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<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/1909.04579">arXiv:1909.04579</a> <span> [<a href="https://arxiv.org/pdf/1909.04579">pdf</a>, <a href="https://arxiv.org/format/1909.04579">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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="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> <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/10.1103/PhysRevD.100.062002">10.1103/PhysRevD.100.062002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the varying flux of atmospheric muons measured with the Large Volume Detector for 24 years </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agafonova%2C+N+Y">N. Yu. Agafonova</a>, <a href="/search/physics?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/physics?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/physics?searchtype=author&query=Ashikhmin%2C+V+V">V. V. Ashikhmin</a>, <a href="/search/physics?searchtype=author&query=Bari%2C+G">G. Bari</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Dobrynina%2C+E+A">E. A. Dobrynina</a>, <a href="/search/physics?searchtype=author&query=Enikeev%2C+R+I">R. I. Enikeev</a>, <a href="/search/physics?searchtype=author&query=Fulgione%2C+W">W. Fulgione</a>, <a href="/search/physics?searchtype=author&query=Galeotti%2C+P">P. Galeotti</a>, <a href="/search/physics?searchtype=author&query=Garbini%2C+M">M. Garbini</a>, <a href="/search/physics?searchtype=author&query=Ghia%2C+P+L">P. L. Ghia</a>, <a href="/search/physics?searchtype=author&query=Giusti%2C+P">P. Giusti</a>, <a href="/search/physics?searchtype=author&query=Kemp%2C+E">E. Kemp</a>, <a href="/search/physics?searchtype=author&query=Malgin%2C+A+S">A. S. Malgin</a>, <a href="/search/physics?searchtype=author&query=Molinario%2C+A">A. Molinario</a>, <a href="/search/physics?searchtype=author&query=Persiani%2C+R">R. Persiani</a>, <a href="/search/physics?searchtype=author&query=Pless%2C+I+A">I. A. Pless</a>, <a href="/search/physics?searchtype=author&query=Rubinetti%2C+S">S. Rubinetti</a>, <a href="/search/physics?searchtype=author&query=Ryazhskaya%2C+O+G">O. G. Ryazhskaya</a>, <a href="/search/physics?searchtype=author&query=Sartorelli%2C+G">G. Sartorelli</a>, <a href="/search/physics?searchtype=author&query=Shakiryanova%2C+I+R">I. R. Shakiryanova</a>, <a href="/search/physics?searchtype=author&query=Selvi%2C+M">M. Selvi</a>, <a href="/search/physics?searchtype=author&query=Taricco%2C+C">C. Taricco</a>, <a href="/search/physics?searchtype=author&query=Trinchero%2C+G+C">G. C. Trinchero</a> , et al. (3 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="1909.04579v2-abstract-short" style="display: inline;"> The Large Volume Detector (LVD), hosted in the INFN Laboratori Nazionali del Gran Sasso, is triggered by atmospheric muons at a rate of $\sim 0.1$~Hz. The data collected over almost a quarter of century are used to study the muon intensity underground. The 50-million muon series, the longest ever exploited by an underground instrument, allows for the accurate long-term monitoring of the muon inten… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.04579v2-abstract-full').style.display = 'inline'; document.getElementById('1909.04579v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.04579v2-abstract-full" style="display: none;"> The Large Volume Detector (LVD), hosted in the INFN Laboratori Nazionali del Gran Sasso, is triggered by atmospheric muons at a rate of $\sim 0.1$~Hz. The data collected over almost a quarter of century are used to study the muon intensity underground. The 50-million muon series, the longest ever exploited by an underground instrument, allows for the accurate long-term monitoring of the muon intensity underground. This is relevant as a study of the background in the Gran Sasso Laboratory, which hosts a variety of long-duration, low-background detectors. We describe the procedure to select muon-like events as well as the method used to compute the exposure. We report the value of the average muon flux measured from 1994 to 2017: $\mathrm{I_渭^0 = 3.35 \pm 0.0005^{stat}\pm 0.03^{sys} \cdot 10^{-4} ~m^{-2} s^{-1}}$. We show that the intensity is modulated around this average value due to temperature variations in the stratosphere. We quantify such a correlation by using temperature data from the European Center for Medium-range Weather Forecasts: we find an effective temperature coefficient $\mathrm{伪_{T}} = 0.94\pm0.01^{stat} \pm0.01^{sys}$, in agreement with other measurements at the same depth. We scrutinise the spectral content of the time series of the muon intensity by means of the Lomb-Scargle analysis. This yields the evidence of a 1-year periodicity, as well as the indication of others, both shorter and longer, suggesting that the series is not a pure sinusoidal wave. Consequently, and for the first time, we characterise the observed modulation in terms of amplitude and position of maximum and minimum on a year-by-year basis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.04579v2-abstract-full').style.display = 'none'; document.getElementById('1909.04579v2-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> 11 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </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">26 pages, 10 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1311.6995">arXiv:1311.6995</a> <span> [<a href="https://arxiv.org/pdf/1311.6995">pdf</a>, <a href="https://arxiv.org/ps/1311.6995">ps</a>, <a href="https://arxiv.org/format/1311.6995">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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> <p class="title is-5 mathjax"> Measurement of cosmic muon charge ratio with the Large Volume Detector </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agafonova%2C+N+Y">N. Yu. Agafonova</a>, <a href="/search/physics?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/physics?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/physics?searchtype=author&query=Bari%2C+G">G. Bari</a>, <a href="/search/physics?searchtype=author&query=Bertoni%2C+R">R. Bertoni</a>, <a href="/search/physics?searchtype=author&query=Boyarkin%2C+V+V">V. V. Boyarkin</a>, <a href="/search/physics?searchtype=author&query=Bressan%2C+E">E. Bressan</a>, <a href="/search/physics?searchtype=author&query=Bruno%2C+G">G. Bruno</a>, <a href="/search/physics?searchtype=author&query=Dadykin%2C+V+L">V. L. Dadykin</a>, <a href="/search/physics?searchtype=author&query=Dobrynina%2C+E+A">E. A. Dobrynina</a>, <a href="/search/physics?searchtype=author&query=Enikeev%2C+R+I">R. I. Enikeev</a>, <a href="/search/physics?searchtype=author&query=Fulgione%2C+W">W. Fulgione</a>, <a href="/search/physics?searchtype=author&query=Galeotti%2C+P">P. Galeotti</a>, <a href="/search/physics?searchtype=author&query=Garbini%2C+M">M. Garbini</a>, <a href="/search/physics?searchtype=author&query=Ghia%2C+P+L">P. L. Ghia</a>, <a href="/search/physics?searchtype=author&query=Giusti%2C+P">P. Giusti</a>, <a href="/search/physics?searchtype=author&query=Kemp%2C+E">E. Kemp</a>, <a href="/search/physics?searchtype=author&query=Malgin%2C+A+S">A. S. Malgin</a>, <a href="/search/physics?searchtype=author&query=Miguez%2C+B">B. Miguez</a>, <a href="/search/physics?searchtype=author&query=Molinario%2C+A">A. Molinario</a>, <a href="/search/physics?searchtype=author&query=Persiani%2C+R">R. Persiani</a>, <a href="/search/physics?searchtype=author&query=Pless%2C+I+A">I. A. Pless</a>, <a href="/search/physics?searchtype=author&query=Ryasny%2C+V+G">V. G. Ryasny</a>, <a href="/search/physics?searchtype=author&query=Ryazhskaya%2C+O+G">O. G. Ryazhskaya</a>, <a href="/search/physics?searchtype=author&query=Saavedra%2C+O">O. Saavedra</a> , et al. (6 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="1311.6995v5-abstract-short" style="display: inline;"> The charge ratio ${k \equiv 渭^+/渭^-}$ for atmospheric muons has been measured using Large Volume Detector (LVD) in the INFN Gran Sasso National Laboratory, Italy (minimal depth is 3000 m w.e.). To reach this depth muons should have the energy at the sea level greater than 1.3 TeV. The muon charge ratio was defined using the number of the decays of stopping positive muons in the LVD iron structure… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.6995v5-abstract-full').style.display = 'inline'; document.getElementById('1311.6995v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1311.6995v5-abstract-full" style="display: none;"> The charge ratio ${k \equiv 渭^+/渭^-}$ for atmospheric muons has been measured using Large Volume Detector (LVD) in the INFN Gran Sasso National Laboratory, Italy (minimal depth is 3000 m w.e.). To reach this depth muons should have the energy at the sea level greater than 1.3 TeV. The muon charge ratio was defined using the number of the decays of stopping positive muons in the LVD iron structure and the decays of positive and negative muons in scintillator. We have obtained the value of the muon charge ratio ${k}$ ${= 1.26 \pm 0.04(stat) \pm 0.11(sys)}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1311.6995v5-abstract-full').style.display = 'none'; document.getElementById('1311.6995v5-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> 14 February, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 November, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2013. </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">16 pages, 7 figures, 1 table. Version submitted for publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1206.2488">arXiv:1206.2488</a> <span> [<a href="https://arxiv.org/pdf/1206.2488">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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> <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"> Determination of a time-shift in the OPERA set-up using high energy horizontal muons in the LVD and OPERA detectors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/physics?searchtype=author&query=Agafonova%2C+N+Y">N. Yu. Agafonova</a>, <a href="/search/physics?searchtype=author&query=Antonioli%2C+P">P. Antonioli</a>, <a href="/search/physics?searchtype=author&query=Ashikhmin%2C+V+V">V. V. Ashikhmin</a>, <a href="/search/physics?searchtype=author&query=Bari%2C+G">G. Bari</a>, <a href="/search/physics?searchtype=author&query=Bressan%2C+E">E. Bressan</a>, <a href="/search/physics?searchtype=author&query=Evans%2C+L">L. Evans</a>, <a href="/search/physics?searchtype=author&query=Garbini%2C+M">M. Garbini</a>, <a href="/search/physics?searchtype=author&query=Giusti%2C+P">P. Giusti</a>, <a href="/search/physics?searchtype=author&query=Malguin%2C+A+S">A. S. Malguin</a>, <a href="/search/physics?searchtype=author&query=Persiani%2C+R">R. Persiani</a>, <a href="/search/physics?searchtype=author&query=Ryasny%2C+V+G">V. G. Ryasny</a>, <a href="/search/physics?searchtype=author&query=Ryazhskaya%2C+O+G">O. G. Ryazhskaya</a>, <a href="/search/physics?searchtype=author&query=Sartorelli%2C+G">G. Sartorelli</a>, <a href="/search/physics?searchtype=author&query=Scapparone%2C+E">E. Scapparone</a>, <a href="/search/physics?searchtype=author&query=Selvi%2C+M">M. Selvi</a>, <a href="/search/physics?searchtype=author&query=Shakirianova%2C+I+R">I. R. Shakirianova</a>, <a href="/search/physics?searchtype=author&query=Votano%2C+L">L. Votano</a>, <a href="/search/physics?searchtype=author&query=Wenninger%2C+H">H. Wenninger</a>, <a href="/search/physics?searchtype=author&query=Yakushev%2C+V+F">V. F. Yakushev</a>, <a href="/search/physics?searchtype=author&query=Zichichi%2C+A">A. Zichichi</a>, <a href="/search/physics?searchtype=author&query=Agafonova%2C+N">N. Agafonova</a>, <a href="/search/physics?searchtype=author&query=Alexandrov%2C+A">A. Alexandrov</a>, <a href="/search/physics?searchtype=author&query=Bertolin%2C+A">A. Bertolin</a>, <a href="/search/physics?searchtype=author&query=Brugnera%2C+R">R. Brugnera</a>, <a href="/search/physics?searchtype=author&query=Buttner%2C+B">B. Buttner</a> , et al. (66 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="1206.2488v1-abstract-short" style="display: inline;"> The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a totally independent way from Time Of Flight (TOF) measurements of CNGS neutrino events. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ~ 160 m, allows the use of very high energy horizontal muo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.2488v1-abstract-full').style.display = 'inline'; document.getElementById('1206.2488v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1206.2488v1-abstract-full" style="display: none;"> The purpose of this work is to report the measurement of a time-shift in the OPERA set-up in a totally independent way from Time Of Flight (TOF) measurements of CNGS neutrino events. The LVD and OPERA experiments are both installed in the same laboratory: LNGS. The relative position of the two detectors, separated by an average distance of ~ 160 m, allows the use of very high energy horizontal muons to cross-calibrate the timing systems of the two detectors, using a TOF technique which is totally independent from TOF of CNGS neutrino events. Indeed, the OPERA-LVD direction lies along the so-called "Teramo anomaly", a region in the Gran Sasso massif where LVD has established, many years ago, the existence of an anomaly in the mountain structure, which exhibits a low m. w. e. thickness for horizontal directions. The "abundant" high-energy horizontal muons (nearly 100 per year) going through LVD and OPERA exist because of this anomaly in the mountain orography. The total live time of the data in coincidence correspond to 1200 days from mid 2007 until March 2012. The time coincidence study of LVD and OPERA detectors is based on 306 cosmic horizontal muon events and shows the existence of a negative time shift in the OPERA set-up of the order of deltaT(AB) = - (73 \pm 9) ns when two calendar periods, A and B, are compared. This result shows a systematic effect in the OPERA timing system from August 2008 until December 2011. The size of the effect is comparable with the neutrino velocity excess recently measured by OPERA. It is probably interesting not to forget that with the MRPC technology developed by the ALICE Bologna group the TOF world record accuracy of 20 ps was reached. That technology can be implemented at LNGS for a high precision determination of TOF with the CNGS neutrino beams of an order of magnitude smaller than the value of the OPERA systematic effect. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1206.2488v1-abstract-full').style.display = 'none'; document.getElementById('1206.2488v1-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> 12 June, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2012. </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> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div 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