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class='morefewer'>Showing up to 2000 entries per page: <a href=/list/astro-ph/new?skip=0&show=1000 rel="nofollow"> fewer</a> | <span style="color: #454545">more</span> | <span style="color: #454545">all</span> </div> <dl id='articles'> <h3>New submissions (showing 68 of 68 entries)</h3> <dt> <a name='item1'>[1]</a> <a href ="/abs/2503.16483" title="Abstract" id="2503.16483"> arXiv:2503.16483 </a> [<a href="/pdf/2503.16483" title="Download PDF" id="pdf-2503.16483" aria-labelledby="pdf-2503.16483">pdf</a>, <a href="https://arxiv.org/html/2503.16483v1" title="View HTML" id="html-2503.16483" aria-labelledby="html-2503.16483" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16483" title="Other formats" id="oth-2503.16483" aria-labelledby="oth-2503.16483">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Multi-category solar radio burst detection based on task-aligned one-stage object detection model </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wang,+M">Mingming Wang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yuan,+G">Guowu Yuan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=He,+H">Hailan He</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tan,+C">Chengming Tan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wu,+H">Hao Wu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhou,+H">Hao Zhou</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 16 pages, 10 figures (Accepted for publication in Astrophysics and Space Science) </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Instrumentation and Methods for Astrophysics (astro-ph.IM)</span> </div> <p class='mathjax'> Accurate identification of solar radio bursts (SRBs) is essential for advancing research in solar physics and predicting space weather. However, the majority of current studies mainly concentrate on detecting whether SRBs are present or absent, often focusing on only one particular type of burst. Moreover, the neural network models used for SRB detection are typically complex, involving a large number of parameters, which results in slower processing speeds. This study establishes a dataset encompassing Type II, Type III, Type IIIs, Type IV, and Type V SRBs collected from e-CALLISTO, including 8,752 SRB spectrum images and achieving annotations for 10,822 SRBs. We propose a multi-category SRB detection model based on task-aligned one-stage object detection (TOOD). TOOD can solve the problem of inconsistent predictions in classification and localization tasks, and it improves the detection recall rate. This model aligns classification and localization tasks and optimizes the neck network by incorporating a channel attention mechanism. This model achieves higher recall and accuracy with fewer parameters. This model can accurately detect five types of SBRs. The experimental results show that the model achieved an accuracy of 79.9\% (AP50) and a recall rate of 95.1\% on the SBRs dataset. A higher recall rate than other models means fewer SRBs are missed in automatic detection. The model we propose has the potential to make a substantial impact on solar physics research and space weather studies. Additionally, the findings in this paper could provide valuable insights for processing other small-sample astronomical <a href="http://datasets.The" rel="external noopener nofollow" class="link-external link-http">this http URL</a> source code and data is available at <a href="https://github.com/onewangqianqian/MobileNetVitv2-TOOD.git" rel="external noopener nofollow" class="link-external link-https">this https URL</a>. </p> </div> </dd> <dt> <a name='item2'>[2]</a> <a href ="/abs/2503.16495" title="Abstract" id="2503.16495"> arXiv:2503.16495 </a> [<a href="/pdf/2503.16495" title="Download PDF" id="pdf-2503.16495" aria-labelledby="pdf-2503.16495">pdf</a>, <a href="/format/2503.16495" title="Other formats" id="oth-2503.16495" aria-labelledby="oth-2503.16495">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Towards sustainable space research in France </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Santerne,+A">Alexandre Santerne</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Meheut,+H">H茅lo茂se Meheut</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Barret,+D">Didier Barret</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bern%C3%A9,+O">Olivier Bern茅</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Berthier,+E">Etienne Berthier</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ducharne,+A">Agn猫s Ducharne</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kn%C3%B6dlseder,+J">J眉rgen Kn枚dlseder</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Marchaudon,+A">Aur茅lie Marchaudon</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pellarin,+T">Thierry Pellarin</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Spiga,+A">Aymeric Spiga</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wolf,+P">Peter Wolf</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Published as a correspondence to Nature Astronomy. Full-text available at <a href="https://rdcu.be/ecSNp" rel="external noopener nofollow" class="link-external link-https">this https URL</a> </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Instrumentation and Methods for Astrophysics (astro-ph.IM)</span>; Physics and Society (physics.soc-ph) </div> <p class='mathjax'> During the 2024's quinquennial scientific roadmap of CNES, a specific group worked on setting recommendations to decrease the environmental footprint of space science activities. This correspondence to Nature Astronomy highlights the efforts of the french space research to move towards sustainability. It relies on two complementary methods: decarbonisation and frugality. </p> </div> </dd> <dt> <a name='item3'>[3]</a> <a href ="/abs/2503.16595" title="Abstract" id="2503.16595"> arXiv:2503.16595 </a> [<a href="/pdf/2503.16595" title="Download PDF" id="pdf-2503.16595" aria-labelledby="pdf-2503.16595">pdf</a>, <a href="https://arxiv.org/html/2503.16595v1" title="View HTML" id="html-2503.16595" aria-labelledby="html-2503.16595" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16595" title="Other formats" id="oth-2503.16595" aria-labelledby="oth-2503.16595">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> JWST's little red dots: an emerging population of young, low-mass AGN cocooned in dense ionized gas </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rusakov,+V">V. Rusakov</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Watson,+D">D. Watson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Nikopoulos,+G+P">G. P. Nikopoulos</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Brammer,+G">G. Brammer</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gottumukkala,+R">R. Gottumukkala</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Harvey,+T">T. Harvey</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Heintz,+K+E">K. E. Heintz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Nielsen,+R+D">R. D. Nielsen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sim,+S+A">S. A. Sim</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sneppen,+A">A. Sneppen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Vijayan,+A+P">A. P. Vijayan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Adams,+N">N. Adams</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Austin,+D">D. Austin</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Conselice,+C+J">C. J. Conselice</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Goolsby,+C">C.M. Goolsby</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Toft,+S">S. Toft</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 46 pages, 25 figures, 4 tables, submitted to Nature </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> JWST has uncovered large numbers of compact galaxies at high redshift with broad hydrogen/helium lines. These include the enigmatic population known as "little red dots" (LRDs). Their nature is debated, but they are thought to be powered by supermassive black holes (SMBHs) or intense star formation. They exhibit unusual properties for SMBHs, such as black holes that are overmassive for their host galaxies and extremely weak X-ray and radio emission. Using the highest-quality JWST spectra, we show here that the lines are broadened by electron scattering with a narrow intrinsic line core. The data require high electron column densities and compact sizes (light days), which, when coupled with their high luminosities can only be explained by SMBH accretion. The narrow intrinsic cores of the lines imply upper limits on the black hole masses of $10^{5-7}$ $M_{\odot}$, two orders of magnitude lower than previous estimates. These are among the lowest mass SMBHs known at high redshift and suggest that this is a population of young, rapidly growing SMBHs. They are enshrouded in a dense cocoon of ionized gas, probably related to their youth, from which they are accreting close to the Eddington limit. Reprocessed nebular emission from the dense cocoon dominates the optical spectrum, explaining most LRD spectral characteristics and helping to suppress radio and X-ray emission. </p> </div> </dd> <dt> <a name='item4'>[4]</a> <a href ="/abs/2503.16596" title="Abstract" id="2503.16596"> arXiv:2503.16596 </a> [<a href="/pdf/2503.16596" title="Download PDF" id="pdf-2503.16596" aria-labelledby="pdf-2503.16596">pdf</a>, <a href="https://arxiv.org/html/2503.16596v1" title="View HTML" id="html-2503.16596" aria-labelledby="html-2503.16596" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16596" title="Other formats" id="oth-2503.16596" aria-labelledby="oth-2503.16596">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> A "Black Hole Star" Reveals the Remarkable Gas-Enshrouded Hearts of the Little Red Dots </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Naidu,+R+P">Rohan P. Naidu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Matthee,+J">Jorryt Matthee</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Katz,+H">Harley Katz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=de+Graaff,+A">Anna de Graaff</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Oesch,+P">Pascal Oesch</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Smith,+A">Aaron Smith</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Greene,+J+E">Jenny E. Greene</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Brammer,+G">Gabriel Brammer</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Weibel,+A">Andrea Weibel</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hviding,+R">Raphael Hviding</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chisholm,+J">John Chisholm</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Labb%C3%A9,+I">Ivo Labb茅</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Simcoe,+R+A">Robert A. Simcoe</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Witten,+C">Callum Witten</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Atek,+H">Hakim Atek</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Baggen,+J+F+W">Josephine F. W. Baggen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Belli,+S">Sirio Belli</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bezanson,+R">Rachel Bezanson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Boogaard,+L+A">Leindert A. Boogaard</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bose,+S">Sownak Bose</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Covelo-Paz,+A">Alba Covelo-Paz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dayal,+P">Pratika Dayal</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fudamoto,+Y">Yoshinobu Fudamoto</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Furtak,+L+J">Lukas J. Furtak</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Giovinazzo,+E">Emma Giovinazzo</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Goulding,+A">Andy Goulding</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gronke,+M">Max Gronke</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Heintz,+K+E">Kasper E. Heintz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hirschmann,+M">Michaela Hirschmann</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Illingworth,+G">Garth Illingworth</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Inoue,+A+K">Akio K. Inoue</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Johnson,+B+D">Benjamin D. Johnson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Leja,+J">Joel Leja</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Leonova,+E">Ecaterina Leonova</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=McConachie,+I">Ian McConachie</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Maseda,+M+V">Michael V. Maseda</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Natarajan,+P">Priyamvada Natarajan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Nelson,+E">Erica Nelson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Setton,+D+J">David J. Setton</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Shivaei,+I">Irene Shivaei</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sobral,+D">David Sobral</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Stefanon,+M">Mauro Stefanon</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tacchella,+S">Sandro Tacchella</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Toft,+S">Sune Toft</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Torralba,+A">Alberto Torralba</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=van+Dokkum,+P">Pieter van Dokkum</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=van+der+Wel,+A">Arjen van der Wel</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Volonteri,+M">Marta Volonteri</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Walter,+F">Fabian Walter</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wang,+B">Bingjie Wang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Watson,+D">Darach Watson</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Submitted. NIRSpec prism spectra featured in this work from JWST program GO-5224 ("Mirage or Miracle", PIs: Oesch & Naidu) are publicly available at <a href="https://zenodo.org/records/15059215" rel="external noopener nofollow" class="link-external link-https">this https URL</a> . See De Graaff et al. in today's arXiv posting for a z=3.5 BH*. Comments greatly appreciated and warmly welcomed! </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span>; Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR) </div> <p class='mathjax'> The physical processes that led to the formation of billion solar mass black holes within the first 700 million years of cosmic time remain a puzzle. Several theoretical scenarios have been proposed to seed and rapidly grow black holes, but direct observations of these mechanisms remain elusive. Here we present a source 660 million years after the Big Bang that displays singular properties: among the largest Hydrogen Balmer breaks reported at any redshift, broad multi-peaked H$\beta$ emission, and Balmer line absorption in multiple transitions. We model this source as a "black hole star" (BH*) where the Balmer break and absorption features are a result of extremely dense, turbulent gas forming a dust-free "atmosphere" around a supermassive black hole. This source may provide evidence of an early black hole embedded in dense gas -- a theoretical configuration proposed to rapidly grow black holes via super-Eddington accretion. Radiation from the BH* appears to dominate almost all observed light, leaving limited room for contribution from its host galaxy. We demonstrate that the recently discovered "Little Red Dots" (LRDs) with perplexing spectral energy distributions can be explained as BH*s embedded in relatively brighter host galaxies. This source provides evidence that black hole masses in the LRDs may be over-estimated by orders of magnitude -- the BH* is effectively dust-free contrary to the steep dust corrections applied while modeling LRDs, and the physics that gives rise to the complex line shapes and luminosities may deviate from assumptions underlying standard scaling relations. </p> </div> </dd> <dt> <a name='item5'>[5]</a> <a href ="/abs/2503.16600" title="Abstract" id="2503.16600"> arXiv:2503.16600 </a> [<a href="/pdf/2503.16600" title="Download PDF" id="pdf-2503.16600" aria-labelledby="pdf-2503.16600">pdf</a>, <a href="https://arxiv.org/html/2503.16600v1" title="View HTML" id="html-2503.16600" aria-labelledby="html-2503.16600" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16600" title="Other formats" id="oth-2503.16600" aria-labelledby="oth-2503.16600">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> A remarkable Ruby: Absorption in dense gas, rather than evolved stars, drives the extreme Balmer break of a Little Red Dot at $z=3.5$ </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=de+Graaff,+A">Anna de Graaff</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rix,+H">Hans-Walter Rix</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Naidu,+R+P">Rohan P. Naidu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Labbe,+I">Ivo Labbe</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wang,+B">Bingjie Wang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Leja,+J">Joel Leja</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Matthee,+J">Jorryt Matthee</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Katz,+H">Harley Katz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Greene,+J+E">Jenny E. Greene</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hviding,+R+E">Raphael E. Hviding</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Baggen,+J">Josephine Baggen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bezanson,+R">Rachel Bezanson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Boogaard,+L+A">Leindert A. Boogaard</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Brammer,+G">Gabriel Brammer</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dayal,+P">Pratika Dayal</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=van+Dokkum,+P">Pieter van Dokkum</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Goulding,+A+D">Andy D. Goulding</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hirschmann,+M">Michaela Hirschmann</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Maseda,+M+V">Michael V. Maseda</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=McConachie,+I">Ian McConachie</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Miller,+T+B">Tim B. Miller</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Nelson,+E">Erica Nelson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Oesch,+P+A">Pascal A. Oesch</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Setton,+D+J">David J. Setton</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Shivaei,+I">Irene Shivaei</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Weibel,+A">Andrea Weibel</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Whitaker,+K+E">Katherine E. Whitaker</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Williams,+C+C">Christina C. Williams</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 19 pages, 9 figures; submitted to A&A. See Naidu et al. for a z=8 Balmer Cliff! </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> The origin of the rest-optical emission of compact, red, high-redshift sources known as `little red dots' (LRDs) poses a major puzzle. If interpreted as starlight, it would imply that LRDs would constitute the densest stellar systems in the Universe. However, alternative models suggest active galactic nuclei (AGN) may instead power the rest-optical continuum. Here, we present JWST/NIRSpec, NIRCam and MIRI observations from the RUBIES and PRIMER programs of The Cliff: a bright LRD at $z=3.55$ with an exceptional Balmer break, twice as strong as that of any high-redshift source previously observed. The spectra also reveal broad Hydrogen (H$\alpha\ \rm FWHM\sim1500$km/s) and He I emission, but no significant metal lines. We demonstrate that massive evolved stellar populations cannot explain the observed spectrum, even when considering unusually steep and strong dust attenuation, or reasonable variations in the initial mass function. Moreover, the formally best-fit stellar mass and compact size ($M_*\sim10^{10.5}\,M_\odot,\ r_{e}\sim40\,$pc) would imply densities at which near-monthly stellar collisions might lead to significant X-ray emission. We argue that the Balmer break, emission lines, and H$\alpha$ absorption line are instead most plausibly explained by a `black hole star' (BH*) scenario, in which dense gas surrounds a powerful ionising source. In contrast to recently proposed BH* models of dust-reddened AGN, we show that spectral fits in the rest UV to near-infrared favour an intrinsically redder continuum over strong dust reddening. This may point to a super-Eddington accreting massive black hole or, possibly, the presence of (super)massive stars in a nuclear star cluster. The Cliff is the clearest evidence to date that at least some LRDs are not ultra-dense, massive galaxies, and are instead powered by a central ionising source embedded in dense, absorbing gas. </p> </div> </dd> <dt> <a name='item6'>[6]</a> <a href ="/abs/2503.16605" title="Abstract" id="2503.16605"> arXiv:2503.16605 </a> [<a href="/pdf/2503.16605" title="Download PDF" id="pdf-2503.16605" aria-labelledby="pdf-2503.16605">pdf</a>, <a href="https://arxiv.org/html/2503.16605v1" title="View HTML" id="html-2503.16605" aria-labelledby="html-2503.16605" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16605" title="Other formats" id="oth-2503.16605" aria-labelledby="oth-2503.16605">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> A Multi-line Analysis of the Distribution and Excitation of CS and H$_2$CS in the HD 163296 Disk </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Law,+C+J">Charles J. Law</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gal,+R+L">Romane Le Gal</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yamato,+Y">Yoshihide Yamato</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhang,+K">Ke Zhang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Guzm%C3%A1n,+V+V">Viviana V. Guzm谩n</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez-Vera,+C">Claudio Hern谩ndez-Vera</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cleeves,+L+I">L. Ilsedore Cleeves</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Guidi,+G">Greta Guidi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Booth,+A+S">Alice S. Booth</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 22 pages, 13 figures, accepted for publication in ApJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Earth and Planetary Astrophysics (astro-ph.EP)</span>; Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR) </div> <p class='mathjax'> The abundance and distribution of sulfur-bearing molecules in protoplanetary disks directly influences the composition and potential habitability of nascent planets in addition to providing powerful probes of the physical gas conditions in the disks themselves. Here, we present new and archival ALMA and SMA observations of CS and H$_2$CS, and their C$^{34}$S and H$_2$C$^{34}$S isotopologues, at high-angular resolution (${\approx}$0."2-0."4; 20-40 au) in the HD 163296 disk, which reveal a central cavity and multi-ringed emission structure. These observations comprise the most comprehensive, multi-line CS data in a planet-forming disk to date, spanning a wide range of excitation conditions from E$_{\rm{u}}$=7.1 K to 129.3 K, and include new detections of C$^{34}$S, H$_2$CS, and H$_2$C$^{34}$S in this system. Using these data, we derive spatially-resolved rotational temperature and column density profiles for all species. We find a column density ratio N(H$_2$CS)/N(CS) $\approx$ 0.5, which is comparable to that of the similar MWC 480 disk and suggests that organic sulfur compounds may constitute a large fraction of the volatile sulfur reservoir in disks around Herbig stars generally. We derive $^{32}$S/$^{34}$S ratios of ${\approx}$5 (CS/C$^{34}$S) and ${\approx}$2 (H$_2$CS/H$_2$C$^{34}$S) based on disk-averaged and spatially-resolved analyses. Both values are consistent across these two pairs of optically-thin molecules and are well-below the expected ISM ratio of ${\approx}$22, suggesting significant sulfur fractionation. We also constrain the CS emitting layer ($z/r\lesssim 0.1$) using the vertical separations of the disk surfaces in the channel maps and based on the known 2D gas structure of the HD 163296 disk combined with our excitation analysis. </p> </div> </dd> <dt> <a name='item7'>[7]</a> <a href ="/abs/2503.16606" title="Abstract" id="2503.16606"> arXiv:2503.16606 </a> [<a href="/pdf/2503.16606" title="Download PDF" id="pdf-2503.16606" aria-labelledby="pdf-2503.16606">pdf</a>, <a href="https://arxiv.org/html/2503.16606v1" title="View HTML" id="html-2503.16606" aria-labelledby="html-2503.16606" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16606" title="Other formats" id="oth-2503.16606" aria-labelledby="oth-2503.16606">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Looking for the 纬-Ray Cascades of the KM3-230213A Neutrino Source </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Crnogor%C4%8Devi%C4%87,+M">Milena Crnogor膷evi膰</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Blanco,+C">Carlos Blanco</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Linden,+T">Tim Linden</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 14 pages (excl. references), 7 figures. Comments welcome! </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; High Energy Physics - Phenomenology (hep-ph) </div> <p class='mathjax'> The extreme energy of the KM3-230213A event could transform our understanding of the most energetic sources in the Universe. However, it also reveals an inconsistency between the KM3NeT detection and strong IceCube constraints on the ultra-high energy neutrino flux. The most congruous explanation for the KM3NeT and IceCube data requires KM3-230213A to be produced by a (potentially transient) source fortuitously located in a region where the KM3NeT acceptance is maximized. In hadronic models of ultra-high-energy neutrino production, such a source would also produce a bright {\gamma}-ray signal, which would cascade to GeV--TeV energies due to interactions with extragalactic background light. We utilize the {\gamma}-Cascade package to model the spectrum, spatial extension, and time-delay of such a source, and scan a region surrounding the KM3NeT event to search for a consistent {\gamma}-ray signal. We find no convincing evidence for a comparable \textit{Fermi}-LAT source and place constraints on a combination of the source redshift and the intergalactic magnetic field strength between the source and Earth. </p> </div> </dd> <dt> <a name='item8'>[8]</a> <a href ="/abs/2503.16607" title="Abstract" id="2503.16607"> arXiv:2503.16607 </a> [<a href="/pdf/2503.16607" title="Download PDF" id="pdf-2503.16607" aria-labelledby="pdf-2503.16607">pdf</a>, <a href="https://arxiv.org/html/2503.16607v1" title="View HTML" id="html-2503.16607" aria-labelledby="html-2503.16607" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16607" title="Other formats" id="oth-2503.16607" aria-labelledby="oth-2503.16607">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Predictions for Detecting a Turndown in the Baryonic Tully Fisher Relation </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ruan,+D">Dilys Ruan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Brooks,+A+M">Alyson M. Brooks</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cruz,+A">Akaxia Cruz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Peter,+A+H">Annika H.G. Peter</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Keller,+B">Ben Keller</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Quinn,+T">Thomas Quinn</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wadsley,+J">James Wadsley</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Adams,+E+A">Elizabeth A.K. Adams</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 15 pages, 10 figures, submitted to MNRAS </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> The baryonic Tully Fisher relation (bTFR) provides an empirical connection between baryonic mass and dynamical mass (measured by the maximum rotation velocity) for galaxies. Due to the impact of baryonic feedback in the shallower potential wells of dwarf galaxies, the bTFR is predicted to turn down at low masses from the extrapolated power-law relation at high masses. The low-mass end of the bTFR is poorly constrained due to small samples and difficulty in connecting the galaxy's gas kinematics to its dark matter halo. Simulations can help us understand this connection and interpret observations. We measure the bTFR with 66 dwarf galaxies from the Marvel-ous and Marvelous Massive Dwarfs hydrodynamic simulations. Our sample has M$_\star = 10^6-10^9$ M$_\odot$, and is mostly gas dominated. We compare five velocity methods: V$_\text{out,circ}$ (spatially resolved mass-enclosed), V$_\text{out,mid}$ (spatially resolved midplane gravitational potential), and unresolved HI linewidths at different percentages of the peak flux (W$_\text{10}$, W$_\text{20}$, and W$_\text{50}$). We find an intrinsic turndown in the bTFR for maximum halo speeds $\lesssim 50$ km s$^{-1}$ (or total baryonic mass, M$_\text{bary}\lesssim 10^{8.5}$ M$_\odot$). We find that observing HI in lower-mass galaxies to the conventional surface density limit of 1M$_\odot$pc$^{-2}$ is not enough to detect a turndown in the bTFR; none of the HI velocity methods (spatially resolved or unresolved) recover the turndown, and we find bTFR slopes consistent with observations of higher-mass galaxies. However, we predict that the turndown can be recovered by resolved rotation curves if the HI limit is $\lesssim 0.08$ M$_\odot$ pc$^{-2}$, which is within the sensitivity of current HI surveys like FEASTS and MHONGOOSE. </p> </div> </dd> <dt> <a name='item9'>[9]</a> <a href ="/abs/2503.16608" title="Abstract" id="2503.16608"> arXiv:2503.16608 </a> [<a href="/pdf/2503.16608" title="Download PDF" id="pdf-2503.16608" aria-labelledby="pdf-2503.16608">pdf</a>, <a href="https://arxiv.org/html/2503.16608v1" title="View HTML" id="html-2503.16608" aria-labelledby="html-2503.16608" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16608" title="Other formats" id="oth-2503.16608" aria-labelledby="oth-2503.16608">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Limits on the atmospheric metallicity and aerosols of the sub-Neptune GJ 3090 b from high-resolution CRIRES+ spectroscopy </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Parker,+L+T">Luke T. Parker</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mendon%C3%A7a,+J+M">Jo茫o M. Mendon莽a</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Diamond-Lowe,+H">Hannah Diamond-Lowe</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Birkby,+J+L">Jayne L. Birkby</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Meech,+A">Annabella Meech</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Vaughan,+S+R">Sophia R. Vaughan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Brogi,+M">Matteo Brogi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fisher,+C">Chloe Fisher</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Buchhave,+L+A">Lars A. Buchhave</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bello-Arufe,+A">Aaron Bello-Arufe</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kreidberg,+L">Laura Kreidberg</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dittmann,+J">Jason Dittmann</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 17 pages, 11 figures. Accepted for publication in MNRAS </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Earth and Planetary Astrophysics (astro-ph.EP)</span> </div> <p class='mathjax'> The sub-Neptune planets have no solar system analogues, and their low bulk densities suggest thick atmospheres containing degenerate quantities of volatiles and H/He, surrounding cores of unknown sizes. Measurements of their atmospheric composition can help break these degeneracies, but many previous studies at low spectral resolution have largely been hindered by clouds or hazes, returning muted spectra. Here, we present the first comprehensive study of a short-period sub-Neptune using ground-based, high-resolution spectroscopy, which is sensitive to the cores of spectral lines that can extend above potential high altitude aerosol layers. We observe four CRIRES+ $\textit{K}$-band transits of the warm sub-Neptune GJ 3090 b (T$_{\text{eq}}$ = 693$\pm$18 K) which orbits an M2V host star. Despite the high quality data and sensitivity to CH$_4$, H$_2$O, NH$_3$, and H$_2$S, we detect no molecular species. Injection-recovery tests are consistent with two degenerate scenarios. First, GJ 3090 b may host a highly metal-enriched atmosphere with $>\,$150 Z$_{\odot}$ and mean molecular weight $>\,$7.1 g mol$^{-1}$, representing a volatile dominated envelope with a H/He mass fraction $x_{\text{H/He}} < 33\%$, and an unconstrained aerosol layer. Second, the data are consistent with a high altitude cloud or haze layer at pressures $<\,$3.3$\times$10$^{-5}~$bar, for any metallicity. GJ 3090 b joins the growing evidence to suggest that high metallicity atmospheres and high altitude aerosol layers are common within the warm (500$~<T_{\text{eq}}<~$800 K) sub-Neptune population. We discuss the observational challenges posed by the M-dwarf host star, and suggest observing strategies for transmission spectroscopy of challenging targets around M-dwarfs for existing and ELT instrumentation. </p> </div> </dd> <dt> <a name='item10'>[10]</a> <a href ="/abs/2503.16609" title="Abstract" id="2503.16609"> arXiv:2503.16609 </a> [<a href="/pdf/2503.16609" title="Download PDF" id="pdf-2503.16609" aria-labelledby="pdf-2503.16609">pdf</a>, <a href="https://arxiv.org/html/2503.16609v1" title="View HTML" id="html-2503.16609" aria-labelledby="html-2503.16609" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16609" title="Other formats" id="oth-2503.16609" aria-labelledby="oth-2503.16609">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> First Measurements of Black Hole Accretion and Radio-jet Timescales in a Young Quasar at the Edge of Reionization </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rojas-Ruiz,+S">Sof铆a Rojas-Ruiz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Momjian,+E">Emmanuel Momjian</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Davies,+F+B">Frederick B. Davies</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ba%C3%B1ados,+E">Eduardo Ba帽ados</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Eilers,+A">Anna-Christina Eilers</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bosman,+S+B">Sarah B. Bosman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Vaidya,+B">Bhargav Vaidya</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Carilli,+C">Chris Carilli</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mazzucchelli,+C">Chiara Mazzucchelli</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Connor,+T">Thomas Connor</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Khusanova,+Y">Yana Khusanova</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 20 pages, 9 figures, submitted to ApJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span>; High Energy Astrophysical Phenomena (astro-ph.HE); Space Physics (physics.space-ph) </div> <p class='mathjax'> We present the first study dedicated to measuring the timescales for black hole accretion and jet launch in a quasar at the edge of Reionization, PSO J352.4034-15.3373 at z = 5.832 $\pm$ 0.001. Previous work presented evidence of the strong radio synchrotron emission from the jet affecting the host galaxy dust-dominated continuum emission at $\nu_{\rm rest}=683$ GHz ($\nu_{\rm obs}=100$ GHz), implying a break in the synchrotron spectrum. In this work, we present quasi-simultaneous observations at 1.5\, GHz - 42\,GHz with the Karl G. Jansky Very Large Array (VLA), and derive a frequency break at $\nu^{\rm break}_{\rm rest} = 196.46$ GHz ($\nu^{\rm break}_{\rm obs} = 28.76$ GHz). Modeling these observations, we calculate the jet spectral aging from the cooling of electrons to be $t_{\mathrm{spec}}\sim 580$ yr. From this measurement, we approximate the dynamical age $t_{\mathrm{dyn}}$ to be $\sim2,000$ yr, implying a recent jet ejection. We compare the jet timescale to the quasar's lifetime ($t_{\mathrm{Q}}$) that indicates the duration of the latest black hole accretion event and is derived from the proximity zone size in the rest-UV/optical spectrum. However, a ghostly Damped Ly$\alpha$ (DLA) system affects this measurement yielding an upper limit of $t_{\mathrm{Q}} \lesssim 10^4$ yr, consistent with the jet lifetime and indicative of a young quasar. This suggests that the triggering of a UV-bright quasar phase may occur within comparable timescales as the launch of a relativistic radio jet. Therefore, we may be witnessing an early stage of black hole and jet interactions in a quasar during the first gigayear of the universe. </p> </div> </dd> <dt> <a name='item11'>[11]</a> <a href ="/abs/2503.16627" title="Abstract" id="2503.16627"> arXiv:2503.16627 </a> [<a href="/pdf/2503.16627" title="Download PDF" id="pdf-2503.16627" aria-labelledby="pdf-2503.16627">pdf</a>, <a href="https://arxiv.org/html/2503.16627v1" title="View HTML" id="html-2503.16627" aria-labelledby="html-2503.16627" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16627" title="Other formats" id="oth-2503.16627" aria-labelledby="oth-2503.16627">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> AREPO-IDORT: Implicit Discrete Ordinates Radiation Transport for Radiation Magnetohydrodynamics on an Unstructured Moving Mesh </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ma,+J">Jing-Ze Ma</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pakmor,+R">R眉diger Pakmor</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Justham,+S">Stephen Justham</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=de+Mink,+S+E">Selma E. de Mink</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 33 pages, 20 figures, 1 table. Submitted to A&A. Comments welcome! If interested to use the code and to download the full test problem package, see the description in Zenodo: <a href="https://zenodo.org/records/15032138" rel="external noopener nofollow" class="link-external link-https">this https URL</a> </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Instrumentation and Methods for Astrophysics (astro-ph.IM)</span>; Earth and Planetary Astrophysics (astro-ph.EP); Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR) </div> <p class='mathjax'> Radiation is crucial not only for observing astrophysical objects, but also for transporting energy and momentum. However, accurate on-the-fly radiation transport in astrophysical simulations is challenging and computationally expensive. Here we introduce AREPO-IDORT (Implicit Discrete Ordinates Radiation Transport), a scheme coupled to the explicit magnetohydrodynamic (MHD) solver in the 3D moving-mesh code AREPO. The discrete ordinates scheme means we directly solve for the specific intensities along discrete directions. We solve the time-dependent relativistic radiation transport equation via an implicit Jacobi-like iterative finite-volume solver, which overcomes the small radiation time-steps needed by explicit methods. Compared to commonly-used moment-based methods, e.g. flux-limited diffusion or M1 closure, this scheme has the advantage of correctly capturing the direction of radiation in both optically-thick and thin regions. It is based on the scheme by Jiang 2021 for the adaptive mesh refinement code ATHENA++, but we generalize the scheme to support (1) an unstructured moving-mesh, (2) local time-stepping, and (3) general equations of state. We show various test problems that commonly-used moment-based methods fail to reproduce accurately. To apply the scheme to a real astrophysics problem, we show the first global 3D radiation hydrodynamic simulation of the entire convective envelope of a red supergiant star. (abridged) For this problem, the radiation module only takes less than half of the total computational cost. Our current scheme assumes grey radiation, is first-order accurate in both time and space (abridged). We expect our scheme will enable more accurate multi-scale radiation MHD simulations involving supersonic bulk motions, ranging from planet formation in protoplanetary disks, stars and associated transients, to accretion flows near black holes. </p> </div> </dd> <dt> <a name='item12'>[12]</a> <a href ="/abs/2503.16637" title="Abstract" id="2503.16637"> arXiv:2503.16637 </a> [<a href="/pdf/2503.16637" title="Download PDF" id="pdf-2503.16637" aria-labelledby="pdf-2503.16637">pdf</a>, <a href="https://arxiv.org/html/2503.16637v1" title="View HTML" id="html-2503.16637" aria-labelledby="html-2503.16637" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16637" title="Other formats" id="oth-2503.16637" aria-labelledby="oth-2503.16637">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Euclid: Star clusters in IC 342, NGC 2403, and Holmberg II </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Larsen,+S+S">S. S. Larsen</a> (1), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ferguson,+A+M+N">A. M. N. Ferguson</a> (2), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Howell,+J+M">J. M. Howell</a> (2), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Annibali,+F">F. Annibali</a> (3), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cuillandre,+J">J.-C. Cuillandre</a> (4), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hunt,+L+K">L. K. Hunt</a> (5), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lan%C3%A7on,+A">A. Lan莽on</a> (6), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Saifollahi,+T">T. Saifollahi</a> (6), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Massari,+D">D. Massari</a> (3), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Le,+M+N">M. N. Le</a> (7 and 8), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Aghanim,+N">N. Aghanim</a> (9), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Altieri,+B">B. Altieri</a> (10), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Amara,+A">A. Amara</a> (11), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Andreon,+S">S. Andreon</a> (12), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Auricchio,+N">N. Auricchio</a> (3), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Baccigalupi,+C">C. Baccigalupi</a> (13 and 14 and 15 and 16), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Baldi,+M">M. Baldi</a> (17 and 3 and 18), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Balestra,+A">A. Balestra</a> (19), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bardelli,+S">S. Bardelli</a> (3), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Battaglia,+P">P. Battaglia</a> (3), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Biviano,+A">A. Biviano</a> (14 and 13), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Branchini,+E">E. Branchini</a> (20 and 21 and 12), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Brescia,+M">M. Brescia</a> (22 and 23), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Brinchmann,+J">J. Brinchmann</a> (24 and 25), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Camera,+S">S. Camera</a> (26 and 27 and 28), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Capobianco,+V">V. Capobianco</a> (28), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Carbone,+C">C. Carbone</a> (29), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Carretero,+J">J. Carretero</a> (30 and 31), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Casas,+S">S. Casas</a> (32), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Castellano,+M">M. Castellano</a> (33), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Castignani,+G">G. Castignani</a> (3), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cavuoti,+S">S. Cavuoti</a> (23 and 34), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chambers,+K+C">K. C. Chambers</a> (35), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cimatti,+A">A. Cimatti</a> (36), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Colodro-Conde,+C">C. Colodro-Conde</a> (7), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Congedo,+G">G. Congedo</a> (2), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Conselice,+C+J">C. J. Conselice</a> (37), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Conversi,+L">L. Conversi</a> (38 and 10), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Copin,+Y">Y. Copin</a> (39), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Courbin,+F">F. Courbin</a> (40 and 41), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Courtois,+H+M">H. M. Courtois</a> (42), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cropper,+M">M. Cropper</a> (43), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Da+Silva,+A">A. Da Silva</a> (44 and 45), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Degaudenzi,+H">H. Degaudenzi</a> (46), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=De+Lucia,+G">G. De Lucia</a> (14), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dole,+H">H. Dole</a> (9), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Douspis,+M">M. Douspis</a> (9), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dubath,+F">F. Dubath</a> (46), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dupac,+X">X. Dupac</a> (10), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dusini,+S">S. Dusini</a> (47), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Escoffier,+S">S. Escoffier</a> (48), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fabricius,+M">M. Fabricius</a> (49 and 50), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Farina,+M">M. Farina</a> (51), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Faustini,+F">F. Faustini</a> (33 and 52), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ferriol,+S">S. Ferriol</a> (39), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fotopoulou,+S">S. Fotopoulou</a> (53), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Frailis,+M">M. Frailis</a> (14), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Franceschi,+E">E. Franceschi</a> (3), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Galeotta,+S">S. Galeotta</a> (14), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=George,+K">K. George</a> (50), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gillis,+B">B. Gillis</a> (2), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Giocoli,+C">C. Giocoli</a> (3 and 18), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=G%C3%B3mez-Alvarez,+P">P. G贸mez-Alvarez</a> (54 and 10), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gracia-Carpio,+J">J. Gracia-Carpio</a> (49), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Grazian,+A">A. Grazian</a> (19), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Grupp,+F">F. Grupp</a> (49 and 50), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Haugan,+S+V+H">S. V. H. Haugan</a> (55), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hoekstra,+H">H. Hoekstra</a> (56), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Holmes,+W">W. Holmes</a> (57), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hormuth,+F">F. Hormuth</a> (58), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hornstrup,+A">A. Hornstrup</a> (59 and 60), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Jahnke,+K">K. Jahnke</a> (61), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Jhabvala,+M">M. Jhabvala</a> (62), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Keih%C3%A4nen,+E">E. Keih盲nen</a> (63), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kermiche,+S">S. Kermiche</a> (48), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kiessling,+A">A. Kiessling</a> (57), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kohley,+R">R. Kohley</a> (10), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kubik,+B">B. Kubik</a> (39), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kuijken,+K">K. Kuijken</a> (56), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=K%C3%BCmmel,+M">M. K眉mmel</a> (50), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kunz,+M">M. Kunz</a> (64), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kurki-Suonio,+H">H. Kurki-Suonio</a> (65 and 66), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Brun,+A+M+C+L">A. M. C. Le Brun</a> (67), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ligori,+S">S. Ligori</a> (28), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lilje,+P+B">P. B. Lilje</a> (55), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lindholm,+V">V. Lindholm</a> (65 and 66), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lloro,+I">I. Lloro</a> (68), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Maino,+D">D. Maino</a> (69 and 29 and 70), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Maiorano,+E">E. Maiorano</a> (3), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mansutti,+O">O. Mansutti</a> (14), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Marggraf,+O">O. Marggraf</a> (71), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Markovic,+K">K. Markovic</a> (57), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Martinelli,+M">M. Martinelli</a> (33 and 72), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Martinet,+N">N. Martinet</a> (73), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Marulli,+F">F. Marulli</a> (74 and 3 and 18), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Massey,+R">R. Massey</a> (75), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Medinaceli,+E">E. Medinaceli</a> (3), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mei,+S">S. Mei</a> (76 and 77), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mellier,+Y">Y. Mellier</a> (78 and 79), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Meneghetti,+M">M. Meneghetti</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Submitted to A&A following internal review </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> We examine the star cluster populations in the three nearby galaxies IC 342, NGC 2403, and Holmberg II, observed as part of the Euclid Early Release Observations programme. Our main focus is on old globular clusters (GCs), for which the wide field-of-view and excellent image quality of Euclid offer substantial advantages over previous work. For IC 342 this is the first study of stellar clusters other than its nuclear cluster. After selection based on size and magnitude criteria, followed by visual inspection, we identify 111 old (> 1 Gyr) GC candidates in IC 342, 50 in NGC 2403 (of which 15 were previously known), and 7 in Holmberg II. In addition, a number of younger and/or intermediate-age candidates are identified. The colour distributions of GC candidates in the two larger galaxies show hints of bimodality with peaks at IE-HE = 0.36 and 0.79 (IC 342) and IE-HE = 0.36 and 0.80 (NGC 2403), corresponding to metallicities of [Fe/H]=-1.5 and [Fe/H]=-0.5, similar to those of the metal-poor and metal-rich GC subpopulations in the Milky Way. The luminosity functions of our GC candidates exhibit an excess of relatively faint objects, relative to a canonical, approximately Gaussian GC luminosity function (GCLF). The excess objects may be similar to those previously identified in other galaxies. The specific frequency of classical old GCs in IC 342, as determined based on the brighter half of the GCLF, appears to be unusually low with SN=0.2-0.3. The combined luminosity function of young and intermediate-age clusters in all three galaxies is consistent with a power-law distribution, dN/dL ~ L^(-2.3+/-0.1) and the total numbers of young clusters brighter than M(IE)=-8 in NGC 2403 and Holmberg II are comparable with those found in their Local Group counterparts, that is, M33 and the Small Magellanic Cloud, respectively. </p> </div> </dd> <dt> <a name='item13'>[13]</a> <a href ="/abs/2503.16647" title="Abstract" id="2503.16647"> arXiv:2503.16647 </a> [<a href="/pdf/2503.16647" title="Download PDF" id="pdf-2503.16647" aria-labelledby="pdf-2503.16647">pdf</a>, <a href="https://arxiv.org/html/2503.16647v1" title="View HTML" id="html-2503.16647" aria-labelledby="html-2503.16647" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16647" title="Other formats" id="oth-2503.16647" aria-labelledby="oth-2503.16647">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Unravelling the dynamics of cosmic vortices: Probing a Kelvin-Helmholtz instability in the jet of 3C 84 </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Paraschos,+G+F">G. F. Paraschos</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mpisketzis,+V">V. Mpisketzis</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 8 pages, 2 figures, accepted for publication in A&A </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; Astrophysics of Galaxies (astro-ph.GA) </div> <p class='mathjax'> Understanding the creation of relativistic jets originating from active galactic nuclei, require a thorough understanding of the accompanying plasma instabilities. Our high sensitivity, high resolution, global very long baseline interferometry observations of the jet in the radio galaxy 3C 84 enable us to study its inner morphology, which resembles a thread-like pattern. We find that this pattern can be described by a Kelvin-Helmholtz instability, consisting of four instability modes. Our model favours a jet described by a Mach number of $M_\textrm{j} = 5.0\pm1.7$ and a sound speed of $\alpha_\textrm{j} = 0.14\pm0.06$. With it, we are able to describe the internal structure of 3C 84 and to tentatively connect the origin of the instability to accretion disc activity. </p> </div> </dd> <dt> <a name='item14'>[14]</a> <a href ="/abs/2503.16662" title="Abstract" id="2503.16662"> arXiv:2503.16662 </a> [<a href="/pdf/2503.16662" title="Download PDF" id="pdf-2503.16662" aria-labelledby="pdf-2503.16662">pdf</a>, <a href="https://arxiv.org/html/2503.16662v1" title="View HTML" id="html-2503.16662" aria-labelledby="html-2503.16662" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16662" title="Other formats" id="oth-2503.16662" aria-labelledby="oth-2503.16662">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Integral field spectroscopy of the planetary nebula NGC 3242 and the puzzling nature of its low ionization structures </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Konstantinou,+L">L. Konstantinou</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Akras,+S">S. Akras</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Garcia-Rojas,+J">J. Garcia-Rojas</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bouvis,+K">K. Bouvis</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gon%C3%A7alves,+D">D.R. Gon莽alves</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Monteiro,+H">H. Monteiro</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Boumis,+P">P. Boumis</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mari,+M+B">M. B. Mari</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Aleman,+I">I. Aleman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Monreal-Ibero,+A">A. Monreal-Ibero</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 18 pages, 21 figures. The paper has been accepted for publication in A&A (date of acceptance 19/3/25) </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span>; Astrophysics of Galaxies (astro-ph.GA) </div> <p class='mathjax'> The physico-chemical properties of the planetary nebula (PN) NGC 3242 are investigated in both 1D and 2D, using Integral Field Unit (IFU) data. This PN has a complex morphology with multiple shells and contains a pair of structures with a lower degree of ionization compared to the main nebular components. These structures are known as low ionization structures (LISs), and their origin is still a mystery. With the capabilities provided by IFU spectroscopy, we aim to gain a better understanding of the behavior of nebular properties in the LISs. Data from the Multi Unit Spectroscopic Explorer (MUSE) at the Very Large Telescope (VLT) were used in order to perform a spatially resolved physico-chemical analysis of NGC 3242 both in 2D, through the analysis of emission line maps, and in 1D, simulating long-slit spectroscopy, with pseudo-slits. Through the deeper investigation of MUSE data, we detect new structures perpendicular to the pair of LISs of NGC 3242, which are mainly seen in the light of [S III] and [N II]. In addition, two arc-like structures are revealed. Moreover, an inner jet-like structure is found through its [Fe III] emission. The interaction of the jet with the rim may be related to the formation of knots and blobs. The higher value of Te, is estimated from the [S III] diagnostic lines, followed by Te ([N II]), Te(H I) and finally Te (He I). In all cases, Te is higher at the inner nebular structures. Regarding electron density, ne, is lower at the LISs, while an increase is observed at the nebular rim. Diagnostic diagrams confirm that NGC 3242 is a highly ionized nebula. Moreover, the MUSE data unveiled for the first time in this PN, the atomic line [C I] {\lambda}8727, primarily emitted from the LISs. This finding suggests that these structures may consist of a molecular core surrounded by neutral and ionized gas </p> </div> </dd> <dt> <a name='item15'>[15]</a> <a href ="/abs/2503.16665" title="Abstract" id="2503.16665"> arXiv:2503.16665 </a> [<a href="/pdf/2503.16665" title="Download PDF" id="pdf-2503.16665" aria-labelledby="pdf-2503.16665">pdf</a>, <a href="https://arxiv.org/html/2503.16665v1" title="View HTML" id="html-2503.16665" aria-labelledby="html-2503.16665" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16665" title="Other formats" id="oth-2503.16665" aria-labelledby="oth-2503.16665">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Evolution of Shock Structures and QPOs After Halting BHL Accretion onto Kerr Black Hole </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Donmez,+O">Orhan Donmez</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 29 pages, 7 figures, 3 Tables. Suggestions and comments are welcome </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> One of the mechanisms responsible for disk formation around the black holes is Bondi-Hoyle-Lyttleton (BHL) <a href="http://accretion.The" rel="external noopener nofollow" class="link-external link-http">this http URL</a> fact that BHL accretion can be interrupted by various astrophysical phenomena, such as stellar winds or astrophysical jets, makes it crucial to study the behavior of shock cones formed by BHL accretion around black holes once the accretion process is halted. Investigating the new plasma structures that emerge in these scenarios can provide insights into observational results. In this context, a new plasma structure forming around the Kerr black hole has been numerically modeled as a function of the black hole spin parameter and the asymptotic velocity of BHL accretion. The numerical analysis revealed that high spin (a/M=0.9) and supersonic flow ( M > 1) are necessary conditions for low-frequency quasi-periodic oscillations (LFQPOs) formation. On the other hand, the fundamental mode of the high-frequency quasi-periodic oscillations (HFQPOs) are found to be independent of both the black hole spin and asymptotic velocity and are instead governed by general relativistic effects. Additionally, the study demonstrated that for 3:2 and 2:1 resonance states to form, nonlinear couplings needs to be occurred when the black hole rotates rapidly. These couplings produce harmonic frequencies, providing an explanation for the observed quasi-periodic oscillation (QPO) resonances in black hole binaries. These findings align with precession models and nonlinear resonance models, both of which play a crucial role in QPO generation. Finally, the LFQPOs and HFQPOs obtained from numerical simulations are consistent with the observed QPO frequencies in the microquasars GRS 1915+105 and XTE J1550-564, as well as in the AGN REJ1034+396, which harbors a supermassive black hole at its center. </p> </div> </dd> <dt> <a name='item16'>[16]</a> <a href ="/abs/2503.16675" title="Abstract" id="2503.16675"> arXiv:2503.16675 </a> [<a href="/pdf/2503.16675" title="Download PDF" id="pdf-2503.16675" aria-labelledby="pdf-2503.16675">pdf</a>, <a href="https://arxiv.org/html/2503.16675v1" title="View HTML" id="html-2503.16675" aria-labelledby="html-2503.16675" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16675" title="Other formats" id="oth-2503.16675" aria-labelledby="oth-2503.16675">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> A Formalism for Calibrating the Instrumental Polarization of Radio Interferometric Arrays at Meter Wavelengths using Unpolarized Sky: A Demonstration using the MWA Observations </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kansabanik,+D">Devojyoti Kansabanik</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Vourlidas,+A">Angelos Vourlidas</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dey,+S">Soham Dey</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mondal,+S">Surajit Mondal</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Oberoi,+D">Divya Oberoi</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 16 pages, 7 figures, 1 table. Accepted for Publication in The Astrophysical Journal Supplement Series </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Instrumentation and Methods for Astrophysics (astro-ph.IM)</span> </div> <p class='mathjax'> Calibration of instrumental polarization is critical for measuring polarized radio emissions from astrophysical sources to extract the magnetic field information in astrophysical, heliospheric, and terrestrial plasmas. At meter wavelengths, calibration of radio polarimetric observations is particularly challenging because of the scarcity of bright polarized sources due to significant Faraday depolarization. Here, we present a novel formalism for polarization calibration using an unpolarized sky model. The formalism is specifically designed for wide-field, low-frequency instruments like the Murchison Widefield Array (MWA), the LOw Frequency ARray (LOFAR), New Extension in Nan莽ay Upgrading LoFAR (NenuFAR), Owens Valley Radio Observatory - Long Wavelength Array (OVRO-LWA), low-frequency telescope of the Square Kilometre Array Observatory (SKAO-low), etc. By leveraging the apparent polarization of the unpolarized sky induced by the polarized primary beam of the radio telescope, this method avoids dependence on bright polarized calibrators. It is also immune to ionospheric Faraday rotation. The validation of the approach via MWA observations confirms the accuracy of the method. This formalism provides a robust framework for low-frequency polarization calibration. It addresses the longstanding calibration challenges and advances the field of low-frequency polarimetry by enabling polarization studies of astrophysical radio sources. </p> </div> </dd> <dt> <a name='item17'>[17]</a> <a href ="/abs/2503.16680" title="Abstract" id="2503.16680"> arXiv:2503.16680 </a> [<a href="/pdf/2503.16680" title="Download PDF" id="pdf-2503.16680" aria-labelledby="pdf-2503.16680">pdf</a>, <a href="https://arxiv.org/html/2503.16680v1" title="View HTML" id="html-2503.16680" aria-labelledby="html-2503.16680" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16680" title="Other formats" id="oth-2503.16680" aria-labelledby="oth-2503.16680">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Catalog-based detection of unrecognized blends in deep optical ground based catalogs </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Liang,+S">Shuang Liang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Adari,+P">Prakruth Adari</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=von+der+Linden,+A">Anja von der Linden</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 22 pages, 17 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span> </div> <p class='mathjax'> In deep, ground-based imaging, about 15%-30% of object detections are expected to correspond to two or more true objects - these are called ``unrecognized blends''. We use Machine Learning algorithms to detect unrecognized blends in deep ground-based photometry using only catalog-level information: colors, magnitude, and size. We compare the performance of Self Organizing Map, Random Forest, k-Nearest Neighbors, and Anomaly Detection algorithms. We test all algorithms on 9-band ($uBVri^{+}z^{++}YJH$) and 1-size (flux_radius in $\textit{i}$-band) measurements of the ground-based COSMOS catalog, and use COSMOS HST data as the truth for unrecognized blend. We find that 17% of objects in the ground-based COSMOS catalog are unrecognized blends. We show that some unrecognized blends can be identified as such using only catalog-level information; but not all blends can be easily identified. Nonetheless, our methods can be used to improve sample purity, and can identify approximately 30% to 80% of unrecognized blends while rejecting 10% to 50% of all detected galaxies (blended or unblended). The results are similar when only optical bands ($uBVri^{+}z^{++}$) and the size information is available. We also investigate the ability of these algorithms to remove photo-z outliers (identified with spectroscopic redshifts), and find that algorithms targeting color outliers perform better than algorithms targeting unrecognized blends. Our method can offer a cleaner galaxy sample with lower blending rates for future cosmological surveys such as the Legacy Survey of Space and Time (LSST), and can potentially improve the accuracy on cosmological parameter constraints at a moderate cost of precision. </p> </div> </dd> <dt> <a name='item18'>[18]</a> <a href ="/abs/2503.16690" title="Abstract" id="2503.16690"> arXiv:2503.16690 </a> [<a href="/pdf/2503.16690" title="Download PDF" id="pdf-2503.16690" aria-labelledby="pdf-2503.16690">pdf</a>, <a href="https://arxiv.org/html/2503.16690v1" title="View HTML" id="html-2503.16690" aria-labelledby="html-2503.16690" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16690" title="Other formats" id="oth-2503.16690" aria-labelledby="oth-2503.16690">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Making the unmodulated pyramid wavefront sensor smart II. First on-sky demonstration of extreme adaptive optics with deep learning </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Landman,+R">R. Landman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Haffert,+S">S.Y. Haffert</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Long,+J">J.D. Long</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Males,+J">J.R. Males</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Close,+L">L.M. Close</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Foster,+W">W.B. Foster</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Van+Gorkom,+K">K. Van Gorkom</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Guyon,+O">O. Guyon</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hedglen,+A">A.D. Hedglen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Johnson,+P">P.T. Johnson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kautz,+M">M.Y. Kautz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kueny,+J">J.K. Kueny</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Li,+J">J. Li</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Liberman,+J">J. Liberman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lumbres,+J">J. Lumbres</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=McEwen,+E">E.A. McEwen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=McLeod,+A">A. McLeod</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Schatz,+L">L. Schatz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tonucci,+E">E. Tonucci</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Twitchell,+K">K. Twitchell</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Accepted for publication in A&A </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Instrumentation and Methods for Astrophysics (astro-ph.IM)</span>; Earth and Planetary Astrophysics (astro-ph.EP); Machine Learning (cs.LG); Optics (physics.optics) </div> <p class='mathjax'> Pyramid wavefront sensors (PWFSs) are the preferred choice for current and future extreme adaptive optics (XAO) systems. Almost all instruments use the PWFS in its modulated form to mitigate its limited linearity range. However, this modulation comes at the cost of a reduction in sensitivity, a blindness to petal-piston modes, and a limit to the sensor's ability to operate at high speeds. Therefore, there is strong interest to use the PWFS without modulation, which can be enabled with nonlinear reconstructors. Here, we present the first on-sky demonstration of XAO with an unmodulated PWFS using a nonlinear reconstructor based on convolutional neural networks. We discuss the real-time implementation on the Magellan Adaptive Optics eXtreme (MagAO-X) instrument using the optimized TensorRT framework and show that inference is fast enough to run the control loop at >2 kHz frequencies. Our on-sky results demonstrate a successful closed-loop operation using a model calibrated with internal source data that delivers stable and robust correction under varying conditions. Performance analysis reveals that our smart PWFS achieves nearly the same Strehl ratio as the highly optimized modulated PWFS under favorable conditions on bright stars. Notably, we observe an improvement in performance on a fainter star under the influence of strong winds. These findings confirm the feasibility of using the PWFS in its unmodulated form and highlight its potential for next-generation instruments. Future efforts will focus on achieving even higher control loop frequencies (>3 kHz), optimizing the calibration procedures, and testing its performance on fainter stars, where more gain is expected for the unmodulated PWFS compared to its modulated counterpart. </p> </div> </dd> <dt> <a name='item19'>[19]</a> <a href ="/abs/2503.16712" title="Abstract" id="2503.16712"> arXiv:2503.16712 </a> [<a href="/pdf/2503.16712" title="Download PDF" id="pdf-2503.16712" aria-labelledby="pdf-2503.16712">pdf</a>, <a href="https://arxiv.org/html/2503.16712v1" title="View HTML" id="html-2503.16712" aria-labelledby="html-2503.16712" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16712" title="Other formats" id="oth-2503.16712" aria-labelledby="oth-2503.16712">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Surveys of clumps, cores, and condensations in Cygnus-X: Searching for Keplerian disks on the scale of 500 au </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pan,+X">Xing Pan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Qiu,+K">Keping Qiu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhang,+Q">Qizhou Zhang</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 19 pages, 15 figures, accepted for A&A </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span>; Solar and Stellar Astrophysics (astro-ph.SR) </div> <p class='mathjax'> Over the past decades, observational evidence of circumstellar disks around massive protostars has been steadily accumulating. However, there have also been cases of non-detections in high-mass star-forming regions, leaving the role and prevalence of disks around massive protostars still uncertain. We used high-resolution (0.2") NOrthern Extended Millimeter Array (NOEMA) observations to study the 1.3 mm continuum and molecular line emission of five massive dense cores in the Cygnus-X cloud complex. Four cores host 2000-au-scale rotating structures previously identified as disk candidates in lower-resolution SMA observations, while the remaining core with no evidence for a disk serves as a comparison. With a resolution of 300 au, the 1.3 mm continuum emission reveals varying levels of fragmentation in our sample, with fragment radii ranging from 150 to 800 AU. In this work, we confirm the existence of two small, stable disks in Keplerian-like rotation at scales of 500 au out of four previously identified disk candidates from the SMA observations at coarser resolution. The lack of evidence for Keplerian disks in other disk candidates identified from the SMA data suggests that rotational signatures observed at 2000 au scales do not necessarily imply the presence of Keplerian disks at smaller scales. Therefore, higher-resolution and higher-sensitivity observations are essential to definitively identify Keplerian disks on smaller scales. </p> </div> </dd> <dt> <a name='item20'>[20]</a> <a href ="/abs/2503.16714" title="Abstract" id="2503.16714"> arXiv:2503.16714 </a> [<a href="/pdf/2503.16714" title="Download PDF" id="pdf-2503.16714" aria-labelledby="pdf-2503.16714">pdf</a>, <a href="https://arxiv.org/html/2503.16714v1" title="View HTML" id="html-2503.16714" aria-labelledby="html-2503.16714" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16714" title="Other formats" id="oth-2503.16714" aria-labelledby="oth-2503.16714">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Deep-TAO: The Deep Learning Transient Astronomical Object data set for Astronomical Transient Event Classification </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Su%C3%A1rez-P%C3%A9rez,+J+F">John F. Su谩rez-P茅rez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=G%C3%B3mez,+C">Catalina G贸mez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Neira,+M">Mauricio Neira</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hoyos,+M+H">Marcela Hern谩ndez Hoyos</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Arbel%C3%A1ez,+P">Pablo Arbel谩ez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Forero-Romero,+J+E">Jaime E. Forero-Romero</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 8 tables, 6 figures, Acepted by the Revista Mexicana de Astronom铆a y Astrof铆sica </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Instrumentation and Methods for Astrophysics (astro-ph.IM)</span> </div> <p class='mathjax'> We present the Deep-learning Transient Astronomical Object (Deep-TAO), a dataset of 1,249,079 annotated images from the Catalina Real-time Transient Survey, including 3,807 transient and 12,500 non-transient sequences. Deep-TAO has been curated to provide a clean, open-access, and user-friendly resource for benchmarking deep learning models. Deep-TAO covers transient classes such as blazars, active galactic nuclei, cataclysmic variables, supernovae, and events of indeterminate nature. The dataset is publicly available in FITS format, with Python routines and Jupyter notebooks for easy data manipulation. Using Deep-TAO, a baseline Convolutional Neural Network outperformed traditional random forest classifiers trained on light curves, demonstrating its potential for advancing transient classification. </p> </div> </dd> <dt> <a name='item21'>[21]</a> <a href ="/abs/2503.16720" title="Abstract" id="2503.16720"> arXiv:2503.16720 </a> [<a href="/pdf/2503.16720" title="Download PDF" id="pdf-2503.16720" aria-labelledby="pdf-2503.16720">pdf</a>, <a href="https://arxiv.org/html/2503.16720v1" title="View HTML" id="html-2503.16720" aria-labelledby="html-2503.16720" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16720" title="Other formats" id="oth-2503.16720" aria-labelledby="oth-2503.16720">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> A parameter scan of dark zone maintenance for high-contrast imaging of exoplanets using theoretical and experimental implementations </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Manojkumar,+S">Saikrishna Manojkumar</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Page,+C+L">Christine L. Page</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pogorelyuk,+L">Leonid Pogorelyuk</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Redmond,+S+F">Susan F. Redmond</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gill,+A+S">Ajay S. Gill</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pueyo,+L">Laurent Pueyo</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Por,+E+H">Emiel H. Por</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Laginja,+I">Iva Laginja</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pourc%C3%ABlot,+R">Raphael Pourc毛lot</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Nickson,+B+F">Bryony F. Nickson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sahoo,+A">Ananya Sahoo</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Nguyen,+M+M">Meiji M. Nguyen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Soummer,+R">R茅mi Soummer</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Perrin,+M+D">Marshall D. Perrin</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Nemati,+B">Bijan Nemati</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cahoy,+K">Kerri Cahoy</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kasdin,+J+N">Jeremy N. Kasdin</a></div> <div class='list-journal-ref'><span class='descriptor'>Journal-ref:</span> Proc. SPIE 13092, Space Telescopes and Instrumentation 2024: Optical, Infrared, and Millimeter Wave, 1309269 (23 August 2024) </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Instrumentation and Methods for Astrophysics (astro-ph.IM)</span>; Earth and Planetary Astrophysics (astro-ph.EP) </div> <p class='mathjax'> Maintaining wavefront stability while directly imaging exoplanets over long exposure times is an ongoing problem in the field of high-contrast imaging. Robust and efficient high-order wavefront sensing and control systems are required for maintaining wavefront stability to counteract mechanical and thermal instabilities. Dark zone maintenance (DZM) has been proposed to address quasi-static optical aberrations and maintain high levels of contrast for coronagraphic space telescopes. To further experimentally test this approach for future missions, such as the Habitable Worlds Observatory, this paper quantifies the differences between the theoretical closed-loop contrast bounds and DZM performance on the High-contrast Imager for Complex Aperture Telescopes(HiCAT) testbed. The quantification of DZM is achieved by traversing important parameters of the system, specifically the total direct photon rate entering the aperture of the instrument, ranging from $1.85 \times 10^6$ to $1.85 \times 10^8$ photons per second, and the wavefront error drift rate, ranging from $\sigma_{drift}$ = 0.3 - 3 $nm/\sqrt{iteration}$, injected via the deformable mirror actuators. This is tested on the HiCAT testbed by injecting random walk drifts using two Boston Micromachines kilo deformable mirrors (DMs). The parameter scan is run on the HiCAT simulator and the HiCAT testbed where the corresponding results are compared to the model-based theoretical contrast bounds to analyze discrepancies. The results indicate an approximate one and a half order of magnitude difference between the theoretical bounds and testbed results. </p> </div> </dd> <dt> <a name='item22'>[22]</a> <a href ="/abs/2503.16729" title="Abstract" id="2503.16729"> arXiv:2503.16729 </a> [<a href="/pdf/2503.16729" title="Download PDF" id="pdf-2503.16729" aria-labelledby="pdf-2503.16729">pdf</a>, <a href="https://arxiv.org/html/2503.16729v1" title="View HTML" id="html-2503.16729" aria-labelledby="html-2503.16729" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16729" title="Other formats" id="oth-2503.16729" aria-labelledby="oth-2503.16729">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> NEIDSpecMatch: stellar parameter estimation with NEID spectra using an empirical library </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Han,+T">Te Han</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Robertson,+P">Paul Robertson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ca%C3%B1as,+C+I">Caleb I. Ca帽as</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Stefansson,+G">Gudmundur Stefansson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kanodia,+S">Shubham Kanodia</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ninan,+J+P">Joe P. Ninan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Alvarado-Montes,+J+A">Jaime A. Alvarado-Montes</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bender,+C+F">Chad F. Bender</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dong,+J">Jiayin Dong</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fernandes,+R">Rachel Fernandes</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gupta,+A+F">Arvind F. Gupta</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Halverson,+S">Samuel Halverson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Krolikowski,+D+M">Daniel M. Krolikowski</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lin,+A+S">Andrea S.J. Lin</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mahadevan,+S">Suvrath Mahadevan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Paredes,+L+A">Leonardo A. Paredes</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Roy,+A">Arpita Roy</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Schwab,+C">Christian Schwab</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Terrien,+R+C">Ryan C. Terrien</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 4 pages, 1 figure. RNAAS accepted </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span>; Astrophysics of Galaxies (astro-ph.GA); High Energy Astrophysical Phenomena (astro-ph.HE); Instrumentation and Methods for Astrophysics (astro-ph.IM) </div> <p class='mathjax'> We introduce NEIDSpecMatch, a tool developed to extract stellar parameters from spectra obtained with the NEID spectrograph. NEIDSpecMatch is based on SpecMatch-Emp and HPFSpecMatch, which estimate stellar parameters by comparing the observed spectrum to well-characterized library spectra. This approach has proven effective for M dwarfs. Utilizing a library of 78 stellar spectra covering effective temperatures from $3000-6000$ K, NEIDSpecMatch derives key parameters, including effective temperature, metallicity, surface gravity, and projected rotational velocity. Cross-validation shows median uncertainties of $\sigma_{T_{\mathrm{eff}}} = 115\,\mathrm{K}$, $\sigma_{[\mathrm{Fe/H}]} = 0.143$, and $\sigma_{\log g} = 0.073$ across 49 orders. We showcase its application by fitting the spectrum of an M-dwarf and discuss its utility across a wide range of spectra observed with NEID. NEIDSpecMatch is pip-installable. </p> </div> </dd> <dt> <a name='item23'>[23]</a> <a href ="/abs/2503.16733" title="Abstract" id="2503.16733"> arXiv:2503.16733 </a> [<a href="/pdf/2503.16733" title="Download PDF" id="pdf-2503.16733" aria-labelledby="pdf-2503.16733">pdf</a>, <a href="https://arxiv.org/html/2503.16733v1" title="View HTML" id="html-2503.16733" aria-labelledby="html-2503.16733" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16733" title="Other formats" id="oth-2503.16733" aria-labelledby="oth-2503.16733">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Testing the bloated star hypothesis in the massive young stellar object IRAS 19520+2759 through optical and infrared variability </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pandey,+R">Rakesh Pandey</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Palau,+A">Aina Palau</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Serna,+J">Javier Serna</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kuiper,+R">Rolf Kuiper</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=S%C3%A1nchez-Monge,+%C3%81">脕lvaro S谩nchez-Monge</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sharma,+S">Saurabh Sharma</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sahai,+R">Raghvendra Sahai</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Contreras,+C+S">Carmen S谩nchez Contreras</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hern%C3%A1ndez,+J">Jes煤s Hern谩ndez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rom%C3%A1n-Z%C3%BA%C3%B1iga,+C">Carlos Rom谩n-Z煤帽iga</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rodler,+F">Florian Rodler</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 18 pages, 15 figures, 1 table. Accepted for publication in MNRAS </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span> </div> <p class='mathjax'> Using optical time series with Telescopi Joan Or贸 (TJO), Gaia, TESS, and NEOWISE archival data, we performed a variability study on the candidate bloated massive young stellar object (MYSO) IRAS 19520+2759. This is the first time that a bloated star candidate has been tested for the theoretically predicted periodic variability. The source is found to be variable at optical and mid-infrared wavelengths and classified as a long-period variable MYSO. The observed TJO data gives a period of the source of $\sim$ 270$\pm$40 days (in the Rc band) and $\sim$ 270$\pm$50 days (in the Ic band), which is very close to the value predicted by the theoretical Period-Luminosity relation for a bloated young star of $\sim 10^5 L\odot$. Additionally, a large period of $\sim$ 460$\pm$80 days (in the G band) and $\sim$ 440$\pm$70 (in the Rp band) is also visible in the Gaia light curve. The physical parameters of the source, such as mass, radius, and accretion rate, based on the theoretical predictions for the spherical accretion case and corresponding to a period of 270--460 days, are $\sim 24$--28$\,M\odot$, $\sim 650$--900$\,R\odot$ and $\sim (6$--$9)\times10^{-3}\,M\odot yr^{-1}$. However, these numbers are very sensitive to the effective temperatures assumed in the models. Additionally, these values strongly depend on the geometry of accretion and could significantly decrease for the case of a MYSO accreting through a disc. The observed periodic variability, the observed colour trend, and the nature of the variability are found to be consistent with the pulsational model for a bloated MYSO. </p> </div> </dd> <dt> <a name='item24'>[24]</a> <a href ="/abs/2503.16752" title="Abstract" id="2503.16752"> arXiv:2503.16752 </a> [<a href="/pdf/2503.16752" title="Download PDF" id="pdf-2503.16752" aria-labelledby="pdf-2503.16752">pdf</a>, <a href="https://arxiv.org/html/2503.16752v1" title="View HTML" id="html-2503.16752" aria-labelledby="html-2503.16752" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16752" title="Other formats" id="oth-2503.16752" aria-labelledby="oth-2503.16752">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> An attempt to determine the magnetic field configuration in the planetary nebula K 3-35 with ALMA </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sabin,+L">L. Sabin</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhang,+Q">Q. Zhang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Miranda,+L">L.F. Miranda</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=G%C3%B3mez-Mu%C3%B1oz,+M+A">M. A. G贸mez-Mu帽oz</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 6 pages, 3 figures, accepted for publication in Monthly Notices of the Royal Astronomical Society </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span>; Astrophysics of Galaxies (astro-ph.GA) </div> <p class='mathjax'> We examined dust polarisation within the planetary nebula (PN) K 3-35 using the Atacama Large Millimeter/Submillimeter Array (ALMA). This investigation aimed to identify and trace the magnetic field within the PN, as it potentially plays a crucial role in shaping this bipolar nebula. Our findings include a marginal detection of the polarised region and low fractional polarisation (peaking at 1.4%). Assuming a certain level of validity, we observed well-organised dust grains aligned along the equatorial plane of the PN, indicating a magnetic field alignment with the outflows. The limited polarisation detection at submillimeter wavelengths in this PN and others may be attributed to a pronounced optical depth. However, our K 3-35 analysis with the code DUSTY does not seem to support this idea. We also modelled the SED of K3-35, and our best-fit models included a mixture of silicates and amorphous carbon. The grains of amorphous carbon are less susceptible to alignment with the magnetic field, which could, at least partially, explain the observed low polarisation. The models presented in this article should be considered preliminary, and a more advanced approach is needed for a more complete interpretation of the results. </p> </div> </dd> <dt> <a name='item25'>[25]</a> <a href ="/abs/2503.16773" title="Abstract" id="2503.16773"> arXiv:2503.16773 </a> [<a href="/pdf/2503.16773" title="Download PDF" id="pdf-2503.16773" aria-labelledby="pdf-2503.16773">pdf</a>, <a href="/format/2503.16773" title="Other formats" id="oth-2503.16773" aria-labelledby="oth-2503.16773">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Hydrodynamics of ultralight complex scalar field dark matter and its impact on the growth of structure </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yang,+Q">Qi Yang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Li,+B">Bohua Li</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Shapiro,+P+R">Paul R. Shapiro</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 13 pages, 8 figures, submitted; comments welcome </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span>; General Relativity and Quantum Cosmology (gr-qc) </div> <p class='mathjax'> The mass window of ultralight axion dark matter motivated by suppressing the growth of structure on subgalactic scales, $m\sim 10^{-22}\,\mathrm{eV}$, is now severely constrained by various observation data (e.g. Lyman-$\alpha$ forest). As an attempt to reopen this mass window, we investigate an alternative ultralight dark matter candidate, the complex scalar field dark matter (SFDM). We derive the relativistic hydrodynamics of the complex SFDM in the framework of cosmological perturbation theory. Our formalism contains two novel ingredients uniquely associated with the complex SFDM model: the Eckart frame defined by the conserved Noether current, and the stiff gauge condition, $c_s^2\equiv (\delta P/\delta\rho)|_s=1$. In the Eckart frame, the complex SFDM is effectively an imperfect fluid with a dissipative energy flux, distinguishing itself from axion dark matter. The energy flux can affect the growth of density fluctuations dynamically. Meanwhile, we apply the stiff gauge condition to find new constitutive equations for the complex SFDM. We revisit the homogeneous evolution of the complex SFDM and present illustrative early-stage solutions for perturbations of the complex SFDM in a simplified setting. We demonstrate the effects of varying the model parameters on the evolution of the perturbation variables. </p> </div> </dd> <dt> <a name='item26'>[26]</a> <a href ="/abs/2503.16844" title="Abstract" id="2503.16844"> arXiv:2503.16844 </a> [<a href="/pdf/2503.16844" title="Download PDF" id="pdf-2503.16844" aria-labelledby="pdf-2503.16844">pdf</a>, <a href="https://arxiv.org/html/2503.16844v1" title="View HTML" id="html-2503.16844" aria-labelledby="html-2503.16844" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16844" title="Other formats" id="oth-2503.16844" aria-labelledby="oth-2503.16844">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Upper limits on the gamma-ray emission from the microquasar V4641 Sgr </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhao,+Z">Zihao Zhao</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Li,+J">Jian Li</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Torres,+D+F">Diego F. Torres</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 10 pages, 6 figures, accepted by ApJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> Following a recent detection of TeV radiation by the Large High Altitude Air Shower Observatory (LHAASO) and the High-Altitude Water Cherenkov Observatory (HAWC), coincident with the direction of the microquasar V4641 Sgr, we search for possible GeV emission from this source. We explored the morphology and temporal features of the source as well as two nearby unassociated point sources which could be a part of extended structure of V4641 Sgr, and compared results with corresponding X-ray and TeV emissions. The 95% confidence level upper limits for the flux from the source, assuming both point and extended source models were 5.38$\times$ 10$^{-13}$ erg cm$^{-2}$ s$^{-1}$ and 1.12$\times$ 10$^{-12}$ erg cm$^{-2}$ s$^{-1}$, respectively. Additionally, no correlation between gamma-ray light curve and X-ray outbursts was observed. </p> </div> </dd> <dt> <a name='item27'>[27]</a> <a href ="/abs/2503.16857" title="Abstract" id="2503.16857"> arXiv:2503.16857 </a> [<a href="/pdf/2503.16857" title="Download PDF" id="pdf-2503.16857" aria-labelledby="pdf-2503.16857">pdf</a>, <a href="https://arxiv.org/html/2503.16857v1" title="View HTML" id="html-2503.16857" aria-labelledby="html-2503.16857" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16857" title="Other formats" id="oth-2503.16857" aria-labelledby="oth-2503.16857">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Observational Comparison Between Confined and Eruptive Flares: Magnetohydrodynamics Instability Parameters in a Similar Magnetic Configuration </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Teraoka,+K">Kouhei Teraoka</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yamasaki,+D">Daiki Yamasaki</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kawabata,+Y">Yusuke Kawabata</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Imada,+S">Shinsuke Imada</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Shimizu,+T">Toshifumi Shimizu</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Accepted for the publication in ApJ, 24 pages, 5 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span> </div> <p class='mathjax'> Unstable states of the solar coronal magnetic field structure result in various flare behaviors. In this study, we compared the confined and eruptive flares that occurred under similar magnetic circumstances in the active region 12673, on 2017 September 6, using the twist number, decay index, and height of magnetic field lines to identify observational behaviors of the flare eruption. We investigated the parameters from the magnetic field lines involved in an initial energy release, which were identified from the positions of the core of flare ribbons, i.e., flare kernels. The magnetic field lines were derived by nonlinear force-free field modeling calculated from the photospheric vector magnetic field obtained by the Solar Dynamics Observatory SDO/Helioseismic and Magnetic Imager, and flare kernels were identified from the 1600 angstrom data obtained by the SDO/Atmospheric Imaging Assembly. The twist number of all the magnetic field lines in the confined flare was below 0.6; however, the twist number in seven out of twenty-four magnetic field lines in the eruptive flare was greater than 0.6. These lines were tall. It is found that the decay index is not a clear discriminator of the confined and eruptive flares. Our study suggests that some magnetic field lines in the kink instability state may be important for eruptive flares, and that taller magnetic field lines may promote flare eruption. </p> </div> </dd> <dt> <a name='item28'>[28]</a> <a href ="/abs/2503.16864" title="Abstract" id="2503.16864"> arXiv:2503.16864 </a> [<a href="/pdf/2503.16864" title="Download PDF" id="pdf-2503.16864" aria-labelledby="pdf-2503.16864">pdf</a>, <a href="https://arxiv.org/html/2503.16864v1" title="View HTML" id="html-2503.16864" aria-labelledby="html-2503.16864" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16864" title="Other formats" id="oth-2503.16864" aria-labelledby="oth-2503.16864">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> A multi-messenger hierarchical triple merger gravitational-wave event pair GW190514-GW190521 inside AGN J124942.3 + 344929 </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Li,+G">Guo-Peng Li</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fan,+X">Xi-Long Fan</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Comments are welcome </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; Astrophysics of Galaxies (astro-ph.GA); Solar and Stellar Astrophysics (astro-ph.SR); General Relativity and Quantum Cosmology (gr-qc) </div> <p class='mathjax'> There is a candidate electromagnetic counterpart to the binary black hole merger GW190521, identified as ZTF19abanrhr within AGN J124942.3 + 344929. Additionally, GW190514 is proposed as a plausible precursor merger to GW190521 within a hierarchical merger scenario. In this study, we investigate the potential association between GW190514 and GW190521 as a hierarchical triple merger associated with ZTF19abanrhr, taking into account of sky position, distance, and mass of the sources using a Bayesian criterion. Our analysis reveals that the association is favored over a random coincidence, with a log Bayes factor of 16.8, corresponding to an odds ratio of $\sim$$199:1$, assuming an astrophysical prior odds of $10^{-5}$. Notably, when accounting for the primary masses of the two gravitational wave events as potential products of mergers in the AGN formation channel, the Bayes factor increases significantly, further enhancing the preference for this association by a factor of $\sim$$10^2$, corresponding to a log Bayes factor of 21.5 and an odds ratio of $\sim$$2\times10^4:1$. Our results suggest strong evidence for the first hierarchical triple merger associated with an electromagnetic counterpart in the AGN formation channel. This work is crucial for understanding the formation mechanisms of massive black holes, the role of AGNs in hierarchical mergers, and the implications of multi-messenger astronomy. </p> </div> </dd> <dt> <a name='item29'>[29]</a> <a href ="/abs/2503.16886" title="Abstract" id="2503.16886"> arXiv:2503.16886 </a> [<a href="/pdf/2503.16886" title="Download PDF" id="pdf-2503.16886" aria-labelledby="pdf-2503.16886">pdf</a>, <a href="https://arxiv.org/html/2503.16886v1" title="View HTML" id="html-2503.16886" aria-labelledby="html-2503.16886" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16886" title="Other formats" id="oth-2503.16886" aria-labelledby="oth-2503.16886">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Insight-HXMT observations of the 2023 outburst in Aql X-1 </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yan,+Z">Zhe Yan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhang,+G">Guobao Zhang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chen,+Y">Yu-Peng Chen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=M%C3%A9ndez,+M">Mariano M茅ndez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mao,+J">Jirong Mao</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lyu,+M">Ming Lyu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhang,+S">Shu Zhang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Jin,+P">Pei Jin</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 6 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> We conducted an analysis of the continuum during the onset and initial decline phases of the 2023 outburst in transient neutron star low-mass X-ray binary Aql X$-$1 using broadband observations from the \textit{Insight-Hard X-ray Modulation Telescope (Insight-HXMT)} instrument. To determine the most appropriate model for the continuum of this outburst, we employed three models to explore the evolution of the spectral component. These observations revealed that the source transitions from the hard state to the soft state. The disk-corona and sphere-corona models both adequately described the spectra of the hard state, while the double blackbody model became preferable after the hard X-ray emission ($>$25 keV) disappeared during the state transition. In the soft state, the total emission is dominated by changes in the disk and other blackbody components. The combination of the sphere-corona model and the double blackbody model is the most suitable model for this outburst. The results suggest that as the source transitioned into the soft state, the emission from the boundary layer was enhanced, and a hot spot occurred. Notably, we identified two type-I X-ray bursts, one of which exhibited a significant hard X-ray deficit (significance $\sim$ 4.82 $\sigma$), which indicates that \textit{Insight-HXMT} has the capability to capture the evolution of the corona in a single burst. </p> </div> </dd> <dt> <a name='item30'>[30]</a> <a href ="/abs/2503.16888" title="Abstract" id="2503.16888"> arXiv:2503.16888 </a> [<a href="/pdf/2503.16888" title="Download PDF" id="pdf-2503.16888" aria-labelledby="pdf-2503.16888">pdf</a>, <a href="https://arxiv.org/html/2503.16888v1" title="View HTML" id="html-2503.16888" aria-labelledby="html-2503.16888" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16888" title="Other formats" id="oth-2503.16888" aria-labelledby="oth-2503.16888">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Probing the Internal Structure of Neutron Stars: A Comparative Analysis of Three Different Classes of Equations of State </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Verma,+A">Anshuman Verma</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Saha,+A+K">Asim Kumar Saha</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Malik,+T">Tuhin Malik</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mallick,+R">Ritam Mallick</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 9 pages, 7 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> Sound speed can be an important tool in unraveling the nature of matter that exists at the cores of neutron stars. In this study, we investigate three major classes of equations of state; monotonous, non-monotonous and discontinuous depending on the nature of the sound speed in neutron stars. The monotonous EoS refers to hadronic models, the non-monotonous refers to the quarkyonic or smooth crossover models and discontinuous refers to discontinuous first-order phase transition models. We generate a large ensemble of EoS for three classes with the model agnostic speed of sound interpolation approach. Our main aim is to check which class of EoS is most favoured by present astrophysical bounds. It is seen that although non-monotonous and discontinuous is favoured thermodynamically, the usual neutron star observations like mass-radius, and f-mode oscillation fail to provide a satisfactory result. The universal relations are also seen to be futile as they show considerable spread and significant overlaps among the different classes. The Bayesian analysis shows slight bias towards the non-monotonous model but fails to provide a decisive answer. </p> </div> </dd> <dt> <a name='item31'>[31]</a> <a href ="/abs/2503.16899" title="Abstract" id="2503.16899"> arXiv:2503.16899 </a> [<a href="/pdf/2503.16899" title="Download PDF" id="pdf-2503.16899" aria-labelledby="pdf-2503.16899">pdf</a>, <a href="https://arxiv.org/html/2503.16899v1" title="View HTML" id="html-2503.16899" aria-labelledby="html-2503.16899" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16899" title="Other formats" id="oth-2503.16899" aria-labelledby="oth-2503.16899">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Property of downstream turbulence driven by the special relativistic shock-clump interaction </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Morikawa,+K">Kanji Morikawa</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ohira,+Y">Yutaka Ohira</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ohmura,+T">Takumi Ohmura</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 12 pages, 12 figures, submitted to MNRAS </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; Plasma Physics (physics.plasm-ph) </div> <p class='mathjax'> Three-dimensional special relativistic magnetohydrodynamic simulations are performed to investigate properties of the downstream turbulence generated by the interaction between a relativistic shock wave and multiple clumps. We analyze the properties of the downstream turbulence by performing the Helmholtz decomposition. It is shown that, in contrast to the non-relativistic shock case, the amplitude of compressive modes is comparable to that of solenoidal modes for the relativistic shock. In addition, many reflected shocks propagate in the downstream region. The strength of the compressive mode, the solenoidal mode, the reflected shock waves, and the amplified magnetic field depend on the amplitude of the upstream density fluctuations. Our simulation results suggest that the wide distribution of the ratio of the magnetic energy to the shock kinetic energy, $\epsilon_B$, in gamma-ray burst afterglows is due to the diversity of the gamma-ray burst environment. Furthermore, the inhomogeneity of density around high-energy astrophysical objects affects the spectrum of accelerated particles because the reflected shock and turbulence can inject and accelerate non-thermal particles in the shock downstream region. The probability distribution of the downstream quantities, power spectra of turbulence, and vortex generation are also analyzed and discussed in this work. </p> </div> </dd> <dt> <a name='item32'>[32]</a> <a href ="/abs/2503.16907" title="Abstract" id="2503.16907"> arXiv:2503.16907 </a> [<a href="/pdf/2503.16907" title="Download PDF" id="pdf-2503.16907" aria-labelledby="pdf-2503.16907">pdf</a>, <a href="https://arxiv.org/html/2503.16907v1" title="View HTML" id="html-2503.16907" aria-labelledby="html-2503.16907" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16907" title="Other formats" id="oth-2503.16907" aria-labelledby="oth-2503.16907">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Gravitational Wave Signatures of Preheating in Higgs--$R^2$ Inflation </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kim,+J">Jinsu Kim</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yang,+Z">Zihao Yang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhang,+Y">Ying-li Zhang</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 12 pages </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span>; High Energy Physics - Phenomenology (hep-ph) </div> <p class='mathjax'> We present a comprehensive analysis of the preheating dynamics and associated gravitational wave signatures in the Higgs--$R^2$ inflationary model. Using lattice simulations, we investigate the post-inflationary evolution of the system across the parameter space, covering both the Higgs-like and $R^2$-like scenarios. We demonstrate that the efficiency of preheating is significantly dependent on the nonminimal coupling parameter $\xi$. As the $\xi$ parameter increases, moving from the $R^2$-like regime to the Higgs-like regime, we observe more efficient preheating. Through detailed numerical computations, efficient preheating is shown to lead to stronger gravitational wave production. The amplitude of the gravitational wave spectrum varies by several orders of magnitude as we move from the $R^2$-like regime to the Higgs-like regime. The resultant gravitational wave signatures can serve as a potential observational probe to distinguish between different parameter regimes of the Higgs--$R^2$ model. </p> </div> </dd> <dt> <a name='item33'>[33]</a> <a href ="/abs/2503.16908" title="Abstract" id="2503.16908"> arXiv:2503.16908 </a> [<a href="/pdf/2503.16908" title="Download PDF" id="pdf-2503.16908" aria-labelledby="pdf-2503.16908">pdf</a>, <a href="https://arxiv.org/html/2503.16908v1" title="View HTML" id="html-2503.16908" aria-labelledby="html-2503.16908" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16908" title="Other formats" id="oth-2503.16908" aria-labelledby="oth-2503.16908">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Investigation of X-ray emission from the unidentified TeV gamma-ray source HESS J1832-085 with Suzaku </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Aktekin,+E">Ebru Aktekin</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 7 pages, 4 Figures, 2 Tables; Accepted for publication in Advances in Space Research on February 28, 2025 </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> Observations conducted with H.E.S.S. at high energies have led to the discovery of numerous gamma-ray sources in the Galactic plane at TeV energies. One of these sources, HESS J1832-085, has been suggested to be a pulsar wind nebula (PWN); however, its nature is not yet fully understood. In this work, we analyze Suzaku data to investigate the X-ray spectral properties of HESS J1832-085. We found that the X-ray spectra are highly absorbed and well-represented by a power-law model with a photon index of $\Gamma \sim 1.5$, and an unabsorbed X-ray flux of $F_{\rm X} \sim 0.3 \times 10^{-11}$ erg cm$^{-2}$ s$^{-1}$ in the 2-10 keV energy band. The gamma-ray flux is approximately 66 times higher than the X-ray flux. Based on our X-ray analysis, we discuss the origin of the source HESS J1832-085. We propose that the PWN scenario is possible, although several issues still need to be resolved. </p> </div> </dd> <dt> <a name='item34'>[34]</a> <a href ="/abs/2503.16937" title="Abstract" id="2503.16937"> arXiv:2503.16937 </a> [<a href="/pdf/2503.16937" title="Download PDF" id="pdf-2503.16937" aria-labelledby="pdf-2503.16937">pdf</a>, <a href="https://arxiv.org/html/2503.16937v1" title="View HTML" id="html-2503.16937" aria-labelledby="html-2503.16937" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16937" title="Other formats" id="oth-2503.16937" aria-labelledby="oth-2503.16937">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> External tides: an important driver of velocity dispersion in molecular clouds </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhou,+J+W">J. W. Zhou</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Accepted for publication in A&A Letter </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> Using the 3D density distribution derived from the 3D dust map of the solar neighborhood, the gravitational potential is obtained by solving the Poisson equation, from which the tidal tensor is computed. In the optimal decomposition, the external tidal tensor follows the same formalism as that of a point mass. The average tidal strength of the clouds, derived from both tidal tensor analysis and pixel-by-pixel computation, shows consistent results. The equivalent velocity dispersion of the clouds, estimated from the average tidal strength, is comparable in magnitude to the velocity dispersion measured from CO (1-0) line emission. This suggests that tidal effects from surrounding material may play a significant role in driving velocity dispersion within the clouds. Future studies should carefully consider these tidal effects in star-forming regions. </p> </div> </dd> <dt> <a name='item35'>[35]</a> <a href ="/abs/2503.16946" title="Abstract" id="2503.16946"> arXiv:2503.16946 </a> [<a href="/pdf/2503.16946" title="Download PDF" id="pdf-2503.16946" aria-labelledby="pdf-2503.16946">pdf</a>, <a href="https://arxiv.org/html/2503.16946v1" title="View HTML" id="html-2503.16946" aria-labelledby="html-2503.16946" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16946" title="Other formats" id="oth-2503.16946" aria-labelledby="oth-2503.16946">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Observational constraints on the origin of the elements. IX. 3D NLTE abundances of metals in the context of Galactic Chemical Evolution Models and 4MOST </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Storm,+N">Nicholas Storm</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bergemann,+M">Maria Bergemann</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Eitner,+P">Philipp Eitner</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hoppe,+R">Richard Hoppe</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kemp,+A+J">Alex J. Kemp</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ruiter,+A+J">Ashley J. Ruiter</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Janka,+H">Hans-Thomas Janka</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sieverding,+A">Andre Sieverding</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=de+Mink,+S+E">Selma E. de Mink</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Seitenzahl,+I+R">Ivo R. Seitenzahl</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Owusu,+E+K">Evans K. Owusu</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 13 pages + 16 pages appendix, 10 figures + 17 figures appendix, accepted to MNRAS </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span>; Astrophysics of Galaxies (astro-ph.GA) </div> <p class='mathjax'> Historically, various methods have been employed to understand the origin of the elements, including observations of elemental abundances which have been compared to Galactic Chemical Evolution (GCE) models. It is also well known that 1D Local Thermodynamic Equilibrium (LTE) measurements fail to accurately capture elemental abundances. Non-LTE (NLTE) effects may play a significant role, and neglecting them leads to erroneous implications in galaxy modelling. In this paper, we calculate 3D NLTE abundances of seven key iron-peak and neutron-capture elements (Mn, Co, Ni, Sr, Y, Ba, Eu) based on carefully assembled 1D LTE literature measurements, and investigate their impact within the context of the OMEGA+ GCE model. Our findings reveal that 3D NLTE abundances are significantly higher for iron-peak elements at [Fe/H]< -3, with (for the first time ever) [Ni/Fe] and (confirming previous studies) [Co/Fe] on average reaching 0.6-0.8 dex, and [Mn/Fe] reaching -0.1 dex, which current 1D core-collapse supernova (CCSN) models cannot explain. We also observe a slightly higher production of neutron-capture elements at low metallicities, with 3D NLTE abundances of Eu being higher by +0.2 dex at [Fe/H]= -3. 3D effects are most significant for iron-peak elements in the very metal-poor regime, with average differences between 3D NLTE and 1D NLTE {reaching} up to 0.15 dex. Thus, ignoring 3D NLTE effects introduces significant biases, so including {them} should be considered whenever possible. </p> </div> </dd> <dt> <a name='item36'>[36]</a> <a href ="/abs/2503.16998" title="Abstract" id="2503.16998"> arXiv:2503.16998 </a> [<a href="/pdf/2503.16998" title="Download PDF" id="pdf-2503.16998" aria-labelledby="pdf-2503.16998">pdf</a>, <a href="/format/2503.16998" title="Other formats" id="oth-2503.16998" aria-labelledby="oth-2503.16998">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Maximising information from weak lensing galaxy surveys </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Maraio,+A">Alessandro Maraio</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 243 pages, PhD thesis awarded by the University of Edinburgh. Partial overlap with <a href="https://arxiv.org/abs/2207.10412" data-arxiv-id="2207.10412" class="link-https">arXiv:2207.10412</a> and <a href="https://arxiv.org/abs/2410.12500" data-arxiv-id="2410.12500" class="link-https">arXiv:2410.12500</a> </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span> </div> <p class='mathjax'> Weak lensing galaxy surveys are currently undergoing a dramatic revolution as the dawn of the Stage-IV surveys are upon us. Hence, ensuring that our analysis methods are as accurate and precise as the raw data is of upmost importance. This motivated the development of a new implementation of the quadratic maximum likelihood power spectrum estimation technique, the application of the theoretical uncertainties approach to mitigate baryonic feedback biases, and to re-evaluating the criterion from which binary scale cuts are derived when aiming to eliminate baryonic biases. These techniques maximise the available information from weak lensing observations while minimising potential systematic biases, and shows how this PhD thesis contributes to the advancement of weak lensing cosmology. </p> </div> </dd> <dt> <a name='item37'>[37]</a> <a href ="/abs/2503.17006" title="Abstract" id="2503.17006"> arXiv:2503.17006 </a> [<a href="/pdf/2503.17006" title="Download PDF" id="pdf-2503.17006" aria-labelledby="pdf-2503.17006">pdf</a>, <a href="https://arxiv.org/html/2503.17006v1" title="View HTML" id="html-2503.17006" aria-labelledby="html-2503.17006" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17006" title="Other formats" id="oth-2503.17006" aria-labelledby="oth-2503.17006">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Prompt Stellar and Binary Black Hole Mergers from Chemically Homogeneous Evolution in Triples </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Vigna-G%C3%B3mez,+A">Alejandro Vigna-G贸mez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Grishin,+E">Evgeni Grishin</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Stegmann,+J">Jakob Stegmann</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Olejak,+A">Aleksandra Olejak</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Popa,+S+A">Silvia A. Popa</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Liu,+B">Bin Liu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rajamuthukumar,+A+S">Abinaya S. Rajamuthukumar</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=van+Son,+L+A+C">Lieke A. C. van Son</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bobrick,+A">Alexey Bobrick</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dorozsmai,+A">Andris Dorozsmai</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 17 pages (including appendices), 8 main figures and 2 additional figures in the appendices. Submitted to A&A </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span>; High Energy Astrophysical Phenomena (astro-ph.HE) </div> <p class='mathjax'> Short-period massive binary stars are predicted to undergo chemically homogeneous evolution (CHE), making them prime candidates for producing binary black holes (BBHs) that may merge within the age of the Universe. Most of these binaries have a tertiary companion, and here we explore how a nearby third body possibly influences this evolutionary channel. Our analysis combines analytic treatments of triple dynamics with insights from detailed stellar evolution models, focusing on the role of the von Zeipel-Lidov-Kozai mechanism while also accounting for tidal and general relativistic apsidal precession. We examine the dynamics of triples at three critical evolutionary stages: the zero-age main sequence, shortly after the main sequence, and at the time of BBH formation. We find that, for triples having outer orbital periods less than 70 d(120 d), the inner binary can merge during(or after) the main-sequence stage, leading to a hydrogen-rich(helium-rich) stellar merger. If a stellar merger is avoided, the inner binary may eventually form a BBH. In mildly hierarchical triples, with outer periods of around 100 d, the tertiary component can trigger a rapid merger of the BBH on timescales comparable to the outer orbital period. Stellar tides play a crucial role in determining the fate of the inner binary in such tight triple systems, as they can suppress the perturbative effects of the third star. When tidal forces damp the oscillations induced by the tertiary, the BBH merger may occur soon after stellar collapse. Notably, these outcomes are not restricted to CHE binaries but can also apply to any BBH formed from stars in tight orbits. Mergers in these systems are characterized by the proximity of a tertiary companion and the presence of recently ejected gas, making them promising candidates for electromagnetic counterparts and gravitational-wave signals influenced by nearby tertiary objects. </p> </div> </dd> <dt> <a name='item38'>[38]</a> <a href ="/abs/2503.17075" title="Abstract" id="2503.17075"> arXiv:2503.17075 </a> [<a href="/pdf/2503.17075" title="Download PDF" id="pdf-2503.17075" aria-labelledby="pdf-2503.17075">pdf</a>, <a href="https://arxiv.org/html/2503.17075v1" title="View HTML" id="html-2503.17075" aria-labelledby="html-2503.17075" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17075" title="Other formats" id="oth-2503.17075" aria-labelledby="oth-2503.17075">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Observer motion and boosting effects on the cosmic background monopole spectrum, solutions and perspectives </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Trombetti,+T">Tiziana Trombetti</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 17 pages, 5 figures, accepted for pubblication in the proceedings of the 17th Marcel Grossmann Meeting </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span> </div> <p class='mathjax'> The peculiar motion of an observer relative to an ideal reference frame at rest with respect to the cosmic background produces boosting effects which modify and transfer at higher multipoles the frequency spectrum of the isotropic background. To mitigate the computational effort needed for accurate theoretical predictions, analytical solutions of a linear system able to evaluate the spherical harmonic expansion coefficients for (analytical or semi-analytical) background representations have been presented, and extended to generic tabulated functions potentially affected by numerical uncertainties. Owing to the dipole spectrum frequency dependence and to precise inter-frequency calibrations, it will be possible to constrain (or even detect) the tiny imprints in the background spectrum from a variety of cosmological and astrophysical processes. </p> </div> </dd> <dt> <a name='item39'>[39]</a> <a href ="/abs/2503.17082" title="Abstract" id="2503.17082"> arXiv:2503.17082 </a> [<a href="/pdf/2503.17082" title="Download PDF" id="pdf-2503.17082" aria-labelledby="pdf-2503.17082">pdf</a>, <a href="https://arxiv.org/html/2503.17082v1" title="View HTML" id="html-2503.17082" aria-labelledby="html-2503.17082" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17082" title="Other formats" id="oth-2503.17082" aria-labelledby="oth-2503.17082">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Collapse of Rotating White Dwarfs and Multimessenger Signals </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kuroda,+T">Takami Kuroda</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kawaguchi,+K">Kyohei Kawaguchi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Shibata,+M">Masaru Shibata</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 20 pages, 13 figures, submitted to MNRAS </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> We present results of numerical relativity simulations of core collapse of rotating magnetized white dwarfs (WDs) in three dimension, aiming at discussing the explosion dynamics and associate multi-messenger signals: gravitational waves (GWs), neutrinos, and electromagnetic counterparts. All WDs initiate gravitational collapse due to electron captures and then experience prompt type explosions after the proto neutron star formation. We observe the explosions dominated by a bipolar structure and the emergence of strong spiral waves in rapidly rotating models. The spiral waves facilitate to increase both the explosion energy and ejecta mass, though the final values still fall in the category of low explosion energy supernovae with small ejecta mass. The spiral waves also produce strong GWs, which may expand the horizon distance of such events against GWs up to $\sim 10$ Mpc for third-generation ground-based detectors. Additionally as an intriguing implication, we demonstrate that such accretion or merger induced collapse of WDs might be able to explain some of the rapidly evolving optical transients, such as fast blue optical transients (FBOTs), as previously suggested. Based on the simulation results together with several assumptions, we confirm that the magnetar may account for the brighter side of observed FBOTs, while a combination of ejecta-envelope interaction which can be also followed by radioactive decay of heavy elements synthesized along with the explosion might still explain the fainter branch even in the absence of magnetar formation. </p> </div> </dd> <dt> <a name='item40'>[40]</a> <a href ="/abs/2503.17083" title="Abstract" id="2503.17083"> arXiv:2503.17083 </a> [<a href="/pdf/2503.17083" title="Download PDF" id="pdf-2503.17083" aria-labelledby="pdf-2503.17083">pdf</a>, <a href="https://arxiv.org/html/2503.17083v1" title="View HTML" id="html-2503.17083" aria-labelledby="html-2503.17083" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17083" title="Other formats" id="oth-2503.17083" aria-labelledby="oth-2503.17083">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> TESS light curves and period changes in low-mass eclipsing binary BB Persei </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wolf,+M">Marek Wolf</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zasche,+P">Petr Zasche</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zejda,+M">Miloslav Zejda</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ma%C5%A1ek,+M">Martin Ma拧ek</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mudray,+A">Andrej Mudray</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ku%C4%8D%C3%A1kov%C3%A1,+H">Hana Ku膷谩kov谩</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Og%C5%82oza,+W">Waldemar Og艂oza</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Merc,+J">Jaroslav Merc</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=K%C3%A1ra,+J">Jan K谩ra</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dienstbier,+V">Vojt臎ch Dienstbier</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Accepted for publication in New Astronomy. 9 pages, 4 figures, 8 tables. This is the authors' version of the accepted manuscript </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span> </div> <p class='mathjax'> We present a detailed analysis of the low-mass detached eclipsing binary system BB Persei, which contains two K-type stars in a circular orbit with a short period of 0.4856 d. We used light curves from the Transiting Exoplanet Survey Satellite, which observed BB Per in five sectors, to determine its photometric properties and a precise orbital ephemeris. The solution of the TESS light curve in Phoebe results in a detached configuration, where the temperature of the primary component was fixed to $T_1 = 5~300$ K according to Lamost, which gives us $T_2 = 5~050 \pm 50$ K for the secondary. The spectral type of the primary component was derived as K0 and the photometric mass ratio was estimated $q = 0.90$. Slow period changes on the current O-C diagram spanning the past 25 years indicate the presence of a third body orbiting the eclipsing pair with an orbital period of about 22 years. The companion could be a red dwarf of spectral type M6 - M7 with a minimal mass of about 0.1 M$_{\odot}$. The characteristics and temporal variation of the dark region on the surface of the secondary component were estimated. </p> </div> </dd> <dt> <a name='item41'>[41]</a> <a href ="/abs/2503.17087" title="Abstract" id="2503.17087"> arXiv:2503.17087 </a> [<a href="/pdf/2503.17087" title="Download PDF" id="pdf-2503.17087" aria-labelledby="pdf-2503.17087">pdf</a>, <a href="https://arxiv.org/html/2503.17087v1" title="View HTML" id="html-2503.17087" aria-labelledby="html-2503.17087" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17087" title="Other formats" id="oth-2503.17087" aria-labelledby="oth-2503.17087">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Searching for continuous gravitational waves from slowly spinning neutron stars with DECIGO, Big Bang Observer, Einstein Telescope and Cosmic Explorer </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pagliaro,+G">Gianluca Pagliaro</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Papa,+M+A">Maria Alessandra Papa</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ming,+J">Jing Ming</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Muratore,+M">Martina Muratore</a></div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; General Relativity and Quantum Cosmology (gr-qc) </div> <p class='mathjax'> We consider stably rotating highly magnetised neutron stars and glitching pulsars. We discuss the prospects for detecting continuous gravitational waves from these sources below 20 Hz with next-generation ground-based facilities such as the Einstein Telescope and Cosmic Explorer and space-based observatories such as DECIGO and Big Bang Observer. We demonstrate that these constitute interesting science targets. We use a robust sensitivity estimation method for future searches based on demonstrated performance. We show that the spin-down upper limit on the gravitational wave amplitude of more than 90% of all highly magnetised pulsars and magnetars suitable for a years-long fully coherent search, exceeds the smallest gravitational wave amplitude estimated detectable with DECIGO and Big Bang Observer. We find that the hidden magnetar candidate PSR J1852+0040 can be detected by Cosmic Explorer if it is emitting at least at 20% of its spin-down luminosity. Finally, post-glitch transient continuous gravitational waves from magnetars are an interesting target for deci-Hz detectors, with all but one of the recorded glitches giving rise to a spin-down limit signal above the smallest detectable level. </p> </div> </dd> <dt> <a name='item42'>[42]</a> <a href ="/abs/2503.17090" title="Abstract" id="2503.17090"> arXiv:2503.17090 </a> [<a href="/pdf/2503.17090" title="Download PDF" id="pdf-2503.17090" aria-labelledby="pdf-2503.17090">pdf</a>, <a href="https://arxiv.org/html/2503.17090v1" title="View HTML" id="html-2503.17090" aria-labelledby="html-2503.17090" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17090" title="Other formats" id="oth-2503.17090" aria-labelledby="oth-2503.17090">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Closeby Habitable Exoplanet Survey (CHES). III. Retrieval of Planetary Masses in Binaries Using the N-body Model with RV and Astrometry Synergy </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Huang,+X">Xiumin Huang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ji,+J">Jianghui Ji</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bao,+C">Chunhui Bao</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tan,+D">Dongjie Tan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wang,+S">Su Wang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dong,+Y">Yao Dong</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chen,+G">Guo Chen</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 18 pages, 8 figures, accepted for publication in ApJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Earth and Planetary Astrophysics (astro-ph.EP)</span>; Astrophysics of Galaxies (astro-ph.GA); Instrumentation and Methods for Astrophysics (astro-ph.IM); Solar and Stellar Astrophysics (astro-ph.SR) </div> <p class='mathjax'> Given that secular perturbations in a binary system not only excite high orbital eccentricities but also alter the planetary orbital inclination, the classical Keplerian orbital model is no longer applicable for orbital retrieval. The combination of a dynamical model and observational data is essential for characterizing the configuration and planetary mass in close binaries. We calculate the theoretical radial velocity (RV) signal in the N-body framework and observe a drift in the RV semi-amplitude, which leads to a reduction in the $m$sin$i$ detection threshold by 20 $M_{\oplus}$, with $\sim$ 100% detection probability in the $m_1$sin$i_1$-$a_1$ parameter space. High-precision RV data with an accuracy of 1 m/s can detect such dynamical effects. For four close-in binaries-GJ 86, GJ 3021, HD 196885, and HD 41004, the deviation between the minimum mass derived from the Keplerian and N-body models is found to be $> 0.2 ~ M_{\mathrm{Jup}}$. High-precision astrometric data are also necessary to resolve the 3D orbits and true masses exoplanets. We generate astrometric simulation data with accuracies corresponding to Gaia (57.8 $\mu$as) and the Closeby Habitable Exoplanet Survey (CHES) (1 $\mu$as), respectively. Joint orbit fitting is performed for RV + Gaia and RV + CHES synergy methods. Compared with the fitting results from the astrometry-only model, the synergy models more effectively constrain the range of orbital inclinations. Using simulation data, we derive precise uncertainties for the true planetary mass, which are critical for determining the evolution of planets around binary stars and multi-planet systems. </p> </div> </dd> <dt> <a name='item43'>[43]</a> <a href ="/abs/2503.17099" title="Abstract" id="2503.17099"> arXiv:2503.17099 </a> [<a href="/pdf/2503.17099" title="Download PDF" id="pdf-2503.17099" aria-labelledby="pdf-2503.17099">pdf</a>, <a href="https://arxiv.org/html/2503.17099v1" title="View HTML" id="html-2503.17099" aria-labelledby="html-2503.17099" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17099" title="Other formats" id="oth-2503.17099" aria-labelledby="oth-2503.17099">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> An Energy-Angular Momentum Phase Function for Rubble Pile Asteroids </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Scheeres,+D">D.J. Scheeres</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Accepted for publication in Icarus </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Earth and Planetary Astrophysics (astro-ph.EP)</span> </div> <p class='mathjax'> This work analyzes the energetics of asteroid rubble piles in order to understand what asteroid morphologies should naturally arise from their formation and evolution process. In doing this, a phase diagram is developed that maps out the range of final minimum energy states that a collapsing gravitational aggregate can achieve as a function of total angular momentum and mass distribution. This is developed assuming properties associated with rubble pile asteroids, and can provide insight into the formation and subsequent evolution of contact binaries and orbital binaries in the solar system as an outcome of catastrophic disruptions. The system angular momentum is used as an independent parameter, combined with resulting minimum energy configurations as a simple function of mass morphology of the final system. The configuration of systems with an energy boosted above the minimum energy state are also considered. This paper considers an ideal case, but outlines general results that can be continued for more precise models of distributed granular media modeled using continuum models or using discrete element models. </p> </div> </dd> <dt> <a name='item44'>[44]</a> <a href ="/abs/2503.17104" title="Abstract" id="2503.17104"> arXiv:2503.17104 </a> [<a href="/pdf/2503.17104" title="Download PDF" id="pdf-2503.17104" aria-labelledby="pdf-2503.17104">pdf</a>, <a href="https://arxiv.org/html/2503.17104v1" title="View HTML" id="html-2503.17104" aria-labelledby="html-2503.17104" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17104" title="Other formats" id="oth-2503.17104" aria-labelledby="oth-2503.17104">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Observations of complex organic molecules in the gas phase of the interstellar medium </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Jimenez-Serra,+I">Izaskun Jimenez-Serra</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Codella,+C">Claudio Codella</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Belloche,+A">Arnaud Belloche</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> To appear in Handbook of Astrochemistry </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span>; Solar and Stellar Astrophysics (astro-ph.SR) </div> <p class='mathjax'> Thanks to the advent of sensitive and broad bandwidth instrumentation, complex organic molecules (COMs) have been found in a wide variety of interstellar environments, not only in our Galaxy but also in external galaxies up to a redshift of 0.89. The detection of COMs in cold environments such as starless or prestellar cores has challenged our understanding of COM formation and new ideas are being implemented in chemical models and explored in laboratory experiments. At the protostellar stage, the advent of new interferometers such as the Atacama Large Millimeter/submillimeter Array (ALMA) has allowed the mapping of the weak emission of COMs in the protostellar envelopes and protoplanetary disks around both low-mass and high-mass protostars, pinpointing their location and revealing differentiation between the different families of molecules. In this way, thermal and non-thermal desorption mechanisms can be probed, constraining the efficiency of formation of COMs in the gas phase versus on grain surfaces. Some degree of continuity in the COM composition is found from the early to late stages of star formation, suggesting that a significant fraction of COMs are formed at the initial conditions of star formation. For extreme environments such as the Galactic Center, cosmic rays and low-velocity shocks seem to influence the COM composition of low and high-density gas components. The spectral confusion limit will be a major challenge for the detection of new COMs in future spectroscopic surveys. However, low-frequency interferometers targeting sources with low-excitation temperatures may help to overcome this limit. </p> </div> </dd> <dt> <a name='item45'>[45]</a> <a href ="/abs/2503.17117" title="Abstract" id="2503.17117"> arXiv:2503.17117 </a> [<a href="/pdf/2503.17117" title="Download PDF" id="pdf-2503.17117" aria-labelledby="pdf-2503.17117">pdf</a>, <a href="https://arxiv.org/html/2503.17117v1" title="View HTML" id="html-2503.17117" aria-labelledby="html-2503.17117" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17117" title="Other formats" id="oth-2503.17117" aria-labelledby="oth-2503.17117">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> A New Statistical Model of Star Speckles for Learning to Detect and Characterize Exoplanets in Direct Imaging Observations </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bodrito,+T">Th茅o Bodrito</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Flasseur,+O">Olivier Flasseur</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mairal,+J">Julien Mairal</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ponce,+J">Jean Ponce</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Langlois,+M">Maud Langlois</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lagrange,+A">Anne-Marie Lagrange</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Accepted to CVPR 2025 </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Instrumentation and Methods for Astrophysics (astro-ph.IM)</span>; Computer Vision and Pattern Recognition (cs.CV); Machine Learning (cs.LG); Applications (stat.AP) </div> <p class='mathjax'> The search for exoplanets is an active field in astronomy, with direct imaging as one of the most challenging methods due to faint exoplanet signals buried within stronger residual starlight. Successful detection requires advanced image processing to separate the exoplanet signal from this nuisance component. This paper presents a novel statistical model that captures nuisance fluctuations using a multi-scale approach, leveraging problem symmetries and a joint spectral channel representation grounded in physical principles. Our model integrates into an interpretable, end-to-end learnable framework for simultaneous exoplanet detection and flux estimation. The proposed algorithm is evaluated against the state of the art using datasets from the SPHERE instrument operating at the Very Large Telescope (VLT). It significantly improves the precision-recall trade-off, notably on challenging datasets that are otherwise unusable by astronomers. The proposed approach is computationally efficient, robust to varying data quality, and well suited for large-scale observational surveys. </p> </div> </dd> <dt> <a name='item46'>[46]</a> <a href ="/abs/2503.17133" title="Abstract" id="2503.17133"> arXiv:2503.17133 </a> [<a href="/pdf/2503.17133" title="Download PDF" id="pdf-2503.17133" aria-labelledby="pdf-2503.17133">pdf</a>, <a href="https://arxiv.org/html/2503.17133v1" title="View HTML" id="html-2503.17133" aria-labelledby="html-2503.17133" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17133" title="Other formats" id="oth-2503.17133" aria-labelledby="oth-2503.17133">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Tidal Amplitudes in the Magellanic Cloud Population of Heartbeat Stars </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=MacLeod,+M">Morgan MacLeod</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Loeb,+A">Abraham Loeb</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Submitted to AAS journals, we welcome feedback or comments </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span>; Astrophysics of Galaxies (astro-ph.GA) </div> <p class='mathjax'> Heartbeat (HB) stars exhibit pulses in their light curves once per orbit due to ellipsoidal distortions from strong tides at periapse. We analyze the population of HB stars in the Magellanic Clouds captured by the OGLE survey, and provide broadband spectral energy distribution fitting to estimate physical properties of the HB stars. The HB stars span a wide range of luminosities, radii, and effective temperatures. However, we find that they cluster near loci of strong tidal influence at periapse, indicating that in nearly all cases, strong tides are indeed responsible for their photometric variability. HB stars tend to populate regions away from the main sequence, where stellar evolution is particularly rapid. We examine the distribution of tidal amplitudes, and show that these can be interpreted through a simplified model of radius growth through stellar evolution and orbital circularization through linear tidal dissipation. When we compare rates of tidal dissipation, we find differences between the modeled modified tidal quality factor among hot ($T_{\rm eff}>6250$~K), $Q_\ast' \gtrsim 10^7$, and cool ($T_{\rm eff}<6250$~K), $Q_\ast'\sim 10^5$, stars, which is qualitatively consistent with models of efficient tidal dissipation in the convective envelopes of cool stars. We find that this model can reproduce the observed observed locations and amplitudes of HB stars in the Hertzsprung-Russell diagram. The hot stars, in particular, extend to amplitudes near, but not beyond, the threshold for nonlinear tidal wave breaking on stellar surfaces, suggesting a physical saturation of tidal amplitudes at this threshold. </p> </div> </dd> <dt> <a name='item47'>[47]</a> <a href ="/abs/2503.17150" title="Abstract" id="2503.17150"> arXiv:2503.17150 </a> [<a href="/pdf/2503.17150" title="Download PDF" id="pdf-2503.17150" aria-labelledby="pdf-2503.17150">pdf</a>, <a href="https://arxiv.org/html/2503.17150v1" title="View HTML" id="html-2503.17150" aria-labelledby="html-2503.17150" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17150" title="Other formats" id="oth-2503.17150" aria-labelledby="oth-2503.17150">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Melnick 39 is a very massive intermediate-period colliding-wind binary </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pollock,+A+M+T">A. M. T. Pollock</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Crowther,+P+A">P. A. Crowther</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bestenlehner,+J+M">J. M. Bestenlehner</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Broos,+P+S">Patrick S. Broos</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Townsley,+L+K">Leisa K. Townsley</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 7 pages, 7 Figures, 5 Tables, accepted for publication by MNRAS </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span> </div> <p class='mathjax'> Individually identified binary systems of very massive stars define fixed points on possible evolutionary pathways that begin with extreme star formation and end in either coalescence of compact remnants or complete disruption as pair-production supernovae. The LMC star Melnick 39 in the Tarantula Nebula is revealed to be an eccentric ($e = 0.618\pm0.014$) binary system of reasonably long period from time-series analysis of Chandra T-ReX X-ray observations. Its X-ray luminosity scales with the inverse of the binary separation, as expected for colliding-wind binaries in the adiabatic regime. The inclusion of optical time-series spectroscopy from the VLT FLAMES Tarantula Survey and archival HST spectroscopy confirms Melnick 39 as a double-lined O2.5If/WN6+O3V-III spectroscopic binary with orbital period near 648 days. We obtain a mass ratio of $q = 0.76 \pm 0.06$, and minimum dynamical masses of $105\pm11$ and $80\pm11$ $M_{solar}$ for the O2.5If/WN6 and O3V-III components, plus photometric evidence for an orbital inclination near 90 degrees. Disentangled spectroscopy allows the physical and wind properties of the primary to be determined, including $T_{\ast}$ = 44 kK, $\log L/L_{solar}$ = 6.2, $\log \dot{M}/M_{solar}$ yr$^{-1}$ = $-5.0$. Its dynamical mass agrees closely with $109 M_{solar}$ obtained from the mass-luminosity relation of very massive stars. </p> </div> </dd> <dt> <a name='item48'>[48]</a> <a href ="/abs/2503.17180" title="Abstract" id="2503.17180"> arXiv:2503.17180 </a> [<a href="/pdf/2503.17180" title="Download PDF" id="pdf-2503.17180" aria-labelledby="pdf-2503.17180">pdf</a>, <a href="https://arxiv.org/html/2503.17180v1" title="View HTML" id="html-2503.17180" aria-labelledby="html-2503.17180" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17180" title="Other formats" id="oth-2503.17180" aria-labelledby="oth-2503.17180">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Chlorine abundances in star-forming regions of the local Universe </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Orte-Garc%C3%ADa,+M">M. Orte-Garc铆a</a> (1 and 2), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Esteban,+C">C. Esteban</a> (1 and 2), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=M%C3%A9ndez-Delgado,+J+E">J. E. M茅ndez-Delgado</a> (3), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Garc%C3%ADa-Rojas,+J">J. Garc铆a-Rojas</a> (1 and 2), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Arellano-C%C3%B3rdova,+K+Z">K. Z. Arellano-C贸rdova</a> (4), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rosales-Ortega,+F+F">F. F. Rosales-Ortega</a> (5), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Reyes-Rodr%C3%ADguez,+E">E. Reyes-Rodr铆guez</a> (2 and 6) ((1) IAC, Spain, (2) ULL, Spain, (3) UNAM, M茅xico (4) IfA, United Kingdom, (5) INAOE, M茅xico, (6) ING, Spain)</div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 14 pages, 11 figures, 4 tables (4 longtables online). Accepted for publication in Astronomy and Astrophysics </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> Aims. We study the behaviour of Cl abundance and its ratios with respect to O, S and Ar abundances in a sample of more than 200 spectra of Galactic and extragalactic H ii regions and star-forming galaxies (SFGs) of the local Universe. Methods. We use the DEep Spectra of Ionised REgions Database (DESIRED) Extended project (DESIRED-E) that comprises more than 2000 spectra of H ii regions and SFGs with direct determinations of electron temperature ($T_e$). From this database we select those spectra where it is possible to determine the Cl$^{2+}$ abundance and whose line ratios meet certain observational criteria. We calculate the physical conditions and Cl, O, S and Ar abundances in an homogeneous manner for all the spectra. We compare with results of photoionisation models to carry out an analysis of which is the most appropriate $T_e$ indicator for the nebular volume where Cl$^{2+}$ lies, proposing a scheme that improves the determination of the Cl$^{2+}$ abundance. We compare the Cl/O ratios obtained using two different ionisation correction factor (ICF) schemes. We also compare the nebular Cl/O distribution with stellar determinations. Results. Our analysis indicates that the ICF scheme proposed by Izotov et al. (2006) better reproduces the observed distributions of the Cl/O ratio. We find that the log(Cl/O) vs. 12+log(O/H) and log(Cl/Ar) vs. 12+log(Ar/H) distributions are not correlated in the whole metallicity range covered by our objects indicating a lockstep evolution of those elements. In contrast, the log(Cl/S) vs. 12+log(S/H) distribution shows a weak correlation with a slight negative slope. </p> </div> </dd> <dt> <a name='item49'>[49]</a> <a href ="/abs/2503.17183" title="Abstract" id="2503.17183"> arXiv:2503.17183 </a> [<a href="/pdf/2503.17183" title="Download PDF" id="pdf-2503.17183" aria-labelledby="pdf-2503.17183">pdf</a>, <a href="https://arxiv.org/html/2503.17183v1" title="View HTML" id="html-2503.17183" aria-labelledby="html-2503.17183" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17183" title="Other formats" id="oth-2503.17183" aria-labelledby="oth-2503.17183">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Halfway to the Peak: ice absorption bands at $z\approx0.5$ with JWST MIRI/MRS </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sajina,+A">Anna Sajina</a> (Tufts University), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pope,+A">Alexandra Pope</a> (UMass Amherst), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Spoon,+H">Henrik Spoon</a> (Cornell), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Armus,+L">Lee Armus</a> (Caltech), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Eleazer,+M">Miriam Eleazer</a> (UMass Amherst), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Farrah,+D">Duncan Farrah</a> (UHawaii Manoa), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lacy,+M">Mark Lacy</a> (NRAO), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lai,+T">Thomas Lai</a> (Caltech), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=McKinney,+J">Jed McKinney</a> (University of Texas Austin), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Veilleux,+S">Sylvain Veilleux</a> (University of Maryland), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yan,+L">Lin Yan</a> (Caltech), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Young,+J">Jason Young</a> (Williams &amp; SETI)</div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 19 pages, 10 figures, accepted for publication in ApJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> This paper presents the first combined detections of CO$_2$, CO, XCN and water ices beyond the local Universe. We find gas-phase CO in addition to the solid phase CO. Our source, SSTXFLS J172458.3+591545, is a $z=0.494$ star-forming galaxy which also hosts a deeply obscured AGN. The profiles of its ice features are consistent with those of other Galactic and local galaxy sources and the implied ice mantle composition is similar to that of even more obscured sources. The ice features indicate the presence of a compact nucleus in our galaxy and allow us to place constraints on its density and temperature ($n>10^5$cm$^{-3}$ and $T=20-90K$). We infer the visual extinction towards this nucleus to be $A_V\approx6-7$. An observed plot of $\tau_{Si}$ vs. $\tau_{CO2}/\tau_{Si}$ can be viewed as a probe for both the total dustiness of a system as well as the clumpiness of the dust along the line of sight. This paper highlights the potential of using {\sl JWST} MIRI spectra to study the dust composition and geometric distribution of sources beyond the local Universe. </p> </div> </dd> <dt> <a name='item50'>[50]</a> <a href ="/abs/2503.17200" title="Abstract" id="2503.17200"> arXiv:2503.17200 </a> [<a href="/pdf/2503.17200" title="Download PDF" id="pdf-2503.17200" aria-labelledby="pdf-2503.17200">pdf</a>, <a href="https://arxiv.org/html/2503.17200v1" title="View HTML" id="html-2503.17200" aria-labelledby="html-2503.17200" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17200" title="Other formats" id="oth-2503.17200" aria-labelledby="oth-2503.17200">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Exploring the secondary peaks of autocorrelation in black hole flare movies </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhang,+Z">Zhenyu Zhang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hou,+Y">Yehui Hou</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Guo,+M">Minyong Guo</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mizuno,+Y">Yosuke Mizuno</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chen,+B">Bin Chen</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 7+5 pages, 2+3 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; General Relativity and Quantum Cosmology (gr-qc) </div> <p class='mathjax'> The strong gravitational field of a black hole bends light, forming multi-level images, yet extracting precise spacetime information from them remains challenging. In this study, we investigate how gravitational lensing leaves unique and detectable signatures in black hole movies using autocorrelation analysis. By examining the two-dimensional autocorrelation of a movie depicting a hotspot orbiting a Kerr black hole, as viewed by a near-axis observer, we identify a persistent secondary peak structure induced by gravitational lensing. Notably, these secondary peaks converge to a fixed point in the time-lag domain, largely independent of the hotspot's orbital radius. This key property suggests that combining future black hole flare observations with advanced autocorrelation analysis could effectively disentangle lensing effects from orbital dynamics, enabling direct measurement of black hole parameters. Our findings establish autocorrelation as a powerful tool for probing spacetime geometry, offering new insights into gravitational physics through time-resolved black hole images. </p> </div> </dd> <dt> <a name='item51'>[51]</a> <a href ="/abs/2503.17202" title="Abstract" id="2503.17202"> arXiv:2503.17202 </a> [<a href="/pdf/2503.17202" title="Download PDF" id="pdf-2503.17202" aria-labelledby="pdf-2503.17202">pdf</a>, <a href="https://arxiv.org/html/2503.17202v1" title="View HTML" id="html-2503.17202" aria-labelledby="html-2503.17202" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17202" title="Other formats" id="oth-2503.17202" aria-labelledby="oth-2503.17202">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Stream Automatic Detection with Convolutional Neural Network (SAD-CNN) </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Vera-Casanova.,+A">Alex Vera-Casanova.</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gonzalez,+N+M">Nicolas Monsalves Gonzalez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=G%C3%B3mez,+F+A">Facundo A. G贸mez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Arancibia.,+M+J">Marcelo Jaque Arancibia.</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fontirroig,+V">Valentina Fontirroig</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pallero.,+D">Diego Pallero.</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pakmor.,+R">R眉diger Pakmor.</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=van+de+Voort.,+F">Freeke van de Voort.</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Grand.,+R+J+J">Robert J. J. Grand.</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bieri.,+R">Rebekka Bieri.</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Marinacci,+F">Federico Marinacci</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 15 pages, 15 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> Context. Galactic halos host faint substructures, such as stellar streams and shells, which provide insights into the hierarchical assembly history of galaxies. To date, such features have been identified in external galaxies by visual inspection. However, with the advent of larger and deeper surveys and the associated increase in data volume, this methodology is becoming impractical. Aims. Here we aim to develop an automated method to detect low surface brightness features in galactic stellar halos. Moreover, we seek to quantify its performance when considering progressively more complex data sets, including different stellar disc orientations and redshifts. Methods. We develop the Stream Automatic Detection with Convolutional Neural Networks, SAD-CNN. This tool is trained on mock surface brightness maps obtained from simulations of the Auriga Project. The model incorporates transfer learning, data augmentation and balanced datasets to optimise its detection capabilities at surface brightness limiting magnitudes ranging from 27 to 31 mag arcsec^-2. Results. The iterative training approach, coupled with transfer learning, allowed the model to adapt to increasingly challenging datasets, achieving precision and recall metrics above 80% in all considered scenarios. The use of a well-balanced training dataset is critical for mitigating biases, ensuring that the CNN accurately distinguishes between galaxies with and without streams. Conclusions. SAD-CNN is a reliable and scalable tool for automating the detection of faint substructures in galactic halos. Its adaptability makes it well-suited for future applications, including the analysis of data from upcoming large astronomical surveys (such as LSST, JWT). </p> </div> </dd> <dt> <a name='item52'>[52]</a> <a href ="/abs/2503.17206" title="Abstract" id="2503.17206"> arXiv:2503.17206 </a> [<a href="/pdf/2503.17206" title="Download PDF" id="pdf-2503.17206" aria-labelledby="pdf-2503.17206">pdf</a>, <a href="https://arxiv.org/html/2503.17206v1" title="View HTML" id="html-2503.17206" aria-labelledby="html-2503.17206" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17206" title="Other formats" id="oth-2503.17206" aria-labelledby="oth-2503.17206">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Dark Matter (S)pins the Planet </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Shi,+H">Haihao Shi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhou,+J">Junda Zhou</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Huang,+Z">Zhenyang Huang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lv,+G">Guoliang Lv</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chen,+X">Xuefei Chen</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 8 pages, 4 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; Cosmology and Nongalactic Astrophysics (astro-ph.CO); Earth and Planetary Astrophysics (astro-ph.EP); High Energy Physics - Phenomenology (hep-ph) </div> <p class='mathjax'> Dark matter heating in planets has been proposed as a potential probe for dark matter detection. Assuming near-equilibrium, we find that dark matter energy input raises planetary temperature and accelerates rotation. The energy distribution depends on planetary properties and external input, suggesting that previous studies have overestimated its heating effect. When dark matter density is high, planetary rotation stabilizes earlier and is primarily governed by dark matter. For Earth, our model predicts a 0.015 K temperature increase and a $10^{-8}$ rad/s angular velocity increase over 100 years. </p> </div> </dd> <dt> <a name='item53'>[53]</a> <a href ="/abs/2503.17216" title="Abstract" id="2503.17216"> arXiv:2503.17216 </a> [<a href="/pdf/2503.17216" title="Download PDF" id="pdf-2503.17216" aria-labelledby="pdf-2503.17216">pdf</a>, <a href="https://arxiv.org/html/2503.17216v1" title="View HTML" id="html-2503.17216" aria-labelledby="html-2503.17216" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17216" title="Other formats" id="oth-2503.17216" aria-labelledby="oth-2503.17216">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> High energy time lags of Gamma Ray Bursts </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Maraventano,+C">C. Maraventano</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ghirlanda,+G">G. Ghirlanda</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Nava,+L">L. Nava</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Di+Salvo,+T">T. Di Salvo</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Leone,+W">W. Leone</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Iaria,+R">R. Iaria</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Burderi,+L">L. Burderi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tsvetkova,+A">A. Tsvetkova</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 18 pages, 11 figures, Submitted to Astronomy & Astrophysics (A&A) </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> Positive lags between the arrival time of different photon energies are commonly observed in Gamma-Ray Bursts (GRBs), where soft photons lag behind harder ones. However, some GRBs exhibit the opposite behavior. In particular, Fermi LAT observations have revealed that high-energy photons often have a delayed onset. We explore spectral lags as a tool to identify emission components, analyzing Fermi GBM and LAT Low Energy (LLE) data. Using the Discrete Correlation Function method, we compute spectral lags in four energy bands (10 keV-100 MeV) for 70 GRBs from the LLE Catalog. Lags between 10 keV and 1 MeV are mostly positive (76%), possibly due to a hard-to-soft spectral evolution. However, lags between the LLE band (30-100 MeV) and GBM (10-100 keV) vary: 40% are positive, while 37% are negative. These negative lags suggest the delayed emergence of an additional high-energy component. Spectral analysis of 56 GRBs reveals that negative lags correspond to an LLE spectral index harder than the GBM high-energy power law. LLE spectral lags can thus serve as a diagnostic tool to identify and characterize emission components, emphasizing the importance of combining temporal and spectral analyses to better understand GRB emission mechanisms. </p> </div> </dd> <dt> <a name='item54'>[54]</a> <a href ="/abs/2503.17218" title="Abstract" id="2503.17218"> arXiv:2503.17218 </a> [<a href="/pdf/2503.17218" title="Download PDF" id="pdf-2503.17218" aria-labelledby="pdf-2503.17218">pdf</a>, <a href="https://arxiv.org/html/2503.17218v1" title="View HTML" id="html-2503.17218" aria-labelledby="html-2503.17218" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17218" title="Other formats" id="oth-2503.17218" aria-labelledby="oth-2503.17218">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Celestial sunflowers -- Survival of rings around small planetary bodies under solar radiation pressure </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Regaly,+Z">Zs. Regaly</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Frohlich,+V">V. Frohlich</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kiss,+C">Cs. Kiss</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Accepted for publication in A&A. 14 pages, 9 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Earth and Planetary Astrophysics (astro-ph.EP)</span> </div> <p class='mathjax'> Context: Rings around giant planets are a common feature of the solar system. Even though solar radiation pressure is known to destabilize rings by exciting the orbital eccentricity of its particles, the Centaur Chariklo (and possibly Chiron), the dwarf planet Haumea, and trans-Neptunian object Quaoar also host rings of solid material. Aims: We explore the dynamical evolution of rings around spherical Chariklo and Haumea analogs, assuming different particle sizes and tilt angles with respect to the planetary orbital plane of the ring. Methods: The ring dynamics were studied using a GPU-based N-body integrator with an 8th-order Hermite scheme for several thousand years, corresponding to 10 solar orbits. The simulations took into account the gravitational effects of the planet and the Sun, radiation pressure, and the shadow cast by the planet. Results: Two families of rings have been identified depending on the ring tilt angle. Slightly tilted rings (<=40 deg) are unstable under a critical particle size. Highly tilted rings (>=50 deg), however, show instability only for a range of particle sizes that spans 1-10 times the critical size. The planetary shadow reduces the critical size by a factor of five and extends the instability region to 0.1-10 times this newly identified critical size. Conclusions: The stabilization of highly inclined rings occurs because the plane of the ring is forced to be perpendicular to the Solar radiation. As a result, the plane of the ring rotates as the planetary bodies revolves: always facing the sun, like a celestial sunflower. Rings which are closely aligned to the orbital plane of the host planet, such as Haumea and Quaoar, presumably consist of particles with a size at least 1-4 um. However, particles in the rings which are highly tilted, like that around Chariklo and Chiron, should consist of particles <=2.5-15 um or >=60-300 um. </p> </div> </dd> <dt> <a name='item55'>[55]</a> <a href ="/abs/2503.17249" title="Abstract" id="2503.17249"> arXiv:2503.17249 </a> [<a href="/pdf/2503.17249" title="Download PDF" id="pdf-2503.17249" aria-labelledby="pdf-2503.17249">pdf</a>, <a href="https://arxiv.org/html/2503.17249v1" title="View HTML" id="html-2503.17249" aria-labelledby="html-2503.17249" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17249" title="Other formats" id="oth-2503.17249" aria-labelledby="oth-2503.17249">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> On the origin of radio polarization in pulsar polar caps </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ben%C3%A1%C4%8Dek,+J">Jan Ben谩膷ek</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Jessner,+A">Axel Jessner</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pohl,+M">Martin Pohl</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rievajov%C3%A1,+T">Tatiana Rievajov谩</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Oswald,+L+S">Lucy S. Oswald</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 13 pages, 9 figures, 1 table; Submitted to A&A </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> A knowledge of polarization properties of coherent radio waves escaping pulsar polar caps is crucial for calculating radiative transfer through the magnetosphere and for obtaining specific predictions of observable radio properties. We describe the pair cascades in the pulsar polar cap, and for the first time, determine the Stokes parameters of the escaping radio waves from first-principle kinetic simulations for a pulsar with an inclination angle of the magnetic axis 60掳. <br>Our model provides a quantitative and qualitative explanation of the observed pulsar radio powers and spectra, the pulse profiles and polarization curves, their temporal variability, the strong Stokes L and weak Stokes V polarization components, as well as the fact that linear polarization decreases with frequency and the non-existence of a radius to frequency relationship. We find that the radio emission from the polar cap can produce a diverse range of observed pulsar properties, including single or double peaked profiles. Most of the Stokes V curves from our simulations appear to be antisymmetric, but symmetric curves are also present at some viewing angles. Although the PA swing of the radiation from the polar cap can be fitted by the rotating vector model (RVM) for most viewing angles, the angles obtained from the RVM do not correspond to the angular distance of the observer from the magnetic axis. Instead, the PA is directly related to the plasma flows in the polar cap and not to the dipole geometry of the magnetic field. The observed range of other polarization features, in addition to our results, can be explained by propagation effects which are not part of the simulation. <br>Our simulations demonstrate that pair discharges determine the majority of its typically observed properties. The usage of RVM for estimations of the magnetic field geometry from observations needs to be reevaluated. </p> </div> </dd> <dt> <a name='item56'>[56]</a> <a href ="/abs/2503.17258" title="Abstract" id="2503.17258"> arXiv:2503.17258 </a> [<a href="/pdf/2503.17258" title="Download PDF" id="pdf-2503.17258" aria-labelledby="pdf-2503.17258">pdf</a>, <a href="https://arxiv.org/html/2503.17258v1" title="View HTML" id="html-2503.17258" aria-labelledby="html-2503.17258" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17258" title="Other formats" id="oth-2503.17258" aria-labelledby="oth-2503.17258">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> On the manifest link between Terzan 5 and the Galactic bulge </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Origlia,+L">L. Origlia</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ferraro,+F+R">F. R. Ferraro</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fanelli,+C">C. Fanelli</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lanzoni,+B">B. Lanzoni</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Massari,+D">D. Massari</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dalessandro,+E">E. Dalessandro</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pallanca,+C">C. Pallanca</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 9 pages, 4 figures. Accepted for publication by A&A </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span>; Solar and Stellar Astrophysics (astro-ph.SR) </div> <p class='mathjax'> We address the chemical link between Terzan 5 (hereafter Ter5) and the Bulge, as probed by the observed distributions of [$\alpha$/Fe] abundance ratios with varying [Fe/H] and by suitable statistical tests to evaluate their significance. We also present a comprehensive review of the kinematic and evolutionary properties of Ter5, based on all the available observational signatures and the scenarios proposed so far in the literature for the formation and evolution of Ter5, based on these observational facts and the recent modeling of its star formation and chemical enrichment history. This analysis confirms the complex nature of this massive stellar system, with robust evidences of a bulge in-situ formation and of a subsequent evolution that cannot be simply explained by a single merging/accretion event of two globulars or a globular and a giant molecular cloud, as proposed in the literature, but it requires a more complex star formation likely accompanied by some self-enrichment. </p> </div> </dd> <dt> <a name='item57'>[57]</a> <a href ="/abs/2503.17271" title="Abstract" id="2503.17271"> arXiv:2503.17271 </a> [<a href="/pdf/2503.17271" title="Download PDF" id="pdf-2503.17271" aria-labelledby="pdf-2503.17271">pdf</a>, <a href="https://arxiv.org/html/2503.17271v1" title="View HTML" id="html-2503.17271" aria-labelledby="html-2503.17271" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17271" title="Other formats" id="oth-2503.17271" aria-labelledby="oth-2503.17271">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> The SPT-Deep Cluster Catalog: Sunyaev-Zel'dovich Selected Clusters from Combined SPT-3G and SPTpol Measurements over 100 Square Degrees </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kornoelje,+K">K. Kornoelje</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bleem,+L+E">L. E. Bleem</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rykoff,+E+S">E. S. Rykoff</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Abbott,+T+M+C">T. M. C. Abbott</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ade,+P+A+R">P. A. R. Ade</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Aguena,+M">M. Aguena</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Alves,+O">O. Alves</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Anderson,+A+J">A. J. Anderson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Andrade-Oliveira,+F">F. Andrade-Oliveira</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ansarinejad,+B">B. Ansarinejad</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Archipley,+M">M. Archipley</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ashby,+M+L+N">M. L. N. Ashby</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Austermann,+J+E">J. E. Austermann</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bacon,+D">D. Bacon</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Balkenhol,+L">L. Balkenhol</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Beall,+J+A">J. A. Beall</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Benabed,+K">K. Benabed</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bender,+A+N">A. N. Bender</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Benson,+B+A">B. A. Benson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bianchini,+F">F. Bianchini</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bocquet,+S">S. Bocquet</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bouchet,+F+R">F. R. Bouchet</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Brooks,+D">D. Brooks</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Burke,+D+L">D. L. Burke</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Calzadilla,+M">M. Calzadilla</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Camphuis,+E">E. Camphuis</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Carlstrom,+J+E">J. E. Carlstrom</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rosell,+A+C">A. Carnero Rosell</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Carretero,+J">J. Carretero</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chang,+C+L">C. L. Chang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chaubal,+P">P. Chaubal</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chiang,+H+C">H. C. Chiang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chichura,+P+M">P. M. Chichura</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chokshi,+A">A. Chokshi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chou,+T">T.-L. Chou</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Citron,+R">R. Citron</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Coerver,+A">A. Coerver</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Moran,+C+C">C. Corbett Moran</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Costanzi,+M">M. Costanzi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Crawford,+T+M">T. M. Crawford</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Crites,+A+T">A. T. Crites</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=da+Costa,+L+N">L. N. da Costa</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Daley,+C">C. Daley</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=de+Haan,+T">T. de Haan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=De+Vicente,+J">J. De Vicente</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Desai,+S">S. Desai</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dibert,+K+R">K. R. Dibert</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dobbs,+M+A">M. A. Dobbs</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Doel,+P">P. Doel</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Doohan,+M">M. Doohan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Doussot,+A">A. Doussot</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dutcher,+D">D. Dutcher</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Everett,+W">W. Everett</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Everett,+S">S. Everett</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Feng,+C">C. Feng</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ferguson,+K+R">K. R. Ferguson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ferrero,+I">I. Ferrero</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fichman,+K">K. Fichman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Flaugher,+B">B. Flaugher</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Floyd,+B">B. Floyd</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Foster,+A">A. Foster</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Friedel,+D">D. Friedel</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Frieman,+J">J. Frieman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Galli,+S">S. Galli</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gallicchio,+J">J. Gallicchio</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gambrel,+A+E">A. E. Gambrel</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Garc'ia-Bellido,+J">J. Garc'ia-Bellido</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gardner,+R+W">R. W. Gardner</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gassis,+R">R. Gassis</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gatti,+M">M. Gatti</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ge,+F">F. Ge</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=George,+E+M">E. M. George</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Giannini,+G">G. Giannini</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Goeckner-Wald,+N">N. Goeckner-Wald</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Grandis,+S">S. Grandis</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gruen,+D">D. Gruen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gruendl,+R+A">R. A. Gruendl</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gualtieri,+R">R. Gualtieri</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Guidi,+F">F. Guidi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mahler,+G">Guillaume Mahler</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Guns,+S">S. Guns</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gupta,+N">N. Gupta</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gutierrez,+G">G. Gutierrez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Halverson,+N+W">N. W. Halverson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hinton,+S+R">S. R. Hinton</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hivon,+E">E. Hivon</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Holder,+G+P">G. P. Holder</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hollowood,+D+L">D. L. Hollowood</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Holzapfel,+W+L">W. L. Holzapfel</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Honscheid,+K">K. Honscheid</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hood,+J+C">J. C. Hood</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hrubes,+J+D">J. D. Hrubes</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hryciuk,+A">A. Hryciuk</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Huang,+N">N. Huang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hubmayr,+J">J. Hubmayr</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Irwin,+K+D">K. D. Irwin</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mena-Fern%C3%A1ndez,+J">J. Mena-Fern谩ndez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=James,+D+J">D. J. James</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=K%C3%A9ruzor%C3%A9,+F">F. K茅ruzor茅</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Khalife,+A+R">A. R. Khalife</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Submitted to ApJ, 20 pages, 9 figures, affiliations at end of document, cluster catalog available at <a href="https://pole.uchicago.edu/public/data/spt3g_deep_cluster_sample/" rel="external noopener nofollow" class="link-external link-https">this https URL</a> </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span>; Astrophysics of Galaxies (astro-ph.GA) </div> <p class='mathjax'> We present a catalog of 500 galaxy cluster candidates in the SPT-Deep field: a 100 deg$^2$ field that combines data from the SPT-3G and SPTpol surveys to reach noise levels of 3.0, 2.2, and 9.0 $\mu$K-arcmin at 95, 150, and 220 GHz, respectively. This is comparable to noise levels expected for the wide field survey of CMB-S4, a next-generation CMB experiment. Candidates are selected via the thermal Sunyaev-Zel'dovich (SZ) effect with a minimum significance of $\xi = 4.0$, resulting in a catalog of purity $\sim 89 \%$. Optical data from the Dark Energy Survey and infrared data from the Spitzer Space Telescope are used to confirm 442 cluster candidates. The clusters span $0.12 < z \lesssim 1.8$ and $1.0 \times 10^{14} M_{\odot}/h_{70} < M_{500c} < 8.7 \times 10^{14} M_{\odot}/h_{70}$. The sample's median redshift is 0.74 and the median mass is $1.7 \times 10^{14} M_{\odot}/h_{70}$; these are the lowest median mass and highest median redshift of any SZ-selected sample to date. We assess the effect of infrared emission from cluster member galaxies on cluster selection by performing a joint fit to the infrared dust and tSZ signals by combining measurements from SPT and overlapping submillimeter data from Herschel/SPIRE. We find that at high redshift ($z>1)$, the tSZ signal is reduced by $17.4^{+3.1}_{-2.9} \%$ ($3.7^{+0.7}_{-0.7}\%$) at 150 GHz (95 GHz) due to dust contamination. We repeat our cluster finding method on dust-nulled SPT maps and find the resulting catalog is consistent with the nominal SPT-Deep catalog, demonstrating dust contamination does not significantly impact the SPT-Deep selection function; we attribute this lack of bias to the inclusion of the SPT 220 GHz band. </p> </div> </dd> <dt> <a name='item58'>[58]</a> <a href ="/abs/2503.17304" title="Abstract" id="2503.17304"> arXiv:2503.17304 </a> [<a href="/pdf/2503.17304" title="Download PDF" id="pdf-2503.17304" aria-labelledby="pdf-2503.17304">pdf</a>, <a href="https://arxiv.org/html/2503.17304v1" title="View HTML" id="html-2503.17304" aria-labelledby="html-2503.17304" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17304" title="Other formats" id="oth-2503.17304" aria-labelledby="oth-2503.17304">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Chronology of our Galaxy from Gaia CMD-fitting (ChronoGal): the early formation of the Milky Way disk and the impact of Gaia-Sausage-Enceladus </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gallart,+C">C. Gallart</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fern%C3%A1ndez-Alvar,+E">E. Fern谩ndez-Alvar</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cassisi,+S">S. Cassisi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ruiz-Lara,+T">T. Ruiz-Lara</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Surot,+F">F. Surot</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Aznar-Menargues,+G">G. Aznar-Menargues</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gonz%C3%A1lez-Koda,+Y">Y. Gonz谩lez-Koda</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mirabal,+D">D. Mirabal</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Queiroz,+A">A.B. Queiroz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rivero,+A">A. Rivero</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 7 pages, 3 figures, to appear in the proceedings of IAU Symposium 395 "Stellar populations in the Milky Way and beyond" (eds. J. Mel茅ndez, C. Chiappini, R. Schiavon, M. Trevisan) </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> The derivation of precise stellar ages is considered the current major challenge to reconstruct the chronology of the Milky Way. Color-magnitude diagram (CMD)-fitting offers a robust alternative to individual age determinations via the derivation of dynamically evolved star formation histories (deSFH) and age-metallicity distributions (Gallart et al. 2024). Our new suite of routines, <a href="http://CMDft.Gaia" rel="external noopener nofollow" class="link-external link-http">this http URL</a>, specifically developed to analyse Gaia CMDs, produce deSFHs which are robust against sensible changes in the input parameters and extremely precise, providing an unprecedentedly detailed characterization of the successive events of star formation that, since its early evolution, have shaped the current Milky Way. Also important is the fact that, thanks to the high completeness of the Gaia photometric data, <a href="http://CMDft.Gaia" rel="external noopener nofollow" class="link-external link-http">this http URL</a> provides the actual number of stars and the mass involved in the different events of star formation. <br>The current analysis of the deSFH for stellar populations within 100 pc of the Sun, as well as for kinematically selected stars in the thin disk, thick disk, and halo, allows us to sketch a tentative picture of Milky Way evolution. The findings indicate that star formation commenced very early in a thick disk, with a small fraction of stars having [M/H]<-0.5 forming more than 12 Gyr ago. This phase culminated in a more prominent 12 Gyr old population with [M/H]~-0.5. Approximately 11 Gyr ago, the merger with GSE triggered an intense burst of star formation, generating most of the thick disk mass and enriching its metallicity to solar levels. Subsequently, the bulk of the star formation in the thin disk started and continues with a somewhat episodic behaviour up to the present time. </p> </div> </dd> <dt> <a name='item59'>[59]</a> <a href ="/abs/2503.17305" title="Abstract" id="2503.17305"> arXiv:2503.17305 </a> [<a href="/pdf/2503.17305" title="Download PDF" id="pdf-2503.17305" aria-labelledby="pdf-2503.17305">pdf</a>, <a href="https://arxiv.org/html/2503.17305v1" title="View HTML" id="html-2503.17305" aria-labelledby="html-2503.17305" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17305" title="Other formats" id="oth-2503.17305" aria-labelledby="oth-2503.17305">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Structure evolution with cosmic backgrounds from radio to far infrared </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Burigana,+C">Carlo Burigana</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Trombetti,+T">Tiziana Trombetti</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bonato,+M">Matteo Bonato</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gorce,+A">Ad茅lie Gorce</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Toffolatti,+L">Luigi Toffolatti</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 19 pages, 3 figures, 1 table. Accepted for publication in the electronic proceedings of Seventeenth Marcel Grossmann Meetings, 7-12 July 2024, Pescara, Italy, that will be published by World Scientific (Remo Ruffini and Gregory Vereshchagin Eds.). Summary review paper of the parallel session on Cosmic backgrounds from radio to far-IR (CM1) </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span> </div> <p class='mathjax'> Cosmic background radiation, both diffuse and discrete in nature, produced at different cosmic epochs before and after recombination, provides key information on the evolution of cosmic structures. We discuss the main classes of sources that contribute to the extragalactic background light from radio to sub-millimetre wavelenghs and the currently open question on the level of the cosmic radio background spectrum. The redshifted 21cm line signal from cosmological neutral Hydrogen during the primeval phases of cosmic structures as a probe of the cosmological reionisation process is presented, along with the route for confident detection of this signal. We then describe the basic formalism and the feasibility to study via a differential approach, based mainly on dipole analysis, the tiny imprints in the CB spectrum expected from a variety of cosmological and astrophysical processes at work during the early phases of cosmic perturbation and structure evolution. Finally, we discuss the identification of high-redshift sub-millimetre lensed galaxies with extreme magnifications in the Planck maps and their use for the comprehension of fundamental processes in early galaxy formation and evolution. </p> </div> </dd> <dt> <a name='item60'>[60]</a> <a href ="/abs/2503.17311" title="Abstract" id="2503.17311"> arXiv:2503.17311 </a> [<a href="/pdf/2503.17311" title="Download PDF" id="pdf-2503.17311" aria-labelledby="pdf-2503.17311">pdf</a>, <a href="https://arxiv.org/html/2503.17311v1" title="View HTML" id="html-2503.17311" aria-labelledby="html-2503.17311" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17311" title="Other formats" id="oth-2503.17311" aria-labelledby="oth-2503.17311">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Early solar wind and dynamo magnetic field topology predictions for (16) Psyche and other asteroids </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Anand,+A">Atma Anand</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Carroll-Nellenback,+J">Jonathan Carroll-Nellenback</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Blackman,+E+G">Eric G. Blackman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tarduno,+J+A">John A. Tarduno</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 14 pages, 2 figures (excluding Supplementary Information); Submitted to Geophysical Research Letters </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Earth and Planetary Astrophysics (astro-ph.EP)</span>; Geophysics (physics.geo-ph); Space Physics (physics.space-ph) </div> <p class='mathjax'> Asteroid (16) Psyche is a metal-rich body that might record an ancient coherent magnetization if some relict crust or mantle is preserved. Herein, we use magnetohydrodynamic simulations to predict (16) Psyche's field, assuming it has such relicts that were magnetized after nebula dispersal via one of two distinct pathways: i. an early solar wind-induced magnetization imparted after a larger body was impacted, forming the present-day asteroid and ii. a core dynamo magnetization imparted in an asteroid that is either presently largely intact or was a rubble pile. For pathway (i) we find the field to be predominantly dipolar and spin axis-aligned. For pathway (ii) we find the field to be either dipolar and spin axis-misaligned, or highly multipolar. Field topology and orientation may thus reveal key details of the nature and history of (16) Psyche, and our framework is broadly applicable to the study of magnetic fields from other asteroids. </p> </div> </dd> <dt> <a name='item61'>[61]</a> <a href ="/abs/2503.17324" title="Abstract" id="2503.17324"> arXiv:2503.17324 </a> [<a href="/pdf/2503.17324" title="Download PDF" id="pdf-2503.17324" aria-labelledby="pdf-2503.17324">pdf</a>, <a href="https://arxiv.org/html/2503.17324v1" title="View HTML" id="html-2503.17324" aria-labelledby="html-2503.17324" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17324" title="Other formats" id="oth-2503.17324" aria-labelledby="oth-2503.17324">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> HST Grism Observations of a z~1.8 Cluster Candidate from the Clusters Occupied by Bent Radio AGN (COBRA) Survey </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Watson,+C+B">Courtney B. Watson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Blanton,+E+L">Elizabeth L. Blanton</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Golden-Marx,+E">Emmet Golden-Marx</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ashby,+M+L+N">Matthew L. N. Ashby</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Randall,+S+W">Scott W. Randall</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wing,+J+D">J. D. Wing</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Douglass,+E+M">E. M. Douglass</a></div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> We present new Hubble Space Telescope/Wide Field Camera 3 G141 grism observations for COBRA1411+3415, originally identified as a high-redshift cluster candidate in the Clusters Occupied by Bent Radio AGN (COBRA) survey using radio, infrared, and optical data. We spectroscopically identify seven cluster members within a 0.5 Mpc radius with grism redshifts in the range $1.8006 \leq z_{grism} \leq 1.8175$, consistent with COBRA1411+3415 being a high-redshift cluster with a mean redshift of $\langle z_{grism}\rangle = 1.8106 \pm 0.0006$. The detection of seven galaxies within this small redshift range is significant above the background distribution of galaxies at the level of 5$\sigma$. The line-of-sight velocity dispersion of the cluster is found to be $\sigma_{\parallel} = 701^{+347}_{-138}$ km/s with a virial mass of $M_{200} \approx 2.2^{+3.3}_{-1.3}\times 10^{14}$ M$_{\odot}$. However, the mass may be lower if the cluster is still in formation. In projected phase-space, we also identify two possible infalling members of COBRA1411+3415 and two additional structures at $z\sim 1.73$ and $z\sim 1.88$. The similar spatial distributions and small projected separation from the main cluster suggest they could be a part of the same large-scale filament and together may form a protocluster system that could eventually merge to form a single, massive cluster. COBRA1411+3415 is the highest redshift cluster to be spectroscopically confirmed using a bent, double-lobed radio source as a cluster tracer. </p> </div> </dd> <dt> <a name='item62'>[62]</a> <a href ="/abs/2503.17327" title="Abstract" id="2503.17327"> arXiv:2503.17327 </a> [<a href="/pdf/2503.17327" title="Download PDF" id="pdf-2503.17327" aria-labelledby="pdf-2503.17327">pdf</a>, <a href="https://arxiv.org/html/2503.17327v1" title="View HTML" id="html-2503.17327" aria-labelledby="html-2503.17327" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17327" title="Other formats" id="oth-2503.17327" aria-labelledby="oth-2503.17327">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Radio Spectral Energy Distribution of Low-$z$ Metal Poor Extreme Starburst Galaxies: Novel insights on the escape of ionizing photons </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bait,+O">Omkar Bait</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Schaerer,+D">Daniel Schaerer</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Izotov,+Y+I">Yuri I. Izotov</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sebastian,+B">Biny Sebastian</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 14 pages, 5 figures, 4 tables; Submitted to Astronomy & Astrophysics </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> Recent optical surveys have found a rare population of low-$z$ ($z \sim 0.01 - 0.06$) extreme star-forming galaxies (xSFGs) that are the most metal-poor galaxies with strong emission lines, extremely high specific star-formation rate and low stellar mass. Using the Hubble Space Telescope Cosmic Origins Spectrograph, it was found that xSFGs are strong Ly$\alpha$ emitters. Their Ly$\alpha$ properties indirectly suggest that they are also strong Ly continuum (LyC) leakers. This along with several other global properties makes them similar to the recently found $z > 6$ reionization-era star-forming (SF) galaxies using the James Webb Space Telescope. Here we aim to study the radio spectral energy distribution (radio-SED) of $8$ xSFGs to understand mechanisms behind the extreme nature of SF in these galaxies, particularly their high ionisation state and possible strong LyC leakage. We present new radio continuum (RC) observations using the upgraded Giant Metrewave Radio Telescope (uGMRT) at Band-$5$ ($1060 - 1460$ MHz) together with the Karl G. Jansky Very Large Array (VLA) at S- ($2-4$ GHz), C- ($4-8$ GHz), X- ($8-12$ GHz) and Ku- ($12-18$ GHz) bands and archival LOw Frequency ARray (LOFAR) survey data between $120-168$ MHz for a few sources. The radio-SED of xSFGs is flat between $6-15$ GHz and shows a strong evidence for a turnover at lower frequencies in the range of $2-10$ GHz. They can be well described using a thermally dominated radio spectra with a free-free absorption component with a high emission measure. Thus the SF complexes in these galaxies are extremely young (pre-SNe stage; below $\sim 5$ Myrs) and the ISM is very dense suggesting a dominance of young massive star clusters. This can explain several extreme star-forming properties, along with the potential leakage of a significant amount of LyC photons in metal-poor extreme starburst galaxies. (abridged) </p> </div> </dd> <dt> <a name='item63'>[63]</a> <a href ="/abs/2503.17335" title="Abstract" id="2503.17335"> arXiv:2503.17335 </a> [<a href="/pdf/2503.17335" title="Download PDF" id="pdf-2503.17335" aria-labelledby="pdf-2503.17335">pdf</a>, <a href="https://arxiv.org/html/2503.17335v1" title="View HTML" id="html-2503.17335" aria-labelledby="html-2503.17335" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17335" title="Other formats" id="oth-2503.17335" aria-labelledby="oth-2503.17335">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Maximum-likelihood regression with systematic errors for astronomy and the physical sciences: II. Hypothesis testing of nested model components for Poisson data </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bonamente,+M">M. Bonamente</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zimmerman,+D">D. Zimmerman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chen,+Y">Y. Chen</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> ApJ 2025, 980 140 </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Instrumentation and Methods for Astrophysics (astro-ph.IM)</span> </div> <p class='mathjax'> A novel model of systematic errors for the regression of Poisson data is applied to hypothesis testing of nested model components with the introduction of a generalization of the $\Delta C$ statistic that applies in the presence of systematic errors. This paper shows that the null-hypothesis parent distribution of this $\Delta C_{sys}$ statistic can be obtained either through a simple numerical procedure, or in a closed form by making certain simplifying assumptions. It is found that the effects of systematic errors on the test statistic can be significant, and therefore the inclusion of sources of systematic errors is crucial for the assessment of the significance of nested model component in practical applications. The methods proposed in this paper provide a simple and accurate means of including systematic errors for hypothesis testing of nested model components in a variety of applications. </p> </div> </dd> <dt> <a name='item64'>[64]</a> <a href ="/abs/2503.17341" title="Abstract" id="2503.17341"> arXiv:2503.17341 </a> [<a href="/pdf/2503.17341" title="Download PDF" id="pdf-2503.17341" aria-labelledby="pdf-2503.17341">pdf</a>, <a href="https://arxiv.org/html/2503.17341v1" title="View HTML" id="html-2503.17341" aria-labelledby="html-2503.17341" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17341" title="Other formats" id="oth-2503.17341" aria-labelledby="oth-2503.17341">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Structure and kinematics of the interacting group NGC 5098/5096 </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Neto,+G+B+L">G. B. Lima Neto</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Capelato,+H+V">H. V. Capelato</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Durret,+F">F. Durret</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Machado,+R+E+G">R. E. G. Machado</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 11 pages, 14 figures, accepted for publication in A&A </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> Most galaxies in the Universe are found in groups, which have various morphologies and dynamical states. Studying how groups evolve is an important step for our understanding in both large-scale structure formation and galaxy evolution. <br>We analysed the system composed by two groups at z = 0.037, NGC 5098, a group dominated by a pair of elliptical galaxies, and NGC 5096, a compact system which appears to be interacting with NGC 5098. We aim to describe its current dynamical state in order to investigate how it fits in our current cosmological framework. <br>Our analysis is based on deep Canada-France-Hawaii Telescope (CFHT/MegaCam) g and r imaging, archival Chandra X-ray data, and publicly available data of the galaxy redshift distribution. We model the surface brightness of the 12 brightest galaxies in the field-of-view and investigate the diffuse intragroup light that we detect. With a redshift sample of 112 galaxies, we study the dynamical states of both groups. <br>We detect low surface brightness diffuse light associated with both galaxy-galaxy interactions and a possible group-group collision. The substructure we found in velocity space indicates a past interaction between both groups. This is further corroborated by the X-ray analysis. <br>We conclude that NGC 5098 and NGC 5096 form a complex system, that may have collided in the past, producing a sloshing observed in X-rays and a large scale diffuse component of intragroup light as well as some important tidal debris. </p> </div> </dd> <dt> <a name='item65'>[65]</a> <a href ="/abs/2503.17342" title="Abstract" id="2503.17342"> arXiv:2503.17342 </a> [<a href="/pdf/2503.17342" title="Download PDF" id="pdf-2503.17342" aria-labelledby="pdf-2503.17342">pdf</a>, <a href="https://arxiv.org/html/2503.17342v1" title="View HTML" id="html-2503.17342" aria-labelledby="html-2503.17342" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17342" title="Other formats" id="oth-2503.17342" aria-labelledby="oth-2503.17342">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Comparison of dynamical dark energy with 螞CDM in light of DESI DR2 </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ormondroyd,+A">A.N. Ormondroyd</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Handley,+W">W.J. Handley</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hobson,+M">M.P. Hobson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lasenby,+A">A.N. Lasenby</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 5 pages, 5 figures, 1 table </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span> </div> <p class='mathjax'> We present an updated reconstruction of the dark energy equation of state, $w(a)$, using the newly released DESI DR2 Baryon Acoustic Oscillation (BAO) data in combination with Pantheon+ and DES5Y Type Ia supernovae measurements, respectively. Building on our previous analysis in <a href="https://arxiv.org/abs/2503.08658" data-arxiv-id="2503.08658" class="link-https">arXiv:2503.08658</a>, which employed a nonparametric flexknot reconstruction approach, we examine whether the evidence for dynamical dark energy persists with the improved precision of the DESI DR2 dataset. We find that while the overall qualitative structure of $w(a)$ remains consistent with our earlier findings, the statistical support for dynamical dark energy is reduced when considering DESI DR2 data alone, particularly for more complex flexknot models with higher numbers of knots. However, the evidence for simpler dynamical models, such as $w$CDM and CPL (which correspond to $n=1$ and $n=2$ knots respectively), increases relative to $\Lambda$CDM with DESI DR2 alone, consistent with previous DESI analyses. When combined with Pantheon+ data, the conclusions remain broadly consistent with our earlier work, but the inclusion of DES5Y supernovae data leads to an increase of preference for flexknot models with more than two knots, placing $w$CDM and CPL on par with $\Lambda$CDM. </p> </div> </dd> <dt> <a name='item66'>[66]</a> <a href ="/abs/2503.17344" title="Abstract" id="2503.17344"> arXiv:2503.17344 </a> [<a href="/pdf/2503.17344" title="Download PDF" id="pdf-2503.17344" aria-labelledby="pdf-2503.17344">pdf</a>, <a href="https://arxiv.org/html/2503.17344v1" title="View HTML" id="html-2503.17344" aria-labelledby="html-2503.17344" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17344" title="Other formats" id="oth-2503.17344" aria-labelledby="oth-2503.17344">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> The impact of the Galactic bar and the Large Magellanic Cloud on hypervelocity star trajectories </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Armstrong,+I">Isabella Armstrong</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Evans,+F+A">Fraser A. Evans</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bovy,+J">Jo Bovy</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 22 pages, 11 figures. Accepted to ApJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> Hypervelocity stars (HVSs) ejected from the Galactic Center (GC) at speeds faster than the Galactic escape velocity are useful tools to provide insight into the Milky Way's dark matter halo. However, most characterizations of HVS orbits assume static models of the Milky Way's gravitational potential. In this work, we assess the influence of the Galactic bar and the Large Magellanic Cloud (LMC) on HVS trajectories, comparing them with those from an axisymmetric potential. We simulate 28,000 HVSs ejected over the last 100 Myr and find that ignoring the bar and LMC can cause their apparent ejection location to drift by up to 100 pc. Applying two standard HVS potential fitting methods to our sample shows that they are unable to perform as designed when non-axisymmetric effects are neglected. We calculate the angle between HVS Galactocentric position and velocity and find the LMC and bar can induce a deflection angle of up to several degrees. Using mock Gaia Data Release 4 observations, however, we show that this deflection is too small in magnitude to be measured in the near future without significantly improved observational uncertainties, particularly in heliocentric distance. Our results emphasize the need to account for the bar and LMC in modeling the Galactic potential using HVSs as a tracer. </p> </div> </dd> <dt> <a name='item67'>[67]</a> <a href ="/abs/2503.17346" title="Abstract" id="2503.17346"> arXiv:2503.17346 </a> [<a href="/pdf/2503.17346" title="Download PDF" id="pdf-2503.17346" aria-labelledby="pdf-2503.17346">pdf</a>, <a href="https://arxiv.org/html/2503.17346v1" title="View HTML" id="html-2503.17346" aria-labelledby="html-2503.17346" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17346" title="Other formats" id="oth-2503.17346" aria-labelledby="oth-2503.17346">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Abundances of refractory ions in Beta Pictoris exocomets </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Vrignaud,+T">T. Vrignaud</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Etangs,+A+L+d">A. Lecavelier des Etangs</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Strom,+P+A">P. A. Strom</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kiefer,+F">F. Kiefer</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 35 pages, 11 figures. Accepted to A&A </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Earth and Planetary Astrophysics (astro-ph.EP)</span> </div> <p class='mathjax'> Beta Pic is a young, A5V star, known for harbouring a large number of exocomets, which frequently transit the star and produce absorption signatures. The physical and chemical properties of these exocomets can be probed by the recently introduced curve of growth approach, which enables column densities measurements in exocomets using observations in numerous spectral lines. Using this approach, we present a new study of archival spectra of Beta Pic obtained with the HST, the HARPS spectrograph, and at the Mont John University Observatory, aimed at constraining the abundance of refractory ions in Beta Pic exocomets. 29 individual objects are studied, all observed in FeII lines (used as a reference ion) and at least one other species (Ni II, Ca II, Cr II...). We find that the refractory composition of exocomets is overall stable, especially for singly ionised species, and consistent with solar abundances. This validates the use of the curve of growth approach to study exocometary composition. We also show that some ions, such as Ca II, are significantly depleted compared to solar abundances, allowing us to constrain the ionisation state in Beta Pic exocomets. We find that most refractory elements (Mg, Ni, Fe...) are split in similar fractions between their first and second ionisation states, with the exception of Ca, mostly ionized twice. A strong correlation between the Al III/Fe II ratio and radial velocity is also found, showing that the most redshifted exocomets tend to be more ionised. These results open the way for further modelling, in order to better understand the physical processes that influence the composition and shape of exocometary tails. </p> </div> </dd> <dt> <a name='item68'>[68]</a> <a href ="/abs/2503.17364" title="Abstract" id="2503.17364"> arXiv:2503.17364 </a> [<a href="/pdf/2503.17364" title="Download PDF" id="pdf-2503.17364" aria-labelledby="pdf-2503.17364">pdf</a>, <a href="https://arxiv.org/html/2503.17364v1" title="View HTML" id="html-2503.17364" aria-labelledby="html-2503.17364" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17364" title="Other formats" id="oth-2503.17364" aria-labelledby="oth-2503.17364">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> On the road to the radius valley: distinguishing between gas dwarfs and water worlds with young transiting exoplanets </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rogers,+J+G">James G. Rogers</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 12 pages, 5 figures, resubmitted to MNRAS after revision </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Earth and Planetary Astrophysics (astro-ph.EP)</span> </div> <p class='mathjax'> The detection of young transiting exoplanets represents a new frontier in our understanding of planet formation and evolution. For the population of observed close-in sub-Neptunes, two proposed formation pathways can reproduce their observed masses and radii at $\sim$Gyr ages: the "gas dwarf" hypothesis and the "water world" hypothesis. We show that a sub-Neptune's size at early ages $\lesssim 100$ Myrs is strongly dependent on the bulk mean molecular weight within its envelope. As a result, gas dwarfs and water worlds should diverge in size at early ages since the mean molecular weight of gas dwarf envelopes is predicted to be smaller than that of water worlds. We construct population models under both scenarios that reproduce Kepler demographics in the age range $\sim1-10$ Gyrs. We find tentative evidence that the gas dwarf model is more consistent with the small population of young exoplanets $< 40$ Myrs from TESS. We show that planet radius is relatively insensitive to planet mass for young, puffy sub-Neptunes, meaning that well-characterised masses are not necessarily required to exploit the effects of mean molecular weight at the population level. We confirm the predicted difference in planet size between the models is also true under mixed-envelope scenarios, in which envelopes consist of mixtures of hydrogen and steam. We highlight that transit surveys of young exoplanets should target the youngest observable stellar clusters to exploit the effects of mean molecular weight. </p> </div> </dd> </dl> <dl id='articles'> <h3>Cross submissions (showing 6 of 6 entries)</h3> <dt> <a name='item69'>[69]</a> <a href ="/abs/2503.16649" title="Abstract" id="2503.16649"> arXiv:2503.16649 </a> (cross-list from gr-qc) [<a href="/pdf/2503.16649" title="Download PDF" id="pdf-2503.16649" aria-labelledby="pdf-2503.16649">pdf</a>, <a href="https://arxiv.org/html/2503.16649v1" title="View HTML" id="html-2503.16649" aria-labelledby="html-2503.16649" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16649" title="Other formats" id="oth-2503.16649" aria-labelledby="oth-2503.16649">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Extreme mass ratio inspirals in dark matter halos: dynamics and distinguishability of halo models </div> <div class='list-authors'><a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Gliorio,+S">Sara Gliorio</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Berti,+E">Emanuele Berti</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Maselli,+A">Andrea Maselli</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Speeney,+N">Nicholas Speeney</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 12 pages, 8 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">General Relativity and Quantum Cosmology (gr-qc)</span>; Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Astrophysical Phenomena (astro-ph.HE) </div> <p class='mathjax'> The gravitational wave (GW) signals from extreme mass-ratio inspirals (EMRIs), a key target for the Laser Interferometer Space Antenna (LISA), will be affected in the presence of dark matter (DM) halos. In this paper we explore whether the effects of DM are detectable by LISA within a fully relativistic framework. We model the massive EMRI component as a nonrotating black hole (BH) surrounded by a DM halo. We compute axial and polar GW fluxes for circular orbits at linear order in the mass ratio for DM density profiles with varying mass and compactness. By comparing the phase evolution with vacuum systems, we find that DM halos can induce dephasings of tens to hundreds of radians over a one-year observation period. We demonstrate that even highly diluted DM distributions can significantly affect the emitted waveforms, and that the resulting GW signals can usually be distinguished from each other. While it is important to generalize these findings to more generic orbits and to spinning BHs, our results suggest that LISA could not only reveal the presence of DM halos, but also discriminate between different halo models. </p> </div> </dd> <dt> <a name='item70'>[70]</a> <a href ="/abs/2503.17084" title="Abstract" id="2503.17084"> arXiv:2503.17084 </a> (cross-list from gr-qc) [<a href="/pdf/2503.17084" title="Download PDF" id="pdf-2503.17084" aria-labelledby="pdf-2503.17084">pdf</a>, <a href="https://arxiv.org/html/2503.17084v1" title="View HTML" id="html-2503.17084" aria-labelledby="html-2503.17084" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17084" title="Other formats" id="oth-2503.17084" aria-labelledby="oth-2503.17084">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> GraFIT: A toolbox for fast and accurate frequency response identification in Gravitational Wave Detectors </div> <div class='list-authors'><a href="https://arxiv.org/search/gr-qc?searchtype=author&query=van+Dael,+M">Mathyn van Dael</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=van+Haren,+M">Max van Haren</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Witvoet,+G">Gert Witvoet</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Swinkels,+B">Bas Swinkels</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Oomen,+T">Tom Oomen</a></div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">General Relativity and Quantum Cosmology (gr-qc)</span>; Instrumentation and Methods for Astrophysics (astro-ph.IM); Systems and Control (eess.SY) </div> <p class='mathjax'> Frequency response function (FRF) measurements are widely used in Gravitational Wave (GW) detectors, e.g., for the design of controllers, calibrating signals and diagnostic problems with system dynamics. The aim of this paper is to present GraFIT: a toolbox that enables fast, inexpensive, and accurate identification of FRF measurements for GW detectors compared to the commonly used approaches, including common spectral analysis techniques. The toolbox consists of a single function to estimate the frequency response function for both open-loop and closed-loop systems and for arbitrary input and output dimensions. The toolbox is validated on two experimental case studies of the Virgo detector, illustrating more than a factor 3 reduction in standard deviation of the estimate for the same measurement times, and comparable standard deviations with up to 10 times less data for the new method with respect to the currently implemented Spectral Analysis method. </p> </div> </dd> <dt> <a name='item71'>[71]</a> <a href ="/abs/2503.17143" title="Abstract" id="2503.17143"> arXiv:2503.17143 </a> (cross-list from nucl-th) [<a href="/pdf/2503.17143" title="Download PDF" id="pdf-2503.17143" aria-labelledby="pdf-2503.17143">pdf</a>, <a href="https://arxiv.org/html/2503.17143v1" title="View HTML" id="html-2503.17143" aria-labelledby="html-2503.17143" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17143" title="Other formats" id="oth-2503.17143" aria-labelledby="oth-2503.17143">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Dipole Polarizability of Finite Nuclei as a Probe of Neutron Stars </div> <div class='list-authors'><a href="https://arxiv.org/search/nucl-th?searchtype=author&query=Koliogiannis,+P">P.S. Koliogiannis</a>, <a href="https://arxiv.org/search/nucl-th?searchtype=author&query=Yuksel,+E">E. Yuksel</a>, <a href="https://arxiv.org/search/nucl-th?searchtype=author&query=Ghosh,+T">T. Ghosh</a>, <a href="https://arxiv.org/search/nucl-th?searchtype=author&query=Paar,+N">N. Paar</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 6 pages, 4 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Nuclear Theory (nucl-th)</span>; High Energy Astrophysical Phenomena (astro-ph.HE); Solar and Stellar Astrophysics (astro-ph.SR); Nuclear Experiment (nucl-ex) </div> <p class='mathjax'> Nuclear ground state and collective excitation properties provide a means to probe the nuclear matter equation of state and establish connections between observables in finite nuclei and neutron stars. Specifically, the electric dipole polarizability, measured with high precision in various neutron-rich nuclei, serves as a robust constraint on the density dependence of the symmetry energy. In this Letter, we employ a class of relativistic energy density functionals in a twofold process: first, to link the electric dipole polarizability from recent experiments to the slope of the symmetry energy, and second, to translate this information into constraints on the tidal deformability and radii of neutron stars, in connection with multimessenger astrophysical observations from pulsars and binary neutron stars. We provide compelling evidence that the electric dipole polarizability represents a key nuclear observable to probe the neutron star properties. By significantly reducing the uncertainties in the mass-radius plane, our findings also align with recent multimessenger observations. </p> </div> </dd> <dt> <a name='item72'>[72]</a> <a href ="/abs/2503.17208" title="Abstract" id="2503.17208"> arXiv:2503.17208 </a> (cross-list from nlin.CD) [<a href="/pdf/2503.17208" title="Download PDF" id="pdf-2503.17208" aria-labelledby="pdf-2503.17208">pdf</a>, <a href="https://arxiv.org/html/2503.17208v1" title="View HTML" id="html-2503.17208" aria-labelledby="html-2503.17208" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17208" title="Other formats" id="oth-2503.17208" aria-labelledby="oth-2503.17208">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Hamiltonian Chaos: From Galactic Dynamics to Plasma Physics </div> <div class='list-authors'><a href="https://arxiv.org/search/nlin?searchtype=author&query=Moges,+H+T">Henok Tenaw Moges</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> PhD Thesis, 177 pages </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Chaotic Dynamics (nlin.CD)</span>; Astrophysics of Galaxies (astro-ph.GA); Dynamical Systems (math.DS); Plasma Physics (physics.plasm-ph) </div> <p class='mathjax'> The primary focus of this thesis is the numerical investigation of chaos in Hamiltonian models describing charged particle orbits in plasma, star motions in barred galaxies, and orbits' diffusion in multidimensional maps. We systematically explore the interplay between magnetic and kinetic chaos in toroidal fusion plasmas, where non-axisymmetric perturbations disrupt smooth magnetic flux surfaces, generating complex particle trajectories. Using the Generalized Alignment Index (GALI) method, we efficiently quantify chaos, compare the behavior of magnetic field lines and particle orbits, visualize the radial distribution of chaotic regions, and offer GALI as a valuable tool for studying plasma physics dynamics. We also study the evolution of phase space structures in a 3D barred galactic potential, following successive 2D and 3D pitchfork and period-doubling bifurcations of periodic orbits. By employing the `color and rotation' technique to visualize the system's 4D Poincar茅 surface of sections, we reveal distinct structural patterns. We further investigate the long-term diffusion transport and chaos properties of single and coupled standard maps, focusing on parameters inducing anomalous diffusion through accelerator modes exhibiting ballistic transport. Using different ensembles of initial conditions in chaotic regions influenced by these modes, we examine asymptotic diffusion rates and time scales, identifying conditions suppressing anomalous transport and leading to long-term convergence to normal diffusion across coupled maps. Lastly, we perform the first comprehensive investigation into the GALI indices for various attractors in continuous and discrete-time dissipative systems, extending the method's application to non-Hamiltonian systems. A key aspect of our work involves analyzing and comparing GALIs' with Lyapunov Exponents for systems exhibiting hyperchaotic motion. </p> </div> </dd> <dt> <a name='item73'>[73]</a> <a href ="/abs/2503.17278" title="Abstract" id="2503.17278"> arXiv:2503.17278 </a> (cross-list from physics.plasm-ph) [<a href="/pdf/2503.17278" title="Download PDF" id="pdf-2503.17278" aria-labelledby="pdf-2503.17278">pdf</a>, <a href="https://arxiv.org/html/2503.17278v1" title="View HTML" id="html-2503.17278" aria-labelledby="html-2503.17278" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17278" title="Other formats" id="oth-2503.17278" aria-labelledby="oth-2503.17278">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Universal fluctuation spectrum of Vlasov-Poisson turbulence </div> <div class='list-authors'><a href="https://arxiv.org/search/physics?searchtype=author&query=Nastac,+M+L">Michael L. Nastac</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Ewart,+R+J">Robert J. Ewart</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Juno,+J">James Juno</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Barnes,+M">Michael Barnes</a>, <a href="https://arxiv.org/search/physics?searchtype=author&query=Schekochihin,+A+A">Alexander A. Schekochihin</a></div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Plasma Physics (physics.plasm-ph)</span>; High Energy Astrophysical Phenomena (astro-ph.HE); Chaotic Dynamics (nlin.CD); Space Physics (physics.space-ph) </div> <p class='mathjax'> The thermal fluctuation spectrum of the electric field arising due to particle noise in a quiescent Vlasov-Poisson plasma was derived in the 1960s. Here, we derive the universal fluctuation spectrum of the electric field, at Debye and sub-Debye scales, for a turbulent Vlasov-Poisson plasma. This spectrum arises from what is likely to be the final cascade - a universal regime to be encountered at the extreme small-scale end of any turbulent cascade in a nearly collisionless plasma. The cascaded invariant is $C_2$, the quadratic Casimir invariant of the particle distribution function. $C_2$ cascades to small scales in position and velocity space via linear and nonlinear phase mixing, in such a way that the time scales of the two processes are critically balanced at every scale. We construct a scaling theory of the fluctuation spectrum of $C_2$ and of the electric field in wavenumber space. The electric-field spectrum is sufficiently steep for the nonlinear mixing to be controlled by the largest-scale electric fields, and so the $C_2$ cascade resembles the Batchelor cascade of a passive scalar. Our theory is supported by simulations of a forced 1D-1V plasma. We predict that the cascade is terminated at the wavenumber where the turbulent electric-field spectrum gives way to the thermal noise spectrum. The time scale for this small-scale cutoff to be reached is the dynamical time of phase-space mixing times a logarithmic factor in the plasma parameter - this is the first concrete demonstration of this property of Vlasov-Poisson turbulence, akin to how fluid turbulence dissipates energy at a rate independent (or nearly independent) of molecular diffusion. In the presence of the sub-Debye phase-space cascade - a scenario that may be ubiquitous - standard collisional plasma theory ceases to be valid. This calls for the development of new collision operators suited to such turbulent environments. </p> </div> </dd> <dt> <a name='item74'>[74]</a> <a href ="/abs/2503.17283" title="Abstract" id="2503.17283"> arXiv:2503.17283 </a> (cross-list from cs.DC) [<a href="/pdf/2503.17283" title="Download PDF" id="pdf-2503.17283" aria-labelledby="pdf-2503.17283">pdf</a>, <a href="https://arxiv.org/html/2503.17283v1" title="View HTML" id="html-2503.17283" aria-labelledby="html-2503.17283" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.17283" title="Other formats" id="oth-2503.17283" aria-labelledby="oth-2503.17283">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Energy Efficiency trends in HPC: what high-energy and astrophysicists need to know </div> <div class='list-authors'><a href="https://arxiv.org/search/cs?searchtype=author&query=Suarez,+E">Estela Suarez</a>, <a href="https://arxiv.org/search/cs?searchtype=author&query=Amaya,+J">Jorge Amaya</a>, <a href="https://arxiv.org/search/cs?searchtype=author&query=Frank,+M">Martin Frank</a>, <a href="https://arxiv.org/search/cs?searchtype=author&query=Freyermuth,+O">Oliver Freyermuth</a>, <a href="https://arxiv.org/search/cs?searchtype=author&query=Girone,+M">Maria Girone</a>, <a href="https://arxiv.org/search/cs?searchtype=author&query=Kostrzewa,+B">Bartosz Kostrzewa</a>, <a href="https://arxiv.org/search/cs?searchtype=author&query=Pfalzner,+S">Susanne Pfalzner</a></div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Distributed, Parallel, and Cluster Computing (cs.DC)</span>; Cosmology and Nongalactic Astrophysics (astro-ph.CO); Solar and Stellar Astrophysics (astro-ph.SR); High Energy Physics - Experiment (hep-ex); High Energy Physics - Lattice (hep-lat); Computational Physics (physics.comp-ph) </div> <p class='mathjax'> The growing energy demands of HPC systems have made energy efficiency a critical concern for system developers and operators. However, HPC users are generally less aware of how these energy concerns influence the design, deployment, and operation of supercomputers even though they experience the consequences. This paper examines the implications of HPC's energy consumption, providing an overview of current trends aimed at improving energy efficiency. We describe how hardware innovations such as energy-efficient processors, novel system architectures, power management techniques, and advanced scheduling policies do have a direct impact on how applications need to be programmed and executed on HPC systems. For application developers, understanding how these new systems work and how to analyse and report the performances of their own software is critical in the dialog with HPC system designers and administrators. The paper aims to raise awareness about energy efficiency among users, particularly in the high energy physics and astrophysics domains, offering practical advice on how to analyse and optimise applications to reduce their energy consumption without compromising on performance. </p> </div> </dd> </dl> <dl id='articles'> <h3>Replacement submissions (showing 31 of 31 entries)</h3> <dt> <a name='item75'>[75]</a> <a href ="/abs/2405.16568" title="Abstract" id="2405.16568"> arXiv:2405.16568 </a> (replaced) [<a href="/pdf/2405.16568" title="Download PDF" id="pdf-2405.16568" aria-labelledby="pdf-2405.16568">pdf</a>, <a href="https://arxiv.org/html/2405.16568v2" title="View HTML" id="html-2405.16568" aria-labelledby="html-2405.16568" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2405.16568" title="Other formats" id="oth-2405.16568" aria-labelledby="oth-2405.16568">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Varaha: A promising sampler for obtaining gravitational wave posteriors </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tiwari,+V">Vaibhav Tiwari</a></div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> Nested sampling is often used in Bayesian statistics problems in astronomy. It operates with a set of live points, iteratively replacing the point with the lowest likelihood with a new point of higher likelihood. Each iteration reduces the enclosed volume by a known factor. The estimated sampling density and the likelihood values of both new and old live points quantify the enclosed probability mass. Although robust, nested sampling often discards a majority of the sampled points ($\sim 99.9\%$) at which likelihood was calculated. Here, we present an efficient method to explicitly calculate the sampling density for small dimensional problems~(ten or less), thereby removing the need to discard samples. The points' sampling density and likelihood values constitute the posterior distribution. We build on the existing version of the sampler Varaha and present an alternate version that is significantly more efficient for expensive likelihoods. These samplers specifically focus on obtaining compact binary parameters from their gravitational wave signals. They provide a viable alternative to nested sampling when the full fifteen-dimensional space is sampled separately for observer-dependent parameters and parameters intrinsic to the binary. </p> </div> </dd> <dt> <a name='item76'>[76]</a> <a href ="/abs/2406.09122" title="Abstract" id="2406.09122"> arXiv:2406.09122 </a> (replaced) [<a href="/pdf/2406.09122" title="Download PDF" id="pdf-2406.09122" aria-labelledby="pdf-2406.09122">pdf</a>, <a href="https://arxiv.org/html/2406.09122v2" title="View HTML" id="html-2406.09122" aria-labelledby="html-2406.09122" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2406.09122" title="Other formats" id="oth-2406.09122" aria-labelledby="oth-2406.09122">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Primordial black hole formation from self-resonant preheating? </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ballesteros,+G">Guillermo Ballesteros</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Juan,+J+I">Joaquim Iguaz Juan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Serpico,+P+D">Paquale D. Serpico</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Taoso,+M">Marco Taoso</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 20 pages, 6 figures. Clarifications added, results unchanged; matches published version in PRD </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span>; General Relativity and Quantum Cosmology (gr-qc); High Energy Physics - Phenomenology (hep-ph); High Energy Physics - Theory (hep-th) </div> <p class='mathjax'> We revisit the question of how generic is the formation of primordial black holes via self-resonant growth of inflaton fluctuations in the post-inflationary, preheating phase. Using analytical and lattice calculations, we find that primordial black hole production is far from being a generic outcome. Also, in most of the parameter space of viable inflationary models, the metric preheating term is subleading to the anharmonic terms and the approximation of a quadratic potential for describing the resonance dynamics is inadequate. Nonetheless, the anharmonicity of the potential cannot be used to rescue the mechanism: The generic outcome of the non-linear evolution of the scalar field in this case is the formation of metastable transients or oscillons, that do not generically collapse into black holes. </p> </div> </dd> <dt> <a name='item77'>[77]</a> <a href ="/abs/2407.01524" title="Abstract" id="2407.01524"> arXiv:2407.01524 </a> (replaced) [<a href="/pdf/2407.01524" title="Download PDF" id="pdf-2407.01524" aria-labelledby="pdf-2407.01524">pdf</a>, <a href="https://arxiv.org/html/2407.01524v2" title="View HTML" id="html-2407.01524" aria-labelledby="html-2407.01524" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2407.01524" title="Other formats" id="oth-2407.01524" aria-labelledby="oth-2407.01524">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Straightening the Ruler: Field-Level Inference of the BAO Scale with LEFTfield </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Babi%C4%87,+I">Ivana Babi膰</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Schmidt,+F">Fabian Schmidt</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tucci,+B">Beatriz Tucci</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 30 pages, 15 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span>; Astrophysics of Galaxies (astro-ph.GA) </div> <p class='mathjax'> Current inferences of the BAO scale from galaxy clustering employ a reconstruction technique at fixed cosmology and bias parameters. Here, we present the first consistent joint Bayesian inference of the isotropic BAO scale, jointly varying the initial conditions as well as all bias coefficients, based on the EFT-based field-level forward model $\texttt{LEFTfield}$. We apply this analysis to mock data generated at a much higher cutoff, or resolution, resulting in a significant model mismatch between mock data and the model used in the inference. We demonstrate that the remaining systematic bias in the BAO scale is below 2% for all data considered and below 1% when Eulerian bias is used for inference. Furthermore, we find that the inferred error on the BAO scale is typically 30%, and up to 50%, smaller compared to that from a replication of the standard post-reconstruction power-spectrum approach, using the same scales as in the field-level inference. The improvement in BAO scale precision grows towards smaller scales (higher $k$). As a validation test, we repeat this comparison on a mock dataset that is linearly biased with respect to a 1LPT (Zel'dovich) density field, following the assumption made in standard reconstruction approaches. We find that field-level inference indeed yields the same error bar as the post-reconstruction power spectrum, which is expectd to be optimal in this case. In summary, a field-level approach to BAO not only allows for a consistent inference of the BAO scale, but promises to achieve more precise measurements on realistic, nonlinearly biased tracers as well. </p> </div> </dd> <dt> <a name='item78'>[78]</a> <a href ="/abs/2407.03882" title="Abstract" id="2407.03882"> arXiv:2407.03882 </a> (replaced) [<a href="/pdf/2407.03882" title="Download PDF" id="pdf-2407.03882" aria-labelledby="pdf-2407.03882">pdf</a>, <a href="https://arxiv.org/html/2407.03882v4" title="View HTML" id="html-2407.03882" aria-labelledby="html-2407.03882" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2407.03882" title="Other formats" id="oth-2407.03882" aria-labelledby="oth-2407.03882">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Cosmology with voids </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bromley,+B+C">Benjamin C. Bromley</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Geller,+M+J">Margaret J. Geller</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> JCAP, accepted, 47 pages, 3 tables, 18 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span> </div> <p class='mathjax'> Voids are dominant features of the cosmic web. We revisit the cosmological information content of voids and connect void properties with the parameters of the background universe. We combine analytical results with a suite of large n-body realizations of large-scale structure in the quasilinear regime to measure the central density and radial outflow of voids. These properties, estimated from multiple voids that span a range of redshifts, provide estimates of the Hubble parameter, $\Omega_M$ and $\Omega_\Lambda$. The analysis assumes access to the full phase-space distribution of mass within voids, a dataset that is not currently observable. The observable properties of the largest void in the universe may also test models. The suite of large n-body realizations enables construction of lightcones reaching ~3,000 $h^{-1}$Mpc. Based on these lightcones, we show that large voids similar to those observed are expected in the standard $\Lambda$CDM model. </p> </div> </dd> <dt> <a name='item79'>[79]</a> <a href ="/abs/2408.09571" title="Abstract" id="2408.09571"> arXiv:2408.09571 </a> (replaced) [<a href="/pdf/2408.09571" title="Download PDF" id="pdf-2408.09571" aria-labelledby="pdf-2408.09571">pdf</a>, <a href="https://arxiv.org/html/2408.09571v2" title="View HTML" id="html-2408.09571" aria-labelledby="html-2408.09571" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2408.09571" title="Other formats" id="oth-2408.09571" aria-labelledby="oth-2408.09571">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Exploring the Dynamical Nature and Radio Halo Emission of Abell 384: A Combined Radio, X-ray and Optical Study </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chatterjee,+S">Swarna Chatterjee</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pillay,+D">Denisha Pillay</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Datta,+A">Abhirup Datta</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Raja,+R">Ramij Raja</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Knowles,+K">Kenda Knowles</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rahaman,+M">Majidul Rahaman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sikhosana,+S">S.P. Sikhosana</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 13 pages, 11 figures, 4 tables, Accepted for publication in MNRAS </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span>; High Energy Astrophysical Phenomena (astro-ph.HE) </div> <p class='mathjax'> Multiwavelength studies of galaxy clusters are crucial for understanding the complex interconnection of the thermal and non-thermal constituents of these massive structures and uncovering the physical processes involved in their formation and evolution. Here, we report a multiwavelength assessment of the galaxy cluster A384, which was previously reported to host a radio halo with a 660 kpc size at MeerKAT 1.28 GHz. The halo is slightly offset from the cluster centre. Our uGMRT observation reveals that the halo extends up to 690 kpc at 407 MHz with a nonuniform spectral index $\alpha^{1284\ \mathrm{MHz}}_{407\ \mathrm{MHz}}$ distribution varying from flat (-0.5) to steep (-1.3) values. In addition, we use legacy GMRT 608 MHz, \textit{XMM-Newton} X-ray, and the Dark Energy Survey optical observations to obtain an extensive understanding of the dynamical nature of the galaxy cluster. The X-ray surface brightness concentration parameter ($C_{\rm{SB}} = 0.16$) and centroid shift ($w = 0.057$) reveal an ongoing dynamical disturbance in the cluster. This is also supported by the elongated 2-D optical galaxy density distribution map of the cluster. The obtained centre shift between optical and X-ray peaks and the asymmetry parameter from optical analysis further supports the dynamical disturbance in the cluster. The radio and X-ray surface brightness follows a sub-linear correlation. Our observations suggest that the cluster is currently in a merging state where particle re-acceleration in the turbulent ICM resulted in the radio halo emission. </p> </div> </dd> <dt> <a name='item80'>[80]</a> <a href ="/abs/2408.10298" title="Abstract" id="2408.10298"> arXiv:2408.10298 </a> (replaced) [<a href="/pdf/2408.10298" title="Download PDF" id="pdf-2408.10298" aria-labelledby="pdf-2408.10298">pdf</a>, <a href="https://arxiv.org/html/2408.10298v2" title="View HTML" id="html-2408.10298" aria-labelledby="html-2408.10298" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2408.10298" title="Other formats" id="oth-2408.10298" aria-labelledby="oth-2408.10298">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Signature of hadron-quark crossover in binary-neutron-star mergers </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fujimoto,+Y">Yuki Fujimoto</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fukushima,+K">Kenji Fukushima</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hotokezaka,+K">Kenta Hotokezaka</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kyutoku,+K">Koutarou Kyutoku</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 25 pages, 18 figures </div> <div class='list-journal-ref'><span class='descriptor'>Journal-ref:</span> Phys. Rev. D 111, 063054 (2025) </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; General Relativity and Quantum Cosmology (gr-qc); Nuclear Theory (nucl-th) </div> <p class='mathjax'> We study observational signatures of the hadron-quark crossover in binary-neutron-star mergers by numerical-relativity simulations with various mass configurations. We employ two equations of state (EoSs) for matter consistent with inference from the observational data. In the crossover scenario the EoS is softened in a density realized in binary-neutron-star mergers and is smoothly continued to quark matter. In the phase transition scenario without crossover, the EoS remains stiff and a first-order phase transition takes place in a density out of reach of mergers. A GW170817-like system forms a remnant massive neutron star in both scenarios, and it collapses into a black hole only in the crossover scenario due to the softening while gravitational-wave emission is strong. This difference is clearly reflected in the sudden shutdown of gravitational waves. For a given EoS, the lifetime of the merger remnant is determined primarily by the total mass of the system. Identifying these features in a variety of future events with the next generation of ground-based gravitational-wave detectors will enable us to clarify details of hadron-quark transition. The mass of the accretion disk surrounding the remnant black hole is affected not only by the lifetime of the remnant but also by the mass ratio of the system. Electromagnetic emission associated with the disk outflow will also be useful for detailed investigation of the hadron-quark transition. </p> </div> </dd> <dt> <a name='item81'>[81]</a> <a href ="/abs/2408.10999" title="Abstract" id="2408.10999"> arXiv:2408.10999 </a> (replaced) [<a href="/pdf/2408.10999" title="Download PDF" id="pdf-2408.10999" aria-labelledby="pdf-2408.10999">pdf</a>, <a href="https://arxiv.org/html/2408.10999v2" title="View HTML" id="html-2408.10999" aria-labelledby="html-2408.10999" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2408.10999" title="Other formats" id="oth-2408.10999" aria-labelledby="oth-2408.10999">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Constraining Extra Mixing during the Main Sequence: What Depletes Lithium Does Not Touch Beryllium </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Reggiani,+H">Henrique Reggiani</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Galarza,+J+Y">Jhon Yana Galarza</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lorenzo-Oliveira,+D">Diego Lorenzo-Oliveira</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Covarrubias,+S">Sofia Covarrubias</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Oyague,+M">Micaela Oyague</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Valle,+R">Rita Valle</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chanam%C3%A9,+J">Julio Chanam茅</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Accepted at AJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span> </div> <p class='mathjax'> Measurements of lithium abundances in solar-type stars have shown that standard models of stellar evolution are incapable of explaining the observed depletion as a function of stellar age. Beryllium is one of the lightest elements that can be measured in stellar photospheres, and it can be burned in relatively low temperatures. Studying its abundances as a function of stellar age can provide important constraints to stellar mixing models, as the level of depletion as a function of time will indicate how deep the photospheric material must be dredged to explain the observed abundances. In an effort to provide the most stringent constraints for non-standard stellar mixing models, we observed a sample of solar-twins and concomitantly analyzed their lithium and beryllium abundances. Unlike what is typically observed for lithium, we found that beryllium does not decrease as a function of stellar age along the main-sequence, constraining models that predict burning of both materials. Based on our data, models that invoke convective overshoot and convective settling are preferred over typical rotationaly-induced mixing models, as the later burn Be in excess while the former do not. Previous works also proposed mixing due to gravity waves as a possible explanation for observed abundances, which can fit our data as well. Furthermore, based on our solar twins, Be depletion likely happens within the first $\sim1$ Gyr. We also confirm previous findings of an increase in Be abundance as a function of metallicity, indicative of galactic production via cosmic ray spallation. </p> </div> </dd> <dt> <a name='item82'>[82]</a> <a href ="/abs/2408.15086" title="Abstract" id="2408.15086"> arXiv:2408.15086 </a> (replaced) [<a href="/pdf/2408.15086" title="Download PDF" id="pdf-2408.15086" aria-labelledby="pdf-2408.15086">pdf</a>, <a href="https://arxiv.org/html/2408.15086v2" title="View HTML" id="html-2408.15086" aria-labelledby="html-2408.15086" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2408.15086" title="Other formats" id="oth-2408.15086" aria-labelledby="oth-2408.15086">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Sample of hydrogen-rich superluminous supernovae from the Zwicky Transient Facility </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pessi,+P">P.J. Pessi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lunnan,+R">R. Lunnan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sollerman,+J">J. Sollerman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Schulze,+S">S. Schulze</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gkini,+A">A. Gkini</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gangopadhyay,+A">A. Gangopadhyay</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yan,+L">L. Yan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gal-Yam,+A">A. Gal-Yam</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Perley,+D">D.A. Perley</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chen,+T">T.-W. Chen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hinds,+K">K.R. Hinds</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Brennan,+S">S.J. Brennan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hu,+Y">Y. Hu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Singh,+A">A. Singh</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Andreoni,+I">I. Andreoni</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cook,+D">D.O. Cook</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fremling,+C">C. Fremling</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ho,+A">A.Y.Q. Ho</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sharma,+Y">Y. Sharma</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=van+Velzen,+S">S. van Velzen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kangas,+T">T. Kangas</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wold,+A">A. Wold</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bellm,+E">E.C. Bellm</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bloom,+J">J.S. Bloom</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Graham,+M">M.J. Graham</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kasliwal,+M">M.M. Kasliwal</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kulkarni,+S">S.R. Kulkarni</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Riddle,+R">R. Riddle</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rusholme,+B">B. Rusholme</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 36 pages. 28 figures. 9 tables </div> <div class='list-journal-ref'><span class='descriptor'>Journal-ref:</span> A&A 695, A142 (2025) </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> Hydrogen-rich superluminous supernovae (SLSNe II) are rare. The exact mechanism producing their extreme light curve peaks is not understood. Analysis of single events and small samples suggest that CSM interaction is the main responsible for their features. However, other mechanisms can not be discarded. Large sample analysis can provide clarification. We aim to characterize the light curves of a sample of 107 SLSNe II to provide valuable information that can be used to validate theoretical models. We analyze the gri light curves of SLSNe II obtained through ZTF. We study peak absolute magnitudes and characteristic timescales. When possible we compute g-r colors, pseudo-bolometric light curves, and estimate lower limits for their total radiated energy. We also study the luminosity distribution of our sample and estimate the percentage of them that would be observable by the LSST. Finally, we compare our sample to other H-rich SNe and to H-poor SLSNe I. SLSNe II are heterogeneous. Their median peak absolute magnitude is -20.3 mag in optical bands. Their rise can take from two weeks to over three months, and their decline from twenty days to over a year. We found no significant correlations between peak magnitude and timescales. SLSNe II tend to show fainter peaks, longer declines and redder colors than SLSNe I. We present the largest sample of SLSNe II light curves to date, comprising of 107 events. Their diversity could be explained by considering different CSM morphologies. Although, theoretical analysis is needed to explore alternative scenarios. Other luminous transients, such as Active Galactic Nuclei, Tidal Disruption Events or SNe Ia-CSM, can easily become contaminants. Thus, good multi-wavelength light curve coverage becomes paramount. LSST could miss 30 percent of the ZTF events in the its footprint in gri bands. Redder bands become important to construct complete samples. </p> </div> </dd> <dt> <a name='item83'>[83]</a> <a href ="/abs/2408.15307" title="Abstract" id="2408.15307"> arXiv:2408.15307 </a> (replaced) [<a href="/pdf/2408.15307" title="Download PDF" id="pdf-2408.15307" aria-labelledby="pdf-2408.15307">pdf</a>, <a href="/format/2408.15307" title="Other formats" id="oth-2408.15307" aria-labelledby="oth-2408.15307">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> The Way To Circumbinary Planets </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Deeg,+H+J">Hans J Deeg</a> (1,2), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Doyle,+L+R">Laurance R Doyle</a> (3) ((1) Instituto de Astrof铆sica de Canarias, (2) Univ. La Laguna, (3) Carl Sagan Center, SETI Institute)</div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> To be published in: Handbook of Exoplanets, 2nd Edition, Hans Deeg and Juan Antonio Belmonte (Eds. in Chief), Springer International Publishing AG, part of Springer Nature. V2 with corrected affiliations and references </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Earth and Planetary Astrophysics (astro-ph.EP)</span>; Solar and Stellar Astrophysics (astro-ph.SR) </div> <p class='mathjax'> Circumbinary planets (CBPs) are planets that orbit around both stars of a binary system. This chapter traces the history of research on CBPs and provides an overview over the current knowledge about CBPs and their detection methods. After early speculations about CBPs, inspired by binary star systems and popularized by fictional works, their scientific exploration began with the identification of circumbinary dust disks and progressed to the detection and characterization of the current sample of CBPs. The major part of this review presents the detection methods for CBPs: eclipse timing variations from the light-travel-time effect and from dynamical interactions, transits, radial velocities, direct imaging, gravitational microlensing and astrometry. Each of these methods is described with its strengths and limitations and the main characeristics of the CBP systems found by them are outlined. The potential habitability of CBPs is considered, taking into account the unique environmental conditions created by orbiting a stellar binary. The importance of multi-method detection strategies is underscored, and future advancements from upcoming missions like PLATO are anticipated, promising to expand the understanding of these intriguing celestial bodies. </p> </div> </dd> <dt> <a name='item84'>[84]</a> <a href ="/abs/2410.06616" title="Abstract" id="2410.06616"> arXiv:2410.06616 </a> (replaced) [<a href="/pdf/2410.06616" title="Download PDF" id="pdf-2410.06616" aria-labelledby="pdf-2410.06616">pdf</a>, <a href="https://arxiv.org/html/2410.06616v4" title="View HTML" id="html-2410.06616" aria-labelledby="html-2410.06616" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2410.06616" title="Other formats" id="oth-2410.06616" aria-labelledby="oth-2410.06616">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Impact of the cosmological expansion on spectral energy density of radiation in the intergalactic medium and once more about Olbers' paradox </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yang,+A">Anguohao Yang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Novosyadlyj,+B">Bohdan Novosyadlyj</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Milinevsky,+G">Gennadi Milinevsky</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 11 pages, 9 figures </div> <div class='list-journal-ref'><span class='descriptor'>Journal-ref:</span> Journal of Physical Studies, v. 29, No. 1, id. 1902 (2025) </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span>; General Relativity and Quantum Cosmology (gr-qc) </div> <p class='mathjax'> We analyse the impact of the expansion of the Universe on the formation of the total spectral energy density of radiation in the intergalactic medium. Assuming the same proper thermal spectrum of sources, we show how the expansion of the Universe changes the nature of the energy distribution of the thermal spectrum: a decrease of the energy density in the Wien range and an increase in the Rayleigh--Jeans range with increasing the redshift of the bulk filled by sources. This is due to the cosmological redshift and the growing contribution of large number of distant sources. The numerical estimations also illustrate the main factors that resolve the Olbers' paradox in the expanding Universe: i) the particle horizon, ii) the finiteness of the volume filled by luminous objects, and iii) the cosmological redshift. Applying the obtained expressions to the epoch of reionization made it possible to estimate the concentration of objects of various classes (stars, globular clusters, dwarf galaxies) necessary for complete reionization of hydrogen at $z=6$. It is shown that even a small part of globular clusters or dwarf galaxies with a thermal spectrum of moderate temperature, from those predicted by Press-Schechter formalism and its improvements, is able to completely reionize hydrogen in the intergalactic medium at $z=6$. </p> </div> </dd> <dt> <a name='item85'>[85]</a> <a href ="/abs/2410.16896" title="Abstract" id="2410.16896"> arXiv:2410.16896 </a> (replaced) [<a href="/pdf/2410.16896" title="Download PDF" id="pdf-2410.16896" aria-labelledby="pdf-2410.16896">pdf</a>, <a href="https://arxiv.org/html/2410.16896v3" title="View HTML" id="html-2410.16896" aria-labelledby="html-2410.16896" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2410.16896" title="Other formats" id="oth-2410.16896" aria-labelledby="oth-2410.16896">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> The Third Konus-Wind Catalog of Short Gamma-Ray bursts </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lysenko,+A+L">Alexandra L. Lysenko</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Svinkin,+D+S">Dmitry S. Svinkin</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Frederiks,+D+D">Dmitry D. Frederiks</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ridnaia,+A+V">Anna V. Ridnaia</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tsvetkova,+A+E">Anastasia E. Tsvetkova</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ulanov,+M+V">Mikhail V. Ulanov</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 16 pages, 8 figures, 8 tables, submitted to PASA </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> In this catalog, we present the results of a systematic study of 199 short gamma-ray bursts (GRBs) detected by Konus-Wind between 2011 January 1 and 2021 August 31. The catalog extends the Second Catalog of short gamma-ray bursts covering the period 1994-2010 by ten years of data. The resulting Konus-Wind short GRB sample includes 494 bursts. From temporal and spectral analyses of the sample, we provide the burst durations, spectral lags, estimates of the minimum variability time scales, rise and decay times, the results of spectral fits with three model functions, the total energy fluences, and the peak energy fluxes of the bursts. We present statistical distributions of these parameters for the complete set of 494 short gamma-ray bursts detected in 1994-2021. We discuss in detail the properties of the bursts with extended emission in the context of the whole short GRB population. Finally, we consider the results in the context of the Type I (merger-origin)/Type II (collapsar-origin) classification, and discuss the extragalactic magnetar giant flare subsample. </p> </div> </dd> <dt> <a name='item86'>[86]</a> <a href ="/abs/2411.08116" title="Abstract" id="2411.08116"> arXiv:2411.08116 </a> (replaced) [<a href="/pdf/2411.08116" title="Download PDF" id="pdf-2411.08116" aria-labelledby="pdf-2411.08116">pdf</a>, <a href="https://arxiv.org/html/2411.08116v2" title="View HTML" id="html-2411.08116" aria-labelledby="html-2411.08116" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2411.08116" title="Other formats" id="oth-2411.08116" aria-labelledby="oth-2411.08116">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Jet Archaeology and Forecasting: Image Variability and Magnetic Field Configuration </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tsunetoe,+Y">Yuh Tsunetoe</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Narayan,+R">Ramesh Narayan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ricarte,+A">Angelo Ricarte</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 20 pages, 17 figures, accepted for publication in ApJ, movie available at <a href="https://youtu.be/FwiKspIXjZk" rel="external noopener nofollow" class="link-external link-https">this https URL</a> </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; Astrophysics of Galaxies (astro-ph.GA) </div> <p class='mathjax'> We investigate how magnetic field variations around accreting black holes on event horizon scales affect the morphology of magnetically-driven jet on larger scales. By performing radiative transfer calculations on general relativistic magnetohydrodynamics simulations, we find that temporal variation in the magnetic flux on the event horizon and the jet power are imprinted on the variability of jet width up to several hundred gravitational radii. When the magnetic flux around the black hole drops and then rises, the jet initially narrows or becomes truncated, then widens, creating a thin-thick pattern that propagates down the jet. This suggests that extended jet observations can provide a history record of horizon-scale magnetic field dynamics, and conversely, upcoming changes in the jet image can be predicted from direct observation of the magnetized accreting plasma near the black hole. Furthermore, the pattern of jet width variations shows acceleration up to the relativistic regime as it moves away from the black hole, aligning with plasma bulk motion. We also find in time-averaged images that both the bulk plasma motion and magnetic field configuration in the jet-launching region, which are sensitive to black hole spin, shape diverse features through relativistic beaming and aberration. Higher black hole spins result in more poloidal bulk motion and toroidal magnetic fields, leading to more symmetric jet images and linear polarization patterns. These results suggest a new method for testing the magnetically arrested disk model and the Blandford-Znajek process, and for determining the black hole spin through observations bridging horizon and jet-launching scales. </p> </div> </dd> <dt> <a name='item87'>[87]</a> <a href ="/abs/2411.09394" title="Abstract" id="2411.09394"> arXiv:2411.09394 </a> (replaced) [<a href="/pdf/2411.09394" title="Download PDF" id="pdf-2411.09394" aria-labelledby="pdf-2411.09394">pdf</a>, <a href="https://arxiv.org/html/2411.09394v2" title="View HTML" id="html-2411.09394" aria-labelledby="html-2411.09394" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2411.09394" title="Other formats" id="oth-2411.09394" aria-labelledby="oth-2411.09394">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Towards Multi Energy Neutrino Astronomy: Diagnosing Enhanced Circumstellar Material around Stripped-Envelope Supernovae </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sawada,+R">Ryo Sawada</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ashida,+Y">Yosuke Ashida</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 13 pages, 7 figures, published in The Astrophysical Journal </div> <div class='list-journal-ref'><span class='descriptor'>Journal-ref:</span> The Astrophysical Journal (2025), Volume 982, id.93, 11 pp </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; High Energy Physics - Experiment (hep-ex) </div> <p class='mathjax'> A novel approach is proposed to reveal a secret birth of enhanced circumstellar material (CSM) surrounding a collapsing massive star using neutrinos as a unique probe. In this scheme, non-thermal TeV-scale neutrinos produced in ejecta-CSM interactions are tied with thermal MeV neutrinos emitted from a pre-explosion burning process, based on a scenario that CSM had been formed via the pre-supernova activity. Taking a representative model of the pre-supernova neutrinos, the spectrum and light curve of the corresponding high-energy CSM neutrinos are calculated at multiple mass-loss efficiencies, which are considered as a systematic uncertainty. In addition, as a part of the method demonstration, the detected event rates along time at JUNO and IceCube, as representative detectors, are estimated for the pre-supernova and CSM neutrinos, respectively, and are compared with the expected background rate at each detector. The presented method is found to be reasonably applicable for the range up to $\sim$1 kpc and even farther with future experimental efforts. The potentialities of other neutrino detectors, such as SK-Gd, Hyper-Kamiokande and KM3NeT, are also discussed. This is a pioneering work of performing astrophysics with neutrinos from diverse energy regimes, initiating multi energy neutrino astronomy in the forthcoming era where next-generation large-scale neutrino telescopes are operating. </p> </div> </dd> <dt> <a name='item88'>[88]</a> <a href ="/abs/2412.02756" title="Abstract" id="2412.02756"> arXiv:2412.02756 </a> (replaced) [<a href="/pdf/2412.02756" title="Download PDF" id="pdf-2412.02756" aria-labelledby="pdf-2412.02756">pdf</a>, <a href="https://arxiv.org/html/2412.02756v2" title="View HTML" id="html-2412.02756" aria-labelledby="html-2412.02756" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2412.02756" title="Other formats" id="oth-2412.02756" aria-labelledby="oth-2412.02756">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Nucleosynthesis Conditions in Outflows of White Dwarfs Collapsing to Neutron Stars </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Batziou,+E">Eirini Batziou</a> (1,2), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Glas,+R">Robert Glas</a> (1), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Janka,+H">H.-Thomas Janka</a> (1), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ehring,+J">Jakob Ehring</a> (3,4,1), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Abdikamalov,+E">Ernazar Abdikamalov</a> (5), <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Just,+O">Oliver Just</a> (6,7) ((1) MPI Astrophysics, Garching, Germany, (2) TUM School of Natural Sciences, Garching, Germany, (3) Academia Sinica, Taipei City, Taiwan, (4) MPI Physics, Garching, Germany, (5) Nazarbayev University, Astana, Kazakhstan, (6) GSI, Darmstadt, Germany, (7) RIKEN, Saitama, Japan)</div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 29 pages, 14 figures, 2 tables; accepted by ApJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; High Energy Physics - Phenomenology (hep-ph) </div> <p class='mathjax'> Accretion-induced collapse (AIC) or merger-induced collapse (MIC) of white dwarfs (WDs) in binary systems is an interesting path to neutron star (NS) and magnetar formation, alternative to stellar core collapse and NS mergers. Such events could add a population of compact remnants in globular clusters, they are expected to produce yet unidentified electromagnetic transients including gamma-ray and radio bursts, and to act as sources of trans-iron elements, neutrinos, and gravitational waves. Here we present the first long-term (>5s post bounce) hydrodynamical simulations in axi-symmetry (2D), using energy- and velocity-dependent three-flavor neutrino transport based on a two-moment scheme. Our set of six models includes initial WD configurations for different masses, central densities, rotation rates, and angular momentum profiles. Our simulations demonstrate that rotation plays a crucial role for the proto-neutron star (PNS) evolution and ejecta properties. We find early neutron-rich ejecta and an increasingly proton-rich neutrino-driven wind at later times in a non-rotating model, in agreement with electron-capture supernova models. In contrast to that and different from previous results, our rotating models eject proton-rich material initially and increasingly more neutron-rich matter as time advances, because an extended accretion torus forms around the PNS and feeds neutrino-driven bipolar outflows for many seconds. AIC and MIC events are thus potential sites of r-process element production, which may imply constraints on their occurrence rates. Finally, our simulations neglect the effects of triaxial deformation and magnetic fields, yet they provide valuable reference cases for comparison with future long-term magneto-hydrodynamic and three-dimensional AIC studies. </p> </div> </dd> <dt> <a name='item89'>[89]</a> <a href ="/abs/2412.09352" title="Abstract" id="2412.09352"> arXiv:2412.09352 </a> (replaced) [<a href="/pdf/2412.09352" title="Download PDF" id="pdf-2412.09352" aria-labelledby="pdf-2412.09352">pdf</a>, <a href="https://arxiv.org/html/2412.09352v2" title="View HTML" id="html-2412.09352" aria-labelledby="html-2412.09352" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2412.09352" title="Other formats" id="oth-2412.09352" aria-labelledby="oth-2412.09352">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Using nebular near-IR spectroscopy to measure asymmetric chemical distributions in 2003fg-like thermonuclear supernovae </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=O'Hora,+J">J. O'Hora</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ashall,+C">C. Ashall</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Shahbandeh,+M">M. Shahbandeh</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hsiao,+E">E. Hsiao</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hoeflich,+P">P. Hoeflich</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Stritzinger,+M+D">M. D. Stritzinger</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Galbany,+L">L. Galbany</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Baron,+E">E. Baron</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=DerKacy,+J">J. DerKacy</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kumar,+S">S. Kumar</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lu,+J">J. Lu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Medler,+K">K. Medler</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Shappee,+B">B. Shappee</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Accepted for publication in ApJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Solar and Stellar Astrophysics (astro-ph.SR)</span>; High Energy Astrophysical Phenomena (astro-ph.HE) </div> <p class='mathjax'> We present an analysis of three near-infrared (NIR; 1.0-2.4 $\mu$m) spectra of the SN 2003fg-like/"super-Chandrasekhar" type Ia supernovae (SNe Ia) SN 2009dc, SN 2020hvf, and SN 2022pul at respective phases +372, +296, and +294~d relative to the epoch of $B$-band maximum. We find that all objects in our sample have asymmetric, or "tilted", [Fe~II] 1.257 and 1.644 $\mu$m profiles. We quantify the asymmetry of these features using five methods: velocity at peak flux, profile tilts, residual testing, velocity fitting, and comparison to deflagration-detonation transition models. Our results demonstrate that, while the profiles of the [Fe II] 1.257 and 1.644 $\mu$m features are widely varied between 2003fg-likes, these features are correlated in shape within the same SN. This implies that line blending is most likely not the dominant cause of the asymmetries inferred from these profiles. Instead, it is more plausible that 2003fg-like SNe have aspherical chemical distributions in their inner regions. These distributions may come from aspherical progenitor systems, such as double white dwarf mergers, or off-center delayed-detonation explosions of Chandrasekhar-mass Carbon-Oxygen white dwarfs. Additional late-phase NIR observation of 2003fg-like SNe and detailed 3-D NLTE modeling of these two explosion scenarios are encouraged. </p> </div> </dd> <dt> <a name='item90'>[90]</a> <a href ="/abs/2501.04772" title="Abstract" id="2501.04772"> arXiv:2501.04772 </a> (replaced) [<a href="/pdf/2501.04772" title="Download PDF" id="pdf-2501.04772" aria-labelledby="pdf-2501.04772">pdf</a>, <a href="https://arxiv.org/html/2501.04772v2" title="View HTML" id="html-2501.04772" aria-labelledby="html-2501.04772" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2501.04772" title="Other formats" id="oth-2501.04772" aria-labelledby="oth-2501.04772">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Deep Photometric Observations of Ultra-Faint Milky Way Satellites Centaurus I and Eridanus IV </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Casey,+Q+O">Quinn O. Casey</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mutlu-Pakdil,+B">Bur莽in Mutlu-Pakdil</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sand,+D+J">David J. Sand</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pace,+A+B">Andrew B. Pace</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Crnojevic,+D">Denija Crnojevic</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Doliva-Dolinsky,+A">Amandine Doliva-Dolinsky</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cerny,+W">William Cerny</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Heiger,+M+E">Mairead E. Heiger</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Riley,+A+H">Alex H. Riley</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ji,+A+P">Alexander P. Ji</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Limberg,+G">Guilherme Limberg</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Marin,+L">Laurella Marin</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Mart%C3%ADnez-V%C3%A1zquez,+C+E">Clara E. Mart铆nez-V谩zquez</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Medina,+G+E">Gustavo E. Medina</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Li,+T+S">Ting S. Li</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Campana,+S+N">Sasha N. Campana</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chaturvedi,+A">Astha Chaturvedi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sakowska,+J+D">Joanna D. Sakowska</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zenteno,+A">Alfredo Zenteno</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Carballo-Bello,+J+A">Julio A. Carballo-Bello</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Navabi,+M">Mahdieh Navabi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bom,+C+R">Clecio R. Bom</a> (DELVE Collaboration)</div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 14 pages, 3 figures. Accepted for publication in ApJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> We present deep Magellan$+$Megacam imaging of Centaurus I (Cen I) and Eridanus IV (Eri IV), two recently discovered Milky Way ultra-faint satellites. Our data reach $\sim2-3$ magnitudes deeper than the discovery data from the DECam Local Volume Exploration (DELVE) Survey. We use these data to constrain their distances, structural properties (e.g., half-light radii, ellipticity, and position angle), and luminosities. We investigate whether these systems show signs of tidal disturbance, and identify new potential member stars using Gaia EDR3. Our deep color-magnitude diagrams show that Cen I and Eri IV are consistent with an old ($\tau\sim 13.0$ Gyr) and metal-poor ($\text{[Fe/H]}\le-2.2$) stellar population. We find Cen I to have a half-light radius of $r_{h}=2.60\pm0.30'$ ($90.6\pm11$ pc), an ellipticity of $\epsilon=0.36\pm0.05$, a distance of $D=119.8\pm4.1$ kpc ($m-M=20.39\pm0.08$ mag), and an absolute magnitude of $M_{V}=-5.39\pm0.19$. Similarly, Eri IV has $r_{h}=3.24\pm0.48'$ ($65.9\pm10$ pc), $\epsilon=0.26\pm0.09$, $D=69.9\pm3.6$ kpc ($m-M=19.22\pm0.11$ mag), and $M_{V}=-3.55\pm0.24$. These systems occupy a space on the size-luminosity plane consistent with other known Milky Way dwarf galaxies which supports the findings from our previous spectroscopic follow-up. Cen I has a well-defined morphology which lacks any clear evidence of tidal disruption, whereas Eri IV hosts a significant extended feature with multiple possible interpretations. </p> </div> </dd> <dt> <a name='item91'>[91]</a> <a href ="/abs/2501.07225" title="Abstract" id="2501.07225"> arXiv:2501.07225 </a> (replaced) [<a href="/pdf/2501.07225" title="Download PDF" id="pdf-2501.07225" aria-labelledby="pdf-2501.07225">pdf</a>, <a href="https://arxiv.org/html/2501.07225v3" title="View HTML" id="html-2501.07225" aria-labelledby="html-2501.07225" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2501.07225" title="Other formats" id="oth-2501.07225" aria-labelledby="oth-2501.07225">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Markarian 590: The AGN Awakens </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Palit,+B">Biswaraj Palit</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=%C5%9Aniegowska,+M">Marzena 艢niegowska</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Markowitz,+A">Alex Markowitz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=R%C3%B3%C5%BCa%C5%84ska,+A">Agata R贸偶a艅ska</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Farah,+J">Joseph Farah</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Howell,+D+A">D. Andrew Howell</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 7 pages, 6 figures; Accepted for publication in MNRAS Letters </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> Changing-Look AGN (CLAGN) Mkn 590 recently underwent a sudden re-ignition, marked by substantial increases in optical/UV and X-ray continuum flux since last couple of years. Swift-XRT observations revealed the re-emergence of a soft X-ray excess (SXE) as the source transitioned from a low-flux state in July 2023 to a significantly higher flux state in October 2024. This evolution was in response to an order-of-magnitude increase in extreme-UV (EUV) continuum emission, detected by Swift-UVOT. Follow-up optical spectra from FLOYDS Faulkes confirmed the enhancement of dynamically broadened Balmer lines, He II emission, and Fe II complex. As the Eddington fraction increased by a factor of $\sim$ 20 over the last 20 months, we found clear evidence of formation of a warm corona, strongly linked to the cold accretion disc underneath. Based on our multi-wavelength study on recent data, we propose that Mkn 590 is currently becoming a Seyfert-1.2, similar to its state in 1990s. </p> </div> </dd> <dt> <a name='item92'>[92]</a> <a href ="/abs/2501.09070" title="Abstract" id="2501.09070"> arXiv:2501.09070 </a> (replaced) [<a href="/pdf/2501.09070" title="Download PDF" id="pdf-2501.09070" aria-labelledby="pdf-2501.09070">pdf</a>, <a href="https://arxiv.org/html/2501.09070v2" title="View HTML" id="html-2501.09070" aria-labelledby="html-2501.09070" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2501.09070" title="Other formats" id="oth-2501.09070" aria-labelledby="oth-2501.09070">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Zapped then Napped? A rapidly quenched remnant leaker candidate with a steep spectroscopic $尾_{UV}$ slope at z=8.5 </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Baker,+W+M">William M. Baker</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=D'Eugenio,+F">Francesco D'Eugenio</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Maiolino,+R">Roberto Maiolino</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bunker,+A+J">Andrew J. Bunker</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Simmonds,+C">Charlotte Simmonds</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Tacchella,+S">Sandro Tacchella</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Witstok,+J">Joris Witstok</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Arribas,+S">Santiago Arribas</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Carniani,+S">Stefano Carniani</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Charlot,+S">St茅phane Charlot</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Chevallard,+J">Jacopo Chevallard</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Curti,+M">Mirko Curti</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Curtis-Lake,+E">Emma Curtis-Lake</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Jones,+G+C">Gareth C. Jones</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Kumari,+N">Nimisha Kumari</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rinaldi,+P">Pierluigi Rinaldi</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Robertson,+B">Brant Robertson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Williams,+C+C">Christina C. Williams</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Willott,+C">Chris Willott</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhu,+Y">Yongda Zhu</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 13 pages, 10 figures, accepted for publication in A&A </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span>; Cosmology and Nongalactic Astrophysics (astro-ph.CO) </div> <p class='mathjax'> We use NIRSpec MSA spectroscopy and NIRCam Photometry to explore the properties of JADES-GS8-RL-1, a rapidly quenched, $z=8.5$ galaxy with a stellar mass of $10^{8.9}M_\odot$, a steep blue UV slope, a Balmer break, and no sign of strong emission lines. With a $\beta_{UV}$=-2.8$\pm 0.2$, as measured from the NIRSpec spectrum, JADES-GS8-RL-1 is consistent with negligible dust attenuation and little to no contribution from the nebular continuum alongside a probable high escape fraction. The $\beta_{UV}$ slope measured from photometry varies from -3.0 in the central regions to -2.2 at the outskirts suggesting possible regional differences in the escape fraction. There are no high-ionisation emission lines, only a tentative 2.9\sig detection of [OII]. Using photometry, this emission appears to be extended, possibly corresponding to weakly ionised gas expelled during or after the quenching process. JADES-GS8-RL-1 is spatially resolved with a half-light radius of 240 pc and has an exponential, disc-like morphology. It appears to have formed all its stars in a short burst within the past 100 Myr with a formation time of $\approx$70 Myr and a quenching time of $\approx$30 Myr. This quenching would have occurred rapidly, making it a more distant example of the kind of low-mass "mini-quenched" galaxies previously observed at high-z. Due to the extremely blue $\beta_{UV}$ slope, our best-fit model predicts a high value for \fesc of >10\%, consistent with the value derived from the $\beta_{UV}$ slope, which when combined with our extraordinarily low O32 upper limit suggests JADES-GS8-RL-1 is a fascinating example of a high-z "remnant leaker" in one of its earliest phases, deep in the epoch of reionisation. </p> </div> </dd> <dt> <a name='item93'>[93]</a> <a href ="/abs/2502.00110" title="Abstract" id="2502.00110"> arXiv:2502.00110 </a> (replaced) [<a href="/pdf/2502.00110" title="Download PDF" id="pdf-2502.00110" aria-labelledby="pdf-2502.00110">pdf</a>, <a href="/format/2502.00110" title="Other formats" id="oth-2502.00110" aria-labelledby="oth-2502.00110">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> New constraints on the evolution of the MHI-M* scaling relation combining CHILES and MIGHTEE-HI data </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bianchetti,+A">Alessandro Bianchetti</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Sinigaglia,+F">Francesco Sinigaglia</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rodighiero,+G">Giulia Rodighiero</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Elson,+E">Ed Elson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Vaccari,+M">Mattia Vaccari</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pisano,+D">D.J. Pisano</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Luber,+N">Nicholas Luber</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Prandoni,+I">Isabella Prandoni</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Hess,+K">Kelley Hess</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Baes,+M">Maarten Baes</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Adams,+E+A">Elizabeth A.K. Adams</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Maccagni,+F+M">Filippo M. Maccagni</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Renzini,+A">Alvio Renzini</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bisigello,+L">Laura Bisigello</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yun,+M">Min Yun</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Momjian,+E">Emmanuel Momjian</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gim,+H+B">Hansung B. Gim</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Pan,+H">Hengxing Pan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Oosterloo,+T+A">Thomas A. Oosterloo</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Dodson,+R">Richard Dodson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Lucero,+D">Danielle Lucero</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Frank,+B+S">Bradley S. Frank</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ilbert,+O">Olivier Ilbert</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Davies,+L+J">Luke J.M. Davies</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Khostovan,+A+A">Ali A. Khostovan</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Salvato,+M">Mara Salvato</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 23 pages, 16 figures, accepted for publication in ApJ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> The improved sensitivity of interferometric facilities to the 21-cm line of atomic hydrogen (HI) enables studies of its properties in galaxies beyond the local Universe. In this work, we perform a 21 cm line spectral stacking analysis combining the MIGHTEE and CHILES surveys in the COSMOS field to derive a robust HI-stellar mass relation at z=0.36. In particular, by stacking thousands of star-forming galaxies subdivided into stellar mass bins, we optimize the signal-to-noise ratio of targets and derive mean HI masses in the different stellar mass intervals for the investigated galaxy population. We combine spectra from the two surveys, estimate HI masses, and derive the scaling relation log10(MHI) = (0.32 +- 0.04)log10(M*) + (6.65 +- 0.36). Our findings indicate that galaxies at z=0.36 are HI richer than those at z=0, but HI poorer than those at z=1, with a slope consistent across redshift, suggesting that stellar mass does not significantly affect HI exchange mechanisms. We also observe a slower growth rate HI relative to the molecular gas, supporting the idea that the accretion of cold gas is slower than the rate of consumption of molecular gas to form stars. This study contributes to understanding the role of atomic gas in galaxy evolution and sets the stage for future development of the field in the upcoming SKA era. </p> </div> </dd> <dt> <a name='item94'>[94]</a> <a href ="/abs/2502.05261" title="Abstract" id="2502.05261"> arXiv:2502.05261 </a> (replaced) [<a href="/pdf/2502.05261" title="Download PDF" id="pdf-2502.05261" aria-labelledby="pdf-2502.05261">pdf</a>, <a href="https://arxiv.org/html/2502.05261v2" title="View HTML" id="html-2502.05261" aria-labelledby="html-2502.05261" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2502.05261" title="Other formats" id="oth-2502.05261" aria-labelledby="oth-2502.05261">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> The Qz5 Survey (I): How the HI Mass Density of the Universe Evolves With Cosmic Time </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Oyarz%C3%BAn,+G+A">Grecco A. Oyarz煤n</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rafelski,+M">Marc Rafelski</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Christensen,+L">Lise Christensen</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ozyurt,+F">Fiona Ozyurt</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Jorgenson,+R+A">Regina A. Jorgenson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Neeleman,+M">Marcel Neeleman</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Fumagalli,+M">Michele Fumagalli</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Prochaska,+J+X">J. Xavier Prochaska</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Worseck,+G">G. Worseck</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Wisz,+M">M.E. Wisz</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Becker,+G+D">George D. Becker</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=L%C3%B3pez,+S">Sebasti谩n L贸pez</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Accepted for publication in ApJ. Main text is composed of 18 pages and 8 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span>; Cosmology and Nongalactic Astrophysics (astro-ph.CO) </div> <p class='mathjax'> We report that the neutral hydrogen (HI) mass density of the Universe ($\rho_{HI}$) increases with cosmic time since $z \sim 5$, peaks at $z \sim 3$, and then decreases toward $z \sim 0$. This is the first result of Qz5, our spectroscopic survey of 63 quasars at $z \gtrsim 5$ with VLT/X-SHOOTER and Keck/ESI aimed at characterizing intervening HI gas absorbers at $z \sim 5$. The main feature of Qz5 is the high resolution ($R \sim 7000 - 9000$) of the spectra, which allows us to (1) accurately detect high column density HI gas absorbers in an increasingly neutral intergalactic medium at $z \sim 5$ and (2) determine the reliability of previous $\rho_{HI}$ measurements derived with lower resolution spectroscopy. We find 5 intervening Damped Ly$\alpha$ absorbers (DLAs) at $z > 4.5$, which corresponds to the lowest DLA incidence rate ($0.034^{0.05}_{0.02}$) at $z \gtrsim 2$. We also measure the lowest $\rho_{HI}$ at $z \gtrsim 2$ from our sample of DLAs and subDLAs, corresponding to $\rho_{HI} = 0.56^{0.82}_{0.31} \times 10^8~$M$_{\odot}~$Mpc$^{-3}$ at $z \sim 5$. Taking into account our measurements at $z \sim 5$ and systematic biases in the DLA detection rate at lower spectral resolutions, we conclude that $\rho_{HI}$ doubles from $z \sim 5$ to $z \sim 3$. From these results emerges a qualitative agreement between how the cosmic densities of HI gas mass, molecular gas mass, and star-formation rate build up with cosmic time. </p> </div> </dd> <dt> <a name='item95'>[95]</a> <a href ="/abs/2503.14605" title="Abstract" id="2503.14605"> arXiv:2503.14605 </a> (replaced) [<a href="/pdf/2503.14605" title="Download PDF" id="pdf-2503.14605" aria-labelledby="pdf-2503.14605">pdf</a>, <a href="https://arxiv.org/html/2503.14605v2" title="View HTML" id="html-2503.14605" aria-labelledby="html-2503.14605" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.14605" title="Other formats" id="oth-2503.14605" aria-labelledby="oth-2503.14605">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> A Million Three-body Binaries Caught by Gaia </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Atallah,+D">Dany Atallah</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ginat,+Y+B">Yonadav Barry Ginat</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Weatherford,+N+C">Newlin C. Weatherford</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 27 pages, 8 figures, 3 tables. Submitted to ApJL. Comments welcome~ </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Astrophysics of Galaxies (astro-ph.GA)</span> </div> <p class='mathjax'> Gaia observations have revealed over a million stellar binary candidates within ~1 kpc of the Sun, predominantly characterized by orbital separations >10^3 AU and eccentricities >0.7. The prevalence of such wide, eccentric binaries has proven challenging to explain through canonical binary formation channels. However, recent advances in our understanding of three-body binary formation (3BBF) -- new binary assembly by the gravitational scattering of three unbound bodies -- have shown that 3BBF in star clusters can efficiently generate wide, highly eccentric binaries. We further explore this possibility by constructing a semi-analytic model of the Galactic binary population in the solar neighborhood, originating from 3BBF in star clusters. The model relies on 3BBF scattering experiments to determine how the 3BBF rate and resulting binary properties scale with local stellar density and velocity dispersion. We then model the Galactic star cluster population, incorporating up-to-date prescriptions for the Galaxy's star formation history as well as the birth properties and internal evolution of its star clusters. Finally, we account for binary destruction induced by perturbations from stellar interactions before cluster escape and and for subsequent changes to binary orbital elements by dynamical interactions in the Galactic field. Without any explicit fine-tuning, our model closely reproduces both the total number of Gaia's wide binaries and their separation distribution, and qualitatively matches the eccentricity distribution, suggesting that 3BBF may be an important formation channel for these enigmatic systems. </p> </div> </dd> <dt> <a name='item96'>[96]</a> <a href ="/abs/2503.15084" title="Abstract" id="2503.15084"> arXiv:2503.15084 </a> (replaced) [<a href="/pdf/2503.15084" title="Download PDF" id="pdf-2503.15084" aria-labelledby="pdf-2503.15084">pdf</a>, <a href="https://arxiv.org/html/2503.15084v2" title="View HTML" id="html-2503.15084" aria-labelledby="html-2503.15084" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.15084" title="Other formats" id="oth-2503.15084" aria-labelledby="oth-2503.15084">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> A constraint on superheavy elements of the GRB-kilonova AT 2023vfi </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Liu,+Z">Zhengyan Liu</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Jiang,+J">Ji-an Jiang</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Zhao,+W">Wen Zhao</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> ApJL accepted </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span> </div> <p class='mathjax'> The discovery of the kilonova (KN) AT 2017gfo, accompanying the gravitational wave event GW170817, provides crucial insight into the synthesis of heavy elements during binary neutron star (BNS) mergers. Following this landmark event, another KN was detected in association with the second-brightest gamma-ray burst (GRB) observed to date, GRB 230307A, and subsequently confirmed by observations of the James Webb Space Telescope (JWST). In this work, we conduct an end-to-end simulation to analyze the temporal evolution of the KN AT 2023vfi associated with GRB 230307A, and constrain the abundances of superheavy elements produced. We find that the temporal evolution of AT 2023vfi is similar to AT 2017gfo in the first week post-burst. Additionally, the \textit{r}-process nuclide abundances of lanthanide-rich ejecta, derived from numerical relativity simulations of BNS mergers, can also successfully interpret the temporal evolution of the KN with the lanthanide-rich ejecta mass of $0.02 M_\odot$, which is consistent with the mass range of dynamical ejecta from numerical simulations in literature. Both findings strongly suggest the hypothesis that GRB 230307A originated from a BNS merger, similar to AT 2017gfo. Based on the first time observation of the KN for JWST, we are able to constrain the superheavy elements of another KN following AT 2017gfo. The pre-radioactive-decay abundances of the superheavy nuclides: $^{222}$Rn, $^{223}$Ra, $^{224}$Ra and $^{225}$Ac, are estimated to be at least on the order of $1 \times 10^{-5}$. These abundance estimates provide valuable insight into the synthesis of superheavy elements in BNS mergers, contributing to our understanding of astrophysical \textit{r}-process nucleosynthesis. </p> </div> </dd> <dt> <a name='item97'>[97]</a> <a href ="/abs/2503.16253" title="Abstract" id="2503.16253"> arXiv:2503.16253 </a> (replaced) [<a href="/pdf/2503.16253" title="Download PDF" id="pdf-2503.16253" aria-labelledby="pdf-2503.16253">pdf</a>, <a href="https://arxiv.org/html/2503.16253v2" title="View HTML" id="html-2503.16253" aria-labelledby="html-2503.16253" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16253" title="Other formats" id="oth-2503.16253" aria-labelledby="oth-2503.16253">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Superluminal Dark Photons as a Solution to the GRB 221009A Anomaly </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Valamontes,+A">Antonios Valamontes</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Markoulakis,+E">Emmanuel Markoulakis</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Adamopoulos,+I">Ioannis Adamopoulos</a></div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Astrophysical Phenomena (astro-ph.HE)</span>; General Relativity and Quantum Cosmology (gr-qc) </div> <p class='mathjax'> The detection of exceptionally high-energy {\gamma}-photons (up to 18 TeV) from GRB 221009A by the LHAASO Collaboration challenges conventional physics. Photon-axion-like particle (ALP) oscillations have been proposed to explain this anomaly, but they rely on specific parameter tuning. We present an alternative explanation involving superluminal dark photons. Building on the frameworks of Markoulakis and Valamontes, we propose that dark photons facilitated faster-than-light (FTL) propagation of information, allowing {\gamma}-photons to bypass extragalactic background light (EBL) attenuation. This hypothesis aligns with cosmological observations and experimental results, including those from the LHC, providing a robust framework for addressing the GRB 221009A anomaly. </p> </div> </dd> <dt> <a name='item98'>[98]</a> <a href ="/abs/2503.16379" title="Abstract" id="2503.16379"> arXiv:2503.16379 </a> (replaced) [<a href="/pdf/2503.16379" title="Download PDF" id="pdf-2503.16379" aria-labelledby="pdf-2503.16379">pdf</a>, <a href="https://arxiv.org/html/2503.16379v2" title="View HTML" id="html-2503.16379" aria-labelledby="html-2503.16379" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2503.16379" title="Other formats" id="oth-2503.16379" aria-labelledby="oth-2503.16379">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> The impact of baryons on the sparsity of simulated galaxy clusters from The Three Hundred Project </div> <div class='list-authors'><a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Corasaniti,+P+S">P. S. Corasaniti</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Richardson,+T+R+G">T. R. G. Richardson</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Ettori,+S">S. Ettori</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=De+Petris,+M">M. De Petris</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rasia,+E">E. Rasia</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Cui,+W">W. Cui</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Yepes,+G">G. Yepes</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Gianfagna,+G">G. Gianfagna</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Bun,+A+M+C+L">A. M. C. Le Bun</a>, <a href="https://arxiv.org/search/astro-ph?searchtype=author&query=Rasera,+Y">Y. Rasera</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 23 pages, 29 figures, accepted in A&A </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Cosmology and Nongalactic Astrophysics (astro-ph.CO)</span> </div> <p class='mathjax'> Measurements of the sparsity of galaxy clusters can be used to probe the cosmological information encoded in the host dark matter halo profile, and infer constraints on the cosmological model parameters. Key to the success of these analyses is the control of potential sources of systematic uncertainty. As an example, the presence of baryons can alter the cluster sparsity with respect to predictions from N-body simulations. Similarly, a radial dependent mass bias, as in the case of masses inferred under the hydrostatic equilibrium (HE) hypothesis, can affect sparsity estimates. We examine the imprint of baryonic processes on the sparsity statistics. Then, we investigate the relation between cluster sparsities and gas mass fraction. Finally, we perform a study of the impact of HE mass bias on sparsity measurements and the implication on cosmological parameter inference analyses. We use catalogues of simulated galaxy clusters from The Three Hundred project and run a comparative analysis of the sparsity of clusters from N-body/hydro simulations implementing different feedback model scenarios. Sparsities which probe the mass profile across a large radial range are affected by the presence of baryons in a way that is particularly sensitive to astrophysical feedback, whereas those probing exclusively external cluster regions are less affected. In the former case, we find the sparsities to be moderately correlated with measurements of the gas fraction in the inner cluster regions. We infer constraints on $S_8$ using synthetic average sparsity measurements generated to evaluate the impact of baryons, selection effects and HE bias. In the case of multiple sparsities these lead to highly bias results. Hence, we calibrate linear bias models that enable us to correct for these effects and recover unbiased constraints that are significantly tighter than those inferred from single sparsity analyses. </p> </div> </dd> <dt> <a name='item99'>[99]</a> <a href ="/abs/2402.05179" title="Abstract" id="2402.05179"> arXiv:2402.05179 </a> (replaced) [<a href="/pdf/2402.05179" title="Download PDF" id="pdf-2402.05179" aria-labelledby="pdf-2402.05179">pdf</a>, <a href="https://arxiv.org/html/2402.05179v3" title="View HTML" id="html-2402.05179" aria-labelledby="html-2402.05179" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2402.05179" title="Other formats" id="oth-2402.05179" aria-labelledby="oth-2402.05179">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Magnetogenesis with gravitational waves and primordial black hole dark matter </div> <div class='list-authors'><a href="https://arxiv.org/search/hep-ph?searchtype=author&query=Balaji,+S">Shyam Balaji</a>, <a href="https://arxiv.org/search/hep-ph?searchtype=author&query=Fairbairn,+M">Malcolm Fairbairn</a>, <a href="https://arxiv.org/search/hep-ph?searchtype=author&query=Olea-Romacho,+M+O">Maria Olalla Olea-Romacho</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 8 pages, 3 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Physics - Phenomenology (hep-ph)</span>; Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Astrophysical Phenomena (astro-ph.HE) </div> <p class='mathjax'> Strongly supercooled first order phase transitions (FOPTs) can produce primordial black hole (PBH) dark matter (DM) along with observable gravitational waves (GWs) from bubble collisions. Such FOPTs may also produce coherent magnetic fields generated by bubble collisions and by turbulence in the primordial plasma. Here we find that the requirement for PBH DM can produce large primordial magnetic fields which subsequently yield intergalactic magnetic fields in the present universe (with magnitude $\lesssim 20$ pG across coherence length scales of $\simeq 0.001$-$0.01$ Mpc, assuming maximally helical magnetic fields) that easily exceed lower bounds from blazar observations. We follow a largely model independent approach and highlight the possibility of producing DM and observable multi-messenger magnetic fields and GW signals visible in next generation experiments. </p> </div> </dd> <dt> <a name='item100'>[100]</a> <a href ="/abs/2405.17721" title="Abstract" id="2405.17721"> arXiv:2405.17721 </a> (replaced) [<a href="/pdf/2405.17721" title="Download PDF" id="pdf-2405.17721" aria-labelledby="pdf-2405.17721">pdf</a>, <a href="https://arxiv.org/html/2405.17721v3" title="View HTML" id="html-2405.17721" aria-labelledby="html-2405.17721" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2405.17721" title="Other formats" id="oth-2405.17721" aria-labelledby="oth-2405.17721">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Rapid detection of gravitational waves from binary black hole mergers using sparse dictionary learning </div> <div class='list-authors'><a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Badger,+C">Charles Badger</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Rahul">Rahul Srinivasan</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Torres-Forn%C3%A9,+A">Alejandro Torres-Forn茅</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Bizouard,+M+A">Marie Anne Bizouard</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Font,+J+A">Jos茅 A. Font</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Sakellariadou,+M">Mairi Sakellariadou</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Lamberts,+A">Astrid Lamberts</a></div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">General Relativity and Quantum Cosmology (gr-qc)</span>; High Energy Astrophysical Phenomena (astro-ph.HE) </div> <p class='mathjax'> Current gravitational wave (GW) detection pipelines for compact binary coalescence based on matched-filtering have reported over 90 confident detections during the first three observing runs of the LIGO-Virgo-KAGRA (LVK) detector network. Decreasing the latency of detection, in particular for future detectors anticipated to have high detection rates, remains an ongoing effort. In this paper, we develop and test a sparse dictionary learning (SDL) algorithm for the rapid detection of GWs. We evaluate the algorithms biases and estimate its GW detection rate for an astrophysical population of binary black holes. The SDL algorithm is assessed using both, simulated data injected into the proposed A+ detector sensitivity and real data containing confident detections from the third LVK observing run. We find that our SDL algorithm can reconstruct a single binary black hole signal in less than 1 s. This suggests that SDL could be regarded as a promising approach for rapid, efficient GW detection in future observing runs of ground-based detectors. </p> </div> </dd> <dt> <a name='item101'>[101]</a> <a href ="/abs/2410.02662" title="Abstract" id="2410.02662"> arXiv:2410.02662 </a> (replaced) [<a href="/pdf/2410.02662" title="Download PDF" id="pdf-2410.02662" aria-labelledby="pdf-2410.02662">pdf</a>, <a href="https://arxiv.org/html/2410.02662v2" title="View HTML" id="html-2410.02662" aria-labelledby="html-2410.02662" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2410.02662" title="Other formats" id="oth-2410.02662" aria-labelledby="oth-2410.02662">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Axion-photon conversion down to the nonrelativistic regime </div> <div class='list-authors'><a href="https://arxiv.org/search/hep-ph?searchtype=author&query=Smarra,+C">Clemente Smarra</a>, <a href="https://arxiv.org/search/hep-ph?searchtype=author&query=Carenza,+P">Pierluca Carenza</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 13 Pages, 7 Figures, text matches the version published by PRD </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Physics - Phenomenology (hep-ph)</span>; Astrophysics of Galaxies (astro-ph.GA); High Energy Physics - Theory (hep-th) </div> <p class='mathjax'> In the presence of a magnetic field, axions can convert into photons and vice versa. The phenomenology of the conversion is captured by a system of two coupled Klein-Gordon equations, which, assuming that the axion is relativistic, is usually recast into a pair of first-order Schr枚dinger-like equations. In such a limit, focusing on a constant magnetic field and plasma frequency, the equations admit an exact analytic solution. The relativistic limit significantly simplifies the calculations and, therefore, it is widely used in phenomenological applications. In this work, we discuss how to evaluate the axion-photon system evolution without relying on such relativistic approximation. In particular, we give an exact analytical solution, valid for any axion energy, in the case that both the magnetic field and plasma frequency are constant. Moreover, we devise an analytic perturbative expansion that allows for tracking the conversion probability in a slightly inhomogeneous magnetic field or plasma frequency, whose characteristic scale of variation is much larger than the typical axion-photon oscillation length. Finally, we discuss a case of resonant axion-photon conversion giving useful simplified formulae that might be directly applied to dark matter axions converting in neutron star magnetospheres. </p> </div> </dd> <dt> <a name='item102'>[102]</a> <a href ="/abs/2410.10280" title="Abstract" id="2410.10280"> arXiv:2410.10280 </a> (replaced) [<a href="/pdf/2410.10280" title="Download PDF" id="pdf-2410.10280" aria-labelledby="pdf-2410.10280">pdf</a>, <a href="https://arxiv.org/html/2410.10280v2" title="View HTML" id="html-2410.10280" aria-labelledby="html-2410.10280" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2410.10280" title="Other formats" id="oth-2410.10280" aria-labelledby="oth-2410.10280">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Dual-Mode Calorimetric Superconducting Nanowire Single Photon Detectors </div> <div class='list-authors'><a href="https://arxiv.org/search/physics?searchtype=author&query=Wu,+H">Hsin-Yeh Wu</a> (1), <a href="https://arxiv.org/search/physics?searchtype=author&query=Besan%C3%A7on,+M">Marc Besan莽on</a> (2), <a href="https://arxiv.org/search/physics?searchtype=author&query=Chen,+J">Jia-Wern Chen</a> (3), <a href="https://arxiv.org/search/physics?searchtype=author&query=Chen,+P">Pisin Chen</a> (1 and 4), <a href="https://arxiv.org/search/physics?searchtype=author&query=Glicenstein,+J">Jean-Fran莽ois Glicenstein</a> (2), <a href="https://arxiv.org/search/physics?searchtype=author&query=Liu,+S">Shu-Xiao Liu</a> (1), <a href="https://arxiv.org/search/physics?searchtype=author&query=Lu,+Y">Yu-Jung Lu</a> (1 and 3)<a href="https://arxiv.org/search/physics?searchtype=author&query=Navick,+X">Xavier-Fran莽ois Navick</a> (2), <a href="https://arxiv.org/search/physics?searchtype=author&query=Paganis,+S">Stathes Paganis</a> (1 and 4), <a href="https://arxiv.org/search/physics?searchtype=author&query=Tuchming,+B">Boris Tuchming</a> (2), <a href="https://arxiv.org/search/physics?searchtype=author&query=Tsionou,+D">Dimitra Tsionou</a> (1), <a href="https://arxiv.org/search/physics?searchtype=author&query=Tsai,+F">Feng-Yang Tsai</a> (3) ((1) National Taiwan University, (2) CEA-IRFU, Paris-Saclay University, (3) Academia Sinica, Taipei, Taiwan, (4) Leung Center for Cosmology and Particle Astrophysics)</div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> Manuscript prepared for APL </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">Instrumentation and Detectors (physics.ins-det)</span>; Instrumentation and Methods for Astrophysics (astro-ph.IM); High Energy Physics - Experiment (hep-ex); Quantum Physics (quant-ph) </div> <p class='mathjax'> A dual-operation mode SNSPD is proposed. In the conventional Geiger mode, the sensor operates at temperatures well below the critical temperature, Tc, working as an event counter without sensitivity to the number of photons impinging the sensor. In the calorimetric mode, the detector is operated at temperatures just below TC and displays calorimetric sensitivity in the range of 15 to 250 absorbed-photon energy equivalent for a photon beam with a wavelength of 515 nm. In this energy sensitive mode, photon absorption causes Joule heating of the SNSPD that becomes partially resistive without the presence of latching. Depending on the application, by tuning the sample temperature and bias current using the same readout system, the SNSPD can readily switch between the two modes. In the calorimetric mode, SNSPD recovery times shorter than the ones in the Geiger mode are observed, reaching values as low as 560 ps. Dual-mode SNSPDs may provide significant advancements in spectroscopy and calorimetry, where precise timing, photon counting and energy resolution are required. </p> </div> </dd> <dt> <a name='item103'>[103]</a> <a href ="/abs/2410.10973" title="Abstract" id="2410.10973"> arXiv:2410.10973 </a> (replaced) [<a href="/pdf/2410.10973" title="Download PDF" id="pdf-2410.10973" aria-labelledby="pdf-2410.10973">pdf</a>, <a href="https://arxiv.org/html/2410.10973v3" title="View HTML" id="html-2410.10973" aria-labelledby="html-2410.10973" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2410.10973" title="Other formats" id="oth-2410.10973" aria-labelledby="oth-2410.10973">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Scalar-Gauss-Bonnet gravity: Infrared causality and detectability of GW observations </div> <div class='list-authors'><a href="https://arxiv.org/search/hep-th?searchtype=author&query=Nie,+W">Wen-Kai Nie</a>, <a href="https://arxiv.org/search/hep-th?searchtype=author&query=Tan,+L">Lin-Tao Tan</a>, <a href="https://arxiv.org/search/hep-th?searchtype=author&query=Zhang,+J">Jun Zhang</a>, <a href="https://arxiv.org/search/hep-th?searchtype=author&query=Zhou,+S">Shuang-Yong Zhou</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> 26 pages, 6 figures </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">High Energy Physics - Theory (hep-th)</span>; Cosmology and Nongalactic Astrophysics (astro-ph.CO); General Relativity and Quantum Cosmology (gr-qc) </div> <p class='mathjax'> We investigate time delays of wave scatterings around black hole backgrounds in scalar-tensor effective field theories of gravity. The scalar-Gauss-Bonnet (sGB) couplings, being corrections of the lowest orders, can give rise to hairy black holes. By requiring infrared causality, we impose lower bounds on the cutoff scales of the theories. With these bounds, we further discuss the detectability of sGB gravity in gravitational waves from binary black hole mergers. Compared with the gravitational effective field theories that contain only the two tensor modes, adding extra degrees of freedom, such as adding a scalar, opens up a detectable window in the planned observations. </p> </div> </dd> <dt> <a name='item104'>[104]</a> <a href ="/abs/2411.04184" title="Abstract" id="2411.04184"> arXiv:2411.04184 </a> (replaced) [<a href="/pdf/2411.04184" title="Download PDF" id="pdf-2411.04184" aria-labelledby="pdf-2411.04184">pdf</a>, <a href="https://arxiv.org/html/2411.04184v2" title="View HTML" id="html-2411.04184" aria-labelledby="html-2411.04184" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2411.04184" title="Other formats" id="oth-2411.04184" aria-labelledby="oth-2411.04184">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> Self-consistent multidimensional Penrose process driven by magnetic reconnection </div> <div class='list-authors'><a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Camilloni,+F">Filippo Camilloni</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Rezzolla,+L">Luciano Rezzolla</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> v2: 7 pages + 3 appendix, 4 figures, matches published version in ApJL </div> <div class='list-journal-ref'><span class='descriptor'>Journal-ref:</span> ApJL 982 L31 (2025) </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">General Relativity and Quantum Cosmology (gr-qc)</span>; High Energy Astrophysical Phenomena (astro-ph.HE) </div> <p class='mathjax'> Astronomical observations and numerical simulations are providing increasing evidence that resistive effects in plasmas around black holes play an important role in determining the phenomenology observed from these objects. In this spirit, we present a general approach to the study of a Penrose process driven by plasmoids that are produced at reconnection sites along current sheets. Our formalism is meant to determine the physical conditions that make a plasmoid-driven Penrose process energetically viable and can be applied to scenarios that are matter- or magnetic-field-dominated, that is, in magnetohydrodynamical or force-free descriptions. By exploring reconnection from an axisymmetric but curved surface, our approach can be considered genuinely multidimensional and allows us to explore conditions that are beyond the ones explored so far and that have been restricted to the equatorial plane. Furthermore, it provides a direct contact with numerical simulations of accretion onto black holes, which exhibit an intense reconnection activity outside the equatorial plane. Finally, to describe the kinematics of the plasma self-consistently, we use the well-known configuration of an equilibrium torus with a purely toroidal magnetic field. For such a torus, we discuss the existence of an ``ergobelt'', \ie a nontrivial surface penetrating the ergosphere and acting as a natural a site for the occurrence of reconnection, and from where we estimate the energetics of a plasmoid-driven Penrose process. </p> </div> </dd> <dt> <a name='item105'>[105]</a> <a href ="/abs/2502.15272" title="Abstract" id="2502.15272"> arXiv:2502.15272 </a> (replaced) [<a href="/pdf/2502.15272" title="Download PDF" id="pdf-2502.15272" aria-labelledby="pdf-2502.15272">pdf</a>, <a href="https://arxiv.org/html/2502.15272v3" title="View HTML" id="html-2502.15272" aria-labelledby="html-2502.15272" rel="noopener noreferrer" target="_blank">html</a>, <a href="/format/2502.15272" title="Other formats" id="oth-2502.15272" aria-labelledby="oth-2502.15272">other</a>] </dt> <dd> <div class='meta'> <div class='list-title mathjax'><span class='descriptor'>Title:</span> The correspondence of generalised entropic cosmology theory with $F(T)$ and $F(Q)$ modified gravity and gravitational waves </div> <div class='list-authors'><a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Nojiri,+S">Shin'ichi Nojiri</a>, <a href="https://arxiv.org/search/gr-qc?searchtype=author&query=Odintsov,+S+D">Sergei D. Odintsov</a></div> <div class='list-comments mathjax'><span class='descriptor'>Comments:</span> LaTeX 22 pages, references added, some corrections are done, the version to appear in Physics of the Dark Universe </div> <div class='list-subjects'><span class='descriptor'>Subjects:</span> <span class="primary-subject">General Relativity and Quantum Cosmology (gr-qc)</span>; Cosmology and Nongalactic Astrophysics (astro-ph.CO); High Energy Physics - Theory (hep-th) </div> <p class='mathjax'> We investigate the correspondence between modified gravity theories and general entropic cosmology theory. Such a theory is proposed by an analogy with Jacobson's work, where the Einstein equation was derived from the Bekenstein-Hawking entropy. We compare FLRW equations obtained in entropic gravity with those in modified gravity theories. It is found the correspondence of $F(T)$ and $F(Q)$ gravities and general entropic gravity. We regard the $F(T)$ and $F(Q)$ gravity theories as effective local theories corresponding to the entropic gravity theories and we investigate the gravitational waves. The obtained equation of the gravitational wave is identical to that in Einstein's gravity except that the gravitational coupling is modified by the functional form of the functions $F(T)$ and $F(Q)$. It is interesting that in the case of the Tsallis entropic cosmology, the gravitational coupling becomes small or large, which may suppress or enhance the emission of the gravitational wave. </p> </div> </dd> </dl> <div class='paging'>Total of 105 entries </div> <div class='morefewer'>Showing up to 2000 entries per page: <a href=/list/astro-ph/new?skip=0&show=1000 rel="nofollow"> fewer</a> | <span style="color: #454545">more</span> | <span style="color: #454545">all</span> </div> </div> </div> </div> </main> <footer style="clear: both;"> <div class="columns is-desktop" role="navigation" aria-label="Secondary" style="margin: -0.75em -0.75em 0.75em -0.75em"> <!-- Macro-Column 1 --> <div class="column" style="padding: 0;"> <div class="columns"> <div class="column"> <ul style="list-style: none; line-height: 2;"> <li><a href="https://info.arxiv.org/about">About</a></li> <li><a href="https://info.arxiv.org/help">Help</a></li> </ul> </div> <div class="column"> <ul style="list-style: none; line-height: 2;"> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>contact arXiv</title><desc>Click here to contact arXiv</desc><path d="M502.3 190.8c3.9-3.1 9.7-.2 9.7 4.7V400c0 26.5-21.5 48-48 48H48c-26.5 0-48-21.5-48-48V195.6c0-5 5.7-7.8 9.7-4.7 22.4 17.4 52.1 39.5 154.1 113.6 21.1 15.4 56.7 47.8 92.2 47.6 35.7.3 72-32.8 92.3-47.6 102-74.1 131.6-96.3 154-113.7zM256 320c23.2.4 56.6-29.2 73.4-41.4 132.7-96.3 142.8-104.7 173.4-128.7 5.8-4.5 9.2-11.5 9.2-18.9v-19c0-26.5-21.5-48-48-48H48C21.5 64 0 85.5 0 112v19c0 7.4 3.4 14.3 9.2 18.9 30.6 23.9 40.7 32.4 173.4 128.7 16.8 12.2 50.2 41.8 73.4 41.4z"/></svg> <a href="https://info.arxiv.org/help/contact.html"> Contact</a> </li> <li> <svg xmlns="http://www.w3.org/2000/svg" viewBox="0 0 512 512" class="icon filter-black" role="presentation"><title>subscribe to arXiv mailings</title><desc>Click here to subscribe</desc><path d="M476 3.2L12.5 270.6c-18.1 10.4-15.8 35.6 2.2 43.2L121 358.4l287.3-253.2c5.5-4.9 13.3 2.6 8.6 8.3L176 407v80.5c0 23.6 28.5 32.9 42.5 15.8L282 426l124.6 52.2c14.2 6 30.4-2.9 33-18.2l72-432C515 7.8 493.3-6.8 476 3.2z"/></svg> <a href="https://info.arxiv.org/help/subscribe"> Subscribe</a> </li> </ul> </div> </div> </div> <!-- End Macro-Column 1 --> <!-- Macro-Column 2 --> <div class="column" style="padding: 0;"> <div class="columns"> <div class="column"> <ul style="list-style: none; 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