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1. GPU accelerated optical light propagation in CORSIKA 8

Author

Baack, Dominik, Reininghaus, Maximilian, Alameddine, Jean-Marco, Albrecht, Johannes, Alvarez-Muniz, Jaime, Jr., Antonio Augusto Alves, Arrabito, Luisa, Bernlöhr, Konrad, Bleicher, Marcus, BREGEON, Johan, Carrere, Matthieu, Dembinski, Hans, Elfner, Hannah, Elsässer, Dominik, Engel, Ralph, Hu, Fan, Fedynitch, Anatoli, Heck, Dieter, Huege, Tim, Kampert, Karl-Heinz, Karastathis, Nikolaos, Nellen, Lukas, Nöthe, Maximilian, Parello, David, Pierog, Tanguy, Pokrandt, Maria, Poctarev, Anton, Prechelt, Remy, Rhode, Wolfgang, Riehn, Felix, Sackel, Maximilian, Sandrock, Alexander, Sampathkumar, Pranav, Schmelling, Michael, Schmidt, André, Sigl, Günter, Soedingrekso, Jan, Spaan, Bernhard, Xu, Donglian, Ammerman-Yebra, Juan, Zas, Enrique, and CORSIKA 8 Collaboration

Subjects
Physics, ddc:530
Abstract

Optical photons, created from fluorescence or Cherenkov emission in atmospheric cascades induced through high energetic cosmic rays are of major interest for several experiments. Experiments like CTA require a significant amount of computing time and funds for the simulation with CORSIKA 7. Since individual photons don’t interact they can be simulated without any order. The traditional sequential approach is simple but leads to reduced utilization of modern hardware infrastructure. The calculations done on each photon have low complexity, compared to the other aspects of the simulation. This, as well as the fact that, besides information about the photon itself, nearly no additional data is needed, favors a data-parallel approach in which several photons are propagated concurrently. The new CORSIKA 8 framework enables the implementation and verification of these methods. With the use of dedicated high parallel acceleration hardware like GPUs the possible benefits with this data-parallel approach are even higher.

Published
2022
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2. CORSIKA 8 -- Contributions to the 37th International Cosmic Ray Conference in Berlin Germany (ICRC 2021)

Author

Alameddine, Jean-Marco, Albrecht, Johannes, Alvarez-Muniz, Jaime, Alves, Antonio Augusto, Arrabito, Luisa, Baack, Dominik, Bernlöhr, Konrad, Bleicher, Marcus, Bregeon, Johan, Carrere, Mathieu, Dembinski, Hans, Elfner, Hannah, Elsässer, Dominik, Engel, Ralph, Fan, Hu, Fedynitch, Anatoli, Heck, Dieter, Huege, Tim, Kampert, Karl-Heinz, Karastathis, Nikolaos, Nellen, Lukas, Nöthe, Maximilian, Parello, David, Pierog, Tanguy, Pokrandt, Maria, Poctarev, Anton, Prechelt, Remy, Reininghaus, Maximilian, Rhode, Wolfgang, Riehn, Felix, Sackel, Maximilian, Sandrock, Alexander, Sampathkumar, Pranav, Schmelling, Michael, Schmidt, André, Sigl, Günter, Soedingrekso, Jan, Spaan, Bernhard, Xu, Donglian, Ammerman-Yebra, Juan, Zas, Enrique, Ulrich, Ralf, 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 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), Digits, Architectures et Logiciels Informatiques (DALI), Laboratoire d'Informatique de Robotique et de Microélectronique de Montpellier (LIRMM), Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Centre National de la Recherche Scientifique (CNRS)-Université de Montpellier (UM)-Université de Perpignan Via Domitia (UPVD), CORSIKA, and HEP, INSPIRE

Subjects
High Energy Astrophysical Phenomena (astro-ph.HE), radio wave, showers: atmosphere, air, Astrophysics::High Energy Astrophysical Phenomena, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, showers, cascade, cascade: electromagnetic, electromagnetic, [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], cosmic radiation, atmosphere, Cherenkov, modular, hadron, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [PHYS.ASTR] Physics [physics]/Astrophysics [astro-ph], [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Astrophysics - High Energy Astrophysical Phenomena, Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

Compilation of the six contributions to the ICRC conference 2021 by the CORSIKA 8 Collaboration. The status of the project is illustrated. In particular, the secondary hadron as well as the electromagnetic cascades are being validated individually, and current results are reviewed. A novel framework for radio emission simulations is presented, which is designed given the modular nature of CORSIKA 8 to support, both, the CoREAS as well as the ZHS formalism. At the same time, first Cherenkov emission calculations are shown which are based on CORSIKA 8 coupled with a GPU Cherenkov emission code. Finally, a new powerful feature of CORSIKA 8 is illustrated, where the entire genealogy of air shower particles can be studied in all details., ICRC 2021 conference, 6 proceedings, 51 pages

Published
2021

3. L'Astronomie gamma haute énergie au sol et dans l'espace

Author

BREGEON, Johan, 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), Université de Montpellier, and Eric Kajfasz(kajfasz@cppm.in2p3.fr)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], gamma-ray astronomy cherenkov space telescope, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], rayon gamma astronomie cherenkov telescope
Abstract

HDR Document; Document HDR

Published
2019

4. Gamma-ray astronomy on ground and in space

Author

BREGEON, Johan, 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), Université de Montpellier, and Eric Kajfasz(kajfasz@cppm.in2p3.fr)

Subjects
[PHYS.ASTR.HE]Physics [physics]/Astrophysics [astro-ph]/High Energy Astrophysical Phenomena [astro-ph.HE], [PHYS.ASTR.IM]Physics [physics]/Astrophysics [astro-ph]/Instrumentation and Methods for Astrophysic [astro-ph.IM], gamma-ray astronomy cherenkov space telescope, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], rayon gamma astronomie cherenkov telescope
Abstract

HDR Document; Document HDR

Published
2019

5. Einstein@Home discovers a radio-quiet gamma-ray millisecond pulsar

Author

Clark, Colin J., Pletsch, Holger J., Aulbert, Carsten, Orienti, Monica, Orlando, Elena, Palatiello, Michele, Paliya, Vaidehi S., de Palma, Francesco, Paneque, David, Perkins, Jeremy S., Persic, Massimo, Pesce-Rollins, Melissa, Porter, Troy A., Beer, Christian, Principe, Giacomo, Rainò, Silvia, Rando, Riccardo, Ray, Paul S., Razzano, Massimiliano, Reimer, Anita, Reimer, Olaf, Romani, Roger W., Saz Parkinson, Pablo M., Sgrò, Carmelo, Bock, Oliver, Siskind, Eric J., Smith, David A., Spada, Francesca, Spandre, Gloria, Spinelli, Paolo, Thayer, Jana B., Thompson, David J., Torres, Diego F., Troja, Eleonora, Vianello, Giacomo, Cuéllar, Andres, Wood, Kent, Wood, Matthew, Fermi-LAT Collaboration, Eggenstein, Heinz-Bernd, Fehrmann, Henning, Kramer, Michael, Kwang, Shawn A., Machenschalk, Bernd, Nieder, Lars, Wu, Jason, Ackermann, Markus, Ajello, Marco, Baldini, Luca, Ballet, Jean, Barbiellini, Guido, Bastieri, Denis, Bellazzini, Ronaldo, Bissaldi, Elisabetta, Blandford, Roger D., Bloom, Elliott D., Guillemot, Lucas, Bonino, Raffaella, Bottacini, Eugenio, Brandt, Terri J., Bregeon, Johan, Bruel, Philippe, Buehler, Rolf, Burnett, Toby H., Buson, Sara, Cameron, Rob A., Caputo, Regina, Kerr, Matthew, Caraveo, Patrizia A., Cavazzuti, Elisabetta, Cecchi, Claudia, Charles, Eric, Chekhtman, Alexandre, Ciprini, Stefano, Cominsky, Lynn R., Costantin, Denise, Cutini, Sara, D'Ammando, Filippo, Johnson, Tyrel J., De Luca, Andrea, Desiante, Rachele, Di Venere, Leonardo, Di Mauro, Mattia, Di Lalla, Niccolò, Digel, Seth W., Favuzzi, Cecilia, Ferrara, Elizabeth C., Franckowiak, Anna, Fukazawa, Yasushi, Camilo, Fernando, Funk, Stefan, Fusco, Piergiorgio, Gargano, Fabio, Gasparrini, Dario, Giglietto, Nico, Giordano, Francesco, Giroletti, Marcello, Gomez-Vargas, Germán A., Green, David, Grenier, Isabelle A., Salvetti, David, Guiriec, Sylvain, Harding, Alice K., Hewitt, John W., Horan, Deirdre, Jóhannesson, Guðlaugur, Kensei, Shiki, Kuss, Michael, La Mura, Giovanni, Larsson, Stefan, Latronico, Luca, Allen, Bruce, Li, Jian, Longo, Francesco, Loparco, Francesco, Lovellette, Michael N., Lubrano, Pasquale, Magill, Jeffrey D., Maldera, Simone, Manfreda, Alberto, Mazziotta, Mario N., McEnery, Julie E., Anderson, David, Michelson, Peter F., Mirabal, Nestor, Mitthumsiri, Warit, Mizuno, Tsunefumi, Monzani, Maria Elena, Morselli, Aldo, Moskalenko, Igor V., Nuss, Eric, Ohsugi, Takashi, Omodei, Nicola, 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)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Centre National de la Recherche Scientifique (CNRS)-Université d'Orléans (UO)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Centre National d’Études Spatiales [Paris] (CNES), Unité Scientifique de la Station de Nançay (USN), Université d'Orléans (UO)-Observatoire des Sciences de l'Univers en région Centre (OSUC), PSL Research University (PSL)-PSL Research University (PSL)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-Centre National de la Recherche Scientifique (CNRS), 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 Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Laboratoire Univers et Particules de Montpellier (LUPM), 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), 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), 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, 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), Université Paris sciences et lettres (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS), Astrophysique Interprétation Modélisation (AIM (UMR7158 / UMR_E_9005 / UM_112)), 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 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), ITA, 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), 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 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)-École polytechnique (X)-Institut National de Physique Nucléaire et de Physique des Particules du CNRS (IN2P3), PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université d'Orléans (UO)-Centre National de la Recherche Scientifique (CNRS)-Centre National d’Études Spatiales [Paris] (CNES), Laboratoire de Physique et Chimie de l'Environnement et de l'Espace ( LPC2E ), Centre National de la Recherche Scientifique ( CNRS ) -Université d'Orléans ( UO ) -Institut national des sciences de l'Univers ( INSU - CNRS ), Unité Scientifique de la Station de Nançay ( USN ), Institut national des sciences de l'Univers ( INSU - CNRS ) -Observatoire de Paris-Université d'Orléans ( UO ) -Centre National de la Recherche Scientifique ( CNRS ), Laboratoire AIM, Université Paris Diderot - Paris 7 ( UPD7 ) -Centre d'Etudes de Saclay, Laboratoire Univers et Particules de Montpellier ( LUPM ), Centre National de la Recherche Scientifique ( CNRS ) -Institut National de Physique Nucléaire et de Physique des Particules du CNRS ( IN2P3 ) -Université Montpellier 2 - Sciences et Techniques ( UM2 ) -Université de Montpellier ( UM ), 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 ), 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 ), Raunvísindastofnun (HÍ), Science Institute (UI), Verkfræði- og náttúruvísindasvið (HÍ), School of Engineering and Natural Sciences (UI), Háskóli Íslands, University of Iceland, Clark, Colin J., Pletsch, Holger J., Wu, Jason, Guillemot, Luca, Kerr, Matthew, Johnson, Tyrel J., Camilo, Fernando, Salvetti, David, Allen, Bruce, Anderson, David, Aulbert, Carsten, Beer, Christian, Bock, Oliver, Cuéllar, Andre, Eggenstein, Heinz-Bernd, Fehrmann, Henning, Kramer, Michael, Kwang, Shawn A., Machenschalk, Bernd, Nieder, Lar, Ackermann, Marku, Ajello, Marco, Baldini, Luca, Ballet, Jean, Barbiellini, Guido, Bastieri, Deni, Bellazzini, Ronaldo, Bissaldi, Elisabetta, Blandford, Roger D., Bloom, Elliott D., Bonino, Raffaella, Bottacini, Eugenio, Brandt, Terri J., Bregeon, Johan, Bruel, Philippe, Buehler, Rolf, Burnett, Toby H., Buson, Sara, Cameron, Rob A., Caputo, Regina, Caraveo, Patrizia A., Cavazzuti, Elisabetta, Cecchi, Claudia, Charles, Eric, Chekhtman, Alexandre, Ciprini, Stefano, Cominsky, Lynn R., Costantin, Denise, Cutini, Sara, D'Ammando, Filippo, De Luca, Andrea, Desiante, Rachele, Di Venere, Leonardo, Di Mauro, Mattia, Di Lalla, Niccolò, Digel, Seth W., Favuzzi, Cecilia, Ferrara, Elizabeth C., Franckowiak, Anna, Fukazawa, Yasushi, Funk, Stefan, Fusco, Piergiorgio, Gargano, Fabio, Gasparrini, Dario, Giglietto, Nico, Giordano, Francesco, Giroletti, Marcello, Gomez-Vargas, Germán A., Green, David, Grenier, Isabelle A., Guiriec, Sylvain, Harding, Alice K., Hewitt, John W., Horan, Deirdre, Jóhannesson, Guolaugur, Kensei, Shiki, Kuss, Michael, La Mura, Giovanni, Larsson, Stefan, Latronico, Luca, Li, Jian, Longo, Francesco, Loparco, Francesco, Lovellette, Michael N., Lubrano, Pasquale, Magill, Jeffrey D., Maldera, Simone, Manfreda, Alberto, Mazziotta, Mario N., Mcenery, Julie E., Michelson, Peter F., Mirabal, Nestor, Mitthumsiri, Warit, Mizuno, Tsunefumi, Monzani, Maria Elena, Morselli, Aldo, Moskalenko, Igor V., Nuss, Eric, Ohsugi, Takashi, Omodei, Nicola, Orienti, Monica, Orlando, Elena, Palatiello, Michele, Paliya, Vaidehi S., De Palma, Francesco, Paneque, David, Perkins, Jeremy S., Persic, Massimo, Pesce-Rollins, Melissa, Porter, Troy A., Principe, Giacomo, Rainò, Silvia, Rando, Riccardo, Ray, Paul S., Razzano, Massimiliano, Reimer, Anita, Reimer, Olaf, Romani, Roger W., Parkinson, Pablo M. Saz, Sgrò, Carmelo, Siskind, Eric J., Smith, David A., Spada, Francesca, Spandre, Gloria, Spinelli, Paolo, Thayer, Jana B., Thompson, David J., Torres, Diego F., Troja, Eleonora, Vianello, Giacomo, Wood, Kent, and Wood, Matthew

Subjects
Einstein@Home, Gammageislar, [ PHYS.ASTR ] Physics [physics]/Astrophysics [astro-ph], Astronomy, Astrophysics::High Energy Astrophysical Phenomena, Population, FOS: Physical sciences, Astrophysics::Cosmology and Extragalactic Astrophysics, 01 natural sciences, law.invention, Telescope, Computer Science::Hardware Architecture, Bulge, Millisecond pulsar, law, 0103 physical sciences, Astrophysics::Solar and Stellar Astrophysics, 010306 general physics, education, 010303 astronomy & astrophysics, Research Articles, Physics, High Energy Astrophysical Phenomena (astro-ph.HE), education.field_of_study, Line-of-sight, Multidisciplinary, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], Nifteindastjörnur, Astrophysics::Instrumentation and Methods for Astrophysics, SciAdv r-articles, Computer Science::Computers and Society, Stjörnusjónaukar, Neutron star, ddc:500, Astrophysics - High Energy Astrophysical Phenomena, [PHYS.ASTR]Physics [physics]/Astrophysics [astro-ph], Fermi Gamma-ray Space Telescope, Research Article
Abstract

Millisecond pulsars (MSPs) are old neutron stars that spin hundreds of times per second and appear to pulsate as their emission beams cross our line of sight. To date, radio pulsations have been detected from all rotation-powered MSPs. In an attempt to discover radio-quiet gamma-ray MSPs, we used the aggregated power from the computers of tens of thousands of volunteers participating in the Einstein@Home distributed computing project to search for pulsations from unidentified gamma-ray sources in Fermi Large Area Telescope data. This survey discovered two isolated MSPs, one of which is the only known rotation-powered MSP to remain undetected in radio observations. These gamma-ray MSPs were discovered in completely blind searches without prior constraints from other observations, raising hopes for detecting MSPs from a predicted Galactic bulge population., This work was supported by the Max-Planck-Gesellschaft, the Deutsche Forschungsgemeinschaft through an Emmy Noether Research Grant [no. PL 710/1-1 (H.J.P.)], and NSF award 1104902. C.J.C. acknowledges support from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 715051; Spiders). W.M. was partially supported by the Thailand Research Fund (grants TRG5880173 and RTA5980003). M.R. was funded by the Italian Ministry of Education, University and Research (contract no. FIRB-2012-RBFR12PM1F). Work at the Naval Research Laboratory is supported by NASA. The Parkes Observatory is part of the Australia Telescope, funded by the Commonwealth of Australia for operation as a National Facility managed by the Commonwealth Scientific and Industrial Research Organisation (CSIRO). 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
2018
Full Text
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6. Structuring Metadata for the Cherenkov Telescope Array

Author

Servillat, Mathieu, Boisson, Catherine, Lefaucheur, Julien, Bregeon, Johan, Sanguillon, Michèle, Contreras, Jose-Luis, Laboratoire Univers et Théories (LUTH (UMR_8102)), Institut national des sciences de l'Univers (INSU - CNRS)-Observatoire de Paris, PSL Research University (PSL)-PSL Research University (PSL)-Université Paris Diderot - Paris 7 (UPD7)-Centre National de la Recherche Scientifique (CNRS), Université Montpellier 2 - Sciences et Techniques (UM2), CTA Consortium, and 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)

Subjects
Cherenkov Telescope Array, data acquisition, Astrophysics::High Energy Astrophysical Phenomena, diffusion, Astrophysics::Instrumentation and Methods for Astrophysics, FOS: Physical sciences, landscape, observatory, Cherenkov counter, gamma ray, Física nuclear, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], Astrophysics - Instrumentation and Methods for Astrophysics, Instrumentation and Methods for Astrophysics (astro-ph.IM)
Abstract

The landscape of ground-based gamma-ray astronomy is drastically changing with the perspective of the Cherenkov Telescope Array (CTA) composed of more than 100 Cherenkov telescopes. For the first time in this energy domain, CTA will be operated as an observatory open to the astronomy community. In this context, a structured high level data model is being developed to describe a CTA observation. The data model includes different classes of metadata on the project definition, the configuration of the instrument, the ambient conditions, the data acquisition and the data processing. This last part relies on the Provenance Data Model developed within the International Virtual Observatory Alliance (IVOA), for which CTA is one of the main use cases. The CTA data model should also be compatible with the Virtual Observatory (VO) for data diffusion. We have thus developed a web-based data diffusion prototype to test this requirement and ensure the compliance., To appear in the ADASS XXVI Proceedings

Published
2019

7. Raman LIDARs for the atmospheric calibrationalong the line-of-sight of CTA

Author

Ballester, Otger, Blanch, Oscar, Boix, Joan, Bregeon, Johan, Brun, Patrick, Çolak, §ıdıka Merve, Doro, Michele, Da Deppo, Vania, Font, Lluís, Gabella, Omar, García-Tenorio García-Balmaseda, Rafael, Gaug, Markus, Maggio, Camilla, Martínez, Manel Cruz, Martínez, Óscar, Adrover, Pere Munar, Ramos, Raúl, Rivoire, Stephane, Staniˇc, Samo, Villar, David, Vasileiadis, George, Wang, Longlong, Zavrtanik, Marko, and Universidad de Sevilla. Departamento de Física Aplicada II

Abstract

The Cherenkov Telescope Array (CTA) is the next generation ground-based observatory forgamma-ray astronomy at very-high energies. Employing more than 100 Imaging AtmosphericCherenkov Telescopes in the northern and southern hemispheres, it was designed to reach un-precedented sensitivity and energy resolution. Understanding and correcting for systematic bi-ases on the absolute energy scale and instrument response functions will be a crucial issue forthe performance of CTA. The LUPM group and the Spanish/Italian/Slovenian collaboration arecurrently building two Raman LIDAR prototypes for the online atmospheric calibration alongthe line-of-sight of the CTA. Requirements for such a solution include the ability to characterizeaerosol extinction at two wavelengths to distances of 30 km with an accuracy better than 5%,within time scales of about a minute, steering capabilities and close interaction with the CTAarray control and data acquisition system as well as other auxiliary instruments. Our Raman LI-DARs have design features that make them different from those used in atmospheric science andare characterized by large collecting mirrors (∼2.5 m2), liquid light-guides that collect the light atthe focal plane and transport it to the readout system, reduced acquisition time and highly preciseRaman spectrometers. The Raman LIDARs will participate in a cross-calibration and character-ization campaign of the atmosphere at the CTA North site at La Palma, together with other sitecharacterization instruments. After a one-year test period there, an in-depth evaluation of the so-lutions adopted by the two projects will lead to a final Raman LIDAR design proposal for bothCTA sites.

Published
2019

8. Einstein@Home discovers a radio-quiet gamma-ray millisecond pulsar

Author

Clark, Colin J., Pletsch, Holger J., Wu, Jason, Guillemot, Lucas, Kerr, Matthew, Johnson, Tyrel J., Camilo, Fernando, Salvetti, David, Allen, Bruce, Anderson, David, Aulbert, Carsten, Beer, Christian, Bock, Oliver, Cuéllar, Andres, Eggenstein, Heinz-Bernd, Fehrmann, Henning, Kramer, Michael, Kwang, Shawn A., Machenschalk, Bernd, Nieder, Lars, Ackermann, Markus, Ajello, Marco, Baldini, Luca, Ballet, Jean, Barbiellini, Guido, Bastieri, Denis, Bellazzini, Ronaldo, Bissaldi, Elisabetta, Blandford, Roger D., Bloom, Elliott D., Bonino, Raffaella, Bottacini, Eugenio, Brandt, Terri J., Bregeon, Johan, Bruel, Philippe, Buehler, Rolf, Burnett, Toby H., Buson, Sara, Cameron, Rob A., Caputo, Regina, Caraveo, Patrizia A., Cavazzuti, Elisabetta, Cecchi, Claudia, Charles, Eric, Chekhtman, Alexandre, Ciprini, Stefano, Cominsky, Lynn R., Costantin, Denise, Cutini, Sara, D'Ammando, Filippo, De Luca, Andrea, Desiante, Rachele, Di Venere, Leonardo, Di Mauro, Mattia, Di Lalla, Niccolò, Digel, Seth W., Favuzzi, Cecilia, Ferrara, Elizabeth C., Franckowiak, Anna, Fukazawa, Yasushi, Funk, Stefan, Fusco, Piergiorgio, Gargano, Fabio, Gasparrini, Dario, Giglietto, Nico, Giordano, Francesco, Giroletti, Marcello, Gomez-Vargas, Germán A., Green, David, Grenier, Isabelle A., Guiriec, Sylvain, Harding, Alice K., Hewitt, John W., Horan, Deirdre, Jóhannesson, Guðlaugur, Kensei, Shiki, Kuss, Michael, La Mura, Giovanni, Larsson, Stefan, Latronico, Luca, Li, Jian, Longo, Francesco, Loparco, Francesco, Lovellette, Michael N., Lubrano, Pasquale, Magill, Jeffrey D., Maldera, Simone, Manfreda, Alberto, Mazziotta, Mario N., McEnery, Julie E., Michelson, Peter F., Mirabal, Nestor, Mitthumsiri, Warit, Mizuno, Tsunefumi, Monzani, Maria Elena, Morselli, Aldo, Moskalenko, Igor V., Nuss, Eric, Ohsugi, Takashi, Omodei, Nicola, Orienti, Monica, Orlando, Elena, Palatiello, Michele, Paliya, Vaidehi S., De Palma, Francesco, Paneque, David, Perkins, Jeremy S., Persic, Massimo, Pesce-Rollins, Melissa, Porter, Troy A., Principe, Giacomo, Rainò, Silvia, Rando, Riccardo, Ray, Paul S., Razzano, Massimiliano, Reimer, Anita, Reimer, Olaf, Romani, Roger W., Saz Parkinson, Pablo M., Sgrò, Carmelo, Siskind, Eric J., Smith, David A., Spada, Francesca, Spandre, Gloria, Spinelli, Paolo, Thayer, Jana B., Thompson, David J., Torres, Diego F., Troja, Eleonora, Vianello, Giacomo, Wood, Kent, and Wood, Matthew

Abstract

Science advances 4(2), eaao7228 - (2018). doi:10.1126/sciadv.aao7228, Millisecond pulsars (MSPs) are old neutron stars that spin hundreds of times per second and appear to pulsate as their emission beams cross our line of sight. To date, radio pulsations have been detected from all rotation-powered MSPs. In an attempt to discover radio-quiet gamma-ray MSPs, we used the aggregated power from the computers of tens of thousands of volunteers participating in the Einstein@Home distributed computing project to search for pulsations from unidentified gamma-ray sources in Fermi Large Area Telescope data. This survey discovered two isolated MSPs, one of which is the only known rotation-powered MSP to remain undetected in radio observations. These gamma-ray MSPs were discovered in completely blind searches without prior constraints from other observations, raising hopes for detecting MSPs from a predicted Galactic bulge population., Published by AAAS, Washington, DC [u.a.]

Published
2018
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9. HESS reveals a lack of TeV emission from the supernova remnant Puppis A (Research Note)

Author

Abramowski, Attila, Aharonian, Felix A., Benkhali, Faical Ait, Akhperjanian, A. G., Angüner, Ekrem Oǧuzhan, Backes, Michael, Balenderan, Shangkari, Balzer, Arnim, Barnacka, Anna, Becherini, Yvonne, Tjus, J. Becker, Berge, David, Bernhard, Sabrina, Bernlöhr, K., Birsin, E., Biteau, Jonathan, Boettcher, Markus, Boisson, Catherine, Bolmont, J., Bordas, Pol, Bregeon, Johan, Brun, Francois, Brun, Pierre, Bryan, Mark, Bulik, Tomasz, Carrigan, Svenja, Casanova, Sabrina, Chadwick, Paula M., Chakraborty, N., Chalme-Calvet, R., Chaves, Ryan C. G., Chretien, M., Colafrancesco, Sergio, Cologna, Gabriele, Conrad, Jan, Couturier, C., Cui, Y., Davids, I. D., Degrange, B., Deil, C., deWilt, P., Djannati-Ataï, A., Domainko, W., Donath, A., Dubus, G., Dutson, K., Dyks, J., Dyrda, M., Edwards, T., Egberts, Kathrin, Eger, P., Espigat, P., Farnier, C., Fegan, S., Feinstein, F., Fernandes, M. V., Fernandez, D., Fiasson, A., Fontaine, G., Foerster, A., Füssling, Matthias, Gabici, S., Gajdus, M., Gallant, Y. A., Garrigoux, T., Giavitto, G., Giebels, B., Glicenstein, J. F., Gottschall, D., Grondin, M. -H., Grudzinska, M., Hadasch, D., Haeffner, S., Hahn, J., Harris, J., Heinzelmann, G., Henri, G., Hermann, G., Hervet, O., Hillert, A., Hinton, James Anthony, Hofmann, W., Hofverberg, P., Holler, Maraike, Horns, D., Ivascenko, A., Jacholkowska, A., Jahn, C., Jamrozy, M., Janiak, M., Jankowsky, F., Jung-Richardt, I., Kastendieck, M. A., Katarzynski, K., Katz, U., Kaufmann, S., Khelifi, B., Kieffer, M., Klepser, S., Klochkov, D., Kluzniak, W., Kolitzus, D., Komin, Nu., Kosack, K., Krakau, S., Krayzel, F., Krueger, P. P., Laffon, H., Lamanna, G., Lefaucheur, J., Lefranc, V., Lemiere, A., Lemoine-Goumard, M., Lenain, J. -P., Lohse, T., Lopatin, A., Lu, C. -C., Marandon, V., Marcowith, A., Marx, R., Maurin, G., Maxted, N., Mayer, Michael, McComb, T. J. L., Mehault, J., Meintjes, P. J., Menzler, U., Meyer, M., Mitchell, A. M. W., Moderski, R., Mohamed, M., Mora, K., Moulin, E., Murach, T., de Naurois, M., Niemiec, J., Nolan, S. J., Oakes, L., Odaka, H., Ohm, S., Opitz, B., Ostrowski, M., Oya, I., Panter, M., Parsons, R. D., Arribas, M. Paz, Pekeur, N. W., Pelletier, G., Petrucci, P. -O, Peyaud, B., Pita, S., Poon, H., Puehlhofer, G., Punch, M., Quirrenbach, A., Raab, S., Reichardt, I., Reimer, A., Reimer, O., Renaud, M., de los Reyes, R., Rieger, F., Romoli, C., Rosier-Lees, S., Rowell, G., Rudak, B., Rulten, C. B., Sahakian, V., Salek, D., Sanchez, David M., Santangelo, A., Schlickeiser, R., Schuessler, F., Schulz, A., Schwanke, U., Schwarzburg, S., Schwemmer, S., Sol, H., Spanier, F., Spengler, G., Spies, F., Stawarz, L., Steenkamp, R., Stegmann, Christian, Stinzing, F., Stycz, K., Sushch, Iurii, Tavernet, J. -P., Tavernier, T., Taylor, A. M., Terrier, R., Tluczykont, M., Trichard, C., Valerius, K., van Eldik, C., van Soelen, B., Vasileiadis, G., Veh, J., Venter, C., Viana, A., Vincent, P., Vink, J., Voelk, H. J., Volpe, F., Vorster, M., Vuillaume, T., Wagner, S. J., Wagner, P., Wagner, R. M., Ward, M., Weidinger, M., Weitzel, Q., White, R., Wierzcholska, A., Willmann, P., Woernlein, A., Wouters, D., Yang, R., Zabalza, V., Zaborov, D., Zacharias, M., Zdziarski, A. A., Zech, A., and Zechlin, H. -S.

Subjects
Astrophysics::High Energy Astrophysical Phenomena, Institut für Physik und Astronomie
Abstract

Context. Puppis A is an interesting similar to 4 kyr-old supernova remnant (SNR) that shows strong evidence of interaction between the forward shock and a molecular cloud. It has been studied in detail from radio frequencies to high-energy (HE, 0.1-100 GeV) gamma-rays. An analysis of the Fermi-LAT data has shown extended HE gamma-ray emission with a 0.2-100 GeV spectrum exhibiting no significant deviation from a power law, unlike most of the GeV-emitting SNRs known to be interacting with molecular clouds. This makes it a promising target for imaging atmospheric Cherenkov telescopes (IACTs) to probe the gamma-ray emission above 100 GeV. Aims. Very-high-energy (VHE, E >= 0.1 TeV) gamma-ray emission from Puppis A has been, for the first time, searched for with the High Energy Stereoscopic System (HESS.). Methods. Stereoscopic imaging of Cherenkov radiation from extensive air showers is used to reconstruct the direction and energy of the incident gamma-rays in order to produce sky images and source spectra. The profile likelihood method is applied to find constraints on the existence of a potential break or cutoff in the photon spectrum. Results. The analysis of the HESS. data does not reveal any significant emission towards Puppis A. The derived upper limits on the differential photon flux imply that its broadband gamma-ray spectrum must exhibit a spectral break or cutoff. By combining Fermi-LAT and HESS. measurements, the 99% confidence-level upper limits on such a cutoff are found to be 450 and 280 GeV, assuming a power law with a simple exponential and a sub-exponential cutoff, respectively. It is concluded that none of the standard limitations (age, size, radiative losses) on the particle acceleration mechanism, assumed to be continuing at present, can explain the lack of VHE signal. The scenario in which particle acceleration has ceased some time ago is considered as an alternative explanation. The HE/VHE spectrum of Puppis A could then exhibit a break of non-radiative origin (as observed in several other interacting SNRs, albeit at somewhat higher energies), owing to the interaction with dense and neutral material, in particular towards the NE region.

Published
2015

10. Contribution to the GLAST-LAT energy calibration and benchmarking of hadronic cascade models under GEANT4

Author

Bregeon, Johan, 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), Université Sciences et Technologies - Bordeaux I, Benoit LOTT(lott@in2p3.fr), and Bregeon, Johan

Subjects
Gamma-ray astronomy, [SDU.ASTR]Sciences of the Universe [physics]/Astrophysics [astro-ph], [PHYS.PHYS.PHYS-INS-DET] Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], CsI, Quenching, Cascade hadronique, Astronomie Gamma, [PHYS.PHYS.PHYS-INS-DET]Physics [physics]/Physics [physics]/Instrumentation and Detectors [physics.ins-det], [SDU.ASTR] Sciences of the Universe [physics]/Astrophysics [astro-ph], hadronic cascade, GLAST, GEANT4
Abstract

GLAST is the new generation of Gamma-ray space telescope and should dramatically improve our knowledge of the Gamma-ray sky when it is launched in September 7th 2007.Data from the beam test that was held at GANIL with low energy ions were analyzed in order to measure the light quenching factor of CsI for all kinds of ions from proton to krypton of energy between 0 and 73MeV per nucleon. These results have been very useful to understand the light quenching for relativistic ions that was measured during the GSI beam test. The knowledge of light quenching in GLAST CsI detectors for high energy ions is required for the on-orbit calibration with cosmic rays to succeed.Hadronic background rejection is another major issue for GLAST, thus, all the algorithms rely on the GLAST official Monte-Carlo simulation, GlastRelease. Hadronic cascade data from the GSI beam test and from another beam test held at CERN on the SPS have been used to benchmark hadronic cascade simulation within the framework of GEANT4, on which GlastRelease is based.Testing the good reproduction of simple parameters in GLAST-like calorimeters for hadronic cascades generated by 1.7GeV, 3.4GeV, 10GeV and 20GeV protons or pions led us to the conclusion that at high energy the default LHEP model is good enough, whereas at low energy the Bertini intra-nuclear cascade model should be used., GLAST est la nouvelle génération de télescope spatial pour l'étude des rayons gamma et devrait très largement améliorer notre connaissance du ciel à haute énergie, dès son lancement en août 2007.Les données du faisceau-test mené au GANIL avec des ions de basse énergie, ont permis de contribuer à l'étalonnage en énergie du LAT. Ces données ont été analysées pour mesurer la non-linéarité de la production de lumière dans le CsI en réponse au dépôt d'énergie des ions, des protons au krypton et pour des énergies allant de 0 à 73MeV par nucléon. Les résultats obtenus se sont révélés complémentaires aux mesures de scintillation du CsI, réalisées lors du faisceau-test mené au GSI pour des ions lourds relativistes . La connaissance de la non-linéarité de la réponse des cristaux de CsI de GLAST aux ions de haute énergie est indispensable pour réaliser l'étalonnage en énergie en orbite des détecteurs à l'aide des rayons cosmiques.Le rejet des évènements hadroniques est un autre problème clé pour GLAST, or, l'élaboration des algorithmes repose sur la simulation Monte-Carlo officielle de GLAST, GlastRelease. Les cascades hadroniques mesurées lors du faisceau-test mené au GSI et lors d'un autre faisceau-test mené au CERN sur le SPS, sont utilisées pour confronter les codes de simulation, disponibles sur la plate-forme logicielle GEANT4 qui est à la base de GlastRelease. En vérifiant la bonne reproduction de certaines observables simples, pour des cascades hadroniques générées par des protons ou de pions de .7GeV , 3.4GeV, 10GeV et 20GeV, on conclue qu'à haute énergie le modèle par défaut, LHEP, est valable, alors qu'à basse énergie, le modèle de cascade intranucléaire de Bertini devrait être utilisé.

Published
2005

11. An x-ray polarimeter for HXMT mission

Author

Costa, Enrico, Bellazzini, Ronaldo, Tagliaferri, Gianpiero, Baldini, Luca, Basso, Stefano, Bregeon, Johan, Brez, Alessandro, Citterio, Oberto, Cotroneo, Vincenzo, Frontera, Filippo, Frutti, Massimo, Matt, Giorgio, Minuti, Massimo, Muleri, Fabio, Paresehi, Giovanni, Perola Giuseppe Cesare, Rubini, Alda, Sgro, Carmelo, Soffitta, Paolo, Spandre, Gloria, and BE Siegmund OHW

Subjects
X-ray Astronomy, Instrumentation, media_common.quotation_subject, Astrophysics::High Energy Astrophysical Phenomena, Polarimetry, FOS: Physical sciences, Astrophysics, NO, Optics, astro-ph, Astrophysics::Galaxy Astrophysics, media_common, X-ray Astronomy, X-ray optics, Polarimetry, Physics, X-ray optics, business.industry, Linear polarization, Astrophysics (astro-ph), Detector, Astrophysics::Instrumentation and Methods for Astrophysics, Polarimeter, Cardinal point, Sky, business, Focus (optics)
Abstract

The development of micropixel gas detectors, capable to image tracks produced in a gas by photoelectrons, makes possible to perform polarimetry of X-ray celestial sources in the focus of grazing incidence X-ray telescopes. HXMT is a mission by the Chinese Space Agency aimed to survey the Hard X-ray Sky with Phoswich detectors, by exploitation of the direct demodulation technique. Since a fraction of the HXMT time will be spent on dedicated pointing of particular sources, it could host, with moderate additional resources a pair of X-ray telescopes, each with a photoelectric X-ray polarimeter in the focal plane. We present the design of the telescopes and the focal plane instrumentation and discuss the performance of this instrument to detect the degree and angle of linear polarization of some representative sources. Notwithstanding the limited resources the proposed instrument can represent a breakthrough in X-ray Polarimetry., 10 pages, 9 figures

Published
2007

13. Performance optimization of the air shower simulation program for the Cherenkov Telescope Array

Author

Arrabito, Luisa, Bernlöhr, Konrad, Bregeon, Johan, Maier, Gernot, Langlois, Philippe, Parello, David, and Revy, Guillaume

Subjects
7. Clean energy
Abstract

23rd International Conference on Computing in High Energy and Nuclear Physics (CHEP 2018), Sofia, Bulgaria, 9 Jul 2018 - 13 Jul 2018; The European physical journal / Web of Conferences Web of Conferences : proceedings proceedings 214, 05041 - (2019). doi:10.1051/epjconf/201921405041, The Cherenkov Telescope Array (CTA), currently under construction,is the next-generation instrument in the field of very high energy gammarayastronomy. The first data are expected by the end of 2018, while the scientificoperations will start in 2022 for a duration of about 30 years. In order tocharacterize the instrument response to the Cherenkov light emitted when cosmicray showers develop in the atmosphere, detailed Monte Carlo simulationswill be regularly performed in parallel to CTA operation. The estimated CPUtime associated to these simulations is very high, of the order of 200 millionsHS06 hours per year. Reducing the CPU time devoted to simulations would alloweither to reduce infrastructure cost or to better cover the large phase space.In this paper, we focus on the main computing step (70% of the whole CPUtime) implemented in the CORSIKA program, and specifically on the moduleresponsible for the propagation of Cherenkov photons in the atmosphere.We present our preliminary studies about different options of code optimization,with a particular focus on vectorization facilities (SIMD instructions). Ourproposals take care, as automatically as possible, of the hardware portabilityconstraints introduced by the grid computing environment that hosts these simulations.Performance evaluation in terms of running-time and accuracy is provided., Published by EDP Sciences, Les Ulis

14. Effect of the uncertainty in the hadronic interaction models on the estimation of the sensitivity of the Cherenkov telescope array

Author

Ohishi, Michiko, Arbeletche, Luan, de Souza, Vitor, Maier, Gernot, Bernlöhr, Konrad, Olaizola, Abelardo Moralejo, Bregeon, Johan, Arrabito, Luisa, and Yoshikoshi, Takanori

Subjects
Cherenkov Telescope Array, interaction: model, current: hadronic, air, pi, energy spectrum, cosmic radiation: interaction, Cherenkov counter: atmosphere, GeV, GLAST, charged particle: cosmic radiation, HESS, TeV, AMS, cosmic radiation: VHE, electromagnetic component, showers: atmosphere, nucleus, imaging, sensitivity, MAGIC, CERN LHC Coll, 13. Climate action, gamma ray, DAMPE, hadron, numerical calculations: Monte Carlo
Abstract

Journal of physics / G 48(7), 075201 - (2021). doi:10.1088/1361-6471/abfce0, Imaging atmospheric Cherenkov telescopes (IACTs) are ground-based indirect detectors for cosmic gamma rays with energies above tens of GeV. The major backgrounds for gamma-ray observations in IACTs are cosmic-ray charged particles. The capability to reject these backgrounds is the most important factor determining the gamma-ray sensitivity of IACT systems. Monte Carlo simulations are used to estimate the residual background rates and sensitivity of the systems during the design and construction phase. Uncertainties in the modeling of high-energy hadronic interactions of cosmic rays with nuclei in the air propagate into the estimates of residual background rates and subsequently into the estimated instrument sensitivity. We investigate the influence of the difference in the current hadronic interaction models on the estimated gamma-ray sensitivity of the Cherenkov Telescope Array using four interaction models (QGSJET-II-03, QGSJET-II-04, EPOS-LHC, and SIBYLL2.3c) implemented in the air shower simulation tool CORSIKA. Variations in background rates of up to a factor 2 with respect to QGSJET-II-03 are observed between the models, mainly due to differences in the $π^0$ production spectrum. These lead to ∼30% differences in the estimated gamma-ray sensitivity in the 1–30 TeV region, assuming a 50 h observation of a gamma-ray point-like source. The presented results also show that IACTs have a significant capability in the verification of hadronic interaction models., Published by IOP Publ., Bristol

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