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value="">Relevance</option></select> </span> </div> <div class="control"> <button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.11460">arXiv:2412.11460</a> <span> [<a href="https://arxiv.org/pdf/2412.11460">pdf</a>, <a href="https://arxiv.org/format/2412.11460">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> <p class="title is-5 mathjax"> Observation of a spectral hardening in cosmic ray boron spectrum with the DAMPE space mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DAMPE+Collaboration"> DAMPE Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Alemanno%2C+F">F. Alemanno</a>, <a href="/search/astro-ph?searchtype=author&query=Altomare%2C+C">C. Altomare</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/astro-ph?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F+C+T">F. C. T. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+P">P. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Boutin%2C+H">H. Boutin</a>, <a href="/search/astro-ph?searchtype=author&query=Cagnoli%2C+I">I. Cagnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+M+S">M. S. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Casilli%2C+E">E. Casilli</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzani%2C+E">E. Catanzani</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+D+Y">D. Y. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+J+L">J. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Z+F">Z. F. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Z+X">Z. X. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Coppin%2C+P">P. Coppin</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+M+Y">M. Y. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+T+S">T. S. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+Y+X">Y. X. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=De+Mitri%2C+I">I. De Mitri</a>, <a href="/search/astro-ph?searchtype=author&query=de+Palma%2C+F">F. de Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Giovanni%2C+A">A. Di Giovanni</a> , et al. (121 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="2412.11460v2-abstract-short" style="display: inline;"> Secondary cosmic ray fluxes are important probes of the propagation and interaction of high-energy particles in the Galaxy. Recent measurements of primary and secondary cosmic ray nuclei have revealed unexpected spectral features that demand a deeper understanding. In this work we report the direct measurement of the cosmic ray boron spectrum from 10 GeV/n to 8 TeV/n with eight years of data colle… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.11460v2-abstract-full').style.display = 'inline'; document.getElementById('2412.11460v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.11460v2-abstract-full" style="display: none;"> Secondary cosmic ray fluxes are important probes of the propagation and interaction of high-energy particles in the Galaxy. Recent measurements of primary and secondary cosmic ray nuclei have revealed unexpected spectral features that demand a deeper understanding. In this work we report the direct measurement of the cosmic ray boron spectrum from 10 GeV/n to 8 TeV/n with eight years of data collected by the Dark Matter Particle Explorer (DAMPE) mission. The measured spectrum shows an evident hardening at $182\pm24$ GeV/n with a spectral power index of $纬_1 = 3.02 \pm 0.01$ before the break and an index change of $螖纬= 0.31 \pm 0.05$ after the break. A simple power law model is disfavored at a confidence level of 8$蟽$. Compared with the hardenings measured in the DAMPE proton and helium spectra, the secondary boron spectrum hardens roughly twice as much as these primaries, which is consistent with a propagation related mechanism to interpret the spectral hardenings of cosmic rays observed at hundreds of GeV/n. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.11460v2-abstract-full').style.display = 'none'; document.getElementById('2412.11460v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 10 figures, submitted to PRL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.00137">arXiv:2304.00137</a> <span> [<a href="https://arxiv.org/pdf/2304.00137">pdf</a>, <a href="https://arxiv.org/ps/2304.00137">ps</a>, <a href="https://arxiv.org/format/2304.00137">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/10.1103/PhysRevD.109.L121101">10.1103/PhysRevD.109.L121101 <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 p+He energy spectrum from 50 GeV to 0.5 PeV with the DAMPE space mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DAMPE+Collaboration"> DAMPE Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Alemanno%2C+F">F. Alemanno</a>, <a href="/search/astro-ph?searchtype=author&query=Altomare%2C+C">C. Altomare</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/astro-ph?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F+C+T">F. C. T. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+P">P. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Cagnoli%2C+I">I. Cagnoli</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+M+S">M. S. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Casilli%2C+E">E. Casilli</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzani%2C+E">E. Catanzani</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+D+Y">D. Y. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+J+L">J. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Z+F">Z. F. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Coppin%2C+P">P. Coppin</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+M+Y">M. Y. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+T+S">T. S. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+Y+X">Y. X. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+H+T">H. T. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=De+Benedittis%2C+A">A. De Benedittis</a>, <a href="/search/astro-ph?searchtype=author&query=De+Mitri%2C+I">I. De Mitri</a>, <a href="/search/astro-ph?searchtype=author&query=de+Palma%2C+F">F. de Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Deliyergiyev%2C+M">M. Deliyergiyev</a> , et al. (130 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="2304.00137v5-abstract-short" style="display: inline;"> Recent observations of the light component of the cosmic-ray spectrum have revealed unexpected features that motivate further and more precise measurements up to the highest energies. The Dark Matter Particle Explorer is a satellite-based cosmic-ray experiment that has been operational since December 2015, continuously collecting data on high-energy cosmic particles with very good statistics, ener… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.00137v5-abstract-full').style.display = 'inline'; document.getElementById('2304.00137v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.00137v5-abstract-full" style="display: none;"> Recent observations of the light component of the cosmic-ray spectrum have revealed unexpected features that motivate further and more precise measurements up to the highest energies. The Dark Matter Particle Explorer is a satellite-based cosmic-ray experiment that has been operational since December 2015, continuously collecting data on high-energy cosmic particles with very good statistics, energy resolution, and particle identification capabilities. In this work, the latest measurements of the energy spectrum of proton+helium in the energy range from 46 GeV to 464 TeV are presented. Among the most distinctive features of the spectrum, a spectral hardening at 600 GeV has been observed, along with a softening at 29 TeV measured with a 6.6蟽 significance. Moreover, the detector features and the analysis approach allowed for the extension of the spectral measurement up to the sub-PeV region. Even if with small statistical significance due to the low number of events, data suggest a new spectral hardening at about 150 TeV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.00137v5-abstract-full').style.display = 'none'; document.getElementById('2304.00137v5-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published on PRD</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.08833">arXiv:2210.08833</a> <span> [<a href="https://arxiv.org/pdf/2210.08833">pdf</a>, <a href="https://arxiv.org/format/2210.08833">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> <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/10.1016/j.scib.2022.10.002">10.1016/j.scib.2022.10.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of spectral hardenings in cosmic-ray boron-to-carbon and boron-to-oxygen flux ratios with DAMPE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DAMPE+Collaboration"> DAMPE Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.08833v2-abstract-short" style="display: inline;"> Boron nuclei in cosmic rays (CRs) are believed to be mainly produced by the fragmentation of heavier nuclei, such as carbon and oxygen, via collisions with the interstellar matter. Therefore, the boron-to-carbon flux ratio (B/C) and the boron-to-oxygen flux ratio (B/O) are very essential probes of the CR propagation. The energy dependence of the B/C ratio from previous balloon-borne and space-base… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08833v2-abstract-full').style.display = 'inline'; document.getElementById('2210.08833v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.08833v2-abstract-full" style="display: none;"> Boron nuclei in cosmic rays (CRs) are believed to be mainly produced by the fragmentation of heavier nuclei, such as carbon and oxygen, via collisions with the interstellar matter. Therefore, the boron-to-carbon flux ratio (B/C) and the boron-to-oxygen flux ratio (B/O) are very essential probes of the CR propagation. The energy dependence of the B/C ratio from previous balloon-borne and space-based experiments can be well described by a single power-law up to about 1 TeV/n within uncertainties. This work reports direct measurements of B/C and B/O in the energy range from 10 GeV/n to 5.6 TeV/n with 6 years of data collected by the Dark Matter Particle Explorer, with high statistics and well controlled systematic uncertainties. The energy dependence of both the B/C and B/O ratios can be well fitted by a broken power-law model rather than a single power-law model, suggesting the existence in both flux ratios of a spectral hardening at about 100 GeV/n. The significance of the break is about $5.6蟽$ and $6.9蟽$ for the GEANT4 simulation, and $4.4蟽$ and $6.9蟽$ for the alternative FLUKA simulation, for B/C and B/O, respectively. These results deviate from the predictions of conventional turbulence theories of the interstellar medium, which point toward a change of turbulence properties of the interstellar medium (ISM) at different scales or novel propagation effects of CRs, and should be properly incorporated in the indirect detection of dark matter via anti-matter particles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08833v2-abstract-full').style.display = 'none'; document.getElementById('2210.08833v2-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 November, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 October, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 9 figures, accepted in Science Bulletin</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Science Bulletin 67, 2162-2166 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2209.04260">arXiv:2209.04260</a> <span> [<a href="https://arxiv.org/pdf/2209.04260">pdf</a>, <a href="https://arxiv.org/format/2209.04260">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Space Physics">physics.space-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/PhysRevD.106.063026">10.1103/PhysRevD.106.063026 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for relativistic fractionally charged particles in space </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DAMPE+Collaboration"> DAMPE Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Alemanno%2C+F">F. Alemanno</a>, <a href="/search/astro-ph?searchtype=author&query=Altomare%2C+C">C. Altomare</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+Q">Q. An</a>, <a href="/search/astro-ph?searchtype=author&query=Azzarello%2C+P">P. Azzarello</a>, <a href="/search/astro-ph?searchtype=author&query=Barbato%2C+F+C+T">F. C. T. Barbato</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardini%2C+P">P. Bernardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bi%2C+X+J">X. J. Bi</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+M+S">M. S. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Casilli%2C+E">E. Casilli</a>, <a href="/search/astro-ph?searchtype=author&query=Catanzani%2C+E">E. Catanzani</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+J">J. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+D+Y">D. Y. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+J+L">J. L. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Z+F">Z. F. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+M+Y">M. Y. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+T+S">T. S. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+Y+X">Y. X. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Dai%2C+H+T">H. T. Dai</a>, <a href="/search/astro-ph?searchtype=author&query=De-Benedittis%2C+A">A. De-Benedittis</a>, <a href="/search/astro-ph?searchtype=author&query=De+Mitri%2C+I">I. De Mitri</a>, <a href="/search/astro-ph?searchtype=author&query=de+Palma%2C+F">F. de Palma</a>, <a href="/search/astro-ph?searchtype=author&query=Deliyergiyev%2C+M">M. Deliyergiyev</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Giovanni%2C+A">A. Di Giovanni</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Santo%2C+M">M. Di Santo</a> , et al. (126 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2209.04260v1-abstract-short" style="display: inline;"> More than a century after the performance of the oil drop experiment, the possible existence of fractionally charged particles FCP still remains unsettled. The search for FCPs is crucial for some extensions of the Standard Model in particle physics. Most of the previously conducted searches for FCPs in cosmic rays were based on experiments underground or at high altitudes. However, there have been… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.04260v1-abstract-full').style.display = 'inline'; document.getElementById('2209.04260v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2209.04260v1-abstract-full" style="display: none;"> More than a century after the performance of the oil drop experiment, the possible existence of fractionally charged particles FCP still remains unsettled. The search for FCPs is crucial for some extensions of the Standard Model in particle physics. Most of the previously conducted searches for FCPs in cosmic rays were based on experiments underground or at high altitudes. However, there have been few searches for FCPs in cosmic rays carried out in orbit other than AMS-01 flown by a space shuttle and BESS by a balloon at the top of the atmosphere. In this study, we conduct an FCP search in space based on on-orbit data obtained using the DArk Matter Particle Explorer (DAMPE) satellite over a period of five years. Unlike underground experiments, which require an FCP energy of the order of hundreds of GeV, our FCP search starts at only a few GeV. An upper limit of $6.2\times 10^{-10}~~\mathrm{cm^{-2}sr^{-1} s^{-1}}$ is obtained for the flux. Our results demonstrate that DAMPE exhibits higher sensitivity than experiments of similar types by three orders of magnitude that more stringently restricts the conditions for the existence of FCP in primary cosmic rays. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2209.04260v1-abstract-full').style.display = 'none'; document.getElementById('2209.04260v1-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 6 figures, accepted by PRD</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> 106, 063026 </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Physical Review D 106.6 (2022): 063026 </p> </li> </ol> <div class="is-hidden-tablet">  <span class="help" style="display: inline-block;"><a href="https://github.com/arXiv/arxiv-search/releases">Search v0.5.6 released 2020-02-24</a>  </span> </div> </div> </main> <footer> <div class="columns is-desktop" role="navigation" aria-label="Secondary">  <div class="column"> <div class="columns"> <div class="column"> <ul class="nav-spaced"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul class="nav-spaced"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 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