NEDA—NEutron Detector Array

The NEutron Detector Array, NEDA, will form the next generation neutron detection system that has been designed to be operated in conjunction with γ-ray arrays, such as the tracking-array AGATA, to aid nuclear spectroscopy studies. NEDA has been designed to be a versatile device, with high-detection efficiency, excellent neutron-γ discrimination, and high rate capabilities. It will be employed in physics campaigns in order to maximise the scientific output, making use of the different stable and radioactive ion beams available in Europe. The first implementation of the neutron detector array NEDA with AGATA 1π was realised at GANIL. This manuscript reviews the various aspects of NEDA

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

Ground-based gamma-ray astronomy has had a major breakthrough with the impressive results obtained using systems of imaging atmospheric Cherenkov telescopes. Ground-based gamma-ray astronomy has a huge potential in astrophysics, particle physics and cosmology. CTA is an international initiative to build the next generation instrument, with a factor of 5-10 improvement in sensitivity in the 100 GeV-10 TeV range and the extension to energies well below 100 GeV and above 100 TeV. CTA will consist of two arrays (one in the north, one in the south) for full sky coverage and will be operated as open observatory. The design of CTA is based on currently available technology. This document reports on the status and presents the major design concepts of CTA

The new neutron multiplicity filter NEDA and its first physics campaign with AGATA

A new neutron multiplicity filter NEDA, after a decade of design, R&D and construction, was employed in its first physics campaign with the AGATA spectrometer. Properties and performance of the array are discussed

The GALILEO γ-ray array at the Legnaro National Laboratories

none84GALILEO, a new 4π high-resolution γ-detection array, based on HPGe detectors, has been developed and installed at the Legnaro National Laboratories. The GALILEO array greatly benefits from a fully-digital read-out chain, customized DAQ, and a variety of complementary detectors to improve the resolving power by the detection of particles, ions or high-energy γ-ray transitions. In this work, a full description of the array, including electronics and DAQ, is presented together with its complementary instrumentation.noneGoasduff A.; Mengoni D.; Recchia F.; Valiente-Dobon J.J.; Menegazzo R.; Benzoni G.; Barrientos D.; Bellato M.; Bez N.; Biasotto M.; Blasi N.; Boiano C.; Boso A.; Bottoni S.; Bracco A.; Brambilla S.; Brugnara D.; Camera F.; Capra S.; Capsoni A.; Cocconi P.; Coelli S.; Cortes M.L.; Crespi F.C.L.; de Angelis G.; Egea F.J.; Fanin C.; Fantinel S.; Gadea A.; Gamba E.R.; Gambalonga A.; Gesmundo C.; Gosta G.; Gottardo A.; Gozzelino A.; Gregor E.T.; Gulmini M.; Ha J.; Hadynska-Klek K.; Illana A.; Isocrate R.; Jaworski G.; John P.R.; Lenzi S.M.; Leoni S.; Lunardi S.; Magalini M.; Marchini N.; Million B.; Modamio V.; Nannini A.; Napoli D.R.; Pasqualato G.; Pellumaj J.; Perez-Vidal R.M.; Pigliapoco S.; Polettini M.; Porzio C.; Pullia A.; Ramina L.; Rampazzo G.; Rampazzo M.; Rebeschini M.; Rezynkina K.; Rocchini M.; Romanato M.; Rosso D.; Saltarelli A.; Scarcioffolo M.; Siciliano M.; Testov D.A.; Tomasella D.; Tomasi F.; Toniolo N.; Ur C.A.; Ventura S.; Veronese F.; Viscione E.; Volpe V.; Wieland O.; Zanon I.; Ziliani S.; Zhang G.; Bazzacco D.Goasduff, A.; Mengoni, D.; Recchia, F.; Valiente-Dobon, J. J.; Menegazzo, R.; Benzoni, G.; Barrientos, D.; Bellato, M.; Bez, N.; Biasotto, M.; Blasi, N.; Boiano, C.; Boso, A.; Bottoni, S.; Bracco, A.; Brambilla, S.; Brugnara, D.; Camera, F.; Capra, S.; Capsoni, A.; Cocconi, P.; Coelli, S.; Cortes, M. L.; Crespi, F. C. L.; de Angelis, G.; Egea, F. J.; Fanin, C.; Fantinel, S.; Gadea, A.; Gamba, E. R.; Gambalonga, A.; Gesmundo, C.; Gosta, G.; Gottardo, A.; Gozzelino, A.; Gregor, E. T.; Gulmini, M.; Ha, J.; Hadynska-Klek, K.; Illana, A.; Isocrate, R.; Jaworski, G.; John, P. R.; Lenzi, S. M.; Leoni, S.; Lunardi, S.; Magalini, M.; Marchini, N.; Million, B.; Modamio, V.; Nannini, A.; Napoli, D. R.; Pasqualato, G.; Pellumaj, J.; Perez-Vidal, R. M.; Pigliapoco, S.; Polettini, M.; Porzio, C.; Pullia, A.; Ramina, L.; Rampazzo, G.; Rampazzo, M.; Rebeschini, M.; Rezynkina, K.; Rocchini, M.; Romanato, M.; Rosso, D.; Saltarelli, A.; Scarcioffolo, M.; Siciliano, M.; Testov, D. A.; Tomasella, D.; Tomasi, F.; Toniolo, N.; Ur, C. A.; Ventura, S.; Veronese, F.; Viscione, E.; Volpe, V.; Wieland, O.; Zanon, I.; Ziliani, S.; Zhang, G.; Bazzacco, D

Conceptual design of the AGATA 2<math display="inline" id="d1e396" altimg="si24.svg"><mi>π</mi></math> array at LNL

International audienceThe Advanced GAmma Tracking Array (AGATA) has been installed at Laboratori Nazionali di Legnaro (LNL), Italy. In this installation, AGATA will consist, at the beginning, of 13 AGATA triple clusters (ATCs) with an angular coverage of 1π, and progressively the number of ATCs will increase up to a 2π angular coverage. This setup will exploit both stable and radioactive ion beams delivered by the Tandem–PIAVE-ALPI accelerator complex and the SPES facility. The new implementation of AGATA at LNL will be used in two different configurations, firstly one coupled to the PRISMA large-acceptance magnetic spectrometer and lately a second one at Zero Degrees, along the beam line. These two configurations will allow us to cover a broad physics program, using different reaction mechanisms, such as Coulomb excitation, fusion-evaporation, transfer and fission at energies close to the Coulomb barrier. These setups have been designed to be coupled with a large variety of complementary detectors such as charged particle detectors, neutron detectors, heavy-ion detectors, high-energy γ-ray arrays, cryogenic and gasjet targets and the plunger device for lifetime measurements. We present in this paper the conceptual design, characteristics and performance figures of this implementation of AGATA at LNL

Conceptual design of the AGATA 2<math display="inline" id="d1e396" altimg="si24.svg"><mi>π</mi></math> array at LNL

International audienceThe Advanced GAmma Tracking Array (AGATA) has been installed at Laboratori Nazionali di Legnaro (LNL), Italy. In this installation, AGATA will consist, at the beginning, of 13 AGATA triple clusters (ATCs) with an angular coverage of 1π, and progressively the number of ATCs will increase up to a 2π angular coverage. This setup will exploit both stable and radioactive ion beams delivered by the Tandem–PIAVE-ALPI accelerator complex and the SPES facility. The new implementation of AGATA at LNL will be used in two different configurations, firstly one coupled to the PRISMA large-acceptance magnetic spectrometer and lately a second one at Zero Degrees, along the beam line. These two configurations will allow us to cover a broad physics program, using different reaction mechanisms, such as Coulomb excitation, fusion-evaporation, transfer and fission at energies close to the Coulomb barrier. These setups have been designed to be coupled with a large variety of complementary detectors such as charged particle detectors, neutron detectors, heavy-ion detectors, high-energy γ-ray arrays, cryogenic and gasjet targets and the plunger device for lifetime measurements. We present in this paper the conceptual design, characteristics and performance figures of this implementation of AGATA at LNL

CTA contributions to the 33rd International Cosmic Ray Conference (ICRC2013)

Compilation of CTA contributions to the proceedings of the 33rd International Cosmic Ray Conference (ICRC2013), which took place in 2-9 July, 2013, in Rio de Janeiro, BrazilComment: Index of CTA conference proceedings at the ICRC2013, Rio de Janeiro (Brazil). v1: placeholder with no arXiv links yet, to be replaced once individual contributions have been all submitted. v2: final with arXiv links to all CTA contributions and full author lis

Introducing the CTA concept

The Cherenkov Telescope Array (CTA) is a new observatory for very high-energy (VHE) gamma rays. CTA has ambitions science goals, for which it is necessary to achieve full-sky coverage, to improve the sensitivity by about an order of magnitude, to span about four decades of energy, from a few tens of GeV to above 100 TeV with enhanced angular and energy resolutions over existing VHE gamma-ray observatories. An international collaboration has formed with more than 1000 members from 27 countries in Europe, Asia, Africa and North and South America. In 2010 the CTA Consortium completed a Design Study and started a three-year Preparatory Phase which leads to production readiness of CTA in 2014. In this paper we introduce the science goals and the concept of CTA, and provide an overview of the project