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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=Desai%2C+S&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Desai%2C+S&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Desai%2C+S&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Desai%2C+S&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Desai%2C+S&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Desai%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/2502.15235">arXiv:2502.15235</a> <span> [<a href="https://arxiv.org/pdf/2502.15235">pdf</a>, <a href="https://arxiv.org/format/2502.15235">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> A Stacked Analysis of GeV Gamma-Ray Emission from SPT-SZ Galaxy Clusters with 16 Years of Fermi-LAT Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Manna%2C+S">Siddhant Manna</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.15235v1-abstract-short" style="display: inline;"> We report a statistically significant detection of cumulative $纬$-ray emission from a stacked sample of SPT-SZ selected galaxy clusters using 16.4 years of data from the Fermi Gamma-Ray Space Telescope's Large Area Telescope (LAT). By analyzing a population of clusters with individual Test Statistic (TS) values $<$ 9.0, we identify a robust cumulative signal with a TS of 75.2, corresponding to app… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.15235v1-abstract-full').style.display = 'inline'; document.getElementById('2502.15235v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.15235v1-abstract-full" style="display: none;"> We report a statistically significant detection of cumulative $纬$-ray emission from a stacked sample of SPT-SZ selected galaxy clusters using 16.4 years of data from the Fermi Gamma-Ray Space Telescope's Large Area Telescope (LAT). By analyzing a population of clusters with individual Test Statistic (TS) values $<$ 9.0, we identify a robust cumulative signal with a TS of 75.2, corresponding to approximately 8.4$蟽$ significance. In contrast, clusters with TS $<$ 4.0 yield a weaker cumulative signal of TS = 9.65, consistent with background fluctuations. The derived $纬$-ray spectrum is well characterized by a power law model with a best-fit spectral index of $-2.59 \pm 0.20$ and an integrated flux of $1.67^{+1.35}_{-1.07} \times 10^{-11}$ ph cm$^{-2}$ s$^{-1}$. The spectral index matches hadronic cosmic-ray interaction predictions but may also include contributions from AGNs within the galaxy clusters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.15235v1-abstract-full').style.display = 'none'; document.getElementById('2502.15235v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">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">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/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/2502.11998">arXiv:2502.11998</a> <span> [<a href="https://arxiv.org/pdf/2502.11998">pdf</a>, <a href="https://arxiv.org/format/2502.11998">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> Determination of Hubble constant from Megamaser Cosmology Project using Profile Likelihood </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barua%2C+S">Shubham Barua</a>, <a href="/search/astro-ph?searchtype=author&query=Ramakrishnan%2C+V">Vyaas Ramakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.11998v1-abstract-short" style="display: inline;"> The Megamaser Cosmology Project inferred a value for the Hubble constant given by $H_0=73.9 \pm 3.0 $ km/sec/Mpc. This value was obtained using Bayesian inference by marginalizing over six nuisance parameters, corresponding to the velocities of the megamaser galaxy systems. We obtain an independent estimate of the Hubble constant with the same data using frequentist inference. For this purpose, we… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.11998v1-abstract-full').style.display = 'inline'; document.getElementById('2502.11998v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.11998v1-abstract-full" style="display: none;"> The Megamaser Cosmology Project inferred a value for the Hubble constant given by $H_0=73.9 \pm 3.0 $ km/sec/Mpc. This value was obtained using Bayesian inference by marginalizing over six nuisance parameters, corresponding to the velocities of the megamaser galaxy systems. We obtain an independent estimate of the Hubble constant with the same data using frequentist inference. For this purpose, we use profile likelihood to dispense with the aforementioned nuisance parameters. The frequentist estimate of the Hubble constant is given by $H_0=73.5^{+3.0}_{-2.9}$ km/sec/Mpc and agrees with the Bayesian estimate to within $0.2蟽$, and both approaches also produce consistent confidence/credible intervals. Therefore, this analysis provides a proof of principle application of profile likelihood in dealing with nuisance parameters in Cosmology, which is complementary to Bayesian analysis. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.11998v1-abstract-full').style.display = 'none'; document.getElementById('2502.11998v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">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">7 pages, 2 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/2502.00805">arXiv:2502.00805</a> <span> [<a href="https://arxiv.org/pdf/2502.00805">pdf</a>, <a href="https://arxiv.org/format/2502.00805">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Constraints on Lorentz Invariance Violation from Gamma-ray Burst rest-frame spectral lags using Profile Likelihood </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ramakrishnan%2C+V">Vyaas Ramakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.00805v1-abstract-short" style="display: inline;"> We reanalyze the spectral lag data for 56 GRBs in the cosmological rest frame to search for Lorentz Invariance Violation using frequentist inference. For this purpose, we use the technique of profile likelihood to deal with the nuisance parameters corresponding to a constant astrophysical spectral lag in the GRB rest frame and the unknown intrinsic scatter, while the parameter of interest is the e… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.00805v1-abstract-full').style.display = 'inline'; document.getElementById('2502.00805v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.00805v1-abstract-full" style="display: none;"> We reanalyze the spectral lag data for 56 GRBs in the cosmological rest frame to search for Lorentz Invariance Violation using frequentist inference. For this purpose, we use the technique of profile likelihood to deal with the nuisance parameters corresponding to a constant astrophysical spectral lag in the GRB rest frame and the unknown intrinsic scatter, while the parameter of interest is the energy scale ($E_{QG}$) for LIV. With this method, we do not obtain a global minimum for $蠂^2$ as a function of $E_{QG}$ up to the Planck scale. Therefore, we can set one-sided lower limits on $E_{QG}$ in a seamless manner. The 95% c.l. lower limits which we obtain on $E_{QG}$ are then given by $E_{QG}\geq 1.22 \times 10^{15}$ GeV and $E_{QG}\geq 6.64\times 10^{5}$ GeV, for linear and quadratic LIV, respectively. Therefore, this work represents yet another proof of principles application of profile likelihood in the search for LIV using GRB spectral lags. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.00805v1-abstract-full').style.display = 'none'; document.getElementById('2502.00805v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">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">4 pages, 2 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/2501.19117">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/2501.10506">arXiv:2501.10506</a> <span> [<a href="https://arxiv.org/pdf/2501.10506">pdf</a>, <a href="https://arxiv.org/format/2501.10506">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"> High-Significance Detection of Correlation Between the Unresolved Gamma-Ray Background and the Large Scale Cosmic Structure </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Thakore%2C+B">B. Thakore</a>, <a href="/search/astro-ph?searchtype=author&query=Negro%2C+M">M. Negro</a>, <a href="/search/astro-ph?searchtype=author&query=Regis%2C+M">M. Regis</a>, <a href="/search/astro-ph?searchtype=author&query=Camera%2C+S">S. Camera</a>, <a href="/search/astro-ph?searchtype=author&query=Gruen%2C+D">D. Gruen</a>, <a href="/search/astro-ph?searchtype=author&query=Fornengo%2C+N">N. Fornengo</a>, <a href="/search/astro-ph?searchtype=author&query=Roodman%2C+A">A. Roodman</a>, <a href="/search/astro-ph?searchtype=author&query=Porredon%2C+A">A. Porredon</a>, <a href="/search/astro-ph?searchtype=author&query=Schutt%2C+T">T. Schutt</a>, <a href="/search/astro-ph?searchtype=author&query=Cuoco%2C+A">A. Cuoco</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=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>, <a href="/search/astro-ph?searchtype=author&query=Cordero%2C+J">J. Cordero</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> , et al. (74 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="2501.10506v1-abstract-short" style="display: inline;"> Our understanding of the $纬$-ray sky has improved dramatically in the past decade, however, the unresolved $纬$-ray background (UGRB) still has a potential wealth of information about the faintest $纬$-ray sources pervading the Universe. Statistical cross-correlations with tracers of cosmic structure can indirectly identify the populations that most characterize the $纬$-ray background. In this study… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10506v1-abstract-full').style.display = 'inline'; document.getElementById('2501.10506v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.10506v1-abstract-full" style="display: none;"> Our understanding of the $纬$-ray sky has improved dramatically in the past decade, however, the unresolved $纬$-ray background (UGRB) still has a potential wealth of information about the faintest $纬$-ray sources pervading the Universe. Statistical cross-correlations with tracers of cosmic structure can indirectly identify the populations that most characterize the $纬$-ray background. In this study, we analyze the angular correlation between the $纬$-ray background and the matter distribution in the Universe as traced by gravitational lensing, leveraging more than a decade of observations from the Fermi-Large Area Telescope (LAT) and 3 years of data from the Dark Energy Survey (DES). We detect a correlation at signal-to-noise ratio of 8.9. Most of the statistical significance comes from large scales, demonstrating, for the first time, that a substantial portion of the UGRB aligns with the mass clustering of the Universe as traced by weak lensing. Blazars provide a plausible explanation for this signal, especially if those contributing to the correlation reside in halos of large mass ($\sim 10^{14} M_{\odot}$) and account for approximately 30-40 % of the UGRB above 10 GeV. Additionally, we observe a preference for a curved $纬$-ray energy spectrum, with a log-parabolic shape being favored over a power-law. We also discuss the possibility of modifications to the blazar model and the inclusion of additional $gamma$-ray sources, such as star-forming galaxies or particle dark matter. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.10506v1-abstract-full').style.display = 'none'; document.getElementById('2501.10506v1-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 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">34 pages, 15 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.05781">arXiv:2501.05781</a> <span> [<a href="https://arxiv.org/pdf/2501.05781">pdf</a>, <a href="https://arxiv.org/format/2501.05781">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Dark Energy Survey Year 6 Results: Point-Spread Function Modeling </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Schutt%2C+T">T. Schutt</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M">M. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Roodman%2C+A">A. Roodman</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</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=Gruendl%2C+R+A">R. A. Gruendl</a>, <a href="/search/astro-ph?searchtype=author&query=Yamamoto%2C+M">M. Yamamoto</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=Gatti%2C+M">M. Gatti</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>, <a href="/search/astro-ph?searchtype=author&query=Troxel%2C+M+A">M. A. Troxel</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=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=Chang%2C+C">C. Chang</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>, <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> , et al. (34 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="2501.05781v1-abstract-short" style="display: inline;"> We present the point-spread function (PSF) modeling for weak lensing shear measurement using the full six years of the Dark Energy Survey (DES Y6) data. We review the PSF estimation procedure using the PIFF (PSFs In the Full FOV) software package and describe the key improvements made to PIFF and modeling diagnostics since the DES year three (Y3) analysis: (i) use of external Gaia and infrared pho… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05781v1-abstract-full').style.display = 'inline'; document.getElementById('2501.05781v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.05781v1-abstract-full" style="display: none;"> We present the point-spread function (PSF) modeling for weak lensing shear measurement using the full six years of the Dark Energy Survey (DES Y6) data. We review the PSF estimation procedure using the PIFF (PSFs In the Full FOV) software package and describe the key improvements made to PIFF and modeling diagnostics since the DES year three (Y3) analysis: (i) use of external Gaia and infrared photometry catalogs to ensure higher purity of the stellar sample used for model fitting, (ii) addition of color-dependent PSF modeling, the first for any weak lensing analysis, and (iii) inclusion of model diagnostics inspecting fourth-order moments, which can bias weak lensing measurements to a similar degree as second-order modeling errors. Through a comprehensive set of diagnostic tests, we demonstrate the improved accuracy of the Y6 models evident in significantly smaller systematic errors than those of the Y3 analysis, in which all $g$ band data were excluded due to insufficiently accurate PSF models. For the Y6 weak lensing analysis, we include $g$ band photometry data in addition to the $riz$ bands, providing a fourth band for photometric redshift estimation. Looking forward to the next generation of wide-field surveys, we describe several ongoing improvements to PIFF, which will be the default PSF modeling software for weak lensing analyses for the Vera C. Rubin Observatory's Legacy Survey of Space and Time. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05781v1-abstract-full').style.display = 'none'; document.getElementById('2501.05781v1-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 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">33 pages, 24 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/2501.05665">arXiv:2501.05665</a> <span> [<a href="https://arxiv.org/pdf/2501.05665">pdf</a>, <a href="https://arxiv.org/format/2501.05665">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Dark Energy Survey Year 6 Results: Cell-based Coadds and Metadetection Weak Lensing Shape Catalogue </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Yamamoto%2C+M">M. Yamamoto</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=Sheldon%2C+E">E. Sheldon</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M">M. Jarvis</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=Menanteau%2C+F">F. Menanteau</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=Mau%2C+S">S. Mau</a>, <a href="/search/astro-ph?searchtype=author&query=Schutt%2C+T">T. Schutt</a>, <a href="/search/astro-ph?searchtype=author&query=Gatti%2C+M">M. Gatti</a>, <a href="/search/astro-ph?searchtype=author&query=Troxel%2C+M+A">M. A. Troxel</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</a>, <a href="/search/astro-ph?searchtype=author&query=Anbajagane%2C+D">D. Anbajagane</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=Gruen%2C+D">D. Gruen</a>, <a href="/search/astro-ph?searchtype=author&query=Huff%2C+E+M">E. M. Huff</a>, <a href="/search/astro-ph?searchtype=author&query=Tabbutt%2C+M">M. Tabbutt</a>, <a href="/search/astro-ph?searchtype=author&query=Tong%2C+A">A. Tong</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=Alarcon%2C+A">A. Alarcon</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=Bechtol%2C+K">K. Bechtol</a>, <a href="/search/astro-ph?searchtype=author&query=Blazek%2C+J">J. Blazek</a> , et al. (59 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.05665v1-abstract-short" style="display: inline;"> We present the Metadetection weak lensing galaxy shape catalogue from the six-year Dark Energy Survey (DES Y6) imaging data. This dataset is the final release from DES, spanning 4422 deg$^2$ of the southern sky. We describe how the catalogue was constructed, including the two new major processing steps, cell-based image coaddition and shear measurements with Metadetection. The DES Y6 Metadetection… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05665v1-abstract-full').style.display = 'inline'; document.getElementById('2501.05665v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.05665v1-abstract-full" style="display: none;"> We present the Metadetection weak lensing galaxy shape catalogue from the six-year Dark Energy Survey (DES Y6) imaging data. This dataset is the final release from DES, spanning 4422 deg$^2$ of the southern sky. We describe how the catalogue was constructed, including the two new major processing steps, cell-based image coaddition and shear measurements with Metadetection. The DES Y6 Metadetection weak lensing shape catalogue consists of 151,922,791 galaxies detected over riz bands, with an effective number density of $n_{\rm eff}$ =8.22 galaxies per arcmin$^2$ and shape noise of $蟽_e$ = 0.29. We carry out a suite of validation tests on the catalogue, including testing for PSF leakage, testing for the impact of PSF modeling errors, and testing the correlation of the shear measurements with galaxy, PSF, and survey properties. In addition to demonstrating that our catalogue is robust for weak lensing science, we use the DES Y6 image simulation suite (Mau, Becker et al. 2025) to estimate the overall multiplicative shear bias of our shear measurement pipeline. We find no detectable multiplicative bias at the roughly half-percent level, with m = (3.4 $\pm$ 6.1) x $10^{-3}$, at 3$蟽$ uncertainty. This is the first time both cell-based coaddition and Metadetection algorithms are applied to observational data, paving the way to the Stage-IV weak lensing surveys. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05665v1-abstract-full').style.display = 'none'; document.getElementById('2501.05665v1-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> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">30 pages, 22 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/2501.04333">arXiv:2501.04333</a> <span> [<a href="https://arxiv.org/pdf/2501.04333">pdf</a>, <a href="https://arxiv.org/ps/2501.04333">ps</a>, <a href="https://arxiv.org/format/2501.04333">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s12036-024-10031-x">10.1007/s12036-024-10031-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Gravitational physics in the context of Indian astronomy: A vision document </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ajith%2C+P">P. Ajith</a>, <a href="/search/astro-ph?searchtype=author&query=Arun%2C+K+G">K. G. Arun</a>, <a href="/search/astro-ph?searchtype=author&query=Bose%2C+S">Sukanta Bose</a>, <a href="/search/astro-ph?searchtype=author&query=Chakraborty%2C+S">Sumanta Chakraborty</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Gopakumar%2C+A">A. Gopakumar</a>, <a href="/search/astro-ph?searchtype=author&query=Kolekar%2C+S">Sanved Kolekar</a>, <a href="/search/astro-ph?searchtype=author&query=Nayak%2C+R">Rajesh Nayak</a>, <a href="/search/astro-ph?searchtype=author&query=Pai%2C+A">Archana Pai</a>, <a href="/search/astro-ph?searchtype=author&query=Sarkar%2C+S">Sudipta Sarkar</a>, <a href="/search/astro-ph?searchtype=author&query=Bagla%2C+J+S">Jasjeet Singh Bagla</a>, <a href="/search/astro-ph?searchtype=author&query=Gupta%2C+P+D">Patrick Das Gupta</a>, <a href="/search/astro-ph?searchtype=author&query=Kashyap%2C+R">Rahul Kashyap</a>, <a href="/search/astro-ph?searchtype=author&query=Kocherlakota%2C+P">Prashant Kocherlakota</a>, <a href="/search/astro-ph?searchtype=author&query=Kumar%2C+P">Prayush Kumar</a>, <a href="/search/astro-ph?searchtype=author&query=Mukhopadhyay%2C+B">Banibrata Mukhopadhyay</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="2501.04333v1-abstract-short" style="display: inline;"> Contributions from the Indian gravity community have played a significant role in shaping several branches of astronomy and astrophysics. This document reviews some of the most important contributions and presents a vision for gravity research in the context of astronomy \& astrophysics in India. This is an expanded version of one of the chapters in the recently released Vision Document of the Ast… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04333v1-abstract-full').style.display = 'inline'; document.getElementById('2501.04333v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.04333v1-abstract-full" style="display: none;"> Contributions from the Indian gravity community have played a significant role in shaping several branches of astronomy and astrophysics. This document reviews some of the most important contributions and presents a vision for gravity research in the context of astronomy \& astrophysics in India. This is an expanded version of one of the chapters in the recently released Vision Document of the Astronomical Society of India. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.04333v1-abstract-full').style.display = 'none'; document.getElementById('2501.04333v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 8 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">Published in JoAA special issue "Indian Astronomy in the Global Context: A compendium of white papers submitted towards the Astronomical Society of India Vision Document (2024"</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Journal of Astrophysics and Astronomy, 46, 1 (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/2412.19240">arXiv:2412.19240</a> <span> [<a href="https://arxiv.org/pdf/2412.19240">pdf</a>, <a href="https://arxiv.org/format/2412.19240">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"> Effect of Peak Absolute Magnitude of Type Ia Supernovae and Sound Horizon Values on Hubble Tension using DESI results </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Barua%2C+S">Shubham Barua</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.19240v1-abstract-short" style="display: inline;"> We apply data-motivated priors on the peak absolute magnitude of Type Ia supernovae ($M$), and on the sound horizon at the drag epoch ($r_d$), to study their impact on the Hubble tension, when compared to the Planck estimated value of the Hubble constant. We use the data from Pantheon$+$, cosmic chronometers, and the latest DESI BAO results for this purpose. We reaffirm the fact that there is a de… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.19240v1-abstract-full').style.display = 'inline'; document.getElementById('2412.19240v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.19240v1-abstract-full" style="display: none;"> We apply data-motivated priors on the peak absolute magnitude of Type Ia supernovae ($M$), and on the sound horizon at the drag epoch ($r_d$), to study their impact on the Hubble tension, when compared to the Planck estimated value of the Hubble constant. We use the data from Pantheon$+$, cosmic chronometers, and the latest DESI BAO results for this purpose. We reaffirm the fact that there is a degeneracy between $M$ and $r_d$, and modifying the $r_d$ values to reconcile the Hubble tension also requires a change in the peak absolute magnitude $M$. For certain $M$ and $r_d$ priors, the tension is found to reduce to as low as (1.2-2) $蟽$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.19240v1-abstract-full').style.display = 'none'; document.getElementById('2412.19240v1-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 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">8 pages, 1 figure</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.03900">arXiv:2412.03900</a> <span> [<a href="https://arxiv.org/pdf/2412.03900">pdf</a>, <a href="https://arxiv.org/format/2412.03900">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"> Search for transient gamma-ray emission from magnetar flares using Fermi-LAT </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ramakrishnan%2C+V">Vyaas Ramakrishnan</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.03900v1-abstract-short" style="display: inline;"> We search for transient gamma-ray emission in the energy range from 0.1-300 GeV using data from the Fermi-LAT telescope in coincidence with magnetar flares. For our analysis we look for coincidence with 15 distinct flares from 11 magnetars using two distinct time windows of $\pm$ 1 day and $\pm$ 15 days. For 14 of these flares from 10 magnetars, we do not see any statistically significant gamma-ra… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.03900v1-abstract-full').style.display = 'inline'; document.getElementById('2412.03900v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.03900v1-abstract-full" style="display: none;"> We search for transient gamma-ray emission in the energy range from 0.1-300 GeV using data from the Fermi-LAT telescope in coincidence with magnetar flares. For our analysis we look for coincidence with 15 distinct flares from 11 magnetars using two distinct time windows of $\pm$ 1 day and $\pm$ 15 days. For 14 of these flares from 10 magnetars, we do not see any statistically significant gamma-ray emission. However, we see two gamma-ray flares from one magnetar, namely 1E 1048.1-5937, with combined significance of $5蟽$, observed after about 10 days from the peak of the X-ray flare. However, this magnetar is located close to the galactic plane (with galactic latitude of -0.52\degree) and this signal could be caused by contamination due to diffuse flux from gamma-ray sources in the galactic plane. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.03900v1-abstract-full').style.display = 'none'; document.getElementById('2412.03900v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 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">24 pages, 17 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.09248">arXiv:2411.09248</a> <span> [<a href="https://arxiv.org/pdf/2411.09248">pdf</a>, <a href="https://arxiv.org/format/2411.09248">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Constraint on Lorentz Invariance Violation for spectral lag transition in GRB 160625B using profile likelihood </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Ganguly%2C+S">Shalini Ganguly</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.09248v2-abstract-short" style="display: inline;"> We reanalyze the spectral lag data for GRB 160625B using frequentist inference in order to constrain the energy scale ($E_{QG}$) of Lorentz Invariance Violation (LIV). For this purpose, we use profile likelihood to deal with the astrophysical nuisance parameters. This is in contrast to Bayesian inference implemented in previous works, where marginalization was carried out over the nuisance paramet… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09248v2-abstract-full').style.display = 'inline'; document.getElementById('2411.09248v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.09248v2-abstract-full" style="display: none;"> We reanalyze the spectral lag data for GRB 160625B using frequentist inference in order to constrain the energy scale ($E_{QG}$) of Lorentz Invariance Violation (LIV). For this purpose, we use profile likelihood to deal with the astrophysical nuisance parameters. This is in contrast to Bayesian inference implemented in previous works, where marginalization was carried out over the nuisance parameters. We show that with profile likelihood, we do not find a global minimum for $蠂^2$ as a function of $E_{QG}$ below the Planck scale for both linear and quadratic models of LIV, whereas bounded credible intervals were previously obtained using Bayesian inference. Therefore, we can set one-sided lower limits in a straightforward manner. We find that $E_{QG} \geq 2.55 \times 10^{16}$ GeV and $E_{QG} \geq 1.85 \times 10^7$ GeV at 95\% c.l., for linear and quadratic LIV, respectively. Therefore, this is the first proof-of-principles application of profile likelihood method to the analysis of GRB spectral lag data to constrain LIV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.09248v2-abstract-full').style.display = 'none'; document.getElementById('2411.09248v2-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, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">4 pages, 2 figures. Accepted for publication in EPJC</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/2410.16394">arXiv:2410.16394</a> <span> [<a href="https://arxiv.org/pdf/2410.16394">pdf</a>, <a href="https://arxiv.org/format/2410.16394">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"> Search for spatial coincidence between IceCube neutrinos and gamma-ray bright red dwarfs </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=M%2C+F+S">Fathima Shifa M</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.16394v1-abstract-short" style="display: inline;"> We search for a spatial coincidence between high energy neutrinos detected by the IceCube neutrino detector and ten red dwarfs which have been observed in gamma-rays. For our analysis, we use the unbinned maximum likelihood method to look for a statistically significant excess. We do not find any such spatial association between any of the red dwarfs and Icecube-detected neutrinos. Therefore, we c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16394v1-abstract-full').style.display = 'inline'; document.getElementById('2410.16394v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.16394v1-abstract-full" style="display: none;"> We search for a spatial coincidence between high energy neutrinos detected by the IceCube neutrino detector and ten red dwarfs which have been observed in gamma-rays. For our analysis, we use the unbinned maximum likelihood method to look for a statistically significant excess. We do not find any such spatial association between any of the red dwarfs and Icecube-detected neutrinos. Therefore, we conclude that none of the gamma-ray bright red dwarfs contribute to the diffuse neutrino flux measured by IceCube. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.16394v1-abstract-full').style.display = 'none'; document.getElementById('2410.16394v1-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">8 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.07956">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/2410.03342">arXiv:2410.03342</a> <span> [<a href="https://arxiv.org/pdf/2410.03342">pdf</a>, <a href="https://arxiv.org/format/2410.03342">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Digital Libraries">cs.DL</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Physics and Society">physics.soc-ph</span> </div> </div> <p class="title is-5 mathjax"> Impact factors of astrophysics journals revisited </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Rithvik%2C+R+V+S">Rayani Venkat Sai Rithvik</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.03342v1-abstract-short" style="display: inline;"> We calculate the 2024 impact factors of 36 most widely used journals in Astrophysics, using the citations collated by NASA/ADS (Astrophysics Data System) and compare them to the official impact factors. This includes journals which publish papers outside of astrophysics such as PRD, EPJC, Nature etc. We also propose a new metric to gauge the impact factor based on the median number of citations in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03342v1-abstract-full').style.display = 'inline'; document.getElementById('2410.03342v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.03342v1-abstract-full" style="display: none;"> We calculate the 2024 impact factors of 36 most widely used journals in Astrophysics, using the citations collated by NASA/ADS (Astrophysics Data System) and compare them to the official impact factors. This includes journals which publish papers outside of astrophysics such as PRD, EPJC, Nature etc. We also propose a new metric to gauge the impact factor based on the median number of citations in a journal and calculate the same for all the journals. We find that the ADS-based impact factors are mostly in agreement, albeit higher than the official impact factors for most journals. The journals with the maximum fractional difference in median-based and old impact factors are JHEAP and PTEP. We find the maximum difference between the ADS and official impact factor for Nature. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.03342v1-abstract-full').style.display = 'none'; document.getElementById('2410.03342v1-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 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">5 pages. 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/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/2408.13634">arXiv:2408.13634</a> <span> [<a href="https://arxiv.org/pdf/2408.13634">pdf</a>, <a href="https://arxiv.org/format/2408.13634">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1007/s10509-024-04357-9">10.1007/s10509-024-04357-9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Enhanced Astronomical Source Classification with Integration of Attention Mechanisms and Vision Transformers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Bhavanam%2C+S+R">Srinadh Reddy Bhavanam</a>, <a href="/search/astro-ph?searchtype=author&query=Channappayya%2C+S+S">Sumohana S. Channappayya</a>, <a href="/search/astro-ph?searchtype=author&query=Srijith%2C+P+K">P. K. Srijith</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.13634v1-abstract-short" style="display: inline;"> Accurate classification of celestial objects is essential for advancing our understanding of the universe. MargNet is a recently developed deep learning-based classifier applied to SDSS DR16 dataset to segregate stars, quasars, and compact galaxies using photometric data. MargNet utilizes a stacked architecture, combining a Convolutional Neural Network (CNN) for image modelling and an Artificial N… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.13634v1-abstract-full').style.display = 'inline'; document.getElementById('2408.13634v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.13634v1-abstract-full" style="display: none;"> Accurate classification of celestial objects is essential for advancing our understanding of the universe. MargNet is a recently developed deep learning-based classifier applied to SDSS DR16 dataset to segregate stars, quasars, and compact galaxies using photometric data. MargNet utilizes a stacked architecture, combining a Convolutional Neural Network (CNN) for image modelling and an Artificial Neural Network (ANN) for modelling photometric parameters. In this study, we propose enhancing MargNet's performance by incorporating attention mechanisms and Vision Transformer (ViT)-based models for processing image data. The attention mechanism allows the model to focus on relevant features and capture intricate patterns within images, effectively distinguishing between different classes of celestial objects. Additionally, we leverage ViTs, a transformer-based deep learning architecture renowned for exceptional performance in image classification tasks. We enhance the model's understanding of complex astronomical images by utilizing ViT's ability to capture global dependencies and contextual information. Our approach uses a curated dataset comprising 240,000 compact and 150,000 faint objects. The models learn classification directly from the data, minimizing human intervention. Furthermore, we explore ViT as a hybrid architecture that uses photometric features and images together as input to predict astronomical objects. Our results demonstrate that the proposed attention mechanism augmented CNN in MargNet marginally outperforms the traditional MargNet and the proposed ViT-based MargNet models. Additionally, the ViT-based hybrid model emerges as the most lightweight and easy-to-train model with classification accuracy similar to that of the best-performing attention-enhanced MargNet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.13634v1-abstract-full').style.display = 'none'; document.getElementById('2408.13634v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 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">33 pages, 11 figures. Accepted for publication in APSS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.10983">arXiv:2408.10983</a> <span> [<a href="https://arxiv.org/pdf/2408.10983">pdf</a>, <a href="https://arxiv.org/format/2408.10983">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.jheap.2024.10.001">10.1016/j.jheap.2024.10.001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for GeV gamma-ray emission from SPT-CL J2012-5649 with six years of DAMPE data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Manna%2C+S">Siddhant Manna</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.10983v2-abstract-short" style="display: inline;"> We search for gamma-ray emission from the galaxy cluster SPT-CL J2012-5649 in the energy range from 3 GeV to 1 TeV using the DArk Matter Particle Explorer (DAMPE) telescope. For our analysis, we use three different templates: point source, radial disk, and radial Gaussian. We do not detect a signal with significance $>3蟽$ for any of these templates at any location within $R_{200}$ of the cluster c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10983v2-abstract-full').style.display = 'inline'; document.getElementById('2408.10983v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.10983v2-abstract-full" style="display: none;"> We search for gamma-ray emission from the galaxy cluster SPT-CL J2012-5649 in the energy range from 3 GeV to 1 TeV using the DArk Matter Particle Explorer (DAMPE) telescope. For our analysis, we use three different templates: point source, radial disk, and radial Gaussian. We do not detect a signal with significance $>3蟽$ for any of these templates at any location within $R_{200}$ of the cluster center. We obtain 95\% C.L. upper limit on the energy flux ranging between $\sim 10^{-6}$ and $10^{-4} \rm{MeV~cm^{-2}~s^{-1}}$ depending on the energy range. These upper limits are consistent with a previously reported non-zero flux detected by Fermi-LAT at $6蟽$ significance. This work represents the first proof of principle search for gamma-ray emission from a single galaxy cluster using DAMPE data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10983v2-abstract-full').style.display = 'none'; document.getElementById('2408.10983v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 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">12 pages, 4 figures. Accepted for publication in JHEAP</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/2407.19081">arXiv:2407.19081</a> <span> [<a href="https://arxiv.org/pdf/2407.19081">pdf</a>, <a href="https://arxiv.org/format/2407.19081">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.33232/001c.124536">10.33232/001c.124536 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Weak Gravitational Lensing around Low Surface Brightness Galaxies in the DES Year 3 Data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Chicoine%2C+N">N. Chicoine</a>, <a href="/search/astro-ph?searchtype=author&query=Prat%2C+J">J. Prat</a>, <a href="/search/astro-ph?searchtype=author&query=Zacharegkas%2C+G">G. Zacharegkas</a>, <a href="/search/astro-ph?searchtype=author&query=Chang%2C+C">C. Chang</a>, <a href="/search/astro-ph?searchtype=author&query=Tanoglidis%2C+D">D. Tanoglidis</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=Anbajagane%2C+D">D. Anbajagane</a>, <a href="/search/astro-ph?searchtype=author&query=Adhikari%2C+S">S. Adhikari</a>, <a href="/search/astro-ph?searchtype=author&query=Amon%2C+A">A. Amon</a>, <a href="/search/astro-ph?searchtype=author&query=Wechsler%2C+R+H">R. H. Wechsler</a>, <a href="/search/astro-ph?searchtype=author&query=Alarcon%2C+A">A. Alarcon</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=Cawthon%2C+R">R. Cawthon</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=Cordero%2C+J">J. Cordero</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=Dodelson%2C+S">S. Dodelson</a>, <a href="/search/astro-ph?searchtype=author&query=Doux%2C+C">C. Doux</a> , et al. (80 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.19081v2-abstract-short" style="display: inline;"> We present galaxy-galaxy lensing measurements using a sample of low surface brightness galaxies (LSBGs) drawn from the Dark Energy Survey Year 3 (Y3) data as lenses. LSBGs are diffuse galaxies with a surface brightness dimmer than the ambient night sky. These dark-matter-dominated objects are intriguing due to potentially unusual formation channels that lead to their diffuse stellar component. Giv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.19081v2-abstract-full').style.display = 'inline'; document.getElementById('2407.19081v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.19081v2-abstract-full" style="display: none;"> We present galaxy-galaxy lensing measurements using a sample of low surface brightness galaxies (LSBGs) drawn from the Dark Energy Survey Year 3 (Y3) data as lenses. LSBGs are diffuse galaxies with a surface brightness dimmer than the ambient night sky. These dark-matter-dominated objects are intriguing due to potentially unusual formation channels that lead to their diffuse stellar component. Given the faintness of LSBGs, using standard observational techniques to characterize their total masses proves challenging. Weak gravitational lensing, which is less sensitive to the stellar component of galaxies, could be a promising avenue to estimate the masses of LSBGs. Our LSBG sample consists of 23,790 galaxies separated into red and blue color types at $g-i\ge 0.60$ and $g-i< 0.60$, respectively. Combined with the DES Y3 shear catalog, we measure the tangential shear around these LSBGs and find signal-to-noise ratios of 6.67 for the red sample, 2.17 for the blue sample, and 5.30 for the full sample. We use the clustering redshifts method to obtain redshift distributions for the red and blue LSBG samples. Assuming all red LSBGs are satellites, we fit a simple model to the measurements and estimate the host halo mass of these LSBGs to be $\log(M_{\rm host}/M_{\odot}) = 12.98 ^{+0.10}_{-0.11}$. We place a 95% upper bound on the subhalo mass at $\log(M_{\rm sub}/M_{\odot})<11.51$. By contrast, we assume the blue LSBGs are centrals, and place a 95% upper bound on the halo mass at $\log(M_\mathrm{host}/M_\odot) < 11.84$. We find that the stellar-to-halo mass ratio of the LSBG samples is consistent with that of the general galaxy population. This work illustrates the viability of using weak gravitational lensing to constrain the halo masses of LSBGs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.19081v2-abstract-full').style.display = 'none'; document.getElementById('2407.19081v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 14 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> FERMILAB-PUB-23-380-PPD </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/2407.10189">arXiv:2407.10189</a> <span> [<a href="https://arxiv.org/pdf/2407.10189">pdf</a>, <a href="https://arxiv.org/format/2407.10189">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Phenomenology">hep-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/10/023">10.1088/1475-7516/2024/10/023 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Dark Matter Annihilation to gamma-rays from SPT-SZ selected Galaxy Clusters </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Manna%2C+S">Siddhant Manna</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</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="2407.10189v2-abstract-short" style="display: inline;"> We search for dark matter annihilation from galaxy clusters in the energy range from 1-300 GeV using nearly 16 years of Fermi-LAT data. For this purpose, we use 350 galaxy clusters selected from the 2500 $\rm{deg^2}$ SPT-SZ survey. We model the dark matter distribution using the NFW profile for the main halo along with the Einasto profile for the substructure. The largest signal is seen for the cl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10189v2-abstract-full').style.display = 'inline'; document.getElementById('2407.10189v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.10189v2-abstract-full" style="display: none;"> We search for dark matter annihilation from galaxy clusters in the energy range from 1-300 GeV using nearly 16 years of Fermi-LAT data. For this purpose, we use 350 galaxy clusters selected from the 2500 $\rm{deg^2}$ SPT-SZ survey. We model the dark matter distribution using the NFW profile for the main halo along with the Einasto profile for the substructure. The largest signal is seen for the cluster SPT-CL J2021-5257 with a significance of around $3蟽$. The best-fit dark matter mass and annihilation cross-section for this cluster are equal to $(60.0 \pm 11.8)$ GeV and $\langle 蟽v \rangle= (6.0 \pm 0.6) \times 10^{-25} \rm{cm^3 s^{-1}}$ for the $\bar{b} b$ annihilation channel. However, this central estimate is in conflict with the limits on annihilation cross-section from dwarf spheroidal galaxies, and hence cannot be attributed to dark matter annihilation. Three other clusters show significance between $2-2.5蟽$, whereas all the remaining clusters show null results. The most stringent 95\% c.l. upper limit for the WIMP annihilation cross-section among all the clusters is from SPT-CL J0455-4159, viz. $\langle 蟽v \rangle = 6.44 \times 10^{-26} \text{cm}^3 \text{s}^{-1}$ for $m_蠂 = 10$ GeV and $b\bar{b}$ annihilation channel. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.10189v2-abstract-full').style.display = 'none'; document.getElementById('2407.10189v2-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 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 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">27 pages, 10 figures. Accepted for publication in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 10 (2024) 023 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.01060">arXiv:2407.01060</a> <span> [<a href="https://arxiv.org/pdf/2407.01060">pdf</a>, <a href="https://arxiv.org/format/2407.01060">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/1475-7516/2024/09/029">10.1088/1475-7516/2024/09/029 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for MeV Gamma-ray emission from TeV bright red dwarfs with COMPTEL </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Shrivastava%2C+N">Niharika Shrivastava</a>, <a href="/search/astro-ph?searchtype=author&query=Manna%2C+S">Siddhant Manna</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</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="2407.01060v2-abstract-short" style="display: inline;"> The SHALON atmospheric Cherenkov telescope has detected very high energy gamma-ray emission at TeV energies from eight red dwarfs, namely, V388 Cas, V547 Cas, V780 Tau, V962 Tau, V1589 Cyg, GJ 1078, GJ 3684 and GL 851.1. Consequently, these red dwarfs have been suggested as sources of ultra-high energy cosmic rays. In this work, we search for soft gamma-ray emission from these TeV bright red dwarf… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01060v2-abstract-full').style.display = 'inline'; document.getElementById('2407.01060v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.01060v2-abstract-full" style="display: none;"> The SHALON atmospheric Cherenkov telescope has detected very high energy gamma-ray emission at TeV energies from eight red dwarfs, namely, V388 Cas, V547 Cas, V780 Tau, V962 Tau, V1589 Cyg, GJ 1078, GJ 3684 and GL 851.1. Consequently, these red dwarfs have been suggested as sources of ultra-high energy cosmic rays. In this work, we search for soft gamma-ray emission from these TeV bright red dwarfs between 0.75-30 MeV using archival data from the COMPTEL gamma-ray imaging telescope, as a follow-up to a similar search for GeV gamma-ray emission using the Fermi-LAT telescope. Although, prima-facie, we detect non-zero photon flux from three red dwarfs with high significance, these signals can attributed to contamination from nearby sources such as Crab and Cygnus, which are within the angular resolution of COMPTEL, and have been previously detected as very bright point sources at MeV energies. Therefore, we could not detect any statistically significant signal ($>3蟽$) from any of these eight red dwarfs from 0.75-30 MeV. We then report the 95% confidence level upper limits on the differential photon flux (at 30 MeV), integral photon flux and integral energy flux for all of the eight red dwarfs. The integral energy flux limits range between $10^{-11}-10^{-10} \rm{ergs/cm^2/s}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01060v2-abstract-full').style.display = 'none'; document.getElementById('2407.01060v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">10 pages, 12 figures. Accepted for publication in JCAP</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> JCAP 09 (2024) 029 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.10931">arXiv:2406.10931</a> <span> [<a href="https://arxiv.org/pdf/2406.10931">pdf</a>, <a href="https://arxiv.org/format/2406.10931">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/10.1140/epjc/s10052-024-13031-x">10.1140/epjc/s10052-024-13031-x <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A test for the redshift dependence of $蟽_8$ using $f蟽_8$ measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Manna%2C+S">Siddhant Manna</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</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="2406.10931v1-abstract-short" style="display: inline;"> We search for a redshift dependence of $蟽_8^0$ using 23 growth rate measurements from redshift space distortions and peculiar velocity measurements as a consistency check of $螞$CDM. For this purpose we use the dataset from arXiv:1806.10822 consisting of 22 measurements, which has been vetted for internal consistencies. Eighteen of these measurements have been obtained from the Gold-2017 sample, co… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.10931v1-abstract-full').style.display = 'inline'; document.getElementById('2406.10931v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.10931v1-abstract-full" style="display: none;"> We search for a redshift dependence of $蟽_8^0$ using 23 growth rate measurements from redshift space distortions and peculiar velocity measurements as a consistency check of $螞$CDM. For this purpose we use the dataset from arXiv:1806.10822 consisting of 22 measurements, which has been vetted for internal consistencies. Eighteen of these measurements have been obtained from the Gold-2017 sample, collated from multiple redshift space distortion surveys between 2009 and 2016, whereas the remaining four have been obtained from the eBOSS DR14 quasar survey. We also added one additional data point from the BOSS DR12 CMASS galaxy sample. We find that for this dataset the $蟽_8^0$ values are consistent between the low redshift and high redshift samples using three different redshift cuts. This implies that the growth rate measurements are consistent with a constant $蟽_8^0$ in accord with $螞$CDM, assuming there are no uncontrolled systematics in this dataset. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.10931v1-abstract-full').style.display = 'none'; document.getElementById('2406.10931v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 16 June, 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">6 pages, 3 figures. Accepted for publication in EPJC</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.08934">arXiv:2406.08934</a> <span> [<a href="https://arxiv.org/pdf/2406.08934">pdf</a>, <a href="https://arxiv.org/format/2406.08934">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348667">10.1051/0004-6361/202348667 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Tully-Fisher Relation of Late-type Galaxies at $0.6 \leq z \leq 2.5$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Sharma%2C+G">Gauri Sharma</a>, <a href="/search/astro-ph?searchtype=author&query=Upadhyaya%2C+V">Varenya Upadhyaya</a>, <a href="/search/astro-ph?searchtype=author&query=Salucci%2C+P">Paolo Salucci</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</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="2406.08934v1-abstract-short" style="display: inline;"> We present a study of the stellar and baryonic Tully-Fisher relation within the redshift range of $0.6 \leq z \leq 2.5$ utilizing observations of \sfgs. This dataset, as explored in \citet{GS23}, comprises of disk-like galaxies spanning a stellar mass range of $8.89 \leq \log(M_{star} \ [\mathrm{M_\odot}]) \leq 11.5$, baryonic mass range of $9.0 \leq \log(M_{bar} [\mathrm{M_\odot}]) \leq 11.5$, an… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.08934v1-abstract-full').style.display = 'inline'; document.getElementById('2406.08934v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.08934v1-abstract-full" style="display: none;"> We present a study of the stellar and baryonic Tully-Fisher relation within the redshift range of $0.6 \leq z \leq 2.5$ utilizing observations of \sfgs. This dataset, as explored in \citet{GS23}, comprises of disk-like galaxies spanning a stellar mass range of $8.89 \leq \log(M_{star} \ [\mathrm{M_\odot}]) \leq 11.5$, baryonic mass range of $9.0 \leq \log(M_{bar} [\mathrm{M_\odot}]) \leq 11.5$, and circular velocity range of $1.65 \leq \log(V_c \ [{\rm km/s}]) \leq 2.85$. Stellar masses of these objects are estimated using spectral energy distribution fitting techniques, while gas masses are determined via scaling relations. Circular velocities are directly derived from the Rotation Curves (RCs), after meticulously correcting for beam smearing and pressure support. Our analysis confirms that our sample adheres to the fundamental mass-size relations of galaxies and reflects the evolution of velocity dispersion in galaxies, in line with previous findings. This reaffirms the reliability of our photometric and kinematic parameters (i.e., $M_{star}$ and $V_c$), thereby enabling a comprehensive examination of the Tully-Fisher relation. To attain robust results, we employed a novel orthogonal likelihood fitting technique designed to minimize intrinsic scatter around the best-fit line, as required at \hz. For the STFR, we obtained a slope of $伪=3.03\pm 0.25$, an offset of $尾= 3.34\pm 0.53$, and an intrinsic scatter of $味_{int}=0.08$ dex. Correspondingly, the BTFR yielded $伪=3.21\pm 0.28$, $尾=3.16\pm 0.61$, and $味_{int}=0.09$ dex. Our findings suggest a subtle deviation in the stellar and baryonic Tully-Fisher relation with respect to local studies, which is most-likely due to the evolutionary processes governing disk formation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.08934v1-abstract-full').style.display = 'none'; document.getElementById('2406.08934v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A. The uniqueness of this work lies in the robustness of circular velocity measurements of high-z galaxies (see Sharma et al. 2023) and the fitting techniques. In particular, we employed an orthogonal likelihood fitting technique, tested and verified on mock observations (see Appendix). Fitting code is publicly available on the GitHub repository (link in paper)</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 689, A318 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.05051">arXiv:2406.05051</a> <span> [<a href="https://arxiv.org/pdf/2406.05051">pdf</a>, <a href="https://arxiv.org/format/2406.05051">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"> Modelling the impact of host galaxy dust on type Ia supernova distance measurements </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Popovic%2C+B">B. Popovic</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=Smith%2C+M">M. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Gait%C3%A1n%2C+S">S. Gonz谩lez-Gait谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Scolnic%2C+D">D. Scolnic</a>, <a href="/search/astro-ph?searchtype=author&query=Duarte%2C+J">J. Duarte</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=Brout%2C+D">D. Brout</a>, <a href="/search/astro-ph?searchtype=author&query=Carollo%2C+D">D. Carollo</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=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=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=Lewis%2C+G+F">G. F. Lewis</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=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=Toy%2C+M">M. Toy</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=Vincenzi%2C+M">M. Vincenzi</a>, <a href="/search/astro-ph?searchtype=author&query=Abbott%2C+T+M+C">T. M. C. Abbott</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="2406.05051v1-abstract-short" style="display: inline;"> Type Ia Supernovae (SNe Ia) are a critical tool in measuring the accelerating expansion of the universe. Recent efforts to improve these standard candles have focused on incorporating the effects of dust on distance measurements with SNe Ia. In this paper, we use the state-of-the-art Dark Energy Survey 5 year sample to evaluate two different families of dust models: empirical extinction models der… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05051v1-abstract-full').style.display = 'inline'; document.getElementById('2406.05051v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.05051v1-abstract-full" style="display: none;"> Type Ia Supernovae (SNe Ia) are a critical tool in measuring the accelerating expansion of the universe. Recent efforts to improve these standard candles have focused on incorporating the effects of dust on distance measurements with SNe Ia. In this paper, we use the state-of-the-art Dark Energy Survey 5 year sample to evaluate two different families of dust models: empirical extinction models derived from SNe Ia data, and physical attenuation models from the spectra of galaxies. Among the SNe Ia-derived models, we find that a logistic function of the total-to-selective extinction RV best recreates the correlations between supernova distance measurements and host galaxy properties, though an additional 0.02 magnitudes of grey scatter are needed to fully explain the scatter in SNIa brightness in all cases. These empirically-derived extinction distributions are highly incompatible with the physical attenuation models from galactic spectral measurements. From these results, we conclude that SNe Ia must either preferentially select extreme ends of galactic dust distributions, or that the characterisation of dust along the SNe Ia line-of-sight is incompatible with that of galactic dust distributions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.05051v1-abstract-full').style.display = 'none'; document.getElementById('2406.05051v1-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/2406.05050">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/2406.05046">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/2405.15213">arXiv:2405.15213</a> <span> [<a href="https://arxiv.org/pdf/2405.15213">pdf</a>, <a href="https://arxiv.org/format/2405.15213">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 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/10.33232/001c.121908">10.33232/001c.121908 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A study of gamma-ray emission from OJ 287 using Fermi-LAT from 2015-2023 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pasumarti%2C+V">Vibhavasu Pasumarti</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.15213v2-abstract-short" style="display: inline;"> We search for gamma-ray emission from OJ287 in the energy range from 0.1-300 GeV during 2015-2023, in coincidence with an extensive observing campaign to monitor the optical flux variability and polarization, as discussed in arXiv:2311.02372. We present results for eight segments in the aforementioned period, with each segment corresponding to an observing season. We report non-zero gamma-ray flux… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.15213v2-abstract-full').style.display = 'inline'; document.getElementById('2405.15213v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.15213v2-abstract-full" style="display: none;"> We search for gamma-ray emission from OJ287 in the energy range from 0.1-300 GeV during 2015-2023, in coincidence with an extensive observing campaign to monitor the optical flux variability and polarization, as discussed in arXiv:2311.02372. We present results for eight segments in the aforementioned period, with each segment corresponding to an observing season. We report non-zero gamma-ray flux (with $>10蟽$ significance) for all the eight segments. The photon and energy flux observed during this period is $\sim 5.2 \times 10^{-8} \rm{ph~cm^{-2}~s^{-1}}$ and $2.75 \times 10^{-5} \rm{MeV~cm^{-2}~s^{-1}}$, respectively, while the SED can be fitted with a power law with a slope of $2.12 \pm 0.02$. The observed luminosity is between $10^{45}-10^{46}$ ergs/sec. Similar to previous works we find a hard cutoff in the gamma-ray spectrum at around 20 GeV. We do not observe any correlations between the peaks in the gamma ray light curves and corresponding optical light cuves in $I$ and $R$ bands, as well as the X-ray light curves from SWIFT between 0.3-10 keV. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.15213v2-abstract-full').style.display = 'none'; document.getElementById('2405.15213v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 24 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">19 pages, 32 figures. Accepted in OJA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.14351">arXiv:2405.14351</a> <span> [<a href="https://arxiv.org/pdf/2405.14351">pdf</a>, <a href="https://arxiv.org/format/2405.14351">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1017/pasa.2024.96">10.1017/pasa.2024.96 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The ORT and the uGMRT Pulsar Monitoring Program : Pulsar Timing Irregularities & the Gaussian Process Realization </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Grover%2C+H">Himanshu Grover</a>, <a href="/search/astro-ph?searchtype=author&query=Joshi%2C+B+C">Bhal Chandra Joshi</a>, <a href="/search/astro-ph?searchtype=author&query=Singha%2C+J">Jaikhomba Singha</a>, <a href="/search/astro-ph?searchtype=author&query=G%C3%BCgercino%C4%9Flu%2C+E">Erbil G眉gercino臒lu</a>, <a href="/search/astro-ph?searchtype=author&query=Arumugam%2C+P">Paramasivan Arumugam</a>, <a href="/search/astro-ph?searchtype=author&query=Bandyopadhyay%2C+D">Debades Bandyopadhyay</a>, <a href="/search/astro-ph?searchtype=author&query=Chibueze%2C+J+O">James O. Chibueze</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Eya%2C+I+O">Innocent O. Eya</a>, <a href="/search/astro-ph?searchtype=author&query=Kundu%2C+A">Anu Kundu</a>, <a href="/search/astro-ph?searchtype=author&query=Urama%2C+J+O">Johnson O. Urama</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.14351v2-abstract-short" style="display: inline;"> The spin-down law of pulsars is generally perturbed by two types of timing irregularities: glitches and timing noise. Glitches are sudden changes in the rotational frequency of pulsars, while timing noise is a discernible stochastic wandering in the phase, period, or spin-down rate of a pulsar. We present the timing results of a sample of glitching pulsars observed using the Ooty Radio Telescope (… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14351v2-abstract-full').style.display = 'inline'; document.getElementById('2405.14351v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.14351v2-abstract-full" style="display: none;"> The spin-down law of pulsars is generally perturbed by two types of timing irregularities: glitches and timing noise. Glitches are sudden changes in the rotational frequency of pulsars, while timing noise is a discernible stochastic wandering in the phase, period, or spin-down rate of a pulsar. We present the timing results of a sample of glitching pulsars observed using the Ooty Radio Telescope (ORT) and the upgraded Giant Metrewave Radio Telescope (uGMRT). Our findings include timing noise analysis for 17 pulsars, with seven being reported for the first time. We detected five glitches in four pulsars and a glitch-like event in PSR J1825-0935. The frequency evolution of glitch in pulsars, J0742-2822 and J1740-3015, is presented for the first time. Additionally, we report timing noise results for three glitching pulsars. The timing noise was analyzed separately in the pre-glitch region and post-glitch regions. We observed an increase in the red noise parameters in the post-glitch regions, where exponential recovery was considered in the noise analysis. Timing noise can introduce ambiguities in the correct evaluation of glitch observations. Hence, it is important to consider timing noise in glitch analysis. We propose an innovative glitch verification approach designed to discern between a glitch and strong timing noise. The novel glitch analysis technique is also demonstrated using the observed data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14351v2-abstract-full').style.display = 'none'; document.getElementById('2405.14351v2-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, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 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">27 pages, 12 figures. Accepted for publication in PASA</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.13491">arXiv:2405.13491</a> <span> [<a href="https://arxiv.org/pdf/2405.13491">pdf</a>, <a href="https://arxiv.org/format/2405.13491">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Euclid. I. Overview of the Euclid mission </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Euclid+Collaboration"> Euclid Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Mellier%2C+Y">Y. Mellier</a>, <a href="/search/astro-ph?searchtype=author&query=Abdurro%27uf"> Abdurro'uf</a>, <a href="/search/astro-ph?searchtype=author&query=Barroso%2C+J+A+A">J. A. Acevedo Barroso</a>, <a href="/search/astro-ph?searchtype=author&query=Ach%C3%BAcarro%2C+A">A. Ach煤carro</a>, <a href="/search/astro-ph?searchtype=author&query=Adamek%2C+J">J. Adamek</a>, <a href="/search/astro-ph?searchtype=author&query=Adam%2C+R">R. Adam</a>, <a href="/search/astro-ph?searchtype=author&query=Addison%2C+G+E">G. E. Addison</a>, <a href="/search/astro-ph?searchtype=author&query=Aghanim%2C+N">N. Aghanim</a>, <a href="/search/astro-ph?searchtype=author&query=Aguena%2C+M">M. Aguena</a>, <a href="/search/astro-ph?searchtype=author&query=Ajani%2C+V">V. Ajani</a>, <a href="/search/astro-ph?searchtype=author&query=Akrami%2C+Y">Y. Akrami</a>, <a href="/search/astro-ph?searchtype=author&query=Al-Bahlawan%2C+A">A. Al-Bahlawan</a>, <a href="/search/astro-ph?searchtype=author&query=Alavi%2C+A">A. Alavi</a>, <a href="/search/astro-ph?searchtype=author&query=Albuquerque%2C+I+S">I. S. Albuquerque</a>, <a href="/search/astro-ph?searchtype=author&query=Alestas%2C+G">G. Alestas</a>, <a href="/search/astro-ph?searchtype=author&query=Alguero%2C+G">G. Alguero</a>, <a href="/search/astro-ph?searchtype=author&query=Allaoui%2C+A">A. Allaoui</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=Allevato%2C+V">V. Allevato</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso-Tetilla%2C+A+V">A. V. Alonso-Tetilla</a>, <a href="/search/astro-ph?searchtype=author&query=Altieri%2C+B">B. Altieri</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez-Candal%2C+A">A. Alvarez-Candal</a>, <a href="/search/astro-ph?searchtype=author&query=Alvi%2C+S">S. Alvi</a>, <a href="/search/astro-ph?searchtype=author&query=Amara%2C+A">A. Amara</a> , et al. (1115 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="2405.13491v2-abstract-short" style="display: inline;"> The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. Euclid is a medium-class mission in the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13491v2-abstract-full').style.display = 'inline'; document.getElementById('2405.13491v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.13491v2-abstract-full" style="display: none;"> The current standard model of cosmology successfully describes a variety of measurements, but the nature of its main ingredients, dark matter and dark energy, remains unknown. Euclid is a medium-class mission in the Cosmic Vision 2015-2025 programme of the European Space Agency (ESA) that will provide high-resolution optical imaging, as well as near-infrared imaging and spectroscopy, over about 14,000 deg^2 of extragalactic sky. In addition to accurate weak lensing and clustering measurements that probe structure formation over half of the age of the Universe, its primary probes for cosmology, these exquisite data will enable a wide range of science. This paper provides a high-level overview of the mission, summarising the survey characteristics, the various data-processing steps, and data products. We also highlight the main science objectives and expected performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.13491v2-abstract-full').style.display = 'none'; document.getElementById('2405.13491v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 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">Accepted for publication in the A&A special issue`Euclid on Sky'</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.02263">arXiv:2405.02263</a> <span> [<a href="https://arxiv.org/pdf/2405.02263">pdf</a>, <a href="https://arxiv.org/format/2405.02263">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> </div> <p class="title is-5 mathjax"> An Optical Gamma-Ray Burst Catalogue with Measured Redshift PART I: Data Release of 535 Gamma-Ray Bursts and Colour Evolution </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Dainotti%2C+M+G">M. G. Dainotti</a>, <a href="/search/astro-ph?searchtype=author&query=De+Simone%2C+B">B. De Simone</a>, <a href="/search/astro-ph?searchtype=author&query=Malik%2C+R+F+M">R. F. Mohideen Malik</a>, <a href="/search/astro-ph?searchtype=author&query=Pasumarti%2C+V">V. Pasumarti</a>, <a href="/search/astro-ph?searchtype=author&query=Levine%2C+D">D. Levine</a>, <a href="/search/astro-ph?searchtype=author&query=Saha%2C+N">N. Saha</a>, <a href="/search/astro-ph?searchtype=author&query=Gendre%2C+B">B. Gendre</a>, <a href="/search/astro-ph?searchtype=author&query=Kido%2C+D">D. Kido</a>, <a href="/search/astro-ph?searchtype=author&query=Watson%2C+A+M">A. M. Watson</a>, <a href="/search/astro-ph?searchtype=author&query=Becerra%2C+R+L">R. L. Becerra</a>, <a href="/search/astro-ph?searchtype=author&query=Belkin%2C+S">S. Belkin</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">S. Desai</a>, <a href="/search/astro-ph?searchtype=author&query=Pedreira%2C+A+C+C+d+E+S">A. C. C. do E. S. Pedreira</a>, <a href="/search/astro-ph?searchtype=author&query=Das%2C+U">U. Das</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+L">L. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Oates%2C+S+R">S. R. Oates</a>, <a href="/search/astro-ph?searchtype=author&query=Cenko%2C+S+B">S. B. Cenko</a>, <a href="/search/astro-ph?searchtype=author&query=Pozanenko%2C+A">A. Pozanenko</a>, <a href="/search/astro-ph?searchtype=author&query=Volnova%2C+A">A. Volnova</a>, <a href="/search/astro-ph?searchtype=author&query=Hu%2C+Y+-">Y. -D. Hu</a>, <a href="/search/astro-ph?searchtype=author&query=Castro-Tirado%2C+A+J">A. J. Castro-Tirado</a>, <a href="/search/astro-ph?searchtype=author&query=Orange%2C+N+B">N. B. Orange</a>, <a href="/search/astro-ph?searchtype=author&query=Moriya%2C+T+J">T. J. Moriya</a>, <a href="/search/astro-ph?searchtype=author&query=Fraija%2C+N">N. Fraija</a>, <a href="/search/astro-ph?searchtype=author&query=Niino%2C+Y">Y. Niino</a> , et al. (27 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="2405.02263v2-abstract-short" style="display: inline;"> We present the largest optical photometry compilation of Gamma-Ray Bursts (GRBs) with redshifts ($z$). We include 64813 observations of 535 events (including upper limits) from 28 February 1997 up to 18 August 2023. We also present a user-friendly web tool \textit{grbLC} which allows users the visualization of photometry, coordinates, redshift, host galaxy extinction, and spectral indices for each… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.02263v2-abstract-full').style.display = 'inline'; document.getElementById('2405.02263v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.02263v2-abstract-full" style="display: none;"> We present the largest optical photometry compilation of Gamma-Ray Bursts (GRBs) with redshifts ($z$). We include 64813 observations of 535 events (including upper limits) from 28 February 1997 up to 18 August 2023. We also present a user-friendly web tool \textit{grbLC} which allows users the visualization of photometry, coordinates, redshift, host galaxy extinction, and spectral indices for each event in our database. Furthermore, we have added a Gamma Ray Coordinate Network (GCN) scraper that can be used to collect data by gathering magnitudes from the GCNs. The web tool also includes a package for uniformly investigating colour evolution. We compute the optical spectral indices for 138 GRBs for which we have at least 4 filters at the same epoch in our sample and craft a procedure to distinguish between GRBs with and without colour evolution. By providing a uniform format and repository for the optical catalogue, this web-based archive is the first step towards unifying several community efforts to gather the photometric information for all GRBs with known redshifts. This catalogue will enable population studies by providing light curves (LCs) with better coverage since we have gathered data from different ground-based locations. Consequently, these LCs can be used to train future LC reconstructions for an extended inference of the redshift. The data gathering also allows us to fill some of the orbital gaps from Swift in crucial points of the LCs, e.g., at the end of the plateau emission or where a jet break is identified. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.02263v2-abstract-full').style.display = 'none'; document.getElementById('2405.02263v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 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">20 pages, 16 figures, 2 tables. Submitted to MNRAS, this version matches the third revision. The Online Materials and data will be available after the publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/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/2404.06334">arXiv:2404.06334</a> <span> [<a href="https://arxiv.org/pdf/2404.06334">pdf</a>, <a href="https://arxiv.org/format/2404.06334">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 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/10.3390/galaxies12060069">10.3390/galaxies12060069 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Calibration of luminosity correlations of gamma-ray bursts using quasars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Purohit%2C+S">Sarveshkumar Purohit</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</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="2404.06334v2-abstract-short" style="display: inline;"> In order to test the efficacy of Gamma-ray Bursts (GRB) as cosmological probes, we characterize the scatter in the correlations between six pairs of GRB observables, which have previously also been studied in arXiv:2011.14040. However, some of these observables depend on the luminosity distance, for which one needs to assume an underlying cosmological model. In order to circumvent this circularity… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.06334v2-abstract-full').style.display = 'inline'; document.getElementById('2404.06334v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.06334v2-abstract-full" style="display: none;"> In order to test the efficacy of Gamma-ray Bursts (GRB) as cosmological probes, we characterize the scatter in the correlations between six pairs of GRB observables, which have previously also been studied in arXiv:2011.14040. However, some of these observables depend on the luminosity distance, for which one needs to assume an underlying cosmological model. In order to circumvent this circularity problem, we use X-ray and UV fluxes of quasars as distance anchors to calculate the luminosity distance in a model-independent manner, which in turn is used to calculate the GRB-related quantities. We find that all six pairs of regression relations show high intrinsic scatter for both the low and high redshift sample. This implies that these GRB observables cannot be used as model-independent high precision cosmological probes. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.06334v2-abstract-full').style.display = 'none'; document.getElementById('2404.06334v2-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 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 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">9 pages, 3 figures. Accepted in Galaxies</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/2404.02153">arXiv:2404.02153</a> <span> [<a href="https://arxiv.org/pdf/2404.02153">pdf</a>, <a href="https://arxiv.org/format/2404.02153">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"> Mass calibration of DES Year-3 clusters via SPT-3G CMB cluster lensing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ansarinejad%2C+B">B. Ansarinejad</a>, <a href="/search/astro-ph?searchtype=author&query=Raghunathan%2C+S">S. Raghunathan</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=Alves%2C+O">O. Alves</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=Andrade-Oliveira%2C+F">F. Andrade-Oliveira</a>, <a href="/search/astro-ph?searchtype=author&query=Archipley%2C+M">M. Archipley</a>, <a href="/search/astro-ph?searchtype=author&query=Balkenhol%2C+L">L. Balkenhol</a>, <a href="/search/astro-ph?searchtype=author&query=Benabed%2C+K">K. Benabed</a>, <a href="/search/astro-ph?searchtype=author&query=Bender%2C+A+N">A. N. Bender</a>, <a href="/search/astro-ph?searchtype=author&query=Benson%2C+B+A">B. A. Benson</a>, <a href="/search/astro-ph?searchtype=author&query=Bertin%2C+E">E. Bertin</a>, <a href="/search/astro-ph?searchtype=author&query=Bianchini%2C+F">F. Bianchini</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=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Bouchet%2C+F+R">F. R. Bouchet</a>, <a href="/search/astro-ph?searchtype=author&query=Brooks%2C+D">D. Brooks</a>, <a href="/search/astro-ph?searchtype=author&query=Bryant%2C+L">L. Bryant</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=Camphuis%2C+E">E. Camphuis</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=Carretero%2C+J">J. Carretero</a> , et al. (120 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="2404.02153v2-abstract-short" style="display: inline;"> We measure the stacked lensing signal in the direction of galaxy clusters in the Dark Energy Survey Year 3 (DES Y3) redMaPPer sample, using cosmic microwave background (CMB) temperature data from SPT-3G, the third-generation CMB camera on the South Pole Telescope (SPT). We estimate the lensing signal using temperature maps constructed from the initial 2 years of data from the SPT-3G 'Main' survey,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.02153v2-abstract-full').style.display = 'inline'; document.getElementById('2404.02153v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.02153v2-abstract-full" style="display: none;"> We measure the stacked lensing signal in the direction of galaxy clusters in the Dark Energy Survey Year 3 (DES Y3) redMaPPer sample, using cosmic microwave background (CMB) temperature data from SPT-3G, the third-generation CMB camera on the South Pole Telescope (SPT). We estimate the lensing signal using temperature maps constructed from the initial 2 years of data from the SPT-3G 'Main' survey, covering 1500 deg$^2$ of the Southern sky. We then use this signal as a proxy for the mean cluster mass of the DES sample. In this work, we employ three versions of the redMaPPer catalogue: a Flux-Limited sample containing 8865 clusters, a Volume-Limited sample with 5391 clusters, and a Volume&Redshift-Limited sample with 4450 clusters. For the three samples, we find the mean cluster masses to be ${M}_{200{\rm{m}}}=1.66\pm0.13$ [stat.]$\pm0.03$ [sys.], $1.97\pm0.18$ [stat.]$\pm0.05$ [sys.], and $2.11\pm0.20$ [stat.]$\pm0.05$ [sys.]$\times{10}^{14}\ {\rm{M}}_{\odot }$, respectively. This is a factor of $\sim2$ improvement relative to the precision of measurements with previous generations of SPT surveys and the most constraining cluster mass measurements using CMB cluster lensing to date. Overall, we find no significant tensions between our results and masses given by redMaPPer mass-richness scaling relations of previous works, which were calibrated using CMB cluster lensing, optical weak lensing, and velocity dispersion measurements from various combinations of DES, SDSS and Planck data. We then divide our sample into 3 redshift and 3 richness bins, finding no significant tensions with optical weak-lensing calibrated masses in these bins. We forecast a $5.7\%$ constraint on the mean cluster mass of the DES Y3 sample with the complete SPT-3G surveys when using both temperature and polarization data and including an additional $\sim1400$ deg$^2$ of observations from the 'Extended' SPT-3G survey. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.02153v2-abstract-full').style.display = 'none'; document.getElementById('2404.02153v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 2 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">23 pages, 9 figures, accepted for publication in JCAP. Minor changes and corrections have been made relative to v1</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.02314">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/2402.11258">arXiv:2402.11258</a> <span> [<a href="https://arxiv.org/pdf/2402.11258">pdf</a>, <a href="https://arxiv.org/format/2402.11258">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 Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</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/10.1140/epjc/s10052-024-12846-y">10.1140/epjc/s10052-024-12846-y <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Generalized Lomb-Scargle Analysis of 22 years of Super-Kamiokande solar $^8$B neutrino data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Pasumarti%2C+V">Vibhavasu Pasumarti</a>, <a href="/search/astro-ph?searchtype=author&query=Desai%2C+S">Shantanu Desai</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="2402.11258v2-abstract-short" style="display: inline;"> We apply the generalized Lomb-Scargle periodogram to 22 years data of solar $^{8}$B neutrino fluxes detected by Super-Kamiokande. The primary motivation of this work was to check if the sinusoidal modulation at a frequency of 9.43/year (with a period of 38 days), which we had found to be marginally significant with the first five years of Super-K data, persists, with the accumulated data. We use f… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.11258v2-abstract-full').style.display = 'inline'; document.getElementById('2402.11258v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.11258v2-abstract-full" style="display: none;"> We apply the generalized Lomb-Scargle periodogram to 22 years data of solar $^{8}$B neutrino fluxes detected by Super-Kamiokande. The primary motivation of this work was to check if the sinusoidal modulation at a frequency of 9.43/year (with a period of 38 days), which we had found to be marginally significant with the first five years of Super-K data, persists, with the accumulated data. We use four different metrics for the calculation of significance. We do not find any evidence for periodicity at the aforementioned frequency or any other frequency with the updated data. Therefore the marginally detected periodicity at 9.43/year with the first five years of data was only a statistical fluctuation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.11258v2-abstract-full').style.display = 'none'; document.getElementById('2402.11258v2-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 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 17 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">8 pages, 3 figures. Accepted for publication in EPJC</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/2402.08455">arXiv:2402.08455</a> <span> [<a href="https://arxiv.org/pdf/2402.08455">pdf</a>, <a href="https://arxiv.org/format/2402.08455">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348615">10.1051/0004-6361/202348615 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The SRG/eROSITA All-Sky Survey: Dark Energy Survey Year 3 Weak Gravitational Lensing by eRASS1 selected Galaxy Clusters </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=Ghirardini%2C+V">V. Ghirardini</a>, <a href="/search/astro-ph?searchtype=author&query=Bocquet%2C+S">S. Bocquet</a>, <a href="/search/astro-ph?searchtype=author&query=Garrel%2C+C">C. Garrel</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=Liu%2C+A">A. Liu</a>, <a href="/search/astro-ph?searchtype=author&query=Kluge%2C+M">M. Kluge</a>, <a href="/search/astro-ph?searchtype=author&query=Kimmig%2C+L">L. Kimmig</a>, <a href="/search/astro-ph?searchtype=author&query=Reiprich%2C+T+H">T. H. Reiprich</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=Artis%2C+E">E. Artis</a>, <a href="/search/astro-ph?searchtype=author&query=Bahar%2C+Y+E">Y. E. Bahar</a>, <a href="/search/astro-ph?searchtype=author&query=Balzer%2C+F">F. Balzer</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">G. Bernstein</a>, <a href="/search/astro-ph?searchtype=author&query=Bulbul%2C+E">E. Bulbul</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=Chiu%2C+I">I. Chiu</a> , et al. (97 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.08455v1-abstract-short" style="display: inline;"> Number counts of galaxy clusters across redshift are a powerful cosmological probe, if a precise and accurate reconstruction of the underlying mass distribution is performed -- a challenge called mass calibration. With the advent of wide and deep photometric surveys, weak gravitational lensing by clusters has become the method of choice to perform this measurement. We measure and validate the weak… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08455v1-abstract-full').style.display = 'inline'; document.getElementById('2402.08455v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.08455v1-abstract-full" style="display: none;"> Number counts of galaxy clusters across redshift are a powerful cosmological probe, if a precise and accurate reconstruction of the underlying mass distribution is performed -- a challenge called mass calibration. With the advent of wide and deep photometric surveys, weak gravitational lensing by clusters has become the method of choice to perform this measurement. We measure and validate the weak gravitational lensing (WL) signature in the shape of galaxies observed in the first 3 years of the DES Y3 caused by galaxy clusters selected in the first all-sky survey performed by SRG/eROSITA. These data are then used to determine the scaling between X-ray photon count rate of the clusters and their halo mass and redshift. We empirically determine the degree of cluster member contamination in our background source sample. The individual cluster shear profiles are then analysed with a Bayesian population model that self-consistently accounts for the lens sample selection and contamination, and includes marginalization over a host of instrumental and astrophysical systematics. To quantify the accuracy of the mass extraction of that model, we perform mass measurements on mock cluster catalogs with realistic synthetic shear profiles. This allows us to establish that hydro-dynamical modelling uncertainties at low lens redshifts ($z<0.6$) are the dominant systematic limitation. At high lens redshift the uncertainties of the sources' photometric redshift calibration dominate. With regard to the X-ray count rate to halo mass relation, we constrain all its parameters. This work sets the stage for a joint analysis with the number counts of eRASS1 clusters to constrain a host of cosmological parameters. We demonstrate that WL mass calibration of galaxy clusters can be performed successfully with source galaxies whose calibration was performed primarily for cosmic shear experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.08455v1-abstract-full').style.display = 'none'; document.getElementById('2402.08455v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 February, 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">27 pages, 18 figures, 2 appendices, submitted to A\&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 687, A178 (2024) </p> </li> 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