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<button class="button is-small is-link">Go</button> </div> </div> </form> </div> </div> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous </a> <a href="/search/?searchtype=author&query=Wollack%2C+E&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Wollack%2C+E&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Wollack%2C+E&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Wollack%2C+E&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Wollack%2C+E&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Wollack%2C+E&start=200" class="pagination-link " aria-label="Page 5" aria-current="page">5 </a> </li> <li><span class="pagination-ellipsis">…</span></li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.14961">arXiv:2502.14961</a> <span> [<a href="https://arxiv.org/pdf/2502.14961">pdf</a>, <a href="https://arxiv.org/format/2502.14961">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> </div> </div> <p class="title is-5 mathjax"> SOFIA/HAWC+ Far-Infrared Polarimetric Large Area CMZ Exploration Survey. V. The Magnetic Field Strength and Morphology in the Sagittarius C Complex </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+R+J">Roy J. Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Par%C3%A9%2C+D+M">Dylan M. Par茅</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+J+A">Jordan A. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Butterfield%2C+N+O">Natalie O. Butterfield</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Karpovich%2C+K">Kaitlyn Karpovich</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="2502.14961v1-abstract-short" style="display: inline;"> We present an analysis of the magnetic field strength and morphology in the Sagittarius C complex (Sgr C; G359.43-0.09) in the Milky Way Galaxy's Central Molecular Zone (CMZ) using the 214 $渭$m polarimetry data acquired with the High-Angular-Resolution Wideband Camera+ (HAWC+) instrument aboard the Stratospheric Observatory for Infrared Astronomy (SOFIA). We use several hundred magnetic field pseu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.14961v1-abstract-full').style.display = 'inline'; document.getElementById('2502.14961v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.14961v1-abstract-full" style="display: none;"> We present an analysis of the magnetic field strength and morphology in the Sagittarius C complex (Sgr C; G359.43-0.09) in the Milky Way Galaxy's Central Molecular Zone (CMZ) using the 214 $渭$m polarimetry data acquired with the High-Angular-Resolution Wideband Camera+ (HAWC+) instrument aboard the Stratospheric Observatory for Infrared Astronomy (SOFIA). We use several hundred magnetic field pseudovectors in the Sgr C region to trace the projected magnetic field orientation within cold molecular gas clouds, and as is the trend throughout the CMZ, they show a higher polarization fraction toward the periphery of the clouds. We conduct a modified Davis-Chandrasekhar-Fermi (DCF) analysis of individual clouds and find that the sky-plane magnetic field strength varies from highly turbulent regions having inferred strengths of $\sim30~渭{\rm G}$ to regions of relatively uniform field orientation having strengths of $\sim 1~{\rm mG}$. The magnetic field orientations suggest that outflows from active star-forming regions, such as the extended green object (EGO) G359.43-0.10 and the protostellar source FIR-4 (G359.43+0.02), cause high turbulence in their vicinity. The magnetic field direction is found to be tangential to the surface of the Sgr C HII region, as well as two [CII] emission cavities around this region. Several other features in the vicinity of Sgr C, especially numerous non-thermal filaments (NTFs) and a diffuse source of X-ray emission towards the southwest of the \hii{} region, are discussed with regard to the observed magnetic field pseudovectors. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.14961v1-abstract-full').style.display = 'none'; document.getElementById('2502.14961v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 18 figures. Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.14473">arXiv:2502.14473</a> <span> [<a href="https://arxiv.org/pdf/2502.14473">pdf</a>, <a href="https://arxiv.org/format/2502.14473">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"> PROTOCALC, A W-band polarized calibrator for CMB Telescopes: application to Simons Observatory and CLASS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Coppi%2C+G">Gabriele Coppi</a>, <a href="/search/astro-ph?searchtype=author&query=Dachlythra%2C+N">Nadia Dachlythra</a>, <a href="/search/astro-ph?searchtype=author&query=Nati%2C+F">Federico Nati</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%BCnner-Planella%2C+R">Rolando D眉nner-Planella</a>, <a href="/search/astro-ph?searchtype=author&query=Adler%2C+A+E">Alexandre E. Adler</a>, <a href="/search/astro-ph?searchtype=author&query=Errard%2C+J">Josquin Errard</a>, <a href="/search/astro-ph?searchtype=author&query=Galitzki%2C+N">Nicholas Galitzki</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yunyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+M+A">Matthew A. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Simon%2C+S+M">Sara M. Simon</a>, <a href="/search/astro-ph?searchtype=author&query=Sang%2C+E+T+K">Ema Tsang King Sang</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+A+V">Amalia Villarrubia Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Zannoni%2C+M">Mario 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="2502.14473v1-abstract-short" style="display: inline;"> Current- and next-generation Cosmic Microwave Background (CMB) experiments will measure polarization anisotropies with unprecedented sensitivities. The need for high precision in these measurements underscores the importance of gaining a comprehensive understanding of instrument properties, with a particular emphasis on the study of the beam properties and, in particular, their polarization charac… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.14473v1-abstract-full').style.display = 'inline'; document.getElementById('2502.14473v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.14473v1-abstract-full" style="display: none;"> Current- and next-generation Cosmic Microwave Background (CMB) experiments will measure polarization anisotropies with unprecedented sensitivities. The need for high precision in these measurements underscores the importance of gaining a comprehensive understanding of instrument properties, with a particular emphasis on the study of the beam properties and, in particular, their polarization characteristics, and the measurement of the polarization angle. In this context, a major challenge lies in the scarcity of millimeter polarized astrophysical sources with sufficient brightness and calibration knowledge to meet the stringent accuracy requirements of future CMB missions. This led to the development of a drone-borne calibration source designed for frequency band centered on approximately 90 GHz band, matching a commonly used channel in ground based CMB measurements. The PROTOtype CALibrator for Cosmology, PROTOCALC, has undergone thorough in-lab testing, and its properties have been subsequently modeled through simulation software integrated into the standard Simons Observatory (SO) analysis pipeline. Moreover, the PROTOCALC system has been tested in the field, having been deployed twice on calibration campaigns with CMB telescopes in the Atacama desert. The data collected constrain the roll angle of the source with a statistical accuracy of $0.045^\circ$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.14473v1-abstract-full').style.display = 'none'; document.getElementById('2502.14473v1-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.08850">arXiv:2502.08850</a> <span> [<a href="https://arxiv.org/pdf/2502.08850">pdf</a>, <a href="https://arxiv.org/format/2502.08850">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> <p class="title is-5 mathjax"> Measurements of the Thermal Sunyaev-Zel'dovich Effect with ACT and DESI Luminous Red Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Liu%2C+R+H">R. Henry Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Schaan%2C+E">Emmanuel Schaan</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+R">Rongpu Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchi%2C+D">Davide Bianchi</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Cole%2C+S">Shaun Cole</a>, <a href="/search/astro-ph?searchtype=author&query=Coulton%2C+W+R">William R. Coulton</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Fanning%2C+K">Kevin Fanning</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">Enrique Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gong%2C+Y">Yulin Gong</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gruen%2C+D">Daniel Gruen</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">Gaston Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Hadzhiyska%2C+B">Boryana Hadzhiyska</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">Klaus Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">Cullan Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">Robert Kehoe</a> , et al. (32 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.08850v1-abstract-short" style="display: inline;"> Cosmic Microwave Background (CMB) photons scatter off the free-electron gas in galaxies and clusters, allowing us to use the CMB as a backlight to probe the gas in and around low-redshift galaxies. The thermal Sunyaev-Zel'dovich effect, sourced by hot electrons in high-density environments, measures the thermal pressure of the target objects, shedding light on halo thermodynamics and galaxy format… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.08850v1-abstract-full').style.display = 'inline'; document.getElementById('2502.08850v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.08850v1-abstract-full" style="display: none;"> Cosmic Microwave Background (CMB) photons scatter off the free-electron gas in galaxies and clusters, allowing us to use the CMB as a backlight to probe the gas in and around low-redshift galaxies. The thermal Sunyaev-Zel'dovich effect, sourced by hot electrons in high-density environments, measures the thermal pressure of the target objects, shedding light on halo thermodynamics and galaxy formation and providing a path toward understanding the baryon distribution around cosmic structures. We use a combination of high-resolution CMB maps from the Atacama Cosmology Telescope (ACT) and photometric luminous red galaxy (LRG) catalogues from the Dark Energy Spectroscopic Instrument (DESI) to measure the thermal Sunyaev-Zel'dovich signal in four redshift bins from $z=0.4$ to $z=1.2$, with a combined detection significance of 19$蟽$ when stacking on the fiducial CMB Compton-$y$ map. We discuss possible sources of contamination, finding that residual dust emission associated with the target galaxies is important and limits current analyses. We discuss several mitigation strategies and quantify the residual modelling uncertainty. This work complements closely-related measurements of the kinematic Sunyaev-Zel'dovich and weak lensing of the same galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.08850v1-abstract-full').style.display = 'none'; document.getElementById('2502.08850v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 13 figures, comments welcome</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.11904">arXiv:2501.11904</a> <span> [<a href="https://arxiv.org/pdf/2501.11904">pdf</a>, <a href="https://arxiv.org/format/2501.11904">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> A Measurement of the Largest-Scale CMB E-mode Polarization with CLASS </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yunyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Eimer%2C+J">Joseph Eimer</a>, <a href="/search/astro-ph?searchtype=author&query=Appel%2C+J">John Appel</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+C">Charles Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Brewer%2C+M">Michael Brewer</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+S+M">Sarah Marie Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bustos%2C+R">Ricardo Bustos</a>, <a href="/search/astro-ph?searchtype=author&query=Chan%2C+C">Carol Chan</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D">David Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+J">Joseph Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Dahal%2C+S">Sumit Dahal</a>, <a href="/search/astro-ph?searchtype=author&query=Datta%2C+R">Rahul Datta</a>, <a href="/search/astro-ph?searchtype=author&query=Couto%2C+J+D">Jullianna Denes Couto</a>, <a href="/search/astro-ph?searchtype=author&query=Denis%2C+K">Kevin Denis</a>, <a href="/search/astro-ph?searchtype=author&query=Dunner%2C+R">Rolando Dunner</a>, <a href="/search/astro-ph?searchtype=author&query=Essinger-Hileman%2C+T">Thomas Essinger-Hileman</a>, <a href="/search/astro-ph?searchtype=author&query=Harrington%2C+K">Kathleen Harrington</a>, <a href="/search/astro-ph?searchtype=author&query=Helson%2C+K">Kyle Helson</a>, <a href="/search/astro-ph?searchtype=author&query=Hubmayr%2C+J">Johannes Hubmayr</a>, <a href="/search/astro-ph?searchtype=author&query=Iuliano%2C+J">Jeffrey Iuliano</a>, <a href="/search/astro-ph?searchtype=author&query=Karakla%2C+J">John Karakla</a>, <a href="/search/astro-ph?searchtype=author&query=Marriage%2C+T">Tobias Marriage</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+N">Nathan Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Perez%2C+C+M">Carolina Morales Perez</a>, <a href="/search/astro-ph?searchtype=author&query=Parker%2C+L">Lucas Parker</a> , et al. (12 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="2501.11904v1-abstract-short" style="display: inline;"> We present measurements of large-scale cosmic microwave background (CMB) E-mode polarization from the Cosmology Large Angular Scale Surveyor (CLASS) 90 GHz data. Using 115 det-yr of observations collected through 2024 with a variable-delay polarization modulator, we achieved a polarization sensitivity of $78\,\mathrm{渭K\,arcmin}$, comparable to Planck at similar frequencies (100 and 143 GHz). The… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.11904v1-abstract-full').style.display = 'inline'; document.getElementById('2501.11904v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.11904v1-abstract-full" style="display: none;"> We present measurements of large-scale cosmic microwave background (CMB) E-mode polarization from the Cosmology Large Angular Scale Surveyor (CLASS) 90 GHz data. Using 115 det-yr of observations collected through 2024 with a variable-delay polarization modulator, we achieved a polarization sensitivity of $78\,\mathrm{渭K\,arcmin}$, comparable to Planck at similar frequencies (100 and 143 GHz). The analysis demonstrates effective mitigation of systematic errors and addresses challenges to large-angular-scale power recovery posed by time-domain filtering in maximum-likelihood map-making. A novel implementation of the pixel-space transfer matrix is introduced, which enables efficient filtering simulations and bias correction in the power spectrum using the quadratic cross-spectrum estimator. Overall, we achieved an unbiased time-domain filtering correction to recover the largest angular scale polarization, with the only power deficit, arising from map-making non-linearity, being characterized as less than $3\%$. Through cross-correlation with Planck, we detected the cosmic reionization at $99.4\%$ significance and measured the reionization optical depth $蟿=0.053^{+0.018}_{-0.019}$, marking the first ground-based attempt at such a measurement. At intermediate angular scales ($\ell>30$), our results, both independently and in cross-correlation with Planck, remain fully consistent with Planck's measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.11904v1-abstract-full').style.display = 'none'; document.getElementById('2501.11904v1-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, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">24 pages, 19 figures, 3 tables; submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.07068">arXiv:2412.07068</a> <span> [<a href="https://arxiv.org/pdf/2412.07068">pdf</a>, <a href="https://arxiv.org/format/2412.07068">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"> The Atacama Cosmology Telescope: Semi-Analytic Covariance Matrices for the DR6 CMB Power Spectra </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Atkins%2C+Z">Zachary Atkins</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zack Li</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+D">David Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">Adriaan J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Giardiello%2C+S">Serena Giardiello</a>, <a href="/search/astro-ph?searchtype=author&query=Herv%C3%ADas-Caimapo%2C+C">Carlos Herv铆as-Caimapo</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+J+C">J. Colin Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Jense%2C+H+T">Hidde T. Jense</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Joshua Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Niemack%2C+M+D">Michael D. Niemack</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+L">Lyman Page</a>, <a href="/search/astro-ph?searchtype=author&query=La+Posta%2C+A">Adrien La Posta</a>, <a href="/search/astro-ph?searchtype=author&query=Louis%2C+T">Thibaut Louis</a>, <a href="/search/astro-ph?searchtype=author&query=Moodley%2C+K">Kavilan Moodley</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+T+W">Thomas W. Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Naess%2C+S">Sigurd Naess</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">Crist贸bal Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</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="2412.07068v1-abstract-short" style="display: inline;"> The Atacama Cosmology Telescope Data Release 6 (ACT DR6) power spectrum is expected to provide state-of-the-art cosmological constraints, with an associated need for precise error modeling. In this paper we design, and evaluate the performance of, an analytic covariance matrix prescription for the DR6 power spectrum that sufficiently accounts for the complicated ACT map properties. We use recent a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07068v1-abstract-full').style.display = 'inline'; document.getElementById('2412.07068v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.07068v1-abstract-full" style="display: none;"> The Atacama Cosmology Telescope Data Release 6 (ACT DR6) power spectrum is expected to provide state-of-the-art cosmological constraints, with an associated need for precise error modeling. In this paper we design, and evaluate the performance of, an analytic covariance matrix prescription for the DR6 power spectrum that sufficiently accounts for the complicated ACT map properties. We use recent advances in the literature to handle sharp features in the signal and noise power spectra, and account for the effect of map-level anisotropies on the covariance matrix. In including inhomogeneous survey depth information, the resulting covariance matrix prescription is structurally similar to that used in the $\textit{Planck}$ Cosmic Microwave Background (CMB) analysis. We quantify the performance of our prescription using comparisons to Monte Carlo simulations, finding better than $3\%$ agreement. This represents an improvement from a simpler, pre-existing prescription, which differs from simulations by $\sim16\%$. We develop a new method to correct the analytic covariance matrix using simulations, after which both prescriptions achieve better than $1\%$ agreement. This correction method outperforms a commonly used alternative, where the analytic correlation matrix is assumed to be accurate when correcting the covariance. Beyond its use for ACT, this framework should be applicable for future high resolution CMB experiments including the Simons Observatory (SO). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07068v1-abstract-full').style.display = 'none'; document.getElementById('2412.07068v1-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 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">22 pages (+11 appendix), 10 figures (+5 appendix), 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/2411.12705">arXiv:2411.12705</a> <span> [<a href="https://arxiv.org/pdf/2411.12705">pdf</a>, <a href="https://arxiv.org/format/2411.12705">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-Efficiency and Low-Noise Detectors for the Upgraded CLASS 90 GHz Focal Plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=N%C3%BA%C3%B1ez%2C+C">Carolina N煤帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Appel%2C+J+W">John W. Appel</a>, <a href="/search/astro-ph?searchtype=author&query=Datta%2C+R">Rahul Datta</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+C+L">Charles L. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Brewer%2C+M+K">Michael K. Brewer</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+S+M">Sarah Marie Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bustos%2C+R">Ricardo Bustos</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Costen%2C+N">Nick Costen</a>, <a href="/search/astro-ph?searchtype=author&query=Couto%2C+J+D">Jullianna Denes Couto</a>, <a href="/search/astro-ph?searchtype=author&query=Dahal%2C+S">Sumit Dahal</a>, <a href="/search/astro-ph?searchtype=author&query=Denis%2C+K+L">Kevin L. Denis</a>, <a href="/search/astro-ph?searchtype=author&query=Eimer%2C+J+R">Joseph R. Eimer</a>, <a href="/search/astro-ph?searchtype=author&query=Essinger-Hileman%2C+T">Thomas Essinger-Hileman</a>, <a href="/search/astro-ph?searchtype=author&query=Iuliano%2C+J">Jeffrey Iuliano</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yunyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Marriage%2C+T+A">Tobias A. Marriage</a>, <a href="/search/astro-ph?searchtype=author&query=Mateo%2C+J">Jennette Mateo</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+M+A">Matthew A. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+R">Rui Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Rostem%2C+K">Karwan Rostem</a>, <a href="/search/astro-ph?searchtype=author&query=Valle%2C+D+A+N">Deniz A. N. Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+D">Duncan Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Zeng%2C+L">Lingzhen Zeng</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="2411.12705v1-abstract-short" style="display: inline;"> We present the in-lab and on-sky performance for the upgraded 90 GHz focal plane of the Cosmology Large Angular Scale Surveyor (CLASS), which had four of its seven detector wafers updated during the austral winter of 2022. The update aimed to improve the transition-edge-sensor (TES) stability and bias range and to realize the high optical efficiency of the sensor design. Modifications included rev… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12705v1-abstract-full').style.display = 'inline'; document.getElementById('2411.12705v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.12705v1-abstract-full" style="display: none;"> We present the in-lab and on-sky performance for the upgraded 90 GHz focal plane of the Cosmology Large Angular Scale Surveyor (CLASS), which had four of its seven detector wafers updated during the austral winter of 2022. The update aimed to improve the transition-edge-sensor (TES) stability and bias range and to realize the high optical efficiency of the sensor design. Modifications included revised circuit terminations, electrical contact between the TES superconductor and the normal metal providing the bulk of the bolometer's heat capacity, and additional filtering on the TES bias lines. The upgrade was successful: 94% of detectors are stable down to 15% of the normal resistance, providing a wide overlapping range of bias voltages for all TESs on a wafer. The median telescope efficiency improved from $0.42^{+0.15}_{-0.22}$ to $0.60^{+0.10}_{-0.32}$ (68% quantiles). For the four upgraded wafers alone, median telescope efficiency increased to $0.65^{+0.06}_{-0.06}$. Given our efficiency estimate for the receiver optics, this telescope efficiency implies a detector efficiency exceeding $0.90$. The overall noise-equivalent temperature of the 90 GHz focal plane improved from 19 $渭$K$\sqrt{s}$ to 11.3 $渭$K$\sqrt{s}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.12705v1-abstract-full').style.display = 'none'; document.getElementById('2411.12705v1-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, 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">18 pages, 10 figures.Submitted to ApJS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.02080">arXiv:2411.02080</a> <span> [<a href="https://arxiv.org/pdf/2411.02080">pdf</a>, <a href="https://arxiv.org/format/2411.02080">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"> Requirements on the gain calibration for LiteBIRD polarisation data with blind component separation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Carralot%2C+F">F. Carralot</a>, <a href="/search/astro-ph?searchtype=author&query=Carones%2C+A">A. Carones</a>, <a href="/search/astro-ph?searchtype=author&query=Krachmalnicoff%2C+N">N. Krachmalnicoff</a>, <a href="/search/astro-ph?searchtype=author&query=Ghigna%2C+T">T. Ghigna</a>, <a href="/search/astro-ph?searchtype=author&query=Novelli%2C+A">A. Novelli</a>, <a href="/search/astro-ph?searchtype=author&query=Pagano%2C+L">L. Pagano</a>, <a href="/search/astro-ph?searchtype=author&query=Piacentini%2C+F">F. Piacentini</a>, <a href="/search/astro-ph?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/astro-ph?searchtype=author&query=Adak%2C+D">D. Adak</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/astro-ph?searchtype=author&query=Azzoni%2C+S">S. Azzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/astro-ph?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/astro-ph?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/astro-ph?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/astro-ph?searchtype=author&query=Basak%2C+S">S. Basak</a>, <a href="/search/astro-ph?searchtype=author&query=Basyrov%2C+A">A. Basyrov</a>, <a href="/search/astro-ph?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolami%2C+M">M. Bortolami</a>, <a href="/search/astro-ph?searchtype=author&query=Brinckmann%2C+T">T. Brinckmann</a>, <a href="/search/astro-ph?searchtype=author&query=Cacciotti%2C+F">F. Cacciotti</a>, <a href="/search/astro-ph?searchtype=author&query=Campeti%2C+P">P. Campeti</a>, <a href="/search/astro-ph?searchtype=author&query=Carinos%2C+E">E. Carinos</a>, <a href="/search/astro-ph?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/2410.19046">arXiv:2410.19046</a> <span> [<a href="https://arxiv.org/pdf/2410.19046">pdf</a>, <a href="https://arxiv.org/format/2410.19046">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: A measurement of galaxy cluster temperatures through relativistic corrections to the thermal Sunyaev-Zeldovich effect </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Coulton%2C+W+R">William R. Coulton</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">Adriaan J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Atkins%2C+Z">Zachary Atkins</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">Elia Stefano Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+H">Hongbo Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Crowley%2C+K+T">Kevin T. Crowley</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M+J">Mark J. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Guan%2C+Y">Yilun Guan</a>, <a href="/search/astro-ph?searchtype=author&query=Herv%C3%ADas-Caimapo%2C+C">Carlos Herv铆as-Caimapo</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+J+C">J. Colin Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">Matt Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Hincks%2C+A+D">Adam D. Hincks</a>, <a href="/search/astro-ph?searchtype=author&query=Kosowsky%2C+A">Arthur Kosowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=van+Marrewijk%2C+J">Joshiwa van Marrewijk</a>, <a href="/search/astro-ph?searchtype=author&query=McCarthy%2C+F">Fiona McCarthy</a>, <a href="/search/astro-ph?searchtype=author&query=Moodley%2C+K">Kavilan Moodley</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">Tony Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Niemack%2C+M+D">Michael D. Niemack</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="2410.19046v1-abstract-short" style="display: inline;"> The high electron temperature in galaxy clusters ($>1\,$keV or $>10^7\,$K) leads to corrections at the level of a few percent in their thermal Sunyaev-Zeldovich effect signatures. Both the size and frequency dependence of these corrections, which are known as relativistic temperature corrections, depend upon the temperature of the objects. In this work we exploit this effect to measure the average… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19046v1-abstract-full').style.display = 'inline'; document.getElementById('2410.19046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.19046v1-abstract-full" style="display: none;"> The high electron temperature in galaxy clusters ($>1\,$keV or $>10^7\,$K) leads to corrections at the level of a few percent in their thermal Sunyaev-Zeldovich effect signatures. Both the size and frequency dependence of these corrections, which are known as relativistic temperature corrections, depend upon the temperature of the objects. In this work we exploit this effect to measure the average temperature of a stack of Compton-$y$ selected clusters. Specifically, we apply the "spectroscopic method" and search for the temperature that best fits the clusters' signal measured at frequencies from 30 to 545 GHz by the Atacama Cosmology Telescope and Planck satellite. We measure the average temperature of clusters detected in the ACT maps to be $8.5\pm 2.4\,$keV, with an additional systematic error of comparable amplitude dominated by passband uncertainty. Upcoming surveys, such as the Simons Observatory and CMB-S4, have the potential to dramatically improve upon these measurements and thereby enable precision studies of cluster temperatures with millimeter observations. The key challenge for future observations will be mitigating instrumental systematic effects, which already limit this analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.19046v1-abstract-full').style.display = 'none'; document.getElementById('2410.19046v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages with 17 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.14404">arXiv:2410.14404</a> <span> [<a href="https://arxiv.org/pdf/2410.14404">pdf</a>, <a href="https://arxiv.org/format/2410.14404">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: a census of bridges between galaxy clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Isopi%2C+G">G. Isopi</a>, <a href="/search/astro-ph?searchtype=author&query=Capalbo%2C+V">V. Capalbo</a>, <a href="/search/astro-ph?searchtype=author&query=Hincks%2C+A+D">A. D. Hincks</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mascolo%2C+L">L. Di Mascolo</a>, <a href="/search/astro-ph?searchtype=author&query=Barbavara%2C+E">E. Barbavara</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Cui%2C+W">W. Cui</a>, <a href="/search/astro-ph?searchtype=author&query=Coulton%2C+W+R">W. R. Coulton</a>, <a href="/search/astro-ph?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">M. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dolag%2C+K">K. Dolag</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">J. Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Fabjan%2C+D">D. Fabjan</a>, <a href="/search/astro-ph?searchtype=author&query=Ferragamo%2C+A">A. Ferragamo</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+A+S">A. S. Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Guan%2C+Y">Y. Guan</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">M. Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">M. Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+J+P">J. P. Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Lokken%2C+M">M. Lokken</a>, <a href="/search/astro-ph?searchtype=author&query=van+Marrewijk%2C+J">J. van Marrewijk</a>, <a href="/search/astro-ph?searchtype=author&query=Moodley%2C+K">K. Moodley</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Orlowski-Scherer%2C+J">J. Orlowski-Scherer</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.14404v1-abstract-short" style="display: inline;"> According to CMB measurements, baryonic matter constitutes about $5\%$ of the mass-energy density of the universe. A significant population of these baryons, for a long time referred to as `missing', resides in a low density, warm-hot intergalactic medium (WHIM) outside galaxy clusters, tracing the ``cosmic web'', a network of large scale dark matter filaments. Various studies have detected this i… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.14404v1-abstract-full').style.display = 'inline'; document.getElementById('2410.14404v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.14404v1-abstract-full" style="display: none;"> According to CMB measurements, baryonic matter constitutes about $5\%$ of the mass-energy density of the universe. A significant population of these baryons, for a long time referred to as `missing', resides in a low density, warm-hot intergalactic medium (WHIM) outside galaxy clusters, tracing the ``cosmic web'', a network of large scale dark matter filaments. Various studies have detected this inter-cluster gas, both by stacking and by observing individual filaments in compact, massive systems. In this paper, we study short filaments (< 10 Mpc) connecting massive clusters ($M_{500} \approx 3\times 10^{14} M_{\odot}$) detected by the Atacama Cosmology Telescope (ACT) using the scattering of CMB light off the ionised gas, a phenomenon known as the thermal Sunyaev-Zeldovich (tSZ) effect. The first part of this work is a search for suitable candidates for high resolution follow-up tSZ observations. We identify four cluster pairs with an intercluster signal above the noise floor (S/N $>$ 2), including two with a tentative $>2蟽$ statistical significance for an intercluster bridge from the ACT data alone. In the second part of this work, starting from the same cluster sample, we directly stack on ${\sim}100$ cluster pairs and observe an excess SZ signal between the stacked clusters of $y=(7.2^{+2.3}_{-2.5})\times 10^{-7}$ with a significance of $3.3蟽$. It is the first tSZ measurement of hot gas between clusters in this range of masses at moderate redshift ($\langle z\rangle\approx 0.5$). We compare this to the signal from simulated cluster pairs with similar redshifts and separations in the THE300 and MAGNETICUM Pathfinder cosmological simulations and find broad consistency. Additionally, we show that our measurement is consistent with scaling relations between filament parameters and mass of the embedded halos identified in simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.14404v1-abstract-full').style.display = 'none'; document.getElementById('2410.14404v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">37 pages, 17 images</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 85A40 (Primary) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.13064">arXiv:2410.13064</a> <span> [<a href="https://arxiv.org/pdf/2410.13064">pdf</a>, <a href="https://arxiv.org/format/2410.13064">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 Atacama Cosmology Telescope: Quantifying Atmospheric Emission above Cerro Toco </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Morris%2C+T+W">Thomas W. Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E">Elia Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bustos%2C+R">Ricardo Bustos</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">Adriaan J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%BCnner%2C+R">Rolando D眉nner</a>, <a href="/search/astro-ph?searchtype=author&query=Halpern%2C+M">Mark Halpern</a>, <a href="/search/astro-ph?searchtype=author&query=Guan%2C+Y">Yilun Guan</a>, <a href="/search/astro-ph?searchtype=author&query=van+Marrewijk%2C+J">Joshiwa van Marrewijk</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">Tony Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Naess%2C+S">Sigurd Naess</a>, <a href="/search/astro-ph?searchtype=author&query=Niemack%2C+M+D">Michael D. Niemack</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+L+A">Lyman A. Page</a>, <a href="/search/astro-ph?searchtype=author&query=Partridge%2C+B">Bruce Partridge</a>, <a href="/search/astro-ph?searchtype=author&query=Puddu%2C+R">Roberto Puddu</a>, <a href="/search/astro-ph?searchtype=author&query=Salatino%2C+M">Maria Salatino</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">Crist贸bal Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+Y">Yuhan Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</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="2410.13064v1-abstract-short" style="display: inline;"> At frequencies below 1\,Hz, fluctuations in atmospheric emission in the Chajnantor region in northern Chile are the primary source of interference for bolometric millimeter-wave observations. This paper focuses on the statistics of these fluctuations using measurements from the Atacama Cosmology Telescope (ACT) and the Atacama Pathfinder Experiment (APEX) water vapor radiometer. After introducing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.13064v1-abstract-full').style.display = 'inline'; document.getElementById('2410.13064v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.13064v1-abstract-full" style="display: none;"> At frequencies below 1\,Hz, fluctuations in atmospheric emission in the Chajnantor region in northern Chile are the primary source of interference for bolometric millimeter-wave observations. This paper focuses on the statistics of these fluctuations using measurements from the Atacama Cosmology Telescope (ACT) and the Atacama Pathfinder Experiment (APEX) water vapor radiometer. After introducing a method for separating atmospheric effects from other systematic effects, we present a direct measurement of the temporal outer scale of turbulence of $蟿_0\approx50$s corresponding to a spatial scale of $L_0\approx500$m. At smaller scales, the fluctuations are well described by the Kolmogorov 2/3 power law until, at yet smaller scales, the effects of beam smearing become important. As a part of this study, we present measurements of the atmosphere by the APEX radiometer over 20 years, focused on fluctuations in precipitable water vapor (PWV). We find that the 30-minute mean of the total PWV is not in general a robust estimator of the level of fluctuations. We show that the microwave frequency spectrum of these fluctuations is in good agreement with predictions by the \texttt{am} code for bands above 90~GHz. We then show that the variance of fluctuations in ACT's mm-wave bands correlates with the variance of fluctuations in PWV measured by APEX, even though the observatories are 6\,km apart and observe different lines of sight. We find that ACT's atmosphere-determined optical efficiencies are consistent with previous planet-based results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.13064v1-abstract-full').style.display = 'none'; document.getElementById('2410.13064v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages plus appendix, 17 figures. Submitted to PRD</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.10808">arXiv:2410.10808</a> <span> [<a href="https://arxiv.org/pdf/2410.10808">pdf</a>, <a href="https://arxiv.org/format/2410.10808">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope DR6 and DESI: Structure growth measurements from the cross-correlation of DESI Legacy Imaging galaxies and CMB lensing from ACT DR6 and Planck PR4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Qu%2C+F+J">Frank J. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Hang%2C+Q">Qianjun Hang</a>, <a href="/search/astro-ph?searchtype=author&query=Farren%2C+G">Gerrit Farren</a>, <a href="/search/astro-ph?searchtype=author&query=Bolliet%2C+B">Boris Bolliet</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Alam%2C+S">Shadab Alam</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+Y">Yan-Chuan Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M+J">Mark J. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">Peter Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Embil-Villagra%2C+C">Carmen Embil-Villagra</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">Enrique Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gluscevic%2C+V">Vera Gluscevic</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G+A">Satya Gontcho A Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">Gaston Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Howlett%2C+C">Cullan Howlett</a>, <a href="/search/astro-ph?searchtype=author&query=Kehoe%2C+R">Robert Kehoe</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Joshua Kim</a> , et al. (29 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.10808v1-abstract-short" style="display: inline;"> We measure the growth of cosmic density fluctuations on large scales and across the redshift range $0.3<z<0.8$ through the cross-correlation of the ACT DR6 CMB lensing map and galaxies from the DESI Legacy Survey, using three galaxy samples spanning the redshifts of $0.3 \lesssim z \lesssim 0.45$, $0.45 \lesssim z \lesssim0.6$, $0.6 \lesssim z \lesssim 0.8$. We adopt a scale cut where non-linear e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10808v1-abstract-full').style.display = 'inline'; document.getElementById('2410.10808v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.10808v1-abstract-full" style="display: none;"> We measure the growth of cosmic density fluctuations on large scales and across the redshift range $0.3<z<0.8$ through the cross-correlation of the ACT DR6 CMB lensing map and galaxies from the DESI Legacy Survey, using three galaxy samples spanning the redshifts of $0.3 \lesssim z \lesssim 0.45$, $0.45 \lesssim z \lesssim0.6$, $0.6 \lesssim z \lesssim 0.8$. We adopt a scale cut where non-linear effects are negligible, so that the cosmological constraints are derived from the linear regime. We determine the amplitude of matter fluctuations over all three redshift bins using ACT data alone to be $S_8\equiv蟽_8(惟_m/0.3)^{0.5}=0.772\pm0.040$ in a joint analysis combining the three redshift bins and ACT lensing alone. Using a combination of ACT and \textit{Planck} data we obtain $S_8=0.765\pm0.032$. The lowest redshift bin used is the least constraining and exhibits a $\sim2蟽$ tension with the other redshift bins; thus we also report constraints excluding the first redshift bin, giving $S_8=0.785\pm0.033$ for the combination of ACT and \textit{Planck}. This result is in excellent agreement at the $0.3蟽$ level with measurements from galaxy lensing, but is $1.8蟽$ lower than predictions based on \textit{Planck} primary CMB data. Understanding whether this hint of discrepancy in the growth of structure at low redshifts arises from a fluctuation, from systematics in data, or from new physics, is a high priority for forthcoming CMB lensing and galaxy cross-correlation analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10808v1-abstract-full').style.display = 'none'; document.getElementById('2410.10808v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">27+9 pages, 20+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/2410.10597">arXiv:2410.10597</a> <span> [<a href="https://arxiv.org/pdf/2410.10597">pdf</a>, <a href="https://arxiv.org/format/2410.10597">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> </div> </div> <p class="title is-5 mathjax"> SOFIA/HAWC+ Far-Infrared Polarimetric Large-Area CMZ Exploration Survey. IV. Relative Magnetic Field Orientation Throughout the CMZ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Par%C3%A9%2C+D+M">Dylan M. Par茅</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Karpovich%2C+K">Kaitlyn Karpovich</a>, <a href="/search/astro-ph?searchtype=author&query=Butterfield%2C+N+O">Natalie O. Butterfield</a>, <a href="/search/astro-ph?searchtype=author&query=Iulliano%2C+J+I">Jeffrey Inara Iulliano</a>, <a href="/search/astro-ph?searchtype=author&query=Pan%2C+X">Xing Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Q">Qizhou Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Nilsson%2C+M">Matthilda Nilsson</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+R+J">Roy J. Zhao</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="2410.10597v2-abstract-short" style="display: inline;"> The nature of the magnetic field structure throughout the Galactic Center (GC) has long been of interest. The recent Far-InfraREd Polarimetric Large-Area CMZ Exploration (FIREPLACE) Survey reveals preliminary connections between the seemingly distinct vertical and horizontal magnetic field distributions previously observed in the GC. We use the statistical techniques of the Histogram of Relative O… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10597v2-abstract-full').style.display = 'inline'; document.getElementById('2410.10597v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.10597v2-abstract-full" style="display: none;"> The nature of the magnetic field structure throughout the Galactic Center (GC) has long been of interest. The recent Far-InfraREd Polarimetric Large-Area CMZ Exploration (FIREPLACE) Survey reveals preliminary connections between the seemingly distinct vertical and horizontal magnetic field distributions previously observed in the GC. We use the statistical techniques of the Histogram of Relative Orientation (HRO) and the Projected Rayleigh Statistic (PRS) to assess whether the CMZ magnetic field preferentially aligns with the structure of the CMZ molecular clouds or the morphology of the non-thermal emission of the GC NTF population. We find that there is a range of magnetic field orientations throughout the population of CMZ molecular clouds, ranging from parallel to perpendicular orientation. We posit these orientations depend on the prevalence of gravitational shear in the GC in contrast with what is observed in Galactic Disk star-forming regions. We also compare the magnetic field orientation from dust polarimetry with individual prominent NTFs, finding a preferred perpendicular relative orientation. This perpendicular orientation indicates that the vertical field component found in the FIREPLACE observations is not spatially confined to the NTFs, providing evidence for a more pervasive vertical field in the GC. From dynamical arguments, we estimate an upper limit on the magnetic field strength for this vertical field, finding B less than or equal to 4 mG. A field close to this upper limit would indicate that the NTFs are not local enhancements of a weaker background field and that the locations of the NTFs depend on proximity to sites of cosmic ray production. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.10597v2-abstract-full').style.display = 'none'; document.getElementById('2410.10597v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.06229">arXiv:2410.06229</a> <span> [<a href="https://arxiv.org/pdf/2410.06229">pdf</a>, <a href="https://arxiv.org/format/2410.06229">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: Large-scale velocity reconstruction with the kinematic Sunyaev--Zel'dovich effect and DESI LRGs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McCarthy%2C+F">Fiona McCarthy</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bean%2C+R">Rachel Bean</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+H">Hongbo Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Coulton%2C+W+R">William R. Coulton</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M+J">Mark J. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Gluscevic%2C+V">Vera Gluscevic</a>, <a href="/search/astro-ph?searchtype=author&query=Guan%2C+Y">Yilun Guan</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+J+C">J. Colin Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+M+C">Matthew C. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Kusiak%2C+A">Aleksandra Kusiak</a>, <a href="/search/astro-ph?searchtype=author&query=Lagu%C3%AB%2C+A">Alex Lagu毛</a>, <a href="/search/astro-ph?searchtype=author&query=MacCrann%2C+N">Niall MacCrann</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Moodley%2C+K">Kavilan Moodley</a>, <a href="/search/astro-ph?searchtype=author&query=Naess%2C+S">Sigurd Naess</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+F+J">Frank J. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Guachalla%2C+B+R">Bernardita Ried Guachalla</a>, <a href="/search/astro-ph?searchtype=author&query=Sehgal%2C+N">Neelima Sehgal</a>, <a href="/search/astro-ph?searchtype=author&query=Sherwin%2C+B+D">Blake D. Sherwin</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">Crist贸bal Sif贸n</a> , et al. (5 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.06229v1-abstract-short" style="display: inline;"> The kinematic Sunyaev--Zel'dovich (kSZ) effect induces a non-zero density-density-temperature bispectrum, which we can use to reconstruct the large-scale velocity field from a combination of cosmic microwave background (CMB) and galaxy density measurements, in a procedure known as ``kSZ velocity reconstruction''. This method has been forecast to constrain large-scale modes with future galaxy and C… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.06229v1-abstract-full').style.display = 'inline'; document.getElementById('2410.06229v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.06229v1-abstract-full" style="display: none;"> The kinematic Sunyaev--Zel'dovich (kSZ) effect induces a non-zero density-density-temperature bispectrum, which we can use to reconstruct the large-scale velocity field from a combination of cosmic microwave background (CMB) and galaxy density measurements, in a procedure known as ``kSZ velocity reconstruction''. This method has been forecast to constrain large-scale modes with future galaxy and CMB surveys, improving their measurement beyond what is possible with the galaxy surveys alone. Such measurements will enable tighter constraints on large-scale signals such as primordial non-Gaussianity, deviations from homogeneity, and modified gravity. In this work, we demonstrate a statistically significant measurement of kSZ velocity reconstruction for the first time, by applying quadratic estimators to the combination of the ACT DR6 CMB+kSZ map and the DESI LRG galaxies (with photometric redshifts) in order to reconstruct the velocity field. We do so using a formalism appropriate for the 2-dimensional projected galaxy fields that we use, which naturally incorporates the curved-sky effects important on the largest scales. We find evidence for the signal by cross-correlating with an external estimate of the velocity field from the spectroscopic BOSS survey and rejecting the null (no-kSZ) hypothesis at $3.8蟽$. Our work presents a first step towards the use of this observable for cosmological analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.06229v1-abstract-full').style.display = 'none'; document.getElementById('2410.06229v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages (main)+5 pages (Appendix); 13 figures (main) + 8 figures (appendix)</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.00826">arXiv:2410.00826</a> <span> [<a href="https://arxiv.org/pdf/2410.00826">pdf</a>, <a href="https://arxiv.org/format/2410.00826">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="Applied Physics">physics.app-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Optics">physics.optics</span> </div> </div> <p class="title is-5 mathjax"> Metal-Mesh Linear Variable Filter for Far-Infrared Wavelengths </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Perido%2C+J">Joanna Perido</a>, <a href="/search/astro-ph?searchtype=author&query=Denis%2C+K">Kevin Denis</a>, <a href="/search/astro-ph?searchtype=author&query=Clancy%2C+S+O">Sean O. Clancy</a>, <a href="/search/astro-ph?searchtype=author&query=Cothard%2C+N+F">Nicholas F. Cothard</a>, <a href="/search/astro-ph?searchtype=author&query=Day%2C+P+K">Peter K. Day</a>, <a href="/search/astro-ph?searchtype=author&query=Glenn%2C+J">Jason Glenn</a>, <a href="/search/astro-ph?searchtype=author&query=Leduc%2C+H">Henry Leduc</a>, <a href="/search/astro-ph?searchtype=author&query=Quijada%2C+M">Manuel Quijada</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+J">Jessica Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E">Edward Wollack</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="2410.00826v1-abstract-short" style="display: inline;"> Future far-infrared (IR) observatories require compact and cost efficient optical linear variable bandpass filters (LVBFs) to define their instrument spectral bands. We have designed novel far-IR LVBFs that consist of metal-mesh bandpass filters comprised of a gold film with cross-slots of varying sizes along a silicon (Si) substrate with anti-reflection (AR) coatings. We present our work on the s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00826v1-abstract-full').style.display = 'inline'; document.getElementById('2410.00826v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.00826v1-abstract-full" style="display: none;"> Future far-infrared (IR) observatories require compact and cost efficient optical linear variable bandpass filters (LVBFs) to define their instrument spectral bands. We have designed novel far-IR LVBFs that consist of metal-mesh bandpass filters comprised of a gold film with cross-slots of varying sizes along a silicon (Si) substrate with anti-reflection (AR) coatings. We present our work on the simulated and measured transmission of non-AR coated and AR coated LVBFs for bandpass peaks from wavelengths of 24 to 36 $渭$m with a resolving power ($R=位_0/螖位$) of R$\approx$6 for non-AR coated LVBFs and R$\approx$4 for AR coated LVBFs. We also present a method to decrease the effects of out-of-band high frequency transmission exhibited by metal-mesh filters by depositing a thin layer of hydrogenated amorphous silicon (a-Si:H) on the metal-mesh of the LVBF. We have fabricated and measured the LVBFs at room temperature and cryogenic temperatures (5 K). We measure a high peak transmission of $\sim$80-90 \% for the AR coated LVBF at 5 K and demonstrate that the a-Si:H LVBF is a promising method to address out-of-band high frequency transmission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.00826v1-abstract-full').style.display = 'none'; document.getElementById('2410.00826v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages, 10 figures, accepted to Applied Optics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.08429">arXiv:2409.08429</a> <span> [<a href="https://arxiv.org/pdf/2409.08429">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: Systematic Transient Search of Single Observation Maps </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+E+K">Emily K. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yaqiong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Naess%2C+S">Sigurd Naess</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+S+E">Susan E. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">Mark Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Gallardo%2C+P+A">P. A. Gallardo</a>, <a href="/search/astro-ph?searchtype=author&query=Guan%2C+Y">Yilun Guan</a>, <a href="/search/astro-ph?searchtype=author&query=Foster%2C+A">Allen Foster</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselfield%2C+M">Matthew Hasselfield</a>, <a href="/search/astro-ph?searchtype=author&query=Herv%C3%ADas-Caimapo%2C+C">Carlos Herv铆as-Caimapo</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">Matt Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Hincks%2C+A+D">Adam D. Hincks</a>, <a href="/search/astro-ph?searchtype=author&query=Ho%2C+A+Y+Q">Anna Y. Q. Ho</a>, <a href="/search/astro-ph?searchtype=author&query=Hood%2C+J+C">John C. Hood II</a>, <a href="/search/astro-ph?searchtype=author&query=Huffenberger%2C+K+M">Kevin M. Huffenberger</a>, <a href="/search/astro-ph?searchtype=author&query=Kosowsky%2C+A">Arthur Kosowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Niemack%2C+M+D">Michael D. Niemack</a>, <a href="/search/astro-ph?searchtype=author&query=Orlowski-Scherer%2C+J">John Orlowski-Scherer</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+L">Lyman Page</a>, <a href="/search/astro-ph?searchtype=author&query=Partridge%2C+B">Bruce Partridge</a>, <a href="/search/astro-ph?searchtype=author&query=Salatino%2C+M">Maria Salatino</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">Crist贸bal Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Staggs%2C+S+T">Suzanne T. Staggs</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="2409.08429v1-abstract-short" style="display: inline;"> We conduct a systematic search for astrophysical transients using data from the Atacama Cosmology Telescope (ACT). The data were taken from 2017 to 2022 in three frequency bands spanning 77 GHz to 277 GHz. In this paper we present a pipeline for transient detection using single observation maps where each pixel of a map contains one observation with an integration time of approximately four minute… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.08429v1-abstract-full').style.display = 'inline'; document.getElementById('2409.08429v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.08429v1-abstract-full" style="display: none;"> We conduct a systematic search for astrophysical transients using data from the Atacama Cosmology Telescope (ACT). The data were taken from 2017 to 2022 in three frequency bands spanning 77 GHz to 277 GHz. In this paper we present a pipeline for transient detection using single observation maps where each pixel of a map contains one observation with an integration time of approximately four minutes. We find 34 transient events at 27 unique locations. All but two of the transients are associated with Galactic stars and exhibit a wide range of properties. We also detect an event coincident with the classical nova, YZ Ret and one event consistent with a flaring active galactic nucleus. We notably do not detect any reverse shock emission from gamma ray bursts, a non-detection which is in tension with current models. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.08429v1-abstract-full').style.display = 'none'; document.getElementById('2409.08429v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 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, 10 figures, 10 tables. First and second author share equal contributions. Article and accompanying data submitted to ApJ. Data tables will be made available upon publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.04535">arXiv:2409.04535</a> <span> [<a href="https://arxiv.org/pdf/2409.04535">pdf</a>, <a href="https://arxiv.org/format/2409.04535">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"> Superclustering with the Atacama Cosmology Telescope and Dark Energy Survey: II. Anisotropic large-scale coherence in hot gas, galaxies, and dark matter </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lokken%2C+M">M. Lokken</a>, <a href="/search/astro-ph?searchtype=author&query=van+Engelen%2C+A">A. van Engelen</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S+S">S. S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Anbajagane%2C+D">D. Anbajagane</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Baxter%2C+E">E. Baxter</a>, <a href="/search/astro-ph?searchtype=author&query=Blazek%2C+J">J. Blazek</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">E. Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Costanzi%2C+M">M. Costanzi</a>, <a href="/search/astro-ph?searchtype=author&query=da+Costa%2C+L+N">L. N. da Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Coulton%2C+W+R">W. R. Coulton</a>, <a href="/search/astro-ph?searchtype=author&query=De+Vicente%2C+J">J. De Vicente</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Doux%2C+C">C. Doux</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">A. J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">J. Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+Z">Z. Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+S">S. Everett</a> , et al. (51 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="2409.04535v1-abstract-short" style="display: inline;"> Statistics that capture the directional dependence of the baryon distribution in the cosmic web enable unique tests of cosmology and astrophysical feedback. We use constrained oriented stacking of thermal Sunyaev-Zel'dovich (tSZ) maps to measure the anisotropic distribution of hot gas $2.5-40$ Mpc away from galaxy clusters embedded in massive filaments and superclusters. The cluster selection and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.04535v1-abstract-full').style.display = 'inline'; document.getElementById('2409.04535v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.04535v1-abstract-full" style="display: none;"> Statistics that capture the directional dependence of the baryon distribution in the cosmic web enable unique tests of cosmology and astrophysical feedback. We use constrained oriented stacking of thermal Sunyaev-Zel'dovich (tSZ) maps to measure the anisotropic distribution of hot gas $2.5-40$ Mpc away from galaxy clusters embedded in massive filaments and superclusters. The cluster selection and orientation (at a scale of $\sim15$ Mpc) use Dark Energy Survey (DES) Year 3 data, while expanded tSZ maps from the Atacama Cosmology Telescope Data Release 6 enable a $\sim3\times$ more significant measurement of the extended gas compared to the technique's proof-of-concept. Decomposing stacks into cosine multipoles of order $m$, we detect a dipole ($m=1$) and quadrupole ($m=2$) at $8-10蟽$, as well as evidence for $m=4$ signal at up to $6蟽$, indicating sensitivity to late-time non-Gaussianity. We compare to the Cardinal simulations with spherical gas models pasted onto dark matter halos. The fiducial tSZ data can discriminate between two models that deplete pressure differently in low-mass halos (mimicking astrophysical feedback), preferring higher average pressure in extended structures. However, uncertainty in the amount of cosmic infrared background contamination reduces the constraining power. Additionally, we apply the technique to DES galaxy density and weak lensing to study for the first time their oriented relationships with tSZ. In the tSZ-to-lensing relation, averaged on 7.5 Mpc (transverse) scales, we observe dependence on redshift but not shape or radial distance. Thus, on large scales, the superclustering of gas pressure, galaxies, and total matter is coherent in shape and extent. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.04535v1-abstract-full').style.display = 'none'; document.getElementById('2409.04535v1-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 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">45 pages, 18 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.02847">arXiv:2409.02847</a> <span> [<a href="https://arxiv.org/pdf/2409.02847">pdf</a>, <a href="https://arxiv.org/format/2409.02847">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/10.1117/12.3018577">10.1117/12.3018577 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Superfluid-tight cryogenic receiver with continuous sub-Kelvin cooling for EXCLAIM </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dahal%2C+S">Sumit Dahal</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">Peter A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+C+J">Christopher J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Barlis%2C+A">Alyssa Barlis</a>, <a href="/search/astro-ph?searchtype=author&query=Barrentine%2C+E+M">Emily M. Barrentine</a>, <a href="/search/astro-ph?searchtype=author&query=Beeman%2C+J+W">Jeffrey W. Beeman</a>, <a href="/search/astro-ph?searchtype=author&query=Bellis%2C+N">Nicholas Bellis</a>, <a href="/search/astro-ph?searchtype=author&query=Bolatto%2C+A+D">Alberto D. Bolatto</a>, <a href="/search/astro-ph?searchtype=author&query=Braianova%2C+V">Victoria Braianova</a>, <a href="/search/astro-ph?searchtype=author&query=Breysse%2C+P+C">Patrick C. Breysse</a>, <a href="/search/astro-ph?searchtype=author&query=Bulcha%2C+B+T">Berhanu T. Bulcha</a>, <a href="/search/astro-ph?searchtype=author&query=Cataldo%2C+G">Giuseppe Cataldo</a>, <a href="/search/astro-ph?searchtype=author&query=Colazo%2C+F+A">Felipe A. Colazo</a>, <a href="/search/astro-ph?searchtype=author&query=Chevres-Fernandez%2C+L">Lee-Roger Chevres-Fernandez</a>, <a href="/search/astro-ph?searchtype=author&query=Cho%2C+C">Chullhee Cho</a>, <a href="/search/astro-ph?searchtype=author&query=Chmaytelli%2C+D+S">Danny S. Chmaytelli</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J+A">Jake A. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Costen%2C+N+P">Nicholas P. Costen</a>, <a href="/search/astro-ph?searchtype=author&query=Cursey%2C+P+W">Paul W. Cursey</a>, <a href="/search/astro-ph?searchtype=author&query=Ehsan%2C+N">Negar Ehsan</a>, <a href="/search/astro-ph?searchtype=author&query=Essinger-Hileman%2C+T+M">Thomas M. Essinger-Hileman</a>, <a href="/search/astro-ph?searchtype=author&query=Glenn%2C+J">Jason Glenn</a>, <a href="/search/astro-ph?searchtype=author&query=Golec%2C+J+E">Joseph E. Golec</a>, <a href="/search/astro-ph?searchtype=author&query=Hays-Wehle%2C+J+P">James P. Hays-Wehle</a>, <a href="/search/astro-ph?searchtype=author&query=Hess%2C+L+A">Larry A. Hess</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="2409.02847v1-abstract-short" style="display: inline;"> The EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) is a balloon-borne telescope designed to survey star formation over cosmological time scales using intensity mapping in the 420 - 540 GHz frequency range. EXCLAIM uses a fully cryogenic telescope coupled to six on-chip spectrometers featuring kinetic inductance detectors (KIDs) to achieve high sensitivity, allowing for fast in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02847v1-abstract-full').style.display = 'inline'; document.getElementById('2409.02847v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.02847v1-abstract-full" style="display: none;"> The EXperiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) is a balloon-borne telescope designed to survey star formation over cosmological time scales using intensity mapping in the 420 - 540 GHz frequency range. EXCLAIM uses a fully cryogenic telescope coupled to six on-chip spectrometers featuring kinetic inductance detectors (KIDs) to achieve high sensitivity, allowing for fast integration in dark atmospheric windows. The telescope receiver is cooled to $\approx$ 1.7 K by immersion in a superfluid helium bath and enclosed in a superfluid-tight shell with a meta-material anti-reflection coated silicon window. In addition to the optics and the spectrometer package, the receiver contains the magnetic shielding, the cryogenic segment of the spectrometer readout, and the sub-Kelvin cooling system. A three-stage continuous adiabatic demagnetization refrigerator (CADR) keeps the detectors at 100 mK while a $^4$He sorption cooler provides a 900 mK thermal intercept for mechanical suspensions and coaxial cables. We present the design of the EXCLAIM receiver and report on the flight-like testing of major receiver components, including the superfluid-tight receiver window and the sub-Kelvin coolers. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02847v1-abstract-full').style.display = 'none'; document.getElementById('2409.02847v1-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 7 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proc. SPIE 13102, Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XII, 131022I (16 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/2409.02109">arXiv:2409.02109</a> <span> [<a href="https://arxiv.org/pdf/2409.02109">pdf</a>, <a href="https://arxiv.org/format/2409.02109">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: Multi-probe cosmology with unWISE galaxies and ACT DR6 CMB lensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Farren%2C+G+S">Gerrit S. Farren</a>, <a href="/search/astro-ph?searchtype=author&query=Krolewski%2C+A">Alex Krolewski</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+F+J">Frank J. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Villagra%2C+C+E">Carmen Embil Villagra</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+J+C">J. Colin Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Joshua Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Moodley%2C+K">Kavilan Moodley</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+L+A">Lyman A. Page</a>, <a href="/search/astro-ph?searchtype=author&query=Partridge%2C+B">Bruce Partridge</a>, <a href="/search/astro-ph?searchtype=author&query=Sehgal%2C+N">Neelima Sehgal</a>, <a href="/search/astro-ph?searchtype=author&query=Sherwin%2C+B+D">Blake D. Sherwin</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">Crist贸bal Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Staggs%2C+S+T">Suzanne T. Staggs</a>, <a href="/search/astro-ph?searchtype=author&query=Van+Engelen%2C+A">Alexander Van Engelen</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</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="2409.02109v2-abstract-short" style="display: inline;"> We present a joint analysis of the CMB lensing power spectra measured from the Data Release 6 of the Atacama Cosmology Telescope and Planck PR4, cross-correlations between the ACT and Planck lensing reconstruction and galaxy clustering from unWISE, and the unWISE clustering auto-spectrum. We obtain 1.5% constraints on the matter density fluctuations at late times parametrised by the best constrain… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02109v2-abstract-full').style.display = 'inline'; document.getElementById('2409.02109v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.02109v2-abstract-full" style="display: none;"> We present a joint analysis of the CMB lensing power spectra measured from the Data Release 6 of the Atacama Cosmology Telescope and Planck PR4, cross-correlations between the ACT and Planck lensing reconstruction and galaxy clustering from unWISE, and the unWISE clustering auto-spectrum. We obtain 1.5% constraints on the matter density fluctuations at late times parametrised by the best constrained parameter combination $S_8^{\rm 3x2pt}\equiv蟽_8 (惟_m/0.3)^{0.4}=0.815\pm0.012$. The commonly used $S_8\equiv蟽_8 (惟_m/0.3)^{0.5}$ parameter is constrained to $S_8=0.816\pm0.015$. In combination with baryon acoustic oscillation (BAO) measurements we find $蟽_8=0.815\pm 0.012$. We also present sound-horizon-independent estimates of the present day Hubble rate of $H_0=66.4^{+3.2}_{-3.7} \,\mathrm{km}\,\mathrm{s}^{-1}\mathrm{Mpc}^{-1}$ from our large scale structure data alone and $H_0=64.3^{+2.1}_{-2.4}\,\mathrm{km}\,\mathrm{s}^{-1}\mathrm{Mpc}^{-1}$ in combination with uncalibrated supernovae from Pantheon+. Using parametric estimates of the evolution of matter density fluctuations, we place constraints on cosmic structure in a range of high redshifts typically inaccessible with cross-correlation analyses. Combining lensing cross- and auto-correlations, we derive a 3.3% constraint on the integrated matter density fluctuations above $z=2.4$, one of the tightest constraints in this redshift range and fully consistent with a $螞$CDM model fit to the primary CMB from Planck. Combining with primary CMB observations and using the extended low redshift coverage of these combined data sets we derive constraints on a variety of extensions to the $螞$CDM model including massive neutrinos, spatial curvature, and dark energy. We find in flat $螞$CDM $\sum m_谓<0.12$ eV at 95% confidence using the LSS data, BAO measurements from SDSS and primary CMB observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02109v2-abstract-full').style.display = 'none'; document.getElementById('2409.02109v2-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, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">30 pages, 15 figures, accepted for publication in PRD, data available under https://portal.nersc.gov/project/act/act_x_unWISE_xcorr+3x2pt/</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/astro-ph?searchtype=author&query=Takase%2C+Y">Y. Takase</a>, <a href="/search/astro-ph?searchtype=author&query=Vacher%2C+L">L. Vacher</a>, <a href="/search/astro-ph?searchtype=author&query=Ishino%2C+H">H. Ishino</a>, <a href="/search/astro-ph?searchtype=author&query=Patanchon%2C+G">G. Patanchon</a>, <a href="/search/astro-ph?searchtype=author&query=Montier%2C+L">L. Montier</a>, <a href="/search/astro-ph?searchtype=author&query=Stever%2C+S+L">S. L. Stever</a>, <a href="/search/astro-ph?searchtype=author&query=Ishizaka%2C+K">K. Ishizaka</a>, <a href="/search/astro-ph?searchtype=author&query=Nagano%2C+Y">Y. Nagano</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+W">W. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/astro-ph?searchtype=author&query=Aizawa%2C+K">K. Aizawa</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/astro-ph?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/astro-ph?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/astro-ph?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/astro-ph?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/astro-ph?searchtype=author&query=Basak%2C+S">S. Basak</a>, <a href="/search/astro-ph?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolami%2C+M">M. Bortolami</a>, <a href="/search/astro-ph?searchtype=author&query=Brinckmann%2C+T">T. Brinckmann</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">E. Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Campeti%2C+P">P. Campeti</a>, <a href="/search/astro-ph?searchtype=author&query=Carinos%2C+E">E. Carinos</a>, <a href="/search/astro-ph?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/astro-ph?searchtype=author&query=Remazeilles%2C+M">M. Remazeilles</a>, <a href="/search/astro-ph?searchtype=author&query=Douspis%2C+M">M. Douspis</a>, <a href="/search/astro-ph?searchtype=author&query=Rubi%C3%B1o-Mart%C3%ADn%2C+J+A">J. A. Rubi帽o-Mart铆n</a>, <a href="/search/astro-ph?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/astro-ph?searchtype=author&query=Chluba%2C+J">J. Chluba</a>, <a href="/search/astro-ph?searchtype=author&query=de+Bernardis%2C+P">P. de Bernardis</a>, <a href="/search/astro-ph?searchtype=author&query=De+Petris%2C+M">M. De Petris</a>, <a href="/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez-Monteagudo%2C+C">C. Hern谩ndez-Monteagudo</a>, <a href="/search/astro-ph?searchtype=author&query=Luzzi%2C+G">G. Luzzi</a>, <a href="/search/astro-ph?searchtype=author&query=Macias-Perez%2C+J">J. Macias-Perez</a>, <a href="/search/astro-ph?searchtype=author&query=Masi%2C+S">S. Masi</a>, <a href="/search/astro-ph?searchtype=author&query=Namikawa%2C+T">T. Namikawa</a>, <a href="/search/astro-ph?searchtype=author&query=Salvati%2C+L">L. Salvati</a>, <a href="/search/astro-ph?searchtype=author&query=Tanimura%2C+H">H. Tanimura</a>, <a href="/search/astro-ph?searchtype=author&query=Aizawa%2C+K">K. Aizawa</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/astro-ph?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/astro-ph?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/astro-ph?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/astro-ph?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/astro-ph?searchtype=author&query=Basak%2C+S">S. Basak</a>, <a href="/search/astro-ph?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Blinov%2C+D">D. Blinov</a>, <a href="/search/astro-ph?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/2407.08912">arXiv:2407.08912</a> <span> [<a href="https://arxiv.org/pdf/2407.08912">pdf</a>, <a href="https://arxiv.org/format/2407.08912">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"> Design and characterization of a 60-cm reflective half-wave plate for the CLASS 90 GHz band telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shi%2C+R">Rui Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Brewer%2C+M+K">Michael K. Brewer</a>, <a href="/search/astro-ph?searchtype=author&query=Chan%2C+C+Y+Y">Carol Yan Yan Chan</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Couto%2C+J+D">Jullianna Denes Couto</a>, <a href="/search/astro-ph?searchtype=author&query=Eimer%2C+J+R">Joseph R. Eimer</a>, <a href="/search/astro-ph?searchtype=author&query=Karakla%2C+J">John Karakla</a>, <a href="/search/astro-ph?searchtype=author&query=Shukawa%2C+K">Koji Shukawa</a>, <a href="/search/astro-ph?searchtype=author&query=Valle%2C+D+A+N">Deniz A. N. Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Appel%2C+J+W">John W. Appel</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+C+L">Charles L. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Dahal%2C+S">Sumit Dahal</a>, <a href="/search/astro-ph?searchtype=author&query=Essinger-Hileman%2C+T">Thomas Essinger-Hileman</a>, <a href="/search/astro-ph?searchtype=author&query=Marriage%2C+T+A">Tobias A. Marriage</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+M+A">Matthew A. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Rostem%2C+K">Karwan Rostem</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</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="2407.08912v1-abstract-short" style="display: inline;"> Front-end polarization modulation enables improved polarization measurement stability by modulating the targeted signal above the low-frequency $1/f$ drifts associated with atmospheric and instrumental instabilities and diminishes the impact of instrumental polarization. In this work, we present the design and characterization of a new 60-cm diameter Reflective Half-Wave Plate (RHWP) polarization… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.08912v1-abstract-full').style.display = 'inline'; document.getElementById('2407.08912v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.08912v1-abstract-full" style="display: none;"> Front-end polarization modulation enables improved polarization measurement stability by modulating the targeted signal above the low-frequency $1/f$ drifts associated with atmospheric and instrumental instabilities and diminishes the impact of instrumental polarization. In this work, we present the design and characterization of a new 60-cm diameter Reflective Half-Wave Plate (RHWP) polarization modulator for the 90 GHz band telescope of the Cosmology Large Angular Scale Surveyor (CLASS) project. The RHWP consists of an array of parallel wires (diameter $50~\mathrm{渭m}$, $175~\mathrm{渭m}$ pitch) positioned $0.88~\mathrm{mm}$ from an aluminum mirror. In lab tests, it was confirmed that the wire resonance frequency ($f_\mathrm{res}$) profile is consistent with the target, $139~\mathrm{Hz}<f_\mathrm{res}<154~\mathrm{Hz}$ in the optically active region (diameter smaller than $150~\mathrm{mm}$), preventing the wire vibration during operation and reducing the RHWP deformation under the wire tension. The mirror tilt relative to the rotating axis was controlled to be $<15''$, corresponding to an increase in beam width due to beam smearing of $<0.6''$, negligible compared to the beam's full-width half-maximum of $36'$. The median and 16/84th percentile of the wire--mirror separation residual was $0.048^{+0.013}_{-0.014}~\mathrm{mm}$ in the optically active region, achieving a modulation efficiency $蔚=96.2_{+0.5}^{-0.4}\%$ with an estimated bandpass of 34 GHz. The angular velocity of the RHWP was maintained to an accuracy of within $0.005\%$ at the nominal rotation frequency ($2.5~\mathrm{Hz}$). The RHWP has been successfully integrated into the CLASS 90 GHz telescope and started taking data in June 2024, replacing the previous modulator that has been in operation since June 2018. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.08912v1-abstract-full').style.display = 'none'; document.getElementById('2407.08912v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">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">23 pages, 12 figures, 1 table, to appear in Proc. SPIE Astronomical Telescopes and 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/2407.08201">arXiv:2407.08201</a> <span> [<a href="https://arxiv.org/pdf/2407.08201">pdf</a>, <a href="https://arxiv.org/format/2407.08201">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> <p class="title is-5 mathjax"> Masses of Sunyaev-Zel'dovich Galaxy Clusters Detected by The Atacama Cosmology Telescope: Stacked Lensing Measurements with Subaru HSC Year 3 data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shirasaki%2C+M">Masato Shirasaki</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">Crist贸bal Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Miyatake%2C+H">Hironao Miyatake</a>, <a href="/search/astro-ph?searchtype=author&query=Lau%2C+E">Erwin Lau</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Z">Zhuowen Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Bahcall%2C+N">Neta Bahcall</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">Mark Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Farahi%2C+A">Arya Farahi</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">Matt Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Lin%2C+Y">Yen-Ting Lin</a>, <a href="/search/astro-ph?searchtype=author&query=Nagai%2C+D">Daisuke Nagai</a>, <a href="/search/astro-ph?searchtype=author&query=Staggs%2C+S+T">Suzanne T. Staggs</a>, <a href="/search/astro-ph?searchtype=author&query=Sunayama%2C+T">Tomomi Sunayama</a>, <a href="/search/astro-ph?searchtype=author&query=Spergel%2C+D">David Spergel</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</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="2407.08201v3-abstract-short" style="display: inline;"> We present a stacked lensing analysis of 96 galaxy clusters selected by the thermal Sunyaev-Zel'dovich (SZ) effect in maps of the cosmic microwave background (CMB). We select foreground galaxy clusters with a $5蟽$-level SZ threshold in CMB observations from the Atacama Cosmology Telescope, while we define background source galaxies for the lensing analysis with secure photometric redshift cuts in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.08201v3-abstract-full').style.display = 'inline'; document.getElementById('2407.08201v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.08201v3-abstract-full" style="display: none;"> We present a stacked lensing analysis of 96 galaxy clusters selected by the thermal Sunyaev-Zel'dovich (SZ) effect in maps of the cosmic microwave background (CMB). We select foreground galaxy clusters with a $5蟽$-level SZ threshold in CMB observations from the Atacama Cosmology Telescope, while we define background source galaxies for the lensing analysis with secure photometric redshift cuts in Year 3 data of the Subaru Hyper Suprime Cam survey. We detect the stacked lensing signal in the range of $0.1 < R\, [h^{-1}\mathrm{Mpc}] < 100$ in each of three cluster redshift bins, $0.092<z\le0.445$, $0.445<z\le0.695$, and $0.695<z\le1.180$, with 32 galaxy clusters in each bin. The cumulative signal-to-noise ratios of the lensing signal are $14.6$, $12.0$, and $6.6$, respectively. Using a halo-based forward model, we then constrain statistical relationships between the mass inferred from the SZ observation (i.e. SZ mass) and the total mass derived from our stacked lensing measurements. At the average SZ mass in the cluster sample ($2.1-2.4\times10^{14}\, h^{-1}M_\odot$), our likelihood analysis shows that the average total mass differs from the SZ counterpart by a factor of $1.3 \pm 0.2$, $1.6 \pm 0.2$, and $1.6 \pm 0.3$ ($68\%$) in the aforementioned redshift ranges, respectively. Our limits are consistent with previous lensing measurements, and we find that the cluster modeling choices can introduce a $1蟽$-level difference in our parameter inferences. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.08201v3-abstract-full').style.display = 'none'; document.getElementById('2407.08201v3-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">34 pages, 17 figures, accepted for publication in Physical Review 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/2407.07152">arXiv:2407.07152</a> <span> [<a href="https://arxiv.org/pdf/2407.07152">pdf</a>, <a href="https://arxiv.org/format/2407.07152">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> <p class="title is-5 mathjax"> Evidence for large baryonic feedback at low and intermediate redshifts from kinematic Sunyaev-Zel'dovich observations with ACT and DESI photometric galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Hadzhiyska%2C+B">B. Hadzhiyska</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Guachalla%2C+B+R">B. Ried Guachalla</a>, <a href="/search/astro-ph?searchtype=author&query=Schaan%2C+E">E. Schaan</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J">J. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">N. Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">E. Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">S. K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">T. Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Coulton%2C+W+R">W. R. Coulton</a>, <a href="/search/astro-ph?searchtype=author&query=Dawson%2C+K">K. Dawson</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">M. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+B">B. Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">A. J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">J. Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Farren%2C+G+S">G. S. Farren</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">A. Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">J. E. Forero-Romero</a>, <a href="/search/astro-ph?searchtype=author&query=Gallardo%2C+P+A">P. A. Gallardo</a>, <a href="/search/astro-ph?searchtype=author&query=Gazta%C3%B1aga%2C+E">E. Gazta帽aga</a>, <a href="/search/astro-ph?searchtype=author&query=Gontcho%2C+S+G">S. Gontcho Gontcho</a>, <a href="/search/astro-ph?searchtype=author&query=Gralla%2C+M">M. Gralla</a> , et al. (48 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="2407.07152v1-abstract-short" style="display: inline;"> Recent advances in cosmological observations have provided an unprecedented opportunity to investigate the distribution of baryons relative to the underlying matter. In this work, we robustly show that the gas is much more extended than the dark matter at 40$蟽$ and the amount of baryonic feedback at $z \lesssim 1$ strongly disfavors low-feedback models such as that of state-of-the-art hydrodynamic… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07152v1-abstract-full').style.display = 'inline'; document.getElementById('2407.07152v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.07152v1-abstract-full" style="display: none;"> Recent advances in cosmological observations have provided an unprecedented opportunity to investigate the distribution of baryons relative to the underlying matter. In this work, we robustly show that the gas is much more extended than the dark matter at 40$蟽$ and the amount of baryonic feedback at $z \lesssim 1$ strongly disfavors low-feedback models such as that of state-of-the-art hydrodynamical simulation IllustrisTNG compared with high-feedback models such as that of the original Illustris simulation. This has important implications for bridging the gap between theory and observations and understanding galaxy formation and evolution. Furthermore, a better grasp of the baryon-dark matter link is critical to future cosmological analyses, which are currently impeded by our limited knowledge of baryonic feedback. Here, we measure the kinematic Sunyaev-Zel'dovich (kSZ) effect from the Atacama Cosmology Telescope (ACT), stacked on the luminous red galaxy (LRG) sample of the Dark Energy Spectroscopic Instrument (DESI) imaging survey. This is the first analysis to use photometric redshifts for reconstructing galaxy velocities. Due to the large number of galaxies comprising the DESI imaging survey, this is the highest signal-to-noise stacked kSZ measurement to date: we detect the signal at 13$蟽$ and find that the gas is more spread out than the dark matter at $\sim$40$蟽$. Our work opens up the possibility to recalibrate large hydrodynamical simulations using the kSZ effect. In addition, our findings point towards a way of alleviating inconsistencies between weak lensing surveys and cosmic microwave background (CMB) experiments such as the `low $S_8$' tension, and shed light on long-standing enigmas in astrophysics such as the `missing baryon' problem. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.07152v1-abstract-full').style.display = 'none'; document.getElementById('2407.07152v1-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 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">20 pages, 8 figures, submitting to PRL</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.04606">arXiv:2407.04606</a> <span> [<a href="https://arxiv.org/pdf/2407.04606">pdf</a>, <a href="https://arxiv.org/format/2407.04606">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope DR6 and DESI: Structure formation over cosmic time with a measurement of the cross-correlation of CMB Lensing and Luminous Red Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Joshua Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Sailer%2C+N">Noah Sailer</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Abril-Cabezas%2C+I">Irene Abril-Cabezas</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+N">Jessica Nicole Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlen%2C+S">Steven Ahlen</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">David Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burtin%2C+E">Etienne Burtin</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">Shi-Fan Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Claybaugh%2C+T">Todd Claybaugh</a>, <a href="/search/astro-ph?searchtype=author&query=Darwish%2C+O">Omar Darwish</a>, <a href="/search/astro-ph?searchtype=author&query=de+la+Macorra%2C+A">Axel de la Macorra</a>, <a href="/search/astro-ph?searchtype=author&query=DeRose%2C+J">Joseph DeRose</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M">Mark Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Dey%2C+A">Arjun Dey</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">Peter Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Embil-Villagra%2C+C">Carmen Embil-Villagra</a>, <a href="/search/astro-ph?searchtype=author&query=Farren%2C+G+S">Gerrit S. Farren</a>, <a href="/search/astro-ph?searchtype=author&query=Font-Ribera%2C+A">Andreu Font-Ribera</a>, <a href="/search/astro-ph?searchtype=author&query=Forero-Romero%2C+J+E">Jaime E. Forero-Romero</a> , et al. (48 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="2407.04606v1-abstract-short" style="display: inline;"> We present a high-significance cross-correlation of CMB lensing maps from the Atacama Cosmology Telescope (ACT) Data Release 6 (DR6) with spectroscopically calibrated luminous red galaxies (LRGs) from the Dark Energy Spectroscopic Instrument (DESI). We detect this cross-correlation at a significance of 38$蟽$; combining our measurement with the Planck Public Release 4 (PR4) lensing map, we detect t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04606v1-abstract-full').style.display = 'inline'; document.getElementById('2407.04606v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.04606v1-abstract-full" style="display: none;"> We present a high-significance cross-correlation of CMB lensing maps from the Atacama Cosmology Telescope (ACT) Data Release 6 (DR6) with spectroscopically calibrated luminous red galaxies (LRGs) from the Dark Energy Spectroscopic Instrument (DESI). We detect this cross-correlation at a significance of 38$蟽$; combining our measurement with the Planck Public Release 4 (PR4) lensing map, we detect the cross-correlation at 50$蟽$. Fitting this jointly with the galaxy auto-correlation power spectrum to break the galaxy bias degeneracy with $蟽_8$, we perform a tomographic analysis in four LRG redshift bins spanning $0.4 \le z \le 1.0$ to constrain the amplitude of matter density fluctuations through the parameter combination $S_8^\times = 蟽_8 \left(惟_m / 0.3\right)^{0.4}$. Prior to unblinding, we confirm with extragalactic simulations that foreground biases are negligible and carry out a comprehensive suite of null and consistency tests. Using a hybrid effective field theory (HEFT) model that allows scales as small as $k_{\rm max}=0.6$ $h/{\rm Mpc}$, we obtain a 3.3% constraint on $S_8^\times = 蟽_8 \left(惟_m / 0.3\right)^{0.4} = 0.792^{+0.024}_{-0.028}$ from ACT data, as well as constraints on $S_8^\times(z)$ that probe structure formation over cosmic time. Our result is consistent with the early-universe extrapolation from primary CMB anisotropies measured by Planck PR4 within 1.2$蟽$. Jointly fitting ACT and Planck lensing cross-correlations we obtain a 2.7% constraint of $S_8^\times = 0.776^{+0.019}_{-0.021}$, which is consistent with the Planck early-universe extrapolation within 2.1$蟽$, with the lowest redshift bin showing the largest difference in mean. The latter may motivate further CMB lensing tomography analyses at $z<0.6$ to assess the impact of potential systematics or the consistency of the $螞$CDM model over cosmic time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.04606v1-abstract-full').style.display = 'none'; document.getElementById('2407.04606v1-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 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">Prepared for submission to JCAP (47 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/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/astro-ph?searchtype=author&query=Ghigna%2C+T">T. Ghigna</a>, <a href="/search/astro-ph?searchtype=author&query=Adler%2C+A">A. Adler</a>, <a href="/search/astro-ph?searchtype=author&query=Aizawa%2C+K">K. Aizawa</a>, <a href="/search/astro-ph?searchtype=author&query=Akamatsu%2C+H">H. Akamatsu</a>, <a href="/search/astro-ph?searchtype=author&query=Akizawa%2C+R">R. Akizawa</a>, <a href="/search/astro-ph?searchtype=author&query=Allys%2C+E">E. Allys</a>, <a href="/search/astro-ph?searchtype=author&query=Anand%2C+A">A. Anand</a>, <a href="/search/astro-ph?searchtype=author&query=Aumont%2C+J">J. Aumont</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J">J. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=Azzoni%2C+S">S. Azzoni</a>, <a href="/search/astro-ph?searchtype=author&query=Baccigalupi%2C+C">C. Baccigalupi</a>, <a href="/search/astro-ph?searchtype=author&query=Ballardini%2C+M">M. Ballardini</a>, <a href="/search/astro-ph?searchtype=author&query=Banday%2C+A+J">A. J. Banday</a>, <a href="/search/astro-ph?searchtype=author&query=Barreiro%2C+R+B">R. B. Barreiro</a>, <a href="/search/astro-ph?searchtype=author&query=Bartolo%2C+N">N. Bartolo</a>, <a href="/search/astro-ph?searchtype=author&query=Basak%2C+S">S. Basak</a>, <a href="/search/astro-ph?searchtype=author&query=Basyrov%2C+A">A. Basyrov</a>, <a href="/search/astro-ph?searchtype=author&query=Beckman%2C+S">S. Beckman</a>, <a href="/search/astro-ph?searchtype=author&query=Bersanelli%2C+M">M. Bersanelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bortolami%2C+M">M. Bortolami</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchet%2C+F">F. Bouchet</a>, <a href="/search/astro-ph?searchtype=author&query=Brinckmann%2C+T">T. Brinckmann</a>, <a href="/search/astro-ph?searchtype=author&query=Campeti%2C+P">P. Campeti</a>, <a href="/search/astro-ph?searchtype=author&query=Carinos%2C+E">E. Carinos</a>, <a href="/search/astro-ph?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/2405.20403">arXiv:2405.20403</a> <span> [<a href="https://arxiv.org/pdf/2405.20403">pdf</a>, <a href="https://arxiv.org/format/2405.20403">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> <p class="title is-5 mathjax"> The Primordial Inflation Explorer (PIXIE): Mission Design and Science Goals </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kogut%2C+A">Alan Kogut</a>, <a href="/search/astro-ph?searchtype=author&query=Switzer%2C+E">Eric Switzer</a>, <a href="/search/astro-ph?searchtype=author&query=Fixsen%2C+D">Dale Fixsen</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">Nabila Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Chluba%2C+J">Jens Chluba</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D">Dave Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Delabrouille%2C+J">Jacques Delabrouille</a>, <a href="/search/astro-ph?searchtype=author&query=Dvorkin%2C+C">Cora Dvorkin</a>, <a href="/search/astro-ph?searchtype=author&query=Hensley%2C+B">Brandon Hensley</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+C">Colin Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Maffei%2C+B">Bruno Maffei</a>, <a href="/search/astro-ph?searchtype=author&query=Pullen%2C+A">Anthony Pullen</a>, <a href="/search/astro-ph?searchtype=author&query=Rotti%2C+A">Aditya Rotti</a>, <a href="/search/astro-ph?searchtype=author&query=Sabyr%2C+A">Alina Sabyr</a>, <a href="/search/astro-ph?searchtype=author&query=Thiele%2C+L">Leander Thiele</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E">Ed Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Zelko%2C+I">Ioana Zelko</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="2405.20403v1-abstract-short" style="display: inline;"> The Primordial Inflation Explorer (PIXIE) is an Explorer-class mission concept to measure the energy spectrum and linear polarization of the cosmic microwave background (CMB). A single cryogenic Fourier transform spectrometer compares the sky to an external blackbody calibration target, measuring the Stokes I, Q, U parameters to levels ~200 Jy/sr in each 2.65 degree diameter beam over the full sky… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.20403v1-abstract-full').style.display = 'inline'; document.getElementById('2405.20403v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.20403v1-abstract-full" style="display: none;"> The Primordial Inflation Explorer (PIXIE) is an Explorer-class mission concept to measure the energy spectrum and linear polarization of the cosmic microwave background (CMB). A single cryogenic Fourier transform spectrometer compares the sky to an external blackbody calibration target, measuring the Stokes I, Q, U parameters to levels ~200 Jy/sr in each 2.65 degree diameter beam over the full sky, in each of 300 frequency channels from 28 GHz to 6 THz. With sensitivity over 1000 times greater than COBE/FIRAS, PIXIE opens a broad discovery space for the origin, contents, and evolution of the universe. Measurements of small distortions from a CMB blackbody spectrum provide a robust determination of the mean electron pressure and temperature in the universe while constraining processes including dissipation of primordial density perturbations, black holes, and the decay or annihilation of dark matter. Full-sky maps of linear polarization measure the optical depth to reionization at nearly the cosmic variance limit and constrain models of primordial inflation. Spectra with sub-percent absolute calibration spanning microwave to far-IR wavelengths provide a legacy data set for analyses including line intensity mapping of extragalactic emission and the cosmic infrared background amplitude and anisotropy. We describe the PIXIE instrument sensitivity, foreground subtraction, and anticipated science return from both the baseline 2-year mission and a potential extended mission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.20403v1-abstract-full').style.display = 'none'; document.getElementById('2405.20403v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">44 pages with 18 figures and 4 tables, including full sensitivity curves. Sensitivity curves are available for download at https://lambda.gsfc.nasa.gov/product/pixie/pixie_baseline_noise_get.html</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13688">arXiv:2405.13688</a> <span> [<a href="https://arxiv.org/pdf/2405.13688">pdf</a>, <a href="https://arxiv.org/format/2405.13688">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="Materials Science">cond-mat.mtrl-sci</span> </div> </div> <p class="title is-5 mathjax"> Vibrational modes as the origin of dielectric loss at 0.27$\unicode{x2013}$100 THz in a-SiC:H </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Buijtendorp%2C+B+T">B. T. Buijtendorp</a>, <a href="/search/astro-ph?searchtype=author&query=Endo%2C+A">A. Endo</a>, <a href="/search/astro-ph?searchtype=author&query=Jellema%2C+W">W. Jellema</a>, <a href="/search/astro-ph?searchtype=author&query=Karatsu%2C+K">K. Karatsu</a>, <a href="/search/astro-ph?searchtype=author&query=Kouwenhoven%2C+K">K. Kouwenhoven</a>, <a href="/search/astro-ph?searchtype=author&query=Lamers%2C+D">D. Lamers</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Linden%2C+A+J">A. J. van der Linden</a>, <a href="/search/astro-ph?searchtype=author&query=Rostem%2C+K">K. Rostem</a>, <a href="/search/astro-ph?searchtype=author&query=Veen%2C+M">M. Veen</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">E. J. Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Baselmans%2C+J+J+A">J. J. A. Baselmans</a>, <a href="/search/astro-ph?searchtype=author&query=Vollebregt%2C+S">S. Vollebregt</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.13688v2-abstract-short" style="display: inline;"> Low-loss deposited dielectrics are beneficial for the advancement of superconducting integrated circuits for astronomy. In the microwave band ($\mathrm{\sim}$1$\unicode{x2013}$10 GHz) the cryogenic and low-power dielectric loss is dominated by two-level systems. However, the origin of the loss in the millimeter-submillimeter band ($\mathrm{\sim}$0.1$\unicode{x2013}$1 THz) is not understood. We mea… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13688v2-abstract-full').style.display = 'inline'; document.getElementById('2405.13688v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13688v2-abstract-full" style="display: none;"> Low-loss deposited dielectrics are beneficial for the advancement of superconducting integrated circuits for astronomy. In the microwave band ($\mathrm{\sim}$1$\unicode{x2013}$10 GHz) the cryogenic and low-power dielectric loss is dominated by two-level systems. However, the origin of the loss in the millimeter-submillimeter band ($\mathrm{\sim}$0.1$\unicode{x2013}$1 THz) is not understood. We measured the loss of hydrogenated amorphous SiC (a-SiC:H) films in the 0.27$\unicode{x2013}$100 THz range using superconducting microstrip resonators and Fourier-transform spectroscopy. The agreement between the loss data and a Maxwell-Helmholtz-Drude dispersion model suggests that vibrational modes above 10 THz dominate the loss in the a-SiC:H above 200 GHz. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13688v2-abstract-full').style.display = 'none'; document.getElementById('2405.13688v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.12829">arXiv:2405.12829</a> <span> [<a href="https://arxiv.org/pdf/2405.12829">pdf</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"> Single Aperture Large Telescope for Universe Studies (SALTUS): Science Overview </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chin%2C+G">Gordon Chin</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+C+M">Carrie M. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Bergner%2C+J">Jennifer Bergner</a>, <a href="/search/astro-ph?searchtype=author&query=Biver%2C+N">Nicolas Biver</a>, <a href="/search/astro-ph?searchtype=author&query=Bjoraker%2C+G+L">Gordon L. Bjoraker</a>, <a href="/search/astro-ph?searchtype=author&query=Cavalie%2C+T">Thibault Cavalie</a>, <a href="/search/astro-ph?searchtype=author&query=DiSanti%2C+M">Michael DiSanti</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+J">Jian-Rong Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Hartogh%2C+P">Paul Hartogh</a>, <a href="/search/astro-ph?searchtype=author&query=Harding%2C+L+K">Leon K. Harding</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+Q">Qing Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+D">Daewook Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Kulesa%2C+C">Craig Kulesa</a>, <a href="/search/astro-ph?searchtype=author&query=de+Lange%2C+G">Gert de Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Leisawitz%2C+D+T">David T. Leisawitz</a>, <a href="/search/astro-ph?searchtype=author&query=Levy%2C+R+C">Rebecca C. Levy</a>, <a href="/search/astro-ph?searchtype=author&query=Lichtenberger%2C+A">Arthur Lichtenberger</a>, <a href="/search/astro-ph?searchtype=author&query=Marronh%2C+D+P">Daniel P. Marronh</a>, <a href="/search/astro-ph?searchtype=author&query=Najita%2C+J">Joan Najita</a>, <a href="/search/astro-ph?searchtype=author&query=Newswander%2C+T">Trent Newswander</a>, <a href="/search/astro-ph?searchtype=author&query=Rieke%2C+G+H">George H. Rieke</a>, <a href="/search/astro-ph?searchtype=author&query=Rigopoulou%2C+D">Dimitra Rigopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Roefsema%2C+P">Peter Roefsema</a>, <a href="/search/astro-ph?searchtype=author&query=Roth%2C+N+X">Nathan X. Roth</a>, <a href="/search/astro-ph?searchtype=author&query=Schwarz%2C+K">Kamber Schwarz</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="2405.12829v1-abstract-short" style="display: inline;"> The SALTUS Probe mission will provide a powerful far-infrared (far-IR) pointed space observatory to explore our cosmic origins and the possibility of life elsewhere. The observatory employs an innovative deployable 14-m aperture, with a sunshield that will radiatively cool the off-axis primary to <45K. This cooled primary reflector works in tandem with cryogenic coherent and incoherent instruments… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12829v1-abstract-full').style.display = 'inline'; document.getElementById('2405.12829v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.12829v1-abstract-full" style="display: none;"> The SALTUS Probe mission will provide a powerful far-infrared (far-IR) pointed space observatory to explore our cosmic origins and the possibility of life elsewhere. The observatory employs an innovative deployable 14-m aperture, with a sunshield that will radiatively cool the off-axis primary to <45K. This cooled primary reflector works in tandem with cryogenic coherent and incoherent instruments that span the 34 to 660 micron far-IR range at both high and moderate spectral resolutions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12829v1-abstract-full').style.display = 'none'; document.getElementById('2405.12829v1-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">49 pages, 10 figures, 3 tables, submitted to SPIE JATIS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.12795">arXiv:2405.12795</a> <span> [<a href="https://arxiv.org/pdf/2405.12795">pdf</a>, <a href="https://arxiv.org/format/2405.12795">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: DR6 Gravitational Lensing and SDSS BOSS cross-correlation measurement and constraints on gravity with the $E_G$ statistic </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Wenzl%2C+L">Lukas Wenzl</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+R">Rui An</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nick Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bean%2C+R">Rachel Bean</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+S">Shi-Fan Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Darwish%2C+O">Omar Darwish</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Farren%2C+G+S">Gerrit S. Farren</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Guan%2C+Y">Yilun Guan</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+I">Ian Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Joshua Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Louis%2C+T">Thibaut Louis</a>, <a href="/search/astro-ph?searchtype=author&query=MacCrann%2C+N">Niall MacCrann</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Marques%2C+G+A">Gabriela A. Marques</a>, <a href="/search/astro-ph?searchtype=author&query=Mehta%2C+Y">Yogesh Mehta</a>, <a href="/search/astro-ph?searchtype=author&query=Niemack%2C+M+D">Michael D. Niemack</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+F+J">Frank J. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Sehgal%2C+N">Neelima Sehgal</a>, <a href="/search/astro-ph?searchtype=author&query=Shaikh%2C+S">Shabbir Shaikh</a>, <a href="/search/astro-ph?searchtype=author&query=Sherwin%2C+B+D">Blake D. Sherwin</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">Crist贸bal Sif贸n</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="2405.12795v2-abstract-short" style="display: inline;"> We derive new constraints on the $E_G$ statistic as a test of gravity, combining the CMB lensing map estimated from Data Release 6 (DR6) of the Atacama Cosmology Telescope with SDSS BOSS CMASS and LOWZ galaxy data. We develop an analysis pipeline to measure the cross-correlation between CMB lensing maps and galaxy data, following a blinding policy and testing the approach through null and consiste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12795v2-abstract-full').style.display = 'inline'; document.getElementById('2405.12795v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.12795v2-abstract-full" style="display: none;"> We derive new constraints on the $E_G$ statistic as a test of gravity, combining the CMB lensing map estimated from Data Release 6 (DR6) of the Atacama Cosmology Telescope with SDSS BOSS CMASS and LOWZ galaxy data. We develop an analysis pipeline to measure the cross-correlation between CMB lensing maps and galaxy data, following a blinding policy and testing the approach through null and consistency checks. By testing the equivalence of the spatial and temporal gravitational potentials, the $E_G$ statistic can distinguish $螞$CDM from alternative models of gravity. We find $E_G= 0.31^{+0.06}_{-0.05}$ for ACT and CMASS data at 68.28\% confidence level, and $E_G = 0.49^{+0.14}_{-0.11}$ for ACT and LOWZ. Systematic errors are estimated to be 3\% and 4\% respectively. Including CMB lensing information from Planck PR4 results in $E_G = 0.34^{+0.05}_{-0.05}$ with CMASS and $E_G= 0.43^{+0.11}_{-0.09}$ with LOWZ. These are consistent with predictions for the $螞$CDM model that best fits the Planck CMB anisotropy and SDSS BOSS BAO, where $E_G^{\rm GR} (z_{\rm eff} = 0.555) = 0.401\pm 0.005$ for CMB lensing combined with CMASS and $E_G^{\rm GR} (z_{\rm eff} = 0.316) = 0.452\pm0.005$ combined with LOWZ. We also find $E_G$ to be scale independent, with PTE $>5\%$, as predicted by general relativity. The methods developed in this work are also applicable to improved future analyses with upcoming spectroscopic galaxy samples and CMB lensing measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12795v2-abstract-full').style.display = 'none'; document.getElementById('2405.12795v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">31 pages, 18 figures, Accepted for publication in PRD</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.17567">arXiv:2404.17567</a> <span> [<a href="https://arxiv.org/pdf/2404.17567">pdf</a>, <a href="https://arxiv.org/format/2404.17567">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"> Sensitivity-Improved Polarization Maps at 40 GHz with CLASS and WMAP data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shi%2C+R">Rui Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Appel%2C+J+W">John W. Appel</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+C+L">Charles L. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bustos%2C+R">Ricardo Bustos</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Dahal%2C+S">Sumit Dahal</a>, <a href="/search/astro-ph?searchtype=author&query=Couto%2C+J+D">Jullianna Denes Couto</a>, <a href="/search/astro-ph?searchtype=author&query=Eimer%2C+J+R">Joseph R. Eimer</a>, <a href="/search/astro-ph?searchtype=author&query=Essinger-Hileman%2C+T">Thomas Essinger-Hileman</a>, <a href="/search/astro-ph?searchtype=author&query=Harrington%2C+K">Kathleen Harrington</a>, <a href="/search/astro-ph?searchtype=author&query=Iuliano%2C+J">Jeffrey Iuliano</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yunyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Marriage%2C+T+A">Tobias A. Marriage</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+M+A">Matthew A. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Rostem%2C+K">Karwan Rostem</a>, <a href="/search/astro-ph?searchtype=author&query=Song%2C+Z">Zeya Song</a>, <a href="/search/astro-ph?searchtype=author&query=Valle%2C+D+A+N">Deniz A. N. Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+D+J">Duncan J. Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Weiland%2C+J+L">Janet L. Weiland</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+Z">Zhilei Xu</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="2404.17567v2-abstract-short" style="display: inline;"> Improved polarization measurements at frequencies below 70 GHz with degree-level angular resolution are crucial for advancing our understanding of the Galactic synchrotron radiation and the potential polarized anomalous microwave emission and ultimately benefiting the detection of primordial $B$ modes. In this study, we present sensitivity-improved 40 GHz polarization maps obtained by combining th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17567v2-abstract-full').style.display = 'inline'; document.getElementById('2404.17567v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.17567v2-abstract-full" style="display: none;"> Improved polarization measurements at frequencies below 70 GHz with degree-level angular resolution are crucial for advancing our understanding of the Galactic synchrotron radiation and the potential polarized anomalous microwave emission and ultimately benefiting the detection of primordial $B$ modes. In this study, we present sensitivity-improved 40 GHz polarization maps obtained by combining the CLASS 40 GHz and WMAP $Q$-band data through a weighted average in the harmonic domain. The decision to include WMAP $Q$-band data stems from similarities in the bandpasses. Leveraging the accurate large-scale measurements from WMAP $Q$ band and the high-sensitivity information from CLASS 40 GHz band at intermediate scales, the noise level at $\ell\in[30, 100]$ is reduced by a factor of $2-3$ in the map space. A pixel domain analysis of the polarized synchrotron spectral index ($尾_s$) using WMAP $K$ band and the combined maps (mean and 16/84th percentile across the $尾_s$ map: $-3.08_{-0.20}^{+0.20}$) reveals a stronger preference for spatial variation (PTE for a uniform $尾_s$ hypothesis smaller than 0.001) than the results obtained using WMAP $K$ and $Ka$ bands ($-3.08_{-0.14}^{+0.14}$). The cross-power spectra of the combined maps follow the same trend as other low-frequency data, and validation through simulations indicates negligible bias introduced by the combination method (sub-percent level in the power spectra). The products of this work are publicly available on $\mathtt{LAMBDA}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.17567v2-abstract-full').style.display = 'none'; document.getElementById('2404.17567v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">19 pages, 16 figures, 1 table, accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.03944">arXiv:2404.03944</a> <span> [<a href="https://arxiv.org/pdf/2404.03944">pdf</a>, <a href="https://arxiv.org/format/2404.03944">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The MeerKAT Massive Distant Clusters Survey: A Radio Halo in a Massive Galaxy Cluster at z = 1.23 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sikhosana%2C+S+P">S. P. Sikhosana</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">M. Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardi%2C+G">G. Bernardi</a>, <a href="/search/astro-ph?searchtype=author&query=Kesebonye%2C+K">K. Kesebonye</a>, <a href="/search/astro-ph?searchtype=author&query=Klutse%2C+D+Y">D. Y. Klutse</a>, <a href="/search/astro-ph?searchtype=author&query=Knowles%2C+K">K. Knowles</a>, <a href="/search/astro-ph?searchtype=author&query=Moodley%2C+K">K. Moodley</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Partridge%2C+B">B. Partridge</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">C. Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas%2C+C">C. Vargas</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E">E. Wollack</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="2404.03944v1-abstract-short" style="display: inline;"> In the current paradigm, high redshift radio halos are expected to be scarce due to inverse Compton energy losses and redshift dimming, which cause them to be intrinsically faint. This low occurrence fraction is predicted by cosmic ray electron turbulent re-acceleration models. To date, only a handful of radio halos have been detected at redshift z > 0.8. We report the MeerKAT detection of a radio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03944v1-abstract-full').style.display = 'inline'; document.getElementById('2404.03944v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.03944v1-abstract-full" style="display: none;"> In the current paradigm, high redshift radio halos are expected to be scarce due to inverse Compton energy losses and redshift dimming, which cause them to be intrinsically faint. This low occurrence fraction is predicted by cosmic ray electron turbulent re-acceleration models. To date, only a handful of radio halos have been detected at redshift z > 0.8. We report the MeerKAT detection of a radio halo hosted by a galaxy cluster ACT-CL J0329.2-2330 at z = 1.23, making it the highest redshift halo detected thus far. Using L-band and UHF-band observations, we derive a radio halo spectral index of $伪^{1.3GHz}_{0.8GHz}$ = 1.3 $\pm$ 0.4 and a radio power of P$_{1.4GHz}$ = (4.4 $\pm$ 1.5) $\times$ 10$^{24}$ W Hz$^{-1}$. This result further confirms that there is rapid magnetic field amplification in galaxy clusters at high redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.03944v1-abstract-full').style.display = 'none'; document.getElementById('2404.03944v1-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">8 pages, 8 figures, and 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.00763">arXiv:2403.00763</a> <span> [<a href="https://arxiv.org/pdf/2403.00763">pdf</a>, <a href="https://arxiv.org/format/2403.00763">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/10.1364/AO.521079">10.1364/AO.521079 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Optical modeling of systematic uncertainties in detector polarization angles for the Atacama Cosmology Telescope </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Murphy%2C+C+C">Colin C. Murphy</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Datta%2C+R">Rahul Datta</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M+J">Mark J. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Hasselfield%2C+M">Matthew Hasselfield</a>, <a href="/search/astro-ph?searchtype=author&query=Koopman%2C+B+J">Brian J. Koopman</a>, <a href="/search/astro-ph?searchtype=author&query=McMahon%2C+J">Jeff McMahon</a>, <a href="/search/astro-ph?searchtype=author&query=Naess%2C+S">Sigurd Naess</a>, <a href="/search/astro-ph?searchtype=author&query=Niemack%2C+M+D">Michael D. Niemack</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+L+A">Lyman A. Page</a>, <a href="/search/astro-ph?searchtype=author&query=Staggs%2C+S+T">Suzanne T. Staggs</a>, <a href="/search/astro-ph?searchtype=author&query=Thornton%2C+R">Robert Thornton</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</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="2403.00763v2-abstract-short" style="display: inline;"> We present an estimate of the Atacama Cosmology Telescope (ACT) detector polarization angle systematic uncertainty from optics perturbation analysis using polarization-sensitive ray tracing in CODE V optical design software. Uncertainties in polarization angle calibration in CMB measurements can limit constraints on cosmic birefringence and other cosmological parameters sensitive to polarization l… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.00763v2-abstract-full').style.display = 'inline'; document.getElementById('2403.00763v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.00763v2-abstract-full" style="display: none;"> We present an estimate of the Atacama Cosmology Telescope (ACT) detector polarization angle systematic uncertainty from optics perturbation analysis using polarization-sensitive ray tracing in CODE V optical design software. Uncertainties in polarization angle calibration in CMB measurements can limit constraints on cosmic birefringence and other cosmological parameters sensitive to polarization leakage. Our framework estimates the angle calibration systematic uncertainties from possible displacements in lens positions and orientations, and anti-reflection coating (ARC) thicknesses and refractive indices. With millimeter displacements in lens positions and percent-level perturbations in ARC thicknesses and indices from design, we find the total systematic uncertainty for three ACT detector arrays operating between 90--220 GHz to be at the tenth of degree scale. Reduced lens position and orientation uncertainties from physical measurements could lead to a reduction in the systematic uncertainty estimated with the framework presented here. This optical modeling may inform polarization angle systematic uncertainties for current and future microwave polarimeters, such as the CCAT Observatory, Simons Observatory, and CMB-S4. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.00763v2-abstract-full').style.display = 'none'; document.getElementById('2403.00763v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">14 pages, 8 figures, version accepted for publication in Applied Optics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Appl. Opt. 63, 5079-5087 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.16364">arXiv:2401.16364</a> <span> [<a href="https://arxiv.org/pdf/2401.16364">pdf</a>, <a href="https://arxiv.org/format/2401.16364">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"> Fabrication and characterization of optical filters from polymeric aerogels loaded with diamond scattering particles </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barlis%2C+A">Alyssa Barlis</a>, <a href="/search/astro-ph?searchtype=author&query=Guo%2C+H">Haiquan Guo</a>, <a href="/search/astro-ph?searchtype=author&query=Helson%2C+K">Kyle Helson</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+C">Charles Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Chan%2C+Y+Y">Yan Yan Chan</a>, <a href="/search/astro-ph?searchtype=author&query=Marriage%2C+T">Tobias Marriage</a>, <a href="/search/astro-ph?searchtype=author&query=Quijada%2C+M">Manuel Quijada</a>, <a href="/search/astro-ph?searchtype=author&query=Tokarz%2C+A">Ariel Tokarz</a>, <a href="/search/astro-ph?searchtype=author&query=Vivod%2C+S">Stephanie Vivod</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E">Edward Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Essinger-Hileman%2C+T">Thomas Essinger-Hileman</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="2401.16364v3-abstract-short" style="display: inline;"> We have developed a suite of infrared-blocking filters made by embedding diamond scattering particles in a polyimide aerogel substrate. We demonstrate the ability to tune the spectral performance of the filters based on both the composition of the base aerogel material and the properties of the scattering particles. We summarize the fabrication, optical modeling, and characterization of these filt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16364v3-abstract-full').style.display = 'inline'; document.getElementById('2401.16364v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.16364v3-abstract-full" style="display: none;"> We have developed a suite of infrared-blocking filters made by embedding diamond scattering particles in a polyimide aerogel substrate. We demonstrate the ability to tune the spectral performance of the filters based on both the composition of the base aerogel material and the properties of the scattering particles. We summarize the fabrication, optical modeling, and characterization of these filters. We investigate two polyimide base aerogel formulations and the effects of loading them with diamond scattering particles of varying sizes and relative densities. We describe a model for the filters' behavior using a combination of Maxwell Garnett and Mie Scattering techniques. We present optical characterization results for diamond-loaded aerogel filters with cutoff frequencies (50% transmittance) ranging between 2.5 and 15 THz, and confirm that the measured spectral performance is in agreement with our optical models. We also measure the filters' refractive index in the microwave and report findings in agreement with Maxwell Garnett model predictions (typically n < 1.08). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.16364v3-abstract-full').style.display = 'none'; document.getElementById('2401.16364v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">18 pages, 11 figures, 3 tables. Submitted to Applied Optics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.13033">arXiv:2401.13033</a> <span> [<a href="https://arxiv.org/pdf/2401.13033">pdf</a>, <a href="https://arxiv.org/format/2401.13033">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: Detection of Patchy Screening of the Cosmic Microwave Background </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Coulton%2C+W+R">William R. Coulton</a>, <a href="/search/astro-ph?searchtype=author&query=Schutt%2C+T">Theo Schutt</a>, <a href="/search/astro-ph?searchtype=author&query=Maniyar%2C+A+S">Abhishek S. Maniyar</a>, <a href="/search/astro-ph?searchtype=author&query=Schaan%2C+E">Emmanuel Schaan</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+R">Rui An</a>, <a href="/search/astro-ph?searchtype=author&query=Atkins%2C+Z">Zachary Atkins</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M+J">Mark J. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">Adriaan J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Gluscevic%2C+V">Vera Gluscevic</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+J+C">J. Colin Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">Matt Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Hincks%2C+A+D">Adam D. Hincks</a>, <a href="/search/astro-ph?searchtype=author&query=Kosowsky%2C+A">Arthur Kosowsky</a>, <a href="/search/astro-ph?searchtype=author&query=Kramer%2C+D">Darby Kramer</a>, <a href="/search/astro-ph?searchtype=author&query=Kusiak%2C+A">Aleksandra Kusiak</a>, <a href="/search/astro-ph?searchtype=author&query=La+Posta%2C+A">Adrien La Posta</a>, <a href="/search/astro-ph?searchtype=author&query=Louis%2C+T">Thibaut Louis</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Marques%2C+G+A">Gabriela A. Marques</a> , et al. (15 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="2401.13033v1-abstract-short" style="display: inline;"> Spatial variations in the cosmic electron density after reionization generate cosmic microwave background anisotropies via Thomson scattering, a process known as the ``patchy screening" effect. In this paper, we propose a new estimator for the patchy screening effect that is designed to mitigate biases from the dominant foreground signals. We use it to measure the cross-correlation between \textit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13033v1-abstract-full').style.display = 'inline'; document.getElementById('2401.13033v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.13033v1-abstract-full" style="display: none;"> Spatial variations in the cosmic electron density after reionization generate cosmic microwave background anisotropies via Thomson scattering, a process known as the ``patchy screening" effect. In this paper, we propose a new estimator for the patchy screening effect that is designed to mitigate biases from the dominant foreground signals. We use it to measure the cross-correlation between \textit{unWISE} galaxies and patchy screening, the latter measured by the Atacama Cosmology Telescope and \textit{Planck} satellite. We report the first detection of the patchy screening effect, with the statistical significance of the cross-correlation exceeding $7蟽$. This measurement directly probes the distribution of electrons around these galaxies and provides strong evidence that gas is more extended than the underlying dark matter. By comparing our measurements to electron profiles extracted from simulations, we demonstrate the power of these observations to constrain galaxy evolution models. Requiring only the 2D positions of objects and no individual redshifts or velocity estimates, this approach is complementary to existing gas probes, such as those based on the kinetic Sunyaev-Zeldovich effect. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.13033v1-abstract-full').style.display = 'none'; document.getElementById('2401.13033v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">See Schutt et al for a detailed comparison of patchy screening estimators. 17 pages with 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/2401.05317">arXiv:2401.05317</a> <span> [<a href="https://arxiv.org/pdf/2401.05317">pdf</a>, <a href="https://arxiv.org/format/2401.05317">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> </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/ad4462">10.3847/1538-4357/ad4462 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> SOFIA/HAWC+ Far-Infrared Polarimetric Large-Area CMZ Exploration (FIREPLACE) Survey III: Full Survey Data Set </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Par%C3%A9%2C+D">Dylan Par茅</a>, <a href="/search/astro-ph?searchtype=author&query=Butterfield%2C+N+O">Natalie O. Butterfield</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+J+A">Jordan A. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Iuliano%2C+J+I">Jeffrey I. Iuliano</a>, <a href="/search/astro-ph?searchtype=author&query=Karpovich%2C+K">Kaitlyn Karpovich</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E">Edward Wollack</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="2401.05317v3-abstract-short" style="display: inline;"> We present the second data release (DR2) of the Far-Infrared Polarimetric Large-Area CMZ Exploration (FIREPLACE) survey. This survey utilized the Stratospheric Observatory for Infrared Astronomy (SOFIA) High-resolution Airborne Wideband Camera plus (HAWC+) instrument at 214 $渭$m (E-band) to observe dust polarization throughout the Central Molecular Zone (CMZ) of the Milky Way. DR2 consists of obse… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.05317v3-abstract-full').style.display = 'inline'; document.getElementById('2401.05317v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.05317v3-abstract-full" style="display: none;"> We present the second data release (DR2) of the Far-Infrared Polarimetric Large-Area CMZ Exploration (FIREPLACE) survey. This survey utilized the Stratospheric Observatory for Infrared Astronomy (SOFIA) High-resolution Airborne Wideband Camera plus (HAWC+) instrument at 214 $渭$m (E-band) to observe dust polarization throughout the Central Molecular Zone (CMZ) of the Milky Way. DR2 consists of observations that were obtained in 2022 covering the region of the CMZ extending roughly from the Brick to the Sgr C molecular clouds (corresponding to a roughly 1$^{\circ}$ $\times$ 0.75$^{\circ}$ region of the sky). We combine DR2 with the first FIREPLACE data release to obtain full coverage of the CMZ (a 1.5$^{\circ}$ $\times$0.75$^{\circ}$ region of the sky). After applying total and polarized intensity significance cuts on the full FIREPLACE data set we obtain $\rm\sim$65,000 Nyquist-sampled polarization pseudovectors. The distribution of polarization pseudovectors confirms a bimodal distribution in the CMZ magnetic field orientations, recovering field components that are oriented predominantly parallel or perpendicular to the Galactic plane. These magnetic field orientations indicate possible connections between the previously observed parallel and perpendicular distributions. We also inspect the magnetic fields toward a set of prominent CMZ molecular clouds (the Brick, Three Little Pigs, 50 km s$\rm^{-1}$, Circum-nuclear Disk, CO 0.02-0.02, 20 km s$\rm^{-1}$, and Sgr C), revealing spatially varying magnetic fields that generally trace the morphologies of the clouds. We find evidence that compression from stellar winds and shear from tidal forces are prominent mechanisms influencing the structure of the magnetic fields observed within the clouds. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.05317v3-abstract-full').style.display = 'none'; document.getElementById('2401.05317v3-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">35 pages, 23 figures, 3 tables. Article is accepted for publication in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 969 (2024) 150 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.01983">arXiv:2401.01983</a> <span> [<a href="https://arxiv.org/pdf/2401.01983">pdf</a>, <a href="https://arxiv.org/format/2401.01983">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> </div> </div> <p class="title is-5 mathjax"> SOFIA/HAWC+ Far-Infrared Polarimetric Large Area CMZ Exploration (FIREPLACE) II: Detection of a Magnetized Dust Ring in the Galactic Center </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Butterfield%2C+N+O">Natalie O. Butterfield</a>, <a href="/search/astro-ph?searchtype=author&query=Guerra%2C+J+A">Jordan A. Guerra</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Morris%2C+M+R">Mark R. Morris</a>, <a href="/search/astro-ph?searchtype=author&query=Pare%2C+D">Dylan Pare</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Costa%2C+A+H">Allison H. Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Hankins%2C+M+J">Matthew J. Hankins</a>, <a href="/search/astro-ph?searchtype=author&query=Staguhn%2C+J">Johannes Staguhn</a>, <a href="/search/astro-ph?searchtype=author&query=Zweibel%2C+E">Ellen Zweibel</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="2401.01983v2-abstract-short" style="display: inline;"> We present the detection of a magnetized dust ring (M0.8-0.2) in the Central Molecular Zone (CMZ) of the Galactic Center. The results presented in this paper utilize the first data release (DR1) of the Far-Infrared Polarimetric Large Area CMZ Exploration (FIREPLACE) survey (i.e., FIREPLACE I; Butterfield et al. 2023). The FIREPLACE survey is a 214 $渭$m polarimetic survey of the Galactic Center usi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.01983v2-abstract-full').style.display = 'inline'; document.getElementById('2401.01983v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.01983v2-abstract-full" style="display: none;"> We present the detection of a magnetized dust ring (M0.8-0.2) in the Central Molecular Zone (CMZ) of the Galactic Center. The results presented in this paper utilize the first data release (DR1) of the Far-Infrared Polarimetric Large Area CMZ Exploration (FIREPLACE) survey (i.e., FIREPLACE I; Butterfield et al. 2023). The FIREPLACE survey is a 214 $渭$m polarimetic survey of the Galactic Center using the SOFIA/HAWC+ telescope. The M0.8-0.2 ring is a region of gas and dust that has a circular morphology with a central depression. The dust polarization in the M0.8-0.2 ring implies a curved magnetic field that traces the ring-like structure of the cloud. We posit an interpretation in which an expanding shell compresses and concentrates the ambient gas and magnetic field. We argue that this compression results in the strengthening of the magnetic field, as we infer from the observations toward the interior of the ring. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.01983v2-abstract-full').style.display = 'none'; document.getElementById('2401.01983v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 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">Accepted for publication in ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.15085">arXiv:2312.15085</a> <span> [<a href="https://arxiv.org/pdf/2312.15085">pdf</a>, <a href="https://arxiv.org/format/2312.15085">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 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/10.1117/12.2630571">10.1117/12.2630571 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cross-Slot Metal-Mesh Bandpass Filters for Far-Infrared Astronomy </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Perido%2C+J">Joanna Perido</a>, <a href="/search/astro-ph?searchtype=author&query=Denis%2C+K">Kevin Denis</a>, <a href="/search/astro-ph?searchtype=author&query=Glenn%2C+J">Jason Glenn</a>, <a href="/search/astro-ph?searchtype=author&query=Cothard%2C+N+F">Nicholas F. Cothard</a>, <a href="/search/astro-ph?searchtype=author&query=Quijada%2C+M">Manuel Quijada</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+J">Jessica Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E">Edward Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Hewagama%2C+T">Tilak Hewagama</a>, <a href="/search/astro-ph?searchtype=author&query=Aslam%2C+S">Shahid Aslam</a>, <a href="/search/astro-ph?searchtype=author&query=Day%2C+P+K">Peter K. Day</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="2312.15085v1-abstract-short" style="display: inline;"> The far-infrared (IR) region is rich with information needed to characterize interstellar dust and to investigate the cold outer planets of the solar system and their icy moons. The proposed sub-orbital observatory the Balloon Experiment for Galactic INfrared Science (BEGINS) will utilize cryogenic instruments to map spectral energy distributions (SEDs) of interstellar dust in the Cygnus molecular… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.15085v1-abstract-full').style.display = 'inline'; document.getElementById('2312.15085v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.15085v1-abstract-full" style="display: none;"> The far-infrared (IR) region is rich with information needed to characterize interstellar dust and to investigate the cold outer planets of the solar system and their icy moons. The proposed sub-orbital observatory the Balloon Experiment for Galactic INfrared Science (BEGINS) will utilize cryogenic instruments to map spectral energy distributions (SEDs) of interstellar dust in the Cygnus molecular cloud complex. A future high priority flagship mission Uranus Orbiter and Probe carrying a net flux radiometer (NFR) will study the in situ heat flux of the icy giants atmosphere to 10 bar pressure. These instruments require far-IR filters to define the instrument spectral bandwidths. Our ultimate goal is to define the instrument bands of BEGINS and the NFR with linear-variable filters (LVFs) and discrete-variable filters (DVFs). The LVFs and DVFs will be made of metal mesh band-pass filters (MMBF) comprised of a 100 nm thick gold film with cross-shaped slots of varying sizes along a silicon (Si) substrate with cyclic olefin copolymer (COC) anti-reflection (AR) coatings. We present our progress towards LVFs and DVFs with simulated and measured transmission of a room temperature, non-AR coated, single-band 44 $渭$m MMBF filter. We have successfully fabricated, measured, and modeled a non-AR coated, room temperature 44 $渭$m MMBF. The transmission at room temperature and non-AR coated was measured to be 27\% with a resolving power of 11. When COC-AR coated on both sides the transmission is expected to increase to 69\% with a resolving power of 10. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.15085v1-abstract-full').style.display = 'none'; document.getElementById('2312.15085v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 December, 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">Journal ref:</span> Millimeter, Submillimeter, and Far-Infrared Detectors and Instrumentation for Astronomy XI. Vol. 12190. SPIE, 2022 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.11956">arXiv:2312.11956</a> <span> [<a href="https://arxiv.org/pdf/2312.11956">pdf</a>, <a href="https://arxiv.org/format/2312.11956">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/10.1364/AO.515508">10.1364/AO.515508 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Anti-reflection coating with mullite and Duroid for large-diameter cryogenic sapphire and alumina optics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sakaguri%2C+K">Kana Sakaguri</a>, <a href="/search/astro-ph?searchtype=author&query=Hasegawa%2C+M">Masaya Hasegawa</a>, <a href="/search/astro-ph?searchtype=author&query=Sakurai%2C+Y">Yuki Sakurai</a>, <a href="/search/astro-ph?searchtype=author&query=Sugiyama%2C+J">Junna Sugiyama</a>, <a href="/search/astro-ph?searchtype=author&query=Farias%2C+N">Nicole Farias</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+C">Charles Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+B+R">Bradley R. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Konishi%2C+K">Kuniaki Konishi</a>, <a href="/search/astro-ph?searchtype=author&query=Kusaka%2C+A">Akito Kusaka</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+A+T">Adrian T. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Matsumura%2C+T">Tomotake Matsumura</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Yumoto%2C+J">Junji Yumoto</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="2312.11956v1-abstract-short" style="display: inline;"> We developed a broadband two-layer anti-reflection (AR) coating for use on a sapphire half-wave plate (HWP) and an alumina infrared (IR) filter for the cosmic microwave background (CMB) polarimetry. Measuring the faint CMB B-mode signals requires maximizing the number of photons reaching the detectors and minimizing spurious polarization due to reflection with an off-axis incident angle. Sapphire… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.11956v1-abstract-full').style.display = 'inline'; document.getElementById('2312.11956v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.11956v1-abstract-full" style="display: none;"> We developed a broadband two-layer anti-reflection (AR) coating for use on a sapphire half-wave plate (HWP) and an alumina infrared (IR) filter for the cosmic microwave background (CMB) polarimetry. Measuring the faint CMB B-mode signals requires maximizing the number of photons reaching the detectors and minimizing spurious polarization due to reflection with an off-axis incident angle. Sapphire and alumina have high refractive indices of 3.1 and are highly reflective without an AR coating. This paper presents the design, fabrication, quality control, and measured performance of an AR coating using thermally-sprayed mullite and Duroid 5880LZ. This technology enables large optical elements with diameters of 600 mm. We also present a newly developed thermography-based nondestructive quality control technique, which is key to assuring good adhesion and preventing delamination when thermal cycling. We demonstrate the average reflectance of about 2.6% (0.9%) for two observing bands centered at 90/150 (220/280) GHz. At room temperature, the average transmittance of a 105 mm square test sample at 220/280 GHz is 83%, and it will increase to 90% at 100 K, attributed to reduced absorption losses. Therefore, our developed layering technique has proved effective for 220/280 GHz applications, particularly in addressing dielectric loss concerns. This AR coating technology has been deployed in the cryogenic HWP and IR filters of the Simons Array and the Simons observatory experiments and applies to future experiments such as CMB-S4. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.11956v1-abstract-full').style.display = 'none'; document.getElementById('2312.11956v1-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 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">Journal ref:</span> Applied Optics Vol. 63, Issue 6, pp. 1618-1627 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.07656">arXiv:2312.07656</a> <span> [<a href="https://arxiv.org/pdf/2312.07656">pdf</a>, <a href="https://arxiv.org/format/2312.07656">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"> Optimization of an Optical Testbed for Characterization of EXCLAIM u-Spec Integrated Spectrometers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rahmani%2C+M">Maryam Rahmani</a>, <a href="/search/astro-ph?searchtype=author&query=Barrentine%2C+E+M">Emily M. Barrentine</a>, <a href="/search/astro-ph?searchtype=author&query=Switzer%2C+E+R">Eric R. Switzer</a>, <a href="/search/astro-ph?searchtype=author&query=Barlis%2C+A">Alyssa Barlis</a>, <a href="/search/astro-ph?searchtype=author&query=Brown%2C+A+D">Ari D. Brown</a>, <a href="/search/astro-ph?searchtype=author&query=Cataldo%2C+G">Giuseppe Cataldo</a>, <a href="/search/astro-ph?searchtype=author&query=Connors%2C+J+A">Jake A. Connors</a>, <a href="/search/astro-ph?searchtype=author&query=Ehsan%2C+N">Negar Ehsan</a>, <a href="/search/astro-ph?searchtype=author&query=Essinger-Hileman%2C+T+M">Thomas M. Essinger-Hileman</a>, <a href="/search/astro-ph?searchtype=author&query=Grant%2C+H">Henry Grant</a>, <a href="/search/astro-ph?searchtype=author&query=Hays-Wehle%2C+J">James Hays-Wehle</a>, <a href="/search/astro-ph?searchtype=author&query=Hsieh%2C+W">Wen-Ting Hsieh</a>, <a href="/search/astro-ph?searchtype=author&query=Mikula%2C+V">Vilem Mikula</a>, <a href="/search/astro-ph?searchtype=author&query=Moseley%2C+S+H">S. Harvey Moseley</a>, <a href="/search/astro-ph?searchtype=author&query=Noroozian%2C+O">Omid Noroozian</a>, <a href="/search/astro-ph?searchtype=author&query=Quijada%2C+M+A">Manuel A. Quijada</a>, <a href="/search/astro-ph?searchtype=author&query=Patel%2C+J">Jessica Patel</a>, <a href="/search/astro-ph?searchtype=author&query=Stevenson%2C+T+R">Thomas R. Stevenson</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+C">Carole Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=U-Yen%2C+K">Kongpop U-Yen</a>, <a href="/search/astro-ph?searchtype=author&query=Volpert%2C+C+G">Carolyn G. Volpert</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</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="2312.07656v1-abstract-short" style="display: inline;"> We describe a testbed to characterize the optical response of compact superconducting on-chip spectrometers in development for the Experiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) mission. EXCLAIM is a balloonborne far-infrared experiment to probe the CO and CII emission lines in galaxies from redshift 3.5 to the present. The spectrometer, called u-Spec, comprises a diffraction… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07656v1-abstract-full').style.display = 'inline'; document.getElementById('2312.07656v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.07656v1-abstract-full" style="display: none;"> We describe a testbed to characterize the optical response of compact superconducting on-chip spectrometers in development for the Experiment for Cryogenic Large-Aperture Intensity Mapping (EXCLAIM) mission. EXCLAIM is a balloonborne far-infrared experiment to probe the CO and CII emission lines in galaxies from redshift 3.5 to the present. The spectrometer, called u-Spec, comprises a diffraction grating on a silicon chip coupled to kinetic inductance detectors (KIDs) read out via a single microwave feedline. We use a prototype spectrometer for EXCLAIM to demonstrate our ability to characterize the spectrometers spectral response using a photomixer source. We utilize an on-chip reference detector to normalize relative to spectral structure from the off-chip optics and a silicon etalon to calibrate the absolute frequency. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.07656v1-abstract-full').style.display = 'none'; document.getElementById('2312.07656v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 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/2311.00615">arXiv:2311.00615</a> <span> [<a href="https://arxiv.org/pdf/2311.00615">pdf</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/10.1088/2515-7647/ace869">10.1088/2515-7647/ace869 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> 2023 Astrophotonics Roadmap: pathways to realizing multi-functional integrated astrophotonic instruments </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jovanovic%2C+N">Nemanja Jovanovic</a>, <a href="/search/astro-ph?searchtype=author&query=Gatkine%2C+P">Pradip Gatkine</a>, <a href="/search/astro-ph?searchtype=author&query=Anugu%2C+N">Narsireddy Anugu</a>, <a href="/search/astro-ph?searchtype=author&query=Amezcua-Correa%2C+R">Rodrigo Amezcua-Correa</a>, <a href="/search/astro-ph?searchtype=author&query=Thakur%2C+R+B">Ritoban Basu Thakur</a>, <a href="/search/astro-ph?searchtype=author&query=Beichman%2C+C">Charles Beichman</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+C">Chad Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Berger%2C+J">Jean-Philippe Berger</a>, <a href="/search/astro-ph?searchtype=author&query=Bigioli%2C+A">Azzurra Bigioli</a>, <a href="/search/astro-ph?searchtype=author&query=Bland-Hawthorn%2C+J">Joss Bland-Hawthorn</a>, <a href="/search/astro-ph?searchtype=author&query=Bourdarot%2C+G">Guillaume Bourdarot</a>, <a href="/search/astro-ph?searchtype=author&query=Bradford%2C+C+M">Charles M. Bradford</a>, <a href="/search/astro-ph?searchtype=author&query=Broeke%2C+R">Ronald Broeke</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+J">Julia Bryant</a>, <a href="/search/astro-ph?searchtype=author&query=Bundy%2C+K">Kevin Bundy</a>, <a href="/search/astro-ph?searchtype=author&query=Cheriton%2C+R">Ross Cheriton</a>, <a href="/search/astro-ph?searchtype=author&query=Cvetojevic%2C+N">Nick Cvetojevic</a>, <a href="/search/astro-ph?searchtype=author&query=Diab%2C+M">Momen Diab</a>, <a href="/search/astro-ph?searchtype=author&query=Diddams%2C+S+A">Scott A. Diddams</a>, <a href="/search/astro-ph?searchtype=author&query=Dinkelaker%2C+A+N">Aline N. Dinkelaker</a>, <a href="/search/astro-ph?searchtype=author&query=Duis%2C+J">Jeroen Duis</a>, <a href="/search/astro-ph?searchtype=author&query=Eikenberry%2C+S">Stephen Eikenberry</a>, <a href="/search/astro-ph?searchtype=author&query=Ellis%2C+S">Simon Ellis</a>, <a href="/search/astro-ph?searchtype=author&query=Endo%2C+A">Akira Endo</a>, <a href="/search/astro-ph?searchtype=author&query=Figer%2C+D+F">Donald F. Figer</a> , et al. (55 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="2311.00615v1-abstract-short" style="display: inline;"> Photonics offer numerous functionalities that can be used to realize astrophotonic instruments. The most spectacular example to date is the ESO Gravity instrument at the Very Large Telescope in Chile. Integrated astrophotonic devices stand to offer critical advantages for instrument development, including extreme miniaturization, as well as integration, superior thermal and mechanical stabilizatio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00615v1-abstract-full').style.display = 'inline'; document.getElementById('2311.00615v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.00615v1-abstract-full" style="display: none;"> Photonics offer numerous functionalities that can be used to realize astrophotonic instruments. The most spectacular example to date is the ESO Gravity instrument at the Very Large Telescope in Chile. Integrated astrophotonic devices stand to offer critical advantages for instrument development, including extreme miniaturization, as well as integration, superior thermal and mechanical stabilization owing to the small footprint, and high replicability offering cost savings. Numerous astrophotonic technologies have been developed to address shortcomings of conventional instruments to date, including for example the development of photonic lanterns, complex aperiodic fiber Bragg gratings, complex beam combiners to enable long baseline interferometry, and laser frequency combs for high precision spectral calibration of spectrometers. Despite these successes, the facility implementation of photonic solutions in astronomical instrumentation is currently limited because of (1) low throughputs from coupling to fibers, coupling fibers to chips, propagation and bend losses, device losses, etc, (2) difficulties with scaling to large channel count devices needed for large bandwidths and high resolutions, and (3) efficient integration of photonics with detectors, to name a few. In this roadmap, we identify 24 areas that need further development. We outline the challenges and advances needed across those areas covering design tools, simulation capabilities, fabrication processes, the need for entirely new components, integration and hybridization and the characterization of devices. To realize these advances the astrophotonics community will have to work cooperatively with industrial partners who have more advanced manufacturing capabilities. With the advances described herein, multi-functional instruments will be realized leading to novel observing capabilities for both ground and space platforms. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.00615v1-abstract-full').style.display = 'none'; document.getElementById('2311.00615v1-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 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">191 pages, 47 figures. This is the version of the article before peer review or editing, as submitted by an author to J. Phys. Photonics. IOP Publishing Ltd is not responsible for any errors or omissions in this version of the manuscript or any version derived from it. The Version of Record is available online at https://iopscience.iop.org/article/10.1088/2515-7647/ace869/meta</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Phys. Photonics 5 042501 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.17535">arXiv:2310.17535</a> <span> [<a href="https://arxiv.org/pdf/2310.17535">pdf</a>, <a href="https://arxiv.org/format/2310.17535">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: Extragalactic Point Sources in the Southern Surveys at 150, 220 and 280 GHz observed between 2008-2010 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vargas%2C+C">Cristian Vargas</a>, <a href="/search/astro-ph?searchtype=author&query=L%C3%B3pez-Caraballo%2C+C+H">Carlos H. L贸pez-Caraballo</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">Elia S. Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Dunner%2C+R">Rolando Dunner</a>, <a href="/search/astro-ph?searchtype=author&query=Farren%2C+G">Gerrit Farren</a>, <a href="/search/astro-ph?searchtype=author&query=Gralla%2C+M">Megan Gralla</a>, <a href="/search/astro-ph?searchtype=author&query=Hall%2C+K+R">Kirsten R. Hall</a>, <a href="/search/astro-ph?searchtype=author&query=Herv%C3%ADas-Caimapo%2C+C">Carlos Herv铆as-Caimapo</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">Matt Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Hincks%2C+A+D">Adam D. Hincks</a>, <a href="/search/astro-ph?searchtype=author&query=Huffenberger%2C+K">Kevin Huffenberger</a>, <a href="/search/astro-ph?searchtype=author&query=Marriage%2C+T">Tobias Marriage</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">Tony Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Niemack%2C+M+D">Michael D. Niemack</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+L">Lyman Page</a>, <a href="/search/astro-ph?searchtype=author&query=Partridge%2C+B">Bruce Partridge</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+F">Felipe Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Rizzo%2C+F">Francesca Rizzo</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">Crist贸bal Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Staggs%2C+S">Suzanne Staggs</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</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="2310.17535v2-abstract-short" style="display: inline;"> We present a multi-frequency, multi-epoch catalog of extragalactic sources. The catalog is based on 150, 220, and 280 GHz observations carried out in 2008, 2009, and 2010 using the Millimeter Bolometric Array Camera on the Atacama Cosmology Telescope. We also present and release 280 GHz maps from 2008 and 2010. The catalog contains 483 sources found in a sky area of ${\sim}600$ square degrees. It… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17535v2-abstract-full').style.display = 'inline'; document.getElementById('2310.17535v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.17535v2-abstract-full" style="display: none;"> We present a multi-frequency, multi-epoch catalog of extragalactic sources. The catalog is based on 150, 220, and 280 GHz observations carried out in 2008, 2009, and 2010 using the Millimeter Bolometric Array Camera on the Atacama Cosmology Telescope. We also present and release 280 GHz maps from 2008 and 2010. The catalog contains 483 sources found in a sky area of ${\sim}600$ square degrees. It was obtained by cross-matching sources found in 11 sub-catalogs, one for each season and frequency band. We also include co-added data from ${\sim}150$ and ${\sim}160$ square degrees using two and three years of overlapping observations. We divide the sources into two populations, synchrotron and dusty emitters, based on their spectral behavior in the 150-280 GHz frequency range. We find 284 synchrotron sources and 183 dusty source candidates. Our cross-matching with catalogs from radio to X-ray results in 251 synchrotron sources (88%) and 92 dusty sources (51%) with counterparts and suggests that 91 dusty candidates are not in existing catalogs. We study the variability and number counts of each population. In the case of synchrotron sources, we find year-to-year variability, with a mean value around 35%. As expected, we find no evidence of dusty source variability. Our number counts generally agree with previous measurements and models, except for dusty sources at 280 GHz, where some models overestimate our results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17535v2-abstract-full').style.display = 'none'; document.getElementById('2310.17535v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 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">24 pages, 16 figures, for associated data products see https://lambda.gsfc.nasa.gov/product/act/act_prod_table.html -- Accepted on Astronomy and Astrophysics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.06120">arXiv:2310.06120</a> <span> [<a href="https://arxiv.org/pdf/2310.06120">pdf</a>, <a href="https://arxiv.org/format/2310.06120">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/10.1051/0004-6361/202348213">10.1051/0004-6361/202348213 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> XLSSC 122 caught in the act of growing up: Spatially resolved SZ observations of a z=1.98 galaxy cluster </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=van+Marrewijk%2C+J">J. van Marrewijk</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Mascolo%2C+L">L. Di Mascolo</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+A+S">A. S. Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">N. Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">E. S. Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M+J">M. J. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Doze%2C+P">P. Doze</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">J. Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Knowles%2C+K">K. Knowles</a>, <a href="/search/astro-ph?searchtype=author&query=Hincks%2C+A">A. Hincks</a>, <a href="/search/astro-ph?searchtype=author&query=Hughes%2C+J+P">J. P. Hughes</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">M. Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Moodley%2C+K">K. Moodley</a>, <a href="/search/astro-ph?searchtype=author&query=Mroczkowski%2C+T">T. Mroczkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Naess%2C+S">S. Naess</a>, <a href="/search/astro-ph?searchtype=author&query=Partridge%2C+B">B. Partridge</a>, <a href="/search/astro-ph?searchtype=author&query=Popping%2C+G">G. Popping</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">C. Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Staggs%2C+S+T">S. T. Staggs</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">E. J. Wollack</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="2310.06120v3-abstract-short" style="display: inline;"> How protoclusters evolved from sparse galaxy overdensities to mature galaxy clusters is still not well understood. In this context, detecting and characterizing the hot ICM at high redshifts (z~2) is key to understanding how the continuous accretion from and mergers along the filamentary large-scale structure impact the first phases of cluster formation. We study the dynamical state and morphology… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06120v3-abstract-full').style.display = 'inline'; document.getElementById('2310.06120v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.06120v3-abstract-full" style="display: none;"> How protoclusters evolved from sparse galaxy overdensities to mature galaxy clusters is still not well understood. In this context, detecting and characterizing the hot ICM at high redshifts (z~2) is key to understanding how the continuous accretion from and mergers along the filamentary large-scale structure impact the first phases of cluster formation. We study the dynamical state and morphology of the z=1.98 galaxy cluster XLSSC 122 with high-resolution observations (~5") of the ICM through the SZ effect. Via Bayesian forward modeling, we map the ICM on scales from the virial radius down to the core of the cluster. To constrain such a broad range of spatial scales, we employ a new technique that jointly forward-models parametric descriptions of the pressure distribution to interferometric ACA and ALMA observations and multi-band imaging data from the 6-m, single-dish Atacama Cosmology Telescope. We detect the SZ effect with $11蟽$ in the ALMA+ACA observations and find a flattened inner pressure profile that is consistent with a non-cool core classification with a significance of $>3蟽$. In contrast to the previous works, we find better agreement between the SZ effect signal and the X-ray emission as well as the cluster member distribution. Further, XLSSC 122 exhibits an excess of SZ flux in the south of the cluster where no X-ray emission is detected. By reconstructing the interferometric observations and modeling in the uv-plane, we obtain a tentative detection of an infalling group or filamentary-like structure that is believed to boost and heat up the ICM while the density of the gas is low. In addition, we provide an improved SZ mass of $M_{500,\mathrm{c}} = 1.66^{+0.23}_{-0.20} \times 10^{14} \rm M_\odot$. Altogether, the observations indicate that we see XLSSC 122 in a dynamic phase of cluster formation while a large reservoir of gas is already thermalized. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.06120v3-abstract-full').style.display = 'none'; document.getElementById('2310.06120v3-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 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">Journal ref:</span> A&A 689, A41 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.00059">arXiv:2310.00059</a> <span> [<a href="https://arxiv.org/pdf/2310.00059">pdf</a>, <a href="https://arxiv.org/format/2310.00059">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Cosmological shocks around galaxy clusters: A coherent investigation with DES, SPT & ACT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Anbajagane%2C+D">D. Anbajagane</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">C. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Baxter%2C+E+J">E. J. Baxter</a>, <a href="/search/astro-ph?searchtype=author&query=Charney%2C+S">S. Charney</a>, <a href="/search/astro-ph?searchtype=author&query=Lokken%2C+M">M. Lokken</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+R">R. An</a>, <a href="/search/astro-ph?searchtype=author&query=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">N. Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+M+R">M. R. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+B+A">B. A. Benson</a>, <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+G+M">G. M. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Bleem%2C+L">L. Bleem</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. R. Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=Kind%2C+M+C">M. Carrasco Kind</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+A">A. Choi</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="2310.00059v2-abstract-short" style="display: inline;"> We search for signatures of cosmological shocks in gas pressure profiles of galaxy clusters using the cluster catalogs from three surveys: the Dark Energy Survey (DES) Year 3, the South Pole Telescope (SPT) SZ survey, and the Atacama Cosmology Telescope (ACT) data releases 4, 5, and 6, and using thermal Sunyaev-Zeldovich (SZ) maps from SPT and ACT. The combined cluster sample contains around… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.00059v2-abstract-full').style.display = 'inline'; document.getElementById('2310.00059v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.00059v2-abstract-full" style="display: none;"> We search for signatures of cosmological shocks in gas pressure profiles of galaxy clusters using the cluster catalogs from three surveys: the Dark Energy Survey (DES) Year 3, the South Pole Telescope (SPT) SZ survey, and the Atacama Cosmology Telescope (ACT) data releases 4, 5, and 6, and using thermal Sunyaev-Zeldovich (SZ) maps from SPT and ACT. The combined cluster sample contains around $10^5$ clusters with mass and redshift ranges $10^{13.7} < M_{\rm 200m}/M_\odot < 10^{15.5}$ and $0.1 < z < 2$, and the total sky coverage of the maps is $\approx 15,000 \,\,{\rm deg}^2$. We find a clear pressure deficit at $R/R_{\rm 200m}\approx 1.1$ in SZ profiles around both ACT and SPT clusters, estimated at $6蟽$ significance, which is qualitatively consistent with a shock-induced thermal non-equilibrium between electrons and ions. The feature is not as clearly determined in profiles around DES clusters. We verify that measurements using SPT or ACT maps are consistent across all scales, including in the deficit feature. The SZ profiles of optically selected and SZ-selected clusters are also consistent for higher mass clusters. Those of less massive, optically selected clusters are suppressed on small scales by factors of 2-5 compared to predictions, and we discuss possible interpretations of this behavior. An oriented stacking of clusters -- where the orientation is inferred from the SZ image, the brightest cluster galaxy, or the surrounding large-scale structure measured using galaxy catalogs -- shows the normalization of the one-halo and two-halo terms vary with orientation. Finally, the location of the pressure deficit feature is statistically consistent with existing estimates of the splashback radius. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.00059v2-abstract-full').style.display = 'none'; document.getElementById('2310.00059v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 September, 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">[v2]: Version accepted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.07221">arXiv:2309.07221</a> <span> [<a href="https://arxiv.org/pdf/2309.07221">pdf</a>, <a href="https://arxiv.org/format/2309.07221">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="Atmospheric and Oceanic Physics">physics.ao-ph</span> </div> </div> <p class="title is-5 mathjax"> CLASS Observations of Atmospheric Cloud Polarization at Millimeter Wavelengths </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yunyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Appel%2C+J+W">John W. Appel</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+C+L">Charles L. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bustos%2C+R">Ricardo Bustos</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+J">Joseph Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Couto%2C+J+D">Jullianna Denes Couto</a>, <a href="/search/astro-ph?searchtype=author&query=Dahal%2C+S">Sumit Dahal</a>, <a href="/search/astro-ph?searchtype=author&query=Datta%2C+R">Rahul Datta</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%BCnner%2C+R">Rolando D眉nner</a>, <a href="/search/astro-ph?searchtype=author&query=Eimer%2C+J+R">Joseph R. Eimer</a>, <a href="/search/astro-ph?searchtype=author&query=Essinger-Hileman%2C+T">Thomas Essinger-Hileman</a>, <a href="/search/astro-ph?searchtype=author&query=Harrington%2C+K">Kathleen Harrington</a>, <a href="/search/astro-ph?searchtype=author&query=Iuliano%2C+J">Jeffrey Iuliano</a>, <a href="/search/astro-ph?searchtype=author&query=Marriage%2C+T+A">Tobias A. Marriage</a>, <a href="/search/astro-ph?searchtype=author&query=Petroff%2C+M+A">Matthew A. Petroff</a>, <a href="/search/astro-ph?searchtype=author&query=Reeves%2C+R+A">Rodrigo A. Reeves</a>, <a href="/search/astro-ph?searchtype=author&query=Rostem%2C+K">Karwan Rostem</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+R">Rui Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Valle%2C+D+A+N">Deniz A. N. Valle</a>, <a href="/search/astro-ph?searchtype=author&query=Watts%2C+D+J">Duncan J. Watts</a>, <a href="/search/astro-ph?searchtype=author&query=Wolff%2C+O+F">Oliver F. Wolff</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+Z">Zhilei Xu</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="2309.07221v1-abstract-short" style="display: inline;"> The dynamic atmosphere imposes challenges to ground-based cosmic microwave background observation, especially for measurements on large angular scales. The hydrometeors in the atmosphere, mostly in the form of clouds, scatter the ambient thermal radiation and are known to be the main linearly polarized source in the atmosphere. This scattering-induced polarization is significantly enhanced for ice… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07221v1-abstract-full').style.display = 'inline'; document.getElementById('2309.07221v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.07221v1-abstract-full" style="display: none;"> The dynamic atmosphere imposes challenges to ground-based cosmic microwave background observation, especially for measurements on large angular scales. The hydrometeors in the atmosphere, mostly in the form of clouds, scatter the ambient thermal radiation and are known to be the main linearly polarized source in the atmosphere. This scattering-induced polarization is significantly enhanced for ice clouds due to the alignment of ice crystals under gravity, which are also the most common clouds seen at the millimeter-astronomy sites at high altitudes. This work presents a multifrequency study of cloud polarization observed by the Cosmology Large Angular Scale Surveyor (CLASS) experiment on Cerro Toco in the Atacama Desert of northern Chile, from 2016 to 2022, at the frequency bands centered around 40, 90, 150, and 220 GHz. Using a machine-learning-assisted cloud classifier, we made connections between the transient polarized emission found in all four frequencies with the clouds imaged by monitoring cameras at the observing site. The polarization angles of the cloud events are found to be mostly $90^\circ$ from the local meridian, which is consistent with the presence of horizontally aligned ice crystals. The 90 and 150 GHz polarization data are consistent with a power law with a spectral index of $3.90\pm0.06$, while an excess/deficit of polarization amplitude is found at 40/220 GHz compared with a Rayleigh scattering spectrum. These results are consistent with Rayleigh-scattering-dominated cloud polarization, with possible effects from supercooled water absorption and/or Mie scattering from a population of large cloud particles that contribute to the 220 GHz polarization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.07221v1-abstract-full').style.display = 'none'; document.getElementById('2309.07221v1-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 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">16 pages, 14 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.05659">arXiv:2309.05659</a> <span> [<a href="https://arxiv.org/pdf/2309.05659">pdf</a>, <a href="https://arxiv.org/format/2309.05659">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad31a5">10.3847/1538-4357/ad31a5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: Cosmology from cross-correlations of unWISE galaxies and ACT DR6 CMB lensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Farren%2C+G+S">Gerrit S. Farren</a>, <a href="/search/astro-ph?searchtype=author&query=Krolewski%2C+A">Alex Krolewski</a>, <a href="/search/astro-ph?searchtype=author&query=MacCrann%2C+N">Niall MacCrann</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">Simone Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Abril-Cabezas%2C+I">Irene Abril-Cabezas</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+R">Rui An</a>, <a href="/search/astro-ph?searchtype=author&query=Atkins%2C+Z">Zachary Atkins</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Darwish%2C+O">Omar Darwish</a>, <a href="/search/astro-ph?searchtype=author&query=Devlin%2C+M+J">Mark J. Devlin</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">Adriaan J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+J+C">J. Colin Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">Matt Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Huffenberger%2C+K+M">Kevin M. Huffenberger</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+J">Joshua Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Louis%2C+T">Thibaut Louis</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Marques%2C+G+A">Gabriela A. Marques</a>, <a href="/search/astro-ph?searchtype=author&query=Moodley%2C+K">Kavilan Moodley</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+L+A">Lyman A. Page</a>, <a href="/search/astro-ph?searchtype=author&query=Partridge%2C+B">Bruce Partridge</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="2309.05659v2-abstract-short" style="display: inline;"> We present tomographic measurements of structure growth using cross-correlations of Atacama Cosmology Telescope (ACT) DR6 and Planck CMB lensing maps with the unWISE Blue and Green galaxy samples, which span the redshift ranges $0.2 \lesssim z \lesssim 1.1$ and $0.3 \lesssim z \lesssim 1.8$, respectively. We improve on prior unWISE cross-correlations not just by making use of the new, high-precisi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05659v2-abstract-full').style.display = 'inline'; document.getElementById('2309.05659v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.05659v2-abstract-full" style="display: none;"> We present tomographic measurements of structure growth using cross-correlations of Atacama Cosmology Telescope (ACT) DR6 and Planck CMB lensing maps with the unWISE Blue and Green galaxy samples, which span the redshift ranges $0.2 \lesssim z \lesssim 1.1$ and $0.3 \lesssim z \lesssim 1.8$, respectively. We improve on prior unWISE cross-correlations not just by making use of the new, high-precision ACT DR6 lensing maps, but also by including additional spectroscopic data for redshift calibration and by analysing our measurements with a more flexible theoretical model. An extensive suite of systematic and null tests within a blind analysis framework ensures that our results are robust. We determine the amplitude of matter fluctuations at low redshifts ($z\simeq 0.2-1.6$), finding $S_8 \equiv 蟽_8 (惟_m / 0.3)^{0.5} = 0.813 \pm 0.021$ using the ACT cross-correlation alone and $S_8 = 0.810 \pm 0.015$ with a combination of Planck and ACT cross-correlations; these measurements are fully consistent with the predictions from primary CMB measurements assuming standard structure growth. The addition of Baryon Acoustic Oscillation data breaks the degeneracy between $蟽_8$ and $惟_m$, allowing us to measure $蟽_8 = 0.813 \pm 0.020$ from the cross-correlation of unWISE with ACT and $蟽_8 = 0.813\pm 0.015$ from the combination of cross-correlations with ACT and Planck. These results also agree with the expectations from primary CMB extrapolations in $螞$CDM cosmology; the consistency of $蟽_8$ derived from our two redshift samples at $z \sim 0.6$ and $1.1$ provides a further check of our cosmological model. Our results suggest that structure formation on linear scales is well described by $螞$CDM even down to low redshifts $z\lesssim 1$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.05659v2-abstract-full').style.display = 'none'; document.getElementById('2309.05659v2-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 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">73 pages (incl. 31 pages of appendices), 52 figures, 16 tables, published in ApJ. Watch G. S. Farren and A. Krolewski discuss the analysis and results under https://cosmologytalks.com/2023/09/11/act-unwise</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2024 ApJ 966 157 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.00675">arXiv:2309.00675</a> <span> [<a href="https://arxiv.org/pdf/2309.00675">pdf</a>, <a href="https://arxiv.org/format/2309.00675">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"> CLASS Angular Power Spectra and Map-Component Analysis for 40 GHz Observations through 2022 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Eimer%2C+J+R">Joseph R. Eimer</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yunyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Brewer%2C+M+K">Michael K. Brewer</a>, <a href="/search/astro-ph?searchtype=author&query=Shi%2C+R">Rui Shi</a>, <a href="/search/astro-ph?searchtype=author&query=Ali%2C+A">Aamir Ali</a>, <a href="/search/astro-ph?searchtype=author&query=Appel%2C+J+W">John W. Appel</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+C+L">Charles L. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bruno%2C+S+M">Sarah Marie Bruno</a>, <a href="/search/astro-ph?searchtype=author&query=Bustos%2C+R">Ricardo Bustos</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+J">Joseph Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Dahal%2C+S">Sumit Dahal</a>, <a href="/search/astro-ph?searchtype=author&query=Datta%2C+R">Rahul Datta</a>, <a href="/search/astro-ph?searchtype=author&query=Couto%2C+J+D">Jullianna Denes Couto</a>, <a href="/search/astro-ph?searchtype=author&query=Denis%2C+K+L">Kevin L. Denis</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%BCnner%2C+R">Rolando D眉nner</a>, <a href="/search/astro-ph?searchtype=author&query=Essinger-Hileman%2C+T">Thomas Essinger-Hileman</a>, <a href="/search/astro-ph?searchtype=author&query=Flux%C3%A1%2C+P">Pedro Flux谩</a>, <a href="/search/astro-ph?searchtype=author&query=Hubmayer%2C+J">Johannes Hubmayer</a>, <a href="/search/astro-ph?searchtype=author&query=Harrington%2C+K">Kathleen Harrington</a>, <a href="/search/astro-ph?searchtype=author&query=Iuliano%2C+J">Jeffrey Iuliano</a>, <a href="/search/astro-ph?searchtype=author&query=Karakla%2C+J">John Karakla</a>, <a href="/search/astro-ph?searchtype=author&query=Marriage%2C+T+A">Tobias A. Marriage</a>, <a href="/search/astro-ph?searchtype=author&query=N%C3%BA%C3%B1ez%2C+C">Carolina N煤帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Parker%2C+L">Lucas Parker</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.00675v2-abstract-short" style="display: inline;"> Measurement of the largest angular scale ($\ell < 30$) features of the cosmic microwave background (CMB) polarization is a powerful way to constrain the optical depth to reionization and search for the signature of inflation through the detection of primordial $B$-modes. We present an analysis of maps covering 73.6\% of the sky made from the $40\,\mathrm{GHz}$ channel of the Cosmology Large Angula… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.00675v2-abstract-full').style.display = 'inline'; document.getElementById('2309.00675v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.00675v2-abstract-full" style="display: none;"> Measurement of the largest angular scale ($\ell < 30$) features of the cosmic microwave background (CMB) polarization is a powerful way to constrain the optical depth to reionization and search for the signature of inflation through the detection of primordial $B$-modes. We present an analysis of maps covering 73.6\% of the sky made from the $40\,\mathrm{GHz}$ channel of the Cosmology Large Angular Scale Surveyor (CLASS) from 2016 August to 2022 May. Taking advantage of the measurement stability enabled by front-end polarization modulation and excellent conditions from the Atacama Desert, we show this channel achieves higher sensitivity than the analogous frequencies from satellite measurements in the range $10 < \ell < 100$. Simulations show the CLASS linear (circular) polarization maps have a white noise level of $125 \,(130)\,\mathrm{渭K\, arcmin}$. We measure the Galaxy-masked $EE$ and $BB$ spectra of diffuse synchrotron radiation and compare to space-based measurements at similar frequencies. In combination with external data, we expand measurements of the spatial variations of the synchrotron spectral energy density (SED) to include new sky regions and measure the diffuse SED in the harmonic domain. We place a new upper limit on a background of circular polarization in the range $5 < \ell < 125$ with the first bin showing $D_\ell < 0.023$ $\mathrm{渭K^2_{CMB}}$ at 95\% confidence. These results establish a new standard for recovery of the largest-scale CMB polarization from the ground and signal exciting possibilities when the higher sensitivity and higher-frequency CLASS channels are included in the analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.00675v2-abstract-full').style.display = 'none'; document.getElementById('2309.00675v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 1 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">38 pages, 25 figures, 6 tables. Accepted to The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.13309">arXiv:2308.13309</a> <span> [<a href="https://arxiv.org/pdf/2308.13309">pdf</a>, <a href="https://arxiv.org/format/2308.13309">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4365/ad50a0">10.3847/1538-4365/ad50a0 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Cosmology Large Angular Scale Surveyor (CLASS): 90 GHz Telescope Pointing, Beam Profile, Window Function, and Polarization Performance </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Datta%2C+R">Rahul Datta</a>, <a href="/search/astro-ph?searchtype=author&query=Brewer%2C+M+K">Michael K. Brewer</a>, <a href="/search/astro-ph?searchtype=author&query=Couto%2C+J+D">Jullianna Denes Couto</a>, <a href="/search/astro-ph?searchtype=author&query=Eimer%2C+J">Joseph Eimer</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Y">Yunyang Li</a>, <a href="/search/astro-ph?searchtype=author&query=Xu%2C+Z">Zhilei Xu</a>, <a href="/search/astro-ph?searchtype=author&query=Ali%2C+A">Aamir Ali</a>, <a href="/search/astro-ph?searchtype=author&query=Appel%2C+J+W">John W. Appel</a>, <a href="/search/astro-ph?searchtype=author&query=Bennett%2C+C+L">Charles L. Bennett</a>, <a href="/search/astro-ph?searchtype=author&query=Bustos%2C+R">Ricardo Bustos</a>, <a href="/search/astro-ph?searchtype=author&query=Chuss%2C+D+T">David T. Chuss</a>, <a href="/search/astro-ph?searchtype=author&query=Cleary%2C+J">Joseph Cleary</a>, <a href="/search/astro-ph?searchtype=author&query=Dahal%2C+S">Sumit Dahal</a>, <a href="/search/astro-ph?searchtype=author&query=Espinoza%2C+F">Francisco Espinoza</a>, <a href="/search/astro-ph?searchtype=author&query=Essinger-Hileman%2C+T">Thomas Essinger-Hileman</a>, <a href="/search/astro-ph?searchtype=author&query=Flux%C3%A1%2C+P">Pedro Flux谩</a>, <a href="/search/astro-ph?searchtype=author&query=Harrington%2C+K">Kathleen Harrington</a>, <a href="/search/astro-ph?searchtype=author&query=Helson%2C+K">Kyle Helson</a>, <a href="/search/astro-ph?searchtype=author&query=Iuliano%2C+J">Jeffrey Iuliano</a>, <a href="/search/astro-ph?searchtype=author&query=Karakla%2C+J">John Karakla</a>, <a href="/search/astro-ph?searchtype=author&query=Marriage%2C+T+A">Tobias A. Marriage</a>, <a href="/search/astro-ph?searchtype=author&query=Novack%2C+S">Sasha Novack</a>, <a href="/search/astro-ph?searchtype=author&query=N%C3%BA%C3%B1ez%2C+C">Carolina N煤帽ez</a>, <a href="/search/astro-ph?searchtype=author&query=Padilla%2C+I+L">Ivan L. Padilla</a>, <a href="/search/astro-ph?searchtype=author&query=Parker%2C+L">Lucas Parker</a> , et al. (9 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="2308.13309v2-abstract-short" style="display: inline;"> The Cosmology Large Angular Scale Surveyor (CLASS) is a telescope array that observes the cosmic microwave background (CMB) over ~75% of the sky from the Atacama Desert, Chile, at frequency bands centered near 40, 90, 150, and 220 GHz. CLASS measures the large angular scale CMB polarization to constrain the tensor-to-scalar ratio and the optical depth to last scattering. This paper presents the op… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13309v2-abstract-full').style.display = 'inline'; document.getElementById('2308.13309v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.13309v2-abstract-full" style="display: none;"> The Cosmology Large Angular Scale Surveyor (CLASS) is a telescope array that observes the cosmic microwave background (CMB) over ~75% of the sky from the Atacama Desert, Chile, at frequency bands centered near 40, 90, 150, and 220 GHz. CLASS measures the large angular scale CMB polarization to constrain the tensor-to-scalar ratio and the optical depth to last scattering. This paper presents the optical characterization of the 90GHz telescope, which has been observing since July 2018. Observations of the Moon establish the pointing while dedicated observations of Jupiter are used for beam calibration. The standard deviations of the pointing error in azimuth, elevation, and boresight angle are 1.3, 2.1, and 2.0 arcminutes, respectively, over the first 3 years of observations. This corresponds to a pointing uncertainty ~7% of the beam's full width at half maximum (FWHM). The effective azimuthally-symmetrized instrument 1D beam estimated at 90 GHz has an FWHM of 0.620+/-0.003 deg and a solid angle of 138.7+/-0.6(stats.)+/-1.1(sys.) usr integrated to a radius of 4 deg. The corresponding beam window function drops to b_ell^2 = 0.93, 0.71, 0.14 at ell = 30, 100, 300, respectively. Far-sidelobes are studied using detector-centered intensity maps of the Moon and measured to be at a level of 10^-3 or below relative to the peak. The polarization angle of Tau A estimated from preliminary survey maps is 149.6+/-0.2(stats.) deg in equatorial coordinates. The instrumental temperature-to-polarization (T-to-P) leakage fraction, inferred from per-detector demodulated Jupiter scan data, has a monopole component at the level of 1.7 x 10^-3, a dipole component with an amplitude of 4.3 x 10^-3, with no evidence of quadrupolar leakage. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13309v2-abstract-full').style.display = 'none'; document.getElementById('2308.13309v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 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">24 pages, 18 figures, submitted to ApJS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal Supplement Series, Volume 273, Number 2 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.06352">arXiv:2307.06352</a> <span> [<a href="https://arxiv.org/pdf/2307.06352">pdf</a>, <a href="https://arxiv.org/format/2307.06352">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: Galactic Dust Structure and the Cosmic PAH Background in Cross-correlation with WISE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rosado%2C+R+C">Rodrigo C贸rdova Rosado</a>, <a href="/search/astro-ph?searchtype=author&query=Hensley%2C+B+S">Brandon S. Hensley</a>, <a href="/search/astro-ph?searchtype=author&query=Clark%2C+S+E">Susan E. Clark</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">Adriaan J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Atkins%2C+Z">Zachary Atkins</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">Elia Stefano Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+S+K">Steve K. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Dunkley%2C+J">Jo Dunkley</a>, <a href="/search/astro-ph?searchtype=author&query=Herv%C3%ADas-Caimapo%2C+C">Carlos Herv铆as-Caimapo</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Z">Zack Li</a>, <a href="/search/astro-ph?searchtype=author&query=Louis%2C+T">Thibaut Louis</a>, <a href="/search/astro-ph?searchtype=author&query=Naess%2C+S">Sigurd Naess</a>, <a href="/search/astro-ph?searchtype=author&query=Page%2C+L+A">Lyman A. Page</a>, <a href="/search/astro-ph?searchtype=author&query=Partridge%2C+B">Bruce Partridge</a>, <a href="/search/astro-ph?searchtype=author&query=Sif%C3%B3n%2C+C">Crist贸bal Sif贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Staggs%2C+S+T">Suzanne T. Staggs</a>, <a href="/search/astro-ph?searchtype=author&query=Vargas%2C+C">Cristian Vargas</a>, <a href="/search/astro-ph?searchtype=author&query=Wollack%2C+E+J">Edward J. Wollack</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="2307.06352v1-abstract-short" style="display: inline;"> We present a cross-correlation analysis between $1'$ resolution total intensity and polarization observations from the Atacama Cosmology Telescope (ACT) at 150 and 220 GHz and 15$''$ mid-infrared photometry from the Wide-field Infrared Survey Explorer (WISE) over 107 12.5$^\circ\times$12.5$^\circ$ patches of sky. We detect a spatially isotropic signal in the WISE$\times$ACT $TT$ cross power spectr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.06352v1-abstract-full').style.display = 'inline'; document.getElementById('2307.06352v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.06352v1-abstract-full" style="display: none;"> We present a cross-correlation analysis between $1'$ resolution total intensity and polarization observations from the Atacama Cosmology Telescope (ACT) at 150 and 220 GHz and 15$''$ mid-infrared photometry from the Wide-field Infrared Survey Explorer (WISE) over 107 12.5$^\circ\times$12.5$^\circ$ patches of sky. We detect a spatially isotropic signal in the WISE$\times$ACT $TT$ cross power spectrum at 30$蟽$ significance that we interpret as the correlation between the cosmic infrared background at ACT frequencies and polycyclic aromatic hydrocarbon (PAH) emission from galaxies in WISE, i.e., the cosmic PAH background. Within the Milky Way, the Galactic dust $TT$ spectra are generally well-described by power laws in $\ell$ over the range 10$^3 < \ell < $10$^4$, but there is evidence both for variability in the power law index and for non-power law behavior in some regions. We measure a positive correlation between WISE total intensity and ACT $E$-mode polarization at 1000$ < \ell \lesssim $6000 at $>$3$蟽$ in each of 35 distinct $\sim$100 deg$^2$ regions of the sky, suggesting alignment between Galactic density structures and the local magnetic field persists to sub-parsec physical scales in these regions. The distribution of $TE$ amplitudes in this $\ell$ range across all 107 regions is biased to positive values, while there is no evidence for such a bias in the $TB$ spectra. This work constitutes the highest-$\ell$ measurements of the Galactic dust $TE$ spectrum to date and indicates that cross-correlation with high-resolution mid-infrared measurements of dust emission is a promising tool for constraining the spatial statistics of dust emission at millimeter wavelengths. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.06352v1-abstract-full').style.display = 'none'; document.getElementById('2307.06352v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 14 figures, submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.01258">arXiv:2307.01258</a> <span> [<a href="https://arxiv.org/pdf/2307.01258">pdf</a>, <a href="https://arxiv.org/format/2307.01258">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> The Atacama Cosmology Telescope: High-resolution component-separated maps across one-third of the sky </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Coulton%2C+W+R">William R. Coulton</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">Mathew S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Duivenvoorden%2C+A+J">Adriaan J. Duivenvoorden</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+J+C">J. Colin Hill</a>, <a href="/search/astro-ph?searchtype=author&query=Abril-Cabezas%2C+I">Irene Abril-Cabezas</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">Peter A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Aiola%2C+S">Simone Aiola</a>, <a href="/search/astro-ph?searchtype=author&query=Alford%2C+T">Tommy Alford</a>, <a href="/search/astro-ph?searchtype=author&query=Amiri%2C+M">Mandana Amiri</a>, <a href="/search/astro-ph?searchtype=author&query=Amodeo%2C+S">Stefania Amodeo</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+R">Rui An</a>, <a href="/search/astro-ph?searchtype=author&query=Atkins%2C+Z">Zachary Atkins</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J+E">Jason E. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">Nicholas Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Battistelli%2C+E+S">Elia Stefano Battistelli</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J+A">James A. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=Bean%2C+R">Rachel Bean</a>, <a href="/search/astro-ph?searchtype=author&query=Beringue%2C+B">Benjamin Beringue</a>, <a href="/search/astro-ph?searchtype=author&query=Bhandarkar%2C+T">Tanay Bhandarkar</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+E">Emily Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Bolliet%2C+B">Boris Bolliet</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+H">Hongbo Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">Erminia Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Calafut%2C+V">Victoria Calafut</a> , et al. (129 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.01258v1-abstract-short" style="display: inline;"> Observations of the millimeter sky contain valuable information on a number of signals, including the blackbody cosmic microwave background (CMB), Galactic emissions, and the Compton-$y$ distortion due to the thermal Sunyaev-Zel'dovich (tSZ) effect. Extracting new insight into cosmological and astrophysical questions often requires combining multi-wavelength observations to spectrally isolate one… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01258v1-abstract-full').style.display = 'inline'; document.getElementById('2307.01258v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.01258v1-abstract-full" style="display: none;"> Observations of the millimeter sky contain valuable information on a number of signals, including the blackbody cosmic microwave background (CMB), Galactic emissions, and the Compton-$y$ distortion due to the thermal Sunyaev-Zel'dovich (tSZ) effect. Extracting new insight into cosmological and astrophysical questions often requires combining multi-wavelength observations to spectrally isolate one component. In this work, we present a new arcminute-resolution Compton-$y$ map, which traces out the line-of-sight-integrated electron pressure, as well as maps of the CMB in intensity and E-mode polarization, across a third of the sky (around 13,000 sq.~deg.). We produce these through a joint analysis of data from the Atacama Cosmology Telescope (ACT) Data Release 4 and 6 at frequencies of roughly 93, 148, and 225 GHz, together with data from the \textit{Planck} satellite at frequencies between 30 GHz and 545 GHz. We present detailed verification of an internal linear combination pipeline implemented in a needlet frame that allows us to efficiently suppress Galactic contamination and account for spatial variations in the ACT instrument noise. These maps provide a significant advance, in noise levels and resolution, over the existing \textit{Planck} component-separated maps and will enable a host of science goals including studies of cluster and galaxy astrophysics, inferences of the cosmic velocity field, primordial non-Gaussianity searches, and gravitational lensing reconstruction of the CMB. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.01258v1-abstract-full').style.display = 'none'; document.getElementById('2307.01258v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">The Compton-y map and associated products will be made publicly available upon publication of the paper. The CMB T and E mode maps will be made available when the DR6 maps are made public</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.17268">arXiv:2306.17268</a> <span> [<a href="https://arxiv.org/pdf/2306.17268">pdf</a>, <a href="https://arxiv.org/format/2306.17268">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"> Cosmological constraints from the tomography of DES-Y3 galaxies with CMB lensing from ACT DR4 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Marques%2C+G+A">G. A. Marques</a>, <a href="/search/astro-ph?searchtype=author&query=Madhavacheril%2C+M+S">M. S. Madhavacheril</a>, <a href="/search/astro-ph?searchtype=author&query=Darwish%2C+O">O. Darwish</a>, <a href="/search/astro-ph?searchtype=author&query=Shaikh%2C+S">S. Shaikh</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Baxter%2C+E+J">E. J. Baxter</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+M+R">M. R. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Blazek%2C+J">J. Blazek</a>, <a href="/search/astro-ph?searchtype=author&query=Bond%2C+J+R">J. Richard Bond</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Cai%2C+H">H. Cai</a>, <a href="/search/astro-ph?searchtype=author&query=Calabrese%2C+E">E. Calabrese</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+M+C+K+J">M. Carrasco Kind J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Cawthon%2C+R">R. Cawthon</a>, <a href="/search/astro-ph?searchtype=author&query=Crocce%2C+M">M. Crocce</a>, <a href="/search/astro-ph?searchtype=author&query=da+Costa%2C+L+N">L. N. da Costa</a>, <a href="/search/astro-ph?searchtype=author&query=Pereira%2C+M+E+S">M. E. S. Pereira</a>, <a href="/search/astro-ph?searchtype=author&query=De+Vicente%2C+J">J. De Vicente</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a> , et al. (70 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.17268v2-abstract-short" style="display: inline;"> We present a measurement of the cross-correlation between the MagLim galaxies selected from the Dark Energy Survey (DES) first three years of observations (Y3) and cosmic microwave background (CMB) lensing from the Atacama Cosmology Telescope (ACT) Data Release 4 (DR4), reconstructed over $\sim 436$ sq.deg. of the sky. Our galaxy sample, which covers $\sim 4143$ sq.deg., is divided into six redshi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17268v2-abstract-full').style.display = 'inline'; document.getElementById('2306.17268v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.17268v2-abstract-full" style="display: none;"> We present a measurement of the cross-correlation between the MagLim galaxies selected from the Dark Energy Survey (DES) first three years of observations (Y3) and cosmic microwave background (CMB) lensing from the Atacama Cosmology Telescope (ACT) Data Release 4 (DR4), reconstructed over $\sim 436$ sq.deg. of the sky. Our galaxy sample, which covers $\sim 4143$ sq.deg., is divided into six redshift bins spanning the redshift range of $0.20<z<1.05$. We adopt a blinding procedure until passing all consistency and systematics tests. After imposing scale cuts for the cross-power spectrum measurement, we reject the null hypothesis of no correlation at 9.1蟽. We constrain cosmological parameters from a joint analysis of galaxy and CMB lensing-galaxy power spectra considering a flat \LCDM model, marginalized over 23 astrophysical and systematic nuisance parameters. We find the clustering amplitude $S_8\equiv 蟽_8 (惟_m/0.3)^{0.5} = 0.75^{+0.04}_{-0.05}$. In addition, we constrain the linear growth of cosmic structure as a function of redshift. Our results are consistent with recent DES Y3 analyses and suggest a preference for a lower $S_8$ compared to results from measurements of CMB anisotropies by the Planck satellite, although at a mild level ($< 2 蟽$) of statistical significance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.17268v2-abstract-full').style.display = 'none'; document.getElementById('2306.17268v2-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 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">42 pages, 17 figures</span> </p> </li> </ol> <nav 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