Galaxy clusters are expected to be both dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at γ-ray energies and are predicted to be sources of large-scale γ-ray emission due to hadronic interactions in the intracluster medium (ICM). In this paper, we estimate the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse γ-ray emission from the Perseus galaxy cluster. We first perform a detailed spatial and spectral modelling of the expected signal for both the DM and the CRp components. For each case, we compute the expected CTA sensitivity accounting for the CTA instrument response functions. The CTA observing strategy of the Perseus cluster is also discussed. In the absence of a diffuse signal (non-detection), CTA should constrain the CRp to thermal energy ratio X500 within the characteristic radius R500 down to about X500 < 3 × 10-3, for a spatial CRp distribution that follows the thermal gas and a CRp spectral index αCRp = 2.3. Under the optimistic assumption of a pure hadronic origin of the Perseus radio mini-halo and depending on the assumed magnetic field profile, CTA should measure αCRp down to about ΔαCRp ≃ 0.1 and the CRp spatial distribution with 10% precision, respectively. Regarding DM, CTA should improve the current ground-based γ-ray DM limits from clusters observations on the velocity-averaged annihilation cross-section by a factor of up to ∼ 5, depending on the modelling of DM halo substructure. In the case of decay of DM particles, CTA will explore a new region of the parameter space, reaching models with τχ > 1027 s for DM masses above 1 TeV. These constraints will provide unprecedented sensitivity to the physics of both CRp acceleration and transport at cluster scale and to TeV DM particle models, especially in the decay scenario.
Prospects for γ-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array / Abe, K.; Abe, S.; Acero, F.; Acharyya, A.; Adam, R.; Aguasca-Cabot, A.; Agudo, I.; Aguirre-Santaella, A.; Alfaro, J.; Alfaro, R.; Alvarez-Crespo, N.; Alves Batista, R.; Amans, J. -P.; Amato, E.; Angüner, E. O.; Antonelli, L. A.; Aramo, C.; Araya, M.; Arcaro, C.; Arrabito, L.; Asano, K.; Ascasíbar, Y.; Aschersleben, J.; Ashkar, H.; Augusto Stuani, L.; Baack, D.; Backes, M.; Baktash, A.; Balazs, C.; Balbo, M.; Ballester, O.; Baquero Larriva, A.; Barbosa Martins, V.; Barres de Almeida, U.; Barrio, J. A.; Batista, P. I.; Batkovic, I.; Batzofin, R.; Baxter, J.; Becerra González, J.; Beck, G.; Becker Tjus, J.; Benbow, W.; Bernete Medrano, J.; Bernlöhr, K.; Berti, A.; Bertucci, B.; Beshley, V.; Bhattacharjee, P.; Bhattacharyya, S.; Bi, B.; Biederbeck, N.; Biland, A.; Bissaldi, E.; Biteau, J.; Blanch, O.; Blazek, J.; Boisson, C.; Bolmont, J.; Bordas, P.; Bosnjak, Z.; Bottacini, E.; Bradascio, F.; Braiding, C.; Bronzini, E.; Brose, R.; Brown, A. M.; Brun, F.; Brunetti, G.; Bucciantini, N.; Bulgarelli, A.; Burelli, I.; Burmistrov, L.; Burton, M.; Bylund, T.; Calisse, P. G.; Campoy-Ordaz, A.; Cantlay, B. K.; Capalbi, M.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Caroff, S.; Carosi, R.; Carquin, E.; Carrasco, M. -S.; Cascone, E.; Cassol, F.; Castro-Tirado, A. J.; Cerasole, D.; Cerruti, M.; Chadwick, P.; Chaty, S.; Chen, A. W.; Chernyakova, M.; Chiavassa, A.; Chudoba, J.; Chytka, L.; Cifuentes, A.; Coimbra Araujo, C. H.; Conforti, V.; Conte, F.; Contreras, J. L.; Cortina, J.; Costa, A.; Costantini, H.; Cotter, G.; Cristofari, P.; Cuevas, O.; Curtis-Ginsberg, Z.; D'Amico, G.; D'Ammando, F.; Dalchenko, M.; Dazzi, F.; de Bony de Lavergne, M.; De Caprio, V.; De Frondat Laadim, F.; de Gouveia Dal Pino, E. M.; De Lotto, B.; De Lucia, M.; De Martino, D.; de Menezes, R.; de Naurois, M.; De Simone, N.; de Souza, V.; del Valle, M. V.; Delagnes, E.; Delgado Giler, A. G.; Delgado, C.; Dell'Aiera, M.; della Volpe, D.; Depaoli, D.; Di Girolamo, T.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Diebold, S.; Djannati-Ataï, A.; Djuvsland, J.; Dominik, R. M.; Donini, A.; Dorner, D.; Dörner, J.; Doro, M.; dos Anjos, R. D. C.; Dournaux, J. -L.; Duangchan, C.; Dubos, C.; Dumora, D.; Dwarkadas, V. V.; Ebr, J.; Eckner, C.; Egberts, K.; Einecke, S.; Elsässer, D.; Emery, G.; Escobar Godoy, M.; Escudero, J.; Esposito, P.; Ettori, S.; Evoli, C.; Falceta-Goncalves, D.; Fallah Ramazani, V.; Fattorini, A.; Faure, A.; Fedorova, E.; Fegan, S.; Feijen, K.; Feng, Q.; Ferrand, G.; Ferrarotto, F.; Fiandrini, E.; Fiasson, A.; Filipovic, M.; Fioretti, V.; Foffano, L.; Font Guiteras, L.; Fontaine, G.; Fröse, S.; Fukazawa, Y.; Fukui, Y.; Gaggero, D.; Galanti, G.; Gallozzi, S.; Gammaldi, V.; Garczarczyk, M.; Gasbarra, C.; Gasparrini, D.; Gaug, M.; Ghalumyan, A.; Gianotti, F.; Giarrusso, M.; Giesbrecht, J.; Giglietto, N.; Giordano, F.; Glicenstein, J. -F.; Göksu, H.; Goldoni, P.; González, J. M.; González, M. M.; Goulart Coelho, J.; Granot, J.; Grau, R.; Gréaux, L.; Green, D.; Green, J. G.; Grenier, I.; Grolleron, G.; Grube, J.; Gueta, O.; Hackfeld, J.; Hadasch, D.; Hamal, P.; Hanlon, W.; Hara, S.; Harvey, V. M.; Hassan, T.; Heckmann, L.; Heller, M.; Hernández Cadena, S.; Hervet, O.; Hie, J.; Hiroshima, N.; Hnatyk, B.; Hnatyk, R.; Hoang, J.; Hoffmann, D.; Hofmann, W.; Holder, J.; Horan, D.; Horvath, P.; Hrupec, D.; Hütten, M.; Iarlori, M.; Inada, T.; Incardona, F.; Inoue, S.; Iocco, F.; Iori, M.; Jamrozy, M.; Janecek, P.; Jankowsky, F.; Jarnot, C.; Jean, P.; Jiménez Martínez, I.; Jin, W.; Juramy-Gilles, C.; Jurysek, J.; Kagaya, M.; Kantzas, D.; Karas, V.; Katagiri, H.; Kataoka, J.; Kaufmann, S.; Kerszberg, D.; Khélifi, B.; Kissmann, R.; Kleiner, T.; Kluge, G.; Kluźniak, W.; Knödlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kornecki, P.; Kosack, K.; Kowal, G.; Kubo, H.; Kushida, J.; La Barbera, A.; La Palombara, N.; Láinez, M.; Lamastra, A.; Lapington, J.; Laporte, P.; Lazarević, S.; Leitgeb, F.; Lemoine-Goumard, M.; Lenain, J. -P.; Leone, F.; Leto, G.; Leuschner, F.; Lindfors, E.; Linhoff, M.; Liodakis, I.; Lombardi, S.; Longo, F.; López-Coto, R.; López-Moya, M.; López-Oramas, A.; Loporchio, S.; Luque-Escamilla, P. L.; Macias, O.; Mackey, J.; Majumdar, P.; Malyshev, D.; Mandat, D.; Manganaro, M.; Manicò, G.; Mariotti, M.; Markoff, S.; Márquez, I.; Marquez, P.; Marsella, G.; Martínez, G. A.; Martínez, M.; Martinez, O.; Marty, C.; Mas-Aguilar, A.; Mastropietro, M.; Maurin, G.; Mazin, D.; Melkumyan, D.; Mello, A. J. T. S.; Meunier, J. -L.; Meyer, D. M. -A.; Meyer, M.; Miceli, D.; Michailidis, M.; Michałowski, J.; Miener, T.; Miranda, J. M.; Mitchell, A.; Mizote, M.; Mizuno, T.; Moderski, R.; Molero, M.; Molfese, C.; Molina, E.; Montaruli, T.; Morcuende, D.; Morik, K.; Morlino, G.; Morselli, A.; Moulin, E.; Moya Zamanillo, V.; Munari, K.; Murach, T.; Muraczewski, A.; Muraishi, H.; Nagataki, S.; Nakamori, T.; Nemmen, R.; Neyroud, N.; Nickel, L.; Niemiec, J.; Nieto, D.; Nievas Rosillo, M.; Nikołajuk, M.; Nishijima, K.; Noda, K.; Nosek, D.; Novotny, V.; Nozaki, S.; O'Brien, P.; Ohishi, M.; Ohtani, Y.; Okumura, A.; Olive, J. -F.; Olmi, B.; Ong, R. A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, E.; Ostrowski, M.; Oya, I.; Pagliaro, A.; Palatiello, M.; Panebianco, G.; Paneque, D.; Pantaleo, F. R.; Paoletti, R.; Paredes, J. M.; Parmiggiani, N.; Patel, S. R.; Patricelli, B.; Pavlović, D.; Pech, M.; Pecimotika, M.; Pensec, U.; Peresano, M.; Pérez-Romero, J.; Peron, G.; Persic, M.; Petrucci, P. -O.; Petruk, O.; Piano, G.; Pierre, E.; Pietropaolo, E.; Pintore, F.; Pirola, G.; Pita, S.; Plard, C.; Podobnik, F.; Pohl, M.; Polo, M.; Pons, E.; Ponti, G.; Prandini, E.; Prast, J.; Principe, G.; Priyadarshi, C.; Produit, N.; Pueschel, E.; Pühlhofer, G.; Pumo, M. L.; Punch, M.; Queiroz, F.; Quirrenbach, A.; Rainò, S.; Rando, R.; Razzaque, S.; Recchia, S.; Regeard, M.; Reichherzer, P.; Reimer, A.; Reimer, O.; Reisenegger, A.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richtler, T.; Rico, J.; Rieger, F.; Righi, C.; Riitano, L.; Rizi, V.; Roache, E.; Rodriguez Fernandez, G.; Rodríguez-Vázquez, J. 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I.; Živec, M.; Zuriaga-Puig, J.; De la Torre Luque, P.; Null, Null; Null, Null; Null, Null. - In: JOURNAL OF COSMOLOGY AND ASTROPARTICLE PHYSICS. - ISSN 1475-7516. - 2024:10(2024). [10.1088/1475-7516/2024/10/004]
Prospects for γ-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array
Bissaldi, E.Membro del Collaboration Group
;Giglietto, N.Membro del Collaboration Group
;Loporchio, S.Membro del Collaboration Group
;Pantaleo, F. R.Membro del Collaboration Group
;
2024-01-01
Abstract
Galaxy clusters are expected to be both dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at γ-ray energies and are predicted to be sources of large-scale γ-ray emission due to hadronic interactions in the intracluster medium (ICM). In this paper, we estimate the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse γ-ray emission from the Perseus galaxy cluster. We first perform a detailed spatial and spectral modelling of the expected signal for both the DM and the CRp components. For each case, we compute the expected CTA sensitivity accounting for the CTA instrument response functions. The CTA observing strategy of the Perseus cluster is also discussed. In the absence of a diffuse signal (non-detection), CTA should constrain the CRp to thermal energy ratio X500 within the characteristic radius R500 down to about X500 < 3 × 10-3, for a spatial CRp distribution that follows the thermal gas and a CRp spectral index αCRp = 2.3. Under the optimistic assumption of a pure hadronic origin of the Perseus radio mini-halo and depending on the assumed magnetic field profile, CTA should measure αCRp down to about ΔαCRp ≃ 0.1 and the CRp spatial distribution with 10% precision, respectively. Regarding DM, CTA should improve the current ground-based γ-ray DM limits from clusters observations on the velocity-averaged annihilation cross-section by a factor of up to ∼ 5, depending on the modelling of DM halo substructure. In the case of decay of DM particles, CTA will explore a new region of the parameter space, reaching models with τχ > 1027 s for DM masses above 1 TeV. These constraints will provide unprecedented sensitivity to the physics of both CRp acceleration and transport at cluster scale and to TeV DM particle models, especially in the decay scenario.I documenti in IRIS sono protetti da copyright e tutti i diritti sono riservati, salvo diversa indicazione.
