-I00. CR is funded by the PhD FPI fellowship PRE2019-090828, and acknowledges the graduate program of the Universitat Autònoma of Barcelona. DFT acknowledges as well USTC and the Chinese Academy of Sciences Presidential Fellowship Initiative 2021VMA0001. AP acknowledges partial support from a Ramon y Cajal fellowship RYC-2017-21810. This work was also supported by the Spanish program Unidad de Excelencia María de Maeztu CEX2020-001058-M.

Published
2022
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10. Relevance of non-activity representation in traveling user behavior profiling for adaptive gamification

Author

Diego F. Torres and María Dalponte Ayastuy

Subjects
Computer science, Human–computer interaction, Profiling (information science), Relevance (information retrieval), Collaboration, Representation (mathematics), computer.software_genre, Categorical variable, computer
Abstract

Collaborative location collecting systems (CLCS) are collaborative systems where users collects location-based data. When these systems are gamified and aim to adapt the game elements to each user, it may require a user traveling behavior profile. This work presents two approaches of traveling user behavior profiling: a raw series built up with categorical data that describes the user's activity in a period, and a timed series that is an enhanced version of the first that includes a representation of the non-activity time frames. The profiling of user traveling behavior can be used in adaptive gamification strategies. The approach is evaluated over a behavioral atoms dataset based on a year of Foursquare check-ins. The results showed that both approaches reflex different aspects of traveling user behavior, and also both could be used in a complementary manner.

Published
2021
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11. Physics Performance of the Large Size Telescope prototype of the Cherenkov Telescope Array

Author

Razmik Mirzoyan, Javier Herrera Llorente, Carlos Delgado, Mario Buscemi, M. Cardillo, Jorge Otero-Santos, Julien Houles, Ulisses Barres de Almeida, Debanjan Bose, Luis Ángel Tejedor, Nicola Giglietto, Stefano Truzzi, Ramon Garcia López, Rune Michael Dominik, Darko Zarić, Toni Šarić, D. Dominis Prester, Alicia López-Oramas, Louis Antonelli, Leonardo Di Venere, Karlo Mrakovcic, Petr Travnicek, Junko Kushida, Lea Heckmann, Andres Baquero Larriva, Katsuaki Asano, Josep Maria Paredes, Elena Moretti, Léa Jouvin, Alessia Spolon, Monica Seglar Arroyo, Roland Walter, Kohta Murase, Arnau Aguasca, Alessandra Lamastra, Marina Manganaro, Miroslav Hrabovsky, Alice Donini, Marc Ribó, Alessio Berti, Francesco Longo, Lukas Nickel, Ilaria Viale, Kazuma Ishio, Tomohiro Inada, Federico Di Pierro, P. Thomas Tam, Ievgen Vovk, Jose Enrique Ruiz, Juan Escudero, Marcos López-Moya, Hidetoshi Kubo, Enrique Garcia, Dario Hrupec, Nikola Godinovic, Tokonatsu Yamamoto, David Sanchez, Irene Jiménez Martínez, Ryo Yamazaki, Davide Miceli, Ks Cheng, Halim Ashkar, Andrea Rugliancich, Satoshi Fukami, Michele Doro, Saša Mićanović, Dominik Elsässer, Dalibor Nosek, Juan Abel Barrio, Tarek M. Hassan, Patricia Marquez, Shuichi Gunji, Armand Fiasson, Hiromitsu Takahashi, Yuki Iwamura, Maria Victoria Fonseca, Pol Bordas, Michiyuki Chikawa, Dusan Mandat, Giovanni Lamanna, Oibar Martinez, Martin Tluczykont, Leonardo Baroncelli, David Hui, Michiko Ohishi, Thomas Vuillaume, Jordi Delgado Mengual, Lovro Pavletić, Andrea Bulgarelli, Mabel Bernardos, Hyuga Abe, Tomohiko Oka, R. C. Shellard, Pietro Grespan, Pierre Aubert, Guillaume Deleglise, Michael Prouza, David H. Green, Lluis Freixas Coromina, Takanori Yoshikoshi, Mireia Nievas, Albert Kong, Thomas Schweizer, David Paneque, Yukiho Kobayashi, Ladislav Chytka, Mario Pecimotika, Juliane Scherpenberg, Edgar Molina, Yating Chai, Oscar Blanch, Masahiro Teshima, Martin Makariev, Pratik Majumdar, M. I. Martínez, Miroslav Pech, Nao Okazaki, Vassil Verguilov, Daniel Nieto, Josefa Becerra Gonzalez, Shuta Tanaka, Moritz Hütten, Daniela Hadasch, Yusuke Suda, Miguel Polo, W. Rhode, Manuel Artero, Alexander Hahn, Aya Bamba, Tsunefumi Mizuno, Fuyuki Tokanai, Thomas Armstrong, Michele Palatiello, Elisa Prandini, Tatsuo Yoshida, Matteo Cerruti, Kohei Hayashi, Karl Mannheim, M. Nöthe, Jose Luis Contreras, Daniel Morcuende, Mykhailo Dalchenko, Kyoshi Nishijima, Gilles Maurin, Marcel Strzys, Franca Cassol, Maurizio Iori, Carlos Díaz, Mika Kagaya, Luis David Medina Miranda, Yasushi Fukazawa, Giacomo Bonnoli, German Martinez, Matthieu Heller, Gaia Verna, Enrique Mestre Guillen, Giovanni Marsella, Jonas Hackfeld, Martin Vacula, Pedro L. Luque-Escamilla, Riccardo Paoletti, Juan Cortina, Yoshiki Ohtani, Vincent Poireau, Francesco Gabriele Saturni, Alessandro Carosi, Ali Baktash, Irene Burelli, Carla Aramo, Vincenzo Rizi, Ruben Lopez-Coto, Jakub Juryšek, Takeshi Nakamori, Jumpei Takata, Ivana Batković, Francesco Giordano, Dai Tateishi, Vincenzo Vitale, Pawel Gliwny, Jose Miguel Miranda, Yuji Sunada, A. Morselli, Julie Prast, Alvaro Mas, Chaitanya Priyadarshi, Tomislav Terzić, Yusuke Inome, Mitsunari Takahashi, Vladimir Karas, Daniel Kerszberg, Monica Vazquez Acosta, Fabian Schüssler, Daniel Mazin, Yukikatsu Terada, Diego F. Torres, Ciro Bigongiari, Alessandro De Angelis, Teresa Montaruli, Riccardo Rando, Daniela Dorner, Abelardo Moralejo, Dieter Horns, Hideaki Katagiri, Ryuji Takeishi, Noah Biederbeck, Vitalii Sliusar, Bernd Schleicher, K. Hirotani, Hiroyasu Tajima, Gabriel Emery, Petar Temnikov, Jelena Strišković, Koji Noda, Dirk Hoffmann, Carlo Francesco Vigorito, Jun Kataoka, Sami Caroff, Josep Martí, Tjark Miener, Martin Will, Mikael Jacquemont, Luca Foffano, Akira Okumura, Julian Sitarek, D. della Volpe, Heide Costantini, Takashi Saito, I. Agudo, Andrii Nagai, Mosè Mariotti, Reiko Orito, Inocencio Monteiro, Thierry Le Flour, Jan Lukas Schubert, Mathieu de Bony de Lavergne, Petra Marusevec, Davide Depaoli, Shunsuke Sakurai, and Seiya Nozaki

Subjects
Physics, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, Astronomy, Cherenkov Telescope Array, law.invention, Telescope, Crab Nebula, law, Astrophysics::Solar and Stellar Astrophysics, Astrophysics::Galaxy Astrophysics, Large size
Abstract

The Large-Sized Telescope (LST) prototype of the future Cherenkov Telescope Array (CTA) is located at the Northern site of CTA, on the Canary Island of La Palma. It is designed to provide optimal performance in the lowest part of the energy range covered by CTA, observing gamma rays down to energies of tens of GeV. The LST prototype started performing astronomical observations in November 2019 during the commissioning of the telescope and it has been taking data since then. In this contribution, we will present the tuning of the characteristics of the telescope in the Monte Carlo (MC) simulations to describe the data obtained, the estimation of its angular and energy resolution, and an evaluation of its sensitivity, both with simulations and with observations of the Crab Nebula.

Published
2021
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12. Fermi Large Area Telescope Performance After 10 Years Of Operation

Author

Soebur Razzaque, R. Buehler, T. A. Porter, J. Li, Peter F. Michelson, Marcello Giroletti, L. Tibaldo, F. Piron, Denis Bastieri, N. Saggini, N. Di Lalla, G. Tosti, Dario Gasparrini, Francesco Longo, A. Fiori, Stefan Larsson, J. G. Thayer, Ioannis Liodakis, F. Fana Dirirsa, W. B. Atwood, Luca Baldini, J. S. Perkins, M. Ceccanti, Alessandro Brez, D. Serini, Sylvain Guiriec, Stefano Ciprini, Mn Mazziotta, S. Rainò, Tsunefumi Mizuno, G. Foglia, M. Razzano, Johann Cohen-Tanugi, J. Bregeon, Sina Chen, L. Di Venere, Michele Pinchera, T. J. Johnson, Seth Digel, Elliott D. Bloom, F. Loparco, M. N. Lovellette, M.-H. Grondin, F. Gargano, Hiroyasu Tajima, R. Primavera, Ronaldo Bellazzini, J. E. Grove, Yasushi Fukazawa, E. Orlando, M. Lemoine-Goumard, Marco Ajello, E. Rapposelli, Roopesh Ojha, Denise A. Smith, E. Hays, P. M. Saz Parkinson, E. J. Siskind, G. Principe, Manuel Meyer, P. Fusco, N. Menon, Diego F. Torres, Melissa Pesce-Rollins, J. Valverde, Matthew Kerr, Elisabetta Bissaldi, H. Poon, M. Orienti, S. Buson, Vaidehi S. Paliya, D. J. Thompson, D. Fabiani, Carmelo Sgrò, Riccardo Rando, Magnus Axelsson, A. Reimer, Massimo Minuti, S. Maldera, J. J. Russell, Warit Mitthumsiri, R. Bagagli, S. Griffin, F. D'Ammando, T. Kamae, G. Martí-Devesa, Z. Pei, E. Cavazzuti, E. Nuss, David Paneque, P. Spinelli, T. Glanzman, M. Bagni, F. de Palma, Alessandro Paccagnella, M. Kuss, Aaron Dominguez, M. Mongelli, Luca Latronico, Igor V. Moskalenko, Gloria Spandre, N. Scolieri, R. A. Cameron, G. Jóhannesson, Gabrijela Zaharijas, Alberto Manfreda, L. Vigiani, Bindu Rani, P. Bruel, Ismaël Cognard, Olaf Reimer, D. Horan, P. de la Torre Luque, L. Guillemot, M. E. Monzani, F. Bellardi, Elizabeth C. Ferrara, David A. Green, I. Mereu, P. Caraveo, S. Cutini, D. J. Suson, C. C. Cheung, R. Bonino, P. Lubrano, M. Gustafsson, J. L. Racusin, M. Negro, Laboratoire de Physique Subatomique et de Cosmologie (LPSC), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP ), Université Grenoble Alpes (UGA), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace (LPC2E), Observatoire des Sciences de l'Univers en région Centre (OSUC), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Centre National de la Recherche Scientifique (CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers en région Centre (OSUC), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Astrophysique de Bordeaux [Pessac] (LAB), Université de Bordeaux (UB)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS), Ajello, M., Atwood, W. B., Axelsson, M., Bagagli, R., Bagni, M., Baldini, L., Bastieri, D., Bellardi, F., Bellazzini, R., Bissaldi, E., Bloom, E. D., Bonino, R., Bregeon, J., Brez, A., Bruel, P., Buehler, R., Buson, S., Cameron, R. A., Caraveo, P. A., Cavazzuti, E., Ceccanti, M., Chen, S., Cheung, C. C., Ciprini, S., Cognard, I., Cohen-Tanugi, J., Cutini, S., D???ammando, F., de la Torre Luque, P., de Palma, F., Digel, S. W., Dirirsa, F., Di Lalla, N., Di Venere, L., Dom??nguez, A., Fabiani, D., Ferrara, E. C., Fiori, A., Foglia, G., Fukazawa, Y., Fusco, P., Gargano, F., Gasparrini, D., Giroletti, M., Glanzman, T., Green, D., Griffin, S., Grondin, M. -H., Grove, J. E., Guillemot, L., Guiriec, S., Gustafsson, M., Hays, E., Horan, D., J??hannesson, G., Johnson, T. J., Kamae, T., Kerr, M., Kuss, M., Larsson, S., Latronico, L., Lemoine-Goumard, M., Li, J., Liodakis, I., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Maldera, S., Manfreda, A., Mart??-Devesa, G., Mazziotta, M. N., Menon, N., Mereu, I., Meyer, M., Michelson, P. F., Minuti, M., Mitthumsiri, W., Mizuno, T., Mongelli, M., Monzani, M. E., Moskalenko, I. V., Negro, M., Nuss, E., Ojha, R., Orienti, M., Orlando, E., Paccagnella, A., Paliya, V. S., Paneque, D., Pei, Z., Perkins, J. S., Pesce-Rollins, M., Pinchera, M., Piron, F., Poon, H., Porter, T. A., Primavera, R., Principe, G., Racusin, J. L., Rain??, S., Rando, R., Rani, B., Rapposelli, E., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Russell, J. J., Saggini, N., Saz Parkinson, P. M., Scolieri, N., Serini, D., Sgr??, C., Siskind, E. J., Smith, D. A., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. G., Thompson, D. J., Tibaldo, L., Torres, D. F., Tosti, G., Valverde, J., Vigiani, L., and Zaharijas, G.

Subjects
Calibration (statistics), Gamma-ray telescopes, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, 030226 pharmacology & pharmacy, 01 natural sciences, 7. Clean energy, law.invention, Telescope, 03 medical and health sciences, 0302 clinical medicine, law, 0103 physical sciences, Instrumentation and Methods for Astrophysics (astro-ph.IM), 010303 astronomy & astrophysics, Condensed Matter::Quantum Gases, Physics, Gamma-ray astronomy, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, Space and Planetary Science, [SDU]Sciences of the Universe [physics], Calibration, Condensed Matter::Strongly Correlated Electrons, Astrophysics - Instrumentation and Methods for Astrophysics, Fermi Gamma-ray Space Telescope
Abstract

The Large Area Telescope (LAT), the primary instrument for the Fermi Gamma-ray Space Telescope (Fermi) mission, is an imaging, wide field-of-view, high-energy gamma-ray telescope, covering the energy range from 30 MeV to more than 300 GeV. We describe the performance of the instrument at the 10-year milestone. LAT performance remains well within the specifications defined during the planning phase, validating the design choices and supporting the compelling case to extend the duration of the Fermi mission. The details provided here will be useful when designing the next generation of high-energy gamma-ray observatories., 60 pages, 28 figures. Published in ApJS

Published
2021
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13. A novel approach for the analysis of the geometry involved in determining light curves of pulsars

Author

Daniele Viganò and Diego F. Torres

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Electromagnetic spectrum, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Tangent, Magnetosphere, Astronomy and Astrophysics, Geometry, Observable, Light curve, Differential geometry, Pulsar, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Reference frame
Abstract

In this work, we introduce the use of the differential geometry Frenet-Serret equations to describe a magnetic line in a pulsar magnetosphere. These equations, which need to be solved numerically, fix the magnetic line in terms of their tangent, normal, and binormal vectors at each position, given assumptions on the radius of curvature and torsion. Once the representation of the magnetic line is defined, we provide the relevant set of transformations between reference frames; the ultimate aim is to express the map of the emission directions in the star co-rotating frame. In this frame, an emission map can be directly read as a light curve seen by observers located at a certain fixed angle with respect to the rotational axis. We provide a detailed step-by-step numerical recipe to obtain the emission map for a given emission process, and give a set of simplified benchmark tests. Key to our approach is that it offers a setting to achieve an effective description of the system's geometry {\it together} with the radiation spectrum. This allows to compute multi-frequency light curves produced by a specific radiation process (and not just geometry) in the pulsar magnetosphere, and intimately relates with averaged observables such as the spectral energy distribution., Comment: Accepted for publication in MNRAS

Published
2019
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14. Probing the hadronic nature of the gamma-ray emission associated with Westerlund 2

Author

Pablo Saz Parkinson, Ruizhi Yang, Emma de Oña Wilhelmi, Roberta Zanin, Ullrich Schwanke, Felix Aharonian, Tim Holch, Diego F. Torres, and Enrique Mestre

Subjects
p p: scattering, gamma-rays: stars, accelerator, indivisdual: Westerlund 2 [open clusters and association], Astrophysics::High Energy Astrophysical Phenomena, Hadron, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, GeV, Radiation, GLAST, stars [gamma-rays], Acceleration, cosmic rays, emission [gamma ray], HESS, scattering [p p], Cluster (physics), TeV, ddc:530, cosmic radiation: acceleration, winds, outflows [stars], cluster, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), stars: winds, outflows, Gamma ray, Astronomy and Astrophysics, Galaxy, gamma ray: emission, Space and Planetary Science, cosmic radiation: galaxy, open clusters and association: indivisdual: Westerlund 2, ddc:520, galaxy [cosmic radiation], spectral, Physics::Accelerator Physics, acceleration [cosmic radiation], Astrophysics - High Energy Astrophysical Phenomena
Abstract

Monthly notices of the Royal Astronomical Society 505(2), 2731 - 2740 (2021). doi:10.1093/mnras/stab1455, Star-forming regions have been proposed as potential Galactic cosmic ray accelerators for decades. Cosmic ray acceleration can be probed through observations of gamma-rays produced in inelastic proton–proton collisions at GeV and TeV energies. In this paper, we analyse more than 11 yr of Fermi–LAT data from the direction of Westerlund 2, one of the most massive and best-studied star-forming regions in our Galaxy. In particular, we investigate the characteristics of the bright pulsar PSR J1023–5746 that dominates the gamma-ray emission below a few GeV at the position of Westerlund 2 and the underlying extended source FGES J1023.3–5747. The analysis results in a clear identification of FGES J1023.3–5747 as the GeV counterpart of the TeV source HESS J1023-575, through its morphological and spectral properties. This identification provides new clues about the origin of the HESS J1023-575 gamma-ray emission, favouring a hadronic origin of the emission, powered by Westerlund 2, rather than a leptonic origin related to either the pulsar wind nebula associated with PSR J1023–5746 or the cluster itself. This result indirectly supports the hypothesis that star-forming regions can contribute to the cosmic ray sea observed in our Galaxy., Published by Oxford Univ. Press, Oxford

Published
2021
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15. Adaptive Gamification in Collaborative systems, a Systematic Mapping Study

Author

Diego F. Torres, María Dalponte Ayastuy, and Alejandro Fernández

Subjects
General Computer Science, Computer science, Ciencias Informáticas, 0102 computer and information sciences, 02 engineering and technology, computer.software_genre, 01 natural sciences, Adaptive gamification, Field (computer science), Theoretical Computer Science, Personalization, Collaborative systems, Taxonomy (general), 0202 electrical engineering, electronic engineering, information engineering, Citizen science, Adaptation (computer science), Structure (mathematical logic), Data science, Ciencias de la Computación, Mass collaboration, 010201 computation theory & mathematics, Systematic mapping, 020201 artificial intelligence & image processing, Collaboration, computer
Abstract

Mass collaboration mediated by technology is now commonplace (Wikipedia, Quora, TripAdvisor). Online, mass collaboration is also present in science in the form of Citizen Science. These collaboration models, which have a large community of contributors coordinated to pursue a common goal, are known as Collaborative systems. This article introduces a study of the published research on the application of adaptive gamification to collaborative systems. The study focuses on works that explicitly discuss an approach of personalization or adaptation of the gamification elements in this type of system. It employs a systematic mapping design in which a categorical structure for classifying the research results is proposed based on the topics that emerged from the papers review. The main contributions of this paper are a formalization of the adaptation strategies and the proposal of a new taxonomy for gamification elements adaptation. The results evidence the lack of research literature in the study of adapting gamification in the field of collaborative systems. Considering the underlying cultural diversity in those projects, the adaptability of gamification design and strategies is a promissory research field., Laboratorio de Investigación y Formación en Informática Avanzada

Published
2021

16. Revisiting the evolution of nonradiative supernova remnants: A hydrodynamical-informed parameterization of the shock positions

Author

Niccolò Bucciantini, B. Olmi, J. M. Martin, Diego F. Torres, Rino Bandiera, Ministerio de Ciencia, Innovación y Universidades (España), ITA, and ESP

Subjects
Physics, Shock wave, High Energy Astrophysical Phenomena (astro-ph.HE), numerical [Methods], Methods: numerical, supernova remnants [ISM], Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astronomy and Astrophysics, Context (language use), Astrophysics, Pulsar wind nebula, Shock waves, Supernova, Pulsar, Space and Planetary Science, Radiative transfer, Hydrodynamics, Astrophysics::Solar and Stellar Astrophysics, Ejecta, Supernova remnant, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants
Abstract

Understanding the evolution of a supernova remnant shell in time is fundamental. Such understanding is critical to build reliable models of the dynamics of the supernova remnant shell interaction with any pulsar wind nebula it might contain. Here, we perform a large study of the parameter space for the one-dimensional spherically symmetric evolution of a supernova remnant, accompanying it by analytical analysis. Assuming, as is usual, an ejecta density profile with a power-law core and an envelope, and a uniform ambient medium, we provide a set of highly-accurate approximations for the evolution of the main structural features of supernova remnants, such as the reverse and forward shocks and the contact discontinuity. We compare our results with previously adopted approximations, showing that existing simplified prescriptions can easily lead to large errors. In particular, in the context of pulsar wind nebulae modelling, an accurate description for the supernova remnant reverse shock is required. We also study in depth the self-similar solutions for the initial phase of evolution, when the reverse shock propagates through the envelope of the ejecta. Since these self-similar solutions are exact, but not fully analytical, we here provide highly-accurate approximations as well., Comment: 15 pages, 8 figures, 6 tables

Published
2021
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17. Optical and ultraviolet pulsed emission from an accreting millisecond pulsar

Author

F. Coti Zelati, Maria Cristina Baglio, Fraser Lewis, A. L. Riverol Rodriguez, A. Miraval Zanon, Luciano Burderi, D. de Martino, M. Cecconi, Filippo Ambrosino, M. Cadelano, Piergiorgio Casella, David M. Russell, Paolo Cretaro, H. Perez Ventura, D. M. Bramich, M. Hernandez Diaz, Roberto Mignani, J. J. San Juan, Alessandro Papitto, Steven E. Campana, P. D'Avanzo, A. Sanna, Diego F. Torres, M. D. Gonzalez Gomez, Ennio Poretti, Franco Meddi, Adriano Ghedina, T. Di Salvo, G. L. Israel, Francesco Leone, Lorenzo Stella, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Ambrosino F., Miraval Zanon A., Papitto A., Coti Zelati F., Campana S., D'Avanzo P., Stella L., Di Salvo T., Burderi L., Casella P., Sanna A., de Martino D., Cadelano M., Ghedina A., Leone F., Meddi F., Cretaro P., Baglio M.C., Poretti E., Mignani R.P., Torres D.F., Israel G.L., Cecconi M., Russell D.M., Gonzalez Gomez M.D., Riverol Rodriguez A.L., Perez Ventura H., Hernandez Diaz M., San Juan J.J., Bramich D.M., and Lewis F.

Subjects
Angular momentum, 010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Magnetosphere, FOS: Physical sciences, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Luminosity, Neutron stars, Settore FIS/05 - Astronomia E Astrofisica, Pulsar, Millisecond pulsar, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, High Energy Astrophysical Phenomena, 0105 earth and related environmental sciences, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astronomy and Astrophysics, Accretion (astrophysics), Particle acceleration, Neutron star, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena
Abstract

Ambrosino, F., et al., Millisecond spinning, low-magnetic-field neutron stars are believed to attain their fast rotation in a 0.1–1-Gyr-long phase during which they accrete matter endowed with angular momentum from a low-mass companion star. Despite extensive searches, coherent periodicities originating from accreting neutron star magnetospheres have been detected only at X-ray energies and in ~10% of the currently known systems. Here we report the detection of optical and ultraviolet coherent pulsations at the X-ray period of the transient low-mass X-ray binary system SAX J1808.4−3658, during an accretion outburst that occurred in August 2019. At the time of the observations, the pulsar was surrounded by an accretion disk, displayed X-ray pulsations and its luminosity was consistent with magnetically funnelled accretion onto the neutron star. Current accretion models fail to account for the luminosity of both optical and ultraviolet pulsations; these are instead more likely to be driven by synchro-curvature radiation in the pulsar magnetosphere or just outside of it. This interpretation would imply that particle acceleration can take place even when mass accretion is going on, and opens up new perspectives in the study of coherent optical/ultraviolet pulsations from fast-spinning accreting neutron stars in low-mass X-ray binary systems., A.M.Z. thanks the HST contact scientist, D. Welty (STScI), for constant support in the observation planning and T. Royle (STScI) for checking the scheduling processes. A.M.Z. thanks A. Riley (STIS Team) for the support in the scientific data analysis. A.M.Z. acknowledges the support of the PHAROS COST Action (CA16214) and A. Ridolfi for his help in data analysis. A.M.Z. would also like to thank G. Benevento for comments on draft. F.C.Z. is supported by a Juan de la Cierva fellowship. S.C. and P.D.A. acknowledge support from ASI grant I/004/11/3. D.d.M., A.P. and L.S. acknowledge financial support from the Italian Space Agency (ASI) and National Institute for Astrophysics (INAF) under agreements ASI-INAF I/037/12/0. L.B., D.d.M., T.D.S., A.P. and L.S. acknowledge financial contributions from ASI-INAF agreement no. 2017-14-H.0, INAF main-stream (principal investigator: T. Belloni; principal investigator: A. De Rosa). D.F.T. acknowledges support from grants PGC2018-095512-B-I00, SGR2017-1383 and AYA2017-92402-EXP. L.B and T.D.S. thank A. Marino for useful discussions and acknowledge financial contributions from the HERMES project financed by the Italian Space Agency (ASI) agreement no. 2016/13 U.O. T.D.S. and L.S. acknowledge the iPeska research grant (principal investigator: A. Possenti) funded under the INAF national call Prin-SKA/CTA approved with the Presidential Decree 70/2016. A.P., F.C.Z., and D.T. acknowledge the International Space Science Institute (ISSI-Beijing), which funded and hosted the international team ‘Understanding and Unifying the Gamma-rays Emitting Scenarios in High Mass and Low Mass X-ray Binaries’.

Published
2021

18. Development of an advanced SiPM camera for the Large Size Telescope of the Cherenkov TelescopeArray Observatory

Author

Miroslav Hrabovsky, Ks Cheng, Michiyuki Chikawa, Shuichi Gunji, David H. Green, Rune Michael Dominik, R. C. Shellard, W. Rhode, Davide Miceli, Juliane van Scherpenberg, Daniela Dorner, Alexander Hahn, Alessia Spolon, Léa Jouvin, Noah Biederbeck, Vladimir Karas, Maurizio Iori, Aya Bamba, D. Dominis Prester, Arnau Aguasca, Mykhailo Dalchenko, Ryuji Takeishi, Dominik Elsässer, Vassil Verguilov, Daniel Mazin, Alessandro De Angelis, Enrique Garcia, Vitalii Sliusar, David Sanchez, Yukikatsu Terada, Teresa Montaruli, Gabriel Emery, Petar Temnikov, Juan Escudero, Enrique Mestre Guillen, Koji Noda, Dirk Hoffmann, Julien Houles, Francesco Longo, Pol Bordas, Hyuga Abe, Yuji Sunada, Dieter Horns, Ievgen Vovk, Leonardo Baroncelli, Akira Okumura, Dario Hrupec, Alessandra Lamastra, Armand Fiasson, Hiromitsu Takahashi, Patricia Marquez, Gaia Verna, Vincenzo Vitale, M. Cardillo, Oibar Martinez, Marcel Strzys, Julian Sitarek, Pierre Aubert, Heide Costantini, Jonas Hackfeld, Fuyuki Tokanai, Juan Abel Barrio, Dusan Mandat, Mitsunari Takahashi, Martin Makariev, Tomohiko Oka, Oscar Blanch, Mireia Nievas, Daniela Hadasch, Yusuke Inome, Daniel Morcuende, Jose Luis Contreras, Tokonatsu Yamamoto, Miguel Polo, Marina Manganaro, Shuta Tanaka, Kohta Murase, Inocencio Monteiro, Kyoshi Nishijima, Tsunefumi Mizuno, Ali Baktash, Yoshiki Ohtani, Juan Cortina, Matteo Cerruti, Marcos López-Moya, Takeshi Nakamori, Martin Vacula, Alessandro Carosi, Shunsuke Sakurai, Gilles Maurin, Federico Di Pierro, Luis David Medina Miranda, Alice Donini, Ruben Lopez-Coto, Vincent Poireau, Lukas Nickel, Kazuma Ishio, Carlos Díaz, Yasushi Fukazawa, Andrea Bulgarelli, Diego F. Torres, Ciro Bigongiari, Jumpei Takata, Elena Moretti, Irene Jiménez Martínez, Dai Tateishi, Jakub Juryšek, Pratik Majumdar, Luis Ángel Tejedor, Jose Miguel Miranda, Michele Doro, Thomas Schweizer, Guillaume Deleglise, Mabel Bernardos, Ladislav Chytka, Mario Pecimotika, Elisa Prandini, Riccardo Rando, Martin Will, Chaitanya Priyadarshi, Jorge Otero-Santos, Pedro L. Luque-Escamilla, Riccardo Paoletti, Seiya Nozaki, Tjark Miener, David Paneque, German Martinez, Daniel Kerszberg, Jan Lukas Schubert, Satoshi Fukami, Dalibor Nosek, Jelena Strišković, P. Thomas Tam, Stefano Truzzi, Michele Palatiello, Ulisses Barres de Almeida, Josep M. Paredes, Petra Marusevec, David Hui, Halim Ashkar, Franca Cassol, Jun Kataoka, Sami Caroff, Junko Kushida, Takanori Yoshikoshi, A. Morselli, Masahiro Teshima, Saša Mićanović, Monica Seglar Arroyo, Lovro Pavletić, Tarek M. Hassan, Marc Ribó, Ivana Batković, R. Walter, Ilaria Viale, Kohei Hayashi, Giovanni Lamanna, Hidetoshi Kubo, Tomohiro Inada, Josep Martí, Abelardo Moralejo, Hideaki Katagiri, Michiko Ohishi, Thomas Vuillaume, Bernd Schleicher, Edgar Molina, K. Hirotani, Hiroyasu Tajima, Mika Kagaya, Matthieu Heller, Giovanni Marsella, Pietro Grespan, Lluis Freixas Coromina, Louis Antonelli, Nao Okazaki, Daniel Nieto, Moritz Hütten, Ramon J. García López, Martin Tluczykont, Michael Prouza, Razmik Mirzoyan, Carlos Delgado, Lea Heckmann, Francesco Gabriele Saturni, Yating Chai, Andrii Nagai, Mosè Mariotti, Pawel Gliwny, Nicola Giglietto, Darko Zarić, Toni Šarić, Andrea Rugliancich, Mathieu de Bony de Lavergne, Javier Herrera Llorente, Mario Buscemi, Karlo Mrakovcic, Petr Travnicek, Monica Vazquez Acosta, Mikael Jacquemont, Luca Foffano, D. della Volpe, Karl Mannheim, M. Nöthe, Alicia López-Oramas, Alessio Berti, Fabian Schüssler, Julie Prast, Alvaro Mas, Manuel Artero, Tomislav Terzić, Andres Baquero Larriva, Katsuaki Asano, Maria Victoria Fonseca, Albert Kong, M. I. Martínez, Miroslav Pech, Jose Enrique Ruiz, Nikola Godinovic, Yusuke Suda, Carlo Vigorito, Ryo Yamazaki, Thomas Armstrong, Tatsuo Yoshida, Davide Depaoli, Irene Burelli, Carla Aramo, Vincenzo Rizi, Leonardo Di Venere, Thierry Le Flour, Jordi Delgado Mengual, Francesco Giordano, Yuki Iwamura, Takashi Saito, I. Agudo, Reiko Orito, Yukiho Kobayashi, Giacomo Bonnoli, Debanjan Bose, and Josefa González

Subjects
Telescope, Photomultiplier, Silicon photomultiplier, Pixel, Duty cycle, Computer science, law, Observatory, Electronic engineering, Cherenkov Telescope Array, Cherenkov radiation, law.invention
Abstract

Silicon photomultipliers (SiPMs) have become the baseline choice for cameras of the small-sized telescopes (SSTs) of the Cherenkov Telescope Array (CTA). On the other hand, SiPMs are relatively new to the field and covering large surfaces and operating at high data rates still are challenges to outperform photomultipliers (PMTs). The higher sensitivity in the near infra-red and longer signals compared to PMTs result in higher night sky background rate for SiPMs. However, the robustness of the SiPMs represents a unique opportunity to ensure long-term operation with low maintenance and better duty cycle than PMTs. The proposed camera for large size telescopes will feature 0.05 degree pixels, low power and fast front-end electronics and a fully digital readout. In this work, we present the status of dedicated simulations and data analysis for the performance estimation. The design features and the different strategies identified, so far, to tackle the demanding requirements and the improved performance are described.

Published
2021

19. The Crab nebula variability at short time-scales with the Cherenkov telescope array

Author

Dmitry Khangulyan, Diego F. Torres, E. de Oña Wilhelmi, Enrique Mestre, Fabio Acero, Roberta Zanin, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), Generalitat de Catalunya, Alexander von Humboldt Foundation, Japan Society for the Promotion of Science, and Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Cherenkov Telescope Array, model [emission], threshold [detector], Astrophysics, GeV, detectors -stars, 01 natural sciences, law.invention, energy: threshold, law, Astrophysics::Solar and Stellar Astrophysics, individual, flare, 010303 astronomy & astrophysics, detectors [Instrumentation], Physics, High Energy Astrophysical Phenomena (astro-ph.HE), instrumentation, Nebula, energy: high, Astrophysics::Instrumentation and Methods for Astrophysics, threshold [energy], flare [Stars], detector: threshold, Supernova, gamma ray: emission, supernovae: individual: Crab Nebula, high [energy], Spectral energy distribution, individual: Crab Nebula [Supernovae], stars: flare, Crab Nebula -stars, Astrophysics - High Energy Astrophysical Phenomena, Flare, supernovae, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, determinant, GLAST, emission: model, emission [gamma ray], 0103 physical sciences, TeV, 010306 general physics, Cherenkov radiation, Astrophysics::Galaxy Astrophysics, instrumentation: detectors, Astronomy and Astrophysics, Crab Nebula, Cherenkov counter, 13. Climate action, Space and Planetary Science, ddc:520, spectral, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract

Monthly notices of the Royal Astronomical Society 509(1), 337 - 346 (2020). doi:10.1093/mnras/staa3599, Since 2009, several rapid and bright flares have been observed at high energies (>100 MeV) from the direction of the Crab Nebula. Several hypotheses have been put forward to explain this phenomenon, but the origin is still unclear. The detection of counterparts at higher energies with the next generation of Cherenkov telescopes will be determinant to constrain the underlying emission mechanisms. We aim at studying the capability of the Cherenkov Telescope Array (CTA) to explore the physics behind the flares, by performing simulations of the Crab Nebula spectral energy distribution, both in flaring and steady state, for different parameters related to the physical conditions in the nebula. In particular, we explore the data recorded by Fermi during two particular flares that occurred in 2011 and 2013. The expected GeV and TeV gamma-ray emission is derived using different radiation models. The resulting emission is convoluted with the CTA response and tested for detection, obtaining an exclusion region for the space of parameters that rule the different flare emission models. Our simulations show different scenarios that may be favourable for achieving the detection of the flares in Crab with CTA, in different regimes of energy. In particular, we find that observations with low sub-100 GeV energy threshold telescopes could provide the most model-constraining results., Published by Oxford Univ. Press, Oxford

Published
2021
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20. Gamma Rays from Fast Black-hole Winds

Author

M. Razzano, Francesco Longo, J. Zrake, S. Buson, Junyao Li, A. Franckowiak, Elisabetta Bissaldi, Diego F. Torres, N. Di Lalla, Luca Baldini, Aaron Dominguez, M. E. Monzani, Sylvain Guiriec, Mn Mazziotta, C. Karwin, Alberto Manfreda, Bindu Rani, Denis Bastieri, Nicola Omodei, F. D'Ammando, G. Jóhannesson, P. M. Saz Parkinson, A. Desai, S. Marchesi, D. Costantin, Peter F. Michelson, Marcello Giroletti, M. Orienti, Marco Ajello, Damiano Caprioli, A. Berretta, Sina Chen, A. Reimer, Igor V. Moskalenko, Olaf Reimer, Carmelo Sgrò, Riccardo Rando, Miloš Kovačević, Z. Pei, A. Morselli, Melissa Pesce-Rollins, Rebecca Diesing, Stefan Larsson, J. L. Racusin, David Paneque, G. Chiaro, M. Kuss, Vaidehi S. Paliya, P. Spinelli, L. Marcotulli, T. A. Porter, G. Principe, S. Maldera, P. Fusco, G. Martí-Devesa, F. de Palma, Francesco Giordano, M. Negro, Dario Gasparrini, J. Ballet, Roger Blandford, I. Mereu, F. Loparco, Matthew Kerr, E. Orlando, S. J. Fegan, Dieter H. Hartmann, S. Cutini, David A. Green, Stefan Funk, D. Horan, George Chartas, Massimo Persic, Regina Caputo, Ronaldo Bellazzini, D. Serini, R. A. Cameron, Nicola Giglietto, P. Lubrano, I. A. Grenier, Guido Barbiellini, P. Bruel, D. Tak, M. N. Lovellette, Ioannis Liodakis, S. Rainò, Tsunefumi Mizuno, Yasushi Fukazawa, Gabrijela Zaharijas, K. S. Wood, E. Troja, Elliott D. Bloom, R. Bonino, E. J. Siskind, D. J. Suson, Luca Latronico, C. C. Cheung, P. de la Torre Luque, F. Gargano, E. Cavazzuti, Gloria Spandre, F. Dirirsa, L. Di Venere, M. Lemoine-Goumard, National Aeronautics and Space Administration (US), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, Ajello, M., Baldini, L., Ballet, J., Barbiellini, G., Bastieri, D., Bellazzini, R., Berretta, A., Bissaldi, E., Blandford, R. D., Bloom, E. D., Bonino, R., Bruel, P., Buson, S., Cameron, R. A., Caprioli, D., Caputo, R., Cavazzuti, E., Chartas, G., Chen, S., Cheung, C. C., Chiaro, G., Costantin, D., Cutini, S., D'Ammando, F., De La Torre Luque, P., De Palma, F., Desai, A., Diesing, R., Di Lalla, N., Dirirsa, F., Di Venere, L., Dominguez, A., Fegan, S. J., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Green, D., Grenier, I. A., Guiriec, S., Hartmann, D., Horan, D., Johannesson, G., Karwin, C., Kerr, M., Kovacevic, M., Kuss, M., Larsson, S., Latronico, L., Lemoine-Goumard, M., Li, J., Liodakis, I., Longo, F., Loparco, F., Lovellette, M. N., Lubrano, P., Maldera, S., Manfreda, A., Marchesi, S., Marcotulli, L., Marti-Devesa, G., Mazziotta, M. N., Mereu, I., Michelson, P. F., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Omodei, N., Orienti, M., Orlando, E., Paliya, V., Paneque, D., Pei, Z., Persic, M., Pesce-Rollins, M., Porter, T. A., Principe, G., Racusin, J. L., Rain, S., Rando, R., Rani, B., Razzano, M., Reimer, A., Reimer, O., Saz Parkinson, P. M., Serini, D., Sgr, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tak, D., Torres, D. F., Troja, E., Wood, K., Zaharijas, G., Zrake, J., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), D???ammando, F., de la Torre Luque, P., de Palma, F., Dom??nguez, A., J??hannesson, G., Kova??evi??, M., Mart??-Devesa, G., Rain??, S., and Sgr??, C.

Subjects
Physics, Active galactic nuclei, Black hole, Black holes, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxies, Astrophysics - Astrophysics of Galaxies, Galaxie, Space and Planetary Science, Galactic winds, Galactic Winds, Astrophysics::Solar and Stellar Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Gamma-rays, Astrophysics::Galaxy Astrophysics
Abstract

Massive black holes at the centers of galaxies can launch powerful wide-angle winds that, if sustained over time, can unbind the gas from the stellar bulges of galaxies. These winds may be responsible for the observed scaling relation between the masses of the central black holes and the velocity dispersion of stars in galactic bulges. Propagating through the galaxy, the wind should interact with the interstellar medium creating a strong shock, similar to those observed in supernovae explosions, which is able to accelerate charged particles to high energies. In this work we use data from the Fermi Large Area Telescope to search for the γ-ray emission from galaxies with an ultrafast outflow (UFO): a fast (v ∼ 0.1 c), highly ionized outflow, detected in absorption at hard X-rays in several nearby active galactic nuclei (AGN). Adopting a sensitive stacking analysis we are able to detect the average γ-ray emission from these galaxies and exclude that it is due to processes other than UFOs. Moreover, our analysis shows that the γ-ray luminosity scales with the AGN bolometric luminosity and that these outflows transfer ∼0.04% of their mechanical power to γ-rays. Interpreting the observed γ-ray emission as produced by cosmic rays (CRs) accelerated at the shock front, we find that the γ-ray emission may attest to the onset of the wind-host interaction and that these outflows can energize charged particles up to the transition region between galactic and extragalactic CRs., Ajello, M., et al., M.A. and C.K. acknowledge support from NSF and NASA through grants AST-1715256, 80NSSC21K1915, and 80NSSC18K1718. R.D. and D.C. acknowledge the Eugene & Niesje Parker Fellowship Fund, NASA (grants NNX17AG30G, 80NSSC18K1218, and 80NSSC18K1726) and the NSF (grants AST-1714658, AST-1909778). G.C. acknowledges financial support from NASA grants 80NSSC20K0438 and 80NSSC19K095.

Published
2021
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21. Knowledge mobilisation crossing boundaries: a multi-perspective framework for agri-food value chains

Author

Mario Lezoche, Guoqing Zhao, Shaofeng Liu, Diego F. Torres, Alejandro Fernández, Hervé Panetto, Leandro Antonelli, Huilan Chen, University of Plymouth, University of Plymouth, School of Marine Science and Engineering, Drake Circus, Plymouth PL4 8AA, UK, Laboratorio de Investigación y Formación en Informática Avanzada [La Plata] (LIFIA), Facultad de Informática [La Plata], Universidad Nacional de la Plata [Argentine] (UNLP)-Universidad Nacional de la Plata [Argentine] (UNLP), Centre de Recherche en Automatique de Nancy (CRAN), and Université de Lorraine (UL)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Value (ethics), boundary classification, Knowledge management, Process (engineering), 0211 other engineering and technologies, Ciencias Informáticas, boundary-spanning mechanisms, Context (language use), 02 engineering and technology, Horticulture, agricultural value chain, 01 natural sciences, knowledge sharing and flowing, knowledge boundaries, 0103 physical sciences, Production (economics), Asset (economics), 010301 acoustics, 2. Zero hunger, 021103 operations research, business.industry, [INFO.INFO-IA]Computer Science [cs]/Computer Aided Engineering, Knowledge sharing, Agricultural value chain, business, Knowledge transfer
Abstract

Knowledge has long been recognised as a valuable asset to individuals, organisations and economy, subsequently knowledge management (KM) has been a well-established area of research. Existing research has developed various classification schemes for knowledge, and a great number of KM process and lifecycle models have been proposed over the last few decades. In particular, knowledge transfer and sharing has received great attention. However, majority of existing work has focused on knowledge sharing within the same organisation or community where people have a shared sense of identity, values and some common practice, hence knowledge process and learning is within relatively homogeneous groups. There is inadequate research to address the issue of knowledge boundaries and approaches to knowledge mobilisation spanning across knowledge boundaries. The knowledge boundaries can erect significant barriers to knowledge sharing and flowing especially in value chain context where there are a great number of players from different domains, with varied level of knowledge, having different and possibly conflicting interests - participating in knowledge sharing activities. This paper will explore how such knowledge boundaries can be identified and how knowledge gaps among different value chain players can be closed by using appropriate boundary-crossing mechanisms. A multi-perspective knowledge mobilisation framework is proposed. Example applications of the knowledge mobilisation framework in agri-food value chain will be illustrated, based on the most recent developments from an EU collaborative project, RUC-APS (standing for Risk and Uncertain Conditions in Agriculture Production Systems), which is funded by European Commission’s Horizon 2020 RISE programme., Laboratorio de Investigación y Formación en Informática Avanzada

Published
2021
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22. Optimizing a Gamified Design Through Reinforcement Learning - a Case Study in Stack Overflow

Author

Alejandro Fernández, Diego F. Torres, and Jonathan Martin

Subjects
Deep reinforcement learning, Optimization, Potential impact, Computer science, Stack Overflow, Context (language use), Knowledge building community, Gamification, Knowledge sharing, Work (electrical), Human–computer interaction, Ciencias de la Computación e Información, Stack overflow, Reinforcement learning, Reinforcement
Abstract

Gamification can be used to foster participation in knowledge sharing communities. While designing and assessing the potential impact of a gamification design in such a context, it is important to avoid work disruption and negative side effects. A gamification optimization approach implemented with deep reinforcement learning based on play-testing approaches helps prevent possible disruptive configuration and has the capability to adapt to different communities or gamification targets. In this research, a case of study for this approach is presented running over the Stack Overflow Q&A community. The approach detects the best configuration for a Contribution, Reinforcement, and Dissemination (CRD) gamification strategy using Stack Overflow historical data in a year. The results show that the approach funds proper gamification strategy configurations. Moreover, those configurations are robust enough to be applied along the time unseen periods.

Published
2021
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23. Sensitivity of the Cherenkov Telescope Array for probing cosmology and fundamental physics with gamma-ray propagation

Author

J.-P. Lenain, A. Domínguez, Jonathan Ivor Davies, T. Armstrong, A. A. Zdziarski, F. Gianotti, M. Balbo, E. O. Angüner, M. Marculewicz, Alasdair E. Gent, Alice Donini, Olivier Hervet, Henry Przybilski, Giacomo Principe, G. Leto, M. Peresano, Stefano Covino, P. A. Caraveo, Gianpiero Tagliaferri, D. de Martino, V. V. Vassiliev, D. Cauz, F. R. Pantaleo, U. Barres de Almeida, Pietro Bruno, E. Lindfors, M. Zavrtanik, G. Hughes, Miriam Lucio Martinez, P. Bordas, Y. Suda, G. S. Varner, R. Rando, K. Cerny, S. Pita, Csaba Balázs, E. Fiandrini, Michael Backes, Tomohiko Oka, Massimo Persic, Andrea Chiavassa, Johannes Veh, A. Stamerra, Fabrizio Tavecchio, B. Biasuzzi, Michael Punch, Soebur Razzaque, F. D'Ammando, P. I. Batista, Bruna Bertucci, F. Longo, Francesco Gabriele Saturni, Michael G. Burton, Bohdan Hnatyk, P. Sangiorgi, E. M. Santos, D. Nosek, Gagik Tovmassian, J. L. Dournaux, Pedro L. Luque-Escamilla, A. Aguirre-Santaella, M. Orienti, Lluis Font, Andreas Quirrenbach, Philippe Laporte, Ralf Kissmann, Francesco Lucarelli, K. Noda, I. Jiménez Martínez, G. Romeo, Wystan Benbow, P. Romano, B. Bi, J. Grube, H.-S. Zechlin, Giacomo Bonnoli, Martin White, J. P. Osborne, Enrico Cascone, Marek Jamrozy, C. Alispach, Miroslav Pech, O. Cuevas, Petr Schovanek, K. Hayashi, V. I. Zhdanov, Javier Coronado-Blázquez, D. Medina Miranda, Barbara Balmaverde, E. de Ona Wilhelmi, Frank M. Rieger, A. Shalchi, J. M. Paredes, Ruben Alfaro, N. Giglietto, Diego Falceta-Gonçalves, Helene Sol, Rodolfo Carosi, Ayan Acharyya, Dominik Elsässer, S. Vercellone, D. Pimentel, T. Mizuno, Alessandro Bruno, Juan Abel Barrio, K. Kosack, Mauro Orlandini, Rodrigo Guedes Lang, P. Marquez, Adrian Biland, Y. Kobayashi, Nicholas F. H Tothill, M. de Naurois, Daniele Spiga, Lili Yang, L. Tibaldo, Pavel Horvath, M. Lopez, I. Sadeh, Marek Nikolajuk, F. Schüssler, Reshmi Mukherjee, Gianpaolo Vettolani, Jürgen Knödlseder, Daniel Nieto, R. Hnatyk, German Martinez, Diego F. Torres, Farinaldo S. Queiroz, N. Parmiggiani, G. Lamanna, Marcos Santander, S. Fegan, I. Vovk, M. Sánchez-Conde, Wiphu Rujopakarn, Norita Kawanaka, R. C. Shellard, Michael C. B. Ashley, J. Jurysek, Francisco J. Franco, Samuel Timothy Spencer, E. Rebert, J. Morales Merino, M. Pecimotika, Marco Berton, Regis Terrier, G. A. Beck, Carlos Díaz, J. L. Contreras, G. Zaharijas, R. Moderski, José-María Martí, A. Insolia, D. Zavrtanik, K. Kohri, Ladislav Chytka, T. Grabarczyk, A. Zech, M. Garczarczyk, Anastasia Sokolenko, J. Lefaucheur, R. A. Cameron, Moritz Hütten, S. Karkar, K. Pfrang, V. Poireau, Asaf Pe'er, A. Reimer, Fabio Acero, L. Freixas Coromina, David Sánchez, Jonathan S. Lapington, Konstantinos N. Gourgouliatos, J.R. Hörandel, Mario Buscemi, Francesco Dazzi, Abelardo Moralejo, J. Bolmont, R. White, A. Rosales de Leon, J. Prast, Sabrina Einecke, Roberto Aloisio, Yvonne Becherini, Andreas Specovius, Shohei Yanagita, Juan Cortina, Miroslav Hrabovsky, Petr Janecek, D. Depaoli, Lucas Taylor, U. Schwanke, H. Abdalla, S. Recchia, Manuela Mallamaci, M. K. Daniel, Q. Feng, L. Baroncelli, Hiromitsu Takahashi, Susumu Inoue, U. Straumann, Masatoshi Ohishi, Roberto Capuzzo-Dolcetta, Nu. Komin, Federico Russo, R. de Cássia dos Anjos, Y. Ohira, Ferdinando Giordano, Nagisa Hiroshima, E. Garcia, Gavin Rowell, V. Bozhilov, Maxim V. Barkov, Dario Hrupec, I. Oya, F. Salesa Greus, Anna Wolter, M. Živec, R. Belmont, R. Adam, T. Reposeur, J. Rico, A. W. Chen, G. Pühlhofer, H. Prokoph, Stefan Wagner, F. Di Pierro, Fabrizio Bocchino, M. de Bony de Lavergne, A. Kong, Masha Chernyakova, M. Pohl, M. Vazquez Acosta, A. Nagai, A. Brill, Dusan Mandat, Jonathan Biteau, Martin Makariev, Catherine Boisson, E. Lyard, Gilles Maurin, H. Martínez-Huerta, Oscar Blanch, Bernd Schleicher, M. Minev, A. Berti, James E. M. Watson, Talvikki Hovatta, M. Valentino, Luis Ángel Tejedor, Elena Amato, M. V. Fonseca, Anderson Caproni, L. Mohrmann, P. Reichherzer, R. L. C. Starling, M. Seglar Arroyo, E. Orlando, B. Rudak, G. Emery, J. A. Green, Salvo Scuderi, M. Prouza, Tom Richtler, Bartłomiej Pilszyk, A. Carosi, Jacek Niemiec, Wolfgang Rhode, G. Ambrosi, D. Ribeiro, A. Wierzcholska, A. Ghalumyan, Eugenio Bottacini, Sylvain Chaty, A. Baquero Larriva, Olaf Reimer, D. Horan, Fabian Leuschner, T. Di Girolamo, Alessandro Caccianiga, Martin Will, Saverio Lombardi, A. Fiasson, Mitsunari Takahashi, J. J. Rodríguez Vázquez, B. De Lotto, V. De Caprio, Stefano Truzzi, Dirk L. Hoffmann, M. Vecchi, Antonio Pagliaro, Jose J. Gonzalez, Wenwu Tian, R. Della Ceca, J. Becerra González, S. Nozaki, T. Vuillaume, S. L. Lloyd, Maria Ionica, Elisabetta Bissaldi, Petr Travnicek, Y. Ascasibar, Carlo Vigorito, F. Tuossenel, Malcolm Fairbairn, O. Martinez, Marco Iarlori, Serena Loporchio, Alessandro Costa, R. Pillera, A. Morselli, M. Heller, Jaime Rosado, E. M. de Gouveia Dal Pino, V. Vitale, A. M. Brown, E. Molina, Takashi Saito, A. De Angelis, Thomas Murach, R. A. Ong, J. Bregeon, P. T. O'Brien, Mikael Jacquemont, P. Cristofari, Francesco Conte, Lab Saha, R. Walter, Vitalii Sliusar, W. Jin, Vito Conforti, N. Produit, H. Siejkowski, Lovro Pavletić, Carole Mundell, G. Rodriguez Fernandez, J. F. Glicenstein, Paresh Sharma, C. Delgado, Vladimír Karas, Luca Foffano, J. Granot, Manuel Meyer, Reiko Orito, G. Umana, G. Chiaro, D. Tonev, R. Wiemann, G. Manicò, J.C. Rodriguez Ramirez, Luca Tosti, Markus Böttcher, Andrea Bulgarelli, C. Díaz-Bahamondes, I. Jung-Richardt, Karol Seweryn, P. Piatteli, Agnieszka Slowikowska, Jan Ebr, M. Ostrowski, J. L. Rodriguez, D. della Volpe, Ermanno Pietropaolo, M. Caprai, T. Montaruli, A. Lopez, Rodrigo Nemmen, R. R. Prado, L. Arrabito, Atreyee Sinha, C. van Eldik, Serguei Vorobiov, Hidetoshi Sano, J. Alfaro, Sabrina Casanova, G. Maneva, B. Vallage, Valentina Fioretti, Carmelo Evoli, P. Kaaret, B. A. W. Mode, Agnieszka Majczyna, Sebastian Diebold, A. Scherer, F. de Palma, S. Hernández Cadena, V. Beshley, T.R.N. Ekoume, David A. Williams, M. Capasso, A. Halim, Alison Mitchell, Tomislav Terzić, Paola Grandi, Lorenzo Amati, Christopher Eckner, David Gascon, K. Nishijima, J. Becker Tjus, B. Khélifi, G. Galanti, Jamie Holder, Vincenzo Rizi, Orel Gueta, Daniele Gaggero, F. Pintore, Utane Sawangwit, Vassil Verguilov, Heide Costantini, F. Arqueros, Daniel Kerszberg, P. M. Chadwick, D. Zarić, Marc Ribó, Olga Sergijenko, Dario Grasso, Hidetoshi Kubo, Daniela Dorner, T. Stolarczyk, M. Gaug, R. Alves Batista, Elisa Bernardini, Vikram V. Dwarkadas, Jim Hinton, Jelena Strišković, Andreu Sanuy, M. Servillat, V. Barbosa Martins, Giovanni Bonanno, S. Gunji, R. Wischnewski, S. Sarkar, Gianluca Giavitto, Takeshi Nakamori, M. Palatka, Maria Letizia Pumo, Camilla Maggio, M. Zacharias, Katsuaki Asano, Valerio Vagelli, Anton Dmytriiev, Ryo Yamazaki, M. Vacula, P. Goldoni, Gilles Fontaine, Hiroshi Muraishi, D. Mazin, Samo Stanič, G. Ghirlanda, M. Polo, M. Nievas, M. Lemoine-Goumard, Oleh Petruk, Jose Miguel Miranda, M. Iori, A. Marcowith, Y. Renier, Satoshi Fukami, M. Roncadelli, F. Leone, Takanori Yoshikoshi, Ana Luiza d'Ávila Viana, Y. Fukui, Max Harvey, Sera Markoff, I. Agudo, P. Temnikov, Vincenzo Testa, R. López-Coto, J.D. Mbarubucyeye, Tjark Miener, David Paneque, V. Gammaldi, T. Hassan Collado, H. Abe, L. Bonneau Arbeletche, S. D. Vergani, Sasa Micanovic, P. Vallania, Marina Manganaro, Elena Torresi, M. Giarrusso, G. Ferrand, Paweł Świerk, B. Patricelli, Matteo Cerruti, N. La Palombara, D. Morcuende-Parrilla, V. de Souza, Toshiaki Inada, Yasushi Fukazawa, Werner Hofmann, Michele Doro, E. Pueschel, A. Araudo, E. Sciacca, Thomas Lohse, A. Djannati-Ataï, Abdalla, H., Abe, H., Acero, F., Acharyya, A., Adam, R., Agudo, I., Aguirre-Santaella, A., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Alves Batista, R., Amati, L., Amato, E., Ambrosi, G., Ang??ner, E. O., Araudo, A., Armstrong, T., Arqueros, F., Arrabito, L., Asano, K., Ascas??bar, Y., Ashley, M., Backes, M., Balazs, C., Balbo, M., Balmaverde, B., Baquero Larriva, A., Barbosa Martins, V., Barkov, M., Baroncelli, L., Barres de Almeida, U., Barrio, J. A., Batista, P. -I., Becerra Gonz??lez, J., Becherini, Y., Beck, G., Becker Tjus, J., Belmont, R., Benbow, W., Bernardini, E., Berti, A., Berton, M., Bertucci, B., Beshley, V., Bi, B., Biasuzzi, B., Biland, A., Bissaldi, E., Biteau, J., Blanch, O., Bocchino, F., Boisson, C., Bolmont, J., Bonanno, G., Bonneau Arbeletche, L., Bonnoli, G., Bordas, P., Bottacini, E., B??ttcher, M., Bozhilov, V., Bregeon, J., Brill, A., Brown, A. M., Bruno, P., Bruno, A., Bulgarelli, A., Burton, M., Buscemi, M., Caccianiga, A., Cameron, R., Capasso, M., Caprai, M., Caproni, A., Capuzzo-Dolcetta, R., Caraveo, P., Carosi, R., Carosi, A., Casanova, S., Cascone, E., Cauz, D., Cerny, K., Cerruti, M., Chadwick, P., Chaty, S., Chen, A., Chernyakova, M., Chiaro, G., Chiavassa, A., Chytka, L., Conforti, V., Conte, F., Contreras, J. L., Coronado-Blazquez, J., Cortina, J., Costa, A., Costantini, H., Covino, S., Cristofari, P., Cuevas, O., D'Ammando, F., Daniel, M. K., Davies, J., Dazzi, F., De Angelis, A., de Bony de Lavergne, M., De Caprio, V., de C??ssia dos Anjos, R., de Gouveia Dal Pino, E. M., De Lotto, B., De Martino, D., de Naurois, M., de O??a Wilhelmi, E., De Palma, F., de Souza, V., Delgado, C., Della Ceca, R., della Volpe, D., Depaoli, D., Di Girolamo, T., Di Pierro, F., D??az, C., D??az-Bahamondes, C., Diebold, S., Djannati-Ata??, A., Dmytriiev, A., Dom??nguez, A., Donini, A., Dorner, D., Doro, M., Dournaux, J., Dwarkadas, V. V., Ebr, J., Eckner, C., Einecke, S., Ekoume, T. R. N., Els??sser, D., Emery, G., Evoli, C., Fairbairn, M., Falceta-Goncalves, D., Fegan, S., Feng, Q., Ferrand, G., Fiandrini, E., Fiasson, A., Fioretti, V., Foffano, L., Fonseca, M. V., Font, L., Fontaine, G., Franco, F. J., Freixas Coromina, L., Fukami, S., Fukazawa, Y., Fukui, Y., Gaggero, D., Galanti, G., Gammaldi, V., Garcia, E., Garczarczyk, M., Gascon, D., Gaug, M., Gent, A., Ghalumyan, A., Ghirlanda, G., Gianotti, F., Giarrusso, M., Giavitto, G., Giglietto, N., Giordano, F., Glicenstein, J., Goldoni, P., Gonz??lez, J. M., Gourgouliatos, K., Grabarczyk, T., Grandi, P., Granot, J., Grasso, D., Green, J., Grube, J., Gueta, O., Gunji, S., Halim, A., Harvey, M., Hassan Collado, T., Hayashi, K., Heller, M., Hern??ndez Cadena, S., Hervet, O., Hinton, J., Hiroshima, N., Hnatyk, B., Hnatyk, R., Hoffmann, D., Hofmann, W., Holder, J., Horan, D., H??randel, J., Horvath, P., Hovatta, T., Hrabovsky, M., Hrupec, D., Hughes, G., H??tten, M., Iarlori, M., Inada, T., Inoue, S., Insolia, A., Ionica, M., Iori, M., Jacquemont, M., Jamrozy, M., Janecek, P., Jim??nez Mart??nez, I., Jin, W., Jung-Richardt, I., Jurysek, J., Kaaret, P., Karas, V., Karkar, S., Kawanaka, N., Kerszberg, D., Kh??lifi, B., Kissmann, R., Kn??dlseder, J., Kobayashi, Y., Kohri, K., Komin, N., Kong, A., Kosack, K., Kubo, H., La Palombara, N., Lamanna, G., Lang, R. G., Lapington, J., Laporte, P., Lefaucheur, J., Lemoine-Goumard, M., Lenain, J., Leone, F., Leto, G., Leuschner, F., Lindfors, E., Lloyd, S., Lohse, T., Lombardi, S., Longo, F., Lopez, A., L??pez, M., L??pez-Coto, R., Loporchio, S., Lucarelli, F., Luque-Escamilla, P. L., Lyard, E., Maggio, C., Majczyna, A., Makariev, M., Mallamaci, M., Mandat, D., Maneva, G., Manganaro, M., Manic??, G., Marcowith, A., Marculewicz, M., Markoff, S., Marquez, P., Mart??, J., Martinez, O., Mart??nez, M., Mart??nez, G., Mart??nez-Huerta, H., Maurin, G., Mazin, D., Mbarubucyeye, J. D., Medina Miranda, D., Meyer, M., Micanovic, S., Miener, T., Minev, M., Miranda, J. M., Mitchell, A., Mizuno, T., Mode, B., Moderski, R., Mohrmann, L., Molina, E., Montaruli, T., Moralejo, A., Morales Merino, J., Morcuende-Parrilla, D., Morselli, A., Mukherjee, R., Mundell, C., Murach, T., Muraishi, H., Nagai, A., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Nievas, M., Nikolajuk, M., Nishijima, K., Noda, K., Nosek, D., Nozaki, S., O'Brien, P., Ohira, Y., Ohishi, M., Oka, T., Ong, R. A., Orienti, M., Orito, R., Orlandini, M., Orlando, E., Osborne, J. P., Ostrowski, M., Oya, I., Pagliaro, A., Palatka, M., Paneque, D., Pantaleo, F. R., Paredes, J. M., Parmiggiani, N., Patricelli, B., Pavleti??, L., Pe'Er, A., Pech, M., Pecimotika, M., Peresano, M., Persic, M., Petruk, O., Pfrang, K., Piatteli, P., Pietropaolo, E., Pillera, R., Pilszyk, B., Pimentel, D., Pintore, F., Pita, S., Pohl, M., Poireau, V., Polo, M., Prado, R. R., Prast, J., Principe, G., Produit, N., Prokoph, H., Prouza, M., Przybilski, H., Pueschel, E., P??hlhofer, G., Pumo, M. L., Punch, M., Queiroz, F., Quirrenbach, A., Rando, R., Razzaque, S., Rebert, E., Recchia, S., Reichherzer, P., Reimer, O., Reimer, A., Renier, Y., Reposeur, T., Rhode, W., Ribeiro, D., Rib??, M., Richtler, T., Rico, J., Rieger, F., Rizi, V., Rodriguez, J., Rodriguez Fernandez, G., Rodriguez Ramirez, J. C., Rodr??guez V??zquez, J. J., Romano, P., Romeo, G., Roncadelli, M., Rosado, J., Rosales de Leon, A., Rowell, G., Rudak, B., Rujopakarn, W., Russo, F., Sadeh, I., Saha, L., Saito, T., Salesa Greus, F., Sanchez, D., S??nchez-Conde, M., Sangiorgi, P., Sano, H., Santander, M., Santos, E. M., Sanuy, A., Sarkar, S., Saturni, F. G., Sawangwit, U., Scherer, A., Schleicher, B., Schovanek, P., Schussler, F., Schwanke, U., Sciacca, E., Scuderi, S., Seglar Arroyo, M., Sergijenko, O., Servillat, M., Seweryn, K., Shalchi, A., Sharma, P., Shellard, R. C., Siejkowski, H., Sinha, A., Sliusar, V., Slowikowska, A., Sokolenko, A., Sol, H., Specovius, A., Spencer, S., Spiga, D., Stamerra, A., Stani??, S., Starling, R., Stolarczyk, T., Straumann, U., Stri??kovi??, J., Suda, Y., wierk, P., Tagliaferri, G., Takahashi, H., Takahashi, M., Tavecchio, F., Taylor, L., Tejedor, L. A., Temnikov, P., Terrier, R., Terzic, T., Testa, V., Tian, W., Tibaldo, L., Tonev, D., Torres, D. F., Torresi, E., Tosti, L., Tothill, N., Tovmassian, G., Travnicek, P., Truzzi, S., Tuossenel, F., Umana, G., Vacula, M., Vagelli, V., Valentino, M., Vallage, B., Vallania, P., van Eldik, C., Varner, G. S., Vassiliev, V., V??zquez Acosta, M., Vecchi, M., Veh, J., Vercellone, S., Vergani, S., Verguilov, V., Vettolani, G. P., Viana, A., Vigorito, C. F., Vitale, V., Vorobiov, S., Vovk, I., Vuillaume, T., Wagner, S. J., Walter, R., Watson, J., White, M., White, R., Wiemann, R., Wierzcholska, A., Will, M., Williams, D. A., Wischnewski, R., Wolter, A., Yamazaki, R., Yanagita, S., Yang, L., Yoshikoshi, T., Zacharias, M., Zaharijas, G., Zaric, D., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zhdanov, V. I., ivec, M., Comisión Nacional de Investigación Científica y Tecnológica (Chile), Ministry of Education, Youth and Sports (Czech Republic), Academy of Finland, Istituto Nazionale di Astrofisica, National Science Centre (Poland), Slovenian Research Agency, European Commission, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia e Innovación (España), Junta de Andalucía, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Laboratoire de Physique des 2 Infinis Irène Joliot-Curie (IJCLab), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Saclay-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Institut de recherche en astrophysique et planétologie (IRAP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), CTA, UAM. Departamento de Física Teórica, Batista, R. A., Anguner, E. O., Ascasibar, Y., Larriva, A. B., Martins, V. B., De Almeida, U. B., Gonzalez, J. B., Tjus, J. B., Arbeletche, L. B., Bottcher, M., Angelis, A. D., De Lavergne, M. D. B., Caprio, V. D., De Dos Anjos, R. C., De Gouveia Dal Pino, E. M., Lotto, B. D., Martino, D. D., De Naurois, M., Wilhelmi, E. D. O., DE PALMA, F., De Souza, V., Ceca, R. D., Volpe, D. D., Girolamo, T. D., Pierro, F. D., Diaz, C., Diaz-Bahamondes, C., Djannati-Atai, A., Dominguez, A., Elsasser, D., Coromina, L. F., Gonzalez, J. M., Collado, T. H., Cadena, S. H., Horandel, J., Hutten, M., Martinez, I. J., Khelifi, B., Knodlseder, J., Palombara, N. L., Lopez, M., Lopez-Coto, R., Manico, G., Marti, J., Martinez, M., Martinez, G., Martinez-Huerta, H., Miranda, D. M., Merino, J. M., Pavletic, L., Puhlhofer, G., Ribo, M., Fernandez, G. R., Ramirez, J. C. R., Vazquez, J. J. R., De Leon, A. R., Greus, F. S., Sanchez-Conde, M., Arroyo, M. S., Stanic, S., Striskovic, J., Swierk, P., Eldik, C. V., Acosta, M. V., Zivec, M., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Abdalla H., Abe H., Acero F., Acharyya A., Adam R., Agudo I., Aguirre-Santaella A., Alfaro R., Alfaro J., Alispach C., Aloisio R., Batista R.A., Amati L., Amato E., Ambrosi G., Anguner E.O., Araudo A., Armstrong T., Arqueros F., Arrabito L., Asano K., Ascasibar Y., Ashley M., Backes M., Balazs C., Balbo M., Balmaverde B., Larriva A.B., Martins V.B., Barkov M., Baroncelli L., De Almeida U.B., Barrio J.A., Batista P.-I., Gonzalez J.B., Becherini Y., Beck G., Tjus J.B., Belmont R., Benbow W., Bernardini E., Berti A., Berton M., Bertucci B., Beshley V., Bi B., Biasuzzi B., Biland A., Bissaldi E., Biteau J., Blanch O., Bocchino F., Boisson C., Bolmont J., Bonanno G., Arbeletche L.B., Bonnoli G., Bordas P., Bottacini E., Bottcher M., Bozhilov V., Bregeon J., Brill A., Brown A.M., Bruno P., Bruno A., Bulgarelli A., Burton M., Buscemi M., Caccianiga A., Cameron R., Capasso M., Caprai M., Caproni A., Capuzzo-Dolcetta R., Caraveo P., Carosi R., Carosi A., Casanova S., Cascone E., Cauz D., Cerny K., Cerruti M., Chadwick P., Chaty S., Chen A., Chernyakova M., Chiaro G., Chiavassa A., Chytka L., Conforti V., Conte F., Contreras J.L., Coronado-Blazquez J., Cortina J., Costa A., Costantini H., Covino S., Cristofari P., Cuevas O., D'Ammando F., Daniel M.K., Davies J., Dazzi F., Angelis A.D., De Lavergne M.D.B., Caprio V.D., De Dos Anjos R.C., De Gouveia Dal Pino E.M., Lotto B.D., Martino D.D., De Naurois M., Wilhelmi E.D.O., Palma F.D., De Souza V., Delgado C., Ceca R.D., Volpe D.D., Depaoli D., Girolamo T.D., Pierro F.D., Diaz C., Diaz-Bahamondes C., Diebold S., Djannati-Atai A., Dmytriiev A., Dominguez A., Donini A., Dorner D., Doro M., Dournaux J., Dwarkadas V.V., Ebr J., Eckner C., Einecke S., Ekoume T.R.N., Elsasser D., Emery G., Evoli C., Fairbairn M., Falceta-Goncalves D., Fegan S., Feng Q., Ferrand G., Fiandrini E., Fiasson A., Fioretti V., Foffano L., Fonseca M.V., Font L., Fontaine G., Franco F.J., Coromina L.F., Fukami S., Fukazawa Y., Fukui Y., Gaggero D., Galanti G., Gammaldi V., Garcia E., Garczarczyk M., Gascon D., Gaug M., Gent A., Ghalumyan A., Ghirlanda G., Gianotti F., Giarrusso M., Giavitto G., Giglietto N., Giordano F., Glicenstein J., Goldoni P., Gonzalez J.M., Gourgouliatos K., Grabarczyk T., Grandi P., Granot J., Grasso D., Green J., Grube J., Gueta O., Gunji S., Halim A., Harvey M., Collado T.H., Hayashi K., Heller M., Cadena S.H., Hervet O., Hinton J., Hiroshima N., Hnatyk B., Hnatyk R., Hoffmann D., Hofmann W., Holder J., Horan D., Horandel J., Horvath P., Hovatta T., Hrabovsky M., Hrupec D., Hughes G., Hutten M., Iarlori M., Inada T., Inoue S., Insolia A., Ionica M., Iori M., Jacquemont M., Jamrozy M., Janecek P., Martinez I.J., Jin W., Jung-Richardt I., Jurysek J., Kaaret P., Karas V., Karkar S., Kawanaka N., Kerszberg D., Khelifi B., Kissmann R., Knodlseder J., Kobayashi Y., Kohri K., Komin N., Kong A., Kosack K., Kubo H., Palombara N.L., Lamanna G., Lang R.G., Lapington J., Laporte P., Lefaucheur J., Lemoine-Goumard M., Lenain J., Leone F., Leto G., Leuschner F., Lindfors E., Lloyd S., Lohse T., Lombardi S., Longo F., Lopez A., Lopez M., Lopez-Coto R., Loporchio S., Lucarelli F., Luque-Escamilla P.L., Lyard E., Maggio C., Majczyna A., Makariev M., Mallamaci M., Mandat D., Maneva G., Manganaro M., Manico G., Marcowith A., Marculewicz M., Markoff S., Marquez P., Marti J., Martinez O., Martinez M., Martinez G., Martinez-Huerta H., Maurin G., Mazin D., Mbarubucyeye J.D., Miranda D.M., Meyer M., Micanovic S., Miener T., Minev M., Miranda J.M., Mitchell A., Mizuno T., Mode B., Moderski R., Mohrmann L., Molina E., Montaruli T., Moralejo A., Merino J.M., Morcuende-Parrilla D., Morselli A., Mukherjee R., Mundell C., Murach T., Muraishi H., Nagai A., Nakamori T., Nemmen R., Niemiec J., Nieto D., Nievas M., Nikolajuk M., Nishijima K., Noda K., Nosek D., Nozaki S., O'Brien P., Ohira Y., Ohishi M., Oka T., Ong R.A., Orienti M., Orito R., Orlandini M., Orlando E., Osborne J.P., Ostrowski M., Oya I., Pagliaro A., Palatka M., Paneque D., Pantaleo F.R., Paredes J.M., Parmiggiani N., Patricelli B., Pavletic L., Pe'Er A., Pech M., Pecimotika M., Peresano M., Persic M., Petruk O., Pfrang K., Piatteli P., Pietropaolo E., Pillera R., Pilszyk B., Pimentel D., Pintore F., Pita S., Pohl M., Poireau V., Polo M., Prado R.R., Prast J., Principe G., Produit N., Prokoph H., Prouza M., Przybilski H., Pueschel E., Puhlhofer G., Pumo M.L., Punch M., Queiroz F., Quirrenbach A., Rando R., Razzaque S., Rebert E., Recchia S., Reichherzer P., Reimer O., Reimer A., Renier Y., Reposeur T., Rhode W., Ribeiro D., Ribo M., Richtler T., Rico J., Rieger F., Rizi V., Rodriguez J., Fernandez G.R., Ramirez J.C.R., Vazquez J.J.R., Romano P., Romeo G., Roncadelli M., Rosado J., De Leon A.R., Rowell G., Rudak B., Rujopakarn W., Russo F., Sadeh I., Saha L., Saito T., Greus F.S., Sanchez D., Sanchez-Conde M., Sangiorgi P., Sano H., Santander M., Santos E.M., Sanuy A., Sarkar S., Saturni F.G., Sawangwit U., Scherer A., Schleicher B., Schovanek P., Schussler F., Schwanke U., Sciacca E., Scuderi S., Arroyo M.S., Sergijenko O., Servillat M., Seweryn K., Shalchi A., Sharma P., Shellard R.C., Siejkowski H., Sinha A., Sliusar V., Slowikowska A., Sokolenko A., Sol H., Specovius A., Spencer S., Spiga D., Stamerra A., Stanic S., Starling R., Stolarczyk T., Straumann U., Striskovic J., Suda Y., Swierk P., Tagliaferri G., Takahashi H., Takahashi M., Tavecchio F., Taylor L., Tejedor L.A., Temnikov P., Terrier R., Terzic T., Testa V., Tian W., Tibaldo L., Tonev D., Torres D.F., Torresi E., Tosti L., Tothill N., Tovmassian G., Travnicek P., Truzzi S., Tuossenel F., Umana G., Vacula M., Vagelli V., Valentino M., Vallage B., Vallania P., Eldik C.V., Varner G.S., Vassiliev V., Acosta M.V., Vecchi M., Veh J., Vercellone S., Vergani S., Verguilov V., Vettolani G.P., Viana A., Vigorito C.F., Vitale V., Vorobiov S., Vovk I., Vuillaume T., Wagner S.J., Walter R., Watson J., White M., White R., Wiemann R., Wierzcholska A., Will M., Williams D.A., Wischnewski R., Wolter A., Yamazaki R., Yanagita S., Yang L., Yoshikoshi T., Zacharias M., Zaharijas G., Zaric D., Zavrtanik M., Zavrtanik D., Zdziarski A.A., Zech A., Zechlin H., Zhdanov V.I., Zivec M., ITA, USA, GBR, FRA, DEU, ESP, AUS, BRA, BGR, CHL, HRV, FIN, JPN, IRL, MEX, NAM, NLD, POL, CZE, SVN, SWE, CHE, UKR, Astronomy, High Energy Astrophys. & Astropart. Phys (API, FNWI), and Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)

Subjects
Gamma ray Astronomy, Cherenkov Telescope Array, axions, MATÉRIA ESCURA, redshift: dependence, Astronomy, Gamma ray experiments, gamma ray experiments, Astrophysics, 01 natural sciences, Cosmology, Observatory, cosmological model: parameter space, gamma ray experiment, High Energy Astrophysical Phenomena (astro-ph.HE), astro-ph.HE, Physics, Cherenkov telescopes, IACT technique, Gamma rays, Cosmic rays, new physics, 4. Education, Settore FIS/01 - Fisica Sperimentale, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma-ray astronomy, violation: Lorentz, 3. Good health, observatory, Extragalactic background light, astro-ph.CO, axion-like particles, Física nuclear, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Cosmology and Nongalactic Astrophysics, gamma ray: propagation, Cosmology and Nongalactic Astrophysics (astro-ph.CO), Active galactic nucleus, Axions, Astrophysics::High Energy Astrophysical Phenomena, Dark matter, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, invariance: Lorentz, jet: relativistic, dark matter: halo, 0103 physical sciences, active galactic nuclei, extragalactic magnetic fields, AGN, Blazar, background, 010308 nuclear & particles physics, Física, Astronomy and Astrophysics, sensitivity, axion, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], absorption, statistical, Blazars, Telescopes
Abstract

Full list of authors: Abdalla, H.; Abe, H.; Acero, F.; Acharyya, A.; Adam, R.; Agudo, I; Aguirre-Santaella, A.; Alfaro, R.; Alfaro, J.; Alispach, C.; Aloisio, R.; Batista, R. Alves; Amati, L.; Amato, E.; Ambrosi, G.; Anguner, E. O.; Araudo, A.; Armstrong, T.; Arqueros, F.; Arrabito, L.; Asano, K.; Ascasibar, Y.; Ashley, M.; Backes, M.; Balazs, C.; Balbo, M.; Balmaverde, B.; Baquero Larriva, A.; Martins, V. Barbosa; Barkov, M.; Baroncelli, L.; de Almeida, U. Barres; Barrio, J. A.; Batista, P-, I; Becerra Gonzalez, J.; Becherini, Y.; Beck, G.; Tjus, J. Becker; Belmont, R.; Benbow, W.; Bernardini, E.; Berti, A.; Berton, M.; Bertucci, B.; Beshley, V; Bi, B.; Biasuzzi, B.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Bocchino, F.; Boisson, C.; Bolmont, J.; Bonanno, G.; Arbeletche, L. Bonneau; Bonnoli, G.; Bordas, P.; Bottacini, E.; Bottcher, M.; Bozhilov, V; Bregeon, J.; Brill, A.; Brown, A. M.; Bruno, P.; Bruno, A.; Bulgarelli, A.; Burton, M.; Buscemi, M.; Caccianiga, A.; Cameron, R.; Capasso, M.; Caprai, M.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Carosi, R.; Carosi, A.; Casanova, S.; Cascone, E.; Cauz, D.; Cerny, K.; Cerruti, M.; Chadwick, P.; Chaty, S.; Chen, A.; Chernyakova, M.; Chiaro, G.; Chiavassa, A.; Chytka, L.; Conforti, V; Conte, F.; Contreras, J. L.; Coronado-Blazquez, J.; Cortina, J.; Costa, A.; Costantini, H.; Covino, S.; Cristofari, P.; Cuevas, O.; D'Ammando, F.; Daniel, M. K.; Davies, J.; Dazzi, F.; De Angelis, A.; de Lavergne, M. de Bony; De Caprio, V; dos Anjos, R. de Cassia; Dal Pino, E. M. de Gouveia; De Lotto, B.; De Martino, D.; de Naurois, M.; Wilhelmi, E. de Ona; De Palma, F.; de Souza, V; Delgado, C.; Della Ceca, R.; della Volpe, D.; Depaoli, D.; Di Girolamo, T.; Di Pierro, F.; Diaz, C.; Diaz-Bahamondes, C.; Diebold, S.; Djannati-Atai, A.; Dmytriiev, A.; Dominguez, A.; Donini, A.; Dorner, D.; Doro, M.; Dournaux, J.; Dwarkadas, V. V.; Ebr, J.; Eckner, C.; Einecke, S.; Ekoume, T. R. N.; Elsaesser, D.; Emery, G.; Evoli, C.; Fairbairn, M.; Falceta-Goncalves, D.; Fegan, S.; Feng, Q.; Ferrand, G.; Fiandrini, E.; Fiasson, A.; Fioretti, V; Foffano, L.; Fonseca, M., V; Font, L.; Fontaine, G.; Franco, F. J.; Freixas Coromina, L.; Fukami, S.; Fukazawa, Y.; Fukui, Y.; Gaggero, D.; Galanti, G.; Gammaldi, V; Garcia, E.; Garczarczyk, M.; Gascon, D.; Gaug, M.; Gent, A.; Ghalumyan, A.; Ghirlanda, G.; Gianotti, F.; Giarrusso, M.; Giavitto, G.; Giglietto, N.; Giordano, F.; Glicenstein, J.; Goldoni, P.; Gonzalez, J. M.; Gourgouliatos, K.; Grabarczyk, T.; Grandi, P.; Granot, J.; Grasso, D.; Green, J.; Grube, J.; Gueta, O.; Gunji, S.; Halim, A.; Harvey, M.; Collado, T. Hassan; Hayashi, K.; Heller, M.; Cadena, S. Hernandez; Hervet, O.; Hinton, J.; Hiroshima, N.; Hnatyk, B.; Hnatyk, R.; Hoffmann, D.; Hofmann, W.; Holder, J.; Horan, D.; Horandel, J.; Horvath, P.; Hovatta, T.; Hrabovsky, M.; Hrupec, D.; Hughes, G.; Hutten, M.; Iarlori, M.; Inada, T.; Inoue, S.; Insolia, A.; Ionica, M.; Iori, M.; Jacquemont, M.; Jamrozy, M.; Janecek, P.; Jimenez Martinez, I; Jin, W.; Jung-Richardt, I; Jurysek, J.; Kaaret, P.; Karas, V; Karkar, S.; Kawanaka, N.; Kerszberg, D.; Khelifi, B.; Kissmann, R.; Knodlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kong, A.; Kosack, K.; Kubo, H.; La Palombara, N.; Lamanna, G.; Lang, R. G.; Lapington, J.; Laporte, P.; Lefaucheur, J.; Lemoine-Goumard, M.; Lenain, J.; Leone, F.; Leto, G.; Leuschner, F.; Lindfors, E.; Lloyd, S.; Lohse, T.; Lombardi, S.; Longo, F.; Lopez, A.; Lopez, M.; Lopez-Coto, R.; Loporchio, S.; Lucarelli, F.; Luque-Escamilla, P. L.; Lyard, E.; Maggio, C.; Majczyna, A.; Makariev, M.; Mallamaci, M.; Mandat, D.; Maneva, G.; Manganaro, M.; Manico, G.; Marcowith, A.; Marculewicz, M.; Markoff, S.; Marquez, P.; Marti, J.; Martinez, O.; Martinez, M.; Martinez, G.; Martinez-Huerta, H.; Maurin, G.; Mazin, D.; Mbarubucyeye, J. D.; Miranda, D. Medina; Meyer, M.; Micanovic, S.; Miener, T.; Minev, M.; Miranda, J. M.; Mitchell, A.; Mizuno, T.; Mode, B.; Moderski, R.; Mohrmann, L.; Molina, E.; Montaruli, T.; Moralejo, A.; Morales Merino, J.; Morcuende-Parrilla, D.; Morselli, A.; Mukherjee, R.; Mundell, C.; Murach, T.; Muraishi, H.; Nagai, A.; Nakamori, T.; Nemmen, R.; Niemiec, J.; Nieto, D.; Nievas, M.; Nikolajuk, M.; Nishijima, K.; Noda, K.; Nosek, D.; Nozaki, S.; Ohira, Y.; Ohishi, M.; Oka, T.; Ong, R. A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, E.; Osborne, J. P.; Ostrowski, M.; Oya, I; Pagliaro, A.; Palatka, M.; Paneque, D.; Pantaleo, F. R.; Paredes, J. M.; Parmiggiani, N.; Patricelli, B.; Pavletic, L.; Pe'er, A.; Pech, M.; Pecimotika, M.; Peresano, M.; Persic, M.; Petruk, O.; Pfrang, K.; Piatteli, P.; Pietropaolo, E.; Pillera, R.; Pilszyk, B.; Pimentel, D.; Pintore, F.; Pita, S.; Pohl, M.; Poireau, V; Polo, M.; Prado, R. R.; Prast, J.; Principe, G.; Produit, N.; Prokoph, H.; Prouza, M.; Przybilski, H.; Pueschel, E.; Puehlhofer, G.; Pumo, M. L.; Punch, M.; Queiroz, F.; Quirrenbach, A.; Rando, R.; Razzaque, S.; Rebert, E.; Recchia, S.; Reichherzer, P.; Reimer, O.; Reimer, A.; Renier, Y.; Reposeur, T.; Rhode, W.; Ribeiro, D.; Ribo, M.; Richtler, T.; Rico, J.; Rieger, F.; Rizi, V; Rodriguez, J.; Fernandez, G. Rodriguez; Ramirez, J. C. Rodriguez; Rodriguez Vazquez, J. J.; Romano, P.; Romeo, G.; Roncadelli, M.; Rosado, J.; de Leon, A. Rosales; Rowell, G.; Rudak, B.; Rujopakarn, W.; Russo, F.; Sadeh, I; Saha, L.; Saito, T.; Greus, F. Salesa; Sanchez, D.; Sanchez-Conde, M.; Sangiorgi, P.; Sano, H.; Santander, M.; Santos, E. M.; Sanuy, A.; Sarkar, S.; Saturni, F. G.; Sawangwit, U.; Scherer, A.; Schleicher, B.; Schovanek, P.; Schussler, F.; Schwanke, U.; Sciacca, E.; Scuderi, S.; Arroyo, M. Seglar; Sergijenko, O.; Servillat, M.; Seweryn, K.; Shalchi, A.; Sharma, P.; Shellard, R. C.; Siejkowski, H.; Sinha, A.; Sliusar, V; Slowikowska, A.; Sokolenko, A.; Sol, H.; Specovius, A.; Spencer, S.; Spiga, D.; Stamerra, A.; Starling, R.; Stolarczyk, T.; Straumann, U.; Striskovic, J.; Suda, Y.; Tagliaferri, G.; Takahashi, H.; Takahashi, M.; Tavecchio, F.; Taylor, L.; Tejedor, L. A.; Temnikov, P.; Terrier, R.; Terzic, T.; Testa, V; Tian, W.; Tibaldo, L.; Tonev, D.; Torres, D. F.; Torresi, E.; Tosti, L.; Tothill, N.; Tovmassian, G.; Travnicek, P.; Truzzi, S.; Tuossenel, F.; Umana, G.; Vacula, M.; Vagelli, V.; Valentino, M.; Vallage, B.; Vallania, P.; van Eldik, C.; Varner, G. S.; Vassiliev, V.; Vazquez Acosta, M.; Vecchi, M.; Veh, J.; Vercellone, S.; Vergani, S.; Verguilov, V.; Vettolani, G. P.; Viana, A.; Vigorito, C. F.; Vitale, V.; Vorobiov, S.; Vovk, I; Vuillaume, T.; Wagner, S. J.; Walter, R.; Watson, J.; White, M.; White, R.; Wiemann, R.; Wierzcholska, A.; Will, M.; Williams, D. A.; Wischnewski, R.; Wolter, A.; Yamazaki, R.; Yanagita, S.; Yang, L.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zaric, D.; Zavrtanik, M.; Zavrtanik, D.; Zdziarski, A. A.; Zech, A.; Zechlin, H.; Zhdanov, V., I; Zivec, M., The Cherenkov Telescope Array (CTA), the new-generation ground-based observatory for γ astronomy, provides unique capabilities to address significant open questions in astrophysics, cosmology, and fundamental physics. We study some of the salient areas of γ cosmology that can be explored as part of the Key Science Projects of CTA, through simulated observations of active galactic nuclei (AGN) and of their relativistic jets. Observations of AGN with CTA will enable a measurement of γ absorption on the extragalactic background light with a statistical uncertainty below 15% up to a redshift z=2 and to constrain or detect γ halos up to intergalactic-magnetic-field strengths of at least 0.3 pG . Extragalactic observations with CTA also show promising potential to probe physics beyond the Standard Model. The best limits on Lorentz invariance violation from γ astronomy will be improved by a factor of at least two to three. CTA will also probe the parameter space in which axion-like particles could constitute a significant fraction, if not all, of dark matter. We conclude on the synergies between CTA and other upcoming facilities that will foster the growth of γ cosmology. © 2021 IOP Publishing Ltd and Sissa Medialab., We gratefully acknowledge financial support from the following agencies and organizations: State Committee of Science of Armenia, Armenia; The Australian Research Council, Astronomy Australia Ltd, The University of Adelaide, Australian National University, Monash University, The University of New South Wales, The University of Sydney, Western Sydney University, Australia; Federal Ministry of Education, Science and Research, and Innsbruck University, Austria; Conselho Nacional de Desenvolvimento Científico e Tecnológico (CNPq), Fundação de Amparo à Pesquisa do Estado do Rio de Janeiro (FAPERJ), Fundação de Amparo à Pesquisa do Estado de São Paulo (FAPESP), Ministry of Science, Technology, Innovations and Communications (MCTIC), Brasil; Ministry of Education and Science, National RI Roadmap Project DO1-153/28.08.2018, Bulgaria; The Natural Sciences and Engineering Research Council of Canada and the Canadian Space Agency, Canada; CONICYT-Chile grants CATA AFB 170002, ANID PIA/APOYO AFB 180002, ACT 1406, FONDECYT-Chile grants, 1161463, 1170171, 1190886, 1171421, 1170345, 1201582, Gemini-ANID 32180007, Chile; Croatian Science Foundation, Rudjer Boskovic Institute, University of Osijek, University of Rijeka, University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture, University of Zagreb, Faculty of Electrical Engineering and Computing, Croa tia; Ministry of Education, Youth and Sports, MEYS M2015046, LM2018105, LTT17006, EU/MEYS CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/18_046/0016007 and CZ.02.1.01/0.0/0.0/16_019/0000754, Czech Republic; Academy of Finland (grant nr.317636 and 320045), Finland; Ministry of Higher Education and Research, CNRS-INSU and CNRS-IN2P3, CEA-Irfu, ANR, Regional Council Ile de France, Labex ENIGMASS, OCEVU, OSUG2020 and P2IO, France; Max Planck Society, BMBF, DESY, Helmholtz Association, Germany; Department of Atomic Energy, Department of Science and Technology, India; Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare (INFN), MIUR, Istituto Nazionale di Astrofisica (INAF-OABRERA) Grant Fondazione Cariplo/Regione Lombardia ID 2014-1980/RST_ERC, Italy; ICRR, University of Tokyo, JSPS, MEXT, Japan; Netherlands Research School for Astronomy (NOVA), Netherlands Organization for Scientific Research (NWO), Netherlands; University of Oslo, Norway; Ministry of Science and Higher Education, DIR/WK/2017/12, the National Centre for Research and Development and the National Science Centre, UMO-2016/22/M/ST9/00583, Poland; Slovenian Research Agency, grants P1-0031, P1-0385, I0-0033, J1-9146, J1-1700, N1-0111, and the Young Researcher program, Slovenia; South African Department of Science and Technology and National Research Foundation through the South African Gamma-Ray Astronomy Programme, South Africa; The Spanish groups acknowledge the Spanish Ministry of Science and Innovation and the Spanish Research State Agency (AEI) through grants AYA2016-79724-C4-1-P, AYA2016-80889-P, AYA2016-76012-C3-1-P, BES-2016-076342, FPA2017-82729-C6-1-R, FPA2017-82729-C6-2-R, FPA2017-82729-C6-3-R, FPA2017-82729-C6-4-R, FPA2017-82729-C6-5-R, FPA2017-82729-C6-6-R, PGC2018-095161-B-I00, PGC2018-095512-B-I00, PID2019-107988GB-C22; the “Centro de Excelencia Severo Ochoa” program through grants no. SEV-2016-0597, SEV-2016-0588, SEV-2017-0709, CEX2019-000920-S; the “Unidad de Excelencia María de Maeztu” program through grant no. MDM-2015-0509; the “Ramón y Cajal” programme through grants RYC-2013-14511, RYC-2017-22665; and the MultiDark Consolider Network FPA2017-90566-REDC. They also acknowledge the Atracción de Talento contract no. 2016-T1/TIC-1542 granted by the Comunidad de Madrid; the “Postdoctoral Junior Leader Fellowship” programme from La Caixa Bank ing Foundation, grants no. LCF/BQ/LI18/11630014 and LCF/BQ/PI18/11630012; the “Programa Operativo” FEDER 2014-2020, Consejería de Economía y Conocimiento de la Junta de Andalucía (Ref. 1257737), PAIDI 2020 (Ref. P18-FR-1580) and Universidad de Jaén; “Programa Operativo de Crecimiento Inteligente” FEDER 2014-2020 (Ref. ESFRI-2017-IAC-12), Ministerio de Ciencia e Innovación, 15% co-financed by Consejería de Economía, Industria, Comercio y Conocimiento del Gobierno de Canarias; the Spanish AEI EQC2018-005094-P FEDER 2014-2020; the European Union’s “Horizon 2020” research and innovation programme under Marie Skłodowska-Curie grant agreement no. 665919; and the ESCAPE project with grant no. GA:824064; Swedish Research Council, Royal Physiographic Society of Lund, Royal Swedish Academy of Sciences, The Swedish National Infrastructure for Computing (SNIC) at Lunarc (Lund), Sweden; State Secretariat for Education, Research and Innovation (SERI) and Swiss National Science Foundation (SNSF), Switzerland; Durham University, Leverhulme Trust, Liverpool University, University of Leicester, University of Oxford, Royal Soci ety, Science and Technology Facilities Council, UK; U.S. National Science Foundation, U.S. Department of Energy, Argonne National Laboratory, Barnard College, University of California, University of Chicago, Columbia University, Georgia Institute of Technology, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI program), Iowa State University, the Smithsonian Institution, Washington University McDonnell Center for the Space Sciences, The University of Wisconsin and the Wisconsin Alumni Research Foundation, USA. The research leading to these results has received funding from the European Union’s Seventh Framework Programme (FP7/2007-2013) under grant agreements No 262053 and No 317446. This project is receiving funding from the European Union’s Horizon 2020 research and innovation programs under agreement No 676134. The research leading to these results has received funding from the European Union’s Horizon 2020 research and innovation program under the Marie Skłodowska-Curie grant agreement GammaRayCascades No 843800. The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat à l’Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucléaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Études Spatiales in France. This work performed in part under DOE Contract DE-AC02-76SF00515.

Published
2021
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24. Reverberation of pulsar wind nebulae (I): Impact of the medium properties and other parameters upon the extent of the compression

Author

Niccolò Bucciantini, Jonathan Martin, Rino Bandiera, B. Olmi, Diego F. Torres, Ministerio de Ciencia, Innovación y Universidades (España), and Istituto Nazionale di Astrofisica

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Reverberation, numerical [Methods], non-thermal [Radiation mechanisms], Methods: numerical, Radiation mechanisms: non-thermal, 010308 nuclear & particles physics, supernova remnants [ISM], Acoustics, Astrophysics::High Energy Astrophysical Phenomena, general [Pulsars], FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Pulsars: general, Pulsar, Space and Planetary Science, Compression (functional analysis), 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, ISM: supernova remnants
Abstract

The standard approach to the long-term evolution of pulsar wind nebulae (PWNe) is based on one-zone models treating the nebula as a uniform system. In particular for the late phase of evolved systems, many of the generally used prescriptions are based on educated guesses for which a proper assessment lacks. Using an advanced radiative code, we evaluate the systematic impact of various parameters, like the properties of the supernova ejecta, of the inner pulsar, as well of the ambient medium, upon the extent of the reverberation phase of PWNe. We investigate how different prescriptions shift the starting time of the reverberation phase, how this affects the amount of the compression, and how much of this can be ascribable to the radiation processes. Some critical aspects are the description of the reverse shock evolution, the efficiency by which at later times material from the ejecta accretes on to the swept-up shell around the PWN, and finally the density, velocity, and pressure profiles in the surrounding supernova remnant. We have explicitly treated the cases of the Crab Nebula, and of J1834.9-0846, taken to be representatives of the more and the less energetic pulsars, respectively. Especially for the latter object, the prediction of large compression factors is confirmed, even larger in the presence of radiative losses, also confirming our former prediction of periods of superefficiency during the reverberation phase of some PWNe., This work has been supported by grants PGC2018-095512-B-I00, SGR2017-1383, AYA2017-92402-EXP, 2017-14-H.O ASI-INAF and INAF MAINSTREAM

Published
2020

25. Exploring the effects of magnetar bursts in pulsar wind nebulae

Author

Bing Zhang, Diego F. Torres, Jonathan Martin, and Ministerio de Ciencia, Innovación y Universidades (España)

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Spectral index, non-thermal [Radiation mechanisms], Radiation mechanisms: non-thermal, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, neutron [Stars], Astronomy and Astrophysics, Astrophysics, Magnetar, 01 natural sciences, Pulsar wind nebula, Stars: neutron, Magnetic field, Decay time, Pulsar, Space and Planetary Science, 0103 physical sciences, Total energy, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Order of magnitude
Abstract

We explore possible effects of a magnetar burst on the radio, X-ray, and gamma-ray flux of a pulsar wind nebula (PWN). We assume that the burst injects electron-positron pairs or powers the magnetic field and explore the total energy at injection and the spectral index needed in order to increase the X-ray flux by about one order of magnitude, as well as its decay time until reaching quiescence. We also explore magnetically powered phenomenology that could explain a temporary increase of the PWN synchrotron emitted flux and perhaps the relatively common lack of PWNe surrounding magnetars. This phenomenological study is of interest for fast radio bursts (FRBs) as well, given that the connection between magnetars and this kind of systems have been recently established observationally., This work has been supported by grants PGC2018-095512-B-I00, SGR2017-1383, and AYA2017-92402-EXP.

Published
2020

26. Motivando la construcción de conocimiento colectivo a través del juego: un análisis de caso implementando medios físicos

Author

Diego F. Torres, María Julieta Lombardelli, and Alejandro Fernández

Subjects
Complementary and alternative medicine, Conceptual framework, Ciencias de la Computación e Información, Ciencia ciudadana, Ludification, Pharmaceutical Science, Pharmacology (medical), Collaborative work, Ludificación, Marco conceptual, Citizen science, Trabajo colaborativo, Wikipedia
Abstract

espanolActualmente, el juego es analizado como un elemento importante para motivar la interaccion de usuarios en diferentes tipos de entornos. Este analisis ha derivado en promover diferentes estrategias para adaptar elementos propios de los juegos y los videojuegos en contextos que no estan disenados como tal, pero en los que se busca estimular la participacion de los usuarios. Una estrategia al aplicar elementos de juego es considerar un modelo centrado en la experiencia del usuario. Sin embargo, para establecer un diseno de juego en contextos en donde prevalece el aspecto colaborativo, se requiere abordar estrategias especificas centradas en su relacion con la comunidad a la que pertenece. Este articulo presenta el diseno de un entorno ludificado basado en el marco conceptual G.A.M.E. acronimo de recopilacion, analisis, modelado y ejecucion (gathering, analysis, modeling and execution), aplicado a una comunidad de construccion colaborativa de conocimiento sobre Buenas Practicas Horticolas, complementado, ademas, con una interfaz fisica. EnglishCurrently, the game is analyzed as an important element to motivate the interaction of users in different types of environments. This analysis has resulted in promoting different strategies to adapt elements of games and video games in contexts that are not designed as such, but in which it seeks to stimulate the participation of users. One strategy when applying game elements is to consider a user experience-centric model. However, to establish a game design in contexts where the collaborative aspect prevails, it is necessary to address specific strategies focused on your relationship with the community to which you belong. This article introduces the design of a gaded environment based on the G.A.M.E. conceptual framework for gathering, analysis, modeling, and execution, applied to a collaborative building community of knowledge of Good Horticultural Practices, complemented by a physical interface portuguesAtualmente, o jogo e analisado como um elemento importante para motivar a interacao dos usuarios em diferentes tipos de ambientes. Essa analise resultou na promocao de diferentes estrategias para adaptar elementos de jogos e videogames em contextos que nao sao desenhados como tal, mas nos quais busca estimular a participacao dos usuarios. Uma estrategia na aplicacao de elementos de jogo e considerar um modelo centrado na experiencia do usuario. No entanto, para estabelecer um design de jogo em contextos onde o aspecto colaborativo prevalece, e necessario abordar estrategias especificas focadas em seu relacionamento com a comunidade a qual voce pertence. Este artigo introduz o desenho de um ambiente gaded baseado no quadro conceitual G.A.M.E. para coleta, analise, modelagem e execucao, (gathering, analysis, modeling and execution) aplicado a uma comunidade de construcao colaborativa de conhecimento de Boas Praticas Horticulturais, complementado por uma interface fisica.

Published
2020
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27. An Extension to Scenarios to Deal with Business Cases for the Decision-Making Processes in the Agribusiness Domain

Author

Julián Grigera, Mariángeles Hozikian, Alejandro Fernández, Roxana Silvia Giandini, Diego F. Torres, Cecilia Challiol, Alejandra Beatriz Lliteras, Pascale Zaraté, Leandro Antonelli, Jonathan Martin, Guy Camilleri, Laboratorio de Investigación y Formación en Informática Avanzada [La Plata] (LIFIA), Facultad de Ciencias Exactas [La Plata], Universidad Nacional de la Plata [Argentine] (UNLP)-Universidad Nacional de la Plata [Argentine] (UNLP), Systèmes Multi-Agents Coopératifs (IRIT-SMAC), Institut de recherche en informatique de Toulouse (IRIT), Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse - Jean Jaurès (UT2J)-Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut National Polytechnique (Toulouse) (Toulouse INP), Université Fédérale Toulouse Midi-Pyrénées-Université Toulouse 1 Capitole (UT1), Université Fédérale Toulouse Midi-Pyrénées, Université Toulouse III - Paul Sabatier (UT3), Consejo Nacional de Investigaciones Científicas y Técnicas [Buenos Aires] (CONICET), Comision de Investigaciones Cientificas de la Provincia de BsAs (CICPBA), Universidad Nacional de Quilmes (UNQ), Argumentation, Décision, Raisonnement, Incertitude et Apprentissage (IRIT-ADRIA), Hernández, Jorge E., and Kacprzyk, Janusz

Subjects
Decision support system, Vocabulary, Glossary, Computer science, media_common.quotation_subject, Decision Support, Ciencias Informáticas, 02 engineering and technology, Machine learning, computer.software_genre, Lexicon, [INFO.INFO-AI]Computer Science [cs]/Artificial Intelligence [cs.AI], Domain (software engineering), Scenarios, 0202 electrical engineering, electronic engineering, information engineering, Business case, media_common, business.industry, 020207 software engineering, [INFO.INFO-RO]Computer Science [cs]/Operations Research [cs.RO], Uncertainties, LEL, Ciencias de la Computación, Decision support, Complement (complexity), Agri-business, 020201 artificial intelligence & image processing, Artificial intelligence, business, computer, Natural language
Abstract

With the aim of pushing innovation through information and communication technology in the agri-business field, working closely with farmers is essential. It is especially important to systematically capture their knowledge in order to analyze, propose and design innovation artifacts (in terms of software applications). In this article, we use Scenarios to capture the knowledge of the experts that is elicited in early meetings previous to the definition of requirements. At those early stages, there are many uncertainties, and we are particularly interested in decision support. Thus, we propose an extension of the Scenarios for dealing with uncertainties. Scenarios are described in natural language, and it is very important to have an unbiased vocabulary. We complement Scenarios with a specific glossary, the Language Extended Lexicon that is also extended to decision support. According to V-model life cycle, every stage has a testing related stage. Thus, we also propose a set of rules to derive tests from the Scenarios. Summing up, we propose (i) an extension to Scenarios and the Language Extended Lexicon templates, (ii) a set of rules to derive tests, and (iii) an application to support the proposed technique. We have applied the proposed approach in a couple of case studies and we are confident that the results are promising. Nevertheless, we need to perform a further exhaustive validation. Laboratorio de Investigación y Formación en Informática Avanzada

Published
2020
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28. Towards a collaborative experience to generate knowledge: Use of gamification in robotics for Good Agricultural Practices

Author

Alejandro Fernández, Julieta Lombardelli, Blas Butera, and Diego F. Torres

Subjects
Good agricultural practice, Agricultural, Knowledge management, business.industry, Computer science, Interface (Java), lcsh:T, Ciencias Informáticas, Robotics, Context (language use), lcsh:Technology, Gamification, Ciencias de la Computación e Información, Cooperative community, Knowledge use, Robot, Artificial intelligence, business, Collaborative, and collaborative
Abstract

Currently gamification strategies are implemented in the most diverse fields. This paper discusses the design of gamification environment on a collaborative wiki on good agricultural practices. The aim of the project is to present a gamification design is complemented by a robotic interface, aimed at increasing customizing the experience from a cooperative community context. The robot interface also presents the possibility of containing a living organism, linked to the actions of the wiki., Laboratorio de Investigación y Formación en Informática Avanzada

Published
2020

29. Introducing the HD+B model for pulsar wind nebulae: a hybrid hydrodynamics/radiative approach

Author

B. Olmi and Diego F. Torres

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, 010308 nuclear & particles physics, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Perspective (graphical), Population, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, 01 natural sciences, Spectral line, Characterization (materials science), Identification (information), Pulsar, Space and Planetary Science, Sky, 0103 physical sciences, Radiative transfer, education, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, media_common
Abstract

Identification and characterization of a rapidly increasing number of pulsar wind nebulae is, and will continue to be, a challenge of high-energy gamma-ray astrophysics. Given that such systems constitute -- by far -- the most numerous expected population in the TeV regime, such characterization is important not only to learn about the sources per se from an individual and population perspective, but also to be able to connect them with observations at other frequencies, especially in radio and X-rays. Also, we need to remove the emission from nebulae in highly confused regions of the sky for revealing other underlying emitters. In this paper we present a new approach for theoretical modelling of pulsar wind nebulae: a hybrid hydrodynamic-radiative model able to reproduce morphological features and spectra of the sources, with relatively limited numerical cost., Comment: 15 pages, 9 figures

Published
2020
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30. The Fourth Catalog of Active Galactic Nuclei Detected by the Fermi Large Area Telescope

Author

Michael Kreter, Carmelo Sgrò, Riccardo Rando, Leonid Petrov, E. Nuss, M. Kuss, Nicola Omodei, M. Orienti, Diego F. Torres, M. Yassine, E. Hays, Francesco Massaro, G. Jóhannesson, L. S. Ojha, S. Harita, Frank K. Schinzel, Marco Ajello, E. Orlando, S. Maldera, B. Lott, R. Itoh, Jean Ballet, S. Garrappa, G. Martí-Devesa, F. Piron, G. M. Madejski, Francesco Longo, Manuel Meyer, Eleonora Torresi, R. Bonino, Giacomo Principe, Stefano Ciprini, J. Li, E. Troja, Marcello Giroletti, Nestor Mirabal, A. Reimer, Stefan Funk, P. van Zyl, Melissa Pesce-Rollins, Eugenio Bottacini, J. F. Ormes, P. Fusco, F. Gargano, Elliott D. Bloom, C. Leto, F. Fana Dirirsa, N. Di Lalla, C. C. Cheung, J. Valverde, Stefan Larsson, Sylvain Guiriec, Alberto Manfreda, Denis Bastieri, Z. Pei, A. Morselli, Igor V. Moskalenko, Soebur Razzaque, P. de la Torre Luque, Mn Mazziotta, Elizabeth C. Ferrara, Olaf Reimer, Justin D. Finke, I. A. Grenier, M. Razzano, F. de Palma, Filippo D'Ammando, D. J. Suson, D. Costantin, Nicola Giglietto, Yutaro Tachibana, Vaidehi S. Paliya, F. Loparco, R. Angioni, E. Cavazzuti, M. N. Lovellette, P. Lubrano, J. Becerra González, H. Poon, Gloria Spandre, E. J. Siskind, Giulia Migliori, Aaron Dominguez, Elisabetta Bissaldi, R. A. Cameron, David A. Green, Rodrigo Nemmen, D. J. Thompson, D. Horan, P. Bruel, Magnus Axelsson, R. de Menezes, Anna Franckowiak, S. Buson, Ioannis Liodakis, S. Rainò, Tsunefumi Mizuno, Yasushi Fukazawa, P. Spinelli, Ronaldo Bellazzini, Francesco Giordano, Fabio Cafardo, Bindu Rani, Dario Gasparrini, Felicia Krauss, Abhishek Desai, Sina Chen, L. Di Venere, Roopesh Ojha, H. A. Peña-Herazo, Massimo Persic, D. Serini, Guido Barbiellini, I. Mereu, S. Cutini, M. E. Monzani, M. Negro, Miloš Kovačević, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Fermi-LAT, National Aeronautics and Space Administration (US), Department of Energy (US), Commissariat à l'Ènergie Atomique et aux Ènergies Alternatives (France), Centre National de la Recherche Scientifique (France), Institut National de Physique Nucléaire et de Physique des Particules (France), Agenzia Spaziale Italiana, Istituto Nazionale di Fisica Nucleare, Ministry of Education, Culture, Sports, Science and Technology (Japan), High Energy Accelerator Research Organization (Japan), Japan Aerospace Exploration Agency, Knut and Alice Wallenberg Foundation, Swedish Research Council, Swedish National Space Board, Istituto Nazionale di Astrofisica, Ajello, M., Angioni, R., Axelsson, M., Ballet, J., Barbiellini, G., Bastieri, D., Becerra Gonzalez, J., Bellazzini, R., Bissaldi, E., Bloom, E. D., Bonino, R., Bottacini, E., Bruel, P., Buson, S., Cafardo, F., Cameron, R. A., Cavazzuti, E., Chen, S., Cheung, C. C., Ciprini, S., Costantin, D., Cutini, S., D'Ammando, F., De La Torre Luque, P., De Menezes, R., De Palma, F., Desai, A., Di Lalla, N., Di Venere, L., Dominguez, A., Dirirsa, F. F., Ferrara, E. C., Finke, J., Franckowiak, A., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Garrappa, S., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Green, D., Grenier, I. A., Guiriec, S., Harita, S., Hays, E., Horan, D., Itoh, R., Johannesson, G., Kovac'Evic', M., Krauss, F., Kreter, M., Kuss, M., Larsson, S., Leto, C., Li, J., Liodakis, I., Longo, F., Loparco, F., Lott, B., Lovellette, M. N., Lubrano, P., Madejski, G. M., Maldera, S., Manfreda, A., Marti-Devesa, G., Massaro, F., Mazziotta, M. N., Mereu, I., Meyer, M., Migliori, G., Mirabal, N., Mizuno, T., Monzani, M. E., Morselli, A., Moskalenko, I. V., Negro, M., Nemmen, R., Nuss, E., Ojha, L. S., Ojha, R., Omodei, N., Orienti, M., Orlando, E., Ormes, J. F., Paliya, V. S., Pei, Z., Peña-Herazo, H., Persic, M., Pesce-Rollins, M., Petrov, L., Piron, F., Poon, H., Principe, G., Raino, S., Rando, R., Rani, B., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Schinzel, F. K., Serini, D., Sgro, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tachibana, Y., Thompson, D. J., Torres, D. F., Torresi, E., Troja, E., Valverde, J., Van Zyl, P., Yassine, M., Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), and 33379009 - Kreter, Michael

Subjects
galaxies [Gamma rays], Astrophysics, Blazar, 01 natural sciences, law.invention, observations [Gamma rays], Spitzer Space Telescope, Astrophysical jet, law, Relativistic jet, 010303 astronomy & astrophysics, ComputingMilieux_MISCELLANEOUS, Quasar, Physics, education.field_of_study, Galaxies: active, Quasars: general, Gamma rays: galaxies, Gamma-ray source, BL Lacertae objects, Astrophysics - High Energy Astrophysical Phenomena, Active galactic nucleus, active [Galaxies], Astrophysics::High Energy Astrophysical Phenomena, Population, BL Lacertae objetcs: general, Astrophysics::Cosmology and Extragalactic Astrophysics, Gamma rays: observations, Telescope, 0103 physical sciences, Active galactic nuclei, Blazars, Gamma-ray sources, Relativistic jets, Quasars, education, Astrophysics::Galaxy Astrophysics, 010308 nuclear & particles physics, general [Quasars], Astronomy and Astrophysics, general [BL Lacertae objetcs], [SDU]Sciences of the Universe [physics], Galaxies: jets, Space and Planetary Science, jets [Galaxies], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract

The fourth catalog of active galactic nuclei (AGNs) detected by the Fermi Gamma-ray Space Telescope Large Area Telescope (4LAC) between 2008 August 4 and 2016 August 2 contains 2863 objects located at high Galactic latitudes (|b| > 10°). It includes 85% more sources than the previous 3LAC catalog based on 4 yr of data. AGNs represent at least 79% of the high-latitude sources in the fourth Fermi-Large Area Telescope Source Catalog (4FGL), which covers the energy range from 50 MeV to 1 TeV. In addition, 344 gamma-ray AGNs are found at low Galactic latitudes. Most of the 4LAC AGNs are blazars (98%), while the remainder are other types of AGNs. The blazar population consists of 24% Flat Spectrum Radio Quasars (FSRQs), 38% BL Lac-type objects, and 38% blazar candidates of unknown types (BCUs). On average, FSRQs display softer spectra and stronger variability in the gamma-ray band than BLQLacs do, confirming previous findings. All AGNs detected by ground-based atmospheric Cerenkov telescopes are also found in the 4LAC., The Fermi LAT Collaboration acknowledges generous ongoing support from a number of agencies and institutes that have supported both the development and the operation of the LAT as well as scientific data analysis. These include the National Aeronautics and Space Administration and the Department of Energy in the United States, the Commissariat `a l’Energie Atomique and the Centre National de la Recherche Scientifique / Institut National de Physique Nucl´eaire et de Physique des Particules in France, the Agenzia Spaziale Italiana and the Istituto Nazionale di Fisica Nucleare in Italy, the Ministry of Education, Culture, Sports, Science and Technology (MEXT), High Energy Accelerator Research Organization (KEK) and Japan Aerospace Exploration Agency (JAXA) in Japan, and the K. A. Wallenberg Foundation, the Swedish Research Council and the Swedish National Space Board in Sweden. Additional support for science analysis during the operations phase is gratefully acknowledged from the Istituto Nazionale di Astrofisica in Italy and the Centre National d’Etudes Spatiales in France. This work performed in part under DOE Contract DE- AC02-76SF00515. This research has made use of data obtained from the high-energy Astrophysics Science Archive Research Center (HEASARC) provided by NASA’s Goddard Space Flight Center; the SIMBAD database operated at CDS, Strasbourg, France; the NASA/IPAC Extragalactic Database (NED) operated by the Jet Propulsion Laboratory, California Institute of Technology, under contract with the National Aeronautics and Space Administration. This research has made use of data archives, catalogs and software tools from the ASDC, a facility managed by the Italian Space Agency (ASI). Part of this work is based on the NVSS (NRAO VLA Sky Survey). The National Radio Astronomy Observatory is operated by Associated Universities, Inc., under contract with the National Science Foundation. This publication makes use of data products from the Two Micron All Sky Survey, which is a joint project of the University of Massachusetts and the Infrared Processing and Analysis Center/California Institute of Technology, funded by the National Aeronautics and Space Administration and the National Science Foundation. This publication makes use of data products from the Wide-field Infrared Survey Explorer, which is a joint project of the University of California, Los Angeles, and the Jet Propulsion Laboratory/California Institute of Technology, funded by the National Aeronautics and Space Administration. Funding for the SDSS and SDSS-II has been provided by the Alfred P. Sloan Foundation, the Participating Institutions, the National Science Foundation, the U.S. Department of Energy, the National Aeronautics and Space Administration, the Japanese Monbukagakusho, the Max Planck Society, and the Higher Education Funding Council for England. The SDSS Web Site is http://www.sdss.org/. The SDSS is managed by the Astrophysical Research Consortium for the Participating Institutions. The Participating Institutions are the American Museum of Natural History, Astrophysical Institute Potsdam, University of Basel, University of Cambridge, Case Western Reserve University, University of Chicago, Drexel University, Fermilab, the Institute for Advanced Study, the Japan Participation Group, Johns Hopkins University, the Joint Institute for Nuclear Astrophysics, the Kavli Institute for Particle Astrophysics and Cosmology, the Korean Scientist Group, the Chinese Academy of Sciences (LAMOST), Los Alamos National Laboratory, the Max-Planck-Institute for Astronomy (MPIA), the Max-Planck-Institute for Astrophysics (MPA), New Mexico State University, Ohio State University, University of Pittsburgh, University of Portsmouth, Princeton University, the United States Naval Observatory, and the University of Washington.

Published
2020
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31. Gamma-ray heartbeat powered by the microquasar SS 433

Author

Emma de Oña Wilhelmi, Y. Su, Jian Li, Ruo-Yu Liu, Matthew Kerr, and Diego F. Torres

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010504 meteorology & atmospheric sciences, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, Binary number, Astronomy and Astrophysics, Quasar, Astrophysics, Compact star, 01 natural sciences, Computer Science::Digital Libraries, Magnetic field, Spitzer Space Telescope, 13. Climate action, 0103 physical sciences, Astrophysics - High Energy Astrophysical Phenomena, Variation (astronomy), 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Fermi Gamma-ray Space Telescope
Abstract

arXiv:2008.10523v1, Microquasars, the local siblings of extragalactic quasars, are binary systems comprising a compact object and a companion star. By accreting matter from their companions, microquasars launch powerful winds and jets, influencing the interstellar environment around them. Steady gamma-ray emission is expected to rise from their central objects, or from interactions between their outflows and the surrounding medium. The latter prediction was recently confirmed with the detection of SS 433 at high (TeV) energies1. In this report, we analyse more than ten years of gigaelectronvolt gamma-ray data from the Fermi Gamma-ray Space Telescope on this source. Detailed scrutiny of the data reveal emission in the vicinity of SS 433, co-spatial with a gas enhancement, and hints of emission possibly associated with a terminal lobe of one of the jets. Both gamma-ray excesses are relatively far from the central binary, and the former shows evidence of a periodic variation at the precessional period of SS 433, linking it with the microquasar. This result challenges obvious interpretations and is unexpected from previously published theoretical models. It provides us with a chance to unveil the particle transport from SS 433 and to probe the structure of the magnetic field in its vicinity.

Published
2020

32. Introducing a special collection of papers in the Journal of High Energy Astrophysics on the Early Results of China's 1st X-ray Astronomy Satellite: Insight-HXMT

Author

Shuang-Nan Zhang and Diego F. Torres

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), X-ray astronomy, High-energy astronomy, Computer science, Physics::Instrumentation and Detectors, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Galactic plane, Computer Science::Digital Libraries, Early results, Space and Planetary Science, Satellite, Astrophysics - High Energy Astrophysical Phenomena, China
Abstract

Insight-HXMT is the first Chinese X-ray astronomical mission, launched successfully on June 15, 2017, from China's Jiuquan Satellite Launch Center. Insight-HXMT was designed to have a broad energy coverage in X-rays, from 1-250 keV, with excellent timing and adequate energy resolution at soft X-rays, and the largest effective area at hard X-rays. Here, we present a collection of papers of the Journal of High Energy Astrophysics on the Early Results of China's 1st X-ray Astronomy Satellite Insight-HXMT. These papers cover the in-orbit performance, the background model, and all calibration results, together with several first results on observations of binaries and details on the Galactic plane survey., Comment: Published to introduce a set of 20+ papers from the HXMT collaboration. Most of the referred papers can be accessed in astro-ph already, and all will be avaialble from JHEAp's webpage too, at https://www.sciencedirect.com/journal/journal-of-high-energy-astrophysics/special-issue/10B0FLKPH6C

Published
2020

33. Exploring the superwind mechanism for generating ultrahigh-energy cosmic rays using large-scale modeling of starbursts

Author

Luis A. Anchordoqui, Diego F. Torres, National Science Foundation (US), National Aeronautics and Space Administration (US), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), and Generalitat de Catalunya

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Cosmic ray, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Astrophysics - Astrophysics of Galaxies, 01 natural sciences, Galaxy, Auger, Astrophysics of Galaxies (astro-ph.GA), 0103 physical sciences, Ultrahigh energy, Astrophysics - High Energy Astrophysical Phenomena, 010306 general physics, Anisotropy, Scale model, Astrophysics::Galaxy Astrophysics
Abstract

The Pierre Auger collaboration has provided a compelling indication for a possible correlation between the arrival directions of ultrahigh-energy cosmic rays and nearby starburst galaxies. Herein we show how the latest large-scale modeling of starburst galaxies is compatible with the cosmic rays producing the anisotropy signal being accelerated at the terminal shock of superwinds., The research of L. A. A. is supported by the U.S. National Science Foundation (NSF Grant No. PHY-1620661) and the National Aeronautics and Space Administration (NASA Grant No. 80NSSC18K0464). The research of D. F. T. is supported by Grants No. PGC2018-095512-BI00, No. AYA2017-92402-EXP, and No. SGR 2017-1383.

Published
2020

34. The X-Ray Outburst of the Galactic Center Magnetar over Six Years of Chandra Observations

Author

Sergio Campana, Alessandro Papitto, Rosalba Perna, G. L. Israel, Daniele Viganò, José A. Pons, Frederick K. Baganoff, Silvia Zane, Gabriele Ponti, Daryl Haggard, A. Borghese, Sandro Mereghetti, Roberto Mignani, Diego F. Torres, Paolo Esposito, Nanda Rea, F. Coti Zelati, Roberto Turolla, Luigi Stella, ITA, Universidad de Alicante. Departamento de Física Aplicada, Astrofísica Relativista, European Commission, Istituto Nazionale di Astrofisica, Natural Sciences and Engineering Research Council of Canada, Fonds de Recherche du Québec, Canadian Institute for Advanced Research, Generalitat Valenciana, Agencia Estatal de Investigación (España), Chandra X-ray Observatory, National Aeronautics and Space Administration (US), and Smithsonian Institution

Subjects
010504 meteorology & atmospheric sciences, Astrophysics::High Energy Astrophysical Phenomena, Financial Contributions, Library science, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Neutron stars, Magnetars, Pulsars, Observatory, 0103 physical sciences, Presidential decree, Cost action, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, 0105 earth and related environmental sciences, Astronomía y Astrofísica, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astronomy and Astrophysics, 13. Climate action, Space and Planetary Science, Astrophysics - High Energy Astrophysical Phenomena, Research center
Abstract

The magnetar SGR J1745-2900, discovered at a distance of parsecs from the Milky Way central black hole, Sagittarius A, represents the closest pulsar to a supermassive black hole ever detected. Furthermore, its intriguing radio emission has been used to study the environment of the black hole, as well as to derive a precise position and proper motion for this object. The discovery of SGR J1745-2900 has led to interesting debates about the number, age, and nature of pulsars expected in the Galactic center region. In this work, we present extensive X-ray monitoring of the outburst of SGR J1745-2900 using the Chandra X-ray Observatory, the only instrument with the spatial resolution to distinguish the magnetar from the supermassive black hole (2.″4 angular distance). It was monitored from its outburst onset in 2013 April until 2019 August, collecting more than 50 Chandra observations for a total of more than 2.3 Ms of data. Soon after the outburst onset, the magnetar emission settled onto a purely thermal emission state that cooled from a temperature of about 0.9-0.6 keV over 6 yr. The pulsar timing properties showed at least two changes in the period derivative, increasing by a factor of about 4 during the outburst decay. We find that the long-term properties of this outburst challenge current models for the magnetar outbursts., N.R., D.V., and A.B. are supported by the H2020 ERC Consolidator Grant “MAGNESIA” under grant agreement No. 817661 (PI: Rea). N.R., F.C.Z., D.V., A.B., and D.F.T. also acknowledge support from grants SGR2017-1383 and PGC2018-095512-BI00. F.C.Z. is supported by a Juan de la Cierva fellowship. A.P. acknowledges financial support from grants ASI/INAF I/037/12/0, ASI/INAF 2017-14- H.0 (PI: Belloni) and from INAF grant “Sostegno alla ricerca scientifica main streams dell’INAF,” Presidential Decree 43/2018 (PI: Belloni). D.H. acknowledges support from the Natural Sciences and Engineering Research Council of Canada (NSERC) Discovery Grant, the Fonds de recherche du Québec–Nature et Technologies (FRQNT) Nouveaux Chercheurs program, and the Canadian Institute for Advanced Research (CIFAR). G.L.I., S.M., and R.T. have been partially supported by PRIN-MIUR 2017. J.A.P. acknowledges support by the Generalitat Valenciana (PROMETEO/2019/071) and by Agencia Estatal de Investigación (PGC2018-095984- B-I00). G.P. is supported by the H2020 ERC Consolidator Grant “Hot Milk” under grant agreement No. 865637. L.S. acknowledges financial contributions from ASI-INAF agreements 2017-14-H.O and I/037/12/0 and from “iPeska” research grant (PI: Andrea Possenti) funded under the INAF call PRIN-SKA/CTA (resolution 70/2016). We acknowledge support from the PHAROS COST Action (CA16214). This article is based on data obtained with the Chandra X-ray Observatory, and on software and tools provided by the High Energy Astrophysics Science Archive Research Center (HEASARC), which is a service of the Astrophysics Science Division at NASA/GSFC and the High Energy Astrophysics Division of the Smithsonian Astrophysical Observatory. We thank the referee for useful suggestions. We are grateful to Giovanni Fazio, Joseph Hora, Gordon Garmire, and Steven Willner, and their proposal co-Is, for sharing their data.

Published
2020

35. The INTEGRAL view of the pulsating hard X-ray sky: from accreting and transitional millisecond pulsars to rotation-powered pulsars and magnetars

Author

R. Iaria, F. Coti Zelati, Alessandro Papitto, Andrii Neronov, Paolo Esposito, V. G. Savchenko, Filippo Ambrosino, Nanda Rea, Ada Paizis, Juri Poutanen, V. De Falco, J. Li, Ph. Laurent, Enrico Bozzo, Teresa Mineo, Maurizio Falanga, A. Riggio, Aga Słowikowska, Andrew Shearer, Sandro Mereghetti, Lucien Kuiper, C. Gouiffes, D. de Martino, M. Forot, W. Hermsen, Andrea Tiengo, Zhaosheng Li, A. Sanna, D. Gotz, T. Di Salvo, Diego F. Torres, Carlo Ferrigno, P. Moran, Département d'Astrophysique (ex SAP) (DAP), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Papitto A., Falanga M., Hermsen W., Mereghetti S., Kuiper L., Poutanen J., Bozzo E., Ambrosino F., Coti Zelati F., De Falco V., de Martino D., Di Salvo T., Esposito P., Ferrigno C., Forot M., Gotz D., Gouiffes C., Iaria R., Laurent P., Li J., Li Z., Mineo T., Moran P., Neronov A., Paizis A., Rea N., Riggio A., Sanna A., Savchenko V., Slowikowska A., Shearer A., Tiengo A., Torres D.F., High Energy Astrophys. & Astropart. Phys (API, FNWI), Ministerio de Ciencia, Innovación y Universidades (España), Agencia Estatal de Investigación (España), Generalitat de Catalunya, Agenzia Spaziale Italiana, Alexander von Humboldt Foundation, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), and Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité)

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics, Magnetar, Quantitative Biology::Other, Computer Science::Digital Libraries, 01 natural sciences, Neutron stars, X-rays: binaries, Settore FIS/05 - Astronomia E Astrofisica, Pulsar, Millisecond pulsar, 0103 physical sciences, Magnetars, Accretion disks, magnetars, neutron stars, pulsar, X-rays:binaries, X-rays:bursts, education, X-rays: bursts, 010303 astronomy & astrophysics, Pulsars, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, 010308 nuclear & particles physics, Crab Pulsar, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Accretion (astrophysics), Neutron star, Space and Planetary Science, Accretion disks, Spin-up, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph]
Abstract

arXiv:2012.01346v1, et al., In the last 25 years a new generation of X-ray satellites imparted a significant leap forward in our knowledge of X-ray pulsars. The discovery of accreting and transitional millisecond pulsars proved that disk accretion can spin up a neutron star to a very high rotation speed. The detection of MeV-GeV pulsed emission from a few hundreds of rotation-powered pulsars probed particle acceleration in the outer magnetosphere, or even beyond. Also, a population of two dozens of magnetars has emerged. INTEGRAL played a central role to achieve these results by providing instruments with high temporal resolution up to the hard X-ray/soft, γ-ray band and a large field of view imager with good angular resolution to spot hard X-ray transients. In this article we review the main contributions by INTEGRAL to our understanding of the pulsating hard X-ray sky, such as the discovery and characterization of several accreting and transitional millisecond pulsars, the generation of the first catalog of hard X-ray/soft γ-ray rotation-powered pulsars, the detection of polarization in the hard X-ray emission from the Crab pulsar, and the discovery of persistent hard X-ray emission from several magnetars., Al. P., D. d. M. and T. D. S. acknowledge financial support from ASI/INAF I/037/12/0, ASI/INAF 2017-14-H.0 (PI: De Rosa, PI: Belloni) and from INAF “Sostegno alla ricerca scientifica main streams dell’INAF”, Presidential Decree 43/2018 and from “SKA/CTA projects”, Presidential Decree N. 70/2016. J.P. was supported by the Ministry of Science and Higher Education of the Russian Federation grant 14.W03.31.0021. The INTEGRAL French teams acknowledge partial funding from the French Space Agency (CNES). Z.L. thanks the International Space Science Institute in Bern for the hospitality. Z.L was supported by National Natural Science Foundation of China (Grant nos. U1938107, 11703021, U1938107, 11873041). Ad. P. and S. M. acknowledge continuous support from the Italian Space Agency ASI through the ASI/INAF agreement n.2019-35-HH. D. F. T and the group at the Institute of Space Sciences acknowledges support via grants PGC2018-095512-B-I00, SGR2017-1383, and AYA2017-92402-EXP. F .C. Z. is supported by a Juan de la Cierva fellowship. V. D. F. acknowledges Silesian University in Opava and Gruppo Nazionale di Fisica Matematica of Istituto Nazionale di Alta Matematica for support. This research was supported by the Polish National Science Centre grant number 2017/25/B/ST9/02805. J.L. acknowledges the support from the Alexander von Humboldt Foundation.

Published
2020
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36. NuSTAR and Parkes observations of the transitional millisecond pulsar binary XSS J12270-4859 in the rotation-powered state

Author

Nanda Rea, D. de Martino, Diego F. Torres, T. M. Belloni, F. Coti Zelati, A. Possenti, M. Burgay, Alessandro Papitto, Agenzia Spaziale Italiana, Istituto Nazionale di Astrofisica, Ministerio de Economía y Competitividad (España), Ministerio de Ciencia, Innovación y Universidades (España), and ITA

Subjects
media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Library science, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, Individual:XSS J12270-4859 (aka 1FGL J1227.9-4852, 2FGL J1227.7-4853, 3FGL J1227.9-4854, PSR J1227-4853) [Stars], 01 natural sciences, Stars: Individual:XSS J12270-4859 (aka 1FGL J1227.9-4852, 2FGL J1227.7-4853, 3FGL J1227.9-4854, PSR J1227-4853), Gammarays: Stars -X-rays: Binaries, State (polity), Millisecond pulsar, Binaries: close, 0103 physical sciences, Presidential decree, Cost action, 010303 astronomy & astrophysics, media_common, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Stars -X-rays: Binaries [Gammarays], Pulsars: General, Astronomy and Astrophysics, General [Pulsars], Space and Planetary Science, Christian ministry, Astrophysics - High Energy Astrophysical Phenomena, Partial support, close [Binaries]
Abstract

We report on the first NuSTAR observation of the transitional millisecond pulsar binary XSS J12270-4859 during its current rotation-powered state, complemented with a 2.5 yr-long radio monitoring at Parkes telescope and archival XMM-Newton and Swift X-ray and optical data. The radio pulsar is mainly detected at 1.4 GHz displaying eclipses over ∼ 40 per cent of the 6.91 h orbital cycle. We derive a new updated radio ephemeris to study the 3- 79 keV light curve that displays a significant orbital modulation with fractional amplitude of 28 ± 3 per cent, a structured maximum centred at the inferior conjunction of the pulsar and no cycle-to-cycle or low-high-flaring mode variabilities. The average X-ray spectrum, extending up to ∼70 keV without a spectral break, is well described by a simple power law with photon index γ = 1.17 ± 0.08 giving a 3-79 keV luminosity of 7.6+3.8 -0.8 × 1032 erg s-1 for a distance of 1.37+0.69 -0.15 kpc. Energy resolved orbital light curves reveal that the modulation is not energy dependent from 3 to 25 keV and is undetected with an upper limit of ∼10 per cent above 25 keV. Comparison with previous X-ray XMM-Newton observations in common energy ranges confirms that themodulation amplitudes vary on time-scales of a fewmonths, indicative of a non-stationary contribution of the intrabinary shock (IBS) formed by the colliding winds of the pulsar and the companion. A more detailed inspection of energy resolved modulations than previously reported gives hints of a mild softening at superior conjunction of the pulsar below 3 keV, likely due to the contribution of the thermal emission from the neutron star. The IBS emission, if extending into the MeV range, would be energetically capable alone to irradiate the donor star., DdM, AP, and TMB acknowledge financial support from the Italian Space Agency (ASI) and National Institute for Astrophysics (INAF) under agreements ASI-INAF I/037/12/0 and ASI-INAF n.2017-14-H.0 and from INAF ‘Sostegno alla ricerca scientifica main streams dell’INAF’, Presidential Decree 43/2018. DdM, AP, MB, and AP also acknowledge support from INAF ‘SKA/CTA projects’, Presidential Decree 70/2016. DFT acknowledges support from the Spanish Ministry of Economy, Industry and Competitiveness grants PGC2018-095512-B-I00, SGR2017-1383, and AYA2017-92402-EXP. FCZ is supported by a Juan de la Cierva fellowship and grants from the Spanish Ministry of Economy, Industry and Comeptitiveness grants SGR2017-1383 and PGC2018-095512-B-I00. We also thank the ‘PHAROS’ COST Action (CA16214) for partial support.

Published
2020

37. Advances in Understanding High-Mass X-ray Binaries with INTEGRALand Future Directions

Author

Jörn Wilms, Colleen A. Wilson-Hodge, Julia Alfonso-Garzon, Paul Hemphill, Antonios Manousakis, J. Rodriguez, Lara Sidoli, P. Romano, Jian Li, Jose M. Torrejon, Katja Pottschmidt, Sergey S. Tsygankov, S. Martínez-Núñez, Andrea Santangelo, Diego F. Torres, A. J. Bird, I. Kreykenbohm, Pere Blay, Victoria Grinberg, Peter Kretschmar, Vanessa McBride, Felix Fürst, N. Masetti, Ignacio Negueruela, J. J. Rodes-Roca, Carlo Ferrigno, Matthias Kühnel, J. Miguel Mas-Hesse, Arash Bodaghee, Andrii Neronov, Pablo Reig, S. Fritz, A. Paizis, Shu Zhang, Alexander A. Lutovinov, Isabel Caballero, Maurizio Falanga, Enrico Bozzo, John A. Tomsick, Masha Chernyakova, Lorenzo Ducci, Roland Walter, S. A. Grebenev, Richard E. Rothschild, M. J. Coe, A. Domingo, Sylvain Chaty, Rüdiger Staubert, Konstantin Postnov, Vito Sguera, Victor Doroshenko, Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC, MDM-2017-0737, Wilms, J. [0000-0003-2065-5410], Santangelo, A. [0000-0003-4187-9560], Grinberg, V. [0000-0003-2538-0188], Sguera, V. [0000-0001-8202-9381], Martínez Núñez, S. [0000-0002-5134-4191], Rodes Roca, J. J. [0000-0003-4363-8138], Agenzia Spaziale Italiana (ASI), Istituto Nazionale Astrofisica (INAF), Russian Foundation for Basic Research (RFBR), Agencia Estatal de Investigación (AEI), Universidad de Alicante. Departamento de Física Aplicada, Universidad de Alicante. Departamento de Física, Ingeniería de Sistemas y Teoría de la Señal, Universidad de Alicante. Instituto Universitario de Física Aplicada a las Ciencias y las Tecnologías, Astrofísica Estelar (AE), Astronomía y Astrofísica, Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), ITA, USA, GBR, FRA, DEU, ESP, CHL, FIN, GRC, IRL, CHN, ZAF, RUS, CHE, Ministerio de Economía y Competitividad (MINECO), and Unidad de Excelencia Científica María de Maeztu Centro de Astrobiología del Instituto Nacional de Técnica Aeroespacial y CSIC

Subjects
Accretion, Integral observatory, Electromagnetic spectrum, X-ray binary, Binary number, magnetic field, 01 natural sciences, Gravitation, observations [Gamma rays], accretion, Física Aplicada, massive [star], binary [X-ray], 010303 astronomy & astrophysics, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, education.field_of_study, energy: high, INTEGRAL observatory, infrared, high [energy], X-ray: binary, Astrophysics - High Energy Astrophysical Phenomena, Phenomenology (particle physics), perturbation, Milky Way, Population, general [Pulsars], FOS: Physical sciences, VHE, X-rays: binaries, stars: neutron, pulsars: general, 0103 physical sciences, education, Astronomía y Astrofísica, 010308 nuclear & particles physics, Astronomy, Astronomy and Astrophysics, neutron [Stars], Galaxy, star: massive, electromagnetic, 13. Climate action, Space and Planetary Science, gravitation, Accretions, ddc:520, binaries [X-rays], galaxy, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], gamma rays: observations
Abstract

New astronomy reviews 86, 101546 (2019). doi:10.1016/j.newar.2020.101546, High mass X-ray binaries are among the brightest X-ray sources in the Milky Way, as well as in nearby Galaxies. Thanks to their highly variable emissions and complex phenomenology, they have attracted the interest of the high energy astrophysical community since the dawn of X-ray Astronomy. In more recent years, they have challenged our comprehension of physical processes in many more energy bands, ranging from the infrared to very high energies.In this review, we provide a broad but concise summary of the physical processes dominating the emission from high mass X-ray binaries across virtually the whole electromagnetic spectrum. These comprise the interaction of stellar winds with the high gravitational and magnetic fields of compact objects, the behaviour of matter under extreme magnetic and gravity conditions, and the perturbation of the massive star evolutionary processes by presence in a binary system.We highlight the role of the INTEGRAL mission in the discovery of many of the most interesting objects in the high mass X-ray binary class and its contribution in reviving the interest for these sources over the past two decades. We show how the INTEGRAL discoveries have not only contributed to significantly increase the number of high mass X-ray binaries known, thus advancing our understanding of the population as a whole, but also have opened new windows of investigation that stimulated the multi-wavelength approach nowadays common in most astrophysical research fields.We conclude the review by providing an overview of future facilities being planned from the X-ray to the very high energy domain that will hopefully help us in finding an answer to the many questions left open after more than 18 years of INTEGRAL scientific observations., Published by Elsevier Science, Amsterdam [u.a.]

Published
2019
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38. Observations of one young and three middle-aged γ-ray pulsars with the Gran Telescopio Canarias

Author

D. Salvetti, Nanda Rea, Vincenzo Testa, Diego F. Torres, E. de Oña Wilhelmi, Roberto Mignani, M. Marelli, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Gran Telescopio Canarias, Physics, Brightness, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, Spectral line, law.invention, Telescope, Pulsar, Space and Planetary Science, law, 0103 physical sciences, Optical emission spectroscopy, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics
Abstract

We used the 10.4m Gran Telescopio Canarias to search for the optical counterparts to four isolated $\gamma$-ray pulsars, all detected in the X-rays by either \xmm\ or \chan\ but not yet in the optical. Three of them are middle-aged pulsars -- PSR\, J1846+0919 (0.36 Myr), PSR\, J2055+2539 (1.2 Myr), PSR\, J2043+2740 (1.2 Myr) -- and one, PSR\, J1907+0602, is a young pulsar (19.5 kyr). For both PSR\, J1907+0602 and PSR\, J2055+2539 we found one object close to the pulsar position. However, in both cases such an object cannot be a viable candidate counterpart to the pulsar. For PSR\, J1907+0602, because it would imply an anomalously red spectrum for the pulsar and for PSR\, J2055+2539 because the pulsar would be unrealistically bright ($r'=20.34\pm0.04$) for the assumed distance and interstellar extinction. For PSR\, J1846+0919, we found no object sufficiently close to the expected position to claim a possible association, whereas for PSR\, J2043+2740 we confirm our previous findings that the object nearest to the pulsar position is an unrelated field star. We used our brightness limits ($g' \approx 27$), the first obtained with a large-aperture telescope for both PSR\, J1846+0919 and PSR\, J2055+2539, to constrain the optical emission properties of these pulsars and investigate the presence of spectral turnovers at low energies in their multi-wavelength spectra., Comment: 10 pages, 11 figures, accpted for publication in MNRAS

Published
2018

39. Nodos: Enciclopedia de las Artes Escénicas

Author

Facundo Correa, Diego F. Torres, Alejandro Fernández, Virginia Cepeda, and Alicia Díaz

Subjects
lcsh:Computer engineering. Computer hardware, General Computer Science, Intangible cultural heritage, Computer science, Ciencias Informáticas, Context (language use), Wiki semántica, lcsh:TK7885-7895, Ontology (information science), The arts, Semantic wiki, lcsh:QA75.5-76.95, Cultural heritage, World Wide Web, Patrimonio cultural intangible, Ontología en artes escénicas, Encyclopedia, Dynamism, Performing arts ontology, lcsh:Electronic computers. Computer science, Performing arts, Semantic Wiki
Abstract

The main goal of Nodos is to promote the collective creation of semantic knowledge regarding performing arts. Recording and curating information about these expressions contributes to the preservation of the Intangible Cultural Heritage, as defined by UNESCO. One of the challenges related to the preservation of information is the large amount of people involved in the creation and development of scenic arts and the dynamism in these theater pieces. The large number of plays presented every year makes it difficult to keep records up to date, resulting in the loss of knowledge about many cultural pieces. This article introduces a way to record such cultural heritage in the context of a citizen science project. Nodos defines an ontology regarding performing arts and also uses a semantic wiki that helps in the implementation of the ontology. An evaluation of usability shows Nodos as an effective initiative to preserve and study performing arts., Nodos es un proyecto que posee como objetivo promover y generar una exhaustiva base de conocimiento sobre artes performáticas. El registro de este tipo de artes contribuye a la preservación del Patrimonio Cultural Intangible definido por UNESCO. Uno de los desafíos está dado por la gran cantidad de personas vinculadas y el dinamismo que presentan las obras. La dificultad de documentar las numerosas obras presentadas cada año conlleva la pérdida de los registros de muchas de las obras. En este artículo se presenta una forma de registrar ese tipo de patrimonio cultural en el contexto de un proyecto de ciencia ciudadana. Específicamente, por medio de la definición de una ontología sobre las artes escénicas y la utilización de una wiki semántica. Finalmente, una evaluación de usabilidad muestra que Nodos es una iniciativa efectiva para preservar y estudiar a las artes escénicas., Laboratorio de Investigación y Formación en Informática Avanzada

Published
2017

40. Synchro-curvature modelling of the multi-frequency non-thermal emission of pulsars

Author

Jian Li, Francesco Coti Zelati, Daniele Viganò, and Diego F. Torres

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Observer (quantum physics), Astrophysics::High Energy Astrophysical Phenomena, Phase (waves), FOS: Physical sciences, Astronomy and Astrophysics, Astrophysics, Curvature, Light curve, Spectral line, Orders of magnitude (time), Pulsar, Space and Planetary Science, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, Scaling
Abstract

We apply a synchro-curvature spectral emission model based on characterizing the dynamics of magnetospheric particles to fit the phase-average spectra of the most extended database for the non-thermal spectra of pulsars. We consider 36 pulsars with well-determined non-thermal spectra from X-rays to gamma-rays. The sample includes Crab and Crab twin, for which the spectra extends even to the optical/ultraviolet and infrared energies. We find that the model --with just three physical parameters and a global scaling-- can fit the observations well across eight orders of magnitude for 18 of the 36 pulsars studied. Additionally, we find a set of 8 pulsars for which the model still provides arguably good fits and another set of 10 pulsars for which the model fails in reproducing the spectra. We discuss why, propose and provide physical interpretations for a simple model extension (related to the geometry of the accelerating system with regards to the observer) that allows dealing with all such cases, ultimately providing very good fits for all pulsars. The extended model is still austere, adding only two additional parameters to the former set, of the same kind of the ones previously used. We use these fits to discuss issues going from the observed spectral origin, to the extent of the dominance of synchrotron or curvature regimes, the use of a model as predictor for searching new non-thermal pulsars starting from gamma-ray surveys, and how the model offers a setting where phase shifts between X-ray and gamma-ray light curves would naturally arise., 20 pages, 15 figures, 2 tables. Accepted for publication in MNRAS on August 14

Published
2019
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41. Long-term gamma-ray observations of the binary HESS J0632+057 with H.E.S.S., MAGIC and VERITAS

Author

Denys Malyshev, Gerd Pühlhofer, Stefan Ohm, Raul Prado, Johannah Moepi, Oscar Blanch, Gernot Maier, Diego F. Torres, M. Lundy, Nukri Komin, Daniela Hadasch, Ben Zitzer, Stefan Schlenstedt, and A. López-Oramas

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, Gamma ray, FOS: Physical sciences, Context (language use), Astrophysics, Light curve, Orbital period, law.invention, Telescope, law, Observatory, Astrophysics::Solar and Stellar Astrophysics, MAGIC (telescope), Astrophysics - High Energy Astrophysical Phenomena, Cherenkov radiation
Abstract

The gamma-ray binary HESS J0632+057 has been observed at very-high energies (E $>$ 100 GeV) for more than ten years by the major systems of imaging atmospheric Cherenkov telescopes. We present a summary of results obtained with the H.E.S.S., MAGIC, and VERITAS experiments based on roughly 440 h of observations in total. This includes a discussion of an unusually bright TeV outburst of HESS J0632+057 in January 2018. The updated gamma-ray light curve now covers all phases of the orbital period with significant detections in almost all orbital phases. Results are discussed in context with simultaneous observations with the X-ray Telescope onboard the Neil Gehrels Swift Observatory., Proceedings of the 36th International Cosmic Ray Conference (ICRC2019) Madison, WI July 24-Aug 1, 2019

Published
2019
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42. The Galactic magnetic field in the light of starburst-generated ultrahigh-energy cosmic rays

Author

Luis A. Anchordoqui, Diego F. Torres, and Jorge F. Soriano

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, Cosmic ray, Hot spot (veterinary medicine), Astrophysics, Astrophysics::Cosmology and Extragalactic Astrophysics, Galaxy, Magnetic field, law.invention, Auger, Telescope, High Energy Physics - Phenomenology, High Energy Physics - Phenomenology (hep-ph), law, Ultrahigh energy, Astrophysics - High Energy Astrophysical Phenomena, Astrophysics::Galaxy Astrophysics
Abstract

Auger data show evidence for a correlation between ultrahigh-energy cosmic rays (UHECRs) and nearby starburst galaxies. This intriguing correlation is consistent with data collected by the Telescope Array, which have revealed a much more pronounced directional ``hot spot'' in arrival directions not far from the starburst galaxy M82. In this work, we assume starbursts are sources of UHECRs and investigate the prospects to use the observed distribution of UHECR arrival directions to constrain Galactic magnetic field models. We show that if the Telescope Array hot spot indeed originates from M82, UHECR data would place a strong constraint on the coherent and turbulent components of the Galactic magnetic field., To appear in Proceedings of the 36th International Cosmic Ray Conference

Published
2019

43. Towards observing reverberating and superefficient pulsar wind nebulae

Author

Diego F. Torres, Tingting Lin, and Francesco Coti Zelati

Subjects
Physics, High Energy Astrophysical Phenomena (astro-ph.HE), Nebula, Reverberation, 010308 nuclear & particles physics, Astrophysics::High Energy Astrophysical Phenomena, Monte Carlo method, Astronomy, FOS: Physical sciences, Astronomy and Astrophysics, Magnetar, 01 natural sciences, Luminosity, Supernova, Pulsar, Space and Planetary Science, 0103 physical sciences, Radiative transfer, Astrophysics - High Energy Astrophysical Phenomena, 010303 astronomy & astrophysics
Abstract

In a recent work, we numerically studied the radiative properties of the reverberation phase of pulsar wind nebulae (PWNe), i.e., when the reverse shock created by the supernova explosion travels back towards the pulsar, compressing the wind bubble. We focused on several well-characterized PWNe and used them as examples for introducing the concept of superefficiency. The latter is a period of the PWN evolution, happening within reverberation, where the luminosity in a given band exceeds the spin-down power at the time. Here, we explore a broad range of PWN models to study their reverberation and superefficiency phases in a systematic way. Armed with these models we consider two aspects: On the one hand, we analyze via Monte Carlo simulations how many Galactic PWNe are expected to be reverberating or in a superefficiency stage at any given time, providing the first such estimations. On the other hand, we focus on searching for observational signatures of such periods. We analyze archival observations and check for the existence of possible candidates for superefficient PWNe. We also provide predictions for the future evolution of the magnetar nebula J1834.9-0846 (which we consider to be starting its reverberation period) along the next 50 years. Using our simulations as input we study how sensitive current and future X-ray satellites (like eXTP or Athena) will be to observe such evolution, concluding that they will be able to track it in detail., Accepted for publication in MNRAS

Published
2019

44. Semantic Support for Scenarios to Improve Communication in Agribusiness

Author

Diego F. Torres, Leandro Antonelli, Jorge E. Hernández, and Mariángeles Hozikian

Subjects
Computer science, media_common.quotation_subject, Information sharing, 020207 software engineering, Context (language use), 02 engineering and technology, Data science, Domain (software engineering), Identification (information), 0202 electrical engineering, electronic engineering, information engineering, 020201 artificial intelligence & image processing, Quality (business), Software system, Dynamism, Set (psychology), media_common
Abstract

Organizations produce and exchange a huge amount of critical information, which main purpose is to obtain acceptable results. Hence, the trend is by considering integrated systems that can be easily adapted to several domains, especially when they need to exchange information. In this context, the agribusiness sector is a good example where massive data is generated, which implies the need for information sharing and collaboration, where the great challenged is support and understand the colliding context. However, every software system relies on its context, with its own rules, dynamism, and languages. Hence, it implies a significant effort to have a complete understanding of the composed domain. For this purpose, scenarios are well-known tools to describe dynamic domains and are commonly described under text-based context. When different stakeholders build Scenarios, it is essential to review them in order to unify their description. Thus, Scenarios under this unified perspective will better support the analysis and identification of relationship between two or more domains. This analysis is the key to design mechanisms to exchange information. Therefore, in the light of this, this paper proposes a semantic definition of Scenarios and a set of queries to identify issues in the Scenarios and improve their quality. In addition to this, a wiki platform to implement the semantic support and the queries is also provided.

Published
2019
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45. Prolonged sub-luminous state of the new transitional pulsar candidate CXOU J110926.4-650224

Author

Carlo Ferrigno, D. de Martino, Alida Odendaal, Alessandro Papitto, Thomas D. Russell, Francesco Coti Zelati, Sergio Campana, David A. H. Buckley, S. M. Mazzola, Mariusz Gromadzki, Jian Li, Diego F. Torres, Simone Migliari, Nanda Rea, Enrico Bozzo, High Energy Astrophys. & Astropart. Phys (API, FNWI), Coti Zelati F., Papitto A., De Martino D., Buckley D.A.H., Odendaal A., Li J., Russell T.D., Torres D.F., Mazzola S.M., Bozzo E., Gromadzki M., Campana S., Rea N., Ferrigno C., Migliari S., DEU, and ESP

Subjects
Photon, X-rays: Binarie, Astrophysics::High Energy Astrophysical Phenomena, Flux, FOS: Physical sciences, Astrophysics, Methods: Data analysi, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, Luminosity, Accretion, accretion disk, Settore FIS/05 - Astronomia E Astrofisica, Pulsar, Methods: Observational, 0103 physical sciences, Emission spectrum, 010303 astronomy & astrophysics, Astrophysics::Galaxy Astrophysics, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), 010308 nuclear & particles physics, Astronomy and Astrophysics, Stars: neutron, X-rays: Individuals: CXOU J110926.4-650224, Neutron star, 13. Climate action, Space and Planetary Science, Magnitude (astronomy), Astrophysics - High Energy Astrophysical Phenomena, Fermi Gamma-ray Space Telescope
Abstract

We report on a multi-wavelength study of the unclassified X-ray source CXOU J110926.4-650224 (J1109). We identified the optical counterpart as a blue star with a magnitude of $\sim$20.1 (3300-10500 $\require{mediawiki-texvc} \AA$). The optical emission was variable on timescales from hundreds to thousands of seconds. The spectrum showed prominent emission lines with variable profiles at different epochs. Simultaneous XMM-Newton and NuSTAR observations revealed a bimodal distribution of the X-ray count rates on timescales as short as tens of seconds, as well as sporadic flaring activity. The average broad-band (0.3-79 keV) spectrum was adequately described by an absorbed power law model with photon index of $\Gamma$=1.63$\pm$0.01 (at 1$\sigma$ c.l.), and the X-ray luminosity was (2.16$\pm$0.04)$\times$10$^{34}$ erg s$^{-1}$ for a distance of 4 kpc. Based on observations with different instruments, the X-ray luminosity has remained relatively steady over the past $\sim$15 years. J1109 is spatially associated with the gamma-ray source FL8Y J1109.8-6500, which was detected with Fermi at an average luminosity of (1.5$\pm$0.2)$\times$10$^{34}$ erg s$^{-1}$ (assuming the distance of J1109) over the 0.1-300 GeV energy band between 2008 and 2016. The source was undetected during ATCA radio observations that were simultaneous with NuSTAR, down to a 3$\sigma$ flux upper limit of 18 $\mu$Jy/beam (at 7.25 GHz). We show that the phenomenological properties of J1109 point to a binary transitional pulsar candidate currently in a sub-luminous accretion disk state, and that the upper limits derived for the radio emission are consistent with the expected radio luminosity for accreting neutron stars at similar X-ray luminosities., Comment: 21 pages, 15 figures, accepted for publication in A&A

Published
2019
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46. Monte Carlo studies for the optimisation of the Cherenkov Telescope Array layout

Author

Katsuaki Asano, Rodrigo Guedes Lang, M. Cieślar, Nicholas F. H Tothill, Gianpiero Tagliaferri, O. Le Blanc, M. Vazquez Acosta, Nicola Giglietto, S. Mangano, Julien Lefaucheur, Tatsuo Yoshida, D. de Martino, Martin Pohl, A. Shalchi, Y. Renier, B. Biasuzzi, T. B. Humensky, E. Fiandrini, Andreas Quirrenbach, Abelardo Moralejo, Carla Aramo, Vincenzo Rizi, J. Knapp, A. Pagliaro, Andrea Santangelo, Michael Punch, Andreas Specovius, A. M. Lopez, P. Peñil Del Campo, Henry Przybilski, J.-P. Lenain, Agnieszka Slowikowska, Satoshi Fukami, M. H. Grondin, S. Schlenstedt, Marek Nikolajuk, F. Schüssler, Maria Concetta Maccarone, Michael Zacharias, Francesco Giordano, T. Suomijärvi, Lorenzo Amati, J. Becker Tjus, Maxim V. Barkov, H. Prokoph, F.G. Saturni, R. J. White, Nu. Komin, María Isabel Bernardos, M. Orienti, Denis Bastieri, Justin Vandenbroucke, P. Vallania, Diego Falceta-Gonçalves, L. Tibaldo, A. Burtovoi, A. Viana, Takanori Yoshikoshi, Roberto Aloisio, Soebur Razzaque, M. Valentino, P. Da Vela, Pol Bordas, Francesco Longo, N. Otte, V. La Parola, E. O. Angüner, Marco Berton, Elina Lindfors, Salvo Scuderi, Hiroyasu Tajima, M. Prouza, E. Mach, P. Goldoni, C. Alispach, M. I. Martínez, Miroslav Pech, Kai Brügge, G. Vasileiadis, A. Nagai, A. Brill, Dusan Mandat, Geoff Romeo, M. Marculewicz, Cameron B Rulten, Fuyuki Tokanai, Luis Ángel Tejedor, Thomas Lohse, Anderson Caproni, Karol Seweryn, G. Bonnoli, D. Ninci, G. Pareschi, Stefan Kimeswenger, I. Sadeh, Łukasz Stawarz, M. Nöthe, Daniel Mazin, Ruben Alfaro, G. Busetto, Massimo Persic, A. Berti, G. Sironi, Pavel Horvath, Włodek Kluźniak, Pietro Bruno, Petr Travnicek, Daniel Kerszberg, M. Hayashida, Tomasz Szepieniec, A. Rugliancich, Marina Manganaro, Y. Ohtani, Samuel Timothy Spencer, L. Di Venere, S. Karkar, M. Füßling, E. de Oña Wilhelmi, Louis Antonelli, M. Lemoine-Goumard, Benjamin Koch, P.-O. Petrucci, M. de Naurois, Felix Werner, S. Sakurai, J. J. Rodríguez Vázquez, Petr Janecek, L. Dangeon, G. Fontaine, Alison Mitchell, Maria Magdalena González, Francesco Dazzi, Philip Kaaret, Reinaldo Santos-Lima, F. Di Pierro, Tomislav Terzić, Grzegorz Kowal, Stefan Wagner, R. A. Cameron, G. S. Varner, M. Roncadelli, Wystan Benbow, C. Bonavolontà, David Kieda, M. A. Leigui de Oliveira, Ullrich Schwanke, Y. Iwamura, K. Sedlaczek, R. C. Shellard, Q. Feng, David A. Williams, A. De Angelis, T. Nagayoshi, P. Sangiorgi, I. A. Minaya, Etienne Lyard, Juan Abel Barrio, B. De Lotto, S. Nozaki, J. Gironnet, L. Mohrmann, Oscar Blanch, Marcello Giroletti, Jean-Luc Meunier, Valentina Fioretti, S. Masuda, V. Vagelli, Rodolfo Canestrari, L. Freixas Coromina, M. Palatka, T. Di Girolamo, Vincenzo Testa, Tsuguya Naito, J. Becerra González, R. Alves Batista, Samo Stanič, S. D. Vergani, Lorenzo Bellizzi, Catherine Boisson, Olivier Hervet, P. Cumani, Konstancja Satalecka, Stefan Funk, Michele Doro, Pedro L. Luque-Escamilla, P. Romano, E. Fedorova, Carlo Vigorito, M. Zavrtanik, Markus Gaug, Stanislav Stefanik, R. J. García López, F. de Palma, V. Beshley, T.R.N. Ekoume, Enrico Congiu, Pierre Brun, Manuela Mallamaci, Barbara Balmaverde, L. Valore, Gino Tosti, Enrico Cascone, Marek Jamrozy, V. I. Zhdanov, Gavin Rowell, Elisabetta Bissaldi, M. Fiori, M. Capalbi, J. Bregeon, Dario Hrupec, F. Toussenel, R. Paoletti, Fulvio Gianotti, Ayan Acharyya, G. Spengler, P. Majumdar, A.A. Zdziarski, A. López-Oramas, M. Mariotti, Juri Poutanen, G. Ferrand, Paweł Świerk, M. Garczarczyk, S. Rainò, Tsunefumi Mizuno, Diego F. Torres, Ciro Bigongiari, Matteo Cerruti, M. Polo, Csaba Balázs, A. Dmytriiev, T. Gasparetto, D. Dorner, A. W. Chen, Elisa Prandini, Vitalii Sliusar, Helene Sol, Rodolfo Carosi, Jonathan Biteau, Vito Conforti, G. Rodriguez Fernandez, Shanta M. Zimmer, J. M. Paredes, S. Vercellone, Jonathan Granot, Alice Donini, Antonio Stamerra, Jaime Rosado, Michael G. Burton, Bohdan Hnatyk, F. D'Ammando, D. Nosek, M. Heller, Gagik Tovmassian, N. Produit, Petr Schovanek, German Martinez, G. Pühlhofer, S. Fegan, A. Kong, G. Morlino, G. Emery, H.-S. Zechlin, Tomasz Bulik, Antonino D'Ai, Riccardo Rando, Rocco Lico, K. Pfrang, D. Hadasch, R. López-Coto, A. Vollhardt, Pankaj Kushwaha, Petar Temnikov, Emmanuel Moulin, Luca Zampieri, Michiko Ohishi, C. Maggio, V. de Souza, Q. Piel, Marc Ribó, Werner Hofmann, A. Wierzcholska, Luisa Arrabito, Gianpaolo Vettolani, J. Pérez-Romero, Paramita Barai, Sylvain Chaty, N. Parmiggiani, V. Vassiliev, K. Nishijima, D. Cauz, S. Caroff, Giuseppe Leto, J.F. Glicenstein, Maria Ionica, Eva Sciacca, A. Bonardi, Juan Carlos Rodríguez-Ramírez, Marcos Santander, H. Siejkowski, Daniela Maria Ribeiro, Ralph Bird, S. Mićanović, D. Zavrtanik, Carole Mundell, Jan Ebr, Koji Noda, Elisa Bernardini, R. Gnatyk, Pierre Jean, M. Nievas Rosillo, M. López, Olga Sergijenko, R. Walter, Oleh Petruk, M. Del Santo, D. Elsasser, Jakub Juryšek, H. Martínez-Huerta, Andreas Zech, Jose J. Gonzalez, Akira Okumura, M. Iori, A. Ghalumyan, Jacco Vink, David Gascon, Jürgen Knödlseder, Daniel Nieto, R. A. Ong, Sabrina Casanova, B. Khélifi, S. Flis, G. Galanti, H. J. Voelk, Jim Hinton, M. Will, David H. Green, Giuseppe Malaguti, B. Rudak, A. Pe'Er, J. L. Dournaux, Andrea Bulgarelli, Frank M. Rieger, A. Djannati-Ataï, F. De Frondat, Lenka Tomankova, Moritz Hütten, Osvaldo Catalano, Hidetoshi Kubo, Tarek M. Hassan, Tomohiro Inada, Farinaldo S. Queiroz, J. Kushida, Daniel Morcuende, Jose Luis Contreras, F. Salesa Greus, Juan Cortina, Andreu Sanuy, S. Vorobiov, G. Maneva, B. Vallage, N. Maxted, N. Renault-Tinacci, P. Munar, M. Seglar-Arroyo, Fabrizio Tavecchio, Z. Ou, Anatolii Zenin, T. Tam, Miroslav Hrabovsky, G. Ambrosi, Giovanni Bonanno, R. Millul, Anastasia Maria Barbano, T. Grabarczyk, J. Zorn, D. Dominis Prester, R. D. Parsons, Luis H. S. Kadowaki, Elena Amato, M. Lallena Arquillo, I. Oya, Jacek Niemiec, Gianluca Giavitto, Marita Krause, Olaf Reimer, Josep Martí, M. Perri, Maria Chernyakova, Takeshi Nakamori, E. M. de Gouveia Dal Pino, Thomas Murach, P. Cristofari, C. Delgado, Fernando Catalani, G. La Rosa, J. Alfaro, Thomas Armstrong, J. Kocot, Léa Jouvin, Markus Böttcher, Rodrigo Nemmen, J. P. Amans, Utane Sawangwit, Y. Kobayashi, Hidetoshi Sano, D. Jankowsky, Heide Costantini, F. Arqueros, B. Bertucci, Sebastian Diebold, L. P. Taylor, Konstantinos N. Gourgouliatos, A. Fiasson, Miroslav Filipovic, R. Moderski, T. Stolarczyk, B. Patricelli, H. Ashkar, Alessandro Costa, Jonathan Blazek, C. Trichard, M. Vecchi, T. Greenshaw, A. Morselli, V. Vitale, A. M. Brown, S. M. Colak, Lili Yang, C. Díaz, J. Rico, P. Caraveo, S. Loporchio, Orel Gueta, Daniele Gaggero, V. De Caprio, R. Wischnewski, A. Sillanpää, C. J. Todero Peixoto, Takashi Saito, I. Agudo, Yasuo Fukui, Roberto Capuzzo-Dolcetta, F. Cassol, Manuel Meyer, Reiko Orito, G. Umana, M. V. Fonseca, U. Barres de Almeida, Saverio Lombardi, D. della Volpe, Giancarlo Cusumano, M. Ostrowski, T. Montaruli, L. Tosti, Garret Cotter, Konrad Bernlöhr, Reshmi Mukherjee, Fabio Iocco, M. Palatiello, Jonathan S. Lapington, U. Straumann, R. de Cássia dos Anjos, Matteo Balbo, Lab Saha, N. Hiroshima, G. Chiaro, D. Tonev, Ermanno Pietropaolo, Atreyee Sinha, Ministerio de Ciencia e Innovación (España), European Commission, Centre de Physique des Particules de Marseille (CPPM), Aix Marseille Université (AMU)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Galaxies, Etoiles, Physique, Instrumentation (GEPI), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Institut de Physique Nucléaire d'Orsay (IPNO), Université Paris-Sud - Paris 11 (UP11)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Théories (LUTH (UMR_8102)), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire de Physique Nucléaire et de Hautes Énergies (LPNHE (UMR_7585)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Leprince-Ringuet (LLR), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), AstroParticule et Cosmologie (APC (UMR_7164)), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Observatoire de Paris, Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Cité (UPCité), Laboratoire d'Annecy de Physique des Particules (LAPP), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS), Institut de Recherches sur les lois Fondamentales de l'Univers (IRFU), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris-Saclay, Centre d'Etudes Nucléaires de Bordeaux Gradignan (CENBG), Université Sciences et Technologies - Bordeaux 1 (UB)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire Midi-Pyrénées (OMP), Institut de Recherche pour le Développement (IRD)-Université Toulouse III - Paul Sabatier (UT3), Université de Toulouse (UT)-Université de Toulouse (UT)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Institut de Recherche pour le Développement (IRD)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Météo-France -Centre National de la Recherche Scientifique (CNRS), Institut de Planétologie et d'Astrophysique de Grenoble (IPAG), Institut national des sciences de l'Univers (INSU - CNRS)-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national des sciences de l'Univers (INSU - CNRS)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP )-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes [2016-2019] (UGA [2016-2019]), Research unit Astroparticle Physics, Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Aix Marseille Université (AMU), PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris Diderot - Paris 7 (UPD7)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS), Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Laboratoire d'Annecy de Physique des Particules (LAPP/Laboratoire d'Annecy-le-Vieux de Physique des Particules), Université Sciences et Technologies - Bordeaux 1-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Université Grenoble Alpes (UGA)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire des Sciences de l'Univers de Grenoble (OSUG), Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université Grenoble Alpes (UGA)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Institut polytechnique de Grenoble - Grenoble Institute of Technology (Grenoble INP)-Institut national de recherche en sciences et technologies pour l'environnement et l'agriculture (IRSTEA)-Université Joseph Fourier - Grenoble 1 (UJF)-Centre National de la Recherche Scientifique (CNRS), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université Paris Diderot - Paris 7 (UPD7), Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Centre National de la Recherche Scientifique (CNRS)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Paris-Sud - Paris 11 (UP11), Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Sorbonne Université (SU)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Université Paris sciences et lettres (PSL)-Université Paris sciences et lettres (PSL)-Centre National de la Recherche Scientifique (CNRS)-Université de Paris (UP), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS), Centre National d'Études Spatiales [Toulouse] (CNES)-Observatoire des Sciences de l'Univers de Grenoble (OSUG ), Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Savoie Mont Blanc (USMB [Université de Savoie] [Université de Chambéry])-Centre National de la Recherche Scientifique (CNRS)-Institut National de Recherche pour l’Agriculture, l’Alimentation et l’Environnement (INRAE)-Université Grenoble Alpes (UGA), Acharyya, A., Agudo, I., Anguner, E. O., Alfaro, R., Alfaro, J., Alispach, C., Aloisio, R., Alves Batista, R., Amans, J. -P., Amati, L., Amato, E., Ambrosi, G., Antonelli, L. A., Aramo, C., Armstrong, T., Arqueros, F., Arrabito, L., Asano, K., Ashkar, H., Balazs, C., Balbo, M., Balmaverde, B., Barai, P., Barbano, A., Barkov, M., Barres de Almeida, U., Barrio, J. A., Bastieri, D., Becerra Gonzalez, J., Becker Tjus, J., Bellizzi, L., Benbow, W., Bernardini, E., Bernardos, M. I., Bernlohr, K., Berti, A., Berton, M., Bertucci, B., Beshley, V., Biasuzzi, B., Bigongiari, C., Bird, R., Bissaldi, E., Biteau, J., Blanch, O., Blazek, J., Boisson, C., Bonanno, G., Bonardi, A., Bonavolonta, C., Bonnoli, G., Bordas, P., Bottcher, M., Bregeon, J., Brill, A., Brown, A. M., Brugge, K., Brun, P., Bruno, P., Bulgarelli, A., Bulik, T., Burton, M., Burtovoi, A., Busetto, G., Cameron, R., Canestrari, R., Capalbi, M., Caproni, A., Capuzzo-Dolcetta, R., Caraveo, P., Caroff, S., Carosi, R., Casanova, S., Cascone, E., Cassol, F., Catalani, F., Catalano, O., Cauz, D., Cerruti, M., Chaty, S., Chen, A., Chernyakova, M., Chiaro, G., Cieslar, M., Colak, S. M., Conforti, V., Congiu, E., Contreras, J. L., Cortina, J., Costa, A., Costantini, H., Cotter, G., Cristofari, P., Cumani, P., Cusumano, G., D'Ai, A., D'Ammando, F., Dangeon, L., Da Vela, P., Dazzi, F., De Angelis, A., De Caprio, V., de Cassia dos Anjos, R., De Frondat, F., de Gouveia Dal Pino, E. M., De Lotto, B., De Martino, D., de Naurois, M., de Ona Wilhelmi, E., de Palma, F., de Souza, V., Del Santo, M., Delgado, C., della Volpe, D., Di Girolamo, T., Di Pierro, F., Di Venere, L., Diaz, C., Diebold, S., Djannati-Atai, A., Dmytriiev, A., Dominis Prester, D., Donini, A., Dorner, D., Doro, M., Dournaux, J. -L., Ebr, J., Ekoume, T. R. N., Elsasser, D., Emery, G., Falceta-Goncalves, D., Fedorova, E., Fegan, S., Feng, Q., Ferrand, G., Fiandrini, E., Fiasson, A., Filipovic, M., Fioretti, V., Fiori, M., Flis, S., Fonseca, M. V., Fontaine, G., Freixas Coromina, L., Fukami, S., Fukui, Y., Funk, S., Fussling, M., Gaggero, D., Galanti, G., Garcia Lopez, R. J., Garczarczyk, M., Gascon, D., Gasparetto, T., Gaug, M., Ghalumyan, A., Gianotti, F., Giavitto, G., Giglietto, N., Giordano, F., Giroletti, M., Gironnet, J., Glicenstein, J. -F., Gnatyk, R., Goldoni, P., Gonzalez, J. M., Gonzalez, M. M., Gourgouliatos, K. N., Grabarczyk, T., Granot, J., Green, D., Greenshaw, T., Grondin, M. -H., Gueta, O., Hadasch, D., Hassan, T., Hayashida, M., Heller, M., Hervet, O., Hinton, J., Hiroshima, N., Hnatyk, B., Hofmann, W., Horvath, P., Hrabovsky, M., Hrupec, D., Humensky, T. B., Hutten, M., Inada, T., Iocco, F., Ionica, M., Iori, M., Iwamura, Y., Jamrozy, M., Janecek, P., Jankowsky, D., Jean, P., Jouvin, L., Jurysek, J., Kaaret, P., Kadowaki, L. H. S., Karkar, S., Kerszberg, D., Khelifi, B., Kieda, D., Kimeswenger, S., Kluzniak, W., Knapp, J., Knodlseder, J., Kobayashi, Y., Koch, B., Kocot, J., Komin, N., Kong, A., Kowal, G., Krause, M., Kubo, H., Kushida, J., Kushwaha, P., La Parola, V., La Rosa, G., Lallena Arquillo, M., Lang, R. G., Lapington, J., Le Blanc, O., Lefaucheur, J., Leigui de Oliveira, M. A., Lemoine-Goumard, M., Lenain, J. -P., Leto, G., Lico, R., Lindfors, E., Lohse, T., Lombardi, S., Longo, F., Lopez, A., Lopez, M., Lopez-Oramas, A., Lopez-Coto, R., Loporchio, S., Luque-Escamilla, P. L., Lyard, E., Maccarone, M. C., Mach, E., Maggio, C., Majumdar, P., Malaguti, G., Mallamaci, M., Mandat, D., Maneva, G., Manganaro, M., Mangano, S., Marculewicz, M., Mariotti, M., Marti, J., Martinez, M., Martinez, G., Martinez-Huerta, H., Masuda, S., Maxted, N., Mazin, D., Meunier, J. -L., Meyer, M., Micanovic, S., Millul, R., Minaya, I. A., Mitchell, A., Mizuno, T., Moderski, R., Mohrmann, L., Montaruli, T., Moralejo, A., Morcuende, D., Morlino, G., Morselli, A., Moulin, E., Mukherjee, R., Munar, P., Mundell, C., Murach, T., Nagai, A., Nagayoshi, T., Naito, T., Nakamori, T., Nemmen, R., Niemiec, J., Nieto, D., Nievas Rosillo, M., Nikolajuk, M., Ninci, D., Nishijima, K., Noda, K., Nosek, D., Nothe, M., Nozaki, S., Ohishi, M., Ohtani, Y., Okumura, A., Ong, R. A., Orienti, M., Orito, R., Ostrowski, M., Otte, N., Ou, Z., Oya, I., Pagliaro, A., Palatiello, M., Palatka, M., Paoletti, R., Paredes, J. M., Pareschi, G., Parmiggiani, N., Parsons, R. D., Patricelli, B., Pe'Er, A., Pech, M., Penil Del Campo, P., Perez-Romero, J., Perri, M., Persic, M., Petrucci, P. -O., Petruk, O., Pfrang, K., Piel, Q., Pietropaolo, E., Pohl, M., Polo, M., Poutanen, J., Prandini, E., Produit, N., Prokoph, H., Prouza, M., Przybilski, H., Puhlhofer, G., Punch, M., Queiroz, F., Quirrenbach, A., Raino, S., Rando, R., Razzaque, S., Reimer, O., Renault-Tinacci, N., Renier, Y., Ribeiro, D., Ribo, M., Rico, J., Rieger, F., Rizi, V., Rodriguez Fernandez, G., Rodriguez-Ramirez, J. C., Rodri-guez Vazquez, J. J., Romano, P., Romeo, G., Roncadelli, M., Rosado, J., Rowell, G., Rudak, B., Rugliancich, A., Rulten, C., Sadeh, I., Saha, L., Saito, T., Sakurai, S., Salesa Greus, F., Sangiorgi, P., Sano, H., Santander, M., Santangelo, A., Santos-Lima, R., Sanuy, A., Satalecka, K., Saturni, F. G., Sawangwit, U., Schlenstedt, S., Schovanek, P., Schussler, F., Schwanke, U., Sciacca, E., Scuderi, S., Sedlaczek, K., Seglar-Arroyo, M., Sergijenko, O., Seweryn, K., Shalchi, A., Shellard, R. C., Siejkowski, H., Sillanpaa, A., Sinha, A., Sironi, G., Sliusar, V., Slowikowska, A., Sol, H., Specovius, A., Spencer, S., Spengler, G., Stamerra, A., Stanic, S., Stawarz, L., Stefanik, S., Stolarczyk, T., Straumann, U., Suomijarvi, T., Swierk, P., Szepieniec, T., Tagliaferri, G., Tajima, H., Tam, T., Tavecchio, F., Taylor, L., Tejedor, L. A., Temnikov, P., Terzic, T., Testa, V., Tibaldo, L., Todero Peixoto, C. J., Tokanai, F., Tomankova, L., Tonev, D., Torres, D. F., Tosti, G., Tosti, L., Tothill, N., Toussenel, F., Tovmassian, G., Travnicek, P., Trichard, C., Umana, G., Vagelli, V., Valentino, M., Vallage, B., Vallania, P., Valore, L., Vandenbroucke, J., Varner, G. S., Vasileiadis, G., Vassiliev, V., Vazquez Acosta, M., Vecchi, M., Vercellone, S., Vergani, S., Vettolani, G. P., Viana, A., Vigorito, C. F., Vink, J., Vitale, V., Voelk, H., Vollhardt, A., Vorobiov, S., Wagner, S. J., Walter, R., Werner, F., White, R., Wierzcholska, A., Will, M., Williams, D. A., Wischnewski, R., Yang, L., Yoshida, T., Yoshikoshi, T., Zacharias, M., Zampieri, L., Zavrtanik, M., Zavrtanik, D., Zdziarski, A. A., Zech, A., Zechlin, H., Zenin, A., Zhdanov, V. I., Zimmer, S., Zorn, J., Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Durham University, Glorieta de la Astronomía s/n, Delegación Coyoacán, Pontificia Universidad Católica de Chile, Département de physique nucléaire et corpusculaire, Università degli Studi dell'Aquila and Gran Sasso Science Institute, Universidade de São Paulo (USP), PSL Research University, INAF - Osservatorio di astrofisica e scienza dello spazio di Bologna, INAF - Osservatorio Astrofisico di Arcetri, INFN Sezione di Perugia, Universitá degli Studi di Perugia, INAF - Osservatorio Astronomico di Roma, INFN Sezione di Napoli, University of Oxford, Universidad Complutense de Madrid, CNRS/IN2P3, University of Tokyo, Monash University, University of Geneva, INAF - Osservatorio Astronomico di Brera, Institute of Physical and Chemical Research, Centro Brasileiro de Pesquisas Físicas, INFN Sezione di Padova and Universitá degli Studi di Padova, Universidad de La Laguna, Ruhr-Universität Bochum, Harvard-Smithsonian Center for Astrophysics, Max-Planck-Institut für Kernphysik, INFN Sezione di Torino, Pidstryhach Institute for Applied Problems in Mechanics and Mathematics NASU, Université Paris-Saclay, University of California, INFN Sezione di Bari and Politecnico di Bari, The Barcelona Institute of Science and Technology, Institute of Physics of the Czech Academy of Sciences, INAF - Osservatorio Astrofisico di Catania, Radboud University Nijmegen, Dipartimento di Scienze Fisiche, IEEC-UB, North-West University, Columbia University, TU Dortmund University, University of Warsaw, Armagh Observatory and Planetarium, Stanford University, INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo, Núcleo de Astrofísica Teórica (NAT/UCS), INAF - Istituto di Astrofisica Spaziale e Fisica Cosmica di Milano, INFN Sezione di Pisa, Polish Academy of Sciences, INAF - Osservatorio Astronomico di Capodimonte, INFN Sezione di Trieste and Università degli Studi di Udine, University of the Witwatersrand, Dublin City University, CIEMAT, CPPM, INAF - Istituto di Radioastronomia, Cherenkov Telescope Array Observatory, Universidade Federal do Paraná (UFPR), Université Paris-Saclay), CSIC), Institut d'Estudis Espacials de Catalunya (IEEC), Institució Catalana de Recerca i Estudis Avançats (ICREA) Barcelona, INFN Sezione di Bari and Università degli Studi di Bari, Universität Tübingen, Obs de Paris, University of Rijeka, Universität Würzburg, LPNHE, Astronomical Observatory of Taras Shevchenko National University of Kyiv, Western Sydney University, INAF - Osservatorio Astronomico di Padova, Deutsches Elektronen-Synchrotron, Nagoya University, University of Amsterdam, Universidad Autónoma de Madrid, INFN Sezione di Trieste and Università degli Studi di Trieste, Universitat Autónoma de Barcelona, Yerevan Physics Institute, Universidad Andrés Bello UNAB, Academic Computer Centre CYFRONET AGH, The Open University of Israel, Max-Planck-Institut für Physik, Oliver Lodge Laboratory, UMR 5797, Konan University, KEK (High Energy Accelerator Research Organization), RCPTM, Josip Juraj Strossmayer University of Osijek, Universidade Estadual Paulista (Unesp), INFN Sezione di Roma, Jagiellonian University, Physikalisches Institut, Université Paul Sabatier, University of Iowa, Leopold-Franzens-Universität, Kyoto University, Tokai University, University of Leicester, Universidade Federal do ABC (UFABC), University of Turku, Humboldt University Berlin, Universidad de Jaén, Saha Institute of Nuclear Physics, Bulgarian Academy of Sciences, Faculty of Physics, University of New South Wales, Universität Zürich, Hiroshima University, INFN Sezione di Roma Tor Vergata, INAF - Istituto di Astrofisica e Planetologia Spaziali (IAPS), University of Bath, Saitama University, Yamanashi-Gakuin University, Yamagata University, Institute of Particle & Nuclear Physics, Tokushima University, Georgia Institute of Technology, Institut de Planétologie et d'Astrophysique de Grenoble, Univ. Savoie Mont Blanc, Universität Potsdam, Linnaeus University, Universität Heidelberg, University of Johannesburg, University of Adelaide, Tuscaloosa, National Astronomical Research Institute of Thailand, Dept of Physics and Astronomy, Nicolaus Copernicus University, University of Nova Gorica, University of Wisconsin, INAF - Osservatorio Astrofisico di Torino, University of Hawai'i at Manoa, Ibaraki University, KVI - Center for Advanced Radiation Technology, University of Utah, USA, GBR, FRA, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7), Angüner, E. O., Becerra González, J., Bernlöhr, K., Bonavolontá, C., Böttcher, M., Brügge, K., Cieślar, M., D’Aí, A., D’Ammando, F., de Cássia dos Anjos, R., de Oña Wilhelmi, E., Díaz, C., Djannati-Ataï, A., Elsässer, D., Füßling, M., Garcia López, R. J., González, J. M., González, M. M., Hütten, M., Khélifi, B., Kluźniak, W., Knödlseder, J., López, M., López-Coto, R., Martí, J., Martínez, M., Martínez, G., Martínez-Huerta, H., Nikołajuk, M., Nöthe, M., Pe’Er, A., Peñil Del Campo, P., Pérez-Romero, J., Pühlhofer, G., Rainò, S., Ribó, M., Rodrí-guez Vázquez, J. J., Sillanpää, A., Stanič, S., Stawarz, Ł., Świerk, P., Vázquez Acosta, M., GRAPPA (ITFA, IoP, FNWI), and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Cherenkov Telescope Array, Astronomy, Monte Carlo method, energy resolution, Monte Carlo simulations, Cherenkov telescopes, IACT technique, gamma rays, cosmic rays, 01 natural sciences, 7. Clean energy, law.invention, Observatory, law, site, Monte Carlo, 010303 astronomy & astrophysics, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, observatory, Cosmic rays, Gamma rays, Astronomy and Astrophysics, ddc:540, Física nuclear, Monte carlo studies, Astrophysics::Earth and Planetary Astrophysics, Astrophysics - Instrumentation and Methods for Astrophysics, performance, FÍSICA DE ALTA ENERGIA, Astrophysics::High Energy Astrophysical Phenomena, Gamma ray, FOS: Physical sciences, energy dependence, Telescope, Optics, CTA - Abteilung Hofmann, 0103 physical sciences, Cherenkov counter: imaging, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Instrumentation and Methods for Astrophysics (astro-ph.IM), Monte Carlo simulation, Cherenkov radiation, CTA, 010308 nuclear & particles physics, business.industry, sensitivity, Cosmic ray, Cherenkov telescope, gamma ray: VHE, business, Energy (signal processing), astro-ph.IM
Abstract

The Cherenkov Telescope Array (CTA) is the major next-generation observatory for ground-based very-high-energy gamma-ray astronomy. It will improve the sensitivity of current ground-based instruments by a factor of five to twenty, depending on the energy, greatly improving both their angular and energy resolutions over four decades in energy (from 20 GeV to 300 TeV). This achievement will be possible by using tens of imaging Cherenkov telescopes of three successive sizes. They will be arranged into two arrays, one per hemisphere, located on the La Palma island (Spain) and in Paranal (Chile). We present here the optimised and final telescope arrays for both CTA sites, as well as their foreseen performance, resulting from the analysis of three different large-scale Monte Carlo productions.© 2019, We gratefully acknowledge financial support from the following agencies and organizations: State Committee of Science of Armenia, Armenia; The Australian Research Council, Astronomy Australia Ltd, The University of Adelaide, Australian National University, Monash University, The University of New South Wales, The University of Sydney, Western Sydney University, Australia; Federal Ministry of Science, Research and Economy, and Innsbruck University, Austria; Conselho Nacional de Desenvolvimento Cientifico e Tecnologico (CNPq), Fundacao de Amparo a Pesquisa do Estado do Rio de Janeiro (FAPERJ), Fundacao de Amparo a Pesquisa do Estado de Sao Paulo (FAPESP), Ministry of Science, Technology, Innovations and Communications (MCTIC), Brasil; Ministry of Education and Science, National RI Roadmap Project D01-153/28.08.2018, Bulgaria; The Natural Sciences and Engineering Research Council of Canada and the Canadian Space Agency, Canada; CONICYT-Chile grants PFB-06, FB0821, ACT 1406, FONDECYT-Chile grants 3160153, 3150314, 1150411, 1161463, 1170171, Pontificia Universidad Catolica de Chile Vice-Rectory of Research internationalization grant under MINEDUC agreement PUC1566, Chile, Croatian Science Foundation, Rudjer Boskovic Institute, University of Osijek, University of Rijeka, University of Split, Faculty of Electrical Engineering, Mechanical Engineering and Naval Architecture, University of Zagreb, Faculty of Electrical Engineering and Computing, Croatia; Ministry of Education, Youth and Sports, MEYS LM2015046, LTT17006 and EU/MEYS CZ.02.1.01/0.0/0.0/16_013/0001403, CZ.02.1.01/0.0/0.0/17_049/0008422, Czech Republic; Ministry of Higher Education and Research, CNRS-INSU and CNRS-IN2P3, CEA-Irfu, ANR, Regional Council Ile-de France, Labex ENIGMASS, OSUG2020, P210 and OCEVU, France; Max Planck Society, BMBF, DESY, Helmholtz Association, Germany; Department of Atomic Energy, Department of Science and Technology, India; Istituto Nazionale di Astrofisica (INAF), Istituto Nazionale di Fisica Nucleare (INFN), MIUR, Istituto Nazionale di Astrofisica (INAF-OABRERA) Grant Fondazione Cariplo/Regione Lombardia ID 2014-1980/RST_ERC, Italy; ICRR, University of Tokyo, JSPS, MEXT, Japan; Netherlands Research School for Astronomy (NOVA), Netherlands Organization for Scientific Research (NWO), Netherlands; University of Oslo, Norway; Ministry of Science and Higher Education, DIR/WK/2017/12, the National Centre for Research and Development and the National Science Centre, UMO-2016/22/M/ST9/00583, Poland; Slovenian Research Agency, Slovenia, grants P1-0031, P1-0385, 10-0033, J1-9146; South African Department of Science and Technology and National Research Foundation through the South African Gamma-Ray Astronomy Programme, South Africa; MINECO National R+D+I, Severo Ochoa, Maria de Maeztu, CDTI, PAIDI, UJA, FPA2017-90566-REDC, Spain; Swedish Research Council, Royal Physiographic Society of Lund, Royal Swedish Academy of Sciences, The Swedish National Infrastructure for Computing (SNIC) at Lunarc (Lund), Sweden; Swiss National Science Foundation (SNSF), Ernest Boninchi Foundation, Switzerland; Durham University, Leverhulme Trust, Liverpool University, University of Leicester, University of Oxford, Royal Society, Science and Technology Facilities Council, UK; U.S. National Science Foundation, U.S.Department of Energy, Argonne National Laboratory, Barnard College, University of California, University of Chicago, Columbia University, Georgia Institute of Technology, Institute for Nuclear and Particle Astrophysics (INPAC-MRPI program), Iowa State University, the Smithsonian Institution, Washington University McDonnell Center for the Space Sciences, The University of Wisconsin and the Wisconsin Alumni Research Foundation, USA. The research leading to these results has received funding from the European Union's Seventh Framework Programme (FP7/2007-2013) under grant agreements no 262053 and no 317446. This project is receiving funding from the European Union's Horizon 2020 research and innovation programs under agreement no 676134.

Published
2019
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47. A Search for Cosmic-ray Proton Anisotropy with the Fermi Large Area Telescope

Author

Eleonora Troja, Soebur Razzaque, Ronaldo Bellazzini, Giacomo Principe, F. Piron, G. Chiaro, M. Kuss, Abhishek Desai, Kazuhiko Hayashi, Regina Caputo, T. A. Porter, E. Orlando, Dario Gasparrini, Hiroyasu Tajima, Keith Bechtol, S. Maldera, Stefano Ciprini, Ioannis Liodakis, E. J. Siskind, Francesco Longo, G. Martí-Devesa, Marco Ajello, J. B. Thayer, S. Rainò, Tsunefumi Mizuno, Matthew Meehan, Olaf Reimer, D. Horan, V. S. Paliya, D. Serini, Diego F. Torres, M. Razzano, Yasushi Fukazawa, Filippo D'Ammando, A. Reimer, Justin Vandenbroucke, G. Jóhannesson, F. de Palma, Manuel Meyer, Alessandro Cuoco, Guido Barbiellini, P. Fusco, I. Mereu, T. J. Brandt, Melissa Pesce-Rollins, Seth Digel, David A. Green, S. J. Fegan, Elizabeth Hays, Peter F. Michelson, Marcello Giroletti, D. J. Suson, S. Cutini, J. W. Hewitt, Eric Nuss, Sina Chen, Massimo Persic, Carmelo Sgrò, Riccardo Rando, G. Spandre, N. Di Lalla, Luca Baldini, Sylvain Guiriec, Mn Mazziotta, D. Costantin, Stephan Zimmer, David Paneque, Luca Latronico, P. de la Torre Luque, Elisabetta Bissaldi, Stefan Funk, Denis Bastieri, Eugenio Bottacini, Alberto Manfreda, Roger Blandford, Nicola Omodei, Johann Cohen-Tanugi, M. Orienti, L. Di Venere, F. Loparco, Nicola Giglietto, Aaron Dominguez, I. A. Grenier, E. Cavazzuti, M. Yassine, R. Bonino, Nestor Mirabal, P. Lubrano, S. Buson, J. Li, Matteo Negro, A. Morselli, R. A. Cameron, P. Bruel, Warit Mitthumsiri, P. Spinelli, Francesco Giordano, F. Gargano, Laboratoire Leprince-Ringuet (LLR), Centre National de la Recherche Scientifique (CNRS)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), Laboratoire Univers et Particules de Montpellier (LUPM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université Montpellier 2 - Sciences et Techniques (UM2), Astrophysique Interprétation Modélisation (AIM (UMR_7158 / UMR_E_9005 / UM_112)), Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Université Paris Diderot - Paris 7 (UPD7), Fermi-LAT, Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-École polytechnique (X)-Centre National de la Recherche Scientifique (CNRS), Université de Montpellier (UM)-Université Montpellier 2 - Sciences et Techniques (UM2)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Centre National de la Recherche Scientifique (CNRS), Commissariat à l'énergie atomique et aux énergies alternatives (CEA)-Institut national des sciences de l'Univers (INSU - CNRS)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Ajello, M., Baldini, L., Barbiellini, G., Bastieri, D., Bechtol, K., Bellazzini, R., Bissaldi, E., Blandford, R. D., Bonino, R., Bottacini, E., Brandt, T. J., Bruel, P., Buson, S., Cameron, R. A., Caputo, R., Cavazzuti, E., Chen, S., Chiaro, G., Ciprini, S., Cohen-Tanugi, J., Costantin, D., Cuoco, A., Cutini, S., D’Ammando, F., de la Torre Luque, P., de Palma, F., Desai, A., Digel, S. W., Di Lalla, N., Di Venere, L., Domínguez, A., Fegan, S. J., Fukazawa, Y., Funk, S., Fusco, P., Gargano, F., Gasparrini, D., Giglietto, N., Giordano, F., Giroletti, M., Green, D., Grenier, I. A., Guiriec, S., Hayashi, K., Hays, E., Hewitt, J. W., Horan, D., Jóhannesson, G., Kuss, M., Latronico, L., Li, J., Liodakis, I., Longo, F., Loparco, F., Lubrano, P., Maldera, S., Manfreda, A., Martí-Devesa, G., Mazziotta, M. N., Meehan, M., Mereu, I., Meyer, M., Michelson, P. F., Mirabal, N., Mitthumsiri, W., Mizuno, T., Morselli, A., Negro, M., Nuss, E., Omodei, N., Orienti, M., Orlando, E., Paliya, V. S., Paneque, D., Persic, M., Pesce-Rollins, M., Piron, F., Porter, T. A., Principe, G., Rainò, S., Rando, R., Razzano, M., Razzaque, S., Reimer, A., Reimer, O., Serini, D., Sgrò, C., Siskind, E. J., Spandre, G., Spinelli, P., Suson, D. J., Tajima, H., Thayer, J. B., Torres, D. F., Troja, E., Vandenbroucke, J., Yassine, M., Zimmer, S., Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), Fermi-Lat Collaboration, T., D'Ammando, F., De La Torre Luque, P., De Palma, F., Dominguez, A., Johannesson, G., Marti-Devesa, G., Raino, S., Sgro, C., ITA, and USA

Subjects
010504 meteorology & atmospheric sciences, Proton, High-energy astronomy, Astrophysics::High Energy Astrophysical Phenomena, Galactic cosmic rays, High-energy astrophysics, Cosmic ray, Astrophysics::Cosmology and Extragalactic Astrophysics, 7. Clean energy, 01 natural sciences, cosmic radiation: anisotropy, GLAST, Galactic cosmic ray, law.invention, Telescope, Primary (astronomy), law, 0103 physical sciences, Nuclear Experiment, Anisotropy, 010303 astronomy & astrophysics, 0105 earth and related environmental sciences, Physics, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy, Astronomy and Astrophysics, cosmic radiation: primary, p: energy, 13. Climate action, Space and Planetary Science, p: cosmic radiation, anisotropy: dipole, ddc:520, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope
Abstract

The Fermi Large Area Telescope (LAT) has amassed a large data set of primary cosmic-ray protons throughout its mission. The LAT's wide field of view and full-sky survey capabilities make it an excellent instrument for studying cosmic-ray anisotropy. As a space-based survey instrument, the LAT is sensitive to anisotropy in both right ascension and declination, while ground-based observations only measure the anisotropy in right ascension. We present the results of the first ever proton anisotropy search using Fermi LAT. The data set uses eight years of data and consists of approximately 179 million protons above 78 GeV, enabling it to probe dipole anisotropy below an amplitude of $10^{-3}$, resulting in the most stringent limits on the declination dependence of the dipole to date. We measure a dipole amplitude $\delta = 3.9\pm1.5 \times 10^{-4}$ with a p-value of 0.01 (pre-trials) for protons with a minimum energy of 78 GeV. We discuss various systematic effects that could give rise to a dipole excess and calculate upper limits on the dipole amplitude as a function of minimum energy. The 95% CL upper limit on the dipole amplitude is $\delta_{UL}=1.3\times 10^{-3}$ for protons with a minimum energy of 78 GeV and $\delta_{UL}=1.2 \times 10^{-3}$ for protons with a minimum energy of 251 GeV., Comment: 15 pages, 11 figures, Contact authors: Matthew Meehan (mrmeehan@wisc.edu) and Justin Vandenbroucke (justin.vandenbroucke@wisc.edu)

Published
2019
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48. Prospects for the characterization of the VHE emission from the Crab nebula and pulsar with the Cherenkov Telescope Array

Author

Enrique Mestre, L Tibaldo, E. de Oña Wilhelmi, Roberta Zanin, Diego F. Torres, Alexander von Humboldt Foundation, Ministerio de Ciencia, Innovación y Universidades (España), Institut de recherche en astrophysique et planétologie (IRAP), Université Toulouse III - Paul Sabatier (UT3), Université Fédérale Toulouse Midi-Pyrénées-Université Fédérale Toulouse Midi-Pyrénées-Observatoire Midi-Pyrénées (OMP), Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS), Institut national des sciences de l'Univers (INSU - CNRS)-Université Toulouse III - Paul Sabatier (UT3), and Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Université Fédérale Toulouse Midi-Pyrénées-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Météo France-Centre National d'Études Spatiales [Toulouse] (CNES)-Centre National de la Recherche Scientifique (CNRS)-Institut de Recherche pour le Développement (IRD)-Centre National de la Recherche Scientifique (CNRS)

Subjects
propagation [particle], Cherenkov Telescope Array, Astrophysics::High Energy Astrophysical Phenomena, Population, VHE [gamma ray], FOS: Physical sciences, Astrophysics, 01 natural sciences, Pulsar wind nebula, rotation, individual: Crab nebula [Supernovae], particle: propagation, Pulsar, 0103 physical sciences, conservation law, structure, education, 010303 astronomy & astrophysics, detectors [Instrumentation], pulsar, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Nebula, 010308 nuclear & particles physics, Crab Pulsar, instrumentation: detectors, pulsars: individual: Crab, Astrophysics::Instrumentation and Methods for Astrophysics, Astronomy and Astrophysics, Light curve, sensitivity, supernovae: individual: Crab nebula, Automatic Keywords, Crab Nebula, gamma ray: VHE, Space and Planetary Science, hydrodynamics, ddc:520, spectral, individual: Crab [Pulsars], Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], asymmetry
Abstract

The Cherenkov Telescope Array (CTA) will be the next generation instrument for the very high energy gamma-ray astrophysics domain. With its enhanced sensitivity in comparison with the current facilities, CTA is expected to shed light on a varied population of sources. In particular, we will achieve a deeper knowledge of the Crab nebula and pulsar, which are the best characterized pulsar wind nebula and rotation powered pulsar, respectively. We aim at studying the capabilities of CTA regarding these objects through simulations, using the main tools currently in development for the CTA future data analysis: Gammapy and ctools. We conclude that, even using conservative Instrument Response Functions, CTA will be able to resolve many uncertainties regarding the spectrum and morphology of the pulsar and its nebula. The large energy range covered by CTA will allow us to disentangle the nebula spectral shape among different hypotheses, corresponding to different underlying emitting mechanisms. In addition, resolving internal structures (smaller than ~ 0.02 degrees in size) in the nebula and unveiling their location, would provide crucial information about the propagation of particles in the magnetized medium. We used a theoretical asymmetric model to characterise the morphology of the nebula and we showed that if predictions of such morphology exist, for instance as a result of hydrodynamical or magneto-hydrodynamical simulations, it can be directly compared with CTA results. We also tested the capability of CTA to detect periodic radiation from the Crab pulsar obtaining a precise measurement of different light curves shapes., Comment: in press in MNRAS

Published
2019
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49. Impacto del COVID-19 en docentes universitarios argentinos: cambio de prácticas, dificultades y aumento del estrés

Author

Ana Casali and Diego F. Torres

Subjects
lcsh:LC8-6691, History, Aprendizaje virtual, lcsh:Special aspects of education, Estres, Educación Superior, COVID-19, Stress, Computer Science Applications, Education, Virtual learning, Ciencias de la Computación e Información, Educación superior, Higher education, lcsh:L, lcsh:Education
Abstract

La pandemia COVID-19 ha provocado cambios profundos en toda la sociedad. A partir de las medidas de aislamiento adoptadas, todo el sistema educativo basado fundamentalmente en la modalidad presencial, se ha visto obligado a sostener el proceso de enseñanza y aprendizaje de forma virtual. Sin embargo, la mayoría de los profesores no estaban preparados para este cambio tan brusco. Muchos tuvieron que adquirir conocimientos sobre el uso de tecnologías y enfoques pedagógicos para llevar adelante sus actividades, aumentando aún más su carga laboral. En este contexto, se han sumado además, otras tareas vinculadas a la atención del hogar y al cuidado de familiares a cargo.. En este contexto, este artículo muestra los resultados de una investigación realizada con profesores universitarios argentinos, cuyo objetivo fue comprender los factores de estrés relacionados con los cambios abruptos llevados a cabo en sus prácticas docentes como resultado de la pandemia. Los resultados obtenidos muestran un aumento significativo en la percepción de estrés en pandemia, una alta tasa de dificultades en el uso de herramientas tecnológicas para pasar de clases presenciales a virtuales, a pesar que la mayoría de las personas encuestadas poseen conocimientos informáticos. The COVID-19 pandemic has caused profound changes throughout society. Because of the isolation measures adopted, the entire educational system based mainly on the face-to-face modality, has been forced to continue the teaching and learning process virtually. However, most of the teachers were not prepared for this abrupt change. Many had to acquire knowledge about the use of technologies and pedagogical approaches to carry out their activities, with a further increase of their workload. In this pandemic situation, other tasks related to home care and care of dependents have also been added. In this context, this article shows the results of an investigation carried out with Argentine university professors, whose objective was to understand the stress factors related to the abrupt changes in their teaching practices as a result of the pandemic's conditions. The results we obtained show a significant increase in the perception of stress in the work conditions under pandemic and a high rate of difficulties in the use of technological tools and methodologies, to go from face-to-face to virtual classes, despite the fact that most of the people surveyed have computer skills.

Published
2021
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50. Observations of three young γ-ray pulsars with the Gran Telescopio Canarias

Author

M. Pierbattista, Diego F. Torres, A. De Luca, Andrew Shearer, E. de Oña Wilhelmi, Vincenzo Testa, Nanda Rea, Roberto Mignani, M. Marelli, and High Energy Astrophys. & Astropart. Phys (API, FNWI)

Subjects
Gran Telescopio Canarias, Astrophysics::High Energy Astrophysical Phenomena, FOS: Physical sciences, Astrophysics, 01 natural sciences, Spectral line, Luminosity, stars: neutron, wind nebula, Pulsar, Spitzer Space Telescope, large-magellanic-cloud, emission, 0103 physical sciences, 010306 general physics, Large Magellanic Cloud, Supernova remnant, 010303 astronomy & astrophysics, optical observations, High Energy Astrophysical Phenomena (astro-ph.HE), Physics, Astronomy, Astronomy and Astrophysics, psr j2021+3651, cta 1, large-area telescope, supernova remnant, Space and Planetary Science, radio-quiet, Astrophysics - High Energy Astrophysical Phenomena, discovery, Fermi Gamma-ray Space Telescope
Abstract

We report the analysis of the first deep optical observations of three isolated $\gamma$-ray pulsars detected by the {\em Fermi Gamma-ray Space Telescope}: the radio-loud PSR\, J0248+6021 and PSR\, J0631+1036, and the radio-quiet PSR\, J0633+0632. The latter has also been detected in the X rays. The pulsars are very similar in their spin-down age ($\tau \sim$40--60 kyrs), spin-down energy ($\dot{E} \sim10^{35}$ erg s$^{-1}$), and dipolar surface magnetic field ($B \sim 3$--$5\times10^{12}$ G). These pulsars are promising targets for multi-wavelength observations, since they have been already detected in $\gamma$ rays and in radio or X-rays. None of them has been detected yet in the optical band. We observed the three pulsar fields in 2014 with the Spanish 10.4m Gran Telescopio Canarias (GTC). We could not find any candidate optical counterpart to the three pulsars close to their most recent radio or {\em Chandra} positions down to $3 \sigma$ limits of $g'\sim27.3$, $g'\sim27$, $g'\sim27.3$ for PSR\, J0248+6021, J0631+1036, and J0633+0632, respectively. From the inferred optical upper limits and estimated distance and interstellar extinction, we derived limits on the pulsar optical luminosity. We also searched for the X-ray counterpart to PSR\, J0248+6021 with \chan\ but we did not detect the pulsar down to a 3$\sigma$ flux limit of $5 \times 10^{-14}$ erg cm$^{-2}$ s$^{-1}$ (0.3--10 keV). For all these pulsars, we compared the optical flux upper limits with the extrapolations in the optical domain of the $\gamma$-ray spectra and compared their multi-wavelength properties with those of other $\gamma$-ray pulsars of comparable age., Comment: 12 pages, 5 figures, accepted for publication in MNRAS

Published
2016

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