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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=Allam%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Allam%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Allam%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Allam%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Allam%2C+S&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Allam%2C+S&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/2502.12914">arXiv:2502.12914</a> <span> [<a href="https://arxiv.org/pdf/2502.12914">pdf</a>, <a href="https://arxiv.org/format/2502.12914">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"> Selection Function of Clusters in Dark Energy Survey Year 3 Data from Cross-Matching with South Pole Telescope Detections </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/astro-ph?searchtype=author&query=Costanzi%2C+M">M. Costanzi</a>, <a href="/search/astro-ph?searchtype=author&query=Mohr%2C+J+J">J. J. Mohr</a>, <a href="/search/astro-ph?searchtype=author&query=Bleem%2C+L+E">L. E. Bleem</a>, <a href="/search/astro-ph?searchtype=author&query=Wu%2C+H+-">H. -Y. Wu</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</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=Carretero%2C+J">J. Carretero</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=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Diehl%2C+H+T">H. T. Diehl</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+S">S. Everett</a>, <a href="/search/astro-ph?searchtype=author&query=Flaugher%2C+B">B. Flaugher</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Bellido%2C+J">J. Garc铆a-Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Gaztanaga%2C+E">E. Gaztanaga</a>, <a href="/search/astro-ph?searchtype=author&query=Gruen%2C+D">D. Gruen</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">R. A. Gruendl</a> , et al. (30 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="2502.12914v1-abstract-short" style="display: inline;"> Galaxy clusters selected based on overdensities of galaxies in photometric surveys provide the largest cluster samples. Yet modeling the selection function of such samples is complicated by non-cluster members projected along the line of sight (projection effects) and the potential detection of unvirialized objects (contamination). We empirically constrain the magnitude of these effects by cross-m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.12914v1-abstract-full').style.display = 'inline'; document.getElementById('2502.12914v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.12914v1-abstract-full" style="display: none;"> Galaxy clusters selected based on overdensities of galaxies in photometric surveys provide the largest cluster samples. Yet modeling the selection function of such samples is complicated by non-cluster members projected along the line of sight (projection effects) and the potential detection of unvirialized objects (contamination). We empirically constrain the magnitude of these effects by cross-matching galaxy clusters selected in the Dark Energy survey data with the \rdmpr$\,$ algorithm with significant detections in three South Pole Telescope surveys (SZ, pol-ECS, pol-500d). For matched clusters, we augment the \rdmpr$\,$catalog by the SPT detection significance. For unmatched objects we use the SPT detection threshold as an upper limit on the SZe signature. Using a Bayesian population model applied to the collected multi-wavelength data, we explore various physically motivated models to describe the relationship between observed richness and halo mass. Our analysis reveals the limitations of a simple lognormal scatter model in describing the data. We rule out significant contamination by unvirialized objects at the high-richness end of the sample. While dedicated simulations offer a well-fitting calibration of projection effects, our findings suggest the presence of redshift-dependent trends that these simulations may not have captured. Our findings highlight that modeling the selection function of optically detected clusters remains a complicated challenge, requiring a combination of simulation and data-driven approaches. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.12914v1-abstract-full').style.display = 'none'; document.getElementById('2502.12914v1-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 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">19 pages, 11 figures, submitted to A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.19117">arXiv:2501.19117</a> <span> [<a href="https://arxiv.org/pdf/2501.19117">pdf</a>, <a href="https://arxiv.org/format/2501.19117">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"> It's not $蟽_8$ : constraining the non-linear matter power spectrum with the Dark Energy Survey Year-5 supernova sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">Paul Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">R. Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+M+S+S">M. S. S. Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Huterer%2C+D">D. Huterer</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffrey%2C+N">N. Jeffrey</a>, <a href="/search/astro-ph?searchtype=author&query=Lahav%2C+O">O. Lahav</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Whiteway%2C+L">L. Whiteway</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">J. Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Blazek%2C+J">J. Blazek</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=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">C. Conselice</a> , et al. (36 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.19117v1-abstract-short" style="display: inline;"> The weak gravitational lensing magnification of Type Ia supernovae (SNe Ia) is sensitive to the matter power spectrum on scales $k>1 h$ Mpc$^{-1}$, making it unwise to interpret SNe Ia lensing in terms of power on linear scales. We compute the probability density function of SNe Ia magnification as a function of standard cosmological parameters, plus an empirical parameter $A_{\rm mod}$ which desc… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.19117v1-abstract-full').style.display = 'inline'; document.getElementById('2501.19117v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.19117v1-abstract-full" style="display: none;"> The weak gravitational lensing magnification of Type Ia supernovae (SNe Ia) is sensitive to the matter power spectrum on scales $k>1 h$ Mpc$^{-1}$, making it unwise to interpret SNe Ia lensing in terms of power on linear scales. We compute the probability density function of SNe Ia magnification as a function of standard cosmological parameters, plus an empirical parameter $A_{\rm mod}$ which describes the suppression or enhancement of matter power on non-linear scales compared to a cold dark matter only model. While baryons are expected to enhance power on the scales relevant to SN Ia lensing, other physics such as neutrino masses or non-standard dark matter may suppress power. Using the Dark Energy Survey Year-5 sample, we find $A_{\rm mod} = 0.77^{+0.69}_{-0.40}$ (68\% credible interval around the median). Although the median is consistent with unity there are hints of power suppression, with $A_{\rm mod} < 1.09$ at 68\% credibility. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.19117v1-abstract-full').style.display = 'none'; document.getElementById('2501.19117v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 January, 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">12 pages, submitted to MNRAS. arXiv admin note: text overlap with arXiv:2410.07956</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DES-2024-0863 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.15679">arXiv:2501.15679</a> <span> [<a href="https://arxiv.org/pdf/2501.15679">pdf</a>, <a href="https://arxiv.org/format/2501.15679">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"> Discovering Strong Gravitational Lenses in the Dark Energy Survey with Interactive Machine Learning and Crowd-sourced Inspection with Space Warps </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez%2C+J">J. Gonz谩lez</a>, <a href="/search/astro-ph?searchtype=author&query=Holloway%2C+P">P. Holloway</a>, <a href="/search/astro-ph?searchtype=author&query=Collett%2C+T">T. Collett</a>, <a href="/search/astro-ph?searchtype=author&query=Verma%2C+A">A. Verma</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+P">P. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=More%2C+A">A. More</a>, <a href="/search/astro-ph?searchtype=author&query=Barroso%2C+J+A">J. Acevedo Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Cartwright%2C+G">G. Cartwright</a>, <a href="/search/astro-ph?searchtype=author&query=Martinez%2C+M">M. Martinez</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+T">T. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+K">K. Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Schuldt%2C+S">S. Schuldt</a>, <a href="/search/astro-ph?searchtype=author&query=Birrer%2C+S">S. Birrer</a>, <a href="/search/astro-ph?searchtype=author&query=Diehl%2C+H+T">H. T. Diehl</a>, <a href="/search/astro-ph?searchtype=author&query=Morgan%2C+R">R. Morgan</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">A. Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Donnell%2C+J+H">J. H. O'Donnell</a>, <a href="/search/astro-ph?searchtype=author&query=Zaborowski%2C+E">E. Zaborowski</a>, <a href="/search/astro-ph?searchtype=author&query=Nord%2C+B">B. Nord</a>, <a href="/search/astro-ph?searchtype=author&query=Baeten%2C+E+M">E. M. Baeten</a>, <a href="/search/astro-ph?searchtype=author&query=Johnson%2C+L+C">L. C. Johnson</a>, <a href="/search/astro-ph?searchtype=author&query=Macmillan%2C+C">C. Macmillan</a>, <a href="/search/astro-ph?searchtype=author&query=Roodman%2C+A">A. Roodman</a>, <a href="/search/astro-ph?searchtype=author&query=Pieres%2C+A">A. Pieres</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="2501.15679v1-abstract-short" style="display: inline;"> We conduct a search for strong gravitational lenses in the Dark Energy Survey (DES) Year 6 imaging data. We implement a pre-trained Vision Transformer (ViT) for our machine learning (ML) architecture and adopt Interactive Machine Learning to construct a training sample with multiple classes to address common types of false positives. Our ML model reduces 236 million DES cutout images to 22,564 tar… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.15679v1-abstract-full').style.display = 'inline'; document.getElementById('2501.15679v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.15679v1-abstract-full" style="display: none;"> We conduct a search for strong gravitational lenses in the Dark Energy Survey (DES) Year 6 imaging data. We implement a pre-trained Vision Transformer (ViT) for our machine learning (ML) architecture and adopt Interactive Machine Learning to construct a training sample with multiple classes to address common types of false positives. Our ML model reduces 236 million DES cutout images to 22,564 targets of interest, including around 85% of previously reported galaxy-galaxy lens candidates discovered in DES. These targets were visually inspected by citizen scientists, who ruled out approximately 90% as false positives. Of the remaining 2,618 candidates, 149 were expert-classified as 'definite' lenses and 516 as 'probable' lenses, with 147 of these candidates being newly identified. Additionally, we trained a second ViT to find double-source plane lens systems, finding at least one double-source system. Our main ViT excels at identifying galaxy-galaxy lenses, consistently assigning high scores to candidates with high confidence. The top 800 ViT-scored images include around 100 of our `definite' lens candidates. This selection is an order of magnitude higher in purity than previous convolutional neural network-based lens searches and demonstrates the feasibility of applying our methodology for discovering large samples of lenses in future surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.15679v1-abstract-full').style.display = 'none'; document.getElementById('2501.15679v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 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">Report number:</span> FERMILAB-PUB-25-0038 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.06664">arXiv:2501.06664</a> <span> [<a href="https://arxiv.org/pdf/2501.06664">pdf</a>, <a href="https://arxiv.org/format/2501.06664">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"> Comparing the DES-SN5YR and Pantheon+ SN cosmology analyses: Investigation based on "Evolving Dark Energy or Supernovae systematics?" </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">R. Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B">B. Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a> , et al. (43 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="2501.06664v1-abstract-short" style="display: inline;"> Recent cosmological analyses measuring distances of Type Ia Supernovae (SNe Ia) and Baryon Acoustic Oscillations (BAO) have all given similar hints at time-evolving dark energy. To examine whether underestimated SN Ia systematics might be driving these results, Efstathiou (2024) compared overlapping SN events between Pantheon+ and DES-SN5YR (20% SNe are in common), and reported evidence for a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06664v1-abstract-full').style.display = 'inline'; document.getElementById('2501.06664v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.06664v1-abstract-full" style="display: none;"> Recent cosmological analyses measuring distances of Type Ia Supernovae (SNe Ia) and Baryon Acoustic Oscillations (BAO) have all given similar hints at time-evolving dark energy. To examine whether underestimated SN Ia systematics might be driving these results, Efstathiou (2024) compared overlapping SN events between Pantheon+ and DES-SN5YR (20% SNe are in common), and reported evidence for a $\sim$0.04 mag offset between the low and high-redshift distance measurements of this subsample of events. If these offsets are arbitrarily subtracted from the entire DES-SN5YR sample, the preference for evolving dark energy is reduced. In this paper, we reproduce this offset and show that it has two sources. First, 43% of the offset is due to DES-SN5YR improvements in the modelling of supernova intrinsic scatter and host galaxy properties. These are scientifically-motivated modelling updates implemented in DES-SN5YR and their associated uncertainties are captured within the DES-SN5YR systematic error budget. Even if the less accurate scatter model and host properties from Pantheon+ are used instead, the DES-SN5YR evidence for evolving dark energy is only reduced from 3.9$蟽$ to 3.3$蟽$. Second, 38% of the offset is due to a misleading comparison because different selection functions characterize the DES subsets included in Pantheon+ and DES-SN5YR and therefore individual SN distance measurements are expected to be different because of different bias corrections. In conclusion, we confirm the validity of the published DES-SN5YR results. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06664v1-abstract-full').style.display = 'none'; document.getElementById('2501.06664v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 January, 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">9 pages, 5 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/2501.05739">arXiv:2501.05739</a> <span> [<a href="https://arxiv.org/pdf/2501.05739">pdf</a>, <a href="https://arxiv.org/format/2501.05739">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"> Dark Energy Survey Year 6 Results: Photometric Data Set for Cosmology </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Sevilla-Noarbe%2C+I">I. Sevilla-Noarbe</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">A. Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Yanny%2C+B">B. Yanny</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">R. A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Sheldon%2C+E">E. Sheldon</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</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=Adamow%2C+M">M. Adamow</a>, <a href="/search/astro-ph?searchtype=author&query=Anbajagane%2C+D">D. Anbajagane</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=Bernstein%2C+G+M">G. M. Bernstein</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=Gschwend%2C+J">J. Gschwend</a>, <a href="/search/astro-ph?searchtype=author&query=Gorsuch%2C+M">M. Gorsuch</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+W+G">W. G. Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M">M. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Jeltema%2C+T">T. Jeltema</a>, <a href="/search/astro-ph?searchtype=author&query=Kron%2C+R">R. Kron</a>, <a href="/search/astro-ph?searchtype=author&query=Manning%2C+T+A">T. A. Manning</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Donnell%2C+J">J. O'Donnell</a>, <a href="/search/astro-ph?searchtype=author&query=Pieres%2C+A">A. Pieres</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez-Monroy%2C+M">M. Rodr铆guez-Monroy</a>, <a href="/search/astro-ph?searchtype=author&query=Cid%2C+D+S">D. Sanchez Cid</a>, <a href="/search/astro-ph?searchtype=author&query=Tabbutt%2C+M">M. Tabbutt</a> , et al. (81 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="2501.05739v2-abstract-short" style="display: inline;"> We describe the photometric data set assembled from the full six years of observations by the Dark Energy Survey (DES) in support of static-sky cosmology analyses. DES Y6 Gold is a curated data set derived from DES Data Release 2 (DR2) that incorporates improved measurement, photometric calibration, object classification and value added information. Y6 Gold comprises nearly $5000~{\rm deg}^2$ of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05739v2-abstract-full').style.display = 'inline'; document.getElementById('2501.05739v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.05739v2-abstract-full" style="display: none;"> We describe the photometric data set assembled from the full six years of observations by the Dark Energy Survey (DES) in support of static-sky cosmology analyses. DES Y6 Gold is a curated data set derived from DES Data Release 2 (DR2) that incorporates improved measurement, photometric calibration, object classification and value added information. Y6 Gold comprises nearly $5000~{\rm deg}^2$ of $grizY$ imaging in the south Galactic cap and includes 669 million objects with a depth of $i_{AB} \sim 23.4$ mag at S/N $\sim 10$ for extended objects and a top-of-the-atmosphere photometric uniformity $< 2~{\rm mmag}$. Y6 Gold augments DES DR2 with simultaneous fits to multi-epoch photometry for more robust galaxy shapes, colors, and photometric redshift estimates. Y6 Gold features improved morphological star-galaxy classification with efficiency $98.6\%$ and contamination $0.8\%$ for galaxies with $17.5 < i_{AB} < 22.5$. Additionally, it includes per-object quality information, and accompanying maps of the footprint coverage, masked regions, imaging depth, survey conditions, and astrophysical foregrounds that are used for cosmology analyses. After quality selections, benchmark samples contain 448 million galaxies and 120 million stars. This paper will be complemented by online data access and documentation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05739v2-abstract-full').style.display = 'none'; document.getElementById('2501.05739v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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">Data products and documentation are publicly available at https://des.ncsa.illinois.edu/releases</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.05683">arXiv:2501.05683</a> <span> [<a href="https://arxiv.org/pdf/2501.05683">pdf</a>, <a href="https://arxiv.org/format/2501.05683">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"> Dark Energy Survey Year 6 Results: Synthetic-source Injection Across the Full Survey Using Balrog </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=Tabbutt%2C+M">M. Tabbutt</a>, <a href="/search/astro-ph?searchtype=author&query=Beas-Gonzalez%2C+J">J. Beas-Gonzalez</a>, <a href="/search/astro-ph?searchtype=author&query=Yanny%2C+B">B. Yanny</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+S">S. Everett</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=Yamamoto%2C+M">M. Yamamoto</a>, <a href="/search/astro-ph?searchtype=author&query=Legnani%2C+E">E. Legnani</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=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Elvin-Poole%2C+J">J. Elvin-Poole</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=Choi%2C+A">A. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Gatti%2C+M">M. Gatti</a>, <a href="/search/astro-ph?searchtype=author&query=Giannini%2C+G">G. Giannini</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">R. A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M">M. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+S">S. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Mena-Fern%C3%A1ndez%2C+J">J. Mena-Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Porredon%2C+A">A. Porredon</a>, <a href="/search/astro-ph?searchtype=author&query=Rodriguez-Monroy%2C+M">M. Rodriguez-Monroy</a>, <a href="/search/astro-ph?searchtype=author&query=Rozo%2C+E">E. Rozo</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Schutt%2C+T">T. Schutt</a>, <a href="/search/astro-ph?searchtype=author&query=Sheldon%2C+E">E. Sheldon</a> , et al. (56 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="2501.05683v1-abstract-short" style="display: inline;"> Synthetic source injection (SSI), the insertion of sources into pixel-level on-sky images, is a powerful method for characterizing object detection and measurement in wide-field, astronomical imaging surveys. Within the Dark Energy Survey (DES), SSI plays a critical role in characterizing all necessary algorithms used in converting images to catalogs, and in deriving quantities needed for the cosm… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05683v1-abstract-full').style.display = 'inline'; document.getElementById('2501.05683v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.05683v1-abstract-full" style="display: none;"> Synthetic source injection (SSI), the insertion of sources into pixel-level on-sky images, is a powerful method for characterizing object detection and measurement in wide-field, astronomical imaging surveys. Within the Dark Energy Survey (DES), SSI plays a critical role in characterizing all necessary algorithms used in converting images to catalogs, and in deriving quantities needed for the cosmology analysis, such as object detection rates, galaxy redshift estimation, galaxy magnification, star-galaxy classification, and photometric performance. We present here a source injection catalog of $146$ million injections spanning the entire 5000 deg$^2$ DES footprint, generated using the Balrog SSI pipeline. Through this sample, we demonstrate that the DES Year 6 (Y6) image processing pipeline provides accurate estimates of the object properties, for both galaxies and stars, at the percent-level, and we highlight specific regimes where the accuracy is reduced. We then show the consistency between SSI and data catalogs, for all galaxy samples developed within the weak lensing and galaxy clustering analyses of DES Y6. The consistency between the two catalogs also extends to their correlations with survey observing properties (seeing, airmass, depth, extinction, etc.). Finally, we highlight a number of applications of this catalog to the DES Y6 cosmology analysis. This dataset is the largest SSI catalog produced at this fidelity and will serve as a key testing ground for exploring the utility of SSI catalogs in upcoming surveys such as the Vera C. Rubin Observatory Legacy Survey of Space and Time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05683v1-abstract-full').style.display = 'none'; document.getElementById('2501.05683v1-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.01551">arXiv:2501.01551</a> <span> [<a href="https://arxiv.org/pdf/2501.01551">pdf</a>, <a href="https://arxiv.org/format/2501.01551">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> </div> </div> <p class="title is-5 mathjax"> Photometry of outer Solar System objects from the Dark Energy Survey II: a joint analysis of trans-Neptunian absolute magnitudes, colors, lightcurves and dynamics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bernardinelli%2C+P+H">Pedro H. Bernardinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+G+M">Gary M. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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=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=Carretero%2C+J">J. Carretero</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=Davis%2C+T+M">T. M. Davis</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=Diehl%2C+H+T">H. T. Diehl</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+S">S. Everett</a>, <a href="/search/astro-ph?searchtype=author&query=Flaugher%2C+B">B. Flaugher</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Bellido%2C+J">J. Garc铆a-Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Gaztanaga%2C+E">E. Gaztanaga</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">R. A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Gutierrez%2C+G">G. Gutierrez</a>, <a href="/search/astro-ph?searchtype=author&query=Herner%2C+K">K. Herner</a>, <a href="/search/astro-ph?searchtype=author&query=Hinton%2C+S+R">S. R. Hinton</a>, <a href="/search/astro-ph?searchtype=author&query=Hollowood%2C+D+L">D. L. Hollowood</a> , et al. (21 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.01551v1-abstract-short" style="display: inline;"> For the 696 trans-Neptunian objects (TNOs) with absolute magnitudes $5.5 < H_r < 8.2$ detected in the Dark Energy Survey (DES), we characterize the relationships between their dynamical state and physical properties -- namely $H_r$, indicating size; colors, indicating surface composition; and flux variation semi-amplitude $A$, indicating asphericity and surface inhomogeneity. We seek ``birth'' phy… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.01551v1-abstract-full').style.display = 'inline'; document.getElementById('2501.01551v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.01551v1-abstract-full" style="display: none;"> For the 696 trans-Neptunian objects (TNOs) with absolute magnitudes $5.5 < H_r < 8.2$ detected in the Dark Energy Survey (DES), we characterize the relationships between their dynamical state and physical properties -- namely $H_r$, indicating size; colors, indicating surface composition; and flux variation semi-amplitude $A$, indicating asphericity and surface inhomogeneity. We seek ``birth'' physical distributions that can recreate these parameters in every dynamical class. We show that the observed colors of these TNOs are consistent with 2 Gaussian distributions in $griz$ space, ``near-IR bright'' (NIRB) and ``near-IR faint'' (NIRF), presumably an inner and outer birth population, respectively. We find a model in which both the NIRB and NIRF $H_r$ and $A$ distributions are independent of current dynamical states, supporting their assignment as birth populations. All objects are consistent with a common rolling $p(H_r)$, but NIRF objects are significantly more variable. Cold classicals (CCs) are purely NIRF, while hot classical (HC), scattered, and detached TNOs are consistent with $\approx70\%$ NIRB, and resonances' NIRB fractions show significant variation. The NIRB component of the HCs and of some resonances have broader inclination distributions than the NIRFs, i.e. their current dynamics retains information about birth location. We find evidence for radial stratification within the birth NIRB population, in that HC NIRBs are on average redder than detached or scattered NIRBs; a similar effect distinguishes CCs from other NIRFs. We estimate total object counts and masses of each class within our $H_r$ range. These results will strongly constrain models of the outer solar system. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.01551v1-abstract-full').style.display = 'none'; document.getElementById('2501.01551v1-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 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">52 pages, 13 figures, 4 appendices. Abstract abridged. Associated repository: https://github.com/bernardinelli/des_tno_likelihood</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DES-2024-0873 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.07765">arXiv:2412.07765</a> <span> [<a href="https://arxiv.org/pdf/2412.07765">pdf</a>, <a href="https://arxiv.org/format/2412.07765">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"> Multiprobe Cosmology from the Abundance of SPT Clusters and DES Galaxy Clustering and Weak Lensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/astro-ph?searchtype=author&query=Krause%2C+E">E. Krause</a>, <a href="/search/astro-ph?searchtype=author&query=To%2C+C">C. To</a>, <a href="/search/astro-ph?searchtype=author&query=Bleem%2C+L+E">L. E. Bleem</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+M">M. Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Mohr%2C+J+J">J. J. Mohr</a>, <a href="/search/astro-ph?searchtype=author&query=Schrabback%2C+T">T. Schrabback</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</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=Bernstein%2C+G+M">G. M. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Blazek%2C+J">J. Blazek</a>, <a href="/search/astro-ph?searchtype=author&query=Camacho%2C+H">H. Camacho</a>, <a href="/search/astro-ph?searchtype=author&query=Campos%2C+A">A. Campos</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=Cawthon%2C+R">R. Cawthon</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">C. Chang</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. (194 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="2412.07765v1-abstract-short" style="display: inline;"> Cosmic shear, galaxy clustering, and the abundance of massive halos each probe the large-scale structure of the universe in complementary ways. We present cosmological constraints from the joint analysis of the three probes, building on the latest analyses of the lensing-informed abundance of clusters identified by the South Pole Telescope (SPT) and of the auto- and cross-correlation of galaxy pos… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07765v1-abstract-full').style.display = 'inline'; document.getElementById('2412.07765v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.07765v1-abstract-full" style="display: none;"> Cosmic shear, galaxy clustering, and the abundance of massive halos each probe the large-scale structure of the universe in complementary ways. We present cosmological constraints from the joint analysis of the three probes, building on the latest analyses of the lensing-informed abundance of clusters identified by the South Pole Telescope (SPT) and of the auto- and cross-correlation of galaxy position and weak lensing measurements (3$\times$2pt) in the Dark Energy Survey (DES). We consider the cosmological correlation between the different tracers and we account for the systematic uncertainties that are shared between the large-scale lensing correlation functions and the small-scale lensing-based cluster mass calibration. Marginalized over the remaining $螞$CDM parameters (including the sum of neutrino masses) and 52 astrophysical modeling parameters, we measure $惟_\mathrm{m}=0.300\pm0.017$ and $蟽_8=0.797\pm0.026$. Compared to constraints from Planck primary CMB anisotropies, our constraints are only 15% wider with a probability to exceed of 0.22 ($1.2蟽$) for the two-parameter difference. We further obtain $S_8\equiv蟽_8(惟_\mathrm{m}/0.3)^{0.5}=0.796\pm0.013$ which is lower than the Planck measurement at the $1.6蟽$ level. The combined SPT cluster, DES 3$\times$2pt, and Planck datasets mildly prefer a non-zero positive neutrino mass, with a 95% upper limit $\sum m_谓<0.25~\mathrm{eV}$ on the sum of neutrino masses. Assuming a $w$CDM model, we constrain the dark energy equation of state parameter $w=-1.15^{+0.23}_{-0.17}$ and when combining with Planck primary CMB anisotropies, we recover $w=-1.20^{+0.15}_{-0.09}$, a $1.7蟽$ difference with a cosmological constant. The precision of our results highlights the benefits of multiwavelength multiprobe cosmology. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.07765v1-abstract-full').style.display = 'none'; document.getElementById('2412.07765v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 December, 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">Submitted to Phys. Rev. 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/2410.22272">arXiv:2410.22272</a> <span> [<a href="https://arxiv.org/pdf/2410.22272">pdf</a>, <a href="https://arxiv.org/format/2410.22272">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"> Dark Energy Survey Year 3: Blue Shear </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=McCullough%2C+J">J. McCullough</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</a>, <a href="/search/astro-ph?searchtype=author&query=Legnani%2C+E">E. Legnani</a>, <a href="/search/astro-ph?searchtype=author&query=Gruen%2C+D">D. Gruen</a>, <a href="/search/astro-ph?searchtype=author&query=Roodman%2C+A">A. Roodman</a>, <a href="/search/astro-ph?searchtype=author&query=Friedrich%2C+O">O. Friedrich</a>, <a href="/search/astro-ph?searchtype=author&query=MacCrann%2C+N">N. MacCrann</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=Myles%2C+J">J. Myles</a>, <a href="/search/astro-ph?searchtype=author&query=Dodelson%2C+S">S. Dodelson</a>, <a href="/search/astro-ph?searchtype=author&query=Samuroff%2C+S">S. Samuroff</a>, <a href="/search/astro-ph?searchtype=author&query=Blazek%2C+J">J. Blazek</a>, <a href="/search/astro-ph?searchtype=author&query=Prat%2C+J">J. Prat</a>, <a href="/search/astro-ph?searchtype=author&query=Honscheid%2C+K">K. Honscheid</a>, <a href="/search/astro-ph?searchtype=author&query=Pieres%2C+A">A. Pieres</a>, <a href="/search/astro-ph?searchtype=author&query=Fert%C3%A9%2C+A">A. Fert茅</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">A. Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+A">A. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro-Alsina%2C+A">A. Navarro-Alsina</a>, <a href="/search/astro-ph?searchtype=author&query=Campos%2C+A">A. Campos</a>, <a href="/search/astro-ph?searchtype=author&query=Malag%C3%B3n%2C+A+A+P">A. A. Plazas Malag贸n</a>, <a href="/search/astro-ph?searchtype=author&query=Porredon%2C+A">A. Porredon</a>, <a href="/search/astro-ph?searchtype=author&query=Farahi%2C+A">A. Farahi</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a> , et al. (93 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="2410.22272v1-abstract-short" style="display: inline;"> Modeling the intrinsic alignment (IA) of galaxies poses a challenge to weak lensing analyses. The Dark Energy Survey is expected to be less impacted by IA when limited to blue, star-forming galaxies. The cosmological parameter constraints from this blue cosmic shear sample are stable to IA model choice, unlike passive galaxies in the full DES Y3 sample, the goodness-of-fit is improved and the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.22272v1-abstract-full').style.display = 'inline'; document.getElementById('2410.22272v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.22272v1-abstract-full" style="display: none;"> Modeling the intrinsic alignment (IA) of galaxies poses a challenge to weak lensing analyses. The Dark Energy Survey is expected to be less impacted by IA when limited to blue, star-forming galaxies. The cosmological parameter constraints from this blue cosmic shear sample are stable to IA model choice, unlike passive galaxies in the full DES Y3 sample, the goodness-of-fit is improved and the $惟_{m}$ and $S_8$ better agree with the cosmic microwave background. Mitigating IA with sample selection, instead of flexible model choices, can reduce uncertainty in $S_8$ by a factor of 1.5. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.22272v1-abstract-full').style.display = 'none'; document.getElementById('2410.22272v1-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 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">Data access available at https://jamiemccullough.github.io/data/blueshear/</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.20205">arXiv:2410.20205</a> <span> [<a href="https://arxiv.org/pdf/2410.20205">pdf</a>, <a href="https://arxiv.org/format/2410.20205">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"> Improving Galaxy Cluster Selection with the Outskirt Stellar Mass of Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kwiecien%2C+M">Matthew Kwiecien</a>, <a href="/search/astro-ph?searchtype=author&query=Jeltema%2C+T">Tesla Jeltema</a>, <a href="/search/astro-ph?searchtype=author&query=Leauthaud%2C+A">Alexie Leauthaud</a>, <a href="/search/astro-ph?searchtype=author&query=Huang%2C+S">Song Huang</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E">Eli Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Heydenreich%2C+S">Sven Heydenreich</a>, <a href="/search/astro-ph?searchtype=author&query=Lange%2C+J">Johannes Lange</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+S">Spencer Everett</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+C">Conghao Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P">Paige Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y">Yuanyuan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Shin%2C+T">Tae-Hyeon Shin</a>, <a href="/search/astro-ph?searchtype=author&query=Golden-Marx%2C+J">Jesse Golden-Marx</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+J+L">J. L. Marshall</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=Bocquet%2C+S">S. Bocquet</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=Carretero%2C+J">J. Carretero</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=Davis%2C+T+M">T. M. Davis</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=Doel%2C+P">P. Doel</a> , et al. (31 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="2410.20205v1-abstract-short" style="display: inline;"> The number density and redshift evolution of optically selected galaxy clusters offer an independent measurement of the amplitude of matter fluctuations, $S_8$. However, recent results have shown that clusters chosen by the redMaPPer algorithm show richness-dependent biases that affect the weak lensing signals and number densities of clusters, increasing uncertainty in the cluster mass calibration… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.20205v1-abstract-full').style.display = 'inline'; document.getElementById('2410.20205v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.20205v1-abstract-full" style="display: none;"> The number density and redshift evolution of optically selected galaxy clusters offer an independent measurement of the amplitude of matter fluctuations, $S_8$. However, recent results have shown that clusters chosen by the redMaPPer algorithm show richness-dependent biases that affect the weak lensing signals and number densities of clusters, increasing uncertainty in the cluster mass calibration and reducing their constraining power. In this work, we evaluate an alternative cluster proxy, outskirt stellar mass, $M_{\textrm{out}}$, defined as the total stellar mass within a $[50,100]$ kpc envelope centered on a massive galaxy. This proxy exhibits scatter comparable to redMaPPer richness, $位$, but is less likely to be subject to projection effects. We compare the Dark Energy Survey Year 3 redMaPPer cluster catalog with a $M_{\textrm{out}}$ selected cluster sample from the Hyper-Suprime Camera survey. We use weak lensing measurements to quantify and compare the scatter of $M_{\textrm{out}}$ and $位$ with halo mass. Our results show $M_{\textrm{out}}$ has a scatter consistent with $位$, with a similar halo mass dependence, and that both proxies contain unique information about the underlying halo mass. We find $位$-selected samples introduce features into the measured $螖危$ signal that are not well fit by a log-normal scatter only model, absent in $M_{\textrm{out}}$ selected samples. Our findings suggest that $M_{\textrm{out}}$ offers an alternative for cluster selection with more easily calibrated selection biases, at least at the generally lower richnesses probed here. Combining both proxies may yield a mass proxy with a lower scatter and more tractable selection biases, enabling the use of lower mass clusters in cosmology. Finally, we find the scatter and slope in the $位-M_{\textrm{out}}$ scaling relation to be $0.49 \pm 0.02$ and $0.38 \pm 0.09$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.20205v1-abstract-full').style.display = 'none'; document.getElementById('2410.20205v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 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">22 pages, 8 figures, 4 tables, submitted to PRD</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-24-0765-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.07956">arXiv:2410.07956</a> <span> [<a href="https://arxiv.org/pdf/2410.07956">pdf</a>, <a href="https://arxiv.org/format/2410.07956">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"> Constraints on compact objects from the Dark Energy Survey five-year supernova sample </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">Paul Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">Tamara M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">Maria Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">Patrick Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">Dillon Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">Ryan Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">Lluis Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Garcia-Bellido%2C+J">Juan Garcia-Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Gill%2C+M+S+S">Mandeep S. S. Gill</a>, <a href="/search/astro-ph?searchtype=author&query=Lahav%2C+O">Ofer Lahav</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">Jason Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">Chris Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Moeller%2C+A">Anais Moeller</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">Masao Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+B+O">Bruno O. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">Mark Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Whiteway%2C+L">Lorne Whiteway</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">Phillip Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</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=da+Costa%2C+L+N">L. N. da Costa</a> , et al. (35 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="2410.07956v2-abstract-short" style="display: inline;"> Gravitational lensing magnification of Type Ia supernovae (SNe Ia) allows information to be obtained about the distribution of matter on small scales. In this paper, we derive limits on the fraction $伪$ of the total matter density in compact objects (which comprise stars, stellar remnants, small stellar groupings and primordial black holes) of mass $M > 0.03 M_{\odot}$ over cosmological distances.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07956v2-abstract-full').style.display = 'inline'; document.getElementById('2410.07956v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.07956v2-abstract-full" style="display: none;"> Gravitational lensing magnification of Type Ia supernovae (SNe Ia) allows information to be obtained about the distribution of matter on small scales. In this paper, we derive limits on the fraction $伪$ of the total matter density in compact objects (which comprise stars, stellar remnants, small stellar groupings and primordial black holes) of mass $M > 0.03 M_{\odot}$ over cosmological distances. Using 1,532 SNe Ia from the Dark Energy Survey Year 5 sample (DES-SN5YR) combined with a Bayesian prior for the absolute magnitude $M$, we obtain $伪< 0.12$ at the 95\% confidence level after marginalisation over cosmological parameters, lensing due to large-scale structure, and intrinsic non-Gaussianity. Similar results are obtained using priors from the cosmic microwave background, baryon acoustic oscillations and galaxy weak lensing, indicating our results do not depend on the background cosmology. We argue our constraints are likely to be conservative (in the sense of the values we quote being higher than the truth), but discuss scenarios in which they could be weakened by systematics of the order of $螖伪\sim 0.04$ <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.07956v2-abstract-full').style.display = 'none'; document.getElementById('2410.07956v2-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 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 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 by MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DES-2024-0853 </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/2409.02184">arXiv:2409.02184</a> <span> [<a href="https://arxiv.org/pdf/2409.02184">pdf</a>, <a href="https://arxiv.org/format/2409.02184">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"> The Hierarchical Growth of Bright Central Galaxies and Intracluster Light as Traced by the Magnitude Gap </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Golden-Marx%2C+J+B">Jesse B. Golden-Marx</a>, <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y">Y. Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Ogando%2C+R+L+C">R. L. C. Ogando</a>, <a href="/search/astro-ph?searchtype=author&query=Yanny%2C+B">B. Yanny</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=Hilton%2C+M">M. Hilton</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=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=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=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+T+-">T. -Y. Cheng</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=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=Everett%2C+S">S. Everett</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrero%2C+I">I. Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Bellido%2C+J">J. Garc铆a-Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Gatti%2C+M">M. Gatti</a>, <a href="/search/astro-ph?searchtype=author&query=Giannini%2C+G">G. Giannini</a>, <a href="/search/astro-ph?searchtype=author&query=Gruen%2C+D">D. Gruen</a> , et al. (25 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="2409.02184v1-abstract-short" style="display: inline;"> Using a sample of 2800 galaxy clusters identified in the Dark Energy Survey across the redshift range $0.20 < z < 0.60$, we characterize the hierarchical assembly of Bright Central Galaxies (BCGs) and the surrounding intracluster light (ICL). To quantify hierarchical formation we use the stellar mass - halo mass (SMHM) relation for the BCG+ICL system and incorporate the magnitude gap (M14), the di… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02184v1-abstract-full').style.display = 'inline'; document.getElementById('2409.02184v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.02184v1-abstract-full" style="display: none;"> Using a sample of 2800 galaxy clusters identified in the Dark Energy Survey across the redshift range $0.20 < z < 0.60$, we characterize the hierarchical assembly of Bright Central Galaxies (BCGs) and the surrounding intracluster light (ICL). To quantify hierarchical formation we use the stellar mass - halo mass (SMHM) relation for the BCG+ICL system and incorporate the magnitude gap (M14), the difference in brightness between the BCG (measured within 30kpc) and 4th brightest cluster member galaxy within 0.5 $R_{200,c}$. The inclusion of M14, which traces BCG hierarchical growth, increases the slope and decreases the intrinsic scatter in the SMHM relation, highlighting that it is a latent variable within the BCG+ICL SMHM relation. Moreover, the correlation with M14 decreases at large radii from the BCG's centre. However, the stellar light within the BCG+ICL transition region (30kpc - 80kpc) most strongly correlates with the dark matter halo mass and has a statistically significant correlation with M14. As the light in the transition region and M14 are independent measurements, the transition region may grow as a result of the BCG's hierarchical two-phase formation. Additionally, as M14 and ICL result from hierarchical growth, we use a stacked sample and find that clusters with large M14 values are characterized by larger ICL and BCG+ICL fractions, which illustrates that the merger processes that build the BCG stellar mass also grow the ICL. Furthermore, this may suggest that M14 combined with the ICL fraction can be used as a method to identify dynamically relaxed clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.02184v1-abstract-full').style.display = 'none'; document.getElementById('2409.02184v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> <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, 5 Figures, submitted to MNRAS on 8/30/2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.03749">arXiv:2408.03749</a> <span> [<a href="https://arxiv.org/pdf/2408.03749">pdf</a>, <a href="https://arxiv.org/format/2408.03749">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"> Suppression of the type Ia supernova host galaxy step in the outer regions of galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Toy%2C+M">M. Toy</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Frohmaier%2C+C">C. Frohmaier</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</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=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a> , et al. (41 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="2408.03749v1-abstract-short" style="display: inline;"> Using 1533 type Ia supernovae (SNe Ia) from the five-year sample of the Dark Energy Survey (DES), we investigate the effects of projected galactocentric separation between the SNe and their host galaxies on their light curves and standardization. We show, for the first time, that the difference in SN Ia post-standardization brightnesses between high and low-mass hosts reduces from $0.078\pm0.011$… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03749v1-abstract-full').style.display = 'inline'; document.getElementById('2408.03749v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.03749v1-abstract-full" style="display: none;"> Using 1533 type Ia supernovae (SNe Ia) from the five-year sample of the Dark Energy Survey (DES), we investigate the effects of projected galactocentric separation between the SNe and their host galaxies on their light curves and standardization. We show, for the first time, that the difference in SN Ia post-standardization brightnesses between high and low-mass hosts reduces from $0.078\pm0.011$ mag in the full sample to $0.036 \pm 0.018$ mag for SNe Ia located in the outer regions of their host galaxies, while increasing to $0.100 \pm 0.014$ mag for SNe in the inner regions. In these inner regions, the step can be reduced (but not removed) using a model where the $R_V$ of dust along the line-of-sight to the SN changes as a function of galaxy properties. To explain the remaining difference, we use the distributions of the SN Ia stretch parameter to test whether the inferred age of SN progenitors are more varied in the inner regions of galaxies. We find that the proportion of high-stretch SNe Ia in red (older) environments is more prominent in outer regions and that the outer regions stretch distributions are overall more homogeneous compared to inner regions, but conclude that this effect cannot explain the reduction in significance of any Hubble residual step in outer regions. We conclude that the standardized distances of SNe Ia located in the outer regions of galaxies are less affected by their global host galaxy properties than those in the inner regions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.03749v1-abstract-full').style.display = 'none'; document.getElementById('2408.03749v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 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/2408.01001">arXiv:2408.01001</a> <span> [<a href="https://arxiv.org/pdf/2408.01001">pdf</a>, <a href="https://arxiv.org/format/2408.01001">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"> Calibrating the Absolute Magnitude of Type Ia Supernovae in Nearby Galaxies using [OII] and Implications for $H_{0}$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dixon%2C+M">M. Dixon</a>, <a href="/search/astro-ph?searchtype=author&query=Mould%2C+J">J. Mould</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+E+N">E. N. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Flynn%2C+C">C. Flynn</a>, <a href="/search/astro-ph?searchtype=author&query=Duffy%2C+A+R">A. R. Duffy</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</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=Conselice%2C+C">C. Conselice</a> , et al. (47 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="2408.01001v2-abstract-short" style="display: inline;"> The present state of cosmology is facing a crisis where there is a fundamental disagreement in measurements of the Hubble constant ($H_{0}$), with significant tension between the early and late universe methods. Type Ia supernovae (SNe Ia) are important to measuring $H_{0}$ through the astronomical distance ladder. However, there remains potential to better standardise SN Ia light curves by using… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.01001v2-abstract-full').style.display = 'inline'; document.getElementById('2408.01001v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.01001v2-abstract-full" style="display: none;"> The present state of cosmology is facing a crisis where there is a fundamental disagreement in measurements of the Hubble constant ($H_{0}$), with significant tension between the early and late universe methods. Type Ia supernovae (SNe Ia) are important to measuring $H_{0}$ through the astronomical distance ladder. However, there remains potential to better standardise SN Ia light curves by using known dependencies on host galaxy properties after the standard light curve width and colour corrections have been applied to the peak SN Ia luminosities. To explore this, we use the 5-year photometrically identified SNe Ia sample obtained by the Dark Energy Survey, along with host galaxy spectra obtained by the Australian Dark Energy Survey. Using host galaxy spectroscopy, we find a significant trend with the equivalent width (EW) of the [OII] $位位$ 3727, 29 doublet, a proxy for specific star formation rate, and Hubble residuals. We find that the correlation with [OII] EW is a powerful alternative to the commonly used mass step after initial light curve corrections. Applying this [OII] EW correction to 20 SNe Ia in calibrator galaxies observed with WiFeS, we examined the impact on SN Ia absolute magnitudes and $H_{0}$. Our [OII] EW corrections result in $H_{0}$ values ranging between 73.04 to 73.51 $\mathrm{km} \mathrm{s}^{-1} \mathrm{Mpc}^{-1}$, with a combined statistical and systematic uncertainty of $\sim$1.31 $\mathrm{km} \mathrm{s}^{-1} \mathrm{Mpc}^{-1}$. However, even with this additional correction, the impact of host galaxy properties in standardising SNe Ia appears limited in reducing the current tension ($\sim$5$蟽$) with the CMB result for $H_{0}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.01001v2-abstract-full').style.display = 'none'; document.getElementById('2408.01001v2-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">16 pages, 13 figures. Accepted for publication in 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/2407.16744">arXiv:2407.16744</a> <span> [<a href="https://arxiv.org/pdf/2407.16744">pdf</a>, <a href="https://arxiv.org/format/2407.16744">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"> Evaluating Cosmological Biases using Photometric Redshifts for Type Ia Supernova Cosmology with the Dark Energy Survey Supernova Program </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Myles%2C+J">J. Myles</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</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="2407.16744v1-abstract-short" style="display: inline;"> Cosmological analyses with Type Ia Supernovae (SNe Ia) have traditionally been reliant on spectroscopy for both classifying the type of supernova and obtaining reliable redshifts to measure the distance-redshift relation. While obtaining a host-galaxy spectroscopic redshift for most SNe is feasible for small-area transient surveys, it will be too resource intensive for upcoming large-area surveys… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16744v1-abstract-full').style.display = 'inline'; document.getElementById('2407.16744v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.16744v1-abstract-full" style="display: none;"> Cosmological analyses with Type Ia Supernovae (SNe Ia) have traditionally been reliant on spectroscopy for both classifying the type of supernova and obtaining reliable redshifts to measure the distance-redshift relation. While obtaining a host-galaxy spectroscopic redshift for most SNe is feasible for small-area transient surveys, it will be too resource intensive for upcoming large-area surveys such as the Vera Rubin Observatory Legacy Survey of Space and Time, which will observe on the order of millions of SNe. Here we use data from the Dark Energy Survey (DES) to address this problem with photometric redshifts (photo-z) inferred directly from the SN light-curve in combination with Gaussian and full p(z) priors from host-galaxy photo-z estimates. Using the DES 5-year photometrically-classified SN sample, we consider several photo-z algorithms as host-galaxy photo-z priors, including the Self-Organizing Map redshifts (SOMPZ), Bayesian Photometric Redshifts (BPZ), and Directional-Neighbourhood Fitting (DNF) redshift estimates employed in the DES 3x2 point analyses. With detailed catalog-level simulations of the DES 5-year sample, we find that the simulated w can be recovered within $\pm$0.02 when using SN+SOMPZ or DNF prior photo-z, smaller than the average statistical uncertainty for these samples of 0.03. With data, we obtain biases in w consistent with simulations within ~1$蟽$ for three of the five photo-z variants. We further evaluate how photo-z systematics interplay with photometric classification and find classification introduces a subdominant systematic component. This work lays the foundation for next-generation fully photometric SNe Ia cosmological analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.16744v1-abstract-full').style.display = 'none'; document.getElementById('2407.16744v1-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 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">19 pages, 9 figures. Submitting to MNRAS, 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/2407.10961">arXiv:2407.10961</a> <span> [<a href="https://arxiv.org/pdf/2407.10961">pdf</a>, <a href="https://arxiv.org/format/2407.10961">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"> Galaxy cluster matter profiles: I. Self-similarity, mass calibration, and observable-mass relation validation employing cluster mass posteriors </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Singh%2C+A">A. Singh</a>, <a href="/search/astro-ph?searchtype=author&query=Mohr%2C+J+J">J. J. Mohr</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+C+T">C. T. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+M">M. Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+J+L">J. L. Marshall</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=Alves%2C+O">O. Alves</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=Bhargava%2C+S">S. Bhargava</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=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=Pereira%2C+M+E+S">M. E. S. Pereira</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Diehl%2C+H+T">H. T. Diehl</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+S">S. Everett</a>, <a href="/search/astro-ph?searchtype=author&query=Flaugher%2C+B">B. Flaugher</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a> , et al. (28 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="2407.10961v2-abstract-short" style="display: inline;"> We present a study of the weak lensing inferred matter profiles $螖危(R)$ of 698 South Pole Telescope thermal Sunyaev-Zel'dovich effect selected and MCMF optically confirmed galaxy clusters in the redshift range $0.25 <z< 0.94$ that have associated weak gravitational lensing shear profiles from the Dark Energy Survey. Rescaling these profiles to account for the mass dependent size and the redshift d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10961v2-abstract-full').style.display = 'inline'; document.getElementById('2407.10961v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.10961v2-abstract-full" style="display: none;"> We present a study of the weak lensing inferred matter profiles $螖危(R)$ of 698 South Pole Telescope thermal Sunyaev-Zel'dovich effect selected and MCMF optically confirmed galaxy clusters in the redshift range $0.25 <z< 0.94$ that have associated weak gravitational lensing shear profiles from the Dark Energy Survey. Rescaling these profiles to account for the mass dependent size and the redshift dependent density produces average rescaled matter profiles $螖危(R/R_\mathrm{200c})/(蟻_\mathrm{crit}R_\mathrm{200c})$ with a lower dispersion than the unscaled $螖危(R)$ versions, indicating a significant degree of self-similarity. Galaxy clusters from hydrodynamical simulations also exhibit matter profiles that suggest a high degree of self-similarity, with RMS variation among the average rescaled matter profiles with redshift and mass falling by a factor of approximately six and 23, respectively, compared to the unscaled average matter profiles. We employed this regularity in a new Bayesian method for weak lensing mass calibration that employs the so-called cluster mass posterior $P(M_\mathrm{200c}|\hat味, \hat位, z)$, which describes the individual cluster masses given their tSZE and optical observables. We validated the method using realistic mock datasets and present observable-mass relation constraints for the SPT$\times$DES sample. We present new validation tests of the observable-mass relation that indicate the underlying power-law form and scatter are adequate to describe the real cluster sample but that also suggest a redshift variation in the intrinsic scatter of the $位$-mass relation may offer a better description. In addition, the average rescaled matter profiles offer high signal-to-noise ratio constraints on the shape of real cluster matter profiles, which are in good agreement with available hydrodynamical $螞$CDM simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10961v2-abstract-full').style.display = 'none'; document.getElementById('2407.10961v2-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 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 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">24 pages, 17 figures, Accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.01685">arXiv:2407.01685</a> <span> [<a href="https://arxiv.org/pdf/2407.01685">pdf</a>, <a href="https://arxiv.org/format/2407.01685">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"> Comparisons Between Resolved Star Formation Rate and Gas Tracers in the Strongly Lensed Galaxy SDSS J0901+1814 at Cosmic Noon </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chen%2C+Q">Qingxiang Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Sharon%2C+C+E">Chelsea E. Sharon</a>, <a href="/search/astro-ph?searchtype=author&query=Algera%2C+H+S">Hiddo S. Algera</a>, <a href="/search/astro-ph?searchtype=author&query=Baker%2C+A+J">Andrew J. Baker</a>, <a href="/search/astro-ph?searchtype=author&query=Keeton%2C+C+R">Charles R. Keeton</a>, <a href="/search/astro-ph?searchtype=author&query=Lutz%2C+D">Dieter Lutz</a>, <a href="/search/astro-ph?searchtype=author&query=Liu%2C+D">Daizhong Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Young%2C+A+J">Anthony J. Young</a>, <a href="/search/astro-ph?searchtype=author&query=Tagore%2C+A">Amit Tagore</a>, <a href="/search/astro-ph?searchtype=author&query=Rivera%2C+J">Jesus Rivera</a>, <a href="/search/astro-ph?searchtype=author&query=Hicks%2C+E+K">Erin K. Hicks</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S+S">Sahar S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+D+L">Douglas L. Tucker</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="2407.01685v1-abstract-short" style="display: inline;"> We report new radio observations of SDSS J090122.37+181432.3, a strongly lensed star-forming galaxy at $z=2.26$. We image 1.4 GHz (L-band) and 3 GHz (S-band) continuum using the VLA and 1.2 mm (band 6) continuum with ALMA, in addition to the CO(7-6) and CI(${\rm ^3P_2\rightarrow ^3\!P_1}$) lines, all at $\lesssim1.^{\prime\prime}7$ resolution. Based on the VLA integrated flux densities, we decompo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01685v1-abstract-full').style.display = 'inline'; document.getElementById('2407.01685v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.01685v1-abstract-full" style="display: none;"> We report new radio observations of SDSS J090122.37+181432.3, a strongly lensed star-forming galaxy at $z=2.26$. We image 1.4 GHz (L-band) and 3 GHz (S-band) continuum using the VLA and 1.2 mm (band 6) continuum with ALMA, in addition to the CO(7-6) and CI(${\rm ^3P_2\rightarrow ^3\!P_1}$) lines, all at $\lesssim1.^{\prime\prime}7$ resolution. Based on the VLA integrated flux densities, we decompose the radio spectrum into its free-free (FF) and non-thermal components. The infrared-radio correlation (IRRC) parameter $q_{\rm TIR}=2.65_{-0.31}^{+0.24}$ is consistent with expectations for star forming galaxies. We obtain radio continuum-derived SFRs that are free of dust extinction, finding $\rm {620}_{-220}^{+280}\,M_\odot\,yr^{-1}$, $\rm {230}_{-160}^{+570}\,M_\odot\,yr^{-1}$, and $\rm {280}_{-120}^{+460}\,M_\odot\,yr^{-1}$ from the FF emission, non-thermal emission, and when accounting for both emission processes, respectively, in agreement with previous results. We estimate the gas mass from the CI(${\rm ^3P_2\rightarrow ^3\!P_1}$) line as $M_{\rm gas}=(1.2\pm0.2)\times10^{11}\,M_\odot$, which is consistent with prior CO(1-0)-derived gas masses. Using our new IR and radio continuum data to map the SFR, we assess the dependence of the Schmidt-Kennicutt relation on choices of SFR and gas tracer for $\sim{\rm kpc}$ scales. The different SFR tracers yield different slopes, with the IR being the steepest, potentially due to highly obscured star formation in J0901. The radio continuum maps have the lowest slopes and overall fidelity for mapping the SFR, despite producing consistent total SFRs. We also find that the Schmidt-Kennicutt relation slope is flattest when using CO(7-6) or CI(${\rm ^3P_2\rightarrow ^3\!P_1}$) to trace gas mass, suggesting that those transitions are not suitable for tracing the bulk molecular gas in galaxies like J0901. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01685v1-abstract-full').style.display = 'none'; document.getElementById('2407.01685v1-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 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">28 pages, 13 figures, 9 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/2406.12675">arXiv:2406.12675</a> <span> [<a href="https://arxiv.org/pdf/2406.12675">pdf</a>, <a href="https://arxiv.org/format/2406.12675">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"> Dark Energy Survey Year 3 Results: Cosmology from galaxy clustering and galaxy-galaxy lensing in harmonic space </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Faga%2C+L">L. Faga</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=Camacho%2C+H">H. Camacho</a>, <a href="/search/astro-ph?searchtype=author&query=Rosenfeld%2C+R">R. Rosenfeld</a>, <a href="/search/astro-ph?searchtype=author&query=Lima%2C+M">M. Lima</a>, <a href="/search/astro-ph?searchtype=author&query=Doux%2C+C">C. Doux</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+X">X. Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Prat%2C+J">J. Prat</a>, <a href="/search/astro-ph?searchtype=author&query=Porredon%2C+A">A. Porredon</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</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=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=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=Bernstein%2C+G+M">G. M. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley-Geer%2C+E">E. Buckley-Geer</a>, <a href="/search/astro-ph?searchtype=author&query=Campos%2C+A">A. Campos</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> , et al. (78 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="2406.12675v1-abstract-short" style="display: inline;"> We present the joint tomographic analysis of galaxy-galaxy lensing and galaxy clustering in harmonic space, using galaxy catalogues from the first three years of observations by the Dark Energy Survey (DES Y3). We utilise the redMaGiC and MagLim catalogues as lens galaxies and the METACALIBRATION catalogue as source galaxies. The measurements of angular power spectra are performed using the pseudo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12675v1-abstract-full').style.display = 'inline'; document.getElementById('2406.12675v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.12675v1-abstract-full" style="display: none;"> We present the joint tomographic analysis of galaxy-galaxy lensing and galaxy clustering in harmonic space, using galaxy catalogues from the first three years of observations by the Dark Energy Survey (DES Y3). We utilise the redMaGiC and MagLim catalogues as lens galaxies and the METACALIBRATION catalogue as source galaxies. The measurements of angular power spectra are performed using the pseudo-$C_\ell$ method, and our theoretical modelling follows the fiducial analyses performed by DES Y3 in configuration space, accounting for galaxy bias, intrinsic alignments, magnification bias, shear magnification bias and photometric redshift uncertainties. We explore different approaches for scale cuts based on non-linear galaxy bias and baryonic effects contamination. Our fiducial covariance matrix is computed analytically, accounting for mask geometry in the Gaussian term, and including non-Gaussian contributions and super-sample covariance terms. To validate our harmonic space pipelines and covariance matrix, we used a suite of 1800 log-normal simulations. We also perform a series of stress tests to gauge the robustness of our harmonic space analysis. In the $螞$CDM model, the clustering amplitude $S_8 =蟽_8(惟_m/0.3)^{0.5}$ is constrained to $S_8 = 0.704\pm 0.029$ and $S_8 = 0.753\pm 0.024$ ($68\%$ C.L.) for the redMaGiC and MagLim catalogues, respectively. For the $w$CDM, the dark energy equation of state is constrained to $w = -1.28 \pm 0.29$ and $w = -1.26^{+0.34}_{-0.27}$, for redMaGiC and MagLim catalogues, respectively. These results are compatible with the corresponding DES Y3 results in configuration space and pave the way for harmonic space analyses using the DES Y6 data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.12675v1-abstract-full').style.display = 'none'; document.getElementById('2406.12675v1-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To be submitted to MNRAS</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-24-0289-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05050">arXiv:2406.05050</a> <span> [<a href="https://arxiv.org/pdf/2406.05050">pdf</a>, <a href="https://arxiv.org/format/2406.05050">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey Supernova Program: Slow supernovae show cosmological time dilation out to $z \sim 1$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=White%2C+R+M+T">R. M. T. White</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Lewis%2C+G+F">G. F. Lewis</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Hinton%2C+S+R">S. R. Hinton</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</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="2406.05050v2-abstract-short" style="display: inline;"> We present a precise measurement of cosmological time dilation using the light curves of 1504 type Ia supernovae from the Dark Energy Survey spanning a redshift range $0.1\lesssim z\lesssim 1.2$. We find that the width of supernova light curves is proportional to $(1+z)$, as expected for time dilation due to the expansion of the Universe. Assuming type Ia supernovae light curves are emitted with a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05050v2-abstract-full').style.display = 'inline'; document.getElementById('2406.05050v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05050v2-abstract-full" style="display: none;"> We present a precise measurement of cosmological time dilation using the light curves of 1504 type Ia supernovae from the Dark Energy Survey spanning a redshift range $0.1\lesssim z\lesssim 1.2$. We find that the width of supernova light curves is proportional to $(1+z)$, as expected for time dilation due to the expansion of the Universe. Assuming type Ia supernovae light curves are emitted with a consistent duration $螖t_{\rm em}$, and parameterising the observed duration as $螖t_{\rm obs}=螖t_{\rm em}(1+z)^b$, we fit for the form of time dilation using two methods. Firstly, we find that a power of $b \approx 1$ minimises the flux scatter in stacked subsamples of light curves across different redshifts. Secondly, we fit each target supernova to a stacked light curve (stacking all supernovae with observed bandpasses matching that of the target light curve) and find $b=1.003\pm0.005$ (stat) $\pm\,0.010$ (sys). Thanks to the large number of supernovae and large redshift-range of the sample, this analysis gives the most precise measurement of cosmological time dilation to date, ruling out any non-time-dilating cosmological models at very high significance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05050v2-abstract-full').style.display = 'none'; document.getElementById('2406.05050v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 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">14 pages, 13 figures. Updated in response to reviewer feedback. Accepted for publication in the Monthly Notices of the Royal Astronomical Society (MNRAS)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-24-0293-PPD, DES-2024-0831 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05049">arXiv:2406.05049</a> <span> [<a href="https://arxiv.org/pdf/2406.05049">pdf</a>, <a href="https://arxiv.org/format/2406.05049">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 Dark Energy Survey Supernova Program: An updated measurement of the Hubble constant using the Inverse Distance Ladder </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">R. Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Hinton%2C+S+R">S. R. Hinton</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">R. C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</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=Asorey%2C+J">J. Asorey</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> , 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="2406.05049v1-abstract-short" style="display: inline;"> We measure the current expansion rate of the Universe, Hubble's constant $H_0$, by calibrating the absolute magnitudes of supernovae to distances measured by Baryon Acoustic Oscillations. This `inverse distance ladder' technique provides an alternative to calibrating supernovae using nearby absolute distance measurements, replacing the calibration with a high-redshift anchor. We use the recent rel… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05049v1-abstract-full').style.display = 'inline'; document.getElementById('2406.05049v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05049v1-abstract-full" style="display: none;"> We measure the current expansion rate of the Universe, Hubble's constant $H_0$, by calibrating the absolute magnitudes of supernovae to distances measured by Baryon Acoustic Oscillations. This `inverse distance ladder' technique provides an alternative to calibrating supernovae using nearby absolute distance measurements, replacing the calibration with a high-redshift anchor. We use the recent release of 1829 supernovae from the Dark Energy Survey spanning $0.01\lt z \lt1.13$ anchored to the recent Baryon Acoustic Oscillation measurements from DESI spanning $0.30 \lt z_{\mathrm{eff}} \lt 2.33$. To trace cosmology to $z=0$, we use the third-, fourth- and fifth-order cosmographic models, which, by design, are agnostic about the energy content and expansion history of the universe. With the inclusion of the higher-redshift DESI-BAO data, the third-order model is a poor fit to both data sets, with the fourth-order model being preferred by the Akaike Information Criterion. Using the fourth-order cosmographic model, we find $H_0=67.19^{+0.66}_{-0.64}\mathrm{~km} \mathrm{~s}^{-1} \mathrm{~Mpc}^{-1}$, in agreement with the value found by Planck without the need to assume Flat-$螞$CDM. However the best-fitting expansion history differs from that of Planck, providing continued motivation to investigate these tensions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05049v1-abstract-full').style.display = 'none'; document.getElementById('2406.05049v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05048">arXiv:2406.05048</a> <span> [<a href="https://arxiv.org/pdf/2406.05048">pdf</a>, <a href="https://arxiv.org/format/2406.05048">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/10.1093/mnras/stae1988">10.1093/mnras/stae1988 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey Supernova Program: Investigating Beyond-$螞$CDM </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">R. Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Carr%2C+A">A. Carr</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Glazebrook%2C+K">K. Glazebrook</a>, <a href="/search/astro-ph?searchtype=author&query=Hinton%2C+S+R">S. R. Hinton</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+G">G. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Toy%2C+M">M. Toy</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="2406.05048v2-abstract-short" style="display: inline;"> We report constraints on a variety of non-standard cosmological models using the full 5-year photometrically-classified type Ia supernova sample from the Dark Energy Survey (DES-SN5YR). Both Akaike Information Criterion (AIC) and Suspiciousness calculations find no strong evidence for or against any of the non-standard models we explore. When combined with external probes, the AIC and Suspiciousne… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05048v2-abstract-full').style.display = 'inline'; document.getElementById('2406.05048v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05048v2-abstract-full" style="display: none;"> We report constraints on a variety of non-standard cosmological models using the full 5-year photometrically-classified type Ia supernova sample from the Dark Energy Survey (DES-SN5YR). Both Akaike Information Criterion (AIC) and Suspiciousness calculations find no strong evidence for or against any of the non-standard models we explore. When combined with external probes, the AIC and Suspiciousness agree that 11 of the 15 models are moderately preferred over Flat-$螞$CDM suggesting additional flexibility in our cosmological models may be required beyond the cosmological constant. We also provide a detailed discussion of all cosmological assumptions that appear in the DES supernova cosmology analyses, evaluate their impact, and provide guidance on using the DES Hubble diagram to test non-standard models. An approximate cosmological model, used to perform bias corrections to the data holds the biggest potential for harbouring cosmological assumptions. We show that even if the approximate cosmological model is constructed with a matter density shifted by $螖惟_m\sim0.2$ from the true matter density of a simulated data set the bias that arises is sub-dominant to statistical uncertainties. Nevertheless, we present and validate a methodology to reduce this bias. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05048v2-abstract-full').style.display = 'none'; document.getElementById('2406.05048v2-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">v1</span> submitted 7 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">Published to MNRAS on 20 August 2024; v2 updates to the accepted version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-24-0291-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05047">arXiv:2406.05047</a> <span> [<a href="https://arxiv.org/pdf/2406.05047">pdf</a>, <a href="https://arxiv.org/format/2406.05047">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 Dark Energy Survey : Detection of weak lensing magnification of supernovae and constraints on dark matter haloes </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shah%2C+P">P. Shah</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Lahav%2C+O">O. Lahav</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">R. C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">J. Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a> , et al. (40 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="2406.05047v1-abstract-short" style="display: inline;"> The residuals of the distance moduli of Type Ia supernovae (SN Ia) relative to a Hubble diagram fit contain information about the inhomogeneity of the universe, due to weak lensing magnification by foreground matter. By correlating the residuals of the Dark Energy Survey Year 5 SN Ia sample (DES-SN5YR) with extra-galactic foregrounds from the DES Y3 Gold catalog, we detect the presence of lensing… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05047v1-abstract-full').style.display = 'inline'; document.getElementById('2406.05047v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05047v1-abstract-full" style="display: none;"> The residuals of the distance moduli of Type Ia supernovae (SN Ia) relative to a Hubble diagram fit contain information about the inhomogeneity of the universe, due to weak lensing magnification by foreground matter. By correlating the residuals of the Dark Energy Survey Year 5 SN Ia sample (DES-SN5YR) with extra-galactic foregrounds from the DES Y3 Gold catalog, we detect the presence of lensing at $6.0 蟽$ significance. This is the first detection with a significance level above $5蟽$. Constraints on the effective mass-to-light ratios and radial profiles of dark-matter haloes surrounding individual galaxies are also obtained. We show that the scatter of SNe Ia around the Hubble diagram is reduced by modifying the standardisation of the distance moduli to include an easily calculable de-lensing (i.e., environmental) term. We use the de-lensed distance moduli to recompute cosmological parameters derived from SN Ia, finding in Flat $w$CDM a difference of $螖惟_{\rm M} = +0.036$ and $螖w = -0.056$ compared to the unmodified distance moduli, a change of $\sim 0.3蟽$. We argue that our modelling of SN Ia lensing will lower systematics on future surveys with higher statistical power. We use the observed dispersion of lensing in DES-SN5YR to constrain $蟽_8$, but caution that the fit is sensitive to uncertainties at small scales. Nevertheless, our detection of SN Ia lensing opens a new pathway to study matter inhomogeneity that complements galaxy-galaxy lensing surveys and has unrelated systematics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05047v1-abstract-full').style.display = 'none'; document.getElementById('2406.05047v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 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">Submitted 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/2406.05046">arXiv:2406.05046</a> <span> [<a href="https://arxiv.org/pdf/2406.05046">pdf</a>, <a href="https://arxiv.org/format/2406.05046">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 Dark Energy Survey Supernova Program: Light curves and 5-Year data release </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Herner%2C+K">K. Herner</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Acevedo%2C+M">M. Acevedo</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Rose%2C+B">B. Rose</a>, <a href="/search/astro-ph?searchtype=author&query=Camilleri%2C+R">R. Camilleri</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Kovacs%2C+E">E. Kovacs</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Toy%2C+M">M. Toy</a> , et al. (60 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.05046v1-abstract-short" style="display: inline;"> We present $griz$ photometric light curves for the full 5 years of the Dark Energy Survey Supernova program (DES-SN), obtained with both forced Point Spread Function (PSF) photometry on Difference Images (DIFFIMG) performed during survey operations, and Scene Modelling Photometry (SMP) on search images processed after the survey. This release contains $31,636$ DIFFIMG and $19,706$ high-quality SMP… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05046v1-abstract-full').style.display = 'inline'; document.getElementById('2406.05046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05046v1-abstract-full" style="display: none;"> We present $griz$ photometric light curves for the full 5 years of the Dark Energy Survey Supernova program (DES-SN), obtained with both forced Point Spread Function (PSF) photometry on Difference Images (DIFFIMG) performed during survey operations, and Scene Modelling Photometry (SMP) on search images processed after the survey. This release contains $31,636$ DIFFIMG and $19,706$ high-quality SMP light curves, the latter of which contains $1635$ photometrically-classified supernovae that pass cosmology quality cuts. This sample spans the largest redshift ($z$) range ever covered by a single SN survey ($0.1<z<1.13$) and is the largest single sample from a single instrument of SNe ever used for cosmological constraints. We describe in detail the improvements made to obtain the final DES-SN photometry and provide a comparison to what was used in the DES-SN3YR spectroscopically-confirmed SN Ia sample. We also include a comparative analysis of the performance of the SMP photometry with respect to the real-time DIFFIMG forced photometry and find that SMP photometry is more precise, more accurate, and less sensitive to the host-galaxy surface brightness anomaly. The public release of the light curves and ancillary data can be found at https://github.com/des-science/DES-SN5YR. Finally, we discuss implications for future transient surveys, such as the forthcoming Vera Rubin Observatory Legacy Survey of Space and Time (LSST). <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05046v1-abstract-full').style.display = 'none'; document.getElementById('2406.05046v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.10881">arXiv:2405.10881</a> <span> [<a href="https://arxiv.org/pdf/2405.10881">pdf</a>, <a href="https://arxiv.org/format/2405.10881">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"> Dark Energy Survey Year 3 results: simulation-based cosmological inference with wavelet harmonics, scattering transforms, and moments of weak lensing mass maps II. Cosmological results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gatti%2C+M">M. Gatti</a>, <a href="/search/astro-ph?searchtype=author&query=Campailla%2C+G">G. Campailla</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffrey%2C+N">N. Jeffrey</a>, <a href="/search/astro-ph?searchtype=author&query=Whiteway%2C+L">L. Whiteway</a>, <a href="/search/astro-ph?searchtype=author&query=Porredon%2C+A">A. Porredon</a>, <a href="/search/astro-ph?searchtype=author&query=Prat%2C+J">J. Prat</a>, <a href="/search/astro-ph?searchtype=author&query=Williamson%2C+J">J. Williamson</a>, <a href="/search/astro-ph?searchtype=author&query=Raveri%2C+M">M. Raveri</a>, <a href="/search/astro-ph?searchtype=author&query=Jain%2C+B">B. Jain</a>, <a href="/search/astro-ph?searchtype=author&query=Ajani%2C+V">V. Ajani</a>, <a href="/search/astro-ph?searchtype=author&query=Giannini%2C+G">G. Giannini</a>, <a href="/search/astro-ph?searchtype=author&query=Yamamoto%2C+M">M. Yamamoto</a>, <a href="/search/astro-ph?searchtype=author&query=Zhou%2C+C">C. Zhou</a>, <a href="/search/astro-ph?searchtype=author&query=Blazek%2C+J">J. Blazek</a>, <a href="/search/astro-ph?searchtype=author&query=Anbajagane%2C+D">D. Anbajagane</a>, <a href="/search/astro-ph?searchtype=author&query=Samuroff%2C+S">S. Samuroff</a>, <a href="/search/astro-ph?searchtype=author&query=Kacprzak%2C+T">T. Kacprzak</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</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">M. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+G">G. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Campos%2C+A">A. Campos</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">C. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a> , et al. (77 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="2405.10881v1-abstract-short" style="display: inline;"> We present a simulation-based cosmological analysis using a combination of Gaussian and non-Gaussian statistics of the weak lensing mass (convergence) maps from the first three years (Y3) of the Dark Energy Survey (DES). We implement: 1) second and third moments; 2) wavelet phase harmonics; 3) the scattering transform. Our analysis is fully based on simulations, spans a space of seven $谓w$CDM cosm… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.10881v1-abstract-full').style.display = 'inline'; document.getElementById('2405.10881v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.10881v1-abstract-full" style="display: none;"> We present a simulation-based cosmological analysis using a combination of Gaussian and non-Gaussian statistics of the weak lensing mass (convergence) maps from the first three years (Y3) of the Dark Energy Survey (DES). We implement: 1) second and third moments; 2) wavelet phase harmonics; 3) the scattering transform. Our analysis is fully based on simulations, spans a space of seven $谓w$CDM cosmological parameters, and forward models the most relevant sources of systematics inherent in the data: masks, noise variations, clustering of the sources, intrinsic alignments, and shear and redshift calibration. We implement a neural network compression of the summary statistics, and we estimate the parameter posteriors using a simulation-based inference approach. Including and combining different non-Gaussian statistics is a powerful tool that strongly improves constraints over Gaussian statistics (in our case, the second moments); in particular, the Figure of Merit $\textrm{FoM}(S_8, 惟_{\textrm{m}})$ is improved by 70 percent ($螞$CDM) and 90 percent ($w$CDM). When all the summary statistics are combined, we achieve a 2 percent constraint on the amplitude of fluctuations parameter $S_8 \equiv 蟽_8 (惟_{\textrm{m}}/0.3)^{0.5}$, obtaining $S_8 = 0.794 \pm 0.017$ ($螞$CDM) and $S_8 = 0.817 \pm 0.021$ ($w$CDM). The constraints from different statistics are shown to be internally consistent (with a $p$-value>0.1 for all combinations of statistics examined). We compare our results to other weak lensing results from the DES Y3 data, finding good consistency; we also compare with results from external datasets, such as \planck{} constraints from the Cosmic Microwave Background, finding statistical agreement, with discrepancies no greater than $<2.2蟽$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.10881v1-abstract-full').style.display = 'none'; document.getElementById('2405.10881v1-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 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">24 pages, 13 figures, to be submitted to PRD. 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/2404.18278">arXiv:2404.18278</a> <span> [<a href="https://arxiv.org/pdf/2404.18278">pdf</a>, <a href="https://arxiv.org/format/2404.18278">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 Gravitational Lensing Imprints of DES Y3 Superstructures on the CMB: A Matched Filtering Approach </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Demirbozan%2C+U">Umut Demirbozan</a>, <a href="/search/astro-ph?searchtype=author&query=Nadathur%2C+S">Seshadri Nadathur</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrero%2C+I">Ismael Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Fosalba%2C+P">Pablo Fosalba</a>, <a href="/search/astro-ph?searchtype=author&query=Kovacs%2C+A">Andras Kovacs</a>, <a href="/search/astro-ph?searchtype=author&query=Miquel%2C+R">Ramon Miquel</a>, <a href="/search/astro-ph?searchtype=author&query=Davies%2C+C+T">Christopher T. Davies</a>, <a href="/search/astro-ph?searchtype=author&query=Pandey%2C+S">Shivam Pandey</a>, <a href="/search/astro-ph?searchtype=author&query=Adamow%2C+M">Monika Adamow</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">Keith Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">Alex Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R">Robert Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+W">Will Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Pieres%2C+A">Adriano Pieres</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A">Ashley Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E">Eli Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Sheldon%2C+E">Erin Sheldon</a>, <a href="/search/astro-ph?searchtype=author&query=Yanny%2C+B">Brian Yanny</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T">Tim Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">Michel Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">Sahar Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+O">Otavio Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">David Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">Emmanuel Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">Sebastian Bocquet</a> , et al. (41 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="2404.18278v2-abstract-short" style="display: inline;"> $ $Low density cosmic voids gravitationally lens the cosmic microwave background (CMB), leaving a negative imprint on the CMB convergence $魏… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18278v2-abstract-full').style.display = 'inline'; document.getElementById('2404.18278v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.18278v2-abstract-full" style="display: none;"> $ $Low density cosmic voids gravitationally lens the cosmic microwave background (CMB), leaving a negative imprint on the CMB convergence $魏$. This effect provides insight into the distribution of matter within voids, and can also be used to study the growth of structure. We measure this lensing imprint by cross-correlating the Planck CMB lensing convergence map with voids identified in the Dark Energy Survey Year 3 data set, covering approximately 4,200 deg$^2$ of the sky. We use two distinct void-finding algorithms: a 2D void-finder which operates on the projected galaxy density field in thin redshift shells, and a new code, Voxel, which operates on the full 3D map of galaxy positions. We employ an optimal matched filtering method for cross-correlation, using the MICE N-body simulation both to establish the template for the matched filter and to calibrate detection significances. Using the DES Y3 photometric luminous red galaxy sample, we measure $A_魏$, the amplitude of the observed lensing signal relative to the simulation template, obtaining $A_魏= 1.03 \pm 0.22$ ($4.6蟽$ significance) for Voxel and $A_魏= 1.02 \pm 0.17$ ($5.9蟽$ significance) for 2D voids, both consistent with $螞$CDM expectations. We additionally invert the 2D void-finding process to identify superclusters in the projected density field, for which we measure $A_魏= 0.87 \pm 0.15$ ($5.9蟽$ significance). The leading source of noise in our measurements is Planck noise, implying that future data from the Atacama Cosmology Telescope (ACT), South Pole Telescope (SPT) and CMB-S4 will increase sensitivity and allow for more precise measurements. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.18278v2-abstract-full').style.display = 'none'; document.getElementById('2404.18278v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 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">16 pages, 9 figures. Accepted for publication in 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/2404.08054">arXiv:2404.08054</a> <span> [<a href="https://arxiv.org/pdf/2404.08054">pdf</a>, <a href="https://arxiv.org/format/2404.08054">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"> Stellar Metallicities from DECam $u$-band Photometry: A Study of Milky Way Ultra-Faint Dwarf Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pan%2C+Y">Yue Pan</a>, <a href="/search/astro-ph?searchtype=author&query=Chiti%2C+A">Anirudh Chiti</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">Alex Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Ji%2C+A+P">Alexander P. Ji</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+T+S">Ting S. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Limberg%2C+G">Guilherme Limberg</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+D+L">Douglas L. Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">Sahar Allam</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="2404.08054v1-abstract-short" style="display: inline;"> We conducted an in-depth analysis of candidate member stars located in the peripheries of three ultra-faint dwarf (UFD) galaxy satellites of the Milky Way: Bo枚tes I (Boo1), Bo枚tes II (Boo2), and Segue I (Seg1). Studying these peripheral stars has previously been difficult due to contamination from the Milky Way foreground. We used $u$-band photometry from the Dark Energy Camera (DECam) to derive m… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08054v1-abstract-full').style.display = 'inline'; document.getElementById('2404.08054v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.08054v1-abstract-full" style="display: none;"> We conducted an in-depth analysis of candidate member stars located in the peripheries of three ultra-faint dwarf (UFD) galaxy satellites of the Milky Way: Bo枚tes I (Boo1), Bo枚tes II (Boo2), and Segue I (Seg1). Studying these peripheral stars has previously been difficult due to contamination from the Milky Way foreground. We used $u$-band photometry from the Dark Energy Camera (DECam) to derive metallicities to efficiently select UFD candidate member stars. This approach was validated on Boo1, where we identified both previously known and new candidate member stars beyond five half-light radii. We then applied a similar procedure to Boo2 and Seg1. Our findings hinted at evidence for tidal features in Boo1 and Seg1, with Boo1 having an elongation consistent with its proper motion and Seg1 showing some distant candidate stars, a few of which are along its elongation and proper motion. We find two Boo2 stars at large distances consistent with being candidate member stars. Using a foreground contamination rate derived from the \emph{Besan莽on} Galaxy model, we ascribed purity estimates to each candidate member star. We recommend further spectroscopic studies on the newly identified high-purity members. Our technique offers promise for future endeavors to detect candidate member stars at large radii in other systems, leveraging metallicity-sensitive filters with the Legacy Survey of Space and Time and the new, narrow-band Ca HK filter on DECam. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.08054v1-abstract-full').style.display = 'none'; document.getElementById('2404.08054v1-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 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">25 pages, 13 figures, machine-readable Tables 3, 4, 5 in source. Submitted to ApJ. 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/2404.06098">arXiv:2404.06098</a> <span> [<a href="https://arxiv.org/pdf/2404.06098">pdf</a>, <a href="https://arxiv.org/format/2404.06098">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"> Weak lensing combined with the kinetic Sunyaev Zel'dovich effect: A study of baryonic feedback </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bigwood%2C+L">L. Bigwood</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</a>, <a href="/search/astro-ph?searchtype=author&query=Schneider%2C+A">A. Schneider</a>, <a href="/search/astro-ph?searchtype=author&query=Salcido%2C+J">J. Salcido</a>, <a href="/search/astro-ph?searchtype=author&query=McCarthy%2C+I+G">I. G. McCarthy</a>, <a href="/search/astro-ph?searchtype=author&query=Preston%2C+C">C. Preston</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+D">D. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Sijacki%2C+D">D. Sijacki</a>, <a href="/search/astro-ph?searchtype=author&query=Schaan%2C+E">E. Schaan</a>, <a href="/search/astro-ph?searchtype=author&query=Ferraro%2C+S">S. Ferraro</a>, <a href="/search/astro-ph?searchtype=author&query=Battaglia%2C+N">N. Battaglia</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+A">A. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Dodelson%2C+S">S. Dodelson</a>, <a href="/search/astro-ph?searchtype=author&query=Roodman%2C+A">A. Roodman</a>, <a href="/search/astro-ph?searchtype=author&query=Pieres%2C+A">A. Pieres</a>, <a href="/search/astro-ph?searchtype=author&query=Ferte%2C+A">A. Ferte</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">A. Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+A">A. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro-Alsina%2C+A">A. Navarro-Alsina</a>, <a href="/search/astro-ph?searchtype=author&query=Campos%2C+A">A. Campos</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</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=Yin%2C+B">B. Yin</a>, <a href="/search/astro-ph?searchtype=author&query=Yanny%2C+B">B. Yanny</a> , et al. (100 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="2404.06098v1-abstract-short" style="display: inline;"> Extracting precise cosmology from weak lensing surveys requires modelling the non-linear matter power spectrum, which is suppressed at small scales due to baryonic feedback processes. However, hydrodynamical galaxy formation simulations make widely varying predictions for the amplitude and extent of this effect. We use measurements of Dark Energy Survey Year 3 weak lensing (WL) and Atacama Cosmolo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.06098v1-abstract-full').style.display = 'inline'; document.getElementById('2404.06098v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.06098v1-abstract-full" style="display: none;"> Extracting precise cosmology from weak lensing surveys requires modelling the non-linear matter power spectrum, which is suppressed at small scales due to baryonic feedback processes. However, hydrodynamical galaxy formation simulations make widely varying predictions for the amplitude and extent of this effect. We use measurements of Dark Energy Survey Year 3 weak lensing (WL) and Atacama Cosmology Telescope DR5 kinematic Sunyaev-Zel'dovich (kSZ) to jointly constrain cosmological and astrophysical baryonic feedback parameters using a flexible analytical model, `baryonification'. First, using WL only, we compare the $S_8$ constraints using baryonification to a simulation-calibrated halo model, a simulation-based emulator model and the approach of discarding WL measurements on small angular scales. We find that model flexibility can shift the value of $S_8$ and degrade the uncertainty. The kSZ provides additional constraints on the astrophysical parameters and shifts $S_8$ to $S_8=0.823^{+0.019}_{-0.020}$, a higher value than attained using the WL-only analysis. We measure the suppression of the non-linear matter power spectrum using WL + kSZ and constrain a mean feedback scenario that is more extreme than the predictions from most hydrodynamical simulations. We constrain the baryon fractions and the gas mass fractions and find them to be generally lower than inferred from X-ray observations and simulation predictions. We conclude that the WL + kSZ measurements provide a new and complementary benchmark for building a coherent picture of the impact of gas around galaxies across observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.06098v1-abstract-full').style.display = 'none'; document.getElementById('2404.06098v1-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.02314">arXiv:2403.02314</a> <span> [<a href="https://arxiv.org/pdf/2403.02314">pdf</a>, <a href="https://arxiv.org/format/2403.02314">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"> Dark Energy Survey Year 3 results: likelihood-free, simulation-based $w$CDM inference with neural compression of weak-lensing map statistics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Jeffrey%2C+N">N. Jeffrey</a>, <a href="/search/astro-ph?searchtype=author&query=Whiteway%2C+L">L. Whiteway</a>, <a href="/search/astro-ph?searchtype=author&query=Gatti%2C+M">M. Gatti</a>, <a href="/search/astro-ph?searchtype=author&query=Williamson%2C+J">J. Williamson</a>, <a href="/search/astro-ph?searchtype=author&query=Alsing%2C+J">J. Alsing</a>, <a href="/search/astro-ph?searchtype=author&query=Porredon%2C+A">A. Porredon</a>, <a href="/search/astro-ph?searchtype=author&query=Prat%2C+J">J. Prat</a>, <a href="/search/astro-ph?searchtype=author&query=Doux%2C+C">C. Doux</a>, <a href="/search/astro-ph?searchtype=author&query=Jain%2C+B">B. Jain</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">C. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+T+-">T. -Y. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Kacprzak%2C+T">T. Kacprzak</a>, <a href="/search/astro-ph?searchtype=author&query=Lemos%2C+P">P. Lemos</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</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=Bernstein%2C+G+M">G. M. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Campos%2C+A">A. Campos</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=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+A">A. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=DeRose%2C+J">J. DeRose</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">A. Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Eckert%2C+K">K. Eckert</a> , et al. (66 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.02314v1-abstract-short" style="display: inline;"> We present simulation-based cosmological $w$CDM inference using Dark Energy Survey Year 3 weak-lensing maps, via neural data compression of weak-lensing map summary statistics: power spectra, peak counts, and direct map-level compression/inference with convolutional neural networks (CNN). Using simulation-based inference, also known as likelihood-free or implicit inference, we use forward-modelled… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02314v1-abstract-full').style.display = 'inline'; document.getElementById('2403.02314v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.02314v1-abstract-full" style="display: none;"> We present simulation-based cosmological $w$CDM inference using Dark Energy Survey Year 3 weak-lensing maps, via neural data compression of weak-lensing map summary statistics: power spectra, peak counts, and direct map-level compression/inference with convolutional neural networks (CNN). Using simulation-based inference, also known as likelihood-free or implicit inference, we use forward-modelled mock data to estimate posterior probability distributions of unknown parameters. This approach allows all statistical assumptions and uncertainties to be propagated through the forward-modelled mock data; these include sky masks, non-Gaussian shape noise, shape measurement bias, source galaxy clustering, photometric redshift uncertainty, intrinsic galaxy alignments, non-Gaussian density fields, neutrinos, and non-linear summary statistics. We include a series of tests to validate our inference results. This paper also describes the Gower Street simulation suite: 791 full-sky PKDGRAV dark matter simulations, with cosmological model parameters sampled with a mixed active-learning strategy, from which we construct over 3000 mock DES lensing data sets. For $w$CDM inference, for which we allow $-1<w<-\frac{1}{3}$, our most constraining result uses power spectra combined with map-level (CNN) inference. Using gravitational lensing data only, this map-level combination gives $惟_{\rm m} = 0.283^{+0.020}_{-0.027}$, ${S_8 = 0.804^{+0.025}_{-0.017}}$, and $w < -0.80$ (with a 68 per cent credible interval); compared to the power spectrum inference, this is more than a factor of two improvement in dark energy parameter ($惟_{\rm DE}, w$) precision. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02314v1-abstract-full').style.display = 'none'; document.getElementById('2403.02314v1-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 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">19 pages, 15 figures, submitted to Monthly Notices of the Royal Astronomical Society</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.18690">arXiv:2402.18690</a> <span> [<a href="https://arxiv.org/pdf/2402.18690">pdf</a>, <a href="https://arxiv.org/format/2402.18690">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 Dark Energy Survey 5-year photometrically classified type Ia supernovae without host-galaxy redshifts </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=M%C3%B6ller%2C+A">A. M枚ller</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Nichol%2C+R+C">R. C. Nichol</a>, <a href="/search/astro-ph?searchtype=author&query=S%C3%A1nchez%2C+B+O">B. O. S谩nchez</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+B+E">B. E. Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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=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=Bertin%2C+E">E. Bertin</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=Castander%2C+F+J">F. J. Castander</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a> , et al. (38 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.18690v2-abstract-short" style="display: inline;"> Current and future Type Ia Supernova (SN Ia) surveys will need to adopt new approaches to classifying SNe and obtaining their redshifts without spectra if they wish to reach their full potential. We present here a novel approach that uses only photometry to identify SNe Ia in the 5-year Dark Energy Survey (DES) dataset using the SuperNNova classifier. Our approach, which does not rely on any infor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18690v2-abstract-full').style.display = 'inline'; document.getElementById('2402.18690v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.18690v2-abstract-full" style="display: none;"> Current and future Type Ia Supernova (SN Ia) surveys will need to adopt new approaches to classifying SNe and obtaining their redshifts without spectra if they wish to reach their full potential. We present here a novel approach that uses only photometry to identify SNe Ia in the 5-year Dark Energy Survey (DES) dataset using the SuperNNova classifier. Our approach, which does not rely on any information from the SN host-galaxy, recovers SNe Ia that might otherwise be lost due to a lack of an identifiable host. We select 2,298 high-quality SNe Ia from the DES 5-year dataset an almost complete sample of detected SNe Ia. More than 700 of these have no spectroscopic host redshift and are potentially new SNIa compared to the DES-SN5YR cosmology analysis. To analyse these SNe Ia, we derive their redshifts and properties using only their light-curves with a modified version of the SALT2 light-curve fitter. Compared to other DES SN Ia samples with spectroscopic redshifts, our new sample has in average higher redshift, bluer and broader light-curves, and fainter host-galaxies. Future surveys such as LSST will also face an additional challenge, the scarcity of spectroscopic resources for follow-up. When applying our novel method to DES data, we reduce the need for follow-up by a factor of four and three for host-galaxy and live SN respectively compared to earlier approaches. Our novel method thus leads to better optimisation of spectroscopic resources for follow-up. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18690v2-abstract-full').style.display = 'none'; document.getElementById('2402.18690v2-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 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted 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/2402.10697">arXiv:2402.10697</a> <span> [<a href="https://arxiv.org/pdf/2402.10697">pdf</a>, <a href="https://arxiv.org/format/2402.10697">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"> Dark Energy Survey: Galaxy Sample for the Baryonic Acoustic Oscillation Measurement from the Final Dataset </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mena-Fern%C3%A1ndez%2C+J">J. Mena-Fern谩ndez</a>, <a href="/search/astro-ph?searchtype=author&query=Rodr%C3%ADguez-Monroy%2C+M">M. Rodr铆guez-Monroy</a>, <a href="/search/astro-ph?searchtype=author&query=Avila%2C+S">S. Avila</a>, <a href="/search/astro-ph?searchtype=author&query=Porredon%2C+A">A. Porredon</a>, <a href="/search/astro-ph?searchtype=author&query=Chan%2C+K+C">K. C. Chan</a>, <a href="/search/astro-ph?searchtype=author&query=Camacho%2C+H">H. Camacho</a>, <a href="/search/astro-ph?searchtype=author&query=Weaverdyck%2C+N">N. Weaverdyck</a>, <a href="/search/astro-ph?searchtype=author&query=Sevilla-Noarbe%2C+I">I. Sevilla-Noarbe</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+E">E. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Cipriano%2C+L+T+S">L. Toribio San Cipriano</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=Ferrero%2C+I">I. Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Cawthon%2C+R">R. Cawthon</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=Elvin-Poole%2C+J">J. Elvin-Poole</a>, <a href="/search/astro-ph?searchtype=author&query=Giannini%2C+G">G. Giannini</a>, <a href="/search/astro-ph?searchtype=author&query=Adamow%2C+M">M. Adamow</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">A. Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">R. A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+W+G">W. G. Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Pieres%2C+A">A. Pieres</a>, <a href="/search/astro-ph?searchtype=author&query=Ross%2C+A+J">A. J. Ross</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Sheldon%2C+E">E. Sheldon</a> , et al. (63 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.10697v1-abstract-short" style="display: inline;"> In this paper we present and validate the galaxy sample used for the analysis of the baryon acoustic oscillation (BAO) signal in the Dark Energy Survey (DES) Y6 data. The definition is based on a color and redshift-dependent magnitude cut optimized to select galaxies at redshifts higher than 0.6, while ensuring a high-quality photo-$z$ determination. The optimization is performed using a Fisher fo… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.10697v1-abstract-full').style.display = 'inline'; document.getElementById('2402.10697v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.10697v1-abstract-full" style="display: none;"> In this paper we present and validate the galaxy sample used for the analysis of the baryon acoustic oscillation (BAO) signal in the Dark Energy Survey (DES) Y6 data. The definition is based on a color and redshift-dependent magnitude cut optimized to select galaxies at redshifts higher than 0.6, while ensuring a high-quality photo-$z$ determination. The optimization is performed using a Fisher forecast algorithm, finding the optimal $i$-magnitude cut to be given by $i$<19.64+2.894$z_{\rm ph}$. For the optimal sample, we forecast an increase in precision in the BAO measurement of $\sim$25% with respect to the Y3 analysis. Our BAO sample has a total of 15,937,556 galaxies in the redshift range 0.6<$z_{\rm ph}$<1.2, and its angular mask covers 4,273.42 deg${}^2$ to a depth of $i$=22.5. We validate its redshift distributions with three different methods: directional neighborhood fitting algorithm (DNF), which is our primary photo-$z$ estimation; direct calibration with spectroscopic redshifts from VIPERS; and clustering redshift using SDSS galaxies. The fiducial redshift distribution is a combination of these three techniques performed by modifying the mean and width of the DNF distributions to match those of VIPERS and clustering redshift. In this paper we also describe the methodology used to mitigate the effect of observational systematics, which is analogous to the one used in the Y3 analysis. This paper is one of the two dedicated to the analysis of the BAO signal in DES Y6. In its companion paper, we present the angular diameter distance constraints obtained through the fitting to the BAO scale. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.10697v1-abstract-full').style.display = 'none'; document.getElementById('2402.10697v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">23 pages, 10 figures. Submitted to PRD</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-24-0072-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.10696">arXiv:2402.10696</a> <span> [<a href="https://arxiv.org/pdf/2402.10696">pdf</a>, <a href="https://arxiv.org/format/2402.10696">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"> Dark Energy Survey: A 2.1% measurement of the angular Baryonic Acoustic Oscillation scale at redshift $z_{\rm eff}$=0.85 from the final dataset </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DES+Collaboration"> DES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Adamow%2C+M">M. Adamow</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</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=Bechtol%2C+K">K. Bechtol</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=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=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Camacho%2C+H">H. Camacho</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=Carollo%2C+D">D. Carollo</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Castander%2C+F+J">F. J. Castander</a>, <a href="/search/astro-ph?searchtype=author&query=Cawthon%2C+R">R. Cawthon</a>, <a href="/search/astro-ph?searchtype=author&query=Chan%2C+K+C">K. C. Chan</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="2402.10696v1-abstract-short" style="display: inline;"> We present the angular diameter distance measurement obtained with the Baryonic Acoustic Oscillation feature from galaxy clustering in the completed Dark Energy Survey, consisting of six years (Y6) of observations. We use the Y6 BAO galaxy sample, optimized for BAO science in the redshift range 0.6<$z$<1.2, with an effective redshift at $z_{\rm eff}$=0.85 and split into six tomographic bins. The s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.10696v1-abstract-full').style.display = 'inline'; document.getElementById('2402.10696v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.10696v1-abstract-full" style="display: none;"> We present the angular diameter distance measurement obtained with the Baryonic Acoustic Oscillation feature from galaxy clustering in the completed Dark Energy Survey, consisting of six years (Y6) of observations. We use the Y6 BAO galaxy sample, optimized for BAO science in the redshift range 0.6<$z$<1.2, with an effective redshift at $z_{\rm eff}$=0.85 and split into six tomographic bins. The sample has nearly 16 million galaxies over 4,273 square degrees. Our consensus measurement constrains the ratio of the angular distance to sound horizon scale to $D_M(z_{\rm eff})/r_d$ = 19.51$\pm$0.41 (at 68.3% confidence interval), resulting from comparing the BAO position in our data to that predicted by Planck $螞$CDM via the BAO shift parameter $伪=(D_M/r_d)/(D_M/r_d)_{\rm Planck}$. To achieve this, the BAO shift is measured with three different methods, Angular Correlation Function (ACF), Angular Power Spectrum (APS), and Projected Correlation Function (PCF) obtaining $伪=$ 0.952$\pm$0.023, 0.962$\pm$0.022, and 0.955$\pm$0.020, respectively, which we combine to $伪=$ 0.957$\pm$0.020, including systematic errors. When compared with the $螞$CDM model that best fits Planck data, this measurement is found to be 4.3% and 2.1$蟽$ below the angular BAO scale predicted. To date, it represents the most precise angular BAO measurement at $z$>0.75 from any survey and the most precise measurement at any redshift from photometric surveys. The analysis was performed blinded to the BAO position and it is shown to be robust against analysis choices, data removal, redshift calibrations and observational systematics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.10696v1-abstract-full').style.display = 'none'; document.getElementById('2402.10696v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to PRD, 39 pages, 12 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-24-0027-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.02929">arXiv:2401.02929</a> <span> [<a href="https://arxiv.org/pdf/2401.02929">pdf</a>, <a href="https://arxiv.org/format/2401.02929">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 Dark Energy Survey: Cosmology Results With ~1500 New High-redshift Type Ia Supernovae Using The Full 5-year Dataset </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=DES+Collaboration"> DES Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Acevedo%2C+M">M. Acevedo</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">J. Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Armstrong%2C+P">P. Armstrong</a>, <a href="/search/astro-ph?searchtype=author&query=Asorey%2C+J">J. Asorey</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=Bassett%2C+B+A">B. A. Bassett</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardinelli%2C+P+H">P. H. Bernardinelli</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=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=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Buckley-Geer%2C+E">E. Buckley-Geer</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</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="2401.02929v3-abstract-short" style="display: inline;"> We present cosmological constraints from the sample of Type Ia supernovae (SN Ia) discovered during the full five years of the Dark Energy Survey (DES) Supernova Program. In contrast to most previous cosmological samples, in which SN are classified based on their spectra, we classify the DES SNe using a machine learning algorithm applied to their light curves in four photometric bands. Spectroscop… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02929v3-abstract-full').style.display = 'inline'; document.getElementById('2401.02929v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.02929v3-abstract-full" style="display: none;"> We present cosmological constraints from the sample of Type Ia supernovae (SN Ia) discovered during the full five years of the Dark Energy Survey (DES) Supernova Program. In contrast to most previous cosmological samples, in which SN are classified based on their spectra, we classify the DES SNe using a machine learning algorithm applied to their light curves in four photometric bands. Spectroscopic redshifts are acquired from a dedicated follow-up survey of the host galaxies. After accounting for the likelihood of each SN being a SN Ia, we find 1635 DES SNe in the redshift range $0.10<z<1.13$ that pass quality selection criteria sufficient to constrain cosmological parameters. This quintuples the number of high-quality $z>0.5$ SNe compared to the previous leading compilation of Pantheon+, and results in the tightest cosmological constraints achieved by any SN data set to date. To derive cosmological constraints we combine the DES supernova data with a high-quality external low-redshift sample consisting of 194 SNe Ia spanning $0.025<z<0.10$. Using SN data alone and including systematic uncertainties we find $惟_{\rm M}=0.352\pm 0.017$ in flat $螞$CDM. Supernova data alone now require acceleration ($q_0<0$ in $螞$CDM) with over $5蟽$ confidence. We find $(惟_{\rm M},w)=(0.264^{+0.074}_{-0.096},-0.80^{+0.14}_{-0.16})$ in flat $w$CDM. For flat $w_0w_a$CDM, we find $(惟_{\rm M},w_0,w_a)=(0.495^{+0.033}_{-0.043},-0.36^{+0.36}_{-0.30},-8.8^{+3.7}_{-4.5})$. Including Planck CMB data, SDSS BAO data, and DES $3\times2$-point data gives $(惟_{\rm M},w)=(0.321\pm0.007,-0.941\pm0.026)$. In all cases dark energy is consistent with a cosmological constant to within $\sim2蟽$. In our analysis, systematic errors on cosmological parameters are subdominant compared to statistical errors; paving the way for future photometrically classified supernova analyses. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02929v3-abstract-full').style.display = 'none'; document.getElementById('2401.02929v3-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 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">22 pages, 12 figures; Accepted by ApJL 29 March 2024; v3 updates to accepted version and includes links to data</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-23-0821-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.02075">arXiv:2401.02075</a> <span> [<a href="https://arxiv.org/pdf/2401.02075">pdf</a>, <a href="https://arxiv.org/format/2401.02075">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"> SPT Clusters with DES and HST Weak Lensing. II. Cosmological Constraints from the Abundance of Massive Halos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/astro-ph?searchtype=author&query=Bleem%2C+L+E">L. E. Bleem</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+M">M. Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Mohr%2C+J+J">J. J. Mohr</a>, <a href="/search/astro-ph?searchtype=author&query=Schrabback%2C+T">T. Schrabback</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</a>, <a href="/search/astro-ph?searchtype=author&query=Ade%2C+P+A+R">P. A. R. Ade</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+S+W">S. W. Allen</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=Anderson%2C+A+J">A. J. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">J. Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Ansarinejad%2C+B">B. Ansarinejad</a>, <a href="/search/astro-ph?searchtype=author&query=Austermann%2C+J+E">J. E. Austermann</a>, <a href="/search/astro-ph?searchtype=author&query=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=Bayliss%2C+M">M. Bayliss</a>, <a href="/search/astro-ph?searchtype=author&query=Beall%2C+J+A">J. A. Beall</a>, <a href="/search/astro-ph?searchtype=author&query=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=Bender%2C+A+N">A. N. Bender</a> , et al. (171 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="2401.02075v2-abstract-short" style="display: inline;"> We present cosmological constraints from the abundance of galaxy clusters selected via the thermal Sunyaev-Zel'dovich (SZ) effect in South Pole Telescope (SPT) data with a simultaneous mass calibration using weak gravitational lensing data from the Dark Energy Survey (DES) and the Hubble Space Telescope (HST). The cluster sample is constructed from the combined SPT-SZ, SPTpol ECS, and SPTpol 500d… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02075v2-abstract-full').style.display = 'inline'; document.getElementById('2401.02075v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.02075v2-abstract-full" style="display: none;"> We present cosmological constraints from the abundance of galaxy clusters selected via the thermal Sunyaev-Zel'dovich (SZ) effect in South Pole Telescope (SPT) data with a simultaneous mass calibration using weak gravitational lensing data from the Dark Energy Survey (DES) and the Hubble Space Telescope (HST). The cluster sample is constructed from the combined SPT-SZ, SPTpol ECS, and SPTpol 500d surveys, and comprises 1,005 confirmed clusters in the redshift range $0.25-1.78$ over a total sky area of 5,200 deg$^2$. We use DES Year 3 weak-lensing data for 688 clusters with redshifts $z<0.95$ and HST weak-lensing data for 39 clusters with $0.6<z<1.7$. The weak-lensing measurements enable robust mass measurements of sample clusters and allow us to empirically constrain the SZ observable--mass relation. For a flat $螞$CDM cosmology, and marginalizing over the sum of massive neutrinos, we measure $惟_\mathrm{m}=0.286\pm0.032$, $蟽_8=0.817\pm0.026$, and the parameter combination $蟽_8\,(惟_\mathrm{m}/0.3)^{0.25}=0.805\pm0.016$. Our measurement of $S_8\equiv蟽_8\,\sqrt{惟_\mathrm{m}/0.3}=0.795\pm0.029$ and the constraint from Planck CMB anisotropies (2018 TT,TE,EE+lowE) differ by $1.1蟽$. In combination with that Planck dataset, we place a 95% upper limit on the sum of neutrino masses $\sum m_谓<0.18$ eV. When additionally allowing the dark energy equation of state parameter $w$ to vary, we obtain $w=-1.45\pm0.31$ from our cluster-based analysis. In combination with Planck data, we measure $w=-1.34^{+0.22}_{-0.15}$, or a $2.2蟽$ difference with a cosmological constant. We use the cluster abundance to measure $蟽_8$ in five redshift bins between 0.25 and 1.8, and we find the results to be consistent with structure growth as predicted by the $螞$CDM model fit to Planck primary CMB data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.02075v2-abstract-full').style.display = 'none'; document.getElementById('2401.02075v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 4 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 Phys. Rev. D. arXiv v2 corresponds to published article</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.09721">arXiv:2312.09721</a> <span> [<a href="https://arxiv.org/pdf/2312.09721">pdf</a>, <a href="https://arxiv.org/format/2312.09721">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/10.1051/0004-6361/202348956">10.1051/0004-6361/202348956 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dark Energy Survey Deep Field photometric redshift performance and training incompleteness assessment </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Cipriano%2C+L+T+S">L. Toribio San Cipriano</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=Sevilla-Noarbe%2C+I">I. Sevilla-Noarbe</a>, <a href="/search/astro-ph?searchtype=author&query=Hartley%2C+W+G">W. G. Hartley</a>, <a href="/search/astro-ph?searchtype=author&query=Myles%2C+J">J. Myles</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</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=Choi%2C+A">A. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=Eckert%2C+K">K. Eckert</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">R. A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Harrison%2C+I">I. Harrison</a>, <a href="/search/astro-ph?searchtype=author&query=Sheldon%2C+E">E. Sheldon</a>, <a href="/search/astro-ph?searchtype=author&query=Yanny%2C+B">B. Yanny</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Campos%2C+A">A. Campos</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=Castander%2C+F+J">F. J. Castander</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">C. Conselice</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> , et al. (33 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.09721v3-abstract-short" style="display: inline;"> Context. The determination of accurate photometric redshifts (photo-zs) in large imaging galaxy surveys is key for cosmological studies. One of the most common approaches are machine learning techniques. These methods require a spectroscopic or reference sample to train the algorithms. Attention has to be paid to the quality and properties of these samples since they are key factors in the estimat… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09721v3-abstract-full').style.display = 'inline'; document.getElementById('2312.09721v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.09721v3-abstract-full" style="display: none;"> Context. The determination of accurate photometric redshifts (photo-zs) in large imaging galaxy surveys is key for cosmological studies. One of the most common approaches are machine learning techniques. These methods require a spectroscopic or reference sample to train the algorithms. Attention has to be paid to the quality and properties of these samples since they are key factors in the estimation of reliable photo-zs. Aims. The goal of this work is to calculate the photo-zs for the Y3 DES Deep Fields catalogue using the DNF machine learning algorithm. Moreover, we want to develop techniques to assess the incompleteness of the training sample and metrics to study how incompleteness affects the quality of photometric redshifts. Finally, we are interested in comparing the performance obtained with respect to the EAzY template fitting approach on Y3 DES Deep Fields catalogue. Methods. We have emulated -- at brighter magnitude -- the training incompleteness with a spectroscopic sample whose redshifts are known to have a measurable view of the problem. We have used a principal component analysis to graphically assess incompleteness and to relate it with the performance parameters provided by DNF. Finally, we have applied the results about the incompleteness to the photo-z computation on Y3 DES Deep Fields with DNF and estimated its performance. Results. The photo-zs for the galaxies on DES Deep Fields have been computed with the DNF algorithm and added to the Y3 DES Deep Fields catalogue. They are available at https://des.ncsa.illinois.edu/releases/y3a2/Y3deepfields. Some techniques have been developed to evaluate the performance in the absence of "true" redshift and to assess completeness. We have studied... (Partial abstract) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.09721v3-abstract-full').style.display = 'none'; document.getElementById('2312.09721v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 15 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 17 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A38 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.13207">arXiv:2310.13207</a> <span> [<a href="https://arxiv.org/pdf/2310.13207">pdf</a>, <a href="https://arxiv.org/format/2310.13207">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"> Dark Energy Survey Year 3 Results: Mis-centering calibration and X-ray-richness scaling relations in redMaPPer clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Kelly%2C+P">P. Kelly</a>, <a href="/search/astro-ph?searchtype=author&query=Jobel%2C+J">J. Jobel</a>, <a href="/search/astro-ph?searchtype=author&query=Eiger%2C+O">O. Eiger</a>, <a href="/search/astro-ph?searchtype=author&query=Abd%2C+A">A. Abd</a>, <a href="/search/astro-ph?searchtype=author&query=Jeltema%2C+T+E">T. E. Jeltema</a>, <a href="/search/astro-ph?searchtype=author&query=Giles%2C+P">P. Giles</a>, <a href="/search/astro-ph?searchtype=author&query=Hollowood%2C+D+L">D. L. Hollowood</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkinson%2C+R+D">R. D. Wilkinson</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+D+J">D. J. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Bhargava%2C+S">S. Bhargava</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+S">S. Everett</a>, <a href="/search/astro-ph?searchtype=author&query=Farahi%2C+A">A. Farahi</a>, <a href="/search/astro-ph?searchtype=author&query=Romer%2C+A+K">A. K. Romer</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Wang%2C+F">F. Wang</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+D">D. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Faridjoo%2C+R">R. Faridjoo</a>, <a href="/search/astro-ph?searchtype=author&query=Franco%2C+J">J. Franco</a>, <a href="/search/astro-ph?searchtype=author&query=Gardner%2C+G">G. Gardner</a>, <a href="/search/astro-ph?searchtype=author&query=Kwiecien%2C+M">M. Kwiecien</a>, <a href="/search/astro-ph?searchtype=author&query=Laubner%2C+D">D. Laubner</a>, <a href="/search/astro-ph?searchtype=author&query=McDaniel%2C+A">A. McDaniel</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Donnell%2C+J+H">J. H. O'Donnell</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+L">L. Sanchez</a> , et al. (54 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="2310.13207v1-abstract-short" style="display: inline;"> We use Dark Energy Survey Year 3 (DES Y3) clusters with archival X-ray data from XMM-Newton and Chandra to assess the centering performance of the redMaPPer cluster finder and to measure key richness observable scaling relations. In terms of centering, we find that 10-20% of redMaPPer clusters are miscentered with no significant difference in bins of low versus high richness ($20<位<40$ and $位>40$)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.13207v1-abstract-full').style.display = 'inline'; document.getElementById('2310.13207v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.13207v1-abstract-full" style="display: none;"> We use Dark Energy Survey Year 3 (DES Y3) clusters with archival X-ray data from XMM-Newton and Chandra to assess the centering performance of the redMaPPer cluster finder and to measure key richness observable scaling relations. In terms of centering, we find that 10-20% of redMaPPer clusters are miscentered with no significant difference in bins of low versus high richness ($20<位<40$ and $位>40$) or redshift ($0.2<z<0.4$ and $0.4 <z < 0.65$). We also investigate the richness bias induced by miscentering. The dominant reasons for miscentering include masked or missing data and the presence of other bright galaxies in the cluster; for half of the miscentered clusters the correct central was one of the other possible centrals identified by redMaPPer, while for $\sim 40$% of miscentered clusters the correct central is not a redMaPPer member with most of these cases due to masking. In addition, we fit the scaling relations between X-ray temperature and richness and between X-ray luminosity and richness. We find a T$_X$-$位$ scatter of $0.21 \pm 0.01$. While the scatter in T$_X$-$位$ is consistent in bins of redshift, we do find modestly different slopes with high-redshift clusters displaying a somewhat shallower relation. Splitting based on richness, we find a marginally larger scatter for our lowest richness bin, $20 < 位< 40$. The X-ray properties of detected, serendipitous clusters are generally consistent with those for targeted clusters, but the depth of the X-ray data for undetected clusters is insufficient to judge whether they are X-ray underluminous in all but one case. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.13207v1-abstract-full').style.display = 'none'; document.getElementById('2310.13207v1-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 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.12213">arXiv:2310.12213</a> <span> [<a href="https://arxiv.org/pdf/2310.12213">pdf</a>, <a href="https://arxiv.org/format/2310.12213">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"> SPT Clusters with DES and HST Weak Lensing. I. Cluster Lensing and Bayesian Population Modeling of Multi-Wavelength Cluster Datasets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Grandis%2C+S">S. Grandis</a>, <a href="/search/astro-ph?searchtype=author&query=Bleem%2C+L+E">L. E. Bleem</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+M">M. Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Mohr%2C+J+J">J. J. Mohr</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Allen%2C+S+W">S. W. Allen</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=Ansarinejad%2C+B">B. Ansarinejad</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bayliss%2C+M">M. Bayliss</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=Brodwin%2C+M">M. Brodwin</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Campos%2C+A">A. Campos</a>, <a href="/search/astro-ph?searchtype=author&query=Canning%2C+R+E+A">R. E. A. Canning</a>, <a href="/search/astro-ph?searchtype=author&query=Carlstrom%2C+J+E">J. E. Carlstrom</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a>, <a href="/search/astro-ph?searchtype=author&query=Kind%2C+M+C">M. Carrasco Kind</a> , et al. (108 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="2310.12213v2-abstract-short" style="display: inline;"> We present a Bayesian population modeling method to analyze the abundance of galaxy clusters identified by the South Pole Telescope (SPT) with a simultaneous mass calibration using weak gravitational lensing data from the Dark Energy Survey (DES) and the Hubble Space Telescope (HST). We discuss and validate the modeling choices with a particular focus on a robust, weak-lensing-based mass calibrati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12213v2-abstract-full').style.display = 'inline'; document.getElementById('2310.12213v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.12213v2-abstract-full" style="display: none;"> We present a Bayesian population modeling method to analyze the abundance of galaxy clusters identified by the South Pole Telescope (SPT) with a simultaneous mass calibration using weak gravitational lensing data from the Dark Energy Survey (DES) and the Hubble Space Telescope (HST). We discuss and validate the modeling choices with a particular focus on a robust, weak-lensing-based mass calibration using DES data. For the DES Year 3 data, we report a systematic uncertainty in weak-lensing mass calibration that increases from 1% at $z=0.25$ to 10% at $z=0.95$, to which we add 2% in quadrature to account for uncertainties in the impact of baryonic effects. We implement an analysis pipeline that joins the cluster abundance likelihood with a multi-observable likelihood for the Sunyaev-Zel'dovich effect, optical richness, and weak-lensing measurements for each individual cluster. We validate that our analysis pipeline can recover unbiased cosmological constraints by analyzing mocks that closely resemble the cluster sample extracted from the SPT-SZ, SPTpol ECS, and SPTpol 500d surveys and the DES Year 3 and HST-39 weak-lensing datasets. This work represents a crucial prerequisite for the subsequent cosmological analysis of the real dataset. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12213v2-abstract-full').style.display = 'none'; document.getElementById('2310.12213v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 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">Accepted for publication in Phys. Rev. D. arXiv v2 corresponds to published article</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.12090">arXiv:2310.12090</a> <span> [<a href="https://arxiv.org/pdf/2310.12090">pdf</a>, <a href="https://arxiv.org/format/2310.12090">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="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Chemical Analysis of the Brightest Star of the Cetus II Ultra-Faint Dwarf Galaxy Candidate </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Webber%2C+K+B">K. B. Webber</a>, <a href="/search/astro-ph?searchtype=author&query=Hansen%2C+T+T">T. T. Hansen</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+J+L">J. L. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Simon%2C+J+D">J. D. Simon</a>, <a href="/search/astro-ph?searchtype=author&query=Pace%2C+A+B">A. B. Pace</a>, <a href="/search/astro-ph?searchtype=author&query=Mutlu-Pakdil%2C+B">B. Mutlu-Pakdil</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">A. Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Mart%C3%8Dnez-V%C3%81zquez%2C+C+E">C. E. Mart脥nez-V脕zquez</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=Alves%2C+O">O. Alves</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</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=Carretero%2C+J">J. Carretero</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=De+Vicente%2C+J">J. De Vicente</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrero%2C+I">I. Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Friedel%2C+D">D. Friedel</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%8Da-Bellido%2C+J">J. Garc脥a-Bellido</a>, <a href="/search/astro-ph?searchtype=author&query=Giannini%2C+G">G. Giannini</a>, <a href="/search/astro-ph?searchtype=author&query=Gruen%2C+D">D. Gruen</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">R. A. Gruendl</a> , et al. (20 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.12090v1-abstract-short" style="display: inline;"> We present a detailed chemical abundance analysis of the brightest star in the ultra-faint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from Carbon to Europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the alp… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12090v1-abstract-full').style.display = 'inline'; document.getElementById('2310.12090v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.12090v1-abstract-full" style="display: none;"> We present a detailed chemical abundance analysis of the brightest star in the ultra-faint dwarf (UFD) galaxy candidate Cetus II from high-resolution Magellan/MIKE spectra. For this star, DES J011740.53-173053, abundances or upper limits of 18 elements from Carbon to Europium are derived. Its chemical abundances generally follow those of other UFD galaxy stars, with a slight enhancement of the alpha-elements (Mg, Si, and Ca) and low neutron-capture element (Sr, Ba, Eu) abundances supporting the classification of Cetus II as a likely UFD. The star exhibits lower Sc, Ti, and V abundances than Milky Way (MW) halo stars with similar metallicity. This signature is consistent with yields from a supernova (SN) originating from a star with a mass of ~11.2 solar masses. In addition, the star has a Potassium abundance of [K/Fe] = 0.81 which is somewhat higher than the K abundances of MW halo stars with similar metallicity, a signature which is also present in a number of UFD galaxies. A comparison including globular clusters (GC) and stellar stream stars suggests that high K is a specific characteristic for some UFD galaxy stars and can thus be used to help classify objects as UFD galaxies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.12090v1-abstract-full').style.display = 'none'; document.getElementById('2310.12090v1-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, 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">15 pages, 7 figures, 5 tables, accepted 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/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/2309.00671">arXiv:2309.00671</a> <span> [<a href="https://arxiv.org/pdf/2309.00671">pdf</a>, <a href="https://arxiv.org/format/2309.00671">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"> Dark Energy Survey Year 6 Results: Intra-Cluster Light from Redshift 0.2 to 0.5 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Zhang%2C+Y">Yuanyuan Zhang</a>, <a href="/search/astro-ph?searchtype=author&query=Golden-Marx%2C+J+B">Jesse B. Golden-Marx</a>, <a href="/search/astro-ph?searchtype=author&query=Ogando%2C+R+L+C">Ricardo L. C. Ogando</a>, <a href="/search/astro-ph?searchtype=author&query=Yanny%2C+B">Brian Yanny</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">Eli S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">Sahar Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</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=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+T+-">T. -Y. Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">C. Conselice</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=Pereira%2C+M+E+S">M. E. S. Pereira</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Diehl%2C+H+T">H. T. Diehl</a>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrero%2C+I">I. Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Flaugher%2C+B">B. Flaugher</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a>, <a href="/search/astro-ph?searchtype=author&query=Gruen%2C+D">D. Gruen</a> , et al. (24 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.00671v1-abstract-short" style="display: inline;"> Using the full six years of imaging data from the Dark Energy Survey, we study the surface brightness profiles of galaxy cluster central galaxies and intra-cluster light. We apply a ``stacking'' method to over four thousand galaxy clusters identified by the redMaPPer cluster finding algorithm in the redshift range of 0.2 to 0.5. This yields high signal-to-noise radial profile measurements of the c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.00671v1-abstract-full').style.display = 'inline'; document.getElementById('2309.00671v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.00671v1-abstract-full" style="display: none;"> Using the full six years of imaging data from the Dark Energy Survey, we study the surface brightness profiles of galaxy cluster central galaxies and intra-cluster light. We apply a ``stacking'' method to over four thousand galaxy clusters identified by the redMaPPer cluster finding algorithm in the redshift range of 0.2 to 0.5. This yields high signal-to-noise radial profile measurements of the central galaxy and intra-cluster light out to 1 Mpc from the cluster center. Using redMaPPer richness as a cluster mass indicator, we find that the intra-cluster light brightness has a strong mass dependence throughout the 0.2 to 0.5 redshift range, and the dependence grows stronger at a larger radius. In terms of redshift evolution, we find some evidence that the central galaxy, as well as the diffuse light within the transition region between the cluster central galaxy and intra-cluster light within 80 kpc from the center, may be growing over time. At larger radii, more than 80 kpc away from the cluster center, we do not find evidence of additional redshift evolution beyond the cluster mass dependence, which is consistent with the findings from the IllustrisTNG hydrodynamic simulation. We speculate that the major driver of intra-cluster light growth, especially at large radii, is associated with cluster mass growth. Finally, we find that the color of the cluster central galaxy and intra-cluster light displays a radial gradient that becomes bluer at a larger radius, which is consistent with a stellar stripping and disruption origin of intra-cluster light as suggested by simulation studies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.00671v1-abstract-full').style.display = 'none'; document.getElementById('2309.00671v1-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 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">Submitted 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/2308.03863">arXiv:2308.03863</a> <span> [<a href="https://arxiv.org/pdf/2308.03863">pdf</a>, <a href="https://arxiv.org/format/2308.03863">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"> Beyond the 3rd moment: A practical study of using lensing convergence CDFs for cosmology with DES Y3 </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=Banerjee%2C+A">A. Banerjee</a>, <a href="/search/astro-ph?searchtype=author&query=Abel%2C+T">T. Abel</a>, <a href="/search/astro-ph?searchtype=author&query=Gatti%2C+M">M. Gatti</a>, <a href="/search/astro-ph?searchtype=author&query=Ajani%2C+V">V. Ajani</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</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=Bernstein%2C+G+M">G. M. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Campos%2C+A">A. Campos</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>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+C">C. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=DeRose%2C+J">J. DeRose</a>, <a href="/search/astro-ph?searchtype=author&query=Diehl%2C+H+T">H. T. Diehl</a>, <a href="/search/astro-ph?searchtype=author&query=Dodelson%2C+S">S. Dodelson</a>, <a href="/search/astro-ph?searchtype=author&query=Doux%2C+C">C. Doux</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">A. Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Eckert%2C+K">K. Eckert</a>, <a href="/search/astro-ph?searchtype=author&query=Elvin-Poole%2C+J">J. Elvin-Poole</a> , et al. (73 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="2308.03863v1-abstract-short" style="display: inline;"> Widefield surveys of the sky probe many clustered scalar fields -- such as galaxy counts, lensing potential, gas pressure, etc. -- that are sensitive to different cosmological and astrophysical processes. Our ability to constrain such processes from these fields depends crucially on the statistics chosen to summarize the field. In this work, we explore the cumulative distribution function (CDF) at… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.03863v1-abstract-full').style.display = 'inline'; document.getElementById('2308.03863v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.03863v1-abstract-full" style="display: none;"> Widefield surveys of the sky probe many clustered scalar fields -- such as galaxy counts, lensing potential, gas pressure, etc. -- that are sensitive to different cosmological and astrophysical processes. Our ability to constrain such processes from these fields depends crucially on the statistics chosen to summarize the field. In this work, we explore the cumulative distribution function (CDF) at multiple scales as a summary of the galaxy lensing convergence field. Using a suite of N-body lightcone simulations, we show the CDFs' constraining power is modestly better than that of the 2nd and 3rd moments of the field, as they approximately capture the information from all moments of the field in a concise data vector. We then study the practical aspects of applying the CDFs to observational data, using the first three years of the Dark Energy Survey (DES Y3) data as an example, and compute the impact of different systematics on the CDFs. The contributions from the point spread function are 2-3 orders of magnitude below the cosmological signal, while those from reduced shear approximation contribute $\lesssim 1\%$ to the signal. Source clustering effects and baryon imprints contribute $1-10\%$. Enforcing scale cuts to limit systematics-driven biases in parameter constraints degrades these constraints a noticeable amount, and this degradation is similar for the CDFs and the moments. We also detect correlations between the observed convergence field and the shape noise field at $13蟽$. We find that the non-Gaussian correlations in the noise field must be modeled accurately to use the CDFs, or other statistics sensitive to all moments, as a rigorous cosmology tool. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.03863v1-abstract-full').style.display = 'none'; document.getElementById('2308.03863v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 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">21 pages, 12 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/2307.13860">arXiv:2307.13860</a> <span> [<a href="https://arxiv.org/pdf/2307.13860">pdf</a>, <a href="https://arxiv.org/format/2307.13860">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"> Detection of the significant impact of source clustering on higher-order statistics with DES Year 3 weak gravitational lensing data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Gatti%2C+M">M. Gatti</a>, <a href="/search/astro-ph?searchtype=author&query=Jeffrey%2C+N">N. Jeffrey</a>, <a href="/search/astro-ph?searchtype=author&query=Whiteway%2C+L">L. Whiteway</a>, <a href="/search/astro-ph?searchtype=author&query=Ajani%2C+V">V. Ajani</a>, <a href="/search/astro-ph?searchtype=author&query=Kacprzak%2C+T">T. Kacprzak</a>, <a href="/search/astro-ph?searchtype=author&query=Z%C3%BCrcher%2C+D">D. Z眉rcher</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">C. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Jain%2C+B">B. Jain</a>, <a href="/search/astro-ph?searchtype=author&query=Blazek%2C+J">J. Blazek</a>, <a href="/search/astro-ph?searchtype=author&query=Krause%2C+E">E. Krause</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</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">M. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+G">G. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Campos%2C+A">A. Campos</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>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+C">C. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Derose%2C+J">J. Derose</a>, <a href="/search/astro-ph?searchtype=author&query=Diehl%2C+H+T">H. T. Diehl</a>, <a href="/search/astro-ph?searchtype=author&query=Dodelson%2C+S">S. Dodelson</a>, <a href="/search/astro-ph?searchtype=author&query=Doux%2C+C">C. Doux</a>, <a href="/search/astro-ph?searchtype=author&query=Eckert%2C+K">K. Eckert</a>, <a href="/search/astro-ph?searchtype=author&query=Elvin-Poole%2C+J">J. Elvin-Poole</a> , et al. (76 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="2307.13860v2-abstract-short" style="display: inline;"> We demonstrate and measure the impact of source galaxy clustering on higher-order summary statistics of weak gravitational lensing data. By comparing simulated data with galaxies that either trace or do not trace the underlying density field, we show this effect can exceed measurement uncertainties for common higher-order statistics for certain analysis choices. Source clustering effects are large… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13860v2-abstract-full').style.display = 'inline'; document.getElementById('2307.13860v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.13860v2-abstract-full" style="display: none;"> We demonstrate and measure the impact of source galaxy clustering on higher-order summary statistics of weak gravitational lensing data. By comparing simulated data with galaxies that either trace or do not trace the underlying density field, we show this effect can exceed measurement uncertainties for common higher-order statistics for certain analysis choices. Source clustering effects are larger at small scales and for statistics applied to combinations of low and high redshift samples, and diminish at high redshift. We evaluate the impact on different weak lensing observables, finding that third moments and wavelet phase harmonics are more affected than peak count statistics. Using Dark Energy Survey Year 3 data we construct null tests for the source-clustering-free case, finding a $p$-value of $p=4\times10^{-3}$ (2.6 $蟽$) using third-order map moments and $p=3\times10^{-11}$ (6.5 $蟽$) using wavelet phase harmonics. The impact of source clustering on cosmological inference can be either be included in the model or minimized through \textit{ad-hoc} procedures (e.g. scale cuts). We verify that the procedures adopted in existing DES Y3 cosmological analyses (using map moments and peaks) were sufficient to render this effect negligible. Failing to account for source clustering can significantly impact cosmological inference from higher-order gravitational lensing statistics, e.g. higher-order N-point functions, wavelet-moment observables (including phase harmonics and scattering transforms), and deep learning or field level summary statistics of weak lensing maps. We provide recipes both to minimise the impact of source clustering and to incorporate source clustering effects into forward-modelled mock data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13860v2-abstract-full').style.display = 'none'; document.getElementById('2307.13860v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 25 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">5 pages, 2 figures, submitted to MNRAS Letters</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.06792">arXiv:2305.06792</a> <span> [<a href="https://arxiv.org/pdf/2305.06792">pdf</a>, <a href="https://arxiv.org/format/2305.06792">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevD.108.023516">10.1103/PhysRevD.108.023516 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Kinematic Sunyaev-Zel'dovich Effect with ACT, DES, and BOSS: a Novel Hybrid Estimator </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Mallaby-Kay%2C+M">M. Mallaby-Kay</a>, <a href="/search/astro-ph?searchtype=author&query=Amodeo%2C+S">S. Amodeo</a>, <a href="/search/astro-ph?searchtype=author&query=Hill%2C+J+C">J. C. Hill</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=Annis%2C+J">J. Annis</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=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=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=Kind%2C+M+C">M. Carrasco Kind</a>, <a href="/search/astro-ph?searchtype=author&query=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+A">A. Choi</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. (58 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.06792v3-abstract-short" style="display: inline;"> The kinematic and thermal Sunyaev-Zel'dovich (kSZ and tSZ) effects probe the abundance and thermodynamics of ionized gas in galaxies and clusters. We present a new hybrid estimator to measure the kSZ effect by combining cosmic microwave background temperature anisotropy maps with photometric and spectroscopic optical survey data. The method interpolates a velocity reconstruction from a spectroscop… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.06792v3-abstract-full').style.display = 'inline'; document.getElementById('2305.06792v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.06792v3-abstract-full" style="display: none;"> The kinematic and thermal Sunyaev-Zel'dovich (kSZ and tSZ) effects probe the abundance and thermodynamics of ionized gas in galaxies and clusters. We present a new hybrid estimator to measure the kSZ effect by combining cosmic microwave background temperature anisotropy maps with photometric and spectroscopic optical survey data. The method interpolates a velocity reconstruction from a spectroscopic catalog at the positions of objects in a photometric catalog, which makes it possible to leverage the high number density of the photometric catalog and the precision of the spectroscopic survey. Combining this hybrid kSZ estimator with a measurement of the tSZ effect simultaneously constrains the density and temperature of free electrons in the photometrically selected galaxies. Using the 1000 deg2 of overlap between the Atacama Cosmology Telescope (ACT) Data Release 5, the first three years of data from the Dark Energy Survey (DES), and the Baryon Oscillation Spectroscopic Survey (BOSS) Data Release 12, we detect the kSZ signal at 4.8$蟽$ and reject the null (no-kSZ) hypothesis at 5.1$蟽$. This corresponds to 2.0$蟽$ per 100,000 photometric objects with a velocity field based on a spectroscopic survey with 1/5th the density of the photometric catalog. For comparison, a recent ACT analysis using exclusively spectroscopic data from BOSS measured the kSZ signal at 2.1$蟽$ per 100,000 objects. Our derived constraints on the thermodynamic properties of the galaxy halos are consistent with previous measurements. With future surveys, such as the Dark Energy Spectroscopic Instrument and the Rubin Observatory Legacy Survey of Space and Time, we expect that this hybrid estimator could result in measurements with significantly better signal-to-noise than those that rely on spectroscopic data alone. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.06792v3-abstract-full').style.display = 'none'; document.getElementById('2305.06792v3-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 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 11 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">19 pages, 15 figures - matches published version</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 108, 023516 - Published 18 July 2023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.02365">arXiv:2305.02365</a> <span> [<a href="https://arxiv.org/pdf/2305.02365">pdf</a>, <a href="https://arxiv.org/format/2305.02365">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> </div> </div> <p class="title is-5 mathjax"> Cool Cores in Clusters of Galaxies in the Dark Energy Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Graham%2C+K">K. Graham</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Donnell%2C+J">J. O'Donnell</a>, <a href="/search/astro-ph?searchtype=author&query=Silverstein%2C+M+M">M. M. Silverstein</a>, <a href="/search/astro-ph?searchtype=author&query=Eiger%2C+O">O. Eiger</a>, <a href="/search/astro-ph?searchtype=author&query=Jeltema%2C+T+E">T. E. Jeltema</a>, <a href="/search/astro-ph?searchtype=author&query=Hollowood%2C+D+L">D. L. Hollowood</a>, <a href="/search/astro-ph?searchtype=author&query=Cross%2C+D">D. Cross</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+S">S. Everett</a>, <a href="/search/astro-ph?searchtype=author&query=Giles%2C+P">P. Giles</a>, <a href="/search/astro-ph?searchtype=author&query=Jobel%2C+J">J. Jobel</a>, <a href="/search/astro-ph?searchtype=author&query=Laubner%2C+D">D. Laubner</a>, <a href="/search/astro-ph?searchtype=author&query=McDaniel%2C+A">A. McDaniel</a>, <a href="/search/astro-ph?searchtype=author&query=Romer%2C+A+K">A. K. Romer</a>, <a href="/search/astro-ph?searchtype=author&query=Swart%2C+A">A. Swart</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=Brooks%2C+D">D. Brooks</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=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=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. (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="2305.02365v1-abstract-short" style="display: inline;"> We search for the presence of cool cores in optically-selected galaxy clusters from the Dark Energy Survey (DES) and investigate their prevalence as a function of redshift and cluster richness. Clusters were selected from the redMaPPer analysis of three years of DES observations that have archival Chandra X-ray observations, giving a sample of 99 clusters with a redshift range of… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.02365v1-abstract-full').style.display = 'inline'; document.getElementById('2305.02365v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.02365v1-abstract-full" style="display: none;"> We search for the presence of cool cores in optically-selected galaxy clusters from the Dark Energy Survey (DES) and investigate their prevalence as a function of redshift and cluster richness. Clusters were selected from the redMaPPer analysis of three years of DES observations that have archival Chandra X-ray observations, giving a sample of 99 clusters with a redshift range of $0.11 < z < 0.87$ and a richness range of $25 < 位< 207$. Using the X-ray data, the core temperature was compared to the outer temperature to identify clusters where the core temperature is a factor of 0.7 or less than the outer temperature. We found a cool core fraction of approximately 20% with no significant trend in the cool core fraction with either redshift or richness. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.02365v1-abstract-full').style.display = 'none'; document.getElementById('2305.02365v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 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">shortened version accepted to RNAAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2305.01695">arXiv:2305.01695</a> <span> [<a href="https://arxiv.org/pdf/2305.01695">pdf</a>, <a href="https://arxiv.org/format/2305.01695">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 Dark Energy Survey Six-Year Calibration Star Catalog </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E+S">E. S. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Tucker%2C+D+L">D. L. Tucker</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</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=Bechtol%2C+K">K. Bechtol</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=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Gruendl%2C+R+A">R. A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Lasker%2C+J">J. Lasker</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+J+A">J. A. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Wester%2C+W+C">W. C. Wester</a>, <a href="/search/astro-ph?searchtype=author&query=Yanny%2C+B">B. Yanny</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">J. Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</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=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Castander%2C+F+J">F. J. Castander</a>, <a href="/search/astro-ph?searchtype=author&query=Choi%2C+A">A. Choi</a>, <a href="/search/astro-ph?searchtype=author&query=da+Costa%2C+L+N">L. N. da Costa</a> , et al. (42 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2305.01695v1-abstract-short" style="display: inline;"> This Technical Note presents a catalog of calibrated reference stars that was generated by the Forward Calibration Method (FGCM) pipeline (arXiv:1706.01542) as part of the FGCM photometric calibration of the full Dark Energy Survey (DES) 6-Year data set (Y6). This catalog provides DES grizY magnitudes for 17 million stars with i-band magnitudes mostly in the range 16 < i < 21 spread over the full… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.01695v1-abstract-full').style.display = 'inline'; document.getElementById('2305.01695v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2305.01695v1-abstract-full" style="display: none;"> This Technical Note presents a catalog of calibrated reference stars that was generated by the Forward Calibration Method (FGCM) pipeline (arXiv:1706.01542) as part of the FGCM photometric calibration of the full Dark Energy Survey (DES) 6-Year data set (Y6). This catalog provides DES grizY magnitudes for 17 million stars with i-band magnitudes mostly in the range 16 < i < 21 spread over the full DES footprint covering 5000 square degrees over the Southern Galactic Cap at galactic latitudes b < -20 degrees (plus a few outlying fields disconnected from the main survey footprint). These stars are calibrated to a uniformity of better than 1.8 milli-mag (0.18%) RMS over the survey area. The absolute calibration of the catalog is computed with reference to the STISNIC.007 spectrum of the Hubble Space Telescope CalSpec standard star C26202; including systematic errors, the absolute flux system is known at the approximately 1% level. As such, these stars provide a useful reference catalog for calibrating grizY-band or grizY-like band photometry in the Southern Hemisphere, particularly for observations within the DES footprint. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2305.01695v1-abstract-full').style.display = 'none'; document.getElementById('2305.01695v1-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 15 figures, Fermilab Technical Note. Official Data Access Site: https://des.ncsa.illinois.edu/releases/other ; Temporary Data Access Site: https://data.darkenergysurvey.org/public_calib/DES_6yr_CalibStarCat/index.html</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-TM-2784-PPD-SCD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.13570">arXiv:2304.13570</a> <span> [<a href="https://arxiv.org/pdf/2304.13570">pdf</a>, <a href="https://arxiv.org/format/2304.13570">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/10.1093/mnras/stad1220">10.1093/mnras/stad1220 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The XMM Cluster Survey: Exploring scaling relations and completeness of the Dark Energy Survey Year 3 redMaPPer cluster catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Upsdell%2C+E+W">E. W. Upsdell</a>, <a href="/search/astro-ph?searchtype=author&query=Giles%2C+P+A">P. A. Giles</a>, <a href="/search/astro-ph?searchtype=author&query=Romer%2C+A+K">A. K. Romer</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkinson%2C+R">R. Wilkinson</a>, <a href="/search/astro-ph?searchtype=author&query=Turner%2C+D+J">D. J. Turner</a>, <a href="/search/astro-ph?searchtype=author&query=Hilton%2C+M">M. Hilton</a>, <a href="/search/astro-ph?searchtype=author&query=Rykoff%2C+E">E. Rykoff</a>, <a href="/search/astro-ph?searchtype=author&query=Farahi%2C+A">A. Farahi</a>, <a href="/search/astro-ph?searchtype=author&query=Bhargava%2C+S">S. Bhargava</a>, <a href="/search/astro-ph?searchtype=author&query=Jeltema%2C+T">T. Jeltema</a>, <a href="/search/astro-ph?searchtype=author&query=Klein%2C+M">M. Klein</a>, <a href="/search/astro-ph?searchtype=author&query=Bermeo%2C+A">A. Bermeo</a>, <a href="/search/astro-ph?searchtype=author&query=Collins%2C+C+A">C. A. Collins</a>, <a href="/search/astro-ph?searchtype=author&query=Ebrahimpour%2C+L">L. Ebrahimpour</a>, <a href="/search/astro-ph?searchtype=author&query=Hollowood%2C+D">D. Hollowood</a>, <a href="/search/astro-ph?searchtype=author&query=Mann%2C+R+G">R. G. Mann</a>, <a href="/search/astro-ph?searchtype=author&query=Manolopoulou%2C+M">M. Manolopoulou</a>, <a href="/search/astro-ph?searchtype=author&query=Miller%2C+C+J">C. J. Miller</a>, <a href="/search/astro-ph?searchtype=author&query=Rooney%2C+P+J">P. J. Rooney</a>, <a href="/search/astro-ph?searchtype=author&query=Sahl%C3%A9n%2C+M">Martin Sahl茅n</a>, <a href="/search/astro-ph?searchtype=author&query=Stott%2C+J+P">J. P. Stott</a>, <a href="/search/astro-ph?searchtype=author&query=Viana%2C+P+T+P">P. T. P. Viana</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=Bacon%2C+D">D. Bacon</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="2304.13570v1-abstract-short" style="display: inline;"> We cross-match and compare characteristics of galaxy clusters identified in observations from two sky surveys using two completely different techniques. One sample is optically selected from the analysis of three years of Dark Energy Survey observations using the redMaPPer cluster detection algorithm. The second is X-ray selected from XMM observations analysed by the XMM Cluster Survey. The sample… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.13570v1-abstract-full').style.display = 'inline'; document.getElementById('2304.13570v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.13570v1-abstract-full" style="display: none;"> We cross-match and compare characteristics of galaxy clusters identified in observations from two sky surveys using two completely different techniques. One sample is optically selected from the analysis of three years of Dark Energy Survey observations using the redMaPPer cluster detection algorithm. The second is X-ray selected from XMM observations analysed by the XMM Cluster Survey. The samples comprise a total area of 57.4 deg$^2$, bounded by the area of 4 contiguous XMM survey regions that overlap the DES footprint. We find that the X-ray selected sample is fully matched with entries in the redMaPPer catalogue, above $位>$20 and within 0.1$< z <$0.9. Conversely, only 38\% of the redMaPPer catalogue is matched to an X-ray extended source. Next, using 120 optically clusters and 184 X-ray selected clusters, we investigate the form of the X-ray luminosity-temperature ($L_{X}-T_{X}$), luminosity-richness ($L_{X}-位$) and temperature-richness ($T_{X}-位$) scaling relations. We find that the fitted forms of the $L_{X}-T_{X}$ relations are consistent between the two selection methods and also with other studies in the literature. However, we find tentative evidence for a steepening of the slope of the relation for low richness systems in the X-ray selected sample. When considering the scaling of richness with X-ray properties, we again find consistency in the relations (i.e., $L_{X}-位$ and $T_{X}-位$) between the optical and X-ray selected samples. This is contrary to previous similar works that find a significant increase in the scatter of the luminosity scaling relation for X-ray selected samples compared to optically selected samples. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.13570v1-abstract-full').style.display = 'none'; document.getElementById('2304.13570v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication 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/2304.01858">arXiv:2304.01858</a> <span> [<a href="https://arxiv.org/pdf/2304.01858">pdf</a>, <a href="https://arxiv.org/format/2304.01858">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/10.3847/1538-3881/acca15">10.3847/1538-3881/acca15 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The Dark Energy Survey Supernova Program: Corrections on photometry due to wavelength-dependent atmospheric effects </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lee%2C+J">J. Lee</a>, <a href="/search/astro-ph?searchtype=author&query=Acevedo%2C+M">M. Acevedo</a>, <a href="/search/astro-ph?searchtype=author&query=Sako%2C+M">M. Sako</a>, <a href="/search/astro-ph?searchtype=author&query=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Sanchez%2C+B">B. Sanchez</a>, <a href="/search/astro-ph?searchtype=author&query=Chen%2C+R">R. Chen</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M">M. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Qu%2C+H">H. Qu</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Kessler%2C+R">R. Kessler</a>, <a href="/search/astro-ph?searchtype=author&query=Lasker%2C+J">J. Lasker</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</a>, <a href="/search/astro-ph?searchtype=author&query=Rosell%2C+A+C">A. Carnero Rosell</a> , et al. (42 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.01858v1-abstract-short" style="display: inline;"> Wavelength-dependent atmospheric effects impact photometric supernova flux measurements for ground-based observations. We present corrections on supernova flux measurements from the Dark Energy Survey Supernova Program's 5YR sample (DES-SN5YR) for differential chromatic refraction (DCR) and wavelength-dependent seeing, and we show their impact on the cosmological parameters $w$ and $惟_m$. We use… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.01858v1-abstract-full').style.display = 'inline'; document.getElementById('2304.01858v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.01858v1-abstract-full" style="display: none;"> Wavelength-dependent atmospheric effects impact photometric supernova flux measurements for ground-based observations. We present corrections on supernova flux measurements from the Dark Energy Survey Supernova Program's 5YR sample (DES-SN5YR) for differential chromatic refraction (DCR) and wavelength-dependent seeing, and we show their impact on the cosmological parameters $w$ and $惟_m$. We use $g-i$ colors of Type Ia supernovae (SNe Ia) to quantify astrometric offsets caused by DCR and simulate point spread functions (PSFs) using the GalSIM package to predict the shapes of the PSFs with DCR and wavelength-dependent seeing. We calculate the magnitude corrections and apply them to the magnitudes computed by the DES-SN5YR photometric pipeline. We find that for the DES-SN5YR analysis, not accounting for the astrometric offsets and changes in the PSF shape cause an average bias of $+0.2$ mmag and $-0.3$ mmag respectively, with standard deviations of $0.7$ mmag and $2.7$ mmag across all DES observing bands (\textit{griz}) throughout all redshifts. When the DCR and seeing effects are not accounted for, we find that $w$ and $惟_m$ are lower by less than $0.004\pm0.02$ and $0.001\pm0.01$ respectively, with $0.02$ and $0.01$ being the $1蟽$ statistical uncertainties. Although we find that these biases do not limit the constraints of the DES-SN5YR sample, future surveys with much higher statistics, lower systematics, and especially those that observe in the $u$ band will require these corrections as wavelength-dependent atmospheric effects are larger at shorter wavelengths. We also discuss limitations of our method and how they can be better accounted for in future surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.01858v1-abstract-full').style.display = 'none'; document.getElementById('2304.01858v1-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 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 13 figures, accepted by the Astronomical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> DES-2022-0740, FERMILAB-PUB-23-040-PPD </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.15156">arXiv:2303.15156</a> <span> [<a href="https://arxiv.org/pdf/2303.15156">pdf</a>, <a href="https://arxiv.org/format/2303.15156">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1093/mnras/stad955">10.1093/mnras/stad955 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Ultracool dwarfs candidates based on six years of the Dark Energy Survey data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ponte%2C+M+d">M. dal Ponte</a>, <a href="/search/astro-ph?searchtype=author&query=Santiago%2C+B">B. Santiago</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=De+Paris%2C+L">L. De Paris</a>, <a href="/search/astro-ph?searchtype=author&query=Pace%2C+A+B">A. B. Pace</a>, <a href="/search/astro-ph?searchtype=author&query=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</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=Carretero%2C+J">J. Carretero</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C">C. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Costanzi%2C+M">M. Costanzi</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</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=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+S">S. Everett</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrero%2C+I">I. Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Flaugher%2C+B">B. Flaugher</a> , et al. (35 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="2303.15156v1-abstract-short" style="display: inline;"> We present a sample of 19,583 ultracool dwarf candidates brighter than z $\leq 23$ selected from the Dark Energy Survey DR2 coadd data matched to VHS DR6, VIKING DR5 and AllWISE covering $\sim$ 4,800 $deg^2$. The ultracool candidates were first pre-selected based on their (i-z), (z-Y), and (Y-J) colours. They were further classified using a method that compares their optical, near-infrared and mid… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15156v1-abstract-full').style.display = 'inline'; document.getElementById('2303.15156v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15156v1-abstract-full" style="display: none;"> We present a sample of 19,583 ultracool dwarf candidates brighter than z $\leq 23$ selected from the Dark Energy Survey DR2 coadd data matched to VHS DR6, VIKING DR5 and AllWISE covering $\sim$ 4,800 $deg^2$. The ultracool candidates were first pre-selected based on their (i-z), (z-Y), and (Y-J) colours. They were further classified using a method that compares their optical, near-infrared and mid-infrared colours against templates of M, L and T dwarfs. 14,099 objects are presented as new L and T candidates and the remaining objects are from the literature, including 5,342 candidates from our previous work. Using this new and deeper sample of ultracool dwarf candidates we also present: 20 new candidate members to nearby young moving groups (YMG) and associations, variable candidate sources and four new wide binary systems composed of two ultracool dwarfs. Finally, we also show the spectra of twelve new ultracool dwarfs discovered by our group and presented here for the first time. These spectroscopically confirmed objects are a sanity check of our selection of ultracool dwarfs and photometric classification method. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15156v1-abstract-full').style.display = 'none'; document.getElementById('2303.15156v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 10 figures, 7 tables. Accepted for publication in 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/2303.13445">arXiv:2303.13445</a> <span> [<a href="https://arxiv.org/pdf/2303.13445">pdf</a>, <a href="https://arxiv.org/format/2303.13445">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Synchronous rotation in the (136199) Eris-Dysnomia system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bernstein%2C+G+M">G. M. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Holler%2C+B+J">B. J. Holler</a>, <a href="/search/astro-ph?searchtype=author&query=Navarro-Escamilla%2C+R">R. Navarro-Escamilla</a>, <a href="/search/astro-ph?searchtype=author&query=Bernardinelli%2C+P+H">P. H. Bernardinelli</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Annis%2C+J">J. Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</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=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>, <a href="/search/astro-ph?searchtype=author&query=Doel%2C+P">P. Doel</a>, <a href="/search/astro-ph?searchtype=author&query=Drlica-Wagner%2C+A">A. Drlica-Wagner</a>, <a href="/search/astro-ph?searchtype=author&query=Everett%2C+S">S. Everett</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrero%2C+I">I. Ferrero</a>, <a href="/search/astro-ph?searchtype=author&query=Frieman%2C+J">J. Frieman</a>, <a href="/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Bellido%2C+J">J. Garc铆a-Bellido</a> , et al. (25 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="2303.13445v1-abstract-short" style="display: inline;"> We combine photometry of Eris from a 6-month campaign on the Palomar 60-inch telescope in 2015, a 1-month Hubble Space Telescope WFC3 campaign in 2018, and Dark Energy Survey data spanning 2013--2018 to determine a light curve of definitive period $15.771\pm 0.008$~days (1-$蟽$ formal uncertainties), with nearly sinusoidal shape and peak-to-peak flux variation of 3\%. This is consistent at part-per… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13445v1-abstract-full').style.display = 'inline'; document.getElementById('2303.13445v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.13445v1-abstract-full" style="display: none;"> We combine photometry of Eris from a 6-month campaign on the Palomar 60-inch telescope in 2015, a 1-month Hubble Space Telescope WFC3 campaign in 2018, and Dark Energy Survey data spanning 2013--2018 to determine a light curve of definitive period $15.771\pm 0.008$~days (1-$蟽$ formal uncertainties), with nearly sinusoidal shape and peak-to-peak flux variation of 3\%. This is consistent at part-per-thousand precision with the $P=15.78590\pm0.00005$~day period of Dysnomia's orbit around Eris, strengthening the recent detection of synchronous rotation of Eris by Szakats et al (2022) with independent data. Photometry from Gaia is consistent with the same light curve. We detect a slope of $0.05\pm0.01$~mag per degree of Eris' brightness with respect to illumination phase, intermediate between Pluto's and Charon's values. Variations of $0.3$~mag are detected in Dysnomia's brightness, plausibly consistent with a double-peaked light curve at the synchronous period. The synchronous rotation of Eris is consistent with simple tidal models initiated with a giant-impact origin of the binary, but is difficult to reconcile with gravitational capture of Dysnomia by Eris. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13445v1-abstract-full').style.display = 'none'; document.getElementById('2303.13445v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 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">Submitted to Planetary Science 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/2302.05184">arXiv:2302.05184</a> <span> [<a href="https://arxiv.org/pdf/2302.05184">pdf</a>, <a href="https://arxiv.org/format/2302.05184">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"> Rates and properties of type Ia supernovae in galaxy clusters within the Dark Energy Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Toy%2C+M">M. Toy</a>, <a href="/search/astro-ph?searchtype=author&query=Wiseman%2C+P">P. Wiseman</a>, <a href="/search/astro-ph?searchtype=author&query=Sullivan%2C+M">M. Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Frohmaier%2C+C">C. Frohmaier</a>, <a href="/search/astro-ph?searchtype=author&query=Graur%2C+O">O. Graur</a>, <a href="/search/astro-ph?searchtype=author&query=Palmese%2C+A">A. Palmese</a>, <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</a>, <a href="/search/astro-ph?searchtype=author&query=Davis%2C+T+M">T. M. Davis</a>, <a href="/search/astro-ph?searchtype=author&query=Galbany%2C+L">L. Galbany</a>, <a href="/search/astro-ph?searchtype=author&query=Kelsey%2C+L">L. Kelsey</a>, <a href="/search/astro-ph?searchtype=author&query=Lidman%2C+C">C. Lidman</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Allam%2C+S">S. Allam</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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=Annis%2C+J">J. Annis</a>, <a href="/search/astro-ph?searchtype=author&query=Bacon%2C+D">D. Bacon</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Burke%2C+D+L">D. L. Burke</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=Carretero%2C+J">J. Carretero</a> , et al. (37 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2302.05184v2-abstract-short" style="display: inline;"> We identify 66 photometrically classified type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) that have occurred within red-sequence selected galaxy clusters. We compare light-curve and host galaxy properties of the cluster SNe to 1024 DES SNe Ia located in field galaxies, the largest comparison of two such samples at high redshift (z > 0.1). We find that cluster SN light curves decline… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05184v2-abstract-full').style.display = 'inline'; document.getElementById('2302.05184v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2302.05184v2-abstract-full" style="display: none;"> We identify 66 photometrically classified type Ia supernovae (SNe Ia) from the Dark Energy Survey (DES) that have occurred within red-sequence selected galaxy clusters. We compare light-curve and host galaxy properties of the cluster SNe to 1024 DES SNe Ia located in field galaxies, the largest comparison of two such samples at high redshift (z > 0.1). We find that cluster SN light curves decline faster than those in the field (97.7 per cent confidence). However, when limiting these samples to host galaxies of similar colour and mass, there is no significant difference in the SN light curve properties. Motivated by previous detections of a higher-normalised SN Ia delay time distribution in galaxy clusters, we measure the intrinsic rate of SNe Ia in cluster and field environments. We find the average ratio of the SN Ia rate per galaxy between high mass ($10\leq\log\mathrm{(M_{*}/M_{\odot})} \leq 11.25$) cluster and field galaxies to be $0.594 \pm0.068$. This difference is mass-dependent, with the ratio declining with increasing mass, which suggests that the stellar populations in cluster hosts are older than those in field hosts. We show that the mass-normalised rate (or SNe per unit mass) in massive-passive galaxies is consistent between cluster and field environments. Additionally, both of these rates are consistent with rates previously measured in clusters at similar redshifts. We conclude that in massive-passive galaxies, which are the dominant hosts of cluster SNe, the cluster DTD is comparable to the field. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2302.05184v2-abstract-full').style.display = 'none'; document.getElementById('2302.05184v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 February, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2023. </p> </li> </ol> <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=Allam%2C+S&start=50" class="pagination-next" >Next </a> <ul 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