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breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Allard%2C+D&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Allard%2C+D&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Allard%2C+D&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <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/2406.13673">arXiv:2406.13673</a> <span> [<a href="https://arxiv.org/pdf/2406.13673">pdf</a>, <a href="https://arxiv.org/format/2406.13673">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> </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.2024.103046">10.1016/j.astropartphys.2024.103046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The EUSO-SPB2 Fluorescence Telescope for the Detection of Ultra-High Energy Cosmic Rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Adams%2C+J+H">James H. Adams Jr.</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Alldredge%2C+P">Phillip Alldredge</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">Luis Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">Anna Anzalone</a>, <a href="/search/?searchtype=author&query=Battisti%2C+M">Matteo Battisti</a>, <a href="/search/?searchtype=author&query=Belov%2C+A+A">Alexander A. Belov</a>, <a href="/search/?searchtype=author&query=Bertaina%2C+M">Mario Bertaina</a>, <a href="/search/?searchtype=author&query=Bertone%2C+P+F">Peter F. Bertone</a>, <a href="/search/?searchtype=author&query=Blin-Bondil%2C+S">Sylvie Blin-Bondil</a>, <a href="/search/?searchtype=author&query=Burton%2C+J">Julia Burton</a>, <a href="/search/?searchtype=author&query=Cafagna%2C+F+S">Francesco S. Cafagna</a>, <a href="/search/?searchtype=author&query=Casolino%2C+M">Marco Casolino</a>, <a href="/search/?searchtype=author&query=%C4%8Cern%C3%BD%2C+K">Karel 膶ern媒</a>, <a href="/search/?searchtype=author&query=Christ%2C+M+J">Mark J. Christ</a>, <a href="/search/?searchtype=author&query=Colalillo%2C+R">Roberta Colalillo</a>, <a href="/search/?searchtype=author&query=Crawford%2C+H+J">Hank J. Crawford</a>, <a href="/search/?searchtype=author&query=Creusot%2C+A">Alexandre Creusot</a>, <a href="/search/?searchtype=author&query=Cummings%2C+A">Austin Cummings</a>, <a href="/search/?searchtype=author&query=Diesing%2C+R">Rebecca Diesing</a>, <a href="/search/?searchtype=author&query=Di+Nola%2C+A">Alessandro Di Nola</a>, <a href="/search/?searchtype=author&query=Ebisuzaki%2C+T">Toshikazu Ebisuzaki</a>, <a href="/search/?searchtype=author&query=Eser%2C+J">Johannes Eser</a>, <a href="/search/?searchtype=author&query=Ferrarese%2C+S">Silvia Ferrarese</a>, <a href="/search/?searchtype=author&query=Filippatos%2C+G">George Filippatos</a> , et al. (57 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="2406.13673v2-abstract-short" style="display: inline;"> The Extreme Universe Space Observatory on a Super Pressure Balloon 2 (EUSO-SPB2) flew on May 13$^{\text{th}}$ and 14$^{\text{th}}$ of 2023. Consisting of two novel optical telescopes, the payload utilized next-generation instrumentation for the observations of extensive air showers from near space. One instrument, the fluorescence telescope (FT) searched for Ultra-High Energy Cosmic Rays (UHECRs)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.13673v2-abstract-full').style.display = 'inline'; document.getElementById('2406.13673v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.13673v2-abstract-full" style="display: none;"> The Extreme Universe Space Observatory on a Super Pressure Balloon 2 (EUSO-SPB2) flew on May 13$^{\text{th}}$ and 14$^{\text{th}}$ of 2023. Consisting of two novel optical telescopes, the payload utilized next-generation instrumentation for the observations of extensive air showers from near space. One instrument, the fluorescence telescope (FT) searched for Ultra-High Energy Cosmic Rays (UHECRs) by recording the atmosphere below the balloon in the near-UV with a 1~$渭$s time resolution using 108 multi-anode photomultiplier tubes with a total of 6,912 channels. Validated by pre-flight measurements during a field campaign, the energy threshold was estimated around 2~EeV with an expected event rate of approximately 1 event per 10 hours of observation. Based on the limited time afloat, the expected number of UHECR observations throughout the flight is between 0 and 2. Consistent with this expectation, no UHECR candidate events have been found. The majority of events appear to be detector artifacts that were not rejected properly due to a shortened commissioning phase. Despite the earlier-than-expected termination of the flight, data were recorded which provide insights into the detectors stability in the near-space environment as well as the diffuse ultraviolet emissivity of the atmosphere, both of which are impactful to future experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.13673v2-abstract-full').style.display = 'none'; document.getElementById('2406.13673v2-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> 20 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astroparticle Physics 165 (2025) 103046 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.06525">arXiv:2401.06525</a> <span> [<a href="https://arxiv.org/pdf/2401.06525">pdf</a>, <a href="https://arxiv.org/format/2401.06525">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> </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.2023.102891">10.1016/j.astropartphys.2023.102891 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> EUSO-SPB1 Mission and Science </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+J">JEM-EUSO Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Abdellaoui%2C+G">G. Abdellaoui</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Adams.%2C+J+H">J. H. Adams. Jr.</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Alonso%2C+G">G. Alonso</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Attallah%2C+R">R. Attallah</a>, <a href="/search/?searchtype=author&query=Attoui%2C+H">H. Attoui</a>, <a href="/search/?searchtype=author&query=Pernas%2C+M+A">M. Ave Pernas</a>, <a href="/search/?searchtype=author&query=Bachmann%2C+R">R. Bachmann</a>, <a href="/search/?searchtype=author&query=Bacholle%2C+S">S. Bacholle</a>, <a href="/search/?searchtype=author&query=Bagheri%2C+M">M. Bagheri</a>, <a href="/search/?searchtype=author&query=Bakiri%2C+M">M. Bakiri</a>, <a href="/search/?searchtype=author&query=Bal%C3%A1z%2C+J">J. Bal谩z</a>, <a href="/search/?searchtype=author&query=Barghini%2C+D">D. Barghini</a>, <a href="/search/?searchtype=author&query=Bartocci%2C+S">S. Bartocci</a>, <a href="/search/?searchtype=author&query=Battisti%2C+M">M. Battisti</a>, <a href="/search/?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/?searchtype=author&query=Beldjilali%2C+B">B. Beldjilali</a>, <a href="/search/?searchtype=author&query=Belenguer%2C+T">T. Belenguer</a> , et al. (271 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="2401.06525v1-abstract-short" style="display: inline;"> The Extreme Universe Space Observatory on a Super Pressure Balloon 1 (EUSO-SPB1) was launched in 2017 April from Wanaka, New Zealand. The plan of this mission of opportunity on a NASA super pressure balloon test flight was to circle the southern hemisphere. The primary scientific goal was to make the first observations of ultra-high-energy cosmic-ray extensive air showers (EASs) by looking down on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.06525v1-abstract-full').style.display = 'inline'; document.getElementById('2401.06525v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.06525v1-abstract-full" style="display: none;"> The Extreme Universe Space Observatory on a Super Pressure Balloon 1 (EUSO-SPB1) was launched in 2017 April from Wanaka, New Zealand. The plan of this mission of opportunity on a NASA super pressure balloon test flight was to circle the southern hemisphere. The primary scientific goal was to make the first observations of ultra-high-energy cosmic-ray extensive air showers (EASs) by looking down on the atmosphere with an ultraviolet (UV) fluorescence telescope from suborbital altitude (33~km). After 12~days and 4~hours aloft, the flight was terminated prematurely in the Pacific Ocean. Before the flight, the instrument was tested extensively in the West Desert of Utah, USA, with UV point sources and lasers. The test results indicated that the instrument had sensitivity to EASs of approximately 3 EeV. Simulations of the telescope system, telescope on time, and realized flight trajectory predicted an observation of about 1 event assuming clear sky conditions. The effects of high clouds were estimated to reduce this value by approximately a factor of 2. A manual search and a machine-learning-based search did not find any EAS signals in these data. Here we review the EUSO-SPB1 instrument and flight and the EAS search. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.06525v1-abstract-full').style.display = 'none'; document.getElementById('2401.06525v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </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">18 pages, 19 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart Phys 154 (2024) 102891 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.08204">arXiv:2312.08204</a> <span>  </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> </div> </div> <p class="title is-5 mathjax"> JEM-EUSO Collaboration contributions to the 38th International Cosmic Ray Conference </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Adams%2C+J+H">J. H. Adams Jr.</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Alldredge%2C+P">P. Alldredge</a>, <a href="/search/?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/?searchtype=author&query=Bagheri%2C+M">M. Bagheri</a>, <a href="/search/?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/?searchtype=author&query=Barghini%2C+D">D. Barghini</a>, <a href="/search/?searchtype=author&query=Battisti%2C+M">M. Battisti</a>, <a href="/search/?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/?searchtype=author&query=Belov%2C+A+A">A. A. Belov</a>, <a href="/search/?searchtype=author&query=Bertaina%2C+M">M. Bertaina</a>, <a href="/search/?searchtype=author&query=Bertone%2C+P+F">P. F. Bertone</a>, <a href="/search/?searchtype=author&query=Bianciotto%2C+M">M. Bianciotto</a>, <a href="/search/?searchtype=author&query=Bisconti%2C+F">F. Bisconti</a>, <a href="/search/?searchtype=author&query=Blaksley%2C+C">C. Blaksley</a>, <a href="/search/?searchtype=author&query=Blin-Bondil%2C+S">S. Blin-Bondil</a>, <a href="/search/?searchtype=author&query=Bolmgren%2C+K">K. Bolmgren</a>, <a href="/search/?searchtype=author&query=Briz%2C+S">S. Briz</a>, <a href="/search/?searchtype=author&query=Burton%2C+J">J. Burton</a>, <a href="/search/?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/?searchtype=author&query=Cambi%C3%A8%2C+G">G. Cambi猫</a> , et al. (133 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="2312.08204v1-abstract-short" style="display: inline;"> This is a collection of papers presented by the JEM-EUSO Collaboration at the 38th International Cosmic Ray Conference (Nagoya, Japan, July 26-August 3, 2023) </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.08204v1-abstract-full" style="display: none;"> This is a collection of papers presented by the JEM-EUSO Collaboration at the 38th International Cosmic Ray Conference (Nagoya, Japan, July 26-August 3, 2023) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08204v1-abstract-full').style.display = 'none'; document.getElementById('2312.08204v1-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> 13 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.12656">arXiv:2311.12656</a> <span> [<a href="https://arxiv.org/pdf/2311.12656">pdf</a>, <a href="https://arxiv.org/format/2311.12656">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 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/10.1140/epjc/s10052-023-12090-w">10.1140/epjc/s10052-023-12090-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Developments and results in the context of the JEM-EUSO program obtained with the ESAF Simulation and Analysis Framework </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Adams%2C+J+H">J. H. Adams Jr.</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Alldredge%2C+P">P. Alldredge</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/?searchtype=author&query=Barghini%2C+D">D. Barghini</a>, <a href="/search/?searchtype=author&query=Battisti%2C+M">M. Battisti</a>, <a href="/search/?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/?searchtype=author&query=Belov%2C+A+A">A. A. Belov</a>, <a href="/search/?searchtype=author&query=Bertaina%2C+M">M. Bertaina</a>, <a href="/search/?searchtype=author&query=Bertone%2C+P+F">P. F. Bertone</a>, <a href="/search/?searchtype=author&query=Bianciotto%2C+M">M. Bianciotto</a>, <a href="/search/?searchtype=author&query=Biermann%2C+P+L">P. L. Biermann</a>, <a href="/search/?searchtype=author&query=Bisconti%2C+F">F. Bisconti</a>, <a href="/search/?searchtype=author&query=Blaksley%2C+C">C. Blaksley</a>, <a href="/search/?searchtype=author&query=Blin-Bondil%2C+S">S. Blin-Bondil</a>, <a href="/search/?searchtype=author&query=Bobik%2C+P">P. Bobik</a>, <a href="/search/?searchtype=author&query=Bolmgren%2C+K">K. Bolmgren</a>, <a href="/search/?searchtype=author&query=Briz%2C+S">S. Briz</a>, <a href="/search/?searchtype=author&query=Burton%2C+J">J. Burton</a>, <a href="/search/?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a> , et al. (150 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="2311.12656v1-abstract-short" style="display: inline;"> JEM--EUSO is an international program for the development of space-based Ultra-High Energy Cosmic Ray observatories. The program consists of a series of missions which are either under development or in the data analysis phase. All instruments are based on a wide-field-of-view telescope, which operates in the near-UV range, designed to detect the fluorescence light emitted by extensive air showers… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12656v1-abstract-full').style.display = 'inline'; document.getElementById('2311.12656v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.12656v1-abstract-full" style="display: none;"> JEM--EUSO is an international program for the development of space-based Ultra-High Energy Cosmic Ray observatories. The program consists of a series of missions which are either under development or in the data analysis phase. All instruments are based on a wide-field-of-view telescope, which operates in the near-UV range, designed to detect the fluorescence light emitted by extensive air showers in the atmosphere. We describe the simulation software ESAFin the framework of the JEM--EUSO program and explain the physical assumptions used. We present here the implementation of the JEM--EUSO, POEMMA, K--EUSO, TUS, Mini--EUSO, EUSO--SPB1 and EUSO--TA configurations in ESAF. For the first time ESAF simulation outputs are compared with experimental data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12656v1-abstract-full').style.display = 'none'; document.getElementById('2311.12656v1-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> 21 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 83, 1028 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.17811">arXiv:2305.17811</a> <span> [<a href="https://arxiv.org/pdf/2305.17811">pdf</a>, <a href="https://arxiv.org/format/2305.17811">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> </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/10.1051/0004-6361/202347034">10.1051/0004-6361/202347034 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> What can be learnt from UHECR anisotropies observations Paper II: intermediate-scale anisotropies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/?searchtype=author&query=Baret%2C+B">Bruny Baret</a>, <a href="/search/?searchtype=author&query=Parizot%2C+E">Etienne Parizot</a> </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="2305.17811v2-abstract-short" style="display: inline;"> Analysing the available data relative to the anisotropies of the ultra-high-energy cosmic rays (UHECR) at intermediate angular scales, we examine to what extent they can be used to constrain the origin of these particles, and what could be gained from a new generation of observatories with increased exposure. We simulate realistic UHECR sky maps for a wide range of scenarios, with the assumption t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.17811v2-abstract-full').style.display = 'inline'; document.getElementById('2305.17811v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.17811v2-abstract-full" style="display: none;"> Analysing the available data relative to the anisotropies of the ultra-high-energy cosmic rays (UHECR) at intermediate angular scales, we examine to what extent they can be used to constrain the origin of these particles, and what could be gained from a new generation of observatories with increased exposure. We simulate realistic UHECR sky maps for a wide range of scenarios, with the assumption that the distribution of UHECR sources follows that of matter in the Universe, also considering possible biases. We produce numerous datasets on which we apply similar analyses as those recently used by the Auger and TA collaborations. We find that: i) the investigated scenarios can easily account for the significance of the anisotropies reported by Auger and TA; ii) the direction in which the maximum flux excess is found in the Auger data differs from where it is found in most of our simulations; iii) for datasets simulated with the same astrophysical scenario, the significance with which the isotropy hypothesis is rejected through the Auger likelihood analysis can be largest either when "all galaxies" or when "starburst" galaxies are used to model the signal, depending on which GMF model is used; iv) the study of the energy evolution of the anisotropy patterns can provide new insight about the origin of UHECRs; v) the direction in which the most significant flux excess is found in the Auger dataset above 8 EeV appears to essentially disappear in the dataset above 32 EeV; vi) this appears to be very uncommon in our simulations, which could point to a failure of some generic assumption in the investigated scenarios, such as the predominance of a unique type of sources in the flux above the ankle, with essentially the same composition and spectrum; vii) a meaningful measurement of their energy evolution, from 10 EeV to the highest energies, will require a significant increase in statistics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.17811v2-abstract-full').style.display = 'none'; document.getElementById('2305.17811v2-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> 9 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </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">29 pages, 23 figures - Sects. 4.2 and 4.3 rewritten to make the quantitative comparison between the simulations and Auger data clearer - Discussion on TA anisotropies moved to the Appendix - A short discussion on the impact of more recent Galactic magnetic models added at the end of the paper. - No change in the discussions and conclusions. - To appear in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A292 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.03986">arXiv:2211.03986</a> <span> [<a href="https://arxiv.org/pdf/2211.03986">pdf</a>, <a href="https://arxiv.org/format/2211.03986">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</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="Nuclear Theory">nucl-th</span> </div> </div> <p class="title is-5 mathjax"> PANDORA project: photo-nuclear reactions below $A=60$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tamii%2C+A">A. Tamii</a>, <a href="/search/?searchtype=author&query=Pellegri%2C+L">L. Pellegri</a>, <a href="/search/?searchtype=author&query=S%C3%B6derstr%C3%B6m%2C+P+-">P. -A. S枚derstr枚m</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Goriely%2C+S">S. Goriely</a>, <a href="/search/?searchtype=author&query=Inakura%2C+T">T. Inakura</a>, <a href="/search/?searchtype=author&query=Khan%2C+E">E. Khan</a>, <a href="/search/?searchtype=author&query=Kido%2C+E">E. Kido</a>, <a href="/search/?searchtype=author&query=Kimura%2C+M">M. Kimura</a>, <a href="/search/?searchtype=author&query=Litvinova%2C+E">E. Litvinova</a>, <a href="/search/?searchtype=author&query=Nagataki%2C+S">S. Nagataki</a>, <a href="/search/?searchtype=author&query=von+Neumann-Cosel%2C+P">P. von Neumann-Cosel</a>, <a href="/search/?searchtype=author&query=Pietralla%2C+N">N. Pietralla</a>, <a href="/search/?searchtype=author&query=Shimizu%2C+N">N. Shimizu</a>, <a href="/search/?searchtype=author&query=Tsoneva%2C+N">N. Tsoneva</a>, <a href="/search/?searchtype=author&query=Utsuno%2C+Y">Y. Utsuno</a>, <a href="/search/?searchtype=author&query=Adachi%2C+S">S. Adachi</a>, <a href="/search/?searchtype=author&query=Adsley%2C+P">P. Adsley</a>, <a href="/search/?searchtype=author&query=Bahini%2C+A">A. Bahini</a>, <a href="/search/?searchtype=author&query=Balabanski%2C+D">D. Balabanski</a>, <a href="/search/?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/?searchtype=author&query=Bekker%2C+J+A+C">J. A. C. Bekker</a>, <a href="/search/?searchtype=author&query=Binda%2C+S+D">S. D. Binda</a>, <a href="/search/?searchtype=author&query=Boicu%2C+E">E. Boicu</a>, <a href="/search/?searchtype=author&query=Bracco%2C+A">A. Bracco</a> , et al. (56 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="2211.03986v2-abstract-short" style="display: inline;"> Photo-nuclear reactions of light nuclei below a mass of $A=60$ are studied experimentally and theoretically by the PANDORA (Photo-Absorption of Nuclei and Decay Observation for Reactions in Astrophysics) project. Two experimental methods, virtual-photon excitation by proton scattering and real-photo absorption by a high-brilliance gamma-ray beam produced by laser Compton scattering, will be applie… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03986v2-abstract-full').style.display = 'inline'; document.getElementById('2211.03986v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.03986v2-abstract-full" style="display: none;"> Photo-nuclear reactions of light nuclei below a mass of $A=60$ are studied experimentally and theoretically by the PANDORA (Photo-Absorption of Nuclei and Decay Observation for Reactions in Astrophysics) project. Two experimental methods, virtual-photon excitation by proton scattering and real-photo absorption by a high-brilliance gamma-ray beam produced by laser Compton scattering, will be applied to measure the photo-absorption cross sections and the decay branching ratio of each decay channel as a function of the photon energy. Several nuclear models, e.g. anti-symmetrized molecular dynamics, mean-field type models, a large-scale shell model, and ab initio models, will be employed to predict the photo-nuclear reactions. The uncertainty in the model predictions will be evaluated from the discrepancies between the model predictions and the experimental data. The data and the predictions will be implemented in a general reaction calculation code TALYS . The results will be applied to the simulation of the photo-disintegration process of ultra-high-energy cosmic rays in inter-galactic propagation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.03986v2-abstract-full').style.display = 'none'; document.getElementById('2211.03986v2-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> 18 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.14015">arXiv:2208.14015</a> <span> [<a href="https://arxiv.org/pdf/2208.14015">pdf</a>, <a href="https://arxiv.org/format/2208.14015">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Methodology">stat.ME</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Statistics Theory">math.ST</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Applications">stat.AP</span> </div> </div> <p class="title is-5 mathjax"> The SPDE approach for spatio-temporal datasets with advection and diffusion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Clarotto%2C+L">Lucia Clarotto</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Romary%2C+T">Thomas Romary</a>, <a href="/search/?searchtype=author&query=Desassis%2C+N">Nicolas Desassis</a> </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="2208.14015v4-abstract-short" style="display: inline;"> In the task of predicting spatio-temporal fields in environmental science using statistical methods, introducing statistical models inspired by the physics of the underlying phenomena that are numerically efficient is of growing interest. Large space-time datasets call for new numerical methods to efficiently process them. The Stochastic Partial Differential Equation (SPDE) approach has proven to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.14015v4-abstract-full').style.display = 'inline'; document.getElementById('2208.14015v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.14015v4-abstract-full" style="display: none;"> In the task of predicting spatio-temporal fields in environmental science using statistical methods, introducing statistical models inspired by the physics of the underlying phenomena that are numerically efficient is of growing interest. Large space-time datasets call for new numerical methods to efficiently process them. The Stochastic Partial Differential Equation (SPDE) approach has proven to be effective for the estimation and the prediction in a spatial context. We present here the advection-diffusion SPDE with first order derivative in time which defines a large class of nonseparable spatio-temporal models. A Gaussian Markov random field approximation of the solution to the SPDE is built by discretizing the temporal derivative with a finite difference method (implicit Euler) and by solving the spatial SPDE with a finite element method (continuous Galerkin) at each time step. The ''Streamline Diffusion'' stabilization technique is introduced when the advection term dominates the diffusion. Computationally efficient methods are proposed to estimate the parameters of the SPDE and to predict the spatio-temporal field by kriging, as well as to perform conditional simulations. The approach is applied to a solar radiation dataset. Its advantages and limitations are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.14015v4-abstract-full').style.display = 'none'; document.getElementById('2208.14015v4-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> 22 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.12501">arXiv:2208.12501</a> <span> [<a href="https://arxiv.org/pdf/2208.12501">pdf</a>, <a href="https://arxiv.org/format/2208.12501">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Statistics Theory">math.ST</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computation">stat.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Methodology">stat.ME</span> </div> </div> <p class="title is-5 mathjax"> Geostatistics for large datasets on Riemannian manifolds: a matrix-free approach </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pereira%2C+M">Mike Pereira</a>, <a href="/search/?searchtype=author&query=Desassis%2C+N">Nicolas Desassis</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a> </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="2208.12501v2-abstract-short" style="display: inline;"> Large or very large spatial (and spatio-temporal) datasets have become common place in many environmental and climate studies. These data are often collected in non-Euclidean spaces (such as the planet Earth) and they often present non-stationary anisotropies. This paper proposes a generic approach to model Gaussian Random Fields (GRFs) on compact Riemannian manifolds that bridges the gap between… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.12501v2-abstract-full').style.display = 'inline'; document.getElementById('2208.12501v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.12501v2-abstract-full" style="display: none;"> Large or very large spatial (and spatio-temporal) datasets have become common place in many environmental and climate studies. These data are often collected in non-Euclidean spaces (such as the planet Earth) and they often present non-stationary anisotropies. This paper proposes a generic approach to model Gaussian Random Fields (GRFs) on compact Riemannian manifolds that bridges the gap between existing works on non-stationary GRFs and random fields on manifolds. This approach can be applied to any smooth compact manifolds, and in particular to any compact surface. By defining a Riemannian metric that accounts for the preferential directions of correlation, our approach yields an interpretation of the ''local anisotropies'' as resulting from ''local'' deformations of the domain. We provide scalable algorithms for the estimation of the parameters and for optimal prediction by kriging and simulation able to tackle very large grids. Stationary and non-stationary illustrations are provided. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.12501v2-abstract-full').style.display = 'none'; document.getElementById('2208.12501v2-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> 6 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.12246">arXiv:2201.12246</a> <span>  </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> </div> </div> <p class="title is-5 mathjax"> JEM-EUSO Collaboration contributions to the 37th International Cosmic Ray Conference </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abdellaoui%2C+G">G. Abdellaoui</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Adams%2C+J+H">J. H. Adams Jr.</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Alonso%2C+G">G. Alonso</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Attallah%2C+R">R. Attallah</a>, <a href="/search/?searchtype=author&query=Attoui%2C+H">H. Attoui</a>, <a href="/search/?searchtype=author&query=Pernas%2C+M+A">M. Ave Pernas</a>, <a href="/search/?searchtype=author&query=Bagheri%2C+M">M. Bagheri</a>, <a href="/search/?searchtype=author&query=Bal%C3%A1z%2C+J">J. Bal谩z</a>, <a href="/search/?searchtype=author&query=Bakiri%2C+M">M. Bakiri</a>, <a href="/search/?searchtype=author&query=Barghini%2C+D">D. Barghini</a>, <a href="/search/?searchtype=author&query=Bartocci%2C+S">S. Bartocci</a>, <a href="/search/?searchtype=author&query=Battisti%2C+M">M. Battisti</a>, <a href="/search/?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/?searchtype=author&query=Beldjilali%2C+B">B. Beldjilali</a>, <a href="/search/?searchtype=author&query=Belenguer%2C+T">T. Belenguer</a>, <a href="/search/?searchtype=author&query=Belkhalfa%2C+N">N. Belkhalfa</a>, <a href="/search/?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/?searchtype=author&query=Belov%2C+A+A">A. A. Belov</a>, <a href="/search/?searchtype=author&query=Benmessai%2C+K">K. Benmessai</a> , et al. (267 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="2201.12246v1-abstract-short" style="display: inline;"> Compilation of papers presented by the JEM-EUSO Collaboration at the 37th International Cosmic Ray Conference (ICRC), held on July 12-23, 2021 (online) in Berlin, Germany. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.12246v1-abstract-full" style="display: none;"> Compilation of papers presented by the JEM-EUSO Collaboration at the 37th International Cosmic Ray Conference (ICRC), held on July 12-23, 2021 (online) in Berlin, Germany. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.12246v1-abstract-full').style.display = 'none'; document.getElementById('2201.12246v1-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> 28 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </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">html page with links to the JEM-EUSO Collaboration papers presented at ICRC-2021, Berlin, Germany</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.10970">arXiv:2111.10970</a> <span> [<a href="https://arxiv.org/pdf/2111.10970">pdf</a>, <a href="https://arxiv.org/format/2111.10970">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Robotics">cs.RO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Artificial Intelligence">cs.AI</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Systems and Control">eess.SY</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/10.1109/AERO53065.2022.9843352">10.1109/AERO53065.2022.9843352 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Operations for Autonomous Spacecraft </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Castano%2C+R">Rebecca Castano</a>, <a href="/search/?searchtype=author&query=Vaquero%2C+T">Tiago Vaquero</a>, <a href="/search/?searchtype=author&query=Rossi%2C+F">Federico Rossi</a>, <a href="/search/?searchtype=author&query=Verma%2C+V">Vandi Verma</a>, <a href="/search/?searchtype=author&query=Van+Wyk%2C+E">Ellen Van Wyk</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Dan Allard</a>, <a href="/search/?searchtype=author&query=Huffmann%2C+B">Bennett Huffmann</a>, <a href="/search/?searchtype=author&query=Murphy%2C+E+M">Erin M. Murphy</a>, <a href="/search/?searchtype=author&query=Dhamani%2C+N">Nihal Dhamani</a>, <a href="/search/?searchtype=author&query=Hewitt%2C+R+A">Robert A. Hewitt</a>, <a href="/search/?searchtype=author&query=Davidoff%2C+S">Scott Davidoff</a>, <a href="/search/?searchtype=author&query=Amini%2C+R">Rashied Amini</a>, <a href="/search/?searchtype=author&query=Barrett%2C+A">Anthony Barrett</a>, <a href="/search/?searchtype=author&query=Castillo-Rogez%2C+J">Julie Castillo-Rogez</a>, <a href="/search/?searchtype=author&query=Chien%2C+S+A">Steve A. Chien</a>, <a href="/search/?searchtype=author&query=Choukroun%2C+M">Mathieu Choukroun</a>, <a href="/search/?searchtype=author&query=Dadaian%2C+A">Alain Dadaian</a>, <a href="/search/?searchtype=author&query=Francis%2C+R">Raymond Francis</a>, <a href="/search/?searchtype=author&query=Gorr%2C+B">Benjamin Gorr</a>, <a href="/search/?searchtype=author&query=Hofstadter%2C+M">Mark Hofstadter</a>, <a href="/search/?searchtype=author&query=Ingham%2C+M">Mitch Ingham</a>, <a href="/search/?searchtype=author&query=Sorice%2C+C">Cristina Sorice</a>, <a href="/search/?searchtype=author&query=Tierney%2C+I">Iain Tierney</a> </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="2111.10970v1-abstract-short" style="display: inline;"> Onboard autonomy technologies such as planning and scheduling, identification of scientific targets, and content-based data summarization, will lead to exciting new space science missions. However, the challenge of operating missions with such onboard autonomous capabilities has not been studied to a level of detail sufficient for consideration in mission concepts. These autonomy capabilities will… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10970v1-abstract-full').style.display = 'inline'; document.getElementById('2111.10970v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.10970v1-abstract-full" style="display: none;"> Onboard autonomy technologies such as planning and scheduling, identification of scientific targets, and content-based data summarization, will lead to exciting new space science missions. However, the challenge of operating missions with such onboard autonomous capabilities has not been studied to a level of detail sufficient for consideration in mission concepts. These autonomy capabilities will require changes to current operations processes, practices, and tools. We have developed a case study to assess the changes needed to enable operators and scientists to operate an autonomous spacecraft by facilitating a common model between the ground personnel and the onboard algorithms. We assess the new operations tools and workflows necessary to enable operators and scientists to convey their desired intent to the spacecraft, and to be able to reconstruct and explain the decisions made onboard and the state of the spacecraft. Mock-ups of these tools were used in a user study to understand the effectiveness of the processes and tools in enabling a shared framework of understanding, and in the ability of the operators and scientists to effectively achieve mission science objectives. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.10970v1-abstract-full').style.display = 'none'; document.getElementById('2111.10970v1-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> 21 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </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, 18 Figures, 1 Table, to be published in IEEE Aerospace 2022 (AeroConf 2022)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings of the 2022 IEEE Aerospace Conference (IEEE AERO 2022), 1-20 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.05724">arXiv:2111.05724</a> <span> [<a href="https://arxiv.org/pdf/2111.05724">pdf</a>, <a href="https://arxiv.org/format/2111.05724">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Methodology">stat.ME</span> </div> </div> <p class="title is-5 mathjax"> Spatial statistics and stochastic partial differential equations: a mechanistic viewpoint </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Roques%2C+L">Lionel Roques</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Soubeyrand%2C+S">Samuel Soubeyrand</a> </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="2111.05724v1-abstract-short" style="display: inline;"> The Stochastic Partial Differential Equation (SPDE) approach, now commonly used in spatial statistics to construct Gaussian random fields, is revisited from a mechanistic perspective based on the movement of microscopic particles, thereby relating pseudo-differential operators to dispersal kernels. We first establish a connection between L茅vy flights and PDEs involving the Fractional Laplacian (FL… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05724v1-abstract-full').style.display = 'inline'; document.getElementById('2111.05724v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.05724v1-abstract-full" style="display: none;"> The Stochastic Partial Differential Equation (SPDE) approach, now commonly used in spatial statistics to construct Gaussian random fields, is revisited from a mechanistic perspective based on the movement of microscopic particles, thereby relating pseudo-differential operators to dispersal kernels. We first establish a connection between L茅vy flights and PDEs involving the Fractional Laplacian (FL) operator. The corresponding Fokker-Planck PDEs will serve as a basis to propose new generalisations by considering a general form of SPDE with terms accounting for dispersal, drift and reaction. We detail the difference between the FL operator (with or without linear reaction term) associated with a fat-tailed dispersal kernel and therefore describing long-distance dependencies, and the damped FL operator associated with a thin-tailed kernel, thus corresponding to short-distance dependencies. Then, SPDE-based random fields with non-stationary external spatially and temporally varying force are illustrated and nonlinear bistable reaction term are introduced. The physical meaning of the latter and possible applications are discussed. Returning to the particulate interpretation of the above-mentioned equations, we describe in a relatively simple case their links with point processes. We unravel the nature of the point processes they generate and show how such mechanistic models, associated to a probabilistic observation model, can be used in a hierarchical setting to estimate the parameters of the particle dynamics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.05724v1-abstract-full').style.display = 'none'; document.getElementById('2111.05724v1-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> 10 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.10761">arXiv:2110.10761</a> <span> [<a href="https://arxiv.org/pdf/2110.10761">pdf</a>, <a href="https://arxiv.org/format/2110.10761">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> </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/10.1051/0004-6361/202142491">10.1051/0004-6361/202142491 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> What can be learnt from UHECR anisotropies observations? Paper I : large-scale anisotropies and composition features </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/?searchtype=author&query=Parizot%2C+E">E. Parizot</a> </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="2110.10761v1-abstract-short" style="display: inline;"> We investigate the implications of the current data regarding large scale anisotropies, and examine to what extent they can be used to constrain the origin of UHECRs and the astrophysical parameters of the source scenarios. We discuss the possibility of observing an associated anisotropy of the composition, the potential benefit of the separation of the different nuclear components and the interes… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.10761v1-abstract-full').style.display = 'inline'; document.getElementById('2110.10761v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.10761v1-abstract-full" style="display: none;"> We investigate the implications of the current data regarding large scale anisotropies, and examine to what extent they can be used to constrain the origin of UHECRs and the astrophysical parameters of the source scenarios. We discuss the possibility of observing an associated anisotropy of the composition, the potential benefit of the separation of the different nuclear components and the interest of observing the UHECR sky with larger exposure future observatories. We simulate UHECR sky maps for various astrophysical scenarios satisfying the current observational constraints, taking into account the energy losses of the UHE protons and nuclei and their deflections by intervening magnetic fields. We investigate scenarios in which the UHECR source distribution follows that of the galaxies, varying the source composition and spectrum, the source density and the magnetic field models. We apply similar analyses as those used by the Auger collaboration. We find that: i) reproducing the observed dipole anisotropy and its energy evolution is relatively easy within our assumptions; ii) this agreement can be obtained with different sets of assumptions on the astrophysical parameters, and is thus not, at this stage, very constraining for UHECR source scenarios; iii) the actual reconstructed direction of the dipole appears non natural in essentially all scenarios investigated, and challenges their main assumptions on the source distribution or the assumed magnetic field configuration, especially in the Galaxy; iv) except for protons, the energy range in which the GZK horizon strongly reduces is a key target for anisotropy searches for each given nuclear species; v) The composition anisotropy naturally expected in our models is unlikely to account for that recently reported by Auger unless the observed amplitude is a strong positive statistical fluctuation of an intrinsically weaker signal. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.10761v1-abstract-full').style.display = 'none'; document.getElementById('2110.10761v1-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> 20 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </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">39 pages, 32 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 664, A120 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.07967">arXiv:2110.07967</a> <span> [<a href="https://arxiv.org/pdf/2110.07967">pdf</a>, <a href="https://arxiv.org/format/2110.07967">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Methodology">stat.ME</span> </div> </div> <p class="title is-5 mathjax"> A new class of $伪$-transformations for the spatial analysis of Compositional Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Clarotto%2C+L">Lucia Clarotto</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Menafoglio%2C+A">Alessandra Menafoglio</a> </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="2110.07967v1-abstract-short" style="display: inline;"> Georeferenced compositional data are prominent in many scientific fields and in spatial statistics. This work addresses the problem of proposing models and methods to analyze and predict, through kriging, this type of data. To this purpose, a novel class of transformations, named the Isometric $伪$-transformation ($伪$-IT), is proposed, which encompasses the traditional Isometric Log-Ratio (ILR) tra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.07967v1-abstract-full').style.display = 'inline'; document.getElementById('2110.07967v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.07967v1-abstract-full" style="display: none;"> Georeferenced compositional data are prominent in many scientific fields and in spatial statistics. This work addresses the problem of proposing models and methods to analyze and predict, through kriging, this type of data. To this purpose, a novel class of transformations, named the Isometric $伪$-transformation ($伪$-IT), is proposed, which encompasses the traditional Isometric Log-Ratio (ILR) transformation. It is shown that the ILR is the limit case of the $伪$-IT as $伪$ tends to 0 and that $伪=1$ corresponds to a linear transformation of the data. Unlike the ILR, the proposed transformation accepts 0s in the compositions when $伪>0$. Maximum likelihood estimation of the parameter $伪$ is established. Prediction using kriging on $伪$-IT transformed data is validated on synthetic spatial compositional data, using prediction scores computed either in the geometry induced by the $伪$-IT, or in the simplex. Application to land cover data shows that the relative superiority of the various approaches w.r.t. a prediction objective depends on whether the compositions contained any zero component. When all components are positive, the limit cases (ILR or linear transformations) are optimal for none of the considered metrics. An intermediate geometry, corresponding to the $伪$-IT with maximum likelihood estimate, better describes the dataset in a geostatistical setting. When the amount of compositions with 0s is not negligible, some side-effects of the transformation gets amplified as $伪$ decreases, entailing poor kriging performances both within the $伪$-IT geometry and for metrics in the simplex. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.07967v1-abstract-full').style.display = 'none'; document.getElementById('2110.07967v1-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 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </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">31 pages and 13 Figures. Supplementary material with 3 Figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 62H99 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2003.11383">arXiv:2003.11383</a> <span> [<a href="https://arxiv.org/pdf/2003.11383">pdf</a>, <a href="https://arxiv.org/format/2003.11383">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Applications">stat.AP</span> </div> </div> <p class="title is-5 mathjax"> Modeling and simulating depositional sequences using latent Gaussian random fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Fabbri%2C+P">Paolo Fabbri</a>, <a href="/search/?searchtype=author&query=Gaetan%2C+C">Carlo Gaetan</a> </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="2003.11383v1-abstract-short" style="display: inline;"> Simulating a depositional (or stratigraphic) sequence conditionally on borehole data is a long-standing problem in hydrogeology and in petroleum geostatistics. This paper presents a new rule-based approach for simulating depositional sequences of surfaces conditionally on lithofacies thickness data. The thickness of each layer is modeled by a transformed latent Gaussian random field allowing for n… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.11383v1-abstract-full').style.display = 'inline'; document.getElementById('2003.11383v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2003.11383v1-abstract-full" style="display: none;"> Simulating a depositional (or stratigraphic) sequence conditionally on borehole data is a long-standing problem in hydrogeology and in petroleum geostatistics. This paper presents a new rule-based approach for simulating depositional sequences of surfaces conditionally on lithofacies thickness data. The thickness of each layer is modeled by a transformed latent Gaussian random field allowing for null thickness thanks to a truncation process. Layers are sequentially stacked above each other following the regional stratigraphic sequence. By choosing adequately the variograms of these random fields, the simulated surfaces separating two layers can be continuous and smooth. Borehole information is often incomplete in the sense that it does not provide direct information as to the exact layer some observed thickness belongs to. The latent Gaussian model proposed in this paper offers a natural solution to this problem by means of a Bayesian setting with a Markov Chain Monte Carlo (MCMC) algorithm that can explore all possible configurations compatible with the data. The model and the associated MCMC algorithm are validated on synthetic data and then applied to a subsoil in the Venetian Plain with a moderately dense network of cored boreholes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2003.11383v1-abstract-full').style.display = 'none'; document.getElementById('2003.11383v1-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> 25 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> math.ST </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.08094">arXiv:2002.08094</a> <span> [<a href="https://arxiv.org/pdf/2002.08094">pdf</a>, <a href="https://arxiv.org/format/2002.08094">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Methodology">stat.ME</span> </div> </div> <p class="title is-5 mathjax"> Semi-parametric resampling with extremes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Opitz%2C+T">Thomas Opitz</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Mari%C3%A9thoz%2C+G">Gr茅goire Mari茅thoz</a> </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="2002.08094v2-abstract-short" style="display: inline;"> Nonparametric resampling methods such as Direct Sampling are powerful tools to simulate new datasets preserving important data features such as spatial patterns from observed datasets while using only minimal assumptions. However, such methods cannot generate extreme events beyond the observed range of data values. We here propose using tools from extreme value theory for stochastic processes to e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.08094v2-abstract-full').style.display = 'inline'; document.getElementById('2002.08094v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.08094v2-abstract-full" style="display: none;"> Nonparametric resampling methods such as Direct Sampling are powerful tools to simulate new datasets preserving important data features such as spatial patterns from observed datasets while using only minimal assumptions. However, such methods cannot generate extreme events beyond the observed range of data values. We here propose using tools from extreme value theory for stochastic processes to extrapolate observed data towards yet unobserved high quantiles. Original data are first enriched with new values in the tail region, and then classical resampling algorithms are applied to enriched data. In a first approach to enrichment that we label "naive resampling", we generate an independent sample of the marginal distribution while keeping the rank order of the observed data. We point out inaccuracies of this approach around the most extreme values, and therefore develop a second approach that works for datasets with many replicates. It is based on the asymptotic representation of extreme events through two stochastically independent components: a magnitude variable, and a profile field describing spatial variation. To generate enriched data, we fix a target range of return levels of the magnitude variable, and we resample magnitudes constrained to this range. We then use the second approach to generate heatwave scenarios of yet unobserved magnitude over France, based on daily temperature reanalysis training data for the years 2010 to 2016. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.08094v2-abstract-full').style.display = 'none'; document.getElementById('2002.08094v2-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> 7 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.08666">arXiv:1912.08666</a> <span>  </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> </div> </div> <p class="title is-5 mathjax"> Contributions to the 36th International Cosmic Ray Conference (ICRC 2019) of the JEM-EUSO Collaboration </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abdellaoui%2C+G">G. Abdellaoui</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Adams%2C+J+H">J. H. Adams Jr.</a>, <a href="/search/?searchtype=author&query=Ahriche%2C+A">A. Ahriche</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allen%2C+L">L. Allen</a>, <a href="/search/?searchtype=author&query=Alonso%2C+G">G. Alonso</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arai%2C+Y">Y. Arai</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Attallah%2C+R">R. Attallah</a>, <a href="/search/?searchtype=author&query=Attoui%2C+H">H. Attoui</a>, <a href="/search/?searchtype=author&query=Pernas%2C+M+A">M. Ave Pernas</a>, <a href="/search/?searchtype=author&query=Bacholle%2C+S">S. Bacholle</a>, <a href="/search/?searchtype=author&query=Bakiri%2C+M">M. Bakiri</a>, <a href="/search/?searchtype=author&query=Baragatti%2C+P">P. Baragatti</a>, <a href="/search/?searchtype=author&query=Barrillon%2C+P">P. Barrillon</a>, <a href="/search/?searchtype=author&query=Bartocci%2C+S">S. Bartocci</a>, <a href="/search/?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/?searchtype=author&query=Beldjilali%2C+B">B. Beldjilali</a>, <a href="/search/?searchtype=author&query=Belenguer%2C+T">T. Belenguer</a>, <a href="/search/?searchtype=author&query=Belkhalfa%2C+N">N. Belkhalfa</a>, <a href="/search/?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/?searchtype=author&query=Belov%2C+A">A. Belov</a> , et al. (287 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="1912.08666v1-abstract-short" style="display: inline;"> Compilation of papers presented by the JEM-EUSO Collaboration at the 36th International Cosmic Ray Conference (ICRC), held July 24 through August 1, 2019 in Madison, Wisconsin. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.08666v1-abstract-full" style="display: none;"> Compilation of papers presented by the JEM-EUSO Collaboration at the 36th International Cosmic Ray Conference (ICRC), held July 24 through August 1, 2019 in Madison, Wisconsin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.08666v1-abstract-full').style.display = 'none'; document.getElementById('1912.08666v1-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> 18 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">links to the 24 papers published in arXiv</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> all published in PoS(ICRC2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.02026">arXiv:1912.02026</a> <span> [<a href="https://arxiv.org/pdf/1912.02026">pdf</a>, <a href="https://arxiv.org/format/1912.02026">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computation">stat.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Methodology">stat.ME</span> </div> </div> <p class="title is-5 mathjax"> Simulating space-time random fields with nonseparable Gneiting-type covariance functions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Emery%2C+X">Xavier Emery</a>, <a href="/search/?searchtype=author&query=Lacaux%2C+C">C茅line Lacaux</a>, <a href="/search/?searchtype=author&query=Lantu%C3%A9joul%2C+C">Christian Lantu茅joul</a> </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="1912.02026v1-abstract-short" style="display: inline;"> Two algorithms are proposed to simulate space-time Gaussian random fields with a covariance function belonging to an extended Gneiting class, the definition of which depends on a completely monotone function associated with the spatial structure and a conditionally negative definite function associated with the temporal structure. In both cases, the simulated random field is constructed as a weigh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.02026v1-abstract-full').style.display = 'inline'; document.getElementById('1912.02026v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.02026v1-abstract-full" style="display: none;"> Two algorithms are proposed to simulate space-time Gaussian random fields with a covariance function belonging to an extended Gneiting class, the definition of which depends on a completely monotone function associated with the spatial structure and a conditionally negative definite function associated with the temporal structure. In both cases, the simulated random field is constructed as a weighted sum of cosine waves, with a Gaussian spatial frequency vector and a uniform phase. The difference lies in the way to handle the temporal component. The first algorithm relies on a spectral decomposition in order to simulate a temporal frequency conditional upon the spatial one, while in the second algorithm the temporal frequency is replaced by an intrinsic random field whose variogram is proportional to the conditionally negative definite function associated with the temporal structure. Both algorithms are scalable as their computational cost is proportional to the number of space-time locations, which may be unevenly spaced in space and/or in time. They are illustrated and validated through synthetic examples. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.02026v1-abstract-full').style.display = 'none'; document.getElementById('1912.02026v1-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> 4 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.02557">arXiv:1808.02557</a> <span> [<a href="https://arxiv.org/pdf/1808.02557">pdf</a>, <a href="https://arxiv.org/format/1808.02557">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> </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/10.1088/1748-0221/13/05/P05023">10.1088/1748-0221/13/05/P05023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> First observations of speed of light tracks by a fluorescence detector looking down on the atmosphere </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abdellaoui%2C+G">G. Abdellaoui</a>, <a href="/search/?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/?searchtype=author&query=Adams%2C+J+H">J. H. Adams Jr.</a>, <a href="/search/?searchtype=author&query=Ahriche%2C+A">A. Ahriche</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allen%2C+L">L. Allen</a>, <a href="/search/?searchtype=author&query=Alonso%2C+G">G. Alonso</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arai%2C+Y">Y. Arai</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Attallah%2C+R">R. Attallah</a>, <a href="/search/?searchtype=author&query=Attoui%2C+H">H. Attoui</a>, <a href="/search/?searchtype=author&query=Pernas%2C+M+A">M. Ave Pernas</a>, <a href="/search/?searchtype=author&query=Bacholle%2C+S">S. Bacholle</a>, <a href="/search/?searchtype=author&query=Bakiri%2C+M">M. Bakiri</a>, <a href="/search/?searchtype=author&query=Baragatti%2C+P">P. Baragatti</a>, <a href="/search/?searchtype=author&query=Barrillon%2C+P">P. Barrillon</a>, <a href="/search/?searchtype=author&query=Bartocci%2C+S">S. Bartocci</a>, <a href="/search/?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/?searchtype=author&query=Beldjilali%2C+B">B. Beldjilali</a>, <a href="/search/?searchtype=author&query=Belenguer%2C+T">T. Belenguer</a>, <a href="/search/?searchtype=author&query=Belkhalfa%2C+N">N. Belkhalfa</a>, <a href="/search/?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/?searchtype=author&query=Belov%2C+A">A. Belov</a> , et al. (289 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="1808.02557v1-abstract-short" style="display: inline;"> EUSO-Balloon is a pathfinder mission for the Extreme Universe Space Observatory onboard the Japanese Experiment Module (JEM-EUSO). It was launched on the moonless night of the 25$^{th}$ of August 2014 from Timmins, Canada. The flight ended successfully after maintaining the target altitude of 38 km for five hours. One part of the mission was a 2.5 hour underflight using a helicopter equipped with… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02557v1-abstract-full').style.display = 'inline'; document.getElementById('1808.02557v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.02557v1-abstract-full" style="display: none;"> EUSO-Balloon is a pathfinder mission for the Extreme Universe Space Observatory onboard the Japanese Experiment Module (JEM-EUSO). It was launched on the moonless night of the 25$^{th}$ of August 2014 from Timmins, Canada. The flight ended successfully after maintaining the target altitude of 38 km for five hours. One part of the mission was a 2.5 hour underflight using a helicopter equipped with three UV light sources (LED, xenon flasher and laser) to perform an inflight calibration and examine the detectors capability to measure tracks moving at the speed of light. We describe the helicopter laser system and details of the underflight as well as how the laser tracks were recorded and found in the data. These are the first recorded laser tracks measured from a fluorescence detector looking down on the atmosphere. Finally, we present a first reconstruction of the direction of the laser tracks relative to the detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02557v1-abstract-full').style.display = 'none'; document.getElementById('1808.02557v1-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> 7 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </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">18 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2018 JINST 13 P05023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.02322">arXiv:1808.02322</a> <span> [<a href="https://arxiv.org/pdf/1808.02322">pdf</a>, <a href="https://arxiv.org/format/1808.02322">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> </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/10.1051/0004-6361/201833683">10.1051/0004-6361/201833683 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Contribution of the Galactic center to the local cosmic-ray flux </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Jaupart%2C+E">Etienne Jaupart</a>, <a href="/search/?searchtype=author&query=Parizot%2C+E">Etienne Parizot</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a> </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="1808.02322v1-abstract-short" style="display: inline;"> Context. Recent observations of unexpected structures in the Galactic Cosmic Ray (GCR) spectrum and composition, as well as growing evidence for episodes of intense dynamical activity in the inner regions of the Galaxy, call for an evaluation of the high-energy particle acceleration associated with such activity and its potential impact on the global GCR phenomenology. Aims. We investigate wheth… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02322v1-abstract-full').style.display = 'inline'; document.getElementById('1808.02322v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.02322v1-abstract-full" style="display: none;"> Context. Recent observations of unexpected structures in the Galactic Cosmic Ray (GCR) spectrum and composition, as well as growing evidence for episodes of intense dynamical activity in the inner regions of the Galaxy, call for an evaluation of the high-energy particle acceleration associated with such activity and its potential impact on the global GCR phenomenology. Aims. We investigate whether particles accelerated during high-power episodes around the Galactic center can account for a significant fraction of the observed GCRs, or conversely what constraints can be derived regarding their Galactic transport if their contributions are negligible. Methods. We address these questions by studying the contribution of a continuous source of energetic particles at the Galactic center to the local GCRs. Particle transport in the Galaxy is described with a two-zone analytical model. We solve for the contribution of a Galactic Center Cosmic-Ray (GCCR) source using Green functions and Bessel expansion, and discuss the required injection power for these GCCRs to influence the global GCR phenomenology at Earth. Results. We find that, with standard parameters for particle propagation in the galactic disk and halo, the GCCRs can make a significant or even dominant contribution to the total CR flux observed at Earth. Depending on the parameters, such a source can account for both the observed proton flux and B-to-C ratio (in the case of a Kraichnan-like scaling of the diffusion coefficient), or potentially produce spectral and composition features. Conclusions. Our results show that the contribution of GCCRs cannot be neglected a priori, and that they can influence the global GCR phenomenology significantly, thereby calling for a reassessement of the standard inferences from a scenario where GCRs are entirely dominated by a single type of sources distributed throughout the Galactic disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.02322v1-abstract-full').style.display = 'none'; document.getElementById('1808.02322v1-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> 7 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </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">10 pages, 13 figures, 1 table, accepted for publication in Astronomy and Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 619, A12 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1807.04145">arXiv:1807.04145</a> <span> [<a href="https://arxiv.org/pdf/1807.04145">pdf</a>, <a href="https://arxiv.org/format/1807.04145">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computation">stat.CO</span> </div> </div> <p class="title is-5 mathjax"> Fast and exact simulation of isotropic Gaussian random fields on $\mathbb{S}^{2}$ and $\mathbb{S}^{2}\times \mathbb{R}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cuevas%2C+F">Francisco Cuevas</a>, <a href="/search/?searchtype=author&query=Porcu%2C+E">Emilio Porcu</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a> </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="1807.04145v1-abstract-short" style="display: inline;"> We provide a method for fast and exact simulation of Gaussian random fields on spheres having isotropic covariance functions. The method proposed is then extended to Gaussian random fields defined over spheres cross time and having covariance functions that depend on geodesic distance in space and on temporal separation. The crux of the method is in the use of block circulant matrices obtained wor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.04145v1-abstract-full').style.display = 'inline'; document.getElementById('1807.04145v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1807.04145v1-abstract-full" style="display: none;"> We provide a method for fast and exact simulation of Gaussian random fields on spheres having isotropic covariance functions. The method proposed is then extended to Gaussian random fields defined over spheres cross time and having covariance functions that depend on geodesic distance in space and on temporal separation. The crux of the method is in the use of block circulant matrices obtained working on regular grids defined over longitude $\times$ latitude. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1807.04145v1-abstract-full').style.display = 'none'; document.getElementById('1807.04145v1-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 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2018. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.04999">arXiv:1806.04999</a> <span> [<a href="https://arxiv.org/pdf/1806.04999">pdf</a>, <a href="https://arxiv.org/ps/1806.04999">ps</a>, <a href="https://arxiv.org/format/1806.04999">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Statistics Theory">math.ST</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Probability">math.PR</span> </div> </div> <p class="title is-5 mathjax"> A general framework for SPDE-based stationary random fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vergara%2C+R+C">Ricardo Carrizo Vergara</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Desassis%2C+N">Nicolas Desassis</a> </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="1806.04999v2-abstract-short" style="display: inline;"> This paper presents theoretical advances in the application of the Stochastic Partial Differential Equation (SPDE) approach in geostatistics. We show a general approach to construct stationary models related to a wide class of linear SPDEs, with applications to spatio-temporal models having non-trivial properties. Within the framework of Generalized Random Fields, a criterion for existence and uni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.04999v2-abstract-full').style.display = 'inline'; document.getElementById('1806.04999v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.04999v2-abstract-full" style="display: none;"> This paper presents theoretical advances in the application of the Stochastic Partial Differential Equation (SPDE) approach in geostatistics. We show a general approach to construct stationary models related to a wide class of linear SPDEs, with applications to spatio-temporal models having non-trivial properties. Within the framework of Generalized Random Fields, a criterion for existence and uniqueness of stationary solutions for this class of SPDEs is proposed and proven. Their covariance are then obtained through their spectral measure. We present a result relating the covariance in the case of a White Noise source term with that of a generic case through convolution. Then, we obtain a variety of SPDE-based stationary random fields. In particular, well-known results regarding the Mat茅rn Model and Markovian models are recovered. A new relationship between the Stein model and a particular SPDE is obtained. New spatio-temporal models obtained from evolution SPDEs of arbitrary temporal derivative order are then obtained, for which properties of separability and symmetry can be controlled. We also obtain results concerning stationary solutions for physically inspired models, such as solutions to the heat equation, the advection-diffusion equation, some Langevin's equations and the wave equation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.04999v2-abstract-full').style.display = 'none'; document.getElementById('1806.04999v2-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> 27 July, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </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">Corrected typos and style. Corrected mistakes in references (verified the cross cite, added new references and erasing non-used ones). Reorganization of the Section 6 in order to obtain a "general to particular" exposition. Appendix E is erased, its content is now present in the corpus. Some clarifications to proofs in Appendix B are added</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.01186">arXiv:1707.01186</a> <span> [<a href="https://arxiv.org/pdf/1707.01186">pdf</a>, <a href="https://arxiv.org/format/1707.01186">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> </div> </div> <p class="title is-5 mathjax"> Probing the Extragalactic Cosmic Rays origin with gamma-ray and neutrino backgrounds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Globus%2C+N">Noemie Globus</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Parizot%2C+E">Etienne Parizot</a>, <a href="/search/?searchtype=author&query=Piran%2C+T">Tsvi Piran</a> </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="1707.01186v1-abstract-short" style="display: inline;"> GeV-TeV gamma-ray and PeV-EeV neutrino backgrounds provide a unique window on the nature of the ultra-high-energy cosmic-rays (UHECRs). We discuss the implications of the recent Fermi-LAT data regarding the extragalactic gamma-ray background (EGB) and related estimates of the contribution of point sources as well as IceCube neutrino data on the origin of the UHECRs. We calculate the diffuse flux o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.01186v1-abstract-full').style.display = 'inline'; document.getElementById('1707.01186v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.01186v1-abstract-full" style="display: none;"> GeV-TeV gamma-ray and PeV-EeV neutrino backgrounds provide a unique window on the nature of the ultra-high-energy cosmic-rays (UHECRs). We discuss the implications of the recent Fermi-LAT data regarding the extragalactic gamma-ray background (EGB) and related estimates of the contribution of point sources as well as IceCube neutrino data on the origin of the UHECRs. We calculate the diffuse flux of cosmogenic $纬$-rays and neutrinos produced during the UHECRs propagation and derive constraints on the possible cosmological evolution of UHECR sources. In particular, we show that the mixed-composition scenario which is in agreement with both (i) Auger measurements of the energy spectrum and composition up to the highest energies and (ii) the ankle-like feature in the light component detected by KASCADE-Grande, is compatible with both the Fermi-LAT measurements and with current IceCube limits. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.01186v1-abstract-full').style.display = 'none'; document.getElementById('1707.01186v1-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> 4 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </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">8 pages, 3 figures, to appear in the Proceedings of the 35th International Cosmic Ray Conference 10-20 July, 2017 Bexco, Busan, Korea</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1707.01177">arXiv:1707.01177</a> <span> [<a href="https://arxiv.org/pdf/1707.01177">pdf</a>, <a href="https://arxiv.org/format/1707.01177">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> </div> </div> <p class="title is-5 mathjax"> Can we reconcile the TA excess and hotspot with Auger observations? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Globus%2C+N">Noemie Globus</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Parizot%2C+E">Etienne Parizot</a>, <a href="/search/?searchtype=author&query=Lachaud%2C+C">Cyril Lachaud</a>, <a href="/search/?searchtype=author&query=Piran%2C+T">Tsvi Piran</a> </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="1707.01177v2-abstract-short" style="display: inline;"> The Telescope Array (TA) shows a 20$^{\circ}$ hotspot as well as an excess of UHECRs above 50~EeV when compared with the Auger spectrum. We consider the possibility that both the TA excess and hotspot are due to a dominant source in the Northern sky. We carry out detailed simulations of UHECR propagation in both the intergalactic medium and the Galaxy, using different values for the intergalactic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.01177v2-abstract-full').style.display = 'inline'; document.getElementById('1707.01177v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1707.01177v2-abstract-full" style="display: none;"> The Telescope Array (TA) shows a 20$^{\circ}$ hotspot as well as an excess of UHECRs above 50~EeV when compared with the Auger spectrum. We consider the possibility that both the TA excess and hotspot are due to a dominant source in the Northern sky. We carry out detailed simulations of UHECR propagation in both the intergalactic medium and the Galaxy, using different values for the intergalactic magnetic field. We consider two general classes of sources: transients and steady, adopting a mixed UHECR composition that is consistent with the one found by Auger. The spatial location of the sources is draw randomly. We generate Auger-like and TA-like data sets from which we determine the spectrum, the sky maps and the level of anisotropy. We find that, while steady sources are favored over transients, it is unlikely to account for all the currently available observational data. While we reproduce fairly well the Auger spectrum for the vast majority of the simulated data sets, most of the simulated data sets with a spectrum compatible with that of TA (at most a few percent depending on density model tested) show a much stronger anisotropy than the one observed. We find that the rare cases in which both the spectrum and the anisotropy are consistent require a steady source within $\sim 10$ Mpc, to account for the flux excess, and a strong extragalactic magnetic field $\sim 10$ nG, to reduce the excessive anisotropy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1707.01177v2-abstract-full').style.display = 'none'; document.getElementById('1707.01177v2-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> 16 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 July, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2017. </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">8 pages, 3 figures, to appear in the Proceedings of the 35th International Cosmic Ray Conference 10-20 July, 2017 Bexco, Busan, Korea</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.04158">arXiv:1703.04158</a> <span> [<a href="https://arxiv.org/pdf/1703.04158">pdf</a>, <a href="https://arxiv.org/format/1703.04158">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> </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/10.3847/2041-8213/aa6af0">10.3847/2041-8213/aa6af0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the Extragalactic Cosmic Rays origin with gamma-ray and neutrino backgrounds </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Globus%2C+N">Noemie Globus</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Parizot%2C+E">Etienne Parizot</a>, <a href="/search/?searchtype=author&query=Piran%2C+T">Tsvi Piran</a> </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="1703.04158v2-abstract-short" style="display: inline;"> GeV-TeV gamma-rays and PeV-EeV neutrino backgrounds provide a unique window on the nature of the ultra-high-energy cosmic-rays (UHECRs). We discuss the implications of the recent Fermi-LAT data regarding the extragalactic gamma-ray background (EGB) and related estimates of the contribution of point sources as well as IceCube neutrino data on the origin of the UHECRs. We calculate the diffuse flux… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.04158v2-abstract-full').style.display = 'inline'; document.getElementById('1703.04158v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.04158v2-abstract-full" style="display: none;"> GeV-TeV gamma-rays and PeV-EeV neutrino backgrounds provide a unique window on the nature of the ultra-high-energy cosmic-rays (UHECRs). We discuss the implications of the recent Fermi-LAT data regarding the extragalactic gamma-ray background (EGB) and related estimates of the contribution of point sources as well as IceCube neutrino data on the origin of the UHECRs. We calculate the diffuse flux of cosmogenic $纬$-rays and neutrinos produced by the UHECRs and derive constraints on the possible cosmological evolution of UHECR sources. In particular, we show that the mixed-composition scenario considered in \citet{Globus2015b}, which is in agreement with both (i) Auger measurements of the energy spectrum and composition up to the highest energies and (ii) the ankle-like feature in the light component detected by KASCADE-Grande, is compatible with both the Fermi-LAT measurements and with current IceCube limits. We also discuss the possibility for future experiments to detect associated cosmogenic neutrinos and further constrain the UHECR models, including possible subdominant UHECR proton sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.04158v2-abstract-full').style.display = 'none'; document.getElementById('1703.04158v2-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> 3 April, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </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">6 pages, 4 figures, accepted without revision in ApJ Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.05319">arXiv:1610.05319</a> <span> [<a href="https://arxiv.org/pdf/1610.05319">pdf</a>, <a href="https://arxiv.org/format/1610.05319">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> </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/10.3847/1538-4357/836/2/163">10.3847/1538-4357/836/2/163 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Can we reconcile the TA excess and hotspot with Auger observations? </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Globus%2C+N">Noemie Globus</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Parizot%2C+E">Etienne Parizot</a>, <a href="/search/?searchtype=author&query=Lachaud%2C+C">Cyril Lachaud</a>, <a href="/search/?searchtype=author&query=Piran%2C+T">Tsvi Piran</a> </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="1610.05319v2-abstract-short" style="display: inline;"> The Telescope Array (TA) shows a 20$^{\circ}$ hotspot as well as an excess of UHECRs above 50~EeV when compared with the Auger spectrum. We consider the possibility that both the TA excess and hotspot are due to a dominant source in the Northern sky. We carry out detailed simulations of UHECR propagation in both the intergalactic medium and the Galaxy, using different values for the intergalactic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.05319v2-abstract-full').style.display = 'inline'; document.getElementById('1610.05319v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.05319v2-abstract-full" style="display: none;"> The Telescope Array (TA) shows a 20$^{\circ}$ hotspot as well as an excess of UHECRs above 50~EeV when compared with the Auger spectrum. We consider the possibility that both the TA excess and hotspot are due to a dominant source in the Northern sky. We carry out detailed simulations of UHECR propagation in both the intergalactic medium and the Galaxy, using different values for the intergalactic magnetic field. We consider two general classes of sources: transients and steady, adopting a mixed UHECR composition that is consistent with the one found by Auger. The spatial location of the sources is draw randomly. We generate Auger-like and TA-like data sets from which we determine the spectrum, the sky maps and the level of anisotropy. We find that, while steady sources are favored over transients, it is unlikely to account for all the currently available observational data. While we reproduce fairly well the Auger spectrum for the vast majority of the simulated data sets, most of the simulated data sets with a spectrum compatible with that of TA (at most a few percent depending on density model tested) show a much stronger anisotropy than the one observed. We find that the rare cases in which both the spectrum and the anisotropy are consistent require a steady source within $\sim 10$ Mpc, to account for the flux excess, and a strong extragalactic magnetic field $\sim 10$ nG, to reduce the excessive anisotropy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.05319v2-abstract-full').style.display = 'none'; document.getElementById('1610.05319v2-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 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">28 pages, 19 figures, accepted in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1607.08372">arXiv:1607.08372</a> <span> [<a href="https://arxiv.org/pdf/1607.08372">pdf</a>, <a href="https://arxiv.org/ps/1607.08372">ps</a>, <a href="https://arxiv.org/format/1607.08372">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Methodology">stat.ME</span> </div> </div> <p class="title is-5 mathjax"> Half-tapering strategy for conditional simulation with large datasets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Marcotte%2C+D">Denis Marcotte</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a> </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="1607.08372v3-abstract-short" style="display: inline;"> Gaussian conditional realizations are routinely used for risk assessment and planning in a variety of Earth sciences applications. Conditional realizations can be obtained by first creating unconditional realizations that are then post-conditioned by kriging. Many efficient algorithms are available for the first step, so the bottleneck resides in the second step. Instead of doing the conditional s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.08372v3-abstract-full').style.display = 'inline'; document.getElementById('1607.08372v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1607.08372v3-abstract-full" style="display: none;"> Gaussian conditional realizations are routinely used for risk assessment and planning in a variety of Earth sciences applications. Conditional realizations can be obtained by first creating unconditional realizations that are then post-conditioned by kriging. Many efficient algorithms are available for the first step, so the bottleneck resides in the second step. Instead of doing the conditional simulations with the desired covariance (F approach) or with a tapered covariance (T approach), we propose to use the taper covariance only in the conditioning step (Half-Taper or HT approach). This enables to speed up the computations and to reduce memory requirements for the conditioning step but also to keep the right short scale variations in the realizations. A criterion based on mean square error of the simulation is derived to help anticipate the similarity of HT to F. Moreover, an index is used to predict the sparsity of the kriging matrix for the conditioning step. Some guides for the choice of the taper function are discussed. The distributions of a series of 1D, 2D and 3D scalar response functions are compared for F, T and HT approaches. The distributions obtained indicate a much better similarity to F with HT than with T. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1607.08372v3-abstract-full').style.display = 'none'; document.getElementById('1607.08372v3-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> 6 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 July, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">39 pages, 2 Tables and 11 Figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1512.05225">arXiv:1512.05225</a> <span> [<a href="https://arxiv.org/pdf/1512.05225">pdf</a>, <a href="https://arxiv.org/ps/1512.05225">ps</a>, <a href="https://arxiv.org/format/1512.05225">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Methodology">stat.ME</span> </div> </div> <p class="title is-5 mathjax"> Means and covariance functions for geostatistical compositional data: an axiomatic approach </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Marchant%2C+T">Thierry Marchant</a> </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="1512.05225v3-abstract-short" style="display: inline;"> This work focuses on the characterization of the central tendency of a sample of compositional data. It provides new results about theoretical properties of means and covariance functions for compositional data, with an axiomatic perspective. Original results that shed new light on the geostatistical modeling of compositional data are presented. As a first result, it is shown that the weighted ari… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.05225v3-abstract-full').style.display = 'inline'; document.getElementById('1512.05225v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1512.05225v3-abstract-full" style="display: none;"> This work focuses on the characterization of the central tendency of a sample of compositional data. It provides new results about theoretical properties of means and covariance functions for compositional data, with an axiomatic perspective. Original results that shed new light on the geostatistical modeling of compositional data are presented. As a first result, it is shown that the weighted arithmetic mean is the only central tendency characteristic satisfying a small set of axioms, namely continuity, reflexivity and marginal stability. Moreover, this set of axioms also implies that the weights must be identical for all parts of the composition. This result has deep consequences on the spatial multivariate covariance modeling of compositional data. In a geostatistical setting, it is shown as a second result that the proportional model of covariance functions (i.e., the product of a covariance matrix and a single correlation function) is the only model that provides identical kriging weights for all components of the compositional data. As a consequence of these two results, the proportional model of covariance function is the only covariance model compatible with reflexivity and marginal stability. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1512.05225v3-abstract-full').style.display = 'none'; document.getElementById('1512.05225v3-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> 23 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 December, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 62H99 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1510.07840">arXiv:1510.07840</a> <span> [<a href="https://arxiv.org/pdf/1510.07840">pdf</a>, <a href="https://arxiv.org/format/1510.07840">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Methodology">stat.ME</span> </div> </div> <p class="title is-5 mathjax"> A Flexible Class of Non-separable Cross-Covariance Functions for Multivariate Space-Time Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bourotte%2C+M">Marc Bourotte</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Porcu%2C+E">Emilio Porcu</a> </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="1510.07840v2-abstract-short" style="display: inline;"> Multivariate space-time data are increasingly available in various scientific disciplines. When analyzing these data, one of the key issues is to describe the multivariate space-time dependencies. Under the Gaussian framework, one needs to propose relevant models for multivariate space-time covariance functions, i.e. matrix-valued mappings with the additional requirement of non-negative definitene… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.07840v2-abstract-full').style.display = 'inline'; document.getElementById('1510.07840v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1510.07840v2-abstract-full" style="display: none;"> Multivariate space-time data are increasingly available in various scientific disciplines. When analyzing these data, one of the key issues is to describe the multivariate space-time dependencies. Under the Gaussian framework, one needs to propose relevant models for multivariate space-time covariance functions, i.e. matrix-valued mappings with the additional requirement of non-negative definiteness. We propose a flexible parametric class of cross-covariance functions for multivariate space-time Gaussian random fields. Space-time components belong to the (univariate) Gneiting class of space-time covariance functions, with Mat茅rn or Cauchy covariance functions in the spatial margins. The smoothness and scale parameters can be different for each variable. We provide sufficient conditions for positive definiteness. A simulation study shows that the parameters of this model can be efficiently estimated using weighted pairwise likelihood, which belongs to the class of composite likelihood methods. We then illustrate the model on a French dataset of weather variables. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1510.07840v2-abstract-full').style.display = 'none'; document.getElementById('1510.07840v2-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> 9 February, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 October, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2015. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1505.01377">arXiv:1505.01377</a> <span> [<a href="https://arxiv.org/pdf/1505.01377">pdf</a>, <a href="https://arxiv.org/format/1505.01377">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> </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.92.021302">10.1103/PhysRevD.92.021302 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A complete model of the CR spectrum and composition across the Galactic to Extragalactic transition </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Globus%2C+N">Noemie Globus</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Parizot%2C+E">Etienne Parizot</a> </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="1505.01377v1-abstract-short" style="display: inline;"> We present a complete phenomenological model accounting for the evolution of the cosmic-ray spectrum and composition with energy, based on the available data over the entire spectrum. We show that there is no need to postulate any additional component, other than one single Galactic component depending on rigidity alone, and one extragalactic component, whose characteristics are similar to those d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.01377v1-abstract-full').style.display = 'inline'; document.getElementById('1505.01377v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1505.01377v1-abstract-full" style="display: none;"> We present a complete phenomenological model accounting for the evolution of the cosmic-ray spectrum and composition with energy, based on the available data over the entire spectrum. We show that there is no need to postulate any additional component, other than one single Galactic component depending on rigidity alone, and one extragalactic component, whose characteristics are similar to those derived from a study of particle acceleration at mildly relativistic shocks in a GRB environment (Globus et al., 2015). In particular, we show that the resulting cosmic ray spectrum and composition satisfy the various constraints derived from the current data in the Galactic/extragalactic transition region, notably from the measurements of KASCADE Grande and Auger. Finally, we derive some generic features that a working phenomenological scenario may exhibit to give a global account of the cosmic ray data with a minimum number of free parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1505.01377v1-abstract-full').style.display = 'none'; document.getElementById('1505.01377v1-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> 6 May, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">7 pages, 3 figures, submitted to Phys. Rev. D Rapid Communications</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 92, 021302 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.1271">arXiv:1409.1271</a> <span> [<a href="https://arxiv.org/pdf/1409.1271">pdf</a>, <a href="https://arxiv.org/format/1409.1271">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> </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/10.1093/mnras/stv893">10.1093/mnras/stv893 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> UHECR acceleration at GRB internal shocks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Globus%2C+N">Noemie Globus</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Mochkovitch%2C+R">Robert Mochkovitch</a>, <a href="/search/?searchtype=author&query=Parizot%2C+E">Etienne Parizot</a> </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="1409.1271v1-abstract-short" style="display: inline;"> We study the acceleration of CR protons and nuclei at GRB internal shocks. Physical quantities and their time evolution are estimated using the internal shock modeling implemented by Daigne & Mochkovitch 1998. We consider different hypotheses about the way the energy dissipated at internal shocks is shared between accelerated CR, e- and B field. We model CR acceleration at mildly relativistic shoc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.1271v1-abstract-full').style.display = 'inline'; document.getElementById('1409.1271v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.1271v1-abstract-full" style="display: none;"> We study the acceleration of CR protons and nuclei at GRB internal shocks. Physical quantities and their time evolution are estimated using the internal shock modeling implemented by Daigne & Mochkovitch 1998. We consider different hypotheses about the way the energy dissipated at internal shocks is shared between accelerated CR, e- and B field. We model CR acceleration at mildly relativistic shocks, including all the significant energy loss processes. We calculate CR and neutrino release from single GRBs, assuming that nuclei heavier than protons are present in the relativistic wind. Protons can only reach maximum energies of ~ 10^19.5 eV, while intermediate and heavy nuclei are able to reach values of ~ 10^20 eV and above. The spectra of nuclei escaping from the acceleration site are found to be very hard while the combined spectrum of protons and neutrons is much softer. We calculate the diffuse UHECR flux expected on Earth using the GRB luminosity function from Wanderman & Piran 2010. Only the models assuming that the prompt emission represent a very small fraction of the energy dissipated at internal shocks, and that most of this dissipated energy is communicated to accelerated CR, are able to reproduce the magnitude of the UHECR flux observed. For these models, the observed shape of the UHECR spectrum can be well reproduced and the evolution of the composition is compatible with the trend suggested by Auger. We discuss implications of the softer proton component for the GCR to EGCR transition in the light of the recent composition analyses (KASCADE-Grande experiment). The associated secondary particle diffuse fluxes do not upset any current observational limit. Diffuse neutrino flux from GRB sources should however be detected with the lifetime of neutrino observatories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.1271v1-abstract-full').style.display = 'none'; document.getElementById('1409.1271v1-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> 3 September, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2014. </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">39 pages, 35 figures, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1401.1119">arXiv:1401.1119</a> <span> [<a href="https://arxiv.org/pdf/1401.1119">pdf</a>, <a href="https://arxiv.org/format/1401.1119">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> </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/10.1051/0004-6361/201423462">10.1051/0004-6361/201423462 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Anisotropy expectations for ultra-high-energy cosmic rays with future high statistics experiments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=d%27Orfeuil%2C+B+R">Benjamin Rouill茅 d'Orfeuil</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/?searchtype=author&query=Lachaud%2C+C">Cyril Lachaud</a>, <a href="/search/?searchtype=author&query=Parizot%2C+E">Etienne Parizot</a>, <a href="/search/?searchtype=author&query=Blaksley%2C+C">Carl Blaksley</a>, <a href="/search/?searchtype=author&query=Nagataki%2C+S">Shigehiro Nagataki</a> </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="1401.1119v1-abstract-short" style="display: inline;"> UHECRs have attracted a lot of attention due to their challengingly high energies and their potential value to constrain physical processes and astrophysical parameters in the most energetic sources of the universe. Current detectors have failed to detect significant anisotropies which had been expected to allow source identification. Some indications about the UHECR composition, which may become… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.1119v1-abstract-full').style.display = 'inline'; document.getElementById('1401.1119v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1401.1119v1-abstract-full" style="display: none;"> UHECRs have attracted a lot of attention due to their challengingly high energies and their potential value to constrain physical processes and astrophysical parameters in the most energetic sources of the universe. Current detectors have failed to detect significant anisotropies which had been expected to allow source identification. Some indications about the UHECR composition, which may become heavier at the highest energies, has even put into question the possibility that such a goal could be achieved soon. We investigate the potential value of a new-generation detector, with 10 times larger exposure, to overcome the current situation and make significant progress in the detection of anisotropies and thus in the study of UHECRs. We take as an example the expected performances of the JEM-EUSO, assuming a uniform full-sky coverage with a total exposure of 300,000 km2 sr yr. We simulate realistic UHECR sky maps for a wide range of possible astrophysical scenarios allowed by the current constraints, taking into account the energy losses and photo-dissociation of the UHECRs, as well as their deflections by magnetic fields. These sky maps, built for the expected statistics of JEM-EUSO as well as for the current Auger statistics, as a reference, are analyzed from the point of view of their intrinsic anisotropies, using the two-point correlation function. A statistical study of the resulting anisotropies is performed for each astrophysical scenario, varying the UHECR source composition and spectrum as well as the source density. We find that significant anisotropies are expected to be detected by a next-generation UHECR detector, for essentially all the astrophysical scenarios studied, and give precise, quantitative meaning to this statement. Our results show that a gain of one order of magnitude in exposure would make a significant difference compared to the existing detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1401.1119v1-abstract-full').style.display = 'none'; document.getElementById('1401.1119v1-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> 6 January, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2014. </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, 28 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 567, A81 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1305.2478">arXiv:1305.2478</a> <span> [<a href="https://arxiv.org/pdf/1305.2478">pdf</a>, <a href="https://arxiv.org/ps/1305.2478">ps</a>, <a href="https://arxiv.org/format/1305.2478">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> </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.2013.01.008">10.1016/j.astropartphys.2013.01.008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An evaluation of the exposure in nadir observation of the JEM-EUSO mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Adams%2C+J+H">J. H. Adams</a>, <a href="/search/?searchtype=author&query=Ahmad%2C+S">S. Ahmad</a>, <a href="/search/?searchtype=author&query=Albert%2C+J+-">J. -N. Albert</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arai%2C+Y">Y. Arai</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Barrillon%2C+P">P. Barrillon</a>, <a href="/search/?searchtype=author&query=Batsch%2C+T">T. Batsch</a>, <a href="/search/?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/?searchtype=author&query=Belenguer%2C+T">T. Belenguer</a>, <a href="/search/?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/?searchtype=author&query=Berlind%2C+A+A">A. A. Berlind</a>, <a href="/search/?searchtype=author&query=Bertaina%2C+M">M. Bertaina</a>, <a href="/search/?searchtype=author&query=Biermann%2C+P+L">P. L. Biermann</a>, <a href="/search/?searchtype=author&query=Biktemerova%2C+S">S. Biktemerova</a>, <a href="/search/?searchtype=author&query=Blaksley%2C+C">C. Blaksley</a>, <a href="/search/?searchtype=author&query=Blecki%2C+J">J. Blecki</a>, <a href="/search/?searchtype=author&query=Blin-Bondil%2C+S">S. Blin-Bondil</a>, <a href="/search/?searchtype=author&query=Bluemer%2C+J">J. Bluemer</a>, <a href="/search/?searchtype=author&query=Bobik%2C+P">P. Bobik</a> , et al. (236 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="1305.2478v1-abstract-short" style="display: inline;"> We evaluate the exposure during nadir observations with JEM-EUSO, the Extreme Universe Space Observatory, on-board the Japanese Experiment Module of the International Space Station. Designed as a mission to explore the extreme energy Universe from space, JEM-EUSO will monitor the Earth's nighttime atmosphere to record the ultraviolet light from tracks generated by extensive air showers initiated b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1305.2478v1-abstract-full').style.display = 'inline'; document.getElementById('1305.2478v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1305.2478v1-abstract-full" style="display: none;"> We evaluate the exposure during nadir observations with JEM-EUSO, the Extreme Universe Space Observatory, on-board the Japanese Experiment Module of the International Space Station. Designed as a mission to explore the extreme energy Universe from space, JEM-EUSO will monitor the Earth's nighttime atmosphere to record the ultraviolet light from tracks generated by extensive air showers initiated by ultra-high energy cosmic rays. In the present work, we discuss the particularities of space-based observation and we compute the annual exposure in nadir observation. The results are based on studies of the expected trigger aperture and observational duty cycle, as well as, on the investigations of the effects of clouds and different types of background light. We show that the annual exposure is about one order of magnitude higher than those of the presently operating ground-based observatories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1305.2478v1-abstract-full').style.display = 'none'; document.getElementById('1305.2478v1-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 May, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">published in Astroparticle Physics by the JEM-EUSO Collaboration</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astroparticle Physics 44 (2013) 76 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1209.3840">arXiv:1209.3840</a> <span> [<a href="https://arxiv.org/pdf/1209.3840">pdf</a>, <a href="https://arxiv.org/format/1209.3840">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> </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/10.1088/1748-0221/7/10/P10011">10.1088/1748-0221/7/10/P10011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Antennas for the Detection of Radio Emission Pulses from Cosmic-Ray induced Air Showers at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a> , et al. (490 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="1209.3840v1-abstract-short" style="display: inline;"> The Pierre Auger Observatory is exploring the potential of the radio detection technique to study extensive air showers induced by ultra-high energy cosmic rays. The Auger Engineering Radio Array (AERA) addresses both technological and scientific aspects of the radio technique. A first phase of AERA has been operating since September 2010 with detector stations observing radio signals at frequenci… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.3840v1-abstract-full').style.display = 'inline'; document.getElementById('1209.3840v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1209.3840v1-abstract-full" style="display: none;"> The Pierre Auger Observatory is exploring the potential of the radio detection technique to study extensive air showers induced by ultra-high energy cosmic rays. The Auger Engineering Radio Array (AERA) addresses both technological and scientific aspects of the radio technique. A first phase of AERA has been operating since September 2010 with detector stations observing radio signals at frequencies between 30 and 80 MHz. In this paper we present comparative studies to identify and optimize the antenna design for the final configuration of AERA consisting of 160 individual radio detector stations. The transient nature of the air shower signal requires a detailed description of the antenna sensor. As the ultra-wideband reception of pulses is not widely discussed in antenna literature, we review the relevant antenna characteristics and enhance theoretical considerations towards the impulse response of antennas including polarization effects and multiple signal reflections. On the basis of the vector effective length we study the transient response characteristics of three candidate antennas in the time domain. Observing the variation of the continuous galactic background intensity we rank the antennas with respect to the noise level added to the galactic signal. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.3840v1-abstract-full').style.display = 'none'; document.getElementById('1209.3840v1-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> 17 September, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2012. </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">Accepted for publication in JINST, 50 pages, 25 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 7 (2012) P10011 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1208.1675">arXiv:1208.1675</a> <span> [<a href="https://arxiv.org/pdf/1208.1675">pdf</a>, <a href="https://arxiv.org/format/1208.1675">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> </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/10.1088/1748-0221/7/09/P09001">10.1088/1748-0221/7/09/P09001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Rapid Atmospheric Monitoring System of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a> , et al. (486 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="1208.1675v1-abstract-short" style="display: inline;"> The Pierre Auger Observatory is a facility built to detect air showers produced by cosmic rays above 10^17 eV. During clear nights with a low illuminated moon fraction, the UV fluorescence light produced by air showers is recorded by optical telescopes at the Observatory. To correct the observations for variations in atmospheric conditions, atmospheric monitoring is performed at regular intervals… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.1675v1-abstract-full').style.display = 'inline'; document.getElementById('1208.1675v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1208.1675v1-abstract-full" style="display: none;"> The Pierre Auger Observatory is a facility built to detect air showers produced by cosmic rays above 10^17 eV. During clear nights with a low illuminated moon fraction, the UV fluorescence light produced by air showers is recorded by optical telescopes at the Observatory. To correct the observations for variations in atmospheric conditions, atmospheric monitoring is performed at regular intervals ranging from several minutes (for cloud identification) to several hours (for aerosol conditions) to several days (for vertical profiles of temperature, pressure, and humidity). In 2009, the monitoring program was upgraded to allow for additional targeted measurements of atmospheric conditions shortly after the detection of air showers of special interest, e.g., showers produced by very high-energy cosmic rays or showers with atypical longitudinal profiles. The former events are of particular importance for the determination of the energy scale of the Observatory, and the latter are characteristic of unusual air shower physics or exotic primary particle types. The purpose of targeted (or "rapid") monitoring is to improve the resolution of the atmospheric measurements for such events. In this paper, we report on the implementation of the rapid monitoring program and its current status. The rapid monitoring data have been analyzed and applied to the reconstruction of air showers of high interest, and indicate that the air fluorescence measurements affected by clouds and aerosols are effectively corrected using measurements from the regular atmospheric monitoring program. We find that the rapid monitoring program has potential for supporting dedicated physics analyses beyond the standard event reconstruction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.1675v1-abstract-full').style.display = 'none'; document.getElementById('1208.1675v1-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> 4 August, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 7 (2012) P09001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1204.5065">arXiv:1204.5065</a> <span> [<a href="https://arxiv.org/pdf/1204.5065">pdf</a>, <a href="https://arxiv.org/format/1204.5065">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> </div> </div> <p class="title is-5 mathjax"> The JEM-EUSO Mission: Status and Prospects in 2011 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Collaboration%2C+T+J">The JEM-EUSO Collaboration</a>, <a href="/search/?searchtype=author&query=%3A"> :</a>, <a href="/search/?searchtype=author&query=Adams%2C+J+H">J. H. Adams Jr</a>, <a href="/search/?searchtype=author&query=Ahmad%2C+S">S. Ahmad</a>, <a href="/search/?searchtype=author&query=Albert%2C+J+-">J. -N. Albert</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Arai%2C+Y">Y. Arai</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/?searchtype=author&query=Barrillon%2C+P">P. Barrillon</a>, <a href="/search/?searchtype=author&query=Batsch%2C+T">T. Batsch</a>, <a href="/search/?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/?searchtype=author&query=Belenguer%2C+T">T. Belenguer</a>, <a href="/search/?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/?searchtype=author&query=Berlind%2C+A+A">A. A. Berlind</a>, <a href="/search/?searchtype=author&query=Bertaina%2C+M">M. Bertaina</a>, <a href="/search/?searchtype=author&query=Biermann%2C+P+L">P. L. Biermann</a>, <a href="/search/?searchtype=author&query=Biktemerova%2C+S">S. Biktemerova</a>, <a href="/search/?searchtype=author&query=Blaksley%2C+C">C. Blaksley</a>, <a href="/search/?searchtype=author&query=Blecki%2C+J">J. Blecki</a>, <a href="/search/?searchtype=author&query=Blin-Bondil%2C+S">S. Blin-Bondil</a>, <a href="/search/?searchtype=author&query=Bluemer%2C+J">J. Bluemer</a> , et al. (235 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="1204.5065v1-abstract-short" style="display: inline;"> Contributions of the JEM-EUSO Collaboration to the 32nd International Cosmic Ray Conference, Beijing, August, 2011. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1204.5065v1-abstract-full" style="display: none;"> Contributions of the JEM-EUSO Collaboration to the 32nd International Cosmic Ray Conference, Beijing, August, 2011. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1204.5065v1-abstract-full').style.display = 'none'; document.getElementById('1204.5065v1-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> 23 April, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2012. </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">33 contributions plus index</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1202.1493">arXiv:1202.1493</a> <span> [<a href="https://arxiv.org/pdf/1202.1493">pdf</a>, <a href="https://arxiv.org/ps/1202.1493">ps</a>, <a href="https://arxiv.org/format/1202.1493">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> </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.84.122005">10.1103/PhysRevD.84.122005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </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.85.029902">10.1103/PhysRevD.85.029902 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for ultra-high energy neutrinos in highly inclined events at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anticic%2C+T">T. Anticic</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a> , et al. (475 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="1202.1493v1-abstract-short" style="display: inline;"> The Surface Detector of the Pierre Auger Observatory is sensitive to neutrinos of all flavours above 0.1 EeV. These interact through charged and neutral currents in the atmosphere giving rise to extensive air showers. When interacting deeply in the atmosphere at nearly horizontal incidence, neutrinos can be distinguished from regular hadronic cosmic rays by the broad time structure of their shower… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.1493v1-abstract-full').style.display = 'inline'; document.getElementById('1202.1493v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1202.1493v1-abstract-full" style="display: none;"> The Surface Detector of the Pierre Auger Observatory is sensitive to neutrinos of all flavours above 0.1 EeV. These interact through charged and neutral currents in the atmosphere giving rise to extensive air showers. When interacting deeply in the atmosphere at nearly horizontal incidence, neutrinos can be distinguished from regular hadronic cosmic rays by the broad time structure of their shower signals in the water-Cherenkov detectors. In this paper we present for the first time an analysis based on down-going neutrinos. We describe the search procedure, the possible sources of background, the method to compute the exposure and the associated systematic uncertainties. No candidate neutrinos have been found in data collected from 1 January 2004 to 31 May 2010. Assuming an E^-2 differential energy spectrum the limit on the single flavour neutrino is (E^2 * dN/dE) < 1.74x10^-7 GeV cm^-2 s^-1 sr^-1 at 90% C.L. in the energy range 1x10^17 eV < E < 1x10^20 eV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.1493v1-abstract-full').style.display = 'none'; document.getElementById('1202.1493v1-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> 7 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2012. </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, 14 figures, published 30 December 2011</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 84, 122005 (2011); Erratum: Phys. Rev. D 85, 029902(E) (2012) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1201.2276">arXiv:1201.2276</a> <span> [<a href="https://arxiv.org/pdf/1201.2276">pdf</a>, <a href="https://arxiv.org/ps/1201.2276">ps</a>, <a href="https://arxiv.org/format/1201.2276">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> </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.2011.12.002">10.1016/j.astropartphys.2011.12.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Description of Atmospheric Conditions at the Pierre Auger Observatory using the Global Data Assimilation System (GDAS) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a> , et al. (477 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="1201.2276v2-abstract-short" style="display: inline;"> Atmospheric conditions at the site of a cosmic ray observatory must be known for reconstructing observed extensive air showers. The Global Data Assimilation System (GDAS) is a global atmospheric model predicated on meteorological measurements and numerical weather predictions. GDAS provides altitude-dependent profiles of the main state variables of the atmosphere like temperature, pressure, and hu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.2276v2-abstract-full').style.display = 'inline'; document.getElementById('1201.2276v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1201.2276v2-abstract-full" style="display: none;"> Atmospheric conditions at the site of a cosmic ray observatory must be known for reconstructing observed extensive air showers. The Global Data Assimilation System (GDAS) is a global atmospheric model predicated on meteorological measurements and numerical weather predictions. GDAS provides altitude-dependent profiles of the main state variables of the atmosphere like temperature, pressure, and humidity. The original data and their application to the air shower reconstruction of the Pierre Auger Observatory are described. By comparisons with radiosonde and weather station measurements obtained on-site in Malarg眉e and averaged monthly models, the utility of the GDAS data is shown. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1201.2276v2-abstract-full').style.display = 'none'; document.getElementById('1201.2276v2-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> 24 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 January, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart. Phys. 35 (2012) 591-607 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.7122">arXiv:1111.7122</a> <span> [<a href="https://arxiv.org/pdf/1111.7122">pdf</a>, <a href="https://arxiv.org/ps/1111.7122">ps</a>, <a href="https://arxiv.org/format/1111.7122">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> </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/10.1088/1475-7516/2011/11/022">10.1088/1475-7516/2011/11/022 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The effect of the geomagnetic field on cosmic ray energy estimates and large scale anisotropy searches on data from the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avenier%2C+M">M. Avenier</a>, <a href="/search/?searchtype=author&query=Avila%2C+G">G. Avila</a> , et al. (473 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="1111.7122v1-abstract-short" style="display: inline;"> We present a comprehensive study of the influence of the geomagnetic field on the energy estimation of extensive air showers with a zenith angle smaller than $60^\circ$, detected at the Pierre Auger Observatory. The geomagnetic field induces an azimuthal modulation of the estimated energy of cosmic rays up to the ~2% level at large zenith angles. We present a method to account for this modulation… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.7122v1-abstract-full').style.display = 'inline'; document.getElementById('1111.7122v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.7122v1-abstract-full" style="display: none;"> We present a comprehensive study of the influence of the geomagnetic field on the energy estimation of extensive air showers with a zenith angle smaller than $60^\circ$, detected at the Pierre Auger Observatory. The geomagnetic field induces an azimuthal modulation of the estimated energy of cosmic rays up to the ~2% level at large zenith angles. We present a method to account for this modulation of the reconstructed energy. We analyse the effect of the modulation on large scale anisotropy searches in the arrival direction distributions of cosmic rays. At a given energy, the geomagnetic effect is shown to induce a pseudo-dipolar pattern at the percent level in the declination distribution that needs to be accounted for. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.7122v1-abstract-full').style.display = 'none'; document.getElementById('1111.7122v1-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> 30 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </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">20 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP11 (2011) 022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.6764">arXiv:1111.6764</a> <span> [<a href="https://arxiv.org/pdf/1111.6764">pdf</a>, <a href="https://arxiv.org/ps/1111.6764">ps</a>, <a href="https://arxiv.org/format/1111.6764">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> </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.nima.2009.11.018">10.1016/j.nima.2009.11.018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Trigger and Aperture of the Surface Detector Array of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abraham%2C+J">J. Abraham</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Aguirre%2C+C">C. Aguirre</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Argir%C3%B2%2C+S">S. Argir貌</a>, <a href="/search/?searchtype=author&query=Arisaka%2C+K">K. Arisaka</a>, <a href="/search/?searchtype=author&query=Arneodo%2C+F">F. Arneodo</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asch%2C+T">T. Asch</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avila%2C+G">G. Avila</a> , et al. (447 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="1111.6764v1-abstract-short" style="display: inline;"> The surface detector array of the Pierre Auger Observatory consists of 1600 water-Cherenkov detectors, for the study of extensive air showers (EAS) generated by ultra-high-energy cosmic rays. We describe the trigger hierarchy, from the identification of candidate showers at the level of a single detector, amongst a large background (mainly random single cosmic ray muons), up to the selection of re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.6764v1-abstract-full').style.display = 'inline'; document.getElementById('1111.6764v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.6764v1-abstract-full" style="display: none;"> The surface detector array of the Pierre Auger Observatory consists of 1600 water-Cherenkov detectors, for the study of extensive air showers (EAS) generated by ultra-high-energy cosmic rays. We describe the trigger hierarchy, from the identification of candidate showers at the level of a single detector, amongst a large background (mainly random single cosmic ray muons), up to the selection of real events and the rejection of random coincidences. Such trigger makes the surface detector array fully efficient for the detection of EAS with energy above $3\times 10^{18}$ eV, for all zenith angles between 0$^\circ$ and 60$^\circ$, independently of the position of the impact point and of the mass of the primary particle. In these range of energies and angles, the exposure of the surface array can be determined purely on the basis of the geometrical acceptance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.6764v1-abstract-full').style.display = 'none'; document.getElementById('1111.6764v1-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> 29 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </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">29 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Nucl. Instrum. Methods A 613 (2010) 29-39 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.6645">arXiv:1111.6645</a> <span> [<a href="https://arxiv.org/pdf/1111.6645">pdf</a>, <a href="https://arxiv.org/ps/1111.6645">ps</a>, <a href="https://arxiv.org/format/1111.6645">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="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.2011.08.001">10.1016/j.astropartphys.2011.08.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Lateral Trigger Probability function for the Ultra-High Energy Cosmic Ray Showers detected by the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avenier%2C+M">M. Avenier</a> , et al. (473 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="1111.6645v1-abstract-short" style="display: inline;"> In this paper we introduce the concept of Lateral Trigger Probability (LTP) function, i.e., the probability for an extensive air shower (EAS) to trigger an individual detector of a ground based array as a function of distance to the shower axis, taking into account energy, mass and direction of the primary cosmic ray. We apply this concept to the surface array of the Pierre Auger Observatory consi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.6645v1-abstract-full').style.display = 'inline'; document.getElementById('1111.6645v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.6645v1-abstract-full" style="display: none;"> In this paper we introduce the concept of Lateral Trigger Probability (LTP) function, i.e., the probability for an extensive air shower (EAS) to trigger an individual detector of a ground based array as a function of distance to the shower axis, taking into account energy, mass and direction of the primary cosmic ray. We apply this concept to the surface array of the Pierre Auger Observatory consisting of a 1.5 km spaced grid of about 1600 water Cherenkov stations. Using Monte Carlo simulations of ultra-high energy showers the LTP functions are derived for energies in the range between 10^{17} and 10^{19} eV and zenith angles up to 65 degs. A parametrization combining a step function with an exponential is found to reproduce them very well in the considered range of energies and zenith angles. The LTP functions can also be obtained from data using events simultaneously observed by the fluorescence and the surface detector of the Pierre Auger Observatory (hybrid events). We validate the Monte-Carlo results showing how LTP functions from data are in good agreement with simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.6645v1-abstract-full').style.display = 'none'; document.getElementById('1111.6645v1-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> 28 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </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">22 pages, 8 figures. Published in Astroparticle Physics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astroparticle Physics 35 (2011) 266-276 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.3290">arXiv:1111.3290</a> <span> [<a href="https://arxiv.org/pdf/1111.3290">pdf</a>, <a href="https://arxiv.org/format/1111.3290">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> </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.2011.10.011">10.1016/j.astropartphys.2011.10.011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Extragalactic propagation of ultrahigh energy cosmic-rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a> </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="1111.3290v1-abstract-short" style="display: inline;"> In this paper we review the extragalactic propagation of ultrahigh energy cosmic-rays (UHECR). We present the different energy loss processes of protons and nuclei, and their expected influence on energy evolution of the UHECR spectrum and composition. We discuss the possible implications of the recent composition analyses provided by the Pierre Auger Observatory. The influence of extragalactic ma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.3290v1-abstract-full').style.display = 'inline'; document.getElementById('1111.3290v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.3290v1-abstract-full" style="display: none;"> In this paper we review the extragalactic propagation of ultrahigh energy cosmic-rays (UHECR). We present the different energy loss processes of protons and nuclei, and their expected influence on energy evolution of the UHECR spectrum and composition. We discuss the possible implications of the recent composition analyses provided by the Pierre Auger Observatory. The influence of extragalactic magnetic fields and possible departures from the rectilinear case are also mentioned as well as the production of secondary cosmogenic neutrinos and photons and the constraints their observation would imply for the UHECRs origin. Finally, we conclude by briefly discussing the relevance of a multi messenger approach for solving the mystery of UHECRs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.3290v1-abstract-full').style.display = 'none'; document.getElementById('1111.3290v1-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 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </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">45 pages, 16 figures Extended version of a paper to be published in the topical issue of Astroparticle Physics on Cosmic-rays</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1111.2472">arXiv:1111.2472</a> <span> [<a href="https://arxiv.org/pdf/1111.2472">pdf</a>, <a href="https://arxiv.org/ps/1111.2472">ps</a>, <a href="https://arxiv.org/format/1111.2472">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> </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.2011.10.004">10.1016/j.astropartphys.2011.10.004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for signatures of magnetically-induced alignment in the arrival directions measured by the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avenier%2C+M">M. Avenier</a> , et al. (474 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="1111.2472v1-abstract-short" style="display: inline;"> We present the results of an analysis of data recorded at the Pierre Auger Observatory in which we search for groups of directionally-aligned events (or `multiplets') which exhibit a correlation between arrival direction and the inverse of the energy. These signatures are expected from sets of events coming from the same source after having been deflected by intervening coherent magnetic fields. T… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.2472v1-abstract-full').style.display = 'inline'; document.getElementById('1111.2472v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1111.2472v1-abstract-full" style="display: none;"> We present the results of an analysis of data recorded at the Pierre Auger Observatory in which we search for groups of directionally-aligned events (or `multiplets') which exhibit a correlation between arrival direction and the inverse of the energy. These signatures are expected from sets of events coming from the same source after having been deflected by intervening coherent magnetic fields. The observation of several events from the same source would open the possibility to accurately reconstruct the position of the source and also measure the integral of the component of the magnetic field orthogonal to the trajectory of the cosmic rays. We describe the largest multiplets found and compute the probability that they appeared by chance from an isotropic distribution. We find no statistically significant evidence for the presence of multiplets arising from magnetic deflections in the present data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1111.2472v1-abstract-full').style.display = 'none'; document.getElementById('1111.2472v1-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> 10 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2011. </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">Accepted for publication in Astroparticle Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1107.4809">arXiv:1107.4809</a> <span> [<a href="https://arxiv.org/pdf/1107.4809">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 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> </div> </div> <p class="title is-5 mathjax"> The Pierre Auger Observatory I: The Cosmic Ray Energy Spectrum and Related Measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avenier%2C+M">M. Avenier</a> , et al. (471 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="1107.4809v1-abstract-short" style="display: inline;"> Studies of the cosmic ray energy spectrum at the highest energies with the Pierre Auger Observatory </span> <span class="abstract-full has-text-grey-dark mathjax" id="1107.4809v1-abstract-full" style="display: none;"> Studies of the cosmic ray energy spectrum at the highest energies with the Pierre Auger Observatory <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.4809v1-abstract-full').style.display = 'none'; document.getElementById('1107.4809v1-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> 24 July, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2011. </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">Contributions to the 32nd International Cosmic Ray Conference, Beijing, China, August 2011</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1107.4807">arXiv:1107.4807</a> <span> [<a href="https://arxiv.org/pdf/1107.4807">pdf</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/10.1088/1742-6596/375/1/052006">10.1088/1742-6596/375/1/052006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Pierre Auger Observatory V: Enhancements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avenier%2C+M">M. Avenier</a> , et al. (471 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="1107.4807v1-abstract-short" style="display: inline;"> Ongoing and planned enhancements of the Pierre Auger Observatory </span> <span class="abstract-full has-text-grey-dark mathjax" id="1107.4807v1-abstract-full" style="display: none;"> Ongoing and planned enhancements of the Pierre Auger Observatory <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.4807v1-abstract-full').style.display = 'none'; document.getElementById('1107.4807v1-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> 24 July, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2011. </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">Contributions to 32nd International Cosmic Ray Conference, Beijing, China, August 2011</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1107.4806">arXiv:1107.4806</a> <span> [<a href="https://arxiv.org/pdf/1107.4806">pdf</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> <p class="title is-5 mathjax"> The Pierre Auger Observatory IV: Operation and Monitoring </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avenier%2C+M">M. Avenier</a> , et al. (471 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="1107.4806v1-abstract-short" style="display: inline;"> Technical reports on operations and monitoring of the Pierre Auger Observatory </span> <span class="abstract-full has-text-grey-dark mathjax" id="1107.4806v1-abstract-full" style="display: none;"> Technical reports on operations and monitoring of the Pierre Auger Observatory <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.4806v1-abstract-full').style.display = 'none'; document.getElementById('1107.4806v1-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> 24 July, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2011. </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">Constributions to 32nd International Cosmic Ray Conference, Beijing, China, August 2011</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1107.4805">arXiv:1107.4805</a> <span> [<a href="https://arxiv.org/pdf/1107.4805">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 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> </div> </div> <p class="title is-5 mathjax"> The Pierre Auger Observatory III: Other Astrophysical Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avenier%2C+M">M. Avenier</a> , et al. (471 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="1107.4805v1-abstract-short" style="display: inline;"> Astrophysical observations of ultra-high-energy cosmic rays with the Pierre Auger Observatory </span> <span class="abstract-full has-text-grey-dark mathjax" id="1107.4805v1-abstract-full" style="display: none;"> Astrophysical observations of ultra-high-energy cosmic rays with the Pierre Auger Observatory <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.4805v1-abstract-full').style.display = 'none'; document.getElementById('1107.4805v1-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> 24 July, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2011. </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">Contributions to the 32nd International Cosmic Ray Conference, Beijing, China, August 2011</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1107.4804">arXiv:1107.4804</a> <span> [<a href="https://arxiv.org/pdf/1107.4804">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 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> </div> </div> <p class="title is-5 mathjax"> The Pierre Auger Observatory II: Studies of Cosmic Ray Composition and Hadronic Interaction models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avenier%2C+M">M. Avenier</a> , et al. (471 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="1107.4804v1-abstract-short" style="display: inline;"> Studies of the composition of the highest energy cosmic rays with the Pierre Auger Observatory, including examination of hadronic physics effects on the structure of extensive air showers. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1107.4804v1-abstract-full" style="display: none;"> Studies of the composition of the highest energy cosmic rays with the Pierre Auger Observatory, including examination of hadronic physics effects on the structure of extensive air showers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.4804v1-abstract-full').style.display = 'none'; document.getElementById('1107.4804v1-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> 24 July, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2011. </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">Contributions to the 32nd International Cosmic Ray Conference, Beijing, China, August 2011</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1107.3722">arXiv:1107.3722</a> <span> [<a href="https://arxiv.org/pdf/1107.3722">pdf</a>, <a href="https://arxiv.org/format/1107.3722">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="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/10.1051/0004-6361/201117673">10.1051/0004-6361/201117673 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on the origin of ultra-high-energy cosmic rays from cosmogenic neutrinos and photons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Decerprit%2C+G">Guillaume Decerprit</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">Denis Allard</a> </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="1107.3722v4-abstract-short" style="display: inline;"> We study the production of cosmogenic neutrinos and photons during the extragalactic propagation of ultra-high-energy cosmic rays (UHECRs). For a wide range of models in cosmological evolution of source luminosity, composition and maximum energy we calculate the expected flux of cosmogenic secondaries by normalizing our cosmic ray output to experimental spectra and comparing the diffuse flux of Ge… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.3722v4-abstract-full').style.display = 'inline'; document.getElementById('1107.3722v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1107.3722v4-abstract-full" style="display: none;"> We study the production of cosmogenic neutrinos and photons during the extragalactic propagation of ultra-high-energy cosmic rays (UHECRs). For a wide range of models in cosmological evolution of source luminosity, composition and maximum energy we calculate the expected flux of cosmogenic secondaries by normalizing our cosmic ray output to experimental spectra and comparing the diffuse flux of GeV-TeV gamma-rays to the experimental one measured by the Fermi satellite. Most of these models yield significant neutrino fluxes for current experiments like IceCube or Pierre Auger. Furthermore, we discuss the possibilities of signing the presence of UHE proton sources either within or outside the cosmic ray horizon using neutrinos or photons observations even if the cosmic ray composition becomes heavier at the highest energies. We discuss the possible constraints that could be brought on the UHECR origin from the different messengers and energy ranges. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1107.3722v4-abstract-full').style.display = 'none'; document.getElementById('1107.3722v4-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 November, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 July, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2011. </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">17 pages, 13 figures, published in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astronomy & Astrophysics, 535, A66 (2011) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1106.3048">arXiv:1106.3048</a> <span> [<a href="https://arxiv.org/pdf/1106.3048">pdf</a>, <a href="https://arxiv.org/ps/1106.3048">ps</a>, <a href="https://arxiv.org/format/1106.3048">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> </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/10.1088/1475-7516/2011/06/022">10.1088/1475-7516/2011/06/022 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Anisotropy and chemical composition of ultra-high energy cosmic rays using arrival directions measured by the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avenier%2C+M">M. Avenier</a> , et al. (468 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="1106.3048v2-abstract-short" style="display: inline;"> The Pierre Auger Collaboration has reported evidence for anisotropy in the distribution of arrival directions of the cosmic rays with energies $E>E_{th}=5.5\times 10^{19}$ eV. These show a correlation with the distribution of nearby extragalactic objects, including an apparent excess around the direction of Centaurus A. If the particles responsible for these excesses at $E>E_{th}$ are heavy nuclei… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.3048v2-abstract-full').style.display = 'inline'; document.getElementById('1106.3048v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1106.3048v2-abstract-full" style="display: none;"> The Pierre Auger Collaboration has reported evidence for anisotropy in the distribution of arrival directions of the cosmic rays with energies $E>E_{th}=5.5\times 10^{19}$ eV. These show a correlation with the distribution of nearby extragalactic objects, including an apparent excess around the direction of Centaurus A. If the particles responsible for these excesses at $E>E_{th}$ are heavy nuclei with charge $Z$, the proton component of the sources should lead to excesses in the same regions at energies $E/Z$. We here report the lack of anisotropies in these directions at energies above $E_{th}/Z$ (for illustrative values of $Z=6,\ 13,\ 26$). If the anisotropies above $E_{th}$ are due to nuclei with charge $Z$, and under reasonable assumptions about the acceleration process, these observations imply stringent constraints on the allowed proton fraction at the lower energies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1106.3048v2-abstract-full').style.display = 'none'; document.getElementById('1106.3048v2-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> 4 July, 2011; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 June, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2011. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP06 (2011) 022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1103.2721">arXiv:1103.2721</a> <span> [<a href="https://arxiv.org/pdf/1103.2721">pdf</a>, <a href="https://arxiv.org/ps/1103.2721">ps</a>, <a href="https://arxiv.org/format/1103.2721">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> </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.2010.12.007">10.1016/j.astropartphys.2010.12.007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for First Harmonic Modulation in the Right Ascension Distribution of Cosmic Rays Detected at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/?searchtype=author&query=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/?searchtype=author&query=Avenier%2C+M">M. Avenier</a>, <a href="/search/?searchtype=author&query=Avila%2C+G">G. Avila</a> , et al. (444 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="1103.2721v1-abstract-short" style="display: inline;"> We present the results of searches for dipolar-type anisotropies in different energy ranges above $2.5\times 10^{17}$ eV with the surface detector array of the Pierre Auger Observatory, reporting on both the phase and the amplitude measurements of the first harmonic modulation in the right-ascension distribution. Upper limits on the amplitudes are obtained, which provide the most stringent bounds… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1103.2721v1-abstract-full').style.display = 'inline'; document.getElementById('1103.2721v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1103.2721v1-abstract-full" style="display: none;"> We present the results of searches for dipolar-type anisotropies in different energy ranges above $2.5\times 10^{17}$ eV with the surface detector array of the Pierre Auger Observatory, reporting on both the phase and the amplitude measurements of the first harmonic modulation in the right-ascension distribution. Upper limits on the amplitudes are obtained, which provide the most stringent bounds at present, being below 2% at 99% $C.L.$ for EeV energies. We also compare our results to those of previous experiments as well as with some theoretical expectations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1103.2721v1-abstract-full').style.display = 'none'; document.getElementById('1103.2721v1-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 March, 2011; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2011. </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">28 pages, 11 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart.Phys.34:627-639,2011 </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" 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