Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants
Creators: name: Acero, F.
name: Acharyya, A.
name: Adam, R.
name: Aguasca-Cabot, A.
name: Agudo, I.
name: Aguirre-Santaella, A.
name: Alfaro, J.
name: Aloisio, R.
name: Crespo, N. Álvarez
name: Alves Batista, R.
name: Amati, L.
name: Amato, E.
name: Ambrosi, G.
name: Angüner, E. O.
name: Aramo, C.
name: Arcaro, C.
name: Armstrong, T.
name: Asano, K.
name: Ascasibar, Y.
name: Aschersleben, J.
name: Backes, M.
name: Baktash, A.
name: Balazs, C.
name: Balbo, M.
name: Ballet, J.
name: Larriva, A. Baquero
name: Barbosa Martins, V.
name: de Almeida, U. Barres
name: Barrio, J. A.
name: Bastieri, D.
name: Baxter, J. R.
name: Becker Tjus, J.
name: Benbow, W.
name: Bernardos-Martín, M. I.
name: Bernete, J.
name: Berti, A.
name: Bertucci, B.
name: Beshley, V.
name: Bhattacharjee, P.
name: Bhattacharyya, S.
name: Biland, A.
name: Bissaldi, E.
name: Biteau, J.
name: Blanch, O.
name: Bordas, P.
name: Bottacini, E.
name: Bregeon, J.
name: Brose, R.
name: Bucciantini, N.
name: Bulgarelli, A.
name: Capasso, M.
name: Dolcetta, R. A. Capuzzo
name: Caraveo, P.
name: Cardillo, M.
name: Carosi, R.
name: Casanova, S.
name: Cascone, E.
name: Cassol, F.
name: Catalani, F.
name: Cerruti, M.
name: Chadwick, P.
name: Chaty, S.
name: Chen, A.
name: Chernyakova, M.
name: Chiavassa, A.
name: Chudoba, J.
name: Coimbra-Araujo, C.
name: Conforti, V.
name: Contreras, J. L.
name: Costa, A.
name: Costantini, H.
name: Cristofari, P.
name: Crocker, R.
name: D'Amico, G.
name: D'Ammando, F.
name: De Angelis, A.
name: De Caprio, V.
name: de Gouveia Dal Pino, E. M.
name: de Ona Wilhelmi, E.
name: de Souza, V.
name: Delgado, C.
name: della Volpe, D.
name: Depaoli, D.
name: Di Girolamo, T.
name: Di Pierro, F.
name: Di Tria, R.
name: Di Venere, L.
name: Diebold, S.
name: Djuvsland, J. I.
name: Donini, A.
name: Doro, M.
name: Anjos, R. d. C. Dos
name: Dwarkadas, V. V.
name: Einecke, S.
name: Elsässer, D.
name: Emery, G.
name: Evoli, C.
name: Falceta-Goncalves, D.
name: Fedorova, E.
name: Fegan, S.
name: Ferrand, G.
name: Fiandrini, E.
name: Filipovic, M.
name: Fioretti, V.
name: Fiori, M.
name: Foffano, L.
name: Fontaine, G.
name: Fukami, S.
name: Galanti, G.
name: Galaz, G.
name: Gammaldi, V.
name: Gasbarra, C.
name: Ghalumyan, A.
name: Ghirlanda, G.
name: Giarrusso, M.
name: Giavitto, G.
name: Giglietto, N.
name: Giordano, F.
name: Giroletti, M.
name: Giuliani, A.
name: Giunti, L.
name: Godinovic, N.
name: Coelho, J. Goulart
name: Gréaux, L.
name: Green, D.
name: Grondin, M.-H.
name: Gueta, O.
name: Gunji, S.
name: Hassan, T.
name: Heller, M.
name: Hernández-Cadena, S.
name: Hinton, J.
name: Hnatyk, B.
name: Hnatyk, R.
name: Hoffmann, D.
name: Hofmann, W.
name: Holder, J.
name: Horan, D.
name: Horvath, P.
name: Hrabovsky, M.
name: Hrupec, D.
name: Inada, T.
name: Incardona, F.
name: Inoue, S.
name: Ishio, K.
name: Jamrozy, M.
name: Janecek, P.
name: Martínez, I. Jiménez
name: Jin, W.
name: Jung-Richardt, I.
name: Jurysek, J.
name: Kaaret, P.
name: Karas, V.
name: Katz, U.
name: Kerszberg, D.
name: Khélifi, B.
name: Kieda, D. B.
name: Kissmann, R.
name: Kleiner, T.
name: Kluge, G.
name: Kluzniak, W.
name: Knödlseder, J.
name: Kobayashi, Y.
name: Kohri, K.
name: Komin, N.
name: Kornecki, P.
name: Kubo, H.
name: La Palombara, N.
name: Láinez, M.
name: Lamastra, A.
name: Lapington, J.
name: Lemoine-Goumard, M.
name: Lenain, J.-P.
name: Leone, F.
name: Leto, G.
name: Leuschner, F.
name: Lindfors, E.
name: Liodakis, I.
name: Lohse, T.
name: Lombardi, S.
name: Longo, F.
name: López-Coto, R.
name: López-Moya, M.
name: López-Oramas, A.
name: Loporchio, S.
name: Luque-Escamilla, P. L.
name: Macias, O.
name: Mackey, J.
name: Majumdar, P.
name: Mandat, D.
name: Manganaro, M.
name: Manicò, G.
name: Marconi, M.
name: Martí, J.
name: Martínez, G.
name: Martinez, M.
name: Martinez, O.
name: Mello, A. J. T. S.
name: Menchiari, S.
name: Meyer, D. M.-A.
name: Micanovic, S.
name: Miceli, D.
name: Miceli, M.
name: Michalowski, J.
name: Miener, T.
name: Miranda, J. M.
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name: Mode, B.
name: Moderski, R.
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name: Montaruli, T.
name: Morcuende, D.
name: Morlino, G.
name: Morselli, A.
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name: Nievas Rosillo, M.
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name: Novosyadlyj, B.
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name: Ohm, S.
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name: Okumura, A.
name: Olmi, B.
name: Ong, R. A.
name: Orienti, M.
name: Orito, R.
name: Orlandini, M.
name: Orlando, E.
name: Orlando, S.
name: Ostrowski, M.
name: Oya, I.
name: Pantaleo, F. R.
name: Paredes, J. M.
name: Patricelli, B.
name: Pecimotika, M.
name: Peresano, M.
name: Pérez-Romero, J.
name: Persic, M.
name: Petruk, O.
name: Piano, G.
name: Pietropaolo, E.
name: Pirola, G.
name: Pittori, C.
name: Pohl, Martin
name: Ponti, G.
name: Prandini, E.
name: Principe, G.
name: Priyadarshi, C.
name: Pueschel, E.
name: Pühlhofer, G.
name: Pumo, M. L.
name: Quirrenbach, A.
name: Rando, R.
name: Razzaque, S.
name: Reichherzer, P.
name: Reimer, A.
name: Reimer, O.
name: Renaud, M.
name: Reposeur, T.
name: Ribó, M.
name: Richtler, T.
name: Rico, J.
name: Rieger, F.
name: Rigoselli, M.
name: Riitano, L.
name: Rizi, V.
name: Roache, E.
name: Romano, P.
name: Romeo, G.
name: Rosado, J.
name: Rowell, G.
name: Rudak, B.
name: Sadeh, I.
name: Safi-Harb, S.
name: Saha, L.
name: Sailer, S.
name: Sánchez-Conde, M.
name: Sarkar, S.
name: Satalecka, K.
name: Saturni, F. G.
name: Scherer, A.
name: Schovánek, P.
name: Schussler, F.
name: Schwanke, U.
name: Scuderi, S.
name: Seglar-Arroyo, M.
name: Sergijenko, O.
name: Servillat, M.
name: Shang, R.-Y.
name: Sharma, P.
name: Siejkowski, H.
name: Sliusar, V.
name: Słowikowska, A.
name: Sol, H.
name: Specovius, A.
name: Spencer, S. T.
name: Spengler, G.
name: Stamerra, A.
name: Stanič, S.
name: Starecki, T.
name: Starling, R.
name: Stolarczyk, T.
name: Pereira, L. A. Stuani
name: Suda, Y.
name: Suomijarvi, T.
name: Sushch, I.
name: Tajima, H.
name: Tam, P.-H. T.
name: Tanaka, S. J.
name: Tavecchio, F.
name: Testa, V.
name: Tian, W.
name: Tibaldo, L.
name: Torres, D. F.
name: Tothill, N.
name: Vallage, B.
name: Vallania, P.
name: van Eldik, C.
name: van Scherpenberg, J.
name: Vandenbroucke, J.
name: Vazquez Acosta, M.
name: Vecchi, M.
name: Vercellone, S.
name: Verna, G.
name: Viana, A.
name: Vignatti, J.
name: Vitale, V.
name: Vodeb, V.
name: Vorobiov, S.
name: Vuillaume, T.
name: Wagner, S. J.
name: Walter, R.
name: White, M.
name: Wierzcholska, A.
name: Will, M.
name: Williams, D.
name: Yang, L.
name: Yoshida, T.
name: Yoshikoshi, T.
name: Zaharijas, G.
name: Zampieri, L.
name: Zavrtanik, D.
name: Zavrtanik, M.
name: Zhdanov, V. I.
name: Z̆ivec, M.
name: Cherenkov Telescope Array Collaboration
Publisher: name: Deutsches Elektronen-Synchrotron, DESY, Hamburg
Year: 2023
Subjects: subject: 540
subject: emission: spectrum
subject: Cherenkov Telescope Array
subject: galaxy
subject: spectral
subject: signature
subject: supernova
subject: observatory
subject: energy spectrum
subject: sensitivity
subject: cosmic radiation
subject: statistical
subject: VHE
subject: hadron
subject: Gamma rays: general
subject: Cosmic rays
subject: Galactic PeVatrons
subject: (Stars:) supernovae: general
subject: Methods: data analysis
subject: Methods: statistical

description: The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3 PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The potential to search for hadronic PeVatrons with the Cherenkov Telescope Array (CTA) is assessed. The focus is on the usage of very high energy γ-ray spectral signatures for the identification of PeVatrons. Assuming that SNRs can accelerate CRs up to knee energies, the number of Galactic SNRs which can be identified as PeVatrons with CTA is estimated within a model for the evolution of SNRs. Additionally, the potential of a follow-up observation strategy under moonlight conditions for PeVatron searches is investigated. Statistical methods for the identification of PeVatrons are introduced, and realistic Monte-Carlo simulations of the response of the CTA observatory to the emission spectra from hadronic PeVatrons are performed. Based on simulations of a simplified model for the evolution for SNRs, the detection of a γ-ray signal from in average 9 Galactic PeVatron SNRs is expected to result from the scan of the Galactic plane with CTA after 10 h of exposure. CTA is also shown to have excellent potential to confirm these sources as PeVatrons in deep observations with O(100) hours of exposure per source.