Nanobeacon: A time calibration device for the KM3NeT neutrino telescope (original) (raw)

The new CLBv4 for the KM3NeT Neutrino Telescope

EPJ Web of Conferences, 2019

The KM3NeT collaboration aims at the construction of a deepsea neutrino observatory in the Mediterranean Sea equipped with thousands of glass spheres, the so-called Digital Optical Modules, each of which contains 31 photomultipliers of small photocathode area. These devices will be used for the detection of the Cherenkov light induced by charged particles produced by the interaction of neutrinos with matter inside or in the vicinity of the KM3NeT detector. The signal acquired by each photomultiplier is sent to a Time to Digital Converter which is part of a Central Logic Board. The Time to Digital Converter resolution is 1 ns and the White Rabbit technology is used to guarantee time synchronization between the optical modules. Due to the large volume to be instrumented by KM3NeT, a cost reduction of the different systems is important so different versions of the Central Logic Board have been designed. The newest version was designed also to also reduce the phase noise in the main clo...

Time calibration of the ANTARES neutrino telescope

Astroparticle Physics, 2011

The ANTARES deep-sea neutrino telescope comprises a three-dimensional array of photomultipliers to detect the Cherenkov light induced by upgoing relativistic charged particles originating from neutrino interactions in the vicinity of the detector. The large scattering length of light in the deep sea facilitates an angular resolution of a few tenths of a degree for neutrino energies exceeding 10 TeV. In order to achieve this optimal performance, the time calibration procedures should ensure a relative time calibration between the photomultipliers at the level of ∼1ns. The methods developed to attain this level of precision are described.

Physics with underwater neutrino telescopes

Progress in Particle and Nuclear Physics, 2010

We give a short review of the ongoing efforts in the construction of large underwater photomultiplier arrays aiming at the detection of neutrinos of astrophysical origin.

A Deep Sea Telescope for High Energy Neutrinos

1999

The ANTARES Collaboration proposes to construct a large area water Cherenkov detector in the deep Mediterranean Sea, optimised for the detection of muons from high-energy astrophysical neutrinos. This paper presents the scientific motivation for building such a device, along with a review of the technical issues involved in its design and construction. The observation of high energy neutrinos will open a new window on the universe. The primary aim is to study particle acceleration mechanisms in energetic astrophysical objects such as AGN's and GRB's, which may also shed light on the origin of ultra-high-energy cosmic rays. At lower energies, non-baryonic dark matter may be detected through the neutrinos produced when gravitationally captured WIMPs annihilate in the cores of the Earth and the Sun. Neutrino oscillations can be measured by studying distortions in the energy spectrum of upward-going atmospheric nu's. The characteristics of the proposed site are an important ...

Absolute angular calibration of a submarine km3 neutrino telescope

Nuclear Instruments and Methods in Physics Research Section A: Accelerators, Spectrometers, Detectors and Associated Equipment, 2011

A requirement for neutrino telescope is the ability to resolve point sources of neutrinos. In order to understand its resolving power a way to perform absolute angular calibration with muons is required. Muons produced by cosmic rays in the atmosphere offer an abundant calibration source. By covering a surface vessel with 200 modules of 5 m 2 plastic scintillator a surface air shower array can be set up. Running this array in coincidence with a deep-sea km 3 size neutrino detector, where the coincidence is defined by the absolute clock timing stamp for each event, would allow absolute angular calibration to be performed. Monte Carlo results simulating the absolute angular calibration of the km 3 size neutrino detector will be presented. Future work and direction will be discussed.

Oscillations of atmospheric neutrinos with a large neutrino telescope

Il Nuovo Cimento A, 1990

The sensitivity of a large water Cerenkov neutrino telescope in detecting possible oscillations (~ ~ ~) and (~-~ ~e) of atmospheric neutrinos is studied, taking also into account the Wolfenstein, Mikheyev and Smirnov matter effects. The large water Cerenkov device is able to detect with high accuracy upward-going muons with energies greater than 10 GeV. After one year running time the search for ~ oscillations will reach the following sensitivity for the oscillation parameters: Am 2 > 3.10-3(eV2), for sin220 = 1, sin220 > 4.10-2, for Am 2 > 0.1 (eV 2) for the oscillation (,~-~ ,~) and ~m 2 > 4.10-~ (eV2), for sin 220 = 1, sin s 20 > 8.10-3, for ~m 2 = 6.10 .2 (eV ~) for the oscillation (,~-. ,~). These limits are well below the current accelerator and reactor limits. It is also stressed the importance of such a measurement in the context of solar ~ puzzle.

CATIROC: an integrated chip for neutrino experiments using photomultiplier tubes

Journal of Instrumentation, 2021

A : An ASIC (Application Specific Integrated Chip) named CATIROC (Charge And Time Integrated Read Out Chip) has been developed for the next-generation neutrino experiments using a large number of photomultiplier tubes (PMTs). Each CATIROC provides the time and the charge measurements for 16 configurable input channels operating in auto-trigger mode. Originally designed for the light emission in water Cherenkov detectors, we show in this paper that its use can be extended to liquid-scintillator based experiments. The ∼ 26000 3-inch PMTs of the JUNO experiment, under construction in China, is a case in point. This paper describes the features of CATIROC with a special attention to the most critical points for its application to the time profile of the light emission in liquid scintillators. The achieved performances in both charge and time measurements can be inputs for future high-precision experiments making use of PMTs or other photo-sensitive detectors.