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S. Aiello,
E. Leonora,
A. Aloisio,
F. Ameli,
I. Amore,
M. Anghinolfi,
A. Anzalone,
G. Barbarino,
E. Barbarito,
M. Battaglieri, [......],
C. Sollima,
M. Spurio,
F. Stefani,
M. Taiuti, G. Terreni,
L. Trasatti,
S. Urso,
M. Vecchi,
P. Vicini,
R. Wischnewski
[show abstract]
[hide abstract]
ABSTRACT: The selection of the photomultiplier plays a crucial role in the R&D activity related to a large-scale underwater neutrino telescope. This paper illustrates the main procedures and facilities used to characterize the performances of 72 large area photomultipliers, Hamamatsu model R7081 sel. The voltage to achieve a gain of 5×107, dark count rate and single photoelectron time and charge properties of the overall response were measured with a properly attenuated 410 nm pulsed laser. A dedicated study of the spurious pulses was also performed. The results prove that the photomultipliers comply with the general requirements imposed by the project.
Nuclear Instruments and Methods in Physics Research Section A Accelerators Spectrometers Detectors and Associated Equipment 01/2009; · 1.21 Impact Factor
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F. Ameli,
S. Aiello,
A. Aloisio,
I. Amore,
M. Anghinolfi,
A. Anzalone,
C. Avanzini,
G. Barbarino,
E. Barbarito,
M. Battaglieri, [......],
V. Sipala,
M. Spurio,
M. Taiuti, G. Terreni,
L. Trasatti,
S. Urso,
V. Valente,
M. Vecchi,
P. Vicini,
R. Wischnewski
[show abstract]
[hide abstract]
ABSTRACT: The NEMO collaboration proposes to build an underwater neutrino telescope located South-East off the Sicily coast. This paper describes the concepts underlying the communication link design going over the whole data acquisition and transport from the front-end electronics to the module sending data on-shore through a fiber optic link which relies on Dense Wavelength Division Multiplexing. An on-shore board, plugged into a PC, extracts and distributes data both to first-level trigger and control systems. Underwater apparatus monitoring and controls are guaranteed by oceanographic instruments and dedicated sensors, whose data are packed and sent back to shore using the same optical link. The communication is fully bidirectional, allowing transmission of timing and control commands. The architecture described here provides a complete real-time data transport layer between the onshore laboratory and the underwater detector. During winter 2006 a first prototype of the apparatus has been deployed: calibration results from the currently working system are here reported.
IEEE Transactions on Nuclear Science 03/2008; · 1.45 Impact Factor
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E. Migneco,
S. Aiello,
A. Aloisio,
F. Ameli,
I. Amore,
M. Anghinolfi,
A. Anzalone,
G. Barbarino,
E. Barbarito,
M. Battaglieri, [......],
F. Speziale,
M. Spurio,
M. Taiuti, G. Terreni,
L. Trasatti,
S. Urso,
V. Valente,
M. Vecchi,
P. Vicini,
R. Wischnewski
[show abstract]
[hide abstract]
ABSTRACT: The status of the activities towards the realization of a km3 Cherenkov neutrino detector carried out by the NEMO Collaboration is described. The realization of a Phase-1 project, which is under way, will validate the proposed technologies for the realization of the km3 detector on a Test Site at 2000 m depth. The realization of a new infrastructure on the candidate site (Phase-2 project) will provide the possibility to test detector components at 3500 m depth.
Nuclear Instruments and Methods in Physics Research Section A Accelerators Spectrometers Detectors and Associated Equipment 01/2008; · 1.21 Impact Factor
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A. Capone,
S. Aiello,
A. Aloisio,
F. Ameli,
I. Amore,
M. Anghinolfi,
A. Anzalone,
G. Barbarino,
E. Barbarito,
M. Battaglieri, [......],
M. Spurio,
F. Stefani,
M. Taiuti, G. Terreni,
L. Trasatti,
S. Urso,
V. Valente,
M. Vecchi,
P. Vicini,
R. Wischnewski
[show abstract]
[hide abstract]
ABSTRACT: The latest results and the activities towards the realization of a km3 Cherenkov neutrino detector carried out by the NEMO Collaboration are described. The realization of a Phase-1 project has validated all relevant technologies proposed for the realization of the km3 detector on a test site at 2000 m depth. The realization of a new infrastructure on the candidate Capo Passero site (for Phase-2 project) will provide the possibility to test detector components at 3500 m depth.
Nuclear Instruments and Methods in Physics Research Section A Accelerators Spectrometers Detectors and Associated Equipment 01/2008; · 1.21 Impact Factor
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I. AMORE,
S. AIELLO,
M. AMBRIOLA,
F. AMELI,
M. ANGHINOLFI,
A. ANZALONE,
G. BARBARINO,
E. BARBARITO,
M. BATTAGLIERI,
R. BELLOTTI, [......],
E. SHIROKOV,
F. SIMEONE,
V. SIPALA,
M. SPURIO,
M. TAIUTI, G. TERRENI,
L. TRASATTI,
S. URSO,
V. VALENTE,
P. VICINI
[show abstract]
[hide abstract]
ABSTRACT: The status of the project is described: the activity on long term characterization of water optical and oceanographic parameters at the Capo Passero site candidate for the Mediterranean km3 neutrino telescope; the feasibility study; the physics performances and underwater technology for the km3; the activity on NEMO Phase 1, a technological demonstrator that has been deployed at 2000 m depth 25 km offshore Catania; the realization of an underwater infrastructure at 3500 m depth at the candidate site (NEMO Phase 2).
International Journal of Modern Physics A 08/2007; 22(21):3509. · 1.05 Impact Factor
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S. Aiello,
M. Ambriola,
F. Ameli,
I. Amore,
M. Anghinolfi,
A. Anzalone,
G. Barbarino,
E. Barbarito,
M. Battaglieri,
R. Bellotti, [......],
E. Shirokov,
F. Simeone,
V. Sipala,
M. Spurio,
M. Taiuti, G. Terreni,
L. Trasatti,
S. Urso,
V. Valente,
P. Vicini
[show abstract]
[hide abstract]
ABSTRACT: In this paper are presented the results of Monte Carlo simulations on the capability of the proposed NEMO-km3 telescope to detect TeV muon neutrinos from Galactic microquasars. For each known microquasar we compute the number of detectable events, together with the atmospheric neutrino and muon background events. We also discuss the detector sensitivity to neutrino fluxes expected from known microquasars, optimizing the event selection also to reject the background; the number of events surviving the event selection are given. The best candidates are the steady microquasars SS433 and GX339-4 for which we estimate a sensitivity of about 5 · 10�11 erg/cm2 s; the predicted fluxes are expected to be well above this sensitivity. For bursting microquasars the most interesting candidates are Cygnus X-3, GRO J1655-40 and XTE J1118+480: their analyses are more complicated because of the stochastic nature of the bursts.
Astroparticle Physics 03/2007; 28(2007):1-9. · 3.22 Impact Factor
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S. Aiello,
M. Ambriola,
F. Ameli,
I. Amore,
M. Anghinolfi,
A. Anzalone,
G. Barbarino,
E. Barbarito,
M. Battaglieri,
R. Bellotti, [......],
E. Shirokov,
F. Simeone,
V. Sipala,
M. Spurio,
M. Taiuti, G. Terreni,
L. Trasatti,
S. Urso,
V. Valente,
P. Vicini
[show abstract]
[hide abstract]
ABSTRACT: In this paper are presented the results of Monte Carlo simulations on the capability of the proposed NEMO-km3 telescope to detect TeV muon neutrinos from Galactic microquasars. For each known microquasar we compute the number of detectable events, together with the atmospheric neutrino and muon background events. We also discuss the detector sensitivity to neutrino fluxes expected from known microquasars, optimizing the event selection also to reject the background; the number of events surviving the event selection are given. The best candidates are the steady microquasars SS433 and GX339-4 for which we estimate a sensitivity of about 5 × 10−11 erg/cm2 s; the predicted fluxes are expected to be well above this sensitivity. For bursting microquasars the most interesting candidates are Cygnus X-3, GRO J1655-40 and XTE J1118+480: their analyses are more complicated because of the stochastic nature of the bursts.
Astroparticle Physics. 03/2007; 28(2007):1-9.
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G. Riccobene,
A. Capone,
S. Aiello,
M. Ambriola,
F. Ameli,
I. Amore,
M. Anghinolfi,
A. Anzalone,
C. Avanzini,
G. Barbarino, [......],
E. Shirokov,
F. Simeone,
V. Sipala,
M. Spurio,
M. Taiuti, G. Terreni,
L. Trasatti,
S. Urso,
V. Valente,
P. Vicini
[show abstract]
[hide abstract]
ABSTRACT: The NEMO (NEutrino Mediterranean Observatory) Collaboration has been carrying out since 1998 an evaluation programme of deep sea sites suitable for the construction of the future Mediterranean km3 Cˇ erenkov neutrino telescope. We investigated the seawater optical and oceanographic properties of several deep sea marine areas close to the Italian Coast. Inherent optical properties (light absorption and attenuation coefficients) have been measured as a function of depth using an experimental apparatus equipped with standard oceanographic probes and the commercial transmissometer AC9 manufactured by WETLabs. This paper reports on the visible light absorption and attenuation coefficients measured in deep seawater of a marine region located in the Southern Ionian Sea, 60–100 km SE of Capo Passero (Sicily). Data show that blue light absorption coefficient is about 0.015 m�1 (corresponding to an absorption length of 67 m) close to the one of optically pure water and it does not show seasonal variation.
Astroparticle Physics 08/2006; 27(2007):1-9. · 3.22 Impact Factor
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E. Migneco,
S. Aiello,
M. Ambriola,
F. Ameli,
I. Amore,
M. Anghinolfi,
A. Anzalone,
G. Barbarino,
E. Barbarito,
M. Battaglieri, [......],
E. Shirokov,
F. Simeone,
V. Sipala,
M. Spurio,
M. Taiuti, G. Terreni,
L. Trasatti,
S. Urso,
V. Valente,
P. Vicini
[show abstract]
[hide abstract]
ABSTRACT: The activities towards the realization of a km3 Cherenkov neutrino detector carried out by the NEMO Collaboration are described. Long-term exploration of a 3500 m deep-sea site close to the Sicilian coast has shown that it is optimal for the installation of the detector. The realization of a Phase-1 project, which is under way, will validate the proposed technologies for the realization of the km3 detector on a Test Site at 2000 m depth. The realization of a new infrastructure on the candidate site (Phase-2 project) will provide the possibility to test detector components at 3500 m depth.
Nuclear Instruments and Methods in Physics Research Section A Accelerators Spectrometers Detectors and Associated Equipment 01/2006; 567(2):444-451. · 1.21 Impact Factor
