Design concepts for the Cherenkov Telescope Array CTA: an advanced facility for ground-based high-energy gamma-ray astronomy

Actis, Marcos Daniel; Agnetta, G.; Aharonian, F.; Akhperjanian, A. G.; Aleksić, J.; Aliu, E.; Allan, Dan; Allekotte, I.; Antico, F.C.; Antonelli, L. A.; Antoranz, P.; Aravantinos, A.; Arlen, T.; Arnaldi, L. H.; Artmann, S.; Asano, Katsuaki; Asorey, H.; Bähr, J.; Bais, A. F.; Baixeras, C.; Bajtlik, Stanisław; Balis, D.; Bamba, Aya; Barbier, C.; Barceló, M.; Barnacka, A.; Barnstedt, J.; Almeida, U. Barres de; Barrio, J. A.; Basso, S.; Bastieri, D.; Bauer, C.; Becerra, J.; Becherini, Y.; Bechtol, K.; Becker, J.; Beckmann, V.; Bednarek, W.; Behera, B.; Beilicke, M.; Belluso, M.; Benallou, M.; Benbow, W.; Berdugo, J.; Berger, K.; Bernardino, T.; Bernlöhr, K.; Biland, A.; Billotta, S.; Bird, T.; Birsin, E.; Bissaldi, E.; Blake, Simon; Blanch, O.; Bobkov, A.; Bogacz, L.; Bogdan, M.; Boisson, C.; Boix, J.; Bolmont, J.; Bonanno, G.; Bonardi, A.; Bonev, T.; Borkowski, J.; Botner, O.; Bottani, A.; Bourgeat, M.; Boutonnet, C.; Bouvier, A.; Brau-Nogué, Sylvie; Braun, I.; Bretz, T.; Briggs, M. S.; Brun, P.; Brunetti, L.; Buckley, J. H.; Bugaev, V.; Bühler, R.; Bulik, T.; Busetto, G.; Buson, S.; Byrum, K.; Cailles, M.; Cameron, R. A.; Canestrari, R.; Cantu, Sarah; Carmona, E.; Carosi, A.; Carr, J.; Carton, Pierre-Henri; Casiraghi, Margherita; Castarede, H.; Catalano, O.; Cavazzani, Stefano; Cazaux, S.; Cerruti, B.; Cerruti, M.; Chadwick, P. M.; Chiang, J.; Chikawa, M.; Cieślar, M.; Ciesielska, M.; Cillis, A.; Clerc, C.; Colin, P.; Colomé, J.; Compin, M.; Conconi, P.; Connaughton, V.; Conrad, J.; Contreras, J. L.; Coppi, P.; Corlier, M.; Corona, P.; Corpace, O.; Corti, Daniele; Cortina, J.; Costantini, H.; Cotter, Garret; Courty, B.; Couturier, Stefan; Covino, S.; Croston, J. H.; Cusumano, G.; Daniel, M. K.; Dazzi, F.; Angelis, A. De; Pozo, E. De Cea del; Pino, E. M. de Gouveia Dal; Jager, O. de; Pérez, I. de la Calle; Vega, G. De La; Lotto, B. De; Naurois, M. de; Wilhelmi, E. de Oña; Souza, V. de; Decerprit, B.; Deil, C.; Delagnes, É.; Deleglise, Guillaume; Mendez, C. Delgado; Dettlaff, T.; Paolo, A. Di; Pierro, F. Di; Díaz, C.; Dick, J.; Dickinson, H. J.; Digel, S. W.; Dimitrov, D.; Disset, G.; Djannati‐Ataï, A.; Doert, M.; Domainko, W.; Dorner, D.; Doro, M.; Dournaux, J.-L.; Dravins, Dainis; Drury, L. O’c.; Dubois, F.; Dubois, R.; Dubus, G.; Dufour, C.; Durand, Dominique; Dyks, J.; Dyrda, M.; Edy, Evelyne; Egberts, K.; Eleftheriadis, C.; Elles, S.; Emmanoulopoulos, D.; Enomoto, R.; Ernenwein, Jean-Pierre; Errando, M.; Etchegoyen, A.; Falcone, A.; Farakos, K.; Farnier, C.; Federici, S.; Feinstein, F.; Ferenc, D.; Fillin-Martino, E.; Fink, David J.; Finley, C.; Finley, J. P.; Firpo, R.; Florin, D.; Föhr, C.; Fokitis, E.; Font, Ll.; Fontaine, G.; Fontana, A.; Förster, A.; Fortson, L.; Fouque, N.; Fransson, Claes; Fraser, G. W.; Fresnillo, L.; Fruck, C.; Fujita, Yutaka; Fukazawa, Yasushi; Funk, S.; Gäbele, W.; Gabici, S.; Gadola, A.; Galante, N.; Gallant, Y. A.; García, Beatriz; López, R. J. García; Garrido, Daniel; Garrido, L.; Gascón, D.; Gasq, C.; Gaug, M.; Gaweda, J.; Geffroy, N.; Ghag, C.; Ghedina, A.; Ghigo, M.; Gianakaki, E.; Giarrusso, S.; Giavitto, G.; Giebels, B.; Giro, E.; Giubilato, P.; Glanzman, T.; Glicenstein, J.-F.; Gochna, M.; Golev, V.; Berisso, M. Gómez; González, Antonio J.; González, F.; Grañena, F.; Graciani, R.; Granot, Jonathan; Gredig, R.; Green, A.; Greenshaw, T.; Grimm, O.; Grube, J.; Grudzińska, M.; Grygorczuk, J.; Guarino, V. J.; Guglielmi, L.; Guilloux, F.; Gunji, S.; Gyuk, G.; Hadasch, D.; Haefner, Dennis; Hagiwara, Rika; Hahn, Joachim; Hallgren, A.; Hara, Shinji; Hardcastle, M. J.; Hassan, Tarek; Haubold, T.; Hauser, M.; Hayashida, M.; Heller, René; Henri, G.; Hermann, G.; Herrero, A.; Hinton, J. A.; Hoffmann, D.; Hofmann, W.; Hofverberg, P.; Horns, D.; Hrupec, Dario; Huan, Hao; Huber, Bernhard A.; Huet, Jean-Michel; Hughes, G.; Hultquist, K.; Humensky, T. B.; Huppert, J.-F.; Ibarra, A.; Illa, J. M.; Ingjald, Johan; Inoue, Yoshiyuki; Inoue, Susumu; Ioka, Kunihito; Jablonski, C.; Jachołkowska, A.; Janiak, M.; Jean, P.; Jensen, Hannes; Jogler, T.; Jung, I.; Kaaret, Philip; Kabuki, S.; Kakuwa, Jun; Kalkuhl, C.; Kankanyan, R.; Kapala, Maria; Karastergiou, A.; Karczewski, M.; Karkar, S.; Karlsson, N.; Kasperek, J.; Katagiri, H.; Katarzyński, K.; Kawanaka, Norita; Kȩdziora, B.; Kendziorra, E.; Khélifi, B.; Kieda, D.; Kifune, T.; Kihm, T.; Klepser, S.; Kluźniak, W.; Knapp, J.; Knappy, A. R.; Kneiske, T.; Knödlseder, J.; Köck, F.; Kodani, K.; Kohri, Kazunori; Kokkotas, Kostas D.; Komin, Nu.; Konopelko, A.; Kosack, K.; Kossakowski, R.; Kostka, P.; Kotuła, J.; Kowal, Grzegorz; Kozioł, J.; Krähenbühl, T.; Krause, J.; Krawczynski, H.; Krennrich, F.; Kretzschmann, A.; Kubo, H.; Kudryavtsev, V. A.; Kushida, J.; Barbera, A. La; Parola, V. La; Rosa, G. La; López, Alicia; Lamanna, G.; Laporte, Philippe; Lavalley, C.; Flour, T. Le; Padellec, A. Le; Lenain, J.‐P.; Lessio, L.; Lieunard, B.; Lindfors, E.; Liolios, A.; Löhse, T.; Lombardi, S.; Lopatin, A.; Lorenz, E.; Lubiński, P.; Luz, O.; Lyard, E.; Maccarone, Maria Concetta; Maccarone, T. J.; Maier, G.; Majumdar, P.; Maltezos, S.; Małkiewicz, P.; Mañá, C.; Manalaysay, A.; Maneva, G.; Mangano, A.; Manigot, P.; Marín, J.; Mariotti, M.; Markoff, Sera; Martínez, G.; Martı́nez, M.; Mastichiadis, A.; Matsumoto, H.; Mattiazzo, Serena; Mazin, D.; McComb, T. J. L.; McCubbin, N. A.; McHardy, I. M.; Medina, C.; Melkumyan, David; Mendes, Andre David Tinoco; Mertsch, Philipp; Meucci, M.; Michałowski, J.; Micolon, P.; Mineo, T.; Mirabal, N.; Mirabel, F.; Miranda, J. M.; Mirzoyan, R.; Mizuno, T.; Moal, B.; Moderski, R.; Molinari, E.; Monteiro, Inocencio; Moralejo, A.; Morello, C.; Mori, Koji; Motta, Giorgio; Mottez, Fabrice; Moulin, Emmanuel; Mukherjee, R.; Munar, P.; Muraishi, H.; Murase, Kohta; Murphy, A. St. J.; Nagataki, Shigehiro; Naito, T.; Nakamori, Takeshi; Nakayama, K.; Naumann, C. L.; Naumann, Dieter; Nayman, P.; Nedbal, D.; Niedźwiecki, A.; Niemiec, J.; Nikolaidis, A.; Nishijima, K.; Nolan, S. J.; Nowak, N.; O’Brien, P. T.; Ochoa, I.; Ohira, Yutaka; Ohishi, M.; Ohka, H.; Okumura, A.; Olivetto, C.; Ong, R. A.; Orito, R.; Orr, M.; Osborne, J. P.; Ostrowski, M.; Otero, Lidia Ana; Otte, A. N.; Ovcharov, E.; Oya, I.; Oziȩbło, A.; Paiano, S.; Pallota, J.; Panazol, J. L.; Paneque, D.; Panter, M.; Paoletti, R.; Papyan, G.; Paredes, J. M.; Pareschi, G.; Parsons, R. D.; Arribas, M. Paz; Pedaletti, G.; Pepato, A.; Peršić, M.; Petrucci, P.-O.; Peyaud, B.; Piechocki, Włodzimierz; Pita, S.; Pivato, G.; Płatos, Ł.; Platzer, R.; Pogosyan, L.; Pohl, M.; Pojmański, G.; Ponz, J. D.; Potter, William J.; Prandini, E.; Preece, R.; Prokoph, H.; Pühlhofer, G.; Punch, M.; Quel, E. J.; Quirrenbach, A.; Rajda, P.; Rando, R.; Rataj, M.; Raue, M.; Reimann, C.T.; Reimann, O.; Reimer, A.; Reimer, O.; Renaud, M.; Renner, S.; Reymond, J. M.; Rhode, W.; Ribó, M.; Ribordy, M.; Rico, J.; Rieger, F.; Ringegni, P.; Ripken, J.; Ristori, P.; Rivoire, S.; Rob, L.; Rodriguez, Samelys; Roeser, U.; Romano, P.; Romero, Gustavo E.; Rosier‐Lees, S.; Rovero, A. C.; Roy, Frank; Royer, S.; Rudak, B.; Rulten, C. B.; Ruppel, J.; Russo, F.; Ryde, F.; Sacco, B.; Saggion, A.; Sahakian, V.; Saito, Koji; Saito, T.; Sakaki, N.; Salazar, Edwin Andrés Quintero; Salini, A.; Sánchez, F.; Conde, M. Á. Sánchez; Santangelo, A.; Santos, E.; Sanuy, A.; Sapozhnikov, L.; Sarkar, S.; Scalzotto, V.; Scapin, V.; Scarcioffolo, M.; Schanz, T.; Schlenstedt, S.; Schlickeiser, R.; Schmidt, Thomas; Schmoll, J.; Schroedter, M.; Schultz, C.; Schultze, J.; Schulz, A.; Schwanke, U.; Schwarzburg, S.; Schweizer, T.; Seiradakis, J. H.; Selmane, S.; Seweryn, K.; Shayduk, M.; Shellard, R. C.; Shibata, T.; Sikora, Marek; Silk, Joseph; Sillanpää, A.; Sitarek, J.; Skole, C.; Smith, N.; Sobczyńska, D.; Haro, Miguel Sofo; Sol, H.; Spanier, F.; Spiga, D.; Spyrou, S.; Stamatescu, V.; Stamerra, A.; Starling, R. L. C.; Stawarz, Ł.; Steenkamp, R.; Stegmann, C.; Steiner, S.; Stergioulas, Nikolaos; Sternberger, R.; Stinzing, F.; Stodulski, M.; Straumann, U.; Suárez, A. Dosil; Suchenek, M.; Sugawara, R.; Sulanke, K.-H.; Sun, S.; Supanitsky, A. D.; Sutcliffe, P.; Szanecki, Michał; Szepieniec, Tomasz; Szostek, A.; Szymkowiak, A. E.; Tagliaferri, G.; Tajima, H.; Takahashi, H.; Takahashi, K.; Takalo, L. O.; Takami, H.; Talbot, R. Gordon; Tam, P. H. T.; Tanaka, M.; Tanimori, T.; Tavani, M.; Tavernet, J.‐P.; Tchernin, C.; Tejedor, Luis; Telezhinsky, I.; Temnikov, P.; Tenzer, C.; Terada, Y.; Terrier, R.; Teshima, M.; Testa, V.; Tibaldo, L.; Tibolla, O.; Tluczykont, M.; Peixoto, C. J. Todero; Tokanai, F.; Tokarz, M.; Toma, Kenji; Torres, D. F.; Tosti, G.; Totani, Tomonori; Toussenel, F.; Vallania, P.; Vallejo, G.; Walt, D. J. van der; Eldik, C. van; Vandenbroucke, J.; Vankov, H.; Vasileiadis, G.; Vassiliev, V. V.; Vegas, I.; Venter, L.; Vercellone, S.; Veyssière, C.; Vialle, J. P.; Videla, M.; Vincent, P.; Vink, Jacco; Vlahakis, N.; Vlahos, L.; Vogler, P.; Vollhardt, A.; Volpe, F.; Gunten, H. P. Von; Vorobiov, S.; Wagner, S. J.; Wagner, R. M.; Wagner, B.; Wakely, S. P.; Walter, P. von; Walter, R.; Warwick, R. S.; Wawer, P.; Wawrzaszek, R.; Webb, N.; Wegner, Peter; Weinstein, A. J.R.; Weitzel, Q.; Welsing, R.; Wetteskind, H.; White, R.; Wierzcholska, A.; Wilkinson, M. I.; Williams, D. A.; Winde, M.; Wischnewski, R.; Wiśniewski, Łukasz; Wolczko, A.; Wood, M.; Xiong, Qian; Yamamoto, Tokonatsu; Yamaoka, K.; Yamazaki, Ryo; Yanagita, S.; Yoffo, B.; Yonetani, M.; Yoshida, A.; Yoshida, Tatsuo; Yoshikoshi, T.; Zabalza, V.; Zagdański, A.; Zajczyk, A.; Zdziarski, A. A.; Zech, A.; Zietara, Krzystof; Ziółkowski, Pawel; Zitelli, V.; Żychowski, P.

doi:10.1007/s10686-011-9247-0

Cited by 779 publications

(574 citation statements)

References 88 publications

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“…This issue is crucial to assessing novae as potential targets for present and future TeV telescopes, such as the Cherenkov Telescope Array (CTA; Actis et al 2011), and current neutrino observatories, such as IceCube (Karle et al 2003). Although the statistics are poor, the time-integrated spectral energy distribution measured by Fermi LAT shows hints for a spectral cut-off or break in the photon energy range E γ ∼ 1−10 GeV (Ackermann et al 2014).…”

Section: Introductionmentioning

confidence: 99%

Novae as Tevatrons: prospects for CTA and IceCube

Metzger

Caprioli

Vurm

et al. 2016

Mon. Not. R. Astron. Soc.

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The discovery of novae as sources of ∼ 0.1 − 1 GeV gamma-rays highlights the key role of shocks and relativistic particle acceleration in these transient systems. Although there is evidence for a spectral cut-off above energies ∼ 1 − 100 GeV at particular epochs in some novae, the maximum particle energy achieved in these accelerators has remained an open question. The high densities of the nova ejecta (∼ 10 orders of magnitude larger than in supernova remnants) render the gas far upstream of the shock neutral and shielded from ionizing radiation. The amplification of the magnetic field needed for diffusive shock acceleration requires ionized gas, thus confining the acceleration process to a narrow photo-ionized layer immediately ahead of the shock. Based on the growth rate in this layer of the hybrid non-resonant cosmic ray current-driven instability (considering also ion-neutral damping), we quantify the maximum particle energy, E max , across the range of shock velocities and upstream densities of interest. We find values of E max ∼ 10 GeV -10 TeV, which are broadly consistent with the inferred spectral cut-offs, but which could also in principle lead to emission extending to higher energies ∼ > 100 GeV accessible to atmosphere Cherenkov telescopes, such as the planned Cherenkov Telescope Array (CTA). Detecting TeV neutrinos with IceCube in hadronic scenarios appears to be more challenging, although the prospects are improved for a particularly nearby event (distance ∼ < kpc) or if the shock power during the earliest, densest phases of the nova outburst is higher than is implied by the observed GeV light curves, due to downscattering of the gamma-rays by electrons within the ejecta. Novae provide ideal nearby laboratories to study magnetic field amplification and the onset of cosmic ray acceleration, because other time-dependent sources (e.g. radio supernovae) typically occur too distant to detect as gamma-ray sources.

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Section: Introductionmentioning

confidence: 99%

Novae as Tevatrons: prospects for CTA and IceCube

Metzger

Caprioli

Vurm

et al. 2016

Mon. Not. R. Astron. Soc.

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“…Left: HERD 5σ continuum sensitivity for one year observation in comparison with all other missions with gamma-ray observation capability, e.g., ISS-CALET [28], DAMPE and Fermi [25], and including the future CTA [26] and the Large High Altitude Air Shower Observatory (LHAASO) [27]. image intensified CMOS (IsCMOS) is proposed, which can greatly reduce the complexity of onboard electronics.…”

Section: Pos(icrc2017)1077mentioning

confidence: 99%

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

Zhang¹,

Adriani²,

Albergo³

et al. 2017

Proceedings of 35th International Cosmic Ray Conference — PoS(ICRC2017)

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PoS(ICRC2017)1077The High Energy cosmic-Radiation Detection (HERD) facility is one of several space astronomy payloads onboard China's Space Station, which is planned for operation starting around 2025 for about 10 years. The main scientific objectives of HERD are searching for signals of dark matter annihilation products, precise cosmic electron (plus positron) spectrum and anisotropy measurements up to 10 TeV, precise cosmic ray spectrum and composition measurements up to the knee energy, and high energy gamma-ray monitoring and survey. HERD is composed of a 3-D cubic calorimeter (CALO) surrounded by microstrip silicon trackers (STKs) from five sides except the bottom. CALO is made of about 7,500 cubes of LYSO crystals, corresponding to about 55 radiation lengths and 3 nuclear interaction lengths, respectively. The top STK microstrips of six X-Y layers are sandwiched with tungsten converters to make precise directional measurements of incoming electrons and gamma-rays. In the baseline design, each of the four side STKs is made of only three layers microstrips. All STKs will also be used for measuring the charge and incoming directions of cosmic rays, as well as identifying back scattered tracks. With this design, HERD can achieve the following performance: energy resolution of 1% for electrons and gamma-rays beyond 100 GeV and 20% for protons from 100 GeV to 1 PeV; electron/proton separation power better than 10 −5 ; effective geometrical factors of >3 m 2 sr for electron and diffuse gamma-rays, >2 m 2 sr for cosmic ray nuclei. R&D is under way for reading out the LYSO signals with optical fiber coupled to image intensified IsCMOS and CALO prototype of 250 LYSO crystals.

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“…The Cherenkov Telescope Array (CTA), a pair of planned next-generation IACT arrays in the northern and southern hemispheres, promises broader energy coverage, dramatically improved (< 0.04 • ) angular resolution, a comparatively large (7 − 8 • ) field of view and order-of-magnitude increase in sensitivity between 100 GeV and 10 TeV [65,66]. LHAASO, a hybrid instrument combining water Cherenkov and particle detectors [67], also promises unprecedented sensitivity between 20 TeV and a PeV.…”

Section: Future Instrumentsmentioning

confidence: 99%

Pulsar Wind Nebulae and Cosmic Rays: A Bedtime Story

Weinstein¹

2014

Nuclear Physics B - Proceedings Supplements

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The role pulsar wind nebulae play in producing our locally observed cosmic ray spectrum remains murky, yet intriguing. Pulsar wind nebulae are born and evolve in conjunction with SNRs, which are favored sites of Galactic cosmic ray acceleration. As a result they frequently complicate interpretation of the gamma-ray emission seen from SNRs. However, pulsar wind nebulae may also contribute directly to the local cosmic ray spectrum, particularly the leptonic component. This paper reviews the current thinking on pulsar wind nebulae and their connection to cosmic ray production from an observational perspective. It also considers how both future technologies and new ways of analyzing existing data can help us to better address the relevant theoretical questions. A number of key points will be illustrated with recent results from the VHE (E > 100 GeV) gamma-ray observatory VERITAS. Keywords: IntroductionThe discovery of cosmic rays in the early twentieth century [1, 2] inaugurated a decades-long, serialized mystery story that has yet to be completed. At the heart of the mystery lies a set of of simple questions. What particles appear in the cosmic ray spectrum that we see from Earth? Where do these particles originate? How are they accelerated? In recent decades direct cosmic ray observations have brought us a wealth of information on the cosmic ray spectrum and its composition, clues to the types of environments in which cosmic rays are born. The interaction of these particles with interstellar magnetic fields, however, prevents them from being traced back to their point of origin.In order to pursue the other half of this mystery-the nature of cosmic ray accelerators-we must use the secondary photon radiation produced in these cosmic ray nurseries. These high-energy (300 MeV -100 GeV) and very high-energy (VHE; E > 100 GeV) gamma rays are not deflected by interstellar magnetic fields and can be used to map cosmic ray populations in and near their parent accelerators. The different processes by which relativistic cosmic ray electrons, protons, and heavier nuclei produce high-energy gamma rays leave characteristic imprints on the gamma-ray energy spectrum of particular astrophysical accelerators. These features may be used to constrain the composition and energy spectrum of accelerated particle populations.The local cosmic ray spectrum is known to be a mix of protons and heavier nuclei, with a smaller admixture of leptons. A mix of astrophysical accelerators within and outside our Galaxy is believed to contribute, including shocks arising in supernova remnants (SNRs), shocks formed by interacting high-velocity winds from massive stars [3], pulsars, and active galactic nuclei (AGN). We focus here on a single subplot of a much larger story-the role played by pulsar wind nebulae (PWNe) in our quest to understand the Galactic cosmic ray spectrum. Dramatis PersonaeNo single gamma-ray observatory provides a complete picture of the gamma-ray sky at all energies and spatial scales. The Fermi Gamma-ray Space Telescope (...

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Design concepts for the Cherenkov Telescope Array CTA: an advanced facility for ground-based high-energy gamma-ray astronomy

Cited by 779 publications

References 88 publications

Novae as Tevatrons: prospects for CTA and IceCube

Novae as Tevatrons: prospects for CTA and IceCube

Introduction to the High Energy cosmic-Radiation Detection (HERD) Facility onboard China’s Future Space Station

Pulsar Wind Nebulae and Cosmic Rays: A Bedtime Story

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