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class="pagination-ellipsis">…</span></li> </ul> </nav> <ol class="breathe-horizontal" start="1"> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2503.02112">arXiv:2503.02112</a> <span> [<a href="https://arxiv.org/pdf/2503.02112">pdf</a>, <a href="https://arxiv.org/format/2503.02112">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Building Machine Learning Challenges for Anomaly Detection in Science </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Campolongo%2C+E+G">Elizabeth G. Campolongo</a>, <a href="/search/?searchtype=author&query=Chou%2C+Y">Yuan-Tang Chou</a>, <a href="/search/?searchtype=author&query=Govorkova%2C+E">Ekaterina Govorkova</a>, <a href="/search/?searchtype=author&query=Bhimji%2C+W">Wahid Bhimji</a>, <a href="/search/?searchtype=author&query=Chao%2C+W">Wei-Lun Chao</a>, <a href="/search/?searchtype=author&query=Harris%2C+C">Chris Harris</a>, <a href="/search/?searchtype=author&query=Hsu%2C+S">Shih-Chieh Hsu</a>, <a href="/search/?searchtype=author&query=Lapp%2C+H">Hilmar Lapp</a>, <a href="/search/?searchtype=author&query=Neubauer%2C+M+S">Mark S. Neubauer</a>, <a href="/search/?searchtype=author&query=Namayanja%2C+J">Josephine Namayanja</a>, <a href="/search/?searchtype=author&query=Subramanian%2C+A">Aneesh Subramanian</a>, <a href="/search/?searchtype=author&query=Harris%2C+P">Philip Harris</a>, <a href="/search/?searchtype=author&query=Anand%2C+A">Advaith Anand</a>, <a href="/search/?searchtype=author&query=Carlyn%2C+D+E">David E. Carlyn</a>, <a href="/search/?searchtype=author&query=Ghosh%2C+S">Subhankar Ghosh</a>, <a href="/search/?searchtype=author&query=Lawrence%2C+C">Christopher Lawrence</a>, <a href="/search/?searchtype=author&query=Moreno%2C+E">Eric Moreno</a>, <a href="/search/?searchtype=author&query=Raikman%2C+R">Ryan Raikman</a>, <a href="/search/?searchtype=author&query=Wu%2C+J">Jiaman Wu</a>, <a href="/search/?searchtype=author&query=Zhang%2C+Z">Ziheng Zhang</a>, <a href="/search/?searchtype=author&query=Adhi%2C+B">Bayu Adhi</a>, <a href="/search/?searchtype=author&query=Gharehtoragh%2C+M+A">Mohammad Ahmadi Gharehtoragh</a>, <a href="/search/?searchtype=author&query=Monsalve%2C+S+A">Sa煤l Alonso Monsalve</a>, <a href="/search/?searchtype=author&query=Babicz%2C+M">Marta Babicz</a>, <a href="/search/?searchtype=author&query=Baig%2C+F">Furqan Baig</a> , et al. (125 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2503.02112v1-abstract-short" style="display: inline;"> Scientific discoveries are often made by finding a pattern or object that was not predicted by the known rules of science. Oftentimes, these anomalous events or objects that do not conform to the norms are an indication that the rules of science governing the data are incomplete, and something new needs to be present to explain these unexpected outliers. The challenge of finding anomalies can be c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.02112v1-abstract-full').style.display = 'inline'; document.getElementById('2503.02112v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2503.02112v1-abstract-full" style="display: none;"> Scientific discoveries are often made by finding a pattern or object that was not predicted by the known rules of science. Oftentimes, these anomalous events or objects that do not conform to the norms are an indication that the rules of science governing the data are incomplete, and something new needs to be present to explain these unexpected outliers. The challenge of finding anomalies can be confounding since it requires codifying a complete knowledge of the known scientific behaviors and then projecting these known behaviors on the data to look for deviations. When utilizing machine learning, this presents a particular challenge since we require that the model not only understands scientific data perfectly but also recognizes when the data is inconsistent and out of the scope of its trained behavior. In this paper, we present three datasets aimed at developing machine learning-based anomaly detection for disparate scientific domains covering astrophysics, genomics, and polar science. We present the different datasets along with a scheme to make machine learning challenges around the three datasets findable, accessible, interoperable, and reusable (FAIR). Furthermore, we present an approach that generalizes to future machine learning challenges, enabling the possibility of large, more compute-intensive challenges that can ultimately lead to scientific discovery. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.02112v1-abstract-full').style.display = 'none'; document.getElementById('2503.02112v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 March, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages 6 figures to be submitted to Nature Communications</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2503.01808">arXiv:2503.01808</a> <span> [<a href="https://arxiv.org/pdf/2503.01808">pdf</a>, <a href="https://arxiv.org/format/2503.01808">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computational Geometry">cs.CG</span> </div> </div> <p class="title is-5 mathjax"> Visualization of Event Graphs for Train Schedules </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Hartleb%2C+J">Johann Hartleb</a>, <a href="/search/?searchtype=author&query=Schmidt%2C+M">Marie Schmidt</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Samuel Wolf</a>, <a href="/search/?searchtype=author&query=Wolff%2C+A">Alexander Wolff</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2503.01808v1-abstract-short" style="display: inline;"> Software that is used to compute or adjust train schedules is based on so-called event graphs. The vertices of such a graph correspond to events; each event is associated with a point in time, a location, and a train. A train line corresponds to a sequence of events (ordered by time) that are associated with the same train. The event graph has a directed edge from an earlier to a later event if th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.01808v1-abstract-full').style.display = 'inline'; document.getElementById('2503.01808v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2503.01808v1-abstract-full" style="display: none;"> Software that is used to compute or adjust train schedules is based on so-called event graphs. The vertices of such a graph correspond to events; each event is associated with a point in time, a location, and a train. A train line corresponds to a sequence of events (ordered by time) that are associated with the same train. The event graph has a directed edge from an earlier to a later event if they are consecutive along a train line. Events that occur at the same location do not occur at the same time. In this paper, we present a way to visualize such graphs, namely time-space diagrams. A time-space diagram is a straight-line drawing of the event graph with the additional constraint that all vertices that belong to the same location lie on the same horizontal line and that the x-coordinate of each vertex is given by its point in time. Hence, it remains to determine the y-coordinates of the locations. A good drawing of a time-space diagram supports users (or software developers) when creating (software for computing) train schedules. To enhance readability, we aim to minimize the number of turns in time-space diagrams. To this end, we establish a connection between this problem and Maximum Betweenness. Then we develop exact reduction rules to reduce the instance size. We also propose a parameterized algorithm and devise a heuristic that we evaluate experimentally on a real-world dataset. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2503.01808v1-abstract-full').style.display = 'none'; document.getElementById('2503.01808v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 March, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2025. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.20472">arXiv:2502.20472</a> <span> [<a href="https://arxiv.org/pdf/2502.20472">pdf</a>, <a href="https://arxiv.org/format/2502.20472">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Soft Condensed Matter">cond-mat.soft</span> </div> </div> <p class="title is-5 mathjax"> Simple molecules and complex chemistry in a protoplanetary disk: A JWST investigation of the highly inclined disk d216-0939 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Potapov%2C+A">Alexey Potapov</a>, <a href="/search/?searchtype=author&query=Linz%2C+H">Hendrik Linz</a>, <a href="/search/?searchtype=author&query=Bouwman%2C+J">Jeroen Bouwman</a>, <a href="/search/?searchtype=author&query=Rocha%2C+W">Will Rocha</a>, <a href="/search/?searchtype=author&query=Martin%2C+J">Johannes Martin</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/?searchtype=author&query=Henning%2C+T">Thomas Henning</a>, <a href="/search/?searchtype=author&query=Terada%2C+H">Hiroshi Terada</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.20472v1-abstract-short" style="display: inline;"> While the number of detected molecules, particularly complex organic molecules, in the solid-state in astrophysical environments is still rather limited, laboratory experiments and astrochemical models predict many potential candidates. Detection of molecules in protoplanetary disks provides a bridge between the chemical evolution of the interstellar medium and the chemistry of planets and their a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.20472v1-abstract-full').style.display = 'inline'; document.getElementById('2502.20472v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.20472v1-abstract-full" style="display: none;"> While the number of detected molecules, particularly complex organic molecules, in the solid-state in astrophysical environments is still rather limited, laboratory experiments and astrochemical models predict many potential candidates. Detection of molecules in protoplanetary disks provides a bridge between the chemical evolution of the interstellar medium and the chemistry of planets and their atmospheres. The excellent spectral sensitivity, broad wavelength coverage and high spatial resolution of the James Webb Space Telescope (JWST) allows for making progress in exploring chemical compositions of various astrophysical environments including planet-forming disks. They are a prerequisite for probing the disk content by means of sensitive absorption studies. In this paper, we present initial results of the JWST Cycle 1 GO program 1741 on d216-0939, a highly inclined TTauri disk located in the outskirts of the Orion Nebula Cluster. We utilise the NIRSpec and MIRI integral field unit spectrographs to cover its spectrum from 1.7 to 28~$渭$m. In the d216-0939 disk, we give assignments of the composition of silicate grains. We unambiguously detect solid-state features of H$_2$O, CO$_2$, $^{13}$CO$_2$, CO, OCN$^-$, and tentatively OCS; species that had been detected recently also in other circumstellar disks. For the first time in disks, we provide unique detections of ices carrying NH$_4^+$ and the complex organic molecule ammonium carbamate (NH$_4^+$NH$_2$COO$^-$). The latter detections speak for a very efficient NH$_3$ chemistry in the disk. We also show the very important role of scattering in the analysis of observational spectra of highly inclined disks. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.20472v1-abstract-full').style.display = 'none'; document.getElementById('2502.20472v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">10 pages, 7 figures, 6 tables, accepted by A&A on February 20, 2025</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.14353">arXiv:2502.14353</a> <span> [<a href="https://arxiv.org/pdf/2502.14353">pdf</a>, <a href="https://arxiv.org/format/2502.14353">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computational Complexity">cs.CC</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Social and Information Networks">cs.SI</span> </div> </div> <p class="title is-5 mathjax"> Eliminating Majority Illusions </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Fioravantes%2C+F">Foivos Fioravantes</a>, <a href="/search/?searchtype=author&query=Lahiri%2C+A">Abhiruk Lahiri</a>, <a href="/search/?searchtype=author&query=Lauerbach%2C+A">Antonio Lauerbach</a>, <a href="/search/?searchtype=author&query=Sabater%2C+L">Llu铆s Sabater</a>, <a href="/search/?searchtype=author&query=Sieper%2C+M+D">Marie Diana Sieper</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Samuel Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.14353v1-abstract-short" style="display: inline;"> An opinion illusion refers to a phenomenon in social networks where agents may witness distributions of opinions among their neighbours that do not accurately reflect the true distribution of opinions in the population as a whole. A specific case of this occurs when there are only two possible choices, such as whether to receive the COVID-19 vaccine or vote on EU membership, which is commonly refe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.14353v1-abstract-full').style.display = 'inline'; document.getElementById('2502.14353v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.14353v1-abstract-full" style="display: none;"> An opinion illusion refers to a phenomenon in social networks where agents may witness distributions of opinions among their neighbours that do not accurately reflect the true distribution of opinions in the population as a whole. A specific case of this occurs when there are only two possible choices, such as whether to receive the COVID-19 vaccine or vote on EU membership, which is commonly referred to as a majority illusion. In this work, we study the topological properties of social networks that lead to opinion illusions and focus on minimizing the number of agents that need to be influenced to eliminate these illusions. To do so, we propose an initial, but systematic study of the algorithmic behaviour of this problem. We show that the problem is NP-hard even for underlying topologies that are rather restrictive, being planar and of bounded diameter. We then look for exact algorithms that scale well as the input grows (FPT). We argue the in-existence of such algorithms even when the number of vertices that must be influenced is bounded, or when the social network is arranged in a ``path-like'' fashion (has bounded pathwidth). On the positive side, we present an FPT algorithm for networks with ``star-like'' structure (bounded vertex cover number). Finally, we construct an FPT algorithm for ``tree-like'' networks (bounded treewidth) when the number of vertices that must be influenced is bounded. This algorithm is then used to provide a PTAS for planar graphs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.14353v1-abstract-full').style.display = 'none'; document.getElementById('2502.14353v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">To be presented in AAMAS'25</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.13807">arXiv:2502.13807</a> <span> [<a href="https://arxiv.org/pdf/2502.13807">pdf</a>, <a href="https://arxiv.org/ps/2502.13807">ps</a>, <a href="https://arxiv.org/format/2502.13807">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Quantum Physics">quant-ph</span> </div> </div> <p class="title is-5 mathjax"> A local, many-worlds, model of quantum correlations with finite information flow </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Montina%2C+A">Alberto Montina</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Stefan Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.13807v2-abstract-short" style="display: inline;"> Ontological theories, such as the de Broglie-Bohm theory, address the measurement problem by introducing auxiliary random variables that specify, in particular, the actual values of macroscopic observables. Such models may be psi-epistemic, meaning the quantum state is not part of the ontology. A serious issue of this route toward a realistic completion of quantum theory is raised by Bell's proof… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.13807v2-abstract-full').style.display = 'inline'; document.getElementById('2502.13807v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.13807v2-abstract-full" style="display: none;"> Ontological theories, such as the de Broglie-Bohm theory, address the measurement problem by introducing auxiliary random variables that specify, in particular, the actual values of macroscopic observables. Such models may be psi-epistemic, meaning the quantum state is not part of the ontology. A serious issue of this route toward a realistic completion of quantum theory is raised by Bell's proof that ontological theories are nonlocal. A possible resolution is to reject the assumption that measurements have single actual outcomes. Indeed, relaxing this premise, Deutsch and Hayden showed that Bell's theorem can be evaded by delaying the buildup of the correlations until the parties compare their outcomes at a meeting point. However, the Deutsch-Hayden theory, which is determinist and psi-ontic, leads to an infinite information flow towards the meeting point. Furthermore, alternative branches are weighted by amplitudes, leading to interpretative issues. By integrating the randomness of single-world theories and the branching of the Deutsch-Hayden theory, we introduce a simple psi-epistemic local model of projective measurements on two spatially separate maximally entangled qubits. Because of its randomness, the model requires two "equally weighted" branches and a finite information flow -- just one bit per measurement is communicated to the meeting point. We explore how this hybrid approach, employing both randomness and branching, addresses key challenges of single-world and Deutsch-Hayden theories. On one hand, the branching allows us to circumvent nonlocality and, possibly, contextuality. On the other hand, randomness makes it more natural and economical to derive quantum probabilities from unweighted counts of branches and ensemble averages. Furthermore, it allows for a reduction of the information flow by stripping the quantum state of its `ontic' rank. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.13807v2-abstract-full').style.display = 'none'; document.getElementById('2502.13807v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 26 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 19 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">We have modified some statements which referred to particular and not broadly accepted approaches to MWI. We highlight our results rather than present a broad discussion on many-worlds interpretation, which is not the purpose of this paper. This version presents a better flow of our reasoning. We also include a mention to Pusey-Barrett-Rudolph theorem</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.11722">arXiv:2502.11722</a> <span> [<a href="https://arxiv.org/pdf/2502.11722">pdf</a>, <a href="https://arxiv.org/format/2502.11722">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> </div> <p class="title is-5 mathjax"> Evidence for an accretion bridge in the DX Cha circumbinary system from VLTI/MATISSE observations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Juh%C3%A1sz%2C+T">T铆mea Juh谩sz</a>, <a href="/search/?searchtype=author&query=Varga%2C+J">J贸zsef Varga</a>, <a href="/search/?searchtype=author&query=%C3%81brah%C3%A1m%2C+P">P茅ter 脕brah谩m</a>, <a href="/search/?searchtype=author&query=K%C3%B3sp%C3%A1l%2C+%C3%81">脕gnes K贸sp谩l</a>, <a href="/search/?searchtype=author&query=Lykou%2C+F">Foteini Lykou</a>, <a href="/search/?searchtype=author&query=Chen%2C+L">Lei Chen</a>, <a href="/search/?searchtype=author&query=Mo%C3%B3r%2C+A">Attila Mo贸r</a>, <a href="/search/?searchtype=author&query=de+Miera%2C+F+C">Fernando Cruz-S谩enz de Miera</a>, <a href="/search/?searchtype=author&query=Lopez%2C+B">Bruno Lopez</a>, <a href="/search/?searchtype=author&query=Matter%2C+A">Alexis Matter</a>, <a href="/search/?searchtype=author&query=van+Boekel%2C+R">Roy van Boekel</a>, <a href="/search/?searchtype=author&query=Hogerheijde%2C+M">Michiel Hogerheijde</a>, <a href="/search/?searchtype=author&query=Abello%2C+M">Margaux Abello</a>, <a href="/search/?searchtype=author&query=Augereau%2C+J">Jean-Charles Augereau</a>, <a href="/search/?searchtype=author&query=Boley%2C+P">Paul Boley</a>, <a href="/search/?searchtype=author&query=Danchi%2C+W+C">William C. Danchi</a>, <a href="/search/?searchtype=author&query=Henning%2C+T">Thomas Henning</a>, <a href="/search/?searchtype=author&query=Letessier%2C+M">Mathis Letessier</a>, <a href="/search/?searchtype=author&query=Ma%2C+J">Jie Ma</a>, <a href="/search/?searchtype=author&query=Priolet%2C+P">Philippe Priolet</a>, <a href="/search/?searchtype=author&query=Scheuck%2C+M">Marten Scheuck</a>, <a href="/search/?searchtype=author&query=Weigelt%2C+G">Gerd Weigelt</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.11722v1-abstract-short" style="display: inline;"> DX Cha (HD 104237) is a spectroscopic binary consisting of a Herbig A7.5Ve-A8Ve primary star and a K3-type companion. Here we report on new $3.55$ micrometer interferometric observations of this source with the Multi Aperture Mid-Infrared Spectroscopic Experiment (MATISSE) at the Very Large Telescope Interferometer (VLTI). To model the four MATISSE observations obtained between 2020 and 2023, we c… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.11722v1-abstract-full').style.display = 'inline'; document.getElementById('2502.11722v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.11722v1-abstract-full" style="display: none;"> DX Cha (HD 104237) is a spectroscopic binary consisting of a Herbig A7.5Ve-A8Ve primary star and a K3-type companion. Here we report on new $3.55$ micrometer interferometric observations of this source with the Multi Aperture Mid-Infrared Spectroscopic Experiment (MATISSE) at the Very Large Telescope Interferometer (VLTI). To model the four MATISSE observations obtained between 2020 and 2023, we constructed a time-dependent interferometric model of the system, using the oimodeler software. The model consists of an asymmetric ring and two point sources on a Keplerian orbit. Our best-fit model consists of a circumbinary ring with a diameter of $0.86$ au ($8.1$ mas), featuring a strong azimuthal asymmetry. We found that the position angle of the asymmetry changes tens of degrees between the MATISSE epochs. The ring is relatively narrow, with a full width at half maximum (FWHM) of $\sim$$0.13$ au ($1.23$ mas). The presence of circumstellar dust emission so close to the binary is unexpected, as previous hydrodynamic simulations predicted an inner disk cavity with a diameter of $\sim$$4$ au ($\sim$$37.5$ mas). Thus, we argue that the narrow envelope of material we detected is probably not a gravitationally stable circumbinary ring, but may be part of tidal accretion streamers channeling material from the inner edge of the disk toward the stars. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.11722v1-abstract-full').style.display = 'none'; document.getElementById('2502.11722v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in ApJ, 11 pages, 5 figures, 5 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.09714">arXiv:2502.09714</a> <span> [<a href="https://arxiv.org/pdf/2502.09714">pdf</a>, <a href="https://arxiv.org/format/2502.09714">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> </div> </div> <p class="title is-5 mathjax"> A Discontinuous Galerkin Method for Simulating 3D Seismic Wave Propagation in Nonlinear Rock Models: Verification and Application to the 2015 Mw 7.8 Gorkha Earthquake </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Niu%2C+Z">Zihua Niu</a>, <a href="/search/?searchtype=author&query=Gabriel%2C+A">Alice-Agnes Gabriel</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/?searchtype=author&query=Ulrich%2C+T">Thomas Ulrich</a>, <a href="/search/?searchtype=author&query=Lyakhovsky%2C+V">Vladimir Lyakhovsky</a>, <a href="/search/?searchtype=author&query=Igel%2C+H">Heiner Igel</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.09714v1-abstract-short" style="display: inline;"> The nonlinear mechanical responses of rocks and soils to seismic waves play an important role in earthquake physics, influencing ground motion from source to site. Continuous geophysical monitoring, such as ambient noise interferometry, has revealed co-seismic wave speed reductions extending tens of kilometers from earthquake sources. However, the mechanisms governing these changes remain challeng… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.09714v1-abstract-full').style.display = 'inline'; document.getElementById('2502.09714v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.09714v1-abstract-full" style="display: none;"> The nonlinear mechanical responses of rocks and soils to seismic waves play an important role in earthquake physics, influencing ground motion from source to site. Continuous geophysical monitoring, such as ambient noise interferometry, has revealed co-seismic wave speed reductions extending tens of kilometers from earthquake sources. However, the mechanisms governing these changes remain challenging to model, especially at regional scales. Using a nonlinear damage model constrained by laboratory experiments, we develop and apply an open-source 3D discontinuous Galerkin method to simulate regional co-seismic wave speed changes during the 2015 Mw7.8 Gorkha earthquake. We find pronounced spatial variations of co-seismic wave speed reduction, ranging from <0.01% to >50%, particularly close to the source and within the Kathmandu Basin. The most significant reduction occurs within the sedimentary basin and varies with basin depths, while wave speed reductions correlate with the fault slip distribution near the source. By comparing ground motions from simulations with elastic, viscoelastic, elastoplastic, and nonlinear damage rheologies, we demonstrate that the nonlinear damage model effectively captures low-frequency ground motion amplification due to strain-dependent wave speed reductions in soft sediments. We verify the accuracy of our approach through comparisons with analytical solutions and assess its scalability on high-performance computing systems. The model shows near-linear strong and weak scaling up to 2048 nodes, enabling efficient large-scale simulations. Our findings provide a physics-based framework to quantify nonlinear earthquake effects and emphasize the importance of damage-induced wave speed variations for seismic hazard assessment and ground motion predictions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.09714v1-abstract-full').style.display = 'none'; document.getElementById('2502.09714v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">38 pages, 9 figures, submitted to JGR: Solid Earth</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2502.07887">arXiv:2502.07887</a> <span> [<a href="https://arxiv.org/pdf/2502.07887">pdf</a>, <a href="https://arxiv.org/format/2502.07887">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Searching for Hot Water World Candidates with CHEOPS: Refining the radii and analysing the internal structures and atmospheric lifetimes of TOI-238 b and TOI-1685 b </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Kubyshkina%2C+D">D. Kubyshkina</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Osborn%2C+H+P">H. P. Osborn</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Kitzmann%2C+D">D. Kitzmann</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Mordasini%2C+C">C. Mordasini</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Fridlund%2C+M">M. Fridlund</a>, <a href="/search/?searchtype=author&query=Pezzotti%2C+C">C. Pezzotti</a>, <a href="/search/?searchtype=author&query=Gandolfi%2C+D">D. Gandolfi</a>, <a href="/search/?searchtype=author&query=Ulmer-Moll%2C+S">S. Ulmer-Moll</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C">S. C. Barros</a>, <a href="/search/?searchtype=author&query=Baumjohann%2C+W">W. Baumjohann</a>, <a href="/search/?searchtype=author&query=Benz%2C+W">W. Benz</a>, <a href="/search/?searchtype=author&query=Billot%2C+N">N. Billot</a> , et al. (63 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2502.07887v1-abstract-short" style="display: inline;"> Studying the composition of exoplanets is one of the most promising approaches to observationally constrain planet formation and evolution processes. However, this endeavour is complicated for small exoplanets by the fact that a wide range of compositions is compatible with their bulk properties. To overcome this issue, we identify triangular regions in the mass-radius space where part of this deg… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.07887v1-abstract-full').style.display = 'inline'; document.getElementById('2502.07887v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2502.07887v1-abstract-full" style="display: none;"> Studying the composition of exoplanets is one of the most promising approaches to observationally constrain planet formation and evolution processes. However, this endeavour is complicated for small exoplanets by the fact that a wide range of compositions is compatible with their bulk properties. To overcome this issue, we identify triangular regions in the mass-radius space where part of this degeneracy is lifted for close-in planets, since low-mass H/He envelopes would not be stable due to high-energy stellar irradiation. Planets in these Hot Water World triangles need to contain at least some heavier volatiles and are therefore interesting targets for atmospheric follow-up observations. We perform a demographic study to show that only few well-characterised planets in these regions are currently known and introduce our CHEOPS GTO programme aimed at identifying more of these potential hot water worlds. Here, we present CHEOPS observations for the first two targets of our programme, TOI-238 b and TOI-1685 b. Combined with TESS photometry and published RVs, we use the precise radii and masses of both planets to study their location relative to the corresponding Hot Water World triangles, perform an interior structure analysis and study the lifetimes of H/He and water-dominated atmospheres under these conditions. We find that TOI-238 b lies, at the 1-sigma level, inside the corresponding triangle. While a pure H/He atmosphere would have evaporated after 0.4-1.3 Myr, it is likely that a water-dominated atmosphere would have survived until the current age of the system, which makes TOI-238 b a promising hot water world candidate. Conversely, TOI-1685 b lies below the mass-radius model for a pure silicate planet, meaning that even though a water-dominated atmosphere would be compatible both with our internal structure and evaporation analysis, we cannot rule out the planet to be a bare core. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2502.07887v1-abstract-full').style.display = 'none'; document.getElementById('2502.07887v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">25 pages, 16 figures, accepted for publication in A&A</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.18484">arXiv:2501.18484</a> <span> [<a href="https://arxiv.org/pdf/2501.18484">pdf</a>, <a href="https://arxiv.org/format/2501.18484">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Soft Condensed Matter">cond-mat.soft</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Statistical Mechanics">cond-mat.stat-mech</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Applied Physics">physics.app-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-ph</span> </div> </div> <p class="title is-5 mathjax"> Nonequilibrium friction and free energy estimates for kinetic coarse-graining -- Driven particles in responsive media </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Milster%2C+S">Sebastian Milster</a>, <a href="/search/?searchtype=author&query=Dzubiella%2C+J">Joachim Dzubiella</a>, <a href="/search/?searchtype=author&query=Stock%2C+G">Gerhard Stock</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Steffen Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.18484v1-abstract-short" style="display: inline;"> Predicting the molecular friction and energy landscapes under nonequilibrium conditions is key to coarse-graining the dynamics of selective solute transport through complex, fluctuating and responsive media, e.g., polymeric materials such as hydrogels, cellular membranes or ion channels. The analysis of equilibrium ensembles already allows such a coarse-graining for very mild nonequilibrium condit… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.18484v1-abstract-full').style.display = 'inline'; document.getElementById('2501.18484v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.18484v1-abstract-full" style="display: none;"> Predicting the molecular friction and energy landscapes under nonequilibrium conditions is key to coarse-graining the dynamics of selective solute transport through complex, fluctuating and responsive media, e.g., polymeric materials such as hydrogels, cellular membranes or ion channels. The analysis of equilibrium ensembles already allows such a coarse-graining for very mild nonequilibrium conditions. Yet in the presence of stronger external driving and/or inhomogeneous setups, the transport process is governed apart from a potential of mean force also by a nontrivial position- and velocity-dependent friction. It is therefore important to find suitable and efficient methods to estimate the mean force and the friction landscape, which then can be used in a low-dimensional, coarse-grained Langevin framework to predict the system's transport properties and timescales. In this work, we evaluate different coarse-graining approaches based on constant-velocity constraint simulations for generating such estimates using two model systems, which are a 1D responsive barrier as a minimalistic model and a single tracer driven through a 3D bead-spring polymer membrane as a more sophisticated problem. Finally, we demonstrate that the estimates from 3D constant-velocity simulations yield the correct velocity-dependent friction, which can be directly utilized for coarse-grained (1D) Langevin simulations with constant external driving forces. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.18484v1-abstract-full').style.display = 'none'; document.getElementById('2501.18484v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 30 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Seven Figures. This preprint is the unedited version of a manuscript that has been sent to a scientific publisher for consideration as an article in a peer-reviewed journal. Copyright with the authors and the publisher after publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.16873">arXiv:2501.16873</a> <span> [<a href="https://arxiv.org/pdf/2501.16873">pdf</a>, <a href="https://arxiv.org/format/2501.16873">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202450165">10.1051/0004-6361/202450165 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Wavelength-dependent far-infrared polarization of HL Tau observed with SOFIA/HAWC+ </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Lietzow-Sinjen%2C+M">Moritz Lietzow-Sinjen</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/?searchtype=author&query=Brunngr%C3%A4ber%2C+R">Robert Brunngr盲ber</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.16873v2-abstract-short" style="display: inline;"> We present the first polarimetric observations of a circumstellar disk in the far-infrared wavelength range. We report flux and linear polarization measurements of the young stellar object HL Tau in the bands A (53 $渭$m), C (89 $渭$m), D (155 $渭$m), and E (216 $渭$m) with SOFIA/HAWC+. The orientation of the polarization vectors is strongly wavelength-dependent and can be attributed to different wave… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16873v2-abstract-full').style.display = 'inline'; document.getElementById('2501.16873v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.16873v2-abstract-full" style="display: none;"> We present the first polarimetric observations of a circumstellar disk in the far-infrared wavelength range. We report flux and linear polarization measurements of the young stellar object HL Tau in the bands A (53 $渭$m), C (89 $渭$m), D (155 $渭$m), and E (216 $渭$m) with SOFIA/HAWC+. The orientation of the polarization vectors is strongly wavelength-dependent and can be attributed to different wavelength-dependent polarization mechanisms in the disk and its local environment. In bands A, C, and D, the orientation of the polarization is roughly consistent with a value of 114掳 at the maximum emission. Hereby, the magnetic field direction is close to that of the spin axis of the disk. In contrast, in band E, the orientation is nearly parallel to the minor axis of the projection of the inclined disk. Based on a viscous accretion disk model combined with a surrounding envelope, we performed polarized three-dimensional Monte Carlo radiative transfer simulations. In particular, we considered polarization due to emission and absorption by aligned dust grains, and polarization due to scattering of the thermal reemission (self-scattering). At wavelengths of 53 $渭$m, 89 $渭$m, and 155 $渭$m, we were able to reproduce the observed orientation of the polarization vectors. Here, the origin of polarization is consistent with polarized emission by aligned non-spherical dust grains. In contrast, at a wavelength of 216 $渭$m, the polarization pattern could not be fully matched, however, applying self-scattering and assuming dust grain radii up to 35 $渭$m, we were able to reproduce the flip in the orientation of polarization. We conclude that the polarization is caused by dichroic emission of aligned dust grains in the envelope, while at longer wavelengths, the envelope becomes transparent and the polarization is dominated by self-scattering in the disk. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.16873v2-abstract-full').style.display = 'none'; document.getElementById('2501.16873v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 6 figures, to be published in Astronomy & Astrophysics (A&A), updated URL to IRSA</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 694, A190 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.14858">arXiv:2501.14858</a> <span> [<a href="https://arxiv.org/pdf/2501.14858">pdf</a>, <a href="https://arxiv.org/format/2501.14858">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451780">10.1051/0004-6361/202451780 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Monte Carlo post-processing for radiation hydro simulations of accreting planets in protoplanetary disks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Krieger%2C+A">Anton Krieger</a>, <a href="/search/?searchtype=author&query=Klahr%2C+H">Hubert Klahr</a>, <a href="/search/?searchtype=author&query=Fuksman%2C+J+D+M">Julio David Melon Fuksman</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.14858v1-abstract-short" style="display: inline;"> This paper is part of a series investigating the observational appearance of planets accreting from their nascent protoplanetary disk (PPD). We evaluate the differences between gas temperature distributions determined in our radiation hydrodynamical (RHD) simulations and those recalculated via post-processing with a Monte Carlo (MC) radiative transport (RT) scheme. Our MCRT simulations were perfor… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.14858v1-abstract-full').style.display = 'inline'; document.getElementById('2501.14858v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.14858v1-abstract-full" style="display: none;"> This paper is part of a series investigating the observational appearance of planets accreting from their nascent protoplanetary disk (PPD). We evaluate the differences between gas temperature distributions determined in our radiation hydrodynamical (RHD) simulations and those recalculated via post-processing with a Monte Carlo (MC) radiative transport (RT) scheme. Our MCRT simulations were performed for global PPD models, each composed of a local 3D high-resolution RHD model embedded in an axisymmetric global disk simulation. We report the level of agreement between the two approaches and point out several caveats that prevent a perfect match between the temperature distributions with our respective methods of choice. Overall, the level of agreement is high, with a typical discrepancy between the RHD and MCRT temperatures of the high-resolution region of only about 10 percent. The largest differences were found close to the disk photosphere, at the transition layer between optically dense and thin regions, as well as in the far-out regions of the PPD, occasionally exceeding values of 40 percent. We identify several reasons for these discrepancies, which are mostly related to general features of typical radiative transfer solvers used in hydrodynamical simulations (angle- and frequency-averaging and ignored scattering) and MCRT methods (ignored internal energy advection and compression and expansion work). This provides a clear pathway to reduce systematic temperature inaccuracies in future works. Based on MCRT simulations, we finally determined the expected error in flux estimates, both for the entire PPD and for planets accreting gas from their ambient disk, independently of the amount of gas piling up in the Hill sphere and the used model resolution. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.14858v1-abstract-full').style.display = 'none'; document.getElementById('2501.14858v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 31 pages, 28 figures, 2 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.06836">arXiv:2501.06836</a> <span> [<a href="https://arxiv.org/pdf/2501.06836">pdf</a>, <a href="https://arxiv.org/format/2501.06836">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> </div> <p class="title is-5 mathjax"> SAM-DA: Decoder Adapter for Efficient Medical Domain Adaptation </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Tejero%2C+J+G">Javier Gamazo Tejero</a>, <a href="/search/?searchtype=author&query=Schmid%2C+M">Moritz Schmid</a>, <a href="/search/?searchtype=author&query=Neila%2C+P+M">Pablo M谩rquez Neila</a>, <a href="/search/?searchtype=author&query=Zinkernagel%2C+M+S">Martin S. Zinkernagel</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/?searchtype=author&query=Sznitman%2C+R">Raphael Sznitman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.06836v1-abstract-short" style="display: inline;"> This paper addresses the domain adaptation challenge for semantic segmentation in medical imaging. Despite the impressive performance of recent foundational segmentation models like SAM on natural images, they struggle with medical domain images. Beyond this, recent approaches that perform end-to-end fine-tuning of models are simply not computationally tractable. To address this, we propose a nove… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06836v1-abstract-full').style.display = 'inline'; document.getElementById('2501.06836v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.06836v1-abstract-full" style="display: none;"> This paper addresses the domain adaptation challenge for semantic segmentation in medical imaging. Despite the impressive performance of recent foundational segmentation models like SAM on natural images, they struggle with medical domain images. Beyond this, recent approaches that perform end-to-end fine-tuning of models are simply not computationally tractable. To address this, we propose a novel SAM adapter approach that minimizes the number of trainable parameters while achieving comparable performances to full fine-tuning. The proposed SAM adapter is strategically placed in the mask decoder, offering excellent and broad generalization capabilities and improved segmentation across both fully supervised and test-time domain adaptation tasks. Extensive validation on four datasets showcases the adapter's efficacy, outperforming existing methods while training less than 1% of SAM's total parameters. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.06836v1-abstract-full').style.display = 'none'; document.getElementById('2501.06836v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">WACV25</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2501.05840">arXiv:2501.05840</a> <span> [<a href="https://arxiv.org/pdf/2501.05840">pdf</a>, <a href="https://arxiv.org/format/2501.05840">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Human-Computer Interaction">cs.HC</span> </div> </div> <p class="title is-5 mathjax"> Applying Think-Aloud in ICTD: A Case Study of a Chatbot Use by Teachers in Rural C么te d'Ivoire </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Cannanure%2C+V+K">Vikram Kamath Cannanure</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sharon Wolf</a>, <a href="/search/?searchtype=author&query=Jasi%C5%84ska%2C+K">Kaja Jasi艅ska</a>, <a href="/search/?searchtype=author&query=Brown%2C+T+X">Timothy X Brown</a>, <a href="/search/?searchtype=author&query=Ogan%2C+A">Amy Ogan</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2501.05840v1-abstract-short" style="display: inline;"> Think-alouds are a common HCI usability method where participants verbalize their thoughts while using interfaces. However, their utility in cross-cultural settings, particularly in the Global South, is unclear, where cultural differences impact user interactions. This paper investigates the usability challenges teachers in rural C么te d'Ivoire faced when using a chatbot designed to support an educ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05840v1-abstract-full').style.display = 'inline'; document.getElementById('2501.05840v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2501.05840v1-abstract-full" style="display: none;"> Think-alouds are a common HCI usability method where participants verbalize their thoughts while using interfaces. However, their utility in cross-cultural settings, particularly in the Global South, is unclear, where cultural differences impact user interactions. This paper investigates the usability challenges teachers in rural C么te d'Ivoire faced when using a chatbot designed to support an educational program. We conducted think-aloud sessions with 20 teachers two weeks after a chatbot deployment, analyzing their navigation, errors, and time spent on tasks. We discuss our approach and findings that helped us identify usability issues and challenging features for improving the chatbot designs. Our note summarizes our reflections on using think-aloud and contributes to discussions on its culturally sensitive adaptation in the Global South. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2501.05840v1-abstract-full').style.display = 'none'; document.getElementById('2501.05840v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 10 January, 2025; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2025. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">ICTD 24, Notes track. International Conference on Information & Communication Technologies and Development 2024</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Report number:</span> ICTD24Note02 <span class="has-text-black-bis has-text-weight-semibold">ACM Class:</span> H.5.2; K.3.1; K.4.2 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2412.08557">arXiv:2412.08557</a> <span> [<a href="https://arxiv.org/pdf/2412.08557">pdf</a>, <a href="https://arxiv.org/format/2412.08557">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202452151">10.1051/0004-6361/202452151 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> CHEOPS observations confirm nodal precession in the WASP-33 system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Smith%2C+A+M+S">A. M. S. Smith</a>, <a href="/search/?searchtype=author&query=Csizmadia%2C+S">Sz. Csizmadia</a>, <a href="/search/?searchtype=author&query=Van+Grootel%2C+V">V. Van Grootel</a>, <a href="/search/?searchtype=author&query=Lendl%2C+M">M. Lendl</a>, <a href="/search/?searchtype=author&query=Persson%2C+C+M">C. M. Persson</a>, <a href="/search/?searchtype=author&query=Olofsson%2C+G">G. Olofsson</a>, <a href="/search/?searchtype=author&query=Ehrenreich%2C+D">D. Ehrenreich</a>, <a href="/search/?searchtype=author&query=G%C3%BCnther%2C+M+N">M. N. G眉nther</a>, <a href="/search/?searchtype=author&query=Heitzmann%2C+A">A. Heitzmann</a>, <a href="/search/?searchtype=author&query=Barros%2C+S+C+C">S. C. C. Barros</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Brandeker%2C+A">A. Brandeker</a>, <a href="/search/?searchtype=author&query=Cabrera%2C+J">J. Cabrera</a>, <a href="/search/?searchtype=author&query=Demangeon%2C+O+D+S">O. D. S. Demangeon</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Harre%2C+J+-">J. -V. Harre</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Hoyer%2C+S">S. Hoyer</a>, <a href="/search/?searchtype=author&query=Kalman%2C+S">Sz. Kalman</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Szab%C3%B3%2C+G+M">Gy. M. Szab贸</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a> , et al. (64 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2412.08557v1-abstract-short" style="display: inline;"> Aims: We aim to observe the transits and occultations of WASP-33b, which orbits a rapidly-rotating $未$ Scuti pulsator, with the goal of measuring the orbital obliquity via the gravity-darkening effect, and constraining the geometric albedo via the occultation depth. Methods: We observed four transits and four occultations with CHEOPS, and employ a variety of techniques to remove the effects of the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.08557v1-abstract-full').style.display = 'inline'; document.getElementById('2412.08557v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2412.08557v1-abstract-full" style="display: none;"> Aims: We aim to observe the transits and occultations of WASP-33b, which orbits a rapidly-rotating $未$ Scuti pulsator, with the goal of measuring the orbital obliquity via the gravity-darkening effect, and constraining the geometric albedo via the occultation depth. Methods: We observed four transits and four occultations with CHEOPS, and employ a variety of techniques to remove the effects of the stellar pulsations from the light curves, as well as the usual CHEOPS systematic effects. We also performed a comprehensive analysis of low-resolution spectral and Gaia data to re-determine the stellar properties of WASP-33. Results: We measure an orbital obliquity 111.3 +0.2 -0.7 degrees, which is consistent with previous measurements made via Doppler tomography. We also measure the planetary impact parameter, and confirm that this parameter is undergoing rapid secular evolution as a result of nodal precession of the planetary orbit. This precession allows us to determine the second-order fluid Love number of the star, which we find agrees well with the predictions of theoretical stellar models. We are unable to robustly measure a unique value of the occultation depth, and emphasise the need for long-baseline observations to better measure the pulsation periods. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2412.08557v1-abstract-full').style.display = 'none'; document.getElementById('2412.08557v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 December, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 12 figures. Accepted for publication in Astronomy & Astrophysics</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 2025 693 A128 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2411.00277">arXiv:2411.00277</a> <span> [<a href="https://arxiv.org/pdf/2411.00277">pdf</a>, <a href="https://arxiv.org/format/2411.00277">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202451981">10.1051/0004-6361/202451981 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Dust mass in protoplanetary disks with porous dust opacities </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Liu%2C+Y">Yao Liu</a>, <a href="/search/?searchtype=author&query=Roussel%2C+H">H茅l猫ne Roussel</a>, <a href="/search/?searchtype=author&query=Linz%2C+H">Hendrik Linz</a>, <a href="/search/?searchtype=author&query=Fang%2C+M">Min Fang</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/?searchtype=author&query=Kirchschlager%2C+F">Florian Kirchschlager</a>, <a href="/search/?searchtype=author&query=Henning%2C+T">Thomas Henning</a>, <a href="/search/?searchtype=author&query=Yang%2C+H">Haifeng Yang</a>, <a href="/search/?searchtype=author&query=Du%2C+F">Fujun Du</a>, <a href="/search/?searchtype=author&query=Flock%2C+M">Mario Flock</a>, <a href="/search/?searchtype=author&query=Wang%2C+H">Hongchi Wang</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2411.00277v1-abstract-short" style="display: inline;"> ALMA surveys have suggested that protoplanetary disks are not massive enough to form the known exoplanet population, under the assumption that the millimeter continuum emission is optically thin. In this work, we investigate how the mass determination is influenced when the porosity of dust grains is considered in radiative transfer models. The results show that disks with porous dust opacities yi… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.00277v1-abstract-full').style.display = 'inline'; document.getElementById('2411.00277v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2411.00277v1-abstract-full" style="display: none;"> ALMA surveys have suggested that protoplanetary disks are not massive enough to form the known exoplanet population, under the assumption that the millimeter continuum emission is optically thin. In this work, we investigate how the mass determination is influenced when the porosity of dust grains is considered in radiative transfer models. The results show that disks with porous dust opacities yield similar dust temperature, but systematically lower millimeter fluxes compared to disks incorporating compact dust grains. Moreover, we recalibrate the relation between dust temperature and stellar luminosity for a wide range of stellar parameters, and calculate the dust masses of a large sample of disks using the traditionally analytic approach. The median dust mass from our calculation is about 6 times higher than the literature result, and this is mostly driven by the different opacities of porous and compact grains. A comparison of the cumulative distribution function between disk dust masses and exoplanet masses show that the median exoplanet mass is about 2 times lower than the median dust mass, if grains are porous, and there are no exoplanetary systems with masses higher than the most massive disks. Our analysis suggests that adopting porous dust opacities may alleviate the mass budget problem for planet formation. As an example illustrating the combined effects of optical depth and porous dust opacities on the mass estimation, we conduct new IRAM/NIKA-2 observations toward the IRAS 04370+2559 disk and perform a detailed radiative transfer modeling of the spectral energy distribution. The best-fit dust mass is roughly 100 times higher than the value from the traditionally analytic calculation. Future spatially resolved observations at various wavelengths are required to better constrain the dust mass. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2411.00277v1-abstract-full').style.display = 'none'; document.getElementById('2411.00277v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">11 pages, 7 figures, Accepted for publication in A&A</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 692, A148 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.21251">arXiv:2410.21251</a> <span> [<a href="https://arxiv.org/pdf/2410.21251">pdf</a>, <a href="https://arxiv.org/format/2410.21251">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Quantum Physics">quant-ph</span> </div> </div> <p class="title is-5 mathjax"> Shot-noise reduction for lattice Hamiltonians </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Eckstein%2C+T">Timo Eckstein</a>, <a href="/search/?searchtype=author&query=Mansuroglu%2C+R">Refik Mansuroglu</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Stefan Wolf</a>, <a href="/search/?searchtype=author&query=N%C3%BCtzel%2C+L">Ludwig N眉tzel</a>, <a href="/search/?searchtype=author&query=Tasler%2C+S">Stephan Tasler</a>, <a href="/search/?searchtype=author&query=Kliesch%2C+M">Martin Kliesch</a>, <a href="/search/?searchtype=author&query=Hartmann%2C+M+J">Michael J. Hartmann</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.21251v2-abstract-short" style="display: inline;"> Efficiently estimating energy expectation values of lattice Hamiltonians on quantum computers is a serious challenge, where established techniques can require excessive sample numbers. Here we introduce geometric partitioning as a scalable alternative. It splits the Hamiltonian into subsystems that extend over multiple lattice sites, for which transformations between their local eigenbasis and the… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.21251v2-abstract-full').style.display = 'inline'; document.getElementById('2410.21251v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.21251v2-abstract-full" style="display: none;"> Efficiently estimating energy expectation values of lattice Hamiltonians on quantum computers is a serious challenge, where established techniques can require excessive sample numbers. Here we introduce geometric partitioning as a scalable alternative. It splits the Hamiltonian into subsystems that extend over multiple lattice sites, for which transformations between their local eigenbasis and the computational basis can be efficiently found. This allows us to reduce the number of measurements as we sample from a more concentrated distribution without diagonalizing the problem. For systems in an energy eigenstate, we prove a lower bound on the sampling number improvement over the "naive" mutually commuting local operator grouping, which grows with the considered subsystem size, consistently showing an advantage for our geometric partitioning strategy. Notably, our lower bounds do not decrease but increase for more correlated states (Theorem 1). For states that are weakly isotropically perturbed around an eigenstate, we show how the sampling number improvement translates to imperfect eigenstate improvements, namely measuring close to the true eigenbasis already for smaller perturbations (Theorem 2). We illustrate our findings on multiple two-dimensional lattice models incl. the transverse field XY- and Ising model as well as the Fermi Hubbard model. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.21251v2-abstract-full').style.display = 'none'; document.getElementById('2410.21251v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 November, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 28 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 + 12 pages, 5 + 0 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.18735">arXiv:2410.18735</a> <span> [<a href="https://arxiv.org/pdf/2410.18735">pdf</a>, <a href="https://arxiv.org/format/2410.18735">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Quantum Physics">quant-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="General Relativity and Quantum Cosmology">gr-qc</span> </div> </div> <p class="title is-5 mathjax"> Flow of dynamical causal structures with an application to correlations </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Baumeler%2C+%C3%84">脛min Baumeler</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Stefan Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.18735v1-abstract-short" style="display: inline;"> Causal models capture cause-effect relations both qualitatively - via the graphical causal structure - and quantitatively - via the model parameters. They offer a powerful framework for analyzing and constructing processes. Here, we introduce a tool - the flow of causal structures - to visualize and explore the dynamical aspect of classical-deterministic processes, arguably like those present in g… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.18735v1-abstract-full').style.display = 'inline'; document.getElementById('2410.18735v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.18735v1-abstract-full" style="display: none;"> Causal models capture cause-effect relations both qualitatively - via the graphical causal structure - and quantitatively - via the model parameters. They offer a powerful framework for analyzing and constructing processes. Here, we introduce a tool - the flow of causal structures - to visualize and explore the dynamical aspect of classical-deterministic processes, arguably like those present in general relativity. The flow describes all possible ways in which the causal structure of a process can evolve. We also present an algorithm to construct its supergraph - the superflow - from the causal structure only. Consequently, the superflow of a given process may describe additional unrealizable evolutions of its causal structure. As an application, we show that if all leafs of a flow are trivial, then the corresponding process produces causal correlations only, i.e., correlations where past data influences future events only. This strengthens the result that processes, where the cycles in their causal structure are chordless, establish causal correlations only. We also discuss the main difficulties for the quantum generalization. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.18735v1-abstract-full').style.display = 'none'; document.getElementById('2410.18735v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 24 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">5 pages, 3 figures, 2 algorithms</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2410.18169">arXiv:2410.18169</a> <span> [<a href="https://arxiv.org/pdf/2410.18169">pdf</a>, <a href="https://arxiv.org/format/2410.18169">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Architecture of TOI-561 planetary system </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Piotto%2C+G">G. Piotto</a>, <a href="/search/?searchtype=author&query=Zingales%2C+T">T. Zingales</a>, <a href="/search/?searchtype=author&query=Borsato%2C+L">L. Borsato</a>, <a href="/search/?searchtype=author&query=Egger%2C+J+A">J. A. Egger</a>, <a href="/search/?searchtype=author&query=Correia%2C+A+C+M">A. C. M. Correia</a>, <a href="/search/?searchtype=author&query=Simon%2C+A+E">A. E. Simon</a>, <a href="/search/?searchtype=author&query=Flor%C3%A9n%2C+H+G">H. G. Flor茅n</a>, <a href="/search/?searchtype=author&query=Sousa%2C+S+G">S. G. Sousa</a>, <a href="/search/?searchtype=author&query=Maxted%2C+P+F+L">P. F. L. Maxted</a>, <a href="/search/?searchtype=author&query=Nardiello%2C+D">D. Nardiello</a>, <a href="/search/?searchtype=author&query=Malavolta%2C+L">L. Malavolta</a>, <a href="/search/?searchtype=author&query=Wilson%2C+T+G">T. G. Wilson</a>, <a href="/search/?searchtype=author&query=Alibert%2C+Y">Y. Alibert</a>, <a href="/search/?searchtype=author&query=Adibekyan%2C+V">V. Adibekyan</a>, <a href="/search/?searchtype=author&query=Bonfanti%2C+A">A. Bonfanti</a>, <a href="/search/?searchtype=author&query=Luque%2C+R">R. Luque</a>, <a href="/search/?searchtype=author&query=Santos%2C+N+C">N. C. Santos</a>, <a href="/search/?searchtype=author&query=Hooton%2C+M+J">M. J. Hooton</a>, <a href="/search/?searchtype=author&query=Fossati%2C+L">L. Fossati</a>, <a href="/search/?searchtype=author&query=Smith%2C+A+M+S">A. M. S. Smith</a>, <a href="/search/?searchtype=author&query=Salmon%2C+S">S. Salmon</a>, <a href="/search/?searchtype=author&query=Lacedelli%2C+G">G. Lacedelli</a>, <a href="/search/?searchtype=author&query=Alonso%2C+R">R. Alonso</a>, <a href="/search/?searchtype=author&query=B%C3%A1rczy%2C+T">T. B谩rczy</a>, <a href="/search/?searchtype=author&query=Navascues%2C+D+B">D. Barrado Navascues</a> , et al. (68 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2410.18169v3-abstract-short" style="display: inline;"> We present new observations from CHEOPS and TESS to clarify the architecture of the planetary system hosted by the old Galactic thick disk star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 days (TOI-561 b), 10.8 days (TOI-561 c), 25.7… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.18169v3-abstract-full').style.display = 'inline'; document.getElementById('2410.18169v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2410.18169v3-abstract-full" style="display: none;"> We present new observations from CHEOPS and TESS to clarify the architecture of the planetary system hosted by the old Galactic thick disk star TOI-561. Our global analysis, which also includes previously published photometric and radial velocity data, incontrovertibly proves that TOI-561 is hosting at least four transiting planets with periods of 0.44 days (TOI-561 b), 10.8 days (TOI-561 c), 25.7 days (TOI-561 d), and 77.1 days (TOI-561 e) and a fifth non-transiting candidate, TOI-561f with a period of 433 days. The precise characterisation of TOI-561's orbital architecture is interesting since old and metal-poor thick disk stars are less likely to host ultra-short period Super-Earths like TOI-561 b. The new period of planet -e is consistent with the value obtained using radial velocity alone and is now known to be $77.14399\pm0.00025$ days, thanks to the new CHEOPS and TESS transits. The new data allowed us to improve its radius ($R_p = 2.517 \pm 0.045 R_{\oplus}$ from 5$\%$ to 2$\%$ precision) and mass ($M_p = 12.4 \pm 1.4 M_{\oplus}$) estimates, implying a density of $蟻_p = 0.778 \pm 0.097 蟻_{\oplus}$. Thanks to recent TESS observations and the focused CHEOPS visit of the transit of TOI-561 e, a good candidate for exomoon searches, the planet's period is finally constrained, allowing us to predict transit times through 2030 with 20-minute accuracy. We present an updated version of the internal structure of the four transiting planets. We finally performed a detailed stability analysis, which confirmed the long-term stability of the outer planet TOI-561 f. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2410.18169v3-abstract-full').style.display = 'none'; document.getElementById('2410.18169v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 31 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 23 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 10 Figures. Accepted on MNRAS. Updated the author list</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.20107">arXiv:2409.20107</a> <span> [<a href="https://arxiv.org/pdf/2409.20107">pdf</a>, <a href="https://arxiv.org/ps/2409.20107">ps</a>, <a href="https://arxiv.org/format/2409.20107">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Optimization and Control">math.OC</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Probability">math.PR</span> </div> </div> <p class="title is-5 mathjax"> Irreducibility of nonsmooth state-space models with an application to CMA-ES </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gissler%2C+A">Armand Gissler</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Shan-Conrad Wolf</a>, <a href="/search/?searchtype=author&query=Auger%2C+A">Anne Auger</a>, <a href="/search/?searchtype=author&query=Hansen%2C+N">Nikolaus Hansen</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.20107v2-abstract-short" style="display: inline;"> We analyze a stochastic process resulting from the normalization of states in the zeroth-order optimization method CMA-ES. On a specific class of minimization problems where the objective function is scaling-invariant, this process defines a time-homogeneous Markov chain whose convergence at a geometric rate can imply the linear convergence of CMA-ES. However, the analysis of the intricate updates… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.20107v2-abstract-full').style.display = 'inline'; document.getElementById('2409.20107v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.20107v2-abstract-full" style="display: none;"> We analyze a stochastic process resulting from the normalization of states in the zeroth-order optimization method CMA-ES. On a specific class of minimization problems where the objective function is scaling-invariant, this process defines a time-homogeneous Markov chain whose convergence at a geometric rate can imply the linear convergence of CMA-ES. However, the analysis of the intricate updates for this process constitute a great mathematical challenge. We establish that this Markov chain is an irreducible and aperiodic T-chain. These contributions represent a first major step for the convergence analysis towards a stationary distribution. We rely for this analysis on conditions for the irreducibility of nonsmooth state-space models on manifolds. To obtain our results, we extend these conditions to address the irreducibility in different hyperparameter settings that define different Markov chains, and to include nonsmooth state spaces. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.20107v2-abstract-full').style.display = 'none'; document.getElementById('2409.20107v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 1 October, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2409.19147">arXiv:2409.19147</a> <span> [<a href="https://arxiv.org/pdf/2409.19147">pdf</a>, <a href="https://arxiv.org/format/2409.19147">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Geophysics">physics.geo-ph</span> </div> </div> <p class="title is-5 mathjax"> Training the Next Generation of Seismologists: Delivering Research-Grade Software Education for Cloud and HPC Computing through Diverse Training Modalities </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Denolle%2C+M">M. Denolle</a>, <a href="/search/?searchtype=author&query=Tape%2C+C">C. Tape</a>, <a href="/search/?searchtype=author&query=Bozda%C4%9F%2C+E">E. Bozda臒</a>, <a href="/search/?searchtype=author&query=Wang%2C+Y">Y. Wang</a>, <a href="/search/?searchtype=author&query=Waldhauser%2C+F">F. Waldhauser</a>, <a href="/search/?searchtype=author&query=Gabriel%2C+A+A">A. A. Gabriel</a>, <a href="/search/?searchtype=author&query=Braunmiller%2C+J">J. Braunmiller</a>, <a href="/search/?searchtype=author&query=Chow%2C+B">B. Chow</a>, <a href="/search/?searchtype=author&query=Ding%2C+L">L. Ding</a>, <a href="/search/?searchtype=author&query=Feng%2C+K+F">K. F. Feng</a>, <a href="/search/?searchtype=author&query=Ghosh%2C+A">A. Ghosh</a>, <a href="/search/?searchtype=author&query=Groebner%2C+N">N. Groebner</a>, <a href="/search/?searchtype=author&query=Gupta%2C+A">A. Gupta</a>, <a href="/search/?searchtype=author&query=Krauss%2C+Z">Z. Krauss</a>, <a href="/search/?searchtype=author&query=McPherson%2C+A">A. McPherson</a>, <a href="/search/?searchtype=author&query=Nagaso%2C+M">M. Nagaso</a>, <a href="/search/?searchtype=author&query=Niu%2C+Z">Z. Niu</a>, <a href="/search/?searchtype=author&query=Ni%2C+Y">Y. Ni</a>, <a href="/search/?searchtype=author&query=Orsvuran%2C+R+%5C">R. \" Orsvuran</a>, <a href="/search/?searchtype=author&query=Pavlis%2C+G">G. Pavlis</a>, <a href="/search/?searchtype=author&query=Rodriguez-Cardozo%2C+F">F. Rodriguez-Cardozo</a>, <a href="/search/?searchtype=author&query=Sawi%2C+T">T. Sawi</a>, <a href="/search/?searchtype=author&query=Schliwa%2C+N">N. Schliwa</a>, <a href="/search/?searchtype=author&query=Schneller%2C+D">D. Schneller</a>, <a href="/search/?searchtype=author&query=Shi%2C+Q">Q. Shi</a> , et al. (6 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2409.19147v1-abstract-short" style="display: inline;"> With the rise of data volume and computing power, seismological research requires more advanced skills in data processing, numerical methods, and parallel computing. We present the experience of conducting training workshops over various forms of delivery to support the adoption of large-scale High-Performance Computing and Cloud computing to advance seismological research. The seismological foci… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19147v1-abstract-full').style.display = 'inline'; document.getElementById('2409.19147v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2409.19147v1-abstract-full" style="display: none;"> With the rise of data volume and computing power, seismological research requires more advanced skills in data processing, numerical methods, and parallel computing. We present the experience of conducting training workshops over various forms of delivery to support the adoption of large-scale High-Performance Computing and Cloud computing to advance seismological research. The seismological foci were on earthquake source parameter estimation in catalogs, forward and adjoint wavefield simulations in 2 and 3 dimensions at local, regional, and global scales, earthquake dynamics, ambient noise seismology, and machine learning. This contribution describes the series of workshops, the learning outcomes of the participants, and lessons learned by the instructors. Our curriculum was grounded on open and reproducible science, large-scale scientific computing and data mining, and computing infrastructure (access and usage) for HPC and the cloud. We also describe the types of teaching materials that have proven beneficial to the instruction and the sustainability of the program. We propose guidelines to deliver future workshops on these topics. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2409.19147v1-abstract-full').style.display = 'none'; document.getElementById('2409.19147v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 September, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2408.10801">arXiv:2408.10801</a> <span> [<a href="https://arxiv.org/pdf/2408.10801">pdf</a>, <a href="https://arxiv.org/format/2408.10801">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Quantum Physics">quant-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1088/2058-9565/ad9ed3">10.1088/2058-9565/ad9ed3 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Solving an Industrially Relevant Quantum Chemistry Problem on Quantum Hardware </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=N%C3%BCtzel%2C+L">Ludwig N眉tzel</a>, <a href="/search/?searchtype=author&query=Gresch%2C+A">Alexander Gresch</a>, <a href="/search/?searchtype=author&query=Hehn%2C+L">Lukas Hehn</a>, <a href="/search/?searchtype=author&query=Marti%2C+L">Lucas Marti</a>, <a href="/search/?searchtype=author&query=Freund%2C+R">Robert Freund</a>, <a href="/search/?searchtype=author&query=Steiner%2C+A">Alex Steiner</a>, <a href="/search/?searchtype=author&query=Marciniak%2C+C+D">Christian D. Marciniak</a>, <a href="/search/?searchtype=author&query=Eckstein%2C+T">Timo Eckstein</a>, <a href="/search/?searchtype=author&query=Stockinger%2C+N">Nina Stockinger</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Stefan Wolf</a>, <a href="/search/?searchtype=author&query=Monz%2C+T">Thomas Monz</a>, <a href="/search/?searchtype=author&query=K%C3%BChn%2C+M">Michael K眉hn</a>, <a href="/search/?searchtype=author&query=Hartmann%2C+M+J">Michael J. Hartmann</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2408.10801v1-abstract-short" style="display: inline;"> Quantum chemical calculations are among the most promising applications for quantum computing. Implementations of dedicated quantum algorithms on available quantum hardware were so far, however, mostly limited to comparatively simple systems without strong correlations. As such, they can also be addressed by classically efficient single-reference methods. In this work, we calculate the lowest ener… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10801v1-abstract-full').style.display = 'inline'; document.getElementById('2408.10801v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2408.10801v1-abstract-full" style="display: none;"> Quantum chemical calculations are among the most promising applications for quantum computing. Implementations of dedicated quantum algorithms on available quantum hardware were so far, however, mostly limited to comparatively simple systems without strong correlations. As such, they can also be addressed by classically efficient single-reference methods. In this work, we calculate the lowest energy eigenvalue of active space Hamiltonians of industrially relevant and strongly correlated metal chelates on trapped ion quantum hardware, and integrate the results into a typical industrial quantum chemical workflow to arrive at chemically meaningful properties. We are able to achieve chemical accuracy by training a variational quantum algorithm on quantum hardware, followed by a classical diagonalization in the subspace of states measured as outputs of the quantum circuit. This approach is particularly measurement-efficient, requiring 600 single-shot measurements per cost function evaluation on a ten qubit system, and allows for efficient post-processing to handle erroneous runs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2408.10801v1-abstract-full').style.display = 'none'; document.getElementById('2408.10801v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 August, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 5 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Quantum Science and Technology 10.1 (2025): 015066 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.20823">arXiv:2407.20823</a> <span> [<a href="https://arxiv.org/pdf/2407.20823">pdf</a>, <a href="https://arxiv.org/format/2407.20823">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Quantum Physics">quant-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.22331/q-2025-02-20-1641">10.22331/q-2025-02-20-1641 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> On multivariate polynomials achievable with quantum signal processing </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Laneve%2C+L">Lorenzo Laneve</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Stefan Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.20823v2-abstract-short" style="display: inline;"> Quantum signal processing (QSP) is a framework which was proven to unify and simplify a large number of known quantum algorithms, as well as discovering new ones. QSP allows one to transform a signal embedded in a given unitary using polynomials. Characterizing which polynomials can be achieved with QSP protocols is an important part of the power of this technique, and while such a characterizatio… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20823v2-abstract-full').style.display = 'inline'; document.getElementById('2407.20823v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.20823v2-abstract-full" style="display: none;"> Quantum signal processing (QSP) is a framework which was proven to unify and simplify a large number of known quantum algorithms, as well as discovering new ones. QSP allows one to transform a signal embedded in a given unitary using polynomials. Characterizing which polynomials can be achieved with QSP protocols is an important part of the power of this technique, and while such a characterization is well-understood in the case of univariate signals, it is unclear which multivariate polynomials can be constructed when the signal is a vector, rather than a scalar. This work uses a slightly different formalism than what is found in the literature, and uses it to find simpler necessary conditions for decomposability, as well as a sufficient condition -- the first, to the best of our knowledge, proven for a (generally inhomogeneous) multivariate polynomial in the context of quantum signal processing. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.20823v2-abstract-full').style.display = 'none'; document.getElementById('2407.20823v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 14 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 30 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 2 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Quantum 9, 1641 (2025) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2407.19920">arXiv:2407.19920</a> <span> [<a href="https://arxiv.org/pdf/2407.19920">pdf</a>, <a href="https://arxiv.org/format/2407.19920">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Algebraic Geometry">math.AG</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Category Theory">math.CT</span> </div> </div> <p class="title is-5 mathjax"> Reconstruction of schemes from their 茅tale topoi </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Carlson%2C+M">Magnus Carlson</a>, <a href="/search/?searchtype=author&query=Haine%2C+P+J">Peter J. Haine</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2407.19920v1-abstract-short" style="display: inline;"> Let $k$ be a field that is finitely generated over its prime field. In Grothendieck's anabelian letter to Faltings, he conjectured that sending a $k$-scheme to its 茅tale topos defines a fully faithful functor from the localization of the category of finite type $k$-schemes at the universal homeomorphisms to a category of topoi. We prove Grothendieck's conjecture for infinite fields of arbitrary ch… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.19920v1-abstract-full').style.display = 'inline'; document.getElementById('2407.19920v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2407.19920v1-abstract-full" style="display: none;"> Let $k$ be a field that is finitely generated over its prime field. In Grothendieck's anabelian letter to Faltings, he conjectured that sending a $k$-scheme to its 茅tale topos defines a fully faithful functor from the localization of the category of finite type $k$-schemes at the universal homeomorphisms to a category of topoi. We prove Grothendieck's conjecture for infinite fields of arbitrary characteristic. In characteristic $0$, this shows that seminormal finite type $k$-schemes can be reconstructed from their 茅tale topoi, generalizing work of Voevodsky. In positive characteristic, this shows that perfections of finite type $k$-schemes can be reconstructed from their 茅tale topoi. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2407.19920v1-abstract-full').style.display = 'none'; document.getElementById('2407.19920v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> July 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Comments very welcome. 39 pages</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2406.14441">arXiv:2406.14441</a> <span> [<a href="https://arxiv.org/pdf/2406.14441">pdf</a>, <a href="https://arxiv.org/format/2406.14441">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Multiagent Systems">cs.MA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Distributed, Parallel, and Cluster Computing">cs.DC</span> </div> </div> <p class="title is-5 mathjax"> Vahana.jl -- A framework (not only) for large-scale agent-based models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=F%C3%BCrst%2C+S">Steffen F眉rst</a>, <a href="/search/?searchtype=author&query=Conrad%2C+T">Tim Conrad</a>, <a href="/search/?searchtype=author&query=Jaeger%2C+C">Carlo Jaeger</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sarah Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2406.14441v1-abstract-short" style="display: inline;"> Agent-based models (ABMs) offer a powerful framework for understanding complex systems. However, their computational demands often become a significant barrier as the number of agents and complexity of the simulation increase. Traditional ABM platforms often struggle to fully exploit modern computing resources, hindering the development of large-scale simulations. This paper presents Vahana.jl, a… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.14441v1-abstract-full').style.display = 'inline'; document.getElementById('2406.14441v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2406.14441v1-abstract-full" style="display: none;"> Agent-based models (ABMs) offer a powerful framework for understanding complex systems. However, their computational demands often become a significant barrier as the number of agents and complexity of the simulation increase. Traditional ABM platforms often struggle to fully exploit modern computing resources, hindering the development of large-scale simulations. This paper presents Vahana.jl, a high performance computing open source framework that aims to address these limitations. Building on the formalism of synchronous graph dynamical systems, Vahana.jl is especially well suited for models with a focus on (social) networks. The framework seamlessly supports distribution across multiple compute nodes, enabling simulations that would otherwise be beyond the capabilities of a single machine. Implemented in Julia, Vahana.jl leverages the interactive Read-Eval-Print Loop (REPL) environment, facilitating rapid model development and experimentation. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2406.14441v1-abstract-full').style.display = 'none'; document.getElementById('2406.14441v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 20 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> June 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">MSC Class:</span> 37E25 <span class="has-text-black-bis has-text-weight-semibold">ACM Class:</span> D.1.3; I.6.5; J.4 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.17698">arXiv:2405.17698</a> <span> [<a href="https://arxiv.org/pdf/2405.17698">pdf</a>, <a href="https://arxiv.org/format/2405.17698">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> </div> <p class="title is-5 mathjax"> BaboonLand Dataset: Tracking Primates in the Wild and Automating Behaviour Recognition from Drone Videos </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Duporge%2C+I">Isla Duporge</a>, <a href="/search/?searchtype=author&query=Kholiavchenko%2C+M">Maksim Kholiavchenko</a>, <a href="/search/?searchtype=author&query=Harel%2C+R">Roi Harel</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Scott Wolf</a>, <a href="/search/?searchtype=author&query=Rubenstein%2C+D">Dan Rubenstein</a>, <a href="/search/?searchtype=author&query=Crofoot%2C+M">Meg Crofoot</a>, <a href="/search/?searchtype=author&query=Berger-Wolf%2C+T">Tanya Berger-Wolf</a>, <a href="/search/?searchtype=author&query=Lee%2C+S">Stephen Lee</a>, <a href="/search/?searchtype=author&query=Barreau%2C+J">Julie Barreau</a>, <a href="/search/?searchtype=author&query=Kline%2C+J">Jenna Kline</a>, <a href="/search/?searchtype=author&query=Ramirez%2C+M">Michelle Ramirez</a>, <a href="/search/?searchtype=author&query=Stewart%2C+C">Charles Stewart</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.17698v3-abstract-short" style="display: inline;"> Using drones to track multiple individuals simultaneously in their natural environment is a powerful approach for better understanding group primate behavior. Previous studies have demonstrated that it is possible to automate the classification of primate behavior from video data, but these studies have been carried out in captivity or from ground-based cameras. To understand group behavior and th… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17698v3-abstract-full').style.display = 'inline'; document.getElementById('2405.17698v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.17698v3-abstract-full" style="display: none;"> Using drones to track multiple individuals simultaneously in their natural environment is a powerful approach for better understanding group primate behavior. Previous studies have demonstrated that it is possible to automate the classification of primate behavior from video data, but these studies have been carried out in captivity or from ground-based cameras. To understand group behavior and the self-organization of a collective, the whole troop needs to be seen at a scale where behavior can be seen in relation to the natural environment in which ecological decisions are made. This study presents a novel dataset from drone videos for baboon detection, tracking, and behavior recognition. The baboon detection dataset was created by manually annotating all baboons in drone videos with bounding boxes. A tiling method was subsequently applied to create a pyramid of images at various scales from the original 5.3K resolution images, resulting in approximately 30K images used for baboon detection. The tracking dataset is derived from the detection dataset, where all bounding boxes are assigned the same ID throughout the video. This process resulted in half an hour of very dense tracking data. The behavior recognition dataset was generated by converting tracks into mini-scenes, a video subregion centered on each animal; each mini-scene was manually annotated with 12 distinct behavior types, resulting in over 20 hours of data. Benchmark results show mean average precision (mAP) of 92.62\% for the YOLOv8-X detection model, multiple object tracking precision (MOTA) of 63.81\% for the BotSort tracking algorithm, and micro top-1 accuracy of 63.97\% for the X3D behavior recognition model. Using deep learning to classify wildlife behavior from drone footage facilitates non-invasive insight into the collective behavior of an entire group. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.17698v3-abstract-full').style.display = 'none'; document.getElementById('2405.17698v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 27 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Dataset will be published shortly</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.14788">arXiv:2405.14788</a> <span> [<a href="https://arxiv.org/pdf/2405.14788">pdf</a>, <a href="https://arxiv.org/format/2405.14788">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> </div> <p class="title is-5 mathjax"> Masked Image Modelling for retinal OCT understanding </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Pissas%2C+T">Theodoros Pissas</a>, <a href="/search/?searchtype=author&query=M%C3%A1rquez-Neila%2C+P">Pablo M谩rquez-Neila</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/?searchtype=author&query=Zinkernagel%2C+M">Martin Zinkernagel</a>, <a href="/search/?searchtype=author&query=Sznitman%2C+R">Raphael Sznitman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.14788v1-abstract-short" style="display: inline;"> This work explores the effectiveness of masked image modelling for learning representations of retinal OCT images. To this end, we leverage Masked Autoencoders (MAE), a simple and scalable method for self-supervised learning, to obtain a powerful and general representation for OCT images by training on 700K OCT images from 41K patients collected under real world clinical settings. We also provide… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14788v1-abstract-full').style.display = 'inline'; document.getElementById('2405.14788v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.14788v1-abstract-full" style="display: none;"> This work explores the effectiveness of masked image modelling for learning representations of retinal OCT images. To this end, we leverage Masked Autoencoders (MAE), a simple and scalable method for self-supervised learning, to obtain a powerful and general representation for OCT images by training on 700K OCT images from 41K patients collected under real world clinical settings. We also provide the first extensive evaluation for a model of OCT on a challenging battery of 6 downstream tasks. Our model achieves strong performance when fully finetuned but can also serve as a versatile frozen feature extractor for many tasks using lightweight adapters. Furthermore, we propose an extension of the MAE pretraining to fuse OCT with an auxiliary modality, namely, IR fundus images and learn a joint model for both. We demonstrate our approach improves performance on a multimodal downstream application. Our experiments utilize most publicly available OCT datasets, thus enabling future comparisons. Our code and model weights are publicly available https://github.com/TheoPis/MIM_OCT. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.14788v1-abstract-full').style.display = 'none'; document.getElementById('2405.14788v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.12727">arXiv:2405.12727</a> <span> [<a href="https://arxiv.org/pdf/2405.12727">pdf</a>, <a href="https://arxiv.org/format/2405.12727">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Feasibility study on retrieving exoplanetary cloud cover distributions using polarimetry </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Winning%2C+S">S. Winning</a>, <a href="/search/?searchtype=author&query=Lietzow-Sinjen%2C+M">M. Lietzow-Sinjen</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">S. Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.12727v1-abstract-short" style="display: inline;"> Context. As a new growing field, exocartography aims to map the surface features of exoplanets that are beyond the resolution of traditional observing techniques. While photometric approaches have been discussed extensively, polarimetry has received less attention despite its promising prospects. Aims. We demonstrate that the limb polarization of an exoplanetary atmosphere offers valuable insigh… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12727v1-abstract-full').style.display = 'inline'; document.getElementById('2405.12727v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.12727v1-abstract-full" style="display: none;"> Context. As a new growing field, exocartography aims to map the surface features of exoplanets that are beyond the resolution of traditional observing techniques. While photometric approaches have been discussed extensively, polarimetry has received less attention despite its promising prospects. Aims. We demonstrate that the limb polarization of an exoplanetary atmosphere offers valuable insights into its cloud cover distribution. Specifically, we determine an upper limit for the polarimetric precision, which is required to extract information about the latitudinal cloud cover of temperate Jovian planets for scenarios of observations with and without host stars. Methods. To compute the scattered stellar radiation of an exoplanetary atmosphere and to study the polarization at various planetary phase angles, we used the three-dimensional Monte Carlo radiative transfer code POLARIS. Results. When the planetary signal can be measured separately from the stellar radiation, information about the latitudinal cloud cover for polar cap models is accessible at polarimetric sensitivities of $0.1$ %. In contrast, a precision of about $10^{-3}$ ppm is required when the stellar flux is included to gain this information. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.12727v1-abstract-full').style.display = 'none'; document.getElementById('2405.12727v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 21 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics. 8 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2405.06839">arXiv:2405.06839</a> <span> [<a href="https://arxiv.org/pdf/2405.06839">pdf</a>, <a href="https://arxiv.org/format/2405.06839">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Nuclear Experiment">nucl-ex</span> </div> </div> <p class="title is-5 mathjax"> Results from the CsI Calorimeter onboard the 2023 ComPair Balloon Flight </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Shy%2C+D">Daniel Shy</a>, <a href="/search/?searchtype=author&query=Woolf%2C+R+S">Richard S. Woolf</a>, <a href="/search/?searchtype=author&query=Sleator%2C+C">Clio Sleator</a>, <a href="/search/?searchtype=author&query=Phlips%2C+B">Bernard Phlips</a>, <a href="/search/?searchtype=author&query=Grove%2C+J+E">J. Eric Grove</a>, <a href="/search/?searchtype=author&query=Wulf%2C+E+A">Eric A. Wulf</a>, <a href="/search/?searchtype=author&query=Johnson-Rambert%2C+M">Mary Johnson-Rambert</a>, <a href="/search/?searchtype=author&query=Davis%2C+M">Mitch Davis</a>, <a href="/search/?searchtype=author&query=Kong%2C+E">Emily Kong</a>, <a href="/search/?searchtype=author&query=Caligiure%2C+T">Thomas Caligiure</a>, <a href="/search/?searchtype=author&query=Crosier%2C+A+W">A. Wilder Crosier</a>, <a href="/search/?searchtype=author&query=Bolotnikov%2C+A">Aleksey Bolotnikov</a>, <a href="/search/?searchtype=author&query=Cannady%2C+N">Nicholas Cannady</a>, <a href="/search/?searchtype=author&query=Carini%2C+G+A">Gabriella A. Carini</a>, <a href="/search/?searchtype=author&query=Caputo%2C+R">Regina Caputo</a>, <a href="/search/?searchtype=author&query=Fried%2C+J">Jack Fried</a>, <a href="/search/?searchtype=author&query=Ghosh%2C+P">Priyarshini Ghosh</a>, <a href="/search/?searchtype=author&query=Griffin%2C+S">Sean Griffin</a>, <a href="/search/?searchtype=author&query=Hays%2C+E">Elizabeth Hays</a>, <a href="/search/?searchtype=author&query=Herrmann%2C+S">Sven Herrmann</a>, <a href="/search/?searchtype=author&query=Kierans%2C+C">Carolyn Kierans</a>, <a href="/search/?searchtype=author&query=Kirschner%2C+N">Nicholas Kirschner</a>, <a href="/search/?searchtype=author&query=Liceaga-Indart%2C+I">Iker Liceaga-Indart</a>, <a href="/search/?searchtype=author&query=Metzler%2C+Z">Zachary Metzler</a>, <a href="/search/?searchtype=author&query=McEnery%2C+J">Julie McEnery</a> , et al. (11 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2405.06839v4-abstract-short" style="display: inline;"> The ComPair gamma-ray telescope is a technology demonstrator for a future gamma-ray telescope called the All-sky Medium Energy Gamma-ray Observatory (AMEGO). The instrument is composed of four subsystems, a double-sided silicon strip detector, a virtual Frisch grid CdZnTe calorimeter, a CsI:Tl based calorimeter, and an anti-coincidence detector (ACD). The CsI calorimeter's goal is to measure the p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.06839v4-abstract-full').style.display = 'inline'; document.getElementById('2405.06839v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2405.06839v4-abstract-full" style="display: none;"> The ComPair gamma-ray telescope is a technology demonstrator for a future gamma-ray telescope called the All-sky Medium Energy Gamma-ray Observatory (AMEGO). The instrument is composed of four subsystems, a double-sided silicon strip detector, a virtual Frisch grid CdZnTe calorimeter, a CsI:Tl based calorimeter, and an anti-coincidence detector (ACD). The CsI calorimeter's goal is to measure the position and energy deposited from high-energy events. To demonstrate the technological readiness, the calorimeter has flown onboard a NASA scientific balloon as part of the GRAPE-ComPair mission and accumulated around 3 hours of float time at an altitude of 40 km. During the flight, the CsI calorimeter observed background radiation, Regener-Pfotzer Maximum, and several gamma-ray activation lines originating from aluminum. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2405.06839v4-abstract-full').style.display = 'none'; document.getElementById('2405.06839v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 29 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> May 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2403.08388">arXiv:2403.08388</a> <span> [<a href="https://arxiv.org/pdf/2403.08388">pdf</a>, <a href="https://arxiv.org/format/2403.08388">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202348354">10.1051/0004-6361/202348354 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Feasibility of detecting shadows in disks induced by infall </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Krieger%2C+A">A. Krieger</a>, <a href="/search/?searchtype=author&query=Kuffmeier%2C+M">M. Kuffmeier</a>, <a href="/search/?searchtype=author&query=Reissl%2C+S">S. Reissl</a>, <a href="/search/?searchtype=author&query=Dullemond%2C+C+P">C. P. Dullemond</a>, <a href="/search/?searchtype=author&query=Ginski%2C+C">C. Ginski</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">S. Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2403.08388v1-abstract-short" style="display: inline;"> Observations performed with high-resolution imaging techniques revealed the existence of shadows in circumstellar disks that can be explained by the misalignment of an inner with respect to an outer disk. The cause of misalignment, however, is still debated. In this study, we investigate the feasibility of observing shadows induced by one prominent scenario that may lead to misalignment, which inv… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.08388v1-abstract-full').style.display = 'inline'; document.getElementById('2403.08388v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2403.08388v1-abstract-full" style="display: none;"> Observations performed with high-resolution imaging techniques revealed the existence of shadows in circumstellar disks that can be explained by the misalignment of an inner with respect to an outer disk. The cause of misalignment, however, is still debated. In this study, we investigate the feasibility of observing shadows induced by one prominent scenario that may lead to misalignment, which involves the late infall of material onto a protostellar system. In particular, we use previously performed hydrodynamical simulations of such events, and generate flux maps in the visible, near-infrared, submillimeter, and millimeter wavelength range using Monte Carlo radiative transfer. Based on that, we derive synthetic observations of these systems performed with the instruments SPHERE/VLT and ALMA, which we use as a basis for our subsequent analysis. We find that near-infrared observations with SPHERE are particularly well suited for detecting shadows via direct imaging alongside other features such as gaps, arcs, and streamers. On the contrary, performing a shadow detection based on reconstructed ALMA observations is very challenging due to the high sensitivity that is required for this task. Thus, in cases that allow for a detection, sophisticated analyses may be needed, for instance by the utilization of carefully constructed azimuthal profiles, aiding the search for potentially shallow shadows. Lastly, we conclude that late infall-induced disk misalignment offers a plausible explanation for the emergence of shadows that are observed in various systems. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2403.08388v1-abstract-full').style.display = 'none'; document.getElementById('2403.08388v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 March, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> March 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 16 pages, 16 figures, 1 table</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 686, A111 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.13161">arXiv:2402.13161</a> <span> [<a href="https://arxiv.org/pdf/2402.13161">pdf</a>, <a href="https://arxiv.org/format/2402.13161">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Mesoscale and Nanoscale Physics">cond-mat.mes-hall</span> </div> </div> <p class="title is-5 mathjax"> Nonadiabatic Dynamics of Molecules Interacting with Metal Surfaces: A Quantum-Classical Approach Based on Langevin Dynamics and the Hierarchical Equations of Motion </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Rudge%2C+S+L">Samuel L. Rudge</a>, <a href="/search/?searchtype=author&query=Kaspar%2C+C">Christoph Kaspar</a>, <a href="/search/?searchtype=author&query=Grether%2C+R+L">Robin L. Grether</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Steffen Wolf</a>, <a href="/search/?searchtype=author&query=Stock%2C+G">Gerhard Stock</a>, <a href="/search/?searchtype=author&query=Thoss%2C+M">Michael Thoss</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.13161v3-abstract-short" style="display: inline;"> A novel mixed quantum-classical approach to simulating nonadiabatic dynamics of molecules at metal surfaces is presented. The method combines the numerically exact hierarchical equations of motion approach for the quantum electronic degrees of freedom with Langevin dynamics for the classical degrees of freedom, namely, low-frequency vibrational modes within the molecule. The approach extends previ… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.13161v3-abstract-full').style.display = 'inline'; document.getElementById('2402.13161v3-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.13161v3-abstract-full" style="display: none;"> A novel mixed quantum-classical approach to simulating nonadiabatic dynamics of molecules at metal surfaces is presented. The method combines the numerically exact hierarchical equations of motion approach for the quantum electronic degrees of freedom with Langevin dynamics for the classical degrees of freedom, namely, low-frequency vibrational modes within the molecule. The approach extends previous mixed quantum-classical methods based on Langevin equations to models containing strong electron-electron or quantum electronic-vibrational interactions, while maintaining a nonperturbative and non-Markovian treatment of the molecule-metal coupling. To demonstrate the approach, nonequilibrium transport observables are calculated for a molecular nanojunction containing strong interactions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.13161v3-abstract-full').style.display = 'none'; document.getElementById('2402.13161v3-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 3 May, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 20 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2402.07103">arXiv:2402.07103</a> <span> [<a href="https://arxiv.org/pdf/2402.07103">pdf</a>, <a href="https://arxiv.org/format/2402.07103">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Statistical Mechanics">cond-mat.stat-mech</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Data Analysis, Statistics and Probability">physics.data-an</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Biomolecules">q-bio.BM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1021/acs.jctc.4c00250">10.1021/acs.jctc.4c00250 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Learning protein-ligand unbinding pathways via single-parameter community detection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=T%C3%A4nzel%2C+V">Victor T盲nzel</a>, <a href="/search/?searchtype=author&query=J%C3%A4ger%2C+M">Miriam J盲ger</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Steffen Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2402.07103v4-abstract-short" style="display: inline;"> Understanding the dynamics of biomolecular complexes, e.g., of protein-ligand (un)binding, requires the understanding of paths such systems take between metastable states. In MD simulation data, paths are usually not observable per se, but need to be inferred from simulation trajectories. Here we present a novel approach to cluster trajectories based on a community detection algorithm that require… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07103v4-abstract-full').style.display = 'inline'; document.getElementById('2402.07103v4-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2402.07103v4-abstract-full" style="display: none;"> Understanding the dynamics of biomolecular complexes, e.g., of protein-ligand (un)binding, requires the understanding of paths such systems take between metastable states. In MD simulation data, paths are usually not observable per se, but need to be inferred from simulation trajectories. Here we present a novel approach to cluster trajectories based on a community detection algorithm that requires the definition of only a single free parameter. Using the streptavidin-biotin complex as benchmark system and the A\textsubscript{2a} adenosine receptor in complex with the inhibitor ZM241385 as an elaborate application, we demonstrate how such clusters of trajectories correspond to pathways, and how the approach helps in the identification of reaction coordinates for a considered (un)binding process. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2402.07103v4-abstract-full').style.display = 'none'; document.getElementById('2402.07103v4-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 2 July, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 10 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> February 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This preprint is the unedited version of a manuscript that has been published as peer-reviewed article by J. Chem. Theory Comput. and can be downloaded for private use only. Copyright with the journal, ACS and the authors</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> J. Chem. Theory Comput. 20, 5058-5067 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.15775">arXiv:2401.15775</a> <span> [<a href="https://arxiv.org/pdf/2401.15775">pdf</a>, <a href="https://arxiv.org/format/2401.15775">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1002/asna.20230126">10.1002/asna.20230126 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Limitations of the modified blackbody fit method for determining molecular cloud properties </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Zielinski%2C+N">N. Zielinski</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">S. Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.15775v1-abstract-short" style="display: inline;"> Achieving a comprehensive understanding of the star and planet formation process is one of the fundamental tasks of astrophysics, requiring detailed knowledge of the physical conditions during the different phases of this process. During the earliest stages, i.e., concerning physical processes in molecular clouds and filaments, the column density N(H2), dust temperature T and dust emissivity index… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.15775v1-abstract-full').style.display = 'inline'; document.getElementById('2401.15775v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.15775v1-abstract-full" style="display: none;"> Achieving a comprehensive understanding of the star and planet formation process is one of the fundamental tasks of astrophysics, requiring detailed knowledge of the physical conditions during the different phases of this process. During the earliest stages, i.e., concerning physical processes in molecular clouds and filaments, the column density N(H2), dust temperature T and dust emissivity index \b{eta} of these objects can be derived by adopting a modified blackbody fit of the far-infrared to (sub-)millimeter spectral energy distributions. However, this often applied method is based on various assumptions. In addition, the observational basis and required, but only assumed cloud properties, such as a limited wavelength-coverage of the spectral energy distribution and dust properties, respectively, may differ between different studies. We review the basic limitations of this method and evaluate their impact on the derived physical properties of the objects of interest, i.e., molecular clouds and filaments. We find that the highest uncertainty when applying this method is introduced by the often poorly constrained dust properties. Therefore, we propose to first derive the optical depth and subsequently the column density with the help of a suitable dust model as the optical depth can be obtained with high accuracy, especially at longer wavelengths. The method provides reliable results up to the high densities and corresponding optical depths observed in molecular clouds. Considering typically used observational data, i.e., measurements obtained with far-infrared instruments like Herschel/PACS, JCMT/SCUBA-2 and SOFIA/HAWC+, data at four wavelengths are sufficient to obtain accurate results. Furthermore, we find that the dust emissivity index \b{eta} derived with this method is not suitable as an indicator of dust grain size. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.15775v1-abstract-full').style.display = 'none'; document.getElementById('2401.15775v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomische Nachrichten, 19 pages, 12 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.12119">arXiv:2401.12119</a> <span> [<a href="https://arxiv.org/pdf/2401.12119">pdf</a>, <a href="https://arxiv.org/format/2401.12119">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Quantum Physics">quant-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Statistical Mechanics">cond-mat.stat-mech</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Classical Physics">physics.class-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1119/5.0198820">10.1119/5.0198820 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Temperature as Joules per Bit </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=B%C3%A9dard%2C+C+A">Charles Alexandre B茅dard</a>, <a href="/search/?searchtype=author&query=Berthelette%2C+S">Sophie Berthelette</a>, <a href="/search/?searchtype=author&query=Coiteux-Roy%2C+X">Xavier Coiteux-Roy</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Stefan Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.12119v2-abstract-short" style="display: inline;"> In statistical mechanics, entropy is defined as a fundamental quantity. However, its unit, J/K, involves that of temperature, which is only subsequently defined - and defined in terms of entropy. This circularity arises with the introduction of Boltzmann's constant into the very expression of entropy. The J/K carried by the constant prevents entropy from finding a unit of its own while simultaneou… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.12119v2-abstract-full').style.display = 'inline'; document.getElementById('2401.12119v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.12119v2-abstract-full" style="display: none;"> In statistical mechanics, entropy is defined as a fundamental quantity. However, its unit, J/K, involves that of temperature, which is only subsequently defined - and defined in terms of entropy. This circularity arises with the introduction of Boltzmann's constant into the very expression of entropy. The J/K carried by the constant prevents entropy from finding a unit of its own while simultaneously obfuscating its informational nature. Following the precepts of information theory, we argue that entropy is well measured in bits and coincides with information capacity at thermodynamic equilibrium. Consequently, not only is the temperature of a system in equilibrium expressed in J/bit, but it acquires a clear meaning: It is the cost in energy to increase its information capacity by 1 bit. Viewing temperature as joules per bit uncovers the strong duality exhibited by Gibbs long ago between available capacity and free energy. It also simplifies Landauer's cost and clarifies that it is a cost of displacement, not of erasure. Replacing the kelvin with the bit as an SI unit would remove Boltzmann's constant from the seven defining constants. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.12119v2-abstract-full').style.display = 'none'; document.getElementById('2401.12119v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 28 February, 2025; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 22 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">15 pages, 3 figures, to be published in the American Journal of Physics</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2401.03437">arXiv:2401.03437</a> <span> [<a href="https://arxiv.org/pdf/2401.03437">pdf</a>, <a href="https://arxiv.org/format/2401.03437">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347535">10.1051/0004-6361/202347535 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Mid-infrared evidence for iron-rich dust in the multi-ringed inner disk of HD 144432 </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Varga%2C+J">J. Varga</a>, <a href="/search/?searchtype=author&query=Waters%2C+L+B+F+M">L. B. F. M. Waters</a>, <a href="/search/?searchtype=author&query=Hogerheijde%2C+M">M. Hogerheijde</a>, <a href="/search/?searchtype=author&query=van+Boekel%2C+R">R. van Boekel</a>, <a href="/search/?searchtype=author&query=Matter%2C+A">A. Matter</a>, <a href="/search/?searchtype=author&query=Lopez%2C+B">B. Lopez</a>, <a href="/search/?searchtype=author&query=Perraut%2C+K">K. Perraut</a>, <a href="/search/?searchtype=author&query=Chen%2C+L">L. Chen</a>, <a href="/search/?searchtype=author&query=Nadella%2C+D">D. Nadella</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">S. Wolf</a>, <a href="/search/?searchtype=author&query=Dominik%2C+C">C. Dominik</a>, <a href="/search/?searchtype=author&query=K%C3%B3sp%C3%A1l%2C+%C3%81">脕. K贸sp谩l</a>, <a href="/search/?searchtype=author&query=%C3%81brah%C3%A1m%2C+P">P. 脕brah谩m</a>, <a href="/search/?searchtype=author&query=Augereau%2C+J+-">J. -C. Augereau</a>, <a href="/search/?searchtype=author&query=Boley%2C+P">P. Boley</a>, <a href="/search/?searchtype=author&query=Bourdarot%2C+G">G. Bourdarot</a>, <a href="/search/?searchtype=author&query=Garatti%2C+A+C+o">A. Caratti o Garatti</a>, <a href="/search/?searchtype=author&query=de+Miera%2C+F+C">F. Cruz-S谩enz de Miera</a>, <a href="/search/?searchtype=author&query=Danchi%2C+W+C">W. C. Danchi</a>, <a href="/search/?searchtype=author&query=Rosas%2C+V+G">V. G谩mez Rosas</a>, <a href="/search/?searchtype=author&query=Henning%2C+T">Th. Henning</a>, <a href="/search/?searchtype=author&query=Hofmann%2C+K+-">K. -H. Hofmann</a>, <a href="/search/?searchtype=author&query=Houll%C3%A9%2C+M">M. Houll茅</a>, <a href="/search/?searchtype=author&query=Isbell%2C+J+W">J. W. Isbell</a>, <a href="/search/?searchtype=author&query=Jaffe%2C+W">W. Jaffe</a> , et al. (18 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2401.03437v1-abstract-short" style="display: inline;"> Context. Rocky planets form by the concentration of solid particles in the inner few au regions of planet-forming disks. Their chemical composition reflects the materials in the disk available in the solid phase at the time the planets were forming. Aims. We aim to constrain the structure and dust composition of the inner disk of the young star HD 144432, using an extensive set of infrared interfe… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.03437v1-abstract-full').style.display = 'inline'; document.getElementById('2401.03437v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2401.03437v1-abstract-full" style="display: none;"> Context. Rocky planets form by the concentration of solid particles in the inner few au regions of planet-forming disks. Their chemical composition reflects the materials in the disk available in the solid phase at the time the planets were forming. Aims. We aim to constrain the structure and dust composition of the inner disk of the young star HD 144432, using an extensive set of infrared interferometric data taken by the Very Large Telescope Interferometer (VLTI), combining PIONIER, GRAVITY, and MATISSE observations. Methods. We introduced a new physical disk model, TGMdust, to image the interferometric data, and to fit the disk structure and dust composition. We also performed equilibrium condensation calculations with GGchem. Results. Our best-fit model has three disk zones with ring-like structures at 0.15, 1.3, and 4.1 au. Assuming that the dark regions in the disk at ~0.9 au and at ~3 au are gaps opened by planets, we estimate the masses of the putative gap-opening planets to be around a Jupiter mass. We find evidence for an optically thin emission ($蟿<0.4$) from the inner two disk zones ($r<4$ au) at $位>3\ 渭$m. Our silicate compositional fits confirm radial mineralogy gradients. To identify the dust component responsible for the infrared continuum emission, we explore two cases for the dust composition, one with a silicate+iron mixture and the other with a silicate+carbon one. We find that the iron-rich model provides a better fit to the spectral energy distribution. Conclusions. We propose that in the warm inner regions ($r<5$ au) of typical planet-forming disks, most if not all carbon is in the gas phase, while iron and iron sulfide grains are major constituents of the solid mixture along with forsterite and enstatite. Our analysis demonstrates the need for detailed studies of the dust in inner disks with new mid-infrared instruments such as MATISSE and JWST/MIRI. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2401.03437v1-abstract-full').style.display = 'none'; document.getElementById('2401.03437v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 January, 2024; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> January 2024. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">29 pages, 24 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A, 681, A47 (2024) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.15283">arXiv:2312.15283</a> <span> [<a href="https://arxiv.org/pdf/2312.15283">pdf</a>, <a href="https://arxiv.org/format/2312.15283">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> </div> <p class="title is-5 mathjax"> Impact of discontinuous grain size distributions on the spectral energy distribution of debris disks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kim%2C+M">Minjae Kim</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.15283v1-abstract-short" style="display: inline;"> The collisional evolution of debris disks is expected to result in a characteristic wavy pattern of the grain size distributions, i.e., an under/overabundance of particles of specific sizes. This perturbed grain size distribution potentially leaves characteristic patterns in the spectral energy distribution (SED) of the disk system. We aim to quantify and understand the specific influence of disco… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.15283v1-abstract-full').style.display = 'inline'; document.getElementById('2312.15283v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.15283v1-abstract-full" style="display: none;"> The collisional evolution of debris disks is expected to result in a characteristic wavy pattern of the grain size distributions, i.e., an under/overabundance of particles of specific sizes. This perturbed grain size distribution potentially leaves characteristic patterns in the spectral energy distribution (SED) of the disk system. We aim to quantify and understand the specific influence of discontinuous particle size distributions on the appearance of debris disks. For this purpose, we consider dust emission models based on two different grain size distributions, i.e., once with a single and once with a broken power law. We compare the spectral index $伪$ ($F_谓\,\propto 谓^{\rm{\,伪}}$) in the case of a continuous grain size distribution with that of a discontinuous grain size distribution. We perform this comparison for central stars with different spectral types and two different disk structures (e.g., slim and broad debris dust rings). Within the considered parameter space, we find a characteristic difference between the spectral slopes of the SED in the different scenarios. More specifically, the overabundance of small grains leads to a steeper slope in the far-infrared/submillimeter regime, while the spectral index in the mm regime is hardly affected. On the other hand, the underabundance of medium-sized grains results in a slight steepening of the far-infrared slope of SED, while its primary effect is on the mm slope of SED, causing it to become shallower. We also find that the impact of an overabundance of small dust particles is more pronounced than that of an underabundance of medium-sized dust particles. Furthermore, we find that the difference between the spectral indices for the two different grain size distributions is largest for debris disks around brighter central stars and broader disks. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.15283v1-abstract-full').style.display = 'none'; document.getElementById('2312.15283v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">14 pages, 10 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.06295">arXiv:2312.06295</a> <span> [<a href="https://arxiv.org/pdf/2312.06295">pdf</a>, <a href="https://arxiv.org/format/2312.06295">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> </div> <p class="title is-5 mathjax"> Cataract-1K: Cataract Surgery Dataset for Scene Segmentation, Phase Recognition, and Irregularity Detection </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ghamsarian%2C+N">Negin Ghamsarian</a>, <a href="/search/?searchtype=author&query=El-Shabrawi%2C+Y">Yosuf El-Shabrawi</a>, <a href="/search/?searchtype=author&query=Nasirihaghighi%2C+S">Sahar Nasirihaghighi</a>, <a href="/search/?searchtype=author&query=Putzgruber-Adamitsch%2C+D">Doris Putzgruber-Adamitsch</a>, <a href="/search/?searchtype=author&query=Zinkernagel%2C+M">Martin Zinkernagel</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/?searchtype=author&query=Schoeffmann%2C+K">Klaus Schoeffmann</a>, <a href="/search/?searchtype=author&query=Sznitman%2C+R">Raphael Sznitman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.06295v1-abstract-short" style="display: inline;"> In recent years, the landscape of computer-assisted interventions and post-operative surgical video analysis has been dramatically reshaped by deep-learning techniques, resulting in significant advancements in surgeons' skills, operation room management, and overall surgical outcomes. However, the progression of deep-learning-powered surgical technologies is profoundly reliant on large-scale datas… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06295v1-abstract-full').style.display = 'inline'; document.getElementById('2312.06295v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.06295v1-abstract-full" style="display: none;"> In recent years, the landscape of computer-assisted interventions and post-operative surgical video analysis has been dramatically reshaped by deep-learning techniques, resulting in significant advancements in surgeons' skills, operation room management, and overall surgical outcomes. However, the progression of deep-learning-powered surgical technologies is profoundly reliant on large-scale datasets and annotations. Particularly, surgical scene understanding and phase recognition stand as pivotal pillars within the realm of computer-assisted surgery and post-operative assessment of cataract surgery videos. In this context, we present the largest cataract surgery video dataset that addresses diverse requisites for constructing computerized surgical workflow analysis and detecting post-operative irregularities in cataract surgery. We validate the quality of annotations by benchmarking the performance of several state-of-the-art neural network architectures for phase recognition and surgical scene segmentation. Besides, we initiate the research on domain adaptation for instrument segmentation in cataract surgery by evaluating cross-domain instrument segmentation performance in cataract surgery videos. The dataset and annotations will be publicly available upon acceptance of the paper. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.06295v1-abstract-full').style.display = 'none'; document.getElementById('2312.06295v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 11 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">12 pages, 5 figures, 7 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2312.03409">arXiv:2312.03409</a> <span> [<a href="https://arxiv.org/pdf/2312.03409">pdf</a>, <a href="https://arxiv.org/format/2312.03409">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> </div> <p class="title is-5 mathjax"> DeepPyramid+: Medical Image Segmentation using Pyramid View Fusion and Deformable Pyramid Reception </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ghamsarian%2C+N">Negin Ghamsarian</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/?searchtype=author&query=Zinkernagel%2C+M">Martin Zinkernagel</a>, <a href="/search/?searchtype=author&query=Schoeffmann%2C+K">Klaus Schoeffmann</a>, <a href="/search/?searchtype=author&query=Sznitman%2C+R">Raphael Sznitman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2312.03409v1-abstract-short" style="display: inline;"> Semantic Segmentation plays a pivotal role in many applications related to medical image and video analysis. However, designing a neural network architecture for medical image and surgical video segmentation is challenging due to the diverse features of relevant classes, including heterogeneity, deformability, transparency, blunt boundaries, and various distortions. We propose a network architectu… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.03409v1-abstract-full').style.display = 'inline'; document.getElementById('2312.03409v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2312.03409v1-abstract-full" style="display: none;"> Semantic Segmentation plays a pivotal role in many applications related to medical image and video analysis. However, designing a neural network architecture for medical image and surgical video segmentation is challenging due to the diverse features of relevant classes, including heterogeneity, deformability, transparency, blunt boundaries, and various distortions. We propose a network architecture, DeepPyramid+, which addresses diverse challenges encountered in medical image and surgical video segmentation. The proposed DeepPyramid+ incorporates two major modules, namely "Pyramid View Fusion" (PVF) and "Deformable Pyramid Reception," (DPR), to address the outlined challenges. PVF replicates a deduction process within the neural network, aligning with the human visual system, thereby enhancing the representation of relative information at each pixel position. Complementarily, DPR introduces shape- and scale-adaptive feature extraction techniques using dilated deformable convolutions, enhancing accuracy and robustness in handling heterogeneous classes and deformable shapes. Extensive experiments conducted on diverse datasets, including endometriosis videos, MRI images, OCT scans, and cataract and laparoscopy videos, demonstrate the effectiveness of DeepPyramid+ in handling various challenges such as shape and scale variation, reflection, and blur degradation. DeepPyramid+ demonstrates significant improvements in segmentation performance, achieving up to a 3.65% increase in Dice coefficient for intra-domain segmentation and up to a 17% increase in Dice coefficient for cross-domain segmentation. DeepPyramid+ consistently outperforms state-of-the-art networks across diverse modalities considering different backbone networks, showcasing its versatility. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2312.03409v1-abstract-full').style.display = 'none'; document.getElementById('2312.03409v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 6 December, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> December 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">13 pages, 3 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.13252">arXiv:2311.13252</a> <span> [<a href="https://arxiv.org/pdf/2311.13252">pdf</a>, <a href="https://arxiv.org/format/2311.13252">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> </div> <p class="title is-5 mathjax"> Improving Monte Carlo radiative transfer in the regime of high optical depths: The minimum scattering order </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Krieger%2C+A">Anton Krieger</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.13252v1-abstract-short" style="display: inline;"> Radiative transfer (RT) simulations are a powerful tool that enables the calculation of synthetic images of a wide range of astrophysical objects. These simulations are often based on the Monte Carlo (MC) method, as it provides the needed versatility that allows the consideration of the diverse and often complex conditions found in those objects. However, this method faces fundamental problems in… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13252v1-abstract-full').style.display = 'inline'; document.getElementById('2311.13252v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.13252v1-abstract-full" style="display: none;"> Radiative transfer (RT) simulations are a powerful tool that enables the calculation of synthetic images of a wide range of astrophysical objects. These simulations are often based on the Monte Carlo (MC) method, as it provides the needed versatility that allows the consideration of the diverse and often complex conditions found in those objects. However, this method faces fundamental problems in the regime of high optical depths which may result in noisy images and underestimated flux values. In this study, we propose an advanced MCRT method, i.e., an enforced minimum scattering order that is aimed at providing a minimum quality of determined flux estimates. For that purpose, we extended our investigations of the scattering order problem and derived an analytic expression for the minimum number of interactions that depends on the albedo and optical depth of the system, which needs to be considered to achieve a certain coverage of the scattering order distribution. The method is based on the utilization of this estimated minimum scattering order and enforces the consideration of a sufficient number of interactions during a simulation. Moreover, we identified two notably distinct cases that shape the kind of complexity that arises in MCRT simulations: the albedo-dominated and the optical depth-dominated case. Based on that, we analyzed implications regarding the best usage of a stretching method as a means to alleviate the scattering order problem. We find that its most suitable application requires taking into account the albedo and the optical depth. Then, we argue that the derived minimum scattering order can be used to assess the performance of a stretching method with regard to the scattering orders its usage promotes. Finally, we stress the need for developing advanced pathfinding techniques to fully solve the problem of MCRT simulations in the regime of high optical depths. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.13252v1-abstract-full').style.display = 'none'; document.getElementById('2311.13252v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 22 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 10 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.10056">arXiv:2311.10056</a> <span> [<a href="https://arxiv.org/pdf/2311.10056">pdf</a>, <a href="https://arxiv.org/format/2311.10056">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Cosmology and Nongalactic Astrophysics">astro-ph.CO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Astrophysics of Galaxies">astro-ph.GA</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="High Energy Astrophysical Phenomena">astro-ph.HE</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> A Collection of German Science Interests in the Next Generation Very Large Array </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kadler%2C+M">M. Kadler</a>, <a href="/search/?searchtype=author&query=Riechers%2C+D+A">D. A. Riechers</a>, <a href="/search/?searchtype=author&query=Agarwal%2C+J">J. Agarwal</a>, <a href="/search/?searchtype=author&query=Baczko%2C+A+-">A. -K. Baczko</a>, <a href="/search/?searchtype=author&query=Beuther%2C+H">H. Beuther</a>, <a href="/search/?searchtype=author&query=Bigiel%2C+F">F. Bigiel</a>, <a href="/search/?searchtype=author&query=Birnstiel%2C+T">T. Birnstiel</a>, <a href="/search/?searchtype=author&query=Boccardi%2C+B">B. Boccardi</a>, <a href="/search/?searchtype=author&query=Bomans%2C+D+J">D. J. Bomans</a>, <a href="/search/?searchtype=author&query=Boogaard%2C+L">L. Boogaard</a>, <a href="/search/?searchtype=author&query=Braun%2C+T+T">T. T. Braun</a>, <a href="/search/?searchtype=author&query=Britzen%2C+S">S. Britzen</a>, <a href="/search/?searchtype=author&query=Br%C3%BCggen%2C+M">M. Br眉ggen</a>, <a href="/search/?searchtype=author&query=Brunthaler%2C+A">A. Brunthaler</a>, <a href="/search/?searchtype=author&query=Caselli%2C+P">P. Caselli</a>, <a href="/search/?searchtype=author&query=Els%C3%A4sser%2C+D">D. Els盲sser</a>, <a href="/search/?searchtype=author&query=von+Fellenberg%2C+S">S. von Fellenberg</a>, <a href="/search/?searchtype=author&query=Flock%2C+M">M. Flock</a>, <a href="/search/?searchtype=author&query=Fromm%2C+C+M">C. M. Fromm</a>, <a href="/search/?searchtype=author&query=Fuhrmann%2C+L">L. Fuhrmann</a>, <a href="/search/?searchtype=author&query=Hartogh%2C+P">P. Hartogh</a>, <a href="/search/?searchtype=author&query=Hoeft%2C+M">M. Hoeft</a>, <a href="/search/?searchtype=author&query=Keenan%2C+R+P">R. P. Keenan</a>, <a href="/search/?searchtype=author&query=Kovalev%2C+Y">Y. Kovalev</a>, <a href="/search/?searchtype=author&query=Kreckel%2C+K">K. Kreckel</a> , et al. (66 additional authors not shown) </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.10056v2-abstract-short" style="display: inline;"> The Next Generation Very Large Array (ngVLA) is a planned radio interferometer providing unprecedented sensitivity at wavelengths between 21 cm and 3 mm. Its 263 antenna element array will be spatially distributed across North America to enable both superb low surface brightness recovery and sub-milliarcsecond angular resolution imaging. The project was developed by the international astronomy com… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.10056v2-abstract-full').style.display = 'inline'; document.getElementById('2311.10056v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.10056v2-abstract-full" style="display: none;"> The Next Generation Very Large Array (ngVLA) is a planned radio interferometer providing unprecedented sensitivity at wavelengths between 21 cm and 3 mm. Its 263 antenna element array will be spatially distributed across North America to enable both superb low surface brightness recovery and sub-milliarcsecond angular resolution imaging. The project was developed by the international astronomy community under the lead of the National Radio Astronomy Observatory (NRAO), and is anticipated to be built between 2027 and 2037. Two workshops have been held in 2022 and 2023 with the goal to discuss and consolidate the scientific interests in the ngVLA within the German astronomical community. This community paper constitutes a collection of 48 science ideas which the German community aims to pursue with the ngVLA in the 2030s. This is not a complete list and the ideas are not developed at the level of a "Science Book", such that the present document is mainly meant provide a basis for further discussion within the community. As such, additional contributions are welcome, and will be considered for inclusion in future revisions. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.10056v2-abstract-full').style.display = 'none'; document.getElementById('2311.10056v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 18 June, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 16 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Version 2.0 (status June 18, 2024): 169 pages, comments and future contributions welcome [v2.0: 7 new science cases added, some minor revisions to other chapters]</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2311.08051">arXiv:2311.08051</a> <span> [<a href="https://arxiv.org/pdf/2311.08051">pdf</a>, <a href="https://arxiv.org/format/2311.08051">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Category Theory">math.CT</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Algebraic Topology">math.AT</span> </div> </div> <p class="title is-5 mathjax"> Proper morphisms of $\infty$-topoi </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Martini%2C+L">Louis Martini</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2311.08051v2-abstract-short" style="display: inline;"> We characterise proper morphisms of $\infty$-topoi in terms of a relativised notion of compactness: we show that a geometric morphism of $\infty$-topoi is proper if and only if it commutes with colimits indexed by filtered internal $\infty$-categories in the target. In particular, our result implies that for any $\infty$-topos, the global sections functor is proper if and only if it preserves filt… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.08051v2-abstract-full').style.display = 'inline'; document.getElementById('2311.08051v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2311.08051v2-abstract-full" style="display: none;"> We characterise proper morphisms of $\infty$-topoi in terms of a relativised notion of compactness: we show that a geometric morphism of $\infty$-topoi is proper if and only if it commutes with colimits indexed by filtered internal $\infty$-categories in the target. In particular, our result implies that for any $\infty$-topos, the global sections functor is proper if and only if it preserves filtered colimits. As an application, we show that every proper and separated map of topological spaces gives rise to a proper morphism between the associated sheaf $\infty$-topoi, generalising a result of Lurie. Along the way, we develop some aspects of the theory of localic higher topoi internal to an $\infty$-topos, which might be of independent interest. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2311.08051v2-abstract-full').style.display = 'none'; document.getElementById('2311.08051v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 February, 2024; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 14 November, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> November 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Update of references</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.18429">arXiv:2310.18429</a> <span> [<a href="https://arxiv.org/pdf/2310.18429">pdf</a>, <a href="https://arxiv.org/format/2310.18429">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computational Physics">physics.comp-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347138">10.1051/0004-6361/202347138 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Improving Monte Carlo radiative transfer simulations: A shift of framework </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Krieger%2C+A">Anton Krieger</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.18429v1-abstract-short" style="display: inline;"> Monte Carlo radiative transfer (MCRT) simulations are a powerful tool for determining the appearance of astrophysical objects, analyzing the prevalent physical conditions within them, and inferring their properties on the basis of real observations. Consequently, a broad variety of codes has been implemented and optimized with the goal of solving this task efficiently. To that end, two distinct fr… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.18429v1-abstract-full').style.display = 'inline'; document.getElementById('2310.18429v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.18429v1-abstract-full" style="display: none;"> Monte Carlo radiative transfer (MCRT) simulations are a powerful tool for determining the appearance of astrophysical objects, analyzing the prevalent physical conditions within them, and inferring their properties on the basis of real observations. Consequently, a broad variety of codes has been implemented and optimized with the goal of solving this task efficiently. To that end, two distinct frameworks have emerged, namely, the extinction and the scattering framework, which form the basis of the path determination procedures of those codes. These procedures affect the step length of simulated photon packages and are used for determining flux estimates. Despite the fact that these simulations play an important role at present and thus require significant computational resources, little attention has been paid to the benefits and the drawbacks of both frameworks so far. In this study, we investigate their differences and assess their performance with regard to the quality of thereby obtained flux estimates, with a particular focus on the required computational demand. To that end, we use a testbed composed of an infinite plane-parallel slab, illuminated from one side, and we determine transmitted intensity using MCRT simulations for both frameworks. We find that there are vast differences between the frameworks with regard to their convergence speed. The scattering framework outperforms the extinction framework across all considered optical depths and albedos when solving this task, particularly in the regime of high optical depths. Its implementation can therefore greatly benefit all modern MCRT codes as it has the potential to significantly reduce required computation times. Thus, we highly recommend its consideration for various tasks that require MCRT simulations. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.18429v1-abstract-full').style.display = 'none'; document.getElementById('2310.18429v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 27 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in A&A, 10 pages, 8 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 680, A67 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.16688">arXiv:2310.16688</a> <span> [<a href="https://arxiv.org/pdf/2310.16688">pdf</a>, <a href="https://arxiv.org/format/2310.16688">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Robotics">cs.RO</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> </div> </div> <p class="title is-5 mathjax"> Learning-based adaption of robotic friction models </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Scholl%2C+P">Philipp Scholl</a>, <a href="/search/?searchtype=author&query=Iskandar%2C+M">Maged Iskandar</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/?searchtype=author&query=Lee%2C+J">Jinoh Lee</a>, <a href="/search/?searchtype=author&query=Bacho%2C+A">Aras Bacho</a>, <a href="/search/?searchtype=author&query=Dietrich%2C+A">Alexander Dietrich</a>, <a href="/search/?searchtype=author&query=Albu-Sch%C3%A4ffer%2C+A">Alin Albu-Sch盲ffer</a>, <a href="/search/?searchtype=author&query=Kutyniok%2C+G">Gitta Kutyniok</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.16688v1-abstract-short" style="display: inline;"> In the Fourth Industrial Revolution, wherein artificial intelligence and the automation of machines occupy a central role, the deployment of robots is indispensable. However, the manufacturing process using robots, especially in collaboration with humans, is highly intricate. In particular, modeling the friction torque in robotic joints is a longstanding problem due to the lack of a good mathemati… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.16688v1-abstract-full').style.display = 'inline'; document.getElementById('2310.16688v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.16688v1-abstract-full" style="display: none;"> In the Fourth Industrial Revolution, wherein artificial intelligence and the automation of machines occupy a central role, the deployment of robots is indispensable. However, the manufacturing process using robots, especially in collaboration with humans, is highly intricate. In particular, modeling the friction torque in robotic joints is a longstanding problem due to the lack of a good mathematical description. This motivates the usage of data-driven methods in recent works. However, model-based and data-driven models often exhibit limitations in their ability to generalize beyond the specific dynamics they were trained on, as we demonstrate in this paper. To address this challenge, we introduce a novel approach based on residual learning, which aims to adapt an existing friction model to new dynamics using as little data as possible. We validate our approach by training a base neural network on a symmetric friction data set to learn an accurate relation between the velocity and the friction torque. Subsequently, to adapt to more complex asymmetric settings, we train a second network on a small dataset, focusing on predicting the residual of the initial network's output. By combining the output of both networks in a suitable manner, our proposed estimator outperforms the conventional model-based approach and the base neural network significantly. Furthermore, we evaluate our method on trajectories involving external loads and still observe a substantial improvement, approximately 60-70\%, over the conventional approach. Our method does not rely on data with external load during training, eliminating the need for external torque sensors. This demonstrates the generalization capability of our approach, even with a small amount of data-only 43 seconds of a robot movement-enabling adaptation to diverse scenarios based on prior knowledge about friction in different settings. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.16688v1-abstract-full').style.display = 'none'; document.getElementById('2310.16688v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.09132">arXiv:2310.09132</a> <span> [<a href="https://arxiv.org/pdf/2310.09132">pdf</a>, <a href="https://arxiv.org/format/2310.09132">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202346767">10.1051/0004-6361/202346767 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Shaping the CO snowline in protoplanetary disks </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Gavino%2C+S">S. Gavino</a>, <a href="/search/?searchtype=author&query=Kobus%2C+J">J. Kobus</a>, <a href="/search/?searchtype=author&query=Dutrey%2C+A">A. Dutrey</a>, <a href="/search/?searchtype=author&query=Guilloteau%2C+S">S. Guilloteau</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">S. Wolf</a>, <a href="/search/?searchtype=author&query=J%C3%B8rgensen%2C+J+K">J. K. J酶rgensen</a>, <a href="/search/?searchtype=author&query=Sharma%2C+R">R. Sharma</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.09132v1-abstract-short" style="display: inline;"> Characterizing the dust thermal structure in protoplanetary disks is a fundamental task as the dust surface temperature can affect both the planetary formation and the chemical evolution. Since the temperature is dependent on many parameters, including the grain size, properly modeling the grain temperature structure can be challenging. Many chemistry disk models usually employ a sophisticated sin… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09132v1-abstract-full').style.display = 'inline'; document.getElementById('2310.09132v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.09132v1-abstract-full" style="display: none;"> Characterizing the dust thermal structure in protoplanetary disks is a fundamental task as the dust surface temperature can affect both the planetary formation and the chemical evolution. Since the temperature is dependent on many parameters, including the grain size, properly modeling the grain temperature structure can be challenging. Many chemistry disk models usually employ a sophisticated single dust structure designed to reproduce the effect of a realistic population presumably composed of a large diversity of sizes. This generally represents a good approximation in most cases. Nonetheless, this dilutes the effects of the complex radiative interactions between the different grain populations on the resulting dust temperature, and thus the chemistry. We seek to show that the radiative interactions between dust grains of different sizes can induce a non-trivial dust temperature structure that cannot be reproduced by a single dust population and that can significantly affect the chemical outcome. The disk thermal structures are computed using the Monte-Carlo radiative transfer code RADMC-3D. The thermal structures are post-processed using the gas-grain code NAUTILUS to calculate the evolution of the chemical abundance. We find that simultaneously using at least two independent dust grain populations in disk models produces a complex temperature structure due to the starlight intercepted by the upper layers of the disk. In particular, we find that micron-sized dust grains are warmer than larger grains and can even show a radial temperature bump in some conditions. This dust temperature spread between the grains populations results in the segregation of the CO snowline and the presence of an unexpected CO gas hole along the midplane. We compare the results with observed close to edge-on class I/II disks. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.09132v1-abstract-full').style.display = 'none'; document.getElementById('2310.09132v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 13 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">21 pages, 19 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 680, A59 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.08501">arXiv:2310.08501</a> <span> [<a href="https://arxiv.org/pdf/2310.08501">pdf</a>, <a href="https://arxiv.org/format/2310.08501">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Machine Learning">cs.LG</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Computer Vision and Pattern Recognition">cs.CV</span> </div> </div> <p class="title is-5 mathjax"> Unsupervised Learning of Object-Centric Embeddings for Cell Instance Segmentation in Microscopy Images </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Wolf%2C+S">Steffen Wolf</a>, <a href="/search/?searchtype=author&query=Lalit%2C+M">Manan Lalit</a>, <a href="/search/?searchtype=author&query=Westmacott%2C+H">Henry Westmacott</a>, <a href="/search/?searchtype=author&query=McDole%2C+K">Katie McDole</a>, <a href="/search/?searchtype=author&query=Funke%2C+J">Jan Funke</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.08501v1-abstract-short" style="display: inline;"> Segmentation of objects in microscopy images is required for many biomedical applications. We introduce object-centric embeddings (OCEs), which embed image patches such that the spatial offsets between patches cropped from the same object are preserved. Those learnt embeddings can be used to delineate individual objects and thus obtain instance segmentations. Here, we show theoretically that, unde… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.08501v1-abstract-full').style.display = 'inline'; document.getElementById('2310.08501v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.08501v1-abstract-full" style="display: none;"> Segmentation of objects in microscopy images is required for many biomedical applications. We introduce object-centric embeddings (OCEs), which embed image patches such that the spatial offsets between patches cropped from the same object are preserved. Those learnt embeddings can be used to delineate individual objects and thus obtain instance segmentations. Here, we show theoretically that, under assumptions commonly found in microscopy images, OCEs can be learnt through a self-supervised task that predicts the spatial offset between image patches. Together, this forms an unsupervised cell instance segmentation method which we evaluate on nine diverse large-scale microscopy datasets. Segmentations obtained with our method lead to substantially improved results, compared to state-of-the-art baselines on six out of nine datasets, and perform on par on the remaining three datasets. If ground-truth annotations are available, our method serves as an excellent starting point for supervised training, reducing the required amount of ground-truth needed by one order of magnitude, thus substantially increasing the practical applicability of our method. Source code is available at https://github.com/funkelab/cellulus. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.08501v1-abstract-full').style.display = 'none'; document.getElementById('2310.08501v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 12 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> Proceedings of the IEEE/CVF International Conference on Computer Vision (ICCV), 2023, pages 21263-21272 </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2310.02795">arXiv:2310.02795</a> <span> [<a href="https://arxiv.org/pdf/2310.02795">pdf</a>, <a href="https://arxiv.org/format/2310.02795">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> </div> </div> <p class="title is-5 mathjax"> Protoplanetary and debris disks in the $畏$ Chamaeleontis Association: A sub-millimeter survey obtained with APEX/LABOCA </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Roccatagliata%2C+V">V. Roccatagliata</a>, <a href="/search/?searchtype=author&query=Sicilia-Aguilar%2C+A">A. Sicilia-Aguilar</a>, <a href="/search/?searchtype=author&query=Kim%2C+M">M. Kim</a>, <a href="/search/?searchtype=author&query=Campbell-White%2C+J">J. Campbell-White</a>, <a href="/search/?searchtype=author&query=Fang%2C+M">M. Fang</a>, <a href="/search/?searchtype=author&query=Murphy%2C+S+J">S. J. Murphy</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">S. Wolf</a>, <a href="/search/?searchtype=author&query=Lawson%2C+W+A">W. A. Lawson</a>, <a href="/search/?searchtype=author&query=Henning%2C+T">Th. Henning</a>, <a href="/search/?searchtype=author&query=Bouwman%2C+J">J. Bouwman</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2310.02795v1-abstract-short" style="display: inline;"> Nearby associations are ideal regions to study coeval samples of protoplanetary and debris disks down to late M-type stars. Those aged 5-10,Myrs, where most of the disk should have already dissipated forming planets, are of particular interest. We present the first complete study of both protoplanetary and debris disks in a young region, using the $畏$ Chamaeleontis association as a test bench to s… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.02795v1-abstract-full').style.display = 'inline'; document.getElementById('2310.02795v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2310.02795v1-abstract-full" style="display: none;"> Nearby associations are ideal regions to study coeval samples of protoplanetary and debris disks down to late M-type stars. Those aged 5-10,Myrs, where most of the disk should have already dissipated forming planets, are of particular interest. We present the first complete study of both protoplanetary and debris disks in a young region, using the $畏$ Chamaeleontis association as a test bench to study the cold disk content. We obtained sub-millimeter data for the entire core population down to late M-type stars, plus a few halo members. We performed a continuum sub-millimeter survey with APEX/LABOCA of all the core populations of $畏$ Cha association. Disk properties have been derived by modeling protoplanetary and debris disks using RADMC 2D and DMS, respectively. We find that protoplanetary disks in $畏$ Cha typically have holes with radii of the order of 0.01 to 0.03 AU, while ring-like emission from the debris disks is located between 20 au and 650 au from the central star. The parallaxes and Gaia eDR3 photometry, in combination with the PARSEC and COLIBRI isochrones, enable us to confirm an age of $畏$ Cha between 7 and 9 Myrs. In general, the disk mass seems insufficient to support accretion over a long time, even for the lowest mass accretors, a clear difference compared with other regions and also a sign that the mass budget is further underestimated. We do not find a correlation between the stellar masses, accretion rates, and disk masses, although this could be due to sample issues. We confirm that the presence of inner holes is not enough to stop accretion unless accompanied by dramatic changes to the total disk mass content. Comparing $畏$ Cha with other regions at different ages, we find that the physical processes responsible for debris disks (e.g., dust growth, dust trapping) efficiently act in less than 5 Myrs. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2310.02795v1-abstract-full').style.display = 'none'; document.getElementById('2310.02795v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 4 October, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> October 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">20 pages, 9 figures, 7 tables</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.08759">arXiv:2309.08759</a> <span> [<a href="https://arxiv.org/pdf/2309.08759">pdf</a>, <a href="https://arxiv.org/format/2309.08759">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Biological Physics">physics.bio-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Statistical Mechanics">cond-mat.stat-mech</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Biomolecules">q-bio.BM</span> </div> </div> <p class="title is-5 mathjax"> Investigation of rare protein conformational transitions via dissipation-corrected targeted molecular dynamics </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Post%2C+M">Matthias Post</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Steffen Wolf</a>, <a href="/search/?searchtype=author&query=Stock%2C+G">Gerhard Stock</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.08759v1-abstract-short" style="display: inline;"> To sample rare events, dissipation-corrected targeted molecular dynamics (dcTMD) applies a constant velocity constraint along a one-dimensional reaction coordinate $s$, which drives an atomistic system from an initial state into a target state. Employing a cumulant approximation of Jarzynski's identity, the free energy $螖G (s)$ is calculated from the mean external work and dissipated work of the p… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.08759v1-abstract-full').style.display = 'inline'; document.getElementById('2309.08759v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.08759v1-abstract-full" style="display: none;"> To sample rare events, dissipation-corrected targeted molecular dynamics (dcTMD) applies a constant velocity constraint along a one-dimensional reaction coordinate $s$, which drives an atomistic system from an initial state into a target state. Employing a cumulant approximation of Jarzynski's identity, the free energy $螖G (s)$ is calculated from the mean external work and dissipated work of the process. By calculating the friction coefficient $螕(s)$ from the dissipated work, in a second step the equilibrium dynamics of the process can be studied by propagating a Langevin equation. While so far dcTMD has been mostly applied to study the unbinding of protein-ligand complexes, here its applicability to rare conformational transitions within a protein and the prediction of their kinetics is investigated. As this typically requires the introduction of multiple collective variables $\{x_j\}= \vec{x}$, a theoretical framework is outlined to calculate the associated free energy $螖G (\vec{x})$ and friction $\matrix螕(\vec{x})$ from dcTMD simulations along coordinate $s$. Adopting the $伪$-$尾$ transition of alanine dipeptide as well as the open-closed transition of T4 lysozyme as representative examples, the virtues and shortcomings of dcTMD to predict protein conformational transitions and the related kinetics are studied. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.08759v1-abstract-full').style.display = 'none'; document.getElementById('2309.08759v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 15 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">This preprint is the unedited version of a manuscript that has been sent to a scientific journal for consideration as a publication and can be downloaded for private use only. Copyright with the journal and its publisher after publication</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.04044">arXiv:2309.04044</a> <span> [<a href="https://arxiv.org/pdf/2309.04044">pdf</a>, <a href="https://arxiv.org/format/2309.04044">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Biological Physics">physics.bio-ph</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Quantitative Methods">q-bio.QM</span> </div> </div> <p class="title is-5 mathjax"> Capturing continuous, long timescale behavioral changes in $\textit{Drosophila melanogaster}$ postural data </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=McKenzie-Smith%2C+G+C">Grace C. McKenzie-Smith</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S+W">Scott W. Wolf</a>, <a href="/search/?searchtype=author&query=Ayroles%2C+J+F">Julien F. Ayroles</a>, <a href="/search/?searchtype=author&query=Shaevitz%2C+J+W">Joshua W. Shaevitz</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.04044v1-abstract-short" style="display: inline;"> Animal behavior spans many timescales, from short, seconds-scale actions to circadian rhythms over many hours to life-long changes during aging. Most quantitative behavior studies have focused on short-timescale behaviors such as locomotion and grooming. Analysis of these data suggests there exists a hierarchy of timescales; however, the limited duration of these experiments prevents the investiga… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.04044v1-abstract-full').style.display = 'inline'; document.getElementById('2309.04044v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.04044v1-abstract-full" style="display: none;"> Animal behavior spans many timescales, from short, seconds-scale actions to circadian rhythms over many hours to life-long changes during aging. Most quantitative behavior studies have focused on short-timescale behaviors such as locomotion and grooming. Analysis of these data suggests there exists a hierarchy of timescales; however, the limited duration of these experiments prevents the investigation of the full temporal structure. To access longer timescales of behavior, we continuously recorded individual $\textit{Drosophila melanogaster}$ at 100 frames per second for up to 7 days at a time in featureless arenas on sucrose-agarose media. We use the deep learning framework SLEAP to produce a full-body postural data set for 47 individuals resulting in nearly 2 billion pose instances. We identify stereotyped behaviors such as grooming, proboscis extension, and locomotion and use the resulting ethograms to explore how the flies' behavior varies across time of day and days in the experiment. We find distinct circadian patterns in all of our stereotyped behavior and also see changes in behavior over the course of the experiment as the flies weaken and die. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.04044v1-abstract-full').style.display = 'none'; document.getElementById('2309.04044v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 7 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">17 pages, 13 figures, authors GCM-S and SWW contributed equally</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2309.03573">arXiv:2309.03573</a> <span> [<a href="https://arxiv.org/pdf/2309.03573">pdf</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Materials Science">cond-mat.mtrl-sci</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Applied Physics">physics.app-ph</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1021/acsmaterialslett.3c01166">10.1021/acsmaterialslett.3c01166 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Impact of TCO Microstructure on the Electronic Properties of Carbazole-based Self-Assembled Monolayers </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Kralj%2C+S">Suzana Kralj</a>, <a href="/search/?searchtype=author&query=Dally%2C+P">Pia Dally</a>, <a href="/search/?searchtype=author&query=Bampoulis%2C+P">Pantelis Bampoulis</a>, <a href="/search/?searchtype=author&query=Vishal%2C+B">Badri Vishal</a>, <a href="/search/?searchtype=author&query=De+Wolf%2C+S">Stefaan De Wolf</a>, <a href="/search/?searchtype=author&query=Morales-Masis%2C+M">Monica Morales-Masis</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2309.03573v2-abstract-short" style="display: inline;"> Carbazole-based self-assembled monolayers (PACz-SAMs), anchored via their phosphonic acid group on a transparent conductive oxide (TCO) have demonstrated excellent performance as hole-selective layers in inverted perovskite solar cells. However, the influence of the TCO microstructure on the work function (WF) shift after SAM anchoring as well as the WF variations at the micro/nanoscale have not b… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03573v2-abstract-full').style.display = 'inline'; document.getElementById('2309.03573v2-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2309.03573v2-abstract-full" style="display: none;"> Carbazole-based self-assembled monolayers (PACz-SAMs), anchored via their phosphonic acid group on a transparent conductive oxide (TCO) have demonstrated excellent performance as hole-selective layers in inverted perovskite solar cells. However, the influence of the TCO microstructure on the work function (WF) shift after SAM anchoring as well as the WF variations at the micro/nanoscale have not been extensively studied yet. Herein, we investigate the effect of the Sn-doped In2O3 (ITO) microstructure on the WF distribution upon 2PACz-SAMs and NiOx/2PACz-SAMs application. For this, ITO substrates with amorphous and polycrystalline (featuring either nanoscale or microscale-sized grains) microstructures are studied. A correlation between the ITO grain orientation and 2PACz-SAMs local potential distribution was found via Kelvin probe force microscopy and electron backscatter diffraction. These variations vanish for amorphous ITO or when adding an amorphous NiOx buffer layer, where a homogeneous surface potential distribution is mapped. Ultraviolet photoelectron spectroscopy confirmed the ITO WF increase after 2PACz-SAMs deposition. Considering the importance of polycrystalline TCOs as high mobility and broadband transparent electrodes, we provide insights to ensure uniform WF distribution upon application of hole transport SAMs, which is critical towards enhanced device performance. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2309.03573v2-abstract-full').style.display = 'none'; document.getElementById('2309.03573v2-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 17 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">v1</span> submitted 7 September, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> September 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">18 pages, 5 figures</span> </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.13253">arXiv:2308.13253</a> <span> [<a href="https://arxiv.org/pdf/2308.13253">pdf</a>, <a href="https://arxiv.org/format/2308.13253">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347057">10.1051/0004-6361/202347057 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> Impact of hot exozodiacal dust on the polarimetric analysis of close-in exoplanets </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Ollmann%2C+K">Kevin Ollmann</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">Sebastian Wolf</a>, <a href="/search/?searchtype=author&query=Lietzow%2C+M">Moritz Lietzow</a>, <a href="/search/?searchtype=author&query=Stuber%2C+T+A">Thomas A. Stuber</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.13253v1-abstract-short" style="display: inline;"> Hot exozodiacal dust (HEZD) found around main-sequence stars through interferometric observations in the photometric bands H to L is located close to the dust sublimation radius, potentially at orbital radii comparable to those of close-in exoplanets. Consequently, HEZD has a potential influence on the analysis of the scattered-light polarization of close-in exoplanets and vice versa. We analyze t… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13253v1-abstract-full').style.display = 'inline'; document.getElementById('2308.13253v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.13253v1-abstract-full" style="display: none;"> Hot exozodiacal dust (HEZD) found around main-sequence stars through interferometric observations in the photometric bands H to L is located close to the dust sublimation radius, potentially at orbital radii comparable to those of close-in exoplanets. Consequently, HEZD has a potential influence on the analysis of the scattered-light polarization of close-in exoplanets and vice versa. We analyze the impact of HEZD on the polarimetric characterization of close-in exoplanets. This study is motivated in particular by the recently proven feasibility of exoplanet polarimetry. Applying the 3D Monte Carlo radiative transfer code POLARIS in an extended and optimized version for radiative transfer in exoplanetary atmospheres and an analytical tool for modeling the HEZD, we simulated and compared the polarization characteristics of the wavelength-dependent scattered-light polarization of HEZD and close-in exoplanets. The varied parameters are the planetary phase angle ($0^\circ-180^\circ$), the dust grain radius ($0.02\ 渭$m $- \ 10\ 渭$m), the HEZD mass ($10^{-10}$$\rm{M}_{\oplus}$ $-\ 10^{-8}$$\rm{M}_{\oplus}$), the orbital inclination ($0^\circ-90^\circ$), the composition of the planetary atmosphere (Mie and Rayleigh scattering atmosphere), the orbital radius of the HEZD ($0.02$ au $-\ 0.4$ au), and the planetary orbital radius ($0.01$ au $-\ 0.05$ au). The dust grain radius has the strongest influence on the polarimetric analysis due to its significant impact on the wavelength-dependent polarization characteristics and the total order of magnitude of the scattered-light polarization. In certain scenarios, the scattered-light polarization of the HEZD even exceeds that of the close-in exoplanet. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.13253v1-abstract-full').style.display = 'none'; document.getElementById('2308.13253v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 25 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy \& Astrophysics. 14 pages, 13 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 677, A187 (2023) </p> </li> <li class="arxiv-result"> <div class="is-marginless"> <p class="list-title is-inline-block"><a href="https://arxiv.org/abs/2308.12160">arXiv:2308.12160</a> <span> [<a href="https://arxiv.org/pdf/2308.12160">pdf</a>, <a href="https://arxiv.org/format/2308.12160">other</a>] </span> </p> <div class="tags is-inline-block"> <span class="tag is-small is-link tooltip is-tooltip-top" data-tooltip="Solar and Stellar Astrophysics">astro-ph.SR</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Earth and Planetary Astrophysics">astro-ph.EP</span> <span class="tag is-small is-grey tooltip is-tooltip-top" data-tooltip="Instrumentation and Methods for Astrophysics">astro-ph.IM</span> </div> <div class="is-inline-block" style="margin-left: 0.5rem"> <div class="tags has-addons"> <span class="tag is-dark is-size-7">doi</span> <span class="tag is-light is-size-7"><a class="" href="https://doi.org/10.1051/0004-6361/202347009">10.1051/0004-6361/202347009 <i class="fa fa-external-link" aria-hidden="true"></i></a></span> </div> </div> </div> <p class="title is-5 mathjax"> The potential of VLTI observations for the study of circumstellar disk variability </p> <p class="authors"> <span class="search-hit">Authors:</span> <a href="/search/?searchtype=author&query=Bensberg%2C+A">A. Bensberg</a>, <a href="/search/?searchtype=author&query=Kobus%2C+J">J. Kobus</a>, <a href="/search/?searchtype=author&query=Wolf%2C+S">S. Wolf</a> </p> <p class="abstract mathjax"> <span class="has-text-black-bis has-text-weight-semibold">Abstract</span>: <span class="abstract-short has-text-grey-dark mathjax" id="2308.12160v1-abstract-short" style="display: inline;"> Context. A characteristic feature of young stellar objects is their variability, which is caused by a variety of different physical processes. High-resolution interferometric observations in the near- and mid-infrared wavelength ranges spanning multiple epochs allow the detailed study of these processes. Aims. We aim at investigating the expected variations of the interferometric observables con… <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.12160v1-abstract-full').style.display = 'inline'; document.getElementById('2308.12160v1-abstract-short').style.display = 'none';">▽ More</a> </span> <span class="abstract-full has-text-grey-dark mathjax" id="2308.12160v1-abstract-full" style="display: none;"> Context. A characteristic feature of young stellar objects is their variability, which is caused by a variety of different physical processes. High-resolution interferometric observations in the near- and mid-infrared wavelength ranges spanning multiple epochs allow the detailed study of these processes. Aims. We aim at investigating the expected variations of the interferometric observables connected to changes in the measured photometric fluxes of a typical variable accreting central young stellar object with a circumstellar disk. Methods. We calculated visibilities and closure phases as well as the photometric flux of brightness distributions obtained using 3D Monte Carlo radiative transfer simulations for a model of a circumstellar disk with an accreting central star. Results. Changes in the accretion luminosity of the central object, that is, an accreting pre-main-sequence star, can lead to significant variations in the visibility and closure phase of the star-disk system measured with instruments at the Very Large Telescope Interferometer (VLTI) that can be related to changes in the photometric flux. Taking into account additional effects due to baseline variation, interferometric observations can provide valuable contributions to the understanding of the underlying processes. Additionally, we provide the web application VLTI B-VAR that allows the impact of the hour angle on the visibility and closure phase for customized intensity maps to be estimated. <a class="is-size-7" style="white-space: nowrap;" onclick="document.getElementById('2308.12160v1-abstract-full').style.display = 'none'; document.getElementById('2308.12160v1-abstract-short').style.display = 'inline';">△ Less</a> </span> </p> <p class="is-size-7"><span class="has-text-black-bis has-text-weight-semibold">Submitted</span> 23 August, 2023; <span class="has-text-black-bis has-text-weight-semibold">originally announced</span> August 2023. </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Comments:</span> <span class="has-text-grey-dark mathjax">Accepted for publication in Astronomy & Astrophysics. 14 pages, 15 figures</span> </p> <p class="comments is-size-7"> <span class="has-text-black-bis has-text-weight-semibold">Journal ref:</span> A&A 677, A126 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