1,721,198 research outputs found
gSeaGen: The KM3NeT GENIE-based code for neutrino telescopes
No full textThe gSeaGen code is a GENIE-based application developed to efficiently generate high statistics samples of events, induced by neutrino interactions, detectable in a neutrino telescope. The gSeaGen code is able to generate events induced by all neutrino flavours, considering topological differences between track-type and shower-like events. Neutrino interactions are simulated taking into account the density and the composition of the media surrounding the detector. The main features of gSeaGen are presented together with some examples of its application within the KM3NeT project
Contributions of KM3NeT to ICRC2023
Get PDFThis document collects the contributions of the KM3NeT collaboration to the
ICRC2023 conference, held from July 26 to August 3, 2023, in Nagoya, Japan.
KM3NeT submitted 38 contributions to ICRC2023, on neutrino- and multimessenger
astronomy, neutrino oscillation physics, cosmic ray physics, searches for dark
matter and exotics, calibration, technical detector descriptions, and art.
Proceedings are published in Proceedings of Science.Comment: 306 pages, many figures. Collection of proceedings contributions to
ICRC2023, published in PoS(ICRC2023), https://pos.sissa.it/444
Design and Development of an acoustic positioning system for a cubic kilometre underwater neutrino telescope
Get PDFEn los últimos años los telescopios submarinos de neutrinos han cobrado una mayor importancia ya que consisten en un nuevo y único instrumento para observar el Universo. Los neutrinos son partículas sin carga e interactúan muy débilmente con la materia que les rodean, pueden escaparse fácilmente de la fuente que los ha producidos y llegar a La Tierra sin ser desviada por los campo magnético y sin interactuar con otras partículas. Esto implica que los neutrinos pueden traer informaciones astrofísicas que otros mensajeros no pueden aportar y abrir una potencial ventana hacia el Universo. Por otro lado, su baja interacción con la materia impone la necesidad de construir un detector de grandes dimensiones del orden de 1 km3 utilizando volumen de agua o hielo y con muchos sensores ópticos para detectar esta interacción de neutrino de alta energía. Un método para detectar neutrinos es a través de la luz Cherenkov emitida por el muon generado después de una interacción de neutrino. Esta partícula, al atravesar el detector con una velocidad superior a la luz en el medio, genera una débil luz azulada llamada radiación de Cherenkov que es detectada por una red de sensores ópticos (fotomultiplicadores). El tiempo de llegada de la luz a los fotomultiplicadores puede ser utilizado para reconstruir la traza del muon y consecuentemente del neutrino que lo ha producido. La precisión en la reconstrucción de la traza del muon depende de la precisión en la medida del tiempo de llegada de la luz y en la precisión en de la posición de los sensores ópticos en el detector. Por esta razón, en telescopios submarinos es necesario un sistema de posicionamiento acústico (APS) capaz de monitorizar el movimiento de los sensores ópticos con una precisión de ~10 cm. Los estudios realizados están enmarcados dentro de las actividades de calibración de posicionamiento acústico en dos colaboraciones europeas para el diseño, construcción y operación de telescopios submarinos de neutrinos en el MediterLarosa ., G. (2012). Design and Development of an acoustic positioning system for a cubic kilometre underwater neutrino telescope [Tesis doctoral]. Universitat Politècnica de València. https://doi.org/10.4995/Thesis/10251/16877Palanci
The prototype detection unit of the KM3NeT detector: KM3NeT Collaboration
No full textA prototype detection unit of the KM3NeT deep-sea neutrino telescope has been installed at 3500m depth 80 km offshore the Italian coast. KM3NeT in its final configuration will contain several hundreds of detection units. Each detection unit is a mechanical structure anchored to the sea floor, held vertical by a submerged buoy and supporting optical modules for the detection of Cherenkov light emitted by charged secondary particles emerging from neutrino interactions. This prototype string implements three optical modules with 31 photomultiplier tubes each. These optical modules were developed by the KM3NeT Collaboration to enhance the detection capability of neutrino interactions. The prototype detection unit was operated since its deployment in May 2014 until its decommissioning in July 2015. Reconstruction of the particle trajectories from the data requires a nanosecond accuracy in the time calibration. A procedure for relative time calibration of the photomultiplier tubes contained in each optical module is described. This procedure is based on the measured coincidences produced in the sea by the 40K background light and can easily be expanded to a detector with several thousands of optical modules. The time offsets between the different optical modules are obtained using LED nanobeacons mounted inside them. A set of data corresponding to 600 h of livetime was analysed. The results show good agreement with Monte Carlo simulations of the expected optical background and the signal from atmospheric muons. An almost background-free sample of muons was selected by filtering the time correlated signals on all the three optical modules. The zenith angle of the selected muons was reconstructed with a precision of about 3∘. © 2016, The Author(s)
Embedded software of the KM3NeT central logic board
Get PDFhttps://www.sciencedirect.com/science/article/pii/S0010465523003818?via%3DihubThe KM3NeT Collaboration is building and operating two deep sea neutrino telescopes at the bottom of the
Mediterranean Sea. The telescopes consist of latices of photomultiplier tubes housed in pressure-resistant glass
spheres, called digital optical modules and arranged in vertical detection units. The two main scientific goals
are the determination of the neutrino mass ordering and the discovery and observation of high-energy neutrino
sources in the Universe. Neutrinos are detected via the Cherenkov light, which is induced by charged particles
originated in neutrino interactions. The photomultiplier tubes convert the Cherenkov light into electrical signals
that are acquired and timestamped by the acquisition electronics. Each optical module houses the acquisition
electronics for collecting and timestamping the photomultiplier signals with one nanosecond accuracy. Once
finished, the two telescopes will have installed more than six thousand optical acquisition nodes, completing
one of the more complex networks in the world in terms of operation and synchronization. The embedded
software running in the acquisition nodes has been designed to provide a framework that will operate with
different hardware versions and functionalities. The hardware will not be accessible once in operation, which
complicates the embedded software architecture. The embedded software provides a set of tools to facilitate
remote manageability of the deployed hardware, including safe reconfiguration of the firmware. This paper
presents the architecture and the techniques, methods and implementation of the embedded software running in
the acquisition nodes of the KM3NeT neutrino telescopes
The prototype detection unit of the KM3NeT detector: KM3NeT Collaboration
No full textA prototype detection unit of the KM3NeT deep-sea neutrino telescope has been installed at 3500m depth 80 km offshore the Italian coast. KM3NeT in its final configuration will contain several hundreds of detection units. Each detection unit is a mechanical structure anchored to the sea floor, held vertical by a submerged buoy and supporting optical modules for the detection of Cherenkov light emitted by charged secondary particles emerging from neutrino interactions. This prototype string implements three optical modules with 31 photomultiplier tubes each. These optical modules were developed by the KM3NeT Collaboration to enhance the detection capability of neutrino interactions. The prototype detection unit was operated since its deployment in May 2014 until its decommissioning in July 2015. Reconstruction of the particle trajectories from the data requires a nanosecond accuracy in the time calibration. A procedure for relative time calibration of the photomultiplier tubes contained in each optical module is described. This procedure is based on the measured coincidences produced in the sea by the 40K background light and can easily be expanded to a detector with several thousands of optical modules. The time offsets between the different optical modules are obtained using LED nanobeacons mounted inside them. A set of data corresponding to 600 h of livetime was analysed. The results show good agreement with Monte Carlo simulations of the expected optical background and the signal from atmospheric muons. An almost background-free sample of muons was selected by filtering the time correlated signals on all the three optical modules. The zenith angle of the selected muons was reconstructed with a precision of about 3∘
Measurement of the atmospheric ν μ flux with six detection units of KM3NeT/ORCA
No full textAbstract A measurement of the atmospheric ν μ + ν ¯ μ flux with energies between 1 and 100 GeV is presented. The measurement has been performed using data taken with the first six detection units of the KM3NeT/ORCA detector, referred to as ORCA6. The data were collected between January 2020 and November 2021 and correspond to 510 days of livetime, with a total exposure of 433 kton · years. Using machine learning classification, 3894 neutrino candidate events have been selected with an atmospheric muon contamination of less than 1 % . The atmospheric ν μ + ν ¯ μ energy spectrum is derived using an unfolding procedure and the impact of systematic uncertainties is estimated. The atmospheric ν μ + ν ¯ μ flux measured using the ORCA6 configuration is in agreement with the values measured by other experiments
Differential Sensitivity of the KM3NeT/ARCA detector to a diffuse neutrino flux and to point-like source emission: exploring the case of the Starburst Galaxies
Get PDFKM3NeT/ARCA is a Cherenkov neutrino telescope under construction in the
Mediterranean sea, optimised for the detection of astrophysical neutrinos with
energies above 1~TeV. In this work, using Monte Carlo simulations
including all-flavour neutrinos, the integrated and differential sensitivities
for KM3NeT/ARCA are presented considering the case of a diffuse neutrino flux
as well as extended and point-like neutrino sources. This analysis is applied
to Starburst Galaxies demonstrating that the detector has the capability of
tracing TeV neutrinos from these sources. Remarkably, after eight years, a hard
power-law spectrum from the nearby Small Magellanic Cloud can be constrained.
The sensitivity and discovery potential for NGC 1068 is also evaluated showing
that KM3NeT/ARCA will discriminate between different astrophysical components
of the measured neutrino flux after 3 years of data taking.Comment: 24 pages, 6 figures, Version 2, submitted to Astroparticle Physic
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