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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.03649">arXiv:1708.03649</a> <span> [<a href="https://arxiv.org/pdf/1708.03649">pdf</a>, <a href="https://arxiv.org/ps/1708.03649">ps</a>, <a href="https://arxiv.org/format/1708.03649">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> An algorithm for the reconstruction of neutrino-induced showers in the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/physics?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/physics?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/physics?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/physics?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/physics?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/physics?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/physics?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/physics?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/physics?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/physics?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/physics?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/physics?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/physics?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/physics?searchtype=author&query=Bourret%2C+S">S. Bourret</a>, <a href="/search/physics?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/physics?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/physics?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/physics?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/physics?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/physics?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/physics?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/physics?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/physics?searchtype=author&query=Celli%2C+S">S. Celli</a>, <a href="/search/physics?searchtype=author&query=Moursli%2C+R+C+E">R. Cherkaoui El Moursli</a> , et al. (102 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1708.03649v2-abstract-short" style="display: inline;"> Muons created by $谓_渭$ charged current (CC) interactions in the water surrounding the ANTARES neutrino telescope have been almost exclusively used so far in searches for cosmic neutrino sources. Due to their long range, highly energetic muons inducing Cherenkov radiation in the water are reconstructed with dedicated algorithms that allow the determination of the parent neutrino direction with a me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.03649v2-abstract-full').style.display = 'inline'; document.getElementById('1708.03649v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.03649v2-abstract-full" style="display: none;"> Muons created by $谓_渭$ charged current (CC) interactions in the water surrounding the ANTARES neutrino telescope have been almost exclusively used so far in searches for cosmic neutrino sources. Due to their long range, highly energetic muons inducing Cherenkov radiation in the water are reconstructed with dedicated algorithms that allow the determination of the parent neutrino direction with a median angular resolution of about \unit{0.4}{\degree} for an $E^{-2}$ neutrino spectrum. In this paper, an algorithm optimised for accurate reconstruction of energy and direction of shower events in the ANTARES detector is presented. Hadronic showers of electrically charged particles are produced by the disintegration of the nucleus both in CC and neutral current (NC) interactions of neutrinos in water. In addition, electromagnetic showers result from the CC interactions of electron neutrinos while the decay of a tau lepton produced in $谓_蟿$ CC interactions will in most cases lead to either a hadronic or an electromagnetic shower. A shower can be approximated as a point source of photons. With the presented method, the shower position is reconstructed with a precision of about \unit{1}{\metre}, the neutrino direction is reconstructed with a median angular resolution between \unit{2}{\degree} and \unit{3}{\degree} in the energy range of \SIrange{1}{1000}{TeV}. In this energy interval, the uncertainty on the reconstructed neutrino energy is about \SIrange{5}{10}{\%}. The increase in the detector sensitivity due to the use of additional information from shower events in the searches for a cosmic neutrino flux is also presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.03649v2-abstract-full').style.display = 'none'; document.getElementById('1708.03649v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2017. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1612.05621">arXiv:1612.05621</a> <span> [<a href="https://arxiv.org/pdf/1612.05621">pdf</a>, <a href="https://arxiv.org/format/1612.05621">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/JHEP05(2017)008">10.1007/JHEP05(2017)008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Intrinsic limits on resolutions in muon- and electron-neutrino charged-current events in the KM3NeT/ORCA detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/physics?searchtype=author&query=Ageron%2C+M">M. Ageron</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/physics?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/physics?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/physics?searchtype=author&query=Anassontzis%2C+E+G">E. G. Anassontzis</a>, <a href="/search/physics?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/physics?searchtype=author&query=Androulakis%2C+G">G. Androulakis</a>, <a href="/search/physics?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/physics?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/physics?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/physics?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G">G. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Barbarito%2C+E">E. Barbarito</a>, <a href="/search/physics?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/physics?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/physics?searchtype=author&query=Belias%2C+A">A. Belias</a>, <a href="/search/physics?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/physics?searchtype=author&query=Berg%2C+A+v+d">A. van den Berg</a>, <a href="/search/physics?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/physics?searchtype=author&query=Beurthey%2C+S">S. Beurthey</a>, <a href="/search/physics?searchtype=author&query=van+Beveren%2C+V">V. van Beveren</a>, <a href="/search/physics?searchtype=author&query=Beverini%2C+N">N. Beverini</a>, <a href="/search/physics?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/physics?searchtype=author&query=Biagioni%2C+A">A. Biagioni</a> , et al. (228 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1612.05621v2-abstract-short" style="display: inline;"> Studying atmospheric neutrino oscillations in the few-GeV range with a multimegaton detector promises to determine the neutrino mass hierarchy. This is the main science goal pursued by the future KM3NeT/ORCA water Cherenkov detector in the Mediterranean Sea. In this paper, the processes that limit the obtainable resolution in both energy and direction in charged-current neutrino events in the ORCA… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.05621v2-abstract-full').style.display = 'inline'; document.getElementById('1612.05621v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.05621v2-abstract-full" style="display: none;"> Studying atmospheric neutrino oscillations in the few-GeV range with a multimegaton detector promises to determine the neutrino mass hierarchy. This is the main science goal pursued by the future KM3NeT/ORCA water Cherenkov detector in the Mediterranean Sea. In this paper, the processes that limit the obtainable resolution in both energy and direction in charged-current neutrino events in the ORCA detector are investigated. These processes include the composition of the hadronic fragmentation products, the subsequent particle propagation and the photon-sampling fraction of the detector. GEANT simulations of neutrino interactions in seawater produced by GENIE are used to study the effects in the 1 - 20 GeV range. It is found that fluctuations in the hadronic cascade in conjunction with the variation of the inelasticity y are most detrimental to the resolutions. The effect of limited photon sampling in the detector is of significantly less importance. These results will therefore also be applicable to similar detectors/media, such as those in ice. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.05621v2-abstract-full').style.display = 'none'; document.getElementById('1612.05621v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 May, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 28 figures, JHEP published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The KM3NeT collaboration, Adri{谩}n-Mart{\'谋}nez, S., Ageron, M. et al. J. High Energ. Phys. (2017) 2017: 8 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1601.07459">arXiv:1601.07459</a> <span> [<a href="https://arxiv.org/pdf/1601.07459">pdf</a>, <a href="https://arxiv.org/format/1601.07459">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/0954-3899/43/8/084001">10.1088/0954-3899/43/8/084001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Letter of Intent for KM3NeT 2.0 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/physics?searchtype=author&query=Ageron%2C+M">M. Ageron</a>, <a href="/search/physics?searchtype=author&query=Aharonian%2C+F">F. Aharonian</a>, <a href="/search/physics?searchtype=author&query=Aiello%2C+S">S. Aiello</a>, <a href="/search/physics?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/physics?searchtype=author&query=Ameli%2C+F">F. Ameli</a>, <a href="/search/physics?searchtype=author&query=Anassontzis%2C+E">E. Anassontzis</a>, <a href="/search/physics?searchtype=author&query=Andre%2C+M">M. Andre</a>, <a href="/search/physics?searchtype=author&query=Androulakis%2C+G">G. Androulakis</a>, <a href="/search/physics?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/physics?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/physics?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/physics?searchtype=author&query=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/physics?searchtype=author&query=Barbarino%2C+G">G. Barbarino</a>, <a href="/search/physics?searchtype=author&query=Barbarito%2C+E">E. Barbarito</a>, <a href="/search/physics?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/physics?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/physics?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/physics?searchtype=author&query=Belias%2C+A">A. Belias</a>, <a href="/search/physics?searchtype=author&query=Berbee%2C+E">E. Berbee</a>, <a href="/search/physics?searchtype=author&query=Berg%2C+A+v+d">A. van den Berg</a>, <a href="/search/physics?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/physics?searchtype=author&query=Beurthey%2C+S">S. Beurthey</a>, <a href="/search/physics?searchtype=author&query=van+Beveren%2C+V">V. van Beveren</a>, <a href="/search/physics?searchtype=author&query=Beverini%2C+N">N. Beverini</a> , et al. (222 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1601.07459v2-abstract-short" style="display: inline;"> The main objectives of the KM3NeT Collaboration are i) the discovery and subsequent observation of high-energy neutrino sources in the Universe and ii) the determination of the mass hierarchy of neutrinos. These objectives are strongly motivated by two recent important discoveries, namely: 1) The high-energy astrophysical neutrino signal reported by IceCube and 2) the sizable contribution of elect… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.07459v2-abstract-full').style.display = 'inline'; document.getElementById('1601.07459v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1601.07459v2-abstract-full" style="display: none;"> The main objectives of the KM3NeT Collaboration are i) the discovery and subsequent observation of high-energy neutrino sources in the Universe and ii) the determination of the mass hierarchy of neutrinos. These objectives are strongly motivated by two recent important discoveries, namely: 1) The high-energy astrophysical neutrino signal reported by IceCube and 2) the sizable contribution of electron neutrinos to the third neutrino mass eigenstate as reported by Daya Bay, Reno and others. To meet these objectives, the KM3NeT Collaboration plans to build a new Research Infrastructure consisting of a network of deep-sea neutrino telescopes in the Mediterranean Sea. A phased and distributed implementation is pursued which maximises the access to regional funds, the availability of human resources and the synergetic opportunities for the earth and sea sciences community. Three suitable deep-sea sites are identified, namely off-shore Toulon (France), Capo Passero (Italy) and Pylos (Greece). The infrastructure will consist of three so-called building blocks. A building block comprises 115 strings, each string comprises 18 optical modules and each optical module comprises 31 photo-multiplier tubes. Each building block thus constitutes a 3-dimensional array of photo sensors that can be used to detect the Cherenkov light produced by relativistic particles emerging from neutrino interactions. Two building blocks will be configured to fully explore the IceCube signal with different methodology, improved resolution and complementary field of view, including the Galactic plane. One building block will be configured to precisely measure atmospheric neutrino oscillations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1601.07459v2-abstract-full').style.display = 'none'; document.getElementById('1601.07459v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">119 pages, published version, revised Eq. 6, 7</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Physics G: Nuclear and Particle Physics, 43 (8), 084001, 2016 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1507.04182">arXiv:1507.04182</a> <span> [<a href="https://arxiv.org/pdf/1507.04182">pdf</a>, <a href="https://arxiv.org/ps/1507.04182">ps</a>, <a href="https://arxiv.org/format/1507.04182">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2016.02.001">10.1016/j.astropartphys.2016.02.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Time calibration with atmospheric muon tracks in the ANTARES neutrino telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Adri%C3%A1n-Mart%C3%ADnez%2C+S">S. Adri谩n-Mart铆nez</a>, <a href="/search/physics?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/physics?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/physics?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/physics?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/physics?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/physics?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/physics?searchtype=author&query=Barrios-Mart%C3%AD%2C+J">J. Barrios-Mart铆</a>, <a href="/search/physics?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/physics?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/physics?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/physics?searchtype=author&query=Bogazzi%2C+C">C. Bogazzi</a>, <a href="/search/physics?searchtype=author&query=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/physics?searchtype=author&query=Bou-Cabo%2C+M">M. Bou-Cabo</a>, <a href="/search/physics?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/physics?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/physics?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/physics?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/physics?searchtype=author&query=Capone%2C+A">A. Capone</a>, <a href="/search/physics?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/physics?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/physics?searchtype=author&query=Chiarusi%2C+T">T. Chiarusi</a>, <a href="/search/physics?searchtype=author&query=Circella%2C+M">M. Circella</a>, <a href="/search/physics?searchtype=author&query=Coniglione%2C+R">R. Coniglione</a>, <a href="/search/physics?searchtype=author&query=Costantini%2C+H">H. Costantini</a> , et al. (105 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1507.04182v1-abstract-short" style="display: inline;"> The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of $\sim$10 TeV the muon and the incident neutrino are almost c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.04182v1-abstract-full').style.display = 'inline'; document.getElementById('1507.04182v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1507.04182v1-abstract-full" style="display: none;"> The ANTARES experiment consists of an array of photomultipliers distributed along 12 lines and located deep underwater in the Mediterranean Sea. It searches for astrophysical neutrinos collecting the Cherenkov light induced by the charged particles, mainly muons, produced in neutrino interactions around the detector. Since at energies of $\sim$10 TeV the muon and the incident neutrino are almost collinear, it is possible to use the ANTARES detector as a neutrino telescope and identify a source of neutrinos in the sky starting from a precise reconstruction of the muon trajectory. To get this result, the arrival times of the Cherenkov photons must be accurately measured. A to perform time calibrations with the precision required to have optimal performances of the instrument is described. The reconstructed tracks of the atmospheric muons in the ANTARES detector are used to determine the relative time offsets between photomultipliers. Currently, this method is used to obtain the time calibration constants for photomultipliers on different lines at a precision level of 0.5 ns. It has also been validated for calibrating photomultipliers on the same line, using a system of LEDs and laser light devices. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1507.04182v1-abstract-full').style.display = 'none'; document.getElementById('1507.04182v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 July, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to Astroparticle Physics (17 pages, 11 figures)</span> </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> 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