A1 Vertaisarvioitu alkuperäisartikkeli tieteellisessä lehdessä
Prospects for a survey of the galactic plane with the Cherenkov Telescope Array
Tekijät: Abe, S.; Abhir, J.; Abhishek, A.; Acero, F.; Acharyya, A.; Adam, R.; Aguasca-Cabot, A.; Agudo, I.; Aguirre-Santaella, A.; Alfaro, J.; Alvarez-Crespo, N.; Batista, R.A.; Amans, J.P.; Amato, E.; Ambrosi, G.; Ambrosino, F.; Angüner, E.O.; Aramo, C.; Arcaro, C.; Arrabito, L.; Asano, K.; Ascasíbar, Y.; Aschersleben, J.; Stuani, L.A.; Backes, M.; Balazs, C.; Balbo, M.; Ballet, J.; Larriva, A.B.; Martins, V.B.; de Almeida, U.B.; Barrio, J.A.; Batković, I.; Batzofin, R.; Baxter, J.; González, J.B.; Beck, G.; Beiske, L.; Belmont, R.; Benbow, W.; Bernardini, E.; Bernete, 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.; Bocchino, F.; Boisson, C.; Bolmont, J.; Arbeletche, L.B.; Bonnoli, G.; Bonollo, A.; Bordas, P.; Bosnjak, Z.; Bottacini, E.; Braiding, C.; Bronzini, E.; Brose, R.; Brown, A.M.; Brun, F.; Brunelli, G.; Bucciantini, N.; Bulgarelli, A.; Burelli, I.; Burmistrov, L.; Burton, M.; Burtovoi, A.; Bylund, T.; Calisse, P.G.; Campoy-Ordaz, A.; Cantlay, B.K.; Caproni, A.; Capuzzo-Dolcetta, R.; Caraveo, P.; Caroff, S.; Carosi, A.; Carosi, R.; Carquin, E.; Carrasco, M.S.; Cascone, E.; Cassol, F.; Castrejon, N.; Castro-Tirado, A.J.; Cerasole, D.; Cerruti, M.; Chadwick, P.M.; Chambery, P.; Chaty, S.; Chen, A.W.; Chernyakova, M.; Chiavassa, A.; Chytka, L.; Cifuentes, A.; Araujo, C.H.C.; Conforti, V.; Conte, F.; Contreras, J.L.; Cortina, J.; Costa, A.; Costantini, H.; Cotter, G.; Crestan, S.; Cristofari, P.; Cuevas, O.; Curtis-Ginsberg, Z.; D’Aì, A.; D’Amico, G.; D’Ammando, F.; Dadina, M.; Dalchenko, M.; David, L.; 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 Ona Wilhelmi, E.; de Souza, V.; del Peral, L.; Giler, A.G.D.; Delgado, C.; Dell’aiera, M.; Della Valle, M.; della Volpe, D.; Depaoli, D.; Di Girolamo, T.; Di Piano, A.; Di Pierro, F.; Di Tria, R.; Di Venere, L.; Díaz, C.; Diebold, S.; Dinesh, A.; Djannati-Ataï, A.; Djuvsland, J.; Domínguez, A.; Dominik, R.M.; Donini, A.; Dörner, J.; Doro, M.; dos Anjos, R.D.C.; Dournaux, J.L.; Duangchan, C.; Dubos, C.; Dubus, G.; Duffy, S.; Dumora, D.; Dwarkadas, V.V.; Ebr, J.; Eckner, C.; Egberts, K.; Einecke, S.; Elsässer, D.; Emery, G.; Errando, M.; Escanuela, C.; Escarate, P.; Godoy, M.E.; Escudero, J.; Esposito, P.; Evoli, C.; Falceta-Goncalves, D.; Fattorini, A.; Fegan, S.; Feijen, K.; Feng, Q.; Ferrand, G.; Ferrarotto, F.; Fiandrini, E.; Fiasson, A.; Filipovic, M.; Fioretti, V.; Fiori, M.; Flores, H.; Foffano, L.; Guiteras, L.F.; Fontaine, G.; Fröse, S.; Fukazawa, Y.; Fukui, Y.; Funk, S.; Furniss, A.; Gaggero, D.; Galanti, G.; Galaz, G.; Gallant, Y.A.; Gallozzi, S.; Gammaldi, V.; Garczarczyk, M.; Gasbarra, C.; Gasparrini, D.; Gaug, M.; Ghalumyan, A.; Giarrusso, M.; Giesbrecht, J.; Giglietto, N.; Giordano, F.; Giuffrida, R.; Giuliani, A.; Glicenstein, J.F.; Glombitza, J.; Godinovic, N.; Goldoni, P.; González, J.M.; Coelho, J.G.; Granot, J.; Grasso, D.; Grau, R.; Gréaux, L.; Green, D.; Green, J.G.; Greenshaw, T.; Grenier, I.; Grolleron, G.; Grondin, M.H.; Gueta, O.; Gunji, S.; Hackfeld, J.; Hadasch, D.; Hanlon, W.; Hara, S.; Harvey, V.M.; Hassan, T.; Hayashi, K.; Heckmann, L.; Heller, M.; Hermann, G.; Cadena, S.H.; Hervet, O.; Hinton, J.; Hiroshima, N.; Hnatyk, B.; Hnatyk, R.; Hofmann, W.; Holder, J.; Holler, M.; Horan, D.; Horvath, P.; Hovatta, T.; Hrabovsky, M.; Iarlori, M.; Inada, T.; Incardona, F.; Inoue, S.; Iocco, F.; Iori, M.; Jamrozy, M.; Janecek, P.; Jankowsky, F.; Jarnot, C.; Jean, P.; Martínez, I.J.; Jin, W.; Juramy-Gilles, C.; Jurysek, J.; Kagaya, M.; Kalekin, O.; Kantzas, D.; Karas, V.; Katagiri, H.; Kataoka, J.; Kaufmann, S.; Kazanas, D.; Kerszberg, D.; Khélifi, B.; Kieda, D.B.; Kissmann, R.; Kleiner, T.; Kluge, G.; Kluźniak, W.; Knödlseder, J.; Kobayashi, Y.; Kohri, K.; Komin, N.; Kornecki, P.; Kosack, K.; Kostunin, D.; Kowal, G.; Kubo, H.; Kushida, J.; La Barbera, A.; La Palombara, N.; Láinez, M.; Lamastra, A.; Lapington, J.; Laporte, P.; Lazarević, S.; Lazendic-Galloway, J.; 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.; Bahilo, J.L.; Lucarelli, F.; Luque-Escamilla, P.L.; Lyard, E.; Macias, O.; Mackey, J.; Maier, G.; Malyshev, D.; Mandat, D.; Manicò, G.; Marcowith, A.; Marinos, P.; Mariotti, M.; Markoff, S.; Marquez, P.; Marsella, G.; Martí, J.; Martin, P.; Martínez, G.A.; Martínez, M.; Martinez, O.; Marty, C.; Mas-Aguilar, A.; Mastropietro, M.; Maurin, G.; Mazin, D.; McKeague, S.; Mello, A.J.T.S.; Menchiari, S.; Mereghetti, S.; Mestre, E.; Meunier, J.L.; Meyer, D.M.A.; Miceli, D.; Miceli, M.; Michailidis, M.; Michałowski, J.; Miener, T.; Miranda, J.M.; Mitchell, A.; Mizuno, T.; Moderski, R.; Mohrmann, L.; Molero, M.; Molfese, C.; Molina, E.; Montaruli, T.; Moralejo, A.; Morcuende, D.; Morik, K.; Morlino, G.; Morselli, A.; Moulin, E.; Zamanillo, V.M.; Mukherjee, R.; Munari, K.; Murach, T.; Muraczewski, A.; Muraishi, H.; Nagataki, S.; Nakamori, T.; Nemmen, R.; Nickel, L.; Niemiec, J.; Nieto, D.; Rosillo, M.N.; Nikołajuk, M.; Nikolić, L.; Noda, K.; Nosek, D.; Novosyadlyj, B.; Novotny, V.; Nozaki, S.; Ohishi, M.; Ohtani, Y.; Okumura, A.; Olive, J.F.; Olmi, B.; Ong, R.A.; Orienti, M.; Orito, R.; Orlandini, M.; Orlando, E.; Orlando, S.; Ostrowski, M.; Oya, I.; Pagano, 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.; Peresano, M.; Pérez-Romero, J.; Pérez-Torres, M.A.; Peron, G.; Persic, M.; Petrucci, P.O.; Petruk, O.; Piano, G.; Pierre, E.; Pietropaolo, E.; Pihet, M.; Pintore, F.; Pittori, C.; Plard, C.; Podobnik, F.; Pohl, M.; Pons, E.; Ponti, G.; Prandini, E.; Principe, G.; Priyadarshi, C.; Produit, N.; Prokhorov, D.; Pueschel, E.; Pühlhofer, G.; Pumo, M.L.; Punch, M.; Queiroz, F.; Quirrenbach, A.; Rando, R.; Ravel, T.; Razzaque, S.; Regeard, M.; Reichherzer, P.; Reimer, A.; Reimer, O.; Remy, Q.; Renaud, M.; Reposeur, T.; Rhode, W.; Ribeiro, D.; Ribó, M.; Richtler, T.; Rico, J.; Rieger, F.; Rigoselli, M.; Rizi, V.; Roache, E.; Fernandez, G.R.; Rodríguez-Vázquez, J.J.; Romano, P.; Romeo, G.; Rosado, J.; de Leon, A.R.; Rowell, G.; Rudak, B.; Ruiter, A.J.; Rulten, C.B.; Russo, F.; Sadeh, I.; Saha, L.; Saito, T.; Salzmann, H.; Sánchez-Conde, M.; Sangiorgi, P.; Sano, H.; Santander, M.; Santangelo, A.; Santos-Lima, R.; Sapienza, V.; Šarić, T.; Sarkar, S.; Saturni, F.G.; Scherer, A.; Schiavone, F.; Schipani, P.; Schleicher, B.; Schovanek, P.; Schubert, J.L.; Schussler, F.; Schwanke, U.; Schwefer, G.; Arroyo, M.S.; Seitenzahl, I.; Sergijenko, O.; Servillat, M.; Sguera, V.; Sharma, P.; Siejkowski, H.; Siqueira, C.; Sizun, P.; Sliusar, V.; Slowikowska, A.; Sol, H.; Spencer, S.T.; Spiga, D.; Stamerra, A.; Stanič, S.; Starling, R.; Stawarz, Ł.; Steinmassl, S.; Steppa, C.; Stolarczyk, T.; Suda, Y.; Suomijärvi, T.; Tajima, H.; Takeishi, R.; Tanaka, S.J.; Tavecchio, F.; Tavernier, T.; Terada, Y.; Terrier, R.; Teshima, M.; Tian, W.W.; Tibaldo, L.; Tibolla, O.; Torradeflot, F.; Torres, D.F.; Tothill, N.; Toussenel, F.; Touzard, V.; Travnicek, P.; Tripodo, G.; Trois, A.; Tsiahina, A.; Tutone, A.; Umana, G.; Vaclavek, L.; Vacula, M.; Vallania, P.; van Eldik, C.; Vassiliev, V.; Acosta, M.L.V.; Vecchi, M.; Ventura, S.; Vercellone, S.; Verna, G.; Viana, A.; Viaux, N.; Vigliano, A.; Vignatti, J.; Vigorito, C.F.; Villanueva, J.; Vink, J.; Vitale, V.; Vodeb, V.; Voisin, V.; Vorobiov, S.; Voutsinas, G.; Vovk, I.; Vuillaume, T.; Waegebaert, V.; Wagner, S.J.; Walter, R.; Wechakama, M.; White, R.; Wierzcholska, A.; Williams, D.A.; Wohlleben, F.; Yamazaki, R.; Yang, L.; Yoshida, T.; Yoshikoshi, T.; Zacharias, M.; Zaharijas, G.; Zampieri, L.; Zanin, R.; Zavrtanik, D.; Zavrtanik, M.; Zdziarski, A.A.; Zech, A.; Zhdanov, V.I.; Ziętara, K.; Živec, M.; Zuriaga-Puig, J.; De la Torre Luque, P.; Guillemot, L.; Smith, D.A.; and The CTA Consortium
Kustantaja: IOP Publishing
Julkaisuvuosi: 2024
Journal: Journal of Cosmology and Astroparticle Physics
Tietokannassa oleva lehden nimi: Journal of Cosmology and Astroparticle Physics
Artikkelin numero: 081
Vuosikerta: 2024
Numero: 10
eISSN: 1475-7516
DOI: https://doi.org/10.1088/1475-7516/2024/10/081
Verkko-osoite: https://doi.org/10.1088/1475-7516/2024/10/081
Rinnakkaistallenteen osoite: https://research.utu.fi/converis/portal/detail/Publication/477083037
Approximately one hundred sources of very-high-energy (VHE) gamma rays are known in the Milky Way, detected with a combination of targeted observations and surveys. A survey of the entire Galactic Plane in the energy range from a few tens of GeV to a few hundred TeV has been proposed as a Key Science Project for the upcoming Cherenkov Telescope Array Observatory (CTAO). This article presents the status of the studies towards the Galactic Plane Survey (GPS). We build and make publicly available a sky model that combines data from recent observations of known gamma-ray emitters with state-of-the-art physically-driven models of synthetic populations of the three main classes of established Galactic VHE sources (pulsar wind nebulae, young and interacting supernova remnants, and compact binary systems), as well as of interstellar emission from cosmic-ray interactions in the Milky Way. We also perform an optimisation of the observation strategy (pointing pattern and scheduling) based on recent estimations of the instrument performance. We use the improved sky model and observation strategy to simulate GPS data corresponding to a total observation time of 1620 hours spread over ten years. Data are then analysed using the methods and software tools under development for real data. Under our model assumptions and for the realisation considered, we show that the GPS has the potential to increase the number of known Galactic VHE emitters by almost a factor of five. This corresponds to the detection of more than two hundred pulsar wind nebulae and a few tens of supernova remnants at average integral fluxes one order of magnitude lower than in the existing sample above 1 TeV, therefore opening the possibility to perform unprecedented population studies. The GPS also has the potential to provide new VHE detections of binary systems and pulsars, to confirm the existence of a hypothetical population of gamma-ray pulsars with an additional TeV emission component, and to detect bright sources capable of accelerating particles to PeV energies (PeVatrons). Furthermore, the GPS will constitute a pathfinder for deeper follow-up observations of these source classes. Finally, we show that we can extract from GPS data an estimate of the contribution to diffuse emission from unresolved sources, and that there are good prospects of detecting interstellar emission and statistically distinguishing different scenarios. Thus, a survey of the entire Galactic plane carried out from both hemispheres with CTAO will ensure a transformational advance in our knowledge of Galactic VHE source populations and interstellar emission.
Ladattava julkaisu This is an electronic reprint of the original article. |  |
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We gratefully acknowledge financial support from the following agencies and organisations: 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), Fundação de Apoio à Ciência, Tecnologia e Inovação do Paraná — Fundação Araucária, 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, W.M. gratefully acknowledges support by the ANID BASAL projects ACE210002 and FB210003, and FONDECYT 11190853; 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, 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; The German Ministry for Education and Research (BMBF), the Max Planck Society, the German Research Foundation (DFG, with Collaborative Research Centres 876 & 1491), and the 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 the government budget lines PGE2021/28.06.000X.411.01, PGE2022/28.06.000X.411.01 and PGE2022/28.06.000X.711.04, and grants PID2022-139117NB-C44, PID2019-104114RBC31, PID2019-107847RB-C44, PID2019-104114RB-C32, PID2019-105510GB-C31, PID2019- 104114RB-C33, PID2019-107847RB-C41, PID2019-107847RB-C43, PID2019-107847RB-C42, PID2019-107988GB-C22, PID2021-124581OB-I00, PID2021-125331NB-I00; the “Centro de Excelencia Severo Ochoa” program through grants no. CEX2019-000920-S, CEX2020-001007- S, CEX2021-001131-S; the “Unidad de Excelencia María de Maeztu” program through grants no. CEX2019-000918-M, CEX2020-001058-M; the “Ramón y Cajal” program through grants RYC2021-032552-I, RYC2021-032991-I, RYC2020-028639-I and RYC-2017-22665; the “Juan de la Cierva-Incorporación” program through grants no. IJC2018-037195-I, IJC2019-040315-I. They also acknowledge the “Atracción de Talento” program of Comunidad de Madrid through grant no. 2019-T2/TIC-12900; the project “Tecnologiás avanzadas para la exploracioń del universo y sus componentes” (PR47/21 TAU), funded by Comunidad de Madrid, by the Recovery, Transformation and Resilience Plan from the Spanish State, and by NextGenerationEU from the European Union through the Recovery and Resilience Facility; the La Caixa Banking Foundation, grant no. LCF/BQ/PI21/11830030; 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 “CERCA” program and the grant 2021SGR00426, both funded by the Generalitat de Catalunya; and the European Union’s Horizon 2020 GA:824064 and NextGenerationEU (PRTR-C17.I1); 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 Society, Science and Technology Facilities Council, U.K.; 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, V.V.D. is funded by NSF grant AST-1911061, Washington University McDonnell Center for the Space Sciences, The University of Wisconsin and the Wisconsin Alumni Research Foundation, U.S.A.. 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.
