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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Amiri%2C+M&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Amiri%2C+M&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Amiri%2C+M&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Amiri%2C+M&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.11217">arXiv:2502.11217</a> <span> [<a href="https://arxiv.org/pdf/2502.11217">pdf</a>, <a href="https://arxiv.org/format/2502.11217">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A Catalog of Local Universe Fast Radio Bursts from CHIME/FRB and the KKO Outrigger </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Amouyal%2C+D">Daniel Amouyal</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">Bridget C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Andrew%2C+S">Shion Andrew</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Cassity%2C+A">Alyssa Cassity</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+S">Shami Chatterjee</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+Y">Yuxin Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Eadie%2C+G+M">Gwendolyn M. Eadie</a>, <a href="/search/astro-ph?searchtype=author&query=Eftekhari%2C+T">Tarraneh Eftekhari</a>, <a href="/search/astro-ph?searchtype=author&query=Fong%2C+W">Wen-fai Fong</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">Mark Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hessels%2C+J+W+T">Jason W. T. Hessels</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+H">Hans Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ibik%2C+A+L">Adaeze L. Ibik</a>, <a href="/search/astro-ph?searchtype=author&query=Joseph%2C+R+C">Ronniy C. Joseph</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J">Jane Kaczmarek</a> , et al. (39 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="2502.11217v1-abstract-short" style="display: inline;"> We present the first catalog of fast radio burst (FRB) host galaxies from CHIME/FRB Outriggers, selected uniformly in the radio and the optical by localizing 81 new bursts to 2'' x ~60'' accuracy using CHIME and the KKO Outrigger, located 66 km from CHIME. Of the 81 localized bursts, we use the Probabilistic Association of Transients to their Hosts (PATH) algorithm to securely identify 21 new FRB… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.11217v1-abstract-full').style.display = 'inline'; document.getElementById('2502.11217v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.11217v1-abstract-full" style="display: none;"> We present the first catalog of fast radio burst (FRB) host galaxies from CHIME/FRB Outriggers, selected uniformly in the radio and the optical by localizing 81 new bursts to 2'' x ~60'' accuracy using CHIME and the KKO Outrigger, located 66 km from CHIME. Of the 81 localized bursts, we use the Probabilistic Association of Transients to their Hosts (PATH) algorithm to securely identify 21 new FRB host galaxies, and compile spectroscopic redshifts for 19 systems, 15 of which are newly obtained via spectroscopic observations. The most nearby source is FRB 20231229A, at a distance of 90 Mpc. One burst in our sample is from a previously reported repeating source in a galaxy merger (FRB 20190303A). Three new FRB host galaxies (FRBs 20230203A, 20230703A, and 20231206A) are found towards X-ray and optically selected galaxy clusters, potentially doubling the sample of known galaxy cluster FRBs. A search for radio counterparts reveals that FRB 20231128A is associated with a luminous persistent radio source (PRS) candidate with high significance ($P_{cc} \sim 10^{-2}$). If its compactness is confirmed, it would be the nearest known compact PRS at $z = 0.1079$. Our catalog significantly increases the statistics of the Macquart relation at low redshifts ($z < 0.2$). In the near future, the completed CHIME/FRB Outriggers array will produce hundreds of FRBs localized with very long baseline interferometry (VLBI). This will significantly expand the known sample and pave the way for future telescopes relying on VLBI for FRB localization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.11217v1-abstract-full').style.display = 'none'; document.getElementById('2502.11217v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </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, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2410.23374">arXiv:2410.23374</a> <span> [<a href="https://arxiv.org/pdf/2410.23374">pdf</a>, <a href="https://arxiv.org/format/2410.23374">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> A repeating fast radio burst source in the outskirts of a quiescent galaxy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shah%2C+V">V. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+K">K. Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">C. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Fong%2C+W">W. Fong</a>, <a href="/search/astro-ph?searchtype=author&query=Eftekhari%2C+T">T. Eftekhari</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">B. C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Andrew%2C+S">S. Andrew</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">M. Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">C. Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">T. Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chatterjee%2C+S">S. Chatterjee</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">A. P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">M. Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+Y">Y. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">F. A. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">E. Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">M. Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hessels%2C+J+W+T">J. W. T. Hessels</a>, <a href="/search/astro-ph?searchtype=author&query=Ibik%2C+A+L">A. L. Ibik</a>, <a href="/search/astro-ph?searchtype=author&query=Jain%2C+N">N. Jain</a>, <a href="/search/astro-ph?searchtype=author&query=Joseph%2C+R+C">R. C. Joseph</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J">J. Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Kahinga%2C+L+A">L. A. Kahinga</a> , et al. (24 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="2410.23374v1-abstract-short" style="display: inline;"> We report the discovery of the repeating fast radio burst source FRB 20240209A using the CHIME/FRB telescope. We have detected 22 bursts from this repeater between February and July 2024, six of which were also recorded at the Outrigger station KKO. The 66-km long CHIME-KKO baseline can provide single-pulse FRB localizations along one dimension with $2^{\prime\prime}$ accuracy. The high declinatio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23374v1-abstract-full').style.display = 'inline'; document.getElementById('2410.23374v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.23374v1-abstract-full" style="display: none;"> We report the discovery of the repeating fast radio burst source FRB 20240209A using the CHIME/FRB telescope. We have detected 22 bursts from this repeater between February and July 2024, six of which were also recorded at the Outrigger station KKO. The 66-km long CHIME-KKO baseline can provide single-pulse FRB localizations along one dimension with $2^{\prime\prime}$ accuracy. The high declination of $\sim$86 degrees for this repeater allowed its detection with a rotating range of baseline vectors, enabling the combined localization region size to be constrained to $1^{\prime\prime}\times2^{\prime\prime}$. We present deep Gemini observations that, combined with the FRB localization, enabled a robust association of FRB 20240209A to the outskirts of a luminous galaxy (P(O|x) = 0.99; $L \approx 5.3 \times 10^{10}\,L_{\odot}$). FRB 20240209A has a projected physical offset of $40 \pm 5$ kpc from the center of its host galaxy, making it the FRB with the largest host galaxy offset to date. When normalized by the host galaxy size, the offset of FRB 20240209A is comparable to that of FRB 20200120E, the only FRB source known to originate in a globular cluster. We consider several explanations for the large offset, including a progenitor that was kicked from the host galaxy or in situ formation in a low-luminosity satellite galaxy of the putative host, but find the most plausible scenario to be a globular cluster origin. This, coupled with the quiescent, elliptical nature of the host as demonstrated in our companion paper, provide strong evidence for a delayed formation channel for the progenitor of the FRB source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.23374v1-abstract-full').style.display = 'none'; document.getElementById('2410.23374v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 October, 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">Submitted to AAS Journals</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. (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="2410.12089v3-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('2410.12089v3-abstract-full').style.display = 'inline'; document.getElementById('2410.12089v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.12089v3-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('2410.12089v3-abstract-full').style.display = 'none'; document.getElementById('2410.12089v3-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 February, 2025; <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. Visit bicepkeck.org for figure pdfs/pngs</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/2408.10444">arXiv:2408.10444</a> <span> [<a href="https://arxiv.org/pdf/2408.10444">pdf</a>, <a href="https://arxiv.org/format/2408.10444">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"> In-Flight Performance of Spider's 280 GHz Receivers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shaw%2C+E+C">Elle C. Shaw</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=Akers%2C+S">S. Akers</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J">J. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J">J. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+D+T">D. T. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Benton%2C+S+J">S. J. Benton</a>, <a href="/search/astro-ph?searchtype=author&query=Bergman%2C+A+S">A. S. Bergman</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=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+S+A">S. A. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+H+C">H. C. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Contaldi%2C+C+R">C. R. Contaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Domagalski%2C+R+S">R. S. Domagalski</a>, <a href="/search/astro-ph?searchtype=author&query=Dor%C3%A9%2C+O">O. Dor茅</a>, <a href="/search/astro-ph?searchtype=author&query=Duff%2C+S+M">S. M. Duff</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">A. J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">H. K. Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Farhang%2C+M">M. Farhang</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=Fissel%2C+L+M">L. M. Fissel</a>, <a href="/search/astro-ph?searchtype=author&query=Fraisse%2C+A+A">A. A. Fraisse</a>, <a href="/search/astro-ph?searchtype=author&query=Freese%2C+K">K. Freese</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+M">M. Galloway</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="2408.10444v1-abstract-short" style="display: inline;"> SPIDER is a balloon-borne instrument designed to map the cosmic microwave background at degree-angular scales in the presence of Galactic foregrounds. SPIDER has mapped a large sky area in the Southern Hemisphere using more than 2000 transition-edge sensors (TESs) during two NASA Long Duration Balloon flights above the Antarctic continent. During its first flight in January 2015, SPIDER observed i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10444v1-abstract-full').style.display = 'inline'; document.getElementById('2408.10444v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.10444v1-abstract-full" style="display: none;"> SPIDER is a balloon-borne instrument designed to map the cosmic microwave background at degree-angular scales in the presence of Galactic foregrounds. SPIDER has mapped a large sky area in the Southern Hemisphere using more than 2000 transition-edge sensors (TESs) during two NASA Long Duration Balloon flights above the Antarctic continent. During its first flight in January 2015, SPIDER observed in the 95 GHz and 150 GHz frequency bands, setting constraints on the B-mode signature of primordial gravitational waves. Its second flight in the 2022-23 season added new receivers at 280 GHz, each using an array of TESs coupled to the sky through feedhorns formed from stacks of silicon wafers. These receivers are optimized to produce deep maps of polarized Galactic dust emission over a large sky area, providing a unique data set with lasting value to the field. In this work, we describe the instrument's performance during SPIDER's second flight. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10444v1-abstract-full').style.display = 'none'; document.getElementById('2408.10444v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 19 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to SPIE Astronomical Telescopes + Instrumentation 2024, JATIS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.00172">arXiv:2408.00172</a> <span> [<a href="https://arxiv.org/pdf/2408.00172">pdf</a>, <a href="https://arxiv.org/format/2408.00172">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/10.3847/1538-4357/ad8133">10.3847/1538-4357/ad8133 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Holographic Beam Measurements of the Canadian Hydrogen Intensity Mapping Experiment (CHIME) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Chakraborty%2C+A">Arnab Chakraborty</a>, <a href="/search/astro-ph?searchtype=author&query=Foreman%2C+S">Simon Foreman</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">Mark Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+A+S">Alex S Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hinshaw%2C+G">Gary Hinshaw</a>, <a href="/search/astro-ph?searchtype=author&query=Landecker%2C+T+L">T. L. Landecker</a>, <a href="/search/astro-ph?searchtype=author&query=MacEachern%2C+J">Joshua MacEachern</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">Kiyoshi W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Milutinovic%2C+N">Nikola Milutinovic</a>, <a href="/search/astro-ph?searchtype=author&query=Newburgh%2C+L">Laura Newburgh</a>, <a href="/search/astro-ph?searchtype=author&query=Ordog%2C+A">Anna Ordog</a>, <a href="/search/astro-ph?searchtype=author&query=Pen%2C+U">Ue-Li Pen</a>, <a href="/search/astro-ph?searchtype=author&query=Pinsonneault-Marotte%2C+T">Tristan Pinsonneault-Marotte</a>, <a href="/search/astro-ph?searchtype=author&query=Reda%2C+A">Alex Reda</a>, <a href="/search/astro-ph?searchtype=author&query=Siegel%2C+S+R">Seth R. Siegel</a>, <a href="/search/astro-ph?searchtype=author&query=Singh%2C+S">Saurabh Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Haochen Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wulf%2C+D">Dallas Wulf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.00172v1-abstract-short" style="display: inline;"> We present the first results of the holographic beam mapping program for the Canadian Hydrogen Intensity Mapping Experiment (CHIME). We describe the implementation of the holographic technique as adapted for CHIME, and introduce the processing pipeline which prepares the raw holographic timestreams for analysis of beam features. We use data from six bright sources across the full 400-800\,MHz obse… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.00172v1-abstract-full').style.display = 'inline'; document.getElementById('2408.00172v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.00172v1-abstract-full" style="display: none;"> We present the first results of the holographic beam mapping program for the Canadian Hydrogen Intensity Mapping Experiment (CHIME). We describe the implementation of the holographic technique as adapted for CHIME, and introduce the processing pipeline which prepares the raw holographic timestreams for analysis of beam features. We use data from six bright sources across the full 400-800\,MHz observing band of CHIME to provide measurements of the co-polar and cross-polar beam response of CHIME in both amplitude and phase for the 1024 dual-polarized feeds instrumented on CHIME. In addition, we present comparisons with independent probes of the CHIME beam which indicate the presence of polarized beam leakage in CHIME. Holographic measurements of the CHIME beam have already been applied in science with CHIME, e.g. in estimating detection significance of far sidelobe FRBs, and in validating the beam models used for CHIME's first detections of \tcm emission (in cross-correlation with measurements of large-scale structure from galaxy surveys and the Lyman-$伪$ forest). Measurements presented in this paper, and future holographic results, will provide a unique data set to characterize the CHIME beam and improve the experiment's prospects for a detection of BAO. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.00172v1-abstract-full').style.display = 'none'; document.getElementById('2408.00172v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">submitted to ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 976 163 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.20982">arXiv:2407.20982</a> <span> [<a href="https://arxiv.org/pdf/2407.20982">pdf</a>, <a href="https://arxiv.org/format/2407.20982">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> <p class="title is-5 mathjax"> Analysis of Polarized Dust Emission from the First Flight of the SPIDER Balloon-Borne Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=SPIDER+Collaboration"> SPIDER Collaboration</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=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Benton%2C+S+J">S. J. Benton</a>, <a href="/search/astro-ph?searchtype=author&query=Bergman%2C+A+S">A. S. Bergman</a>, <a href="/search/astro-ph?searchtype=author&query=Bihary%2C+R">R. Bihary</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=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+J+A">J. A. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+S+A">S. A. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+H+C">H. C. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Contaldi%2C+C+R">C. R. Contaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Dor%C3%A9%2C+O">O. Dor茅</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">A. J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">H. K. Eriksen</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=Fraisse%2C+A+A">A. A. Fraisse</a>, <a href="/search/astro-ph?searchtype=author&query=Freese%2C+K">K. Freese</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+M">M. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Gambrel%2C+A+E">A. E. Gambrel</a>, <a href="/search/astro-ph?searchtype=author&query=Gandilo%2C+N+N">N. N. Gandilo</a>, <a href="/search/astro-ph?searchtype=author&query=Ganga%2C+K">K. Ganga</a>, <a href="/search/astro-ph?searchtype=author&query=Gourapura%2C+S">S. Gourapura</a>, <a href="/search/astro-ph?searchtype=author&query=Gualtieri%2C+R">R. Gualtieri</a>, <a href="/search/astro-ph?searchtype=author&query=Gudmundsson%2C+J+E">J. E. Gudmundsson</a> , et al. (45 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.20982v1-abstract-short" style="display: inline;"> Using data from the first flight of SPIDER and from Planck HFI, we probe the properties of polarized emission from interstellar dust in the SPIDER observing region. Component separation algorithms operating in both the spatial and harmonic domains are applied to probe their consistency and to quantify modeling errors associated with their assumptions. Analyses spanning the full SPIDER region demon… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20982v1-abstract-full').style.display = 'inline'; document.getElementById('2407.20982v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.20982v1-abstract-full" style="display: none;"> Using data from the first flight of SPIDER and from Planck HFI, we probe the properties of polarized emission from interstellar dust in the SPIDER observing region. Component separation algorithms operating in both the spatial and harmonic domains are applied to probe their consistency and to quantify modeling errors associated with their assumptions. Analyses spanning the full SPIDER region demonstrate that i) the spectral energy distribution of diffuse Galactic dust emission is broadly consistent with a modified-blackbody (MBB) model with a spectral index of $尾_\mathrm{d}=1.45\pm0.05$ $(1.47\pm0.06)$ for $E$ ($B$)-mode polarization, slightly lower than that reported by Planck for the full sky; ii) its angular power spectrum is broadly consistent with a power law; and iii) there is no significant detection of line-of-sight decorrelation of the astrophysical polarization. The size of the SPIDER region further allows for a statistically meaningful analysis of the variation in foreground properties within it. Assuming a fixed dust temperature $T_\mathrm{d}=19.6$ K, an analysis of two independent sub-regions of that field results in inferred values of $尾_\mathrm{d}=1.52\pm0.06$ and $尾_\mathrm{d}=1.09\pm0.09$, which are inconsistent at the $3.9\,蟽$ level. Furthermore, a joint analysis of SPIDER and Planck 217 and 353 GHz data within a subset of the SPIDER region is inconsistent with a simple MBB at more than $3\,蟽$, assuming a common morphology of polarized dust emission over the full range of frequencies. These modeling uncertainties have a small--but non-negligible--impact on limits on the cosmological tensor-to-scalar ratio derived from the \spider dataset. The fidelity of the component separation approaches of future CMB polarization experiments may thus have a significant impact on their constraining power. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20982v1-abstract-full').style.display = 'none'; document.getElementById('2407.20982v1-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 15 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2402.07898">arXiv:2402.07898</a> <span> [<a href="https://arxiv.org/pdf/2402.07898">pdf</a>, <a href="https://arxiv.org/format/2402.07898">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"> CHIME/FRB Outriggers: KKO Station System and Commissioning Results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lanman%2C+A+E">Adam E. Lanman</a>, <a href="/search/astro-ph?searchtype=author&query=Andrew%2C+S">Shion Andrew</a>, <a href="/search/astro-ph?searchtype=author&query=Lazda%2C+M">Mattias Lazda</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+V">Vishwangi Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Balasubramanian%2C+A">Arvind Balasubramanian</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Carlson%2C+M">Mark Carlson</a>, <a href="/search/astro-ph?searchtype=author&query=Cliche%2C+J">Jean-Fran莽ois Cliche</a>, <a href="/search/astro-ph?searchtype=author&query=Gusinskaia%2C+N">Nina Gusinskaia</a>, <a href="/search/astro-ph?searchtype=author&query=Hendricksen%2C+I+T">Ian T. Hendricksen</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J+F">J. F. Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Landecker%2C+T">Tom Landecker</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">Calvin Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Mckinven%2C+R">Ryan Mckinven</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Milutinovic%2C+N">Nikola Milutinovic</a>, <a href="/search/astro-ph?searchtype=author&query=Nimmo%2C+K">Kenzie Nimmo</a>, <a href="/search/astro-ph?searchtype=author&query=Pearlman%2C+A+B">Aaron B. Pearlman</a>, <a href="/search/astro-ph?searchtype=author&query=Renard%2C+A">Andre Renard</a>, <a href="/search/astro-ph?searchtype=author&query=Rahman%2C+M">Mubdi Rahman</a>, <a href="/search/astro-ph?searchtype=author&query=Shaw%2C+J+R">J. Richard Shaw</a>, <a href="/search/astro-ph?searchtype=author&query=Siegel%2C+S+R">Seth R. Siegel</a> , et al. (21 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="2402.07898v2-abstract-short" style="display: inline;"> Localizing fast radio bursts (FRBs) to their host galaxies is an essential step to better understanding their origins and using them as cosmic probes. The CHIME/FRB Outrigger program aims to add VLBI-localization capabilities to CHIME, such that FRBs may be localized to tens of milliarcsecond precision at the time of their discovery, more than sufficient for host galaxy identification. The first-b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07898v2-abstract-full').style.display = 'inline'; document.getElementById('2402.07898v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.07898v2-abstract-full" style="display: none;"> Localizing fast radio bursts (FRBs) to their host galaxies is an essential step to better understanding their origins and using them as cosmic probes. The CHIME/FRB Outrigger program aims to add VLBI-localization capabilities to CHIME, such that FRBs may be localized to tens of milliarcsecond precision at the time of their discovery, more than sufficient for host galaxy identification. The first-built outrigger telescope is KKO, located 66 kilometers west of CHIME. Cross-correlating KKO with CHIME can achieve arcsecond-scale localization in right ascension while avoiding the worst effects of the ionosphere. This paper presents measurements of KKO's performance throughout its commissioning phase, as well as a summary of its design and function. We demonstrate KKO's capabilities as a standalone instrument by producing full-sky images, mapping the angular and frequency structure of the primary beam, and measuring feed positions. To demonstrate the localization capabilities of the CHIME -- KKO baseline, we collected five separate observations each for a set of twenty bright pulsars, and aimed to measure their positions to within 5~arcseconds. All of these pulses were successfully localized to within this specification. The next two outriggers are expected to be commissioned in 2024, and will enable subarcsecond localizations for approximately hundreds of FRBs each year. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07898v2-abstract-full').style.display = 'none'; document.getElementById('2402.07898v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">41 pages, 17 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.00111">arXiv:2311.00111</a> <span> [<a href="https://arxiv.org/pdf/2311.00111">pdf</a>, <a href="https://arxiv.org/format/2311.00111">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Updating the first CHIME/FRB catalog of fast radio bursts with baseband data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+C">The CHIME/FRB Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">Bridget C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Andrew%2C+S">Shion Andrew</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Breitman%2C+D">Daniela Breitman</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A+M">Amanda M. Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+A">Fengqiu Adam Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Eadie%2C+G">Gwendolyn Eadie</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Gaensler%2C+B+M">B. M. Gaensler</a>, <a href="/search/astro-ph?searchtype=author&query=Giri%2C+U">Utkarsh Giri</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera-Martin%2C+A">Antonio Herrera-Martin</a>, <a href="/search/astro-ph?searchtype=author&query=Hopkins%2C+H">Hans Hopkins</a>, <a href="/search/astro-ph?searchtype=author&query=Ibik%2C+A+L">Adaeze L. Ibik</a>, <a href="/search/astro-ph?searchtype=author&query=Joseph%2C+R+C">Ronniy C. Joseph</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J+F">J. F. Kaczmarek</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.00111v2-abstract-short" style="display: inline;"> In 2021, a catalog of 536 fast radio bursts (FRBs) detected with the Canadian Hydrogen Intensity Mapping Experiment (CHIME) radio telescope was released by the CHIME/FRB Collaboration. This large collection of bursts, observed with a single instrument and uniform selection effects, has advanced our understanding of the FRB population. Here we update the results for 140 of these FRBs for which chan… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00111v2-abstract-full').style.display = 'inline'; document.getElementById('2311.00111v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.00111v2-abstract-full" style="display: none;"> In 2021, a catalog of 536 fast radio bursts (FRBs) detected with the Canadian Hydrogen Intensity Mapping Experiment (CHIME) radio telescope was released by the CHIME/FRB Collaboration. This large collection of bursts, observed with a single instrument and uniform selection effects, has advanced our understanding of the FRB population. Here we update the results for 140 of these FRBs for which channelized raw voltage ('baseband') data are available. With the voltages measured by the telescope's antennas, it is possible to maximize the telescope sensitivity in any direction within the primary beam, an operation called 'beamforming'. This allows us to increase the signal-to-noise ratio (S/N) of the bursts and to localize them to sub-arcminute precision. The improved localization is also used to correct the beam response of the instrument and to measure fluxes and fluences with a ~10% uncertainty. Additionally, the time resolution is increased by three orders of magnitude relative to that in the first CHIME/FRB catalog, and, applying coherent dedispersion, burst morphologies can be studied in detail. Polarization information is also available for the full sample of 140 FRBs, providing an unprecedented dataset to study the polarization properties of the population. We release the baseband data beamformed to the most probable position of each FRB. These data are analyzed in detail in a series of accompanying papers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00111v2-abstract-full').style.display = 'none'; document.getElementById('2311.00111v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 31 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.10849">arXiv:2310.10849</a> <span> [<a href="https://arxiv.org/pdf/2310.10849">pdf</a>, <a href="https://arxiv.org/format/2310.10849">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10909-024-03100-6">10.1007/s10909-024-03100-6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Results and Limits of Time Division Multiplexing for the BICEP Array High Frequency Receivers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</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=Cheshire%2C+J">J. 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+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=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>, <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> , 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="2310.10849v2-abstract-short" style="display: inline;"> Time-Division Multiplexing is the readout architecture of choice for many ground and space experiments, as it is a very mature technology with proven outstanding low-frequency noise stability, which represents a central challenge in multiplexing. Once fully populated, each of the two BICEP Array high frequency receivers, observing at 150GHz and 220/270GHz, will have 7776 TES detectors tiled on the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.10849v2-abstract-full').style.display = 'inline'; document.getElementById('2310.10849v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.10849v2-abstract-full" style="display: none;"> Time-Division Multiplexing is the readout architecture of choice for many ground and space experiments, as it is a very mature technology with proven outstanding low-frequency noise stability, which represents a central challenge in multiplexing. Once fully populated, each of the two BICEP Array high frequency receivers, observing at 150GHz and 220/270GHz, will have 7776 TES detectors tiled on the focal plane. The constraints set by these two receivers required a redesign of the warm readout electronics. The new version of the standard Multi Channel Electronics, developed and built at the University of British Columbia, is presented here for the first time. BICEP Array operates Time Division Multiplexing readout technology to the limits of its capabilities in terms of multiplexing rate, noise and crosstalk, and applies them in rigorously demanding scientific application requiring extreme noise performance and systematic error control. Future experiments like CMB-S4 plan to use TES bolometers with Time Division/SQUID-based readout for an even larger number of detectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.10849v2-abstract-full').style.display = 'none'; document.getElementById('2310.10849v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 7 figures, Submitted to Journal of Low Temperature Physics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Low Temperature Physics (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.04404">arXiv:2309.04404</a> <span> [<a href="https://arxiv.org/pdf/2309.04404">pdf</a>, <a href="https://arxiv.org/format/2309.04404">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"> A Detection of Cosmological 21 cm Emission from CHIME in Cross-correlation with eBOSS Measurements of the Lyman-$伪$ Forest </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=CHIME+Collaboration"> CHIME Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Chakraborty%2C+A">Arnab Chakraborty</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Fandino%2C+M">Mateus Fandino</a>, <a href="/search/astro-ph?searchtype=author&query=Foreman%2C+S">Simon Foreman</a>, <a href="/search/astro-ph?searchtype=author&query=Gan%2C+H">Hyoyin Gan</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">Mark Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+A+S">Alex S. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hinshaw%2C+G">Gary Hinshaw</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%B6fer%2C+C">Carolin H枚fer</a>, <a href="/search/astro-ph?searchtype=author&query=Landecker%2C+T+L">T. L. Landecker</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zack Li</a>, <a href="/search/astro-ph?searchtype=author&query=MacEachern%2C+J">Joshua MacEachern</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K">Kiyoshi Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Milutinovic%2C+N">Nikola Milutinovic</a>, <a href="/search/astro-ph?searchtype=author&query=Mirhosseini%2C+A">Arash Mirhosseini</a>, <a href="/search/astro-ph?searchtype=author&query=Newburgh%2C+L">Laura Newburgh</a>, <a href="/search/astro-ph?searchtype=author&query=Ordog%2C+A">Anna Ordog</a>, <a href="/search/astro-ph?searchtype=author&query=Paul%2C+S">Sourabh Paul</a>, <a href="/search/astro-ph?searchtype=author&query=Pen%2C+U">Ue-Li Pen</a>, <a href="/search/astro-ph?searchtype=author&query=Pinsonneault-Marotte%2C+T">Tristan Pinsonneault-Marotte</a>, <a href="/search/astro-ph?searchtype=author&query=Reda%2C+A">Alex Reda</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.04404v1-abstract-short" style="display: inline;"> We report the detection of 21 cm emission at an average redshift $\bar{z} = 2.3$ in the cross-correlation of data from the Canadian Hydrogen Intensity Mapping Experiment (CHIME) with measurements of the Lyman-$伪$ forest from eBOSS. Data collected by CHIME over 88 days in the $400-500$~MHz frequency band ($1.8 < z < 2.5$) are formed into maps of the sky and high-pass delay filtered to suppress the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.04404v1-abstract-full').style.display = 'inline'; document.getElementById('2309.04404v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.04404v1-abstract-full" style="display: none;"> We report the detection of 21 cm emission at an average redshift $\bar{z} = 2.3$ in the cross-correlation of data from the Canadian Hydrogen Intensity Mapping Experiment (CHIME) with measurements of the Lyman-$伪$ forest from eBOSS. Data collected by CHIME over 88 days in the $400-500$~MHz frequency band ($1.8 < z < 2.5$) are formed into maps of the sky and high-pass delay filtered to suppress the foreground power, corresponding to removing cosmological scales with $k_\parallel \lesssim 0.13\ \text{Mpc}^{-1}$ at the average redshift. Line-of-sight spectra to the eBOSS background quasar locations are extracted from the CHIME maps and combined with the Lyman-$伪$ forest flux transmission spectra to estimate the 21 cm-Lyman-$伪$ cross-correlation function. Fitting a simulation-derived template function to this measurement results in a $9蟽$ detection significance. The coherent accumulation of the signal through cross-correlation is sufficient to enable a detection despite excess variance from foreground residuals $\sim6-10$ times brighter than the expected thermal noise level in the correlation function. These results are the highest-redshift measurement of \tcm emission to date, and set the stage for future 21 cm intensity mapping analyses at $z>1.8$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.04404v1-abstract-full').style.display = 'none'; document.getElementById('2309.04404v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.01258">arXiv:2307.01258</a> <span> [<a href="https://arxiv.org/pdf/2307.01258">pdf</a>, <a href="https://arxiv.org/format/2307.01258">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"> The Atacama Cosmology Telescope: High-resolution component-separated maps across one-third of the sky </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Coulton%2C+W+R">William R. Coulton</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">Adriaan J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+J+C">J. Colin Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Abril-Cabezas%2C+I">Irene Abril-Cabezas</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">Peter A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Aiola%2C+S">Simone Aiola</a>, <a href="/search/astro-ph?searchtype=author&query=Alford%2C+T">Tommy Alford</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Amodeo%2C+S">Stefania Amodeo</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+R">Rui An</a>, <a href="/search/astro-ph?searchtype=author&query=Atkins%2C+Z">Zachary Atkins</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J+E">Jason E. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">Elia Stefano Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J+A">James A. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Bean%2C+R">Rachel Bean</a>, <a href="/search/astro-ph?searchtype=author&query=Beringue%2C+B">Benjamin Beringue</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandarkar%2C+T">Tanay Bhandarkar</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+E">Emily Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Bolliet%2C+B">Boris Bolliet</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+H">Hongbo Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Calafut%2C+V">Victoria Calafut</a> , et al. (129 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.01258v1-abstract-short" style="display: inline;"> Observations of the millimeter sky contain valuable information on a number of signals, including the blackbody cosmic microwave background (CMB), Galactic emissions, and the Compton-$y$ distortion due to the thermal Sunyaev-Zel'dovich (tSZ) effect. Extracting new insight into cosmological and astrophysical questions often requires combining multi-wavelength observations to spectrally isolate one… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01258v1-abstract-full').style.display = 'inline'; document.getElementById('2307.01258v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.01258v1-abstract-full" style="display: none;"> Observations of the millimeter sky contain valuable information on a number of signals, including the blackbody cosmic microwave background (CMB), Galactic emissions, and the Compton-$y$ distortion due to the thermal Sunyaev-Zel'dovich (tSZ) effect. Extracting new insight into cosmological and astrophysical questions often requires combining multi-wavelength observations to spectrally isolate one component. In this work, we present a new arcminute-resolution Compton-$y$ map, which traces out the line-of-sight-integrated electron pressure, as well as maps of the CMB in intensity and E-mode polarization, across a third of the sky (around 13,000 sq.~deg.). We produce these through a joint analysis of data from the Atacama Cosmology Telescope (ACT) Data Release 4 and 6 at frequencies of roughly 93, 148, and 225 GHz, together with data from the \textit{Planck} satellite at frequencies between 30 GHz and 545 GHz. We present detailed verification of an internal linear combination pipeline implemented in a needlet frame that allows us to efficiently suppress Galactic contamination and account for spatial variations in the ACT instrument noise. These maps provide a significant advance, in noise levels and resolution, over the existing \textit{Planck} component-separated maps and will enable a host of science goals including studies of cluster and galaxy astrophysics, inferences of the cosmic velocity field, primordial non-Gaussianity searches, and gravitational lensing reconstruction of the CMB. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01258v1-abstract-full').style.display = 'none'; document.getElementById('2307.01258v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">The Compton-y map and associated products will be made publicly available upon publication of the paper. The CMB T and E mode maps will be made available when the DR6 maps are made public</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.05203">arXiv:2304.05203</a> <span> [<a href="https://arxiv.org/pdf/2304.05203">pdf</a>, <a href="https://arxiv.org/format/2304.05203">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 - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acff5f">10.3847/1538-4357/acff5f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: DR6 Gravitational Lensing Map and Cosmological Parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+F+J">Frank J. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Sherwin%2C+B+D">Blake D. Sherwin</a>, <a href="/search/astro-ph?searchtype=author&query=MacCrann%2C+N">Niall MacCrann</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yaqiong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Abril-Cabezas%2C+I">Irene Abril-Cabezas</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">Peter A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Aiola%2C+S">Simone Aiola</a>, <a href="/search/astro-ph?searchtype=author&query=Alford%2C+T">Tommy Alford</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Amodeo%2C+S">Stefania Amodeo</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+R">Rui An</a>, <a href="/search/astro-ph?searchtype=author&query=Atkins%2C+Z">Zachary Atkins</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J+E">Jason E. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">Elia Stefano Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J+A">James A. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Bean%2C+R">Rachel Bean</a>, <a href="/search/astro-ph?searchtype=author&query=Beringue%2C+B">Benjamin Beringue</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandarkar%2C+T">Tanay Bhandarkar</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+E">Emily Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Bolliet%2C+B">Boris Bolliet</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+H">Hongbo Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a> , et al. (134 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.05203v2-abstract-short" style="display: inline;"> We present cosmological constraints from a gravitational lensing mass map covering 9400 sq. deg. reconstructed from CMB measurements made by the Atacama Cosmology Telescope (ACT) from 2017 to 2021. In combination with BAO measurements (from SDSS and 6dF), we obtain the amplitude of matter fluctuations $蟽_8 = 0.819 \pm 0.015$ at 1.8% precision, $S_8\equiv蟽_8({惟_{\rm m}}/0.3)^{0.5}=0.840\pm0.028$ an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.05203v2-abstract-full').style.display = 'inline'; document.getElementById('2304.05203v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.05203v2-abstract-full" style="display: none;"> We present cosmological constraints from a gravitational lensing mass map covering 9400 sq. deg. reconstructed from CMB measurements made by the Atacama Cosmology Telescope (ACT) from 2017 to 2021. In combination with BAO measurements (from SDSS and 6dF), we obtain the amplitude of matter fluctuations $蟽_8 = 0.819 \pm 0.015$ at 1.8% precision, $S_8\equiv蟽_8({惟_{\rm m}}/0.3)^{0.5}=0.840\pm0.028$ and the Hubble constant $H_0= (68.3 \pm 1.1)\, \text{km}\,\text{s}^{-1}\,\text{Mpc}^{-1}$ at 1.6% precision. A joint constraint with CMB lensing measured by the Planck satellite yields even more precise values: $蟽_8 = 0.812 \pm 0.013$, $S_8\equiv蟽_8({惟_{\rm m}}/0.3)^{0.5}=0.831\pm0.023$ and $H_0= (68.1 \pm 1.0)\, \text{km}\,\text{s}^{-1}\,\text{Mpc}^{-1}$. These measurements agree well with $螞$CDM-model extrapolations from the CMB anisotropies measured by Planck. To compare these constraints to those from the KiDS, DES, and HSC galaxy surveys, we revisit those data sets with a uniform set of assumptions, and find $S_8$ from all three surveys are lower than that from ACT+Planck lensing by varying levels ranging from 1.7-2.1$蟽$. These results motivate further measurements and comparison, not just between the CMB anisotropies and galaxy lensing, but also between CMB lensing probing $z\sim 0.5-5$ on mostly-linear scales and galaxy lensing at $z\sim 0.5$ on smaller scales. We combine our CMB lensing measurements with CMB anisotropies to constrain extensions of $螞$CDM, limiting the sum of the neutrino masses to $\sum m_谓 < 0.13$ eV (95% c.l.), for example. Our results provide independent confirmation that the universe is spatially flat, conforms with general relativity, and is described remarkably well by the $螞$CDM model, while paving a promising path for neutrino physics with gravitational lensing from upcoming ground-based CMB surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.05203v2-abstract-full').style.display = 'none'; document.getElementById('2304.05203v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">32 pages, 17 figures, replaced with version accepted in ApJ (Feb 2024). Cosmological likelihood data and mass maps are public here: https://lambda.gsfc.nasa.gov/product/act/actadv_prod_table.html ; likelihood software is here: https://github.com/ACTCollaboration/act_dr6_lenslike . Also see companion papers Qu et al and MacCrann et al</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, Volume 962, 2024, Page 113 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.05202">arXiv:2304.05202</a> <span> [<a href="https://arxiv.org/pdf/2304.05202">pdf</a>, <a href="https://arxiv.org/format/2304.05202">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/acfe06">10.3847/1538-4357/acfe06 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: A Measurement of the DR6 CMB Lensing Power Spectrum and its Implications for Structure Growth </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Qu%2C+F+J">Frank J. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Sherwin%2C+B+D">Blake D. Sherwin</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Han%2C+D">Dongwon Han</a>, <a href="/search/astro-ph?searchtype=author&query=Crowley%2C+K+T">Kevin T. Crowley</a>, <a href="/search/astro-ph?searchtype=author&query=Abril-Cabezas%2C+I">Irene Abril-Cabezas</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">Peter A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Aiola%2C+S">Simone Aiola</a>, <a href="/search/astro-ph?searchtype=author&query=Alford%2C+T">Tommy Alford</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Amodeo%2C+S">Stefania Amodeo</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+R">Rui An</a>, <a href="/search/astro-ph?searchtype=author&query=Atkins%2C+Z">Zachary Atkins</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J+E">Jason E. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">Elia Stefano Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J+A">James A. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Bean%2C+R">Rachel Bean</a>, <a href="/search/astro-ph?searchtype=author&query=Beringue%2C+B">Benjamin Beringue</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandarkar%2C+T">Tanay Bhandarkar</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+E">Emily Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Bolliet%2C+B">Boris Bolliet</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+H">Hongbo Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a> , et al. (133 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.05202v2-abstract-short" style="display: inline;"> We present new measurements of cosmic microwave background (CMB) lensing over $9400$ sq. deg. of the sky. These lensing measurements are derived from the Atacama Cosmology Telescope (ACT) Data Release 6 (DR6) CMB dataset, which consists of five seasons of ACT CMB temperature and polarization observations. We determine the amplitude of the CMB lensing power spectrum at $2.3\%$ precision ($43蟽$ sign… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.05202v2-abstract-full').style.display = 'inline'; document.getElementById('2304.05202v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.05202v2-abstract-full" style="display: none;"> We present new measurements of cosmic microwave background (CMB) lensing over $9400$ sq. deg. of the sky. These lensing measurements are derived from the Atacama Cosmology Telescope (ACT) Data Release 6 (DR6) CMB dataset, which consists of five seasons of ACT CMB temperature and polarization observations. We determine the amplitude of the CMB lensing power spectrum at $2.3\%$ precision ($43蟽$ significance) using a novel pipeline that minimizes sensitivity to foregrounds and to noise properties. To ensure our results are robust, we analyze an extensive set of null tests, consistency tests, and systematic error estimates and employ a blinded analysis framework. The baseline spectrum is well fit by a lensing amplitude of $A_{\mathrm{lens}}=1.013\pm0.023$ relative to the Planck 2018 CMB power spectra best-fit $螞$CDM model and $A_{\mathrm{lens}}=1.005\pm0.023$ relative to the $\text{ACT DR4} + \text{WMAP}$ best-fit model. From our lensing power spectrum measurement, we derive constraints on the parameter combination $S^{\mathrm{CMBL}}_8 \equiv 蟽_8 \left({惟_m}/{0.3}\right)^{0.25}$ of $S^{\mathrm{CMBL}}_8= 0.818\pm0.022$ from ACT DR6 CMB lensing alone and $S^{\mathrm{CMBL}}_8= 0.813\pm0.018$ when combining ACT DR6 and Planck NPIPE CMB lensing power spectra. These results are in excellent agreement with $螞$CDM model constraints from Planck or $\text{ACT DR4} + \text{WMAP}$ CMB power spectrum measurements. Our lensing measurements from redshifts $z\sim0.5$--$5$ are thus fully consistent with $螞$CDM structure growth predictions based on CMB anisotropies probing primarily $z\sim1100$. We find no evidence for a suppression of the amplitude of cosmic structure at low redshifts <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.05202v2-abstract-full').style.display = 'none'; document.getElementById('2304.05202v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">45+22 pages, 50 figures. v2 matches with published version in ApJ. Cosmological likelihood data and lensing maps are here: https://lambda.gsfc.nasa.gov/product/act/actadv_prod_table.html ; likelihood software is here: https://github.com/ACTCollaboration/act_dr6_lenslike . Also see companion papers Madhavacheril et al and MacCrann et al</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-23-237-PPD </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/2208.02755">arXiv:2208.02755</a> <span> [<a href="https://arxiv.org/pdf/2208.02755">pdf</a>, <a href="https://arxiv.org/format/2208.02755">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"> Thermal Testing for Cryogenic CMB Instrument Optical Design </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Goldfinger%2C+D+C">D. C. Goldfinger</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">J. 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+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=Grayson%2C+J">J. Grayson</a>, <a href="/search/astro-ph?searchtype=author&query=Grimes%2C+P+K">P. K. Grimes</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="2208.02755v1-abstract-short" style="display: inline;"> Observations of the Cosmic Microwave Background rely on cryogenic instrumentation with cold detectors, readout, and optics providing the low noise performance and instrumental stability required to make more sensitive measurements. It is therefore critical to optimize all aspects of the cryogenic design to achieve the necessary performance, with low temperature components and acceptable system coo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.02755v1-abstract-full').style.display = 'inline'; document.getElementById('2208.02755v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.02755v1-abstract-full" style="display: none;"> Observations of the Cosmic Microwave Background rely on cryogenic instrumentation with cold detectors, readout, and optics providing the low noise performance and instrumental stability required to make more sensitive measurements. It is therefore critical to optimize all aspects of the cryogenic design to achieve the necessary performance, with low temperature components and acceptable system cooling requirements. In particular, we will focus on our use of thermal filters and cold optics, which reduce the thermal load passed along to the cryogenic stages. To test their performance, we have made a series of in situ measurements while integrating the third receiver for the BICEP Array telescope. In addition to characterizing the behavior of this receiver, these measurements continue to refine the models that are being used to inform design choices being made for future instruments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.02755v1-abstract-full').style.display = 'none'; document.getElementById('2208.02755v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 8 figures, Proceedings of SPIE 2022</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2208.01080">arXiv:2208.01080</a> <span> [<a href="https://arxiv.org/pdf/2208.01080">pdf</a>, <a href="https://arxiv.org/format/2208.01080">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"> 2022 Upgrade and Improved Low Frequency Camera Sensitivity for CMB Observation at the South Pole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Soliman%2C+A">A. Soliman</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=Cheshire%2C+J">J. 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+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="2208.01080v1-abstract-short" style="display: inline;"> Constraining the Galactic foregrounds with multi-frequency Cosmic Microwave Background (CMB) observations is an essential step towards ultimately reaching the sensitivity to measure primordial gravitational waves (PGWs), the sign of inflation after the Big-Bang that would be imprinted on the CMB. The BICEP Array telescope is a set of multi-frequency cameras designed to constrain the energy scale o… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01080v1-abstract-full').style.display = 'inline'; document.getElementById('2208.01080v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2208.01080v1-abstract-full" style="display: none;"> Constraining the Galactic foregrounds with multi-frequency Cosmic Microwave Background (CMB) observations is an essential step towards ultimately reaching the sensitivity to measure primordial gravitational waves (PGWs), the sign of inflation after the Big-Bang that would be imprinted on the CMB. The BICEP Array telescope is a set of multi-frequency cameras designed to constrain the energy scale of inflation through CMB B-mode searches while also controlling the polarized galactic foregrounds. The lowest frequency BICEP Array receiver (BA1) has been observing from the South Pole since 2020 and provides 30 GHz and 40 GHz data to characterize the Galactic synchrotron in our CMB maps. In this paper, we present the design of the BA1 detectors and the full optical characterization of the camera including the on-sky performance at the South Pole. The paper also introduces the design challenges during the first observing season including the effect of out-of-band photons on detectors performance. It also describes the tests done to diagnose that effect and the new upgrade to minimize these photons, as well as installing more dichroic detectors during the 2022 deployment season to improve the BA1 sensitivity. We finally report background noise measurements of the detectors with the goal of having photon noise dominated detectors in both optical channels. BA1 achieves an improvement in mapping speed compared to the previous deployment season. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2208.01080v1-abstract-full').style.display = 'none'; document.getElementById('2208.01080v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Proceedings of SPIE Astronomical Telescopes + Instrumentation 2022 (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/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/2207.13876">arXiv:2207.13876</a> <span> [<a href="https://arxiv.org/pdf/2207.13876">pdf</a>, <a href="https://arxiv.org/format/2207.13876">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"> Characterization of the John A. Galt telescope for radio holography with CHIME </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Reda%2C+A">Alex Reda</a>, <a href="/search/astro-ph?searchtype=author&query=Pinsonneault-Marotte%2C+T">Tristan Pinsonneault-Marotte</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+M">Meiling Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Chakraborty%2C+A">Arnab Chakraborty</a>, <a href="/search/astro-ph?searchtype=author&query=Foreman%2C+S">Simon Foreman</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">Mark Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+A+S">Alex S. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%B6fer%2C+C">Carolin H枚fer</a>, <a href="/search/astro-ph?searchtype=author&query=Kania%2C+J">Joseph Kania</a>, <a href="/search/astro-ph?searchtype=author&query=Landecker%2C+T+L">T. L. Landecker</a>, <a href="/search/astro-ph?searchtype=author&query=MacEachern%2C+J">Joshua MacEachern</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K">Kiyoshi Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Milutinovic%2C+N">Nikola Milutinovic</a>, <a href="/search/astro-ph?searchtype=author&query=Newburgh%2C+L">Laura Newburgh</a>, <a href="/search/astro-ph?searchtype=author&query=Ordog%2C+A">Anna Ordog</a>, <a href="/search/astro-ph?searchtype=author&query=Paul%2C+S">Sourabh Paul</a>, <a href="/search/astro-ph?searchtype=author&query=Shaw%2C+J+R">J. Richard Shaw</a>, <a href="/search/astro-ph?searchtype=author&query=Siegel%2C+S+R">Seth R. Siegel</a>, <a href="/search/astro-ph?searchtype=author&query=Smegal%2C+R">Rick Smegal</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+H">Haochen Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wulf%2C+D">Dallas Wulf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2207.13876v3-abstract-short" style="display: inline;"> The Canadian Hydrogen Intensity Mapping Experiment (CHIME) will measure the 21 cm emission of astrophysical neutral hydrogen to probe large scale structure at redshifts z=0.8-2.5. However, detecting the 21 cm signal beneath substantially brighter foregrounds remains a key challenge. Due to the high dynamic range between 21 cm and foreground emission, an exquisite calibration of instrument systemat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13876v3-abstract-full').style.display = 'inline'; document.getElementById('2207.13876v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2207.13876v3-abstract-full" style="display: none;"> The Canadian Hydrogen Intensity Mapping Experiment (CHIME) will measure the 21 cm emission of astrophysical neutral hydrogen to probe large scale structure at redshifts z=0.8-2.5. However, detecting the 21 cm signal beneath substantially brighter foregrounds remains a key challenge. Due to the high dynamic range between 21 cm and foreground emission, an exquisite calibration of instrument systematics, notably the telescope beam, is required to successfully filter out the foregrounds. One technique being used to achieve a high fidelity measurement of the CHIME beam is radio holography, wherein signals from each of CHIME's analog inputs are correlated with the signal from a co-located reference antenna, the 26 m John A. Galt telescope, as the 26 m Galt telescope tracks a bright point source transiting over CHIME. In this work we present an analysis of several of the Galt telescope's properties. We employ driftscan measurements of several bright sources, along with background estimates derived from the 408 MHz Haslam map, to estimate the Galt system temperature. To determine the Galt telescope's beam shape, we perform and analyze a raster scan of the bright radio source Cassiopeia A. Finally, we use early holographic measurements to measure the Galt telescope's geometry with respect to CHIME for the holographic analysis of the CHIME and Galt interferometric data set. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2207.13876v3-abstract-full').style.display = 'none'; document.getElementById('2207.13876v3-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 September, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 July, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2022. </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/2203.08024">arXiv:2203.08024</a> <span> [<a href="https://arxiv.org/pdf/2203.08024">pdf</a>, <a href="https://arxiv.org/format/2203.08024">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</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> <p class="title is-5 mathjax"> Snowmass 2021 CMB-S4 White Paper </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abazajian%2C+K">Kevork Abazajian</a>, <a href="/search/astro-ph?searchtype=author&query=Abdulghafour%2C+A">Arwa Abdulghafour</a>, <a href="/search/astro-ph?searchtype=author&query=Addison%2C+G+E">Graeme E. Addison</a>, <a href="/search/astro-ph?searchtype=author&query=Adshead%2C+P">Peter Adshead</a>, <a href="/search/astro-ph?searchtype=author&query=Ahmed%2C+Z">Zeeshan Ahmed</a>, <a href="/search/astro-ph?searchtype=author&query=Ajello%2C+M">Marco Ajello</a>, <a href="/search/astro-ph?searchtype=author&query=Akerib%2C+D">Daniel Akerib</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+S+W">Steven W. Allen</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+D">David Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+M">Marcelo Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+M+A">Mustafa A. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+A">Adam Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Ansarinejad%2C+B">Behzad Ansarinejad</a>, <a href="/search/astro-ph?searchtype=author&query=Archipley%2C+M">Melanie Archipley</a>, <a href="/search/astro-ph?searchtype=author&query=Arnold%2C+K+S">Kam S. Arnold</a>, <a href="/search/astro-ph?searchtype=author&query=Ashby%2C+M">Matt Ashby</a>, <a href="/search/astro-ph?searchtype=author&query=Aung%2C+H">Han Aung</a>, <a href="/search/astro-ph?searchtype=author&query=Baccigalupi%2C+C">Carlo Baccigalupi</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+C">Carina Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Bakshi%2C+A">Abhishek Bakshi</a>, <a href="/search/astro-ph?searchtype=author&query=Bard%2C+D">Debbie Bard</a>, <a href="/search/astro-ph?searchtype=author&query=Barkats%2C+D">Denis Barkats</a>, <a href="/search/astro-ph?searchtype=author&query=Barron%2C+D">Darcy Barron</a>, <a href="/search/astro-ph?searchtype=author&query=Barry%2C+P+S">Peter S. Barry</a> , et al. (331 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="2203.08024v1-abstract-short" style="display: inline;"> This Snowmass 2021 White Paper describes the Cosmic Microwave Background Stage 4 project CMB-S4, which is designed to cross critical thresholds in our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. We provide an overview of the science case, the technical design, and project plan. </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.08024v1-abstract-full" style="display: none;"> This Snowmass 2021 White Paper describes the Cosmic Microwave Background Stage 4 project CMB-S4, which is designed to cross critical thresholds in our understanding of the origin and evolution of the Universe, from the highest energies at the dawn of time through the growth of structure to the present day. We provide an overview of the science case, the technical design, and project plan. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.08024v1-abstract-full').style.display = 'none'; document.getElementById('2203.08024v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Contribution to Snowmass 2021. arXiv admin note: substantial text overlap with arXiv:1908.01062, arXiv:1907.04473</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.01242">arXiv:2202.01242</a> <span> [<a href="https://arxiv.org/pdf/2202.01242">pdf</a>, <a href="https://arxiv.org/format/2202.01242">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/acb13f">10.3847/1538-4357/acb13f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Detection of Cosmological 21 cm Emission with the Canadian Hydrogen Intensity Mapping Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=CHIME+Collaboration"> CHIME Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T">Tianyue Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+M">Meiling Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Fandino%2C+M">Mateus Fandino</a>, <a href="/search/astro-ph?searchtype=author&query=Foreman%2C+S">Simon Foreman</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">Mark Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+A+S">Alex S. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hinshaw%2C+G">Gary Hinshaw</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%B6fer%2C+C">Carolin H枚fer</a>, <a href="/search/astro-ph?searchtype=author&query=Kania%2C+J">Joseph Kania</a>, <a href="/search/astro-ph?searchtype=author&query=Landecker%2C+T+L">T. L. Landecker</a>, <a href="/search/astro-ph?searchtype=author&query=MacEachern%2C+J">Joshua MacEachern</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K">Kiyoshi Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Milutinovic%2C+N">Nikola Milutinovic</a>, <a href="/search/astro-ph?searchtype=author&query=Mirhosseini%2C+A">Arash Mirhosseini</a>, <a href="/search/astro-ph?searchtype=author&query=Newburgh%2C+L">Laura Newburgh</a>, <a href="/search/astro-ph?searchtype=author&query=Ordog%2C+A">Anna Ordog</a>, <a href="/search/astro-ph?searchtype=author&query=Pen%2C+U">Ue-Li Pen</a>, <a href="/search/astro-ph?searchtype=author&query=Pinsonneault-Marotte%2C+T">Tristan Pinsonneault-Marotte</a>, <a href="/search/astro-ph?searchtype=author&query=Polzin%2C+A">Ava Polzin</a>, <a href="/search/astro-ph?searchtype=author&query=Reda%2C+A">Alex Reda</a> , et al. (8 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="2202.01242v1-abstract-short" style="display: inline;"> We present a detection of 21-cm emission from large-scale structure (LSS) between redshift 0.78 and 1.43 made with the Canadian Hydrogen Intensity Mapping Experiment (CHIME). Radio observations acquired over 102 nights are used to construct maps which are foreground filtered and stacked on the angular and spectral locations of luminous red galaxies (LRG), emission line galaxies (ELG), and quasars… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.01242v1-abstract-full').style.display = 'inline'; document.getElementById('2202.01242v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.01242v1-abstract-full" style="display: none;"> We present a detection of 21-cm emission from large-scale structure (LSS) between redshift 0.78 and 1.43 made with the Canadian Hydrogen Intensity Mapping Experiment (CHIME). Radio observations acquired over 102 nights are used to construct maps which are foreground filtered and stacked on the angular and spectral locations of luminous red galaxies (LRG), emission line galaxies (ELG), and quasars (QSO) from the eBOSS clustering catalogs. We find decisive evidence for a detection when stacking on all three tracers of LSS, with the logarithm of the Bayes Factor equal to 18.9 (LRG), 10.8 (ELG), and 56.3 (QSO). An alternative frequentist interpretation, based on the likelihood-ratio test, yields a detection significance of $7.1蟽$ (LRG), $5.7蟽$ (ELG), and $11.1蟽$ (QSO). These are the first 21-cm intensity mapping measurements made with an interferometer. We constrain the effective clustering amplitude of neutral hydrogen (HI), defined as $\mathcal{A}_{\rm HI}\equiv 10^{3}\,惟_\mathrm{HI}\left(b_\mathrm{HI}+\langle\,f渭^{2}\rangle\right)$, where $惟_\mathrm{HI}$ is the cosmic abundance of HI, $b_\mathrm{HI}$ is the linear bias of HI, and $\langle\,f渭^{2}\rangle=0.552$ encodes the effect of redshift-space distortions at linear order. We find $\mathcal{A}_\mathrm{HI}=1.51^{+3.60}_{-0.97}$ for LRGs $(z=0.84)$, $\mathcal{A}_\mathrm{HI}=6.76^{+9.04}_{-3.79}$ for ELGs $(z=0.96)$, and $\mathcal{A}_\mathrm{HI}=1.68^{+1.10}_{-0.67}$ for QSOs $(z=1.20)$, with constraints limited by modeling uncertainties at nonlinear scales. We are also sensitive to bias in the spectroscopic redshifts of each tracer, and find a non-zero bias $螖\,v= -66 \pm 20 \mathrm{km/s}$ for the QSOs. We split the QSO catalog into three redshift bins and have a decisive detection in each, with the upper bin at $z=1.30$ producing the highest redshift 21-cm intensity mapping measurement thus far. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.01242v1-abstract-full').style.display = 'none'; document.getElementById('2202.01242v1-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 February, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">66 pages, 30 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.11822">arXiv:2201.11822</a> <span> [<a href="https://arxiv.org/pdf/2201.11822">pdf</a>, <a href="https://arxiv.org/format/2201.11822">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/ac6b9f">10.3847/1538-4357/ac6b9f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Using the Sun to Measure the Primary Beam Response of the Canadian Hydrogen Intensity Mapping Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=CHIME+Collaboration"> CHIME Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Boskovic%2C+A">Anja Boskovic</a>, <a href="/search/astro-ph?searchtype=author&query=Cliche%2C+J">Jean-Fran莽ois Cliche</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+M">Meiling Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Fandino%2C+M">Mateus Fandino</a>, <a href="/search/astro-ph?searchtype=author&query=Foreman%2C+S">Simon Foreman</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">Mark Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+A+S">Alex S. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hinshaw%2C+G">Gary Hinshaw</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%B6fer%2C+C">Carolin H枚fer</a>, <a href="/search/astro-ph?searchtype=author&query=Kania%2C+J">Joseph Kania</a>, <a href="/search/astro-ph?searchtype=author&query=Landecker%2C+T+L">T. L. Landecker</a>, <a href="/search/astro-ph?searchtype=author&query=MacEachern%2C+J">Joshua MacEachern</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K">Kiyoshi Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Newburgh%2C+L">Laura Newburgh</a>, <a href="/search/astro-ph?searchtype=author&query=Ordog%2C+A">Anna Ordog</a>, <a href="/search/astro-ph?searchtype=author&query=Pinsonneault-Marotte%2C+T">Tristan Pinsonneault-Marotte</a>, <a href="/search/astro-ph?searchtype=author&query=Polzin%2C+A">Ava Polzin</a>, <a href="/search/astro-ph?searchtype=author&query=Reda%2C+A">Alex Reda</a>, <a href="/search/astro-ph?searchtype=author&query=Shaw%2C+J+R">J. Richard Shaw</a>, <a href="/search/astro-ph?searchtype=author&query=Siegel%2C+S+R">Seth R. Siegel</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.11822v5-abstract-short" style="display: inline;"> We present a beam pattern measurement of the Canadian Hydrogen Intensity Mapping Experiment (CHIME) made using the Sun as a calibration source. As CHIME is a pure drift scan instrument, we rely on the seasonal North-South motion of the Sun to probe the beam at different elevations. This semiannual range in elevation, combined with the radio brightness of the Sun, enables a beam measurement which s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.11822v5-abstract-full').style.display = 'inline'; document.getElementById('2201.11822v5-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.11822v5-abstract-full" style="display: none;"> We present a beam pattern measurement of the Canadian Hydrogen Intensity Mapping Experiment (CHIME) made using the Sun as a calibration source. As CHIME is a pure drift scan instrument, we rely on the seasonal North-South motion of the Sun to probe the beam at different elevations. This semiannual range in elevation, combined with the radio brightness of the Sun, enables a beam measurement which spans ~7,200 square degrees on the sky without the need to move the telescope. We take advantage of observations made near solar minimum to minimize the impact of solar variability, which is observed to be <10% in intensity over the observation period. The resulting data set is highly complementary to other CHIME beam measurements -- both in terms of angular coverage and systematics -- and plays an important role in the ongoing program to characterize the CHIME primary beam. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.11822v5-abstract-full').style.display = 'none'; document.getElementById('2201.11822v5-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 9 figures, Accepted by ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 923 100 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2201.07869">arXiv:2201.07869</a> <span> [<a href="https://arxiv.org/pdf/2201.07869">pdf</a>, <a href="https://arxiv.org/format/2201.07869">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/10.3847/1538-4365/ac6fd9">10.3847/1538-4365/ac6fd9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> An Overview of CHIME, the Canadian Hydrogen Intensity Mapping Experiment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+CHIME+Collaboration"> The CHIME Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Boskovic%2C+A">Anja Boskovic</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T">Tianyue Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cliche%2C+J">Jean-Fran莽ois Cliche</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+M">Meiling Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Denman%2C+N">Nolan Denman</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Fandino%2C+M">Mateus Fandino</a>, <a href="/search/astro-ph?searchtype=author&query=Foreman%2C+S">Simon Foreman</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">Mark Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hanna%2C+D">David Hanna</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+A+S">Alex S. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hinshaw%2C+G">Gary Hinshaw</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%B6fer%2C+C">Carolin H枚fer</a>, <a href="/search/astro-ph?searchtype=author&query=Kania%2C+J">Joseph Kania</a>, <a href="/search/astro-ph?searchtype=author&query=Klages%2C+P">Peter Klages</a>, <a href="/search/astro-ph?searchtype=author&query=Landecker%2C+T+L">T. L. Landecker</a>, <a href="/search/astro-ph?searchtype=author&query=MacEachern%2C+J">Joshua MacEachern</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K">Kiyoshi Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">Juan Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Milutinovic%2C+N">Nikola Milutinovic</a>, <a href="/search/astro-ph?searchtype=author&query=Mirhosseini%2C+A">Arash Mirhosseini</a>, <a href="/search/astro-ph?searchtype=author&query=Newburgh%2C+L">Laura Newburgh</a> , et al. (18 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2201.07869v3-abstract-short" style="display: inline;"> The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is a drift scan radio telescope operating across the 400-800 MHz band. CHIME is located at the Dominion Radio Astrophysical Observatory near Penticton, BC Canada. The instrument is designed to map neutral hydrogen over the redshift range 0.8 to 2.5 to constrain the expansion history of the Universe. This goal drives the design features of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07869v3-abstract-full').style.display = 'inline'; document.getElementById('2201.07869v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2201.07869v3-abstract-full" style="display: none;"> The Canadian Hydrogen Intensity Mapping Experiment (CHIME) is a drift scan radio telescope operating across the 400-800 MHz band. CHIME is located at the Dominion Radio Astrophysical Observatory near Penticton, BC Canada. The instrument is designed to map neutral hydrogen over the redshift range 0.8 to 2.5 to constrain the expansion history of the Universe. This goal drives the design features of the instrument. CHIME consists of four parallel cylindrical reflectors, oriented north-south, each 100 m $\times$ 20 m and outfitted with a 256 element dual-polarization linear feed array. CHIME observes a two degree wide stripe covering the entire meridian at any given moment, observing 3/4 of the sky every day due to Earth rotation. An FX correlator utilizes FPGAs and GPUs to digitize and correlate the signals, with different correlation products generated for cosmological, fast radio burst, pulsar, VLBI, and 21 cm absorber backends. For the cosmology backend, the $N_\mathrm{feed}^2$ correlation matrix is formed for 1024 frequency channels across the band every 31 ms. A data receiver system applies calibration and flagging and, for our primary cosmological data product, stacks redundant baselines and integrates for 10 s. We present an overview of the instrument, its performance metrics based on the first three years of science data, and we describe the current progress in characterizing CHIME's primary beam response. We also present maps of the sky derived from CHIME data; we are using versions of these maps for a cosmological stacking analysis as well as for investigation of Galactic foregrounds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2201.07869v3-abstract-full').style.display = 'none'; document.getElementById('2201.07869v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2022. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">40 pages, 31 figures, 2 tables. Accepted by ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2112.00820">arXiv:2112.00820</a> <span> [<a href="https://arxiv.org/pdf/2112.00820">pdf</a>, <a href="https://arxiv.org/format/2112.00820">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/s10909-022-02729-5">10.1007/s10909-022-02729-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> In-flight gain monitoring of SPIDER's transition-edge sensor arrays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Filippini%2C+J+P">J. P. Filippini</a>, <a href="/search/astro-ph?searchtype=author&query=Gambrel%2C+A+E">A. E. Gambrel</a>, <a href="/search/astro-ph?searchtype=author&query=Rahlin%2C+A+S">A. S. Rahlin</a>, <a href="/search/astro-ph?searchtype=author&query=Young%2C+E+Y">E. Y. Young</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=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Benton%2C+S+J">S. J. Benton</a>, <a href="/search/astro-ph?searchtype=author&query=Bergman%2C+A+S">A. S. Bergman</a>, <a href="/search/astro-ph?searchtype=author&query=Bihary%2C+R">R. Bihary</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=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+J+A">J. A. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+S+A">S. A. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+H+C">H. C. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Contaldi%2C+C+R">C. R. Contaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Dore%2C+O">O. Dore</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">A. J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">H. K. Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Farhang%2C+M">M. Farhang</a>, <a href="/search/astro-ph?searchtype=author&query=Fraisse%2C+A+A">A. A. Fraisse</a>, <a href="/search/astro-ph?searchtype=author&query=Freese%2C+K">K. Freese</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+M">M. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Gandilo%2C+N+N">N. N. Gandilo</a>, <a href="/search/astro-ph?searchtype=author&query=Ganga%2C+K">K. Ganga</a>, <a href="/search/astro-ph?searchtype=author&query=Gualtieri%2C+R">R. Gualtieri</a> , et al. (45 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2112.00820v2-abstract-short" style="display: inline;"> Experiments deploying large arrays of transition-edge sensors (TESs) often require a robust method to monitor gain variations with minimal loss of observing time. We propose a sensitive and non-intrusive method for monitoring variations in TES responsivity using small square waves applied to the TES bias. We construct an estimator for a TES's small-signal power response from its electrical respons… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.00820v2-abstract-full').style.display = 'inline'; document.getElementById('2112.00820v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2112.00820v2-abstract-full" style="display: none;"> Experiments deploying large arrays of transition-edge sensors (TESs) often require a robust method to monitor gain variations with minimal loss of observing time. We propose a sensitive and non-intrusive method for monitoring variations in TES responsivity using small square waves applied to the TES bias. We construct an estimator for a TES's small-signal power response from its electrical response that is exact in the limit of strong electrothermal feedback. We discuss the application and validation of this method using flight data from SPIDER, a balloon-borne telescope that observes the polarization of the cosmic microwave background with more than 2000 TESs. This method may prove useful for future balloon- and space-based instruments, where observing time and ground control bandwidth are limited. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2112.00820v2-abstract-full').style.display = 'none'; document.getElementById('2112.00820v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 June, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 December, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2021. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">7 pages, 3 figures; Proceedings of the 19th International Workshop on Low Temperature Detectors (LTD19); Minor updates to match published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Low Temperature Physics (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2111.14785">arXiv:2111.14785</a> <span> [<a href="https://arxiv.org/pdf/2111.14785">pdf</a>, <a href="https://arxiv.org/format/2111.14785">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"> BICEP Array: 150 GHz detector module development </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schillaci%2C+A">A. Schillaci</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=Cheshire%2C+J">J. 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=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">D. Goldfinger</a>, <a href="/search/astro-ph?searchtype=author&query=Grayson%2C+J+A">J. A. Grayson</a> , et al. (59 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="2111.14785v1-abstract-short" style="display: inline;"> The BICEP/Keck Collaboration is currently leading the quest to the highest sensitivity measurements of the polarized CMB anisotropies on degree scale with a series of cryogenic telescopes, of which BICEP Array is the latest Stage-3 upgrade with a total of $\sim32,000$ detectors. The instrument comprises 4 receivers spanning 30 to 270 GHz, with the low-frequency 30/40 GHz deployed to the South Pole… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14785v1-abstract-full').style.display = 'inline'; document.getElementById('2111.14785v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.14785v1-abstract-full" style="display: none;"> The BICEP/Keck Collaboration is currently leading the quest to the highest sensitivity measurements of the polarized CMB anisotropies on degree scale with a series of cryogenic telescopes, of which BICEP Array is the latest Stage-3 upgrade with a total of $\sim32,000$ detectors. The instrument comprises 4 receivers spanning 30 to 270 GHz, with the low-frequency 30/40 GHz deployed to the South Pole Station in late 2019. The full complement of receivers is forecast to set the most stringent constraints on the tensor to scalar ratio $r$. Building on these advances, the overarching small-aperture telescope concept is already being used as the reference for further Stage-4 experiment design. In this paper I will present the development of the BICEP Array 150 GHz detector module and its fabrication requirements, with highlights on the high-density time division multiplexing (TDM) design of the cryogenic circuit boards. The low-impedance wiring required between the detectors and the first-stage SQUID amplifiers is crucial to maintain a stiff voltage bias on the detectors. A novel multi-layer FR4 Printed Circuit Board (PCB) with superconducting traces, capable of reading out up to 648 detectors, is presented along with its validation tests. I will also describe an ultra-high density TDM detector module we developed for a CMB-S4-like experiment that allows up to 1,920 detectors to be read out. TDM has been chosen as the detector readout technology for the Cosmic Microwave Background Stage-4 (CMB-S4) experiment based on its proven low-noise performance, predictable costs and overall maturity of the architecture. The heritage for TDM is rooted in mm- and submm-wave experiments dating back 20 years and has since evolved to support a multiplexing factor of 64x in Stage-3 experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.14785v1-abstract-full').style.display = 'none'; document.getElementById('2111.14785v1-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">9 pages, 5 figure, Proceeding of LTD19 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/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/2111.01113">arXiv:2111.01113</a> <span> [<a href="https://arxiv.org/pdf/2111.01113">pdf</a>, <a href="https://arxiv.org/format/2111.01113">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/ac562f">10.3847/1538-4357/ac562f <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Simulation-Based Method for Correcting Mode Coupling in CMB Angular Power Spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Leung%2C+J+S+-">J. S. -Y. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+J">J. Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Nagy%2C+J+M">J. M. Nagy</a>, <a href="/search/astro-ph?searchtype=author&query=Netterfield%2C+C+B">C. B. Netterfield</a>, <a href="/search/astro-ph?searchtype=author&query=Shariff%2C+J+A">J. A. Shariff</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=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Benton%2C+S+J">S. J. Benton</a>, <a href="/search/astro-ph?searchtype=author&query=Bergman%2C+A+S">A. S. Bergman</a>, <a href="/search/astro-ph?searchtype=author&query=Bihary%2C+R">R. Bihary</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=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+J+A">J. A. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+S+A">S. A. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+H+C">H. C. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Contaldi%2C+C+R">C. R. Contaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Dor%C3%A9%2C+O">O. Dor茅</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">A. J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">H. K. Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Farhang%2C+M">M. Farhang</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=Fraisse%2C+A+A">A. A. Fraisse</a>, <a href="/search/astro-ph?searchtype=author&query=Freese%2C+K">K. Freese</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+M">M. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Gambrel%2C+A+E">A. E. Gambrel</a> , et al. (45 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="2111.01113v2-abstract-short" style="display: inline;"> Modern CMB analysis pipelines regularly employ complex time-domain filters, beam models, masking, and other techniques during the production of sky maps and their corresponding angular power spectra. However, these processes can generate couplings between multipoles from the same spectrum and from different spectra, in addition to the typical power attenuation. Within the context of pseudo-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.01113v2-abstract-full').style.display = 'inline'; document.getElementById('2111.01113v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.01113v2-abstract-full" style="display: none;"> Modern CMB analysis pipelines regularly employ complex time-domain filters, beam models, masking, and other techniques during the production of sky maps and their corresponding angular power spectra. However, these processes can generate couplings between multipoles from the same spectrum and from different spectra, in addition to the typical power attenuation. Within the context of pseudo-$C_\ell$ based, MASTER-style analyses, the net effect of the time-domain filtering is commonly approximated by a multiplicative transfer function, $F_{\ell}$, that can fail to capture mode mixing and is dependent on the spectrum of the signal. To address these shortcomings, we have developed a simulation-based spectral correction approach that constructs a two-dimensional transfer matrix, $J_{\ell\ell'}$, which contains information about mode mixing in addition to mode attenuation. We demonstrate the application of this approach on data from the first flight of the SPIDER balloon-borne CMB experiment. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.01113v2-abstract-full').style.display = 'none'; document.getElementById('2111.01113v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">14 pages, 7 figures; updated to match published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 928(2):109, 2022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.00576">arXiv:2110.00576</a> <span> [<a href="https://arxiv.org/pdf/2110.00576">pdf</a>, <a href="https://arxiv.org/format/2110.00576">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/10.3847/1538-3881/ac397a">10.3847/1538-3881/ac397a <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A clock stabilization system for CHIME/FRB Outriggers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mena-Parra%2C+J">J. Mena-Parra</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">C. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Cary%2C+S">S. Cary</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">K. W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=Kaczmarek%2C+J+F">J. F. Kaczmarek</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">K. Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">T. Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Cliche%2C+J+-">J. -F. Cliche</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">M. Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V+M">V. M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Landecker%2C+T+L">T. L. Landecker</a>, <a href="/search/astro-ph?searchtype=author&query=Lanman%2C+A">A. Lanman</a>, <a href="/search/astro-ph?searchtype=author&query=Sievers%2C+J+L">J. L. Sievers</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2110.00576v1-abstract-short" style="display: inline;"> The Canadian Hydrogen Intensity Mapping Experiment (CHIME) has emerged as the prime telescope for detecting fast radio bursts (FRBs). CHIME/FRB Outriggers will be a dedicated very-long-baseline interferometry (VLBI) instrument consisting of outrigger telescopes at continental baselines working with CHIME and its specialized real-time transient-search backend (CHIME/FRB) to detect and localize FRBs… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00576v1-abstract-full').style.display = 'inline'; document.getElementById('2110.00576v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.00576v1-abstract-full" style="display: none;"> The Canadian Hydrogen Intensity Mapping Experiment (CHIME) has emerged as the prime telescope for detecting fast radio bursts (FRBs). CHIME/FRB Outriggers will be a dedicated very-long-baseline interferometry (VLBI) instrument consisting of outrigger telescopes at continental baselines working with CHIME and its specialized real-time transient-search backend (CHIME/FRB) to detect and localize FRBs with 50 mas precision. In this paper we present a minimally invasive clock stabilization system that effectively transfers the CHIME digital backend reference clock from its original GPS-disciplined ovenized crystal oscillator to a passive hydrogen maser. This enables us to combine the long-term stability and absolute time tagging of the GPS clock with the short and intermediate-term stability of the maser to reduce the clock timing errors between VLBI calibration observations. We validate the system with VLBI-style observations of Cygnus A over a 400 m baseline between CHIME and the CHIME Pathfinder, demonstrating agreement between sky-based and maser-based timing measurements at the 30 ps rms level on timescales ranging from one minute to up to nine days, and meeting the stability requirements for CHIME/FRB Outriggers. In addition, we present an alternate reference clock solution for outrigger stations which lack the infrastructure to support a passive hydrogen maser. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.00576v1-abstract-full').style.display = 'none'; document.getElementById('2110.00576v1-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">15 pages, 7 figures, submitted to AJ</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/2106.04352">arXiv:2106.04352</a> <span> [<a href="https://arxiv.org/pdf/2106.04352">pdf</a>, <a href="https://arxiv.org/format/2106.04352">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div 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/10.3847/1538-4365/ac33ab">10.3847/1538-4365/ac33ab <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The First CHIME/FRB Fast Radio Burst Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+T+C">The CHIME/FRB Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Andersen%2C+B+C">Bridget C. Andersen</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K">Kevin Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+S">Sabrina Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bhardwaj%2C+M">Mohit Bhardwaj</a>, <a href="/search/astro-ph?searchtype=author&query=Boyce%2C+M+M">Michelle M. Boyce</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">Charanjot Brar</a>, <a href="/search/astro-ph?searchtype=author&query=Breitman%2C+D">Daniela Breitman</a>, <a href="/search/astro-ph?searchtype=author&query=Cassanelli%2C+T">Tomas Cassanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Chawla%2C+P">Pragya Chawla</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+T">Tianyue Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Cliche%2C+J+-">J. -F. Cliche</a>, <a href="/search/astro-ph?searchtype=author&query=Cook%2C+A">Amanda Cook</a>, <a href="/search/astro-ph?searchtype=author&query=Cubranic%2C+D">Davor Cubranic</a>, <a href="/search/astro-ph?searchtype=author&query=Curtin%2C+A+P">Alice P. Curtin</a>, <a href="/search/astro-ph?searchtype=author&query=Deng%2C+M">Meiling Deng</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">Matt Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Fengqiu"> Fengqiu</a>, <a href="/search/astro-ph?searchtype=author&query=Dong"> Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Eadie%2C+G">Gwendolyn Eadie</a>, <a href="/search/astro-ph?searchtype=author&query=Fandino%2C+M">Mateus Fandino</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">Emmanuel Fonseca</a> , et al. (52 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="2106.04352v3-abstract-short" style="display: inline;"> We present a catalog of 536 fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) Project between 400 and 800 MHz from 2018 July 25 to 2019 July 1, including 62 bursts from 18 previously reported repeating sources. The catalog represents the first large sample, including bursts from repeaters and non-repeaters, observed in a single sur… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.04352v3-abstract-full').style.display = 'inline'; document.getElementById('2106.04352v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.04352v3-abstract-full" style="display: none;"> We present a catalog of 536 fast radio bursts (FRBs) detected by the Canadian Hydrogen Intensity Mapping Experiment Fast Radio Burst (CHIME/FRB) Project between 400 and 800 MHz from 2018 July 25 to 2019 July 1, including 62 bursts from 18 previously reported repeating sources. The catalog represents the first large sample, including bursts from repeaters and non-repeaters, observed in a single survey with uniform selection effects. This facilitates comparative and absolute studies of the FRB population. We show that repeaters and apparent non-repeaters have sky locations and dispersion measures (DMs) that are consistent with being drawn from the same distribution. However, bursts from repeating sources differ from apparent non-repeaters in intrinsic temporal width and spectral bandwidth. Through injection of simulated events into our detection pipeline, we perform an absolute calibration of selection effects to account for systematic biases. We find evidence for a population of FRBs - comprising a large fraction of the overall population - with a scattering time at 600 MHz in excess of 10 ms, of which only a small fraction are observed by CHIME/FRB. We infer a power-law index for the cumulative fluence distribution of $伪=-1.40\pm0.11(\textrm{stat.})^{+0.06}_{-0.09}(\textrm{sys.})$, consistent with the $-3/2$ expectation for a non-evolving population in Euclidean space. We find $伪$ is steeper for high-DM events and shallower for low-DM events, which is what would be expected when DM is correlated with distance. We infer a sky rate of $[525\pm30(\textrm{stat.})^{+140}_{-130}({\textrm{sys.}})]/\textrm{sky}/\textrm{day}$ above a fluence of 5 Jy ms at 600 MHz, with scattering time at $600$ MHz under 10 ms, and DM above 100 pc cm$^{-3}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.04352v3-abstract-full').style.display = 'none'; document.getElementById('2106.04352v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 January, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">67 pages, 27 figures, 5 tables. Published in ApJS and updated with changes reflected in an erratum (affecting the sky rate). Extended figures and data at https://www.chime-frb.ca/catalog</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2104.01172">arXiv:2104.01172</a> <span> [<a href="https://arxiv.org/pdf/2104.01172">pdf</a>, <a href="https://arxiv.org/format/2104.01172">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/ac230b">10.3847/1538-4357/ac230b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The XFaster Power Spectrum and Likelihood Estimator for the Analysis of Cosmic Microwave Background Maps </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gambrel%2C+A+E">A. E. Gambrel</a>, <a href="/search/astro-ph?searchtype=author&query=Rahlin%2C+A+S">A. S. Rahlin</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+X">X. Song</a>, <a href="/search/astro-ph?searchtype=author&query=Contaldi%2C+C+R">C. R. Contaldi</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=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Benton%2C+S+J">S. J. Benton</a>, <a href="/search/astro-ph?searchtype=author&query=Bergman%2C+A+S">A. S. Bergman</a>, <a href="/search/astro-ph?searchtype=author&query=Bihary%2C+R">R. Bihary</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=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+J+A">J. A. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+S+A">S. A. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+H+C">H. C. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">A. J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">H. K. Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Farhang%2C+M">M. Farhang</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=Fraisse%2C+A+A">A. A. Fraisse</a>, <a href="/search/astro-ph?searchtype=author&query=Freese%2C+K">K. Freese</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+M">M. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Gandilo%2C+N+N">N. N. Gandilo</a>, <a href="/search/astro-ph?searchtype=author&query=Gualtieri%2C+R">R. Gualtieri</a>, <a href="/search/astro-ph?searchtype=author&query=Gudmundsson%2C+J+E">J. E. Gudmundsson</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">M. Halpern</a> , et al. (42 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="2104.01172v2-abstract-short" style="display: inline;"> We present the XFaster analysis package. XFaster is a fast, iterative angular power spectrum estimator based on a diagonal approximation to the quadratic Fisher matrix estimator. XFaster uses Monte Carlo simulations to compute noise biases and filter transfer functions and is thus a hybrid of both Monte Carlo and quadratic estimator methods. In contrast to conventional pseudo-$C_\ell$ based method… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.01172v2-abstract-full').style.display = 'inline'; document.getElementById('2104.01172v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2104.01172v2-abstract-full" style="display: none;"> We present the XFaster analysis package. XFaster is a fast, iterative angular power spectrum estimator based on a diagonal approximation to the quadratic Fisher matrix estimator. XFaster uses Monte Carlo simulations to compute noise biases and filter transfer functions and is thus a hybrid of both Monte Carlo and quadratic estimator methods. In contrast to conventional pseudo-$C_\ell$ based methods, the algorithm described here requires a minimal number of simulations, and does not require them to be precisely representative of the data to estimate accurate covariance matrices for the bandpowers. The formalism works with polarization-sensitive observations and also data sets with identical, partially overlapping, or independent survey regions. The method was first implemented for the analysis of BOOMERanG data, and also used as part of the Planck analysis. Here, we describe the full, publicly available analysis package, written in Python, as developed for the analysis of data from the 2015 flight of the SPIDER instrument. The package includes extensions for self-consistently estimating null spectra and for estimating fits for Galactic foreground contributions. We show results from the extensive validation of XFaster using simulations, and its application to the SPIDER data set. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2104.01172v2-abstract-full').style.display = 'none'; document.getElementById('2104.01172v2-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 April, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">18 pages, 11 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2103.13334">arXiv:2103.13334</a> <span> [<a href="https://arxiv.org/pdf/2103.13334">pdf</a>, <a href="https://arxiv.org/format/2103.13334">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"> A Constraint on Primordial $B$-Modes from the First Flight of the SPIDER Balloon-Borne Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=SPIDER+Collaboration"> SPIDER Collaboration</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=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Benton%2C+S+J">S. J. Benton</a>, <a href="/search/astro-ph?searchtype=author&query=Bergman%2C+A+S">A. S. Bergman</a>, <a href="/search/astro-ph?searchtype=author&query=Bihary%2C+R">R. Bihary</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=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bonetti%2C+J+A">J. A. Bonetti</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+S+A">S. A. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+H+C">H. C. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Contaldi%2C+C+R">C. R. Contaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Dor%C3%A9%2C+O">O. Dor茅</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">A. J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">H. K. Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Farhang%2C+M">M. Farhang</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=Fraisse%2C+A+A">A. A. Fraisse</a>, <a href="/search/astro-ph?searchtype=author&query=Freese%2C+K">K. Freese</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+M">M. Galloway</a>, <a href="/search/astro-ph?searchtype=author&query=Gambrel%2C+A+E">A. E. Gambrel</a>, <a href="/search/astro-ph?searchtype=author&query=Gandilo%2C+N+N">N. N. Gandilo</a>, <a href="/search/astro-ph?searchtype=author&query=Ganga%2C+K">K. Ganga</a>, <a href="/search/astro-ph?searchtype=author&query=Gualtieri%2C+R">R. Gualtieri</a>, <a href="/search/astro-ph?searchtype=author&query=Gudmundsson%2C+J+E">J. E. Gudmundsson</a> , et al. (46 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="2103.13334v1-abstract-short" style="display: inline;"> We present the first linear polarization measurements from the 2015 long-duration balloon flight of SPIDER, an experiment designed to map the polarization of the cosmic microwave background (CMB) on degree angular scales. Results from these measurements include maps and angular power spectra from observations of 4.8% of the sky at 95 and 150 GHz, along with the results of internal consistency test… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.13334v1-abstract-full').style.display = 'inline'; document.getElementById('2103.13334v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2103.13334v1-abstract-full" style="display: none;"> We present the first linear polarization measurements from the 2015 long-duration balloon flight of SPIDER, an experiment designed to map the polarization of the cosmic microwave background (CMB) on degree angular scales. Results from these measurements include maps and angular power spectra from observations of 4.8% of the sky at 95 and 150 GHz, along with the results of internal consistency tests on these data. While the polarized CMB anisotropy from primordial density perturbations is the dominant signal in this region of sky, Galactic dust emission is also detected with high significance; Galactic synchrotron emission is found to be negligible in the SPIDER bands. We employ two independent foreground-removal techniques in order to explore the sensitivity of the cosmological result to the assumptions made by each. The primary method uses a dust template derived from Planck data to subtract the Galactic dust signal. A second approach, employing a joint analysis of SPIDER and Planck data in the harmonic domain, assumes a modified-blackbody model for the spectral energy distribution of the dust with no constraint on its spatial morphology. Using a likelihood that jointly samples the template amplitude and $r$ parameter space, we derive 95% upper limits on the primordial tensor-to-scalar ratio from Feldman-Cousins and Bayesian constructions, finding $r<0.11$ and $r<0.19$, respectively. Roughly half the uncertainty in $r$ derives from noise associated with the template subtraction. New data at 280 GHz from SPIDER's second flight will complement the Planck polarization maps, providing powerful measurements of the polarized Galactic dust emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2103.13334v1-abstract-full').style.display = 'none'; document.getElementById('2103.13334v1-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 March, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">29 pages, 13 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2012.12407">arXiv:2012.12407</a> <span> [<a href="https://arxiv.org/pdf/2012.12407">pdf</a>, <a href="https://arxiv.org/format/2012.12407">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/10.1117/12.2562941">10.1117/12.2562941 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Design and pre-flight performance of SPIDER 280 GHz receivers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shaw%2C+E+C">E. C. Shaw</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=Akers%2C+S">S. Akers</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J">J. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J">J. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+D+T">D. T. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Benton%2C+S+J">S. J. Benton</a>, <a href="/search/astro-ph?searchtype=author&query=Bergman%2C+A+S">A. S. Bergman</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=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+S+A">S. A. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+H+C">H. C. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Contaldi%2C+C+R">C. R. Contaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Domagalski%2C+R+S">R. S. Domagalski</a>, <a href="/search/astro-ph?searchtype=author&query=Dor%C3%A9%2C+O">O. Dor茅</a>, <a href="/search/astro-ph?searchtype=author&query=Duff%2C+S+M">S. M. Duff</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">A. J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Eriksen%2C+H+K">H. K. Eriksen</a>, <a href="/search/astro-ph?searchtype=author&query=Farhang%2C+M">M. Farhang</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=Fissel%2C+L+M">L. M. Fissel</a>, <a href="/search/astro-ph?searchtype=author&query=Fraisse%2C+A+A">A. A. Fraisse</a>, <a href="/search/astro-ph?searchtype=author&query=Freese%2C+K">K. Freese</a>, <a href="/search/astro-ph?searchtype=author&query=Galloway%2C+M">M. Galloway</a> , et al. (57 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="2012.12407v1-abstract-short" style="display: inline;"> In this work we describe upgrades to the Spider balloon-borne telescope in preparation for its second flight, currently planned for December 2021. The Spider instrument is optimized to search for a primordial B-mode polarization signature in the cosmic microwave background at degree angular scales. During its first flight in 2015, Spider mapped ~10% of the sky at 95 and 150 GHz. The payload for th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12407v1-abstract-full').style.display = 'inline'; document.getElementById('2012.12407v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.12407v1-abstract-full" style="display: none;"> In this work we describe upgrades to the Spider balloon-borne telescope in preparation for its second flight, currently planned for December 2021. The Spider instrument is optimized to search for a primordial B-mode polarization signature in the cosmic microwave background at degree angular scales. During its first flight in 2015, Spider mapped ~10% of the sky at 95 and 150 GHz. The payload for the second Antarctic flight will incorporate three new 280 GHz receivers alongside three refurbished 95- and 150 GHz receivers from Spider's first flight. In this work we discuss the design and characterization of these new receivers, which employ over 1500 feedhorn-coupled transition-edge sensors. We describe pre-flight laboratory measurements of detector properties, and the optical performance of completed receivers. These receivers will map a wide area of the sky at 280 GHz, providing new information on polarized Galactic dust emission that will help to separate it from the cosmological signal. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.12407v1-abstract-full').style.display = 'none'; document.getElementById('2012.12407v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 8 figures; as published in the conference proceedings for SPIE Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X (2020)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> "Design and pre-flight performance of SPIDER 280 GHz receivers," Proc. SPIE 11453, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy X, 114532F (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/2012.09363">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/2012.04047">arXiv:2012.04047</a> <span> [<a href="https://arxiv.org/pdf/2012.04047">pdf</a>, <a href="https://arxiv.org/format/2012.04047">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Receiver development for BICEP Array, a next-generation CMB polarimeter at the South Pole </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Moncelsi%2C+L">L. Moncelsi</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=Buza%2C+V">V. Buza</a>, <a href="/search/astro-ph?searchtype=author&query=Cheshire%2C+J">J. 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+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=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>, <a href="/search/astro-ph?searchtype=author&query=Grimes%2C+P">P. Grimes</a>, <a href="/search/astro-ph?searchtype=author&query=Hall%2C+G">G. Hall</a> , et al. (50 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="2012.04047v1-abstract-short" style="display: inline;"> A detection of curl-type ($B$-mode) polarization of the primary CMB would be direct evidence for the inflationary paradigm of the origin of the Universe. The BICEP/Keck Array (BK) program targets the degree angular scales, where the power from primordial $B$-mode polarization is expected to peak, with ever-increasing sensitivity and has published the most stringent constraints on inflation to date… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.04047v1-abstract-full').style.display = 'inline'; document.getElementById('2012.04047v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2012.04047v1-abstract-full" style="display: none;"> A detection of curl-type ($B$-mode) polarization of the primary CMB would be direct evidence for the inflationary paradigm of the origin of the Universe. The BICEP/Keck Array (BK) program targets the degree angular scales, where the power from primordial $B$-mode polarization is expected to peak, with ever-increasing sensitivity and has published the most stringent constraints on inflation to date. BICEP Array (BA) is the Stage-3 instrument of the BK program and will comprise four BICEP3-class receivers observing at 30/40, 95, 150 and 220/270 GHz with a combined 32,000+ detectors; such wide frequency coverage is necessary for control of the Galactic foregrounds, which also produce degree-scale $B$-mode signal. The 30/40 GHz receiver is designed to constrain the synchrotron foreground and has begun observing at the South Pole in early 2020. By the end of a 3-year observing campaign, the full BICEP Array instrument is projected to reach $蟽_r$ between 0.002 and 0.004, depending on foreground complexity and degree of removal of $B$-modes due to gravitational lensing (delensing). This paper presents an overview of the design, measured on-sky performance and calibration of the first BA receiver. We also give a preview of the added complexity in the time-domain multiplexed readout of the 7,776-detector 150 GHz receiver. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2012.04047v1-abstract-full').style.display = 'none'; document.getElementById('2012.04047v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 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 of SPIE 2020 (AS111). This article supersedes arXiv:1808.00568 and arXiv:2002.05228</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/2008.05681">arXiv:2008.05681</a> <span> [<a href="https://arxiv.org/pdf/2008.05681">pdf</a>, <a href="https://arxiv.org/format/2008.05681">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/10.3847/1538-4365/abfdcb">10.3847/1538-4365/abfdcb <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The CHIME Pulsar Project: System Overview </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+C">CHIME/Pulsar Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Bandura%2C+K+M">K. M. Bandura</a>, <a href="/search/astro-ph?searchtype=author&query=Boyle%2C+P+J">P. J. Boyle</a>, <a href="/search/astro-ph?searchtype=author&query=Brar%2C+C">C. Brar</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=Crowter%2C+K">K. Crowter</a>, <a href="/search/astro-ph?searchtype=author&query=Cubranic%2C+D">D. Cubranic</a>, <a href="/search/astro-ph?searchtype=author&query=Demorest%2C+P+B">P. B. Demorest</a>, <a href="/search/astro-ph?searchtype=author&query=Denman%2C+N+T">N. T. Denman</a>, <a href="/search/astro-ph?searchtype=author&query=Dobbs%2C+M">M. Dobbs</a>, <a href="/search/astro-ph?searchtype=author&query=Dong%2C+F+Q">F. Q. Dong</a>, <a href="/search/astro-ph?searchtype=author&query=Fandino%2C+M">M. Fandino</a>, <a href="/search/astro-ph?searchtype=author&query=Fonseca%2C+E">E. Fonseca</a>, <a href="/search/astro-ph?searchtype=author&query=Good%2C+D+C">D. C. Good</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">M. Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+A+S">A. S. Hill</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%B6fer%2C+C">C. H枚fer</a>, <a href="/search/astro-ph?searchtype=author&query=Kaspi%2C+V+M">V. M. Kaspi</a>, <a href="/search/astro-ph?searchtype=author&query=Landecker%2C+T+L">T. L. Landecker</a>, <a href="/search/astro-ph?searchtype=author&query=Leung%2C+C">C. Leung</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+H+-">H. -H. Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Luo%2C+J">J. Luo</a>, <a href="/search/astro-ph?searchtype=author&query=Masui%2C+K+W">K. W. Masui</a>, <a href="/search/astro-ph?searchtype=author&query=McKee%2C+J+W">J. W. McKee</a> , et al. (20 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2008.05681v2-abstract-short" style="display: inline;"> We present the design, implementation and performance of a digital backend constructed for the Canadian Hydrogen Intensity Mapping Experiment (CHIME) that uses accelerated computing to observe radio pulsars and transient radio sources. When operating, the CHIME correlator outputs 10 independent streams of beamformed data for the CHIME/Pulsar backend that digitally track specified celestial positio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.05681v2-abstract-full').style.display = 'inline'; document.getElementById('2008.05681v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.05681v2-abstract-full" style="display: none;"> We present the design, implementation and performance of a digital backend constructed for the Canadian Hydrogen Intensity Mapping Experiment (CHIME) that uses accelerated computing to observe radio pulsars and transient radio sources. When operating, the CHIME correlator outputs 10 independent streams of beamformed data for the CHIME/Pulsar backend that digitally track specified celestial positions. Each of these independent streams are processed by the CHIME/Pulsar backend system which can coherently dedisperse, in real-time, up to dispersion measure values of 2500 pc/cm$^{-3}$ . The tracking beams and real-time analysis system are autonomously controlled by a priority-based algorithm that schedules both known sources and positions of interest for observation with observing cadences as small as one day. Given the distribution of known pulsars and radio-transient sources, the CHIME/Pulsar system can monitor up to 900 positions once per sidereal day and observe all sources with declinations greater than $-20^\circ$ once every $\sim$2 weeks. We also discuss the science program enabled through the current modes of data acquisition for CHIME/Pulsar that centers on timing and searching experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.05681v2-abstract-full').style.display = 'none'; document.getElementById('2008.05681v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 13 August, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 9 figures, 1 table. Submitted to ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.07289">arXiv:2007.07289</a> <span> [<a href="https://arxiv.org/pdf/2007.07289">pdf</a>, <a href="https://arxiv.org/format/2007.07289">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/10.1088/1475-7516/2020/12/045">10.1088/1475-7516/2020/12/045 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: A Measurement of the Cosmic Microwave Background Power Spectra at 98 and 150 GHz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselfield%2C+M">Matthew Hasselfield</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+S+P">Shuay-Pwu Patty Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Koopman%2C+B">Brian Koopman</a>, <a href="/search/astro-ph?searchtype=author&query=Lungu%2C+M">Marius Lungu</a>, <a href="/search/astro-ph?searchtype=author&query=Abitbol%2C+M+H">Maximilian H. Abitbol</a>, <a href="/search/astro-ph?searchtype=author&query=Addison%2C+G+E">Graeme E. Addison</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">Peter A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Aiola%2C+S">Simone Aiola</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+D">David Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Amodeo%2C+S">Stefania Amodeo</a>, <a href="/search/astro-ph?searchtype=author&query=Angile%2C+E">Elio Angile</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J+E">Jason E. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=Baildon%2C+T">Taylor Baildon</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nick Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J+A">James A. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Bean%2C+R">Rachel Bean</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+D+T">Daniel T. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+S+M">Sarah Marie Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Calafut%2C+V">Victoria Calafut</a>, <a href="/search/astro-ph?searchtype=author&query=Campusano%2C+L+E">Luis E. Campusano</a>, <a href="/search/astro-ph?searchtype=author&query=Carrero%2C+F">Felipe Carrero</a> , et al. (114 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.07289v2-abstract-short" style="display: inline;"> We present the temperature and polarization angular power spectra of the CMB measured by the Atacama Cosmology Telescope (ACT) from 5400 deg$^2$ of the 2013-2016 survey, which covers $>$15000 deg$^2$ at 98 and 150 GHz. For this analysis we adopt a blinding strategy to help avoid confirmation bias and, related to this, show numerous checks for systematic error done before unblinding. Using the like… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.07289v2-abstract-full').style.display = 'inline'; document.getElementById('2007.07289v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.07289v2-abstract-full" style="display: none;"> We present the temperature and polarization angular power spectra of the CMB measured by the Atacama Cosmology Telescope (ACT) from 5400 deg$^2$ of the 2013-2016 survey, which covers $>$15000 deg$^2$ at 98 and 150 GHz. For this analysis we adopt a blinding strategy to help avoid confirmation bias and, related to this, show numerous checks for systematic error done before unblinding. Using the likelihood for the cosmological analysis we constrain secondary sources of anisotropy and foreground emission, and derive a "CMB-only" spectrum that extends to $\ell=4000$. At large angular scales, foreground emission at 150 GHz is $\sim$1% of TT and EE within our selected regions and consistent with that found by Planck. Using the same likelihood, we obtain the cosmological parameters for $螞$CDM for the ACT data alone with a prior on the optical depth of $蟿=0.065\pm0.015$. $螞$CDM is a good fit. The best-fit model has a reduced $蠂^2$ of 1.07 (PTE=0.07) with $H_0=67.9\pm1.5$ km/s/Mpc. We show that the lensing BB signal is consistent with $螞$CDM and limit the celestial EB polarization angle to $蠄_P =-0.07^{\circ}\pm0.09^{\circ}$. We directly cross correlate ACT with Planck and observe generally good agreement but with some discrepancies in TE. All data on which this analysis is based will be publicly released. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.07289v2-abstract-full').style.display = 'none'; document.getElementById('2007.07289v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages, 27 figures, products available on the NASA LAMBDA website, version accepted for publication in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2007.07288">arXiv:2007.07288</a> <span> [<a href="https://arxiv.org/pdf/2007.07288">pdf</a>, <a href="https://arxiv.org/format/2007.07288">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/10.1088/1475-7516/2020/12/047">10.1088/1475-7516/2020/12/047 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: DR4 Maps and Cosmological Parameters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Aiola%2C+S">Simone Aiola</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Maurin%2C+L">Lo茂c Maurin</a>, <a href="/search/astro-ph?searchtype=author&query=Naess%2C+S">Sigurd Naess</a>, <a href="/search/astro-ph?searchtype=author&query=Schmitt%2C+B+L">Benjamin L. Schmitt</a>, <a href="/search/astro-ph?searchtype=author&query=Abitbol%2C+M+H">Maximilian H. Abitbol</a>, <a href="/search/astro-ph?searchtype=author&query=Addison%2C+G+E">Graeme E. Addison</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">Peter A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+D">David Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Amodeo%2C+S">Stefania Amodeo</a>, <a href="/search/astro-ph?searchtype=author&query=Angile%2C+E">Elio Angile</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J+E">Jason E. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=Baildon%2C+T">Taylor Baildon</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nick Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J+A">James A. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Bean%2C+R">Rachel Bean</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+D+T">Daniel T. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+S+M">Sarah Marie Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Calafut%2C+V">Victoria Calafut</a>, <a href="/search/astro-ph?searchtype=author&query=Campusano%2C+L+E">Luis E. Campusano</a>, <a href="/search/astro-ph?searchtype=author&query=Carrero%2C+F">Felipe Carrero</a>, <a href="/search/astro-ph?searchtype=author&query=Chesmore%2C+G+E">Grace E. Chesmore</a>, <a href="/search/astro-ph?searchtype=author&query=Cho%2C+H">Hsiao-mei Cho</a> , et al. (116 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2007.07288v2-abstract-short" style="display: inline;"> We present new arcminute-resolution maps of the Cosmic Microwave Background temperature and polarization anisotropy from the Atacama Cosmology Telescope, using data taken from 2013-2016 at 98 and 150 GHz. The maps cover more than 17,000 deg$^2$, the deepest 600 deg$^2$ with noise levels below 10 $渭$K-arcmin. We use the power spectrum derived from almost 6,000 deg$^2$ of these maps to constrain cos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.07288v2-abstract-full').style.display = 'inline'; document.getElementById('2007.07288v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2007.07288v2-abstract-full" style="display: none;"> We present new arcminute-resolution maps of the Cosmic Microwave Background temperature and polarization anisotropy from the Atacama Cosmology Telescope, using data taken from 2013-2016 at 98 and 150 GHz. The maps cover more than 17,000 deg$^2$, the deepest 600 deg$^2$ with noise levels below 10 $渭$K-arcmin. We use the power spectrum derived from almost 6,000 deg$^2$ of these maps to constrain cosmology. The ACT data enable a measurement of the angular scale of features in both the divergence-like polarization and the temperature anisotropy, tracing both the velocity and density at last-scattering. From these one can derive the distance to the last-scattering surface and thus infer the local expansion rate, $H_0$. By combining ACT data with large-scale information from WMAP we measure $H_0 = 67.6 \pm 1.1$ km/s/Mpc, at 68% confidence, in excellent agreement with the independently-measured Planck satellite estimate (from ACT alone we find $H_0 = 67.9 \pm 1.5$ km/s/Mpc). The $螞$CDM model provides a good fit to the ACT data, and we find no evidence for deviations: both the spatial curvature, and the departure from the standard lensing signal in the spectrum, are zero to within 1$蟽$; the number of relativistic species, the primordial Helium fraction, and the running of the spectral index are consistent with $螞$CDM predictions to within $1.5 - 2.2蟽$. We compare ACT, WMAP, and Planck at the parameter level and find good consistency; we investigate how the constraints on the correlated spectral index and baryon density parameters readjust when adding CMB large-scale information that ACT does not measure. The DR4 products presented here will be publicly released on the NASA Legacy Archive for Microwave Background Data Analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2007.07288v2-abstract-full').style.display = 'none'; document.getElementById('2007.07288v2-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 December, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 July, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">33 pages, 24 figures, products available on the NASA LAMBDA website, version accepted for publication in JCAP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2002.05771">arXiv:2002.05771</a> <span> [<a href="https://arxiv.org/pdf/2002.05771">pdf</a>, <a href="https://arxiv.org/format/2002.05771">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10909-020-02415-4">10.1007/s10909-020-02415-4 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Particle response of antenna-coupled TES arrays: results from SPIDER and the lab </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Osherson%2C+B">B. Osherson</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=Fu%2C+J">J. Fu</a>, <a href="/search/astro-ph?searchtype=author&query=Gramillano%2C+R+V">R. V. Gramillano</a>, <a href="/search/astro-ph?searchtype=author&query=Gualtieri%2C+R">R. Gualtieri</a>, <a href="/search/astro-ph?searchtype=author&query=Shaw%2C+E+C">E. C. Shaw</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=Amiri%2C+M">M. Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Benton%2C+S+J">S. J. Benton</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=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Bryan%2C+S+A">S. A. Bryan</a>, <a href="/search/astro-ph?searchtype=author&query=Chiang%2C+H+C">H. C. Chiang</a>, <a href="/search/astro-ph?searchtype=author&query=Contaldi%2C+C+R">C. R. Contaldi</a>, <a href="/search/astro-ph?searchtype=author&query=Dore%2C+O">O. Dore</a>, <a href="/search/astro-ph?searchtype=author&query=Fraisse%2C+A+A">A. A. Fraisse</a>, <a href="/search/astro-ph?searchtype=author&query=Gambrel%2C+A+E">A. E. Gambrel</a>, <a href="/search/astro-ph?searchtype=author&query=Gandilo%2C+N+N">N. N. Gandilo</a>, <a href="/search/astro-ph?searchtype=author&query=Gudmundsson%2C+J+E">J. E. Gudmundsson</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">M. Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+J">J. Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselfield%2C+M">M. Hasselfield</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+G">G. Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Holmes%2C+W">W. Holmes</a>, <a href="/search/astro-ph?searchtype=author&query=Hristov%2C+V+V">V. V. Hristov</a> , et al. (23 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2002.05771v1-abstract-short" style="display: inline;"> Future mm-wave and sub-mm space missions will employ large arrays of multiplexed Transition Edge Sensor (TES) bolometers. Such instruments must contend with the high flux of cosmic rays beyond our atmosphere that induce "glitches" in bolometer data, which posed a challenge to data analysis from the Planck bolometers. Future instruments will face the additional challenges of shared substrate wafers… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.05771v1-abstract-full').style.display = 'inline'; document.getElementById('2002.05771v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2002.05771v1-abstract-full" style="display: none;"> Future mm-wave and sub-mm space missions will employ large arrays of multiplexed Transition Edge Sensor (TES) bolometers. Such instruments must contend with the high flux of cosmic rays beyond our atmosphere that induce "glitches" in bolometer data, which posed a challenge to data analysis from the Planck bolometers. Future instruments will face the additional challenges of shared substrate wafers and multiplexed readout wiring. In this work we explore the susceptibility of modern TES arrays to the cosmic ray environment of space using two data sets: the 2015 long-duration balloon flight of the SPIDER cosmic microwave background polarimeter, and a laboratory exposure of SPIDER flight hardware to radioactive sources. We find manageable glitch rates and short glitch durations, leading to minimal effect on SPIDER analysis. We constrain energy propagation within the substrate through a study of multi-detector coincidences, and give a preliminary look at pulse shapes in laboratory data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2002.05771v1-abstract-full').style.display = 'none'; document.getElementById('2002.05771v1-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 February, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2020. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">9 pages, 6 figures, Proceedings of the 18th International Workshop on Low Temperature Detectors</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" 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