Skip to main navigation Skip to search Skip to main content

Sensitivity of the Cherenkov Telescope Array to TeV photon emission from the Large Magellanic Cloud

  • A. Acharyya
  • , R. Adam
  • , A. Aguasca-Cabot
  • , I. Agudo
  • , A. Aguirre-Santaella
  • , J. Alfaro
  • , R. Aloisio
  • , R. Alves Batista
  • , E. Amato
  • , E. O. Angüner
  • , C. Aramo
  • , C. Arcaro
  • , K. Asano
  • , J. Aschersleben
  • , H. Ashkar
  • , M. Backes
  • , A. Baktash
  • , C. Balazs
  • , M. Balbo
  • , J. Ballet
  • A. Bamba, A. Baquero Larriva, V. Barbosa Martins, U. Barres de Almeida, J. A. Barrio, D. Bastieri, P. Batista, I. Batkovic, J. R. Baxter, J. Becerra González, J. Becker Tjus, W. Benbow, E. Bernardini, M. I.Bernardos Martín, J. Bernete Medrano, A. Berti, B. Bertucci, V. Beshley, P. Bhattacharjee, S. Bhattacharyya, C. Bigongiari, A. Biland, E. Bissaldi, F. Bocchino, P. Bordas, J. Borkowski, E. Bottacini, M. Böttcher, F. Bradascio, A. M. Brown, A. Bulgarelli, L. Burmistrov, S. Caroff, A. Carosi, E. Carquín, S. Casanova, E. Cascone, F. Cassol, M. Cerruti, P. Chadwick, S. Chaty, A. Chen, A. Chiavassa, L. Chytka, V. Conforti, J. Cortina, A. Costa, H. Costantini, G. Cotter, S. Crestan, P. Cristofari, F. D'Ammando, M. Dalchenko, F. Dazzi, A. De Angelis, V. De Caprio, E. M. de Gouveia Dal Pino, D. De Martino, M. de Naurois, V. de Souza, M. V. del Valle, A. G. Delgado Giler, C. Delgado, D. della Volpe, D. Depaoli, T. Di Girolamo, A. Di Piano, F. Di Pierro, R. Di Tria, L. Di Venere, S. Diebold, M. Doro, D. Dumora, V. V. Dwarkadas, C. Eckner, K. Egberts, G. Emery, J. Escudero, D. Falceta-Goncalves, E. Fedorova, S. Fegan, Q. Feng, D. Ferenc, G. Ferrand, E. Fiandrini, M. Filipovic, V. Fioretti, L. Foffano, G. Fontaine, Y. Fukui, D. Gaggero, G. Galanti, G. Galaz, S. Gallozzi, V. Gammaldi, M. Garczarczyk, C. Gasbarra, D. Gasparrini, A. Ghalumyan, M. Giarrusso, G. Giavitto, N. Giglietto, F. Giordano, A. Giuliani, J. F. Glicenstein, P. Goldoni, J. Goulart Coelho, J. Granot, D. Green, J. G. Green, M. H. Grondin, O. Gueta, D. Hadasch, P. Hamal, T. Hassan, K. Hayashi, M. Heller, S. Hernández Cadena, N. Hiroshima, B. Hnatyk, R. Hnatyk, W. Hofmann, J. Holder, M. Holler, D. Horan, P. Horvath, M. Hrabovsky, M. Hütten, M. Iarlori, T. Inada, F. Incardona, S. Inoue, F. Iocco, M. Jamrozy, W. Jin, I. Jung-Richardt, J. Juryšek, D. Kantzas, V. Karas, H. Katagiri, D. Kerszberg, J. Knödlseder, N. Komin, P. Kornecki, K. Kosack, G. Kowal, H. Kubo, A. Lamastra, J. Lapington, M. Lemoine-Goumard, J. P. Lenain, F. Leone, G. Leto, F. Leuschner, E. Lindfors, T. Lohse, S. Lombardi, F. Longo, R. López-Coto, A. López-Oramas, S. Loporchio, P. L. Luque-Escamilla, O. Macias, P. Majumdar, D. Mandat, S. Mangano, G. Manicò, M. Mariotti, P. Marquez, G. Marsella, J. Martí, P. Martin, M. Martínez, D. Mazin, S. Menchiari, D. M.A. Meyer, D. Miceli, M. Miceli, J. Michałowski, A. Mitchell, R. Moderski, L. Mohrmann, M. Molero, E. Molina, T. Montaruli, A. Moralejo, D. Morcuende, A. Morselli, E. Moulin, V. Moya, R. Mukherjee, K. Munari, A. Muraczewski, S. Nagataki, T. Nakamori, A. Nayak, J. Niemiec, M. Nievas, M. Nikołajuk, K. Nishijima, K. Noda, D. Nosek, B. Novosyadlyj, S. Nozaki, M. Ohishi, S. Ohm, A. Okumura, B. Olmi, R. A. Ong, M. Orienti, R. Orito, M. Orlandini, E. Orlando, S. Orlando, M. Ostrowski, I. Oya, A. Pagliaro, M. Palatka, F. R. Pantaleo, R. Paoletti, J. M. Paredes, N. Parmiggiani, B. Patricelli, M. Pech, M. Pecimotika, M. Persic, O. Petruk, E. Pierre, E. Pietropaolo, G. Pirola, M. Pohl, E. Prandini, C. Priyadarshi, G. Pühlhofer, M. L. Pumo, M. Punch, F. S. Queiroz, A. Quirrenbach, S. Rainò, R. Rando, S. Razzaque, A. Reimer, O. Reimer, T. Reposeur, M. Ribó, T. Richtler, J. Rico, F. Rieger, M. Rigoselli, V. Rizi, E. Roache, G. Rodriguez Fernandez, P. Romano, G. Romeo, J. Rosado, A. Rosales de Leon, B. Rudak, C. Rulten, I. Sadeh, T. Saito, M. Sánchez-Conde, H. Sano, A. Santangelo, R. Santos-Lima, S. Sarkar, F. G. Saturni, A. Scherer, P. Schovanek, F. Schussler, U. Schwanke, O. Sergijenko, M. Servillat, H. Siejkowski, C. Siqueira, S. Spencer, A. Stamerra, S. Stanič, C. Steppa, T. Stolarczyk, Y. Suda, T. Tavernier, M. Teshima, L. Tibaldo, D. F. Torres, N. Tothill, M. Vacula, B. Vallage, P. Vallania, C. van Eldik, M. Vázquez Acosta, M. Vecchi, S. Ventura, S. Vercellone, A. Viana, C. F. Vigorito, J. Vink, V. Vitale, V. Vodeb, S. Vorobiov, T. Vuillaume, S. J. Wagner, R. Walter, M. White, A. Wierzcholska, M. Will, R. Yamazaki, L. Yang, T. Yoshikoshi, M. Zacharias, G. Zaharijas, D. Zavrtanik, M. Zavrtanik, A. A. Zdziarski, V. I. Zhdanov, K. Ziętara, M. Živec
  • University of Alabama
  • Université de Nice
  • Ip Paris
  • University of Barcelona
  • Instituto de Astrofísica de Andalucía-CSIC
  • Universidad Autónoma de Madrid
  • Pontificia Universidad Católica de Chile
  • Gran Sasso Science Institute
  • Laboratori Nazionali del Gran Sasso
  • Osservatorio Astrofisico Di Arcetri
  • Sceintific and Technological Research Council of Turkey
  • INFN Sezione di Napoli
  • University of Padova
  • University of Tokyo
  • University of Groningen
  • University of Namibia
  • North-West University
  • Universität Hamburg
  • Monash University
  • Université de Genève
  • CEA/UVSQ/CNRS
  • Research Center for the Early Universe
  • IPARCOS-UCM (Instituto de Física de Partículas y del Cosmos)
  • Universidad del Azuay
  • c/o DESY
  • Centro Brasileiro de Pesquisas Fisicas
  • Research Unit; CIBERNED and Universidad de La Laguna
  • Ruhr-University Bochum
  • Center for Astrophysics | Harvard & Smithsonian
  • Centro de Investigaciones Energéticas Medioambientales y Tecnológicas (CIEMAT)
  • Max-Planck-Institut für Physik
  • University of Perugia
  • Pidstryhach Institute for Applied Problems in Mechanics and Mathematics NASU
  • Université Savoie Mont Blanc
  • University of Nova Gorica
  • Osservatorio Astronomico di Roma
  • ETH Zurich
  • INFN Sezione di Bari
  • Politecnico di Bari
  • Istituto di Astrofisica e Planetologia Spaziali (IAPS)
  • Nicolaus Copernicus Astronomical Center of the Polish Academy of Sciences
  • Université Paris-Saclay
  • Durham University
  • INAF Istituto di Astrofisica Spaziale e Fisica Cosmica, Bologna
  • University of Geneva
  • Universidad Técnica Federico Santa María
  • Institute for Nuclear Physics
  • Osservatorio Astronomico di Capodimonte
  • Aix-Marseille Université
  • Astroparticule and Cosmol APC
  • University of the Witwatersrand, Johannesburg
  • INFN Sezione di Torino
  • University of Turin
  • Joint Laboratory of Optics
  • INAF Osservatorio Astrofisico di Catania
  • University of Oxford
  • INAF Istituto di Astrofisica Spaziale e Fisica Cosmica, Milan
  • GEPI - Galaxies, Etoiles, Physique, Instrumentation
  • University of São Paulo
  • Max-Planck-Institut für Kernphysik
  • University of Naples Federico II
  • Università degli studi di Bari Aldo Moro
  • University of Tübingen
  • UMR 5797
  • University of Chicago
  • Chemin de Bellevue
  • University of Potsdam
  • National University of Kyiv
  • University of California, Davis
  • RIKEN (The Institute of Physical and Chemical Research)
  • Western Sydney University
  • Nagoya University
  • Istituto Nazionale di Fisica Nucleare, Sezione di Pisa
  • INFN Roma Tor Vergata
  • Yerevan Physics Institute
  • INFN Sezione di Catania
  • Universidade Federal Do Paraná - Setor Palotina
  • Universidade Federal do Espírito Santo
  • The Open University of Israel
  • George Washington University
  • Institute of Physics of the Czech Academy of Sciences
  • National Institute of Technology, Ichinoseki College
  • Universidad Nacional Autónoma de México
  • The Bartol Research Institute
  • University of Innsbruck
  • Università Dell'Aquila
  • Jagiellonian University
  • Friedrich-Alexander University (FAU) Erlangen-Nürnberg and Universitätsklinikum Erlangen
  • of Sciences
  • Ibaraki University
  • The Barcelona Institute of Science and Technology
  • IRAP/CNRS
  • University of Leicester
  • Sorbonne Université
  • Università degli Studi di Catania
  • University of Turku
  • Humboldt-Universität zu Berlin
  • University of Trieste
  • University of Jaen
  • University of Amsterdam
  • Saha Institute of Nuclear Physics
  • University of Palermo
  • University of Siena
  • Columbia University
  • Yamagata University
  • University of Białystok
  • Tokai University
  • Charles University
  • National University of Lviv
  • University of California, Los Angeles
  • Tokushima University
  • Cherenkov Telescope Array Observatory
  • INAF Istituto di Astrofisica Spaziale e Fisica Cosmica di Palermo
  • University of Pisa
  • University of Rijeka
  • INAF Osservatorio Astronomico di Padova
  • The Federal University of Rio Grande do Norte
  • Landessternwarte Heidelberg
  • University of Johannesburg
  • Universidad de Concepción
  • National Academy of Sciences of Ukraine
  • Agh University of Science and Technology Faculty of Computer Science
  • Academic Computer Centre Cyfronet AGH
  • Cherenkov Telescope Array Observatory gGmbH
  • Hiroshima University
  • Campus UAB
  • University of Adelaide
  • Aoyama Gakuin University
  • Sun Yat-Sen University

Research output: Contribution to journalArticlepeer-review

Abstract

A deep survey of the Large Magellanic Cloud at ∼0.1-100 TeV photon energies with the Cherenkov Telescope Array is planned. We assess the detection prospects based on a model for the emission of the galaxy, comprising the four known TeV emitters, mock populations of sources, and interstellar emission on galactic scales. We also assess the detectability of 30 Doradus and SN 1987A, and the constraints that can be derived on the nature of dark matter. The survey will allow for fine spectral studies of N 157B, N 132D, LMC P3, and 30 Doradus C, and half a dozen other sources should be revealed, mainly pulsar-powered objects. The remnant from SN 1987A could be detected if it produces cosmic-ray nuclei with a flat power-law spectrum at high energies, or with a steeper index 2.3-2.4 pending a flux increase by a factor of >3-4 over ∼2015-2035. Large-scale interstellar emission remains mostly out of reach of the survey if its >10 GeV spectrum has a soft photon index ∼2.7, but degree-scale 0.1-10 TeV pion-decay emission could be detected if the cosmic-ray spectrum hardens above >100 GeV. The 30 Doradus star-forming region is detectable if acceleration efficiency is on the order of 1−10 per cent of the mechanical luminosity and diffusion is suppressed by two orders of magnitude within <100 pc. Finally, the survey could probe the canonical velocity-averaged cross-section for self-annihilation of weakly interacting massive particles for cuspy Navarro-Frenk-White profiles.

Original languageEnglish
Pages (from-to)5353-5387
Number of pages35
JournalMonthly Notices of the Royal Astronomical Society
Volume523
Issue number4
DOIs
Publication statusPublished - 1 Aug 2023

Keywords

  • Magellanic Clouds
  • acceleration of particles
  • dark matter
  • gamma-rays: general

Fingerprint

Dive into the research topics of 'Sensitivity of the Cherenkov Telescope Array to TeV photon emission from the Large Magellanic Cloud'. Together they form a unique fingerprint.

Cite this