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</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/2411.10428">arXiv:2411.10428</a> <span> [<a href="https://arxiv.org/pdf/2411.10428">pdf</a>, <a href="https://arxiv.org/format/2411.10428">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="Optics">physics.optics</span> </div> </div> <p class="title is-5 mathjax"> BICEP/Keck XIX: Extremely Thin Composite Polymer Vacuum Windows for BICEP and Other High Throughput Millimeter Wave Telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+B">BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Carter%2C+K">K. Carter</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Corrigan%2C+L">L. Corrigan</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Crystian%2C+S">S. Crystian</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A+J">A. J. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E">E. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Echter%2C+M">M. Echter</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Elwood%2C+B+D">B. D. Elwood</a> , et al. (69 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="2411.10428v1-abstract-short" style="display: inline;"> Millimeter-wave refracting telescopes targeting the degree-scale structure of the cosmic microwave background (CMB) have recently grown to diffraction-limited apertures of over 0.5 meters. These instruments are entirely housed in vacuum cryostats to support their sub-kelvin bolometric detectors and to minimize radiative loading from thermal emission due to absorption loss in their transmissive opt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10428v1-abstract-full').style.display = 'inline'; document.getElementById('2411.10428v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.10428v1-abstract-full" style="display: none;"> Millimeter-wave refracting telescopes targeting the degree-scale structure of the cosmic microwave background (CMB) have recently grown to diffraction-limited apertures of over 0.5 meters. These instruments are entirely housed in vacuum cryostats to support their sub-kelvin bolometric detectors and to minimize radiative loading from thermal emission due to absorption loss in their transmissive optical elements. The large vacuum window is the only optical element in the system at ambient temperature, and therefore minimizing loss in the window is crucial for maximizing detector sensitivity. This motivates the use of low-loss polymer materials and a window as thin as practicable. However, the window must simultaneously meet the requirement to keep sufficient vacuum, and therefore must limit gas permeation and remain mechanically robust against catastrophic failure under pressure. We report on the development of extremely thin composite polyethylene window technology that meets these goals. Two windows have been deployed for two full observing seasons on the BICEP3 and BA150 CMB telescopes at the South Pole. On BICEP3, the window has demonstrated a 6% improvement in detector sensitivity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.10428v1-abstract-full').style.display = 'none'; document.getElementById('2411.10428v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">20 pages, 12 figures, 4 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.12089">arXiv:2410.12089</a> <span> [<a href="https://arxiv.org/pdf/2410.12089">pdf</a>, <a href="https://arxiv.org/format/2410.12089">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> BICEP/Keck XVIII: Measurement of BICEP3 polarization angles and consequences for constraining cosmic birefringence and inflation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+B">BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A+J">A. J. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E">E. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Elwood%2C+B+D">B. D. Elwood</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fortes%2C+A">A. Fortes</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+M">M. Gao</a> , et al. (61 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.12089v2-abstract-short" style="display: inline;"> We use a custom-made calibrator to measure individual detectors' polarization angles of BICEP3, a small aperture telescope observing the cosmic microwave background (CMB) at 95GHz from the South Pole. We describe our calibration strategy and the statistical and systematic uncertainties associated with the measurement. We reach an unprecedented precision for such measurement on a CMB experiment, wi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.12089v2-abstract-full').style.display = 'inline'; document.getElementById('2410.12089v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.12089v2-abstract-full" style="display: none;"> We use a custom-made calibrator to measure individual detectors' polarization angles of BICEP3, a small aperture telescope observing the cosmic microwave background (CMB) at 95GHz from the South Pole. We describe our calibration strategy and the statistical and systematic uncertainties associated with the measurement. We reach an unprecedented precision for such measurement on a CMB experiment, with a repeatability for each detector pair of $0.02掳$. We show that the relative angles measured using this method are in excellent agreement with those extracted from CMB data. Because the absolute measurement is currently limited by a systematic uncertainty, we do not derive cosmic birefringence constraints from BICEP3 data in this work. Rather, we forecast the sensitivity of BICEP3 sky maps for such analysis. We investigate the relative contributions of instrument noise, lensing, and dust, as well as astrophysical and instrumental systematics. We also explore the constraining power of different angle estimators, depending on analysis choices. We establish that the BICEP3 2-year dataset (2017--2018) has an on-sky sensitivity to the cosmic birefringence angle of $蟽= 0.078掳$, which could be improved to $蟽= 0.055掳$ by adding all of the existing BICEP3 data (through 2023). Furthermore, we emphasize the possibility of using the BICEP3 sky patch as a polarization calibration source for CMB experiments, which with the present data could reach a precision of $0.035掳$. Finally, in the context of inflation searches, we investigate the impact of detector-to-detector variations in polarization angles as they may bias the tensor-to-scalar ratio r. We show that while the effect is expected to remain subdominant to other sources of systematic uncertainty, it can be reliably calibrated using polarization angle measurements such as the ones we present in this paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.12089v2-abstract-full').style.display = 'none'; document.getElementById('2410.12089v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 Pages, 17 Figures, 6 Tables, as submitted to 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/2409.16440">arXiv:2409.16440</a> <span> [<a href="https://arxiv.org/pdf/2409.16440">pdf</a>, <a href="https://arxiv.org/format/2409.16440">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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"> Calibration Measurements of the BICEP3 and BICEP Array CMB Polarimeters from 2017 to 2024 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Giannakopoulos%2C+C">Christos Giannakopoulos</a>, <a href="/search/astro-ph?searchtype=author&query=Verg%C3%A8s%2C+C">Clara Verg猫s</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Zeeshan Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">Denis Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">Ritoban Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">Colin A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">Dominic Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">James J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">Hans Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">Victor Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">James R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">Jake Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">James Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">Michael Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A+J">Ari Jozef Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E">Edward Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">Marion Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">Lionel Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">Miranda Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Elwood%2C+B+D">Brodi D. Elwood</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">Sofia Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">Jeff P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fortes%2C+A">Antonio Fortes</a> , et al. (61 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="2409.16440v1-abstract-short" style="display: inline;"> The BICEP3 and BICEP Array polarimeters are small-aperture refracting telescopes located at the South Pole designed to measure primordial gravitational wave signatures in the Cosmic Microwave Background (CMB) polarization, predicted by inflation. Constraining the inflationary signal requires not only excellent sensitivity, but also careful control of instrumental systematics. Both instruments use… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16440v1-abstract-full').style.display = 'inline'; document.getElementById('2409.16440v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.16440v1-abstract-full" style="display: none;"> The BICEP3 and BICEP Array polarimeters are small-aperture refracting telescopes located at the South Pole designed to measure primordial gravitational wave signatures in the Cosmic Microwave Background (CMB) polarization, predicted by inflation. Constraining the inflationary signal requires not only excellent sensitivity, but also careful control of instrumental systematics. Both instruments use antenna-coupled orthogonally polarized detector pairs, and the polarized sky signal is reconstructed by taking the difference in each detector pair. As a result, the differential response between detectors within a pair becomes an important systematic effect we must control. Additionally, mapping the intensity and polarization response in regions away from the main beam can inform how sidelobe levels affect CMB measurements. Extensive calibration measurements are taken in situ every austral summer for control of instrumental systematics and instrument characterisation. In this work, we detail the set of beam calibration measurements that we conduct on the BICEP receivers, from deep measurements of main beam response to polarized beam response and sidelobe mapping. We discuss the impact of these measurements for instrumental systematics studies and design choices for future CMB receivers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.16440v1-abstract-full').style.display = 'none'; document.getElementById('2409.16440v1-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">13 pages, 7 figures, 1 table, Proceedings paper SPIE 2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.02296">arXiv:2409.02296</a> <span> [<a href="https://arxiv.org/pdf/2409.02296">pdf</a>, <a href="https://arxiv.org/format/2409.02296">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> <p class="title is-5 mathjax"> Development of the 220/270 GHz Receiver of BICEP Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+B">The BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Nakato%2C+Y">Y. Nakato</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cantrall%2C+B">B. Cantrall</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A+J">A. J. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E">E. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Elwood%2C+B+D">B. D. Elwood</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fortes%2C+A">A. Fortes</a> , et al. (61 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="2409.02296v1-abstract-short" style="display: inline;"> Measurements of B-mode polarization in the CMB sourced from primordial gravitational waves would provide information on the energy scale of inflation and its potential form. To achieve these goals, one must carefully characterize the Galactic foregrounds, which can be distinguished from the CMB by conducting measurements at multiple frequencies. BICEP Array is the latest-generation multi-frequency… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02296v1-abstract-full').style.display = 'inline'; document.getElementById('2409.02296v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.02296v1-abstract-full" style="display: none;"> Measurements of B-mode polarization in the CMB sourced from primordial gravitational waves would provide information on the energy scale of inflation and its potential form. To achieve these goals, one must carefully characterize the Galactic foregrounds, which can be distinguished from the CMB by conducting measurements at multiple frequencies. BICEP Array is the latest-generation multi-frequency instrument of the BICEP/Keck program, which specifically targets degree-scale primordial B-modes in the CMB. In its final configuration, this telescope will consist of four small-aperture receivers, spanning frequency bands from 30 to 270 GHz. The 220/270 GHz receiver designed to characterize Galactic dust is currently undergoing commissioning at Stanford University and is scheduled to deploy to the South Pole during the 2024--2025 austral summer. Here, we will provide an overview of this high-frequency receiver and discuss the integration status and test results as it is being commissioned. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02296v1-abstract-full').style.display = 'none'; document.getElementById('2409.02296v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.19469">arXiv:2405.19469</a> <span> [<a href="https://arxiv.org/pdf/2405.19469">pdf</a>, <a href="https://arxiv.org/format/2405.19469">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Constraining Inflation with the BICEP/Keck CMB Polarization Experiments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+B">The BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E+V">E. V. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Elwood%2C+B">B. Elwood</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+M">M. Gao</a> , et al. (63 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="2405.19469v2-abstract-short" style="display: inline;"> The BICEP/$\textit{Keck}$ (BK) series of cosmic microwave background (CMB) polarization experiments has, over the past decade and a half, produced a series of field-leading constraints on cosmic inflation via measurements of the "B-mode" polarization of the CMB. Primordial B modes are directly tied to the amplitude of primordial gravitational waves (PGW), their strength parameterized by the tensor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19469v2-abstract-full').style.display = 'inline'; document.getElementById('2405.19469v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.19469v2-abstract-full" style="display: none;"> The BICEP/$\textit{Keck}$ (BK) series of cosmic microwave background (CMB) polarization experiments has, over the past decade and a half, produced a series of field-leading constraints on cosmic inflation via measurements of the "B-mode" polarization of the CMB. Primordial B modes are directly tied to the amplitude of primordial gravitational waves (PGW), their strength parameterized by the tensor-to-scalar ratio, $r$, and thus the energy scale of inflation. Having set the most sensitive constraints to-date on $r$, $蟽(r)=0.009$ ($r_{0.05}<0.036, 95\%$ C.L.) using data through the 2018 observing season ("BK18"), the BICEP/$\textit{Keck}$ program has continued to improve its dataset in the years since. We give a brief overview of the BK program and the "BK18" result before discussing the program's ongoing efforts, including the deployment and performance of the $\textit{Keck Array}$'s successor instrument, BICEP Array, improvements to data processing and internal consistency testing, new techniques such as delensing, and how those will ultimately serve to allow BK reach $蟽(r) \lesssim 0.003$ using data through the 2027 observing season. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.19469v2-abstract-full').style.display = 'none'; document.getElementById('2405.19469v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">9 pages, 5 figures. Contribution to the 2024 Cosmology session of the 58th Rencontres de Moriond</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.08038">arXiv:2210.08038</a> <span> [<a href="https://arxiv.org/pdf/2210.08038">pdf</a>, <a href="https://arxiv.org/format/2210.08038">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acc85c">10.3847/1538-4357/acc85c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BICEP / Keck XVII: Line of Sight Distortion Analysis: Estimates of Gravitational Lensing, Anisotropic Cosmic Birefringence, Patchy Reionization, and Systematic Errors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+B">BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E+V">E. V. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fliescher%2C+S">S. Fliescher</a> , et al. (70 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.08038v2-abstract-short" style="display: inline;"> We present estimates of line-of-sight distortion fields derived from the 95 GHz and 150 GHz data taken by BICEP2, BICEP3, and Keck Array up to the 2018 observing season, leading to cosmological constraints and a study of instrumental and astrophysical systematics. Cosmological constraints are derived from three of the distortion fields concerning gravitational lensing from large-scale structure, p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08038v2-abstract-full').style.display = 'inline'; document.getElementById('2210.08038v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.08038v2-abstract-full" style="display: none;"> We present estimates of line-of-sight distortion fields derived from the 95 GHz and 150 GHz data taken by BICEP2, BICEP3, and Keck Array up to the 2018 observing season, leading to cosmological constraints and a study of instrumental and astrophysical systematics. Cosmological constraints are derived from three of the distortion fields concerning gravitational lensing from large-scale structure, polarization rotation from magnetic fields or an axion-like field, and the screening effect of patchy reionization. We measure an amplitude of the lensing power spectrum $A_L^{蠁蠁}=0.95 \pm 0.20$. We constrain polarization rotation, expressed as the coupling constant of a Chern-Simons electromagnetic term $g_{a纬} \leq 2.6 \times 10^{-2}/H_I$, where $H_I$ is the inflationary Hubble parameter, and an amplitude of primordial magnetic fields smoothed over 1 Mpc $B_{1\text{Mpc}} \leq 6.6 \;\text{nG}$ at 95 GHz. We constrain the root mean square of optical-depth fluctuations in a simple "crinkly surface" model of patchy reionization, finding $A^蟿<0.19$ ($2蟽$) for the coherence scale of $L_c=100$. We show that all of the distortion fields of the 95 GHz and 150 GHz polarization maps are consistent with simulations including lensed-$螞$CDM, dust, and noise, with no evidence for instrumental systematics. In some cases, the EB and TB quadratic estimators presented here are more sensitive than our previous map-based null tests at identifying and rejecting spurious B-modes that might arise from instrumental effects. Finally, we verify that the standard deprojection filtering in the BICEP/Keck data processing is effective at removing temperature to polarization leakage. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.08038v2-abstract-full').style.display = 'none'; document.getElementById('2210.08038v2-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 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">34 pages, 19 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 (2023) 949 43 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.05684">arXiv:2210.05684</a> <span> [<a href="https://arxiv.org/pdf/2210.05684">pdf</a>, <a href="https://arxiv.org/ps/2210.05684">ps</a>, <a href="https://arxiv.org/format/2210.05684">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acb64c">10.3847/1538-4357/acb64c <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BICEP / Keck XVI: Characterizing Dust Polarization through Correlations with Neutral Hydrogen </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+B">BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+S+E">S. E. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E+V">E. V. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2210.05684v2-abstract-short" style="display: inline;"> We characterize Galactic dust filaments by correlating BICEP/Keck and Planck data with polarization templates based on neutral hydrogen (H I) observations. Dust polarization is important for both our understanding of astrophysical processes in the interstellar medium (ISM) and the search for primordial gravitational waves in the cosmic microwave background (CMB). In the diffuse ISM, H I is strongl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.05684v2-abstract-full').style.display = 'inline'; document.getElementById('2210.05684v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.05684v2-abstract-full" style="display: none;"> We characterize Galactic dust filaments by correlating BICEP/Keck and Planck data with polarization templates based on neutral hydrogen (H I) observations. Dust polarization is important for both our understanding of astrophysical processes in the interstellar medium (ISM) and the search for primordial gravitational waves in the cosmic microwave background (CMB). In the diffuse ISM, H I is strongly correlated with the dust and partly organized into filaments that are aligned with the local magnetic field. We analyze the deep BICEP/Keck data at 95, 150, and 220 GHz, over the low-column-density region of sky where BICEP/Keck has set the best limits on primordial gravitational waves. We separate the H I emission into distinct velocity components and detect dust polarization correlated with the local Galactic H I but not with the H I associated with Magellanic Stream I. We present a robust, multifrequency detection of polarized dust emission correlated with the filamentary H I morphology template down to 95 GHz. For assessing its utility for foreground cleaning, we report that the H I morphology template correlates in B modes at a $\sim$10-65$\%$ level over the multipole range $20 < \ell < 200$ with the BICEP/Keck maps, which contain contributions from dust, CMB, and noise components. We measure the spectral index of the filamentary dust component spectral energy distribution to be $尾= 1.54 \pm 0.13$. We find no evidence for decorrelation in this region between the filaments and the rest of the dust field or from the inclusion of dust associated with the intermediate velocity H I. Finally, we explore the morphological parameter space in the H I-based filamentary model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.05684v2-abstract-full').style.display = 'none'; document.getElementById('2210.05684v2-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">27 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 945 72 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2207.14796">arXiv:2207.14796</a> <span> [<a href="https://arxiv.org/pdf/2207.14796">pdf</a>, <a href="https://arxiv.org/format/2207.14796">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Improved Polarization Calibration of the BICEP3 CMB Polarimeter at the South Pole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Verg%C3%A8s%2C+C">C. Verg猫s</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A+J">A. J. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E+V">E. V. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M+I">M. I. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Giannakopoulos%2C+C">C. Giannakopoulos</a>, <a href="/search/astro-ph?searchtype=author&query=Goeckner-Wald%2C+N">N. Goeckner-Wald</a>, <a href="/search/astro-ph?searchtype=author&query=Goldfinger%2C+D+C">D. C. Goldfinger</a>, <a href="/search/astro-ph?searchtype=author&query=Grayson%2C+J">J. Grayson</a> , et al. (61 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="2207.14796v2-abstract-short" style="display: inline;"> The BICEP3 Polarimeter is a small aperture, refracting telescope, dedicated to the observation of the Cosmic Microwave Background (CMB) at 95GHz. It is designed to target degree angular scale polarization patterns, in particular the very-much-sought-after primordial B-mode signal, which is a unique signature of cosmic inflation. The polarized signal from the sky is reconstructed by differencing co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.14796v2-abstract-full').style.display = 'inline'; document.getElementById('2207.14796v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.14796v2-abstract-full" style="display: none;"> The BICEP3 Polarimeter is a small aperture, refracting telescope, dedicated to the observation of the Cosmic Microwave Background (CMB) at 95GHz. It is designed to target degree angular scale polarization patterns, in particular the very-much-sought-after primordial B-mode signal, which is a unique signature of cosmic inflation. The polarized signal from the sky is reconstructed by differencing co-localized, orthogonally polarized superconducting Transition Edge Sensor (TES) bolometers. In this work, we present absolute measurements of the polarization response of the detectors for more than $\sim 800$ functioning detector pairs of the BICEP3 experiment, out of a total of $\sim 1000$. We use a specifically designed Rotating Polarized Source (RPS) to measure the polarization response at multiple source and telescope boresight rotation angles, to fully map the response over 360 degrees. We present here polarization properties extracted from on-site calibration data taken in January 2022. A similar calibration campaign was performed in 2018, but we found that our constraint was dominated by systematics on the level of $\sim0.5^\circ$. After a number of improvements to the calibration set-up, we are now able to report a significantly lower level of systematic contamination. In the future, such precise measurements will be used to constrain physics beyond the standard cosmological model, namely cosmic birefringence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.14796v2-abstract-full').style.display = 'none'; document.getElementById('2207.14796v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to: SPIE Astronomical Telescopes + Instrumentation (AS22)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.16556">arXiv:2203.16556</a> <span> [<a href="https://arxiv.org/pdf/2203.16556">pdf</a>, <a href="https://arxiv.org/format/2203.16556">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.58027/3q8k-ew90">10.58027/3q8k-ew90 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Latest Constraints on Inflationary B-modes from the BICEP/Keck Telescopes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+B">BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C">C. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E+V">E. V. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fliescher%2C+S">S. Fliescher</a> , et al. (71 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2203.16556v1-abstract-short" style="display: inline;"> For the past decade, the BICEP/Keck collaboration has been operating a series of telescopes at the Amundsen-Scott South Pole Station measuring degree-scale $B$-mode polarization imprinted in the Cosmic Microwave Background (CMB) by primordial gravitational waves (PGWs). These telescopes are compact refracting polarimeters mapping about 2% of the sky, observing at a broad range of frequencies to ac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.16556v1-abstract-full').style.display = 'inline'; document.getElementById('2203.16556v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.16556v1-abstract-full" style="display: none;"> For the past decade, the BICEP/Keck collaboration has been operating a series of telescopes at the Amundsen-Scott South Pole Station measuring degree-scale $B$-mode polarization imprinted in the Cosmic Microwave Background (CMB) by primordial gravitational waves (PGWs). These telescopes are compact refracting polarimeters mapping about 2% of the sky, observing at a broad range of frequencies to account for the polarized foreground from Galactic synchrotron and thermal dust emission. Our latest publication "BK18" utilizes the data collected up to the 2018 observing season, in conjunction with the publicly available WMAP and Planck data, to constrain the tensor-to-scalar ratio $r$. It particularly includes (1) the 3-year BICEP3 data which is the current deepest CMB polarization map at the foreground-minimum 95 GHz; and (2) the Keck 220 GHz map with a higher signal-to-noise ratio on the dust foreground than the Planck 353 GHz map. We fit the auto- and cross-spectra of these maps to a multicomponent likelihood model ($螞$CDM+dust+synchrotron+noise+$r$) and find it to be an adequate description of the data at the current noise level. The likelihood analysis yields $蟽(r)=0.009$. The inference of $r$ from our baseline model is tightened to $r_{0.05}=0.014^{+0.010}_{-0.011}$ and $r_{0.05}<0.036$ at 95% confidence, meaning that the BICEP/Keck $B$-mode data is the most powerful existing dataset for the constraint of PGWs. The up-coming BICEP Array telescope is projected to reach $蟽(r) \lesssim 0.003$ using data up to 2027. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.16556v1-abstract-full').style.display = 'none'; document.getElementById('2203.16556v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 6 figures, contribution to the 2022 Cosmology session of the 56th Rencontres de Moriond</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.14751">arXiv:2111.14751</a> <span> [<a href="https://arxiv.org/pdf/2111.14751">pdf</a>, <a href="https://arxiv.org/format/2111.14751">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/10.1007/s10909-023-02967-1">10.1007/s10909-023-02967-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Plastic Laminate Antireflective Coatings for Millimeter-wave Optics in BICEP Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">Marion Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Zeeshan Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">Denis Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">Ritoban Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">Colin A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">Dominic Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">James J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">Victor Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">James R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">Jake Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">James Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">Michael Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A+J">Ari Jozef Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E">Edward Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">Lionel Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">Miranda Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">Sofia Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">Jeff P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Giannakopoulos%2C+C">Christos Giannakopoulos</a>, <a href="/search/astro-ph?searchtype=author&query=Goeckner-Wald%2C+N">Neil Goeckner-Wald</a>, <a href="/search/astro-ph?searchtype=author&query=Goldfinger%2C+D">David Goldfinger</a>, <a href="/search/astro-ph?searchtype=author&query=Grayson%2C+J+A">James A. Grayson</a>, <a href="/search/astro-ph?searchtype=author&query=Grimes%2C+P">Paul Grimes</a> , et al. (60 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="2111.14751v1-abstract-short" style="display: inline;"> The BICEP/Keck series of experiments target the Cosmic Microwave Background at degree-scale resolution from the South Pole. Over the next few years, the "Stage-3" BICEP Array (BA) telescope will improve the program's frequency coverage and sensitivity to primordial B-mode polarization by an order of magnitude. The first receiver in the array, BA1, began observing at 30/40 GHz in early 2020. The ne… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14751v1-abstract-full').style.display = 'inline'; document.getElementById('2111.14751v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.14751v1-abstract-full" style="display: none;"> The BICEP/Keck series of experiments target the Cosmic Microwave Background at degree-scale resolution from the South Pole. Over the next few years, the "Stage-3" BICEP Array (BA) telescope will improve the program's frequency coverage and sensitivity to primordial B-mode polarization by an order of magnitude. The first receiver in the array, BA1, began observing at 30/40 GHz in early 2020. The next two receivers, BA2 and BA3, are currently being assembled and will map the southern sky at frequencies ranging from 95 GHz to 150 GHz. Common to all BA receivers is a refractive, on-axis, cryogenic optical design that focuses microwave radiation onto a focal plane populated with antenna-coupled bolometers. High-performance antireflective coatings up to 760 mm in aperture are needed for each element in the optical chain, and must withstand repeated thermal cycles down to 4 K. Here we present the design and fabrication of the 30/40 GHz anti-reflection coatings for the recently deployed BA1 receiver, then discuss laboratory measurements of their reflectance. We review the lamination method for these single- and dual-layer plastic coatings with indices matched to various polyethylene, nylon and alumina optics. We also describe ongoing efforts to optimize coatings for the next BA cryostats, which may inform technological choices for future Small-Aperture Telescopes of the CMB "Stage 4" experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14751v1-abstract-full').style.display = 'none'; document.getElementById('2111.14751v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 4 figures. Submitted to Journal of Low Temperature Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.00483">arXiv:2110.00483</a> <span> [<a href="https://arxiv.org/pdf/2110.00483">pdf</a>, <a href="https://arxiv.org/format/2110.00483">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1103/PhysRevLett.127.151301">10.1103/PhysRevLett.127.151301 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BICEP / Keck XIII: Improved Constraints on Primordial Gravitational Waves using Planck, WMAP, and BICEP/Keck Observations through the 2018 Observing Season </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+B">BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C">C. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E+V">E. V. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fliescher%2C+S">S. Fliescher</a> , et al. (68 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.00483v1-abstract-short" style="display: inline;"> We present results from an analysis of all data taken by the BICEP2, Keck Array and BICEP3 CMB polarization experiments up to and including the 2018 observing season. We add additional Keck Array observations at 220 GHz and BICEP3 observations at 95 GHz to the previous 95/150/220 GHz data set. The $Q/U$ maps now reach depths of 2.8, 2.8 and 8.8 $渭{\mathrm K}_{cmb}$ arcmin at 95, 150 and 220 GHz re… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00483v1-abstract-full').style.display = 'inline'; document.getElementById('2110.00483v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.00483v1-abstract-full" style="display: none;"> We present results from an analysis of all data taken by the BICEP2, Keck Array and BICEP3 CMB polarization experiments up to and including the 2018 observing season. We add additional Keck Array observations at 220 GHz and BICEP3 observations at 95 GHz to the previous 95/150/220 GHz data set. The $Q/U$ maps now reach depths of 2.8, 2.8 and 8.8 $渭{\mathrm K}_{cmb}$ arcmin at 95, 150 and 220 GHz respectively over an effective area of $\approx 600$ square degrees at 95 GHz and $\approx 400$ square degrees at 150 & 220 GHz. The 220 GHz maps now achieve a signal-to-noise on polarized dust emission exceeding that of Planck at 353 GHz. We take auto- and cross-spectra between these maps and publicly available WMAP and Planck maps at frequencies from 23 to 353 GHz and evaluate the joint likelihood of the spectra versus a multicomponent model of lensed-$螞$CDM+$r$+dust+synchrotron+noise. The foreground model has seven parameters, and no longer requires a prior on the frequency spectral index of the dust emission taken from measurements on other regions of the sky. This model is an adequate description of the data at the current noise levels. The likelihood analysis yields the constraint $r_{0.05}<0.036$ at 95% confidence. Running maximum likelihood search on simulations we obtain unbiased results and find that $蟽(r)=0.009$. These are the strongest constraints to date on primordial gravitational waves. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00483v1-abstract-full').style.display = 'none'; document.getElementById('2110.00483v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages, 24 figures, as published in PRL, data and figures available for download at http://bicepkeck.org</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. Lett. 127, 151301 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.00482">arXiv:2110.00482</a> <span> [<a href="https://arxiv.org/pdf/2110.00482">pdf</a>, <a href="https://arxiv.org/format/2110.00482">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="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ac4886">10.3847/1538-4357/ac4886 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BICEP / Keck XV: The BICEP3 CMB Polarimeter and the First Three Year Data Set </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+B">BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C">C. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E+V">E. V. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fliescher%2C+S">S. Fliescher</a> , et al. (68 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.00482v1-abstract-short" style="display: inline;"> We report on the design and performance of the BICEP3 instrument and its first three-year data set collected from 2016 to 2018. BICEP3 is a 52cm aperture, refracting telescope designed to observe the polarization of the cosmic microwave background (CMB) on degree angular scales at 95GHz. It started science observation at the South Pole in 2016 with 2400 antenna-coupled transition-edge sensor (TES)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00482v1-abstract-full').style.display = 'inline'; document.getElementById('2110.00482v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.00482v1-abstract-full" style="display: none;"> We report on the design and performance of the BICEP3 instrument and its first three-year data set collected from 2016 to 2018. BICEP3 is a 52cm aperture, refracting telescope designed to observe the polarization of the cosmic microwave background (CMB) on degree angular scales at 95GHz. It started science observation at the South Pole in 2016 with 2400 antenna-coupled transition-edge sensor (TES) bolometers. The receiver first demonstrated new technologies such as large-diameter alumina optics, Zotefoam infrared filters, and flux-activated SQUIDs, allowing $\sim 10\times$ higher optical throughput compared to the Keck design. BICEP3 achieved instrument noise-equivalent temperatures of 9.2, 6.8 and 7.1$渭\text{K}_{\text{CMB}}\sqrt{\text{s}}$ and reached Stokes $Q$ and $U$ map depths of 5.9, 4.4 and 4.4$渭$K-arcmin in 2016, 2017 and 2018, respectively. The combined three-year data set achieved a polarization map depth of 2.8$渭$K-arcmin over an effective area of 585 square degrees, which is the deepest CMB polarization map made to date at 95GHz. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00482v1-abstract-full').style.display = 'none'; document.getElementById('2110.00482v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">35 pages, 35 figures, as submitted to ApJ, data and figures available for download at http://bicepkeck.org</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal 927, 77 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2108.03316">arXiv:2108.03316</a> <span> [<a href="https://arxiv.org/pdf/2108.03316">pdf</a>, <a href="https://arxiv.org/format/2108.03316">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - 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/10.1103/PhysRevD.105.022006">10.1103/PhysRevD.105.022006 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BICEP / Keck XIV: Improved constraints on axion-like polarization oscillations in the cosmic microwave background </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+B">BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E+V">E. V. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fliescher%2C+S">S. Fliescher</a> , et al. (68 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="2108.03316v2-abstract-short" style="display: inline;"> 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 direc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.03316v2-abstract-full').style.display = 'inline'; document.getElementById('2108.03316v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2108.03316v2-abstract-full" style="display: none;"> 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 $g_{蠁纬} < (4.5 \times 10^{-12}~\mathrm{GeV}^{-1}) m/(10^{-21}~\mathrm{eV}$), 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. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2108.03316v2-abstract-full').style.display = 'none'; document.getElementById('2108.03316v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 3 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 105, 022006 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.02386">arXiv:2102.02386</a> <span> [<a href="https://arxiv.org/pdf/2102.02386">pdf</a>, <a href="https://arxiv.org/format/2102.02386">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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 class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2562729">10.1117/12.2562729 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Analysis of Temperature-to-Polarization Leakage in BICEP3 and Keck CMB Data from 2016 to 2018 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+B">The BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Germaine%2C+T+S">T. St. Germaine</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E">E. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fliescher%2C+S">S. Fliescher</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2102.02386v1-abstract-short" style="display: inline;"> The BICEP/Keck Array experiment is a series of small-aperture refracting telescopes observing degree-scale Cosmic Microwave Background polarization from the South Pole in search of a primordial $B$-mode signature. As a pair differencing experiment, an important systematic that must be controlled is the differential beam response between the co-located, orthogonally polarized detectors. We use high… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.02386v1-abstract-full').style.display = 'inline'; document.getElementById('2102.02386v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.02386v1-abstract-full" style="display: none;"> The BICEP/Keck Array experiment is a series of small-aperture refracting telescopes observing degree-scale Cosmic Microwave Background polarization from the South Pole in search of a primordial $B$-mode signature. As a pair differencing experiment, an important systematic that must be controlled is the differential beam response between the co-located, orthogonally polarized detectors. We use high-fidelity, in-situ measurements of the beam response to estimate the temperature-to-polarization (T $\rightarrow$ P) leakage in our latest data including observations from 2016 through 2018. This includes three years of BICEP3 observing at 95 GHz, and multifrequency data from Keck Array. Here we present band-averaged far-field beam maps, differential beam mismatch, and residual beam power (after filtering out the leading difference modes via deprojection) for these receivers. We show preliminary results of "beam map simulations," which use these beam maps to observe a simulated temperature (no $Q/U$) sky to estimate T $\rightarrow$ P leakage in our real data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.02386v1-abstract-full').style.display = 'none'; document.getElementById('2102.02386v1-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 February, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 4 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. SPIE 11453, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X, 114532E (15 December 2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.09363">arXiv:2012.09363</a> <span> [<a href="https://arxiv.org/pdf/2012.09363">pdf</a>, <a href="https://arxiv.org/format/2012.09363">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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 class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1117/12.2562066">10.1117/12.2562066 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observing low elevation sky and the CMB Cold Spot with BICEP3 at the South Pole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kang%2C+J">J. Kang</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E">E. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fliescher%2C+S">S. Fliescher</a>, <a href="/search/astro-ph?searchtype=author&query=Goeckner-Wald%2C+N">N. Goeckner-Wald</a>, <a href="/search/astro-ph?searchtype=author&query=Goldfinger%2C+D+C">D. C. Goldfinger</a> , et al. (62 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.09363v2-abstract-short" style="display: inline;"> BICEP3 is a 520 mm aperture on-axis refracting telescope at the South Pole, which observes the polarization of the cosmic microwave background (CMB) at 95 GHz to search for the B-mode signal from inflationary gravitational waves. In addition to this main target, we have developed a low-elevation observation strategy to extend coverage of the Southern sky at the South Pole, where BICEP3 can quickly… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.09363v2-abstract-full').style.display = 'inline'; document.getElementById('2012.09363v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.09363v2-abstract-full" style="display: none;"> BICEP3 is a 520 mm aperture on-axis refracting telescope at the South Pole, which observes the polarization of the cosmic microwave background (CMB) at 95 GHz to search for the B-mode signal from inflationary gravitational waves. In addition to this main target, we have developed a low-elevation observation strategy to extend coverage of the Southern sky at the South Pole, where BICEP3 can quickly achieve degree-scale E-mode measurements over a large area. An interesting E-mode measurement is probing a potential polarization anomaly around the CMB Cold Spot. During the austral summer seasons of 2018-19 and 2019-20, BICEP3 observed the sky with a flat mirror to redirect the beams to various low elevation ranges. The preliminary data analysis shows degree-scale E-modes measured with high signal-to-noise ratio. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.09363v2-abstract-full').style.display = 'none'; document.getElementById('2012.09363v2-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 10 figures; Figure 7 shows the correct file</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. SPIE 11453, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X, 114532D (13 December 2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2012.05934">arXiv:2012.05934</a> <span> [<a href="https://arxiv.org/pdf/2012.05934">pdf</a>, <a href="https://arxiv.org/format/2012.05934">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> <p class="title is-5 mathjax"> Polarization Calibration of the BICEP3 CMB polarimeter at the South Pole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Denison%2C+E">E. Denison</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Eiben%2C+M">M. Eiben</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fliescher%2C+S">S. Fliescher</a>, <a href="/search/astro-ph?searchtype=author&query=Goeckner-Wald%2C+N">N. Goeckner-Wald</a>, <a href="/search/astro-ph?searchtype=author&query=Goldfinger%2C+D+C">D. C. Goldfinger</a>, <a href="/search/astro-ph?searchtype=author&query=Grayson%2C+J+A">J. A. Grayson</a> , et al. (62 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2012.05934v1-abstract-short" style="display: inline;"> The BICEP3 CMB Polarimeter is a small-aperture refracting telescope located at the South Pole and is specifically designed to search for the possible signature of inflationary gravitational waves in the Cosmic Microwave Background (CMB). The experiment measures polarization on the sky by differencing the signal of co-located, orthogonally polarized antennas coupled to Transition Edge Sensor (TES)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.05934v1-abstract-full').style.display = 'inline'; document.getElementById('2012.05934v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.05934v1-abstract-full" style="display: none;"> The BICEP3 CMB Polarimeter is a small-aperture refracting telescope located at the South Pole and is specifically designed to search for the possible signature of inflationary gravitational waves in the Cosmic Microwave Background (CMB). The experiment measures polarization on the sky by differencing the signal of co-located, orthogonally polarized antennas coupled to Transition Edge Sensor (TES) detectors. We present precise measurements of the absolute polarization response angles and polarization efficiencies for nearly all of BICEP3s $\sim800$ functioning polarization-sensitive detector pairs from calibration data taken in January 2018. Using a Rotating Polarized Source (RPS), we mapped polarization response for each detector over a full 360 degrees of source rotation and at multiple telescope boresight rotations from which per-pair polarization properties were estimated. In future work, these results will be used to constrain signals predicted by exotic physical models such as Cosmic Birefringence. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.05934v1-abstract-full').style.display = 'none'; document.getElementById('2012.05934v1-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceedings submitted to SPIE 2020 (AS111). 12 pages, 5 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.08163">arXiv:2011.08163</a> <span> [<a href="https://arxiv.org/pdf/2011.08163">pdf</a>, <a href="https://arxiv.org/format/2011.08163">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link 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/10.1103/PhysRevD.103.022004">10.1103/PhysRevD.103.022004 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Demonstration of Improved Constraints on Primordial Gravitational Waves with Delensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=BICEP%2FKeck"> BICEP/Keck</a>, <a href="/search/astro-ph?searchtype=author&query=Collaborations%2C+S">SPTpol Collaborations</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+A+J">A. J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J+E">J. E. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=Avva%2C+J+S">J. S. Avva</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J+A">J. A. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+A+N">A. N. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+B+A">B. A. Benson</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchini%2C+F">F. Bianchini</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bleem%2C+L+E">L. E. Bleem</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Carlstrom%2C+J+E">J. E. Carlstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C+L">C. L. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+H+C">H. C. Chiang</a> , et al. (117 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.08163v2-abstract-short" style="display: inline;"> We present a constraint on the tensor-to-scalar ratio, $r$, derived from measurements of cosmic microwave background (CMB) polarization $B$-modes with "delensing," whereby the uncertainty on $r$ contributed by the sample variance of the gravitational lensing $B$-modes is reduced by cross-correlating against a lensing $B$-mode template. This template is constructed by combining an estimate of the p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.08163v2-abstract-full').style.display = 'inline'; document.getElementById('2011.08163v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.08163v2-abstract-full" style="display: none;"> We present a constraint on the tensor-to-scalar ratio, $r$, derived from measurements of cosmic microwave background (CMB) polarization $B$-modes with "delensing," whereby the uncertainty on $r$ contributed by the sample variance of the gravitational lensing $B$-modes is reduced by cross-correlating against a lensing $B$-mode template. This template is constructed by combining an estimate of the polarized CMB with a tracer of the projected large-scale structure. The large-scale-structure tracer used is a map of the cosmic infrared background derived from Planck satellite data, while the polarized CMB map comes from a combination of South Pole Telescope, BICEP/Keck, and Planck data. We expand the BICEP/Keck likelihood analysis framework to accept a lensing template and apply it to the BICEP/Keck data set collected through 2014 using the same parametric foreground modelling as in the previous analysis. From simulations, we find that the uncertainty on $r$ is reduced by $\sim10\%$, from $蟽(r)$= 0.024 to 0.022, which can be compared with a $\sim26\%$ reduction obtained when using a perfect lensing template. Applying the technique to the real data, the constraint on $r$ is improved from $r_{0.05} < 0.090$ to $r_{0.05} < 0.082$ (95\% C.L.). This is the first demonstration of improvement in an $r$ constraint through delensing. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.08163v2-abstract-full').style.display = 'none'; document.getElementById('2011.08163v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 11 figures; match published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 103, 022004 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.03483">arXiv:2011.03483</a> <span> [<a href="https://arxiv.org/pdf/2011.03483">pdf</a>, <a href="https://arxiv.org/format/2011.03483">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - 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/10.1103/PhysRevD.103.042002">10.1103/PhysRevD.103.042002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> BICEP / Keck XII: Constraints on axion-like polarization oscillations in the cosmic microwave background </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+B">BICEP/Keck Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">D. Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bischoff%2C+C+A">C. A. Bischoff</a>, <a href="/search/astro-ph?searchtype=author&query=Bock%2C+J+J">J. J. Bock</a>, <a href="/search/astro-ph?searchtype=author&query=Boenish%2C+H">H. Boenish</a>, <a href="/search/astro-ph?searchtype=author&query=Bullock%2C+E">E. Bullock</a>, <a href="/search/astro-ph?searchtype=author&query=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J">J. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Cornelison%2C+J">J. Cornelison</a>, <a href="/search/astro-ph?searchtype=author&query=Crumrine%2C+M">M. Crumrine</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Duband%2C+L">L. Duband</a>, <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Fliescher%2C+S">S. Fliescher</a>, <a href="/search/astro-ph?searchtype=author&query=Goeckner-Wald%2C+N">N. Goeckner-Wald</a>, <a href="/search/astro-ph?searchtype=author&query=Grayson%2C+J">J. Grayson</a>, <a href="/search/astro-ph?searchtype=author&query=Hall%2C+G">G. Hall</a> , et al. (58 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2011.03483v2-abstract-short" style="display: inline;"> We present a search for axion-like polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. A local axion field induces an all-sky, temporally sinusoidal rotation of CMB polarization. A CMB polarimeter can thus function as a direct-detection experiment for axion-like dark matter. We develop techniques to extract an oscillation signal. Many elements… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.03483v2-abstract-full').style.display = 'inline'; document.getElementById('2011.03483v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.03483v2-abstract-full" style="display: none;"> We present a search for axion-like polarization oscillations in the cosmic microwave background (CMB) with observations from the Keck Array. A local axion field induces an all-sky, temporally sinusoidal rotation of CMB polarization. A CMB polarimeter can thus function as a direct-detection experiment for axion-like dark matter. We develop techniques to extract an oscillation signal. Many elements of the method are generic to CMB polarimetry experiments and can be adapted for other datasets. As a first demonstration, we process data from the 2012 observing season to set upper limits on the axion-photon coupling constant in the mass range $10^{-21}$-$10^{-18}~\mathrm{eV}$, which corresponds to oscillation periods on the order of hours to months. We find no statistically significant deviations from the background model. For periods larger than $24~\mathrm{hr}$ (mass $m < 4.8 \times 10^{-20}~\mathrm{eV}$), the median 95%-confidence upper limit is equivalent to a rotation amplitude of $0.68^\circ$, which constrains the axion-photon coupling constant to $g_{蠁纬} < \left ( 1.1 \times 10^{-11}~\mathrm{GeV}^{-1} \right ) m/\left (10^{-21}~\mathrm{eV} \right )$, if axion-like particles constitute all of the dark matter. The constraints can be improved substantially with data already collected by the BICEP series of experiments. Current and future CMB polarimetry experiments are expected to achieve sufficient sensitivity to rule out unexplored regions of the axion parameter space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.03483v2-abstract-full').style.display = 'none'; document.getElementById('2011.03483v2-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 6 figures, 2 tables</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 103, 042002 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/1912.04272">arXiv:1912.04272</a> <span> [<a href="https://arxiv.org/pdf/1912.04272">pdf</a>, <a href="https://arxiv.org/format/1912.04272">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 Detectors">physics.ins-det</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/10.1364/AO.383921">10.1364/AO.383921 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Broadband, millimeter-wave antireflection coatings for large-format, cryogenic aluminum oxide optics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Nadolski%2C+A">A. Nadolski</a>, <a href="/search/astro-ph?searchtype=author&query=Vieira%2C+J+D">J. D. Vieira</a>, <a href="/search/astro-ph?searchtype=author&query=Sobrin%2C+J+A">J. A. Sobrin</a>, <a href="/search/astro-ph?searchtype=author&query=Kofman%2C+A+M">A. M. Kofman</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Z. Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+A+J">A. J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Avva%2C+J+S">J. S. Avva</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">R. Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+A+N">A. N. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+B+A">B. A. Benson</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+L">L. Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Carlstrom%2C+J+E">J. E. Carlstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Carter%2C+F+W">F. W. Carter</a>, <a href="/search/astro-ph?searchtype=author&query=Cecil%2C+T+W">T. W. Cecil</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C+L">C. L. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J+R">J. R. Cheshire IV</a>, <a href="/search/astro-ph?searchtype=author&query=Chesmore%2C+G+E">G. E. Chesmore</a>, <a href="/search/astro-ph?searchtype=author&query=Cliche%2C+J+F">J. F. Cliche</a>, <a href="/search/astro-ph?searchtype=author&query=Cukierman%2C+A">A. Cukierman</a>, <a href="/search/astro-ph?searchtype=author&query=de+Haan%2C+T">T. de Haan</a>, <a href="/search/astro-ph?searchtype=author&query=Dierickx%2C+M">M. Dierickx</a>, <a href="/search/astro-ph?searchtype=author&query=Ding%2C+J">J. Ding</a>, <a href="/search/astro-ph?searchtype=author&query=Dutcher%2C+D">D. Dutcher</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+W">W. Everett</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="1912.04272v2-abstract-short" style="display: inline;"> We present two prescriptions for broadband (~77 - 252 GHz), millimeter-wave antireflection coatings for cryogenic, sintered polycrystalline aluminum oxide optics: one for large-format (700 mm diameter) planar and plano-convex elements, the other for densely packed arrays of quasi-optical elements, in our case 5 mm diameter half-spheres (called "lenslets"). The coatings comprise three layers of com… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.04272v2-abstract-full').style.display = 'inline'; document.getElementById('1912.04272v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="1912.04272v2-abstract-full" style="display: none;"> We present two prescriptions for broadband (~77 - 252 GHz), millimeter-wave antireflection coatings for cryogenic, sintered polycrystalline aluminum oxide optics: one for large-format (700 mm diameter) planar and plano-convex elements, the other for densely packed arrays of quasi-optical elements, in our case 5 mm diameter half-spheres (called "lenslets"). The coatings comprise three layers of commercially-available, polytetrafluoroethylene-based, dielectric sheet material. The lenslet coating is molded to fit the 150 mm diameter arrays directly while the large-diameter lenses are coated using a tiled approach. We review the fabrication processes for both prescriptions then discuss laboratory measurements of their transmittance and reflectance. In addition, we present the inferred refractive indices and loss tangents for the coating materials and the aluminum oxide substrate. We find that at 150 GHz and 300 K the large-format coating sample achieves (97 +/- 2)% transmittance and the lenslet coating sample achieves (94 +/- 3)% transmittance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('1912.04272v2-abstract-full').style.display = 'none'; document.getElementById('1912.04272v2-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 March, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 December, 2019; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2019. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">19 pages, 11 figures; submitted 05 Dec 2019, accepted 26 Feb 2020</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Applied Optics, Vol. 59, Issue 10, pp. 3285-3295 (2020) </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 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 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