The positioning system of the ANTARES Neutrino Telescope

Adrián-Martínez, S.; Ageron, M.; Aguilar, J. A.; Samarai, I. Al; Albert, A.; André, M.; Anghinolfi, M.; Anton, G.; Anvar, S.; Ardid, M.; Jesus, A.C. Assis; Astraatmadja, T.; Aubert, J.J.; Baret, B.; Basa, S.; Bertín, V.; Biagi, S.; Bigi, A.; Bigongiari, C.; Bogazzi, C.; Bou-Cabo, M.; Bouhou, B.; Bouwhuis, M. C.; Brünner, J.; Busto, J.; Camarena, F.; Capone, A.; Cârloganu, C.; Carminati, G.; Carr, J.; Cecchini, S.; Charif, Z.; Charvis, Philippe; Chiarusi, T.; Circella, M.; Coniglione, R.; Costantini, H.; Coyle, P.; Curtil, C.; Bonis, G. De; Decowski, M. P.; Dekeyser, I.; Deschamps, A.; Distefano, C.; Donzaud, C.; Dornic, D.; Dorosti, Q.; Drouhin, D.; Eberl, T.; Emanuele, U.; Enzenhöfer, A.; Ernenwein, Jean-Pierre; Escoffier, S.; Fermani, P.; Ferri, M.; Flaminio, V.; Folger, F.; Fritsch, U.; Fuda, J.-L.; Galatà, S.; Giacomelli, G.; Giordano, V.; Gómez-González, J.; Graf, Κ.; Guillard, G.; Halladjian, G.; Hallewell, G. D.; Haren, Hans van; Hartman, J.; Heijboer, A.; Hello, Y.; Hernández-Rey, J. J.; Herold, B.; Hößl, J.; Hsu, C. C.; Jong, M. de; Kadler, M.; Kalekin, O.; Kappes, A.; Katz, U.; Kavatsyuk, O.; Keller, P.; Kooijman, P.; Kopper, C.; Kouchner, A.; Kreykenbohm, I.; Kulikovskiy, V.; Lahmann, R.; Lamare, P.; Larosa, G.; Lattuada, D.; Lefèvre, D.; Suu, A. Le van; Lim, G.; Presti, D. Lo; Loehner, H.; Loucatos, S.; Mangano, S.; Marcelin, M.; Margiotta, A.; Martínez-Mora, J. A.; Meli, A.; Montaruli, T.; Moscoso, L.; Motz, H.; Neff, M.; Nezri, E.; Niess, V.; Palioselitis, D.; Păvălaş, G. E.; Payet, K.; Payre, P.; Petrović, J.; Piattelli, P.; Picot-Clémente, N.; Popa, V.; Pradier, T.; Presani, E.; Racca, C.; Real, D.; Reed, C. M.; Riccobene, G.; Richardt, C.; Richter, R.; Rivière, C.; Robert, Aymeric; Roensch, K.; Rostovtsev, A.; Ruiz-Rivas, J.; Rujoiu, M.; Russo, G.; Salesa, F.; Samtleben, D. F. E.; Schöck, F. M.; Schuller, J. P.; Schüßler, F.; Seitz, T.; Shanidze, R.; Simeone, F.; Spies, A.; Spurio, M.; Steijger, J. J. M.; Stolarczyk, Th.; Sánchez-Losa, A.; Taiuti, M.; Tamburini, Christian; Toscano, S.; Vallage, B.; Elewyck, V. Van; Vannoni, G.; Vecchi, M.; Vernin, P.; Wagner, S. J.; Wijnker, G.; Wilms, J.; Wolf, E. de; Yepes, H.; Zaborov, D.; Zornoza, J.D.; Zúñiga, J.

doi:10.1088/1748-0221/7/08/t08002

Cited by 75 publications

(57 citation statements)

References 12 publications

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“…The search was performed with the most recent official offline data set, produced incorporating dedicated calibrations, in terms of positioning [40], timing [41] and efficiency [27]. This sample is dominated by background events from misreconstructed down-going atmospheric muons.…”

Section: Discussionmentioning

confidence: 99%

Search for high-energy neutrinos from gravitational wave event GW151226 and candidate LVT151012 with ANTARES and IceCube

Albert¹,

André²,

Anghinolfi³

et al. 2017

Phys. Rev. D

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The Advanced LIGO observatories detected gravitational waves from two binary black hole mergers during their first observation run (O1). We present a high-energy neutrino follow-up search for the second gravitational wave event, GW151226, as well as for gravitational wave candidate LVT151012. We find two and four neutrino candidates detected by IceCube, and one and zero detected by ANTARES, within AE500 s around the respective gravitational wave signals, consistent with the expected background rate. None of these neutrino candidates are found to be directionally coincident with GW151226 or LVT151012. We use nondetection to constrain isotropic-equivalent high-energy neutrino emission from GW151226, adopting the GW event's 3D localization, to less than 2 × 10 51 -2 × 10 54 erg.

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Section: Discussionmentioning

confidence: 99%

Search for high-energy neutrinos from gravitational wave event GW151226 and candidate LVT151012 with ANTARES and IceCube

Albert¹,

André²,

Anghinolfi³

et al. 2017

Phys. Rev. D

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“…The top of the string consists of a buoy and they are anchored on the sea bed. The absolute position of the detector components as a function of time is obtained through an acoustic triangulation system combined with an orientation system that permits to determine the inclination and orientation of the single storeys [11]. The absolute UTC time accuracy is guaranteed by a GPS system and by the 25 MHz clock of the detector.…”

Section: The Antares Detectormentioning

confidence: 99%

Indirect Dark Matter search with the ANTARES Deep-Sea Cherenkov detector

Fermani

2014

EPJ Web of Conferences

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Abstract. In 2008 the ANTARES collaboration completed the construction of an underwater neutrino telescope in the Mediterranean Sea, located 40 km off the French coast at a depth of 2475 m. With an effective area for upward muon detection of about 0.05 km 2 , depending on neutrino energy, ANTARES is the largest neutrino detector currently operating in the Northern hemisphere. The experiment aims to detect high-energy neutrinos up to 10 4 TeV using a 3-dimensional array of 885 photomultipliers distributed in 25 storeys along 12 vertical lines. The detection is based on the measurement of Cherenkov light emitted by charged leptons resulting from charged-current neutrino interactions in the matter surrounding the telescope. The accurate measurements of the photon arrival times and of the deposited charge together with a precise knowledge of the actual positions and orientations of the photo sensors allow the reconstruction of the direction of neutrinos with good angular resolution (about 0.3˚for muon neutrinos above a few TeV) and of their energy. ANTARES is performing an indirect search for dark matter by looking for a statistical excess of neutrinos coming from astrophysical massive objects, such as the Sun, the Earth and the Galactic Centre. This excess could be an evidence of the possible annihilation of dark matter particles in the centre of these objects. In the most accepted scenario, the dark matter is composed by WIMP particles. These particles can be scattered by the nuclei of these astrophysical bodies and get gravitationally trapped, accumulating in their inner core. Here they can interact with other WIMPs, in self-annihilation reactions, producing some standard model particles that, in subsequent steps, originate neutrinos that can be detected at Earth. The preliminary results of the sensitivity of the ANTARES neutrino telescope to the indirect detection of dark matter fluxes will be presented for different dark matter models.

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“…This transceiver can be used either as emitter or as receiver as it is not equipped with a preamplifier. This sensor type is studied at IGIC-UPV 6 . It is planned to use this devices as emitters for the KM3NeT acoustic positioning system.…”

Section: Sensor Typesmentioning

confidence: 99%

“…It is not necessary to equip each optical sensor with an acoustic receiver as it is possible to interpolate the sensor positions between two distant acoustic receivers using a model of the shape of the DU, cf. the positioning system in ANTARES [6]. It is possible to use either complete commercial systems or to combine different emitters and receivers to a dedicated system.…”

Section: Introductionmentioning

confidence: 99%

Acoustic calibration for the KM3NeT pre-production module

Enzenhöfer

2013

Nuclear Instruments and Methods in Physics Research Section A:

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The proposed large scale Cherenkov neutrino telescope KM3NeT will carry photo-sensors on flexible structures, the detection units. The Mediterranean Sea, where KM3NeT will be installed, constitutes a highly dynamic environment in which the detection units are constantly in motion. Thus it is necessary to monitor the exact sensor positions continuously to achieve the desired resolution for the neutrino telescope. A common way to perform this monitoring is the use of acoustic positioning systems with emitters and receivers based on the piezoelectric effect. The acoustic receivers are attached to detection units whereas the emitters are located at known positions on the sea floor. There are complete commercial systems for this application with sufficient precision. But these systems are limited in the use of their data and inefficient as they were designed to perform only this single task. Several working groups in the KM3NeT consortium are cooperating to custom-design a positioning system for the specific requirements of KM3NeT. Most of the studied solutions hold the possibility to extend the application area from positioning to additional tasks like acoustic particle detection or monitoring of the deep-sea acoustic environment. The KM3NeT Pre-Production Module (PPM) is a test system to verify the correct operation and interoperability of the major involved hardware and software components developed for KM3NeT. In the context of the PPM, alternative designs of acoustic sensors including small piezoelectric elements equipped with preamplifiers inside the same housing as the optical sensors will be tested. These will be described in this article.

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The positioning system of the ANTARES Neutrino Telescope

Cited by 75 publications

References 12 publications

Search for high-energy neutrinos from gravitational wave event GW151226 and candidate LVT151012 with ANTARES and IceCube

Search for high-energy neutrinos from gravitational wave event GW151226 and candidate LVT151012 with ANTARES and IceCube

Indirect Dark Matter search with the ANTARES Deep-Sea Cherenkov detector

Acoustic calibration for the KM3NeT pre-production module

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