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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/2410.16042">arXiv:2410.16042</a> <span> [<a href="https://arxiv.org/pdf/2410.16042">pdf</a>, <a href="https://arxiv.org/format/2410.16042">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/10.1051/0004-6361/202450889">10.1051/0004-6361/202450889 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A new method of reconstructing images of gamma-ray telescopes applied to the LST-1 of CTAO </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Project%2C+C">CTA-LST Project</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Alispach%2C+C">C. Alispach</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+N+A">N. Alvarez Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosino%2C+D">D. Ambrosino</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arbet-Engels%2C+A">A. Arbet-Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+P">P. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Balbo%2C+M">M. Balbo</a>, <a href="/search/astro-ph?searchtype=author&query=Bamba%2C+A">A. Bamba</a>, <a href="/search/astro-ph?searchtype=author&query=Larriva%2C+A+B">A. Baquero Larriva</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Jim%C3%A9nez%2C+L+B">L. Barrios Jim茅nez</a>, <a href="/search/astro-ph?searchtype=author&query=Batkovic%2C+I">I. Batkovic</a> , et al. (283 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="2410.16042v1-abstract-short" style="display: inline;"> Imaging atmospheric Cherenkov telescopes (IACTs) are used to observe very high-energy photons from the ground. Gamma rays are indirectly detected through the Cherenkov light emitted by the air showers they induce. The new generation of experiments, in particular the Cherenkov Telescope Array Observatory (CTAO), sets ambitious goals for discoveries of new gamma-ray sources and precise measurements… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16042v1-abstract-full').style.display = 'inline'; document.getElementById('2410.16042v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.16042v1-abstract-full" style="display: none;"> Imaging atmospheric Cherenkov telescopes (IACTs) are used to observe very high-energy photons from the ground. Gamma rays are indirectly detected through the Cherenkov light emitted by the air showers they induce. The new generation of experiments, in particular the Cherenkov Telescope Array Observatory (CTAO), sets ambitious goals for discoveries of new gamma-ray sources and precise measurements of the already discovered ones. To achieve these goals, both hardware and data analysis must employ cutting-edge techniques. This also applies to the LST-1, the first IACT built for the CTAO, which is currently taking data on the Canary island of La Palma. This paper introduces a new event reconstruction technique for IACT data, aiming to improve the image reconstruction quality and the discrimination between the signal and the background from misidentified hadrons and electrons. The technique models the development of the extensive air shower signal, recorded as a waveform per pixel, seen by CTAO telescopes' cameras. Model parameters are subsequently passed to random forest regressors and classifiers to extract information on the primary particle. The new reconstruction was applied to simulated data and to data from observations of the Crab Nebula performed by the LST-1. The event reconstruction method presented here shows promising performance improvements. The angular and energy resolution, and the sensitivity, are improved by 10 to 20% over most of the energy range. At low energy, improvements reach up to 22%, 47%, and 50%, respectively. A future extension of the method to stereoscopic analysis for telescope arrays will be the next important step. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16042v1-abstract-full').style.display = 'none'; document.getElementById('2410.16042v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Accepted in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 691, A328 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.05292">arXiv:2408.05292</a> <span> [<a href="https://arxiv.org/pdf/2408.05292">pdf</a>, <a href="https://arxiv.org/format/2408.05292">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"> Large-scale cosmic ray anisotropies with 19 years of data from the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosone%2C+A">A. Ambrosone</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Dourado%2C+L+A">L. Andrade Dourado</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a> , et al. (333 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="2408.05292v2-abstract-short" style="display: inline;"> Results are presented for the measurement of large-scale anisotropies in the arrival directions of ultra-high-energy cosmic rays detected at the Pierre Auger Observatory during 19 years of operation, prior to AugerPrime, the upgrade of the Observatory. The 3D dipole amplitude and direction are reconstructed above $4\,$EeV in four energy bins. Besides the established dipolar anisotropy in right asc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.05292v2-abstract-full').style.display = 'inline'; document.getElementById('2408.05292v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.05292v2-abstract-full" style="display: none;"> Results are presented for the measurement of large-scale anisotropies in the arrival directions of ultra-high-energy cosmic rays detected at the Pierre Auger Observatory during 19 years of operation, prior to AugerPrime, the upgrade of the Observatory. The 3D dipole amplitude and direction are reconstructed above $4\,$EeV in four energy bins. Besides the established dipolar anisotropy in right ascension above $8\,$EeV, the Fourier amplitude of the $8$ to $16\,$EeV energy bin is now also above the $5蟽$ discovery level. No time variation of the dipole moment above $8\,$EeV is found, setting an upper limit to the rate of change of such variations of $0.3\%$ per year at the $95\%$ confidence level. Additionally, the results for the angular power spectrum are shown, demonstrating no other statistically significant multipoles. The results for the equatorial dipole component down to $0.03\,$EeV are presented, using for the first time a data set obtained with a trigger that has been optimized for lower energies. Finally, model predictions are discussed and compared with observations, based on two source emission scenarios obtained in the combined fit of spectrum and composition above $0.6\,$EeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.05292v2-abstract-full').style.display = 'none'; document.getElementById('2408.05292v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">Minor modifications, accepted for publication in Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.06874">arXiv:2407.06874</a> <span> [<a href="https://arxiv.org/pdf/2407.06874">pdf</a>, <a href="https://arxiv.org/format/2407.06874">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"> The flux of ultra-high-energy cosmic rays along the supergalactic plane measured at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Dourado%2C+L+A">L. Andrade Dourado</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a> , et al. (342 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="2407.06874v1-abstract-short" style="display: inline;"> Ultra-high-energy cosmic rays are known to be mainly of extragalactic origin, and their propagation is limited by energy losses, so their arrival directions are expected to correlate with the large-scale structure of the local Universe. In this work, we investigate the possible presence of intermediate-scale excesses in the flux of the most energetic cosmic rays from the direction of the supergala… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06874v1-abstract-full').style.display = 'inline'; document.getElementById('2407.06874v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.06874v1-abstract-full" style="display: none;"> Ultra-high-energy cosmic rays are known to be mainly of extragalactic origin, and their propagation is limited by energy losses, so their arrival directions are expected to correlate with the large-scale structure of the local Universe. In this work, we investigate the possible presence of intermediate-scale excesses in the flux of the most energetic cosmic rays from the direction of the supergalactic plane region using events with energies above 20 EeV recorded with the surface detector array of the Pierre Auger Observatory up to 31 December 2022, with a total exposure of 135,000 km^2 sr yr. The strongest indication for an excess that we find, with a post-trial significance of 3.1蟽, is in the Centaurus region, as in our previous reports, and it extends down to lower energies than previously studied. We do not find any strong hints of excesses from any other region of the supergalactic plane at the same angular scale. In particular, our results do not confirm the reports by the Telescope Array collaboration of excesses from two regions in the Northern Hemisphere at the edge of the field of view of the Pierre Auger Observatory. With a comparable exposure, our results in those regions are in good agreement with the expectations from an isotropic distribution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.06874v1-abstract-full').style.display = 'none'; document.getElementById('2407.06874v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">submitted to 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/2407.02343">arXiv:2407.02343</a> <span> [<a href="https://arxiv.org/pdf/2407.02343">pdf</a>, <a href="https://arxiv.org/format/2407.02343">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"> A detailed study of the very-high-energy Crab pulsar emission with the LST-1 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Project%2C+C">CTA-LST Project</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+N+A">N. Alvarez Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arbet-Engels%2C+A">A. Arbet-Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+P">P. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Bamba%2C+A">A. Bamba</a>, <a href="/search/astro-ph?searchtype=author&query=Larriva%2C+A+B">A. Baquero Larriva</a>, <a href="/search/astro-ph?searchtype=author&query=Baroncelli%2C+L">L. Baroncelli</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Batkovic%2C+I">I. Batkovic</a>, <a href="/search/astro-ph?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a> , et al. (272 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="2407.02343v1-abstract-short" style="display: inline;"> Context: There are currently three pulsars firmly detected by imaging atmospheric Cherenkov telescopes (IACTs), two of them reaching TeV energies, challenging models of very-high-energy (VHE) emission in pulsars. More precise observations are needed to better characterize pulsar emission at these energies. The LST-1 is the prototype of the Large-Sized Telescope, that will be part of the Cherenkov… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.02343v1-abstract-full').style.display = 'inline'; document.getElementById('2407.02343v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.02343v1-abstract-full" style="display: none;"> Context: There are currently three pulsars firmly detected by imaging atmospheric Cherenkov telescopes (IACTs), two of them reaching TeV energies, challenging models of very-high-energy (VHE) emission in pulsars. More precise observations are needed to better characterize pulsar emission at these energies. The LST-1 is the prototype of the Large-Sized Telescope, that will be part of the Cherenkov Telescope Array Observatory (CTAO). Its improved performance over previous IACTs makes it well suited for studying pulsars. Aims: To study the Crab pulsar emission with the LST-1, improving and complementing the results from other telescopes. These observations can also be used to characterize the potential of the LST-1 to study other pulsars and detect new ones. Methods: We analyzed a total of $\sim$103 hours of gamma-ray observations of the Crab pulsar conducted with the LST-1 in the period from September 2020 to January 2023. The observations were carried out at zenith angles less than 50 degrees. A new analysis of the Fermi-LAT data was also performed, including $\sim$14 years of observations. Results: The Crab pulsar phaseogram, long-term light-curve, and phase-resolved spectra are reconstructed with the LST-1 from 20 GeV to 450 GeV for P1 and up to 700 GeV for P2. The pulsed emission is detected with a significance of 15.2$蟽$. The two characteristic emission peaks of the Crab pulsar are clearly detected (>10$蟽$), as well as the so-called bridge emission (5.7$蟽$). We find that both peaks are well described by power laws, with spectral indices of $\sim$3.44 and $\sim$3.03 respectively. The joint analysis of Fermi-LAT and LST-1 data shows a good agreement between both instruments in the overlapping energy range. The detailed results obtained in the first observations of the Crab pulsar with LST-1 show the potential that CTAO will have to study this type of sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.02343v1-abstract-full').style.display = 'none'; document.getElementById('2407.02343v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.07439">arXiv:2406.07439</a> <span> [<a href="https://arxiv.org/pdf/2406.07439">pdf</a>, <a href="https://arxiv.org/format/2406.07439">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Search for photons above 10$^{18}$ eV by simultaneously measuring the atmospheric depth and the muon content of air showers at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Dourado%2C+L+A">L. Andrade Dourado</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a> , et al. (342 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="2406.07439v1-abstract-short" style="display: inline;"> The Pierre Auger Observatory is the most sensitive instrument to detect photons with energies above $10^{17}$ eV. It measures extensive air showers generated by ultra high energy cosmic rays using a hybrid technique that exploits the combination of a fluorescence detector with a ground array of particle detectors. The signatures of a photon-induced air shower are a larger atmospheric depth of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07439v1-abstract-full').style.display = 'inline'; document.getElementById('2406.07439v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.07439v1-abstract-full" style="display: none;"> The Pierre Auger Observatory is the most sensitive instrument to detect photons with energies above $10^{17}$ eV. It measures extensive air showers generated by ultra high energy cosmic rays using a hybrid technique that exploits the combination of a fluorescence detector with a ground array of particle detectors. The signatures of a photon-induced air shower are a larger atmospheric depth of the shower maximum ($X_{max}$) and a steeper lateral distribution function, along with a lower number of muons with respect to the bulk of hadron-induced cascades. In this work, a new analysis technique in the energy interval between 1 and 30 EeV (1 EeV = $10^{18}$ eV) has been developed by combining the fluorescence detector-based measurement of $X_{max}$ with the specific features of the surface detector signal through a parameter related to the air shower muon content, derived from the universality of the air shower development. No evidence of a statistically significant signal due to photon primaries was found using data collected in about 12 years of operation. Thus, upper bounds to the integral photon flux have been set using a detailed calculation of the detector exposure, in combination with a data-driven background estimation. The derived 95% confidence level upper limits are 0.0403, 0.01113, 0.0035, 0.0023, and 0.0021 km$^{-2}$ sr$^{-1}$ yr$^{-1}$ above 1, 2, 3, 5, and 10 EeV, respectively, leading to the most stringent upper limits on the photon flux in the EeV range. Compared with past results, the upper limits were improved by about 40% for the lowest energy threshold and by a factor 3 above 3 EeV, where no candidates were found and the expected background is negligible. The presented limits can be used to probe the assumptions on chemical composition of ultra-high energy cosmic rays and allow for the constraint of the mass and lifetime phase space of super-heavy dark matter particles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07439v1-abstract-full').style.display = 'none'; document.getElementById('2406.07439v1-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 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">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 22 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/2406.06319">arXiv:2406.06319</a> <span> [<a href="https://arxiv.org/pdf/2406.06319">pdf</a>, <a href="https://arxiv.org/format/2406.06319">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> <p class="title is-5 mathjax"> Measurement of the Depth of Maximum of Air-Shower Profiles with energies between $\mathbf{10^{18.5}}$ and $\mathbf{10^{20}}$ eV using the Surface Detector of the Pierre Auger Observatory and Deep Learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Dourado%2C+L+A">L. Andrade Dourado</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a> , et al. (342 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="2406.06319v1-abstract-short" style="display: inline;"> We report an investigation of the mass composition of cosmic rays with energies from 3 to 100 EeV (1 EeV=$10^{18}$ eV) using the distributions of the depth of shower maximum $X_\mathrm{max}$. The analysis relies on ${\sim}50,000$ events recorded by the Surface Detector of the Pierre Auger Observatory and a deep-learning-based reconstruction algorithm. Above energies of 5 EeV, the data set offers a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06319v1-abstract-full').style.display = 'inline'; document.getElementById('2406.06319v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.06319v1-abstract-full" style="display: none;"> We report an investigation of the mass composition of cosmic rays with energies from 3 to 100 EeV (1 EeV=$10^{18}$ eV) using the distributions of the depth of shower maximum $X_\mathrm{max}$. The analysis relies on ${\sim}50,000$ events recorded by the Surface Detector of the Pierre Auger Observatory and a deep-learning-based reconstruction algorithm. Above energies of 5 EeV, the data set offers a 10-fold increase in statistics with respect to fluorescence measurements at the Observatory. After cross-calibration using the Fluorescence Detector, this enables the first measurement of the evolution of the mean and the standard deviation of the $X_\mathrm{max}$ distributions up to 100 EeV. Our findings are threefold: (1.) The evolution of the mean logarithmic mass towards a heavier composition with increasing energy can be confirmed and is extended to 100 EeV. (2.) The evolution of the fluctuations of $X_\mathrm{max}$ towards a heavier and purer composition with increasing energy can be confirmed with high statistics. We report a rather heavy composition and small fluctuations in $X_\mathrm{max}$ at the highest energies. (3.) We find indications for a characteristic structure beyond a constant change in the mean logarithmic mass, featuring three breaks that are observed in proximity to the ankle, instep, and suppression features in the energy spectrum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06319v1-abstract-full').style.display = 'none'; document.getElementById('2406.06319v1-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 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">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to Phys. Rev. D, 28 pages, 18 figures, 5 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.06315">arXiv:2406.06315</a> <span> [<a href="https://arxiv.org/pdf/2406.06315">pdf</a>, <a href="https://arxiv.org/format/2406.06315">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> <p class="title is-5 mathjax"> Inference of the Mass Composition of Cosmic Rays with energies from $\mathbf{10^{18.5}}$ to $\mathbf{10^{20}}$ eV using the Pierre Auger Observatory and Deep Learning </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Dourado%2C+L+A">L. Andrade Dourado</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a> , et al. (342 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="2406.06315v1-abstract-short" style="display: inline;"> We present measurements of the atmospheric depth of the shower maximum $X_\mathrm{max}$, inferred for the first time on an event-by-event level using the Surface Detector of the Pierre Auger Observatory. Using deep learning, we were able to extend measurements of the $X_\mathrm{max}$ distributions up to energies of 100 EeV ($10^{20}$ eV), not yet revealed by current measurements, providing new ins… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06315v1-abstract-full').style.display = 'inline'; document.getElementById('2406.06315v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.06315v1-abstract-full" style="display: none;"> We present measurements of the atmospheric depth of the shower maximum $X_\mathrm{max}$, inferred for the first time on an event-by-event level using the Surface Detector of the Pierre Auger Observatory. Using deep learning, we were able to extend measurements of the $X_\mathrm{max}$ distributions up to energies of 100 EeV ($10^{20}$ eV), not yet revealed by current measurements, providing new insights into the mass composition of cosmic rays at extreme energies. Gaining a 10-fold increase in statistics compared to the Fluorescence Detector data, we find evidence that the rate of change of the average $X_\mathrm{max}$ with the logarithm of energy features three breaks at $6.5\pm0.6~(\mathrm{stat})\pm1~(\mathrm{sys})$ EeV, $11\pm 2~(\mathrm{stat})\pm1~(\mathrm{sys})$ EeV, and $31\pm5~(\mathrm{stat})\pm3~(\mathrm{sys})$ EeV, in the vicinity to the three prominent features (ankle, instep, suppression) of the cosmic-ray flux. The energy evolution of the mean and standard deviation of the measured $X_\mathrm{max}$ distributions indicates that the mass composition becomes increasingly heavier and purer, thus being incompatible with a large fraction of light nuclei between 50 EeV and 100 EeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06315v1-abstract-full').style.display = 'none'; document.getElementById('2406.06315v1-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 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">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to Phys. Rev. Lett., 10 pages, 3 figures, 1 table</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03533">arXiv:2404.03533</a> <span> [<a href="https://arxiv.org/pdf/2404.03533">pdf</a>, <a href="https://arxiv.org/format/2404.03533">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/10.1088/1475-7516/2024/07/094">10.1088/1475-7516/2024/07/094 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Impact of the Magnetic Horizon on the Interpretation of the Pierre Auger Observatory Spectrum and Composition Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Mocellin%2C+A+B">A. Bartz Mocellin</a> , et al. (342 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="2404.03533v2-abstract-short" style="display: inline;"> The flux of ultra-high energy cosmic rays reaching Earth above the ankle energy (5 EeV) can be described as a mixture of nuclei injected by extragalactic sources with very hard spectra and a low rigidity cutoff. Extragalactic magnetic fields existing between the Earth and the closest sources can affect the observed CR spectrum by reducing the flux of low-rigidity particles reaching Earth. We perfo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03533v2-abstract-full').style.display = 'inline'; document.getElementById('2404.03533v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03533v2-abstract-full" style="display: none;"> The flux of ultra-high energy cosmic rays reaching Earth above the ankle energy (5 EeV) can be described as a mixture of nuclei injected by extragalactic sources with very hard spectra and a low rigidity cutoff. Extragalactic magnetic fields existing between the Earth and the closest sources can affect the observed CR spectrum by reducing the flux of low-rigidity particles reaching Earth. We perform a combined fit of the spectrum and distributions of depth of shower maximum measured with the Pierre Auger Observatory including the effect of this magnetic horizon in the propagation of UHECRs in the intergalactic space. We find that, within a specific range of the various experimental and phenomenological systematics, the magnetic horizon effect can be relevant for turbulent magnetic field strengths in the local neighbourhood of order $B_{\rm rms}\simeq (50-100)\,{\rm nG}\,(20\rm{Mpc}/{d_{\rm s})( 100\,\rm{kpc}/L_{\rm coh}})^{1/2}$, with $d_{\rm s}$ the typical intersource separation and $L_{\rm coh}$ the magnetic field coherence length. When this is the case, the inferred slope of the source spectrum becomes softer and can be closer to the expectations of diffusive shock acceleration, i.e., $\propto E^{-2}$. An additional cosmic-ray population with higher source density and softer spectra, presumably also extragalactic and dominating the cosmic-ray flux at EeV energies, is also required to reproduce the overall spectrum and composition results for all energies down to 0.6~EeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03533v2-abstract-full').style.display = 'none'; document.getElementById('2404.03533v2-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> 1 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">Matches published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP07(2024)094 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.04857">arXiv:2403.04857</a> <span> [<a href="https://arxiv.org/pdf/2403.04857">pdf</a>, <a href="https://arxiv.org/format/2403.04857">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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> </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/10.1088/1475-7516/2024/07/047">10.1088/1475-7516/2024/07/047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dark Matter Line Searches with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abhir%2C+J">J. Abhir</a>, <a href="/search/astro-ph?searchtype=author&query=Abhishek%2C+A">A. Abhishek</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Crespo%2C+N">N. Alvarez-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Angel%2C+L">L. Angel</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arnesen%2C+T+T+H">T. T. H. Arnesen</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascasibar%2C+Y">Y. Ascasibar</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Ashkar%2C+H">H. Ashkar</a> , et al. (540 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="2403.04857v2-abstract-short" style="display: inline;"> Monochromatic gamma-ray signals constitute a potential smoking gun signature for annihilating or decaying dark matter particles that could relatively easily be distinguished from astrophysical or instrumental backgrounds. We provide an updated assessment of the sensitivity of the Cherenkov Telescope Array (CTA) to such signals, based on observations of the Galactic centre region as well as of sele… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04857v2-abstract-full').style.display = 'inline'; document.getElementById('2403.04857v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.04857v2-abstract-full" style="display: none;"> Monochromatic gamma-ray signals constitute a potential smoking gun signature for annihilating or decaying dark matter particles that could relatively easily be distinguished from astrophysical or instrumental backgrounds. We provide an updated assessment of the sensitivity of the Cherenkov Telescope Array (CTA) to such signals, based on observations of the Galactic centre region as well as of selected dwarf spheroidal galaxies. We find that current limits and detection prospects for dark matter masses above 300 GeV will be significantly improved, by up to an order of magnitude in the multi-TeV range. This demonstrates that CTA will set a new standard for gamma-ray astronomy also in this respect, as the world's largest and most sensitive high-energy gamma-ray observatory, in particular due to its exquisite energy resolution at TeV energies and the adopted observational strategy focussing on regions with large dark matter densities. Throughout our analysis, we use up-to-date instrument response functions, and we thoroughly model the effect of instrumental systematic uncertainties in our statistical treatment. We further present results for other potential signatures with sharp spectral features, e.g.~box-shaped spectra, that would likewise very clearly point to a particle dark matter origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.04857v2-abstract-full').style.display = 'none'; document.getElementById('2403.04857v2-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">44 pages JCAP style (excluding author list and references), 19 figures; minor changes to match published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 07 (2024) 047 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.10740">arXiv:2401.10740</a> <span> [<a href="https://arxiv.org/pdf/2401.10740">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> </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.109.102001">10.1103/PhysRevD.109.102001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Testing Hadronic-Model Predictions of Depth of Maximum of Air-Shower Profiles and Ground-Particle Signals using Hybrid Data of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Mocellin%2C+A+B">A. Bartz Mocellin</a> , et al. (346 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="2401.10740v3-abstract-short" style="display: inline;"> We test the predictions of hadronic interaction models regarding the depth of maximum of air-shower profiles, $X_{max}$, and ground-particle signals in water-Cherenkov detectors at 1000 m from the shower core, $S(1000)$, using the data from the fluorescence and surface detectors of the Pierre Auger Observatory. The test consists in fitting the measured two-dimensional ($S(1000)$, $X_{max}$) distri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.10740v3-abstract-full').style.display = 'inline'; document.getElementById('2401.10740v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.10740v3-abstract-full" style="display: none;"> We test the predictions of hadronic interaction models regarding the depth of maximum of air-shower profiles, $X_{max}$, and ground-particle signals in water-Cherenkov detectors at 1000 m from the shower core, $S(1000)$, using the data from the fluorescence and surface detectors of the Pierre Auger Observatory. The test consists in fitting the measured two-dimensional ($S(1000)$, $X_{max}$) distributions using templates for simulated air showers produced with hadronic interaction models EPOS-LHC, QGSJet II-04, Sibyll 2.3d and leaving the scales of predicted $X_{max}$ and the signals from hadronic component at ground as free fit parameters. The method relies on the assumption that the mass composition remains the same at all zenith angles, while the longitudinal shower development and attenuation of ground signal depend on the mass composition in a correlated way. The analysis was applied to 2239 events detected by both the fluorescence and surface detectors of the Pierre Auger Observatory with energies between $10^{18.5}$ to $10^{19.0}$ eV and zenith angles below $60^\circ$. We found, that within the assumptions of the method, the best description of the data is achieved if the predictions of the hadronic interaction models are shifted to deeper $X_{max}$ values and larger hadronic signals at all zenith angles. Given the magnitude of the shifts and the data sample size, the statistical significance of the improvement of data description using the modifications considered in the paper is larger than $5蟽$ even for any linear combination of experimental systematic uncertainties. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.10740v3-abstract-full').style.display = 'none'; document.getElementById('2401.10740v3-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 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">Published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 109 (2024) 102001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.14541">arXiv:2311.14541</a> <span> [<a href="https://arxiv.org/pdf/2311.14541">pdf</a>, <a href="https://arxiv.org/format/2311.14541">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</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/10.1103/PhysRevD.109.L081101">10.1103/PhysRevD.109.L081101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraints on metastable superheavy dark matter coupled to sterile neutrinos with the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Mocellin%2C+A+B">A. Bartz Mocellin</a> , et al. (346 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="2311.14541v2-abstract-short" style="display: inline;"> Dark matter particles could be superheavy, provided their lifetime is much longer than the age of the universe. Using the sensitivity of the Pierre Auger Observatory to ultra-high energy neutrinos and photons, we constrain a specific extension of the Standard Model of particle physics that meets the lifetime requirement for a superheavy particle by coupling it to a sector of ultra-light sterile ne… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.14541v2-abstract-full').style.display = 'inline'; document.getElementById('2311.14541v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.14541v2-abstract-full" style="display: none;"> Dark matter particles could be superheavy, provided their lifetime is much longer than the age of the universe. Using the sensitivity of the Pierre Auger Observatory to ultra-high energy neutrinos and photons, we constrain a specific extension of the Standard Model of particle physics that meets the lifetime requirement for a superheavy particle by coupling it to a sector of ultra-light sterile neutrinos. Our results show that, for a typical dark coupling constant of 0.1, the mixing angle $胃_m$ between active and sterile neutrinos must satisfy, roughly, $胃_m \lesssim 1.5\times 10^{-6}(M_X/10^9~\mathrm{GeV})^{-2}$ for a mass $M_X$ of the dark-matter particle between $10^8$ and $10^{11}~$GeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.14541v2-abstract-full').style.display = 'none'; document.getElementById('2311.14541v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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">Comments:</span> <span class="has-text-grey-dark mathjax">Version accepted for publication in PRD Letters, including Supplemental Material</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 109 L081101 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.19966">arXiv:2310.19966</a> <span> [<a href="https://arxiv.org/pdf/2310.19966">pdf</a>, <a href="https://arxiv.org/format/2310.19966">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> <p class="title is-5 mathjax"> Radio Measurements of the Depth of Air-Shower Maximum at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Anukriti"> Anukriti</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a> , et al. (350 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="2310.19966v1-abstract-short" style="display: inline;"> The Auger Engineering Radio Array (AERA), part of the Pierre Auger Observatory, is currently the largest array of radio antenna stations deployed for the detection of cosmic rays, spanning an area of $17$ km$^2$ with 153 radio stations. It detects the radio emission of extensive air showers produced by cosmic rays in the $30-80$ MHz band. Here, we report the AERA measurements of the depth of the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.19966v1-abstract-full').style.display = 'inline'; document.getElementById('2310.19966v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.19966v1-abstract-full" style="display: none;"> The Auger Engineering Radio Array (AERA), part of the Pierre Auger Observatory, is currently the largest array of radio antenna stations deployed for the detection of cosmic rays, spanning an area of $17$ km$^2$ with 153 radio stations. It detects the radio emission of extensive air showers produced by cosmic rays in the $30-80$ MHz band. Here, we report the AERA measurements of the depth of the shower maximum ($X_\text{max}$), a probe for mass composition, at cosmic-ray energies between $10^{17.5}$ to $10^{18.8}$ eV, which show agreement with earlier measurements with the fluorescence technique at the Pierre Auger Observatory. We show advancements in the method for radio $X_\text{max}$ reconstruction by comparison to dedicated sets of CORSIKA/CoREAS air-shower simulations, including steps of reconstruction-bias identification and correction, which is of particular importance for irregular or sparse radio arrays. Using the largest set of radio air-shower measurements to date, we show the radio $X_\text{max}$ resolution as a function of energy, reaching a resolution better than $15$ g cm$^{-2}$ at the highest energies, demonstrating that radio $X_\text{max}$ measurements are competitive with the established high-precision fluorescence technique. In addition, we developed a procedure for performing an extensive data-driven study of systematic uncertainties, including the effects of acceptance bias, reconstruction bias, and the investigation of possible residual biases. These results have been cross-checked with air showers measured independently with both the radio and fluorescence techniques, a setup unique to the Pierre Auger Observatory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.19966v1-abstract-full').style.display = 'none'; document.getElementById('2310.19966v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Submitted to Phys. Rev. D</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.19963">arXiv:2310.19963</a> <span> [<a href="https://arxiv.org/pdf/2310.19963">pdf</a>, <a href="https://arxiv.org/format/2310.19963">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> <p class="title is-5 mathjax"> Demonstrating Agreement between Radio and Fluorescence Measurements of the Depth of Maximum of Extensive Air Showers at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Anukriti"> Anukriti</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a> , et al. (350 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="2310.19963v1-abstract-short" style="display: inline;"> We show, for the first time, radio measurements of the depth of shower maximum ($X_\text{max}$) of air showers induced by cosmic rays that are compared to measurements of the established fluorescence method at the same location. Using measurements at the Pierre Auger Observatory we show full compatibility between our radio and the previously published fluorescence data set, and between a subset of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.19963v1-abstract-full').style.display = 'inline'; document.getElementById('2310.19963v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.19963v1-abstract-full" style="display: none;"> We show, for the first time, radio measurements of the depth of shower maximum ($X_\text{max}$) of air showers induced by cosmic rays that are compared to measurements of the established fluorescence method at the same location. Using measurements at the Pierre Auger Observatory we show full compatibility between our radio and the previously published fluorescence data set, and between a subset of air showers observed simultaneously with both radio and fluorescence techniques, a measurement setup unique to the Pierre Auger Observatory. Furthermore, we show radio $X_\text{max}$ resolution as a function of energy and demonstrate the ability to make competitive high-resolution $X_\text{max}$ measurements with even a sparse radio array. With this, we show that the radio technique is capable of cosmic-ray mass composition studies, both at Auger and at other experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.19963v1-abstract-full').style.display = 'none'; document.getElementById('2310.19963v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Submitted to Phys. Rev. Lett</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.08616">arXiv:2310.08616</a> <span> [<a href="https://arxiv.org/pdf/2310.08616">pdf</a>, <a href="https://arxiv.org/format/2310.08616">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="Atmospheric and Oceanic Physics">physics.ao-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</span> </div> </div> <p class="title is-5 mathjax"> Ground observations of a space laser for the assessment of its in-orbit performance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Lux%2C+O">O. Lux</a>, <a href="/search/astro-ph?searchtype=author&query=Krisch%2C+I">I. Krisch</a>, <a href="/search/astro-ph?searchtype=author&query=Reitebuch%2C+O">O. Reitebuch</a>, <a href="/search/astro-ph?searchtype=author&query=Huber%2C+D">D. Huber</a>, <a href="/search/astro-ph?searchtype=author&query=Wernham%2C+D">D. Wernham</a>, <a href="/search/astro-ph?searchtype=author&query=Parrinello%2C+T">T. Parrinello</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Anukriti"> Anukriti</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a> , et al. (358 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="2310.08616v1-abstract-short" style="display: inline;"> The wind mission Aeolus of the European Space Agency was a groundbreaking achievement for Earth observation. Between 2018 and 2023, the space-borne lidar instrument ALADIN onboard the Aeolus satellite measured atmospheric wind profiles with global coverage which contributed to improving the accuracy of numerical weather prediction. The precision of the wind observations, however, declined over the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.08616v1-abstract-full').style.display = 'inline'; document.getElementById('2310.08616v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.08616v1-abstract-full" style="display: none;"> The wind mission Aeolus of the European Space Agency was a groundbreaking achievement for Earth observation. Between 2018 and 2023, the space-borne lidar instrument ALADIN onboard the Aeolus satellite measured atmospheric wind profiles with global coverage which contributed to improving the accuracy of numerical weather prediction. The precision of the wind observations, however, declined over the course of the mission due to a progressive loss of the atmospheric backscatter signal. The analysis of the root cause was supported by the Pierre Auger Observatory in Argentina whose fluorescence detector registered the ultraviolet laser pulses emitted from the instrument in space, thereby offering an estimation of the laser energy at the exit of the instrument for several days in 2019, 2020 and 2021. The reconstruction of the laser beam not only allowed for an independent assessment of the Aeolus performance, but also helped to improve the accuracy in the determination of the laser beam's ground track on single pulse level. The results presented in this paper set a precedent for the monitoring of space lasers by ground-based telescopes and open new possibilities for the calibration of cosmic-ray observatories. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.08616v1-abstract-full').style.display = 'none'; document.getElementById('2310.08616v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">10 pages, 10 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/2310.07413">arXiv:2310.07413</a> <span> [<a href="https://arxiv.org/pdf/2310.07413">pdf</a>, <a href="https://arxiv.org/format/2310.07413">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"> Chasing Gravitational Waves with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Green%2C+J+G">Jarred Gershon Green</a>, <a href="/search/astro-ph?searchtype=author&query=Carosi%2C+A">Alessandro Carosi</a>, <a href="/search/astro-ph?searchtype=author&query=Nava%2C+L">Lara Nava</a>, <a href="/search/astro-ph?searchtype=author&query=Patricelli%2C+B">Barbara Patricelli</a>, <a href="/search/astro-ph?searchtype=author&query=Sch%C3%BCssler%2C+F">Fabian Sch眉ssler</a>, <a href="/search/astro-ph?searchtype=author&query=Seglar-Arroyo%2C+M">Monica Seglar-Arroyo</a>, <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+C">Cta Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+K">Kazuki Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">Shotaro Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">Atreya Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">Remi Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">Arnau Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">Ivan Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">Jorge Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Crespo%2C+N">Nuria Alvarez-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">Rafael Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J">Jean-Philippe Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">Elena Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosino%2C+F">Filippo Ambrosino</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">Ekrem Oguzhan Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">Lucio Angelo Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">Cornelia Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">Luisa Arrabito</a> , et al. (545 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="2310.07413v3-abstract-short" style="display: inline;"> The detection of gravitational waves from a binary neutron star merger by Advanced LIGO and Advanced Virgo (GW170817), along with the discovery of the electromagnetic counterparts of this gravitational wave event, ushered in a new era of multimessenger astronomy, providing the first direct evidence that BNS mergers are progenitors of short gamma-ray bursts (GRBs). Such events may also produce very… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.07413v3-abstract-full').style.display = 'inline'; document.getElementById('2310.07413v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.07413v3-abstract-full" style="display: none;"> The detection of gravitational waves from a binary neutron star merger by Advanced LIGO and Advanced Virgo (GW170817), along with the discovery of the electromagnetic counterparts of this gravitational wave event, ushered in a new era of multimessenger astronomy, providing the first direct evidence that BNS mergers are progenitors of short gamma-ray bursts (GRBs). Such events may also produce very-high-energy (VHE, > 100GeV) photons which have yet to be detected in coincidence with a gravitational wave signal. The Cherenkov Telescope Array (CTA) is a next-generation VHE observatory which aims to be indispensable in this search, with an unparalleled sensitivity and ability to slew anywhere on the sky within a few tens of seconds. New observing modes and follow-up strategies are being developed for CTA to rapidly cover localization areas of gravitational wave events that are typically larger than the CTA field of view. This work will evaluate and provide estimations on the expected number of of gravitational wave events that will be observable with CTA, considering both on- and off-axis emission. In addition, we will present and discuss the prospects of potential follow-up strategies with CTA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.07413v3-abstract-full').style.display = 'none'; document.getElementById('2310.07413v3-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> 5 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Presented at the 38th International Cosmic Ray Conference (ICRC 2023), 2023 (arXiv:2309.08219)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> CTA-ICRC/2023/30 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.01954">arXiv:2310.01954</a> <span> [<a href="https://arxiv.org/pdf/2310.01954">pdf</a>, <a href="https://arxiv.org/format/2310.01954">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/10.1051/0004-6361/202346927">10.1051/0004-6361/202346927 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance of the joint LST-1 and MAGIC observations evaluated with Crab Nebula data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acciari%2C+V+A">V. A. Acciari</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+N+A">N. Alvarez Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Aniello%2C+T">T. Aniello</a>, <a href="/search/astro-ph?searchtype=author&query=Ansoldi%2C+S">S. Ansoldi</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arbet-Engels%2C+A">A. Arbet-Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+P">P. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Baack%2C+D">D. Baack</a>, <a href="/search/astro-ph?searchtype=author&query=Babi%C4%87%2C+A">A. Babi膰</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Bamba%2C+A">A. Bamba</a>, <a href="/search/astro-ph?searchtype=author&query=Larriva%2C+A+B">A. Baquero Larriva</a>, <a href="/search/astro-ph?searchtype=author&query=Baroncelli%2C+L">L. Baroncelli</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Batkovi%C4%87%2C+I">I. Batkovi膰</a> , et al. (344 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="2310.01954v1-abstract-short" style="display: inline;"> Aims. LST-1, the prototype of the Large-Sized Telescope for the upcoming Cherenkov Telescope Array Observatory, is concluding its commissioning in Observatorio del Roque de los Muchachos on the island of La Palma. The proximity of LST-1 (Large-Sized Telescope 1) to the two MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes permits observations of the same gamma-ray events with both syste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.01954v1-abstract-full').style.display = 'inline'; document.getElementById('2310.01954v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.01954v1-abstract-full" style="display: none;"> Aims. LST-1, the prototype of the Large-Sized Telescope for the upcoming Cherenkov Telescope Array Observatory, is concluding its commissioning in Observatorio del Roque de los Muchachos on the island of La Palma. The proximity of LST-1 (Large-Sized Telescope 1) to the two MAGIC (Major Atmospheric Gamma Imaging Cherenkov) telescopes permits observations of the same gamma-ray events with both systems. Methods. We describe the joint LST-1+MAGIC analysis pipeline and use simultaneous Crab Nebula observations and Monte Carlo simulations to assess the performance of the three-telescope system. The addition of the LST-1 telescope allows the recovery of events in which one of the MAGIC images is too dim to survive analysis quality cuts. Results. Thanks to the resulting increase in the collection area and stronger background rejection, we find a significant improvement in sensitivity, allowing the detection of 30% weaker fluxes in the energy range between 200 GeV and 3 TeV. The spectrum of the Crab Nebula, reconstructed in the energy range ~60 GeV to ~10 TeV, is in agreement with previous measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.01954v1-abstract-full').style.display = 'none'; document.getElementById('2310.01954v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 680, A66 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.16294">arXiv:2309.16294</a> <span> [<a href="https://arxiv.org/pdf/2309.16294">pdf</a>, <a href="https://arxiv.org/format/2309.16294">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> <p class="title is-5 mathjax"> The Pierre Auger Observatory Open Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Dourado%2C+L+A">L. Andrade Dourado</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Apollonio%2C+L">L. Apollonio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a> , et al. (336 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="2309.16294v3-abstract-short" style="display: inline;"> The Pierre Auger Collaboration has embraced the concept of open access to their research data since its foundation, with the aim of giving access to the widest possible community. A gradual process of release began as early as 2007 when 1% of the cosmic-ray data was made public, along with 100% of the space-weather information. In February 2021, a portal was released containing 10% of cosmic-ray d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16294v3-abstract-full').style.display = 'inline'; document.getElementById('2309.16294v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.16294v3-abstract-full" style="display: none;"> The Pierre Auger Collaboration has embraced the concept of open access to their research data since its foundation, with the aim of giving access to the widest possible community. A gradual process of release began as early as 2007 when 1% of the cosmic-ray data was made public, along with 100% of the space-weather information. In February 2021, a portal was released containing 10% of cosmic-ray data collected from 2004 to 2018, during Phase I of the Observatory. The Portal included detailed documentation about the detection and reconstruction procedures, analysis codes that can be easily used and modified and, additionally, visualization tools. Since then the Portal has been updated and extended. In 2023, a catalog of the 100 highest-energy cosmic-ray events examined in depth has been included. A specific section dedicated to educational use has been developed with the expectation that these data will be explored by a wide and diverse community including professional and citizen-scientists, and used for educational and outreach initiatives. This paper describes the context, the spirit and the technical implementation of the release of data by the largest cosmic-ray detector ever built, and anticipates its future developments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.16294v3-abstract-full').style.display = 'none'; document.getElementById('2309.16294v3-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">27 pages, 8 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/2309.06235">arXiv:2309.06235</a> <span> [<a href="https://arxiv.org/pdf/2309.06235">pdf</a>, <a href="https://arxiv.org/format/2309.06235">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> <p class="title is-5 mathjax"> AugerPrime Surface Detector Electronics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Anukriti"> Anukriti</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a> , et al. (346 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="2309.06235v3-abstract-short" style="display: inline;"> Operating since 2004, the Pierre Auger Observatory has led to major advances in our understanding of the ultra-high-energy cosmic rays. The latest findings have revealed new insights that led to the upgrade of the Observatory, with the primary goal of obtaining information on the primary mass of the most energetic cosmic rays on a shower-by-shower basis. In the framework of the upgrade, called Aug… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.06235v3-abstract-full').style.display = 'inline'; document.getElementById('2309.06235v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.06235v3-abstract-full" style="display: none;"> Operating since 2004, the Pierre Auger Observatory has led to major advances in our understanding of the ultra-high-energy cosmic rays. The latest findings have revealed new insights that led to the upgrade of the Observatory, with the primary goal of obtaining information on the primary mass of the most energetic cosmic rays on a shower-by-shower basis. In the framework of the upgrade, called AugerPrime, the 1660 water-Cherenkov detectors of the surface array are equipped with plastic scintillators and radio antennas, allowing us to enhance the composition sensitivity. To accommodate new detectors and to increase experimental capabilities, the electronics is also upgraded. This includes better timing with up-to-date GPS receivers, higher sampling frequency, increased dynamic range, and more powerful local processing of the data. In this paper, the design characteristics of the new electronics and the enhanced dynamic range will be described. The manufacturing and test processes will be outlined and the test results will be discussed. The calibration of the SD detector and various performance parameters obtained from the analysis of the first commissioning data will also be presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.06235v3-abstract-full').style.display = 'none'; document.getElementById('2309.06235v3-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> 8 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.03712">arXiv:2309.03712</a> <span> [<a href="https://arxiv.org/pdf/2309.03712">pdf</a>, <a href="https://arxiv.org/format/2309.03712">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1088/1475-7516/2024/10/004">10.1088/1475-7516/2024/10/004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Prospects for $纬$-ray observations of the Perseus galaxy cluster with the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Crespo%2C+N">N. Alvarez-Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amans%2C+J+-">J. -P. Amans</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Araya%2C+M">M. Araya</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Arrabito%2C+L">L. Arrabito</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascas%C3%ADbar%2C+Y">Y. Ascas铆bar</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a> , et al. (542 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="2309.03712v1-abstract-short" style="display: inline;"> Galaxy clusters are expected to be dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at gamma-ray energies and are predicted to be sources of large-scale gamma-ray emission due to hadronic interactions in the intracluster med… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03712v1-abstract-full').style.display = 'inline'; document.getElementById('2309.03712v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03712v1-abstract-full" style="display: none;"> Galaxy clusters are expected to be dark matter (DM) reservoirs and storage rooms for the cosmic-ray protons (CRp) that accumulate along the cluster's formation history. Accordingly, they are excellent targets to search for signals of DM annihilation and decay at gamma-ray energies and are predicted to be sources of large-scale gamma-ray emission due to hadronic interactions in the intracluster medium. We estimate the sensitivity of the Cherenkov Telescope Array (CTA) to detect diffuse gamma-ray emission from the Perseus galaxy cluster. We perform a detailed spatial and spectral modelling of the expected signal for the DM and the CRp components. For each, we compute the expected CTA sensitivity. The observing strategy of Perseus is also discussed. In the absence of a diffuse signal (non-detection), CTA should constrain the CRp to thermal energy ratio within the radius $R_{500}$ down to about $X_{500}<3\times 10^{-3}$, for a spatial CRp distribution that follows the thermal gas and a CRp spectral index $伪_{\rm CRp}=2.3$. Under the optimistic assumption of a pure hadronic origin of the Perseus radio mini-halo and depending on the assumed magnetic field profile, CTA should measure $伪_{\rm CRp}$ down to about $螖伪_{\rm CRp}\simeq 0.1$ and the CRp spatial distribution with 10% precision. Regarding DM, CTA should improve the current ground-based gamma-ray DM limits from clusters observations on the velocity-averaged annihilation cross-section by a factor of up to $\sim 5$, depending on the modelling of DM halo substructure. In the case of decay of DM particles, CTA will explore a new region of the parameter space, reaching models with $蟿_蠂>10^{27}$s for DM masses above 1 TeV. These constraints will provide unprecedented sensitivity to the physics of both CRp acceleration and transport at cluster scale and to TeV DM particle models, especially in the decay scenario. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03712v1-abstract-full').style.display = 'none'; document.getElementById('2309.03712v1-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">93 pages (including author list, appendix and references), 143 figures. Submitted to JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP10(2024)004 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.10839">arXiv:2307.10839</a> <span> [<a href="https://arxiv.org/pdf/2307.10839">pdf</a>, <a href="https://arxiv.org/format/2307.10839">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="General Relativity and Quantum Cosmology">gr-qc</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/acc862">10.3847/1538-4357/acc862 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for UHE Photons from Gravitational Wave Sources with the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a> , et al. (346 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="2307.10839v1-abstract-short" style="display: inline;"> A search for time-directional coincidences of ultra-high-energy (UHE) photons above 10 EeV with gravitational wave (GW) events from the LIGO/Virgo runs O1 to O3 is conducted with the Pierre Auger Observatory. Due to the distinctive properties of photon interactions and to the background expected from hadronic showers, a subset of the most interesting GW events is selected based on their localizati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10839v1-abstract-full').style.display = 'inline'; document.getElementById('2307.10839v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.10839v1-abstract-full" style="display: none;"> A search for time-directional coincidences of ultra-high-energy (UHE) photons above 10 EeV with gravitational wave (GW) events from the LIGO/Virgo runs O1 to O3 is conducted with the Pierre Auger Observatory. Due to the distinctive properties of photon interactions and to the background expected from hadronic showers, a subset of the most interesting GW events is selected based on their localization quality and distance. Time periods of 1000 s around and 1 day after the GW events are analyzed. No coincidences are observed. Upper limits on the UHE photon fluence from a GW event are derived that are typically at $\sim$7 MeV cm$^{-2}$ (time period 1000~s) and $\sim$35 MeV cm$^{-2}$ (time period 1 day). Due to the proximity of the binary neutron star merger GW170817, the energy of the source transferred into UHE photons above 40 EeV is constrained to be less than 20% of its total gravitational wave energy. These are the first limits on UHE photons from GW sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.10839v1-abstract-full').style.display = 'none'; document.getElementById('2307.10839v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">15 pages</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 952 (2023) 91 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.12960">arXiv:2306.12960</a> <span> [<a href="https://arxiv.org/pdf/2306.12960">pdf</a>, <a href="https://arxiv.org/ps/2306.12960">ps</a>, <a href="https://arxiv.org/format/2306.12960">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> <p class="title is-5 mathjax"> Observations of the Crab Nebula and Pulsar with the Large-Sized Telescope Prototype of the Cherenkov Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Project%2C+C">CTA-LST Project</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+H">H. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+K">K. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+N+A">N. Alvarez Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arbet-Engels%2C+A">A. Arbet-Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+P">P. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Bamba%2C+A">A. Bamba</a>, <a href="/search/astro-ph?searchtype=author&query=Larriva%2C+A+B">A. Baquero Larriva</a>, <a href="/search/astro-ph?searchtype=author&query=Baroncelli%2C+L">L. Baroncelli</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Batkovic%2C+I">I. Batkovic</a>, <a href="/search/astro-ph?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a> , et al. (467 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="2306.12960v3-abstract-short" style="display: inline;"> CTA (Cherenkov Telescope Array) is the next generation ground-based observatory for gamma-ray astronomy at very-high energies. The Large-Sized Telescope prototype (LST-1) is located at the Northern site of CTA, on the Canary Island of La Palma. LSTs are designed to provide optimal performance in the lowest part of the energy range covered by CTA, down to $\simeq 20$ GeV. LST-1 started performing a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.12960v3-abstract-full').style.display = 'inline'; document.getElementById('2306.12960v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.12960v3-abstract-full" style="display: none;"> CTA (Cherenkov Telescope Array) is the next generation ground-based observatory for gamma-ray astronomy at very-high energies. The Large-Sized Telescope prototype (LST-1) is located at the Northern site of CTA, on the Canary Island of La Palma. LSTs are designed to provide optimal performance in the lowest part of the energy range covered by CTA, down to $\simeq 20$ GeV. LST-1 started performing astronomical observations in November 2019, during its commissioning phase, and it has been taking data since then. We present the first LST-1 observations of the Crab Nebula, the standard candle of very-high energy gamma-ray astronomy, and use them, together with simulations, to assess the basic performance parameters of the telescope. The data sample consists of around 36 hours of observations at low zenith angles collected between November 2020 and March 2022. LST-1 has reached the expected performance during its commissioning period - only a minor adjustment of the preexisting simulations was needed to match the telescope behavior. The energy threshold at trigger level is estimated to be around 20 GeV, rising to $\simeq 30$ GeV after data analysis. Performance parameters depend strongly on energy, and on the strength of the gamma-ray selection cuts in the analysis: angular resolution ranges from 0.12 to 0.40 degrees, and energy resolution from 15 to 50%. Flux sensitivity is around 1.1% of the Crab Nebula flux above 250 GeV for a 50-h observation (12% for 30 minutes). The spectral energy distribution (in the 0.03 - 30 TeV range) and the light curve obtained for the Crab Nebula agree with previous measurements, considering statistical and systematic uncertainties. A clear periodic signal is also detected from the pulsar at the center of the Nebula. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.12960v3-abstract-full').style.display = 'none'; document.getElementById('2306.12960v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Accepted in ApJ. v3: updated author list and acknowledgements, fixed typos and other minor issues</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.16693">arXiv:2305.16693</a> <span> [<a href="https://arxiv.org/pdf/2305.16693">pdf</a>, <a href="https://arxiv.org/format/2305.16693">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/10.1088/1475-7516/2024/01/022">10.1088/1475-7516/2024/01/022 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining models for the origin of ultra-high-energy cosmic rays with a novel combined analysis of arrival directions, spectrum, and composition data measured at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a> , et al. (349 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="2305.16693v2-abstract-short" style="display: inline;"> The combined fit of the measured energy spectrum and shower maximum depth distributions of ultra-high-energy cosmic rays is known to constrain the parameters of astrophysical models with homogeneous source distributions. Studies of the distribution of the cosmic-ray arrival directions show a better agreement with models in which a fraction of the flux is non-isotropic and associated with the nearb… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.16693v2-abstract-full').style.display = 'inline'; document.getElementById('2305.16693v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.16693v2-abstract-full" style="display: none;"> The combined fit of the measured energy spectrum and shower maximum depth distributions of ultra-high-energy cosmic rays is known to constrain the parameters of astrophysical models with homogeneous source distributions. Studies of the distribution of the cosmic-ray arrival directions show a better agreement with models in which a fraction of the flux is non-isotropic and associated with the nearby radio galaxy Centaurus A or with catalogs such as that of starburst galaxies. Here, we present a novel combination of both analyses by a simultaneous fit of arrival directions, energy spectrum, and composition data measured at the Pierre Auger Observatory. We find that a model containing a flux contribution from the starburst galaxy catalog of around 20% at 40 EeV with a magnetic field blurring of around $20^\circ$ for a rigidity of 10 EV provides a fair simultaneous description of all three observables. The starburst galaxy model is favored with a significance of $4.5蟽$ (considering experimental systematic effects) compared to a reference model with only homogeneously distributed background sources. By investigating a scenario with Centaurus A as a single source in combination with the homogeneous background, we confirm that this region of the sky provides the dominant contribution to the observed anisotropy signal. Models containing a catalog of jetted active galactic nuclei whose flux scales with the $纬$-ray emission are, however, disfavored as they cannot adequately describe the measured arrival directions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.16693v2-abstract-full').style.display = 'none'; document.getElementById('2305.16693v2-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">Journal ref:</span> JCAP01(2024)022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.15007">arXiv:2303.15007</a> <span> [<a href="https://arxiv.org/pdf/2303.15007">pdf</a>, <a href="https://arxiv.org/format/2303.15007">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.2023.102850">10.1016/j.astropartphys.2023.102850 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Sensitivity of the Cherenkov Telescope Array to spectral signatures of hadronic PeVatrons with application to Galactic Supernova Remnants </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Consortium%2C+T+C+T+A">The Cherenkov Telescope Array Consortium</a>, <a href="/search/astro-ph?searchtype=author&query=Acero%2C+F">F. Acero</a>, <a href="/search/astro-ph?searchtype=author&query=Acharyya%2C+A">A. Acharyya</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguirre-Santaella%2C+A">A. Aguirre-Santaella</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+J">J. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+N+%C3%81">N. 脕lvarez Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Amati%2C+L">L. Amati</a>, <a href="/search/astro-ph?searchtype=author&query=Amato%2C+E">E. Amato</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ang%C3%BCner%2C+E+O">E. O. Ang眉ner</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arcaro%2C+C">C. Arcaro</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+T">T. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Ascasibar%2C+Y">Y. Ascasibar</a>, <a href="/search/astro-ph?searchtype=author&query=Aschersleben%2C+J">J. Aschersleben</a>, <a href="/search/astro-ph?searchtype=author&query=Backes%2C+M">M. Backes</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Balazs%2C+C">C. Balazs</a>, <a href="/search/astro-ph?searchtype=author&query=Balbo%2C+M">M. Balbo</a> , et al. (334 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="2303.15007v1-abstract-short" style="display: inline;"> The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3~PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The pote… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15007v1-abstract-full').style.display = 'inline'; document.getElementById('2303.15007v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15007v1-abstract-full" style="display: none;"> The local Cosmic Ray (CR) energy spectrum exhibits a spectral softening at energies around 3~PeV. Sources which are capable of accelerating hadrons to such energies are called hadronic PeVatrons. However, hadronic PeVatrons have not yet been firmly identified within the Galaxy. Several source classes, including Galactic Supernova Remnants (SNRs), have been proposed as PeVatron candidates. The potential to search for hadronic PeVatrons with the Cherenkov Telescope Array (CTA) is assessed. The focus is on the usage of very high energy $纬$-ray spectral signatures for the identification of PeVatrons. Assuming that SNRs can accelerate CRs up to knee energies, the number of Galactic SNRs which can be identified as PeVatrons with CTA is estimated within a model for the evolution of SNRs. Additionally, the potential of a follow-up observation strategy under moonlight conditions for PeVatron searches is investigated. Statistical methods for the identification of PeVatrons are introduced, and realistic Monte--Carlo simulations of the response of the CTA observatory to the emission spectra from hadronic PeVatrons are performed. Based on simulations of a simplified model for the evolution for SNRs, the detection of a $纬$-ray signal from in average 9 Galactic PeVatron SNRs is expected to result from the scan of the Galactic plane with CTA after 10 hours of exposure. CTA is also shown to have excellent potential to confirm these sources as PeVatrons in deep observations with $\mathcal{O}(100)$ hours of exposure per source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15007v1-abstract-full').style.display = 'none'; document.getElementById('2303.15007v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">34 pages, 16 figures, 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/2211.16020">arXiv:2211.16020</a> <span> [<a href="https://arxiv.org/pdf/2211.16020">pdf</a>, <a href="https://arxiv.org/format/2211.16020">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> <p class="title is-5 mathjax"> A Catalog of the Highest-Energy Cosmic Rays Recorded During Phase I of Operation of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a> , et al. (354 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="2211.16020v1-abstract-short" style="display: inline;"> A catalog containing details of the highest-energy cosmic rays recorded through the detection of extensive air-showers at the Pierre Auger Observatory is presented with the aim of opening the data to detailed examination. Descriptions of the 100 showers created by the highest-energy particles recorded between 1 January 2004 and 31 December 2020 are given for cosmic rays that have energies in the r… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.16020v1-abstract-full').style.display = 'inline'; document.getElementById('2211.16020v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.16020v1-abstract-full" style="display: none;"> A catalog containing details of the highest-energy cosmic rays recorded through the detection of extensive air-showers at the Pierre Auger Observatory is presented with the aim of opening the data to detailed examination. Descriptions of the 100 showers created by the highest-energy particles recorded between 1 January 2004 and 31 December 2020 are given for cosmic rays that have energies in the range 78 EeV to 166 EeV. Details are also given of a further nine very-energetic events that have been used in the calibration procedure adopted to determine the energy of each primary. A sky plot of the arrival directions of the most energetic particles is shown. No interpretations of the data are offered. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.16020v1-abstract-full').style.display = 'none'; document.getElementById('2211.16020v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">Article accepted for publication in ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2211.02857">arXiv:2211.02857</a> <span> [<a href="https://arxiv.org/pdf/2211.02857">pdf</a>, <a href="https://arxiv.org/format/2211.02857">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/10.1088/1475-7516/2023/05/024">10.1088/1475-7516/2023/05/024 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining the sources of ultra-high-energy cosmic rays across and above the ankle with the spectrum and composition data measured at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Halim%2C+A+A">A. Abdul Halim</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a> , et al. (343 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="2211.02857v2-abstract-short" style="display: inline;"> In this work we present the interpretation of the energy spectrum and mass composition data as measured by the Pierre Auger Collaboration above $6 \times 10^{17}$ eV. We use an astrophysical model with two extragalactic source populations to model the hardening of the cosmic-ray flux at around $5\times 10^{18}$ eV (the so-called "ankle" feature) as a transition between these two components. We fin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.02857v2-abstract-full').style.display = 'inline'; document.getElementById('2211.02857v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2211.02857v2-abstract-full" style="display: none;"> In this work we present the interpretation of the energy spectrum and mass composition data as measured by the Pierre Auger Collaboration above $6 \times 10^{17}$ eV. We use an astrophysical model with two extragalactic source populations to model the hardening of the cosmic-ray flux at around $5\times 10^{18}$ eV (the so-called "ankle" feature) as a transition between these two components. We find our data to be well reproduced if sources above the ankle emit a mixed composition with a hard spectrum and a low rigidity cutoff. The component below the ankle is required to have a very soft spectrum and a mix of protons and intermediate-mass nuclei. The origin of this intermediate-mass component is not well constrained and it could originate from either Galactic or extragalactic sources. To the aim of evaluating our capability to constrain astrophysical models, we discuss the impact on the fit results of the main experimental systematic uncertainties and of the assumptions about quantities affecting the air shower development as well as the propagation and redshift distribution of injected ultra-high-energy cosmic rays (UHECRs). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2211.02857v2-abstract-full').style.display = 'none'; document.getElementById('2211.02857v2-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">Submitted to JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP05(2023)024 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.12959">arXiv:2210.12959</a> <span> [<a href="https://arxiv.org/pdf/2210.12959">pdf</a>, <a href="https://arxiv.org/format/2210.12959">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/10.3390/universe8110579">10.3390/universe8110579 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searches for Ultra-High-Energy Photons at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+J+A">J. A. Bellido</a> , et al. (340 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="2210.12959v1-abstract-short" style="display: inline;"> The Pierre Auger Observatory, being the largest air-shower experiment in the world, offers an unprecedented exposure to neutral particles at the highest energies. Since the start of data taking more than 18 years ago, various searches for ultra-high-energy (UHE, $E\gtrsim10^{17}\,\text{eV}$) photons have been performed: either for a diffuse flux of UHE photons, for point sources of UHE photons or… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12959v1-abstract-full').style.display = 'inline'; document.getElementById('2210.12959v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.12959v1-abstract-full" style="display: none;"> The Pierre Auger Observatory, being the largest air-shower experiment in the world, offers an unprecedented exposure to neutral particles at the highest energies. Since the start of data taking more than 18 years ago, various searches for ultra-high-energy (UHE, $E\gtrsim10^{17}\,\text{eV}$) photons have been performed: either for a diffuse flux of UHE photons, for point sources of UHE photons or for UHE photons associated with transient events like gravitational wave events. In the present paper, we summarize these searches and review the current results obtained using the wealth of data collected by the Pierre Auger Observatory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.12959v1-abstract-full').style.display = 'none'; document.getElementById('2210.12959v1-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 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">Review article accepted for publication in Universe (special issue on ultra-high energy photons)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-22-810-AD-PPD-SCD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Universe 8 (2022) 579 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.00775">arXiv:2210.00775</a> <span> [<a href="https://arxiv.org/pdf/2210.00775">pdf</a>, <a href="https://arxiv.org/format/2210.00775">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/10.1051/0004-6361/202245086">10.1051/0004-6361/202245086 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-wavelength study of the galactic PeVatron candidate LHAASO J2108+5157 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Aguasca-Cabot%2C+A">A. Aguasca-Cabot</a>, <a href="/search/astro-ph?searchtype=author&query=Agudo%2C+I">I. Agudo</a>, <a href="/search/astro-ph?searchtype=author&query=Crespo%2C+N+A">N. Alvarez Crespo</a>, <a href="/search/astro-ph?searchtype=author&query=Antonelli%2C+L+A">L. A. Antonelli</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arbet-Engels%2C+A">A. Arbet-Engels</a>, <a href="/search/astro-ph?searchtype=author&query=Artero%2C+M">M. Artero</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+P">P. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Baktash%2C+A">A. Baktash</a>, <a href="/search/astro-ph?searchtype=author&query=Bamba%2C+A">A. Bamba</a>, <a href="/search/astro-ph?searchtype=author&query=Larriva%2C+A+B">A. Baquero Larriva</a>, <a href="/search/astro-ph?searchtype=author&query=Baroncelli%2C+L">L. Baroncelli</a>, <a href="/search/astro-ph?searchtype=author&query=de+Almeida%2C+U+B">U. Barres de Almeida</a>, <a href="/search/astro-ph?searchtype=author&query=Barrio%2C+J+A">J. A. Barrio</a>, <a href="/search/astro-ph?searchtype=author&query=Batkovic%2C+I">I. Batkovic</a>, <a href="/search/astro-ph?searchtype=author&query=Baxter%2C+J">J. Baxter</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J+B">J. Becerra Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+E">E. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardos%2C+M+I">M. I. Bernardos</a>, <a href="/search/astro-ph?searchtype=author&query=Medrano%2C+J+B">J. Bernete Medrano</a>, <a href="/search/astro-ph?searchtype=author&query=Berti%2C+A">A. Berti</a>, <a href="/search/astro-ph?searchtype=author&query=Bhattacharjee%2C+P">P. Bhattacharjee</a>, <a href="/search/astro-ph?searchtype=author&query=Biederbeck%2C+N">N. Biederbeck</a> , et al. (245 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="2210.00775v4-abstract-short" style="display: inline;"> LHAASO J2108+5157 is one of the few known unidentified Ultra-High-Energy (UHE) gamma-ray sources with no Very-High-Energy (VHE) counterpart, recently discovered by the LHAASO collaboration. We observed LHAASO J2108+5157 in the X-ray band with XMM-Newton in 2021 for a total of 3.8 hours and at TeV energies with the Large-Sized Telescope prototype (LST-1), yielding 49 hours of good quality data. In… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.00775v4-abstract-full').style.display = 'inline'; document.getElementById('2210.00775v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.00775v4-abstract-full" style="display: none;"> LHAASO J2108+5157 is one of the few known unidentified Ultra-High-Energy (UHE) gamma-ray sources with no Very-High-Energy (VHE) counterpart, recently discovered by the LHAASO collaboration. We observed LHAASO J2108+5157 in the X-ray band with XMM-Newton in 2021 for a total of 3.8 hours and at TeV energies with the Large-Sized Telescope prototype (LST-1), yielding 49 hours of good quality data. In addition, we analyzed 12 years of Fermi-LAT data, to better constrain emission of its High-Energy (HE) counterpart 4FGL J2108.0+5155. We found an excess (3.7 sigma) in the LST-1 data at energies E > 3 TeV. Further analysis in the whole LST-1 energy range assuming a point-like source, resulted in a hint (2.2 sigma) of hard emission which can be described with a single power law with photon index Gamma = 1.6 +- 0.2 between 0.3 - 100 TeV. We did not find any significant extended emission which could be related to a Supernova Remnant (SNR) or Pulsar Wind Nebula (PWN) in the XMM-Newton data, which puts strong constraints on possible synchrotron emission of relativistic electrons. The LST-1 and LHAASO observations can be explained as inverse Compton-dominated leptonic emission of relativistic electrons with a cutoff energy of $100^{+70}_{-30}$ TeV. The low magnetic field in the source imposed by the X-ray upper limits on synchrotron emission is compatible with a hypothesis of a PWN or a TeV halo. The lack of a pulsar in the neighborhood of the UHE source is a challenge to the PWN/TeV-halo scenario. The UHE gamma rays can also be explained as $蟺^0$ decay-dominated hadronic emission due to interaction of relativistic protons with one of the two known molecular clouds in the direction of the source. The hard spectrum in the LST-1 band is compatible with protons escaping a shock around a middle-aged SNR because of their high low-energy cut-off. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.00775v4-abstract-full').style.display = 'none'; document.getElementById('2210.00775v4-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">26 pages, 9 figures, 5 tables; Astronomy and Astrophysics (accepted on 6 March 2023)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 673, A75 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.05926">arXiv:2209.05926</a> <span> [<a href="https://arxiv.org/pdf/2209.05926">pdf</a>, <a href="https://arxiv.org/format/2209.05926">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"> Search for photons above 10$^{19}$ eV with the surface detector of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+J+A">J. A. Bellido</a> , et al. (343 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="2209.05926v3-abstract-short" style="display: inline;"> We use the surface detector of the Pierre Auger Observatory to search for air showers initiated by photons with an energy above $10^{19}$ eV. Photons in the zenith angle range from 30$^\circ$ to 60$^\circ$ can be identified in the overwhelming background of showers initiated by charged cosmic rays through the broader time structure of the signals induced in the water-Cherenkov detectors of the arr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05926v3-abstract-full').style.display = 'inline'; document.getElementById('2209.05926v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.05926v3-abstract-full" style="display: none;"> We use the surface detector of the Pierre Auger Observatory to search for air showers initiated by photons with an energy above $10^{19}$ eV. Photons in the zenith angle range from 30$^\circ$ to 60$^\circ$ can be identified in the overwhelming background of showers initiated by charged cosmic rays through the broader time structure of the signals induced in the water-Cherenkov detectors of the array and the steeper lateral distribution of shower particles reaching ground. Applying the search method to data collected between January 2004 and June 2020, upper limits at 95\% CL are set to an $E^{-2}$ diffuse flux of ultra-high energy photons above $10^{19}$ eV, $2{\times}10^{19}$ eV and $4{\times}10^{19}$ eV amounting to $2.11{\times}10^{-3}$, $3.12{\times}10^{-4}$ and $1.72{\times}10^{-4}$ km$^{-2}$ sr$^{-1}$ yr$^{-1}$, respectively. While the sensitivity of the present search around $2 \times 10^{19}$ eV approaches expectations of cosmogenic photon fluxes in the case of a pure-proton composition, it is one order of magnitude above those from more realistic mixed-composition models. The inferred limits have also implications for the search of super-heavy dark matter that are discussed and illustrated. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.05926v3-abstract-full').style.display = 'none'; document.getElementById('2209.05926v3-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">21 pages, 8 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/2208.02353">arXiv:2208.02353</a> <span> [<a href="https://arxiv.org/pdf/2208.02353">pdf</a>, <a href="https://arxiv.org/format/2208.02353">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Cosmological implications of photon-flux upper limits at ultra-high energies in scenarios of Planckian-interacting massive particles for dark matter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a> , et al. (352 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="2208.02353v2-abstract-short" style="display: inline;"> Using the data of the Pierre Auger Observatory, we report on a search for signatures that would be suggestive of super-heavy particles decaying in the Galactic halo. From the lack of signal, we present upper limits for different energy thresholds above ${\gtrsim}10^8$\,GeV on the secondary by-product fluxes expected from the decay of the particles. Assuming that the energy density of these super-h… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.02353v2-abstract-full').style.display = 'inline'; document.getElementById('2208.02353v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.02353v2-abstract-full" style="display: none;"> Using the data of the Pierre Auger Observatory, we report on a search for signatures that would be suggestive of super-heavy particles decaying in the Galactic halo. From the lack of signal, we present upper limits for different energy thresholds above ${\gtrsim}10^8$\,GeV on the secondary by-product fluxes expected from the decay of the particles. Assuming that the energy density of these super-heavy particles matches that of dark matter observed today, we translate the upper bounds on the particle fluxes into tight constraints on the couplings governing the decay process as a function of the particle mass. Instantons, which are non-perturbative solutions to Yang-Mills equations, can give rise to decay channels otherwise forbidden and transform stable particles into meta-stable ones. Assuming such instanton-induced decay processes, we derive a bound on the reduced coupling constant of gauge interactions in the dark sector: $伪_X \lesssim 0.09$, for $10^{9} \lesssim M_X/\text{GeV} < 10^{19}$. Conversely, we obtain that, for instance, a reduced coupling constant $伪_X = 0.09$ excludes masses $M_X \gtrsim 3\times 10^{13}~$GeV. In the context of dark matter production from gravitational interactions alone during the reheating epoch, we derive constraints on the parameter space that involves, in addition to $M_X$ and $伪_X$, the Hubble rate at the end of inflation, the reheating efficiency, and the non-minimal coupling of the Higgs with curvature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.02353v2-abstract-full').style.display = 'none'; document.getElementById('2208.02353v2-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">15 pages, 8 figures, Accompanying paper of arXiv:2203.08854, accepted for publication in Phys. Rev. D</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.D 107 (2023) 4, 042002 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.13492">arXiv:2206.13492</a> <span> [<a href="https://arxiv.org/pdf/2206.13492">pdf</a>, <a href="https://arxiv.org/format/2206.13492">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/ac7d4e">10.3847/1538-4357/ac7d4e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Arrival Directions of Cosmic Rays above 32 EeV from Phase One of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a> , et al. (350 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="2206.13492v2-abstract-short" style="display: inline;"> A promising energy range to look for angular correlation between cosmic rays of extragalactic origin and their sources is at the highest energies, above few tens of EeV ($1\:{\rm EeV}\equiv 10^{18}\:$eV). Despite the flux of these particles being extremely low, the area of ${\sim}\:3{,}000 \: \text{km}^2$ covered at the Pierre Auger Observatory, and the 17-year data-taking period of the Phase 1 of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.13492v2-abstract-full').style.display = 'inline'; document.getElementById('2206.13492v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.13492v2-abstract-full" style="display: none;"> A promising energy range to look for angular correlation between cosmic rays of extragalactic origin and their sources is at the highest energies, above few tens of EeV ($1\:{\rm EeV}\equiv 10^{18}\:$eV). Despite the flux of these particles being extremely low, the area of ${\sim}\:3{,}000 \: \text{km}^2$ covered at the Pierre Auger Observatory, and the 17-year data-taking period of the Phase 1 of its operations, have enabled us to measure the arrival directions of more than 2,600 ultra-high energy cosmic rays above $32\:\text{EeV}$. We publish this data set, the largest available at such energies from an integrated exposure of $122{,}000 \: \text{km}^2\:\text{sr}\:\text{yr}$, and search it for anisotropies over the $3.4蟺$ steradians covered with the Observatory. Evidence for a deviation in excess of isotropy at intermediate angular scale, with ${\sim}\:15^\circ$ Gaussian spread or ${\sim}\:25^\circ$ top-hat radius, is obtained at the $4\:蟽$ significance level for cosmic-ray energies above ${\sim}\:40\:\text{EeV}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.13492v2-abstract-full').style.display = 'none'; document.getElementById('2206.13492v2-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> 5 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Published version, 33 pages, 10 figures. Dataset and analysis software available at https://doi.org/10.5281/zenodo.6504276</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-22-491-AD-PPD-SCD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 935 170 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2206.10938">arXiv:2206.10938</a> <span> [<a href="https://arxiv.org/pdf/2206.10938">pdf</a>, <a href="https://arxiv.org/format/2206.10938">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> <p class="title is-5 mathjax"> Investigating Hadronic Interactions at Ultra-High Energies with the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goos%2C+I">Isabel Goos</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a> , et al. (352 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="2206.10938v1-abstract-short" style="display: inline;"> The development of an extensive air shower depends not only on the nature of the primary ultra-high-energy cosmic ray but also on the properties of the hadronic interactions. For energies above those achievable in human-made accelerators, hadronic interactions are only accessible through the studies of extensive air showers, which can be measured at the Pierre Auger Observatory. With its hybrid de… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.10938v1-abstract-full').style.display = 'inline'; document.getElementById('2206.10938v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2206.10938v1-abstract-full" style="display: none;"> The development of an extensive air shower depends not only on the nature of the primary ultra-high-energy cosmic ray but also on the properties of the hadronic interactions. For energies above those achievable in human-made accelerators, hadronic interactions are only accessible through the studies of extensive air showers, which can be measured at the Pierre Auger Observatory. With its hybrid detector design, the Pierre Auger Observatory measures both the longitudinal development of showers in the atmosphere and the lateral distribution of particles that arrive at the ground. This way, observables that are sensitive to hadronic interactions at ultra-high energies can be obtained. While the hadronic interaction cross-section can be assessed from the longitudinal profiles, the number of muons and their fluctuations measured with the ground detectors are linked to other physical properties. In addition to these direct studies, we discuss here how measurements of the atmospheric depth of the maximum of air-shower profiles and the characteristics of the muon signal at the ground can be used to test the self-consistency of the post-LHC hadronic models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2206.10938v1-abstract-full').style.display = 'none'; document.getElementById('2206.10938v1-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 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">Proceedings of VHEPU 56th Rencontres de Moriond 2022</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.14864">arXiv:2205.14864</a> <span> [<a href="https://arxiv.org/pdf/2205.14864">pdf</a>, <a href="https://arxiv.org/format/2205.14864">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/ac7393">10.3847/1538-4357/ac7393 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for photons with energies above $2{\times}10^{17}$ eV using hybrid data from the low-energy extensions of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a> , et al. (351 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="2205.14864v1-abstract-short" style="display: inline;"> Ultra-high-energy photons with energies exceeding $10^{17}$ eV offer a wealth of connections to different aspects of cosmic-ray astrophysics as well as to gamma-ray and neutrino astronomy. The recent observations of photons with energies in the $10^{15}$ eV range further motivate searches for even higher-energy photons. In this paper, we present a search for photons with energies exceeding… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.14864v1-abstract-full').style.display = 'inline'; document.getElementById('2205.14864v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.14864v1-abstract-full" style="display: none;"> Ultra-high-energy photons with energies exceeding $10^{17}$ eV offer a wealth of connections to different aspects of cosmic-ray astrophysics as well as to gamma-ray and neutrino astronomy. The recent observations of photons with energies in the $10^{15}$ eV range further motivate searches for even higher-energy photons. In this paper, we present a search for photons with energies exceeding $2{\times}10^{17}$ eV using about 5.5 years of hybrid data from the low-energy extensions of the Pierre Auger Observatory. The upper limits on the integral photon flux derived here are the most stringent ones to date in the energy region between $10^{17}$ and $10^{18}$ eV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.14864v1-abstract-full').style.display = 'none'; document.getElementById('2205.14864v1-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 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">Accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-22-441-AD-PPD-SCD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 933 (2022) 125 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.08854">arXiv:2203.08854</a> <span> [<a href="https://arxiv.org/pdf/2203.08854">pdf</a>, <a href="https://arxiv.org/format/2203.08854">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</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/10.1103/PhysRevLett.130.061001">10.1103/PhysRevLett.130.061001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits to gauge coupling in the dark sector set by the non-observation of instanton-induced decay of Super-Heavy Dark Matter in the Pierre Auger Observatory data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Yebra%2C+J+A">J. Ammerman Yebra</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Avocone%2C+E">E. Avocone</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a> , et al. (352 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="2203.08854v3-abstract-short" style="display: inline;"> Instantons, which are non-perturbative solutions to Yang-Mills equations, provide a signal for the occurrence of quantum tunneling between distinct classes of vacua. They can give rise to decays of particles otherwise forbidden. Using data collected at the Pierre Auger Observatory, we search for signatures of such instanton-induced processes that would be suggestive of super-heavy particles decayi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08854v3-abstract-full').style.display = 'inline'; document.getElementById('2203.08854v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.08854v3-abstract-full" style="display: none;"> Instantons, which are non-perturbative solutions to Yang-Mills equations, provide a signal for the occurrence of quantum tunneling between distinct classes of vacua. They can give rise to decays of particles otherwise forbidden. Using data collected at the Pierre Auger Observatory, we search for signatures of such instanton-induced processes that would be suggestive of super-heavy particles decaying in the Galactic halo. These particles could have been produced during the post-inflationary epoch and match the relic abundance of dark matter inferred today. The non-observation of the signatures searched for allows us to derive a bound on the reduced coupling constant of gauge interactions in the dark sector: $伪_X \lesssim 0.09$, for $10^{9} \lesssim M_X/{\rm GeV} < 10^{19}$. Conversely, we obtain that, for instance, a reduced coupling constant $伪_X = 0.09$ excludes masses $M_X \gtrsim 3\times 10^{13}~$GeV. In the context of dark matter production from gravitational interactions alone, we illustrate how these bounds are complementary to those obtained on the Hubble rate at the end of inflation from the non-observation of tensor modes in the cosmological microwave background. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08854v3-abstract-full').style.display = 'none'; document.getElementById('2203.08854v3-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 December, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">9 pages, 3 figures, accepted for publication in Phys. Rev. Lett</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett. 130 (2023) 6, 061001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.08169">arXiv:2203.08169</a> <span> [<a href="https://arxiv.org/pdf/2203.08169">pdf</a>, <a href="https://arxiv.org/format/2203.08169">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div 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/10.1117/1.JATIS.8.1.014007">10.1117/1.JATIS.8.1.014007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Design and Performance of the Prototype Schwarzschild-Couder Telescope Camera </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">Colin B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">Giovanni Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">Michelangelo Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arlen%2C+T">Timothy Arlen</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">Wystan Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bertucci%2C+B">Bruna Bertucci</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">Elisabetta Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">Jonathan Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=Bitossi%2C+M">Massimiliano Bitossi</a>, <a href="/search/astro-ph?searchtype=author&query=Boiano%2C+A">Alfonso Boiano</a>, <a href="/search/astro-ph?searchtype=author&query=Bonavolont%C3%A0%2C+C">Carmela Bonavolont脿</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+R">Richard Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Bouvier%2C+A">Aurelien Bouvier</a>, <a href="/search/astro-ph?searchtype=author&query=Buscemi%2C+M">Mario Buscemi</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">Aryeh Brill</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+M">Anthony M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">James H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Canestrari%2C+R">Rodolfo Canestrari</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">Massimo Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Caprai%2C+M">Mirco Caprai</a>, <a href="/search/astro-ph?searchtype=author&query=Coppi%2C+P">Paolo Coppi</a>, <a href="/search/astro-ph?searchtype=author&query=Covault%2C+C+E">Corbin E. Covault</a>, <a href="/search/astro-ph?searchtype=author&query=Depaoli%2C+D">Davide Depaoli</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Venere%2C+L">Leonardo Di Venere</a> , et al. (64 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="2203.08169v1-abstract-short" style="display: inline;"> The prototype Schwarzschild-Couder Telescope (pSCT) is a candidate for a medium-sized telescope in the Cherenkov Telescope Array. The pSCT is based on a novel dual mirror optics design which reduces the plate scale and allows for the use of silicon photomultipliers as photodetectors. The prototype pSCT camera currently has only the central sector instrumented with 25 camera modules (1600 pixels)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08169v1-abstract-full').style.display = 'inline'; document.getElementById('2203.08169v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.08169v1-abstract-full" style="display: none;"> The prototype Schwarzschild-Couder Telescope (pSCT) is a candidate for a medium-sized telescope in the Cherenkov Telescope Array. The pSCT is based on a novel dual mirror optics design which reduces the plate scale and allows for the use of silicon photomultipliers as photodetectors. The prototype pSCT camera currently has only the central sector instrumented with 25 camera modules (1600 pixels), providing a 2.68$^{\circ}$ field of view (FoV). The camera electronics are based on custom TARGET (TeV array readout with GSa/s sampling and event trigger) application specific integrated circuits. Field programmable gate arrays sample incoming signals at a gigasample per second. A single backplane provides camera-wide triggers. An upgrade of the pSCT camera is in progress, which will fully populate the focal plane. This will increase the number of pixels to 11,328, the number of backplanes to 9, and the FoV to 8.04$^{\circ}$. Here we give a detailed description of the pSCT camera, including the basic concept, mechanical design, detectors, electronics, current status and first light. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08169v1-abstract-full').style.display = 'none'; document.getElementById('2203.08169v1-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Astron. Telesc. Instrum. Syst. 8(1), 014007 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.07313">arXiv:2201.07313</a> <span> [<a href="https://arxiv.org/pdf/2201.07313">pdf</a>, <a href="https://arxiv.org/format/2201.07313">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/ac6def">10.3847/1538-4357/ac6def <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Spatial Correlations of Neutrinos with Ultra-High-Energy Cosmic Rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+ANTARES+collaboration"> The ANTARES collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+S">S. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Andr%C3%A9%2C+M">M. Andr茅</a>, <a href="/search/astro-ph?searchtype=author&query=Anghinolfi%2C+M">M. Anghinolfi</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+M">M. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Ardid%2C+S">S. Ardid</a>, <a href="/search/astro-ph?searchtype=author&query=Aubert%2C+J+-">J. -J. Aubert</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Basa%2C+S">S. Basa</a>, <a href="/search/astro-ph?searchtype=author&query=Belhorma%2C+B">B. Belhorma</a>, <a href="/search/astro-ph?searchtype=author&query=Bendahman%2C+M">M. Bendahman</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+V">V. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Biagi%2C+S">S. Biagi</a>, <a href="/search/astro-ph?searchtype=author&query=Bissinger%2C+M">M. Bissinger</a>, <a href="/search/astro-ph?searchtype=author&query=Boumaaza%2C+J">J. Boumaaza</a>, <a href="/search/astro-ph?searchtype=author&query=Bouta%2C+M">M. Bouta</a>, <a href="/search/astro-ph?searchtype=author&query=Bouwhuis%2C+M+C">M. C. Bouwhuis</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%A2nza%C5%9F%2C+H">H. Br芒nza艧</a>, <a href="/search/astro-ph?searchtype=author&query=Bruijn%2C+R">R. Bruijn</a>, <a href="/search/astro-ph?searchtype=author&query=Brunner%2C+J">J. Brunner</a>, <a href="/search/astro-ph?searchtype=author&query=Busto%2C+J">J. Busto</a>, <a href="/search/astro-ph?searchtype=author&query=Caiffi%2C+B">B. Caiffi</a>, <a href="/search/astro-ph?searchtype=author&query=Calvo%2C+D">D. Calvo</a> , et al. (1025 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="2201.07313v3-abstract-short" style="display: inline;"> For several decades, the origin of ultra-high-energy cosmic rays (UHECRs) has been an unsolved question of high-energy astrophysics. One approach for solving this puzzle is to correlate UHECRs with high-energy neutrinos, since neutrinos are a direct probe of hadronic interactions of cosmic rays and are not deflected by magnetic fields. In this paper, we present three different approaches for corre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07313v3-abstract-full').style.display = 'inline'; document.getElementById('2201.07313v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.07313v3-abstract-full" style="display: none;"> For several decades, the origin of ultra-high-energy cosmic rays (UHECRs) has been an unsolved question of high-energy astrophysics. One approach for solving this puzzle is to correlate UHECRs with high-energy neutrinos, since neutrinos are a direct probe of hadronic interactions of cosmic rays and are not deflected by magnetic fields. In this paper, we present three different approaches for correlating the arrival directions of neutrinos with the arrival directions of UHECRs. The neutrino data is provided by the IceCube Neutrino Observatory and ANTARES, while the UHECR data with energies above $\sim$50 EeV is provided by the Pierre Auger Observatory and the Telescope Array. All experiments provide increased statistics and improved reconstructions with respect to our previous results reported in 2015. The first analysis uses a high-statistics neutrino sample optimized for point-source searches to search for excesses of neutrinos clustering in the vicinity of UHECR directions. The second analysis searches for an excess of UHECRs in the direction of the highest-energy neutrinos. The third analysis searches for an excess of pairs of UHECRs and highest-energy neutrinos on different angular scales. None of the analyses has found a significant excess, and previously reported over-fluctuations are reduced in significance. Based on these results, we further constrain the neutrino flux spatially correlated with UHECRs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07313v3-abstract-full').style.display = 'none'; document.getElementById('2201.07313v3-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 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">39 pages, 7 figures, 4 tables; updated source files including xml authorlist</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-22-033-AD-PPD-SCD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 934 164 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.06773">arXiv:2112.06773</a> <span> [<a href="https://arxiv.org/pdf/2112.06773">pdf</a>, <a href="https://arxiv.org/format/2112.06773">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/10.1088/1475-7516/2022/01/023">10.1088/1475-7516/2022/01/023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Testing effects of Lorentz invariance violation in the propagation of astroparticles with the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Cheminant%2C+K+A">K. Almeida Cheminant</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+J+A">J. A. Bellido</a> , et al. (352 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="2112.06773v2-abstract-short" style="display: inline;"> Lorentz invariance violation (LIV) is often described by dispersion relations of the form $E_i^2=m_i^2+p_i^2+未_{i,n} E^{2+n}$ with delta different based on particle type $i$, with energy $E$, momentum $p$ and rest mass $m$. Kinematics and energy thresholds of interactions are modified once the LIV terms become comparable to the squared masses of the particles involved. Thus, the strongest constrai… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.06773v2-abstract-full').style.display = 'inline'; document.getElementById('2112.06773v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.06773v2-abstract-full" style="display: none;"> Lorentz invariance violation (LIV) is often described by dispersion relations of the form $E_i^2=m_i^2+p_i^2+未_{i,n} E^{2+n}$ with delta different based on particle type $i$, with energy $E$, momentum $p$ and rest mass $m$. Kinematics and energy thresholds of interactions are modified once the LIV terms become comparable to the squared masses of the particles involved. Thus, the strongest constraints on the LIV coefficients $未_{i,n}$ tend to come from the highest energies. At sufficiently high energies, photons produced by cosmic ray interactions as they propagate through the Universe could be subluminal and unattenuated over cosmological distances. Cosmic ray interactions can also be modified and lead to detectable fingerprints in the energy spectrum and mass composition observed on Earth. The data collected at the Pierre Auger Observatory are therefore possibly sensitive to both the electromagnetic and hadronic sectors of LIV. In this article, we explore these two sectors by comparing the energy spectrum and the composition of cosmic rays and the upper limits on the photon flux from the Pierre Auger Observatory with simulations including LIV. Constraints on LIV parameters depend strongly on the mass composition of cosmic rays at the highest energies. For the electromagnetic sector, while no constraints can be obtained in the absence of protons beyond $10^{19}$ eV, we obtain $未_{纬,0} > -10^{-21}$, $未_{纬,1} > -10^{-40}$ eV$^{-1}$ and $未_{纬,2} > -10^{-58}$ eV$^{-2}$ in the case of a subdominant proton component up to $10^{20}$ eV. For the hadronic sector, we study the best description of the data as a function of LIV coefficients and we derive constraints in the hadronic sector such as $未_{\mathrm{had},0} < 10^{-19}$, $未_{\mathrm{had},1} < 10^{-38}$ eV$^{-1}$ and $未_{\mathrm{had},2}< 10^{-57}$ eV$^{-2}$ at 5$蟽$ CL. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.06773v2-abstract-full').style.display = 'none'; document.getElementById('2112.06773v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">Comments: Published version, 22 pages, 8 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-21-716-AD-PPD-SCD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 01 (2022) 023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.07463">arXiv:2110.07463</a> <span> [<a href="https://arxiv.org/pdf/2110.07463">pdf</a>, <a href="https://arxiv.org/format/2110.07463">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</span> </div> </div> <p class="title is-5 mathjax"> Prototype Schwarzschild-Couder Telescope for the Cherenkov Telescope Array: Commissioning the Optical System </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">C. B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+P+I">P. I. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bertucci%2C+B">B. Bertucci</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bitossi%2C+M">M. Bitossi</a>, <a href="/search/astro-ph?searchtype=author&query=Boiano%2C+A">A. Boiano</a>, <a href="/search/astro-ph?searchtype=author&query=Bonavolont%C3%A0%2C+C">C. Bonavolont脿</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+R">R. Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Canestrari%2C+R">R. Canestrari</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Caprai%2C+M">M. Caprai</a>, <a href="/search/astro-ph?searchtype=author&query=Covault%2C+C+E">C. E. Covault</a>, <a href="/search/astro-ph?searchtype=author&query=Depaoli%2C+D">D. Depaoli</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Venere%2C+L">L. Di Venere</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Fegan%2C+S">S. Fegan</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Fiandrini%2C+E">E. Fiandrini</a> , et al. (47 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="2110.07463v1-abstract-short" style="display: inline;"> A prototype Schwarzschild-Couder Telescope (pSCT) has been constructed at the Fred Lawrence Whipple Observatory as a candidate for the medium-sized telescopes of the Cherenkov Telescope Array Observatory (CTAO). CTAO is currently entering early construction phase of the project and once completed it will vastly improve very high energy gamma-ray detection component in multi-wavelength and multi-me… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.07463v1-abstract-full').style.display = 'inline'; document.getElementById('2110.07463v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.07463v1-abstract-full" style="display: none;"> A prototype Schwarzschild-Couder Telescope (pSCT) has been constructed at the Fred Lawrence Whipple Observatory as a candidate for the medium-sized telescopes of the Cherenkov Telescope Array Observatory (CTAO). CTAO is currently entering early construction phase of the project and once completed it will vastly improve very high energy gamma-ray detection component in multi-wavelength and multi-messenger observations due to significantly improved sensitivity, angular resolution and field of view comparing to the current generation of the ground-based gamma-ray observatories H.E.S.S., MAGIC and VERITAS. The pSCT uses a dual aspheric mirror design with a $9.7$ m primary mirror and $5.4$ m secondary mirror, both of which are segmented. The Schwarzschild-Couder (SC) optical system (OS) selected for the prototype telescope achieves wide field of view of $8$ degrees and simultaneously reduces the focal plane plate scale allowing an unprecedented compact ($0.78$m diameter) implementation of the high-resolution camera ($6$mm/ $0.067$deg per imaging pixel with $11,328$ pixels) based on the silicon photo-multipliers (SiPMs). The OS of the telescope is designed to eliminate spherical and comatic aberrations and minimize astigmatism to radically improve off-axis imaging and consequently angular resolution across all the field of view with respect to the conventional single-mirror telescopes. Fast and high imaging resolution OS of the pSCT comes with the challenging submillimeter-precision custom alignment system, which was successfully demonstrated with an on-axis point spread function (PSF) of $2.9$ arcmin prior to the first-light detection of the Crab Nebula in 2020. Ongoing and future commissioning activities are reported. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.07463v1-abstract-full').style.display = 'none'; document.getElementById('2110.07463v1-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 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">Journal ref:</span> Proceedings of Science, PoS(ICRC2021)717 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.13400">arXiv:2109.13400</a> <span> [<a href="https://arxiv.org/pdf/2109.13400">pdf</a>, <a href="https://arxiv.org/format/2109.13400">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/10.1140/epjc/s10052-021-09700-w">10.1140/epjc/s10052-021-09700-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The energy spectrum of cosmic rays beyond the turn-down around $10^{17}$ eV as measured with the surface detector of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+J+A">J. A. Bellido</a> , et al. (352 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="2109.13400v3-abstract-short" style="display: inline;"> We present a measurement of the cosmic-ray spectrum above 100\,PeV using the part of the surface detector of the Pierre Auger Observatory that has a spacing of 750~m. An inflection of the spectrum is observed, confirming the presence of the so-called \emph{second-knee} feature. The spectrum is then combined with that of the 1500\,m array to produce a single measurement of the flux, linking this sp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.13400v3-abstract-full').style.display = 'inline'; document.getElementById('2109.13400v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.13400v3-abstract-full" style="display: none;"> We present a measurement of the cosmic-ray spectrum above 100\,PeV using the part of the surface detector of the Pierre Auger Observatory that has a spacing of 750~m. An inflection of the spectrum is observed, confirming the presence of the so-called \emph{second-knee} feature. The spectrum is then combined with that of the 1500\,m array to produce a single measurement of the flux, linking this spectral feature with the three additional breaks at the highest energies. The combined spectrum, with an energy scale set calorimetrically via fluorescence telescopes and using a single detector type, results in the most statistically and systematically precise measurement of spectral breaks yet obtained. These measurements are critical for furthering our understanding of the highest energy cosmic rays. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.13400v3-abstract-full').style.display = 'none'; document.getElementById('2109.13400v3-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">Published version, 25 pages, 20 figures, 11 tables Updated April 2022 to fix typo in Table 10</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-21-474-AD-AE-SCD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C (2021) 81:966 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.06225">arXiv:2109.06225</a> <span> [<a href="https://arxiv.org/pdf/2109.06225">pdf</a>, <a href="https://arxiv.org/format/2109.06225">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/10.22323/1.395.0830">10.22323/1.395.0830 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of the Crab Nebula by the prototype Schwarzschild-Couder Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">C. B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+P+I">P. I. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bertucci%2C+B">B. Bertucci</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bitossi%2C+M">M. Bitossi</a>, <a href="/search/astro-ph?searchtype=author&query=Boiano%2C+A">A. Boiano</a>, <a href="/search/astro-ph?searchtype=author&query=Bonavolont%C3%A0%2C+C">C. Bonavolont脿</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+R">R. Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+M">A. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Canestrari%2C+R">R. Canestrari</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Caprai%2C+M">M. Caprai</a>, <a href="/search/astro-ph?searchtype=author&query=Covault%2C+C+E">C. E. Covault</a>, <a href="/search/astro-ph?searchtype=author&query=Depaoli%2C+D">D. Depaoli</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Venere%2C+L">L. Di Venere</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Fegan%2C+S">S. Fegan</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a> , et al. (49 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="2109.06225v1-abstract-short" style="display: inline;"> The Schwarzschild-Couder Telescope (SCT) is a medium-sized telescope technology proposed for the Cherenkov Telescope Array. It uses a novel dual-mirror optical design that removes comatic aberrations across its entire field of view. The SCT camera employs high-resolution silicon photomultiplier (SiPM) sensors with a pixel size of 4 arcminutes. A prototype SCT (pSCT) has been constructed at the Fre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.06225v1-abstract-full').style.display = 'inline'; document.getElementById('2109.06225v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.06225v1-abstract-full" style="display: none;"> The Schwarzschild-Couder Telescope (SCT) is a medium-sized telescope technology proposed for the Cherenkov Telescope Array. It uses a novel dual-mirror optical design that removes comatic aberrations across its entire field of view. The SCT camera employs high-resolution silicon photomultiplier (SiPM) sensors with a pixel size of 4 arcminutes. A prototype SCT (pSCT) has been constructed at the Fred Lawrence Whipple Observatory in Arizona, USA. An observing campaign in 2020, with a partial camera of 1600 pixels (2.7 degrees by 2.7 degrees field of view) resulted in detection of the Crab Nebula at 8.6 sigma statistical significance. Work on the pSCT camera and optical system is ongoing to improve performance and prepare for an upcoming camera upgrade. The pSCT camera upgrade will replace the current camera modules with improved SiPMs and readout electronics and will expand the camera to its full design field of view of 8 degrees in diameter (11,328 pixels). The fully upgraded pSCT will enable next-generation very-high-energy gamma-ray astrophysics through excellent background rejection and angular resolution. In this presentation we describe first results from the successful operation of the pSCT and future plans. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.06225v1-abstract-full').style.display = 'none'; document.getElementById('2109.06225v1-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">9 pages, 3 figures, 2 tables, contribution to ICRC 2021, similar to 10.1016/j.astropartphys.2021.102562 (arXiv:2012.08448)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings of Science, PoS(ICRC2021)830 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2109.05127">arXiv:2109.05127</a> <span> [<a href="https://arxiv.org/pdf/2109.05127">pdf</a>, <a href="https://arxiv.org/format/2109.05127">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/10.22323/1.395.0748">10.22323/1.395.0748 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Design and performance of the prototype Schwarzschild-Couder Telescope camera </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">C. B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+P+I">P. I. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bertucci%2C+B">B. Bertucci</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bitossi%2C+M">M. Bitossi</a>, <a href="/search/astro-ph?searchtype=author&query=Boiano%2C+A">A. Boiano</a>, <a href="/search/astro-ph?searchtype=author&query=Bonavolonta%2C+C">C. Bonavolonta</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+R">R. Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+M">A. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Caprai%2C+M">M. Caprai</a>, <a href="/search/astro-ph?searchtype=author&query=Covault%2C+C+E">C. E. Covault</a>, <a href="/search/astro-ph?searchtype=author&query=Depaoli%2C+D">D. Depaoli</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Venere%2C+L">L. Di Venere</a>, <a href="/search/astro-ph?searchtype=author&query=Errando%2C+M">M. Errando</a>, <a href="/search/astro-ph?searchtype=author&query=Fegan%2C+S">S. Fegan</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Fiandrini%2C+E">E. Fiandrini</a> , et al. (49 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="2109.05127v1-abstract-short" style="display: inline;"> The Cherenkov Telescope Array (CTA) is the next-generation ground-based observatory for very-high-energy gamma-ray astronomy. An innovative 9.7 m aperture, dual-mirror Schwarzschild-Couder Telescope (SCT) design is a candidate design for CTA Medium-Sized Telescopes. A prototype SCT (pSCT) has been constructed at the Fred Lawrence Whipple Observatory in Arizona, USA. Its camera is currently partial… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.05127v1-abstract-full').style.display = 'inline'; document.getElementById('2109.05127v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2109.05127v1-abstract-full" style="display: none;"> The Cherenkov Telescope Array (CTA) is the next-generation ground-based observatory for very-high-energy gamma-ray astronomy. An innovative 9.7 m aperture, dual-mirror Schwarzschild-Couder Telescope (SCT) design is a candidate design for CTA Medium-Sized Telescopes. A prototype SCT (pSCT) has been constructed at the Fred Lawrence Whipple Observatory in Arizona, USA. Its camera is currently partially instrumented with 1600 pixels covering a field of view of 2.7 degrees square. The small plate scale of the optical system allows densely packed silicon photomultipliers to be used, which combined with high-density trigger and waveform readout electronics enable the high-resolution camera. The camera's electronics are capable of imaging air shower development at a rate of one billion samples per second. We describe the commissioning and performance of the pSCT camera, including trigger and waveform readout performance, calibration, and absolute GPS time stamping. We also present the upgrade to the camera, which is currently underway. The upgrade will fully populate the focal plane, increasing the field of view to 8 degree diameter, and lower the front-end electronics noise, enabling a lower trigger threshold and improved reconstruction and background rejection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2109.05127v1-abstract-full').style.display = 'none'; document.getElementById('2109.05127v1-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 September, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">8 pages, 5 figures, Proceedings of the 37th International Cosmic Ray Conference (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/2101.11747">arXiv:2101.11747</a> <span> [<a href="https://arxiv.org/pdf/2101.11747">pdf</a>, <a href="https://arxiv.org/format/2101.11747">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/10.1088/1748-0221/16/07/T07008">10.1088/1748-0221/16/07/T07008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Design and implementation of the AMIGA embedded system for data acquisition </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (361 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="2101.11747v3-abstract-short" style="display: inline;"> The Auger Muon Infill Ground Array (AMIGA) is part of the AugerPrime upgrade of the Pierre Auger Observatory. It consists of particle counters buried 2.3 m underground next to the water-Cherenkov stations that form the 23.5 km$^2$ large infilled array. The reduced distance between detectors in this denser area allows the lowering of the energy threshold for primary cosmic ray reconstruction down t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.11747v3-abstract-full').style.display = 'inline'; document.getElementById('2101.11747v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.11747v3-abstract-full" style="display: none;"> The Auger Muon Infill Ground Array (AMIGA) is part of the AugerPrime upgrade of the Pierre Auger Observatory. It consists of particle counters buried 2.3 m underground next to the water-Cherenkov stations that form the 23.5 km$^2$ large infilled array. The reduced distance between detectors in this denser area allows the lowering of the energy threshold for primary cosmic ray reconstruction down to about 10$^{17}$ eV. At the depth of 2.3 m the electromagnetic component of cosmic ray showers is almost entirely absorbed so that the buried scintillators provide an independent and direct measurement of the air showers muon content. This work describes the design and implementation of the AMIGA embedded system, which provides centralized control, data acquisition and environment monitoring to its detectors. The presented system was firstly tested in the engineering array phase ended in 2017, and lately selected as the final design to be installed in all new detectors of the production phase. The system was proven to be robust and reliable and has worked in a stable manner since its first deployment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.11747v3-abstract-full').style.display = 'none'; document.getElementById('2101.11747v3-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 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Accepted for publication at JINST. Published version, 34 pages, 15 figures, 4 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-21-032-AD-AE-E-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 16 T07008 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.11602">arXiv:2101.11602</a> <span> [<a href="https://arxiv.org/pdf/2101.11602">pdf</a>, <a href="https://arxiv.org/format/2101.11602">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/10.1088/1748-0221/16/06/P06027">10.1088/1748-0221/16/06/P06027 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The FRAM robotic telescope for atmospheric monitoring at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (355 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="2101.11602v3-abstract-short" style="display: inline;"> FRAM (F/Photometric Robotic Atmospheric Monitor) is a robotic telescope operated at the Pierre Auger Observatory in Argentina for the purposes of atmospheric monitoring using stellar photometry. As a passive system which does not produce any light that could interfere with the observations of the fluorescence telescopes of the observatory, it complements the active monitoring systems that use lase… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.11602v3-abstract-full').style.display = 'inline'; document.getElementById('2101.11602v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.11602v3-abstract-full" style="display: none;"> FRAM (F/Photometric Robotic Atmospheric Monitor) is a robotic telescope operated at the Pierre Auger Observatory in Argentina for the purposes of atmospheric monitoring using stellar photometry. As a passive system which does not produce any light that could interfere with the observations of the fluorescence telescopes of the observatory, it complements the active monitoring systems that use lasers. We discuss the applications of stellar photometry for atmospheric monitoring at optical observatories in general and the particular modes of operation employed by the Auger FRAM. We describe in detail the technical aspects of FRAM, the hardware and software requirements for a successful operation of a robotic telescope for such a purpose and their implementation within the FRAM system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.11602v3-abstract-full').style.display = 'none'; document.getElementById('2101.11602v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Published version, 27 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 16 P06027 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.02946">arXiv:2101.02946</a> <span> [<a href="https://arxiv.org/pdf/2101.02946">pdf</a>, <a href="https://arxiv.org/format/2101.02946">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </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/10.1088/1748-0221/16/07/P07019">10.1088/1748-0221/16/07/P07019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Deep-Learning based Reconstruction of the Shower Maximum $X_{\mathrm{max}}$ using the Water-Cherenkov Detectors of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (348 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="2101.02946v2-abstract-short" style="display: inline;"> The atmospheric depth of the air shower maximum $X_{\mathrm{max}}$ is an observable commonly used for the determination of the nuclear mass composition of ultra-high energy cosmic rays. Direct measurements of $X_{\mathrm{max}}$ are performed using observations of the longitudinal shower development with fluorescence telescopes. At the same time, several methods have been proposed for an indirect e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02946v2-abstract-full').style.display = 'inline'; document.getElementById('2101.02946v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.02946v2-abstract-full" style="display: none;"> The atmospheric depth of the air shower maximum $X_{\mathrm{max}}$ is an observable commonly used for the determination of the nuclear mass composition of ultra-high energy cosmic rays. Direct measurements of $X_{\mathrm{max}}$ are performed using observations of the longitudinal shower development with fluorescence telescopes. At the same time, several methods have been proposed for an indirect estimation of $X_{\mathrm{max}}$ from the characteristics of the shower particles registered with surface detector arrays. In this paper, we present a deep neural network (DNN) for the estimation of $X_{\mathrm{max}}$. The reconstruction relies on the signals induced by shower particles in the ground based water-Cherenkov detectors of the Pierre Auger Observatory. The network architecture features recurrent long short-term memory layers to process the temporal structure of signals and hexagonal convolutions to exploit the symmetry of the surface detector array. We evaluate the performance of the network using air showers simulated with three different hadronic interaction models. Thereafter, we account for long-term detector effects and calibrate the reconstructed $X_{\mathrm{max}}$ using fluorescence measurements. Finally, we show that the event-by-event resolution in the reconstruction of the shower maximum improves with increasing shower energy and reaches less than $25~\mathrm{g/cm^{2}}$ at energies above $2\times 10^{19}~\mathrm{eV}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.02946v2-abstract-full').style.display = 'none'; document.getElementById('2101.02946v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Published version, 29 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-21-084-AD-AE-SCD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 16 P07019 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.08448">arXiv:2012.08448</a> <span> [<a href="https://arxiv.org/pdf/2012.08448">pdf</a>, <a href="https://arxiv.org/format/2012.08448">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.2021.102562">10.1016/j.astropartphys.2021.102562 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of the Crab Nebula with the 9.7 m Prototype Schwarzschild-Couder Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C+B">C. B. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arlen%2C+T">T. Arlen</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+P+I">P. I. Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bertucci%2C+B">B. Bertucci</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Biteau%2C+J">J. Biteau</a>, <a href="/search/astro-ph?searchtype=author&query=Bitossi%2C+M">M. Bitossi</a>, <a href="/search/astro-ph?searchtype=author&query=Boiano%2C+A">A. Boiano</a>, <a href="/search/astro-ph?searchtype=author&query=Bonavolont%C3%A0%2C+C">C. Bonavolont脿</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+R">R. Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Bouvier%2C+A">A. Bouvier</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+M">A. M. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Byrum%2C+K">K. Byrum</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Canestrari%2C+R">R. Canestrari</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Caprai%2C+M">M. Caprai</a>, <a href="/search/astro-ph?searchtype=author&query=Covault%2C+C+E">C. E. Covault</a> , et al. (83 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="2012.08448v1-abstract-short" style="display: inline;"> The Schwarzschild-Couder Telescope (SCT) is a telescope concept proposed for the Cherenkov Telescope Array. It employs a dual-mirror optical design to remove comatic aberrations over an $8^{\circ}$ field of view, and a high-density silicon photomultiplier camera (with a pixel resolution of 4 arcmin) to record Cherenkov emission from cosmic ray and gamma-ray initiated particle cascades in the atmos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.08448v1-abstract-full').style.display = 'inline'; document.getElementById('2012.08448v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.08448v1-abstract-full" style="display: none;"> The Schwarzschild-Couder Telescope (SCT) is a telescope concept proposed for the Cherenkov Telescope Array. It employs a dual-mirror optical design to remove comatic aberrations over an $8^{\circ}$ field of view, and a high-density silicon photomultiplier camera (with a pixel resolution of 4 arcmin) to record Cherenkov emission from cosmic ray and gamma-ray initiated particle cascades in the atmosphere. The prototype SCT (pSCT), comprising a 9.7 m diameter primary mirror and a partially instrumented camera with 1536 pixels, has been constructed at the Fred Lawrence Whipple Observatory. The telescope was inaugurated in January 2019, with commissioning continuing throughout 2019. We describe the first campaign of observations with the pSCT, conducted in January and February of 2020, and demonstrate the detection of gamma-ray emission from the Crab Nebula with a statistical significance of $8.6蟽$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.08448v1-abstract-full').style.display = 'none'; document.getElementById('2012.08448v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </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">13 pages, 12 figures, 3 tables, submitted to 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/2012.08016">arXiv:2012.08016</a> <span> [<a href="https://arxiv.org/pdf/2012.08016">pdf</a>, <a href="https://arxiv.org/format/2012.08016">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/10.1088/1748-0221/16/04/P04003">10.1088/1748-0221/16/04/P04003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibration of the underground muon detector of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Vel%C3%A1zquez%2C+J+C+A">J. C. Arteaga Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (348 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="2012.08016v2-abstract-short" style="display: inline;"> To obtain direct measurements of the muon content of extensive air showers with energy above $10^{16.5}$ eV, the Pierre Auger Observatory is currently being equipped with an underground muon detector (UMD), consisting of 219 10 $\mathrm{m^2}$-modules, each segmented into 64 scintillators coupled to silicon photomultipliers (SiPMs). Direct access to the shower muon content allows for the study of b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.08016v2-abstract-full').style.display = 'inline'; document.getElementById('2012.08016v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.08016v2-abstract-full" style="display: none;"> To obtain direct measurements of the muon content of extensive air showers with energy above $10^{16.5}$ eV, the Pierre Auger Observatory is currently being equipped with an underground muon detector (UMD), consisting of 219 10 $\mathrm{m^2}$-modules, each segmented into 64 scintillators coupled to silicon photomultipliers (SiPMs). Direct access to the shower muon content allows for the study of both of the composition of primary cosmic rays and of high-energy hadronic interactions in the forward direction. As the muon density can vary between tens of muons per m$^2$ close to the intersection of the shower axis with the ground to much less than one per m$^2$ when far away, the necessary broad dynamic range is achieved by the simultaneous implementation of two acquisition modes in the read-out electronics: the binary mode, tuned to count single muons, and the ADC mode, suited to measure a high number of them. In this work, we present the end-to-end calibration of the muon detector modules: first, the SiPMs are calibrated by means of the binary channel, and then, the ADC channel is calibrated using atmospheric muons, detected in parallel to the shower data acquisition. The laboratory and field measurements performed to develop the implementation of the full calibration chain of both binary and ADC channels are presented and discussed. The calibration procedure is reliable to work with the high amount of channels in the UMD, which will be operated continuously, in changing environmental conditions, for several years. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.08016v2-abstract-full').style.display = 'none'; document.getElementById('2012.08016v2-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 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </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 version, 25 pages, 12 figures, 0 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-678-AD-E-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST (2021) 16 P04003 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.06633">arXiv:2011.06633</a> <span> [<a href="https://arxiv.org/pdf/2011.06633">pdf</a>, <a href="https://arxiv.org/format/2011.06633">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div 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/10.1088/1748-0221/16/01/P01026">10.1088/1748-0221/16/01/P01026 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Design, upgrade and characterization of the silicon photomultiplier front-end for the AMIGA detector at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+J+A">J. A. Bellido</a> , et al. (335 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="2011.06633v2-abstract-short" style="display: inline;"> AMIGA (Auger Muons and Infill for the Ground Array) is an upgrade of the Pierre Auger Observatory to complement the study of ultra-high-energy cosmic rays (UHECR) by measuring the muon content of extensive air showers (EAS). It consists of an array of 61 water Cherenkov detectors on a denser spacing in combination with underground scintillation detectors used for muon density measurement. Each det… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06633v2-abstract-full').style.display = 'inline'; document.getElementById('2011.06633v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.06633v2-abstract-full" style="display: none;"> AMIGA (Auger Muons and Infill for the Ground Array) is an upgrade of the Pierre Auger Observatory to complement the study of ultra-high-energy cosmic rays (UHECR) by measuring the muon content of extensive air showers (EAS). It consists of an array of 61 water Cherenkov detectors on a denser spacing in combination with underground scintillation detectors used for muon density measurement. Each detector is composed of three scintillation modules, with 10 m$^2$ detection area per module, buried at 2.3 m depth, resulting in a total detection area of 30 m$^2$. Silicon photomultiplier sensors (SiPM) measure the amount of scintillation light generated by charged particles traversing the modules. In this paper, the design of the front-end electronics to process the signals of those SiPMs and test results from the laboratory and from the Pierre Auger Observatory are described. Compared to our previous prototype, the new electronics shows a higher performance, higher efficiency and lower power consumption, and it has a new acquisition system with increased dynamic range that allows measurements closer to the shower core. The new acquisition system is based on the measurement of the total charge signal that the muonic component of the cosmic ray shower generates in the detector. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.06633v2-abstract-full').style.display = 'none'; document.getElementById('2011.06633v2-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </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">40 pages, 33 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-605-AD-E-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 16 (2021) P01026 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.13027">arXiv:2010.13027</a> <span> [<a href="https://arxiv.org/pdf/2010.13027">pdf</a>, <a href="https://arxiv.org/format/2010.13027">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/10.1117/12.2568134">10.1117/12.2568134 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Verification of the Optical System of the 9.7-m Prototype Schwarzschild-Couder Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adams%2C+C">C. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosi%2C+G">G. Ambrosi</a>, <a href="/search/astro-ph?searchtype=author&query=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Benbow%2C+W">W. Benbow</a>, <a href="/search/astro-ph?searchtype=author&query=Bertucci%2C+B">B. Bertucci</a>, <a href="/search/astro-ph?searchtype=author&query=Bissaldi%2C+E">E. Bissaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Bitossi%2C+M">M. Bitossi</a>, <a href="/search/astro-ph?searchtype=author&query=Boiano%2C+A">A. Boiano</a>, <a href="/search/astro-ph?searchtype=author&query=Bonavolont%C3%A0%2C+C">C. Bonavolont脿</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+R">R. Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Brill%2C+A">A. Brill</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley%2C+J+H">J. H. Buckley</a>, <a href="/search/astro-ph?searchtype=author&query=Byrum%2C+K">K. Byrum</a>, <a href="/search/astro-ph?searchtype=author&query=Cameron%2C+R+A">R. A. Cameron</a>, <a href="/search/astro-ph?searchtype=author&query=Capasso%2C+M">M. Capasso</a>, <a href="/search/astro-ph?searchtype=author&query=Caprai%2C+M">M. Caprai</a>, <a href="/search/astro-ph?searchtype=author&query=Covault%2C+C+E">C. E. Covault</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Venere%2C+L">L. Di Venere</a>, <a href="/search/astro-ph?searchtype=author&query=Fegan%2C+S">S. Fegan</a>, <a href="/search/astro-ph?searchtype=author&query=Feng%2C+Q">Q. Feng</a>, <a href="/search/astro-ph?searchtype=author&query=Fiandrini%2C+E">E. Fiandrini</a>, <a href="/search/astro-ph?searchtype=author&query=Furniss%2C+A">A. Furniss</a>, <a href="/search/astro-ph?searchtype=author&query=Garczarczyk%2C+M">M. Garczarczyk</a> , et al. (55 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="2010.13027v1-abstract-short" style="display: inline;"> For the first time in the history of ground-based $纬$-ray astronomy, the on-axis performance of the dual mirror, aspheric, aplanatic Schwarzschild-Couder optical system has been demonstrated in a $9.7$-m aperture imaging atmospheric Cherenkov telescope. The novel design of the prototype Schwarzschild-Couder Telescope (pSCT) is motivated by the need of the next-generation Cherenkov Telescope Array… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.13027v1-abstract-full').style.display = 'inline'; document.getElementById('2010.13027v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.13027v1-abstract-full" style="display: none;"> For the first time in the history of ground-based $纬$-ray astronomy, the on-axis performance of the dual mirror, aspheric, aplanatic Schwarzschild-Couder optical system has been demonstrated in a $9.7$-m aperture imaging atmospheric Cherenkov telescope. The novel design of the prototype Schwarzschild-Couder Telescope (pSCT) is motivated by the need of the next-generation Cherenkov Telescope Array (CTA) observatory to have the ability to perform wide ($\geq 8^{\circ}$) field-of-view observations simultaneously with superior imaging of atmospheric cascades (resolution of $0.067^{\circ}$ per pixel or better). The pSCT design, if implemented in the CTA installation, has the potential to improve significantly both the $纬$-ray angular resolution and the off-axis sensitivity of the observatory, reaching nearly the theoretical limit of the technique and thereby making a major impact on the CTA observatory sky survey programs, follow-up observations of multi-messenger transients with poorly known initial localization, as well as on the spatially resolved spectroscopic studies of extended $纬$-ray sources. This contribution reports on the initial alignment procedures and point-spread-function results for the challenging segmented aspheric primary and secondary mirrors of the pSCT. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.13027v1-abstract-full').style.display = 'none'; document.getElementById('2010.13027v1-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </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">19 pages, 11 figures, proceedings for SPIE Optical Engineering + Applications, 2020, Online Only</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.10953">arXiv:2010.10953</a> <span> [<a href="https://arxiv.org/pdf/2010.10953">pdf</a>, <a href="https://arxiv.org/format/2010.10953">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/abb476">10.3847/1538-4357/abb476 <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 from TXS 0506+056 using the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bellido%2C+J+A">J. A. Bellido</a> , et al. (342 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="2010.10953v1-abstract-short" style="display: inline;"> Results of a search for ultra-high-energy neutrinos with the Pierre Auger Observatory from the direction of the blazar TXS 0506+056 are presented. They were obtained as part of the follow-up that stemmed from the detection of high-energy neutrinos and gamma rays with IceCube, \textit{Fermi}-LAT, MAGIC, and other detectors of electromagnetic radiation in several bands. The Pierre Auger Observatory… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.10953v1-abstract-full').style.display = 'inline'; document.getElementById('2010.10953v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.10953v1-abstract-full" style="display: none;"> Results of a search for ultra-high-energy neutrinos with the Pierre Auger Observatory from the direction of the blazar TXS 0506+056 are presented. They were obtained as part of the follow-up that stemmed from the detection of high-energy neutrinos and gamma rays with IceCube, \textit{Fermi}-LAT, MAGIC, and other detectors of electromagnetic radiation in several bands. The Pierre Auger Observatory is sensitive to neutrinos in the energy range from 100 PeV to 100 EeV and in the zenith angle range from $胃=60^\circ$ to $胃=95^\circ$, where the zenith angle is measured from the vertical direction. No neutrinos from the direction of TXS 0506+056 have been found. The results were analyzed in three periods: One of 6 months around the detection of IceCube-170922A, coinciding with a flare period of TXS 0506+056, a second one of 110 days during which the IceCube collaboration found an excess of 13 neutrinos from a direction compatible with TXS 0506+056, and a third one from 2004 January 1 up to 2018 August 31, over which the Pierre Auger Observatory has been taking data. The sensitivity of the Observatory is addressed for different spectral indices by considering the fluxes that would induce a single expected event during the observation period. For indices compatible with those measured by the IceCube collaboration the expected number of neutrinos at the Observatory is well-below one. Spectral indices as hard as 1.5 would have to apply in this energy range to expect a single event to have been detected. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.10953v1-abstract-full').style.display = 'none'; document.getElementById('2010.10953v1-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2020. </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 version, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Published in The Astrophysical Journal, 902:105, 2020 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.06488">arXiv:2008.06488</a> <span> [<a href="https://arxiv.org/pdf/2008.06488">pdf</a>, <a href="https://arxiv.org/format/2008.06488">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/PhysRevLett.125.121106">10.1103/PhysRevLett.125.121106 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Features of the energy spectrum of cosmic rays above $2.5{\times} 10^{18}$ eV using the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (358 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="2008.06488v2-abstract-short" style="display: inline;"> We report a measurement of the energy spectrum of cosmic rays above $2.5{\times} 10^{18}$ eV based on $215,030$ events. New results are presented: at about $1.3{\times} 10^{19}$ eV, the spectral index changes from $2.51 \pm 0.03 \textrm{ (stat.)} \pm 0.05 \textrm{ (sys.)}$ to $3.05 \pm 0.05 \textrm{ (stat.)}\pm 0.10\textrm{ (sys.)}$, evolving to… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.06488v2-abstract-full').style.display = 'inline'; document.getElementById('2008.06488v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.06488v2-abstract-full" style="display: none;"> We report a measurement of the energy spectrum of cosmic rays above $2.5{\times} 10^{18}$ eV based on $215,030$ events. New results are presented: at about $1.3{\times} 10^{19}$ eV, the spectral index changes from $2.51 \pm 0.03 \textrm{ (stat.)} \pm 0.05 \textrm{ (sys.)}$ to $3.05 \pm 0.05 \textrm{ (stat.)}\pm 0.10\textrm{ (sys.)}$, evolving to $5.1\pm0.3\textrm{ (stat.)} \pm 0.1\textrm{ (sys.)}$ beyond $5{\times} 10^{19}$ eV, while no significant dependence of spectral features on the declination is seen in the accessible range. These features of the spectrum can be reproduced in models with energy-dependent mass composition. The energy density in cosmic rays above $5{\times} 10^{18}$ eV is $(5.66 \pm 0.03 \textrm{ (stat.)} \pm 1.40 \textrm{ (sys.)} ) {\times} 10^{53}~$erg Mpc$^{-3}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.06488v2-abstract-full').style.display = 'none'; document.getElementById('2008.06488v2-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </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 version; 2 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-431-E-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 125, 121106 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.06486">arXiv:2008.06486</a> <span> [<a href="https://arxiv.org/pdf/2008.06486">pdf</a>, <a href="https://arxiv.org/format/2008.06486">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.102.062005">10.1103/PhysRevD.102.062005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the cosmic-ray energy spectrum above $2.5{\times} 10^{18}$ eV using the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+Pierre+Auger+Collaboration"> The Pierre Auger Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aab%2C+A">A. Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">P. Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">M. Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Albury%2C+J+M">J. M. Albury</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">J. Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">J. Alvarez-Mu帽iz</a>, <a href="/search/astro-ph?searchtype=author&query=Batista%2C+R+A">R. Alves Batista</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">G. A. Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andrada%2C+B">B. Andrada</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+P+R+A">P. R. Ara煤jo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H">H. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">P. Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Badescu%2C+A+M">A. M. Badescu</a>, <a href="/search/astro-ph?searchtype=author&query=Bakalova%2C+A">A. Bakalova</a>, <a href="/search/astro-ph?searchtype=author&query=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F">F. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (358 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="2008.06486v2-abstract-short" style="display: inline;"> We report a measurement of the energy spectrum of cosmic rays for energies above $2.5 {\times} 10^{18}~$eV based on 215,030 events recorded with zenith angles below $60^\circ$. A key feature of the work is that the estimates of the energies are independent of assumptions about the unknown hadronic physics or of the primary mass composition. The measurement is the most precise made hitherto with th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.06486v2-abstract-full').style.display = 'inline'; document.getElementById('2008.06486v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.06486v2-abstract-full" style="display: none;"> We report a measurement of the energy spectrum of cosmic rays for energies above $2.5 {\times} 10^{18}~$eV based on 215,030 events recorded with zenith angles below $60^\circ$. A key feature of the work is that the estimates of the energies are independent of assumptions about the unknown hadronic physics or of the primary mass composition. The measurement is the most precise made hitherto with the accumulated exposure being so large that the measurements of the flux are dominated by systematic uncertainties except at energies above $5 {\times} 10^{19}~$eV. The principal conclusions are: (1) The flattening of the spectrum near $5 {\times} 10^{18}~$eV, the so-called "ankle", is confirmed. (2) The steepening of the spectrum at around $5 {\times} 10^{19}~$eV is confirmed. (3) A new feature has been identified in the spectrum: in the region above the ankle the spectral index $纬$ of the particle flux ($\propto E^{-纬}$) changes from $2.51 \pm 0.03~{\rm (stat.)} \pm 0.05~{\rm (sys.)}$ to $3.05 \pm 0.05~{\rm (stat.)} \pm 0.10~{\rm (sys.)}$ before changing sharply to $5.1 \pm 0.3~{\rm (stat.)} \pm 0.1~{\rm (sys.)}$ above $5 {\times} 10^{19}~$eV. (4) No evidence for any dependence of the spectrum on declination has been found other than a mild excess from the Southern Hemisphere that is consistent with the anisotropy observed above $8 {\times} 10^{18}~$eV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.06486v2-abstract-full').style.display = 'none'; document.getElementById('2008.06486v2-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </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 version; 16 figures, 6 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-432-E-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 102, 062005 (2020) </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Aramo%2C+C&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Aramo%2C+C&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Aramo%2C+C&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Aramo%2C+C&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Aramo%2C+C&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> </ul> </nav> <div class="is-hidden-tablet">  <span class="help" style="display: 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