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[2108.03316] BICEP / Keck XIV: Improved constraints on axion-like polarization oscillations in the cosmic microwave background

<?xml version="1.0" encoding="UTF-8"?> <!DOCTYPE html PUBLIC "-//W3C//DTD XHTML 1.0 Transitional//EN" "http://www.w3.org/TR/xhtml1/DTD/xhtml1-transitional.dtd"> <html xmlns="http://www.w3.org/1999/xhtml" lang="en" xml:lang="en"> <head> <title>[2108.03316] BICEP / Keck XIV: Improved constraints on axion-like polarization oscillations in the cosmic microwave background</title> <meta name="viewport" content="width=device-width, initial-scale=1"> <link rel="apple-touch-icon" sizes="180x180" href="/static/browse/0.3.4/images/icons/apple-touch-icon.png"> <link rel="icon" type="image/png" sizes="32x32" href="/static/browse/0.3.4/images/icons/favicon-32x32.png"> <link rel="icon" type="image/png" sizes="16x16" href="/static/browse/0.3.4/images/icons/favicon-16x16.png"> <link rel="manifest" href="/static/browse/0.3.4/images/icons/site.webmanifest"> <link rel="mask-icon" href="/static/browse/0.3.4/images/icons/safari-pinned-tab.svg" color="#5bbad5"> <meta name="msapplication-TileColor" content="#da532c"> <meta name="theme-color" content="#ffffff"> <link rel="stylesheet" type="text/css" media="screen" href="/static/browse/0.3.4/css/arXiv.css?v=20240822" /> <link rel="stylesheet" type="text/css" media="print" href="/static/browse/0.3.4/css/arXiv-print.css?v=20200611" /> <link rel="stylesheet" type="text/css" media="screen" href="/static/browse/0.3.4/css/browse_search.css" /> <script language="javascript" src="/static/browse/0.3.4/js/accordion.js" /></script> <link rel="stylesheet" type="text/css" media="screen" href="/static/browse/0.3.4/css/slider.css?v=1.15" /> <script src="//code.jquery.com/jquery-latest.min.js" type="text/javascript"></script> <script type="text/javascript" src="/static/browse/0.3.4/js/donate.js?v=1.11"></script><link rel="canonical" href="https://arxiv.org/abs/2108.03316"/> <meta name="description" content="Abstract page for arXiv paper 2108.03316: BICEP / Keck XIV: Improved constraints on axion-like polarization oscillations in the cosmic microwave background"><meta property="og:type" content="website" /> <meta property="og:site_name" content="arXiv.org" /> <meta property="og:title" content="BICEP / Keck XIV: Improved constraints on axion-like polarization oscillations in the cosmic microwave background" /> <meta property="og:url" content="https://arxiv.org/abs/2108.03316v2" /> <meta property="og:image" content="/static/browse/0.3.4/images/arxiv-logo-fb.png" /> <meta property="og:image:secure_url" content="/static/browse/0.3.4/images/arxiv-logo-fb.png" /> <meta property="og:image:width" content="1200" /> <meta property="og:image:height" content="700" /> <meta property="og:image:alt" content="arXiv logo"/> <meta property="og:description" content="We present an improved search for axion-like polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. An all-sky, temporally sinusoidal rotation of CMB polarization, equivalent to a time-variable cosmic birefringence, is an observable manifestation of a local axion field and potentially allows a CMB polarimeter to detect axion-like dark matter directly. We describe improvements to the method presented in previous work, and we demonstrate the updated method with an expanded dataset consisting of the 2012-2015 observing seasons. We set limits on the axion-photon coupling constant for mass $m$ in the range $10^{-23}$-$10^{-18}~\mathrm{eV}$, which corresponds to oscillation periods on the order of hours to years. Our results are consistent with the background model. For periods between $1$ and $30~\mathrm{d}$ ($1.6 \times 10^{-21} \leq m \leq 4.8 \times 10^{-20}~\mathrm{eV}$), the $95\%$-confidence upper limits on rotation amplitude are approximately constant with a median of $0.27^\circ$, which constrains the axion-photon coupling constant to $g_{蠒纬} &lt; (4.5 \times 10^{-12}~\mathrm{GeV}^{-1}) m/(10^{-21}~\mathrm{eV}$), if axion-like particles constitute all of the dark matter. More than half of the collected BICEP dataset has yet to be analyzed, and several current and future CMB polarimetry experiments can apply the methods presented here to achieve comparable or superior constraints. In the coming years, oscillation measurements can achieve the sensitivity to rule out unexplored regions of the axion parameter space."/> <meta name="twitter:site" content="@arxiv"/> <meta name="twitter:card" content="summary"/> <meta name="twitter:title" content="BICEP / Keck XIV: Improved constraints on axion-like polarization..."/> <meta name="twitter:description" content="We present an improved search for axion-like polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. An all-sky, temporally sinusoidal rotation of..."/> <meta name="twitter:image" content="https://static.arxiv.org/icons/twitter/arxiv-logo-twitter-square.png"/> <meta name="twitter:image:alt" content="arXiv logo"/> <link rel="stylesheet" media="screen" type="text/css" href="/static/browse/0.3.4/css/tooltip.css"/><link rel="stylesheet" media="screen" type="text/css" href="https://static.arxiv.org/js/bibex-dev/bibex.css?20200709"/> <script src="/static/browse/0.3.4/js/mathjaxToggle.min.js" type="text/javascript"></script> <script src="//code.jquery.com/jquery-latest.min.js" type="text/javascript"></script> <script src="//cdn.jsdelivr.net/npm/js-cookie@2/src/js.cookie.min.js" type="text/javascript"></script> <script src="//cdn.jsdelivr.net/npm/dompurify@2.3.5/dist/purify.min.js"></script> <script src="/static/browse/0.3.4/js/toggle-labs.js?20241022" type="text/javascript"></script> <script src="/static/browse/0.3.4/js/cite.js" type="text/javascript"></script><meta name="citation_title" content="BICEP / Keck XIV: Improved constraints on axion-like polarization oscillations in the cosmic microwave background" /><meta name="citation_author" content="Keck Collaboration" /><meta name="citation_author" content="Ade, P. A. R." /><meta name="citation_author" content="Ahmed, Z." /><meta name="citation_author" content="Amiri, M." /><meta name="citation_author" content="Barkats, D." /><meta name="citation_author" content="Thakur, R. Basu" /><meta name="citation_author" content="Bischoff, C. A." /><meta name="citation_author" content="Beck, D." /><meta name="citation_author" content="Bock, J. J." /><meta name="citation_author" content="Boenish, H." /><meta name="citation_author" content="Bullock, E." /><meta name="citation_author" content="Buza, V." /><meta name="citation_author" content="Cheshire IV, J. R." /><meta name="citation_author" content="Connors, J." /><meta name="citation_author" content="Cornelison, J." /><meta name="citation_author" content="Crumrine, M." /><meta name="citation_author" content="Cukierman, A." /><meta name="citation_author" content="Denison, E. V." /><meta name="citation_author" content="Dierickx, M." /><meta name="citation_author" content="Duband, L." /><meta name="citation_author" content="Eiben, M." /><meta name="citation_author" content="Fatigoni, S." /><meta name="citation_author" content="Filippini, J. P." /><meta name="citation_author" content="Fliescher, S." /><meta name="citation_author" content="Goeckner-Wald, N." /><meta name="citation_author" content="Goldfinger, D. C." /><meta name="citation_author" content="Grayson, J." /><meta name="citation_author" content="Grimes, P." /><meta name="citation_author" content="Hall, G." /><meta name="citation_author" content="Halal, G." /><meta name="citation_author" content="Halpern, M." /><meta name="citation_author" content="Hand, E." /><meta name="citation_author" content="Harrison, S." /><meta name="citation_author" content="Henderson, S." /><meta name="citation_author" content="Hildebrandt, S. R." /><meta name="citation_author" content="Hilton, G. C." /><meta name="citation_author" content="Hubmayr, J." /><meta name="citation_author" content="Hui, H." /><meta name="citation_author" content="Irwin, K. D." /><meta name="citation_author" content="Kang, J." /><meta name="citation_author" content="Karkare, K. S." /><meta name="citation_author" content="Karpel, E." /><meta name="citation_author" content="Kefeli, S." /><meta name="citation_author" content="Kernasovskiy, S. A." /><meta name="citation_author" content="Kovac, J. M." /><meta name="citation_author" content="Kuo, C. L." /><meta name="citation_author" content="Lau, K." /><meta name="citation_author" content="Leitch, E. M." /><meta name="citation_author" content="Lennox, A." /><meta name="citation_author" content="Megerian, K. G." /><meta name="citation_author" content="Minutolo, L." /><meta name="citation_author" content="Moncelsi, L." /><meta name="citation_author" content="Nakato, Y." /><meta name="citation_author" content="Namikawa, T." /><meta name="citation_author" content="Nguyen, H. T." /><meta name="citation_author" content="O&#39;Brient, R." /><meta name="citation_author" content="Ogburn IV, R. W." /><meta name="citation_author" content="Palladino, S." /><meta name="citation_author" content="Prouve, T." /><meta name="citation_author" content="Pryke, C." /><meta name="citation_author" content="Racine, B." /><meta name="citation_author" content="Reintsema, C. D." /><meta name="citation_author" content="Richter, S." /><meta name="citation_author" content="Schillaci, A." /><meta name="citation_author" content="Schwarz, R." /><meta name="citation_author" content="Schmitt, B. L." /><meta name="citation_author" content="Sheehy, C. D." /><meta name="citation_author" content="Soliman, A." /><meta name="citation_author" content="Germaine, T. St." /><meta name="citation_author" content="Steinbach, B." /><meta name="citation_author" content="Sudiwala, R. V." /><meta name="citation_author" content="Teply, G. P." /><meta name="citation_author" content="Thompson, K. L." /><meta name="citation_author" content="Tolan, J. E." /><meta name="citation_author" content="Tucker, C." /><meta name="citation_author" content="Turner, A. D." /><meta name="citation_author" content="Umilta, C." /><meta name="citation_author" content="Verges, C." /><meta name="citation_author" content="Vieregg, A. G." /><meta name="citation_author" content="Wandui, A." /><meta name="citation_author" content="Weber, A. C." /><meta name="citation_author" content="Wiebe, D. V." /><meta name="citation_author" content="Willmert, J." /><meta name="citation_author" content="Wong, C. L." /><meta name="citation_author" content="Wu, W. L. K." /><meta name="citation_author" content="Yang, H." /><meta name="citation_author" content="Yoon, K. W." /><meta name="citation_author" content="Young, E." /><meta name="citation_author" content="Yu, C." /><meta name="citation_author" content="Zeng, L." /><meta name="citation_author" content="Zhang, C." /><meta name="citation_author" content="Zhang, S." /><meta name="citation_doi" content="10.1103/PhysRevD.105.022006" /><meta name="citation_date" content="2021/08/06" /><meta name="citation_online_date" content="2022/03/14" /><meta name="citation_pdf_url" content="http://arxiv.org/pdf/2108.03316" /><meta name="citation_arxiv_id" content="2108.03316" /><meta name="citation_abstract" content="We present an improved search for axion-like polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. An all-sky, temporally sinusoidal rotation of CMB polarization, equivalent to a time-variable cosmic birefringence, is an observable manifestation of a local axion field and potentially allows a CMB polarimeter to detect axion-like dark matter directly. We describe improvements to the method presented in previous work, and we demonstrate the updated method with an expanded dataset consisting of the 2012-2015 observing seasons. We set limits on the axion-photon coupling constant for mass $m$ in the range $10^{-23}$-$10^{-18}~\mathrm{eV}$, which corresponds to oscillation periods on the order of hours to years. Our results are consistent with the background model. For periods between $1$ and $30~\mathrm{d}$ ($1.6 \times 10^{-21} \leq m \leq 4.8 \times 10^{-20}~\mathrm{eV}$), the $95\%$-confidence upper limits on rotation amplitude are approximately constant with a median of $0.27^\circ$, which constrains the axion-photon coupling constant to $g_{\phi\gamma} &lt; (4.5 \times 10^{-12}~\mathrm{GeV}^{-1}) m/(10^{-21}~\mathrm{eV}$), if axion-like particles constitute all of the dark matter. More than half of the collected BICEP dataset has yet to be analyzed, and several current and future CMB polarimetry experiments can apply the methods presented here to achieve comparable or superior constraints. In the coming years, oscillation measurements can achieve the sensitivity to rule out unexplored regions of the axion parameter space." /> </head> <body class="with-cu-identity"> <aside class="slider-wrapper bps-banner forum blue"> <a class="close-slider bps-banner" href="#"><img src="/static/browse/0.3.4/images/icons/close-slider.png" alt="close this message"></a> <div class="columns"> <img role="presentation" class="bps-banner-image" src="/static/browse/0.3.4/images/icons/smileybones-pixel.png" alt="arXiv Smilely Bones"> <div class="copy-donation bps-banner"> <h2>Happy Giving Tuesday - support arXiv today!</h2> <p>Thank you to everyone who makes arXiv possible. 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trackback:ping="/trackback/2108.03316" /> </rdf:RDF> --><div id="abs-outer"> <div class="leftcolumn"> <div class="subheader"> <h1>Astrophysics > Cosmology and Nongalactic Astrophysics</h1> </div> <div class="header-breadcrumbs-mobile"> <strong>arXiv:2108.03316</strong> (astro-ph) </div> <link rel="stylesheet" type="text/css" href="/static/base/1.0.1/css/abs.css"> <div id="content-inner"> <div id="abs"> <div class="dateline"> [Submitted on 6 Aug 2021 (<a href="https://arxiv.org/abs/2108.03316v1">v1</a>), last revised 14 Mar 2022 (this version, v2)]</div> <h1 class="title mathjax"><span class="descriptor">Title:</span>BICEP / Keck XIV: Improved constraints on axion-like polarization oscillations in the cosmic microwave background</h1> <div class="authors"><span class="descriptor">Authors:</span><a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=BICEP/Keck+Collaboration" rel="nofollow">BICEP/Keck Collaboration</a>: <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Ade,+P+A+R" rel="nofollow">P. A. R. Ade</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Ahmed,+Z" rel="nofollow">Z. Ahmed</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Amiri,+M" rel="nofollow">M. Amiri</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Barkats,+D" rel="nofollow">D. Barkats</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Thakur,+R+B" rel="nofollow">R. Basu Thakur</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Bischoff,+C+A" rel="nofollow">C. A. Bischoff</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Beck,+D" rel="nofollow">D. Beck</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Bock,+J+J" rel="nofollow">J. J. Bock</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Boenish,+H" rel="nofollow">H. Boenish</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Bullock,+E" rel="nofollow">E. Bullock</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Buza,+V" rel="nofollow">V. Buza</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Cheshire,+J+R" rel="nofollow">J. R. Cheshire IV</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Connors,+J" rel="nofollow">J. Connors</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Cornelison,+J" rel="nofollow">J. Cornelison</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Crumrine,+M" rel="nofollow">M. Crumrine</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Cukierman,+A" rel="nofollow">A. Cukierman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Denison,+E+V" rel="nofollow">E. V. Denison</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Dierickx,+M" rel="nofollow">M. Dierickx</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Duband,+L" rel="nofollow">L. Duband</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Eiben,+M" rel="nofollow">M. Eiben</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Fatigoni,+S" rel="nofollow">S. Fatigoni</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Filippini,+J+P" rel="nofollow">J. P. Filippini</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Fliescher,+S" rel="nofollow">S. Fliescher</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Goeckner-Wald,+N" rel="nofollow">N. Goeckner-Wald</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Goldfinger,+D+C" rel="nofollow">D. C. Goldfinger</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Grayson,+J" rel="nofollow">J. Grayson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Grimes,+P" rel="nofollow">P. Grimes</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Hall,+G" rel="nofollow">G. Hall</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Halal,+G" rel="nofollow">G. Halal</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Halpern,+M" rel="nofollow">M. Halpern</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Hand,+E" rel="nofollow">E. Hand</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Harrison,+S" rel="nofollow">S. Harrison</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Henderson,+S" rel="nofollow">S. 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Wiebe</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Willmert,+J" rel="nofollow">J. Willmert</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Wong,+C+L" rel="nofollow">C. L. Wong</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Wu,+W+L+K" rel="nofollow">W. L. K. Wu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Yang,+H" rel="nofollow">H. Yang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Yoon,+K+W" rel="nofollow">K. W. Yoon</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Young,+E" rel="nofollow">E. Young</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Yu,+C" rel="nofollow">C. Yu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Zeng,+L" rel="nofollow">L. Zeng</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Zhang,+C" rel="nofollow">C. Zhang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&amp;query=Zhang,+S" rel="nofollow">S. Zhang</a></div> <div id="download-button-info" hidden>View a PDF of the paper titled BICEP / Keck XIV: Improved constraints on axion-like polarization oscillations in the cosmic microwave background, by BICEP/Keck Collaboration: P. A. R. Ade and 90 other authors</div> <a class="mobile-submission-download" href="/pdf/2108.03316">View PDF</a> <blockquote class="abstract mathjax"> <span class="descriptor">Abstract:</span>We present an improved search for axion-like polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. An all-sky, temporally sinusoidal rotation of CMB polarization, equivalent to a time-variable cosmic birefringence, is an observable manifestation of a local axion field and potentially allows a CMB polarimeter to detect axion-like dark matter directly. We describe improvements to the method presented in previous work, and we demonstrate the updated method with an expanded dataset consisting of the 2012-2015 observing seasons. We set limits on the axion-photon coupling constant for mass $m$ in the range $10^{-23}$-$10^{-18}~\mathrm{eV}$, which corresponds to oscillation periods on the order of hours to years. Our results are consistent with the background model. For periods between $1$ and $30~\mathrm{d}$ ($1.6 \times 10^{-21} \leq m \leq 4.8 \times 10^{-20}~\mathrm{eV}$), the $95\%$-confidence upper limits on rotation amplitude are approximately constant with a median of $0.27^\circ$, which constrains the axion-photon coupling constant to $g_{\phi\gamma} &lt; (4.5 \times 10^{-12}~\mathrm{GeV}^{-1}) m/(10^{-21}~\mathrm{eV}$), if axion-like particles constitute all of the dark matter. More than half of the collected BICEP dataset has yet to be analyzed, and several current and future CMB polarimetry experiments can apply the methods presented here to achieve comparable or superior constraints. In the coming years, oscillation measurements can achieve the sensitivity to rule out unexplored regions of the axion parameter space. </blockquote> <!--CONTEXT--> <div class="metatable"> <table summary="Additional metadata"> <tr> <td class="tablecell label">Comments:</td> <td class="tablecell comments mathjax">14 pages, 3 figures</td> </tr> <tr> <td class="tablecell label">Subjects:</td> <td class="tablecell subjects"> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span>; High Energy Physics - Experiment (hep-ex); High Energy Physics - Phenomenology (hep-ph)</td> </tr><tr> <td class="tablecell label">Cite as:</td> <td class="tablecell arxivid"><span class="arxivid"><a href="https://arxiv.org/abs/2108.03316">arXiv:2108.03316</a> [astro-ph.CO]</span></td> </tr> <tr> <td class="tablecell label">&nbsp;</td> <td class="tablecell arxividv">(or <span class="arxivid"> <a href="https://arxiv.org/abs/2108.03316v2">arXiv:2108.03316v2</a> [astro-ph.CO]</span> for this version) </td> </tr> <tr> <td class="tablecell label">&nbsp;</td> <td class="tablecell arxivdoi"> <a href="https://doi.org/10.48550/arXiv.2108.03316" id="arxiv-doi-link">https://doi.org/10.48550/arXiv.2108.03316</a><div class="button-and-tooltip"> <button class="more-info" aria-describedby="more-info-desc-1"> <svg height="15" role="presentation" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512"><path fill="currentColor" d="M256 8C119.043 8 8 119.083 8 256c0 136.997 111.043 248 248 248s248-111.003 248-248C504 119.083 392.957 8 256 8zm0 110c23.196 0 42 18.804 42 42s-18.804 42-42 42-42-18.804-42-42 18.804-42 42-42zm56 254c0 6.627-5.373 12-12 12h-88c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h12v-64h-12c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h64c6.627 0 12 5.373 12 12v100h12c6.627 0 12 5.373 12 12v24z" class=""></path></svg> <span class="visually-hidden">Focus to learn more</span> </button> <!-- tooltip description --> <div role="tooltip" id="more-info-desc-1"> <span class="left-corner"></span> arXiv-issued DOI via DataCite</div> </div> </td> </tr> <tr> <td class="tablecell label">Journal&nbsp;reference:</td> <td class="tablecell jref">Phys. 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D 105, 022006 (2022)</td> </tr> <tr> <td class="tablecell label"> <abbr title="Digital Object Identifier">Related DOI</abbr>: </td> <td class="tablecell doi"><a href="https://doi.org/10.1103/PhysRevD.105.022006" data-doi="10.1103/PhysRevD.105.022006" class="link-https link-external" rel="external noopener nofollow">https://doi.org/10.1103/PhysRevD.105.022006</a> <!-- accessible tooltip example --> <div class="button-and-tooltip"> <button class="more-info" aria-describedby="more-info-desc-1"> <svg height="15" role="presentation" xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512"><path fill="currentColor" d="M256 8C119.043 8 8 119.083 8 256c0 136.997 111.043 248 248 248s248-111.003 248-248C504 119.083 392.957 8 256 8zm0 110c23.196 0 42 18.804 42 42s-18.804 42-42 42-42-18.804-42-42 18.804-42 42-42zm56 254c0 6.627-5.373 12-12 12h-88c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h12v-64h-12c-6.627 0-12-5.373-12-12v-24c0-6.627 5.373-12 12-12h64c6.627 0 12 5.373 12 12v100h12c6.627 0 12 5.373 12 12v24z" class=""></path></svg> <span class="visually-hidden">Focus to learn more</span> </button> <!-- tooltip description --> <div role="tooltip" id="more-info-desc-1"> <span class="left-corner"></span> DOI(s) linking to related resources </div> </div> </td> </tr> </table> </div> </div> </div> <div class="submission-history"> <h2>Submission history</h2> From: Ari Cukierman [<a href="/show-email/7702d984/2108.03316" rel="nofollow">view email</a>] <br/> <strong><a href="/abs/2108.03316v1" rel="nofollow">[v1]</a></strong> Fri, 6 Aug 2021 22:07:44 UTC (293 KB)<br/> <strong>[v2]</strong> Mon, 14 Mar 2022 16:31:10 UTC (294 KB)<br/> </div> </div> <!--end leftcolumn--> <div class="extra-services"> <div class="full-text"> <a name="other"></a> <span class="descriptor">Full-text links:</span> <h2>Access Paper:</h2> <ul> <div id="download-button-info" hidden> View a PDF of the paper titled BICEP / Keck XIV: Improved constraints on axion-like polarization oscillations in the cosmic microwave background, by BICEP/Keck Collaboration: P. 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