https://doi.org/10.1140/epjc/s10052-015-3868-9
Regular Article - Experimental Physics
The prototype detection unit of the KM3NeT detector
KM3NeT Collaboration
1
Instituto de Investigación para la Gestión Integrada de las Zonas Costeras, Universitat Politècnica de València, Gandia, Spain
2
Aix Marseille Université CNRS/IN2P3, CPPM UMR 7346, 13288, Marseille, France
3
DIAS, Dublin, Ireland
4
INFN, Sezione di Catania, Catania, Italy
5
GRPHE, Université de Haute Alsace, IUT de Colmar, Colmar, France
6
INFN, Sezione di Roma, Rome, Italy
7
Deparment of Physics, National and Kapodistrian University of Athens, Athens, Greece
8
INFN, Sezione di Genova, Genova, Italy
9
Erlangen Centre for Astroparticle Physics, Friedrich-Alexander-Universität Erlangen-Nürnberg, Erlangen, Germany
10
CEA, Irfu/Sedi, Centre de Saclay, Gif-sur-Yvette, France
11
INFN, Sezione di Napoli, Naples, Italy
12
Institute of Nuclear Physics, NCSR “Demokritos”, Athens, Greece
13
Nikhef, Amsterdam, The Netherlands
14
Dipartimento di Fisica, Università ‘Federico II’, Naples, Italy
15
INFN, Sezione di Bari, Bari, Italy
16
APC,Université Paris Diderot, CNRS/IN2P3 CEA/IRFU, Observatoire de Paris, Sorbonne Paris Cité, 75205, Paris, France
17
KVI-CART, University of Groningen, Groningen, The Netherlands
18
INFN, Sezione di Pisa, Pisa, Italy
19
Dipartimento di Fisica, Università di Pisa, Pisa, Italy
20
INFN, Laboratori Nazionali del Sud, Catania, Italy
21
School of Science and Technology, Hellenic Open University, Patras, Greece
22
Leiden Institute of Physics, Leiden University, Leiden, The Netherlands
23
Dipartimento di Fisica, Università di Roma La Sapienza, Rome, Italy
24
Dipartimento di Fisica, Università di Salerno, Fisciano, Italy
25
Institute of Physics, University of Amsterdam, Amsterdam, The Netherlands
26
IFIC-Instituto de Física Corpuscular, (CSIC-Universitat de València), Valencia, Spain
27
Institute of Space Science, Bucharest, Romania
28
INFN, Sezione di Bologna, Bologna, Italy
29
Dipartimento di Fisica e Astronomia, Università di Bologna, Bologna, Italy
30
Université Paris-Sud, 91405, Orsay Cedex, France
31
University Würzburg, Würzburg, Germany
32
INFN, Laboratori Nazionali di Frascati, Frascati, Italy
33
NIOZ, Texel, The Netherlands
34
Eberhard Karls Universität Tübingen, Tübingen, Germany
35
Utrecht University, Utrecht, The Netherlands
36
Dr. Remeis Sternwarte, Friedrich-Alexander-Universität Erlangen-Nürnberg, Bamberg, Germany
37
Physics Department, University of Cyprus, Nicosia, Cyprus
38
IPHC, CNRS/IN2P3, Strasbourg, France
39
Oceanlab, University of Aberdeen, Aberdeen, UK
40
Dipartimento di Fisica, Università di Genova, Genova, Italy
41
CEA, Irfu/SPP, Centre de Saclay, Gif-sur-Yvette, France
42
Department of Physics and Astronomy, University of Sheffield, Sheffield, UK
* e-mail: simone.biagi@bo.infn.it
Received:
7
October
2015
Accepted:
22
December
2015
Published online:
29
January
2016
A 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 K 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
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© The Author(s), 2016