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breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Masi%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Masi%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Masi%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Masi%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Masi%2C+S&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Masi%2C+S&start=200" class="pagination-link " aria-label="Page 5" aria-current="page">5 </a> </li> <li> <a 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class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Carralot%2C+F">F. Carralot</a>, <a href="/search/?searchtype=author&query=Carones%2C+A">A. Carones</a>, <a href="/search/?searchtype=author&query=Krachmalnicoff%2C+N">N. Krachmalnicoff</a>, <a href="/search/?searchtype=author&query=Ghigna%2C+T">T. Ghigna</a>, <a href="/search/?searchtype=author&query=Novelli%2C+A">A. Novelli</a>, <a href="/search/?searchtype=author&query=Pagano%2C+L">L. Pagano</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">F. Piacentini</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Adak%2C+D">D. Adak</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Azzoni%2C+S">S. Azzoni</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Basak%2C+S">S. Basak</a>, <a href="/search/?searchtype=author&query=Basyrov%2C+A">A. Basyrov</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Bortolami%2C+M">M. Bortolami</a>, <a href="/search/?searchtype=author&query=Brinckmann%2C+T">T. Brinckmann</a>, <a href="/search/?searchtype=author&query=Cacciotti%2C+F">F. Cacciotti</a>, <a href="/search/?searchtype=author&query=Campeti%2C+P">P. Campeti</a>, <a href="/search/?searchtype=author&query=Carinos%2C+E">E. Carinos</a>, <a href="/search/?searchtype=author&query=Casas%2C+F+J">F. J. Casas</a> , et al. (84 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="2411.02080v1-abstract-short" style="display: inline;"> Future cosmic microwave background (CMB) experiments are primarily targeting a detection of the primordial $B$-mode polarisation. The faintness of this signal requires exquisite control of systematic effects which may bias the measurements. In this work, we derive requirements on the relative calibration accuracy of the overall polarisation gain ($螖g_谓$) for LiteBIRD experiment, through the applic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.02080v1-abstract-full').style.display = 'inline'; document.getElementById('2411.02080v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.02080v1-abstract-full" style="display: none;"> Future cosmic microwave background (CMB) experiments are primarily targeting a detection of the primordial $B$-mode polarisation. The faintness of this signal requires exquisite control of systematic effects which may bias the measurements. In this work, we derive requirements on the relative calibration accuracy of the overall polarisation gain ($螖g_谓$) for LiteBIRD experiment, through the application of the blind Needlet Internal Linear Combination (NILC) foreground-cleaning method. We find that minimum variance techniques, as NILC, are less affected by gain calibration uncertainties than a parametric approach, which requires a proper modelling of these instrumental effects. The tightest constraints are obtained for frequency channels where the CMB signal is relatively brighter (166 GHz channel, $螖{g}_谓\approx 0.16 \%$), while, with a parametric approach, the strictest requirements were on foreground-dominated channels. We then propagate gain calibration uncertainties, corresponding to the derived requirements, into all frequency channels simultaneously. We find that the overall impact on the estimated $r$ is lower than the required budget for LiteBIRD by almost a factor $5$. The adopted procedure to derive requirements assumes a simple Galactic model. We therefore assess the robustness of obtained results against more realistic scenarios by injecting the gain calibration uncertainties, according to the requirements, into LiteBIRD simulated maps and assuming intermediate- and high-complexity sky models. In this case, we employ the so-called Multi-Clustering NILC (MC-NILC) foreground-cleaning pipeline and obtain that the impact of gain calibration uncertainties on $r$ is lower than the LiteBIRD gain systematics budget for the intermediate-complexity sky model. For the high-complexity case, instead, it would be necessary to tighten the requirements by a factor $1.8$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.02080v1-abstract-full').style.display = 'none'; document.getElementById('2411.02080v1-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 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">29 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/2409.20272">arXiv:2409.20272</a> <span> [<a href="https://arxiv.org/pdf/2409.20272">pdf</a>, <a href="https://arxiv.org/format/2409.20272">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="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> KISS: instrument description and performance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mac%C3%ADas-P%C3%A9rez%2C+J+F">J. F. Mac铆as-P茅rez</a>, <a href="/search/?searchtype=author&query=Fern%C3%A1ndez-Torreiro%2C+M">M. Fern谩ndez-Torreiro</a>, <a href="/search/?searchtype=author&query=Catalano%2C+A">A. Catalano</a>, <a href="/search/?searchtype=author&query=Fasano%2C+A">A. Fasano</a>, <a href="/search/?searchtype=author&query=Aguiar%2C+M">M. Aguiar</a>, <a href="/search/?searchtype=author&query=Beelen%2C+A">A. Beelen</a>, <a href="/search/?searchtype=author&query=Benoit%2C+A">A. Benoit</a>, <a href="/search/?searchtype=author&query=Bideaud%2C+A">A. Bideaud</a>, <a href="/search/?searchtype=author&query=Bounmy%2C+J">J. Bounmy</a>, <a href="/search/?searchtype=author&query=Bourrion%2C+O">O. Bourrion</a>, <a href="/search/?searchtype=author&query=Calvo%2C+M">M. Calvo</a>, <a href="/search/?searchtype=author&query=Castro-Almaz%C3%A1n%2C+J+A">J. A. Castro-Almaz谩n</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=de+Petris%2C+M">M. de Petris</a>, <a href="/search/?searchtype=author&query=de+Taoro%2C+A+P">A. P. de Taoro</a>, <a href="/search/?searchtype=author&query=Garde%2C+G">G. Garde</a>, <a href="/search/?searchtype=author&query=G%C3%A9nova-Santos%2C+R+T">R. T. G茅nova-Santos</a>, <a href="/search/?searchtype=author&query=Gomez%2C+A">A. Gomez</a>, <a href="/search/?searchtype=author&query=G%C3%B3mez-Renasco%2C+M+F">M. F. G贸mez-Renasco</a>, <a href="/search/?searchtype=author&query=Goupy%2C+J">J. Goupy</a>, <a href="/search/?searchtype=author&query=Hoarau%2C+C">C. Hoarau</a>, <a href="/search/?searchtype=author&query=Hoyland%2C+R">R. Hoyland</a>, <a href="/search/?searchtype=author&query=Lagache%2C+G">G. Lagache</a>, <a href="/search/?searchtype=author&query=Marpaud%2C+J">J. Marpaud</a>, <a href="/search/?searchtype=author&query=Marton%2C+M">M. Marton</a> , et al. (13 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="2409.20272v1-abstract-short" style="display: inline;"> Kinetic inductance detectors (KIDs) have been proven as reliable systems for astrophysical observations, especially in the millimetre range. Their compact size enables to optimally fill the focal plane, thus boosting sensitivity. The KISS (KIDs Interferometric Spectral Surveyor) instrument is a millimetre camera that consists of two KID arrays of 316 pixels each coupled to a Martin-Puplett interfe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.20272v1-abstract-full').style.display = 'inline'; document.getElementById('2409.20272v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.20272v1-abstract-full" style="display: none;"> Kinetic inductance detectors (KIDs) have been proven as reliable systems for astrophysical observations, especially in the millimetre range. Their compact size enables to optimally fill the focal plane, thus boosting sensitivity. The KISS (KIDs Interferometric Spectral Surveyor) instrument is a millimetre camera that consists of two KID arrays of 316 pixels each coupled to a Martin-Puplett interferometer (MPI). The addition of the MPI grants the KIDs camera the ability to provide spectral information in the 100 and 300 GHz range. In this paper we report the main properties of the KISS instrument and its observations. We also describe the calibration and data analysis procedures used. We present a complete model of the observed data including the sky signal and several identified systematics. We have developed a full photometric and spectroscopic data analysis pipeline that translates our observations into science-ready products. We show examples of the results of this pipeline on selected sources: Moon, Jupiter and Venus. We note the presence of a deficit of response with respect to expectations and laboratory measurements. The detectors noise level is consistent with values obtained during laboratory measurements, pointing to a sub-optimal coupling between the instrument and the telescope as the most probable origin for the problem. This deficit is large enough as to prevent the detection of galaxy clusters, which were KISS main scientific objective. Nevertheless, we have demonstrated the feasibility of this kind of instrument, in the prospect for other KID interferometers (such as the CONCERTO instrument). As this regard, we have developed key instrumental technologies such as optical conception, readout electronics and raw calibration procedures, as well as, adapted data analysis procedures. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.20272v1-abstract-full').style.display = 'none'; document.getElementById('2409.20272v1-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, 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">23 pages, 15 figures. Accepted for publication in Publications of the Astronomical Society of the Pacific</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.18714">arXiv:2409.18714</a> <span> [<a href="https://arxiv.org/pdf/2409.18714">pdf</a>, <a href="https://arxiv.org/format/2409.18714">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"> Spectral Imaging with QUBIC: building astrophysical components from Time-Ordered-Data using Bolometric Interferometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Regnier%2C+M">M. Regnier</a>, <a href="/search/?searchtype=author&query=Laclavere%2C+T">T. Laclavere</a>, <a href="/search/?searchtype=author&query=Hamilton%2C+J">J-Ch. Hamilton</a>, <a href="/search/?searchtype=author&query=Bunn%2C+E">E. Bunn</a>, <a href="/search/?searchtype=author&query=Chabirand%2C+V">V. Chabirand</a>, <a href="/search/?searchtype=author&query=Chanial%2C+P">P. Chanial</a>, <a href="/search/?searchtype=author&query=Goetz%2C+L">L. Goetz</a>, <a href="/search/?searchtype=author&query=Kardum%2C+L">L. Kardum</a>, <a href="/search/?searchtype=author&query=Masson%2C+P">P. Masson</a>, <a href="/search/?searchtype=author&query=Granese%2C+N+M">N. Miron Granese</a>, <a href="/search/?searchtype=author&query=Sc%C3%B3ccola%2C+C+G">C. G. Sc贸ccola</a>, <a href="/search/?searchtype=author&query=Torchinsky%2C+S+A">S. A. Torchinsky</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">E. Battistelli</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=Costanza%2C+B">B. Costanza</a>, <a href="/search/?searchtype=author&query=De+Bernardis%2C+P">P. De Bernardis</a>, <a href="/search/?searchtype=author&query=De+Gasperis%2C+G">G. De Gasperis</a>, <a href="/search/?searchtype=author&query=Ferazzoli%2C+S">S. Ferazzoli</a>, <a href="/search/?searchtype=author&query=Flood%2C+A">A. Flood</a>, <a href="/search/?searchtype=author&query=Ganga%2C+K">K. Ganga</a>, <a href="/search/?searchtype=author&query=Gervasi%2C+M">M. Gervasi</a>, <a href="/search/?searchtype=author&query=Grandsire%2C+L">L. Grandsire</a>, <a href="/search/?searchtype=author&query=Manzan%2C+E+.">E . Manzan</a> , et al. (11 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="2409.18714v1-abstract-short" style="display: inline;"> The detection of B-modes in the CMB polarization pattern is a major issue in modern cosmology and must therefore be handled with analytical methods that produce reliable results. We describe a method that uses the frequency dependency of the QUBIC synthesized beam to perform component separation at the map-making stage, to obtain more precise results. We aim to demonstrate the feasibility of compo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.18714v1-abstract-full').style.display = 'inline'; document.getElementById('2409.18714v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.18714v1-abstract-full" style="display: none;"> The detection of B-modes in the CMB polarization pattern is a major issue in modern cosmology and must therefore be handled with analytical methods that produce reliable results. We describe a method that uses the frequency dependency of the QUBIC synthesized beam to perform component separation at the map-making stage, to obtain more precise results. We aim to demonstrate the feasibility of component separation during the map-making stage in time domain space. This new technique leads to a more accurate description of the data and reduces the biases in cosmological analysis. The method uses a library for highly parallel computation which facilitates the programming and permits the description of experiments as easily manipulated operators. These operators can be combined to obtain a joint analysis using several experiments leading to maximized precision. The results show that the method works well and permits end-to-end analysis for the CMB experiments, and in particular, for QUBIC. The method includes astrophysical foregrounds, and also systematic effects like gain variation in the detectors. We developed a software pipeline that produces uncertainties on tensor-to-scalar ratio at the level of $蟽(r) \sim 0.023$ using only QUBIC simulated data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.18714v1-abstract-full').style.display = 'none'; document.getElementById('2409.18714v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 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">15 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/2409.18698">arXiv:2409.18698</a> <span> [<a href="https://arxiv.org/pdf/2409.18698">pdf</a>, <a href="https://arxiv.org/format/2409.18698">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"> Spectral Imaging with QUBIC: building frequency maps from Time-Ordered-Data using Bolometric Interferometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Chanial%2C+P">P. Chanial</a>, <a href="/search/?searchtype=author&query=Regnier%2C+M">M. Regnier</a>, <a href="/search/?searchtype=author&query=Hamilton%2C+J">J-Ch. Hamilton</a>, <a href="/search/?searchtype=author&query=Bunn%2C+E">E. Bunn</a>, <a href="/search/?searchtype=author&query=Chabirand%2C+V">V. Chabirand</a>, <a href="/search/?searchtype=author&query=Flood%2C+A">A. Flood</a>, <a href="/search/?searchtype=author&query=Lerena%2C+M+M+G">M. M. Gamboa Lerena</a>, <a href="/search/?searchtype=author&query=Kardum%2C+L">L. Kardum</a>, <a href="/search/?searchtype=author&query=Laclavere%2C+T">T. Laclavere</a>, <a href="/search/?searchtype=author&query=Manzan%2C+E+.">E . Manzan</a>, <a href="/search/?searchtype=author&query=Mousset%2C+L">L. Mousset</a>, <a href="/search/?searchtype=author&query=Stolpovskiy%2C+M">M. Stolpovskiy</a>, <a href="/search/?searchtype=author&query=Torchinsky%2C+S+A">S. A. Torchinsky</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">E. Battistelli</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=Costanza%2C+B">B. Costanza</a>, <a href="/search/?searchtype=author&query=De+Bernardis%2C+P">P. De Bernardis</a>, <a href="/search/?searchtype=author&query=De+Gasperis%2C+G">G. De Gasperis</a>, <a href="/search/?searchtype=author&query=Ferazzoli%2C+S">S. Ferazzoli</a>, <a href="/search/?searchtype=author&query=Ganga%2C+K">K. Ganga</a>, <a href="/search/?searchtype=author&query=Gervasi%2C+M">M. Gervasi</a>, <a href="/search/?searchtype=author&query=Grandsire%2C+L">L. Grandsire</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a> , et al. (10 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="2409.18698v1-abstract-short" style="display: inline;"> The search for relics from the inflation era in the form of B-mode polarization of the CMB is a major challenge in cosmology. The main obstacle appears to come from the complexity of Galactic foregrounds that need to be removed. Multi-frequency observations are key to mitigating their contamination and mapping primordial fluctuations. We present "Spectral-Imaging", a method to reconstruct sub-freq… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.18698v1-abstract-full').style.display = 'inline'; document.getElementById('2409.18698v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.18698v1-abstract-full" style="display: none;"> The search for relics from the inflation era in the form of B-mode polarization of the CMB is a major challenge in cosmology. The main obstacle appears to come from the complexity of Galactic foregrounds that need to be removed. Multi-frequency observations are key to mitigating their contamination and mapping primordial fluctuations. We present "Spectral-Imaging", a method to reconstruct sub-frequency maps of the CMB polarization within the instrument's physical bandwidth, a unique feature of Bolometric Interferometry that could be crucial for foreground mitigation as it provides an increased spectral resolution. Our technique uses the frequency evolution of the shape of the Bolometric Interferometer's synthesized beam to reconstruct frequency information from the time domain data. We reconstruct sub-frequency maps using an inverse problem approach based on detailed modeling of the instrument acquisition. We use external data to regularize the convergence of the estimator and account for bandpass mismatch and varying angular resolution. The reconstructed maps are unbiased and allow exploiting the spectral-imaging capacity of QUBIC. Using end-to-end simulations of the QUBIC instrument, we perform a cross-spectra analysis to extract a forecast on the tensor-to-scalar ratio constraint of $蟽(r) = 0.0225$ after component separation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.18698v1-abstract-full').style.display = 'none'; document.getElementById('2409.18698v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 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">14 pages, 8 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/2408.03040">arXiv:2408.03040</a> <span> [<a href="https://arxiv.org/pdf/2408.03040">pdf</a>, <a href="https://arxiv.org/format/2408.03040">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"> Multi-dimensional optimisation of the scanning strategy for the LiteBIRD space mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Takase%2C+Y">Y. Takase</a>, <a href="/search/?searchtype=author&query=Vacher%2C+L">L. Vacher</a>, <a href="/search/?searchtype=author&query=Ishino%2C+H">H. Ishino</a>, <a href="/search/?searchtype=author&query=Patanchon%2C+G">G. Patanchon</a>, <a href="/search/?searchtype=author&query=Montier%2C+L">L. Montier</a>, <a href="/search/?searchtype=author&query=Stever%2C+S+L">S. L. Stever</a>, <a href="/search/?searchtype=author&query=Ishizaka%2C+K">K. Ishizaka</a>, <a href="/search/?searchtype=author&query=Nagano%2C+Y">Y. Nagano</a>, <a href="/search/?searchtype=author&query=Wang%2C+W">W. Wang</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Aizawa%2C+K">K. Aizawa</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Basak%2C+S">S. Basak</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Bortolami%2C+M">M. Bortolami</a>, <a href="/search/?searchtype=author&query=Brinckmann%2C+T">T. Brinckmann</a>, <a href="/search/?searchtype=author&query=Calabrese%2C+E">E. Calabrese</a>, <a href="/search/?searchtype=author&query=Campeti%2C+P">P. Campeti</a>, <a href="/search/?searchtype=author&query=Carinos%2C+E">E. Carinos</a>, <a href="/search/?searchtype=author&query=Carones%2C+A">A. Carones</a> , et al. (83 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="2408.03040v2-abstract-short" style="display: inline;"> Large angular scale surveys in the absence of atmosphere are essential for measuring the primordial $B$-mode power spectrum of the Cosmic Microwave Background (CMB). Since this proposed measurement is about three to four orders of magnitude fainter than the temperature anisotropies of the CMB, in-flight calibration of the instruments and active suppression of systematic effects are crucial. We inv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03040v2-abstract-full').style.display = 'inline'; document.getElementById('2408.03040v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.03040v2-abstract-full" style="display: none;"> Large angular scale surveys in the absence of atmosphere are essential for measuring the primordial $B$-mode power spectrum of the Cosmic Microwave Background (CMB). Since this proposed measurement is about three to four orders of magnitude fainter than the temperature anisotropies of the CMB, in-flight calibration of the instruments and active suppression of systematic effects are crucial. We investigate the effect of changing the parameters of the scanning strategy on the in-flight calibration effectiveness, the suppression of the systematic effects themselves, and the ability to distinguish systematic effects by null-tests. Next-generation missions such as LiteBIRD, modulated by a Half-Wave Plate (HWP), will be able to observe polarisation using a single detector, eliminating the need to combine several detectors to measure polarisation, as done in many previous experiments and hence avoiding the consequent systematic effects. While the HWP is expected to suppress many systematic effects, some of them will remain. We use an analytical approach to comprehensively address the mitigation of these systematic effects and identify the characteristics of scanning strategies that are the most effective for implementing a variety of calibration strategies in the multi-dimensional space of common spacecraft scan parameters. We also present Falcons, a fast spacecraft scanning simulator that we developed to investigate this scanning parameter space. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03040v2-abstract-full').style.display = 'none'; document.getElementById('2408.03040v2-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">v1</span> submitted 6 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.17555">arXiv:2407.17555</a> <span> [<a href="https://arxiv.org/pdf/2407.17555">pdf</a>, <a href="https://arxiv.org/format/2407.17555">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"> LiteBIRD Science Goals and Forecasts. Mapping the Hot Gas in the Universe </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Remazeilles%2C+M">M. Remazeilles</a>, <a href="/search/?searchtype=author&query=Douspis%2C+M">M. Douspis</a>, <a href="/search/?searchtype=author&query=Rubi%C3%B1o-Mart%C3%ADn%2C+J+A">J. A. Rubi帽o-Mart铆n</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Chluba%2C+J">J. Chluba</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Hern%C3%A1ndez-Monteagudo%2C+C">C. Hern谩ndez-Monteagudo</a>, <a href="/search/?searchtype=author&query=Luzzi%2C+G">G. Luzzi</a>, <a href="/search/?searchtype=author&query=Macias-Perez%2C+J">J. Macias-Perez</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Namikawa%2C+T">T. Namikawa</a>, <a href="/search/?searchtype=author&query=Salvati%2C+L">L. Salvati</a>, <a href="/search/?searchtype=author&query=Tanimura%2C+H">H. Tanimura</a>, <a href="/search/?searchtype=author&query=Aizawa%2C+K">K. Aizawa</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Basak%2C+S">S. Basak</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Blinov%2C+D">D. Blinov</a>, <a href="/search/?searchtype=author&query=Bortolami%2C+M">M. Bortolami</a> , et al. (82 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="2407.17555v2-abstract-short" style="display: inline;"> We assess the capabilities of the LiteBIRD mission to map the hot gas distribution in the Universe through the thermal Sunyaev-Zeldovich (SZ) effect. Our analysis relies on comprehensive simulations incorporating various sources of Galactic and extragalactic foreground emission, while accounting for specific instrumental characteristics of LiteBIRD, such as detector sensitivities, frequency-depend… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.17555v2-abstract-full').style.display = 'inline'; document.getElementById('2407.17555v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.17555v2-abstract-full" style="display: none;"> We assess the capabilities of the LiteBIRD mission to map the hot gas distribution in the Universe through the thermal Sunyaev-Zeldovich (SZ) effect. Our analysis relies on comprehensive simulations incorporating various sources of Galactic and extragalactic foreground emission, while accounting for specific instrumental characteristics of LiteBIRD, such as detector sensitivities, frequency-dependent beam convolution, inhomogeneous sky scanning, and $1/f$ noise. We implement a tailored component-separation pipeline to map the thermal SZ Compton $y$-parameter over 98% of the sky. Despite lower angular resolution for galaxy cluster science, LiteBIRD provides full-sky coverage and, compared to the Planck satellite, enhanced sensitivity, as well as more frequency bands to enable the construction of an all-sky $y$-map, with reduced foreground contamination at large and intermediate angular scales. By combining LiteBIRD and Planck channels in the component-separation pipeline, we obtain an optimal $y$-map that leverages the advantages of both experiments, with the higher angular resolution of the Planck channels enabling the recovery of compact clusters beyond the LiteBIRD beam limitations, and the numerous sensitive LiteBIRD channels further mitigating foregrounds. The added value of LiteBIRD is highlighted through the examination of maps, power spectra, and one-point statistics of the various sky components. After component separation, the $1/f$ noise from LiteBIRD is effectively mitigated below the thermal SZ signal at all multipoles. Cosmological constraints on $S_8=蟽_8\left(惟_{\rm m}/0.3\right)^{0.5}$ obtained from the LiteBIRD-Planck combined $y$-map power spectrum exhibits a 15% reduction in uncertainty compared to constraints from Planck alone. This improvement can be attributed to the increased portion of uncontaminated sky available in the LiteBIRD-Planck combined $y$-map. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.17555v2-abstract-full').style.display = 'none'; document.getElementById('2407.17555v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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">38 pages, 13 figures, abstract shortened. Updated to match version accepted by 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/2407.15294">arXiv:2407.15294</a> <span> [<a href="https://arxiv.org/pdf/2407.15294">pdf</a>, <a href="https://arxiv.org/format/2407.15294">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"> Systematic effects induced by half-wave plate differential optical load and TES nonlinearity for LiteBIRD </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Micheli%2C+S">Silvia Micheli</a>, <a href="/search/?searchtype=author&query=de+Haan%2C+T">Tijmen de Haan</a>, <a href="/search/?searchtype=author&query=Ghigna%2C+T">Tommaso Ghigna</a>, <a href="/search/?searchtype=author&query=Novelli%2C+A">Alessandro Novelli</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">Francesco Piacentini</a>, <a href="/search/?searchtype=author&query=Pisano%2C+G">Giampaolo Pisano</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">Fabio Columbro</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">Alessandro Coppolecchia</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">Giuseppe D'Alessandro</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">Luca Lamagna</a>, <a href="/search/?searchtype=author&query=Marchitelli%2C+E">Elisabetta Marchitelli</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">Silvia Masi</a>, <a href="/search/?searchtype=author&query=Occhiuzzi%2C+A">Andrea Occhiuzzi</a>, <a href="/search/?searchtype=author&query=Paiella%2C+A">Alessandro Paiella</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="2407.15294v1-abstract-short" style="display: inline;"> LiteBIRD, a forthcoming satellite mission, aims to measure the polarization of the Cosmic Microwave Background (CMB) across the entire sky. The experiment will employ three telescopes, Transition-Edge Sensor (TES) bolometers and rotating Half-Wave Plates (HWPs) at cryogenic temperatures to ensure high sensitivity and systematic effects mitigation. This study is focused on the Mid- and High-Frequen… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.15294v1-abstract-full').style.display = 'inline'; document.getElementById('2407.15294v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.15294v1-abstract-full" style="display: none;"> LiteBIRD, a forthcoming satellite mission, aims to measure the polarization of the Cosmic Microwave Background (CMB) across the entire sky. The experiment will employ three telescopes, Transition-Edge Sensor (TES) bolometers and rotating Half-Wave Plates (HWPs) at cryogenic temperatures to ensure high sensitivity and systematic effects mitigation. This study is focused on the Mid- and High-Frequency Telescopes (MHFT), which will use rotating metal mesh HWPs. We investigate how power variations due to HWP differential emissivity and transmittance combine with TES nonlinear responsivity, resulting in an effective instrumental polarization. We present the results of simulations for the current HWP design, modeling the TES deviation from linearity as a second-order response. We quantify the level of acceptable residual nonlinearity assuming the mission requirement on the tensor-to-scalar ratio, $未r < 0.001$. Moreover, we provide an accuracy requirement on the measurement of TES responsivity nonlinearity level for MHFT channels. Lastly, we present possible mitigation methods that will be developed in future studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.15294v1-abstract-full').style.display = 'none'; document.getElementById('2407.15294v1-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 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">Proceedings of SPIE Astronomical Telescopes + Instrumentation 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/2406.09349">arXiv:2406.09349</a> <span> [<a href="https://arxiv.org/pdf/2406.09349">pdf</a>, <a href="https://arxiv.org/format/2406.09349">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"> Measuring the CMB spectral distortions with COSMO: the multi-mode antenna system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Manzan%2C+E">E. Manzan</a>, <a href="/search/?searchtype=author&query=Albano%2C+L">L. Albano</a>, <a href="/search/?searchtype=author&query=Franceschet%2C+C">C. Franceschet</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Cacciotti%2C+F">F. Cacciotti</a>, <a href="/search/?searchtype=author&query=Capponi%2C+A">A. Capponi</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Conenna%2C+G">G. Conenna</a>, <a href="/search/?searchtype=author&query=Coppi%2C+G">G. Coppi</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=De+Gasperis%2C+G">G. De Gasperis</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Gervasi%2C+M">M. Gervasi</a>, <a href="/search/?searchtype=author&query=Isopi%2C+G">G. Isopi</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">L. Lamagna</a>, <a href="/search/?searchtype=author&query=Limonta%2C+A">A. Limonta</a>, <a href="/search/?searchtype=author&query=Marchitelli%2C+E">E. Marchitelli</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=Montonati%2C+F">F. Montonati</a>, <a href="/search/?searchtype=author&query=Nati%2C+F">F. Nati</a>, <a href="/search/?searchtype=author&query=Occhiuzzi%2C+A">A. Occhiuzzi</a> , et al. (7 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="2406.09349v1-abstract-short" style="display: inline;"> In this work, we present the design and manufacturing of the two multi-mode antenna arrays of the COSMO experiment and the preliminary beam pattern measurements of their fundamental mode compared with simulations. COSMO is a cryogenic Martin-Puplett Fourier Transform Spectrometer that aims at measuring the isotropic y-type spectral distortion of the Cosmic Microwave Background from Antarctica, b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.09349v1-abstract-full').style.display = 'inline'; document.getElementById('2406.09349v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.09349v1-abstract-full" style="display: none;"> In this work, we present the design and manufacturing of the two multi-mode antenna arrays of the COSMO experiment and the preliminary beam pattern measurements of their fundamental mode compared with simulations. COSMO is a cryogenic Martin-Puplett Fourier Transform Spectrometer that aims at measuring the isotropic y-type spectral distortion of the Cosmic Microwave Background from Antarctica, by performing differential measurements between the sky and an internal, cryogenic reference blackbody. To reduce the atmospheric contribution, a spinning wedge mirror performs fast sky-dips at varying elevations while fast, low-noise Kinetic Inductance detectors scan the interferogram. Two arrays of antennas couple the radiation to the detectors. Each array consists of nine smooth-walled multi-mode feed-horns, operating in the $120-180$ GHz and $210-300$ GHz range, respectively. The multi-mode propagation helps increase the instrumental sensitivity without employing large focal planes with hundreds of detectors. The two arrays have a step-linear and a linear profile, respectively, and are obtained by superimposing aluminum plates made with CNC milling. The simulated multi-mode beam pattern has a $\sim 20^{\circ} - 26^{\circ}$ FWHM for the low-frequency array and $\sim 16^{\circ}$ FWHM for the high-frequency one. The side lobes are below $-15$ dB. To characterize the antenna response, we measured the beam pattern of the fundamental mode using a Vector Network Analyzer, in far-field conditions inside an anechoic chamber at room temperature. We completed the measurements of the low-frequency array and found a good agreement with the simulations. We also identified a few non-idealities that we attribute to the measuring setup and will further investigate. A comprehensive multi-mode measurement will be feasible at cryogenic temperature once the full receiver is integrated. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.09349v1-abstract-full').style.display = 'none'; document.getElementById('2406.09349v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">To appear in Proceedings of the SPIE Astronomical Telescopes + Instrumentation, 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/2406.02724">arXiv:2406.02724</a> <span> [<a href="https://arxiv.org/pdf/2406.02724">pdf</a>, <a href="https://arxiv.org/format/2406.02724">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"> The LiteBIRD mission to explore cosmic inflation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ghigna%2C+T">T. Ghigna</a>, <a href="/search/?searchtype=author&query=Adler%2C+A">A. Adler</a>, <a href="/search/?searchtype=author&query=Aizawa%2C+K">K. Aizawa</a>, <a href="/search/?searchtype=author&query=Akamatsu%2C+H">H. Akamatsu</a>, <a href="/search/?searchtype=author&query=Akizawa%2C+R">R. Akizawa</a>, <a href="/search/?searchtype=author&query=Allys%2C+E">E. Allys</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Austermann%2C+J">J. Austermann</a>, <a href="/search/?searchtype=author&query=Azzoni%2C+S">S. Azzoni</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Basak%2C+S">S. Basak</a>, <a href="/search/?searchtype=author&query=Basyrov%2C+A">A. Basyrov</a>, <a href="/search/?searchtype=author&query=Beckman%2C+S">S. Beckman</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Bortolami%2C+M">M. Bortolami</a>, <a href="/search/?searchtype=author&query=Bouchet%2C+F">F. Bouchet</a>, <a href="/search/?searchtype=author&query=Brinckmann%2C+T">T. Brinckmann</a>, <a href="/search/?searchtype=author&query=Campeti%2C+P">P. Campeti</a>, <a href="/search/?searchtype=author&query=Carinos%2C+E">E. Carinos</a>, <a href="/search/?searchtype=author&query=Carones%2C+A">A. Carones</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="2406.02724v1-abstract-short" style="display: inline;"> LiteBIRD, the next-generation cosmic microwave background (CMB) experiment, aims for a launch in Japan's fiscal year 2032, marking a major advancement in the exploration of primordial cosmology and fundamental physics. Orbiting the Sun-Earth Lagrangian point L2, this JAXA-led strategic L-class mission will conduct a comprehensive mapping of the CMB polarization across the entire sky. During its 3-… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.02724v1-abstract-full').style.display = 'inline'; document.getElementById('2406.02724v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.02724v1-abstract-full" style="display: none;"> LiteBIRD, the next-generation cosmic microwave background (CMB) experiment, aims for a launch in Japan's fiscal year 2032, marking a major advancement in the exploration of primordial cosmology and fundamental physics. Orbiting the Sun-Earth Lagrangian point L2, this JAXA-led strategic L-class mission will conduct a comprehensive mapping of the CMB polarization across the entire sky. During its 3-year mission, LiteBIRD will employ three telescopes within 15 unique frequency bands (ranging from 34 through 448 GHz), targeting a sensitivity of 2.2\,$渭$K-arcmin and a resolution of 0.5$^\circ$ at 100\,GHz. Its primary goal is to measure the tensor-to-scalar ratio $r$ with an uncertainty $未r = 0.001$, including systematic errors and margin. If $r \geq 0.01$, LiteBIRD expects to achieve a $>5蟽$ detection in the $\ell=$2-10 and $\ell=$11-200 ranges separately, providing crucial insight into the early Universe. We describe LiteBIRD's scientific objectives, the application of systems engineering to mission requirements, the anticipated scientific impact, and the operations and scanning strategies vital to minimizing systematic effects. We will also highlight LiteBIRD's synergies with concurrent CMB projects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.02724v1-abstract-full').style.display = 'none'; document.getElementById('2406.02724v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">23 pages, 9 figures, 1 table, SPIE Astronomical Telescopes + Instrumentation 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/2404.04414">arXiv:2404.04414</a> <span> [<a href="https://arxiv.org/pdf/2404.04414">pdf</a>, <a href="https://arxiv.org/format/2404.04414">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/10.1051/epjconf/202429300049">10.1051/epjconf/202429300049 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> OLIMPO: a Balloon-Borne SZE Imager to Probe ICM Dynamics and the WHIM </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sayers%2C+J">Jack Sayers</a>, <a href="/search/?searchtype=author&query=Avestruz%2C+C">Camille Avestruz</a>, <a href="/search/?searchtype=author&query=Thakur%2C+R+B">Ritoban Basu Thakur</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">Elia Stefano Battistelli</a>, <a href="/search/?searchtype=author&query=Bulbul%2C+E">Esra Bulbul</a>, <a href="/search/?searchtype=author&query=Caccioti%2C+F">Federico Caccioti</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">Fabio Columbro</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">Alessandro Coppolecchia</a>, <a href="/search/?searchtype=author&query=Cray%2C+S">Scott Cray</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">Giuseppe D'Alessandro</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=de+Petris%2C+M">Marco de Petris</a>, <a href="/search/?searchtype=author&query=Hanany%2C+S">Shaul Hanany</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">Luca Lamagna</a>, <a href="/search/?searchtype=author&query=Lau%2C+E">Erwin Lau</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">Silvia Masi</a>, <a href="/search/?searchtype=author&query=Paiella%2C+A">Allesandro Paiella</a>, <a href="/search/?searchtype=author&query=Pettinari%2C+G">Giorgio Pettinari</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">Francesco Piacentini</a>, <a href="/search/?searchtype=author&query=Rapaport%2C+E">Eitan Rapaport</a>, <a href="/search/?searchtype=author&query=Rudnick%2C+L">Larry Rudnick</a>, <a href="/search/?searchtype=author&query=Zhuravleva%2C+I">Irina Zhuravleva</a>, <a href="/search/?searchtype=author&query=ZuHuone%2C+J">John ZuHuone</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="2404.04414v1-abstract-short" style="display: inline;"> OLIMPO is a proposed Antarctic balloon-borne Sunyaev-Zel'dovich effect (SZE) imager to study gas dynamics associated with structure formation along with the properties of the warm-hot intergalactic medium (WHIM) residing in the connective filaments. During a 25 day flight OLIMPO will image a total of 10 z~0.05 galaxy clusters and 8 bridges at 145, 250, 365, and 460 GHz at an angular resolution of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04414v1-abstract-full').style.display = 'inline'; document.getElementById('2404.04414v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.04414v1-abstract-full" style="display: none;"> OLIMPO is a proposed Antarctic balloon-borne Sunyaev-Zel'dovich effect (SZE) imager to study gas dynamics associated with structure formation along with the properties of the warm-hot intergalactic medium (WHIM) residing in the connective filaments. During a 25 day flight OLIMPO will image a total of 10 z~0.05 galaxy clusters and 8 bridges at 145, 250, 365, and 460 GHz at an angular resolution of 1.0'-3.3'. The maps will be significantly deeper than those planned from CMB-S4 and CCAT-P, and will have excellent fidelity to the large angular scales of our low-z targets, which are difficult to probe from the ground. In combination with X-ray data from eROSITA and XRISM we will transform our current static view of galaxy clusters into a full dynamic picture by measuring the internal intra-cluster medium (ICM) velocity structure with the kinematic SZE, X-ray spectroscopy, and the power spectrum of ICM fluctuations. Radio observations from ASKAP and MeerKAT will be used to better understand the connection between ICM turbulence and shocks with the relativistic plasma. Beyond the cluster boundary, we will combine thermal SZE maps from OLIMPO with X-ray imaging from eROSITA to measure the thermodynamics of the WHIM residing in filaments, providing a better understanding of its properties and its contribution to the total baryon budget. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.04414v1-abstract-full').style.display = 'none'; document.getElementById('2404.04414v1-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">From the proceedings of the mm Universe 2023</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.16763">arXiv:2403.16763</a> <span> [<a href="https://arxiv.org/pdf/2403.16763">pdf</a>, <a href="https://arxiv.org/format/2403.16763">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"> LiteBIRD Science Goals and Forecasts: Primordial Magnetic Fields </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Paoletti%2C+D">D. Paoletti</a>, <a href="/search/?searchtype=author&query=Rubino-Martin%2C+J">J. Rubino-Martin</a>, <a href="/search/?searchtype=author&query=Shiraishi%2C+M">M. Shiraishi</a>, <a href="/search/?searchtype=author&query=Molinari%2C+D">D. Molinari</a>, <a href="/search/?searchtype=author&query=Chluba%2C+J">J. Chluba</a>, <a href="/search/?searchtype=author&query=Finelli%2C+F">F. Finelli</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Errard%2C+J">J. Errard</a>, <a href="/search/?searchtype=author&query=Gruppuso%2C+A">A. Gruppuso</a>, <a href="/search/?searchtype=author&query=Lonappan%2C+A+I">A. I. Lonappan</a>, <a href="/search/?searchtype=author&query=Tartari%2C+A">A. Tartari</a>, <a href="/search/?searchtype=author&query=Allys%2C+E">E. Allys</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Bortolami%2C+M">M. Bortolami</a>, <a href="/search/?searchtype=author&query=Brinckmann%2C+T">T. Brinckmann</a>, <a href="/search/?searchtype=author&query=Calabrese%2C+E">E. Calabrese</a>, <a href="/search/?searchtype=author&query=Campeti%2C+P">P. Campeti</a>, <a href="/search/?searchtype=author&query=Carones%2C+A">A. Carones</a>, <a href="/search/?searchtype=author&query=Casas%2C+F+J">F. J. Casas</a> , et al. (75 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="2403.16763v1-abstract-short" style="display: inline;"> We present detailed forecasts for the constraints on primordial magnetic fields (PMFs) that will be obtained with the LiteBIRD satellite. The constraints are driven by the effects of PMFs on the CMB anisotropies: the gravitational effects of magnetically-induced perturbations; the effects on the thermal and ionization history of the Universe; the Faraday rotation imprint on the CMB polarization; a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16763v1-abstract-full').style.display = 'inline'; document.getElementById('2403.16763v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.16763v1-abstract-full" style="display: none;"> We present detailed forecasts for the constraints on primordial magnetic fields (PMFs) that will be obtained with the LiteBIRD satellite. The constraints are driven by the effects of PMFs on the CMB anisotropies: the gravitational effects of magnetically-induced perturbations; the effects on the thermal and ionization history of the Universe; the Faraday rotation imprint on the CMB polarization; and the non-Gaussianities induced in polarization anisotropies. LiteBIRD represents a sensitive probe for PMFs and by exploiting all the physical effects, it will be able to improve the current limit coming from Planck. In particular, thanks to its accurate $B$-mode polarization measurement, LiteBIRD will improve the constraints on infrared configurations for the gravitational effect, giving $B_{\rm 1\,Mpc}^{n_{\rm B} =-2.9} < 0.8$ nG at 95% C.L., potentially opening the possibility to detect nanogauss fields with high significance. We also observe a significant improvement in the limits when marginalized over the spectral index, $B_{1\,{\rm Mpc}}^{\rm marg}< 2.2$ nG at 95% C.L. From the thermal history effect, which relies mainly on $E$-mode polarization data, we obtain a significant improvement for all PMF configurations, with the marginalized case, $\sqrt{\langle B^2\rangle}^{\rm marg}<0.50$ nG at 95% C.L. Faraday rotation constraints will take advantage of the wide frequency coverage of LiteBIRD and the high sensitivity in $B$ modes, improving the limits by orders of magnitude with respect to current results, $B_{1\,{\rm Mpc}}^{n_{\rm B} =-2.9} < 3.2$ nG at 95% C.L. Finally, non-Gaussianities of the $B$-mode polarization can probe PMFs at the level of 1 nG, again significantly improving the current bounds from Planck. Altogether our forecasts represent a broad collection of complementary probes, providing conservative limits on PMF characteristics that will be achieved with LiteBIRD. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.16763v1-abstract-full').style.display = 'none'; document.getElementById('2403.16763v1-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">51 pages, 24 figures, abstract shortened</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.09001">arXiv:2312.09001</a> <span> [<a href="https://arxiv.org/pdf/2312.09001">pdf</a>, <a href="https://arxiv.org/format/2312.09001">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"> Impact of beam far side-lobe knowledge in the presence of foregrounds for LiteBIRD </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Leloup%2C+C">C. Leloup</a>, <a href="/search/?searchtype=author&query=Patanchon%2C+G">G. Patanchon</a>, <a href="/search/?searchtype=author&query=Errard%2C+J">J. Errard</a>, <a href="/search/?searchtype=author&query=Franceschet%2C+C">C. Franceschet</a>, <a href="/search/?searchtype=author&query=Gudmundsson%2C+J+E">J. E. Gudmundsson</a>, <a href="/search/?searchtype=author&query=Henrot-Versill%C3%A9%2C+S">S. Henrot-Versill茅</a>, <a href="/search/?searchtype=author&query=Imada%2C+H">H. Imada</a>, <a href="/search/?searchtype=author&query=Ishino%2C+H">H. Ishino</a>, <a href="/search/?searchtype=author&query=Matsumura%2C+T">T. Matsumura</a>, <a href="/search/?searchtype=author&query=Puglisi%2C+G">G. Puglisi</a>, <a href="/search/?searchtype=author&query=Wang%2C+W">W. Wang</a>, <a href="/search/?searchtype=author&query=Adler%2C+A">A. Adler</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Aurlien%2C+R">R. Aurlien</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Basyrov%2C+A">A. Basyrov</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Blinov%2C+D">D. Blinov</a>, <a href="/search/?searchtype=author&query=Bortolami%2C+M">M. Bortolami</a>, <a href="/search/?searchtype=author&query=Brinckmann%2C+T">T. Brinckmann</a>, <a href="/search/?searchtype=author&query=Campeti%2C+P">P. Campeti</a> , et al. (86 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="2312.09001v1-abstract-short" style="display: inline;"> We present a study of the impact of an uncertainty in the beam far side-lobe knowledge on the measurement of the Cosmic Microwave Background $B$-mode signal at large scale. It is expected to be one of the main source of systematic effects in future CMB observations. Because it is crucial for all-sky survey missions to take into account the interplays between beam systematic effects and all the dat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09001v1-abstract-full').style.display = 'inline'; document.getElementById('2312.09001v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.09001v1-abstract-full" style="display: none;"> We present a study of the impact of an uncertainty in the beam far side-lobe knowledge on the measurement of the Cosmic Microwave Background $B$-mode signal at large scale. It is expected to be one of the main source of systematic effects in future CMB observations. Because it is crucial for all-sky survey missions to take into account the interplays between beam systematic effects and all the data analysis steps, the primary goal of this paper is to provide the methodology to carry out the end-to-end study of their effect for a space-borne CMB polarization experiment, up to the cosmological results in the form of a bias $未r$ on the tensor-to-scalar ratio $r$. LiteBIRD is dedicated to target the measurement of CMB primordial $B$ modes by reaching a sensitivity of $蟽\left( r \right) \leq 10^{-3}$ assuming $r=0$. As a demonstration of our framework, we derive the relationship between the knowledge of the beam far side-lobes and the tentatively allocated error budget under given assumptions on design, simulation and component separation method. We assume no mitigation of the far side-lobes effect at any stage of the analysis pipeline. We show that $未r$ is mostly due to the integrated fractional power difference between the estimated beams and the true beams in the far side-lobes region, with little dependence on the actual shape of the beams, for low enough $未r$. Under our set of assumptions, in particular considering the specific foreground cleaning method we used, we find that the integrated fractional power in the far side-lobes should be known at a level as tight as $\sim 10^{-4}$, to achieve the required limit on the bias $未r < 1.9 \times 10^{-5}$. The framework and tools developed for this study can be easily adapted to provide requirements under different design, data analysis frameworks and for other future space-borne experiments beyond LiteBIRD. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09001v1-abstract-full').style.display = 'none'; document.getElementById('2312.09001v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.05194">arXiv:2312.05194</a> <span> [<a href="https://arxiv.org/pdf/2312.05194">pdf</a>, <a href="https://arxiv.org/format/2312.05194">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"> LiteBIRD Science Goals and Forecasts: Improving Sensitivity to Inflationary Gravitational Waves with Multitracer Delensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Namikawa%2C+T">T. Namikawa</a>, <a href="/search/?searchtype=author&query=Lonappan%2C+A+I">A. I. Lonappan</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/?searchtype=author&query=Benabed%2C+K">K. Benabed</a>, <a href="/search/?searchtype=author&query=Challinor%2C+A">A. Challinor</a>, <a href="/search/?searchtype=author&query=Diego-Palazuelos%2C+P">P. Diego-Palazuelos</a>, <a href="/search/?searchtype=author&query=Errard%2C+J">J. Errard</a>, <a href="/search/?searchtype=author&query=Farrens%2C+S">S. Farrens</a>, <a href="/search/?searchtype=author&query=Gruppuso%2C+A">A. Gruppuso</a>, <a href="/search/?searchtype=author&query=Krachmalnicoff%2C+N">N. Krachmalnicoff</a>, <a href="/search/?searchtype=author&query=Migliaccio%2C+M">M. Migliaccio</a>, <a href="/search/?searchtype=author&query=Mart%C3%ADnez-Gonz%C3%A1lez%2C+E">E. Mart铆nez-Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Pettorino%2C+V">V. Pettorino</a>, <a href="/search/?searchtype=author&query=Piccirilli%2C+G">G. Piccirilli</a>, <a href="/search/?searchtype=author&query=Ruiz-Granda%2C+M">M. Ruiz-Granda</a>, <a href="/search/?searchtype=author&query=Sherwin%2C+B">B. Sherwin</a>, <a href="/search/?searchtype=author&query=Starck%2C+J">J. Starck</a>, <a href="/search/?searchtype=author&query=Vielva%2C+P">P. Vielva</a>, <a href="/search/?searchtype=author&query=Akizawa%2C+R">R. Akizawa</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Aurlien%2C+R">R. Aurlien</a>, <a href="/search/?searchtype=author&query=Azzoni%2C+S">S. Azzoni</a> , et al. (97 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="2312.05194v1-abstract-short" style="display: inline;"> We estimate the efficiency of mitigating the lensing $B$-mode polarization, the so-called delensing, for the $LiteBIRD$ experiment with multiple external data sets of lensing-mass tracers. The current best bound on the tensor-to-scalar ratio, $r$, is limited by lensing rather than Galactic foregrounds. Delensing will be a critical step to improve sensitivity to $r$ as measurements of $r$ become mo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05194v1-abstract-full').style.display = 'inline'; document.getElementById('2312.05194v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.05194v1-abstract-full" style="display: none;"> We estimate the efficiency of mitigating the lensing $B$-mode polarization, the so-called delensing, for the $LiteBIRD$ experiment with multiple external data sets of lensing-mass tracers. The current best bound on the tensor-to-scalar ratio, $r$, is limited by lensing rather than Galactic foregrounds. Delensing will be a critical step to improve sensitivity to $r$ as measurements of $r$ become more and more limited by lensing. In this paper, we extend the analysis of the recent $LiteBIRD$ forecast paper to include multiple mass tracers, i.e., the CMB lensing maps from $LiteBIRD$ and CMB-S4-like experiment, cosmic infrared background, and galaxy number density from $Euclid$- and LSST-like survey. We find that multi-tracer delensing will further improve the constraint on $r$ by about $20\%$. In $LiteBIRD$, the residual Galactic foregrounds also significantly contribute to uncertainties of the $B$-modes, and delensing becomes more important if the residual foregrounds are further reduced by an improved component separation method. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05194v1-abstract-full').style.display = 'none'; document.getElementById('2312.05194v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">21 pages, 7 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/2312.05184">arXiv:2312.05184</a> <span> [<a href="https://arxiv.org/pdf/2312.05184">pdf</a>, <a href="https://arxiv.org/format/2312.05184">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/10.1088/1475-7516/2024/06/009">10.1088/1475-7516/2024/06/009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LiteBIRD Science Goals and Forecasts: A full-sky measurement of gravitational lensing of the CMB </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lonappan%2C+A+I">A. I. Lonappan</a>, <a href="/search/?searchtype=author&query=Namikawa%2C+T">T. Namikawa</a>, <a href="/search/?searchtype=author&query=Piccirilli%2C+G">G. Piccirilli</a>, <a href="/search/?searchtype=author&query=Diego-Palazuelos%2C+P">P. Diego-Palazuelos</a>, <a href="/search/?searchtype=author&query=Ruiz-Granda%2C+M">M. Ruiz-Granda</a>, <a href="/search/?searchtype=author&query=Migliaccio%2C+M">M. Migliaccio</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/?searchtype=author&query=Benabed%2C+K">K. Benabed</a>, <a href="/search/?searchtype=author&query=Challinor%2C+A">A. Challinor</a>, <a href="/search/?searchtype=author&query=Errard%2C+J">J. Errard</a>, <a href="/search/?searchtype=author&query=Farrens%2C+S">S. Farrens</a>, <a href="/search/?searchtype=author&query=Gruppuso%2C+A">A. Gruppuso</a>, <a href="/search/?searchtype=author&query=Krachmalnicoff%2C+N">N. Krachmalnicoff</a>, <a href="/search/?searchtype=author&query=Mart%C3%ADnez-Gonz%C3%A1lez%2C+E">E. Mart铆nez-Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Pettorino%2C+V">V. Pettorino</a>, <a href="/search/?searchtype=author&query=Sherwin%2C+B">B. Sherwin</a>, <a href="/search/?searchtype=author&query=Starck%2C+J">J. Starck</a>, <a href="/search/?searchtype=author&query=Vielva%2C+P">P. Vielva</a>, <a href="/search/?searchtype=author&query=Akizawa%2C+R">R. Akizawa</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Aurlien%2C+R">R. Aurlien</a>, <a href="/search/?searchtype=author&query=Azzoni%2C+S">S. Azzoni</a> , et al. (97 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="2312.05184v1-abstract-short" style="display: inline;"> We explore the capability of measuring lensing signals in $LiteBIRD$ full-sky polarization maps. With a $30$ arcmin beam width and an impressively low polarization noise of $2.16\,渭$K-arcmin, $LiteBIRD$ will be able to measure the full-sky polarization of the cosmic microwave background (CMB) very precisely. This unique sensitivity also enables the reconstruction of a nearly full-sky lensing map u… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05184v1-abstract-full').style.display = 'inline'; document.getElementById('2312.05184v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.05184v1-abstract-full" style="display: none;"> We explore the capability of measuring lensing signals in $LiteBIRD$ full-sky polarization maps. With a $30$ arcmin beam width and an impressively low polarization noise of $2.16\,渭$K-arcmin, $LiteBIRD$ will be able to measure the full-sky polarization of the cosmic microwave background (CMB) very precisely. This unique sensitivity also enables the reconstruction of a nearly full-sky lensing map using only polarization data, even considering its limited capability to capture small-scale CMB anisotropies. In this paper, we investigate the ability to construct a full-sky lensing measurement in the presence of Galactic foregrounds, finding that several possible biases from Galactic foregrounds should be negligible after component separation by harmonic-space internal linear combination. We find that the signal-to-noise ratio of the lensing is approximately $40$ using only polarization data measured over $90\%$ of the sky. This achievement is comparable to $Planck$'s recent lensing measurement with both temperature and polarization and represents a four-fold improvement over $Planck$'s polarization-only lensing measurement. The $LiteBIRD$ lensing map will complement the $Planck$ lensing map and provide several opportunities for cross-correlation science, especially in the northern hemisphere. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05184v1-abstract-full').style.display = 'none'; document.getElementById('2312.05184v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.00717">arXiv:2312.00717</a> <span> [<a href="https://arxiv.org/pdf/2312.00717">pdf</a>, <a href="https://arxiv.org/format/2312.00717">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="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> LiteBIRD Science Goals and Forecasts. A Case Study of the Origin of Primordial Gravitational Waves using Large-Scale CMB Polarization </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Campeti%2C+P">P. Campeti</a>, <a href="/search/?searchtype=author&query=Komatsu%2C+E">E. Komatsu</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Carones%2C+A">A. Carones</a>, <a href="/search/?searchtype=author&query=Errard%2C+J">J. Errard</a>, <a href="/search/?searchtype=author&query=Finelli%2C+F">F. Finelli</a>, <a href="/search/?searchtype=author&query=Flauger%2C+R">R. Flauger</a>, <a href="/search/?searchtype=author&query=Galli%2C+S">S. Galli</a>, <a href="/search/?searchtype=author&query=Galloni%2C+G">G. Galloni</a>, <a href="/search/?searchtype=author&query=Giardiello%2C+S">S. Giardiello</a>, <a href="/search/?searchtype=author&query=Hazumi%2C+M">M. Hazumi</a>, <a href="/search/?searchtype=author&query=Henrot-Versill%C3%A9%2C+S">S. Henrot-Versill茅</a>, <a href="/search/?searchtype=author&query=Hergt%2C+L+T">L. T. Hergt</a>, <a href="/search/?searchtype=author&query=Kohri%2C+K">K. Kohri</a>, <a href="/search/?searchtype=author&query=Leloup%2C+C">C. Leloup</a>, <a href="/search/?searchtype=author&query=Lesgourgues%2C+J">J. Lesgourgues</a>, <a href="/search/?searchtype=author&query=Macias-Perez%2C+J">J. Macias-Perez</a>, <a href="/search/?searchtype=author&query=Mart%C3%ADnez-Gonz%C3%A1lez%2C+E">E. Mart铆nez-Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Matarrese%2C+S">S. Matarrese</a>, <a href="/search/?searchtype=author&query=Matsumura%2C+T">T. Matsumura</a>, <a href="/search/?searchtype=author&query=Montier%2C+L">L. Montier</a>, <a href="/search/?searchtype=author&query=Namikawa%2C+T">T. Namikawa</a>, <a href="/search/?searchtype=author&query=Paoletti%2C+D">D. Paoletti</a> , et al. (85 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="2312.00717v1-abstract-short" style="display: inline;"> We study the possibility of using the $LiteBIRD$ satellite $B$-mode survey to constrain models of inflation producing specific features in CMB angular power spectra. We explore a particular model example, i.e. spectator axion-SU(2) gauge field inflation. This model can source parity-violating gravitational waves from the amplification of gauge field fluctuations driven by a pseudoscalar "axionlike… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.00717v1-abstract-full').style.display = 'inline'; document.getElementById('2312.00717v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.00717v1-abstract-full" style="display: none;"> We study the possibility of using the $LiteBIRD$ satellite $B$-mode survey to constrain models of inflation producing specific features in CMB angular power spectra. We explore a particular model example, i.e. spectator axion-SU(2) gauge field inflation. This model can source parity-violating gravitational waves from the amplification of gauge field fluctuations driven by a pseudoscalar "axionlike" field, rolling for a few e-folds during inflation. The sourced gravitational waves can exceed the vacuum contribution at reionization bump scales by about an order of magnitude and can be comparable to the vacuum contribution at recombination bump scales. We argue that a satellite mission with full sky coverage and access to the reionization bump scales is necessary to understand the origin of the primordial gravitational wave signal and distinguish among two production mechanisms: quantum vacuum fluctuations of spacetime and matter sources during inflation. We present the expected constraints on model parameters from $LiteBIRD$ satellite simulations, which complement and expand previous studies in the literature. We find that $LiteBIRD$ will be able to exclude with high significance standard single-field slow-roll models, such as the Starobinsky model, if the true model is the axion-SU(2) model with a feature at CMB scales. We further investigate the possibility of using the parity-violating signature of the model, such as the $TB$ and $EB$ angular power spectra, to disentangle it from the standard single-field slow-roll scenario. We find that most of the discriminating power of $LiteBIRD$ will reside in $BB$ angular power spectra rather than in $TB$ and $EB$ correlations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.00717v1-abstract-full').style.display = 'none'; document.getElementById('2312.00717v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 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">22 pages, 13 figures. Submitted to 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/2311.02779">arXiv:2311.02779</a> <span> [<a href="https://arxiv.org/pdf/2311.02779">pdf</a>, <a href="https://arxiv.org/format/2311.02779">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"> Measuring the CMB primordial B-modes with Bolometric Interferometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=Ade%2C+P">P. Ade</a>, <a href="/search/?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/?searchtype=author&query=Amico%2C+G">G. Amico</a>, <a href="/search/?searchtype=author&query=Arnaldi%2C+L+H">L. H. Arnaldi</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Banfi%2C+S">S. Banfi</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=B%C3%A9lier%2C+B">B. B茅lier</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Bernard%2C+J+-">J. -Ph. Bernard</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Bonaparte%2C+J">J. Bonaparte</a>, <a href="/search/?searchtype=author&query=Bonilla%2C+J+D">J. D. Bonilla</a>, <a href="/search/?searchtype=author&query=Bunn%2C+E">E. Bunn</a>, <a href="/search/?searchtype=author&query=Buzi%2C+D">D. Buzi</a>, <a href="/search/?searchtype=author&query=Cacciotti%2C+F">F. Cacciotti</a>, <a href="/search/?searchtype=author&query=Camilieri%2C+D">D. Camilieri</a>, <a href="/search/?searchtype=author&query=Cavaliere%2C+F">F. Cavaliere</a>, <a href="/search/?searchtype=author&query=Chanial%2C+P">P. Chanial</a>, <a href="/search/?searchtype=author&query=Chapron%2C+C">C. Chapron</a>, <a href="/search/?searchtype=author&query=Colombo%2C+L">L. Colombo</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a> , et al. (89 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="2311.02779v1-abstract-short" style="display: inline;"> The Q&U Bolometric Interferometer for Cosmology (QUBIC) is the first bolometric interferometer designed to measure the primordial B-mode polarization of the Cosmic Microwave Background (CMB). Bolometric interferometry is a novel technique that combines the sensitivity of bolometric detectors with the control of systematic effects that is typical of interferometry, both key features in the quest fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.02779v1-abstract-full').style.display = 'inline'; document.getElementById('2311.02779v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.02779v1-abstract-full" style="display: none;"> The Q&U Bolometric Interferometer for Cosmology (QUBIC) is the first bolometric interferometer designed to measure the primordial B-mode polarization of the Cosmic Microwave Background (CMB). Bolometric interferometry is a novel technique that combines the sensitivity of bolometric detectors with the control of systematic effects that is typical of interferometry, both key features in the quest for the faint signal of the primordial B-modes. A unique feature is the so-called "spectral imaging", i.e., the ability to recover the sky signal in several sub-bands within the physical band during data analysis. This feature provides an in-band spectral resolution of 螖谓/谓 \sim 0.04 that is unattainable by a traditional imager. This is a key tool for controlling the Galactic foregrounds contamination. In this paper, we describe the principles of bolometric interferometry, the current status of the QUBIC experiment and future prospects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.02779v1-abstract-full').style.display = 'none'; document.getElementById('2311.02779v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">To appear in Proc. of the mm Universe 2023 conference, Grenoble (France), June 2023, published by F. Mayet et al. (Eds), EPJ Web of conferences, EDP Sciences</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.01814">arXiv:2311.01814</a> <span> [<a href="https://arxiv.org/pdf/2311.01814">pdf</a>, <a href="https://arxiv.org/format/2311.01814">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 advantage of Bolometric Interferometry for controlling Galactic foreground contamination in CMB primordial B-modes measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Manzan%2C+E">E. Manzan</a>, <a href="/search/?searchtype=author&query=Regnier%2C+M">M. Regnier</a>, <a href="/search/?searchtype=author&query=Hamilton%2C+J">J-Ch. Hamilton</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=Errard%2C+J">J. Errard</a>, <a href="/search/?searchtype=author&query=Zapelli%2C+L">L. Zapelli</a>, <a href="/search/?searchtype=author&query=Torchinsky%2C+S+A">S. A. Torchinsky</a>, <a href="/search/?searchtype=author&query=Paradiso%2C+S">S. Paradiso</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">E. Battistelli</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=De+Bernardis%2C+P">P. De Bernardis</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=Gervasi%2C+M">M. Gervasi</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Piat%2C+M">M. Piat</a>, <a href="/search/?searchtype=author&query=Rasztocky%2C+E">E. Rasztocky</a>, <a href="/search/?searchtype=author&query=Romero%2C+G+E">G. E Romero</a>, <a href="/search/?searchtype=author&query=Scoccola%2C+C+G">C. G. Scoccola</a>, <a href="/search/?searchtype=author&query=Zannoni%2C+M">M. Zannoni</a>, <a href="/search/?searchtype=author&query=Collaboration%2C+t+Q">the QUBIC Collaboration</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.01814v1-abstract-short" style="display: inline;"> In the quest for the faint primordial B-mode polarization of the Cosmic Microwave Background, three are the key requirements for any present or future experiment: an utmost sensitivity, excellent control over instrumental systematic effects and over Galactic foreground contamination. Bolometric Interferometry (BI) is a novel technique that matches them all by combining the sensitivity of bolometri… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01814v1-abstract-full').style.display = 'inline'; document.getElementById('2311.01814v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.01814v1-abstract-full" style="display: none;"> In the quest for the faint primordial B-mode polarization of the Cosmic Microwave Background, three are the key requirements for any present or future experiment: an utmost sensitivity, excellent control over instrumental systematic effects and over Galactic foreground contamination. Bolometric Interferometry (BI) is a novel technique that matches them all by combining the sensitivity of bolometric detectors, the control of instrumental systematics from interferometry and a software-based, tunable, in-band spectral resolution due to its ability to perform band-splitting during data analysis (spectral imaging). In this paper, we investigate how the spectral imaging capability of BI can help in detecting residual contamination in case an over-simplified model of foreground emission is assumed in the analysis. To mimic this situation, we focus on the next generation of ground-based CMB experiment, CMB-S4, and compare its anticipated sensitivities, frequency and sky coverage with a hypothetical version of the same experiment based on BI, CMB-S4/BI, assuming that line-of-sight (LOS) frequency decorrelation is present in dust emission but is not accounted for during component separation. We show results from a Monte-Carlo analysis based on a parametric component separation method (FGBuster), highlighting how BI has the potential to diagnose the presence of foreground residuals in estimates of the tensor-to-scalar ratio $r$ in the case of unaccounted Galactic dust LOS frequency decorrelation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.01814v1-abstract-full').style.display = 'none'; document.getElementById('2311.01814v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 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">To appear in Proc. of the mm Universe 2023 conference, Grenoble (France), June 2023, published by F. Mayet et al. (Eds), EPJ Web of conferences, EDP Sciences</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.18029">arXiv:2310.18029</a> <span> [<a href="https://arxiv.org/pdf/2310.18029">pdf</a>, <a href="https://arxiv.org/format/2310.18029">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"> Observing galaxy clusters and the cosmic web through the Sunyaev Zel'dovich effect with MISTRAL </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=Barbavara%2C+E">E. Barbavara</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Cacciotti%2C+F">F. Cacciotti</a>, <a href="/search/?searchtype=author&query=Capalbo%2C+V">V. Capalbo</a>, <a href="/search/?searchtype=author&query=Carbone%2C+A">A. Carbone</a>, <a href="/search/?searchtype=author&query=Carretti%2C+E">E. Carretti</a>, <a href="/search/?searchtype=author&query=Ciccalotti%2C+D">D. Ciccalotti</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=Cruciani%2C+A">A. Cruciani</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Govoni%2C+F">F. Govoni</a>, <a href="/search/?searchtype=author&query=Isopi%2C+G">G. Isopi</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">L. Lamagna</a>, <a href="/search/?searchtype=author&query=Levati%2C+E">E. Levati</a>, <a href="/search/?searchtype=author&query=Marongiu%2C+P">P. Marongiu</a>, <a href="/search/?searchtype=author&query=Mascia%2C+A">A. Mascia</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/?searchtype=author&query=Murgia%2C+M">M. Murgia</a>, <a href="/search/?searchtype=author&query=Navarrini%2C+A">A. Navarrini</a>, <a href="/search/?searchtype=author&query=Novelli%2C+A">A. Novelli</a>, <a href="/search/?searchtype=author&query=Occhiuzzi%2C+A">A. Occhiuzzi</a> , et al. (11 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="2310.18029v1-abstract-short" style="display: inline;"> Galaxy clusters and surrounding medium, can be studied using X-ray bremsstrahlung emission and Sunyaev Zel'dovich (SZ) effect. Both astrophysical probes, sample the same environment with different parameters dependance. The SZ effect is relatively more sensitive in low density environments and thus is useful to study the filamentary structures of the cosmic web. In addition, observations of the ma… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.18029v1-abstract-full').style.display = 'inline'; document.getElementById('2310.18029v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.18029v1-abstract-full" style="display: none;"> Galaxy clusters and surrounding medium, can be studied using X-ray bremsstrahlung emission and Sunyaev Zel'dovich (SZ) effect. Both astrophysical probes, sample the same environment with different parameters dependance. The SZ effect is relatively more sensitive in low density environments and thus is useful to study the filamentary structures of the cosmic web. In addition, observations of the matter distribution require high angular resolution in order to be able to map the matter distribution within and around galaxy clusters. MISTRAL is a camera working at 90GHz which, once coupled to the Sardinia Radio Telescope, can reach $12''$ angular resolution over $4'$ field of view (f.o.v.). The forecasted sensitivity is $NEFD \simeq 10-15mJy \sqrt{s}$ and the mapping speed is $MS= 380'^{2}/mJy^{2}/h$. MISTRAL was recently installed at the focus of the SRT and soon will take its first photons. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.18029v1-abstract-full').style.display = 'none'; document.getElementById('2310.18029v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 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">To appear in Proc. of the mm Universe 2023 conference, Grenoble (France), June 2023, published by F. Mayet et al. (Eds), EPJ Web of conferences, EDP Sciences</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.02957">arXiv:2309.02957</a> <span> [<a href="https://arxiv.org/pdf/2309.02957">pdf</a>, <a href="https://arxiv.org/format/2309.02957">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/10.1051/0004-6361/202347890">10.1051/0004-6361/202347890 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Identifying frequency decorrelated dust residuals in B-mode maps by exploiting the spectral capability of bolometric interferometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Regnier%2C+M">M. Regnier</a>, <a href="/search/?searchtype=author&query=Manzan%2C+E">E. Manzan</a>, <a href="/search/?searchtype=author&query=Hamilton%2C+J+-">J. -Ch Hamilton</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=Errard%2C+J">J. Errard</a>, <a href="/search/?searchtype=author&query=Zapelli%2C+L">L. Zapelli</a>, <a href="/search/?searchtype=author&query=Torchinsky%2C+S+A">S. A. Torchinsky</a>, <a href="/search/?searchtype=author&query=Paradiso%2C+S">S. Paradiso</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">E. Battistelli</a>, <a href="/search/?searchtype=author&query=De+Bernardis%2C+P">P. De Bernardis</a>, <a href="/search/?searchtype=author&query=Colombo%2C+L">L. Colombo</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=Garcia%2C+B">B. Garcia</a>, <a href="/search/?searchtype=author&query=Gervasi%2C+M">M. Gervasi</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Mousset%2C+L">L. Mousset</a>, <a href="/search/?searchtype=author&query=Granese%2C+N+M">N. Miron Granese</a>, <a href="/search/?searchtype=author&query=O%27Sullivan%2C+C">C. O'Sullivan</a>, <a href="/search/?searchtype=author&query=Piat%2C+M">M. Piat</a>, <a href="/search/?searchtype=author&query=Rasztocky%2C+E">E. Rasztocky</a>, <a href="/search/?searchtype=author&query=Romero%2C+G+E">G. E. Romero</a>, <a href="/search/?searchtype=author&query=Scoccola%2C+C+G">C. G. Scoccola</a>, <a href="/search/?searchtype=author&query=Zannoni%2C+M">M. Zannoni</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="2309.02957v2-abstract-short" style="display: inline;"> Astrophysical polarized foregrounds represent the most critical challenge in Cosmic Microwave Background (CMB) B-mode experiments. Multi-frequency observations can be used to constrain astrophysical foregrounds to isolate the CMB contribution. However, recent observations indicate that foreground emission may be more complex than anticipated. We investigate how the increased spectral resolution… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.02957v2-abstract-full').style.display = 'inline'; document.getElementById('2309.02957v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.02957v2-abstract-full" style="display: none;"> Astrophysical polarized foregrounds represent the most critical challenge in Cosmic Microwave Background (CMB) B-mode experiments. Multi-frequency observations can be used to constrain astrophysical foregrounds to isolate the CMB contribution. However, recent observations indicate that foreground emission may be more complex than anticipated. We investigate how the increased spectral resolution provided by band splitting in Bolometric Interferometry (BI) through a technique called spectral imaging can help control the foreground contamination in the case of unaccounted Galactic dust frequency decorrelation along the line-of-sight. We focus on the next generation ground-based CMB experiment CMB-S4, and compare its anticipated sensitivities, frequency and sky coverage with a hypothetical version of the same experiment based on BI. We perform a Monte-Carlo analysis based on parametric component separation methods (FGBuster and Commander) and compute the likelihood on the recovered tensor-to-scalar ratio. The main result of this analysis is that spectral imaging allows us to detect systematic uncertainties on r from frequency decorrelation when this effect is not accounted for in component separation. Conversely, an imager would detect a biased value of r and would be unable to spot the presence of a systematic effect. We find a similar result in the reconstruction of the dust spectral index, where we show that with BI we can measure more precisely the dust spectral index also when frequency decorrelation is present. The in-band frequency resolution provided by BI allows us to identify dust LOS frequency decorrelation residuals where an imager of similar performance would fail. This opens the prospect to exploit this potential in the context of future CMB polarization experiments that will be challenged by complex foregrounds in their quest for B-modes detection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.02957v2-abstract-full').style.display = 'none'; document.getElementById('2309.02957v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 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">13 Pages, 15 figures, 4 tables. Accepted by A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A271 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2302.05228">arXiv:2302.05228</a> <span> [<a href="https://arxiv.org/pdf/2302.05228">pdf</a>, <a href="https://arxiv.org/format/2302.05228">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/10.1051/0004-6361/202346155">10.1051/0004-6361/202346155 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tensor-to-scalar ratio forecasts for extended LiteBIRD frequency configurations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fuskeland%2C+U">U. Fuskeland</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Aurlien%2C+R">R. Aurlien</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Eriksen%2C+H+K">H. K. Eriksen</a>, <a href="/search/?searchtype=author&query=Errard%2C+J">J. Errard</a>, <a href="/search/?searchtype=author&query=G%C3%A9nova-Santos%2C+R+T">R. T. G茅nova-Santos</a>, <a href="/search/?searchtype=author&query=Hasebe%2C+T">T. Hasebe</a>, <a href="/search/?searchtype=author&query=Hubmayr%2C+J">J. Hubmayr</a>, <a href="/search/?searchtype=author&query=Imada%2C+H">H. Imada</a>, <a href="/search/?searchtype=author&query=Krachmalnicoff%2C+N">N. Krachmalnicoff</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">L. Lamagna</a>, <a href="/search/?searchtype=author&query=Pisano%2C+G">G. Pisano</a>, <a href="/search/?searchtype=author&query=Poletti%2C+D">D. Poletti</a>, <a href="/search/?searchtype=author&query=Remazeilles%2C+M">M. Remazeilles</a>, <a href="/search/?searchtype=author&query=Thompson%2C+K+L">K. L. Thompson</a>, <a href="/search/?searchtype=author&query=Vacher%2C+L">L. Vacher</a>, <a href="/search/?searchtype=author&query=Wehus%2C+I+K">I. K. Wehus</a>, <a href="/search/?searchtype=author&query=Azzoni%2C+S">S. Azzoni</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Basyrov%2C+A">A. Basyrov</a>, <a href="/search/?searchtype=author&query=Beck%2C+D">D. Beck</a> , et al. (92 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="2302.05228v2-abstract-short" style="display: inline;"> LiteBIRD is a planned JAXA-led CMB B-mode satellite experiment aiming for launch in the late 2020s, with a primary goal of detecting the imprint of primordial inflationary gravitational waves. Its current baseline focal-plane configuration includes 15 frequency bands between 40 and 402 GHz, fulfilling the mission requirements to detect the amplitude of gravitational waves with the total uncertaint… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05228v2-abstract-full').style.display = 'inline'; document.getElementById('2302.05228v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.05228v2-abstract-full" style="display: none;"> LiteBIRD is a planned JAXA-led CMB B-mode satellite experiment aiming for launch in the late 2020s, with a primary goal of detecting the imprint of primordial inflationary gravitational waves. Its current baseline focal-plane configuration includes 15 frequency bands between 40 and 402 GHz, fulfilling the mission requirements to detect the amplitude of gravitational waves with the total uncertainty on the tensor-to-scalar ratio, $未r$, down to $未r<0.001$. A key aspect of this performance is accurate astrophysical component separation, and the ability to remove polarized thermal dust emission is particularly important. In this paper we note that the CMB frequency spectrum falls off nearly exponentially above 300 GHz relative to the thermal dust SED, and a relatively minor high frequency extension can therefore result in even lower uncertainties and better model reconstructions. Specifically, we compare the baseline design with five extended configurations, while varying the underlying dust modeling, in each of which the HFT (High-Frequency Telescope) frequency range is shifted logarithmically towards higher frequencies, with an upper cutoff ranging between 400 and 600 GHz. In each case, we measure the tensor-to-scalar ratio $r$ uncertainty and bias using both parametric and minimum-variance component-separation algorithms. When the thermal dust sky model includes a spatially varying spectral index and temperature, we find that the statistical uncertainty on $r$ after foreground cleaning may be reduced by as much as 30--50 % by extending the upper limit of the frequency range from 400 to 600 GHz, with most of the improvement already gained at 500 GHz. We also note that a broader frequency range leads to better ability to discriminate between models through higher $蠂^2$ sensitivity. (abridged) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05228v2-abstract-full').style.display = 'none'; document.getElementById('2302.05228v2-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 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">18 pages, 13 figures. Published in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 676, A42 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2210.03161">arXiv:2210.03161</a> <span> [<a href="https://arxiv.org/pdf/2210.03161">pdf</a>, <a href="https://arxiv.org/format/2210.03161">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"> Status of QUBIC, the Q&U Bolometer for Cosmology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mousset%2C+L">L. Mousset</a>, <a href="/search/?searchtype=author&query=Ade%2C+P">P. Ade</a>, <a href="/search/?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/?searchtype=author&query=Amico%2C+G">G. Amico</a>, <a href="/search/?searchtype=author&query=Arnaldi%2C+L+H">L. H. Arnaldi</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Banfi%2C+S">S. Banfi</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=B%C3%A9lier%2C+B">B. B茅lier</a>, <a href="/search/?searchtype=author&query=Berg%C3%A9%2C+L">L. Berg茅</a>, <a href="/search/?searchtype=author&query=Bernard%2C+J+-">J. -Ph. Bernard</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Bonaparte%2C+J">J. Bonaparte</a>, <a href="/search/?searchtype=author&query=Bonilla%2C+J+D">J. D. Bonilla</a>, <a href="/search/?searchtype=author&query=Bunn%2C+E">E. Bunn</a>, <a href="/search/?searchtype=author&query=Buzi%2C+D">D. Buzi</a>, <a href="/search/?searchtype=author&query=Camilieri%2C+D">D. Camilieri</a>, <a href="/search/?searchtype=author&query=Cavaliere%2C+F">F. Cavaliere</a>, <a href="/search/?searchtype=author&query=Chanial%2C+P">P. Chanial</a>, <a href="/search/?searchtype=author&query=Chapron%2C+C">C. Chapron</a>, <a href="/search/?searchtype=author&query=Colombo%2C+S">S. Colombo</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=Costanza%2C+B">B. Costanza</a> , et al. (86 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="2210.03161v1-abstract-short" style="display: inline;"> The Q&U Bolometric Interferometer for Cosmology (QUBIC) is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Back-ground (CMB), which is one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical foregr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.03161v1-abstract-full').style.display = 'inline'; document.getElementById('2210.03161v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2210.03161v1-abstract-full" style="display: none;"> The Q&U Bolometric Interferometer for Cosmology (QUBIC) is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Back-ground (CMB), which is one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical foregrounds which can only be controlled through multichroic observations. QUBIC is designed to address these observational issues with a novel approach that combines the advantages of interferometry in terms of control of instrumental systematics with those of bolometric detectors in terms of wide-band, background-limited sensitivity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2210.03161v1-abstract-full').style.display = 'none'; document.getElementById('2210.03161v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 October, 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">Contribution to the 2022 Cosmology session of the 33rd Rencontres de Blois. arXiv admin note: substantial text overlap with arXiv:2203.08947</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2205.03668">arXiv:2205.03668</a> <span> [<a href="https://arxiv.org/pdf/2205.03668">pdf</a>, <a href="https://arxiv.org/ps/2205.03668">ps</a>, <a href="https://arxiv.org/format/2205.03668">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/s10686-022-09882-5">10.1007/s10686-022-09882-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Performance of the polarization leakage correction in the PILOT data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bernard%2C+J">J-Ph. Bernard</a>, <a href="/search/?searchtype=author&query=Bernard%2C+A">A. Bernard</a>, <a href="/search/?searchtype=author&query=Roussel%2C+H">H. Roussel</a>, <a href="/search/?searchtype=author&query=Choubani%2C+I">I. Choubani</a>, <a href="/search/?searchtype=author&query=Alina%2C+D">D. Alina</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Hughes%2C+A">A. Hughes</a>, <a href="/search/?searchtype=author&query=Ristorcelli%2C+I">I. Ristorcelli</a>, <a href="/search/?searchtype=author&query=Stever%2C+S">S. Stever</a>, <a href="/search/?searchtype=author&query=Sugiyama%2C+T+M+S">T. Matsumura S. Sugiyama</a>, <a href="/search/?searchtype=author&query=Komatsu%2C+K">K. Komatsu</a>, <a href="/search/?searchtype=author&query=de+Gasperis%2C+G">G. de Gasperis</a>, <a href="/search/?searchtype=author&query=Ferriere%2C+K">K. Ferriere</a>, <a href="/search/?searchtype=author&query=Guillet%2C+V">V. Guillet</a>, <a href="/search/?searchtype=author&query=Ysard%2C+N">N. Ysard</a>, <a href="/search/?searchtype=author&query=Ade%2C+P">P. Ade</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Bray%2C+N">N. Bray</a>, <a href="/search/?searchtype=author&query=Crane%2C+B">B. Crane</a>, <a href="/search/?searchtype=author&query=Dubois%2C+J+P">J. P. Dubois</a>, <a href="/search/?searchtype=author&query=Griffin%2C+M">M. Griffin</a>, <a href="/search/?searchtype=author&query=Hargrave%2C+P">P. Hargrave</a>, <a href="/search/?searchtype=author&query=Longval%2C+Y">Y. Longval</a>, <a href="/search/?searchtype=author&query=Louvel%2C+S">S. Louvel</a>, <a href="/search/?searchtype=author&query=Maffei%2C+B">B. Maffei</a> , et al. (11 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="2205.03668v1-abstract-short" style="display: inline;"> The Polarized Instrument for Long-wavelength Observation of the Tenuous interstellar medium (PILOT) is a balloon-borne experiment that aims to measure the polarized emission of thermal dust at a wavelength of 240 um (1.2 THz). The PILOT experiment flew from Timmins, Ontario, Canada in 2015 and 2019 and from Alice Springs, Australia in April 2017. The in-flight performance of the instrument during… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.03668v1-abstract-full').style.display = 'inline'; document.getElementById('2205.03668v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2205.03668v1-abstract-full" style="display: none;"> The Polarized Instrument for Long-wavelength Observation of the Tenuous interstellar medium (PILOT) is a balloon-borne experiment that aims to measure the polarized emission of thermal dust at a wavelength of 240 um (1.2 THz). The PILOT experiment flew from Timmins, Ontario, Canada in 2015 and 2019 and from Alice Springs, Australia in April 2017. The in-flight performance of the instrument during the second flight was described in Mangilli et al. 2019. In this paper, we present data processing steps that were not presented in Mangilli et al. 2019 and that we have recently implemented to correct for several remaining instrumental effects. The additional data processing concerns corrections related to detector cross-talk and readout circuit memory effects, and leakage from total intensity to polarization. We illustrate the above effects and the performance of our corrections using data obtained during the third flight of PILOT, but the methods used to assess the impact of these effects on the final science-ready data, and our strategies for correcting them will be applied to all PILOT data. We show that the above corrections, and in particular that for the intensity to polarization leakage, which is most critical for accurate polarization measurements with PILOT, are accurate to better than 0.4 % as measured on Jupiter during flight#3. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2205.03668v1-abstract-full').style.display = 'none'; document.getElementById('2205.03668v1-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 May, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2022. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2204.04222">arXiv:2204.04222</a> <span> [<a href="https://arxiv.org/pdf/2204.04222">pdf</a>, <a href="https://arxiv.org/format/2204.04222">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"> High angular resolution Sunyaev Zel'dovich observations: the case of MISTRAL </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=Barbavara%2C+E">E. Barbavara</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Cacciotti%2C+F">F. Cacciotti</a>, <a href="/search/?searchtype=author&query=Capalbo%2C+V">V. Capalbo</a>, <a href="/search/?searchtype=author&query=Carretti%2C+E">E. Carretti</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=Cruciani%2C+A">A. Cruciani</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Govoni%2C+F">F. Govoni</a>, <a href="/search/?searchtype=author&query=Isopi%2C+G">G. Isopi</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">L. Lamagna</a>, <a href="/search/?searchtype=author&query=Marongiu%2C+P">P. Marongiu</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Mele%2C+L">L. Mele</a>, <a href="/search/?searchtype=author&query=Molinari%2C+E">E. Molinari</a>, <a href="/search/?searchtype=author&query=Murgia%2C+M">M. Murgia</a>, <a href="/search/?searchtype=author&query=Navarrini%2C+A">A. Navarrini</a>, <a href="/search/?searchtype=author&query=Orlati%2C+A">A. Orlati</a>, <a href="/search/?searchtype=author&query=Paiella%2C+A">A. Paiella</a>, <a href="/search/?searchtype=author&query=Pettinari%2C+G">G. Pettinari</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">F. Piacentini</a>, <a href="/search/?searchtype=author&query=Pisanu%2C+T">T. Pisanu</a> , et al. (3 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="2204.04222v1-abstract-short" style="display: inline;"> The MIllimeter Sardinia radio Telescope Receiver based on Array of Lumped elements kids, MISTRAL, is a millimetric ($\simeq 90GHz$) multipixel camera being built for the Sardinia Radio Telescope. It is going to be a facility instrument and will sample the sky with 12 arcsec angular resolution, 4 arcmin field of view, through 408 Kinetic Inductance Detectors (KIDs). The construction and the beginni… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04222v1-abstract-full').style.display = 'inline'; document.getElementById('2204.04222v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2204.04222v1-abstract-full" style="display: none;"> The MIllimeter Sardinia radio Telescope Receiver based on Array of Lumped elements kids, MISTRAL, is a millimetric ($\simeq 90GHz$) multipixel camera being built for the Sardinia Radio Telescope. It is going to be a facility instrument and will sample the sky with 12 arcsec angular resolution, 4 arcmin field of view, through 408 Kinetic Inductance Detectors (KIDs). The construction and the beginning of commissioning is planned to be in 2022. MISTRAL will allow the scientific community to propose a wide variety of scientific cases including protoplanetary discs study, star forming regions, galaxies radial profiles, and high angular resolution measurements of the Sunyaev Zel'dovich (SZ) effect with the investigation of the morphology of galaxy cluster and the search for the Cosmic Web. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2204.04222v1-abstract-full').style.display = 'none'; document.getElementById('2204.04222v1-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 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">18 pages, 6 figure, accepted for pubblication in the International Journal of Modern Physics D</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2203.06142">arXiv:2203.06142</a> <span> [<a href="https://arxiv.org/pdf/2203.06142">pdf</a>, <a href="https://arxiv.org/format/2203.06142">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/10.1016/j.jheap.2022.04.002">10.1016/j.jheap.2022.04.002 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmology Intertwined: A Review of the Particle Physics, Astrophysics, and Cosmology Associated with the Cosmological Tensions and Anomalies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Abdalla%2C+E">Elcio Abdalla</a>, <a href="/search/?searchtype=author&query=Abell%C3%A1n%2C+G+F">Guillermo Franco Abell谩n</a>, <a href="/search/?searchtype=author&query=Aboubrahim%2C+A">Amin Aboubrahim</a>, <a href="/search/?searchtype=author&query=Agnello%2C+A">Adriano Agnello</a>, <a href="/search/?searchtype=author&query=Akarsu%2C+O">Ozgur Akarsu</a>, <a href="/search/?searchtype=author&query=Akrami%2C+Y">Yashar Akrami</a>, <a href="/search/?searchtype=author&query=Alestas%2C+G">George Alestas</a>, <a href="/search/?searchtype=author&query=Aloni%2C+D">Daniel Aloni</a>, <a href="/search/?searchtype=author&query=Amendola%2C+L">Luca Amendola</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L+A">Luis A. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Anderson%2C+R+I">Richard I. Anderson</a>, <a href="/search/?searchtype=author&query=Arendse%2C+N">Nikki Arendse</a>, <a href="/search/?searchtype=author&query=Asgari%2C+M">Marika Asgari</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">Mario Ballardini</a>, <a href="/search/?searchtype=author&query=Barger%2C+V">Vernon Barger</a>, <a href="/search/?searchtype=author&query=Basilakos%2C+S">Spyros Basilakos</a>, <a href="/search/?searchtype=author&query=Batista%2C+R+C">Ronaldo C. Batista</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">Elia S. Battistelli</a>, <a href="/search/?searchtype=author&query=Battye%2C+R">Richard Battye</a>, <a href="/search/?searchtype=author&query=Benetti%2C+M">Micol Benetti</a>, <a href="/search/?searchtype=author&query=Benisty%2C+D">David Benisty</a>, <a href="/search/?searchtype=author&query=Berlin%2C+A">Asher Berlin</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=Berti%2C+E">Emanuele Berti</a>, <a href="/search/?searchtype=author&query=Bidenko%2C+B">Bohdan Bidenko</a> , et al. (178 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="2203.06142v3-abstract-short" style="display: inline;"> In this paper we will list a few important goals that need to be addressed in the next decade, also taking into account the current discordances between the different cosmological probes, such as the disagreement in the value of the Hubble constant $H_0$, the $蟽_8$--$S_8$ tension, and other less statistically significant anomalies. While these discordances can still be in part the result of system… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06142v3-abstract-full').style.display = 'inline'; document.getElementById('2203.06142v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2203.06142v3-abstract-full" style="display: none;"> In this paper we will list a few important goals that need to be addressed in the next decade, also taking into account the current discordances between the different cosmological probes, such as the disagreement in the value of the Hubble constant $H_0$, the $蟽_8$--$S_8$ tension, and other less statistically significant anomalies. While these discordances can still be in part the result of systematic errors, their persistence after several years of accurate analysis strongly hints at cracks in the standard cosmological scenario and the necessity for new physics or generalisations beyond the standard model. In this paper, we focus on the $5.0\,蟽$ tension between the {\it Planck} CMB estimate of the Hubble constant $H_0$ and the SH0ES collaboration measurements. After showing the $H_0$ evaluations made from different teams using different methods and geometric calibrations, we list a few interesting new physics models that could alleviate this tension and discuss how the next decade's experiments will be crucial. Moreover, we focus on the tension of the {\it Planck} CMB data with weak lensing measurements and redshift surveys, about the value of the matter energy density $惟_m$, and the amplitude or rate of the growth of structure ($蟽_8,f蟽_8$). We list a few interesting models proposed for alleviating this tension, and we discuss the importance of trying to fit a full array of data with a single model and not just one parameter at a time. Additionally, we present a wide range of other less discussed anomalies at a statistical significance level lower than the $H_0$--$S_8$ tensions which may also constitute hints towards new physics, and we discuss possible generic theoretical approaches that can collectively explain the non-standard nature of these signals.[Abridged] <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2203.06142v3-abstract-full').style.display = 'none'; document.getElementById('2203.06142v3-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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. 224 pages, 27 figures. Accepted for publication in JHEAp</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. High En. Astrophys. 2204, 002 (2022) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.02773">arXiv:2202.02773</a> <span> [<a href="https://arxiv.org/pdf/2202.02773">pdf</a>, <a href="https://arxiv.org/format/2202.02773">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/10.1093/ptep/ptac150">10.1093/ptep/ptac150 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing Cosmic Inflation with the LiteBIRD Cosmic Microwave Background Polarization Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=LiteBIRD+Collaboration"> LiteBIRD Collaboration</a>, <a href="/search/?searchtype=author&query=Allys%2C+E">E. Allys</a>, <a href="/search/?searchtype=author&query=Arnold%2C+K">K. Arnold</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Aurlien%2C+R">R. Aurlien</a>, <a href="/search/?searchtype=author&query=Azzoni%2C+S">S. Azzoni</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Banerji%2C+R">R. Banerji</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Bautista%2C+L">L. Bautista</a>, <a href="/search/?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/?searchtype=author&query=Beckman%2C+S">S. Beckman</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Boulanger%2C+F">F. Boulanger</a>, <a href="/search/?searchtype=author&query=Brilenkov%2C+M">M. Brilenkov</a>, <a href="/search/?searchtype=author&query=Bucher%2C+M">M. Bucher</a>, <a href="/search/?searchtype=author&query=Calabrese%2C+E">E. Calabrese</a>, <a href="/search/?searchtype=author&query=Campeti%2C+P">P. Campeti</a>, <a href="/search/?searchtype=author&query=Carones%2C+A">A. Carones</a>, <a href="/search/?searchtype=author&query=Casas%2C+F+J">F. J. Casas</a>, <a href="/search/?searchtype=author&query=Catalano%2C+A">A. Catalano</a>, <a href="/search/?searchtype=author&query=Chan%2C+V">V. Chan</a>, <a href="/search/?searchtype=author&query=Cheung%2C+K">K. Cheung</a> , et al. (166 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="2202.02773v3-abstract-short" style="display: inline;"> LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. The Japan Aerospace Exploration Agency (JAXA) selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with an expected launch in the late 2020s using JAXA's H3 rocket. LiteBIRD is… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.02773v3-abstract-full').style.display = 'inline'; document.getElementById('2202.02773v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.02773v3-abstract-full" style="display: none;"> LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. The Japan Aerospace Exploration Agency (JAXA) selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with an expected launch in the late 2020s using JAXA's H3 rocket. LiteBIRD is planned to orbit the Sun-Earth Lagrangian point L2, where it will map the cosmic microwave background (CMB) polarization over the entire sky for three years, with three telescopes in 15 frequency bands between 34 and 448 GHz, to achieve an unprecedented total sensitivity of 2.2$渭$K-arcmin, with a typical angular resolution of 0.5$^\circ$ at 100 GHz. The primary scientific objective of LiteBIRD is to search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. We provide an overview of the LiteBIRD project, including scientific objectives, mission and system requirements, operation concept, spacecraft and payload module design, expected scientific outcomes, potential design extensions and synergies with other projects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.02773v3-abstract-full').style.display = 'none'; document.getElementById('2202.02773v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">155 pages, accepted for publication in PTEP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2202.01324">arXiv:2202.01324</a> <span> [<a href="https://arxiv.org/pdf/2202.01324">pdf</a>, <a href="https://arxiv.org/format/2202.01324">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/10.1088/1475-7516/2022/04/029">10.1088/1475-7516/2022/04/029 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Polarization angle requirements for CMB B-mode experiments. Application to the LiteBIRD satellite </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Vielva%2C+P">P. Vielva</a>, <a href="/search/?searchtype=author&query=Mart%C3%ADnez-Gonz%C3%A1lez%2C+E">E. Mart铆nez-Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Casas%2C+F+J">F. J. Casas</a>, <a href="/search/?searchtype=author&query=Matsumura%2C+T">T. Matsumura</a>, <a href="/search/?searchtype=author&query=Henrot-Versill%C3%A9%2C+S">S. Henrot-Versill茅</a>, <a href="/search/?searchtype=author&query=Komatsu%2C+E">E. Komatsu</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Aurlien%2C+R">R. Aurlien</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/?searchtype=author&query=Calabrese%2C+E">E. Calabrese</a>, <a href="/search/?searchtype=author&query=Cheung%2C+K">K. Cheung</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=de+Haan%2C+T">T. de Haan</a>, <a href="/search/?searchtype=author&query=de+la+Hoz%2C+E">E. de la Hoz</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Della+Torre%2C+S">S. Della Torre</a>, <a href="/search/?searchtype=author&query=Diego-Palazuelos%2C+P">P. Diego-Palazuelos</a>, <a href="/search/?searchtype=author&query=Eriksen%2C+H+K">H. K. Eriksen</a>, <a href="/search/?searchtype=author&query=Errard%2C+J">J. Errard</a>, <a href="/search/?searchtype=author&query=Finelli%2C+F">F. Finelli</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="2202.01324v2-abstract-short" style="display: inline;"> A methodology to provide the polarization angle requirements for different sets of detectors, at a given frequency of a CMB polarization experiment, is presented. The uncertainties in the polarization angle of each detector set are related to a given bias on the tensor-to-scalar ratio $r$ parameter. The approach is grounded in using a linear combination of the detector sets to obtain the CMB polar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.01324v2-abstract-full').style.display = 'inline'; document.getElementById('2202.01324v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2202.01324v2-abstract-full" style="display: none;"> A methodology to provide the polarization angle requirements for different sets of detectors, at a given frequency of a CMB polarization experiment, is presented. The uncertainties in the polarization angle of each detector set are related to a given bias on the tensor-to-scalar ratio $r$ parameter. The approach is grounded in using a linear combination of the detector sets to obtain the CMB polarization signal. In addition, assuming that the uncertainties on the polarization angle are in the small angle limit (lower than a few degrees), it is possible to derive analytic expressions to establish the requirements. The methodology also accounts for possible correlations among detectors, that may originate from the optics, wafers, etc. The approach is applied to the LiteBIRD space mission. We show that, for the most restrictive case (i.e., full correlation of the polarization angle systematics among detector sets), the requirements on the polarization angle uncertainties are of around 1 arcmin at the most sensitive frequency bands (i.e., $\approx 150$ GHz) and of few tens of arcmin at the lowest (i.e., $\approx 40$ GHz) and highest (i.e., $\approx 400$ GHz) observational bands. Conversely, for the least restrictive case (i.e., no correlation of the polarization angle systematics among detector sets), the requirements are $\approx 5$ times less restrictive than for the previous scenario. At the global and the telescope levels, polarization angle knowledge of a few arcmins is sufficient for correlated global systematic errors and can be relaxed by a factor of two for fully uncorrelated errors in detector polarization angle. The reported uncertainty levels are needed in order to have the bias on $r$ due to systematics below the limit established by the LiteBIRD collaboration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2202.01324v2-abstract-full').style.display = 'none'; document.getElementById('2202.01324v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">26 pages, 6 figures. Minor changes to match the final version 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/2111.09140">arXiv:2111.09140</a> <span> [<a href="https://arxiv.org/pdf/2111.09140">pdf</a>, <a href="https://arxiv.org/format/2111.09140">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/10.1088/1475-7516/2022/01/039">10.1088/1475-7516/2022/01/039 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> In-flight polarization angle calibration for LiteBIRD: blind challenge and cosmological implications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Krachmalnicoff%2C+N">Nicoletta Krachmalnicoff</a>, <a href="/search/?searchtype=author&query=Matsumura%2C+T">Tomotake Matsumura</a>, <a href="/search/?searchtype=author&query=de+la+Hoz%2C+E">Elena de la Hoz</a>, <a href="/search/?searchtype=author&query=Basak%2C+S">Soumen Basak</a>, <a href="/search/?searchtype=author&query=Gruppuso%2C+A">Alessandro Gruppuso</a>, <a href="/search/?searchtype=author&query=Minami%2C+Y">Yuto Minami</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">Carlo Baccigalupi</a>, <a href="/search/?searchtype=author&query=Komatsu%2C+E">Eiichiro Komatsu</a>, <a href="/search/?searchtype=author&query=Mart%C3%ADnez-Gonz%C3%A1lez%2C+E">Enrique Mart铆nez-Gonz谩lez</a>, <a href="/search/?searchtype=author&query=Vielva%2C+P">Patricio Vielva</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">Jonathan Aumont</a>, <a href="/search/?searchtype=author&query=Aurlien%2C+R">Ragnhild Aurlien</a>, <a href="/search/?searchtype=author&query=Azzoni%2C+S">Susanna Azzoni</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">Anthony J. Banday</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">Rita B. Barreiro</a>, <a href="/search/?searchtype=author&query=Bartolo%2C+N">Nicola Bartolo</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">Marco Bersanelli</a>, <a href="/search/?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/?searchtype=author&query=Carones%2C+A">Alessandro Carones</a>, <a href="/search/?searchtype=author&query=Casas%2C+F+J">Francisco J. Casas</a>, <a href="/search/?searchtype=author&query=Cheung%2C+K">Kolen Cheung</a>, <a href="/search/?searchtype=author&query=Chinone%2C+Y">Yuji Chinone</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">Fabio Columbro</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=Diego-Palazuelos%2C+P">Patricia Diego-Palazuelos</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="2111.09140v2-abstract-short" style="display: inline;"> We present a demonstration of the in-flight polarization angle calibration for the JAXA/ISAS second strategic large class mission, LiteBIRD, and estimate its impact on the measurement of the tensor-to-scalar ratio parameter, r, using simulated data. We generate a set of simulated sky maps with CMB and polarized foreground emission, and inject instrumental noise and polarization angle offsets to th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.09140v2-abstract-full').style.display = 'inline'; document.getElementById('2111.09140v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.09140v2-abstract-full" style="display: none;"> We present a demonstration of the in-flight polarization angle calibration for the JAXA/ISAS second strategic large class mission, LiteBIRD, and estimate its impact on the measurement of the tensor-to-scalar ratio parameter, r, using simulated data. We generate a set of simulated sky maps with CMB and polarized foreground emission, and inject instrumental noise and polarization angle offsets to the 22 (partially overlapping) LiteBIRD frequency channels. Our in-flight angle calibration relies on nulling the EB cross correlation of the polarized signal in each channel. This calibration step has been carried out by two independent groups with a blind analysis, allowing an accuracy of the order of a few arc-minutes to be reached on the estimate of the angle offsets. Both the corrected and uncorrected multi-frequency maps are propagated through the foreground cleaning step, with the goal of computing clean CMB maps. We employ two component separation algorithms, the Bayesian-Separation of Components and Residuals Estimate Tool (B-SeCRET), and the Needlet Internal Linear Combination (NILC). We find that the recovered CMB maps obtained with algorithms that do not make any assumptions about the foreground properties, such as NILC, are only mildly affected by the angle miscalibration. However, polarization angle offsets strongly bias results obtained with the parametric fitting method. Once the miscalibration angles are corrected by EB nulling prior to the component separation, both component separation algorithms result in an unbiased estimation of the r parameter. While this work is motivated by the conceptual design study for LiteBIRD, its framework can be broadly applied to any CMB polarization experiment. In particular, the combination of simulation plus blind analysis provides a robust forecast by taking into account not only detector sensitivity but also systematic effects. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.09140v2-abstract-full').style.display = 'none'; document.getElementById('2111.09140v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 January, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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">Submitted to 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/2111.08388">arXiv:2111.08388</a> <span> [<a href="https://arxiv.org/pdf/2111.08388">pdf</a>, <a href="https://arxiv.org/format/2111.08388">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2022/06/009">10.1088/1475-7516/2022/06/009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Total power horn-coupled 150 GHz LEKID array for space applications </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Paiella%2C+A">A. Paiella</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Cruciani%2C+A">A. Cruciani</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">L. Lamagna</a>, <a href="/search/?searchtype=author&query=Pettinari%2C+G">G. Pettinari</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">F. Piacentini</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Cavaliere%2C+F">F. Cavaliere</a>, <a href="/search/?searchtype=author&query=Franceschet%2C+C">C. Franceschet</a>, <a href="/search/?searchtype=author&query=Gervasi%2C+M">M. Gervasi</a>, <a href="/search/?searchtype=author&query=Limonta%2C+A">A. Limonta</a>, <a href="/search/?searchtype=author&query=Mandelli%2C+S">S. Mandelli</a>, <a href="/search/?searchtype=author&query=Manzan%2C+E">E. Manzan</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=Passerini%2C+A">A. Passerini</a>, <a href="/search/?searchtype=author&query=Tommasi%2C+E">E. Tommasi</a>, <a href="/search/?searchtype=author&query=Volpe%2C+A">A. Volpe</a>, <a href="/search/?searchtype=author&query=Zannoni%2C+M">M. Zannoni</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="2111.08388v2-abstract-short" style="display: inline;"> We have developed two arrays of lumped element kinetic inductance detectors working in the D-band, and optimised for the low radiative background conditions of a satellite mission aiming at precision measurements of the Cosmic Microwave Background (CMB). The first detector array is sensitive to the total power of the incoming radiation to which is coupled via single-mode waveguides and corrugated… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.08388v2-abstract-full').style.display = 'inline'; document.getElementById('2111.08388v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.08388v2-abstract-full" style="display: none;"> We have developed two arrays of lumped element kinetic inductance detectors working in the D-band, and optimised for the low radiative background conditions of a satellite mission aiming at precision measurements of the Cosmic Microwave Background (CMB). The first detector array is sensitive to the total power of the incoming radiation to which is coupled via single-mode waveguides and corrugated feed-horns, while the second is sensitive to the polarisation of the radiation thanks to orthomode transducers. Here, we focus on the total power detector array, which is suitable, for instance, for precision measurements of unpolarised spectral distortions of the CMB, where detecting both polarisations provides a sensitivity advantage. We describe the optimisation of the array design, fabrication and packaging, the dark and optical characterisation, and the performance of the black-body calibrator used for the optical tests. We show that almost all the detectors of the array are photon-noise limited under the radiative background of a 3.6 K black-body. This result, combined with the weak sensitivity to cosmic rays hits demonstrated with the OLIMPO flight, validates the idea of using lumped elements kinetic inductance detectors for precision, space-based CMB missions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.08388v2-abstract-full').style.display = 'none'; document.getElementById('2111.08388v2-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, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 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">To be submitted to 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/2111.00246">arXiv:2111.00246</a> <span> [<a href="https://arxiv.org/pdf/2111.00246">pdf</a>, <a href="https://arxiv.org/format/2111.00246">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"> BISOU: a balloon project to measure the CMB spectral distortions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Maffei%2C+B">B. Maffei</a>, <a href="/search/?searchtype=author&query=Abitbol%2C+M+H">M. H. Abitbol</a>, <a href="/search/?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">E. Battistelli</a>, <a href="/search/?searchtype=author&query=Chluba%2C+J">J. Chluba</a>, <a href="/search/?searchtype=author&query=Coulon%2C+X">X. Coulon</a>, <a href="/search/?searchtype=author&query=De+Bernardis%2C+P">P. De Bernardis</a>, <a href="/search/?searchtype=author&query=Douspis%2C+M">M. Douspis</a>, <a href="/search/?searchtype=author&query=Grain%2C+J">J. Grain</a>, <a href="/search/?searchtype=author&query=Gervasoni%2C+S">S. Gervasoni</a>, <a href="/search/?searchtype=author&query=Hill%2C+J+C">J. C. Hill</a>, <a href="/search/?searchtype=author&query=Kogut%2C+A">A. Kogut</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Matsumura%2C+T">T. Matsumura</a>, <a href="/search/?searchtype=author&query=Sullivan%2C+C+O">C. O Sullivan</a>, <a href="/search/?searchtype=author&query=Pagano%2C+L">L. Pagano</a>, <a href="/search/?searchtype=author&query=Pisano%2C+G">G. Pisano</a>, <a href="/search/?searchtype=author&query=Remazeilles%2C+M">M. Remazeilles</a>, <a href="/search/?searchtype=author&query=Ritacco%2C+A">A. Ritacco</a>, <a href="/search/?searchtype=author&query=Rotti%2C+A">A. Rotti</a>, <a href="/search/?searchtype=author&query=Sauvage%2C+V">V. Sauvage</a>, <a href="/search/?searchtype=author&query=Savini%2C+G">G. Savini</a>, <a href="/search/?searchtype=author&query=Stever%2C+S+L">S. L. Stever</a>, <a href="/search/?searchtype=author&query=Tartari%2C+A">A. Tartari</a> , et al. (2 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="2111.00246v1-abstract-short" style="display: inline;"> The BISOU (Balloon Interferometer for Spectral Observations of the Universe) project aims to study the viability and prospects of a balloon-borne spectrometer, pathfinder of a future space mission dedicated to the measurements of the CMB spectral distortions. We present here a preliminary concept based on previous space mission proposals, together with some sensitivity calculation results for the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.00246v1-abstract-full').style.display = 'inline'; document.getElementById('2111.00246v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2111.00246v1-abstract-full" style="display: none;"> The BISOU (Balloon Interferometer for Spectral Observations of the Universe) project aims to study the viability and prospects of a balloon-borne spectrometer, pathfinder of a future space mission dedicated to the measurements of the CMB spectral distortions. We present here a preliminary concept based on previous space mission proposals, together with some sensitivity calculation results for the observation goals, showing that a 5-sigma measurement of the y-distortions is achievable. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2111.00246v1-abstract-full').style.display = 'none'; document.getElementById('2111.00246v1-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, 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">12 pages. To be published on the proceedings of the 16th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Astrophysics and Relativistic Field Theories (MG16) - 5-9 July 2021. Online Conference, Italy. http://www.icra.it/mg/mg16/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2110.12254">arXiv:2110.12254</a> <span> [<a href="https://arxiv.org/pdf/2110.12254">pdf</a>, <a href="https://arxiv.org/format/2110.12254">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"> The COSmic Monopole Observer (COSMO) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">E. Battistelli</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">L. Lamagna</a>, <a href="/search/?searchtype=author&query=Marchitelli%2C+E">E. Marchitelli</a>, <a href="/search/?searchtype=author&query=Mele%2C+L">L. Mele</a>, <a href="/search/?searchtype=author&query=Paiella%2C+A">A. Paiella</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">F. Piacentini</a>, <a href="/search/?searchtype=author&query=Pisano%2C+G">G. Pisano</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Franceschet%2C+C">C. Franceschet</a>, <a href="/search/?searchtype=author&query=Manzan%2C+E">E. Manzan</a>, <a href="/search/?searchtype=author&query=Mennella%2C+D">D. Mennella</a>, <a href="/search/?searchtype=author&query=Realini%2C+S">S. Realini</a>, <a href="/search/?searchtype=author&query=Cibella%2C+S">S. Cibella</a>, <a href="/search/?searchtype=author&query=Martini%2C+F">F. Martini</a>, <a href="/search/?searchtype=author&query=Pettinari%2C+G">G. Pettinari</a>, <a href="/search/?searchtype=author&query=Coppi%2C+G">G. Coppi</a>, <a href="/search/?searchtype=author&query=Gervasi%2C+M">M. Gervasi</a>, <a href="/search/?searchtype=author&query=Limonta%2C+A">A. Limonta</a>, <a href="/search/?searchtype=author&query=Zannoni%2C+M">M. Zannoni</a> , et al. (2 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="2110.12254v1-abstract-short" style="display: inline;"> The COSmic Monopole Observer (COSMO) is an experiment to measure low-level spectral distortions in the isotropic component of the Cosmic Microwave Background (CMB). Deviations from a pure blackbody spectrum are expected at low level ($<$ 1 ppm) due to several astrophysical and cosmological phenomena, and promise to provide important independent information on the early and late phases of the unive… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.12254v1-abstract-full').style.display = 'inline'; document.getElementById('2110.12254v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2110.12254v1-abstract-full" style="display: none;"> The COSmic Monopole Observer (COSMO) is an experiment to measure low-level spectral distortions in the isotropic component of the Cosmic Microwave Background (CMB). Deviations from a pure blackbody spectrum are expected at low level ($<$ 1 ppm) due to several astrophysical and cosmological phenomena, and promise to provide important independent information on the early and late phases of the universe. They have not been detected yet, due to the extreme accuracy required, the best upper limits being still those from the COBE-FIRAS mission. COSMO is based on a cryogenic differential Fourier Transform Spectrometer, measuring the spectral brightness difference between the sky and an accurate cryogenic blackbody. The first implementation of COSMO, funded by the Italian PRIN and PNRA programs, will operate from the Concordia station at Dome-C, in Antarctica, and will take advantage of a fast sky-dip technique to get rid of atmospheric emission and its fluctuations, separating them from the monopole component of the sky brightness. Here we describe the instrument design, its capabilities, the current status. We also discuss its subsequent implementation in a balloon-flight, which has been studied within the COSMOS program of the Italian Space Agency. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2110.12254v1-abstract-full').style.display = 'none'; document.getElementById('2110.12254v1-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 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">To be published on the proceedings of the 16th Marcel Grossmann Meeting on Recent Developments in Theoretical and Experimental General Relativity, Astrophysics and Relativistic Field Theories (MG16) - 5-9 July 2021. Online Conference, Italy - http://www.icra.it/mg/mg16/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2107.04611">arXiv:2107.04611</a> <span> [<a href="https://arxiv.org/pdf/2107.04611">pdf</a>, <a href="https://arxiv.org/format/2107.04611">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="Astrophysics of Galaxies">astro-ph.GA</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/10.1093/mnras/stab3391">10.1093/mnras/stab3391 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A high-resolution view of the filament of gas between Abell 399 and Abell 401 from the Atacama Cosmology Telescope and MUSTANG-2 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hincks%2C+A+D">Adam D. Hincks</a>, <a href="/search/?searchtype=author&query=Radiconi%2C+F">Federico Radiconi</a>, <a href="/search/?searchtype=author&query=Romero%2C+C">Charles Romero</a>, <a href="/search/?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/?searchtype=author&query=Mroczkowski%2C+T">Tony Mroczkowski</a>, <a href="/search/?searchtype=author&query=Austermann%2C+J+E">Jason E. Austermann</a>, <a href="/search/?searchtype=author&query=Barbavara%2C+E">Eleonora Barbavara</a>, <a href="/search/?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">Elia Battistelli</a>, <a href="/search/?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=Devlin%2C+M+J">Mark J. Devlin</a>, <a href="/search/?searchtype=author&query=Dicker%2C+S+R">Simon R. Dicker</a>, <a href="/search/?searchtype=author&query=Duff%2C+S+M">Shannon M. Duff</a>, <a href="/search/?searchtype=author&query=Duivenvoorden%2C+A+J">Adriaan J. Duivenvoorden</a>, <a href="/search/?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/?searchtype=author&query=D%C3%BCnner%2C+R">Rolando D眉nner</a>, <a href="/search/?searchtype=author&query=Gallardo%2C+P+A">Patricio A. Gallardo</a>, <a href="/search/?searchtype=author&query=Govoni%2C+F">Federica Govoni</a>, <a href="/search/?searchtype=author&query=Hill%2C+J+C">J. Colin Hill</a>, <a href="/search/?searchtype=author&query=Hilton%2C+M">Matt Hilton</a>, <a href="/search/?searchtype=author&query=Hubmayr%2C+J">Johannes Hubmayr</a>, <a href="/search/?searchtype=author&query=Hughes%2C+J+P">John P. Hughes</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">Luca Lamagna</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="2107.04611v2-abstract-short" style="display: inline;"> We report a significant detection of the hot intergalactic medium in the filamentary bridge connecting the galaxy clusters Abell 399 and Abell 401. This result is enabled by a low-noise, high-resolution map of the thermal Sunyaev-Zeldovich signal from the Atacama Cosmology Telescope (ACT) and Planck satellite. The ACT data provide the $1.65'$ resolution that allows us to clearly separate the profi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.04611v2-abstract-full').style.display = 'inline'; document.getElementById('2107.04611v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2107.04611v2-abstract-full" style="display: none;"> We report a significant detection of the hot intergalactic medium in the filamentary bridge connecting the galaxy clusters Abell 399 and Abell 401. This result is enabled by a low-noise, high-resolution map of the thermal Sunyaev-Zeldovich signal from the Atacama Cosmology Telescope (ACT) and Planck satellite. The ACT data provide the $1.65'$ resolution that allows us to clearly separate the profiles of the clusters, whose centres are separated by $37'$, from the gas associated with the filament. A model that fits for only the two clusters is ruled out compared to one that includes a bridge component at $>5蟽$. Using a gas temperature determined from Suzaku X-ray data, we infer a total mass of $(3.3\pm0.7)\times10^{14}\,\mathrm{M}_{\odot}$ associated with the filament, comprising about $8\%$ of the entire Abell 399-Abell 401 system. We fit two phenomenological models to the filamentary structure; the favoured model has a width transverse to the axis joining the clusters of ${\sim}1.9\,\mathrm{Mpc}$. When combined with the Suzaku data, we find a gas density of $(0.88\pm0.24)\times10^{-4}\,\mathrm{cm}^{-3}$, considerably lower than previously reported. We show that this can be fully explained by a geometry in which the axis joining Abell 399 and Abell 401 has a large component along the line of sight, such that the distance between the clusters is significantly greater than the $3.2\,\mathrm{Mpc}$ projected separation on the plane of the sky. Finally, we present initial results from higher resolution ($12.7"$ effective) imaging of the bridge with the MUSTANG-2 receiver on the Green Bank Telescope. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2107.04611v2-abstract-full').style.display = 'none'; document.getElementById('2107.04611v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 November, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 July, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 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">23 pages, 10 figures, 3 tables. This is a pre-copyedited, author-produced PDF of an article accepted for publication in the Monthly Notices of the Royal Astronomical Society following peer review. The version of record is available online at: https://academic.oup.com/mnras/advance-article/doi/10.1093/mnras/stab3391/6442294</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2106.04841">arXiv:2106.04841</a> <span> [<a href="https://arxiv.org/pdf/2106.04841">pdf</a>, <a href="https://arxiv.org/format/2106.04841">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/10.3847/1538-4357/ac1860">10.3847/1538-4357/ac1860 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Crab Nebula as a Calibrator for wide-beam Cosmic Microwave Background polarization surveys </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Masi%2C+S">Silvia Masi</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">Fabio Columbro</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">Alessandro Coppolecchia</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">Giuseppe D'Alessandro</a>, <a href="/search/?searchtype=author&query=Mele%2C+L">Lorenzo Mele</a>, <a href="/search/?searchtype=author&query=Paiella%2C+A">Alessandro Paiella</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">Francesco Piacentini</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="2106.04841v1-abstract-short" style="display: inline;"> We analyze the effect of polarized diffuse emission in the calibration of wide-beam mm-wave polarimeters, when using the Crab Nebula as a reference source for both polarized brightness and polarization angle. We show that, for CMB polarization experiments aiming at detecting B-mode in a scenario with a tensor to scalar ratio $r \sim 0.001$, wide (a few degrees in diameter), precise ($蟽_Q$ , $蟽_U$… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.04841v1-abstract-full').style.display = 'inline'; document.getElementById('2106.04841v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2106.04841v1-abstract-full" style="display: none;"> We analyze the effect of polarized diffuse emission in the calibration of wide-beam mm-wave polarimeters, when using the Crab Nebula as a reference source for both polarized brightness and polarization angle. We show that, for CMB polarization experiments aiming at detecting B-mode in a scenario with a tensor to scalar ratio $r \sim 0.001$, wide (a few degrees in diameter), precise ($蟽_Q$ , $蟽_U$ $\sim$ 20 $渭$$K_{CMB}$ arcmin), high angular resolution ($< \mathrm{FWHM}$) reference maps are needed to properly take into account the effects of diffuse polarized emission and avoid significant bias in the calibration. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2106.04841v1-abstract-full').style.display = 'none'; document.getElementById('2106.04841v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 June, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2021. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2105.10453">arXiv:2105.10453</a> <span> [<a href="https://arxiv.org/pdf/2105.10453">pdf</a>, <a href="https://arxiv.org/format/2105.10453">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/10.1051/0004-6361/202040011">10.1051/0004-6361/202040011 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Study of the thermal and nonthermal emission components in M31: the Sardinia Radio Telescope view at 6.6 GHz </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fatigoni%2C+S">S. Fatigoni</a>, <a href="/search/?searchtype=author&query=Radiconi%2C+F">F. Radiconi</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=Murgia%2C+M">M. Murgia</a>, <a href="/search/?searchtype=author&query=Carretti%2C+E">E. Carretti</a>, <a href="/search/?searchtype=author&query=Castangia%2C+P">P. Castangia</a>, <a href="/search/?searchtype=author&query=Concu%2C+R">R. Concu</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Fritz%2C+J">J. Fritz</a>, <a href="/search/?searchtype=author&query=Genova-Santos%2C+R">R. Genova-Santos</a>, <a href="/search/?searchtype=author&query=Govoni%2C+F">F. Govoni</a>, <a href="/search/?searchtype=author&query=Guidi%2C+F">F. Guidi</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">L. Lamagna</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Melis%2C+A">A. Melis</a>, <a href="/search/?searchtype=author&query=Paladini%2C+R">R. Paladini</a>, <a href="/search/?searchtype=author&query=Perez-Toledo%2C+F+M">F. M. Perez-Toledo</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">F. Piacentini</a>, <a href="/search/?searchtype=author&query=Poppi%2C+S">S. Poppi</a>, <a href="/search/?searchtype=author&query=Rebolo%2C+R">R. Rebolo</a>, <a href="/search/?searchtype=author&query=Rubino-Martin%2C+J+A">J. A. Rubino-Martin</a>, <a href="/search/?searchtype=author&query=Surcis%2C+G">G. Surcis</a>, <a href="/search/?searchtype=author&query=Tarchi%2C+A">A. Tarchi</a>, <a href="/search/?searchtype=author&query=Vacca%2C+V">V. Vacca</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="2105.10453v1-abstract-short" style="display: inline;"> The Andromeda galaxy is the best-known large galaxy besides our own Milky Way. Several images and studies exist at all wavelengths from radio to hard X-ray. Nevertheless, only a few observations are available in the microwave range where its average radio emission reaches the minimum. In this paper, we want to study the radio morphology of the galaxy, decouple thermal from nonthermal emission, and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.10453v1-abstract-full').style.display = 'inline'; document.getElementById('2105.10453v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2105.10453v1-abstract-full" style="display: none;"> The Andromeda galaxy is the best-known large galaxy besides our own Milky Way. Several images and studies exist at all wavelengths from radio to hard X-ray. Nevertheless, only a few observations are available in the microwave range where its average radio emission reaches the minimum. In this paper, we want to study the radio morphology of the galaxy, decouple thermal from nonthermal emission, and extract the star formation rate. We also aim to derive a complete catalog of radio sources for the mapped patch of sky. We observed the Andromeda galaxy with the Sardinia Radio Telescope at 6.6 GHz with very high sensitivity and angular resolution, and an unprecedented sky coverage. Using new 6.6 GHz data and Effelsberg radio telescope ancillary data, we confirm that, globally, the spectral index is $\sim 0.7-0.8$, while in the star forming regions it decreases to $\sim 0.5$. By disentangling (gas) thermal and nonthermal emission, we find that at 6.6 GHz, thermal emission follows the distribution of HII regions around the ring. Nonthermal emission within the ring appears smoother and more uniform than thermal emission because of diffusion of the cosmic ray electrons away from their birthplaces. This causes the magnetic fields to appear almost constant in intensity. Furthermore, we calculated a map of the star formation rate based on the map of thermal emission. Integrating within a radius of $R_{max}=15$ kpc, we obtained a total star formation rate of $0.19 \pm 0.01$ $M_{\odot}$/yr in agreement with previous results in the literature. Finally, we correlated our radio data with infrared images of the Andromeda galaxy. We find an unexpectedly high correlation between nonthermal and mid-infrared data in the central region, with a correlation parameter $r=0.93$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2105.10453v1-abstract-full').style.display = 'none'; document.getElementById('2105.10453v1-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 May, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">36 pages, 31 figures, 10 tables. Accepted for publication in the 4. Extragalactic astronomy section of A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 651, A98 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2102.00809">arXiv:2102.00809</a> <span> [<a href="https://arxiv.org/pdf/2102.00809">pdf</a>, <a href="https://arxiv.org/format/2102.00809">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/10.1117/12.2562243">10.1117/12.2562243 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Overview of the Medium and High Frequency Telescopes of the LiteBIRD satellite mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montier%2C+L">L. Montier</a>, <a href="/search/?searchtype=author&query=Mot%2C+B">B. Mot</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Maffei%2C+B">B. Maffei</a>, <a href="/search/?searchtype=author&query=Pisano%2C+G">G. Pisano</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Gudmundsson%2C+J+E">J. E. Gudmundsson</a>, <a href="/search/?searchtype=author&query=Henrot-Versill%C3%A9%2C+S">S. Henrot-Versill茅</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">L. Lamagna</a>, <a href="/search/?searchtype=author&query=Montgomery%2C+J">J. Montgomery</a>, <a href="/search/?searchtype=author&query=Prouv%C3%A9%2C+T">T. Prouv茅</a>, <a href="/search/?searchtype=author&query=Russell%2C+M">M. Russell</a>, <a href="/search/?searchtype=author&query=Savini%2C+G">G. Savini</a>, <a href="/search/?searchtype=author&query=Stever%2C+S">S. Stever</a>, <a href="/search/?searchtype=author&query=Thompson%2C+K+L">K. L. Thompson</a>, <a href="/search/?searchtype=author&query=Tsujimoto%2C+M">M. Tsujimoto</a>, <a href="/search/?searchtype=author&query=Tucker%2C+C">C. Tucker</a>, <a href="/search/?searchtype=author&query=Westbrook%2C+B">B. Westbrook</a>, <a href="/search/?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/?searchtype=author&query=Adler%2C+A">A. Adler</a>, <a href="/search/?searchtype=author&query=Allys%2C+E">E. Allys</a>, <a href="/search/?searchtype=author&query=Arnold%2C+K">K. Arnold</a>, <a href="/search/?searchtype=author&query=Auguste%2C+D">D. Auguste</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Aurlien%2C+R">R. Aurlien</a> , et al. (212 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="2102.00809v1-abstract-short" style="display: inline;"> LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.00809v1-abstract-full').style.display = 'inline'; document.getElementById('2102.00809v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2102.00809v1-abstract-full" style="display: none;"> LiteBIRD is a JAXA-led Strategic Large-Class mission designed to search for the existence of the primordial gravitational waves produced during the inflationary phase of the Universe, through the measurements of their imprint onto the polarization of the cosmic microwave background (CMB). These measurements, requiring unprecedented sensitivity, will be performed over the full sky, at large angular scales, and over 15 frequency bands from 34GHz to 448GHz. The LiteBIRD instruments consist of three telescopes, namely the Low-, Medium- and High-Frequency Telescope (respectively LFT, MFT and HFT). We present in this paper an overview of the design of the Medium-Frequency Telescope (89-224GHz) and the High-Frequency Telescope (166-448GHz), the so-called MHFT, under European responsibility, which are two cryogenic refractive telescopes cooled down to 5K. They include a continuous rotating half-wave plate as the first optical element, two high-density polyethylene (HDPE) lenses and more than three thousand transition-edge sensor (TES) detectors cooled to 100mK. We provide an overview of the concept design and the remaining specific challenges that we have to face in order to achieve the scientific goals of LiteBIRD. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2102.00809v1-abstract-full').style.display = 'none'; document.getElementById('2102.00809v1-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 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">SPIE Conference</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. of SPIE Vol. 11443 14432G (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.12449">arXiv:2101.12449</a> <span> [<a href="https://arxiv.org/pdf/2101.12449">pdf</a>, <a href="https://arxiv.org/format/2101.12449">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="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 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/10.1117/12.2563050">10.1117/12.2563050 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> LiteBIRD: JAXA's new strategic L-class mission for all-sky surveys of cosmic microwave background polarization </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hazumi%2C+M">M. Hazumi</a>, <a href="/search/?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/?searchtype=author&query=Adler%2C+A">A. Adler</a>, <a href="/search/?searchtype=author&query=Allys%2C+E">E. Allys</a>, <a href="/search/?searchtype=author&query=Arnold%2C+K">K. Arnold</a>, <a href="/search/?searchtype=author&query=Auguste%2C+D">D. Auguste</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Aurlien%2C+R">R. Aurlien</a>, <a href="/search/?searchtype=author&query=Austermann%2C+J">J. Austermann</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Banjeri%2C+R">R. Banjeri</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Basak%2C+S">S. Basak</a>, <a href="/search/?searchtype=author&query=Beall%2C+J">J. Beall</a>, <a href="/search/?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/?searchtype=author&query=Beckman%2C+S">S. Beckman</a>, <a href="/search/?searchtype=author&query=Bermejo%2C+J">J. Bermejo</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Bonis%2C+J">J. Bonis</a>, <a href="/search/?searchtype=author&query=Borrill%2C+J">J. Borrill</a>, <a href="/search/?searchtype=author&query=Boulanger%2C+F">F. Boulanger</a>, <a href="/search/?searchtype=author&query=Bounissou%2C+S">S. Bounissou</a>, <a href="/search/?searchtype=author&query=Brilenkov%2C+M">M. Brilenkov</a> , et al. (213 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="2101.12449v1-abstract-short" style="display: inline;"> LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. JAXA selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with its expected launch in the late 2020s using JAXA's H3 rocket. LiteBIRD plans to map the cosmic microwave backgrou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.12449v1-abstract-full').style.display = 'inline'; document.getElementById('2101.12449v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.12449v1-abstract-full" style="display: none;"> LiteBIRD, the Lite (Light) satellite for the study of B-mode polarization and Inflation from cosmic background Radiation Detection, is a space mission for primordial cosmology and fundamental physics. JAXA selected LiteBIRD in May 2019 as a strategic large-class (L-class) mission, with its expected launch in the late 2020s using JAXA's H3 rocket. LiteBIRD plans to map the cosmic microwave background (CMB) polarization over the full sky with unprecedented precision. Its main scientific objective is to carry out a definitive search for the signal from cosmic inflation, either making a discovery or ruling out well-motivated inflationary models. The measurements of LiteBIRD will also provide us with an insight into the quantum nature of gravity and other new physics beyond the standard models of particle physics and cosmology. To this end, LiteBIRD will perform full-sky surveys for three years at the Sun-Earth Lagrangian point L2 for 15 frequency bands between 34 and 448 GHz with three telescopes, to achieve a total sensitivity of 2.16 micro K-arcmin with a typical angular resolution of 0.5 deg. at 100GHz. We provide an overview of the LiteBIRD project, including scientific objectives, mission requirements, top-level system requirements, operation concept, and expected scientific outcomes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.12449v1-abstract-full').style.display = 'none'; document.getElementById('2101.12449v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">20 pages, 9 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. of SPIE Vol. 11443 114432F (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.06787">arXiv:2101.06787</a> <span> [<a href="https://arxiv.org/pdf/2101.06787">pdf</a>, <a href="https://arxiv.org/format/2101.06787">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2022/04/037">10.1088/1475-7516/2022/04/037 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> QUBIC IV: Performance of TES Bolometers and Readout Electronics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Piat%2C+M">M. Piat</a>, <a href="/search/?searchtype=author&query=Stankowiak%2C+G">G. Stankowiak</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Alessandro%2C+G+D">G. D Alessandro</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Grandsire%2C+L">L. Grandsire</a>, <a href="/search/?searchtype=author&query=Hamilton%2C+J+-">J. -Ch. Hamilton</a>, <a href="/search/?searchtype=author&query=Hoang%2C+T+D">T. D. Hoang</a>, <a href="/search/?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=Mousset%2C+L">L. Mousset</a>, <a href="/search/?searchtype=author&query=Sullivan%2C+C+O">C. O Sullivan</a>, <a href="/search/?searchtype=author&query=Prele%2C+D">D. Prele</a>, <a href="/search/?searchtype=author&query=Tartari%2C+A">A. Tartari</a>, <a href="/search/?searchtype=author&query=Thermeau%2C+J+-">J. -P. Thermeau</a>, <a href="/search/?searchtype=author&query=Torchinsky%2C+S+A">S. A. Torchinsky</a>, <a href="/search/?searchtype=author&query=Voisin%2C+F">F. Voisin</a>, <a href="/search/?searchtype=author&query=Zannoni%2C+M">M. Zannoni</a>, <a href="/search/?searchtype=author&query=Ade%2C+P">P. Ade</a>, <a href="/search/?searchtype=author&query=Alberro%2C+J+G">J. G. Alberro</a>, <a href="/search/?searchtype=author&query=Almela%2C+A">A. Almela</a>, <a href="/search/?searchtype=author&query=Amico%2C+G">G. Amico</a>, <a href="/search/?searchtype=author&query=Arnaldi%2C+L+H">L. H. Arnaldi</a> , et al. (104 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="2101.06787v2-abstract-short" style="display: inline;"> A prototype version of the Q & U bolometric interferometer for cosmology (QUBIC) underwent a campaign of testing in the laboratory at Astroparticle Physics and Cosmology laboratory in Paris (APC). The detection chain is currently made of 256 NbSi transition edge sensors (TES) cooled to 320 mK. The readout system is a 128:1 time domain multiplexing scheme based on 128 SQUIDs cooled at 1 K that are… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.06787v2-abstract-full').style.display = 'inline'; document.getElementById('2101.06787v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.06787v2-abstract-full" style="display: none;"> A prototype version of the Q & U bolometric interferometer for cosmology (QUBIC) underwent a campaign of testing in the laboratory at Astroparticle Physics and Cosmology laboratory in Paris (APC). The detection chain is currently made of 256 NbSi transition edge sensors (TES) cooled to 320 mK. The readout system is a 128:1 time domain multiplexing scheme based on 128 SQUIDs cooled at 1 K that are controlled and amplified by an SiGe application specific integrated circuit at 40 K. We report the performance of this readout chain and the characterization of the TES. The readout system has been functionally tested and characterized in the lab and in QUBIC. The low noise amplifier demonstrated a white noise level of 0.3 nV.Hz^-0.5. Characterizations of the QUBIC detectors and readout electronics includes the measurement of I-V curves, time constant and the noise equivalent power. The QUBIC TES bolometer array has approximately 80% detectors within operational parameters. It demonstrated a thermal decoupling compatible with a phonon noise of about 5.10^-17 W.Hz^-0.5 at 410 mK critical temperature. While still limited by microphonics from the pulse tubes and noise aliasing from readout system, the instrument noise equivalent power is about 2.10^-16 W.Hz^-0.5, enough for the demonstration of bolometric interferometry. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.06787v2-abstract-full').style.display = 'none'; document.getElementById('2101.06787v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 October, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">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/2101.06342">arXiv:2101.06342</a> <span> [<a href="https://arxiv.org/pdf/2101.06342">pdf</a>, <a href="https://arxiv.org/format/2101.06342">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/10.1117/12.2561841">10.1117/12.2561841 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Concept Design of Low Frequency Telescope for CMB B-mode Polarization satellite LiteBIRD </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Sekimoto%2C+Y">Y. Sekimoto</a>, <a href="/search/?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/?searchtype=author&query=Adler%2C+A">A. Adler</a>, <a href="/search/?searchtype=author&query=Allys%2C+E">E. Allys</a>, <a href="/search/?searchtype=author&query=Arnold%2C+K">K. Arnold</a>, <a href="/search/?searchtype=author&query=Auguste%2C+D">D. Auguste</a>, <a href="/search/?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/?searchtype=author&query=Aurlien%2C+R">R. Aurlien</a>, <a href="/search/?searchtype=author&query=Austermann%2C+J">J. Austermann</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/?searchtype=author&query=Banerji%2C+R">R. Banerji</a>, <a href="/search/?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/?searchtype=author&query=Basak%2C+S">S. Basak</a>, <a href="/search/?searchtype=author&query=Beall%2C+J">J. Beall</a>, <a href="/search/?searchtype=author&query=Beck%2C+D">D. Beck</a>, <a href="/search/?searchtype=author&query=Beckman%2C+S">S. Beckman</a>, <a href="/search/?searchtype=author&query=Bermejo%2C+J">J. Bermejo</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Bonis%2C+J">J. Bonis</a>, <a href="/search/?searchtype=author&query=Borrill%2C+J">J. Borrill</a>, <a href="/search/?searchtype=author&query=Boulanger%2C+F">F. Boulanger</a>, <a href="/search/?searchtype=author&query=Bounissou%2C+S">S. Bounissou</a>, <a href="/search/?searchtype=author&query=Brilenkov%2C+M">M. Brilenkov</a> , et al. (212 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="2101.06342v1-abstract-short" style="display: inline;"> LiteBIRD has been selected as JAXA's strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) $B$-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray li… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.06342v1-abstract-full').style.display = 'inline'; document.getElementById('2101.06342v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.06342v1-abstract-full" style="display: none;"> LiteBIRD has been selected as JAXA's strategic large mission in the 2020s, to observe the cosmic microwave background (CMB) $B$-mode polarization over the full sky at large angular scales. The challenges of LiteBIRD are the wide field-of-view (FoV) and broadband capabilities of millimeter-wave polarization measurements, which are derived from the system requirements. The possible paths of stray light increase with a wider FoV and the far sidelobe knowledge of $-56$ dB is a challenging optical requirement. A crossed-Dragone configuration was chosen for the low frequency telescope (LFT : 34--161 GHz), one of LiteBIRD's onboard telescopes. It has a wide field-of-view ($18^\circ \times 9^\circ$) with an aperture of 400 mm in diameter, corresponding to an angular resolution of about 30 arcminutes around 100 GHz. The focal ratio f/3.0 and the crossing angle of the optical axes of 90$^\circ$ are chosen after an extensive study of the stray light. The primary and secondary reflectors have rectangular shapes with serrations to reduce the diffraction pattern from the edges of the mirrors. The reflectors and structure are made of aluminum to proportionally contract from warm down to the operating temperature at $5\,$K. A 1/4 scaled model of the LFT has been developed to validate the wide field-of-view design and to demonstrate the reduced far sidelobes. A polarization modulation unit (PMU), realized with a half-wave plate (HWP) is placed in front of the aperture stop, the entrance pupil of this system. A large focal plane with approximately 1000 AlMn TES detectors and frequency multiplexing SQUID amplifiers is cooled to 100 mK. The lens and sinuous antennas have broadband capability. Performance specifications of the LFT and an outline of the proposed verification plan are presented. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.06342v1-abstract-full').style.display = 'none'; document.getElementById('2101.06342v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">21 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> SPIE proceedings 1145310 (2020) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.05188">arXiv:2101.05188</a> <span> [<a href="https://arxiv.org/pdf/2101.05188">pdf</a>, <a href="https://arxiv.org/format/2101.05188">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/10.1007/s10909-022-02919-1">10.1007/s10909-022-02919-1 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Polarization Modulator Unit for the Mid- and High-Frequency Telescopes of the LiteBIRD mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Columbro%2C+F">Fabio Columbro</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">Luca Lamagna</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">Silvia Masi</a>, <a href="/search/?searchtype=author&query=Paiella%2C+A">Alessandro Paiella</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">Francesco Piacentini</a>, <a href="/search/?searchtype=author&query=Pisano%2C+G">Giampaolo Pisano</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="2101.05188v1-abstract-short" style="display: inline;"> The LiteBIRD mission is a JAXA strategic L-class mission for all sky CMB surveys which will be launched in the 2020s. The main target of the mission is the detection of primordial gravitational waves with a sensitivity ofthe tensor-to-scalar ratio 未r <0.001. The polarization modulator unit (PMU) represents a critical and powerful component to suppress 1/f noise contribution and mitigate systematic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05188v1-abstract-full').style.display = 'inline'; document.getElementById('2101.05188v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.05188v1-abstract-full" style="display: none;"> The LiteBIRD mission is a JAXA strategic L-class mission for all sky CMB surveys which will be launched in the 2020s. The main target of the mission is the detection of primordial gravitational waves with a sensitivity ofthe tensor-to-scalar ratio 未r <0.001. The polarization modulator unit (PMU) represents a critical and powerful component to suppress 1/f noise contribution and mitigate systematic uncertainties induced by detector gain drift, both for the high-frequency telescope (HFT) and for the mid-frequency telescope (MFT). Each PMUs based on a continuously-rotating transmissive half-wave plate (HWP) held by a superconducting magnetic bearing in a 5K environment. In this proceeding we will present the design and expected performance of the LiteBIRD PMUs and testing performed on every PMU subsystem with a room-temperature rotating disk used as a stand-in for the cryogenic HWP rotor. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.05188v1-abstract-full').style.display = 'none'; document.getElementById('2101.05188v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">16 pages, 6 figures, SPIE Proceeding no. 11443-282</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2101.03833">arXiv:2101.03833</a> <span> [<a href="https://arxiv.org/pdf/2101.03833">pdf</a>, <a href="https://arxiv.org/format/2101.03833">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"> The optical design of the LiteBIRD Middle and High Frequency Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lamagna%2C+L">L. Lamagna</a>, <a href="/search/?searchtype=author&query=Gudmundsson%2C+J+E">J. E. Gudmundsson</a>, <a href="/search/?searchtype=author&query=Imada%2C+H">H. Imada</a>, <a href="/search/?searchtype=author&query=Hargrave%2C+P">P. Hargrave</a>, <a href="/search/?searchtype=author&query=Franceschet%2C+C">C. Franceschet</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Austermann%2C+J">J. Austermann</a>, <a href="/search/?searchtype=author&query=Bounissou%2C+S">S. Bounissou</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Henrot-Versille%2C+S">S. Henrot-Versille</a>, <a href="/search/?searchtype=author&query=Hubmayr%2C+J">J. Hubmayr</a>, <a href="/search/?searchtype=author&query=Jaehnig%2C+G">G. Jaehnig</a>, <a href="/search/?searchtype=author&query=Keskitalo%2C+R">R. Keskitalo</a>, <a href="/search/?searchtype=author&query=Maffei%2C+B">B. Maffei</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Matsumura%2C+T">T. Matsumura</a>, <a href="/search/?searchtype=author&query=Montier%2C+L">L. Montier</a>, <a href="/search/?searchtype=author&query=Mot%2C+B">B. Mot</a>, <a href="/search/?searchtype=author&query=Noviello%2C+F">F. Noviello</a>, <a href="/search/?searchtype=author&query=O%27Sullivan%2C+C">C. O'Sullivan</a>, <a href="/search/?searchtype=author&query=Paiella%2C+A">A. Paiella</a>, <a href="/search/?searchtype=author&query=Pisano%2C+G">G. Pisano</a>, <a href="/search/?searchtype=author&query=Realini%2C+S">S. Realini</a>, <a href="/search/?searchtype=author&query=Ritacco%2C+A">A. Ritacco</a> , et al. (4 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="2101.03833v1-abstract-short" style="display: inline;"> LiteBIRD is a JAXA strategic L-class mission devoted to the measurement of polarization of the Cosmic Microwave Background, searching for the signature of primordial gravitational waves in the B-modes pattern of the polarization. The onboard instrumentation includes a Middle and High Frequency Telescope (MHFT), based on a pair of cryogenically cooled refractive telescopes covering, respectively, t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03833v1-abstract-full').style.display = 'inline'; document.getElementById('2101.03833v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2101.03833v1-abstract-full" style="display: none;"> LiteBIRD is a JAXA strategic L-class mission devoted to the measurement of polarization of the Cosmic Microwave Background, searching for the signature of primordial gravitational waves in the B-modes pattern of the polarization. The onboard instrumentation includes a Middle and High Frequency Telescope (MHFT), based on a pair of cryogenically cooled refractive telescopes covering, respectively, the 89-224 GHz and the 166-448 GHz bands. Given the high target sensitivity and the careful systematics control needed to achieve the scientific goals of the mission, optical modeling and characterization are performed with the aim to capture most of the physical effects potentially affecting the real performance of the two refractors. We describe the main features of the MHFT, its design drivers and the major challenges in system optimization and characterization. We provide the current status of the development of the optical system and we describe the current plan of activities related to optical performance simulation and validation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2101.03833v1-abstract-full').style.display = 'none'; document.getElementById('2101.03833v1-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 January, 2021; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">17 pages, 13 figures, SPIE Proceeding no. 11443-283</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2011.02213">arXiv:2011.02213</a> <span> [<a href="https://arxiv.org/pdf/2011.02213">pdf</a>, <a href="https://arxiv.org/format/2011.02213">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/10.1088/1475-7516/2022/04/034">10.1088/1475-7516/2022/04/034 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> QUBIC I: Overview and ScienceProgram </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hamilton%2C+J+-">J. -Ch. Hamilton</a>, <a href="/search/?searchtype=author&query=Mousset%2C+L">L. Mousset</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=Bigot-Sazy%2C+M+-">M. -A. Bigot-Sazy</a>, <a href="/search/?searchtype=author&query=Chanial%2C+P">P. Chanial</a>, <a href="/search/?searchtype=author&query=Charlassier%2C+R">R. Charlassier</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Lerena%2C+M+M+G">M. M. Gamboa Lerena</a>, <a href="/search/?searchtype=author&query=Grandsire%2C+L">L. Grandsire</a>, <a href="/search/?searchtype=author&query=Lau%2C+S">S. Lau</a>, <a href="/search/?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=O%27Sullivan%2C+C">C. O'Sullivan</a>, <a href="/search/?searchtype=author&query=Piat%2C+M">M. Piat</a>, <a href="/search/?searchtype=author&query=Riccardi%2C+G">G. Riccardi</a>, <a href="/search/?searchtype=author&query=Sc%C3%B3ccola%2C+C">C. Sc贸ccola</a>, <a href="/search/?searchtype=author&query=Stolpovskiy%2C+M">M. Stolpovskiy</a>, <a href="/search/?searchtype=author&query=Tartari%2C+A">A. Tartari</a>, <a href="/search/?searchtype=author&query=Torchinsky%2C+S+A">S. A. Torchinsky</a>, <a href="/search/?searchtype=author&query=Voisin%2C+F">F. Voisin</a>, <a href="/search/?searchtype=author&query=Zannoni%2C+M">M. Zannoni</a>, <a href="/search/?searchtype=author&query=Ade%2C+P">P. Ade</a> , et al. (105 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="2011.02213v2-abstract-short" style="display: inline;"> The Q $\&$ U Bolometric Interferometer for Cosmology (QUBIC) is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Background (CMB), which is one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.02213v2-abstract-full').style.display = 'inline'; document.getElementById('2011.02213v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2011.02213v2-abstract-full" style="display: none;"> The Q $\&$ U Bolometric Interferometer for Cosmology (QUBIC) is a novel kind of polarimeter optimized for the measurement of the B-mode polarization of the Cosmic Microwave Background (CMB), which is one of the major challenges of observational cosmology. The signal is expected to be of the order of a few tens of nK, prone to instrumental systematic effects and polluted by various astrophysical foregrounds which can only be controlled through multichroic observations. QUBIC is designed to address these observational issues with a novel approach that combines the advantages of interferometry in terms of control of instrumental systematic effects with those of bolometric detectors in terms of wide-band, background-limited sensitivity. The QUBIC synthesized beam has a frequency-dependent shape that results in the ability to produce maps of the CMB polarization in multiple sub-bands within the two physical bands of the instrument (150 and 220 GHz). These features make QUBIC complementary to other instruments and makes it particularly well suited to characterize and remove Galactic foreground contamination. In this article, first of a series of eight, we give an overview of the QUBIC instrument design, the main results of the calibration campaign, and present the scientific program of QUBIC including not only the measurement of primordial B-modes, but also the measurement of Galactic foregrounds. We give forecasts for typical observations and measurements: with three years of integration on the sky and assuming perfect foreground removal as well as stable atmospheric conditions from our site in Argentina, our simulations show that we can achieve a statistical sensitivity to the effective tensor-to-scalar ratio (including primordial and foreground B-modes) $蟽(r)=0.015$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2011.02213v2-abstract-full').style.display = 'none'; document.getElementById('2011.02213v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 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">34 pages, 16 figures, accepted for publication by JCAP. Overview paper for a series of 8 QUBIC articles special JCAP edition dedicated to QUBIC</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2010.15119">arXiv:2010.15119</a> <span> [<a href="https://arxiv.org/pdf/2010.15119">pdf</a>, <a href="https://arxiv.org/format/2010.15119">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2022/04/035">10.1088/1475-7516/2022/04/035 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> QUBIC II: Spectro-Polarimetry with Bolometric Interferometry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Mousset%2C+L">L. Mousset</a>, <a href="/search/?searchtype=author&query=Lerena%2C+M+M+G">M. M. Gamboa Lerena</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Chanial%2C+P">P. Chanial</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=Dashyan%2C+G">G. Dashyan</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Grandsire%2C+L">L. Grandsire</a>, <a href="/search/?searchtype=author&query=Hamilton%2C+J+-">J. -Ch. Hamilton</a>, <a href="/search/?searchtype=author&query=Incardona%2C+F">F. Incardona</a>, <a href="/search/?searchtype=author&query=Landau%2C+S">S. Landau</a>, <a href="/search/?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=O%27Sullivan%2C+C">C. O'Sullivan</a>, <a href="/search/?searchtype=author&query=Piat%2C+M">M. Piat</a>, <a href="/search/?searchtype=author&query=Ricciardi%2C+G">G. Ricciardi</a>, <a href="/search/?searchtype=author&query=Sc%C3%B3ccola%2C+C+G">C. G. Sc贸ccola</a>, <a href="/search/?searchtype=author&query=Stolpovskiy%2C+M">M. Stolpovskiy</a>, <a href="/search/?searchtype=author&query=Tartari%2C+A">A. Tartari</a>, <a href="/search/?searchtype=author&query=Thermeau%2C+J+-">J. -P. Thermeau</a>, <a href="/search/?searchtype=author&query=Torchinsky%2C+S+A">S. A. Torchinsky</a>, <a href="/search/?searchtype=author&query=Voisin%2C+F">F. Voisin</a>, <a href="/search/?searchtype=author&query=Zannoni%2C+M">M. Zannoni</a> , et al. (106 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="2010.15119v3-abstract-short" style="display: inline;"> Bolometric interferometry is a novel technique that has the ability to perform spectral imaging. A bolometric interferometer observes the sky in a wide frequency band and can reconstruct sky maps in several sub-bands within the physical band in post-processing of the data. This provides a powerful spectral method to discriminate between the cosmic microwave background (CMB) and astrophysical foreg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.15119v3-abstract-full').style.display = 'inline'; document.getElementById('2010.15119v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2010.15119v3-abstract-full" style="display: none;"> Bolometric interferometry is a novel technique that has the ability to perform spectral imaging. A bolometric interferometer observes the sky in a wide frequency band and can reconstruct sky maps in several sub-bands within the physical band in post-processing of the data. This provides a powerful spectral method to discriminate between the cosmic microwave background (CMB) and astrophysical foregrounds. In this paper, the methodology is illustrated with examples based on the Q \& U Bolometric Interferometer for Cosmology (QUBIC) which is a ground-based instrument designed to measure the B-mode polarization of the sky at millimeter wavelengths. We consider the specific cases of point source reconstruction and Galactic dust mapping and we characterize the point spread function as a function of frequency. We study the noise properties of spectral imaging, especially the correlations between sub-bands, using end-to-end simulations together with a fast noise simulator. We conclude showing that spectral imaging performance are nearly optimal up to five sub-bands in the case of QUBIC. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2010.15119v3-abstract-full').style.display = 'none'; document.getElementById('2010.15119v3-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 March, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 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">27 pages, 18 figures. Accepted by JCAP on July 6, 2021. Second paper of series of 8 in a special JCAP edition on QUBIC</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.12721">arXiv:2008.12721</a> <span> [<a href="https://arxiv.org/pdf/2008.12721">pdf</a>, <a href="https://arxiv.org/format/2008.12721">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2022/04/040">10.1088/1475-7516/2022/04/040 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> QUBIC VII: The feedhorn-switch system of the technological demonstrator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cavaliere%2C+F">F. Cavaliere</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=Zannoni%2C+M">M. Zannoni</a>, <a href="/search/?searchtype=author&query=Battaglia%2C+P">P. Battaglia</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=Burke%2C+D">D. Burke</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Franceschet%2C+C">C. Franceschet</a>, <a href="/search/?searchtype=author&query=Grandsire%2C+L">L. Grandsire</a>, <a href="/search/?searchtype=author&query=Hamilton%2C+J+-">J. -Ch. Hamilton</a>, <a href="/search/?searchtype=author&query=Maffei%2C+B">B. Maffei</a>, <a href="/search/?searchtype=author&query=Manzan%2C+E">E. Manzan</a>, <a href="/search/?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=O%27Sullivan%2C+C">C. O'Sullivan</a>, <a href="/search/?searchtype=author&query=Passerini%2C+A">A. Passerini</a>, <a href="/search/?searchtype=author&query=Pezzotta%2C+F">F. Pezzotta</a>, <a href="/search/?searchtype=author&query=Piat%2C+M">M. Piat</a>, <a href="/search/?searchtype=author&query=Tartari%2C+A">A. Tartari</a>, <a href="/search/?searchtype=author&query=Torchinsky%2C+S+A">S. A. Torchinsky</a>, <a href="/search/?searchtype=author&query=Vigan%C3%B2%2C+D">D. Vigan貌</a>, <a href="/search/?searchtype=author&query=Voisin%2C+F">F. Voisin</a>, <a href="/search/?searchtype=author&query=Ade%2C+P">P. Ade</a> , et al. (106 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="2008.12721v3-abstract-short" style="display: inline;"> We present the design, manufacturing and performance of the horn-switch system developed for the technological demonstrator of QUBIC (the $Q$\&$U$ Bolometric Interferometer for Cosmology). This system is constituted of 64 back-to-back dual-band (150\,GHz and 220\,GHz) corrugated feed-horns interspersed with mechanical switches used to select desired baselines during the instrument self-calibration… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.12721v3-abstract-full').style.display = 'inline'; document.getElementById('2008.12721v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.12721v3-abstract-full" style="display: none;"> We present the design, manufacturing and performance of the horn-switch system developed for the technological demonstrator of QUBIC (the $Q$\&$U$ Bolometric Interferometer for Cosmology). This system is constituted of 64 back-to-back dual-band (150\,GHz and 220\,GHz) corrugated feed-horns interspersed with mechanical switches used to select desired baselines during the instrument self-calibration. We manufactured the horns in aluminum platelets milled by photo-chemical etching and mechanically tightened with screws. The switches are based on steel blades that open and close the wave-guide between the back-to-back horns and are operated by miniaturized electromagnets. We also show the current development status of the feedhorn-switch system for the QUBIC full instrument, based on an array of 400 horn-switch assemblies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.12721v3-abstract-full').style.display = 'none'; document.getElementById('2008.12721v3-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 April, 2022; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 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">30 pages, 28 figures. Accepted for submission to 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/2008.11286">arXiv:2008.11286</a> <span> [<a href="https://arxiv.org/pdf/2008.11286">pdf</a>, <a href="https://arxiv.org/format/2008.11286">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/10.1016/j.astropartphys.2021.102607">10.1016/j.astropartphys.2021.102607 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmology Intertwined IV: The Age of the Universe and its Curvature </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Di+Valentino%2C+E">Eleonora Di Valentino</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L+A">Luis A. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Akarsu%2C+O">Ozgur Akarsu</a>, <a href="/search/?searchtype=author&query=Ali-Haimoud%2C+Y">Yacine Ali-Haimoud</a>, <a href="/search/?searchtype=author&query=Amendola%2C+L">Luca Amendola</a>, <a href="/search/?searchtype=author&query=Arendse%2C+N">Nikki Arendse</a>, <a href="/search/?searchtype=author&query=Asgari%2C+M">Marika Asgari</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">Mario Ballardini</a>, <a href="/search/?searchtype=author&query=Basilakos%2C+S">Spyros Basilakos</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">Elia Battistelli</a>, <a href="/search/?searchtype=author&query=Benetti%2C+M">Micol Benetti</a>, <a href="/search/?searchtype=author&query=Birrer%2C+S">Simon Birrer</a>, <a href="/search/?searchtype=author&query=Bouchet%2C+F+R">Fran莽ois R. Bouchet</a>, <a href="/search/?searchtype=author&query=Bruni%2C+M">Marco Bruni</a>, <a href="/search/?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/?searchtype=author&query=Camarena%2C+D">David Camarena</a>, <a href="/search/?searchtype=author&query=Capozziello%2C+S">Salvatore Capozziello</a>, <a href="/search/?searchtype=author&query=Chen%2C+A">Angela Chen</a>, <a href="/search/?searchtype=author&query=Chluba%2C+J">Jens Chluba</a>, <a href="/search/?searchtype=author&query=Chudaykin%2C+A">Anton Chudaykin</a>, <a href="/search/?searchtype=author&query=Colg%C3%A1in%2C+E+%C3%93">Eoin 脫 Colg谩in</a>, <a href="/search/?searchtype=author&query=Cyr-Racine%2C+F">Francis-Yan Cyr-Racine</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez%2C+J+d+C">Javier de Cruz P茅rez</a>, <a href="/search/?searchtype=author&query=Delabrouille%2C+J">Jacques Delabrouille</a> , et al. (66 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="2008.11286v4-abstract-short" style="display: inline;"> A precise measurement of the curvature of the Universe is of primeval importance for cosmology since it could not only confirm the paradigm of primordial inflation but also help in discriminating between different early Universe scenarios. The recent observations, while broadly consistent with a spatially flat standard $螞$ Cold Dark Matter ($螞$CDM) model, are showing tensions that still allow (and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11286v4-abstract-full').style.display = 'inline'; document.getElementById('2008.11286v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.11286v4-abstract-full" style="display: none;"> A precise measurement of the curvature of the Universe is of primeval importance for cosmology since it could not only confirm the paradigm of primordial inflation but also help in discriminating between different early Universe scenarios. The recent observations, while broadly consistent with a spatially flat standard $螞$ Cold Dark Matter ($螞$CDM) model, are showing tensions that still allow (and, in some cases, even suggest) a few percent deviations from a flat universe. In particular, the Planck Cosmic Microwave Background power spectra, assuming the nominal likelihood, prefer a closed universe at more than 99\% confidence level. While new physics could be in action, this anomaly may be the result of an unresolved systematic error or just a statistical fluctuation. However, since a positive curvature allows a larger age of the Universe, an accurate determination of the age of the oldest objects provides a smoking gun in confirming or falsifying the current flat $螞$CDM model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11286v4-abstract-full').style.display = 'none'; document.getElementById('2008.11286v4-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">Snowmass2021 - Letter of Interest</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart. Phys. 131, 102607 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.11285">arXiv:2008.11285</a> <span> [<a href="https://arxiv.org/pdf/2008.11285">pdf</a>, <a href="https://arxiv.org/format/2008.11285">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/10.1016/j.astropartphys.2021.102604">10.1016/j.astropartphys.2021.102604 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmology Intertwined III: $f 蟽_8$ and $S_8$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Di+Valentino%2C+E">Eleonora Di Valentino</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L+A">Luis A. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Akarsu%2C+O">Ozgur Akarsu</a>, <a href="/search/?searchtype=author&query=Ali-Haimoud%2C+Y">Yacine Ali-Haimoud</a>, <a href="/search/?searchtype=author&query=Amendola%2C+L">Luca Amendola</a>, <a href="/search/?searchtype=author&query=Arendse%2C+N">Nikki Arendse</a>, <a href="/search/?searchtype=author&query=Asgari%2C+M">Marika Asgari</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">Mario Ballardini</a>, <a href="/search/?searchtype=author&query=Basilakos%2C+S">Spyros Basilakos</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">Elia Battistelli</a>, <a href="/search/?searchtype=author&query=Benetti%2C+M">Micol Benetti</a>, <a href="/search/?searchtype=author&query=Birrer%2C+S">Simon Birrer</a>, <a href="/search/?searchtype=author&query=Bouchet%2C+F+R">Fran莽ois R. Bouchet</a>, <a href="/search/?searchtype=author&query=Bruni%2C+M">Marco Bruni</a>, <a href="/search/?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/?searchtype=author&query=Camarena%2C+D">David Camarena</a>, <a href="/search/?searchtype=author&query=Capozziello%2C+S">Salvatore Capozziello</a>, <a href="/search/?searchtype=author&query=Chen%2C+A">Angela Chen</a>, <a href="/search/?searchtype=author&query=Chluba%2C+J">Jens Chluba</a>, <a href="/search/?searchtype=author&query=Chudaykin%2C+A">Anton Chudaykin</a>, <a href="/search/?searchtype=author&query=Colg%C3%A1in%2C+E+%C3%93">Eoin 脫 Colg谩in</a>, <a href="/search/?searchtype=author&query=Cyr-Racine%2C+F">Francis-Yan Cyr-Racine</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez%2C+J+d+C">Javier de Cruz P茅rez</a>, <a href="/search/?searchtype=author&query=Delabrouille%2C+J">Jacques Delabrouille</a> , et al. (67 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="2008.11285v4-abstract-short" style="display: inline;"> The standard $螞$ Cold Dark Matter cosmological model provides a wonderful fit to current cosmological data, but a few tensions and anomalies became statistically significant with the latest data analyses. While these anomalies could be due to the presence of systematic errors in the experiments, they could also indicate the need for new physics beyond the standard model. In this Letter of Interest… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11285v4-abstract-full').style.display = 'inline'; document.getElementById('2008.11285v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.11285v4-abstract-full" style="display: none;"> The standard $螞$ Cold Dark Matter cosmological model provides a wonderful fit to current cosmological data, but a few tensions and anomalies became statistically significant with the latest data analyses. While these anomalies could be due to the presence of systematic errors in the experiments, they could also indicate the need for new physics beyond the standard model. In this Letter of Interest we focus on the tension of the Planck data with weak lensing measurements and redshift surveys, about the value of the matter energy density $惟_m$, and the amplitude or rate of the growth of structure ($蟽_8,f蟽_8$). We list a few interesting models for solving this tension, and we discuss the importance of trying to fit with a single model a full array of data and not just one parameter at a time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11285v4-abstract-full').style.display = 'none'; document.getElementById('2008.11285v4-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">Snowmass2021 - Letter of Interest</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart. Phys. 131, 102604 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.11284">arXiv:2008.11284</a> <span> [<a href="https://arxiv.org/pdf/2008.11284">pdf</a>, <a href="https://arxiv.org/format/2008.11284">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/10.1016/j.astropartphys.2021.102605">10.1016/j.astropartphys.2021.102605 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmology Intertwined II: The Hubble Constant Tension </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Di+Valentino%2C+E">Eleonora Di Valentino</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L+A">Luis A. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Akarsu%2C+O">Ozgur Akarsu</a>, <a href="/search/?searchtype=author&query=Ali-Haimoud%2C+Y">Yacine Ali-Haimoud</a>, <a href="/search/?searchtype=author&query=Amendola%2C+L">Luca Amendola</a>, <a href="/search/?searchtype=author&query=Arendse%2C+N">Nikki Arendse</a>, <a href="/search/?searchtype=author&query=Asgari%2C+M">Marika Asgari</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">Mario Ballardini</a>, <a href="/search/?searchtype=author&query=Basilakos%2C+S">Spyros Basilakos</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">Elia Battistelli</a>, <a href="/search/?searchtype=author&query=Benetti%2C+M">Micol Benetti</a>, <a href="/search/?searchtype=author&query=Birrer%2C+S">Simon Birrer</a>, <a href="/search/?searchtype=author&query=Bouchet%2C+F+R">Fran莽ois R. Bouchet</a>, <a href="/search/?searchtype=author&query=Bruni%2C+M">Marco Bruni</a>, <a href="/search/?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/?searchtype=author&query=Camarena%2C+D">David Camarena</a>, <a href="/search/?searchtype=author&query=Capozziello%2C+S">Salvatore Capozziello</a>, <a href="/search/?searchtype=author&query=Chen%2C+A">Angela Chen</a>, <a href="/search/?searchtype=author&query=Chluba%2C+J">Jens Chluba</a>, <a href="/search/?searchtype=author&query=Chudaykin%2C+A">Anton Chudaykin</a>, <a href="/search/?searchtype=author&query=Colg%C3%A1in%2C+E+%C3%93">Eoin 脫 Colg谩in</a>, <a href="/search/?searchtype=author&query=Cyr-Racine%2C+F">Francis-Yan Cyr-Racine</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez%2C+J+d+C">Javier de Cruz P茅rez</a>, <a href="/search/?searchtype=author&query=Delabrouille%2C+J">Jacques Delabrouille</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="2008.11284v4-abstract-short" style="display: inline;"> The current cosmological probes have provided a fantastic confirmation of the standard $螞$ Cold Dark Matter cosmological model, that has been constrained with unprecedented accuracy. However, with the increase of the experimental sensitivity a few statistically significant tensions between different independent cosmological datasets emerged. While these tensions can be in portion the result of sys… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11284v4-abstract-full').style.display = 'inline'; document.getElementById('2008.11284v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.11284v4-abstract-full" style="display: none;"> The current cosmological probes have provided a fantastic confirmation of the standard $螞$ Cold Dark Matter cosmological model, that has been constrained with unprecedented accuracy. However, with the increase of the experimental sensitivity a few statistically significant tensions between different independent cosmological datasets emerged. While these tensions can be in portion the result of systematic errors, the persistence after several years of accurate analysis strongly hints at cracks in the standard cosmological scenario and the need for new physics. In this Letter of Interest we will focus on the $4.4蟽$ tension between the Planck estimate of the Hubble constant $H_0$ and the SH0ES collaboration measurements. After showing the $H_0$ evaluations made from different teams using different methods and geometric calibrations, we will list a few interesting new physics models that could solve this tension and discuss how the next decade experiments will be crucial. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11284v4-abstract-full').style.display = 'none'; document.getElementById('2008.11284v4-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">Snowmass2021 - Letter of Interest</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart. Phys. 131, 102605 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.11283">arXiv:2008.11283</a> <span> [<a href="https://arxiv.org/pdf/2008.11283">pdf</a>, <a href="https://arxiv.org/ps/2008.11283">ps</a>, <a href="https://arxiv.org/format/2008.11283">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/10.1016/j.astropartphys.2021.102606">10.1016/j.astropartphys.2021.102606 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmology Intertwined I: Perspectives for the Next Decade </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Di+Valentino%2C+E">Eleonora Di Valentino</a>, <a href="/search/?searchtype=author&query=Anchordoqui%2C+L+A">Luis A. Anchordoqui</a>, <a href="/search/?searchtype=author&query=Akarsu%2C+O">Ozgur Akarsu</a>, <a href="/search/?searchtype=author&query=Ali-Haimoud%2C+Y">Yacine Ali-Haimoud</a>, <a href="/search/?searchtype=author&query=Amendola%2C+L">Luca Amendola</a>, <a href="/search/?searchtype=author&query=Arendse%2C+N">Nikki Arendse</a>, <a href="/search/?searchtype=author&query=Asgari%2C+M">Marika Asgari</a>, <a href="/search/?searchtype=author&query=Ballardini%2C+M">Mario Ballardini</a>, <a href="/search/?searchtype=author&query=Basilakos%2C+S">Spyros Basilakos</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E">Elia Battistelli</a>, <a href="/search/?searchtype=author&query=Benetti%2C+M">Micol Benetti</a>, <a href="/search/?searchtype=author&query=Birrer%2C+S">Simon Birrer</a>, <a href="/search/?searchtype=author&query=Bouchet%2C+F+R">Fran莽ois R. Bouchet</a>, <a href="/search/?searchtype=author&query=Bruni%2C+M">Marco Bruni</a>, <a href="/search/?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/?searchtype=author&query=Camarena%2C+D">David Camarena</a>, <a href="/search/?searchtype=author&query=Capozziello%2C+S">Salvatore Capozziello</a>, <a href="/search/?searchtype=author&query=Chen%2C+A">Angela Chen</a>, <a href="/search/?searchtype=author&query=Chluba%2C+J">Jens Chluba</a>, <a href="/search/?searchtype=author&query=Chudaykin%2C+A">Anton Chudaykin</a>, <a href="/search/?searchtype=author&query=Colg%C3%A1in%2C+E+%C3%93">Eoin 脫 Colg谩in</a>, <a href="/search/?searchtype=author&query=Cyr-Racine%2C+F">Francis-Yan Cyr-Racine</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">Paolo de Bernardis</a>, <a href="/search/?searchtype=author&query=P%C3%A9rez%2C+J+d+C">Javier de Cruz P茅rez</a>, <a href="/search/?searchtype=author&query=Delabrouille%2C+J">Jacques Delabrouille</a> , et al. (67 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="2008.11283v4-abstract-short" style="display: inline;"> The standard $螞$ Cold Dark Matter cosmological model provides an amazing description of a wide range of astrophysical and astronomical data. However, there are a few big open questions, that make the standard model look like a first-order approximation to a more realistic scenario that still needs to be fully understood. In this Letter of Interest we will list a few important goals that need to be… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11283v4-abstract-full').style.display = 'inline'; document.getElementById('2008.11283v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.11283v4-abstract-full" style="display: none;"> The standard $螞$ Cold Dark Matter cosmological model provides an amazing description of a wide range of astrophysical and astronomical data. However, there are a few big open questions, that make the standard model look like a first-order approximation to a more realistic scenario that still needs to be fully understood. In this Letter of Interest we will list a few important goals that need to be addressed in the next decade, also taking into account the current discordances present between the different cosmological probes, as the Hubble constant $H_0$ value, the $蟽_8 - S_8$ tension, and the anomalies present in the Planck results. Finally, we will give an overview of upgraded experiments and next-generation space-missions and facilities on Earth, that will be of crucial importance to address all these questions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11283v4-abstract-full').style.display = 'none'; document.getElementById('2008.11283v4-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 October, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">Snowmass2021 - Letter of Interest</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart. Phys. 131, 102606 (2021) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.11049">arXiv:2008.11049</a> <span> [<a href="https://arxiv.org/pdf/2008.11049">pdf</a>, <a href="https://arxiv.org/format/2008.11049">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/10.1088/1475-7516/2021/08/008">10.1088/1475-7516/2021/08/008 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The large scale polarization explorer (LSPE) for CMB measurements: performance forecast </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=The+LSPE+collaboration"> The LSPE collaboration</a>, <a href="/search/?searchtype=author&query=Addamo%2C+G">G. Addamo</a>, <a href="/search/?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/?searchtype=author&query=Baldini%2C+A+M">A. M. Baldini</a>, <a href="/search/?searchtype=author&query=Battaglia%2C+P+M">P. M. Battaglia</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=Ba%C3%B9%2C+A">A. Ba霉</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/?searchtype=author&query=Biasotti%2C+M">M. Biasotti</a>, <a href="/search/?searchtype=author&query=Boscaleri%2C+A">A. Boscaleri</a>, <a href="/search/?searchtype=author&query=Caccianiga%2C+B">B. Caccianiga</a>, <a href="/search/?searchtype=author&query=Caprioli%2C+S">S. Caprioli</a>, <a href="/search/?searchtype=author&query=Cavaliere%2C+F">F. Cavaliere</a>, <a href="/search/?searchtype=author&query=Cei%2C+F">F. Cei</a>, <a href="/search/?searchtype=author&query=Cleary%2C+K+A">K. A. Cleary</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Coppi%2C+G">G. Coppi</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=Cuttaia%2C+F">F. Cuttaia</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=De+Gasperis%2C+G">G. De Gasperis</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Fafone%2C+V">V. Fafone</a> , et al. (80 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="2008.11049v3-abstract-short" style="display: inline;"> [Abridged] The measurement of the polarization of the Cosmic Microwave Background radiation is one of the current frontiers in cosmology. In particular, the detection of the primordial B-modes, could reveal the presence of gravitational waves in the early Universe. The detection of such component is at the moment the most promising technique to probe the inflationary theory describing the very ear… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11049v3-abstract-full').style.display = 'inline'; document.getElementById('2008.11049v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.11049v3-abstract-full" style="display: none;"> [Abridged] The measurement of the polarization of the Cosmic Microwave Background radiation is one of the current frontiers in cosmology. In particular, the detection of the primordial B-modes, could reveal the presence of gravitational waves in the early Universe. The detection of such component is at the moment the most promising technique to probe the inflationary theory describing the very early evolution of the Universe. We present the updated performance forecast of the Large Scale Polarization Explorer (LSPE), a program dedicated to the measurement of the CMB polarization. LSPE is composed of two instruments: Strip, a radiometer-based telescope on the ground in Tenerife, and SWIPE (Short-Wavelength Instrument for the Polarization Explorer) a bolometer-based instrument designed to fly on a winter arctic stratospheric long-duration balloon. The program is among the few dedicated to observation of the Northern Hemisphere, while most of the international effort is focused into ground-based observation in the Southern Hemisphere. Measurements are currently scheduled in Winter 2021/22 for SWIPE, with a flight duration up to 15 days, and in Summer 2021 with two years observations for Strip. We describe the main features of the two instruments, identifying the most critical aspects of the design, in terms of impact into performance forecast. We estimate the expected sensitivity of each instrument and propagate their combined observing power to the sensitivity to cosmological parameters, including the effect of scanning strategy, component separation, residual foregrounds and partial sky coverage. We also set requirements on the control of the most critical systematic effects and describe techniques to mitigate their impact. LSPE can reach a sensitivity in tensor-to-scalar ratio of $蟽_r<0.01$, and improve constrains on other cosmological parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.11049v3-abstract-full').style.display = 'none'; document.getElementById('2008.11049v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 9 August, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">Submitted to JCAP. Abstract abridged for arXiv submission</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Cosmology and Astroparticle Physics, Volume 2021, August 2021 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2008.10667">arXiv:2008.10667</a> <span> [<a href="https://arxiv.org/pdf/2008.10667">pdf</a>, <a href="https://arxiv.org/format/2008.10667">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/10.1088/1475-7516/2022/04/039">10.1088/1475-7516/2022/04/039 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> QUBIC VI: cryogenic half wave plate rotator, design and performances </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=Mele%2C+L">L. Mele</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=Amico%2C+G">G. Amico</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Coppolecchia%2C+A">A. Coppolecchia</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Grandsire%2C+L">L. Grandsire</a>, <a href="/search/?searchtype=author&query=Hamilton%2C+J+-">J. -Ch. Hamilton</a>, <a href="/search/?searchtype=author&query=Lamagna%2C+L">L. Lamagna</a>, <a href="/search/?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=O%27Sullivan%2C+C">C. O'Sullivan</a>, <a href="/search/?searchtype=author&query=Paiella%2C+A">A. Paiella</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">F. Piacentini</a>, <a href="/search/?searchtype=author&query=Piat%2C+M">M. Piat</a>, <a href="/search/?searchtype=author&query=Pisano%2C+G">G. Pisano</a>, <a href="/search/?searchtype=author&query=Presta%2C+G">G. Presta</a>, <a href="/search/?searchtype=author&query=Tartari%2C+A">A. Tartari</a>, <a href="/search/?searchtype=author&query=Torchinsky%2C+S+A">S. A. Torchinsky</a>, <a href="/search/?searchtype=author&query=Voisin%2C+F">F. Voisin</a>, <a href="/search/?searchtype=author&query=Zannoni%2C+M">M. Zannoni</a>, <a href="/search/?searchtype=author&query=Ade%2C+P">P. Ade</a> , et al. (104 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="2008.10667v2-abstract-short" style="display: inline;"> Inflation Gravity Waves B-Modes polarization detection is the ultimate goal of modern large angular scale cosmic microwave background (CMB) experiments around the world. A big effort is undergoing with the deployment of many ground-based, balloon-borne and satellite experiments using different methods to separate this faint polarized component from the incoming radiation. One of the largely used t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.10667v2-abstract-full').style.display = 'inline'; document.getElementById('2008.10667v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.10667v2-abstract-full" style="display: none;"> Inflation Gravity Waves B-Modes polarization detection is the ultimate goal of modern large angular scale cosmic microwave background (CMB) experiments around the world. A big effort is undergoing with the deployment of many ground-based, balloon-borne and satellite experiments using different methods to separate this faint polarized component from the incoming radiation. One of the largely used technique is the Stokes Polarimetry that uses a rotating half-wave plate (HWP) and a linear polarizer to separate and modulate the polarization components with low residual cross-polarization. This paper describes the QUBIC Stokes Polarimeter highlighting its design features and its performances. A common systematic with these devices is the generation of large spurious signals synchronous with the rotation and proportional to the emissivity of the optical elements. A key feature of the QUBIC Stokes Polarimeter is to operate at cryogenic temperature in order to minimize this unwanted component. Moving efficiently this large optical element at low temperature constitutes a big engineering challenge in order to reduce friction power dissipation. Big attention has been given during the designing phase to minimize the differential thermal contractions between parts. The rotation is driven by a stepper motor placed outside the cryostat to avoid thermal load dissipation at cryogenic temperature. The tests and the results presented in this work show that the QUBIC polarimeter can easily achieve a precision below 0.1掳 in positioning simply using the stepper motor precision and the optical absolute encoder. The rotation induces only few mK of extra power load on the second cryogenic stage (~ 8 K). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.10667v2-abstract-full').style.display = 'none'; document.getElementById('2008.10667v2-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 November, 2020; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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">Part of a series of 8 papers on QUBIC to be submitted to a special issue of 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/2008.10659">arXiv:2008.10659</a> <span> [<a href="https://arxiv.org/pdf/2008.10659">pdf</a>, <a href="https://arxiv.org/format/2008.10659">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2022/04/038">10.1088/1475-7516/2022/04/038 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> QUBIC V: Cryogenic system design and performance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=Chapron%2C+C">C. Chapron</a>, <a href="/search/?searchtype=author&query=Columbro%2C+F">F. Columbro</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Grandsire%2C+L">L. Grandsire</a>, <a href="/search/?searchtype=author&query=Hamilton%2C+J+-">J. -Ch. Hamilton</a>, <a href="/search/?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a>, <a href="/search/?searchtype=author&query=Mele%2C+L">L. Mele</a>, <a href="/search/?searchtype=author&query=May%2C+A">A. May</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=O%27Sullivan%2C+C">C. O'Sullivan</a>, <a href="/search/?searchtype=author&query=Paiella%2C+A">A. Paiella</a>, <a href="/search/?searchtype=author&query=Piacentini%2C+F">F. Piacentini</a>, <a href="/search/?searchtype=author&query=Piat%2C+M">M. Piat</a>, <a href="/search/?searchtype=author&query=Piccirillo%2C+L">L. Piccirillo</a>, <a href="/search/?searchtype=author&query=Presta%2C+G">G. Presta</a>, <a href="/search/?searchtype=author&query=Schillaci%2C+A">A. Schillaci</a>, <a href="/search/?searchtype=author&query=Tartari%2C+A">A. Tartari</a>, <a href="/search/?searchtype=author&query=Thermeau%2C+J+-">J. -P. Thermeau</a>, <a href="/search/?searchtype=author&query=Torchinsky%2C+S+A">S. A. Torchinsky</a>, <a href="/search/?searchtype=author&query=Voisin%2C+F">F. Voisin</a>, <a href="/search/?searchtype=author&query=Zannoni%2C+M">M. Zannoni</a> , et al. (104 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="2008.10659v2-abstract-short" style="display: inline;"> Current experiments aimed at measuring the polarization of the Cosmic Microwave Background (CMB) use cryogenic detector arrays and cold optical systems to boost the mapping speed of the sky survey. For these reasons, large volume cryogenic systems, with large optical windows, working continuously for years, are needed. Here we report on the cryogenic system of the QUBIC (Q and U Bolometric Interfe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.10659v2-abstract-full').style.display = 'inline'; document.getElementById('2008.10659v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.10659v2-abstract-full" style="display: none;"> Current experiments aimed at measuring the polarization of the Cosmic Microwave Background (CMB) use cryogenic detector arrays and cold optical systems to boost the mapping speed of the sky survey. For these reasons, large volume cryogenic systems, with large optical windows, working continuously for years, are needed. Here we report on the cryogenic system of the QUBIC (Q and U Bolometric Interferometer for Cosmology) experiment: we describe its design, fabrication, experimental optimization and validation in the Technological Demonstrator configuration. The QUBIC cryogenic system is based on a large volume cryostat, using two pulse-tube refrigerators to cool at ~3K a large (~1 m^3) volume, heavy (~165kg) instrument, including the cryogenic polarization modulator, the corrugated feedhorns array, and the lower temperature stages; a 4He evaporator cooling at ~1K the interferometer beam combiner; a 3He evaporator cooling at ~0.3K the focal-plane detector arrays. The cryogenic system has been tested and validated for more than 6 months of continuous operation. The detector arrays have reached a stable operating temperature of 0.33K, while the polarization modulator has been operated from a ~10K base temperature. The system has been tilted to cover the boresight elevation range 20 deg -90 deg without significant temperature variations. The instrument is now ready for deployment to the high Argentinean Andes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.10659v2-abstract-full').style.display = 'none'; document.getElementById('2008.10659v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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">This is one of a series of papers on the QUBIC experiment status - This version of the paper matches the one accepted for publication on Journal of Cosmology and Astroparticle 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/2008.10119">arXiv:2008.10119</a> <span> [<a href="https://arxiv.org/pdf/2008.10119">pdf</a>, <a href="https://arxiv.org/format/2008.10119">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/10.1088/1475-7516/2022/04/041">10.1088/1475-7516/2022/04/041 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> QUBIC VIII: Optical design and performance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=O%27Sullivan%2C+C">C. O'Sullivan</a>, <a href="/search/?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/?searchtype=author&query=Amico%2C+G">G. Amico</a>, <a href="/search/?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/?searchtype=author&query=Burke%2C+D">D. Burke</a>, <a href="/search/?searchtype=author&query=Buzi%2C+D">D. Buzi</a>, <a href="/search/?searchtype=author&query=Chapron%2C+C">C. Chapron</a>, <a href="/search/?searchtype=author&query=Conversi%2C+L">L. Conversi</a>, <a href="/search/?searchtype=author&query=D%27Alessandro%2C+G">G. D'Alessandro</a>, <a href="/search/?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/?searchtype=author&query=De+Leo%2C+M">M. De Leo</a>, <a href="/search/?searchtype=author&query=Gayer%2C+D">D. Gayer</a>, <a href="/search/?searchtype=author&query=Grandsire%2C+L">L. Grandsire</a>, <a href="/search/?searchtype=author&query=Hamilton%2C+J+-">J. -Ch. Hamilton</a>, <a href="/search/?searchtype=author&query=Marnieros%2C+S">S. Marnieros</a>, <a href="/search/?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/?searchtype=author&query=Mattei%2C+A">A. Mattei</a>, <a href="/search/?searchtype=author&query=Mennella%2C+A">A. Mennella</a>, <a href="/search/?searchtype=author&query=Mousset%2C+L">L. Mousset</a>, <a href="/search/?searchtype=author&query=Murphy%2C+J+D">J. D. Murphy</a>, <a href="/search/?searchtype=author&query=Pelosi%2C+A">A. Pelosi</a>, <a href="/search/?searchtype=author&query=Perciballi%2C+M">M. Perciballi</a>, <a href="/search/?searchtype=author&query=Piat%2C+M">M. Piat</a>, <a href="/search/?searchtype=author&query=Scully%2C+S">S. Scully</a>, <a href="/search/?searchtype=author&query=Tartari%2C+A">A. Tartari</a> , et al. (104 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="2008.10119v2-abstract-short" style="display: inline;"> The Q and U Bolometric Interferometer for Cosmology (QUBIC) is a ground-based experiment that aims to detect B-mode polarisation anisotropies in the CMB at angular scales around the l=100 recombination peak. Systematic errors make ground-based observations of B modes at millimetre wavelengths very challenging and QUBIC mitigates these problems in a somewhat complementary way to other existing or p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.10119v2-abstract-full').style.display = 'inline'; document.getElementById('2008.10119v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2008.10119v2-abstract-full" style="display: none;"> The Q and U Bolometric Interferometer for Cosmology (QUBIC) is a ground-based experiment that aims to detect B-mode polarisation anisotropies in the CMB at angular scales around the l=100 recombination peak. Systematic errors make ground-based observations of B modes at millimetre wavelengths very challenging and QUBIC mitigates these problems in a somewhat complementary way to other existing or planned experiments using the novel technique of bolometric interferometry. This technique takes advantage of the sensitivity of an imager and the systematic error control of an interferometer. A cold reflective optical combiner superimposes there-emitted beams from 400 aperture feedhorns on two focal planes. A shielding system composedof a fixed groundshield, and a forebaffle that moves with the instrument, limits the impact of local contaminants. The modelling, design, manufacturing and preliminary measurements of the optical components are described in this paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2008.10119v2-abstract-full').style.display = 'none'; document.getElementById('2008.10119v2-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, 2021; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">Part of a series of 8 papers on QUBIC to be published in a special issue of JCAP. 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