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</div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <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=Castillo%2C+J+A&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Castillo%2C+J+A&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Castillo%2C+J+A&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.09035">arXiv:2007.09035</a> <span> [<a href="https://arxiv.org/pdf/2007.09035">pdf</a>, <a href="https://arxiv.org/format/2007.09035">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/10.1088/1748-0221/15/10/P10021">10.1088/1748-0221/15/10/P10021 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reconstruction of Events Recorded 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=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. (356 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="2007.09035v4-abstract-short" style="display: inline;"> Cosmic rays arriving at Earth collide with the upper parts of the atmosphere, thereby inducing extensive air showers. When secondary particles from the cascade arrive at the ground, they are measured by surface detector arrays. We describe the methods applied to the measurements of the surface detector of the Pierre Auger Observatory to reconstruct events with zenith angles less than $60^\circ$ us… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.09035v4-abstract-full').style.display = 'inline'; document.getElementById('2007.09035v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.09035v4-abstract-full" style="display: none;"> Cosmic rays arriving at Earth collide with the upper parts of the atmosphere, thereby inducing extensive air showers. When secondary particles from the cascade arrive at the ground, they are measured by surface detector arrays. We describe the methods applied to the measurements of the surface detector of the Pierre Auger Observatory to reconstruct events with zenith angles less than $60^\circ$ using the timing and signal information recorded using the water-Cherenkov detector stations. In addition, we assess the accuracy of these methods in reconstructing the arrival directions of the primary cosmic ray particles and the sizes of the induced showers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.09035v4-abstract-full').style.display = 'none'; document.getElementById('2007.09035v4-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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, 36 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-487-AD-E-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 15 (2020) P10021 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.04139">arXiv:2007.04139</a> <span> [<a href="https://arxiv.org/pdf/2007.04139">pdf</a>, <a href="https://arxiv.org/format/2007.04139">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/10.1088/1748-0221/15/09/P09002">10.1088/1748-0221/15/09/P09002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Studies on the response of a water-Cherenkov detector of the Pierre Auger Observatory to atmospheric muons using an RPC hodoscope </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. (353 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="2007.04139v2-abstract-short" style="display: inline;"> Extensive air showers, originating from ultra-high energy cosmic rays, have been successfully measured through the use of arrays of water-Cherenkov detectors (WCDs). Sophisticated analyses exploiting WCD data have made it possible to demonstrate that shower simulations, based on different hadronic-interaction models, cannot reproduce the observed number of muons at the ground. The accurate knowled… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.04139v2-abstract-full').style.display = 'inline'; document.getElementById('2007.04139v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.04139v2-abstract-full" style="display: none;"> Extensive air showers, originating from ultra-high energy cosmic rays, have been successfully measured through the use of arrays of water-Cherenkov detectors (WCDs). Sophisticated analyses exploiting WCD data have made it possible to demonstrate that shower simulations, based on different hadronic-interaction models, cannot reproduce the observed number of muons at the ground. The accurate knowledge of the WCD response to muons is paramount in establishing the exact level of this discrepancy. In this work, we report on a study of the response of a WCD of the Pierre Auger Observatory to atmospheric muons performed with a hodoscope made of resistive plate chambers (RPCs), enabling us to select and reconstruct nearly 600 thousand single muon trajectories with zenith angles ranging from 0$^\circ$ to 55$^\circ$. Comparison of distributions of key observables between the hodoscope data and the predictions of dedicated simulations allows us to demonstrate the accuracy of the latter at a level of 2%. As the WCD calibration is based on its response to atmospheric muons, the hodoscope data are also exploited to show the long-term stability of the procedure. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.04139v2-abstract-full').style.display = 'none'; document.getElementById('2007.04139v2-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 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-285-PPD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 15 (2020) P09002 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2004.10591">arXiv:2004.10591</a> <span> [<a href="https://arxiv.org/pdf/2004.10591">pdf</a>, <a href="https://arxiv.org/format/2004.10591">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/10.1088/1475-7516/2020/06/017">10.1088/1475-7516/2020/06/017 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for magnetically-induced signatures in the arrival directions of ultra-high-energy cosmic rays 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=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. (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="2004.10591v2-abstract-short" style="display: inline;"> We search for signals of magnetically-induced effects in the arrival directions of ultra-high-energy cosmic rays detected at the Pierre Auger Observatory. We apply two different methods. One is a search for sets of events that show a correlation between their arrival direction and the inverse of their energy, which would be expected if they come from the same point-like source, they have the same… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.10591v2-abstract-full').style.display = 'inline'; document.getElementById('2004.10591v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2004.10591v2-abstract-full" style="display: none;"> We search for signals of magnetically-induced effects in the arrival directions of ultra-high-energy cosmic rays detected at the Pierre Auger Observatory. We apply two different methods. One is a search for sets of events that show a correlation between their arrival direction and the inverse of their energy, which would be expected if they come from the same point-like source, they have the same electric charge and their deflection is relatively small and coherent. We refer to these sets of events as "multiplets". The second method, called "thrust", is a principal axis analysis aimed to detect the elongated patterns in a region of interest. We study the sensitivity of both methods using a benchmark simulation and we apply them to data in two different searches. The first search is done assuming as source candidates a list of nearby active galactic nuclei and starburst galaxies. The second is an all-sky blind search. We report the results and we find no statistically significant features. We discuss the compatibility of these results with the indications on the mass composition inferred from data of the Pierre Auger Observatory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2004.10591v2-abstract-full').style.display = 'none'; document.getElementById('2004.10591v2-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, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 April, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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; correction of a minor typo</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-177-E-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Published in JCAP06(2020)017 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.06172">arXiv:2002.06172</a> <span> [<a href="https://arxiv.org/pdf/2002.06172">pdf</a>, <a href="https://arxiv.org/format/2002.06172">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/ab7236">10.3847/1538-4357/ab7236 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmic-ray anisotropies in right ascension measured by 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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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. (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="2002.06172v1-abstract-short" style="display: inline;"> We present measurements of the large-scale cosmic-ray anisotropies in right ascension, using data collected by the surface detector array of the Pierre Auger Observatory over more than 14 years. We determine the equatorial dipole component, $\vec{d}_\perp$, through a Fourier analysis in right ascension that includes weights for each event so as to account for the main detector-induced systematic e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.06172v1-abstract-full').style.display = 'inline'; document.getElementById('2002.06172v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.06172v1-abstract-full" style="display: none;"> We present measurements of the large-scale cosmic-ray anisotropies in right ascension, using data collected by the surface detector array of the Pierre Auger Observatory over more than 14 years. We determine the equatorial dipole component, $\vec{d}_\perp$, through a Fourier analysis in right ascension that includes weights for each event so as to account for the main detector-induced systematic effects. For the energies at which the trigger efficiency of the array is small, the ``East-West'' method is employed. Besides using the data from the array with detectors separated by 1500 m, we also include data from the smaller but denser sub-array of detectors with 750 m separation, which allows us to extend the analysis down to $\sim 0.03$ EeV. The most significant equatorial dipole amplitude obtained is that in the cumulative bin above 8~EeV, $d_\perp=6.0^{+1.0}_{-0.9}$%, which is inconsistent with isotropy at the 6$蟽$ level. In the bins below 8 EeV, we obtain 99% CL upper-bounds on $d_\perp$ at the level of 1 to 3 percent. At energies below 1 EeV, even though the amplitudes are not significant, the phases determined in most of the bins are not far from the right ascension of the Galactic center, at $伪_{\rm GC}=-94^\circ$, suggesting a predominantly Galactic origin for anisotropies at these energies. The reconstructed dipole phases in the energy bins above 4 EeV point instead to right ascensions that are almost opposite to the Galactic center one, indicative of an extragalactic cosmic ray origin. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.06172v1-abstract-full').style.display = 'none'; document.getElementById('2002.06172v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">Accepted by ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-20-076 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Published in Astrophys. J 891 (2020)142 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1909.09073">arXiv:1909.09073</a> <span> [<a href="https://arxiv.org/pdf/1909.09073">pdf</a>, <a href="https://arxiv.org/format/1909.09073">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The Pierre Auger Observatory: Contributions to the 36th International Cosmic Ray Conference (ICRC 2019) </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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=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=Baur%2C+S">S. Baur</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="1909.09073v1-abstract-short" style="display: inline;"> Contributions of the Pierre Auger Collaboration to the 36th International Cosmic Ray Conference (ICRC 2019), 24 July - 1 August 2019, Madison, Wisconsin, USA. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1909.09073v1-abstract-full" style="display: none;"> Contributions of the Pierre Auger Collaboration to the 36th International Cosmic Ray Conference (ICRC 2019), 24 July - 1 August 2019, Madison, Wisconsin, USA. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1909.09073v1-abstract-full').style.display = 'none'; document.getElementById('1909.09073v1-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 September, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">compendium of 29 proceedings for the ICRC 2019</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.07422">arXiv:1906.07422</a> <span> [<a href="https://arxiv.org/pdf/1906.07422">pdf</a>, <a href="https://arxiv.org/format/1906.07422">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/10.1088/1475-7516/2019/10/022">10.1088/1475-7516/2019/10/022 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the origin of ultra-high-energy cosmic rays with neutrinos in the EeV energy range 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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=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=Baur%2C+S">S. Baur</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (367 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="1906.07422v2-abstract-short" style="display: inline;"> Neutrinos with energies above $10^{17}$ eV are detectable with the Surface Detector Array of the Pierre Auger Observatory. The identification is efficiently performed for neutrinos of all flavors interacting in the atmosphere at large zenith angles, as well as for Earth-skimming $蟿$ neutrinos with nearly tangential trajectories relative to the earth. No neutrino candidates were found in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.07422v2-abstract-full').style.display = 'inline'; document.getElementById('1906.07422v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.07422v2-abstract-full" style="display: none;"> Neutrinos with energies above $10^{17}$ eV are detectable with the Surface Detector Array of the Pierre Auger Observatory. The identification is efficiently performed for neutrinos of all flavors interacting in the atmosphere at large zenith angles, as well as for Earth-skimming $蟿$ neutrinos with nearly tangential trajectories relative to the earth. No neutrino candidates were found in $\sim\,14.7$ years of data taken up to 31 August 2018. This leads to restrictive upper bounds on their flux. The $90\%$ C.L. single-flavor limit to the diffuse flux of ultra-high-energy neutrinos with an $E_谓^{-2}$ spectrum in the energy range $1.0 \times 10^{17}~{\rm eV} - 2.5 \times 10^{19}~{\rm eV}$ is $E^2 {\rm d}N_谓/{\rm d}E_谓< 4.4 \times 10^{-9}~{\rm GeV~cm^{-2}~s^{-1}~sr^{-1}}$, placing strong constraints on several models of neutrino production at EeV energies and on the properties of the sources of ultra-high-energy cosmic rays. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.07422v2-abstract-full').style.display = 'none'; document.getElementById('1906.07422v2-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 October, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version, 27 pages, 7 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-19-280 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 10 (2019) 022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1906.07419">arXiv:1906.07419</a> <span> [<a href="https://arxiv.org/pdf/1906.07419">pdf</a>, <a href="https://arxiv.org/format/1906.07419">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/10.1088/1475-7516/2019/11/004">10.1088/1475-7516/2019/11/004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limits on point-like sources of ultra-high-energy 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=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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=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=Baur%2C+S">S. Baur</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (367 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="1906.07419v2-abstract-short" style="display: inline;"> With the Surface Detector array (SD) of the Pierre Auger Observatory we can detect neutrinos with energy between $10^{17}\,$eV and $10^{20}\,$eV from point-like sources across the sky, from close to the Southern Celestial Pole up to $60^\circ$ in declination, with peak sensitivities at declinations around $\sim -53^\circ$ and $\sim+55^\circ$, and an unmatched sensitivity for arrival directions in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.07419v2-abstract-full').style.display = 'inline'; document.getElementById('1906.07419v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1906.07419v2-abstract-full" style="display: none;"> With the Surface Detector array (SD) of the Pierre Auger Observatory we can detect neutrinos with energy between $10^{17}\,$eV and $10^{20}\,$eV from point-like sources across the sky, from close to the Southern Celestial Pole up to $60^\circ$ in declination, with peak sensitivities at declinations around $\sim -53^\circ$ and $\sim+55^\circ$, and an unmatched sensitivity for arrival directions in the Northern hemisphere. A search has been performed for highly-inclined air showers induced by neutrinos of all flavours with no candidate events found in data taken between 1 Jan 2004 and 31 Aug 2018. Upper limits on the neutrino flux from point-like steady sources have been derived as a function of source declination. An unrivaled sensitivity is achieved in searches for transient sources with emission lasting over an hour or less, if they occur within the field of view corresponding to the zenith angle range between $60^\circ$ and $~95^\circ$ where the SD of the Pierre Auger Observatory is most sensitive to neutrinos. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1906.07419v2-abstract-full').style.display = 'none'; document.getElementById('1906.07419v2-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 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 June, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-19-279 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 11 (2019) 004 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1904.11918">arXiv:1904.11918</a> <span> [<a href="https://arxiv.org/pdf/1904.11918">pdf</a>, <a href="https://arxiv.org/format/1904.11918">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/10.3389/fspas.2019.00024">10.3389/fspas.2019.00024 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-Messenger Physics 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=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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=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=Baur%2C+S">S. Baur</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (368 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="1904.11918v1-abstract-short" style="display: inline;"> An overview of the multi-messenger capabilities of the Pierre Auger Observatory is presented. The techniques and performance of searching for Ultra-High Energy neutrinos, photons and neutrons are described. Some of the most relevant results are reviewed, such as stringent upper bounds that were placed to a flux of diffuse cosmogenic neutrinos and photons, bounds placed on neutrinos emitted from co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.11918v1-abstract-full').style.display = 'inline'; document.getElementById('1904.11918v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1904.11918v1-abstract-full" style="display: none;"> An overview of the multi-messenger capabilities of the Pierre Auger Observatory is presented. The techniques and performance of searching for Ultra-High Energy neutrinos, photons and neutrons are described. Some of the most relevant results are reviewed, such as stringent upper bounds that were placed to a flux of diffuse cosmogenic neutrinos and photons, bounds placed on neutrinos emitted from compact binary mergers that were detected by LIGO and Virgo during their first and second observing runs, as well as searches for high energy photons and neutrons from the Galactic center that constrain the properties of the putative Galactic PeVatron, observed by the H.E.S.S.\ collaboration. The observation of directional correlations between ultra-high energy cosmic rays and either high energy astrophysical neutrinos or specific source populations, weighted by their electromagnetic radiation, are also discussed. They constitute additional multi-messenger approaches aimed at identifying the sources of high energy cosmic rays. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1904.11918v1-abstract-full').style.display = 'none'; document.getElementById('1904.11918v1-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 April, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 7 figures, Review published in Frontiers in Astronomy and Space Sciences</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-19-135 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> April 2019 | Volume 6 | Article 24 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1901.08040">arXiv:1901.08040</a> <span> [<a href="https://arxiv.org/pdf/1901.08040">pdf</a>, <a href="https://arxiv.org/format/1901.08040">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/10.1103/PhysRevD.100.082003">10.1103/PhysRevD.100.082003 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Data-driven estimation of the invisible energy of cosmic ray showers 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=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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=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=Baur%2C+S">S. Baur</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (367 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="1901.08040v3-abstract-short" style="display: inline;"> The determination of the primary energy of extensive air showers using the fluorescence detection technique requires an estimation of the energy carried away by particles that do not deposit all their energy in the atmosphere. This estimation is typically made using Monte Carlo simulations and thus depends on the assumed primary particle mass and on model predictions for neutrino and muon producti… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.08040v3-abstract-full').style.display = 'inline'; document.getElementById('1901.08040v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1901.08040v3-abstract-full" style="display: none;"> The determination of the primary energy of extensive air showers using the fluorescence detection technique requires an estimation of the energy carried away by particles that do not deposit all their energy in the atmosphere. This estimation is typically made using Monte Carlo simulations and thus depends on the assumed primary particle mass and on model predictions for neutrino and muon production. In this work we present a new method to obtain the invisible energy from events detected by the Pierre Auger Observatory. The method uses measurements of the muon number at ground level, and it allows us to reduce significantly the systematic uncertainties related to the mass composition and the high energy hadronic interaction models, and consequently to improve the estimation of the energy scale of the Observatory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1901.08040v3-abstract-full').style.display = 'none'; document.getElementById('1901.08040v3-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 November, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 January, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version, 18 pages, 10 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-19-040 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 100, 082003 (2019) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1811.04660">arXiv:1811.04660</a> <span> [<a href="https://arxiv.org/pdf/1811.04660">pdf</a>, <a href="https://arxiv.org/format/1811.04660">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/10.1088/1475-7516/2019/03/018">10.1088/1475-7516/2019/03/018 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the average shape of longitudinal profiles of cosmic-ray 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=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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=ez-Mu%C3%B1iz%2C+J+A">J. Alvar ez-Mu帽iz</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=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=Baur%2C+S">S. Baur</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (363 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="1811.04660v2-abstract-short" style="display: inline;"> The profile of the longitudinal development of showers produced by ultra-high energy cosmic rays carries information related to the interaction properties of the primary particles with atmospheric nuclei. In this work, we present the first measurement of the average shower profile in traversed atmospheric depth at the Pierre Auger Observatory. The shapes of profiles are well reproduced by the Gais… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.04660v2-abstract-full').style.display = 'inline'; document.getElementById('1811.04660v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1811.04660v2-abstract-full" style="display: none;"> The profile of the longitudinal development of showers produced by ultra-high energy cosmic rays carries information related to the interaction properties of the primary particles with atmospheric nuclei. In this work, we present the first measurement of the average shower profile in traversed atmospheric depth at the Pierre Auger Observatory. The shapes of profiles are well reproduced by the Gaisser-Hillas parametrization within the range studied, for E > 10^{17.8} eV. A detailed analysis of the systematic uncertainties is performed using 10 years of data and a full detector simulation. The average shape is quantified using two variables related to the width and asymmetry of the profile, and the results are compared with predictions of hadronic interaction models for different primary particles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1811.04660v2-abstract-full').style.display = 'none'; document.getElementById('1811.04660v2-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 May, 2019; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 November, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version, 20 pages, 6 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-18-633 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP03(2019)018 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1808.03579">arXiv:1808.03579</a> <span> [<a href="https://arxiv.org/pdf/1808.03579">pdf</a>, <a href="https://arxiv.org/ps/1808.03579">ps</a>, <a href="https://arxiv.org/format/1808.03579">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/aae689">10.3847/1538-4357/aae689 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Large-scale cosmic-ray anisotropies above 4 EeV measured by 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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=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=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=Baur%2C+S">S. Baur</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="1808.03579v2-abstract-short" style="display: inline;"> We present a detailed study of the large-scale anisotropies of cosmic rays with energies above 4 EeV measured using the Pierre Auger Observatory. For the energy bins [4,8] EeV and $E\geq 8$ EeV, the most significant signal is a dipolar modulation in right ascension at energies above 8 EeV, as previously reported. In this paper we further scrutinize the highest-energy bin by splitting it into three… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.03579v2-abstract-full').style.display = 'inline'; document.getElementById('1808.03579v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1808.03579v2-abstract-full" style="display: none;"> We present a detailed study of the large-scale anisotropies of cosmic rays with energies above 4 EeV measured using the Pierre Auger Observatory. For the energy bins [4,8] EeV and $E\geq 8$ EeV, the most significant signal is a dipolar modulation in right ascension at energies above 8 EeV, as previously reported. In this paper we further scrutinize the highest-energy bin by splitting it into three energy ranges. We find that the amplitude of the dipole increases with energy above 4 EeV. The growth can be fitted with a power law with index $尾=0.79\pm 0.19$. The directions of the dipoles are consistent with an extragalactic origin of these anisotropies at all the energies considered. Additionally we have estimated the quadrupolar components of the anisotropy: they are not statistically significant. We discuss the results in the context of the predictions from different models for the distribution of ultrahigh-energy sources and cosmic magnetic fields. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1808.03579v2-abstract-full').style.display = 'none'; document.getElementById('1808.03579v2-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 December, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 August, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version, 16 pages, 7 figures, 8 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-18-393 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 868 (2018) 4 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1806.05386">arXiv:1806.05386</a> <span> [<a href="https://arxiv.org/pdf/1806.05386">pdf</a>, <a href="https://arxiv.org/format/1806.05386">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/10.1088/1475-7516/2018/10/026">10.1088/1475-7516/2018/10/026 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of inclined EeV air showers with the radio 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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arsene%2C+N">N. Arsene</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=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=Baur%2C+S">S. Baur</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+H">K. H. Becker</a> , et al. (370 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="1806.05386v2-abstract-short" style="display: inline;"> With the Auger Engineering Radio Array (AERA) of the Pierre Auger Observatory, we have observed the radio emission from 561 extensive air showers with zenith angles between 60$^\circ$ and 84$^\circ$. In contrast to air showers with more vertical incidence, these inclined air showers illuminate large ground areas of several km$^2$ with radio signals detectable in the 30 to 80\,MHz band. A compariso… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.05386v2-abstract-full').style.display = 'inline'; document.getElementById('1806.05386v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1806.05386v2-abstract-full" style="display: none;"> With the Auger Engineering Radio Array (AERA) of the Pierre Auger Observatory, we have observed the radio emission from 561 extensive air showers with zenith angles between 60$^\circ$ and 84$^\circ$. In contrast to air showers with more vertical incidence, these inclined air showers illuminate large ground areas of several km$^2$ with radio signals detectable in the 30 to 80\,MHz band. A comparison of the measured radio-signal amplitudes with Monte Carlo simulations of a subset of 50 events for which we reconstruct the energy using the Auger surface detector shows agreement within the uncertainties of the current analysis. As expected for forward-beamed radio emission undergoing no significant absorption or scattering in the atmosphere, the area illuminated by radio signals grows with the zenith angle of the air shower. Inclined air showers with EeV energies are thus measurable with sparse radio-antenna arrays with grid sizes of a km or more. This is particularly attractive as radio detection provides direct access to the energy in the electromagnetic cascade of an air shower, which in case of inclined air showers is not accessible by arrays of particle detectors on the ground. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1806.05386v2-abstract-full').style.display = 'none'; document.getElementById('1806.05386v2-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, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version, 14 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-18-259 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP10(2018)026 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1801.06160">arXiv:1801.06160</a> <span> [<a href="https://arxiv.org/pdf/1801.06160">pdf</a>, <a href="https://arxiv.org/format/1801.06160">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/10.3847/2041-8213/aaa66d">10.3847/2041-8213/aaa66d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Indication of anisotropy in arrival directions of ultra-high-energy cosmic rays through comparison to the flux pattern of extragalactic gamma-ray sources </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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arsene%2C+N">N. Arsene</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=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=Beatty%2C+J+J">J. J. Beatty</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. (368 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="1801.06160v2-abstract-short" style="display: inline;"> A new analysis of the dataset from the Pierre Auger Observatory provides evidence for anisotropy in the arrival directions of ultra-high-energy cosmic rays on an intermediate angular scale, which is indicative of excess arrivals from strong, nearby sources. The data consist of 5514 events above 20 EeV with zenith angles up to 80 deg recorded before 2017 April 30. Sky models have been created for t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.06160v2-abstract-full').style.display = 'inline'; document.getElementById('1801.06160v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1801.06160v2-abstract-full" style="display: none;"> A new analysis of the dataset from the Pierre Auger Observatory provides evidence for anisotropy in the arrival directions of ultra-high-energy cosmic rays on an intermediate angular scale, which is indicative of excess arrivals from strong, nearby sources. The data consist of 5514 events above 20 EeV with zenith angles up to 80 deg recorded before 2017 April 30. Sky models have been created for two distinct populations of extragalactic gamma-ray emitters: active galactic nuclei from the second catalog of hard Fermi-LAT sources (2FHL) and starburst galaxies from a sample that was examined with Fermi-LAT. Flux-limited samples, which include all types of galaxies from the Swift-BAT and 2MASS surveys, have been investigated for comparison. The sky model of cosmic-ray density constructed using each catalog has two free parameters, the fraction of events correlating with astrophysical objects and an angular scale characterizing the clustering of cosmic rays around extragalactic sources. A maximum-likelihood ratio test is used to evaluate the best values of these parameters and to quantify the strength of each model by contrast with isotropy. It is found that the starburst model fits the data better than the hypothesis of isotropy with a statistical significance of 4.0 sigma, the highest value of the test statistic being for energies above 39 EeV. The three alternative models are favored against isotropy with 2.7-3.2 sigma significance. The origin of the indicated deviation from isotropy is examined and prospects for more sensitive future studies are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1801.06160v2-abstract-full').style.display = 'none'; document.getElementById('1801.06160v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 January, 2018; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2018. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version, 10 pages, 3 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-17-358 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Aab. et al., The Astrophysical Journal Letters, 853:L29 (2018) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.07249">arXiv:1710.07249</a> <span> [<a href="https://arxiv.org/pdf/1710.07249">pdf</a>, <a href="https://arxiv.org/format/1710.07249">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"> Inferences on Mass Composition and Tests of Hadronic Interactions from 0.3 to 100 EeV 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=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=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> , et al. (381 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="1710.07249v1-abstract-short" style="display: inline;"> We present a new method for probing the hadronic interaction models at ultra-high energy and extracting details about mass composition. This is done using the time profiles of the signals recorded with the water-Cherenkov detectors of the Pierre Auger Observatory. The profiles arise from a mix of the muon and electromagnetic components of air-showers. Using the risetimes of the recorded signals we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.07249v1-abstract-full').style.display = 'inline'; document.getElementById('1710.07249v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.07249v1-abstract-full" style="display: none;"> We present a new method for probing the hadronic interaction models at ultra-high energy and extracting details about mass composition. This is done using the time profiles of the signals recorded with the water-Cherenkov detectors of the Pierre Auger Observatory. The profiles arise from a mix of the muon and electromagnetic components of air-showers. Using the risetimes of the recorded signals we define a new parameter, which we use to compare our observations with predictions from simulations. We find, firstly, inconsistencies between our data and predictions over a greater energy range and with substantially more events than in previous studies. Secondly, by calibrating the new parameter with fluorescence measurements from observations made at the Auger Observatory, we can infer the depth of shower maximum for a sample of over 81,000 events extending from 0.3 EeV to over 100 EeV. Above 30 EeV, the sample is nearly fourteen times larger than currently available from fluorescence measurements and extending the covered energy range by half a decade. The energy dependence of the average depth of shower maximum is compared to simulations and interpreted in terms of the mean of the logarithmic mass. We find good agreement with previous work and extend the measurement of the mean depth of shower maximum to greater energies than before, reducing significantly the statistical uncertainty associated with the inferences about mass composition. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.07249v1-abstract-full').style.display = 'none'; document.getElementById('1710.07249v1-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 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages; 18 figures; version 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">Report number:</span> FERMILAB-PUB-17-357 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1710.05839">arXiv:1710.05839</a> <span> [<a href="https://arxiv.org/pdf/1710.05839">pdf</a>, <a href="https://arxiv.org/format/1710.05839">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aa9aed">10.3847/2041-8213/aa9aed <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for High-energy Neutrinos from Binary Neutron Star Merger GW170817 with ANTARES, IceCube, and the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Albert%2C+A">A. Albert</a>, <a href="/search/astro-ph?searchtype=author&query=Andre%2C+M">M. Andre</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=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=Avgitas%2C+T">T. Avgitas</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Barrios-Marti%2C+J">J. Barrios-Marti</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=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=Bormuth%2C+R">R. Bormuth</a>, <a href="/search/astro-ph?searchtype=author&query=Bourret%2C+S">S. Bourret</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=Branzacs%2C+H">H. Branzacs</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=Capone%2C+A">A. Capone</a>, <a href="/search/astro-ph?searchtype=author&query=Caramete%2C+L">L. Caramete</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+J">J. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Celli%2C+S">S. Celli</a>, <a href="/search/astro-ph?searchtype=author&query=Moursli%2C+R+C+E">R. Cherkaoui El Moursli</a> , et al. (1916 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="1710.05839v2-abstract-short" style="display: inline;"> The Advanced LIGO and Advanced Virgo observatories recently discovered gravitational waves from a binary neutron star inspiral. A short gamma-ray burst (GRB) that followed the merger of this binary was also recorded by the Fermi Gamma-ray Burst Monitor (Fermi-GBM), and the Anticoincidence Shield for the Spectrometer for the International Gamma-Ray Astrophysics Laboratory (INTEGRAL), indicating par… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.05839v2-abstract-full').style.display = 'inline'; document.getElementById('1710.05839v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1710.05839v2-abstract-full" style="display: none;"> The Advanced LIGO and Advanced Virgo observatories recently discovered gravitational waves from a binary neutron star inspiral. A short gamma-ray burst (GRB) that followed the merger of this binary was also recorded by the Fermi Gamma-ray Burst Monitor (Fermi-GBM), and the Anticoincidence Shield for the Spectrometer for the International Gamma-Ray Astrophysics Laboratory (INTEGRAL), indicating particle acceleration by the source. The precise location of the event was determined by optical detections of emission following the merger. We searched for high-energy neutrinos from the merger in the GeV--EeV energy range using the ANTARES, IceCube, and Pierre Auger Observatories. No neutrinos directionally coincident with the source were detected within $\pm500$ s around the merger time. Additionally, no MeV neutrino burst signal was detected coincident with the merger. We further carried out an extended search in the direction of the source for high-energy neutrinos within the 14-day period following the merger, but found no evidence of emission. We used these results to probe dissipation mechanisms in relativistic outflows driven by the binary neutron star merger. The non-detection is consistent with model predictions of short GRBs observed at a large off-axis angle. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1710.05839v2-abstract-full').style.display = 'none'; document.getElementById('1710.05839v2-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 November, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 2 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> LIGO-P1700344 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.07321">arXiv:1709.07321</a> <span> [<a href="https://arxiv.org/pdf/1709.07321">pdf</a>, <a href="https://arxiv.org/format/1709.07321">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/10.1126/science.aan4338">10.1126/science.aan4338 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of a Large-scale Anisotropy in the Arrival Directions of Cosmic Rays above $8 \times 10^{18}$ eV </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=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=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> , et al. (382 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="1709.07321v1-abstract-short" style="display: inline;"> Cosmic rays are atomic nuclei arriving from outer space that reach the highest energies observed in nature. Clues to their origin come from studying the distribution of their arrival directions. Using $3 \times 10^4$ cosmic rays above $8 \times 10^{18}$ electron volts, recorded with the Pierre Auger Observatory from a total exposure of 76,800 square kilometers steradian year, we report an anisotro… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.07321v1-abstract-full').style.display = 'inline'; document.getElementById('1709.07321v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.07321v1-abstract-full" style="display: none;"> Cosmic rays are atomic nuclei arriving from outer space that reach the highest energies observed in nature. Clues to their origin come from studying the distribution of their arrival directions. Using $3 \times 10^4$ cosmic rays above $8 \times 10^{18}$ electron volts, recorded with the Pierre Auger Observatory from a total exposure of 76,800 square kilometers steradian year, we report an anisotropy in the arrival directions. The anisotropy, detected at more than the 5.2$蟽$ level of significance, can be described by a dipole with an amplitude of $6.5_{-0.9}^{+1.3}$% towards right ascension $伪_{d} = 100 \pm 10$ degrees and declination $未_{d} = -24_{-13}^{+12}$ degrees. That direction indicates an extragalactic origin for these ultra-high energy particles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.07321v1-abstract-full').style.display = 'none'; document.getElementById('1709.07321v1-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 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages (with supplementary material), 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-17-354 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Science 357 (22 September 2017) 1266 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1709.01537">arXiv:1709.01537</a> <span> [<a href="https://arxiv.org/pdf/1709.01537">pdf</a>, <a href="https://arxiv.org/format/1709.01537">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/10.1016/j.astropartphys.2017.09.001">10.1016/j.astropartphys.2017.09.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Spectral Calibration of the Fluorescence Telescopes 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=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=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> , et al. (381 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="1709.01537v3-abstract-short" style="display: inline;"> We present a novel method to measure precisely the relative spectral response of the fluorescence telescopes of the Pierre Auger Observatory. We used a portable light source based on a xenon flasher and a monochromator to measure the relative spectral efficiencies of eight telescopes in steps of 5 nm from 280 nm to 440 nm. Each point in a scan had approximately 2 nm FWHM out of the monochromator.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.01537v3-abstract-full').style.display = 'inline'; document.getElementById('1709.01537v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1709.01537v3-abstract-full" style="display: none;"> We present a novel method to measure precisely the relative spectral response of the fluorescence telescopes of the Pierre Auger Observatory. We used a portable light source based on a xenon flasher and a monochromator to measure the relative spectral efficiencies of eight telescopes in steps of 5 nm from 280 nm to 440 nm. Each point in a scan had approximately 2 nm FWHM out of the monochromator. Different sets of telescopes in the observatory have different optical components, and the eight telescopes measured represent two each of the four combinations of components represented in the observatory. We made an end-to-end measurement of the response from different combinations of optical components, and the monochromator setup allowed for more precise and complete measurements than our previous multi-wavelength calibrations. We find an overall uncertainty in the calibration of the spectral response of most of the telescopes of 1.5% for all wavelengths; the six oldest telescopes have larger overall uncertainties of about 2.2%. We also report changes in physics measureables due to the change in calibration, which are generally small. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1709.01537v3-abstract-full').style.display = 'none'; document.getElementById('1709.01537v3-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 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 September, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version. Added journal reference and DOI. Added Report Number</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-17-355 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astroparticle Physics 95 (2017) 44-56 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1708.06592">arXiv:1708.06592</a> <span> [<a href="https://arxiv.org/pdf/1708.06592">pdf</a>, <a href="https://arxiv.org/format/1708.06592">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="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> The Pierre Auger Observatory: Contributions to the 35th International Cosmic Ray Conference (ICRC 2017) </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=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=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. (373 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1708.06592v2-abstract-short" style="display: inline;"> Contributions of the Pierre Auger Collaboration to the 35th International Cosmic Ray Conference (ICRC 2017), 12-20 July 2017, Bexco, Busan, Korea. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1708.06592v2-abstract-full" style="display: none;"> Contributions of the Pierre Auger Collaboration to the 35th International Cosmic Ray Conference (ICRC 2017), 12-20 July 2017, Bexco, Busan, Korea. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1708.06592v2-abstract-full').style.display = 'none'; document.getElementById('1708.06592v2-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 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 August, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">compendium of 26 proceedings for the ICRC 2017</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1703.06193">arXiv:1703.06193</a> <span> [<a href="https://arxiv.org/pdf/1703.06193">pdf</a>, <a href="https://arxiv.org/format/1703.06193">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/10.1088/1748-0221/12/03/P03002">10.1088/1748-0221/12/03/P03002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Muon Counting using Silicon Photomultipliers in the AMIGA 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=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Ambrosio%2C+M">M. Ambrosio</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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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> , et al. (400 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="1703.06193v2-abstract-short" style="display: inline;"> AMIGA (Auger Muons and Infill for the Ground Array) is an upgrade of the Pierre Auger Observatory designed to extend its energy range of detection and to directly measure the muon content of the cosmic ray primary particle showers. The array will be formed by an infill of surface water-Cherenkov detectors associated with buried scintillation counters employed for muon counting. Each counter is com… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.06193v2-abstract-full').style.display = 'inline'; document.getElementById('1703.06193v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1703.06193v2-abstract-full" style="display: none;"> AMIGA (Auger Muons and Infill for the Ground Array) is an upgrade of the Pierre Auger Observatory designed to extend its energy range of detection and to directly measure the muon content of the cosmic ray primary particle showers. The array will be formed by an infill of surface water-Cherenkov detectors associated with buried scintillation counters employed for muon counting. Each counter is composed of three scintillation modules, with a 10 m$^2$ detection area per module. In this paper, a new generation of detectors, replacing the current multi-pixel photomultiplier tube (PMT) with silicon photo sensors (aka. SiPMs), is proposed. The selection of the new device and its front-end electronics is explained. A method to calibrate the counting system that ensures the performance of the detector is detailed. This method has the advantage of being able to be carried out in a remote place such as the one where the detectors are deployed. High efficiency results, i.e. 98 % efficiency for the highest tested overvoltage, combined with a low probability of accidental counting ($\sim$2 %), show a promising performance for this new system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1703.06193v2-abstract-full').style.display = 'none'; document.getElementById('1703.06193v2-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 October, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 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-16-656-AD-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 12 (2017) P03002 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1702.01392">arXiv:1702.01392</a> <span> [<a href="https://arxiv.org/pdf/1702.01392">pdf</a>, <a href="https://arxiv.org/format/1702.01392">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/10.1088/1748-0221/12/10/T10005">10.1088/1748-0221/12/10/T10005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibration of the Logarithmic-Periodic Dipole Antenna (LPDA) Radio Stations at the Pierre Auger Observatory using an Octocopter </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=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=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> , et al. (380 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="1702.01392v3-abstract-short" style="display: inline;"> An in-situ calibration of a logarithmic periodic dipole antenna with a frequency coverage of 30 MHz to 80 MHz is performed. Such antennas are part of a radio station system used for detection of cosmic ray induced air showers at the Engineering Radio Array of the Pierre Auger Observatory, the so-called Auger Engineering Radio Array (AERA). The directional and frequency characteristics of the broad… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.01392v3-abstract-full').style.display = 'inline'; document.getElementById('1702.01392v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1702.01392v3-abstract-full" style="display: none;"> An in-situ calibration of a logarithmic periodic dipole antenna with a frequency coverage of 30 MHz to 80 MHz is performed. Such antennas are part of a radio station system used for detection of cosmic ray induced air showers at the Engineering Radio Array of the Pierre Auger Observatory, the so-called Auger Engineering Radio Array (AERA). The directional and frequency characteristics of the broadband antenna are investigated using a remotely piloted aircraft (RPA) carrying a small transmitting antenna. The antenna sensitivity is described by the vector effective length relating the measured voltage with the electric-field components perpendicular to the incoming signal direction. The horizontal and meridional components are determined with an overall uncertainty of 7.4^{+0.9}_{-0.3} % and 10.3^{+2.8}_{-1.7} % respectively. The measurement is used to correct a simulated response of the frequency and directional response of the antenna. In addition, the influence of the ground conductivity and permittivity on the antenna response is simulated. Both have a negligible influence given the ground conditions measured at the detector site. The overall uncertainties of the vector effective length components result in an uncertainty of 8.8^{+2.1}_{-1.3} % in the square root of the energy fluence for incoming signal directions with zenith angles smaller than 60掳. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1702.01392v3-abstract-full').style.display = 'none'; document.getElementById('1702.01392v3-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 June, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 February, 2017; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2017. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version. Updated online abstract only. Manuscript is unchanged with respect to v2. 39 pages, 15 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-17-046 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 12 (2017) T10005 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1612.07155">arXiv:1612.07155</a> <span> [<a href="https://arxiv.org/pdf/1612.07155">pdf</a>, <a href="https://arxiv.org/ps/1612.07155">ps</a>, <a href="https://arxiv.org/format/1612.07155">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/10.1088/1475-7516/2017/04/038">10.1088/1475-7516/2017/04/038 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Combined fit of spectrum and composition data as measured by 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=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=Balaceanu%2C+A">A. Balaceanu</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=Beatty%2C+J+J">J. J. Beatty</a> , et al. (375 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1612.07155v3-abstract-short" style="display: inline;"> We present a combined fit of a simple astrophysical model of UHECR sources to both the energy spectrum and mass composition data measured by the Pierre Auger Observatory. The fit has been performed for energies above $5 \cdot 10^{18}$ eV, i.e.~the region of the all-particle spectrum above the so-called "ankle" feature. The astrophysical model we adopted consists of identical sources uniformly dist… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.07155v3-abstract-full').style.display = 'inline'; document.getElementById('1612.07155v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.07155v3-abstract-full" style="display: none;"> We present a combined fit of a simple astrophysical model of UHECR sources to both the energy spectrum and mass composition data measured by the Pierre Auger Observatory. The fit has been performed for energies above $5 \cdot 10^{18}$ eV, i.e.~the region of the all-particle spectrum above the so-called "ankle" feature. The astrophysical model we adopted consists of identical sources uniformly distributed in a comoving volume, where nuclei are accelerated through a rigidity-dependent mechanism. The fit results suggest sources characterized by relatively low maximum injection energies, hard spectra and heavy chemical composition. We also show that uncertainties about physical quantities relevant to UHECR propagation and shower development have a non-negligible impact on the fit results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.07155v3-abstract-full').style.display = 'none'; document.getElementById('1612.07155v3-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 February, 2018; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Corrected typos in values of SD vertical spectrum energy bias (B.5); Added expression for SD inclined spectrum energy resolution (B.6), erroneously claimed to have been published before</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-618 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP04(2017)038 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1612.04155">arXiv:1612.04155</a> <span> [<a href="https://arxiv.org/pdf/1612.04155">pdf</a>, <a href="https://arxiv.org/ps/1612.04155">ps</a>, <a href="https://arxiv.org/format/1612.04155">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/2041-8213/aa61a5">10.3847/2041-8213/aa61a5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A targeted search for point sources of EeV photons 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=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=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=Balaceanu%2C+A">A. Balaceanu</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=Beatty%2C+J+J">J. J. Beatty</a> , et al. (375 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1612.04155v2-abstract-short" style="display: inline;"> Simultaneous measurements of air showers with the fluorescence and surface detectors of the Pierre Auger Observatory allow a sensitive search for EeV photon point sources. Several Galactic and extragalactic candidate objects are grouped in classes to reduce the statistical penalty of many trials from that of a blind search and are analyzed for a significant excess above the background expectation.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.04155v2-abstract-full').style.display = 'inline'; document.getElementById('1612.04155v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.04155v2-abstract-full" style="display: none;"> Simultaneous measurements of air showers with the fluorescence and surface detectors of the Pierre Auger Observatory allow a sensitive search for EeV photon point sources. Several Galactic and extragalactic candidate objects are grouped in classes to reduce the statistical penalty of many trials from that of a blind search and are analyzed for a significant excess above the background expectation. The presented search does not find any evidence for photon emission at candidate sources, and combined $p$-values for every class are reported. Particle and energy flux upper limits are given for selected candidate sources. These limits significantly constrain predictions of EeV proton emission models from non-transient Galactic and nearby extragalactic sources, as illustrated for the particular case of the Galactic center region. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.04155v2-abstract-full').style.display = 'none'; document.getElementById('1612.04155v2-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 March, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-655 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Letters, 837:L25 (7pp), 2017 March 10 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1612.01517">arXiv:1612.01517</a> <span> [<a href="https://arxiv.org/pdf/1612.01517">pdf</a>, <a href="https://arxiv.org/format/1612.01517">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2017/04/009;">10.1088/1475-7516/2017/04/009; <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2020/09/E02">10.1088/1475-7516/2020/09/E02 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for photons with energies above 10$^{18}$ eV using the hybrid 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=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=Balaceanu%2C+A">A. Balaceanu</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=Beatty%2C+J+J">J. J. Beatty</a> , et al. (375 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1612.01517v3-abstract-short" style="display: inline;"> A search for ultra-high energy photons with energies above 1 EeV is performed using nine years of data collected by the Pierre Auger Observatory in hybrid operation mode. An unprecedented separation power between photon and hadron primaries is achieved by combining measurements of the longitudinal air-shower development with the particle content at ground measured by the fluorescence and surface d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.01517v3-abstract-full').style.display = 'inline'; document.getElementById('1612.01517v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1612.01517v3-abstract-full" style="display: none;"> A search for ultra-high energy photons with energies above 1 EeV is performed using nine years of data collected by the Pierre Auger Observatory in hybrid operation mode. An unprecedented separation power between photon and hadron primaries is achieved by combining measurements of the longitudinal air-shower development with the particle content at ground measured by the fluorescence and surface detectors, respectively. Only three photon candidates at energies 1 - 2 EeV are found, which is compatible with the expected hadron-induced background. Upper limits on the integral flux of ultra-high energy photons of 0.038, 0.010, 0.009, 0.008 and 0.007 km$^{-2}$ sr$^{-1}$ yr$^{-1}$ are derived at 95% C.L. for energy thresholds of 1, 2, 3, 5 and 10 EeV. These limits bound the fractions of photons in the all-particle integral flux below 0.14%, 0.17%, 0.42%, 0.86% and 2.9%. For the first time the photon fraction at EeV energies is constrained at the sub-percent level. The improved limits are below the flux of diffuse photons predicted by some astrophysical scenarios for cosmogenic photon production. The new results rule-out the early top-down models $-$ in which ultra-high energy cosmic rays are produced by, e.g., the decay of super-massive particles $-$ and challenge the most recent super-heavy dark matter models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1612.01517v3-abstract-full').style.display = 'none'; document.getElementById('1612.01517v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 September, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 December, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Corrected version after erratum published in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-657 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP04(2017)009; JCAP09(2020)E02 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1611.06812">arXiv:1611.06812</a> <span> [<a href="https://arxiv.org/pdf/1611.06812">pdf</a>, <a href="https://arxiv.org/ps/1611.06812">ps</a>, <a href="https://arxiv.org/format/1611.06812">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/10.1088/1475-7516/2017/06/026">10.1088/1475-7516/2017/06/026 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Multi-resolution anisotropy studies of ultrahigh-energy cosmic rays detected 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=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=Balaceanu%2C+A">A. Balaceanu</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=Baus%2C+C">C. Baus</a> , et al. (378 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="1611.06812v2-abstract-short" style="display: inline;"> We report a multi-resolution search for anisotropies in the arrival directions of cosmic rays detected at the Pierre Auger Observatory with local zenith angles up to $80^\circ$ and energies in excess of 4 EeV ($4 \times 10^{18}$ eV). This search is conducted by measuring the angular power spectrum and performing a needlet wavelet analysis in two independent energy ranges. Both analyses are complem… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.06812v2-abstract-full').style.display = 'inline'; document.getElementById('1611.06812v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1611.06812v2-abstract-full" style="display: none;"> We report a multi-resolution search for anisotropies in the arrival directions of cosmic rays detected at the Pierre Auger Observatory with local zenith angles up to $80^\circ$ and energies in excess of 4 EeV ($4 \times 10^{18}$ eV). This search is conducted by measuring the angular power spectrum and performing a needlet wavelet analysis in two independent energy ranges. Both analyses are complementary since the angular power spectrum achieves a better performance in identifying large-scale patterns while the needlet wavelet analysis, considering the parameters used in this work, presents a higher efficiency in detecting smaller-scale anisotropies, potentially providing directional information on any observed anisotropies. No deviation from isotropy is observed on any angular scale in the energy range between 4 and 8 EeV. Above 8 EeV, an indication for a dipole moment is captured; while no other deviation from isotropy is observed for moments beyond the dipole one. The corresponding $p$-values obtained after accounting for searches blindly performed at several angular scales, are $1.3 \times 10^{-5}$ in the case of the angular power spectrum, and $2.5 \times 10^{-3}$ in the case of the needlet analysis. While these results are consistent with previous reports making use of the same data set, they provide extensions of the previous works through the thorough scans of the angular scales. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1611.06812v2-abstract-full').style.display = 'none'; document.getElementById('1611.06812v2-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 June, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version. Added journal reference and DOI. Added Report Number</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-556-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 06 (2017) 026 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1610.08509">arXiv:1610.08509</a> <span> [<a href="https://arxiv.org/pdf/1610.08509">pdf</a>, <a href="https://arxiv.org/format/1610.08509">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.117.192001">10.1103/PhysRevLett.117.192001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Testing Hadronic Interactions at Ultrahigh Energies with Air Showers Measured by 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=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</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=Ambrosio%2C+M">M. Ambrosio</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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a> , et al. (413 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="1610.08509v2-abstract-short" style="display: inline;"> Ultrahigh energy cosmic ray air showers probe particle physics at energies beyond the reach of accelerators. Here we introduce a new method to test hadronic interaction models without relying on the absolute energy calibration, and apply it to events with primary energy 6-16 EeV (E_CM = 110-170 TeV), whose longitudinal development and lateral distribution were simultaneously measured by the Pierre… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.08509v2-abstract-full').style.display = 'inline'; document.getElementById('1610.08509v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1610.08509v2-abstract-full" style="display: none;"> Ultrahigh energy cosmic ray air showers probe particle physics at energies beyond the reach of accelerators. Here we introduce a new method to test hadronic interaction models without relying on the absolute energy calibration, and apply it to events with primary energy 6-16 EeV (E_CM = 110-170 TeV), whose longitudinal development and lateral distribution were simultaneously measured by the Pierre Auger Observatory. The average hadronic shower is 1.33 +- 0.16 (1.61 +- 0.21) times larger than predicted using the leading LHC-tuned models EPOS-LHC (QGSJetII-04), with a corresponding excess of muons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1610.08509v2-abstract-full').style.display = 'none'; document.getElementById('1610.08509v2-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> 31 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 October, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version. Added journal reference and DOI. Added Report Number</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-504-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 117, 192001 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.08567">arXiv:1609.08567</a> <span> [<a href="https://arxiv.org/pdf/1609.08567">pdf</a>, <a href="https://arxiv.org/format/1609.08567">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.physletb.2016.09.039">10.1016/j.physletb.2016.09.039 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Evidence for a mixed mass composition at the `ankle' in the cosmic-ray spectrum </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=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Ambrosio%2C+M">M. Ambrosio</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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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> , et al. (401 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="1609.08567v2-abstract-short" style="display: inline;"> We report a first measurement for ultra-high energy cosmic rays of the correlation between the depth of shower maximum and the signal in the water Cherenkov stations of air-showers registered simultaneously by the fluorescence and the surface detectors of the Pierre Auger Observatory. Such a correlation measurement is a unique feature of a hybrid air-shower observatory with sensitivity to both the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.08567v2-abstract-full').style.display = 'inline'; document.getElementById('1609.08567v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.08567v2-abstract-full" style="display: none;"> We report a first measurement for ultra-high energy cosmic rays of the correlation between the depth of shower maximum and the signal in the water Cherenkov stations of air-showers registered simultaneously by the fluorescence and the surface detectors of the Pierre Auger Observatory. Such a correlation measurement is a unique feature of a hybrid air-shower observatory with sensitivity to both the electromagnetic and muonic components. It allows an accurate determination of the spread of primary masses in the cosmic-ray flux. Up till now, constraints on the spread of primary masses have been dominated by systematic uncertainties. The present correlation measurement is not affected by systematics in the measurement of the depth of shower maximum or the signal in the water Cherenkov stations. The analysis relies on general characteristics of air showers and is thus robust also with respect to uncertainties in hadronic event generators. The observed correlation in the energy range around the `ankle' at $\lg(E/{\rm eV})=18.5-19.0$ differs significantly from expectations for pure primary cosmic-ray compositions. A light composition made up of proton and helium only is equally inconsistent with observations. The data are explained well by a mixed composition including nuclei with mass $A > 4$. Scenarios such as the proton dip model, with almost pure compositions, are thus disfavoured as the sole explanation of the ultrahigh-energy cosmic-ray flux at Earth. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.08567v2-abstract-full').style.display = 'none'; document.getElementById('1609.08567v2-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 November, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version. Added journal reference and DOI. Added Report Number</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-412-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Lett. B762 (2016) 288-295 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1609.04451">arXiv:1609.04451</a> <span> [<a href="https://arxiv.org/pdf/1609.04451">pdf</a>, <a href="https://arxiv.org/ps/1609.04451">ps</a>, <a href="https://arxiv.org/format/1609.04451">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.94.082002">10.1103/PhysRevD.94.082002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for ultrarelativistic magnetic monopoles 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=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=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=Ambrosio%2C+M">M. Ambrosio</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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a> , et al. (389 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="1609.04451v2-abstract-short" style="display: inline;"> We present a search for ultra-relativistic magnetic monopoles with the Pierre Auger Observatory. Such particles, possibly a relic of phase transitions in the early universe, would deposit a large amount of energy along their path through the atmosphere, comparable to that of ultrahigh-energy cosmic rays (UHECRs). The air shower profile of a magnetic monopole can be effectively distinguished by the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.04451v2-abstract-full').style.display = 'inline'; document.getElementById('1609.04451v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1609.04451v2-abstract-full" style="display: none;"> We present a search for ultra-relativistic magnetic monopoles with the Pierre Auger Observatory. Such particles, possibly a relic of phase transitions in the early universe, would deposit a large amount of energy along their path through the atmosphere, comparable to that of ultrahigh-energy cosmic rays (UHECRs). The air shower profile of a magnetic monopole can be effectively distinguished by the fluorescence detector from that of standard UHECRs. No candidate was found in the data collected between 2004 and 2012, with an expected background of less than 0.1 event from UHECRs. The corresponding 90% confidence level (C.L.) upper limits on the flux of ultra-relativistic magnetic monopoles range from $10^{-19}$ (cm$^{2}$ sr s)$^{-1}$ for a Lorentz factor $纬=10^9$ to $2.5 \times10^{-21}$ (cm$^{2}$ sr s)$^{-1}$ for $纬=10^{12}$. These results - the first obtained with a UHECR detector - improve previously published limits by up to an order of magnitude. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1609.04451v2-abstract-full').style.display = 'none'; document.getElementById('1609.04451v2-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, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 September, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version. Corrected title. Added journal reference and DOI. Added Report Number</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-373-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 94, 082002 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1608.07378">arXiv:1608.07378</a> <span> [<a href="https://arxiv.org/pdf/1608.07378">pdf</a>, <a href="https://arxiv.org/format/1608.07378">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.94.122007">10.1103/PhysRevD.94.122007 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ultrahigh-energy neutrino follow-up of Gravitational Wave events GW150914 and GW151226 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=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=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=Ambrosio%2C+M">M. Ambrosio</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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</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=Balaceanu%2C+A">A. Balaceanu</a>, <a href="/search/astro-ph?searchtype=author&query=Luz%2C+R+J+B">R. J. Barreira Luz</a> , et al. (388 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="1608.07378v2-abstract-short" style="display: inline;"> On September 14, 2015 the Advanced LIGO detectors observed their first gravitational-wave (GW) transient GW150914. This was followed by a second GW event observed on December 26, 2015. Both events were inferred to have arisen from the merger of black holes in binary systems. Such a system may emit neutrinos if there are magnetic fields and disk debris remaining from the formation of the two black… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.07378v2-abstract-full').style.display = 'inline'; document.getElementById('1608.07378v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1608.07378v2-abstract-full" style="display: none;"> On September 14, 2015 the Advanced LIGO detectors observed their first gravitational-wave (GW) transient GW150914. This was followed by a second GW event observed on December 26, 2015. Both events were inferred to have arisen from the merger of black holes in binary systems. Such a system may emit neutrinos if there are magnetic fields and disk debris remaining from the formation of the two black holes. With the surface detector array of the Pierre Auger Observatory we can search for neutrinos with energy above 100 PeV from point-like sources across the sky with equatorial declination from about -65 deg. to +60 deg., and in particular from a fraction of the 90% confidence-level (CL) inferred positions in the sky of GW150914 and GW151226. A targeted search for highly-inclined extensive air showers, produced either by interactions of downward-going neutrinos of all flavors in the atmosphere or by the decays of tau leptons originating from tau-neutrino interactions in the Earth's crust (Earth-skimming neutrinos), yielded no candidates in the Auger data collected within $\pm 500$ s around or 1 day after the coordinated universal time (UTC) of GW150914 and GW151226, as well as in the same search periods relative to the UTC time of the GW candidate event LVT151012. From the non-observation we constrain the amount of energy radiated in ultrahigh-energy neutrinos from such remarkable events. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1608.07378v2-abstract-full').style.display = 'none'; document.getElementById('1608.07378v2-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 January, 2017; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 August, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published version. Added journal reference and DOI. Added Report Number</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-337-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 94, 122007 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1605.02564">arXiv:1605.02564</a> <span> [<a href="https://arxiv.org/pdf/1605.02564">pdf</a>, <a href="https://arxiv.org/format/1605.02564">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </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.116.241101">10.1103/PhysRevLett.116.241101 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Measurement of the Radiation Energy in the Radio Signal of Extensive Air Showers as a Universal Estimator of Cosmic-Ray Energy </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">Alexander Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">Pedro Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">Marco Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E">Eun-Joo Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">Imen Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I">Ivone Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">Ingomar Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">Patrick Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">Alejandro Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">Jesus Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">Jaime Alvarez-Mu帽iz</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=Ambrosio%2C+M">Michelangelo Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">Amin Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">Gioacchino Alex Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">Luis Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">Sofia Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">Fernando Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">Nicusor Arsene</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H+G">Hern谩n Gonzalo Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">Pedro Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">Gualberto Avila</a> , et al. (425 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="1605.02564v2-abstract-short" style="display: inline;"> We measure the energy emitted by extensive air showers in the form of radio emission in the frequency range from 30 to 80 MHz. Exploiting the accurate energy scale of the Pierre Auger Observatory, we obtain a radiation energy of 15.8 \pm 0.7 (stat) \pm 6.7 (sys) MeV for cosmic rays with an energy of 1 EeV arriving perpendicularly to a geomagnetic field of 0.24 G, scaling quadratically with the cos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.02564v2-abstract-full').style.display = 'inline'; document.getElementById('1605.02564v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1605.02564v2-abstract-full" style="display: none;"> We measure the energy emitted by extensive air showers in the form of radio emission in the frequency range from 30 to 80 MHz. Exploiting the accurate energy scale of the Pierre Auger Observatory, we obtain a radiation energy of 15.8 \pm 0.7 (stat) \pm 6.7 (sys) MeV for cosmic rays with an energy of 1 EeV arriving perpendicularly to a geomagnetic field of 0.24 G, scaling quadratically with the cosmic-ray energy. A comparison with predictions from state-of-the-art first-principle calculations shows agreement with our measurement. The radiation energy provides direct access to the calorimetric energy in the electromagnetic cascade of extensive air showers. Comparison with our result thus allows the direct calibration of any cosmic-ray radio detector against the well-established energy scale of the Pierre Auger Observatory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1605.02564v2-abstract-full').style.display = 'none'; document.getElementById('1605.02564v2-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 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 May, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Replaced with published version. Added journal reference and DOI. Supplemental material in the ancillary files</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-169-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 116, 241101 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.03637">arXiv:1604.03637</a> <span> [<a href="https://arxiv.org/pdf/1604.03637">pdf</a>, <a href="https://arxiv.org/format/1604.03637">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The Pierre Auger Observatory Upgrade - Preliminary Design Report </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=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">M. Ave</a>, <a href="/search/astro-ph?searchtype=author&query=Avenier%2C+M">M. Avenier</a> , et al. (440 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="1604.03637v1-abstract-short" style="display: inline;"> The Pierre Auger Observatory has begun a major Upgrade of its already impressive capabilities, with an emphasis on improved mass composition determination using the surface detectors of the Observatory. Known as AugerPrime, the upgrade will include new 4 m$^2$ plastic scintillator detectors on top of all 1660 water-Cherenkov detectors, updated and more flexible surface detector electronics, a larg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.03637v1-abstract-full').style.display = 'inline'; document.getElementById('1604.03637v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.03637v1-abstract-full" style="display: none;"> The Pierre Auger Observatory has begun a major Upgrade of its already impressive capabilities, with an emphasis on improved mass composition determination using the surface detectors of the Observatory. Known as AugerPrime, the upgrade will include new 4 m$^2$ plastic scintillator detectors on top of all 1660 water-Cherenkov detectors, updated and more flexible surface detector electronics, a large array of buried muon detectors, and an extended duty cycle for operations of the fluorescence detectors. This Preliminary Design Report was produced by the Collaboration in April 2015 as an internal document and information for funding agencies. It outlines the scientific and technical case for AugerPrime. We now release it to the public via the arXiv server. We invite you to review the large number of fundamental results already achieved by the Observatory and our plans for the future. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.03637v1-abstract-full').style.display = 'none'; document.getElementById('1604.03637v1-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 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">201 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1604.00978">arXiv:1604.00978</a> <span> [<a href="https://arxiv.org/pdf/1604.00978">pdf</a>, <a href="https://arxiv.org/format/1604.00978">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.93.072006">10.1103/PhysRevD.93.072006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Azimuthal asymmetry in the risetime of the surface detector signals 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=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Ambrosio%2C+M">M. Ambrosio</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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Awal%2C+N">N. Awal</a> , et al. (414 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="1604.00978v2-abstract-short" style="display: inline;"> The azimuthal asymmetry in the risetime of signals in Auger surface detector stations is a source of information on shower development. The azimuthal asymmetry is due to a combination of the longitudinal evolution of the shower and geometrical effects related to the angles of incidence of the particles into the detectors. The magnitude of the effect depends upon the zenith angle and state of devel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.00978v2-abstract-full').style.display = 'inline'; document.getElementById('1604.00978v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1604.00978v2-abstract-full" style="display: none;"> The azimuthal asymmetry in the risetime of signals in Auger surface detector stations is a source of information on shower development. The azimuthal asymmetry is due to a combination of the longitudinal evolution of the shower and geometrical effects related to the angles of incidence of the particles into the detectors. The magnitude of the effect depends upon the zenith angle and state of development of the shower and thus provides a novel observable, $(\sec 胃)_\mathrm{max}$, sensitive to the mass composition of cosmic rays above $3 \times 10^{18}$ eV. By comparing measurements with predictions from shower simulations, we find for both of our adopted models of hadronic physics (QGSJETII-04 and EPOS-LHC) an indication that the mean cosmic-ray mass increases slowly with energy, as has been inferred from other studies. However, the mass estimates are dependent on the shower model and on the range of distance from the shower core selected. Thus the method has uncovered further deficiencies in our understanding of shower modelling that must be resolved before the mass composition can be inferred from $(\sec 胃)_\mathrm{max}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1604.00978v2-abstract-full').style.display = 'none'; document.getElementById('1604.00978v2-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 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 April, 2016; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2016. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Replaced with published version. Added journal reference and DOI</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-16-094-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 93, 072006 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.09408">arXiv:1511.09408</a> <span> [<a href="https://arxiv.org/pdf/1511.09408">pdf</a>, <a href="https://arxiv.org/ps/1511.09408">ps</a>, <a href="https://arxiv.org/format/1511.09408">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/10.1088/1475-7516/2016/01/037">10.1088/1475-7516/2016/01/037 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for correlations between the arrival directions of IceCube neutrino events and ultrahigh-energy cosmic rays detected by the Pierre Auger Observatory and the Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+IceCube+Collaboration"> The IceCube Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aartsen%2C+M+G">M. G. Aartsen</a>, <a href="/search/astro-ph?searchtype=author&query=Abraham%2C+K">K. Abraham</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahrens%2C+M">M. Ahrens</a>, <a href="/search/astro-ph?searchtype=author&query=Altmann%2C+D">D. Altmann</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+T">T. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Ansseau%2C+I">I. Ansseau</a>, <a href="/search/astro-ph?searchtype=author&query=Archinger%2C+M">M. Archinger</a>, <a href="/search/astro-ph?searchtype=author&query=Arguelles%2C+C">C. Arguelles</a>, <a href="/search/astro-ph?searchtype=author&query=Arlen%2C+T+C">T. C. Arlen</a>, <a href="/search/astro-ph?searchtype=author&query=Auffenberg%2C+J">J. Auffenberg</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+V">V. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Beiser%2C+E">E. Beiser</a>, <a href="/search/astro-ph?searchtype=author&query=Berghaus%2C+P">P. Berghaus</a>, <a href="/search/astro-ph?searchtype=author&query=Berley%2C+D">D. Berley</a> , et al. (848 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="1511.09408v2-abstract-short" style="display: inline;"> This paper presents the results of different searches for correlations between very high-energy neutrino candidates detected by IceCube and the highest-energy cosmic rays measured by the Pierre Auger Observatory and the Telescope Array. We first consider samples of cascade neutrino events and of high-energy neutrino-induced muon tracks, which provided evidence for a neutrino flux of astrophysical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.09408v2-abstract-full').style.display = 'inline'; document.getElementById('1511.09408v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.09408v2-abstract-full" style="display: none;"> This paper presents the results of different searches for correlations between very high-energy neutrino candidates detected by IceCube and the highest-energy cosmic rays measured by the Pierre Auger Observatory and the Telescope Array. We first consider samples of cascade neutrino events and of high-energy neutrino-induced muon tracks, which provided evidence for a neutrino flux of astrophysical origin, and study their cross-correlation with the ultrahigh-energy cosmic ray (UHECR) samples as a function of angular separation. We also study their possible directional correlations using a likelihood method stacking the neutrino arrival directions and adopting different assumptions on the size of the UHECR magnetic deflections. Finally, we perform another likelihood analysis stacking the UHECR directions and using a sample of through-going muon tracks optimized for neutrino point-source searches with sub-degree angular resolution. No indications of correlations at discovery level are obtained for any of the searches performed. The smallest of the p-values comes from the search for correlation between UHECRs with IceCube high-energy cascades, a result that should continue to be monitored. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.09408v2-abstract-full').style.display = 'none'; document.getElementById('1511.09408v2-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 January, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Replaced with published version. Added journal reference and DOI</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-15-520-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP01(2016)037 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.02109">arXiv:1511.02109</a> <span> [<a href="https://arxiv.org/pdf/1511.02109">pdf</a>, <a href="https://arxiv.org/format/1511.02109">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> The IceCube Neutrino Observatory, the Pierre Auger Observatory and the Telescope Array: Joint Contribution to the 34th International Cosmic Ray Conference (ICRC 2015) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=IceCube+Collaboration"> IceCube Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Aartsen%2C+M+G">M. G. Aartsen</a>, <a href="/search/astro-ph?searchtype=author&query=Abraham%2C+K">K. Abraham</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahrens%2C+M">M. Ahrens</a>, <a href="/search/astro-ph?searchtype=author&query=Altmann%2C+D">D. Altmann</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+T">T. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Ansseau%2C+I">I. Ansseau</a>, <a href="/search/astro-ph?searchtype=author&query=Archinger%2C+M">M. Archinger</a>, <a href="/search/astro-ph?searchtype=author&query=Arguelles%2C+C">C. Arguelles</a>, <a href="/search/astro-ph?searchtype=author&query=Arlen%2C+T+C">T. C. Arlen</a>, <a href="/search/astro-ph?searchtype=author&query=Auffenberg%2C+J">J. Auffenberg</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Baum%2C+V">V. Baum</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Beiser%2C+E">E. Beiser</a>, <a href="/search/astro-ph?searchtype=author&query=BenZvi%2C+S">S. BenZvi</a>, <a href="/search/astro-ph?searchtype=author&query=Berghaus%2C+P">P. Berghaus</a> , et al. (869 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="1511.02109v1-abstract-short" style="display: inline;"> We have conducted three searches for correlations between ultra-high energy cosmic rays detected by the Telescope Array and the Pierre Auger Observatory, and high-energy neutrino candidate events from IceCube. Two cross-correlation analyses with UHECRs are done: one with 39 cascades from the IceCube `high-energy starting events' sample and the other with 16 high-energy `track events'. The angular… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.02109v1-abstract-full').style.display = 'inline'; document.getElementById('1511.02109v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.02109v1-abstract-full" style="display: none;"> We have conducted three searches for correlations between ultra-high energy cosmic rays detected by the Telescope Array and the Pierre Auger Observatory, and high-energy neutrino candidate events from IceCube. Two cross-correlation analyses with UHECRs are done: one with 39 cascades from the IceCube `high-energy starting events' sample and the other with 16 high-energy `track events'. The angular separation between the arrival directions of neutrinos and UHECRs is scanned over. The same events are also used in a separate search using a maximum likelihood approach, after the neutrino arrival directions are stacked. To estimate the significance we assume UHECR magnetic deflections to be inversely proportional to their energy, with values $3^\circ$, $6^\circ$ and $9^\circ$ at 100 EeV to allow for the uncertainties on the magnetic field strength and UHECR charge. A similar analysis is performed on stacked UHECR arrival directions and the IceCube sample of through-going muon track events which were optimized for neutrino point-source searches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.02109v1-abstract-full').style.display = 'none'; document.getElementById('1511.02109v1-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">one proceeding, the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands; will appear in PoS(ICRC2015)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1511.02103">arXiv:1511.02103</a> <span> [<a href="https://arxiv.org/pdf/1511.02103">pdf</a>, <a href="https://arxiv.org/format/1511.02103">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"> Pierre Auger Observatory and Telescope Array: Joint Contributions to the 34th International Cosmic Ray Conference (ICRC 2015) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Telescope+Array+Collaboration"> Telescope Array Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R+U">R. U. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+M">M. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Abu-Zayyad%2C+T">T. Abu-Zayyad</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+M">M. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Azuma%2C+R">R. Azuma</a>, <a href="/search/astro-ph?searchtype=author&query=Barcikowski%2C+E">E. Barcikowski</a>, <a href="/search/astro-ph?searchtype=author&query=Belz%2C+J+W">J. W. Belz</a>, <a href="/search/astro-ph?searchtype=author&query=Bergman%2C+D+R">D. R. Bergman</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+S+A">S. A. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Cady%2C+R">R. Cady</a>, <a href="/search/astro-ph?searchtype=author&query=Chae%2C+M+J">M. J. Chae</a>, <a href="/search/astro-ph?searchtype=author&query=Cheon%2C+B+G">B. G. Cheon</a>, <a href="/search/astro-ph?searchtype=author&query=Chiba%2C+J">J. Chiba</a>, <a href="/search/astro-ph?searchtype=author&query=Chikawa%2C+M">M. Chikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Cho%2C+W+R">W. R. Cho</a>, <a href="/search/astro-ph?searchtype=author&query=Fujii%2C+T">T. Fujii</a>, <a href="/search/astro-ph?searchtype=author&query=Fukushima%2C+M">M. Fukushima</a>, <a href="/search/astro-ph?searchtype=author&query=Goto%2C+T">T. Goto</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+W">W. Hanlon</a>, <a href="/search/astro-ph?searchtype=author&query=Hayashi%2C+Y">Y. Hayashi</a>, <a href="/search/astro-ph?searchtype=author&query=Hayashida%2C+N">N. Hayashida</a>, <a href="/search/astro-ph?searchtype=author&query=Hibino%2C+K">K. Hibino</a>, <a href="/search/astro-ph?searchtype=author&query=Honda%2C+K">K. Honda</a>, <a href="/search/astro-ph?searchtype=author&query=Ikeda%2C+D">D. Ikeda</a> , et al. (553 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="1511.02103v1-abstract-short" style="display: inline;"> Joint contributions of the Pierre Auger Collaboration and the Telescope Array Collaboration to the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1511.02103v1-abstract-full" style="display: none;"> Joint contributions of the Pierre Auger Collaboration and the Telescope Array Collaboration to the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1511.02103v1-abstract-full').style.display = 'none'; document.getElementById('1511.02103v1-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">3 proceedings, the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands; will appear in PoS(ICRC2015)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1509.03732">arXiv:1509.03732</a> <span> [<a href="https://arxiv.org/pdf/1509.03732">pdf</a>, <a href="https://arxiv.org/format/1509.03732">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: Contributions to the 34th International Cosmic Ray Conference (ICRC 2015) </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=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</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=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=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</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=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=Arqueros%2C+F">F. Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">N. Arsene</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=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">G. Avila</a> , et al. (427 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="1509.03732v1-abstract-short" style="display: inline;"> Contributions of the Pierre Auger Collaboration to the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands </span> <span class="abstract-full has-text-grey-dark mathjax" id="1509.03732v1-abstract-full" style="display: none;"> Contributions of the Pierre Auger Collaboration to the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1509.03732v1-abstract-full').style.display = 'none'; document.getElementById('1509.03732v1-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 September, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 proceedings, the 34th International Cosmic Ray Conference, 30 July - 6 August 2015, The Hague, The Netherlands; will appear in PoS(ICRC2015)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1508.04267">arXiv:1508.04267</a> <span> [<a href="https://arxiv.org/pdf/1508.04267">pdf</a>, <a href="https://arxiv.org/format/1508.04267">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/10.1103/PhysRevD.93.122005">10.1103/PhysRevD.93.122005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Energy Estimation of Cosmic Rays with the Engineering Radio Array 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">Alexander Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">Pedro Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">Marco Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E">Eun-Joo Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">Imen Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I">Ivone Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">Ingomar Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">Patrick Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">Alejandro Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">Jesus Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">Jaime Alvarez-Mu帽iz</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=Ambrosio%2C+M">Michelangelo Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">Amin Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anastasi%2C+G+A">Gioacchino Alex Anastasi</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">Luis Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">Sofia Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">Fernando Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">Nicusor Arsene</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H+G">Hern谩n Gonzalo Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">Pedro Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+G">Gualberto Avila</a> , et al. (426 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="1508.04267v2-abstract-short" style="display: inline;"> The Auger Engineering Radio Array (AERA) is part of the Pierre Auger Observatory and is used to detect the radio emission of cosmic-ray air showers. These observations are compared to the data of the surface detector stations of the Observatory, which provide well-calibrated information on the cosmic-ray energies and arrival directions. The response of the radio stations in the 30 to 80 MHz regime… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.04267v2-abstract-full').style.display = 'inline'; document.getElementById('1508.04267v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1508.04267v2-abstract-full" style="display: none;"> The Auger Engineering Radio Array (AERA) is part of the Pierre Auger Observatory and is used to detect the radio emission of cosmic-ray air showers. These observations are compared to the data of the surface detector stations of the Observatory, which provide well-calibrated information on the cosmic-ray energies and arrival directions. The response of the radio stations in the 30 to 80 MHz regime has been thoroughly calibrated to enable the reconstruction of the incoming electric field. For the latter, the energy deposit per area is determined from the radio pulses at each observer position and is interpolated using a two-dimensional function that takes into account signal asymmetries due to interference between the geomagnetic and charge-excess emission components. The spatial integral over the signal distribution gives a direct measurement of the energy transferred from the primary cosmic ray into radio emission in the AERA frequency range. We measure 15.8 MeV of radiation energy for a 1 EeV air shower arriving perpendicularly to the geomagnetic field. This radiation energy -- corrected for geometrical effects -- is used as a cosmic-ray energy estimator. Performing an absolute energy calibration against the surface-detector information, we observe that this radio-energy estimator scales quadratically with the cosmic-ray energy as expected for coherent emission. We find an energy resolution of the radio reconstruction of 22% for the data set and 17% for a high-quality subset containing only events with at least five radio stations with signal. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1508.04267v2-abstract-full').style.display = 'none'; document.getElementById('1508.04267v2-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 June, 2016; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 August, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Replaced with published version. Added journal reference and DOI</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-15-354-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 93, 122005 (2016) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1504.05397">arXiv:1504.05397</a> <span> [<a href="https://arxiv.org/pdf/1504.05397">pdf</a>, <a href="https://arxiv.org/format/1504.05397">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.91.092008">10.1103/PhysRevD.91.092008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An improved limit to the diffuse flux of ultra-high energy neutrinos 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=Aab%2C+A">Alexander Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">Pedro Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">Marco Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E">Eun-Joo Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">Imen Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I">Ivone Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">Ingomar Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">Patrick Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">Alejandro Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">Jesus Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">Jaime Alvarez-Mu帽iz</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=Ambrosio%2C+M">Michelangelo Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">Amin Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">Luis Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">Sofia Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Aranda%2C+V+M">Victor Manuel Aranda</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">Fernando Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">Nicusor Arsene</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H+G">Hern谩n Gonzalo Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">Pedro Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">Maximo Ave</a> , et al. (440 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="1504.05397v2-abstract-short" style="display: inline;"> Neutrinos in the cosmic ray flux with energies near 1 EeV and above are detectable with the Surface Detector array of the Pierre Auger Observatory. We report here on searches through Auger data from 1 January 2004 until 20 June 2013. No neutrino candidates were found, yielding a limit to the diffuse flux of ultra-high energy neutrinos that challenges the Waxman-Bahcall bound predictions. Neutrino… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.05397v2-abstract-full').style.display = 'inline'; document.getElementById('1504.05397v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1504.05397v2-abstract-full" style="display: none;"> Neutrinos in the cosmic ray flux with energies near 1 EeV and above are detectable with the Surface Detector array of the Pierre Auger Observatory. We report here on searches through Auger data from 1 January 2004 until 20 June 2013. No neutrino candidates were found, yielding a limit to the diffuse flux of ultra-high energy neutrinos that challenges the Waxman-Bahcall bound predictions. Neutrino identification is attempted using the broad time-structure of the signals expected in the SD stations, and is efficiently done for neutrinos of all flavors interacting in the atmosphere at large zenith angles, as well as for "Earth-skimming" neutrino interactions in the case of tau neutrinos. In this paper the searches for downward-going neutrinos in the zenith angle bins $60^\circ-75^\circ$ and $75^\circ-90^\circ$ as well as for upward-going neutrinos, are combined to give a single limit. The $90\%$ C.L. single-flavor limit to the diffuse flux of ultra-high energy neutrinos with an $E^{-2}$ spectrum in the energy range $1.0 \times 10^{17}$ eV - $2.5 \times 10^{19}$ eV is $E_谓^2 dN_谓/dE_谓< 6.4 \times 10^{-9}~ {\rm GeV~ cm^{-2}~ s^{-1}~ sr^{-1}}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1504.05397v2-abstract-full').style.display = 'none'; document.getElementById('1504.05397v2-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 April, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Replaced with published version. Added journal reference and DOI</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-15-150-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 91, 092008 (2015) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1503.07786">arXiv:1503.07786</a> <span> [<a href="https://arxiv.org/pdf/1503.07786">pdf</a>, <a href="https://arxiv.org/format/1503.07786">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2015/08/049">10.1088/1475-7516/2015/08/049 <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 spectrum above $4{\times}10^{18}$ eV using inclined events detected 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=Aab%2C+A">Alexander Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">Pedro Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">Marco Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E">Eun-Joo Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">Imen Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I">Ivone Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">Ingomar Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">Patrick Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">Alejandro Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">Jesus Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">Jaime Alvarez-Mu帽iz</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=Ambrosio%2C+M">Michelangelo Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">Amin Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">Luis Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">Sofia Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Aranda%2C+V+M">Victor Manuel Aranda</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">Fernando Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Arsene%2C+N">Nicusor Arsene</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H+G">Hern谩n Gonzalo Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">Pedro Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">Maximo Ave</a> , et al. (439 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="1503.07786v2-abstract-short" style="display: inline;"> A measurement of the cosmic-ray spectrum for energies exceeding $4{\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\times}10^{18}$ eV, the "ankle", the fl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.07786v2-abstract-full').style.display = 'inline'; document.getElementById('1503.07786v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1503.07786v2-abstract-full" style="display: none;"> A measurement of the cosmic-ray spectrum for energies exceeding $4{\times}10^{18}$ eV is presented, which is based on the analysis of showers with zenith angles greater than $60^{\circ}$ detected with the Pierre Auger Observatory between 1 January 2004 and 31 December 2013. The measured spectrum confirms a flux suppression at the highest energies. Above $5.3{\times}10^{18}$ eV, the "ankle", the flux can be described by a power law $E^{-纬}$ with index $纬=2.70 \pm 0.02 \,\text{(stat)} \pm 0.1\,\text{(sys)}$ followed by a smooth suppression region. For the energy ($E_\text{s}$) at which the spectral flux has fallen to one-half of its extrapolated value in the absence of suppression, we find $E_\text{s}=(5.12\pm0.25\,\text{(stat)}^{+1.0}_{-1.2}\,\text{(sys)}){\times}10^{19}$ eV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1503.07786v2-abstract-full').style.display = 'none'; document.getElementById('1503.07786v2-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 November, 2015; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 March, 2015; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2015. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Replaced with published version. Added journal reference and DOI</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-15-099-AD-AE-CD-TD </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 08 (2015) 049 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1409.3128">arXiv:1409.3128</a> <span> [<a href="https://arxiv.org/pdf/1409.3128">pdf</a>, <a href="https://arxiv.org/ps/1409.3128">ps</a>, <a href="https://arxiv.org/format/1409.3128">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/10.1088/0004-637X/794/2/172">10.1088/0004-637X/794/2/172 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Searches for Large-Scale Anisotropy in the Arrival Directions of Cosmic Rays Detected above Energy of $10^{19}$ eV at the Pierre Auger Observatory and the Telescope Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Auger%2C+T+P">The Pierre Auger</a>, <a href="/search/astro-ph?searchtype=author&query=Collaborations%2C+T+A">Telescope Array Collaborations</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</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=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</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=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</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=Arqueros%2C+F">F. Arqueros</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=Aublin%2C+J">J. Aublin</a> , et al. (584 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="1409.3128v1-abstract-short" style="display: inline;"> Spherical harmonic moments are well-suited for capturing anisotropy at any scale in the flux of cosmic rays. An unambiguous measurement of the full set of spherical harmonic coefficients requires full-sky coverage. This can be achieved by combining data from observatories located in both the northern and southern hemispheres. To this end, a joint analysis using data recorded at the Telescope Array… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.3128v1-abstract-full').style.display = 'inline'; document.getElementById('1409.3128v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1409.3128v1-abstract-full" style="display: none;"> Spherical harmonic moments are well-suited for capturing anisotropy at any scale in the flux of cosmic rays. An unambiguous measurement of the full set of spherical harmonic coefficients requires full-sky coverage. This can be achieved by combining data from observatories located in both the northern and southern hemispheres. To this end, a joint analysis using data recorded at the Telescope Array and the Pierre Auger Observatory above $10^{19}$ eV is presented in this work. The resulting multipolar expansion of the flux of cosmic rays allows us to perform a series of anisotropy searches, and in particular to report on the angular power spectrum of cosmic rays above $10^{19}$ eV. No significant deviation from isotropic expectations is found throughout the analyses performed. Upper limits on the amplitudes of the dipole and quadrupole moments are derived as a function of the direction in the sky, varying between 7% and 13% for the dipole and between 7% and 10% for a symmetric quadrupole. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1409.3128v1-abstract-full').style.display = 'none'; document.getElementById('1409.3128v1-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, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 13 figures, to appear in The Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 794, 172 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1407.3214">arXiv:1407.3214</a> <span> [<a href="https://arxiv.org/pdf/1407.3214">pdf</a>, <a href="https://arxiv.org/ps/1407.3214">ps</a>, <a href="https://arxiv.org/format/1407.3214">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2014/08/019">10.1088/1475-7516/2014/08/019 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Reconstruction of inclined air showers detected 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=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=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</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=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</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=Arqueros%2C+F">F. Arqueros</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=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">M. Ave</a> , et al. (463 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="1407.3214v1-abstract-short" style="display: inline;"> We describe the method devised to reconstruct inclined cosmic-ray air showers with zenith angles greater than $60^\circ$ detected with the surface array of the Pierre Auger Observatory. The measured signals at the ground level are fitted to muon density distributions predicted with atmospheric cascade models to obtain the relative shower size as an overall normalization parameter. The method is ev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.3214v1-abstract-full').style.display = 'inline'; document.getElementById('1407.3214v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1407.3214v1-abstract-full" style="display: none;"> We describe the method devised to reconstruct inclined cosmic-ray air showers with zenith angles greater than $60^\circ$ detected with the surface array of the Pierre Auger Observatory. The measured signals at the ground level are fitted to muon density distributions predicted with atmospheric cascade models to obtain the relative shower size as an overall normalization parameter. The method is evaluated using simulated showers to test its performance. The energy of the cosmic rays is calibrated using a sub-sample of events reconstructed with both the fluorescence and surface array techniques. The reconstruction method described here provides the basis of complementary analyses including an independent measurement of the energy spectrum of ultra-high energy cosmic rays using very inclined events collected by the Pierre Auger Observatory. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1407.3214v1-abstract-full').style.display = 'none'; document.getElementById('1407.3214v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 July, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27 pages, 19 figures, accepted for publication in Journal of Cosmology and Astroparticle Physics (JCAP)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.4038">arXiv:1406.4038</a> <span> [<a href="https://arxiv.org/pdf/1406.4038">pdf</a>, <a href="https://arxiv.org/ps/1406.4038">ps</a>, <a href="https://arxiv.org/format/1406.4038">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/10.1088/2041-8205/789/2/L34">10.1088/2041-8205/789/2/L34 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Targeted Search for Point Sources of EeV Neutrons </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=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</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=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</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=Arqueros%2C+F">F. Arqueros</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=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">M. Ave</a> , et al. (460 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="1406.4038v1-abstract-short" style="display: inline;"> A flux of neutrons from an astrophysical source in the Galaxy can be detected in the Pierre Auger Observatory as an excess of cosmic-ray air showers arriving from the direction of the source. To avoid the statistical penalty for making many trials, classes of objects are tested in combinations as nine "target sets", in addition to the search for a neutron flux from the Galactic Center or from the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.4038v1-abstract-full').style.display = 'inline'; document.getElementById('1406.4038v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.4038v1-abstract-full" style="display: none;"> A flux of neutrons from an astrophysical source in the Galaxy can be detected in the Pierre Auger Observatory as an excess of cosmic-ray air showers arriving from the direction of the source. To avoid the statistical penalty for making many trials, classes of objects are tested in combinations as nine "target sets", in addition to the search for a neutron flux from the Galactic Center or from the Galactic Plane. Within a target set, each candidate source is weighted in proportion to its electromagnetic flux, its exposure to the Auger Observatory, and its flux attenuation factor due to neutron decay. These searches do not find evidence for a neutron flux from any class of candidate sources. Tabulated results give the combined p-value for each class, with and without the weights, and also the flux upper limit for the most significant candidate source within each class. These limits on fluxes of neutrons significantly constrain models of EeV proton emission from non-transient discrete sources in the Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.4038v1-abstract-full').style.display = 'none'; document.getElementById('1406.4038v1-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 June, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, accepted for publication in The Astrophysical Journal Letters</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 789 (2014) L34 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1406.2912">arXiv:1406.2912</a> <span> [<a href="https://arxiv.org/pdf/1406.2912">pdf</a>, <a href="https://arxiv.org/ps/1406.2912">ps</a>, <a href="https://arxiv.org/format/1406.2912">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/10.1088/0004-637X/789/2/160">10.1088/0004-637X/789/2/160 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for point sources of EeV photons </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pierre+Auger+Collaboration"> 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=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Samarai%2C+I+A">I. Al Samarai</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</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=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</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=Arqueros%2C+F">F. Arqueros</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=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">M. Ave</a> , et al. (461 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="1406.2912v1-abstract-short" style="display: inline;"> Measurements of air showers made using the hybrid technique developed with the fluorescence and surface detectors of the Pierre Auger Observatory allow a sensitive search for point sources of EeV photons anywhere in the exposed sky. A multivariate analysis reduces the background of hadronic cosmic rays. The search is sensitive to a declination band from -85掳 to +20掳, in an energy range from 10^17.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.2912v1-abstract-full').style.display = 'inline'; document.getElementById('1406.2912v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1406.2912v1-abstract-full" style="display: none;"> Measurements of air showers made using the hybrid technique developed with the fluorescence and surface detectors of the Pierre Auger Observatory allow a sensitive search for point sources of EeV photons anywhere in the exposed sky. A multivariate analysis reduces the background of hadronic cosmic rays. The search is sensitive to a declination band from -85掳 to +20掳, in an energy range from 10^17.3 eV to 10^18.5 eV. No photon point source has been detected. An upper limit on the photon flux has been derived for every direction. The mean value of the energy flux limit that results from this, assuming a photon spectral index of -2, is 0.06 eV cm^-2 s^-1, and no celestial direction exceeds 0.25 eV cm^-2 s^-1. These upper limits constrain scenarios in which EeV cosmic ray protons are emitted by non-transient sources in the Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1406.2912v1-abstract-full').style.display = 'none'; document.getElementById('1406.2912v1-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, 2014; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2014. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 pages, 10 figures, accepted for publication in The Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ, 789, 160 (2014) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1310.4620">arXiv:1310.4620</a> <span> [<a href="https://arxiv.org/pdf/1310.4620">pdf</a>, <a href="https://arxiv.org/format/1310.4620">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/10.1007/s13538-014-0218-6">10.1007/s13538-014-0218-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Highlights from the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Letessier-Selvon%2C+A">Antoine Letessier-Selvon</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=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</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-Muniz%2C+J">J. Alvarez-Muniz</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=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Antivcic%2C+T">T. Antivcic</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</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=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">M. Ave</a> , et al. (472 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="1310.4620v2-abstract-short" style="display: inline;"> The Pierre Auger Observatory is the world's largest cosmic ray observatory. Our current exposure reaches nearly 40,000 km$^2$ str and provides us with an unprecedented quality data set. The performance and stability of the detectors and their enhancements are described. Data analyses have led to a number of major breakthroughs. Among these we discuss the energy spectrum and the searches for large-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.4620v2-abstract-full').style.display = 'inline'; document.getElementById('1310.4620v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1310.4620v2-abstract-full" style="display: none;"> The Pierre Auger Observatory is the world's largest cosmic ray observatory. Our current exposure reaches nearly 40,000 km$^2$ str and provides us with an unprecedented quality data set. The performance and stability of the detectors and their enhancements are described. Data analyses have led to a number of major breakthroughs. Among these we discuss the energy spectrum and the searches for large-scale anisotropies. We present analyses of our X$_{max}$ data and show how it can be interpreted in terms of mass composition. We also describe some new analyses that extract mass sensitive parameters from the 100% duty cycle SD data. A coherent interpretation of all these recent results opens new directions. The consequences regarding the cosmic ray composition and the properties of UHECR sources are briefly discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.4620v2-abstract-full').style.display = 'none'; document.getElementById('1310.4620v2-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 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 12 figures, talk given at the 33rd International Cosmic Ray Conference, Rio de Janeiro 2013</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> ICRC2013 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1310.0647">arXiv:1310.0647</a> <span> [<a href="https://arxiv.org/pdf/1310.0647">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Pierre Auger Observatory and Telescope Array: Joint Contributions to the 33rd International Cosmic Ray Conference (ICRC 2013) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Array%2C+T+T">The Telescope Array</a>, <a href="/search/astro-ph?searchtype=author&query=Collaborations%2C+P+A">Pierre Auger Collaborations</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abu-Zayyad%2C+T">T. Abu-Zayyad</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+M">M. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+R">R. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Azuma%2C+R">R. Azuma</a>, <a href="/search/astro-ph?searchtype=author&query=Barcikowski%2C+E">E. Barcikowski</a>, <a href="/search/astro-ph?searchtype=author&query=Belz%2C+J+W">J. W Belz</a>, <a href="/search/astro-ph?searchtype=author&query=Bergman%2C+D+R">D. R. Bergman</a>, <a href="/search/astro-ph?searchtype=author&query=Blake%2C+S+A">S. A. Blake</a>, <a href="/search/astro-ph?searchtype=author&query=Cady%2C+R">R. Cady</a>, <a href="/search/astro-ph?searchtype=author&query=Chae%2C+M+J">M. J. Chae</a>, <a href="/search/astro-ph?searchtype=author&query=Cheon%2C+B+G">B. G. Cheon</a>, <a href="/search/astro-ph?searchtype=author&query=Chiba%2C+J">J. Chiba</a>, <a href="/search/astro-ph?searchtype=author&query=Chikawa%2C+M">M. Chikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Cho%2C+W+R">W. R. Cho</a>, <a href="/search/astro-ph?searchtype=author&query=Fujii%2C+T">T. Fujii</a>, <a href="/search/astro-ph?searchtype=author&query=Fukushima%2C+M">M. Fukushima</a>, <a href="/search/astro-ph?searchtype=author&query=Goto%2C+K">K. Goto</a>, <a href="/search/astro-ph?searchtype=author&query=Hanlon%2C+W">W. Hanlon</a>, <a href="/search/astro-ph?searchtype=author&query=Hayashi%2C+Y">Y. Hayashi</a>, <a href="/search/astro-ph?searchtype=author&query=Hayashida%2C+N">N. Hayashida</a>, <a href="/search/astro-ph?searchtype=author&query=Hibino%2C+K">K. Hibino</a>, <a href="/search/astro-ph?searchtype=author&query=Honda%2C+K">K. Honda</a> , et al. (598 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="1310.0647v1-abstract-short" style="display: inline;"> Joint contributions of the Pierre Auger and Telescope Array Collaborations to the 33rd International Cosmic Ray Conference, Rio de Janeiro, Brazil, July 2013: cross-calibration of the fluorescence telescopes, large scale anisotropies and mass composition. </span> <span class="abstract-full has-text-grey-dark mathjax" id="1310.0647v1-abstract-full" style="display: none;"> Joint contributions of the Pierre Auger and Telescope Array Collaborations to the 33rd International Cosmic Ray Conference, Rio de Janeiro, Brazil, July 2013: cross-calibration of the fluorescence telescopes, large scale anisotropies and mass composition. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1310.0647v1-abstract-full').style.display = 'none'; document.getElementById('1310.0647v1-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 October, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Joint contributions of the Pierre Auger and Telescope Array Collaborations to the 33rd International Cosmic Ray Conference, Rio de Janeiro, Brazil, July 2013</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1307.5059">arXiv:1307.5059</a> <span> [<a href="https://arxiv.org/pdf/1307.5059">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> <p class="title is-5 mathjax"> The Pierre Auger Observatory: Contributions to the 33rd International Cosmic Ray Conference (ICRC 2013) </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">Alexander Aab</a>, <a href="/search/astro-ph?searchtype=author&query=Abreu%2C+P">Pedro Abreu</a>, <a href="/search/astro-ph?searchtype=author&query=Aglietta%2C+M">Marco Aglietta</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">Markus Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E">Eun-Joo Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I">Ivone Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">Ingomar Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">Jeff Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">Patrick Allison</a>, <a href="/search/astro-ph?searchtype=author&query=Almela%2C+A">Alejandro Almela</a>, <a href="/search/astro-ph?searchtype=author&query=Castillo%2C+J+A">Jesus Alvarez Castillo</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Mu%C3%B1iz%2C+J">Jaime Alvarez-Mu帽iz</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=Ambrosio%2C+M">Michelangelo Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">Amin Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">Luis Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">Sofia Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">Tome Anti膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">Carla Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">Fernando Arqueros</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+H+G">Hern谩n Gonzalo Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Assis%2C+P">Pedro Assis</a>, <a href="/search/astro-ph?searchtype=author&query=Aublin%2C+J">Julien Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">Maximo Ave</a> , et al. (473 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1307.5059v1-abstract-short" style="display: inline;"> Contributions of the Pierre Auger Collaboration to the 33rd International Cosmic Ray Conference, Rio de Janeiro, Brazil, July 2013 </span> <span class="abstract-full has-text-grey-dark mathjax" id="1307.5059v1-abstract-full" style="display: none;"> Contributions of the Pierre Auger Collaboration to the 33rd International Cosmic Ray Conference, Rio de Janeiro, Brazil, July 2013 <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1307.5059v1-abstract-full').style.display = 'none'; document.getElementById('1307.5059v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 July, 2013; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2013. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contributions to the 33rd International Cosmic Ray Conference, Rio de Janeiro, Brazil, July 2013</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1209.3840">arXiv:1209.3840</a> <span> [<a href="https://arxiv.org/pdf/1209.3840">pdf</a>, <a href="https://arxiv.org/format/1209.3840">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/7/10/P10011">10.1088/1748-0221/7/10/P10011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Antennas for the Detection of Radio Emission Pulses from Cosmic-Ray induced Air Showers at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/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=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</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=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</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=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">M. Ave</a> , et al. (490 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1209.3840v1-abstract-short" style="display: inline;"> The Pierre Auger Observatory is exploring the potential of the radio detection technique to study extensive air showers induced by ultra-high energy cosmic rays. The Auger Engineering Radio Array (AERA) addresses both technological and scientific aspects of the radio technique. A first phase of AERA has been operating since September 2010 with detector stations observing radio signals at frequenci… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.3840v1-abstract-full').style.display = 'inline'; document.getElementById('1209.3840v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1209.3840v1-abstract-full" style="display: none;"> The Pierre Auger Observatory is exploring the potential of the radio detection technique to study extensive air showers induced by ultra-high energy cosmic rays. The Auger Engineering Radio Array (AERA) addresses both technological and scientific aspects of the radio technique. A first phase of AERA has been operating since September 2010 with detector stations observing radio signals at frequencies between 30 and 80 MHz. In this paper we present comparative studies to identify and optimize the antenna design for the final configuration of AERA consisting of 160 individual radio detector stations. The transient nature of the air shower signal requires a detailed description of the antenna sensor. As the ultra-wideband reception of pulses is not widely discussed in antenna literature, we review the relevant antenna characteristics and enhance theoretical considerations towards the impulse response of antennas including polarization effects and multiple signal reflections. On the basis of the vector effective length we study the transient response characteristics of three candidate antennas in the time domain. Observing the variation of the continuous galactic background intensity we rank the antennas with respect to the noise level added to the galactic signal. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1209.3840v1-abstract-full').style.display = 'none'; document.getElementById('1209.3840v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 September, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in JINST, 50 pages, 25 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 7 (2012) P10011 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1208.1675">arXiv:1208.1675</a> <span> [<a href="https://arxiv.org/pdf/1208.1675">pdf</a>, <a href="https://arxiv.org/format/1208.1675">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1748-0221/7/09/P09001">10.1088/1748-0221/7/09/P09001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Rapid Atmospheric Monitoring System of the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/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=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</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=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Anti%C4%8Di%C4%87%2C+T">T. Anti膷i膰</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</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=Aublin%2C+J">J. Aublin</a> , et al. (486 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1208.1675v1-abstract-short" style="display: inline;"> The Pierre Auger Observatory is a facility built to detect air showers produced by cosmic rays above 10^17 eV. During clear nights with a low illuminated moon fraction, the UV fluorescence light produced by air showers is recorded by optical telescopes at the Observatory. To correct the observations for variations in atmospheric conditions, atmospheric monitoring is performed at regular intervals… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.1675v1-abstract-full').style.display = 'inline'; document.getElementById('1208.1675v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1208.1675v1-abstract-full" style="display: none;"> The Pierre Auger Observatory is a facility built to detect air showers produced by cosmic rays above 10^17 eV. During clear nights with a low illuminated moon fraction, the UV fluorescence light produced by air showers is recorded by optical telescopes at the Observatory. To correct the observations for variations in atmospheric conditions, atmospheric monitoring is performed at regular intervals ranging from several minutes (for cloud identification) to several hours (for aerosol conditions) to several days (for vertical profiles of temperature, pressure, and humidity). In 2009, the monitoring program was upgraded to allow for additional targeted measurements of atmospheric conditions shortly after the detection of air showers of special interest, e.g., showers produced by very high-energy cosmic rays or showers with atypical longitudinal profiles. The former events are of particular importance for the determination of the energy scale of the Observatory, and the latter are characteristic of unusual air shower physics or exotic primary particle types. The purpose of targeted (or "rapid") monitoring is to improve the resolution of the atmospheric measurements for such events. In this paper, we report on the implementation of the rapid monitoring program and its current status. The rapid monitoring data have been analyzed and applied to the reconstruction of air showers of high interest, and indicate that the air fluorescence measurements affected by clouds and aerosols are effectively corrected using measurements from the regular atmospheric monitoring program. We find that the rapid monitoring program has potential for supporting dedicated physics analyses beyond the standard event reconstruction. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1208.1675v1-abstract-full').style.display = 'none'; document.getElementById('1208.1675v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 August, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JINST 7 (2012) P09001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1202.1493">arXiv:1202.1493</a> <span> [<a href="https://arxiv.org/pdf/1202.1493">pdf</a>, <a href="https://arxiv.org/ps/1202.1493">ps</a>, <a href="https://arxiv.org/format/1202.1493">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.84.122005">10.1103/PhysRevD.84.122005 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.85.029902">10.1103/PhysRevD.85.029902 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A search for ultra-high energy neutrinos in highly inclined events at the Pierre Auger Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/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=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahn%2C+E+J">E. J. Ahn</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+F+M">I. F. M. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/astro-ph?searchtype=author&query=Allekotte%2C+I">I. Allekotte</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+J">J. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Allison%2C+P">P. Allison</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=Ambrosio%2C+M">M. Ambrosio</a>, <a href="/search/astro-ph?searchtype=author&query=Aminaei%2C+A">A. Aminaei</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Andringa%2C+S">S. Andringa</a>, <a href="/search/astro-ph?searchtype=author&query=Anticic%2C+T">T. Anticic</a>, <a href="/search/astro-ph?searchtype=author&query=Aramo%2C+C">C. Aramo</a>, <a href="/search/astro-ph?searchtype=author&query=Arganda%2C+E">E. Arganda</a>, <a href="/search/astro-ph?searchtype=author&query=Arqueros%2C+F">F. Arqueros</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=Aublin%2C+J">J. Aublin</a>, <a href="/search/astro-ph?searchtype=author&query=Ave%2C+M">M. Ave</a> , et al. (475 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1202.1493v1-abstract-short" style="display: inline;"> The Surface Detector of the Pierre Auger Observatory is sensitive to neutrinos of all flavours above 0.1 EeV. These interact through charged and neutral currents in the atmosphere giving rise to extensive air showers. When interacting deeply in the atmosphere at nearly horizontal incidence, neutrinos can be distinguished from regular hadronic cosmic rays by the broad time structure of their shower… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.1493v1-abstract-full').style.display = 'inline'; document.getElementById('1202.1493v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1202.1493v1-abstract-full" style="display: none;"> The Surface Detector of the Pierre Auger Observatory is sensitive to neutrinos of all flavours above 0.1 EeV. These interact through charged and neutral currents in the atmosphere giving rise to extensive air showers. When interacting deeply in the atmosphere at nearly horizontal incidence, neutrinos can be distinguished from regular hadronic cosmic rays by the broad time structure of their shower signals in the water-Cherenkov detectors. In this paper we present for the first time an analysis based on down-going neutrinos. We describe the search procedure, the possible sources of background, the method to compute the exposure and the associated systematic uncertainties. No candidate neutrinos have been found in data collected from 1 January 2004 to 31 May 2010. Assuming an E^-2 differential energy spectrum the limit on the single flavour neutrino is (E^2 * dN/dE) < 1.74x10^-7 GeV cm^-2 s^-1 sr^-1 at 90% C.L. in the energy range 1x10^17 eV < E < 1x10^20 eV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1202.1493v1-abstract-full').style.display = 'none'; document.getElementById('1202.1493v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 February, 2012; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2012. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 14 figures, published 30 December 2011</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 84, 122005 (2011); Erratum: Phys. Rev. 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