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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=Adams%2C+J&start=50" class="pagination-next" >Next </a> <ul class="pagination-list"> <li> <a href="/search/?searchtype=author&query=Adams%2C+J&start=0" class="pagination-link is-current" aria-label="Goto page 1">1 </a> </li> <li> <a href="/search/?searchtype=author&query=Adams%2C+J&start=50" class="pagination-link " aria-label="Page 2" aria-current="page">2 </a> </li> <li> <a href="/search/?searchtype=author&query=Adams%2C+J&start=100" class="pagination-link " aria-label="Page 3" aria-current="page">3 </a> </li> <li> <a href="/search/?searchtype=author&query=Adams%2C+J&start=150" class="pagination-link " aria-label="Page 4" aria-current="page">4 </a> </li> <li> <a href="/search/?searchtype=author&query=Adams%2C+J&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/2501.16440">arXiv:2501.16440</a> <span> [<a href="https://arxiv.org/pdf/2501.16440">pdf</a>, <a href="https://arxiv.org/format/2501.16440">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"> Time-Integrated Southern-Sky Neutrino Source Searches with 10 Years of IceCube Starting-Track Events at Energies Down to 1 TeV </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (402 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="2501.16440v1-abstract-short" style="display: inline;"> In the IceCube Neutrino Observatory, a signal of astrophysical neutrinos is obscured by backgrounds from atmospheric neutrinos and muons produced in cosmic-ray interactions. IceCube event selections used to isolate the astrophysical neutrino signal often focus on t/he morphology of the light patterns recorded by the detector. The analyses presented here use the new IceCube Enhanced Starting Track… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16440v1-abstract-full').style.display = 'inline'; document.getElementById('2501.16440v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.16440v1-abstract-full" style="display: none;"> In the IceCube Neutrino Observatory, a signal of astrophysical neutrinos is obscured by backgrounds from atmospheric neutrinos and muons produced in cosmic-ray interactions. IceCube event selections used to isolate the astrophysical neutrino signal often focus on t/he morphology of the light patterns recorded by the detector. The analyses presented here use the new IceCube Enhanced Starting Track Event Selection (ESTES), which identifies events likely generated by muon neutrino interactions within the detector geometry, focusing on neutrino energies of 1-500 TeV with a median angular resolution of 1.4掳. Selecting for starting track events filters out not only the atmospheric-muon background, but also the atmospheric-neutrino background in the southern sky. This improves IceCube's muon neutrino sensitivity to southern-sky neutrino sources, especially for Galactic sources that are not expected to produce a substantial flux of neutrinos above 100 TeV. In this work, the ESTES sample was applied for the first time to searches for astrophysical sources of neutrinos, including a search for diffuse neutrino emission from the Galactic plane. No significant excesses were identified from any of the analyses; however, constraining limits are set on the hadronic emission from TeV gamma-ray Galactic plane objects and models of the diffuse Galactic plane neutrino flux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16440v1-abstract-full').style.display = 'none'; document.getElementById('2501.16440v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 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">23 pages, 8 figures, 4 tables. Submitted to ApJ</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.09276">arXiv:2501.09276</a> <span> [<a href="https://arxiv.org/pdf/2501.09276">pdf</a>, <a href="https://arxiv.org/format/2501.09276">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 neutrino doublets and triplets using 11.4 years of IceCube data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (402 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="2501.09276v1-abstract-short" style="display: inline;"> We report a search for high-energy astrophysical neutrino multiplets, detections of multiple neutrino clusters in the same direction within 30 days, based on an analysis of 11.4 years of IceCube data. A new search method optimized for transient neutrino emission with a monthly time scale is employed, providing a higher sensitivity to neutrino fluxes. This result is sensitive to neutrino transient… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.09276v1-abstract-full').style.display = 'inline'; document.getElementById('2501.09276v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.09276v1-abstract-full" style="display: none;"> We report a search for high-energy astrophysical neutrino multiplets, detections of multiple neutrino clusters in the same direction within 30 days, based on an analysis of 11.4 years of IceCube data. A new search method optimized for transient neutrino emission with a monthly time scale is employed, providing a higher sensitivity to neutrino fluxes. This result is sensitive to neutrino transient emission, reaching per-flavor flux of approximately $10^{-10}\ {\rm erg}\ {\rm cm}^{-2}\ {\rm sec}^{-1}$ from the Northern sky in the energy range $E\gtrsim 50$~TeV. The number of doublets and triplets identified in this search is compatible with the atmospheric background hypothesis, which leads us to set limits on the nature of neutrino transient sources with emission timescales of one month. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.09276v1-abstract-full').style.display = 'none'; document.getElementById('2501.09276v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 January, 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/2412.11861">arXiv:2412.11861</a> <span> [<a href="https://arxiv.org/pdf/2412.11861">pdf</a>, <a href="https://arxiv.org/format/2412.11861">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"> Cosmic Stillness: High Quiescent Galaxy Fractions Across Upper Mass Scales in the Early Universe to z = 7 with JWST </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Russell%2C+T+A">Tobias A. Russell</a>, <a href="/search/astro-ph?searchtype=author&query=Dobric%2C+N">Neva Dobric</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Austin%2C+D">Duncan Austin</a>, <a href="/search/astro-ph?searchtype=author&query=Harvey%2C+T">Thomas Harvey</a>, <a href="/search/astro-ph?searchtype=author&query=Trussler%2C+J">James Trussler</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+L">Leonardo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Westcott%2C+L">Lewi Westcott</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+H">Honor Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">Rogier A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">Rolf A. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+M+A">Madeline A. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+R">Rafael Ortiz III</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A">Aaron Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C+R+E">Russell E. Ryan Jr</a>, <a href="/search/astro-ph?searchtype=author&query=Summers%2C+J">Jake Summers</a> , et al. (3 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.11861v1-abstract-short" style="display: inline;"> We present a detailed investigation into the abundance and morphology of high redshift quenched galaxies at $3 < z < 7$ using James Webb Space Telescope data in the NEP, CEERS and JADES fields. Within these fields, we identify 90 candidate passive galaxies using specific star formation rates modelled with the BAGPIPES SED fitting code, which is more effective at identifying recently quenched syste… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.11861v1-abstract-full').style.display = 'inline'; document.getElementById('2412.11861v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.11861v1-abstract-full" style="display: none;"> We present a detailed investigation into the abundance and morphology of high redshift quenched galaxies at $3 < z < 7$ using James Webb Space Telescope data in the NEP, CEERS and JADES fields. Within these fields, we identify 90 candidate passive galaxies using specific star formation rates modelled with the BAGPIPES SED fitting code, which is more effective at identifying recently quenched systems than the classical UVJ method. With this sample of galaxies, we find number densities broadly consistent with other works and a rapidly evolving passive fraction of high mass galaxies ($\log_{10}{(M_{\star}/M_{\odot})} > $ 9.5) between $3 < z < 5$. We find that the fraction of galaxies with low star formation rates and mass 9.5 $ < \log_{10}{(M_{\star}/M_{\odot})} < $ 10.5 decreases from $\sim$25% at $3 < z < 4$ to $\sim$2% at $5 < z < 7$. Our passive sample of galaxies is shown to exhibit more compact light profiles compared to star-forming counterparts and some exhibit traces of AGN activity through detections in either the X-ray or radio. At the highest redshifts ($z > 6.5$) passive selections start to include examples of 'little red dots' which complicates any conclusions until their nature is better understood. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.11861v1-abstract-full').style.display = 'none'; document.getElementById('2412.11861v1-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 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, 5 tables, 11 figures, submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.05046">arXiv:2412.05046</a> <span> [<a href="https://arxiv.org/pdf/2412.05046">pdf</a>, <a href="https://arxiv.org/format/2412.05046">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"> Observation of Cosmic-Ray Anisotropy in the Southern Hemisphere with Twelve Years of Data Collected by the IceCube Neutrino Observatory </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguado%2C+T">T. Aguado</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (413 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.05046v1-abstract-short" style="display: inline;"> We analyzed the 7.92$\times 10^{11}$ cosmic-ray-induced muon events collected by the IceCube Neutrino Observatory from May 13, 2011, when the fully constructed experiment started to take data, to May 12, 2023. This dataset provides an up-to-date cosmic-ray arrival direction distribution in the Southern Hemisphere with unprecedented statistical accuracy covering more than a full period length of a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05046v1-abstract-full').style.display = 'inline'; document.getElementById('2412.05046v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.05046v1-abstract-full" style="display: none;"> We analyzed the 7.92$\times 10^{11}$ cosmic-ray-induced muon events collected by the IceCube Neutrino Observatory from May 13, 2011, when the fully constructed experiment started to take data, to May 12, 2023. This dataset provides an up-to-date cosmic-ray arrival direction distribution in the Southern Hemisphere with unprecedented statistical accuracy covering more than a full period length of a solar cycle. Improvements in Monte Carlo event simulation and better handling of year-to-year differences in data processing significantly reduce systematic uncertainties below the level of statistical fluctuations compared to the previously published results. We confirm the observation of a change in the angular structure of the cosmic-ray anisotropy between 10 TeV and 1 PeV, more specifically in the 100-300 TeV energy range. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.05046v1-abstract-full').style.display = 'none'; document.getElementById('2412.05046v1-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> 6 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.04944">arXiv:2411.04944</a> <span> [<a href="https://arxiv.org/pdf/2411.04944">pdf</a>, <a href="https://arxiv.org/format/2411.04944">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"> Galaxy Mergers in the Epoch of Reionization II: Major Merger-Triggered Star Formation and AGN Activities at $z = 4.5 - 8.5$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Duan%2C+Q">Qiao Duan</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qiong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Harvey%2C+T">Thomas Harvey</a>, <a href="/search/astro-ph?searchtype=author&query=Austin%2C+D">Duncan Austin</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+L">Leonardo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Duncan%2C+K+J">Kenneth J. Duncan</a>, <a href="/search/astro-ph?searchtype=author&query=Trussler%2C+J">James Trussler</a>, <a href="/search/astro-ph?searchtype=author&query=Pascalau%2C+R+G">Robert G. Pascalau</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">Rogier A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">Thomas J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Du%2C+X">Xiaojing Du</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">Rolf A. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+M+A">Madeline A. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+R">Rafael Ortiz III</a> , et al. (7 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.04944v1-abstract-short" style="display: inline;"> Galaxy mergers are a key driver of galaxy formation and evolution, including the triggering of AGN and star formation to a still unknown degree. We thus investigate the impact of galaxy mergers on star formation and AGN activity using a sample of 3,330 galaxies at $z = [4.5, 8.5]$ from eight JWST fields (CEERS, JADES GOODS-S, NEP-TDF, NGDEEP, GLASS, El-Gordo, SMACS-0723, and MACS-0416), collective… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.04944v1-abstract-full').style.display = 'inline'; document.getElementById('2411.04944v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.04944v1-abstract-full" style="display: none;"> Galaxy mergers are a key driver of galaxy formation and evolution, including the triggering of AGN and star formation to a still unknown degree. We thus investigate the impact of galaxy mergers on star formation and AGN activity using a sample of 3,330 galaxies at $z = [4.5, 8.5]$ from eight JWST fields (CEERS, JADES GOODS-S, NEP-TDF, NGDEEP, GLASS, El-Gordo, SMACS-0723, and MACS-0416), collectively covering an unmasked area of 189 arcmin$^2$. We focuses on star formation rate (SFR) enhancement, AGN fraction, and AGN excess in major merger ($渭> 1/4$) close-pair samples, defined by $螖z < 0.3$ and projected separations $r_p < 100$ kpc, compared to non-merger samples. We find that SFR enhancement occurs only at $r_p < 20$ kpc, with values of $0.25 \pm 0.10$ dex and $0.26 \pm 0.11$ dex above the non-merger medians for $z = [4.5, 6.5]$ and $z = [6.5, 8.5]$, respectively. No other statistically significant enhancements in galaxy sSFR or stellar mass are observed at any projected separation or redshift bin. We also compare our observational results with predictions from the SC-SAM simulation and find no evidence of star formation enhancement in the simulations at any separation range. Finally, we examine the AGN fraction and AGN excess, finding that the fraction of AGNs in AGN-galaxy pairs, relative to the total AGN population, is $3.25^{+1.50}_{-1.06}$ times greater than the fraction of galaxy pairs relative to the overall galaxy population at the same redshift. We find that nearly all AGNs have a companion within 100 kpc and observe an excess AGN fraction in close-pair samples compared to non-merger samples. This excess is found to be $1.26 \pm 0.06$ and $1.34 \pm 0.06$ for AGNs identified via the inferred BPT diagram and photometric SED selection, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.04944v1-abstract-full').style.display = 'none'; document.getElementById('2411.04944v1-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 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">17 Pages, 7 Figures, Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.10963">arXiv:2409.10963</a> <span> [<a href="https://arxiv.org/pdf/2409.10963">pdf</a>, <a href="https://arxiv.org/format/2409.10963">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"> JWST PRIMER: A lack of outshining in four normal z =4-6 galaxies from the ALMA-CRISTAL Survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Lines%2C+N+E+P">N. E. P. Lines</a>, <a href="/search/astro-ph?searchtype=author&query=Bowler%2C+R+A+A">R. A. A. Bowler</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">N. J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Fisher%2C+R">R. Fisher</a>, <a href="/search/astro-ph?searchtype=author&query=Varadaraj%2C+R+G">R. G. Varadaraj</a>, <a href="/search/astro-ph?searchtype=author&query=Nakazato%2C+Y">Y. Nakazato</a>, <a href="/search/astro-ph?searchtype=author&query=Aravena%2C+M">M. Aravena</a>, <a href="/search/astro-ph?searchtype=author&query=Assef%2C+R+J">R. J. Assef</a>, <a href="/search/astro-ph?searchtype=author&query=Birkin%2C+J+E">J. E. Birkin</a>, <a href="/search/astro-ph?searchtype=author&query=Ceverino%2C+D">D. Ceverino</a>, <a href="/search/astro-ph?searchtype=author&query=da+Cunha%2C+E">E. da Cunha</a>, <a href="/search/astro-ph?searchtype=author&query=Cullen%2C+F">F. Cullen</a>, <a href="/search/astro-ph?searchtype=author&query=De+Looze%2C+I">I. De Looze</a>, <a href="/search/astro-ph?searchtype=author&query=Donnan%2C+C+T">C. T. Donnan</a>, <a href="/search/astro-ph?searchtype=author&query=Dunlop%2C+J+S">J. S. Dunlop</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrara%2C+A">A. Ferrara</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Herrera-Camus%2C+R">R. Herrera-Camus</a>, <a href="/search/astro-ph?searchtype=author&query=Ikeda%2C+R">R. Ikeda</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Killi%2C+M">M. Killi</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+J">J. Li</a>, <a href="/search/astro-ph?searchtype=author&query=McLeod%2C+D+J">D. J. McLeod</a>, <a href="/search/astro-ph?searchtype=author&query=McLure%2C+R+J">R. J. McLure</a>, <a href="/search/astro-ph?searchtype=author&query=Mitsuhashi%2C+I">I. Mitsuhashi</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.10963v1-abstract-short" style="display: inline;"> We present a spatially resolved analysis of four star-forming galaxies at $z = 4.44-5.64$ using data from the JWST PRIMER and ALMA-CRISTAL surveys to probe the stellar and inter-stellar medium properties on the sub-kpc scale. In the $1-5\,渭{\rm m}$ JWST NIRCam imaging we find that the galaxies are composed of multiple clumps (between $2$ and $\sim 8$) separated by $\simeq 5\,{\rm kpc}$, with compa… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.10963v1-abstract-full').style.display = 'inline'; document.getElementById('2409.10963v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.10963v1-abstract-full" style="display: none;"> We present a spatially resolved analysis of four star-forming galaxies at $z = 4.44-5.64$ using data from the JWST PRIMER and ALMA-CRISTAL surveys to probe the stellar and inter-stellar medium properties on the sub-kpc scale. In the $1-5\,渭{\rm m}$ JWST NIRCam imaging we find that the galaxies are composed of multiple clumps (between $2$ and $\sim 8$) separated by $\simeq 5\,{\rm kpc}$, with comparable morphologies and sizes in the rest-frame UV and optical. Using BAGPIPES to perform pixel-by-pixel SED fitting to the JWST data we show that the SFR ($\simeq 25\,{\rm M}_{\odot}/{\rm yr}$) and stellar mass (${\rm log}_{10}(M_{\star}/{\rm M}_{\odot}) \simeq 9.5$) derived from the resolved analysis are in close ($ \lesssim 0.3\,{\rm dex}$) agreement with those obtained by fitting the integrated photometry. In contrast to studies of lower-mass sources, we thus find a reduced impact of outshining of the older (more massive) stellar populations in these normal $z \simeq 5$ galaxies. Our JWST analysis recovers bluer rest-frame UV slopes ($尾\simeq -2.1$) and younger ages ($\simeq 100\,{\rm Myr}$) than archival values. We find that the dust continuum from ALMA-CRISTAL seen in two of these galaxies correlates, as expected, with regions of redder rest-frame UV slopes and the SED-derived $A_{\rm V}$, as well as the peak in the stellar mass map. We compute the resolved IRX-$尾$ relation, showing that the IRX is consistent with the local starburst attenuation curve and further demonstrating the presence of an inhomogeneous dust distribution within the galaxies. A comparison of the CRISTAL sources to those from the FirstLight zoom-in simulation of galaxies with the same $M_{\star}$ and SFR reveals similar age and colour gradients, suggesting that major mergers may be important in the formation of clumpy galaxies at this epoch. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.10963v1-abstract-full').style.display = 'none'; document.getElementById('2409.10963v1-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 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, 8 figures, 3 tables, plus 4 page appendix. Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.05643">arXiv:2409.05643</a> <span> [<a href="https://arxiv.org/pdf/2409.05643">pdf</a>, <a href="https://arxiv.org/format/2409.05643">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> System performance of a cryogenic test-bed for the time-division multiplexing readout for NewAthena X-IFU </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vaccaro%2C+D">Davide Vaccaro</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Kuur%2C+J">Jan van der Kuur</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Hulst%2C+P">Paul van der Hulst</a>, <a href="/search/astro-ph?searchtype=author&query=Vos%2C+T">Tobias Vos</a>, <a href="/search/astro-ph?searchtype=author&query=de+Wit%2C+M">Martin de Wit</a>, <a href="/search/astro-ph?searchtype=author&query=Gottardi%2C+L">Luciano Gottardi</a>, <a href="/search/astro-ph?searchtype=author&query=Ravensberg%2C+K">Kevin Ravensberg</a>, <a href="/search/astro-ph?searchtype=author&query=Taralli%2C+E">Emanuele Taralli</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">Joseph Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Bandler%2C+S">Simon Bandler</a>, <a href="/search/astro-ph?searchtype=author&query=Bennet%2C+D">Douglas Bennet</a>, <a href="/search/astro-ph?searchtype=author&query=Chervenak%2C+J">James Chervenak</a>, <a href="/search/astro-ph?searchtype=author&query=Doriese%2C+B">Bertrand Doriese</a>, <a href="/search/astro-ph?searchtype=author&query=Durkin%2C+M">Malcolm Durkin</a>, <a href="/search/astro-ph?searchtype=author&query=Gard%2C+J">Johnathon Gard</a>, <a href="/search/astro-ph?searchtype=author&query=Reintsema%2C+C">Carl Reintsema</a>, <a href="/search/astro-ph?searchtype=author&query=Sakai%2C+K">Kazuhiro Sakai</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+S">Steven Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Ullom%2C+J">Joel Ullom</a>, <a href="/search/astro-ph?searchtype=author&query=Wakeham%2C+N">Nicholas Wakeham</a>, <a href="/search/astro-ph?searchtype=author&query=Herder%2C+J+d">Jan-Willem den Herder</a>, <a href="/search/astro-ph?searchtype=author&query=jackson%2C+B">Brian jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Khosropanah%2C+P">Pourya Khosropanah</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+J">Jian-Rong Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Roelfsema%2C+P">Peter Roelfsema</a> , et al. (1 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="2409.05643v3-abstract-short" style="display: inline;"> The X-ray Integral Field Unit (X-IFU) is an instrument of ESA's future NewAthena space observatory, with the goal to provide high-energy resolution ($<$ 4 eV at X-ray energies up to 7 keV) and high-spatial resolution (9") spectroscopic imaging over the X-ray energy range from 200 eV to 12 keV, by means of an array of about 1500 transition-edge sensors (TES) read out via SQUID time-division multipl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.05643v3-abstract-full').style.display = 'inline'; document.getElementById('2409.05643v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.05643v3-abstract-full" style="display: none;"> The X-ray Integral Field Unit (X-IFU) is an instrument of ESA's future NewAthena space observatory, with the goal to provide high-energy resolution ($<$ 4 eV at X-ray energies up to 7 keV) and high-spatial resolution (9") spectroscopic imaging over the X-ray energy range from 200 eV to 12 keV, by means of an array of about 1500 transition-edge sensors (TES) read out via SQUID time-division multiplexing (TDM). A TDM-based laboratory test-bed has been assembled at SRON, hosting an array of $75\times 75\ \upmu$m$^2$ TESs that are read out via 2-column $\times$ 32-row TDM. A system component that is critical to high-performance operation is the wiring harness that connects the room-temperature electronics to the cryogenic readout componentry. We report here on our characterization of such a test-bed, whose harness has a length close to what envisioned for X-IFU, which allowed to achieve a co-added energy resolution at a level of 2.7~eV FWHM at 6~keV via 32-row readout. In addition, we provide an outlook on the integration of TDM readout into the X-IFU Focal-Plane Assembly Development Model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.05643v3-abstract-full').style.display = 'none'; document.getElementById('2409.05643v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 5 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 9 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">Submitted for publication to Journal of Astronomical Telescopes, Instrumentation and Systems. arXiv admin note: text overlap with arXiv:2403.02978</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.09472">arXiv:2407.09472</a> <span> [<a href="https://arxiv.org/pdf/2407.09472">pdf</a>, <a href="https://arxiv.org/format/2407.09472">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"> Galaxy Mergers in the Epoch of Reionization I: A JWST Study of Pair Fractions, Merger Rates, and Stellar Mass Accretion Rates at $z = 4.5-11.5$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Duan%2C+Q">Qiao Duan</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qiong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Austin%2C+D">Duncan Austin</a>, <a href="/search/astro-ph?searchtype=author&query=Harvey%2C+T">Thomas Harvey</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Duncan%2C+K+J">Kenneth J. Duncan</a>, <a href="/search/astro-ph?searchtype=author&query=Trussler%2C+J">James Trussler</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+L">Leonardo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Westcott%2C+L">Lewi Westcott</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+H">Honor Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">Rogier A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T+J">Thomas J. Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Du%2C+X">Xiaojing Du</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">Rolf A. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+M+A">Madeline A. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a> , et al. (8 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.09472v2-abstract-short" style="display: inline;"> We present a full analysis of galaxy major merger pair fractions, merger rates, and mass accretion rates, thus uncovering the role of mergers in galaxy formation at the earliest previously unexplored epoch of $4.5<z<11.5$. We target galaxies with masses $\log_{10}(\mathrm{M}_*/\mathrm{M}_\odot) = 8.0 - 10.0$, utilizing data from eight JWST Cycle-1 fields (CEERS, JADES GOODS-S, NEP-TDF, NGDEEP, GLA… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.09472v2-abstract-full').style.display = 'inline'; document.getElementById('2407.09472v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.09472v2-abstract-full" style="display: none;"> We present a full analysis of galaxy major merger pair fractions, merger rates, and mass accretion rates, thus uncovering the role of mergers in galaxy formation at the earliest previously unexplored epoch of $4.5<z<11.5$. We target galaxies with masses $\log_{10}(\mathrm{M}_*/\mathrm{M}_\odot) = 8.0 - 10.0$, utilizing data from eight JWST Cycle-1 fields (CEERS, JADES GOODS-S, NEP-TDF, NGDEEP, GLASS, El-Gordo, SMACS-0723, MACS-0416), covering an unmasked area of 189.36 $\mathrm{arcmin}^2$. We develop a new probabilistic pair-counting methodology that integrates full photometric redshift posteriors and corrects for detection incompleteness to quantify close pairs with physical projected separations between 20 and 50 kpc. Our analysis reveals an increase in pair fractions up to $z = 8$, reaching $0.211 \pm 0.065$, followed by a statistically flat evolution to $z = 11.5$. We find that the galaxy merger rate increases from the local Universe up to $z = 6$ and then stabilizes at a value of $\sim 6$ Gyr$^{-1}$ up to $z = 11.5$. We fit both a power-law and a power-law + exponential model to our pair fraction and merger rate redshift evolution, finding that the latter model describes the trends more accurately, particularly at $z = 8.0 - 11.5$. In addition, we measure that the average galaxy increases its stellar mass due to mergers by a factor of $2.77 \pm 0.99$ from redshift $z = 10.5$ to $z = 5.0$. Lastly, we investigate the impact of mergers on galaxy stellar mass growth, revealing that mergers contribute $71 \pm 25\%$ as much to galaxy stellar mass increases as star formation from gas. This indicates that mergers drive about half of galaxy assembly at high redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.09472v2-abstract-full').style.display = 'none'; document.getElementById('2407.09472v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 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">30 Pages, 15 Figures, Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.01351">arXiv:2407.01351</a> <span> [<a href="https://arxiv.org/pdf/2407.01351">pdf</a>, <a href="https://arxiv.org/format/2407.01351">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/10.3847/1538-4357/ad643d">10.3847/1538-4357/ad643d <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing the connection between IceCube neutrinos and MOJAVE AGN </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (399 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="2407.01351v1-abstract-short" style="display: inline;"> Active Galactic Nuclei (AGN) are prime candidate sources of the high-energy, astrophysical neutrinos detected by IceCube. This is demonstrated by the real-time multi-messenger detection of the blazar TXS 0506+056 and the recent evidence of neutrino emission from NGC 1068 from a separate time-averaged study. However, the production mechanism of the astrophysical neutrinos in AGN is not well establi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01351v1-abstract-full').style.display = 'inline'; document.getElementById('2407.01351v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.01351v1-abstract-full" style="display: none;"> Active Galactic Nuclei (AGN) are prime candidate sources of the high-energy, astrophysical neutrinos detected by IceCube. This is demonstrated by the real-time multi-messenger detection of the blazar TXS 0506+056 and the recent evidence of neutrino emission from NGC 1068 from a separate time-averaged study. However, the production mechanism of the astrophysical neutrinos in AGN is not well established which can be resolved via correlation studies with photon observations. For neutrinos produced due to photohadronic interactions in AGN, in addition to a correlation of neutrinos with high-energy photons, there would also be a correlation of neutrinos with photons emitted at radio wavelengths. In this work, we perform an in-depth stacking study of the correlation between 15 GHz radio observations of AGN reported in the MOJAVE XV catalog, and ten years of neutrino data from IceCube. We also use a time-dependent approach which improves the statistical power of the stacking analysis. No significant correlation was found for both analyses and upper limits are reported. When compared to the IceCube diffuse flux, at 100 TeV and for a spectral index of 2.5, the upper limits derived are $\sim3\%$ and $\sim9\%$ for the time-averaged and time-dependent case, respectively. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.01351v1-abstract-full').style.display = 'none'; document.getElementById('2407.01351v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 Pages 7 Figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> 973:97 (14pp), </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> The Astrophysical Journal, 973:97 (14pp), 2024 October 1 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.13673">arXiv:2406.13673</a> <span> [<a href="https://arxiv.org/pdf/2406.13673">pdf</a>, <a href="https://arxiv.org/format/2406.13673">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> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2024.103046">10.1016/j.astropartphys.2024.103046 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The EUSO-SPB2 Fluorescence Telescope for the Detection of Ultra-High Energy Cosmic Rays </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J+H">James H. Adams Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Allard%2C+D">Denis Allard</a>, <a href="/search/astro-ph?searchtype=author&query=Alldredge%2C+P">Phillip Alldredge</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">Luis Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Anzalone%2C+A">Anna Anzalone</a>, <a href="/search/astro-ph?searchtype=author&query=Battisti%2C+M">Matteo Battisti</a>, <a href="/search/astro-ph?searchtype=author&query=Belov%2C+A+A">Alexander A. Belov</a>, <a href="/search/astro-ph?searchtype=author&query=Bertaina%2C+M">Mario Bertaina</a>, <a href="/search/astro-ph?searchtype=author&query=Bertone%2C+P+F">Peter F. Bertone</a>, <a href="/search/astro-ph?searchtype=author&query=Blin-Bondil%2C+S">Sylvie Blin-Bondil</a>, <a href="/search/astro-ph?searchtype=author&query=Burton%2C+J">Julia Burton</a>, <a href="/search/astro-ph?searchtype=author&query=Cafagna%2C+F+S">Francesco S. Cafagna</a>, <a href="/search/astro-ph?searchtype=author&query=Casolino%2C+M">Marco Casolino</a>, <a href="/search/astro-ph?searchtype=author&query=%C4%8Cern%C3%BD%2C+K">Karel 膶ern媒</a>, <a href="/search/astro-ph?searchtype=author&query=Christ%2C+M+J">Mark J. Christ</a>, <a href="/search/astro-ph?searchtype=author&query=Colalillo%2C+R">Roberta Colalillo</a>, <a href="/search/astro-ph?searchtype=author&query=Crawford%2C+H+J">Hank J. Crawford</a>, <a href="/search/astro-ph?searchtype=author&query=Creusot%2C+A">Alexandre Creusot</a>, <a href="/search/astro-ph?searchtype=author&query=Cummings%2C+A">Austin Cummings</a>, <a href="/search/astro-ph?searchtype=author&query=Diesing%2C+R">Rebecca Diesing</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Nola%2C+A">Alessandro Di Nola</a>, <a href="/search/astro-ph?searchtype=author&query=Ebisuzaki%2C+T">Toshikazu Ebisuzaki</a>, <a href="/search/astro-ph?searchtype=author&query=Eser%2C+J">Johannes Eser</a>, <a href="/search/astro-ph?searchtype=author&query=Ferrarese%2C+S">Silvia Ferrarese</a>, <a href="/search/astro-ph?searchtype=author&query=Filippatos%2C+G">George Filippatos</a> , et al. (57 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.13673v2-abstract-short" style="display: inline;"> The Extreme Universe Space Observatory on a Super Pressure Balloon 2 (EUSO-SPB2) flew on May 13$^{\text{th}}$ and 14$^{\text{th}}$ of 2023. Consisting of two novel optical telescopes, the payload utilized next-generation instrumentation for the observations of extensive air showers from near space. One instrument, the fluorescence telescope (FT) searched for Ultra-High Energy Cosmic Rays (UHECRs)… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.13673v2-abstract-full').style.display = 'inline'; document.getElementById('2406.13673v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.13673v2-abstract-full" style="display: none;"> The Extreme Universe Space Observatory on a Super Pressure Balloon 2 (EUSO-SPB2) flew on May 13$^{\text{th}}$ and 14$^{\text{th}}$ of 2023. Consisting of two novel optical telescopes, the payload utilized next-generation instrumentation for the observations of extensive air showers from near space. One instrument, the fluorescence telescope (FT) searched for Ultra-High Energy Cosmic Rays (UHECRs) by recording the atmosphere below the balloon in the near-UV with a 1~$渭$s time resolution using 108 multi-anode photomultiplier tubes with a total of 6,912 channels. Validated by pre-flight measurements during a field campaign, the energy threshold was estimated around 2~EeV with an expected event rate of approximately 1 event per 10 hours of observation. Based on the limited time afloat, the expected number of UHECR observations throughout the flight is between 0 and 2. Consistent with this expectation, no UHECR candidate events have been found. The majority of events appear to be detector artifacts that were not rejected properly due to a shortened commissioning phase. Despite the earlier-than-expected termination of the flight, data were recorded which provide insights into the detectors stability in the near-space environment as well as the diffuse ultraviolet emissivity of the atmosphere, both of which are impactful to future experiments. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.13673v2-abstract-full').style.display = 'none'; document.getElementById('2406.13673v2-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 19 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">Journal ref:</span> Astroparticle Physics 165 (2025) 103046 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.07601">arXiv:2406.07601</a> <span> [<a href="https://arxiv.org/pdf/2406.07601">pdf</a>, <a href="https://arxiv.org/format/2406.07601">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="High Energy Physics - Experiment">hep-ex</span> </div> </div> <p class="title is-5 mathjax"> IceCube Search for Neutrino Emission from X-ray Bright Seyfert Galaxies </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (400 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="2406.07601v1-abstract-short" style="display: inline;"> The recent IceCube detection of TeV neutrino emission from the nearby active galaxy NGC 1068 suggests that active galactic nuclei (AGN) could make a sizable contribution to the diffuse flux of astrophysical neutrinos. The absence of TeV $纬$-rays from NGC 1068 indicates neutrino production in the vicinity of the supermassive black hole, where the high radiation density leads to $纬$-ray attenuation.… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07601v1-abstract-full').style.display = 'inline'; document.getElementById('2406.07601v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.07601v1-abstract-full" style="display: none;"> The recent IceCube detection of TeV neutrino emission from the nearby active galaxy NGC 1068 suggests that active galactic nuclei (AGN) could make a sizable contribution to the diffuse flux of astrophysical neutrinos. The absence of TeV $纬$-rays from NGC 1068 indicates neutrino production in the vicinity of the supermassive black hole, where the high radiation density leads to $纬$-ray attenuation. Therefore, any potential neutrino emission from similar sources is not expected to correlate with high-energy $纬$-rays. Disk-corona models predict neutrino emission from Seyfert galaxies to correlate with keV X-rays, as they are tracers of coronal activity. Using through-going track events from the Northern Sky recorded by IceCube between 2011 and 2021, we report results from a search for individual and aggregated neutrino signals from 27 additional Seyfert galaxies that are contained in the BAT AGN Spectroscopic Survey (BASS). Besides the generic single power-law, we evaluate the spectra predicted by the disk-corona model. Assuming all sources to be intrinsically similar to NGC 1068, our findings constrain the collective neutrino emission from X-ray bright Seyfert galaxies in the Northern Hemisphere, but, at the same time, show excesses of neutrinos that could be associated with the objects NGC 4151 and CGCG 420-015. These excesses result in a 2.7$蟽$ significance with respect to background expectations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.07601v1-abstract-full').style.display = 'none'; document.getElementById('2406.07601v1-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 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">17 pages, 9 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.06684">arXiv:2406.06684</a> <span> [<a href="https://arxiv.org/pdf/2406.06684">pdf</a>, <a href="https://arxiv.org/format/2406.06684">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 neutrino emission from hard X-ray AGN with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (401 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="2406.06684v2-abstract-short" style="display: inline;"> Active Galactic Nuclei (AGN) are promising candidate sources of high-energy astrophysical neutrinos since they provide environments rich in matter and photon targets where cosmic ray interactions may lead to the production of gamma rays and neutrinos. We searched for high-energy neutrino emission from AGN using the $\textit{Swift}$-BAT Spectroscopic Survey (BASS) catalog of hard X-ray sources and… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06684v2-abstract-full').style.display = 'inline'; document.getElementById('2406.06684v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.06684v2-abstract-full" style="display: none;"> Active Galactic Nuclei (AGN) are promising candidate sources of high-energy astrophysical neutrinos since they provide environments rich in matter and photon targets where cosmic ray interactions may lead to the production of gamma rays and neutrinos. We searched for high-energy neutrino emission from AGN using the $\textit{Swift}$-BAT Spectroscopic Survey (BASS) catalog of hard X-ray sources and 12 years of IceCube muon track data. First, upon performing a stacked search, no significant emission was found. Second, we searched for neutrinos from a list of 43 candidate sources and found an excess from the direction of two sources, Seyfert galaxies NGC 1068 and NGC 4151. We observed NGC 1068 at flux $蠁_{谓_渭+\bar谓_渭}$ = $4.02_{-1.52}^{+1.58} \times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized at 1 TeV, with power-law spectral index, $纬$ = 3.10$^{+0.26}_{-0.22}$, consistent with previous IceCube results. The observation of a neutrino excess from the direction of NGC 4151 is at a post-trial significance of 2.9$蟽$. If interpreted as an astrophysical signal, the excess observed from NGC 4151 corresponds to a flux $蠁_{谓_渭+\bar谓_渭}$ = $1.51_{-0.81}^{+0.99} \times 10^{-11}$ TeV$^{-1}$ cm$^{-2}$ s$^{-1}$ normalized at 1 TeV and $纬$ = 2.83$^{+0.35}_{-0.28}$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.06684v2-abstract-full').style.display = 'none'; document.getElementById('2406.06684v2-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 10 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/2406.04617">arXiv:2406.04617</a> <span> [<a href="https://arxiv.org/pdf/2406.04617">pdf</a>, <a href="https://arxiv.org/format/2406.04617">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"> JWST view of four infant galaxies at z=8.31-8.49 in the MACS0416 field and implications for reionization </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ma%2C+Z">Zhiyuan Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+B">Bangzheng Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+C">Cheng Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+H">Haojing Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Foo%2C+N">Nicholas Foo</a>, <a href="/search/astro-ph?searchtype=author&query=Egami%2C+E">Eiichi Egami</a>, <a href="/search/astro-ph?searchtype=author&query=Diego%2C+J+M">Jose M. Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">Rolf A. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Summers%2C+J">Jake Summers</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">Rogier A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Silva%2C+J+C+J">Jordan C. J. D'Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+M+A">Madeline A. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+R">Rafael Ortiz III</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A">Aaron Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C%2C+R+E">Russell E. Ryan, Jr.</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.04617v2-abstract-short" style="display: inline;"> New JWST/NIRCam wide-field slitless spectroscopy provides redshifts for four z>8 galaxies located behind the lensing cluster MACS J0416.1-2403. Two of them, "Y1" and "JD", have previously reported spectroscopic redshifts based on ALMA measurements of [OIII] 88 $渭$m and/or [CII] 157.7 $渭$m lines. Y1 is a merging system of three components, and the existing redshift z=8.31 is confirmed. However, JD… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.04617v2-abstract-full').style.display = 'inline'; document.getElementById('2406.04617v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.04617v2-abstract-full" style="display: none;"> New JWST/NIRCam wide-field slitless spectroscopy provides redshifts for four z>8 galaxies located behind the lensing cluster MACS J0416.1-2403. Two of them, "Y1" and "JD", have previously reported spectroscopic redshifts based on ALMA measurements of [OIII] 88 $渭$m and/or [CII] 157.7 $渭$m lines. Y1 is a merging system of three components, and the existing redshift z=8.31 is confirmed. However, JD is at z=8.34 instead of the previously claimed z=9.28. JD's close companion, "JD-N", which was a previously discovered z>8 candidate, is now identified at the same redshift as JD. JD and JD-N form an interacting pair. A new candidate at z>8, "f090d_018", is also confirmed and is at z=8.49. These four objects are likely part of an overdensity that signposts a large structure extending ~165 kpc in projected distance and ~48.7 Mpc in radial distance. They are magnified by less than one magnitude and have intrinsic $M_{UV}$ ranging from -19.57 to -20.83 mag. Their spectral energy distributions show that the galaxies are all very young with ages ~ 4-18 Myr and stellar masses about $10^{7-8}$ ${\rm M_\odot}$. These infant galaxies have very different star formation rates ranging from a few to over a hundred $\rm{M_\odot}$ yr$^{-1}$, but only two of them (JD and f090d_018) have blue rest-frame UV slopes $尾<-2.0$ indicative of a high Lyman-continuum photon escape fraction that could contribute significantly to the cosmic hydrogen-reionizing background. Interestingly, these two galaxies are the least massive and least active ones among the four. The other two systems have much flatter UV slopes largely because of their high dust extinction ($A_{\rm V}$=0.9-1.0 mag). Their much lower indicated escape fractions show that even very young, actively star-forming galaxies can have negligible contribution to reionization when they quickly form dust throughout their bodies. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.04617v2-abstract-full').style.display = 'none'; document.getElementById('2406.04617v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">18 pages, 6 figures, after addressing the referee report</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.03817">arXiv:2405.03817</a> <span> [<a href="https://arxiv.org/pdf/2405.03817">pdf</a>, <a href="https://arxiv.org/format/2405.03817">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 joint multimessenger signals from potential Galactic PeVatrons with HAWC and IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Alfaro%2C+R">R. Alfaro</a>, <a href="/search/astro-ph?searchtype=author&query=Alvarez%2C+C">C. Alvarez</a>, <a href="/search/astro-ph?searchtype=author&query=Arteaga-Vel%C3%A1zquez%2C+J+C">J. C. Arteaga-Vel谩zquez</a>, <a href="/search/astro-ph?searchtype=author&query=Rojas%2C+D+A">D. Avila Rojas</a>, <a href="/search/astro-ph?searchtype=author&query=Solares%2C+H+A+A">H. A. Ayala Solares</a>, <a href="/search/astro-ph?searchtype=author&query=Babu%2C+R">R. Babu</a>, <a href="/search/astro-ph?searchtype=author&query=Belmont-Moreno%2C+E">E. Belmont-Moreno</a>, <a href="/search/astro-ph?searchtype=author&query=Caballero-Mora%2C+K+S">K. S. Caballero-Mora</a>, <a href="/search/astro-ph?searchtype=author&query=Capistr%C3%A1n%2C+T">T. Capistr谩n</a>, <a href="/search/astro-ph?searchtype=author&query=Carrami%C3%B1ana%2C+A">A. Carrami帽ana</a>, <a href="/search/astro-ph?searchtype=author&query=Casanova%2C+S">S. Casanova</a>, <a href="/search/astro-ph?searchtype=author&query=Cotti%2C+U">U. Cotti</a>, <a href="/search/astro-ph?searchtype=author&query=Cotzomi%2C+J">J. Cotzomi</a>, <a href="/search/astro-ph?searchtype=author&query=de+Le%C3%B3n%2C+S+C">S. Couti帽o de Le贸n</a>, <a href="/search/astro-ph?searchtype=author&query=De+la+Fuente%2C+E">E. De la Fuente</a>, <a href="/search/astro-ph?searchtype=author&query=Depaoli%2C+D">D. Depaoli</a>, <a href="/search/astro-ph?searchtype=author&query=Di+Lalla%2C+N">N. Di Lalla</a>, <a href="/search/astro-ph?searchtype=author&query=Hernandez%2C+R+D">R. Diaz Hernandez</a>, <a href="/search/astro-ph?searchtype=author&query=D%C3%ADaz-V%C3%A9lez%2C+J+C">J. C. D铆az-V茅lez</a>, <a href="/search/astro-ph?searchtype=author&query=Engel%2C+K">K. Engel</a>, <a href="/search/astro-ph?searchtype=author&query=Ergin%2C+T">T. Ergin</a>, <a href="/search/astro-ph?searchtype=author&query=Fan%2C+K+L">K. L. Fan</a>, <a href="/search/astro-ph?searchtype=author&query=Fang%2C+K">K. Fang</a>, <a href="/search/astro-ph?searchtype=author&query=Fraija%2C+N">N. Fraija</a>, <a href="/search/astro-ph?searchtype=author&query=Fraija%2C+S">S. Fraija</a> , et al. (469 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="2405.03817v1-abstract-short" style="display: inline;"> Galactic PeVatrons are sources that can accelerate cosmic rays to PeV energies. The high-energy cosmic rays are expected to interact with the surrounding ambient material or radiation, resulting in the production of gamma rays and neutrinos. To optimize for the detection of such associated production of gamma rays and neutrinos for a given source morphology and spectrum, a multi-messenger analysis… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03817v1-abstract-full').style.display = 'inline'; document.getElementById('2405.03817v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.03817v1-abstract-full" style="display: none;"> Galactic PeVatrons are sources that can accelerate cosmic rays to PeV energies. The high-energy cosmic rays are expected to interact with the surrounding ambient material or radiation, resulting in the production of gamma rays and neutrinos. To optimize for the detection of such associated production of gamma rays and neutrinos for a given source morphology and spectrum, a multi-messenger analysis that combines gamma rays and neutrinos is required. In this study, we use the Multi-Mission Maximum Likelihood framework (3ML) with IceCube Maximum Likelihood Analysis software (i3mla) and HAWC Accelerated Likelihood (HAL) to search for a correlation between 22 known gamma-ray sources from the third HAWC gamma-ray catalog and 14 years of IceCube track-like data. No significant neutrino emission from the direction of the HAWC sources was found. We report the best-fit gamma-ray model and 90% CL neutrino flux limit from the 22 sources. From the neutrino flux limit, we conclude that the gamma-ray emission from five of the sources can not be produced purely from hadronic interactions. We report the limit for the fraction of gamma rays produced by hadronic interactions for these five sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.03817v1-abstract-full').style.display = 'none'; document.getElementById('2405.03817v1-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 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.19589">arXiv:2404.19589</a> <span> [<a href="https://arxiv.org/pdf/2404.19589">pdf</a>, <a href="https://arxiv.org/format/2404.19589">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 Physics - Experiment">hep-ex</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Detectors">physics.ins-det</span> </div> </div> <p class="title is-5 mathjax"> Acceptance Tests of more than 10 000 Photomultiplier Tubes for the multi-PMT Digital Optical Modules of the IceCube Upgrade </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (399 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="2404.19589v2-abstract-short" style="display: inline;"> More than 10,000 photomultiplier tubes (PMTs) with a diameter of 80 mm will be installed in multi-PMT Digital Optical Modules (mDOMs) of the IceCube Upgrade. These have been tested and pre-calibrated at two sites. A throughput of more than 1000 PMTs per week with both sites was achieved with a modular design of the testing facilities and highly automated testing procedures. The testing facilities… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.19589v2-abstract-full').style.display = 'inline'; document.getElementById('2404.19589v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.19589v2-abstract-full" style="display: none;"> More than 10,000 photomultiplier tubes (PMTs) with a diameter of 80 mm will be installed in multi-PMT Digital Optical Modules (mDOMs) of the IceCube Upgrade. These have been tested and pre-calibrated at two sites. A throughput of more than 1000 PMTs per week with both sites was achieved with a modular design of the testing facilities and highly automated testing procedures. The testing facilities can easily be adapted to other PMTs, such that they can, e.g., be re-used for testing the PMTs for IceCube-Gen2. Single photoelectron response, high voltage dependence, time resolution, prepulse, late pulse, afterpulse probabilities, and dark rates were measured for each PMT. We describe the design of the testing facilities, the testing procedures, and the results of the acceptance tests. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.19589v2-abstract-full').style.display = 'none'; document.getElementById('2404.19589v2-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 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 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">24 pages, 19 figures, 2 tables, submitted to JINST</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2404.10751">arXiv:2404.10751</a> <span> [<a href="https://arxiv.org/pdf/2404.10751">pdf</a>, <a href="https://arxiv.org/format/2404.10751">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"> EPOCHS III: Unbiased UV continuum slopes at 6.5<z<13 from combined PEARLS GTO and public JWST NIRCam imaging </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Austin%2C+D">Duncan Austin</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Harvey%2C+T">Thomas Harvey</a>, <a href="/search/astro-ph?searchtype=author&query=Duan%2C+Q">Qiao Duan</a>, <a href="/search/astro-ph?searchtype=author&query=Trussler%2C+J">James Trussler</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qiong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Juodzbalis%2C+I">Ignas Juodzbalis</a>, <a href="/search/astro-ph?searchtype=author&query=Ormerod%2C+K">Katherine Ormerod</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+L">Leonardo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Westcott%2C+L">Lewi Westcott</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+H">Honor Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Wilkins%2C+S+M">Stephen M. Wilkins</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatawdekar%2C+R">Rachana Bhatawdekar</a>, <a href="/search/astro-ph?searchtype=author&query=Caruana%2C+J">Joseph Caruana</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Silva%2C+J+C+J">Jordan C. J. D'Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Furtak%2C+L+J">Lukas J. Furtak</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">Rolf A. Jansen</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2404.10751v1-abstract-short" style="display: inline;"> We present an analysis of rest-frame UV continuum slopes, $尾$, using a sample of 1011 galaxies at $6.5<z<13$ from the EPOCHS photometric sample collated from the GTO PEARLS and public ERS/GTO/GO (JADES, CEERS, NGDEEP, GLASS) JWST NIRCam imaging across $178.9~\mathrm{arcmin}^2$ of unmasked blank sky. We correct our UV slopes for the photometric error coupling bias using $200,000$ power law SEDs for… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10751v1-abstract-full').style.display = 'inline'; document.getElementById('2404.10751v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2404.10751v1-abstract-full" style="display: none;"> We present an analysis of rest-frame UV continuum slopes, $尾$, using a sample of 1011 galaxies at $6.5<z<13$ from the EPOCHS photometric sample collated from the GTO PEARLS and public ERS/GTO/GO (JADES, CEERS, NGDEEP, GLASS) JWST NIRCam imaging across $178.9~\mathrm{arcmin}^2$ of unmasked blank sky. We correct our UV slopes for the photometric error coupling bias using $200,000$ power law SEDs for each $尾=\{-1,-1.5,-2,-2.5,-3\}$ in each field, finding biases as large as $螖尾\simeq-0.55$ for the lowest SNR galaxies in our sample. Additionally, we simulate the impact of rest-UV line emission (including Ly$伪$) and damped Ly$伪$ systems on our measured $尾$, finding biases as large as $0.5-0.6$ for the most extreme systems. We find a decreasing trend with redshift of $尾=-1.51\pm0.08-(0.097\pm0.010)\times z$, with potential evidence for Pop.~III stars or top-heavy initial mass functions (IMFs) in a subsample of 68 $尾+蟽_尾<-2.8$ galaxies. At $z\simeq11.5$, we measure an extremely blue $尾(M_{\mathrm{UV}}=-19)=-2.73\pm0.06$, deviating from simulations, indicative of low-metallicity galaxies with non-zero Lyman continuum escape fractions $f_{\mathrm{esc, LyC}}\gtrsim0$ and minimal dust content. The observed steepening of $\mathrm{d}尾/\mathrm{d}\log_{10}(M_{\star}/\mathrm{M}_{\odot})$ from $0.22\pm0.02$ at $z=7$ to $0.81\pm0.13$ at $z=11.5$ implies that dust produced in core-collapse supernovae (SNe) at early times may be ejected via outflows from low mass galaxies. We also observe a flatter $\mathrm{d}尾/\mathrm{d}M_{\mathrm{UV}}=0.03\pm0.02$ at $z=7$ and a shallower $\mathrm{d}尾/\mathrm{d}\log_{10}(M_{\star} / \mathrm{M}_{\odot})$ at $z<11$ than seen by HST, unveiling a new population of low mass, faint, galaxies reddened by dust produced in the stellar winds of asymptotic giant branch (AGB) stars or carbon-rich Wolf-Rayet binaries. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2404.10751v1-abstract-full').style.display = 'none'; document.getElementById('2404.10751v1-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 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">37 pages, 18 figures, 8 tables. Data available via the Github page at https://github.com/duncanaustin98/EPOCHS-III-data. Submitted to ApJ on 16/04/2024</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.03908">arXiv:2403.03908</a> <span> [<a href="https://arxiv.org/pdf/2403.03908">pdf</a>, <a href="https://arxiv.org/format/2403.03908">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad8c29">10.3847/1538-4357/ad8c29 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> EPOCHS IV: SED Modelling Assumptions and their impact on the Stellar Mass Function at 46.5 < z < 13.5$ using PEARLS and public JWST observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Harvey%2C+T">Thomas Harvey</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Austin%2C+D">Duncan Austin</a>, <a href="/search/astro-ph?searchtype=author&query=Juodzbalis%2C+I">Ignas Juodzbalis</a>, <a href="/search/astro-ph?searchtype=author&query=Trussler%2C+J">James Trussler</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qiong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Ormerod%2C+K">Katherine Ormerod</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+L">Leonardo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Lovell%2C+C+C">Christopher C. Lovell</a>, <a href="/search/astro-ph?searchtype=author&query=Duan%2C+Q">Qiao Duan</a>, <a href="/search/astro-ph?searchtype=author&query=Westcott%2C+L">Lewi Westcott</a>, <a href="/search/astro-ph?searchtype=author&query=Harris%2C+H">Honor Harris</a>, <a href="/search/astro-ph?searchtype=author&query=Bhatawdekar%2C+R">Rachana Bhatawdekar</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Caruana%2C+J">Joseph Caruana</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+C">Cheng Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Furtak%2C+L+J">Lukas J. Furtak</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Hathi%2C+N+P">Nimish P. Hathi</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">Rolf A. Jansen</a> , et al. (9 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.03908v2-abstract-short" style="display: inline;"> We utilize deep JWST NIRCam observations for the first direct constraints on the Galaxy Stellar Mass Function (GSMF) at $z>10$. Our EPOCHS v1 sample includes 1120 galaxy candidates at $6.5<z<13.5$ taken from a consistent reduction and analysis of publicly available deep JWST NIRCam data covering the PEARLS, CEERS, GLASS, JADES GOOD-S, NGDEEP, and SMACS0723 surveys, totalling 187 arcmin$^2$. We inv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.03908v2-abstract-full').style.display = 'inline'; document.getElementById('2403.03908v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.03908v2-abstract-full" style="display: none;"> We utilize deep JWST NIRCam observations for the first direct constraints on the Galaxy Stellar Mass Function (GSMF) at $z>10$. Our EPOCHS v1 sample includes 1120 galaxy candidates at $6.5<z<13.5$ taken from a consistent reduction and analysis of publicly available deep JWST NIRCam data covering the PEARLS, CEERS, GLASS, JADES GOOD-S, NGDEEP, and SMACS0723 surveys, totalling 187 arcmin$^2$. We investigate the impact of SED fitting methods, assumed star formation histories (SFH), dust laws, and priors on galaxy masses and the resultant GSMF. Whilst our fiducial GSMF agrees with the literature at $z<13.5$, we find that the assumed SFH model has a large impact on the GSMF and stellar mass density (SMD), finding a 0.75~dex increase in the SMD at $z=10.5$ between a flexible non-parametric and standard parametric SFH. Overall, we find a flatter SMD evolution at $z \geq 9$ than some studies predict, suggesting a rapid buildup of stellar mass in the early Universe. We find no incompatibility between our results and those of standard cosmological models, as suggested previously, although the most massive galaxies may require a high star formation efficiency. We find that the "Little Red Dot" galaxies dominate the $z=7$ GSMF at high-masses, necessitating a better understanding of the relative contributions of AGN and stellar emission. We show that assuming a theoretically motivated top-heavy IMF reduces stellar mass by 0.5~dex without affecting fit quality, but our results remain consistent with existing cosmological models with a standard IMF. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.03908v2-abstract-full').style.display = 'none'; document.getElementById('2403.03908v2-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 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 6 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">36 pages, 16 figures. Published in ApJ. Data is avaible on Github: https://github.com/tHarvey303/EpochsIV . Comments to corresponding author welcome at thomas.harvey-3@manchester.ac.uk</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 978 89 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.02978">arXiv:2403.02978</a> <span> [<a href="https://arxiv.org/pdf/2403.02978">pdf</a>, <a href="https://arxiv.org/format/2403.02978">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> System performance of a TDM test-bed with long flex harness towards the new X-IFU FPA-DM </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Vaccaro%2C+D">D. Vaccaro</a>, <a href="/search/astro-ph?searchtype=author&query=de+Wit%2C+M">M. de Wit</a>, <a href="/search/astro-ph?searchtype=author&query=van+der+Kuur%2C+J">J. van der Kuur</a>, <a href="/search/astro-ph?searchtype=author&query=Gottardi%2C+L">L. Gottardi</a>, <a href="/search/astro-ph?searchtype=author&query=Ravensberg%2C+K">K. Ravensberg</a>, <a href="/search/astro-ph?searchtype=author&query=Taralli%2C+E">E. Taralli</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Bandler%2C+S+R">S. R. Bandler</a>, <a href="/search/astro-ph?searchtype=author&query=Chervenak%2C+J+A">J. A. Chervenak</a>, <a href="/search/astro-ph?searchtype=author&query=Doriese%2C+W+B">W. B. Doriese</a>, <a href="/search/astro-ph?searchtype=author&query=Durkin%2C+M">M. Durkin</a>, <a href="/search/astro-ph?searchtype=author&query=Reintsema%2C+C">C. Reintsema</a>, <a href="/search/astro-ph?searchtype=author&query=Sakai%2C+K">K. Sakai</a>, <a href="/search/astro-ph?searchtype=author&query=Smith%2C+S+J">S. J. Smith</a>, <a href="/search/astro-ph?searchtype=author&query=Wakeham%2C+N+A">N. A. Wakeham</a>, <a href="/search/astro-ph?searchtype=author&query=Jackson%2C+B">B. Jackson</a>, <a href="/search/astro-ph?searchtype=author&query=Khosropanah%2C+P">P. Khosropanah</a>, <a href="/search/astro-ph?searchtype=author&query=Gao%2C+J+R">J. R. Gao</a>, <a href="/search/astro-ph?searchtype=author&query=Herder%2C+J+W+A+d">J. W. A. den Herder</a>, <a href="/search/astro-ph?searchtype=author&query=Roelfsema%2C+P">P. Roelfsema</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.02978v1-abstract-short" style="display: inline;"> SRON (Netherlands Institute for Space Research) is developing the Focal Plane Assembly (FPA) for Athena X-IFU, whose Demonstration Model (DM) will use for the first time a time domain multiplexing (TDM)-based readout system for the on-board transition-edge sensors (TES). We report on the characterization activities on a TDM setup provided by NASA Goddard Space Flight Center (GSFC) and National Ins… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02978v1-abstract-full').style.display = 'inline'; document.getElementById('2403.02978v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.02978v1-abstract-full" style="display: none;"> SRON (Netherlands Institute for Space Research) is developing the Focal Plane Assembly (FPA) for Athena X-IFU, whose Demonstration Model (DM) will use for the first time a time domain multiplexing (TDM)-based readout system for the on-board transition-edge sensors (TES). We report on the characterization activities on a TDM setup provided by NASA Goddard Space Flight Center (GSFC) and National Institute for Standards and Technology (NIST) and tested in SRON cryogenic test facilities. The goal of these activities is to study the impact of the longer harness, closer to X-IFU specs, in a different EMI environment and switching from a single-ended to a differential readout scheme. In this contribution we describe the advancement in the debugging of the system in the SRON cryostat, which led to the demonstration of the nominal spectral performance of 2.8 eV at 5.9~keV with 16-row multiplexing, as well as an outlook for the future endeavours for the TDM readout integration on X-IFU's FPA-DM at SRON. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02978v1-abstract-full').style.display = 'none'; document.getElementById('2403.02978v1-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 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">Under publication in Journal of Low Temperature Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.02516">arXiv:2403.02516</a> <span> [<a href="https://arxiv.org/pdf/2403.02516">pdf</a>, <a href="https://arxiv.org/format/2403.02516">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="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1103/PhysRevLett.132.151001">10.1103/PhysRevLett.132.151001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of Seven Astrophysical Tau Neutrino Candidates with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=IceCube+Collaboration"> IceCube Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (380 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="2403.02516v3-abstract-short" style="display: inline;"> We report on a measurement of astrophysical tau neutrinos with 9.7 years of IceCube data. Using convolutional neural networks trained on images derived from simulated events, seven candidate $谓_蟿$ events were found with visible energies ranging from roughly 20 TeV to 1 PeV and a median expected parent $谓_蟿$ energy of about 200 TeV. Considering backgrounds from astrophysical and atmospheric neutrin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02516v3-abstract-full').style.display = 'inline'; document.getElementById('2403.02516v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.02516v3-abstract-full" style="display: none;"> We report on a measurement of astrophysical tau neutrinos with 9.7 years of IceCube data. Using convolutional neural networks trained on images derived from simulated events, seven candidate $谓_蟿$ events were found with visible energies ranging from roughly 20 TeV to 1 PeV and a median expected parent $谓_蟿$ energy of about 200 TeV. Considering backgrounds from astrophysical and atmospheric neutrinos, and muons from $蟺^\pm/K^\pm$ decays in atmospheric air showers, we obtain a total estimated background of about 0.5 events, dominated by non-$谓_蟿$ astrophysical neutrinos. Thus, we rule out the absence of astrophysical $谓_蟿$ at the $5蟽$ level. The measured astrophysical $谓_蟿$ flux is consistent with expectations based on previously published IceCube astrophysical neutrino flux measurements and neutrino oscillations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02516v3-abstract-full').style.display = 'none'; document.getElementById('2403.02516v3-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">Accepted for publication in Physical Review Letters. This version includes full author list metadata</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys.Rev.Lett. 132 (2024) 15, 151001 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.02470">arXiv:2403.02470</a> <span> [<a href="https://arxiv.org/pdf/2403.02470">pdf</a>, <a href="https://arxiv.org/format/2403.02470">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> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</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/10.1088/1748-0221/19/06/P06026">10.1088/1748-0221/19/06/P06026 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improved modeling of in-ice particle showers for IceCube event reconstruction </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (394 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="2403.02470v2-abstract-short" style="display: inline;"> The IceCube Neutrino Observatory relies on an array of photomultiplier tubes to detect Cherenkov light produced by charged particles in the South Pole ice. IceCube data analyses depend on an in-depth characterization of the glacial ice, and on novel approaches in event reconstruction that utilize fast approximations of photoelectron yields. Here, a more accurate model is derived for event reconstr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02470v2-abstract-full').style.display = 'inline'; document.getElementById('2403.02470v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.02470v2-abstract-full" style="display: none;"> The IceCube Neutrino Observatory relies on an array of photomultiplier tubes to detect Cherenkov light produced by charged particles in the South Pole ice. IceCube data analyses depend on an in-depth characterization of the glacial ice, and on novel approaches in event reconstruction that utilize fast approximations of photoelectron yields. Here, a more accurate model is derived for event reconstruction that better captures our current knowledge of ice optical properties. When evaluated on a Monte Carlo simulation set, the median angular resolution for in-ice particle showers improves by over a factor of three compared to a reconstruction based on a simplified model of the ice. The most substantial improvement is obtained when including effects of birefringence due to the polycrystalline structure of the ice. When evaluated on data classified as particle showers in the high-energy starting events sample, a significantly improved description of the events is observed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.02470v2-abstract-full').style.display = 'none'; document.getElementById('2403.02470v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 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">28 pages, 18 figures, 1 table, submitted to JINST, updated to account for comments received</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2024 JINST 19 P06026 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.18026">arXiv:2402.18026</a> <span> [<a href="https://arxiv.org/pdf/2402.18026">pdf</a>, <a href="https://arxiv.org/format/2402.18026">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/10.1103/PhysRevD.110.022001">10.1103/PhysRevD.110.022001 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Characterization of the Astrophysical Diffuse Neutrino Flux using Starting Track Events in IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Bash%2C+S">S. Bash</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (394 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="2402.18026v1-abstract-short" style="display: inline;"> A measurement of the diffuse astrophysical neutrino spectrum is presented using IceCube data collected from 2011-2022 (10.3 years). We developed novel detection techniques to search for events with a contained vertex and exiting track induced by muon neutrinos undergoing a charged-current interaction. Searching for these starting track events allows us to not only more effectively reject atmospher… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18026v1-abstract-full').style.display = 'inline'; document.getElementById('2402.18026v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.18026v1-abstract-full" style="display: none;"> A measurement of the diffuse astrophysical neutrino spectrum is presented using IceCube data collected from 2011-2022 (10.3 years). We developed novel detection techniques to search for events with a contained vertex and exiting track induced by muon neutrinos undergoing a charged-current interaction. Searching for these starting track events allows us to not only more effectively reject atmospheric muons but also atmospheric neutrino backgrounds in the southern sky, opening a new window to the sub-100 TeV astrophysical neutrino sky. The event selection is constructed using a dynamic starting track veto and machine learning algorithms. We use this data to measure the astrophysical diffuse flux as a single power law flux (SPL) with a best-fit spectral index of $纬= 2.58 ^{+0.10}_{-0.09}$ and per-flavor normalization of $蠁^{\mathrm{Astro}}_{\mathrm{per-flavor}} = 1.68 ^{+0.19}_{-0.22} \times 10^{-18} \times \mathrm{GeV}^{-1} \mathrm{cm}^{-2} \mathrm{s}^{-1} \mathrm{sr}^{-1}$ (at 100 TeV). The sensitive energy range for this dataset is 3 - 550 TeV under the SPL assumption. This data was also used to measure the flux under a broken power law, however we did not find any evidence of a low energy cutoff. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.18026v1-abstract-full').style.display = 'none'; document.getElementById('2402.18026v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 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, 28 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Phys. Rev. D 110, 022001 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.15971">arXiv:2401.15971</a> <span> [<a href="https://arxiv.org/pdf/2401.15971">pdf</a>, <a href="https://arxiv.org/format/2401.15971">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 sizes of bright Lyman-break galaxies at $z\simeq3-5$ with JWST PRIMER </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Varadaraj%2C+R+G">R. G. Varadaraj</a>, <a href="/search/astro-ph?searchtype=author&query=Bowler%2C+R+A+A">R. A. A. Bowler</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M+J">M. J. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">N. J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Choustikov%2C+N">N. Choustikov</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Carnall%2C+A+C">A. C. Carnall</a>, <a href="/search/astro-ph?searchtype=author&query=McLeod%2C+D+J">D. J. McLeod</a>, <a href="/search/astro-ph?searchtype=author&query=Dunlop%2C+J+S">J. S. Dunlop</a>, <a href="/search/astro-ph?searchtype=author&query=Donnan%2C+C+T">C. T. Donnan</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.15971v2-abstract-short" style="display: inline;"> We use data from the JWST Public Release IMaging for Extragalactic Research (PRIMER) survey to measure the size scaling relations of 1668 rest-frame UV-bright Lyman-break galaxies (LBGs) at $z=3-5$ with stellar masses $\mathrm{log}_{10}(M_{\star}/M_{\odot}) > 9$. The sample was selected from seeing-dominated ground-based data, presenting an unbiased sampling of the morphology and size distribution… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.15971v2-abstract-full').style.display = 'inline'; document.getElementById('2401.15971v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.15971v2-abstract-full" style="display: none;"> We use data from the JWST Public Release IMaging for Extragalactic Research (PRIMER) survey to measure the size scaling relations of 1668 rest-frame UV-bright Lyman-break galaxies (LBGs) at $z=3-5$ with stellar masses $\mathrm{log}_{10}(M_{\star}/M_{\odot}) > 9$. The sample was selected from seeing-dominated ground-based data, presenting an unbiased sampling of the morphology and size distributions of luminous sources. We fit S茅rsic profiles to eight NIRCam bands and also measure a non-parametric half-light radius. We find that the size distributions with both measurements are well-fit by a log-normal distribution at all redshifts, consistent with disk formation models where size is governed by host dark-matter halo angular momentum. We find a size-redshift evolution of $R_{e} = 3.51(1+z)^{-0.60\pm0.22}$ kpc, in agreement with JWST studies. When considering the typical (modal) size over $z=3-5$, we find little evolution with bright LBGs remaining compact at $R_{e}\simeq0.7-0.9$ kpc. Simultaneously, we find evidence for a build-up of large ($R_{e} > 2$ kpc) galaxies by $z=3$. We find some evidence for a negatively sloped size-mass relation at $z=5$ when S茅rsic profiles are used to fit the data in F200W. The intrinsic scatter in our size-mass relations increases at higher redshifts. Additionally, measurements probing the rest-UV (F200W) show larger intrinsic scatter than those probing the rest-optical (F356W). Finally, we leverage rest-UV and rest-optical photometry to show that disky galaxies are well established by $z=5$, but are beginning to undergo dissipative processes, such as mergers, by $z=3$. The agreement of our size-mass and size-luminosity relations with simulations provides tentative evidence for centrally concentrated star formation at high-redshift. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.15971v2-abstract-full').style.display = 'none'; document.getElementById('2401.15971v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 29 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 9 figures, 3 tables. Accepted to MNRAS. 2 figures added in appendix</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.11994">arXiv:2401.11994</a> <span> [<a href="https://arxiv.org/pdf/2401.11994">pdf</a>, <a href="https://arxiv.org/format/2401.11994">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"> Citizen Science for IceCube: Name that Neutrino </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (391 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.11994v1-abstract-short" style="display: inline;"> Name that Neutrino is a citizen science project where volunteers aid in classification of events for the IceCube Neutrino Observatory, an immense particle detector at the geographic South Pole. From March 2023 to September 2023, volunteers did classifications of videos produced from simulated data of both neutrino signal and background interactions. Name that Neutrino obtained more than 128,000 cl… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11994v1-abstract-full').style.display = 'inline'; document.getElementById('2401.11994v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.11994v1-abstract-full" style="display: none;"> Name that Neutrino is a citizen science project where volunteers aid in classification of events for the IceCube Neutrino Observatory, an immense particle detector at the geographic South Pole. From March 2023 to September 2023, volunteers did classifications of videos produced from simulated data of both neutrino signal and background interactions. Name that Neutrino obtained more than 128,000 classifications by over 1,800 registered volunteers that were compared to results obtained by a deep neural network machine-learning algorithm. Possible improvements for both Name that Neutrino and the deep neural network are discussed. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.11994v1-abstract-full').style.display = 'none'; document.getElementById('2401.11994v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.06525">arXiv:2401.06525</a> <span> [<a href="https://arxiv.org/pdf/2401.06525">pdf</a>, <a href="https://arxiv.org/format/2401.06525">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> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1016/j.astropartphys.2023.102891">10.1016/j.astropartphys.2023.102891 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> EUSO-SPB1 Mission and Science </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Collaboration%2C+J">JEM-EUSO Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abdellaoui%2C+G">G. Abdellaoui</a>, <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Adams.%2C+J+H">J. H. Adams. Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/astro-ph?searchtype=author&query=Alonso%2C+G">G. Alonso</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Asano%2C+K">K. Asano</a>, <a href="/search/astro-ph?searchtype=author&query=Attallah%2C+R">R. Attallah</a>, <a href="/search/astro-ph?searchtype=author&query=Attoui%2C+H">H. Attoui</a>, <a href="/search/astro-ph?searchtype=author&query=Pernas%2C+M+A">M. Ave Pernas</a>, <a href="/search/astro-ph?searchtype=author&query=Bachmann%2C+R">R. Bachmann</a>, <a href="/search/astro-ph?searchtype=author&query=Bacholle%2C+S">S. Bacholle</a>, <a href="/search/astro-ph?searchtype=author&query=Bagheri%2C+M">M. Bagheri</a>, <a href="/search/astro-ph?searchtype=author&query=Bakiri%2C+M">M. Bakiri</a>, <a href="/search/astro-ph?searchtype=author&query=Bal%C3%A1z%2C+J">J. Bal谩z</a>, <a href="/search/astro-ph?searchtype=author&query=Barghini%2C+D">D. Barghini</a>, <a href="/search/astro-ph?searchtype=author&query=Bartocci%2C+S">S. Bartocci</a>, <a href="/search/astro-ph?searchtype=author&query=Battisti%2C+M">M. Battisti</a>, <a href="/search/astro-ph?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/astro-ph?searchtype=author&query=Beldjilali%2C+B">B. Beldjilali</a>, <a href="/search/astro-ph?searchtype=author&query=Belenguer%2C+T">T. Belenguer</a> , et al. (271 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.06525v1-abstract-short" style="display: inline;"> The Extreme Universe Space Observatory on a Super Pressure Balloon 1 (EUSO-SPB1) was launched in 2017 April from Wanaka, New Zealand. The plan of this mission of opportunity on a NASA super pressure balloon test flight was to circle the southern hemisphere. The primary scientific goal was to make the first observations of ultra-high-energy cosmic-ray extensive air showers (EASs) by looking down on… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.06525v1-abstract-full').style.display = 'inline'; document.getElementById('2401.06525v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.06525v1-abstract-full" style="display: none;"> The Extreme Universe Space Observatory on a Super Pressure Balloon 1 (EUSO-SPB1) was launched in 2017 April from Wanaka, New Zealand. The plan of this mission of opportunity on a NASA super pressure balloon test flight was to circle the southern hemisphere. The primary scientific goal was to make the first observations of ultra-high-energy cosmic-ray extensive air showers (EASs) by looking down on the atmosphere with an ultraviolet (UV) fluorescence telescope from suborbital altitude (33~km). After 12~days and 4~hours aloft, the flight was terminated prematurely in the Pacific Ocean. Before the flight, the instrument was tested extensively in the West Desert of Utah, USA, with UV point sources and lasers. The test results indicated that the instrument had sensitivity to EASs of approximately 3 EeV. Simulations of the telescope system, telescope on time, and realized flight trajectory predicted an observation of about 1 event assuming clear sky conditions. The effects of high clouds were estimated to reduce this value by approximately a factor of 2. A manual search and a machine-learning-based search did not find any EAS signals in these data. Here we review the EUSO-SPB1 instrument and flight and the EAS search. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.06525v1-abstract-full').style.display = 'none'; document.getElementById('2401.06525v1-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 19 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Astropart Phys 154 (2024) 102891 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.11603">arXiv:2312.11603</a> <span> [<a href="https://arxiv.org/pdf/2312.11603">pdf</a>, <a href="https://arxiv.org/format/2312.11603">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202349119">10.1051/0004-6361/202349119 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> JWST's PEARLS: 119 multiply imaged galaxies behind MACS0416, lensing properties of caustic crossing galaxies, and the relation between halo mass and number of globular clusters at $z=0.4$ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Diego%2C+J+M">Jose M. Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Willner%2C+S">Steven Willner</a>, <a href="/search/astro-ph?searchtype=author&query=Harvey%2C+T">Tom Harvey</a>, <a href="/search/astro-ph?searchtype=author&query=Broadhurst%2C+T">Tom Broadhurst</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">Rolf A. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Summers%2C+J">Jake Summers</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">Rogier A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Silva%2C+J+C+J">Jordan C. J. D'Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+M+A">Madeline A. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+R">Rafael Ortiz III</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A">Aaron Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C%2C+R+E">Russell E. Ryan, Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Willmer%2C+C+N+A">Christopher N. A. Willmer</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+H">Haojing Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+F">Fengwu Sun</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.11603v2-abstract-short" style="display: inline;"> We present a new lens model for the $z=0.396$ galaxy cluster MACS J0416.1$-$2403 based on a previously known set of 77 spectroscopically confirmed, multiply imaged galaxies plus an additional set of 42 candidate multiply imaged galaxies from past HST and new JWST data. The new galaxies lack spectroscopic redshifts but have geometric and/or photometric redshift estimates that are presented here. Th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.11603v2-abstract-full').style.display = 'inline'; document.getElementById('2312.11603v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.11603v2-abstract-full" style="display: none;"> We present a new lens model for the $z=0.396$ galaxy cluster MACS J0416.1$-$2403 based on a previously known set of 77 spectroscopically confirmed, multiply imaged galaxies plus an additional set of 42 candidate multiply imaged galaxies from past HST and new JWST data. The new galaxies lack spectroscopic redshifts but have geometric and/or photometric redshift estimates that are presented here. The new model predicts magnifications and time delays for all multiple images. The full set of constraints totals 343, constituting the largest sample of multiple images lensed by a single cluster to date. Caustic-crossing galaxies lensed by this cluster are especially interesting. Some of these galaxies show transient events, most of which are interpreted as micro-lensing of stars at cosmological distances. These caustic-crossing arcs are expected to show similar events in future, deeper JWST observations. We provide time delay and magnification models for all these arcs. The time delays and the magnifications for different arcs are generally anti-correlated, as expected from $N$-body simulations. In the major sub-halos of the cluster, the dark-matter mass from our lens model correlates well with the observed number of globular clusters. This confirms earlier results, derived at lower redshifts, which suggest that globular clusters can be used as powerful mass proxies for the halo masses when lensing constraints are scarce or not available. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.11603v2-abstract-full').style.display = 'none'; document.getElementById('2312.11603v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 18 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages and 11 figures. Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 690, A114 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.11515">arXiv:2312.11515</a> <span> [<a href="https://arxiv.org/pdf/2312.11515">pdf</a>, <a href="https://arxiv.org/format/2312.11515">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/10.3847/1538-4357/ad220b">10.3847/1538-4357/ad220b <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad683e">10.3847/1538-4357/ad683e <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for 10--1000 GeV neutrinos from Gamma Ray Bursts with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=IceCube+Collaboration"> IceCube Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (384 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.11515v3-abstract-short" style="display: inline;"> We present the results of a search for 10--1,000 GeV neutrinos from 2,268 gamma-ray bursts over 8 years of IceCube-DeepCore data. This work probes burst physics below the photosphere where electromagnetic radiation cannot escape. Neutrinos of tens of GeVs are predicted in sub-photospheric collision of free streaming neutrons with bulk-jet protons. In a first analysis, we searched for the most sign… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.11515v3-abstract-full').style.display = 'inline'; document.getElementById('2312.11515v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.11515v3-abstract-full" style="display: none;"> We present the results of a search for 10--1,000 GeV neutrinos from 2,268 gamma-ray bursts over 8 years of IceCube-DeepCore data. This work probes burst physics below the photosphere where electromagnetic radiation cannot escape. Neutrinos of tens of GeVs are predicted in sub-photospheric collision of free streaming neutrons with bulk-jet protons. In a first analysis, we searched for the most significant neutrino-GRB coincidence using six overlapping time windows centered on the prompt phase of each GRB. In a second analysis, we conducted a search for a group of GRBs, each individually too weak to be detectable, but potentially significant when combined. No evidence of neutrino emission is found for either analysis. The most significant neutrino coincidence is for Fermi-GBM GRB bn 140807500, with a p-value of 0.097 corrected for all trials. The binomial test used to search for a group of GRBs had a p-value of 0.65 after all trial corrections. The binomial test found a group consisting only of GRB bn 140807500 and no additional GRBs. The neutrino limits of this work complement those obtained by IceCube at TeV to PeV energies. We compare our findings for the large set of GRBs as well as GRB 221009A to the sub-photospheric neutron-proton collision model and find that GRB 221009A provides the most constraining limit on baryon loading. For a jet Lorentz factor of 300 (800), the baryon loading on GRB 221009A is lower than 3.85 (2.13) at a 90% confidence level. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.11515v3-abstract-full').style.display = 'none'; document.getElementById('2312.11515v3-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 12 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 964 126 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.10063">arXiv:2312.10063</a> <span> [<a href="https://arxiv.org/pdf/2312.10063">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Physics and Society">physics.soc-ph</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"> Accelerating pathways to leadership for underrepresented groups in STEM </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=2030STEM+Collaboration"> 2030STEM Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J+D">Jennifer D. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Bess%2C+C">Cameron Bess</a>, <a href="/search/astro-ph?searchtype=author&query=Brumbeg%2C+J">Joshua Brumbeg</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+R">Ruth Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Faherty%2C+J+K">Jacqueline K. Faherty</a>, <a href="/search/astro-ph?searchtype=author&query=Ginete%2C+D">Daren Ginete</a>, <a href="/search/astro-ph?searchtype=author&query=Holford%2C+M">Mand毛 Holford</a>, <a href="/search/astro-ph?searchtype=author&query=Jefferson%2C+B">Bobby Jefferson</a>, <a href="/search/astro-ph?searchtype=author&query=Garbarino%2C+J">Jeanne Garbarino</a>, <a href="/search/astro-ph?searchtype=author&query=Mays%2C+A">Alfred Mays</a>, <a href="/search/astro-ph?searchtype=author&query=Nwafor-Okoli%2C+C">Chinyere Nwafor-Okoli</a>, <a href="/search/astro-ph?searchtype=author&query=Ramirez-Ruiz%2C+E">Enrico Ramirez-Ruiz</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.10063v1-abstract-short" style="display: inline;"> The vision of 2030STEM is to address systemic barriers in institutional structures and funding mechanisms required to achieve full inclusion in Science, Technology, Engineering, and Mathematics (STEM) and accelerate leadership pathways for individuals from underrepresented populations across STEM sectors. 2030STEM takes a systems-level approach to create a community of practice that can test, lear… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.10063v1-abstract-full').style.display = 'inline'; document.getElementById('2312.10063v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.10063v1-abstract-full" style="display: none;"> The vision of 2030STEM is to address systemic barriers in institutional structures and funding mechanisms required to achieve full inclusion in Science, Technology, Engineering, and Mathematics (STEM) and accelerate leadership pathways for individuals from underrepresented populations across STEM sectors. 2030STEM takes a systems-level approach to create a community of practice that can test, learn and promote programs and policies that affirm and value cultural identities in STEM. To achieve parity and full representation in the STEM workforce, a variety of changes are needed across academia and STEM professional industries (e.g., business, finance, biotech, government) to accelerate underrepresented groups into positions of leadership throughout the STEM ecosystem. Through a series of subject matter interviews, roundtables, and curated analysis four major themes have surfaced, which, if implemented, could exponentially accelerate the creation of critical pathways to leadership, break down pre-existing barriers and biases, intentionally elevate the voices, value, and research of underrepresented groups in STEM, and implement new structural strategies at scale. This white paper provides a summary of innovative new practices designed to accelerate inclusion, including expanding on known global toolkits, new funding strategies, and the structural changes required throughout various STEM professions to propel pathways to leadership for underrepresented groups. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.10063v1-abstract-full').style.display = 'none'; document.getElementById('2312.10063v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 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/2312.08204">arXiv:2312.08204</a> <span>  </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"> JEM-EUSO Collaboration contributions to the 38th International Cosmic Ray Conference </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J+H">J. H. Adams Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/astro-ph?searchtype=author&query=Alldredge%2C+P">P. Alldredge</a>, <a href="/search/astro-ph?searchtype=author&query=Aloisio%2C+R">R. Aloisio</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Bagheri%2C+M">M. Bagheri</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Barghini%2C+D">D. Barghini</a>, <a href="/search/astro-ph?searchtype=author&query=Battisti%2C+M">M. Battisti</a>, <a href="/search/astro-ph?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/astro-ph?searchtype=author&query=Belov%2C+A+A">A. A. Belov</a>, <a href="/search/astro-ph?searchtype=author&query=Bertaina%2C+M">M. Bertaina</a>, <a href="/search/astro-ph?searchtype=author&query=Bertone%2C+P+F">P. F. Bertone</a>, <a href="/search/astro-ph?searchtype=author&query=Bianciotto%2C+M">M. Bianciotto</a>, <a href="/search/astro-ph?searchtype=author&query=Bisconti%2C+F">F. Bisconti</a>, <a href="/search/astro-ph?searchtype=author&query=Blaksley%2C+C">C. Blaksley</a>, <a href="/search/astro-ph?searchtype=author&query=Blin-Bondil%2C+S">S. Blin-Bondil</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmgren%2C+K">K. Bolmgren</a>, <a href="/search/astro-ph?searchtype=author&query=Briz%2C+S">S. Briz</a>, <a href="/search/astro-ph?searchtype=author&query=Burton%2C+J">J. Burton</a>, <a href="/search/astro-ph?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a>, <a href="/search/astro-ph?searchtype=author&query=Cambi%C3%A8%2C+G">G. Cambi猫</a> , et al. (133 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.08204v1-abstract-short" style="display: inline;"> This is a collection of papers presented by the JEM-EUSO Collaboration at the 38th International Cosmic Ray Conference (Nagoya, Japan, July 26-August 3, 2023) </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.08204v1-abstract-full" style="display: none;"> This is a collection of papers presented by the JEM-EUSO Collaboration at the 38th International Cosmic Ray Conference (Nagoya, Japan, July 26-August 3, 2023) <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.08204v1-abstract-full').style.display = 'none'; document.getElementById('2312.08204v1-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 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.05362">arXiv:2312.05362</a> <span> [<a href="https://arxiv.org/pdf/2312.05362">pdf</a>, <a href="https://arxiv.org/format/2312.05362">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="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/ad3730">10.3847/1538-4357/ad3730 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> All-Sky Search for Transient Astrophysical Neutrino Emission with 10 Years of IceCube Cascade Events </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (382 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.05362v2-abstract-short" style="display: inline;"> We present the results of a time-dependent search for neutrino flares in data collected by IceCube between May 2011 and 2021. This data set contains cascade-like events originating from charged-current electron neutrino and tau neutrino interactions and all-flavor neutral-current interactions. IceCube's previous all-sky searches for neutrino flares used data sets consisting of track-like events or… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05362v2-abstract-full').style.display = 'inline'; document.getElementById('2312.05362v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.05362v2-abstract-full" style="display: none;"> We present the results of a time-dependent search for neutrino flares in data collected by IceCube between May 2011 and 2021. This data set contains cascade-like events originating from charged-current electron neutrino and tau neutrino interactions and all-flavor neutral-current interactions. IceCube's previous all-sky searches for neutrino flares used data sets consisting of track-like events originating from charged-current muon neutrino interactions. The cascade data sets are statistically independent of the track data sets and provide a new opportunity to observe the transient all-sky landscape. This search uses the spatial, temporal, and energy information of the cascade-like events to conduct searches for the most statistically significant neutrino flares in the northern and southern skies. No statistically significant time-dependent neutrino emission was observed. For the most statistically significant location in the northern sky, $p_\mathrm{global} =$ 0.71, and in the southern sky, $p_\mathrm{global} =$ 0.51. These results are compatible with the background hypothesis. Assuming an E$^{-2.53}$ spectrum from the diffuse astrophysical neutrino flux as measured with cascades, these results are used to calculate upper limits at the 90\% confidence level on neutrino flares of varying duration and constrain the contribution of these flares to the diffuse astrophysical neutrino flux. These constraints are independent of a specified class of astrophysical objects and show that multiple unresolved transient sources may contribute to the diffuse astrophysical neutrino flux. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.05362v2-abstract-full').style.display = 'none'; document.getElementById('2312.05362v2-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to The Astrophysical Journal</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.13754">arXiv:2311.13754</a> <span> [<a href="https://arxiv.org/pdf/2311.13754">pdf</a>, <a href="https://arxiv.org/format/2311.13754">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> JWST's PEARLS: Improved Flux Calibration for NIRCam </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ma%2C+Z">Zhiyuan Ma</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+H">Haojing Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Sun%2C+B">Bangzheng Sun</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">Rolf A. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Summers%2C+J">Jake Summers</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">Rogier A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Silva%2C+J+C+J">Jordan C. J. D'Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+M+A">Madeline A. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">Mario Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+R">Rafael Ortiz III</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A">Aaron Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C%2C+R+E">Russell E. Ryan, Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Willmer%2C+C+N+A">Christopher N. A. Willmer</a>, <a href="/search/astro-ph?searchtype=author&query=Hammel%2C+H+B">Heidi B. Hammel</a>, <a href="/search/astro-ph?searchtype=author&query=Milam%2C+S+N">Stefanie N. Milam</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+C">Cheng Cheng</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.13754v2-abstract-short" style="display: inline;"> The Prime Extragalactic Areas for Reionization and Lensing Science (PEARLS), a JWST GTO program, obtained a set of unique NIRCam observations that have enabled us to significantly improve the default photometric calibration across both NIRCam modules. The observations consisted of three epochs of 4-band (F150W, F200W, F356W, and F444W) NIRCam imaging in the Spitzer IRAC Dark Field (IDF). The three… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13754v2-abstract-full').style.display = 'inline'; document.getElementById('2311.13754v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.13754v2-abstract-full" style="display: none;"> The Prime Extragalactic Areas for Reionization and Lensing Science (PEARLS), a JWST GTO program, obtained a set of unique NIRCam observations that have enabled us to significantly improve the default photometric calibration across both NIRCam modules. The observations consisted of three epochs of 4-band (F150W, F200W, F356W, and F444W) NIRCam imaging in the Spitzer IRAC Dark Field (IDF). The three epochs were six months apart and spanned the full duration of Cycle 1. As the IDF is in the JWST continuous viewing zone, we were able to design the observations such that the two modules of NIRCam, modules A and B, were flipped by 180 degrees and completely overlapped each other's footprints in alternate epochs. We were therefore able to directly compare the photometry of the same objects observed with different modules and detectors, and we found significant photometric residuals up to ~ 0.05 mag in some detectors and filters, for the default version of the calibration files that we used (jwst_1039.pmap). Moreover, there are multiplicative gradients present in the data obtained in the two long-wavelength bands. The problem is less severe in the data reduced using the latest pmap (jwst_1130.pmap as of September 2023), but it is still present, and is non-negligible. We provide a recipe to correct for this systematic effect to bring the two modules onto a more consistent calibration, to a photometric precision better than ~ 0.02 mag. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13754v2-abstract-full').style.display = 'none'; document.getElementById('2311.13754v2-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 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 8 figures, 3 tables. Accepted to PASP</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.12656">arXiv:2311.12656</a> <span> [<a href="https://arxiv.org/pdf/2311.12656">pdf</a>, <a href="https://arxiv.org/format/2311.12656">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 Physics - Experiment">hep-ex</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/s10052-023-12090-w">10.1140/epjc/s10052-023-12090-w <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Developments and results in the context of the JEM-EUSO program obtained with the ESAF Simulation and Analysis Framework </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abe%2C+S">S. Abe</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J+H">J. H. Adams Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Allard%2C+D">D. Allard</a>, <a href="/search/astro-ph?searchtype=author&query=Alldredge%2C+P">P. Alldredge</a>, <a href="/search/astro-ph?searchtype=author&query=Anchordoqui%2C+L">L. Anchordoqui</a>, <a href="/search/astro-ph?searchtype=author&query=Anzalone%2C+A">A. Anzalone</a>, <a href="/search/astro-ph?searchtype=author&query=Arnone%2C+E">E. Arnone</a>, <a href="/search/astro-ph?searchtype=author&query=Baret%2C+B">B. Baret</a>, <a href="/search/astro-ph?searchtype=author&query=Barghini%2C+D">D. Barghini</a>, <a href="/search/astro-ph?searchtype=author&query=Battisti%2C+M">M. Battisti</a>, <a href="/search/astro-ph?searchtype=author&query=Bayer%2C+J">J. Bayer</a>, <a href="/search/astro-ph?searchtype=author&query=Bellotti%2C+R">R. Bellotti</a>, <a href="/search/astro-ph?searchtype=author&query=Belov%2C+A+A">A. A. Belov</a>, <a href="/search/astro-ph?searchtype=author&query=Bertaina%2C+M">M. Bertaina</a>, <a href="/search/astro-ph?searchtype=author&query=Bertone%2C+P+F">P. F. Bertone</a>, <a href="/search/astro-ph?searchtype=author&query=Bianciotto%2C+M">M. Bianciotto</a>, <a href="/search/astro-ph?searchtype=author&query=Biermann%2C+P+L">P. L. Biermann</a>, <a href="/search/astro-ph?searchtype=author&query=Bisconti%2C+F">F. Bisconti</a>, <a href="/search/astro-ph?searchtype=author&query=Blaksley%2C+C">C. Blaksley</a>, <a href="/search/astro-ph?searchtype=author&query=Blin-Bondil%2C+S">S. Blin-Bondil</a>, <a href="/search/astro-ph?searchtype=author&query=Bobik%2C+P">P. Bobik</a>, <a href="/search/astro-ph?searchtype=author&query=Bolmgren%2C+K">K. Bolmgren</a>, <a href="/search/astro-ph?searchtype=author&query=Briz%2C+S">S. Briz</a>, <a href="/search/astro-ph?searchtype=author&query=Burton%2C+J">J. Burton</a>, <a href="/search/astro-ph?searchtype=author&query=Cafagna%2C+F">F. Cafagna</a> , et al. (150 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.12656v1-abstract-short" style="display: inline;"> JEM--EUSO is an international program for the development of space-based Ultra-High Energy Cosmic Ray observatories. The program consists of a series of missions which are either under development or in the data analysis phase. All instruments are based on a wide-field-of-view telescope, which operates in the near-UV range, designed to detect the fluorescence light emitted by extensive air showers… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12656v1-abstract-full').style.display = 'inline'; document.getElementById('2311.12656v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.12656v1-abstract-full" style="display: none;"> JEM--EUSO is an international program for the development of space-based Ultra-High Energy Cosmic Ray observatories. The program consists of a series of missions which are either under development or in the data analysis phase. All instruments are based on a wide-field-of-view telescope, which operates in the near-UV range, designed to detect the fluorescence light emitted by extensive air showers in the atmosphere. We describe the simulation software ESAFin the framework of the JEM--EUSO program and explain the physical assumptions used. We present here the implementation of the JEM--EUSO, POEMMA, K--EUSO, TUS, Mini--EUSO, EUSO--SPB1 and EUSO--TA configurations in ESAF. For the first time ESAF simulation outputs are compared with experimental data. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.12656v1-abstract-full').style.display = 'none'; document.getElementById('2311.12656v1-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 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur. Phys. J. C 83, 1028 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.17409">arXiv:2310.17409</a> <span> [<a href="https://arxiv.org/pdf/2310.17409">pdf</a>, <a href="https://arxiv.org/format/2310.17409">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"> MIGHTEE: multi-wavelength counterparts in the COSMOS field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Whittam%2C+I+H">I. H. Whittam</a>, <a href="/search/astro-ph?searchtype=author&query=Prescott%2C+M">M. Prescott</a>, <a href="/search/astro-ph?searchtype=author&query=Hale%2C+C+L">C. L. Hale</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M+.+J">M . J. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Heywood%2C+I">I. Heywood</a>, <a href="/search/astro-ph?searchtype=author&query=An%2C+F">Fangxia An</a>, <a href="/search/astro-ph?searchtype=author&query=Glowacki%2C+M">M. Glowacki</a>, <a href="/search/astro-ph?searchtype=author&query=Maddox%2C+N">N. Maddox</a>, <a href="/search/astro-ph?searchtype=author&query=Marchetti%2C+L">L. Marchetti</a>, <a href="/search/astro-ph?searchtype=author&query=Morabito%2C+L+K">L. K. Morabito</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">N. J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Bowler%2C+R+A+A">R. A. A. Bowler</a>, <a href="/search/astro-ph?searchtype=author&query=Hatfield%2C+P+W">P. W. Hatfield</a>, <a href="/search/astro-ph?searchtype=author&query=Varadaraj%2C+R+G">R. G. Varadaraj</a>, <a href="/search/astro-ph?searchtype=author&query=Collier%2C+J">J. Collier</a>, <a href="/search/astro-ph?searchtype=author&query=Frank%2C+B">B. Frank</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+A+R">A. R. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Santos%2C+M+G">M. G. Santos</a>, <a href="/search/astro-ph?searchtype=author&query=Vaccari%2C+M">M. Vaccari</a>, <a href="/search/astro-ph?searchtype=author&query=Afonso%2C+J">J. Afonso</a>, <a href="/search/astro-ph?searchtype=author&query=Ao%2C+Y">Y. Ao</a>, <a href="/search/astro-ph?searchtype=author&query=Delhaize%2C+J">J. Delhaize</a>, <a href="/search/astro-ph?searchtype=author&query=Knowles%2C+K">K. Knowles</a>, <a href="/search/astro-ph?searchtype=author&query=Kolwa%2C+S">S. Kolwa</a>, <a href="/search/astro-ph?searchtype=author&query=Randriamampandry%2C+S+M">S. M. Randriamampandry</a> , et al. (4 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.17409v1-abstract-short" style="display: inline;"> In this paper we combine the Early Science radio continuum data from the MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) Survey, with optical and near-infrared data and release the cross-matched catalogues. The radio data used in this work covers $0.86$ deg$^2$ of the COSMOS field, reaches a thermal noise of $1.7$ $渭$Jy/beam and contains $6102$ radio components. We visually in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17409v1-abstract-full').style.display = 'inline'; document.getElementById('2310.17409v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.17409v1-abstract-full" style="display: none;"> In this paper we combine the Early Science radio continuum data from the MeerKAT International GHz Tiered Extragalactic Exploration (MIGHTEE) Survey, with optical and near-infrared data and release the cross-matched catalogues. The radio data used in this work covers $0.86$ deg$^2$ of the COSMOS field, reaches a thermal noise of $1.7$ $渭$Jy/beam and contains $6102$ radio components. We visually inspect and cross-match the radio sample with optical and near-infrared data from the Hyper Suprime-Cam (HSC) and UltraVISTA surveys. This allows the properties of active galactic nuclei and star-forming populations of galaxies to be probed out to $z \approx 5$. Additionally, we use the likelihood ratio method to automatically cross-match the radio and optical catalogues and compare this to the visually cross-matched catalogue. We find that 94 per cent of our radio source catalogue can be matched with this method, with a reliability of $95$ per cent. We proceed to show that visual classification will still remain an essential process for the cross-matching of complex and extended radio sources. In the near future, the MIGHTEE survey will be expanded in area to cover a total of $\sim$20~deg$^2$; thus the combination of automated and visual identification will be critical. We compare redshift distribution of SFG and AGN to the SKADS and T-RECS simulations and find more AGN than predicted at $z \sim 1$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.17409v1-abstract-full').style.display = 'none'; document.getElementById('2310.17409v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 15 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/2309.13008">arXiv:2309.13008</a> <span> [<a href="https://arxiv.org/pdf/2309.13008">pdf</a>, <a href="https://arxiv.org/format/2309.13008">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"> PEARLS: JWST counterparts of micro-Jy radio sources in the Time Domain Field </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Willner%2C+S+P">S. P. Willner</a>, <a href="/search/astro-ph?searchtype=author&query=Gim%2C+H+B">H. B. Gim</a>, <a href="/search/astro-ph?searchtype=author&query=Polletta%2C+M+d+C">M. del Carmen Polletta</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">S. H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Willmer%2C+C+N+A">C. N. A. Willmer</a>, <a href="/search/astro-ph?searchtype=author&query=Zhao%2C+X">X. Zhao</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Silva%2C+J+C+J">J. C. J. D'Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">R. A. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">A. M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Summers%2C+J">J. Summers</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">R. A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">D. Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">S. P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">B. Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">N. A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+M+A">M. A. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Nonino%2C+M">M. Nonino</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+R">R. Ortiz III</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">N. Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A">A. Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=Rutkowski%2C+M+J">M. J. Rutkowski</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C%2C+R+E">R. E. Ryan, Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Tompkins%2C+S">S. Tompkins</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+H">H. Yan</a> , et al. (16 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.13008v2-abstract-short" style="display: inline;"> The Time Domain Field (TDF) near the North Ecliptic Pole in JWST's continuous-viewing zone will become a premier "blank field" for extragalactic science. JWST/NIRCam data in a 16 arcmin$^2$ portion of the TDF identify 4.4 $渭$m counterparts for 62 of 63 3 GHz sources with S(3 GHz) > 5 渭Jy. The one unidentified radio source may be a lobe of a nearby Seyfert galaxy, or it may be an infrared-faint rad… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.13008v2-abstract-full').style.display = 'inline'; document.getElementById('2309.13008v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.13008v2-abstract-full" style="display: none;"> The Time Domain Field (TDF) near the North Ecliptic Pole in JWST's continuous-viewing zone will become a premier "blank field" for extragalactic science. JWST/NIRCam data in a 16 arcmin$^2$ portion of the TDF identify 4.4 $渭$m counterparts for 62 of 63 3 GHz sources with S(3 GHz) > 5 渭Jy. The one unidentified radio source may be a lobe of a nearby Seyfert galaxy, or it may be an infrared-faint radio source. The bulk properties of the radio-host galaxies are consistent with those found by previous work: redshifts range from 0.14 to 4.4 with a median redshift of 1.33. The radio emission arises primarily from star formation in $\sim 2/3$ of the sample and from an active galactic nucleus in $\sim 1/3$, but just over half the sample shows evidence for an AGN either in the spectral energy distribution or by radio excess. All but three counterparts are brighter than magnitude 23 AB at 4.4 $渭$m, and the exquisite resolution of JWST identifies correct counterparts for sources for which observations with lower angular resolution would mis-identify a nearby bright source as the counterpart when the correct one is faint and red. Up to 11% of counterparts might have been unidentified or misidentified absent NIRCam observations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.13008v2-abstract-full').style.display = 'none'; document.getElementById('2309.13008v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ. V2 adds an author and some acknowledgments inadvertently omitted</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.12130">arXiv:2309.12130</a> <span> [<a href="https://arxiv.org/pdf/2309.12130">pdf</a>, <a href="https://arxiv.org/format/2309.12130">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/10.3847/1538-4357/ad18d6">10.3847/1538-4357/ad18d6 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Continuous and Transient Neutrino Emission Associated with IceCube's Highest-Energy Tracks: An 11-Year Analysis </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Ausborm%2C+L">L. Ausborm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (385 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.12130v2-abstract-short" style="display: inline;"> IceCube alert events are neutrinos with a moderate-to-high probability of having astrophysical origin. In this study, we analyze 11 years of IceCube data and investigate 122 alert events and a selection of high-energy tracks detected between 2009 and the end of 2021. This high-energy event selection (alert events + high-energy tracks) has an average probability of $\geq 0.5$ to be of astrophysical… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12130v2-abstract-full').style.display = 'inline'; document.getElementById('2309.12130v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.12130v2-abstract-full" style="display: none;"> IceCube alert events are neutrinos with a moderate-to-high probability of having astrophysical origin. In this study, we analyze 11 years of IceCube data and investigate 122 alert events and a selection of high-energy tracks detected between 2009 and the end of 2021. This high-energy event selection (alert events + high-energy tracks) has an average probability of $\geq 0.5$ to be of astrophysical origin. We search for additional continuous and transient neutrino emission within the high-energy events' error regions. We find no evidence for significant continuous neutrino emission from any of the alert event directions. The only locally significant neutrino emission is the transient emission associated with the blazar TXS~0506+056, with a local significance of $ 3 蟽$, which confirms previous IceCube studies. When correcting for 122 test positions, the global p-value is $0.156$ and is compatible with the background hypothesis. We constrain the total continuous flux emitted from all 122 test positions at 100~TeV to be below $1.2 \times 10^{-15}$~(TeV cm$^2$ s)$^{-1}$ at 90% confidence assuming an $E^{-2}$ spectrum. This corresponds to 4.5% of IceCube's astrophysical diffuse flux. Overall, we find no indication that alert events, in general, are linked to lower-energetic continuous or transient neutrino emission. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.12130v2-abstract-full').style.display = 'none'; document.getElementById('2309.12130v2-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 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 21 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted by ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2024 ApJ 964 40 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.10038">arXiv:2309.10038</a> <span> [<a href="https://arxiv.org/pdf/2309.10038">pdf</a>, <a href="https://arxiv.org/format/2309.10038">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/10.1093/mnras/stae921">10.1093/mnras/stae921 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A JWST investigation into the bar fraction at redshifts 1 < z < 3 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Conte%2C+Z+A+L">Zoe A. Le Conte</a>, <a href="/search/astro-ph?searchtype=author&query=Gadotti%2C+D+A">Dimitri A. Gadotti</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+L">Leonardo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=de+S%C3%A1-Freitas%2C+C">Camila de S谩-Freitas</a>, <a href="/search/astro-ph?searchtype=author&query=Kim%2C+T">Taehyun Kim</a>, <a href="/search/astro-ph?searchtype=author&query=Neumann%2C+J">Justus Neumann</a>, <a href="/search/astro-ph?searchtype=author&query=Fragkoudi%2C+F">Francesca Fragkoudi</a>, <a href="/search/astro-ph?searchtype=author&query=Athanassoula%2C+E">E. Athanassoula</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.10038v3-abstract-short" style="display: inline;"> The presence of a stellar bar in a disc galaxy indicates that the galaxy hosts in its main part a dynamically settled disc and that bar-driven processes are taking place in shaping its evolution. Studying the cosmic evolution of the bar fraction in disc galaxies is therefore essential to understand galaxy evolution in general. Previous studies have found, using the Hubble Space Telescope (HST), th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.10038v3-abstract-full').style.display = 'inline'; document.getElementById('2309.10038v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.10038v3-abstract-full" style="display: none;"> The presence of a stellar bar in a disc galaxy indicates that the galaxy hosts in its main part a dynamically settled disc and that bar-driven processes are taking place in shaping its evolution. Studying the cosmic evolution of the bar fraction in disc galaxies is therefore essential to understand galaxy evolution in general. Previous studies have found, using the Hubble Space Telescope (HST), that the bar fraction significantly declines from the local Universe to redshifts near one. Using the first four pointings from the James Webb Space Telescope (JWST) Cosmic Evolution Early Release Science Survey (CEERS) and the initial public observations for the Public Release Imaging for Extragalactic Research (PRIMER), we extend the studies of the bar fraction in disc galaxies to redshifts $1 \leq z \leq 3$, i.e., for the first time beyond redshift two. We only use galaxies that are also present in the Cosmic Assembly Near-IR Deep Extragalactic Legacy Survey (CANDELS) on the Extended Groth Strip (EGS) and Ultra Deep Survey (UDS) HST observations. An optimised sample of 368 close-to-face-on galaxies is visually classified to find the fraction of bars in disc galaxies in two redshift bins: $1 \leq z \leq 2$ and $2 < z \leq 3$. The bar fraction decreases from $\approx 17.8^{+ 5.1}_{- 4.8}$ per cent to $\approx 13.8^{+ 6.5}_{- 5.8}$ per cent (from the lower to the higher redshift bin), but is about twice the bar fraction found using bluer HST filters. Our results show that bar-driven evolution might commence at early cosmic times and that dynamically settled discs are already present at a lookback time of $\sim 11$ Gyrs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.10038v3-abstract-full').style.display = 'none'; document.getElementById('2309.10038v3-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 18 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in MNRAS; 18 pages, 10 figures; final version includes new disc classification and mass cut, but results remain the same; Figs. 6 and 7 summarise the main results</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.04377">arXiv:2309.04377</a> <span> [<a href="https://arxiv.org/pdf/2309.04377">pdf</a>, <a href="https://arxiv.org/format/2309.04377">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/10.1093/mnras/stad3597">10.1093/mnras/stad3597 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> EPOCHS VI: The Size and Shape Evolution of Galaxies since z ~ 8 with JWST Observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Ormerod%2C+K">K. Ormerod</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">C. J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">N. J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Harvey%2C+T">T. Harvey</a>, <a href="/search/astro-ph?searchtype=author&query=Austin%2C+D">D. Austin</a>, <a href="/search/astro-ph?searchtype=author&query=Trussler%2C+J">J. Trussler</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+L">L. Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Caruana%2C+J">J. Caruana</a>, <a href="/search/astro-ph?searchtype=author&query=Lucatelli%2C+G">G. Lucatelli</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Q. Li</a>, <a href="/search/astro-ph?searchtype=author&query=Roper%2C+W+J">W. J. Roper</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.04377v2-abstract-short" style="display: inline;"> We present the results of a size and structural analysis of 1395 galaxies at $0.5 \leq z \lesssim 8$ with stellar masses $\log \left(M_* / M_{\odot}\right)$ $>$ 9.5 within the JWST Public CEERS field that overlaps with the HST CANDELS EGS observations. We use GALFIT to fit single S茅rsic models to the rest-frame optical profile of our galaxies, which is a mass-selected sample complete to our redshi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.04377v2-abstract-full').style.display = 'inline'; document.getElementById('2309.04377v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.04377v2-abstract-full" style="display: none;"> We present the results of a size and structural analysis of 1395 galaxies at $0.5 \leq z \lesssim 8$ with stellar masses $\log \left(M_* / M_{\odot}\right)$ $>$ 9.5 within the JWST Public CEERS field that overlaps with the HST CANDELS EGS observations. We use GALFIT to fit single S茅rsic models to the rest-frame optical profile of our galaxies, which is a mass-selected sample complete to our redshift and mass limit. Our primary result is that at fixed rest-frame wavelength and stellar mass, galaxies get progressively smaller, evolving as $\sim (1+z)^{-0.71\pm0.19}$ up to $z \sim 8$. We discover that the vast majority of massive galaxies at high redshifts have low S茅rsic indices, thus do not contain steep, concentrated light profiles. Additionally, we explore the evolution of the size-stellar mass relationship, finding a correlation such that more massive systems are larger up to $z \sim 3$. This relationship breaks down at $z > 3$, where we find that galaxies are of similar sizes, regardless of their star formation rates and S茅rsic index, varying little with mass. We show that galaxies are more compact at redder wavelengths, independent of sSFR or stellar mass up to $z \sim 3$. We demonstrate the size evolution of galaxies continues up to $z \sim 8$, showing that the process or causes for this evolution is active at early times. We discuss these results in terms of ideas behind galaxy formation and evolution at early epochs, such as their importance in tracing processes driving size evolution, including minor mergers and AGN activity. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.04377v2-abstract-full').style.display = 'none'; document.getElementById('2309.04377v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to MNRAS</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.11391">arXiv:2308.11391</a> <span> [<a href="https://arxiv.org/pdf/2308.11391">pdf</a>, <a href="https://arxiv.org/format/2308.11391">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/10.1051/0004-6361/202346777">10.1051/0004-6361/202346777 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Probing magnetic fields in the circumgalactic medium using polarization data from MIGHTEE </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=B%C3%B6ckmann%2C+K">K. B枚ckmann</a>, <a href="/search/astro-ph?searchtype=author&query=Br%C3%BCggen%2C+M">M. Br眉ggen</a>, <a href="/search/astro-ph?searchtype=author&query=Heesen%2C+V">V. Heesen</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+A">A. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=O%27Sullivan%2C+S+P">S. P. O'Sullivan</a>, <a href="/search/astro-ph?searchtype=author&query=Heywood%2C+I">I. Heywood</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M">M. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Scaife%2C+A">A. Scaife</a>, <a href="/search/astro-ph?searchtype=author&query=Stil%2C+J">J. Stil</a>, <a href="/search/astro-ph?searchtype=author&query=Taylor%2C+R">R. Taylor</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">N. J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Bowler%2C+R+A+A">R. A. A. Bowler</a>, <a href="/search/astro-ph?searchtype=author&query=Tudorache%2C+M+N">M. N. Tudorache</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="2308.11391v1-abstract-short" style="display: inline;"> The detection and study of magnetic fields surrounding galaxies is important to understand galaxy evolution since magnetic fields are tracers for dynamical processes in the circumgalactic medium (CGM) and can have a significant impact on the evolution of the CGM. The Faraday rotation measure (RM) of the polarized light of background radio sources passing through the magnetized CGM of intervening g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.11391v1-abstract-full').style.display = 'inline'; document.getElementById('2308.11391v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.11391v1-abstract-full" style="display: none;"> The detection and study of magnetic fields surrounding galaxies is important to understand galaxy evolution since magnetic fields are tracers for dynamical processes in the circumgalactic medium (CGM) and can have a significant impact on the evolution of the CGM. The Faraday rotation measure (RM) of the polarized light of background radio sources passing through the magnetized CGM of intervening galaxies can be used as a tracer for the strength and extent of magnetic fields around galaxies. We use rotation measures observed by the MIGHTEE-POL (MeerKAT International GHz Tiered Extragalactic Exploration POLarisation) survey by MeerKAT in the XMM-LSS and COSMOS fields to investigate the RM around foreground star-forming galaxies. We use spectroscopic catalogs of star-forming and blue cloud galaxies to measure the RM of MIGHTEE-POL sources as a function of the impact parameter from the intervening galaxy. We then repeat this procedure using a deeper galaxy catalog with photometric redshifts. For the spectroscopic star-forming sample we find a redshift-corrected |RM| excess of 5.6 +/- 2.3 rad m-2 which corresponds to a 2.5 sigma significance around galaxies with a median redshift of z = 0.46 for impact parameters below 130 kpc only selecting the intervenor with the smallest impact parameter. Making use of a photometric galaxy catalog and taking into account all intervenors with Mg < -13.6 mag, the signal disappears. We find no indication for a correlation between redshift and RM, nor do we find a connection between the total number of intervenors to the total |RM| . We have presented tentative evidence that the CGM of star-forming galaxies is permeated by coherent magnetic fields within the virial radius. We conclude that mostly bright, star-forming galaxies with impact parameters less than 130 kpc significantly contribute to the RM of the background radio source. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.11391v1-abstract-full').style.display = 'none'; document.getElementById('2308.11391v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 8 figures, accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 678, A56 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.13048">arXiv:2307.13048</a> <span>  </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"> The IceCube-Gen2 Collaboration -- Contributions to the 38th International Cosmic Ray Conference (ICRC2023) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=IceCube-Gen2"> IceCube-Gen2</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Audehm%2C+J">J. Audehm</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (432 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.13048v1-abstract-short" style="display: inline;"> IceCube-Gen2 is a planned next-generation neutrino observatory at the South Pole that builds upon the successful design of IceCube. Integrating two complementary detection technologies for neutrinos, optical and radio Cherenkov emission, in combination with a surface array for cosmic ray air shower detection, IceCube-Gen2 will cover a broad neutrino energy range from MeV to EeV. This index of cont… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13048v1-abstract-full').style.display = 'inline'; document.getElementById('2307.13048v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.13048v1-abstract-full" style="display: none;"> IceCube-Gen2 is a planned next-generation neutrino observatory at the South Pole that builds upon the successful design of IceCube. Integrating two complementary detection technologies for neutrinos, optical and radio Cherenkov emission, in combination with a surface array for cosmic ray air shower detection, IceCube-Gen2 will cover a broad neutrino energy range from MeV to EeV. This index of contributions to the 38th International Cosmic Ray Conference in Nagoya, Japan (July 26 - August 3, 2023) describes research and development efforts for IceCube-Gen2. Included are summaries of the design, status, and sensitivity of the IceCube-Gen2 optical, surface, and radio components; performance studies of next-generation optical sensors detecting optical Cherenkov radiation from cosmic ray and neutrino events; reconstruction techniques of radio and optical events in terms of energy, direction, and neutrino flavor; and sensitivity studies of astrophysical neutrino flavors, diffuse neutrino fluxes, and cosmic ray anisotropies. Contributions related to IceCube and the scheduled IceCube Upgrade are available in a separate collection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13048v1-abstract-full').style.display = 'none'; document.getElementById('2307.13048v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To access the list of contributions, please follow the "HTML" link. Links to individual contributions will fill in as authors upload their material</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.13047">arXiv:2307.13047</a> <span>  </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"> The IceCube Collaboration -- Contributions to the 38th International Cosmic Ray Conference (ICRC2023) </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=IceCube"> IceCube</a>, <a href="/search/astro-ph?searchtype=author&query=%3A"> :</a>, <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (382 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.13047v1-abstract-short" style="display: inline;"> The IceCube Observatory at the South Pole has been operating in its full configuration since May 2011 with a duty cycle of about 99%. Its main component consists of a cubic-kilometer array of optical sensors deployed deep in the Glacial ice designed for the detection of high-energy astrophysical neutrinos. A surface array for cosmic ray air shower detection, IceTop, and a denser inner subdetector,… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13047v1-abstract-full').style.display = 'inline'; document.getElementById('2307.13047v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.13047v1-abstract-full" style="display: none;"> The IceCube Observatory at the South Pole has been operating in its full configuration since May 2011 with a duty cycle of about 99%. Its main component consists of a cubic-kilometer array of optical sensors deployed deep in the Glacial ice designed for the detection of high-energy astrophysical neutrinos. A surface array for cosmic ray air shower detection, IceTop, and a denser inner subdetector, DeepCore, significantly enhance the capabilities of the observatory, making it a multipurpose facility. This list of contributions to the 38th International Cosmic Ray Conference in Nagoya, Japan (July 26 - August 3, 2023) summarizes the latest results from IceCube covering a broad set of key questions in physics and astrophysics. The papers in this index are grouped topically to highlight IceCube contributions related to high-energy neutrino and multi-messenger astrophysics, cosmic-ray physics, low-energy neutrino transients such as Galactic supernovae, fundamental physics, detector calibration and event reconstruction, education and public outreach, and research and development for the IceCube Upgrade, a scheduled dense sensor infill complemented by calibration devices. Contributions related to IceCube-Gen2, the future extension of IceCube, are available in a separate collection. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.13047v1-abstract-full').style.display = 'none'; document.getElementById('2307.13047v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To access the list of contributions, please follow the "HTML" link. Links to individual contributions will fill in as authors upload their material</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.07576">arXiv:2307.07576</a> <span> [<a href="https://arxiv.org/pdf/2307.07576">pdf</a>, <a href="https://arxiv.org/format/2307.07576">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="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Physics - Experiment">hep-ex</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acf713">10.3847/1538-4357/acf713 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Search for Extended Sources of Neutrino Emission in the Galactic Plane with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a>, <a href="/search/astro-ph?searchtype=author&query=Benning%2C+C">C. Benning</a> , et al. (383 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.07576v2-abstract-short" style="display: inline;"> The Galactic plane, harboring a diffuse neutrino flux, is a particularly interesting target to study potential cosmic-ray acceleration sites. Recent gamma-ray observations by HAWC and LHAASO have presented evidence for multiple Galactic sources that exhibit a spatially extended morphology and have energy spectra continuing beyond 100 TeV. A fraction of such emission could be produced by interactio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.07576v2-abstract-full').style.display = 'inline'; document.getElementById('2307.07576v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.07576v2-abstract-full" style="display: none;"> The Galactic plane, harboring a diffuse neutrino flux, is a particularly interesting target to study potential cosmic-ray acceleration sites. Recent gamma-ray observations by HAWC and LHAASO have presented evidence for multiple Galactic sources that exhibit a spatially extended morphology and have energy spectra continuing beyond 100 TeV. A fraction of such emission could be produced by interactions of accelerated hadronic cosmic rays, resulting in an excess of high-energy neutrinos clustered near these regions. Using 10 years of IceCube data comprising track-like events that originate from charged-current muon neutrino interactions, we perform a dedicated search for extended neutrino sources in the Galaxy. We find no evidence for time-integrated neutrino emission from the potential extended sources studied in the Galactic plane. The most significant location, at 2.6$蟽$ post-trials, is a 1.7$^\circ$ sized region coincident with the unidentified TeV gamma-ray source 3HWC J1951+266. We provide strong constraints on hadronic emission from several regions in the Galaxy. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.07576v2-abstract-full').style.display = 'none'; document.getElementById('2307.07576v2-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 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 4 figures, 5 tables including an appendix. Accepted for publication in Astrophysical Journal</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 956 20 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2307.04427">arXiv:2307.04427</a> <span> [<a href="https://arxiv.org/pdf/2307.04427">pdf</a>, <a href="https://arxiv.org/format/2307.04427">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="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</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/10.1126/science.adc9818">10.1126/science.adc9818 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of high-energy neutrinos from the Galactic plane </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Ahrens%2C+M">M. Ahrens</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Alves%2C+A+A">A. A. Alves Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anderson%2C+T">T. Anderson</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S">S. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Baur%2C+S">S. Baur</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a> , et al. (364 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2307.04427v1-abstract-short" style="display: inline;"> The origin of high-energy cosmic rays, atomic nuclei that continuously impact Earth's atmosphere, has been a mystery for over a century. Due to deflection in interstellar magnetic fields, cosmic rays from the Milky Way arrive at Earth from random directions. However, near their sources and during propagation, cosmic rays interact with matter and produce high-energy neutrinos. We search for neutrin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.04427v1-abstract-full').style.display = 'inline'; document.getElementById('2307.04427v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2307.04427v1-abstract-full" style="display: none;"> The origin of high-energy cosmic rays, atomic nuclei that continuously impact Earth's atmosphere, has been a mystery for over a century. Due to deflection in interstellar magnetic fields, cosmic rays from the Milky Way arrive at Earth from random directions. However, near their sources and during propagation, cosmic rays interact with matter and produce high-energy neutrinos. We search for neutrino emission using machine learning techniques applied to ten years of data from the IceCube Neutrino Observatory. We identify neutrino emission from the Galactic plane at the 4.5$蟽$ level of significance, by comparing diffuse emission models to a background-only hypothesis. The signal is consistent with modeled diffuse emission from the Galactic plane, but could also arise from a population of unresolved point sources. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2307.04427v1-abstract-full').style.display = 'none'; document.getElementById('2307.04427v1-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted on May 12th, 2022; Accepted on May 4th, 2023</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Science 380, 6652, 1338-1343 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2306.13037">arXiv:2306.13037</a> <span> [<a href="https://arxiv.org/pdf/2306.13037">pdf</a>, <a href="https://arxiv.org/format/2306.13037">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.3847/1538-4357/acffb9">10.3847/1538-4357/acffb9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Magellanic System Stars Identified in SMACS J0723.3-7327 James Webb Space Telescope Early Release Observations Images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Summers%2C+J">Jake Summers</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R+A">Rogier A. Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R+A">Rolf A. Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Carleton%2C+T">Timothy Carleton</a>, <a href="/search/astro-ph?searchtype=author&query=Kamieneski%2C+P+S">Patrick S. Kamieneski</a>, <a href="/search/astro-ph?searchtype=author&query=Holwerda%2C+B+W">Benne W. Holwerda</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Diego%2C+J+M">Jose M. Diego</a>, <a href="/search/astro-ph?searchtype=author&query=Willmer%2C+C+N+A">Christopher N. A. Willmer</a>, <a href="/search/astro-ph?searchtype=author&query=Ortiz%2C+R">Rafael Ortiz III</a>, <a href="/search/astro-ph?searchtype=author&query=Cheng%2C+C">Cheng Cheng</a>, <a href="/search/astro-ph?searchtype=author&query=Pigarelli%2C+A">Alex Pigarelli</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A">Aaron Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Silva%2C+J+C+J">Jordan C. J. D'Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Tompkins%2C+S">Scott Tompkins</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+H">Haojing Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N">Norman Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A">Anton Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+M+A">Madeline A. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a> , et al. (1 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2306.13037v2-abstract-short" style="display: inline;"> We identify 71 distant stars in JWST/NIRCam ERO images of the field of galaxy cluster SMACS J0723.3-7327 (SMACS 0723). Given the relatively small ($\sim$$10^{\circ}$) angular separation between SMACS 0723 and the Large Magellanic Cloud, it is likely that these stars are associated with the LMC outskirts or Leading Arm. This is further bolstered by a spectral energy distribution analysis, which sug… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.13037v2-abstract-full').style.display = 'inline'; document.getElementById('2306.13037v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2306.13037v2-abstract-full" style="display: none;"> We identify 71 distant stars in JWST/NIRCam ERO images of the field of galaxy cluster SMACS J0723.3-7327 (SMACS 0723). Given the relatively small ($\sim$$10^{\circ}$) angular separation between SMACS 0723 and the Large Magellanic Cloud, it is likely that these stars are associated with the LMC outskirts or Leading Arm. This is further bolstered by a spectral energy distribution analysis, which suggests an excess of stars at a physical distance of $40-100$ kpc, consistent with being associated with or located behind the Magellanic system. In particular, we find that the overall surface density of stars brighter than 27.0 mag in the field of SMACS 0723 is $\sim$2.3 times that of stars in a blank field with similar galactic latitude (the North Ecliptic Pole Time Domain Field), and that the density of stars in the SMACS 0723 field with SED-derived distances consistent with the Magellanic system is $\sim$6.1 times larger than that of the blank field. The candidate stars at these distances are consistent with a stellar population at the same distance modulus with [Fe/H] $= -1.0$ and an age of $\sim$$5.0$ Gyr. On the assumption that all of the 71 stars are associated with the LMC, then the stellar density of the LMC at the location of the SMACS 0723 field is $\sim$$740$ stars kpc$^{-3}$, which helps trace the density of stars in the LMC outskirts. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2306.13037v2-abstract-full').style.display = 'none'; document.getElementById('2306.13037v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 June, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in ApJ</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 958 108 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.13721">arXiv:2304.13721</a> <span> [<a href="https://arxiv.org/pdf/2304.13721">pdf</a>, <a href="https://arxiv.org/format/2304.13721">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"> EPOCHS Paper II: The Ultraviolet Luminosity Function from $7.5<z<13.5$ using 180 square arcminutes of deep, blank-fields from the PEARLS Survey and Public JWST data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">Nathan J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Conselice%2C+C+J">Christopher J. Conselice</a>, <a href="/search/astro-ph?searchtype=author&query=Austin%2C+D">Duncan Austin</a>, <a href="/search/astro-ph?searchtype=author&query=Harvey%2C+T">Thomas Harvey</a>, <a href="/search/astro-ph?searchtype=author&query=Ferreira%2C+L">Leonardo Ferreira</a>, <a href="/search/astro-ph?searchtype=author&query=Trussler%2C+J">James Trussler</a>, <a href="/search/astro-ph?searchtype=author&query=Juodzbalis%2C+I">Ignas Juodzbalis</a>, <a href="/search/astro-ph?searchtype=author&query=Li%2C+Q">Qiong Li</a>, <a href="/search/astro-ph?searchtype=author&query=Windhorst%2C+R">Rogier Windhorst</a>, <a href="/search/astro-ph?searchtype=author&query=Cohen%2C+S+H">Seth H. Cohen</a>, <a href="/search/astro-ph?searchtype=author&query=Jansen%2C+R">Rolf Jansen</a>, <a href="/search/astro-ph?searchtype=author&query=Summers%2C+J">Jake Summers</a>, <a href="/search/astro-ph?searchtype=author&query=Tompkins%2C+S">Scott Tompkins</a>, <a href="/search/astro-ph?searchtype=author&query=Driver%2C+S+P">Simon P. Driver</a>, <a href="/search/astro-ph?searchtype=author&query=Robotham%2C+A">Aaron Robotham</a>, <a href="/search/astro-ph?searchtype=author&query=D%27Silva%2C+J+C+J">Jordan C. J. D'Silva</a>, <a href="/search/astro-ph?searchtype=author&query=Yan%2C+H">Haojing Yan</a>, <a href="/search/astro-ph?searchtype=author&query=Coe%2C+D">Dan Coe</a>, <a href="/search/astro-ph?searchtype=author&query=Frye%2C+B">Brenda Frye</a>, <a href="/search/astro-ph?searchtype=author&query=Grogin%2C+N+A">Norman A. Grogin</a>, <a href="/search/astro-ph?searchtype=author&query=Koekemoer%2C+A+M">Anton M. Koekemoer</a>, <a href="/search/astro-ph?searchtype=author&query=Marshall%2C+M+A">Madeline A. Marshall</a>, <a href="/search/astro-ph?searchtype=author&query=Pirzkal%2C+N">Nor Pirzkal</a>, <a href="/search/astro-ph?searchtype=author&query=Ryan%2C%2C+R+E">Russell E. Ryan, Jr.</a>, <a href="/search/astro-ph?searchtype=author&query=Maksym%2C+W+P">W. Peter Maksym</a> , et al. (12 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.13721v3-abstract-short" style="display: inline;"> We present an analysis of the ultraviolet luminosity function (UV LF) and star formation rate density of distant galaxies ($7.5 < z < 13.5$) in the `blank' fields of the Prime Extragalactic Areas for Reionization Science (PEARLS) survey combined with Early Release Science (ERS) data from the CEERS, GLASS, NGDEEP surveys/fields and the first data release of JADES. We use strict quality cuts on EAZY… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.13721v3-abstract-full').style.display = 'inline'; document.getElementById('2304.13721v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.13721v3-abstract-full" style="display: none;"> We present an analysis of the ultraviolet luminosity function (UV LF) and star formation rate density of distant galaxies ($7.5 < z < 13.5$) in the `blank' fields of the Prime Extragalactic Areas for Reionization Science (PEARLS) survey combined with Early Release Science (ERS) data from the CEERS, GLASS, NGDEEP surveys/fields and the first data release of JADES. We use strict quality cuts on EAZY photometric redshifts to obtain a reliable selection and characterisation of high-redshift ($z>6.5$) galaxies from a consistently processed set of deep, near-infrared imaging. Within an area of 180 arcmin$^{2}$, we identify 1046 candidate galaxies at redshifts $z>6.5$ and we use this sample to study the ultraviolet luminosity function (UV LF) in four redshift bins between $7.5<z<13.5$. The measured number density of galaxies at $z=8$ and $z=9$ match those of past observations undertaken by the {\em Hubble Space Telescope} (HST). Our $z=10.5$ measurements lie between early JWST results and past HST results, indicating cosmic variance may be the cause of previous high density measurements. However, number densities of UV luminous galaxies at $z=12.5$ are high compared to predictions from simulations. When examining the star formation rate density of galaxies at this time period, our observations are still largely consistent with a constant star formation efficiency, are slightly lower than previous early estimations using JWST and support galaxy driven reionization at $z\leq8$. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.13721v3-abstract-full').style.display = 'none'; document.getElementById('2304.13721v3-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 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 26 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">28 Pages, 4 Tables, 10 Figures, V2 updated paper: Accepted in ApJ, analysis now includes completed PEARLS NEP-TDF Field and JADES DR1, updated image calibrations for all fields, more detailed completeness analysis conducted. V3 updated paper: corrected minor issues in acknowledgements section</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.12675">arXiv:2304.12675</a> <span> [<a href="https://arxiv.org/pdf/2304.12675">pdf</a>, <a href="https://arxiv.org/format/2304.12675">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 correlations of high-energy neutrinos detected in IceCube with radio-bright AGN and gamma-ray emission from blazars </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (379 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.12675v1-abstract-short" style="display: inline;"> The IceCube Neutrino Observatory sends realtime neutrino alerts with high probability of being astrophysical in origin. We present a new method to correlate these events and possible candidate sources using $2,089$ blazars from the Fermi-LAT 4LAC-DR2 catalog and with $3,413$ AGNs from the Radio Fundamental Catalog. No statistically significant neutrino emission was found in any of the catalog sear… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.12675v1-abstract-full').style.display = 'inline'; document.getElementById('2304.12675v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.12675v1-abstract-full" style="display: none;"> The IceCube Neutrino Observatory sends realtime neutrino alerts with high probability of being astrophysical in origin. We present a new method to correlate these events and possible candidate sources using $2,089$ blazars from the Fermi-LAT 4LAC-DR2 catalog and with $3,413$ AGNs from the Radio Fundamental Catalog. No statistically significant neutrino emission was found in any of the catalog searches. The result is compatible with a small fraction, $<1$%, of AGNs being neutrino emitters and prior evidence for neutrino emission presented by IceCube and other authors from sources such as TXS 0506+056 and PKS 1502+06. We also present cross-checks to other analyses that claim a significant correlation using similar data samples, and we find that adding more information on the neutrino events and more data overall makes the result compatible with background. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.12675v1-abstract-full').style.display = 'none'; document.getElementById('2304.12675v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2304.02494">arXiv:2304.02494</a> <span> [<a href="https://arxiv.org/pdf/2304.02494">pdf</a>, <a href="https://arxiv.org/format/2304.02494">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/10.1093/mnras/stad2081">10.1093/mnras/stad2081 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The bright end of the galaxy luminosity function at $z \simeq 7$ from the VISTA VIDEO survey </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Varadaraj%2C+R+G">R. G. Varadaraj</a>, <a href="/search/astro-ph?searchtype=author&query=Bowler%2C+R+A+A">R. A. A. Bowler</a>, <a href="/search/astro-ph?searchtype=author&query=Jarvis%2C+M+J">M. J. Jarvis</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+N+J">N. J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=H%C3%A4u%C3%9Fler%2C+B">B. H盲u脽ler</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="2304.02494v2-abstract-short" style="display: inline;"> We have conducted a search for $z\simeq7$ Lyman break galaxies over 8.2 square degrees of near-infrared imaging from the VISTA Deep Extragalactic Observations (VIDEO) survey in the XMM-Newton - Large Scale Structure (XMM-LSS) and the Extended Chandra Deep Field South (ECDF-S) fields. Candidate galaxies were selected from a full photometric redshift analysis down to a $Y+J$ depth of 25.3 ($5蟽$), ut… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02494v2-abstract-full').style.display = 'inline'; document.getElementById('2304.02494v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.02494v2-abstract-full" style="display: none;"> We have conducted a search for $z\simeq7$ Lyman break galaxies over 8.2 square degrees of near-infrared imaging from the VISTA Deep Extragalactic Observations (VIDEO) survey in the XMM-Newton - Large Scale Structure (XMM-LSS) and the Extended Chandra Deep Field South (ECDF-S) fields. Candidate galaxies were selected from a full photometric redshift analysis down to a $Y+J$ depth of 25.3 ($5蟽$), utilizing deep auxiliary optical and Spitzer/IRAC data to remove brown dwarf and red interloper galaxy contaminants. Our final sample consists of 28 candidate galaxies at $6.5\le z \le7.5$ with $-23.5 \le M_{\mathrm{UV}} \le -21.6$. We derive stellar masses of $9.1 \le \mathrm{log}_{10}(M/M_{\odot}) \le 10.9$ for the sample, suggesting that these candidates represent some of the most massive galaxies known at this epoch. We measure the rest-frame UV luminosity function (LF) at $z\simeq7$, confirming previous findings of a gradual decline in number density at the bright-end ($M_{\mathrm{UV}} < -22$) that is well described by a double-power law (DPL). We show that quasar contamination in this magnitude range is expected to be minimal, in contrast to conclusions from recent pure-parallel Hubble studies. Our results are up to a factor of ten lower than previous determinations from optical-only ground-based studies at $M_{\rm UV} \lesssim - 23$. We find that the inclusion of $YJHK_{s}$ photometry is vital for removing brown-dwarf contaminants, and $z \simeq 7$ samples based on red-optical data alone could be highly contaminated ($\gtrsim 50$ per cent). In comparison with other robust $z > 5$ samples, our results further support little evolution in the very bright-end of the rest-frame UV LF from $z = 5-10$, potentially signalling a lack of mass quenching and/or dust obscuration in the most massive galaxies in the first Gyr. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.02494v2-abstract-full').style.display = 'none'; document.getElementById('2304.02494v2-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 July, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 5 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 6 figures, 5 tables (plus additional figures/tables in Appendix). 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/2304.01174">arXiv:2304.01174</a> <span> [<a href="https://arxiv.org/pdf/2304.01174">pdf</a>, <a href="https://arxiv.org/format/2304.01174">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/10.3847/1538-4365/acfa95">10.3847/1538-4365/acfa95 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> IceCat-1: the IceCube Event Catalog of Alert Tracks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (369 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2304.01174v4-abstract-short" style="display: inline;"> We present a catalog of likely astrophysical neutrino track-like events from the IceCube Neutrino Observatory. IceCube began reporting likely astrophysical neutrinos in 2016 and this system was updated in 2019. The catalog presented here includes events that were reported in real-time since 2019, as well as events identified in archival data samples starting from 2011. We report 275 neutrino event… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.01174v4-abstract-full').style.display = 'inline'; document.getElementById('2304.01174v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2304.01174v4-abstract-full" style="display: none;"> We present a catalog of likely astrophysical neutrino track-like events from the IceCube Neutrino Observatory. IceCube began reporting likely astrophysical neutrinos in 2016 and this system was updated in 2019. The catalog presented here includes events that were reported in real-time since 2019, as well as events identified in archival data samples starting from 2011. We report 275 neutrino events from two selection channels as the first entries in the catalog, the IceCube Event Catalog of Alert Tracks, which will see ongoing extensions with additional alerts. The gold and bronze alert channels respectively provide neutrino candidates with 50\% and 30\% probability of being astrophysical, on average assuming an astrophysical neutrino power law energy spectral index of 2.19. For each neutrino alert, we provide the reconstructed energy, direction, false alarm rate, probability of being astrophysical in origin, and likelihood contours describing the spatial uncertainty in the alert's reconstructed location. We also investigate a directional correlation of these neutrino events with gamma-ray and X-ray catalogs including 4FGL, 3HWC, TeVCat and Swift-BAT. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2304.01174v4-abstract-full').style.display = 'none'; document.getElementById('2304.01174v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 April, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 3 April, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> April 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Published in ApJS. Figure 4 and 6 corrected. Online version of the catalog is available on dataverse at https://doi.org/10.7910/DVN/SCRUCD</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> 2023 ApJS 269 25 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.15970">arXiv:2303.15970</a> <span> [<a href="https://arxiv.org/pdf/2303.15970">pdf</a>, <a href="https://arxiv.org/format/2303.15970">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/10.3847/1538-4357/aceefc">10.3847/1538-4357/aceefc <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> A Search for IceCube sub-TeV Neutrinos Correlated with Gravitational-Wave Events Detected By LIGO/Virgo </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (364 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.15970v3-abstract-short" style="display: inline;"> The LIGO/Virgo collaboration published the catalogs GWTC-1, GWTC-2.1 and GWTC-3 containing candidate gravitational-wave (GW) events detected during its runs O1, O2 and O3. These GW events can be possible sites of neutrino emission. In this paper, we present a search for neutrino counterparts of 90 GW candidates using IceCube DeepCore, the low-energy infill array of the IceCube Neutrino Observatory… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15970v3-abstract-full').style.display = 'inline'; document.getElementById('2303.15970v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.15970v3-abstract-full" style="display: none;"> The LIGO/Virgo collaboration published the catalogs GWTC-1, GWTC-2.1 and GWTC-3 containing candidate gravitational-wave (GW) events detected during its runs O1, O2 and O3. These GW events can be possible sites of neutrino emission. In this paper, we present a search for neutrino counterparts of 90 GW candidates using IceCube DeepCore, the low-energy infill array of the IceCube Neutrino Observatory. The search is conducted using an unbinned maximum likelihood method, within a time window of 1000 s and uses the spatial and timing information from the GW events. The neutrinos used for the search have energies ranging from a few GeV to several tens of TeV. We do not find any significant emission of neutrinos, and place upper limits on the flux and the isotropic-equivalent energy emitted in low-energy neutrinos. We also conduct a binomial test to search for source populations potentially contributing to neutrino emission. We report a non-detection of a significant neutrino-source population with this test. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.15970v3-abstract-full').style.display = 'none'; document.getElementById('2303.15970v3-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 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> ApJ 959 (2023) 96 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.13663">arXiv:2303.13663</a> <span> [<a href="https://arxiv.org/pdf/2303.13663">pdf</a>, <a href="https://arxiv.org/format/2303.13663">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="High Energy Physics - Phenomenology">hep-ph</span> </div> </div> <p class="title is-5 mathjax"> Search for neutrino lines from dark matter annihilation and decay with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=The+IceCube+Collaboration"> The IceCube Collaboration</a>, <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a> , et al. (373 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.13663v1-abstract-short" style="display: inline;"> Dark Matter particles in the Galactic Center and halo can annihilate or decay into a pair of neutrinos producing a monochromatic flux of neutrinos. The spectral feature of this signal is unique and it is not expected from any astrophysical production mechanism. Its observation would constitute a dark matter smoking gun signal. We performed the first dedicated search with a neutrino telescope for s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13663v1-abstract-full').style.display = 'inline'; document.getElementById('2303.13663v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.13663v1-abstract-full" style="display: none;"> Dark Matter particles in the Galactic Center and halo can annihilate or decay into a pair of neutrinos producing a monochromatic flux of neutrinos. The spectral feature of this signal is unique and it is not expected from any astrophysical production mechanism. Its observation would constitute a dark matter smoking gun signal. We performed the first dedicated search with a neutrino telescope for such signal, by looking at both the angular and energy information of the neutrino events. To this end, a total of five years of IceCube's DeepCore data has been used to test dark matter masses ranging from 10~GeV to 40~TeV. No significant neutrino excess was found and upper limits on the annihilation cross section, as well as lower limits on the dark matter lifetime, were set. The limits reached are of the order of $10^{-24}$~cm$^3/s$ for an annihilation and up to $10^{27}$ seconds for decaying Dark Matter. Using the same data sample we also derive limits for dark matter annihilation or decay into a pair of Standard Model charged particles. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.13663v1-abstract-full').style.display = 'none'; document.getElementById('2303.13663v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.04682">arXiv:2303.04682</a> <span> [<a href="https://arxiv.org/pdf/2303.04682">pdf</a>, <a href="https://arxiv.org/format/2303.04682">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/10.1140/epjc/s10052-023-11679-5">10.1140/epjc/s10052-023-11679-5 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Observation of Seasonal Variations of the Flux of High-Energy Atmospheric Neutrinos with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (369 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.04682v2-abstract-short" style="display: inline;"> Atmospheric muon neutrinos are produced by meson decays in cosmic-ray-induced air showers. The flux depends on meteorological quantities such as the air temperature, which affects the density of air. Competition between decay and re-interaction of those mesons in the first particle production generations gives rise to a higher neutrino flux when the air density in the stratosphere is lower, corres… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.04682v2-abstract-full').style.display = 'inline'; document.getElementById('2303.04682v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.04682v2-abstract-full" style="display: none;"> Atmospheric muon neutrinos are produced by meson decays in cosmic-ray-induced air showers. The flux depends on meteorological quantities such as the air temperature, which affects the density of air. Competition between decay and re-interaction of those mesons in the first particle production generations gives rise to a higher neutrino flux when the air density in the stratosphere is lower, corresponding to a higher temperature. A measurement of a temperature dependence of the atmospheric $谓_渭$ flux provides a novel method for constraining hadro\-nic interaction models of air showers. It is particularly sensitive to the production of kaons. Studying this temperature dependence for the first time requires a large sample of high-energy neutrinos as well as a detailed understanding of atmospheric properties. We report the significant ($> 10 蟽$) observation of a correlation between the rate of more than 260,000 neutrinos, detected by IceCube between 2012 and 2018, and atmospheric temperatures of the stratosphere, measured by the Atmospheric Infrared Sounder (AIRS) instrument aboard NASA's AQUA satellite. For the observed 10$\%$ seasonal change of effective atmospheric temperature we measure a 3.5(3)$\%$ change in the muon neutrino flux. This observed correlation deviates by about 2-3 standard deviations from the expected correlation of 4.3$\%$ as obtained from theoretical predictions under the assumption of various hadronic interaction models <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.04682v2-abstract-full').style.display = 'none'; document.getElementById('2303.04682v2-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 May, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 8 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Preprint submitted to EPJC</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Eur.Phys.J.C 83 (2023) 9, 777 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2303.03316">arXiv:2303.03316</a> <span> [<a href="https://arxiv.org/pdf/2303.03316">pdf</a>, <a href="https://arxiv.org/format/2303.03316">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/10.3847/2041-8213/acd2c9">10.3847/2041-8213/acd2c9 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Constraining High-Energy Neutrino Emission from Supernovae with IceCube </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/astro-ph?searchtype=author&query=Abbasi%2C+R">R. Abbasi</a>, <a href="/search/astro-ph?searchtype=author&query=Ackermann%2C+M">M. Ackermann</a>, <a href="/search/astro-ph?searchtype=author&query=Adams%2C+J">J. Adams</a>, <a href="/search/astro-ph?searchtype=author&query=Agarwalla%2C+S+K">S. K. Agarwalla</a>, <a href="/search/astro-ph?searchtype=author&query=Aguilar%2C+J+A">J. A. Aguilar</a>, <a href="/search/astro-ph?searchtype=author&query=Ahlers%2C+M">M. Ahlers</a>, <a href="/search/astro-ph?searchtype=author&query=Alameddine%2C+J+M">J. M. Alameddine</a>, <a href="/search/astro-ph?searchtype=author&query=Amin%2C+N+M">N. M. Amin</a>, <a href="/search/astro-ph?searchtype=author&query=Andeen%2C+K">K. Andeen</a>, <a href="/search/astro-ph?searchtype=author&query=Anton%2C+G">G. Anton</a>, <a href="/search/astro-ph?searchtype=author&query=Arg%C3%BCelles%2C+C">C. Arg眉elles</a>, <a href="/search/astro-ph?searchtype=author&query=Ashida%2C+Y">Y. Ashida</a>, <a href="/search/astro-ph?searchtype=author&query=Athanasiadou%2C+S">S. Athanasiadou</a>, <a href="/search/astro-ph?searchtype=author&query=Axani%2C+S+N">S. N. Axani</a>, <a href="/search/astro-ph?searchtype=author&query=Bai%2C+X">X. Bai</a>, <a href="/search/astro-ph?searchtype=author&query=V.%2C+A+B">A. Balagopal V.</a>, <a href="/search/astro-ph?searchtype=author&query=Baricevic%2C+M">M. Baricevic</a>, <a href="/search/astro-ph?searchtype=author&query=Barwick%2C+S+W">S. W. Barwick</a>, <a href="/search/astro-ph?searchtype=author&query=Basu%2C+V">V. Basu</a>, <a href="/search/astro-ph?searchtype=author&query=Bay%2C+R">R. Bay</a>, <a href="/search/astro-ph?searchtype=author&query=Beatty%2C+J+J">J. J. Beatty</a>, <a href="/search/astro-ph?searchtype=author&query=Becker%2C+K+-">K. -H. Becker</a>, <a href="/search/astro-ph?searchtype=author&query=Tjus%2C+J+B">J. Becker Tjus</a>, <a href="/search/astro-ph?searchtype=author&query=Beise%2C+J">J. Beise</a>, <a href="/search/astro-ph?searchtype=author&query=Bellenghi%2C+C">C. Bellenghi</a> , et al. (364 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2303.03316v1-abstract-short" style="display: inline;"> Core-collapse supernovae are a promising potential high-energy neutrino source class. We test for correlation between seven years of IceCube neutrino data and a catalog containing more than 1000 core-collapse supernovae of types IIn and IIP and a sample of stripped-envelope supernovae. We search both for neutrino emission from individual supernovae, and for combined emission from the whole superno… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03316v1-abstract-full').style.display = 'inline'; document.getElementById('2303.03316v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2303.03316v1-abstract-full" style="display: none;"> Core-collapse supernovae are a promising potential high-energy neutrino source class. We test for correlation between seven years of IceCube neutrino data and a catalog containing more than 1000 core-collapse supernovae of types IIn and IIP and a sample of stripped-envelope supernovae. We search both for neutrino emission from individual supernovae, and for combined emission from the whole supernova sample through a stacking analysis. No significant spatial or temporal correlation of neutrinos with the cataloged supernovae was found. The overall deviation of all tested scenarios from the background expectation yields a p-value of 93% which is fully compatible with background. The derived upper limits on the total energy emitted in neutrinos are $1.7\times 10^{48}$ erg for stripped-envelope supernovae, $2.8\times 10^{48}$ erg for type IIP, and $1.3\times 10^{49}$ erg for type IIn SNe, the latter disfavouring models with optimistic assumptions for neutrino production in interacting supernovae. We conclude that strippe-envelope supernovae and supernovae of type IIn do not contribute more than $14.6\%$ and $33.9\%$ respectively to the diffuse neutrino flux in the energy range of about $10^3-10^5$ GeV, assuming that the neutrino energy spectrum follows a power-law with an index of $-2.5$. Under the same assumption, we can only constrain the contribution of type IIP SNe to no more than $59.9\%$. Thus core-collapse supernovae of types IIn and stripped-envelope supernovae can both be ruled out as the dominant source of the diffuse neutrino flux under the given assumptions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2303.03316v1-abstract-full').style.display = 'none'; document.getElementById('2303.03316v1-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 March, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Submitted to ApJ Letters</span> </p> </li> </ol> <nav class="pagination is-small is-centered breathe-horizontal" role="navigation" aria-label="pagination"> <a href="" class="pagination-previous is-invisible">Previous 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