Showing 1–50 of 247 results for author: Beck, T

The Periastron Passage of T Tauri South B as Viewed by ALMA: Millimeter Flux Variations and Dust Heating Triggered by Orbital Motion

Authors: Tracy L. Beck, Stephane Guilloteau, Gail Schaefer, Edwige Chapillon, Anne Dutrey, Emmanuel Di Folco

Abstract: We present 225 and 350 GHz imaging of the iconic T Tauri system using the Atacama Large Millimeter submillimeter Array (ALMA). T Tauri is a hierarchical triple system, and the close binary T Tau Sa/Sb underwent periastron passage in March 2023. The ALMA images were obtained in epochs spanning November 2019 through June 2023, and therefore covered the time frame of the recent periastron passage. We… ▽ More We present 225 and 350 GHz imaging of the iconic T Tauri system using the Atacama Large Millimeter submillimeter Array (ALMA). T Tauri is a hierarchical triple system, and the close binary T Tau Sa/Sb underwent periastron passage in March 2023. The ALMA images were obtained in epochs spanning November 2019 through June 2023, and therefore covered the time frame of the recent periastron passage. We clearly resolve the Sa-Sb binary in two epochs of high-resolution measurements with ALMA. We find increases in millimeter flux from heating of the Sa disk and the wider distribution of dust in the environment of the binary. This heating is likely in response to increased stellar accretion activity triggered by orbital motion during the dynamic periastron passage of T Tau Sb around Sa. Resolved, extended millimeter emission is also found to change morphology and increase in flux in the immediate environment of the Sa-Sb binary after periastron passage. This may suggest an increase in nonthermal emission from magnetic interaction, gravitational disruption of the circumstellar disks as the stars passed through periastron, or both of these phenomena. We also detected structures in the compact (24 au radius), thermal dust disk around T Tau N. In particular, we identify a crescent-shaped emission excess just outside a shallow gap at 12 au radius that appears to move at Keplerian speed. Future measurement of dust spectral indices can clarify the origin of increased and variable millimeter emission in the environment of the T Tau S binary. △ Less

Submitted 3 March, 2026; originally announced March 2026.

Comments: 11 pages, 8 figures

Journal ref: The Astrophysical Journal, 2026, Volume 999, Number 1, page 122

Convergent-Beam X-ray Crystallography

Authors: Chufeng Li, Margarita Zakharova, Mauro Prasciolu, Jia Chyi Wong, Holger Fleckenstein, Nikolay Ivanov, Wenhui Zhang, Mansi Butola, J. Lukas Dresselhaus, Ivan De Gennaro Aquino, Dmitry Egorov, Philipp Middendorf, Alessa Henkel, Bjarne Klopprogge, Lars Klemeyer, Tobias Beck, Oleksandr Yefanov, Miriam Barthelmess, Janina Sprenger, Dominik Oberthuer, Saša Bajt, Henry N. Chapman

Abstract: Molecular and polymeric crystals show a wide range of functional properties that arise from the interplay between the atomic-scale structure of their constituent molecules and the organization of these molecules within the crystal lattice at macroscopic length scales. X-ray diffraction can provide structural information at these disparate length scales, but usually only through experiments that ad… ▽ More Molecular and polymeric crystals show a wide range of functional properties that arise from the interplay between the atomic-scale structure of their constituent molecules and the organization of these molecules within the crystal lattice at macroscopic length scales. X-ray diffraction can provide structural information at these disparate length scales, but usually only through experiments that address one or the other of molecular (or unit-cell) structure versus crystal structure. Consequently, the accuracy of determined molecular or polymer structures may be limited by unaccounted crystal inhomogeneities of the crystal lattice and the characterization of crystalline materials might not reveal the underlying causes of crystal morphology. Here we introduce X-ray convergent-beam diffraction to obtain spatially-resolved structural information from crystals by projection topographic imaging. Using highly focusing X-ray multilayer Laue lenses, we show that Bragg reflections can be mapped into tomographic images of the crystal, for the characterization of strain and defects at high resolution. We demonstrate how the crystal morphology obtained this way can be accounted for when determining structure factors as a function of position in the crystal. The approach may assist in studies such as diffusion and binding in MOFS, protein-drug binding, crystal growth, and the mechanical responses of photo-reactive or thermally driven dynamic crystals. △ Less

Submitted 15 February, 2026; originally announced February 2026.

Gas-depleted planet formation occurred in the four-planet system around the red dwarf LHS 1903

Authors: Thomas G. Wilson, Anna M. Simpson, Andrew Collier Cameron, Ryan Cloutier, Vardan Adibekyan, Ancy Anna John, Yann Alibert, Manu Stalport, Jo Ann Egger, Andrea Bonfanti, Nicolas Billot, Pascal Guterman, Pierre F. L. Maxted, Attila E. Simon, Sergio G. Sousa, Malcolm Fridlund, Mathias Beck, Anja Bekkelien, Sebastien Salmon, Valerie Van Grootel, Luca Fossati, Alexander James Mustill, Hugh P. Osborn, Tiziano Zingales, Matthew J. Hooton , et al. (151 additional authors not shown)

Abstract: Small exoplanet radii show two populations, referred to as super-Earths and sub-Neptunes, separated by a gap known as the radius valley. This may be produced by the removal of atmospheres due to stellar or internal heating, or lack of an initial envelope. We us transit photometry and radial velocity measurements to detect and characterize four planets orbiting LHS 1903, a red dwarf (M-dwarf) star… ▽ More Small exoplanet radii show two populations, referred to as super-Earths and sub-Neptunes, separated by a gap known as the radius valley. This may be produced by the removal of atmospheres due to stellar or internal heating, or lack of an initial envelope. We us transit photometry and radial velocity measurements to detect and characterize four planets orbiting LHS 1903, a red dwarf (M-dwarf) star in the Milky Way's thick disk. The planets have orbital periods between 2.2 and 29.3 days, and span the radius valley within a single planetary system. The derived densities indicate that LHS 1903 b is rocky, while LHS 1903 c and LHS 1903 d have extended atmospheres. Although the most distant planet from the host star, LHS 1903 e, has no gaseous envelope, indicating it formed from gas-depleted material. △ Less

Submitted 11 February, 2026; originally announced February 2026.

Comments: Accepted for publication in Science

Nodal Deficiency of Neumann Eigenfunctions on a Symmetric Dumbbell Domain

Authors: Thomas Beck, Andrew Lyons

Abstract: We study the nodal deficiency of pairs of Neumann eigenfunctions defined over symmetric dumbbell domains. As the width of the connecting neck shrinks, these eigenfunctions converge to Neumann eigenfunctions defined over the ends of the dumbbell, together with a one-dimensional Sturm-Liouville solution in the neck. In this limit, the corresponding eigenvalues become degenerate, with multiplicity tw… ▽ More We study the nodal deficiency of pairs of Neumann eigenfunctions defined over symmetric dumbbell domains. As the width of the connecting neck shrinks, these eigenfunctions converge to Neumann eigenfunctions defined over the ends of the dumbbell, together with a one-dimensional Sturm-Liouville solution in the neck. In this limit, the corresponding eigenvalues become degenerate, with multiplicity two. The nodal deficiency, defined as the difference between the eigenvalue index and the nodal domain count, is known by the Courant nodal domain theorem to be nonnegative. We show that, for small neck widths, the nodal deficiencies of the dumbbell eigenfunctions are no smaller than the nodal deficiencies of the limiting eigenfunctions in the ends, and we provide conditions under which equality is achieved. As a consequence, we establish a criterion for identifying eigenfunctions of zero nodal deficiency for the dumbbell domain. △ Less

Submitted 23 January, 2026; originally announced January 2026.

Comments: 29 pages, 5 figures, the authors welcome all comments

MSC Class: 35P99; 35J25

Harnessing Quantum Computing for Energy Materials: Opportunities and Challenges

Authors: Seongmin Kim, In-Saeng Suh, Travis S. Humble, Thomas Beck, Eungkyu Lee, Tengfei Luo

Abstract: Developing high-performance materials is critical for diverse energy applications to increase efficiency, improve sustainability and reduce costs. Classical computational methods have enabled important breakthroughs in energy materials development, but they face scaling and time-complexity limitations, particularly for high-dimensional or strongly correlated material systems. Quantum computing (QC… ▽ More Developing high-performance materials is critical for diverse energy applications to increase efficiency, improve sustainability and reduce costs. Classical computational methods have enabled important breakthroughs in energy materials development, but they face scaling and time-complexity limitations, particularly for high-dimensional or strongly correlated material systems. Quantum computing (QC) promises to offer a paradigm shift by exploiting quantum bits with their superposition and entanglement to address challenging problems intractable for classical approaches. This perspective discusses the opportunities in leveraging QC to advance energy materials research and the challenges QC faces in solving complex and high-dimensional problems. We present cases on how QC, when combined with classical computing methods, can be used for the design and simulation of practical energy materials. We also outline the outlook for error-corrected, fault-tolerant QC capable of achieving predictive accuracy and quantum advantage for complex material systems. △ Less

Submitted 23 January, 2026; originally announced January 2026.

Comments: This manuscript is published in ACS Energy Letters at: https://doi.org/10.1021/acsenergylett.5c04009

Journal ref: ACS Energy Lett. 2026

JWST/NIRSpec Detects Warm CO Emission in the Terrestrial-Planet Zone of HD 131488

Authors: Cicero X. Lu, Isabel Rebollido, Sean Brittain, Tracy Beck, Christine H. Chen, Kadin Worthen, Joan Najita, Chen Xie, Aoife Brennan, Amaya Moro-Martin, John Debes, Kevin France, Luca Matrà, Marshall Perrin, Aki Roberge

Abstract: We have obtained a high-resolution, JWST NIRSpec $2.87$ -- $5.14$ $μ$m spectrum of the debris disk around HD 131488. We discover CO fundamental emission indicating the presence of warm fluorescent gas within $\sim10$ AU of the star. The large discrepancy in CO's vibrational and rotational temperature indicates that CO is out of thermal equilibrium and is excited with UV fluorescence. Our UV fluore… ▽ More We have obtained a high-resolution, JWST NIRSpec $2.87$ -- $5.14$ $μ$m spectrum of the debris disk around HD 131488. We discover CO fundamental emission indicating the presence of warm fluorescent gas within $\sim10$ AU of the star. The large discrepancy in CO's vibrational and rotational temperature indicates that CO is out of thermal equilibrium and is excited with UV fluorescence. Our UV fluorescence model gives a best fit of $1150\,$K with an effective temperature of $450$, $332$, and $125\,$K for the warm CO gas kinetic temperature within $0.5$, $1$, and $10\,$AU to the star and a gas vibrational temperature of $8800\,$K. The newly discovered warm CO gas population likely resides between sub-AU scales and $\sim\,10\,$AU, interior to the cold CO reservoir detected beyond $35\,$AU with HST STIS and ALMA. The discovery of warm, fluorescent gas in a debris disk is the first such detection ever made. The detection of warm CO raises the possibility of unseen molecules (H$_2$O, H$_2$, etc) as collisional partners to excite the warm gas. We estimated a lower mass limit for CO of $1.25\times 10^{-7}\text{M}_{\oplus}$, which is $10^{-5}$ of the cold CO mass detected with ALMA and HST. We demonstrate that UV fluorescence emerges as a promising avenue for detecting tenuous gas at $10^{-7}$ Earth-mass level in debris disks with JWST. △ Less

Submitted 12 December, 2025; originally announced December 2025.

Comments: 30 Pages, 15 Figures, 6 Tables; Accepted to ApJ; Data Behind Figure 2 Available on the Journal Publisher Site

The LCLStream Ecosystem for Multi-Institutional Dataset Exploration

Authors: David Rogers, Valerio Mariani, Cong Wang, Ryan Coffee, Wilko Kroeger, Murali Shankar, Hans Thorsten Schwander, Tom Beck, Frédéric Poitevin, Jana Thayer

Abstract: We describe a new end-to-end experimental data streaming framework designed from the ground up to support new types of applications -- AI training, extremely high-rate X-ray time-of-flight analysis, crystal structure determination with distributed processing, and custom data science applications and visualizers yet to be created. Throughout, we use design choices merging cloud microservices with t… ▽ More We describe a new end-to-end experimental data streaming framework designed from the ground up to support new types of applications -- AI training, extremely high-rate X-ray time-of-flight analysis, crystal structure determination with distributed processing, and custom data science applications and visualizers yet to be created. Throughout, we use design choices merging cloud microservices with traditional HPC batch execution models for security and flexibility. This project makes a unique contribution to the DOE Integrated Research Infrastructure (IRI) landscape. By creating a flexible, API-driven data request service, we address a significant need for high-speed data streaming sources for the X-ray science data analysis community. With the combination of data request API, mutual authentication web security framework, job queue system, high-rate data buffer, and complementary nature to facility infrastructure, the LCLStreamer framework has prototyped and implemented several new paradigms critical for future generation experiments. △ Less

Submitted 6 February, 2026; v1 submitted 4 October, 2025; originally announced October 2025.

Comments: 3 figures

Journal ref: In Proc. SCA/HPCAsiaWS '26. ACM, New York, 433-442 (2026)

Lifetimes of the $2^+_1$ and $4^+_1$ states of the neutron-rich nuclide $^{200}$Pt

Authors: C. M. Nickel, V. Werner, P. R. John, U. Ahmed, T. Beck, M. Boromiza, C. Clisu-Stan, A. Coman, C. Costache, N. M. Florea, K. E. Ide, A. Ionescu, R. Lică, N. M. Mărginean, R. Mărginean, A. Mitu, H. Mayr, C. Mihai, R. E. Mihai, S. Pascu, N. Pietralla, L. Stan, T. Stetz, A. E. Turturică, S. Ujeniuc , et al. (2 additional authors not shown)

Abstract: The lifetimes of the $2^+_1$ and $4^+_1$ states of $^{200}$Pt were measured applying the recoil-distance Doppler-shift method. Excited states were populated in the $^{198}$Pt($^{18}$O, $^{16}$O)$^{200}$Pt two-neutron transfer reaction at the $9\,\text{MV}$ tandem accelerator at the IFIN-HH in Măgurele, Romania. The resulting $B(E2)$ values of the $2^+_1 \rightarrow 0^+_1$ and… ▽ More The lifetimes of the $2^+_1$ and $4^+_1$ states of $^{200}$Pt were measured applying the recoil-distance Doppler-shift method. Excited states were populated in the $^{198}$Pt($^{18}$O, $^{16}$O)$^{200}$Pt two-neutron transfer reaction at the $9\,\text{MV}$ tandem accelerator at the IFIN-HH in Măgurele, Romania. The resulting $B(E2)$ values of the $2^+_1 \rightarrow 0^+_1$ and $4^+_1 \rightarrow 2^+_1$ transitions as well as the $B_{4/2}$ ratio of $2.08(32)$ indicate the nuclear structure evolving towards sphericity when approaching the neutron shell closure at $N = 126$. The $B(E2; 2^+_1 \rightarrow 0^+_1)$ values of Pt and Hg are compared to values of Te, Xe and Ba as both regions of the nuclear chart show similar structural effects. △ Less

Submitted 26 September, 2025; v1 submitted 25 September, 2025; originally announced September 2025.

Comments: 8 pages, 6 figures, 2 tables

Equipartition and the temperature of maximum density of TIP4/2005 water

Authors: Dilipkumar N. Asthagiri, Thiago Pinheiro dos Santos, Thomas L. Beck

Abstract: We simulate TIP4P/2005 water in the temperature range of 257 K to 318 K with time-steps $δ=$ 0.25, 0.50, 2.00, and 4.00 fs. The density-temperature behavior obtained using 0.25 or 0.50 fs are in excellent agreement with each other but differ from those obtained using time-steps that have been shown earlier to lead to a breakdown of equipartition. The temperature of maximum density (TMD) is 277.15… ▽ More We simulate TIP4P/2005 water in the temperature range of 257 K to 318 K with time-steps $δ=$ 0.25, 0.50, 2.00, and 4.00 fs. The density-temperature behavior obtained using 0.25 or 0.50 fs are in excellent agreement with each other but differ from those obtained using time-steps that have been shown earlier to lead to a breakdown of equipartition. The temperature of maximum density (TMD) is 277.15 K with $δt = 0.25\;\mathrm{or}\; 0.50$ fs, but is shifted to progressively lower values for longer time-steps, a trend that holds for different thermostat/barostat combinations. Enhancing the water-water dispersion interaction, as has been recommended for simulating disordered proteins in TIP4P/2005, degrades the description of the liquid-vapor phase envelope. A key takeaway from this study is that using sufficiently short time-steps ($\leq 0.5$ fs) to preserve equipartition is essential for obtaining meaningful liquid water properties and for producing reliable data to parametrize biomolecular simulation models, as correct-ensemble sampling is fundamental to ensure reproducibility across codes and simulation alogrithms. △ Less

Submitted 18 October, 2025; v1 submitted 20 August, 2025; originally announced August 2025.

The Role of Quantum Computing in Advancing Scientific High-Performance Computing: A perspective from the ADAC Institute

Authors: Gilles Buchs, Thomas Beck, Ryan Bennink, Daniel Claudino, Andrea Delgado, Nur Aiman Fadel, Peter Groszkowski, Kathleen Hamilton, Travis Humble, Neeraj Kumar, Ang Li, Phillip Lotshaw, Olli Mukkula, Ryousei Takano, Amit Saxena, In-Saeng Suh, Miwako Tsuji, Roel Van Beeumen, Ugo Varetto, Yan Wang, Kazuya Yamazaki, Mikael P. Johansson

Abstract: Quantum computing (QC) has gained significant attention over the past two decades due to its potential for speeding up classically demanding tasks. This transition from an academic focus to a thriving commercial sector is reflected in substantial global investments. While advancements in qubit counts and functionalities continues at a rapid pace, current quantum systems still lack the scalability… ▽ More Quantum computing (QC) has gained significant attention over the past two decades due to its potential for speeding up classically demanding tasks. This transition from an academic focus to a thriving commercial sector is reflected in substantial global investments. While advancements in qubit counts and functionalities continues at a rapid pace, current quantum systems still lack the scalability for practical applications, facing challenges such as too high error rates and limited coherence times. This perspective paper examines the relationship between QC and high-performance computing (HPC), highlighting their complementary roles in enhancing computational efficiency. It is widely acknowledged that even fully error-corrected QCs will not be suited for all computational task. Rather, future compute infrastructures are anticipated to employ quantum acceleration within hybrid systems that integrate HPC and QC. While QCs can enhance classical computing, traditional HPC remains essential for maximizing quantum acceleration. This integration is a priority for supercomputing centers and companies, sparking innovation to address the challenges of merging these technologies. The Accelerated Data Analytics and Computing Institute (ADAC) is comprised of globally leading HPC centers. ADAC has established a Quantum Computing Working Group to promote and catalyze collaboration among its members. This paper synthesizes insights from the QC Working Group, supplemented by findings from a member survey detailing ongoing projects and strategic directions. By outlining the current landscape and challenges of QC integration into HPC ecosystems, this work aims to provide HPC specialists with a deeper understanding of QC and its future implications for computationally intensive endeavors. △ Less

Submitted 27 January, 2026; v1 submitted 15 August, 2025; originally announced August 2025.

Comments: 46 pages, 3 figures

Determination of proton and neutron contributions to the $0_{g.s.}^+ \rightarrow 2_1^+$ excitations in $^{42}$Si and $^{44}$S using inelastic proton scattering in inverse kinematics and intermediate energy Coulomb excitation

Authors: L. A. Riley, I. Conroy, A. M. Himmelreich, M. Heinze, J. Kosa, B. McNulty, P. D. Cottle, M. Spieker, A. Volya, A. L. Conley, D. Houlihan, B. Kelly, K. W. Kemper, Sk M. Ali, T. Beck, S. A. Gillespie, M. Hausmann, S. Noji, J. Pereira, D. Weisshaar, J. Chung-Jung, P. Farris, A. Gade, G. Grauvogel, A. M. Hill , et al. (4 additional authors not shown)

Abstract: We have measured the $0_{g.s.}^+ \rightarrow 2_1^+$ transition in the neutron rich $N=28$ isotope $^{42}$Si using the probes of intermediate energy Coulomb excitation and inelastic proton scattering in inverse kinematics at the Facility for Rare Isotope Beams with beam particle rates of $\approx 5$ particles/s. The results of these two measurements allowed us to determine $M_n/M_p$, the ratio of t… ▽ More We have measured the $0_{g.s.}^+ \rightarrow 2_1^+$ transition in the neutron rich $N=28$ isotope $^{42}$Si using the probes of intermediate energy Coulomb excitation and inelastic proton scattering in inverse kinematics at the Facility for Rare Isotope Beams with beam particle rates of $\approx 5$ particles/s. The results of these two measurements allowed us to determine $M_n/M_p$, the ratio of the neutron and proton transition matrix elements for the $0_{g.s.}^+ \rightarrow 2_1^+$ transition. In addition, we have measured the $0_{\mathrm{g.s.}}^+ \rightarrow 2_1^+$ transition in the isotone $^{44}$S using inverse kinematics inelastic proton scattering. By comparing the $^{44}$S proton scattering result with a recent intermediate energy Coulomb excitation result on the same transition, we were able to determine $M_n/M_p$ for the $0_{g.s.}^+ \rightarrow 2_1^+$ transition in this nucleus as well. This work strengthens the evidence that $^{42}$Si has a stable quadrupole deformation in its ground state and that $^{44}$S does not. Both conclusions are further supported by shell model calculations carried out with the FSU interaction. △ Less

Submitted 1 August, 2025; originally announced August 2025.

Comments: 32 pages, 12 figures

Journal ref: Phys. Rev. C 112, 014331 (2025)

Data Readiness for Scientific AI at Scale

Authors: Wesley Brewer, Patrick Widener, Valentine Anantharaj, Feiyi Wang, Tom Beck, Arjun Shankar, Sarp Oral

Abstract: This paper examines how Data Readiness for AI (DRAI) principles apply to leadership-scale scientific datasets used to train foundation models. We analyze archetypal workflows across four representative domains - climate, nuclear fusion, bio/health, and materials - to identify common preprocessing patterns and domain-specific constraints. We introduce a two-dimensional readiness framework composed… ▽ More This paper examines how Data Readiness for AI (DRAI) principles apply to leadership-scale scientific datasets used to train foundation models. We analyze archetypal workflows across four representative domains - climate, nuclear fusion, bio/health, and materials - to identify common preprocessing patterns and domain-specific constraints. We introduce a two-dimensional readiness framework composed of Data Readiness Levels (raw to AI-ready) and Data Processing Stages (ingest to shard), both tailored to high performance computing (HPC) environments. This framework outlines key challenges in transforming scientific data for scalable AI training, emphasizing transformer-based generative models. Together, these dimensions form a conceptual maturity matrix that characterizes scientific data readiness and guides infrastructure development toward standardized, cross-domain support for scalable and reproducible AI for science. △ Less

Submitted 30 July, 2025; originally announced July 2025.

Comments: 10 pages, 1 figure, 2 tables

ACM Class: I.2.6

Exploring the Capabilities of the Frontier Large Language Models for Nuclear Energy Research

Authors: Ahmed Almeldein, Mohammed Alnaggar, Rick Archibald, Tom Beck, Arpan Biswas, Rike Bostelmann, Wes Brewer, Chris Bryan, Christopher Calle, Cihangir Celik, Rajni Chahal, Jong Youl Choi, Arindam Chowdhury, Mark Cianciosa, Franklin Curtis, Gregory Davidson, Sebastian De Pascuale, Lisa Fassino, Ana Gainaru, Yashika Ghai, Luke Gibson, Qian Gong, Christopher Greulich, Scott Greenwood, Cory Hauck , et al. (25 additional authors not shown)

Abstract: The AI for Nuclear Energy workshop at Oak Ridge National Laboratory evaluated the potential of Large Language Models (LLMs) to accelerate fusion and fission research. Fourteen interdisciplinary teams explored diverse nuclear science challenges using ChatGPT, Gemini, Claude, and other AI models over a single day. Applications ranged from developing foundation models for fusion reactor control to au… ▽ More The AI for Nuclear Energy workshop at Oak Ridge National Laboratory evaluated the potential of Large Language Models (LLMs) to accelerate fusion and fission research. Fourteen interdisciplinary teams explored diverse nuclear science challenges using ChatGPT, Gemini, Claude, and other AI models over a single day. Applications ranged from developing foundation models for fusion reactor control to automating Monte Carlo simulations, predicting material degradation, and designing experimental programs for advanced reactors. Teams employed structured workflows combining prompt engineering, deep research capabilities, and iterative refinement to generate hypotheses, prototype code, and research strategies. Key findings demonstrate that LLMs excel at early-stage exploration, literature synthesis, and workflow design, successfully identifying research gaps and generating plausible experimental frameworks. However, significant limitations emerged, including difficulties with novel materials designs, advanced code generation for modeling and simulation, and domain-specific details requiring expert validation. The successful outcomes resulted from expert-driven prompt engineering and treating AI as a complementary tool rather than a replacement for physics-based methods. The workshop validated AI's potential to accelerate nuclear energy research through rapid iteration and cross-disciplinary synthesis while highlighting the need for curated nuclear-specific datasets, workflow automation, and specialized model development. These results provide a roadmap for integrating AI tools into nuclear science workflows, potentially reducing development cycles for safer, more efficient nuclear energy systems while maintaining rigorous scientific standards. △ Less

Submitted 26 June, 2025; v1 submitted 10 June, 2025; originally announced June 2025.

Water ice in the debris disk around HD 181327

Authors: Chen Xie, Christine H. Chen, Carey M. Lisse, Dean C. Hines, Tracy Beck, Sarah K. Betti, Noemí Pinilla-Alonso, Carl Ingebretsen, Kadin Worthen, András Gáspár, Schuyler G. Wolff, Bryce T. Bolin, Laurent Pueyo, Marshall D. Perrin, John A. Stansberry, Jarron M. Leisenring

Abstract: Debris disks are exoplanetary systems that contain planets, minor bodies (i.e., asteroids, Kuiper belt objects, comets, etc.), and micron-sized debris dust. Since water ice is the most common frozen volatile, it plays an essential role in the formation of planets and minor bodies. Although water ice has been commonly found in Kuiper belt objects and comets in the Solar System, no definitive eviden… ▽ More Debris disks are exoplanetary systems that contain planets, minor bodies (i.e., asteroids, Kuiper belt objects, comets, etc.), and micron-sized debris dust. Since water ice is the most common frozen volatile, it plays an essential role in the formation of planets and minor bodies. Although water ice has been commonly found in Kuiper belt objects and comets in the Solar System, no definitive evidence for water ice in debris disks has been obtained to date. Here, we report the discovery of water ice in the HD 181327 disk using the James Webb Space Telescope Near-Infrared Spectrograph. We detect the solid-state broad absorption feature of water ice at 3 $μ$m and a distinct Fresnel peak feature at 3.1 $μ$m, a characteristic of large water-ice particles. This implies the presence of a water-ice reservoir in the HD 181327 exoKuiper belt. Gradients of water-ice features at different stellocentric distances reveal a dynamic process of destroying and replenishing water ice in the disk, with estimated water-ice mass fractions ranging from 0.1% at ~85 au to 14% at ~113 au. It is highly plausible that the icy bodies that release water ice in HD 181327 could be the extra-solar counterparts of some of the Kuiper belt objects in our Solar System, supported by their spectral similarity. △ Less

Submitted 6 January, 2026; v1 submitted 13 May, 2025; originally announced May 2025.

Comments: Published in Nature on May 14th, 2025, https://www.nature.com/articles/s41586-025-08920-4

Journal ref: Nature 641, 608-611 2025

On non-local exchange and scattering operators in domain decomposition methods

Authors: Thomas Beck, Yaiza Canzani, Jeremy L. Marzuola

Abstract: We study non-local exchange and scattering operators arising in domain decomposition algorithms for solving elliptic problems on domains in $\mathbb{R}^2$. Motivated by recent formulations of the Optimized Schwarz Method introduced by Claeys, we rigorously analyze the behavior of a family of non-local exchange operators $Π_γ$, defined in terms of boundary integral operators associated to the funda… ▽ More We study non-local exchange and scattering operators arising in domain decomposition algorithms for solving elliptic problems on domains in $\mathbb{R}^2$. Motivated by recent formulations of the Optimized Schwarz Method introduced by Claeys, we rigorously analyze the behavior of a family of non-local exchange operators $Π_γ$, defined in terms of boundary integral operators associated to the fundamental solution for $-Δ+ γ^{-2}$, with $γ> 0$. Our first main result establishes precise estimates comparing $Π_γ$ to its local counterpart $Π_0$ as $γ\to 0$, providing a quantitative bridge between the classical and non-local formulations of the Optimized Schwarz Method. In addition, we investigate the corresponding scattering operators, proving norm estimates that relate them to their classical analogues through a detailed analysis of the associated Dirichlet-to-Neumann operators. Our results clarify the relationship between classical and non-local formulations of domain decomposition methods and yield new insights that are essential for the analysis of these algorithms, particularly in the presence of cross points and for domains with curvilinear polygonal boundaries. △ Less

Submitted 8 April, 2025; originally announced April 2025.

Comments: 30 pages, 1 figure, comments welcome!

MSC Class: 35J25; 65N12

The edge-on disk Tau042021: icy grains at high altitudes and a wind containing astronomical PAHs

Authors: E. Dartois, J. A. Noble, M. K. McClure, J. A. Sturm, T. L. Beck, N. Arulanantham, M. N. Drozdovskaya, C. C. Espaillat, D. Harsono, M. -E. Palumbo, Y. J. Pendleton, K. M. Pontoppidan

Abstract: Spectra of the nearly edge-on protoplanetary disks observed with the JWST have shown ice absorption bands of varying optical depths and peculiar profiles, challenging radiative transfer modelling and our understanding of dust and ice in disks. We build models including dust grain size, shape, and composition to reproduce JWST IFU spectroscopy of the large edge-on disk Tau042021. We explore radiati… ▽ More Spectra of the nearly edge-on protoplanetary disks observed with the JWST have shown ice absorption bands of varying optical depths and peculiar profiles, challenging radiative transfer modelling and our understanding of dust and ice in disks. We build models including dust grain size, shape, and composition to reproduce JWST IFU spectroscopy of the large edge-on disk Tau042021. We explore radiative transfer models using different dust grain size distributions, including grains of effective radii a_eff = 0.005-3000 microns. Scattering properties of distributions of triaxial ellipsoidal grains are calculated. We consider compositions with silicates, amorphous carbon, and mixtures of H2O, CO2, and CO. We use RADMC-3D Monte Carlo radiative transfer models of Tau042021 to simulate the spectral cubes observed with JWST-NIRSpec and MIRI. We compare the results to observations, including H2O at 3.05 microns, CO at 4.67 microns, and CO2 at 4.27 microns and to archival JWST-NIRCam and ALMA continuum images. The observed near- to mid-infrared imply dust distributions with grain sizes up to several tens of microns. The intensity distribution perpendicular to the disk exhibits emission profile wings extending into the upper disk atmosphere at altitudes exceeding the classical scale height expected in the isothermal hydrostatic limit. We produce ice map images demonstrating the presence of icy dust grains up to altitudes high above the disk midplane, more than three hydrostatic equilibrium scale heights. We demonstrate the presence of a wind containing the carriers of astronomical PAH bands. The wind appears as an X-shaped emission at 3.3, 6.2, 7.7 and 11.3 microns, characteristic wavelengths of the infrared astronomical PAH bands. We associate the spatial distribution of this component with carriers of astronomical PAH bands that form a layer of emission at the interface with the H2 wind. △ Less

Submitted 31 March, 2025; originally announced March 2025.

Comments: Accepted for publication in Astronomy and Astrophysics

Journal ref: A&A 698, A8 (2025)

Class I/II Jets with JWST: Mass loss rates, Asymmetries, and Binary induced Wigglings

Authors: Naman S. Bajaj, Ilaria Pascucci, Tracy L. Beck, Suzan Edwards, Sylvie Cabrit, Joan R. Najita, Kamber Schwarz, Dmitry Semenov, Colette Salyk, Uma Gorti, Sean D. Brittain, Sebastiaan Krijt, Maxime Ruaud, James Muzerolle Page

Abstract: We present JWST NIRSpec spectro-imaging observations of jets from four edge-on protoplanetary disks that exhibit clear signatures of MHD disk winds. Bipolar jets are detected and spatially resolved in over 30 shock-excited forbidden lines, multiple Paschen and Brackett series lines of atomic hydrogen, and the high-energy excitation line of atomic helium (1.083 um). This helium line is the brightes… ▽ More We present JWST NIRSpec spectro-imaging observations of jets from four edge-on protoplanetary disks that exhibit clear signatures of MHD disk winds. Bipolar jets are detected and spatially resolved in over 30 shock-excited forbidden lines, multiple Paschen and Brackett series lines of atomic hydrogen, and the high-energy excitation line of atomic helium (1.083 um). This helium line is the brightest jet-tracer towards HH 30 and FS TauB, which also exhibit asymmetric intensity between their red- and blue-shifted lobes in all tracers, including the [Fe II] and [He I] lines. Extinction maps reveal no significant differences across the lobes, suggesting an asymmetric jet-launching mechanism rather than environmental effects. Diagnostic line ratios yield consistent shock speeds of 50-60 km/s, jet ionization fractions of 0.1-0.2, and pre-shock electron densities of 1000 /cm^3. Combined with pixel-by-pixel electron density maps and [Fe II] line luminosities, we estimate jet mass-loss rates using three independent methods, averaging around a few 10^(-9) solar masses/yr. We estimate the accretion rates for these sources as 10 times the jet mass loss rates and find them to match well with the independently derived accretion estimates of other Class II sources in the Taurus star-forming region. Owing to JWST's high precision, we also investigate jet wiggling and find Tau 042021 to showcase the perfect case of mirror-symmetric wiggling, which can only be explained by the motion of the jet source around a stellar companion. Modeling this wiggling suggests Tau 042021 to host 0.33 and 0.07 solar masses binary at the center with binary separation of 1.35 au and an orbital period of 2.5 years. △ Less

Submitted 30 March, 2025; originally announced March 2025.

Comments: Accepted for publication in the Astronomical Journal. 15 figures and 3 tables

Bridging Paradigms: Designing for HPC-Quantum Convergence

Authors: Amir Shehata, Peter Groszkowski, Thomas Naughton, Murali Gopalakrishnan Meena, Elaine Wong, Daniel Claudino, Rafael Ferreira da Silvaa, Thomas Beck

Abstract: This paper presents a comprehensive software stack architecture for integrating quantum computing (QC) capabilities with High-Performance Computing (HPC) environments. While quantum computers show promise as specialized accelerators for scientific computing, their effective integration with classical HPC systems presents significant technical challenges. We propose a hardware-agnostic software fra… ▽ More This paper presents a comprehensive software stack architecture for integrating quantum computing (QC) capabilities with High-Performance Computing (HPC) environments. While quantum computers show promise as specialized accelerators for scientific computing, their effective integration with classical HPC systems presents significant technical challenges. We propose a hardware-agnostic software framework that supports both current noisy intermediate-scale quantum devices and future fault-tolerant quantum computers, while maintaining compatibility with existing HPC workflows. The architecture includes a quantum gateway interface, standardized APIs for resource management, and robust scheduling mechanisms to handle both simultaneous and interleaved quantum-classical workloads. Key innovations include: (1) a unified resource management system that efficiently coordinates quantum and classical resources, (2) a flexible quantum programming interface that abstracts hardware-specific details, (3) A Quantum Platform Manager API that simplifies the integration of various quantum hardware systems, and (4) a comprehensive tool chain for quantum circuit optimization and execution. We demonstrate our architecture through implementation of quantum-classical algorithms, including the variational quantum linear solver, showcasing the framework's ability to handle complex hybrid workflows while maximizing resource utilization. This work provides a foundational blueprint for integrating QC capabilities into existing HPC infrastructures, addressing critical challenges in resource management, job scheduling, and efficient data movement between classical and quantum resources. △ Less

Submitted 15 July, 2025; v1 submitted 3 March, 2025; originally announced March 2025.

Comments: 14 pages, 14 figures

Journal ref: Future Generation Computer Systems, Volume 174, January 2026, 107980

Puzzling $B(E2;0^+\rightarrow 2^+)$ strength in the proton dripline nucleus $^{36}$Ca

Authors: Z. C. Xu, S. M. Wang, T. Beck, A. Gade, W. Nazarewicz

Abstract: Recent measurements of the $E2$ transition rate from the ground state to the first 2$^+$ excited state of the proton dripline nucleus $^{36}$Ca show an unusual pattern when compared to its isotopic neighbor $^{38}$Ca: despite having a higher $E_x(2_1^+)$ excitation energy, the $B(E2; 0^+_1\rightarrow 2^+_1)$ rate in $^{36}$Ca is larger. The question that naturally arises is to what extent this obs… ▽ More Recent measurements of the $E2$ transition rate from the ground state to the first 2$^+$ excited state of the proton dripline nucleus $^{36}$Ca show an unusual pattern when compared to its isotopic neighbor $^{38}$Ca: despite having a higher $E_x(2_1^+)$ excitation energy, the $B(E2; 0^+_1\rightarrow 2^+_1)$ rate in $^{36}$Ca is larger. The question that naturally arises is to what extent this observation can be attributed to the unbound character of the $2^+_1$ state. To understand the influence of the continuum space on the low-energy properties of $^{36}$Ca, we carried out Gamow shell model calculations that can account for the continuum coupling effects associated with the occupation of unbound $fp$ shells. We found that in the threshold $2^+$ state, $^{36}$Ca is spatially diffused, which impacts the observed $B(E2)$ trend. △ Less

Submitted 16 July, 2025; v1 submitted 19 February, 2025; originally announced February 2025.

Comments: 6 pages, 5 figures

Journal ref: Phys. Rev. C 112, L011302 (2025)

Deviations from the Porter-Thomas Distribution due to Nonstatistical $γ$ Decay below the $^{150}$Nd Neutron Separation Threshold

Authors: O. Papst, J. Isaak, V. Werner, D. Savran, N. Pietralla, G. Battaglia, T. Beck, M. Beuschlein, S. W. Finch, U. Friman-Gayer, K. E. Ide, R. V. F. Janssens, M. D. Jones, J. Kleemann, B. Löher, M. Scheck, M. Spieker, W. Tornow, R. Zidarova, A. Zilges

Abstract: We introduce a new method for the study of fluctuations of partial transition widths based on nuclear resonance fluorescence experiments with quasimonochromatic linearly polarized photon beams below particle separation thresholds. It is based on the average branching of decays of $J=1$ states of an even-even nucleus to the $2^+_1$ state in comparison to the ground state. Between 5 and 7 MeV, a con… ▽ More We introduce a new method for the study of fluctuations of partial transition widths based on nuclear resonance fluorescence experiments with quasimonochromatic linearly polarized photon beams below particle separation thresholds. It is based on the average branching of decays of $J=1$ states of an even-even nucleus to the $2^+_1$ state in comparison to the ground state. Between 5 and 7 MeV, a constant average branching ratio for $γ$ decays from $1^-$ states of 0.490(16) is observed for the nuclide $^{150}$Nd. Assuming $χ^2$-distributed partial transition widths, this average branching ratio is related to a degree of freedom of $ν= 1.93(12)$, rejecting the validity of the Porter-Thomas distribution, requiring $ν=1$. The observed deviation can be explained by nonstatistical effects in the $γ$-decay behavior with contributions in the range of 9.4(10)% up to 94(10)%. △ Less

Submitted 30 July, 2025; v1 submitted 31 January, 2025; originally announced January 2025.

Comments: 7 pages, 2 figures

Journal ref: Phys. Rev. Lett. 135, 052501 (2025)

KU AIGEN ICL EDI@BC8 Track 3: Advancing Phenotype Named Entity Recognition and Normalization for Dysmorphology Physical Examination Reports

Authors: Hajung Kim, Chanhwi Kim, Jiwoong Sohn, Tim Beck, Marek Rei, Sunkyu Kim, T Ian Simpson, Joram M Posma, Antoine Lain, Mujeen Sung, Jaewoo Kang

Abstract: The objective of BioCreative8 Track 3 is to extract phenotypic key medical findings embedded within EHR texts and subsequently normalize these findings to their Human Phenotype Ontology (HPO) terms. However, the presence of diverse surface forms in phenotypic findings makes it challenging to accurately normalize them to the correct HPO terms. To address this challenge, we explored various models f… ▽ More The objective of BioCreative8 Track 3 is to extract phenotypic key medical findings embedded within EHR texts and subsequently normalize these findings to their Human Phenotype Ontology (HPO) terms. However, the presence of diverse surface forms in phenotypic findings makes it challenging to accurately normalize them to the correct HPO terms. To address this challenge, we explored various models for named entity recognition and implemented data augmentation techniques such as synonym marginalization to enhance the normalization step. Our pipeline resulted in an exact extraction and normalization F1 score 2.6\% higher than the mean score of all submissions received in response to the challenge. Furthermore, in terms of the normalization F1 score, our approach surpassed the average performance by 1.9\%. These findings contribute to the advancement of automated medical data extraction and normalization techniques, showcasing potential pathways for future research and application in the biomedical domain. △ Less

Submitted 16 January, 2025; originally announced January 2025.

Comments: This article is part of the Proceedings of the BioCreative VIII Challenge and Workshop: Curation and Evaluation in the era of Generative Models

A Predicted Great Dimming of T Tauri: Has it Begun?

Authors: Tracy L. Beck

Abstract: The optical star in the T Tauri triple system is the prototype of young sun-like stars in our galaxy. This complex and dynamic system has evidence for misaligned disks and outflows, and molecular material in a circumbinary ring that obscures the southern infrared binary, T Tau South. Observations by members of the American Association of Variable Star Observers (AAVSO) show that T Tau North, the o… ▽ More The optical star in the T Tauri triple system is the prototype of young sun-like stars in our galaxy. This complex and dynamic system has evidence for misaligned disks and outflows, and molecular material in a circumbinary ring that obscures the southern infrared binary, T Tau South. Observations by members of the American Association of Variable Star Observers (AAVSO) show that T Tau North, the optical star, has dimmed by up to ~2 magnitudes in the visual over the course of the past decade. The dimming across the B, V, R and I bands has a color character typical of changes in ISM extinction, suggesting an increase in obscuration along the line of sight to T Tau North. Material associated with the circumbinary ring around T Tau South has been predicted to occult the optical star via wide-scale orbital motion of the system. Through analysis of the geometrical configuration and motion of dust structures in the system, it seems that a great dimming of T Tau North by line-of-sight material associated with the T Tau South binary has, in fact, begun. Based on the extent and motion of the circumbinary ring material associated with the southern binary, T Tau North will likely experience dimming events for decades to come and may disappear entirely from the optical sky as the densest mid-plane region of the ring traverses our line of sight. △ Less

Submitted 10 January, 2025; originally announced January 2025.

Comments: Accepted for Publication in the Astronomical Journal

Isolated one-phonon mixed-symmetry 2+ state of the radioactive neutron-rich nuclide 132Te

Authors: T. Stetz, H. Mayr, V. Werner, N. Pietralla, Y. Tsunoda, T. Otsuka, G. Rainovski, T. Beck, R. Borcea, S. Calinescu, C. Costache, I. E. Dinescu, K. E. Ide, A. N. Ionescu, P. Koseoglou, R. Lica, N. Mărginean, R. E. Mihai, C. M. Nickel, C. R. Nita, L. Stan, S. Toma, R. Zidarova

Abstract: The $M1$ transition strengths between excited $2^+$ states of the neutron-rich, radioactive nuclide $^{132}$Te have been studied through direct lifetime measurements using the Doppler-shift attenuation method in a two-neutron transfer reaction on a $^{130}$Te target. An unambiguous identification of the lowest-lying mixed-symmetry $2^+$ state has been achieved on the basis of the large… ▽ More The $M1$ transition strengths between excited $2^+$ states of the neutron-rich, radioactive nuclide $^{132}$Te have been studied through direct lifetime measurements using the Doppler-shift attenuation method in a two-neutron transfer reaction on a $^{130}$Te target. An unambiguous identification of the lowest-lying mixed-symmetry $2^+$ state has been achieved on the basis of the large $B(M1;2^+_2\rightarrow2^+_1$)=0.18(2) $μ_\mathrm{N}^2$ transition strength, in agreement with shell-model calculations. Results are compared to the shell model, and the analysis of both, data and calculations, unambiguously identifies the second-excited $2^+$ state of $^{132}$Te as the one-quadrupole phonon mixed-symmetry state of this isotope. A lowering of the energy and $B(M1;2^+_\mathrm{ms}\rightarrow 2^+_1)$ strength within the $N$=80 isotones toward the $Z$=50 shell closure is observed, which goes alongside with the lowering of the $E2$ collectivity approaching the magic proton shell. △ Less

Submitted 3 September, 2025; v1 submitted 20 December, 2024; originally announced January 2025.

Protoplanetary discs around sun-like stars appear to live longer when the metallicity is low

Authors: Guido De Marchi, Giovanna Giardino, Katia Biazzo, Nino Panagia, Elena Sabbi, Tracy L. Beck, Massimo Robberto, Peter Zeidler, Olivia C. Jones, Margaret Meixner, Katja Fahrion, Nolan Habel, Conor Nally, Alec S. Hirschauer, David R. Soderblom, Omnarayani Nayak, Laura Lenkic, Ciaran Rogers, Bernhard Brandl, Charles D. Keyes

Abstract: Previous Hubble Space Telescope (HST) observations of the star-forming cluster NGC 346 in the Small Magellanic Cloud (SMC) had revealed a large population of pre-main sequence (PMS) candidates, characterised by Halpha excess emission in their photometry. However, without access to spectroscopy, the nature of these objects remained unclear. Using the NIRSpec instrument on board JWST, we studied a s… ▽ More Previous Hubble Space Telescope (HST) observations of the star-forming cluster NGC 346 in the Small Magellanic Cloud (SMC) had revealed a large population of pre-main sequence (PMS) candidates, characterised by Halpha excess emission in their photometry. However, without access to spectroscopy, the nature of these objects remained unclear. Using the NIRSpec instrument on board JWST, we studied a sample of these stars, with masses in the range ~0.9-1.8 Msun, effective temperatures in the range 4,500-8,000 K, and PMS ages between ~0.1 and 30 Myr. Here we present the first spectra of solar-mass PMS stars in the metal-poor SMC (Z=1/8 Zsun) and discuss the physical properties of ten representative sources with good signal-to-noise ratio. The observations indicate that even the oldest of these PMS candidates are still accreting gas with typical rates of ~10^{-8} Msun/yr for stars older than ~10 Myr, confirming their PMS nature. The spectra also reveal near-infrared excess and molecular hydrogen excitation lines consistent with the presence of discs around these stars. These findings suggest that in a low-metallicity environment circumstellar discs can live longer than previously thought. △ Less

Submitted 16 December, 2024; v1 submitted 13 December, 2024; originally announced December 2024.

Comments: 17 pages, 7 figures, to be published in The Astrophysical Journal, Vol 977, Article 214

Journal ref: ApJ, 977 (2024) 214

A joint effort to discover and characterize two resonant mini Neptunes around TOI-1803 with TESS, HARPS-N and CHEOPS

Authors: T. Zingales, L. Malavolta, L. Borsato, D. Turrini, A. Bonfanti, D. Polychroni, G. Mantovan, D. Nardiello, V. Nascimbeni, A. F. Lanza, A. Bekkelien, A. Sozzetti, C. Broeg, L. Naponiello, M. Lendl, A. S. Bonomo, A. E. Simon, S. Desidera, G. Piotto, L. Mancini, M. J. Hooton, A. Bignamini, J. A. Egger, A. Maggio, Y. Alibert , et al. (108 additional authors not shown)

Abstract: We present the discovery of two mini Neptunes near a 2:1 orbital resonance configuration orbiting the K0 star TOI-1803. We describe their orbital architecture in detail and suggest some possible formation and evolution scenarios. Using CHEOPS, TESS, and HARPS-N datasets we can estimate the radius and the mass of both planets. We used a multidimensional Gaussian Process with a quasi-periodic kernel… ▽ More We present the discovery of two mini Neptunes near a 2:1 orbital resonance configuration orbiting the K0 star TOI-1803. We describe their orbital architecture in detail and suggest some possible formation and evolution scenarios. Using CHEOPS, TESS, and HARPS-N datasets we can estimate the radius and the mass of both planets. We used a multidimensional Gaussian Process with a quasi-periodic kernel to disentangle the planetary components from the stellar activity in the HARPS-N dataset. We performed dynamical modeling to explain the orbital configuration and performed planetary formation and evolution simulations. For the least dense planet, we define possible atmospheric characterization scenarios with simulated JWST observations. TOI-1803 b and TOI-1803 c have orbital periods of $\sim$6.3 and $\sim$12.9 days, respectively, residing in close proximity to a 2:1 orbital resonance. Ground-based photometric follow-up observations revealed significant transit timing variations (TTV) with an amplitude of $\sim$10 min and $\sim$40 min, respectively, for planet -b and -c. With the masses computed from the radial velocities data set, we obtained a density of (0.39$\pm$0.10) $ρ_{earth}$ and (0.076$\pm$0.038) $ρ_{earth}$ for planet -b and -c, respectively. TOI-1803 c is among the least dense mini Neptunes currently known, and due to its inflated atmosphere, it is a suitable target for transmission spectroscopy with JWST. We report the discovery of two mini Neptunes close to a 2:1 orbital resonance. The detection of significant TTVs from ground-based photometry opens scenarios for a more precise mass determination. TOI-1803 c is one of the least dense mini Neptune known so far, and it is of great interest among the scientific community since it could constrain our formation scenarios. △ Less

Submitted 6 December, 2024; originally announced December 2024.

Comments: 26 Pages, 21 Figures Accepted for Publication in Astronomy & Astrophysics

Journal ref: A&A 695, A273 (2025)

In-beam $γ$-ray spectroscopy towards the proton dripline: The curious case of $^{32}$Ar

Authors: T. Beck, A. Gade, B. A. Brown, Y. Utsuno, D. Weisshaar, D. Bazin, K. W. Brown, R. J. Charity, P. J. Farris, S. A. Gillespie, A. M. Hill, J. Li, B. Longfellow, W. Reviol, D. Rhodes

Abstract: High-resolution in-beam $γ$-ray spectroscopy was used to study excited states of the neutron-deficient nucleus $^{32}$Ar populated in fast-beam induced four- and six-nucleon removal reactions from $^{36,38}$Ca. One new $γ$-ray transition and indications for an additional two were found, allowing for a glimpse at the level scheme beyond the known $2^+_1$ state. The nature of the new $1900(4)$-keV t… ▽ More High-resolution in-beam $γ$-ray spectroscopy was used to study excited states of the neutron-deficient nucleus $^{32}$Ar populated in fast-beam induced four- and six-nucleon removal reactions from $^{36,38}$Ca. One new $γ$-ray transition and indications for an additional two were found, allowing for a glimpse at the level scheme beyond the known $2^+_1$ state. The nature of the new $1900(4)$-keV transition is discussed in the context of the known energy spectrum of the mirror nucleus $^{32}$Si and shell-model calculations using the FSU and SDPF-M cross-shell effective interactions. Its resulting parent state at $3767(5)$ keV, more than $1.3$ MeV above the proton separation energy, is tentatively assigned to have mixed sd-shell and $2p$-$2h$ character. It might either be the mirror of the $J^π=2^+_2$ state of $^{32}$Si at $4230.8(8)$ keV, but with a decay branch favoring a transition to the $2^+_1$ over the ground state, or the mirror of the $4983.9(11)$-keV state with quantum numbers $0^+$. The resulting mirror-energy differences of $-473(5)$ and $-1218(5)$ keV are both sizable when compared to systematics; in the latter case it would, in fact, be among the largest reported to date in the entire nuclear chart or suggest the potential existence of an additional, hitherto unidentified, low-lying $0^+$ state of $^{32}$Si. △ Less

Submitted 6 December, 2024; originally announced December 2024.

Comments: 8 pages, 3 figures

Consequences of the failure of equipartition for the p-V behavior of liquid water and the hydration free energy components of a small protein

Authors: Dilipkumar N. Asthagiri, Arjun Valiya Parambathu, Thomas L. Beck

Abstract: Earlier we showed that in the molecular dynamics simulation of a rigid model of water it is necessary to use an integration time-step $δt \leq 0.5$ fs to ensure equipartition between translational and rotational modes. Here we extend that study in the $NVT$ ensemble to $NpT$ conditions and to an aqueous protein. We study neat liquid water with the rigid, SPC/E model and the protein BBA (PDB ID: 1F… ▽ More Earlier we showed that in the molecular dynamics simulation of a rigid model of water it is necessary to use an integration time-step $δt \leq 0.5$ fs to ensure equipartition between translational and rotational modes. Here we extend that study in the $NVT$ ensemble to $NpT$ conditions and to an aqueous protein. We study neat liquid water with the rigid, SPC/E model and the protein BBA (PDB ID: 1FME) solvated in the rigid, TIP3P model. We examine integration time-steps ranging from $0.5$ fs to $4.0$ fs for various thermostat plus barostat combinations. We find that a small $δt$ is necessary to ensure consistent prediction of the simulation volume. Hydrogen mass repartitioning alleviates the problem somewhat, but is ineffective for the typical time-step used with this approach. The compressibility, a measure of volume fluctuations, and the dielectric constant, a measure of dipole moment fluctuations, are also seen to be sensitive to $δt$. Using the mean volume estimated from the $NpT$ simulation, we examine the electrostatic and van der Waals contribution to the hydration free energy of the protein in the $NVT$ ensemble. These contributions are also sensitive to $δt$. In going from $δt = 2$ fs to $δt = 0.5$ fs, the change in the net electrostatic plus van der Waals contribution to the hydration of BBA is already in excess of the folding free energy reported for this protein. △ Less

Submitted 28 January, 2025; v1 submitted 4 December, 2024; originally announced December 2024.

Ice inventory towards the protostar Ced 110 IRS4 observed with the James Webb Space Telescope. Results from the ERS Ice Age program

Authors: W. R. M. Rocha, M. K. McClure, J. A. Sturm, T. L. Beck, Z. L. Smith, H. Dickinson, F. Sun, E. Egami, A. C. A. Boogert, H. J. Fraser, E. Dartois, I. Jimenez-Serra, J. A. Noble, J. Bergner, P. Caselli, S. B. Charnley, J. Chiar, L. Chu, I. Cooke, N. Crouzet, E. F. van Dishoeck, M. N. Drozdovskaya, R. Garrod, D. Harsono, S. Ioppolo , et al. (15 additional authors not shown)

Abstract: This work focuses on the ice features toward the binary protostellar system Ced 110 IRS 4A and 4B, and observed with JWST as part of the Early Release Science Ice Age collaboration. We aim to explore the JWST observations of the binary protostellar system Ced~110~IRS4A and IRS4B to unveil and quantify the ice inventories toward these sources. We compare the ice abundances with those found for the… ▽ More This work focuses on the ice features toward the binary protostellar system Ced 110 IRS 4A and 4B, and observed with JWST as part of the Early Release Science Ice Age collaboration. We aim to explore the JWST observations of the binary protostellar system Ced~110~IRS4A and IRS4B to unveil and quantify the ice inventories toward these sources. We compare the ice abundances with those found for the same molecular cloud. The analysis is performed by fitting or comparing laboratory infrared spectra of ices to the observations. Spectral fits are carried out with the ENIIGMA fitting tool that searches for the best fit. For Ced~110~IRS4B, we detected the major ice species H$_2$O, CO, CO$_2$ and NH$_3$. All species are found in a mixture except for CO and CO$_2$, which have both mixed and pure ice components. In the case of Ced~110~IRS4A, we detected the same major species as in Ced~110~IRS4B, as well as the following minor species CH$_4$, SO$_2$, CH$_3$OH, OCN$^-$, NH$_4^+$ and HCOOH. Tentative detection of N$_2$O ice (7.75~$μ$m), forsterite dust (11.2~$μ$m) and CH$_3^+$ gas emission (7.18~$μ$m) in the primary source are also presented. Compared with the two lines of sight toward background stars in the Chameleon I molecular cloud, the protostar has similar ice abundances, except in the case of the ions that are higher in IRS4A. The clearest differences are the absence of the 7.2 and 7.4~$μ$m absorption features due to HCOO$^-$ and icy complex organic molecules in IRS4A and evidence of thermal processing in both IRS4A and IRS4B as probed by the CO$_2$ ice features. We conclude that the binary protostellar system Ced~110~IRS4A and IRS4B has a large inventory of icy species. The similar ice abundances in comparison to the starless regions in the same molecular cloud suggest that the chemical conditions of the protostar were set at earlier stages in the molecular cloud. △ Less

Submitted 29 November, 2024; originally announced November 2024.

Comments: 33 pages, 19 Figures. Accepted for publication in Astronomy & Astrophysics

Journal ref: A&A 693, A288 (2025)

In-beam $γ$-ray spectroscopy of negative-parity states of $^{37}$K populated in dissipative reactions

Authors: T. Beck, A. Gade, B. A. Brown, D. Weisshaar, D. Bazin, K. W. Brown, R. J. Charity, P. J. Farris, S. A. Gillespie, A. M. Hill, J. Li, B. Longfellow, W. Reviol, D. Rhodes

Abstract: In-beam $γ$-ray spectroscopy was used to study excited states of the neutron-deficient nucleus $^{37}$K populated in fast-beam inelastic-scattering and proton-removal reactions at high-momentum loss. New $γ$-ray transitions and $γγ$ coincidence relationships were established using the $γ$-ray tracking array GRETINA. The extension of the level scheme up to the first $(13/2^-)$ state highlights the… ▽ More In-beam $γ$-ray spectroscopy was used to study excited states of the neutron-deficient nucleus $^{37}$K populated in fast-beam inelastic-scattering and proton-removal reactions at high-momentum loss. New $γ$-ray transitions and $γγ$ coincidence relationships were established using the $γ$-ray tracking array GRETINA. The extension of the level scheme up to the first $(13/2^-)$ state highlights the potential of this recently demonstrated population pathway for studies of isospin symmetry involving mirror-energy differences. The nature of the newly identified states is discussed in comparison to shell-model calculations with the FSU cross-shell effective interaction. The calculated occupation numbers of individual orbitals are shown to offer a consistent explanation of the measured mirror-energy differences between $^{37}$K and $^{37}$Ar. △ Less

Submitted 23 November, 2024; originally announced November 2024.

Comments: 8 pages, 6 figures

Journal ref: Phys. Rev. C 110, 014305 (2024)

Architecture of TOI-561 planetary system

Authors: G. Piotto, T. Zingales, L. Borsato, J. A. Egger, A. C. M. Correia, A. E. Simon, H. G. Florén, S. G. Sousa, P. F. L. Maxted, D. Nardiello, L. Malavolta, T. G. Wilson, Y. Alibert, V. Adibekyan, A. Bonfanti, R. Luque, N. C. Santos, M. J. Hooton, L. Fossati, A. M. S. Smith, S. Salmon, G. Lacedelli, R. Alonso, T. Bárczy, D. Barrado Navascues , et al. (68 additional authors not shown)

Abstract: 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… ▽ More 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 $ρ_p = 0.778 \pm 0.097 ρ_{\oplus}$. 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. △ Less

Submitted 31 October, 2024; v1 submitted 23 October, 2024; originally announced October 2024.

Comments: 13 pages, 10 Figures. Accepted on MNRAS. Updated the author list

JWST/NIRSpec Reveals the Nested Morphology of Disk Winds from Young Stars

Authors: Ilaria Pascucci, Tracy L. Beck, Sylvie Cabrit, Naman S. Bajaj, Suzan Edwards, Fabien Louvet, Joan Najita, Bennett N. Skinner, Uma Gorti, Colette Salyk, Sean D. Brittain, Sebastiaan Krijt, James Muzerolle Page, Maxime Ruaud, Kamber Schwarz, Dmitry Semenov, Gaspard Duchene, Marion Villenave

Abstract: Radially extended disk winds could be the key to unlocking how protoplanetary disks accrete and how planets form and migrate. A distinctive characteristic is their nested morphology of velocity and chemistry. Here we report JWST/NIRSpec spectro-imaging of four young stars with edge-on disks in the Taurus star-forming region that demonstrate the ubiquity of this structure. In each source, a fast co… ▽ More Radially extended disk winds could be the key to unlocking how protoplanetary disks accrete and how planets form and migrate. A distinctive characteristic is their nested morphology of velocity and chemistry. Here we report JWST/NIRSpec spectro-imaging of four young stars with edge-on disks in the Taurus star-forming region that demonstrate the ubiquity of this structure. In each source, a fast collimated jet traced by [Fe II] is nested inside a hollow cavity within wider lower-velocity H2 and, in one case, also CO ro-vibrational (v=1-0) emission. Furthermore, in one of our sources, ALMA CO(2-1) emission, paired with our NIRSpec images, reveals the nested wind structure extends further outward. This nested wind morphology strongly supports theoretical predictions for wind-driven accretion and underscores the need for theoretical work to assess the role of winds in the formation and evolution of planetary systems △ Less

Submitted 23 October, 2024; originally announced October 2024.

Comments: This preprint has not undergone peer review or any post-submission improvements or corrections. The Version of Record of this article is published in Nature Astronomy and is available online at https://doi.org/10.1038/s41550-024-02385-7

Llettuce: An Open Source Natural Language Processing Tool for the Translation of Medical Terms into Uniform Clinical Encoding

Authors: James Mitchell-White, Reza Omdivar, Benjamin Partridge, Esmond Urwin, Karthikeyan Sivakumar, Ruizhe Li, Andy Rae, Xiaoyan Wang, Theresia Mina, Tom Giles, Diego Garcia-Gil, Tim Beck, John Chambers, Grazziela Figueredo, Philip R Quinlan

Abstract: This paper introduces Llettuce, an open-source tool designed to address the complexities of converting medical terms into OMOP standard concepts. Unlike existing solutions such as the Athena database search and Usagi, which struggle with semantic nuances and require substantial manual input, Llettuce leverages advanced natural language processing, including large language models and fuzzy matching… ▽ More This paper introduces Llettuce, an open-source tool designed to address the complexities of converting medical terms into OMOP standard concepts. Unlike existing solutions such as the Athena database search and Usagi, which struggle with semantic nuances and require substantial manual input, Llettuce leverages advanced natural language processing, including large language models and fuzzy matching, to automate and enhance the mapping process. Developed with a focus on GDPR compliance, Llettuce can be deployed locally, ensuring data protection while maintaining high performance in converting informal medical terms to standardised concepts. △ Less

Submitted 12 March, 2026; v1 submitted 4 October, 2024; originally announced October 2024.

The K2-24 planetary system revisited by CHEOPS

Authors: V. Nascimbeni, L. Borsato, P. Leonardi, S. G. Sousa, T. G. Wilson, A. Fortier, A. Heitzmann, G. Mantovan, R. Luque, T. Zingales, G. Piotto, Y. Alibert, R. Alonso, T. Bárczy, D. Barrado Navascues, S. C. Barros, W. Baumjohann, T. Beck, W. Benz, N. Billot, F. Biondi, A. Brandeker, C. Broeg, M. -D. Busch, A. Collier Cameron , et al. (60 additional authors not shown)

Abstract: K2-24 is a planetary system composed of two transiting low-density Neptunians locked in an almost perfect 2:1 resonance and showing large TTVs, i.e., an excellent laboratory to search for signatures of planetary migration. Previous studies performed with K2, Spitzer and RV data tentatively claimed a significant non-zero eccentricity for one or both planets, possibly high enough to challenge the sc… ▽ More K2-24 is a planetary system composed of two transiting low-density Neptunians locked in an almost perfect 2:1 resonance and showing large TTVs, i.e., an excellent laboratory to search for signatures of planetary migration. Previous studies performed with K2, Spitzer and RV data tentatively claimed a significant non-zero eccentricity for one or both planets, possibly high enough to challenge the scenario of pure disk migration through resonant capture. With 13 new CHEOPS light curves (seven of planet -b, six of planet -c), we carried out a global photometric and dynamical re-analysis by including all the available literature data as well. We got the most accurate set of planetary parameters to date for the K2-24 system, including radii and masses at 1% and 5% precision (now essentially limited by the uncertainty on stellar parameters) and non-zero eccentricities $e_b=0.0498_{-0.0018}^{+0.0011}$, $e_c=0.0282_{-0.0007}^{+0.0003}$ detected at very high significance for both planets. Such relatively large values imply the need for an additional physical mechanism of eccentricity excitation during or after the migration stage. Also, while the accuracy of the previous TTV model had drifted by up to 0.5 days at the current time, we constrained the orbital solution firmly enough to predict the forthcoming transits for the next ~15 years, thus enabling an efficient follow-up with top-level facilities such as JWST or ESPRESSO. △ Less

Submitted 16 September, 2024; v1 submitted 4 September, 2024; originally announced September 2024.

Comments: 19 pages, 11 figures, 8 tables. Accepted for publication in A&A on September 4, 2024. Typos corrected

Journal ref: A&A 690, A349 (2024)

Integrating Quantum Computing Resources into Scientific HPC Ecosystems

Authors: Thomas Beck, Alessandro Baroni, Ryan Bennink, Gilles Buchs, Eduardo Antonio Coello Perez, Markus Eisenbach, Rafael Ferreira da Silva, Muralikrishnan Gopalakrishnan Meena, Kalyan Gottiparthi, Peter Groszkowski, Travis S. Humble, Ryan Landfield, Ketan Maheshwari, Sarp Oral, Michael A. Sandoval, Amir Shehata, In-Saeng Suh, Christopher Zimmer

Abstract: Quantum Computing (QC) offers significant potential to enhance scientific discovery in fields such as quantum chemistry, optimization, and artificial intelligence. Yet QC faces challenges due to the noisy intermediate-scale quantum era's inherent external noise issues. This paper discusses the integration of QC as a computational accelerator within classical scientific high-performance computing (… ▽ More Quantum Computing (QC) offers significant potential to enhance scientific discovery in fields such as quantum chemistry, optimization, and artificial intelligence. Yet QC faces challenges due to the noisy intermediate-scale quantum era's inherent external noise issues. This paper discusses the integration of QC as a computational accelerator within classical scientific high-performance computing (HPC) systems. By leveraging a broad spectrum of simulators and hardware technologies, we propose a hardware-agnostic framework for augmenting classical HPC with QC capabilities. Drawing on the HPC expertise of the Oak Ridge National Laboratory (ORNL) and the HPC lifecycle management of the Department of Energy (DOE), our approach focuses on the strategic incorporation of QC capabilities and acceleration into existing scientific HPC workflows. This includes detailed analyses, benchmarks, and code optimization driven by the needs of the DOE and ORNL missions. Our comprehensive framework integrates hardware, software, workflows, and user interfaces to foster a synergistic environment for quantum and classical computing research. This paper outlines plans to unlock new computational possibilities, driving forward scientific inquiry and innovation in a wide array of research domains. △ Less

Submitted 28 August, 2024; originally announced August 2024.

Hints of a sulfur-rich atmosphere around the 1.6 R$_{\oplus}$ Super-Earth L98-59 d from JWST NIRSpec G395H transmission spectroscopy

Authors: Amélie Gressier, Néstor Espinoza, Natalie H. Allen, David K. Sing, Agnibha Banerjee, Joanna K. Barstow, Jeff A. Valenti, Nikole K. Lewis, Stephan M. Birkmann, Ryan C. Challener, Elena Manjavacas, Catarina Alves de Oliveira, Nicolas Crouzet, Tracy. L Beck

Abstract: Detecting atmospheres around planets with a radius below 1.6 R$_{\oplus}$, commonly referred to as rocky planets (Rogers_2015, Rogers_2021), has proven to be challenging. However, rocky planets orbiting M-dwarfs are ideal candidates due to their favorable planet-to-star radius ratio. Here, we present one transit observation of the Super-Earth L98-59d (1.58 R$_{\oplus}$, 2.31 M$_{\oplus}$), at the… ▽ More Detecting atmospheres around planets with a radius below 1.6 R$_{\oplus}$, commonly referred to as rocky planets (Rogers_2015, Rogers_2021), has proven to be challenging. However, rocky planets orbiting M-dwarfs are ideal candidates due to their favorable planet-to-star radius ratio. Here, we present one transit observation of the Super-Earth L98-59d (1.58 R$_{\oplus}$, 2.31 M$_{\oplus}$), at the limit of rocky/gas-rich, using the JWST NIRSpec G395H mode covering the 2.8 to 5.1 microns wavelength range. The extracted transit spectrum from a single transit observation deviates from a flat line by 2.6 to 5.6$σ$, depending on the data reduction and retrieval setup. The hints of an atmospheric detection are driven by a large absorption feature between 3.3 to 4.8 microns. A stellar contamination retrieval analysis rejected the source of this feature as being due to stellar inhomogeneities, making the best fit an atmospheric model including sulfur-bearing species, suggesting that the atmosphere of L98-59d may not be at equilibrium. This result will need to be confirmed by the analysis of the second NIRSpec G395H visit in addition to the NIRISS SOSS transit observation. △ Less

Submitted 28 August, 2024; originally announced August 2024.

Comments: Accepted for publication in the Astrophysical Journal Letters (ApJL), August 25, 2024

Properties of outer solar system pebbles during planetesimal formation from meteor observations

Authors: Peter Jenniskens, Paul R. Estrada, Stuart Pilorz, Peter S. Gural, Dave Samuels, Steve Rau, Timothy M. C. Abbott, Jim Albers, Scott Austin, Dan Avner, Jack W. Baggaley, Tim Beck, Solvay Blomquist, Mustafa Boyukata, Martin Breukers, Walt Cooney, Tim Cooper, Marcelo De Cicco, Hadrien Devillepoix, Eric Egland, Elize Fahl, Megan Gialluca, Bryant Grigsby, Toni Hanke, Barbara Harris , et al. (20 additional authors not shown)

Abstract: In the late stages of accretion leading up to the formation of planetesimals, particles grew to pebbles the size of 1-mm to tens of cm. That is the same size range that dominates the present-day comet mass loss. Meteoroids that size cause visible meteors on Earth. Here, we hypothesize that the size distribution and the physical and chemical properties of young meteoroid streams still contain infor… ▽ More In the late stages of accretion leading up to the formation of planetesimals, particles grew to pebbles the size of 1-mm to tens of cm. That is the same size range that dominates the present-day comet mass loss. Meteoroids that size cause visible meteors on Earth. Here, we hypothesize that the size distribution and the physical and chemical properties of young meteoroid streams still contain information about the conditions in the solar nebula during these late stages of accretion. From observations of 47 young meteor showers, we find that freshly ejected meteoroids from long-period comets tend to have low bulk density and are distributed with equal surface area per log-mass interval (magnitude distribution index chi ~ 1.85), suggesting gentle accretion conditions. Jupiter-family comets, on the other hand, mostly produce meteoroids twice as dense and distributed with a steeper chi ~ 2.15 or even chi ~ 2.5, which implies that those pebbles grew from particles fragmenting in a collisional cascade or by catastrophic collisions, respectively. Both comet populations contain an admixture of compact materials that are sometimes sodium-poor, but Jupiter-family comets show a higher percentage (~8% on average) than long-period comet showers (~4%), and a wider range. While there are exceptions in both groups, the implication is that most long-period comets formed under gentle particle growth conditions, possibly near the 30 AU edge of the Trans Neptunian Disk, while most Jupiter family comets formed closer to the Sun where pebbles reached or passed the fragmentation barrier. This is possible if the Scattered Disk represents all objects scattered by Neptune during its migration, while the present-day outer Oort cloud formed only during and after the Sun had moved away from sibling stars. △ Less

Submitted 21 August, 2024; originally announced August 2024.

Comments: 82 pages, 14 figures, 3 tables

MSC Class: 85

Journal ref: Icarus, 2024

TOI-757 b: an eccentric transiting mini-Neptune on a 17.5-d orbit

Authors: A. Alqasim, N. Grieves, N. M. Rosário, D. Gandolfi, J. H. Livingston, S. Sousa, K. A. Collins, J. K. Teske, M. Fridlund, J. A. Egger, J. Cabrera, C. Hellier, A. F. Lanza, V. Van Eylen, F. Bouchy, R. J. Oelkers, G. Srdoc, S. Shectman, M. Günther, E. Goffo, T. Wilson, L. M. Serrano, A. Brandeker, S. X. Wang, A. Heitzmann , et al. (107 additional authors not shown)

Abstract: We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-day orbit transiting a bright star ($V = 9.7$ mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry wi… ▽ More We report the spectroscopic confirmation and fundamental properties of TOI-757 b, a mini-Neptune on a 17.5-day orbit transiting a bright star ($V = 9.7$ mag) discovered by the TESS mission. We acquired high-precision radial velocity measurements with the HARPS, ESPRESSO, and PFS spectrographs to confirm the planet detection and determine its mass. We also acquired space-borne transit photometry with the CHEOPS space telescope to place stronger constraints on the planet radius, supported with ground-based LCOGT photometry. WASP and KELT photometry were used to help constrain the stellar rotation period. We also determined the fundamental parameters of the host star. We find that TOI-757 b has a radius of $R_{\mathrm{p}} = 2.5 \pm 0.1 R_{\oplus}$ and a mass of $M_{\mathrm{p}} = 10.5^{+2.2}_{-2.1} M_{\oplus}$, implying a bulk density of $ρ_{\text{p}} = 3.6 \pm 0.8$ g cm$^{-3}$. Our internal composition modeling was unable to constrain the composition of TOI-757 b, highlighting the importance of atmospheric observations for the system. We also find the planet to be highly eccentric with $e$ = 0.39$^{+0.08}_{-0.07}$, making it one of the very few highly eccentric planets among precisely characterized mini-Neptunes. Based on comparisons to other similar eccentric systems, we find a likely scenario for TOI-757 b's formation to be high eccentricity migration due to a distant outer companion. We additionally propose the possibility of a more intrinsic explanation for the high eccentricity due to star-star interactions during the earlier epoch of the Galactic disk formation, given the low metallicity and older age of TOI-757. △ Less

Submitted 29 July, 2024; originally announced July 2024.

Comments: Accepted for publication in MNRAS; 26 pages, 14 figures, 6 tables

Two-phase problems: Perron solutions and regularity of the Neumann problem in convex cones

Authors: Thomas Beck, Daniela De Silva, Ovidiu Savin

Abstract: We investigate a fully nonlinear two-phase free boundary problem with a Neumann boundary condition on the boundary of a general convex set $K \subset \mathbb{R}^n$ with corners. We show that the interior regularity theory developed by Caffarelli for the classical two-phase problem in his pioneer works \cite{C1,C2}, can be extended up to the boundary for the Neumann boundary condition under very mi… ▽ More We investigate a fully nonlinear two-phase free boundary problem with a Neumann boundary condition on the boundary of a general convex set $K \subset \mathbb{R}^n$ with corners. We show that the interior regularity theory developed by Caffarelli for the classical two-phase problem in his pioneer works \cite{C1,C2}, can be extended up to the boundary for the Neumann boundary condition under very mild regularity assumptions on the convex domain $K$. To start, we establish a general existence theorem for the Dirichlet two-phase problem driven by two different fully nonlinear operators, which is a result of independent interest. △ Less

Submitted 28 July, 2024; originally announced July 2024.

Observation of Aerosolization-induced Morphological Changes in Viral Capsids

Authors: Abhishek Mall, Anna Munke, Zhou Shen, Parichita Mazumder, Johan Bielecki, Juncheng E, Armando Estillore, Chan Kim, Romain Letrun, Jannik Lübke, Safi Rafie-Zinedine, Adam Round, Ekaterina Round, Michael Rütten, Amit K. Samanta, Abhisakh Sarma, Tokushi Sato, Florian Schulz, Carolin Seuring, Tamme Wollweber, Lena Worbs, Patrik Vagovic, Richard Bean, Adrian P. Mancuso, Ne-Te Duane Loh , et al. (5 additional authors not shown)

Abstract: Single-stranded RNA viruses co-assemble their capsid with the genome and variations in capsid structures can have significant functional relevance. In particular, viruses need to respond to a dehydrating environment to prevent genomic degradation and remain active upon rehydration. Theoretical work has predicted low-energy buckling transitions in icosahedral capsids which could protect the virus f… ▽ More Single-stranded RNA viruses co-assemble their capsid with the genome and variations in capsid structures can have significant functional relevance. In particular, viruses need to respond to a dehydrating environment to prevent genomic degradation and remain active upon rehydration. Theoretical work has predicted low-energy buckling transitions in icosahedral capsids which could protect the virus from further dehydration. However, there has been no direct experimental evidence, nor molecular mechanism, for such behaviour. Here we observe this transition using X-ray single particle imaging of MS2 bacteriophages after aerosolization. Using a combination of machine learning tools, we classify hundreds of thousands of single particle diffraction patterns to learn the structural landscape of the capsid morphology as a function of time spent in the aerosol phase. We found a previously unreported compact conformation as well as intermediate structures which suggest an incoherent buckling transition which does not preserve icosahedral symmetry. Finally, we propose a mechanism of this buckling, where a single 19-residue loop is destabilised, leading to the large observed morphology change. Our results provide experimental evidence for a mechanism by which viral capsids protect themselves from dehydration. In the process, these findings also demonstrate the power of single particle X-ray imaging and machine learning methods in studying biomolecular structural dynamics. △ Less

Submitted 16 July, 2024; originally announced July 2024.

Comments: 10 pages, 4 figures plus 9 pages supplementary information

Characterisation of the Warm-Jupiter TOI-1130 system with CHEOPS and photo-dynamical approach

Authors: L. Borsato, D. Degen, A. Leleu, M. J. Hooton, J. A. Egger, A. Bekkelien, A. Brandeker, A. Collier Cameron, M. N. Günther, V. Nascimbeni, C. M. Persson, A. Bonfanti, T. G. Wilson, A. C. M. Correia, T. Zingales, T. Guillot, A. H. M. J. Triaud, G. Piotto, D. Gandolfi, L. Abe, Y. Alibert, R. Alonso, T. Bárczy, D. Barrado Navascues, S. C. C. Barros , et al. (71 additional authors not shown)

Abstract: Among the thousands of exoplanets discovered to date, approximately a few hundred gas giants on short-period orbits are classified as "lonely" and only a few are in a multi-planet system with a smaller companion on a close orbit. The processes that formed multi-planet systems hosting gas giants on close orbits are poorly understood, and only a few examples of this kind of system have been observed… ▽ More Among the thousands of exoplanets discovered to date, approximately a few hundred gas giants on short-period orbits are classified as "lonely" and only a few are in a multi-planet system with a smaller companion on a close orbit. The processes that formed multi-planet systems hosting gas giants on close orbits are poorly understood, and only a few examples of this kind of system have been observed and well characterised. Within the contest of multi-planet system hosting gas-giant on short orbits, we characterise TOI-1130 system by measuring masses and orbital parameters. This is a 2-transiting planet system with a Jupiter-like planet (c) on a 8.35 days orbit and a Neptune-like planet (b) on an inner (4.07 days) orbit. Both planets show strong anti-correlated transit timing variations (TTVs). Furthermore, radial velocity (RV) analysis showed an additional linear trend, a possible hint of a non-transiting candidate planet on a far outer orbit. Since 2019, extensive transit and radial velocity observations of the TOI-1130 have been acquired using TESS and various ground-based facilities. We present a new photo-dynamical analysis of all available transit and RV data, with the addition of new CHEOPS and ASTEP+ data that achieve the best precision to date on the planetary radii and masses and on the timings of each transit. We were able to model interior structure of planet b constraining the presence of a gaseous envelope of H/He, while it was not possible to assess the possible water content. Furthermore, we analysed the resonant state of the two transiting planets, and we found that they lie just outside the resonant region. This could be the result of the tidal evolution that the system underwent. We obtained both masses of the planets with a precision less than 1.5%, and radii with a precision of about 1% and 3% for planet b and c, respectively. △ Less

Submitted 8 July, 2024; originally announced July 2024.

Comments: 22 pages, 10 figures, Accepted for publication by Astronomy and Astrophysics

Journal ref: A&A 689, A52 (2024)

Gamma decay of the $^{154}$Sm Isovector Giant Dipole Resonance: Smekal-Raman Scattering as a Novel Probe of Nuclear Ground-State Deformation

Authors: J. Kleemann, N. Pietralla, U. Friman-Gayer, J. Isaak, O. Papst, K. Prifti, V. Werner, A. D. Ayangeakaa, T. Beck, G. Colò, M. L. Cortés, S. W. Finch, M. Fulghieri, D. Gribble, K. E. Ide, X. K. -H. James, R. V. F. Janssens, S. R. Johnson, P. Koseoglou, Krishichayan, D. Savran, W. Tornow

Abstract: Gamma decays of the isovector giant dipole resonance (GDR) of the deformed nucleus $^{154}$Sm from $2^+_1$-Smekal-Raman and elastic scattering were measured using linearly polarized, quasimonochromatic photon beams. The two scattering processes were disentangled through their distinct angular distributions. Their branching ratio and cross sections were determined at six excitation energies coverin… ▽ More Gamma decays of the isovector giant dipole resonance (GDR) of the deformed nucleus $^{154}$Sm from $2^+_1$-Smekal-Raman and elastic scattering were measured using linearly polarized, quasimonochromatic photon beams. The two scattering processes were disentangled through their distinct angular distributions. Their branching ratio and cross sections were determined at six excitation energies covering the $^{154}$Sm GDR. Both agree with the predictions of the geometrical model for the GDR and establish $γ$ decay as an observable sensitive to the structure of the resonance. Consequently, the data place strong constraints on the nuclear shape, including the degree of triaxiality. The derived $^{154}$Sm shape parameters $β=0.2926(26)$ and $γ=5.0(14)$ agree well with other measurements and recent Monte Carlo Shell-Model calculations. △ Less

Submitted 20 January, 2025; v1 submitted 28 June, 2024; originally announced June 2024.

Comments: 7 pages, 3 figures, 3 tables

Journal ref: Phys. Rev. Lett. 134, 022503 (2025)

CHEOPS in-flight performance: A comprehensive look at the first 3.5 years of operations

Authors: A. Fortier, A. E. Simon, C. Broeg, G. Olofsson, A. Deline, T. G. Wilson, P. F. L. Maxted, A. Brandeker, A. Collier Cameron, M. Beck, A. Bekkelien, N. Billot, A. Bonfanti, G. Bruno, J. Cabrera, L. Delrez, B. -O. Demory, D. Futyan, H. -G. Florén, M. N. Günther, A. Heitzmann, S. Hoyer, K. G. Isaak, S. G. Sousa, M. Stalport , et al. (106 additional authors not shown)

Abstract: CHEOPS is a space telescope specifically designed to monitor transiting exoplanets orbiting bright stars. In September 2023, CHEOPS completed its nominal mission and remains in excellent operational conditions. The mission has been extended until the end of 2026. Scientific and instrumental data have been collected throughout in-orbit commissioning and nominal operations, enabling a comprehensive… ▽ More CHEOPS is a space telescope specifically designed to monitor transiting exoplanets orbiting bright stars. In September 2023, CHEOPS completed its nominal mission and remains in excellent operational conditions. The mission has been extended until the end of 2026. Scientific and instrumental data have been collected throughout in-orbit commissioning and nominal operations, enabling a comprehensive analysis of the mission's performance. In this article, we present the results of this analysis with a twofold goal. First, we aim to inform the scientific community about the present status of the mission and what can be expected as the instrument ages. Secondly, we intend for this publication to serve as a legacy document for future missions, providing insights and lessons learned from the successful operation of CHEOPS. To evaluate the instrument performance in flight, we developed a comprehensive monitoring and characterisation programme. It consists of dedicated observations that allow us to characterise the instrument's response. In addition to the standard collection of nominal science and housekeeping data, these observations provide input for detecting, modelling, and correcting instrument systematics, discovering and addressing anomalies, and comparing the instrument's actual performance with expectations. The precision of the CHEOPS measurements has enabled the mission objectives to be met and exceeded. Careful modelling of the instrumental systematics allows the data quality to be significantly improved during the light curve analysis phase, resulting in more precise scientific measurements. CHEOPS is compliant with the driving scientific requirements of the mission. Although visible, the ageing of the instrument has not affected the mission's performance. △ Less

Submitted 3 June, 2024; originally announced June 2024.

Comments: Accepted for publication in Astronomy and Astrophysics

HIP 41378 observed by CHEOPS: Where is planet d?

Authors: S. Sulis, L. Borsato, S. Grouffal, H. P. Osborn, A. Santerne, A. Brandeker, M. N. Günther, A. Heitzmann, M. Lendl, M. Fridlund, D. Gandolfi, Y. Alibert, R. Alonso, T. Bárczy, D. Barrado Navascues, S. C. Barros, W. Baumjohann, T. Beck, W. Benz, M. Bergomi, N. Billot, A. Bonfanti, C. Broeg, A. Collier Cameron, C. Corral van Damme , et al. (62 additional authors not shown)

Abstract: HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter-McLaughlin effect, $P_\mathrm{d} = 278.36$ d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on $P_\mathrm{d}= 278.36$ d, but th… ▽ More HIP 41378 d is a long-period planet that has only been observed to transit twice, three years apart, with K2. According to stability considerations and a partial detection of the Rossiter-McLaughlin effect, $P_\mathrm{d} = 278.36$ d has been determined to be the most likely orbital period. We targeted HIP 41378 d with CHEOPS at the predicted transit timing based on $P_\mathrm{d}= 278.36$ d, but the observations show no transit. We find that large ($>22.4$ hours) transit timing variations (TTVs) could explain this non-detection during the CHEOPS observation window. We also investigated the possibility of an incorrect orbital solution, which would have major implications for our knowledge of this system. If $P_\mathrm{d} \neq 278.36$ d, the periods that minimize the eccentricity would be $101.22$ d and $371.14$ d. The shortest orbital period will be tested by TESS, which will observe HIP 41378 in Sector 88 starting in January 2025. Our study shows the importance of a mission like CHEOPS, which today is the only mission able to make long observations (i.e., from space) to track the ephemeris of long-period planets possibly affected by large TTVs. △ Less

Submitted 30 May, 2024; originally announced May 2024.

Comments: Accepted for publication in Astronomy and Astrophysics

Journal ref: A&A 686, L18 (2024)

Photo-dynamical characterisation of the TOI-178 resonant chain

Authors: A. Leleu, J. -B. Delisle, L. Delrez, E. M. Bryant, A. Brandeker, H. P. Osborn, N. Hara, T. G. Wilson, N. Billot, M. Lendl, D. Ehrenreich, H. Chakraborty, M. N. Günther, M. J. Hooton, Y. Alibert, R. Alonso, D. R. Alves, D. R. Anderson, I. Apergis, D. Armstrong, T. Bárczy, D. Barrado Navascues, S. C. C. Barros, M. P. Battley, W. Baumjohann , et al. (82 additional authors not shown)

Abstract: The TOI-178 system consists of a nearby late K-dwarf transited by six planets in the super-Earth to mini-Neptune regime, with radii ranging from 1.2 to 2.9 earth radius and orbital periods between 1.9 and 20.7 days. All planets but the innermost one form a chain of Laplace resonances. The fine-tuning and fragility of such orbital configurations ensure that no significant scattering or collision ev… ▽ More The TOI-178 system consists of a nearby late K-dwarf transited by six planets in the super-Earth to mini-Neptune regime, with radii ranging from 1.2 to 2.9 earth radius and orbital periods between 1.9 and 20.7 days. All planets but the innermost one form a chain of Laplace resonances. The fine-tuning and fragility of such orbital configurations ensure that no significant scattering or collision event has taken place since the formation and migration of the planets in the protoplanetary disc, hence providing important anchors for planet formation models. We aim to improve the characterisation of the architecture of this key system, and in particular the masses and radii of its planets. In addition, since this system is one of the few resonant chains that can be characterised by both photometry and radial velocities, we aim to use it as a test bench for the robustness of the planetary mass determination with each technique. We perform a global analysis of all available photometry and radial velocity. We also try different sets of priors on the masses and eccentricity, as well as different stellar activity models, to study their effects on the masses estimated by each method. We show how stellar activity is preventing us from obtaining a robust mass estimation for the three outer planets using radial velocity data alone. We also show that our joint photo-dynamical and radial velocity analysis resulted in a robust mass determination for planets c to g, with precision of 12% for the mass of planet c, and better than 10% for planets d to g. The new precisions on the radii range from 2 to 3%. The understanding of this synergy between photometric and radial velocity measurements will be valuable during the PLATO mission. We also show that TOI-178 is indeed currently locked in the resonant configuration, librating around an equilibrium of the chain. △ Less

Submitted 22 May, 2024; originally announced May 2024.

Journal ref: A&A 688, A211 (2024)

A warm Neptune's methane reveals core mass and vigorous atmospheric mixing

Authors: David K. Sing, Zafar Rustamkulov, Daniel P. Thorngren, Joanna K. Barstow, Pascal Tremblin, Catarina Alves de Oliveira, Tracy L. Beck, Stephan M. Birkmann, Ryan C. Challener, Nicolas Crouzet, Néstor Espinoza, Pierre Ferruit, Giovanna Giardino, Amélie Gressier, Elspeth K. H. Lee, Nikole K. Lewis, Roberto Maiolino, Elena Manjavacas, Bernard J. Rauscher, Marco Sirianni, Jeff A. Valenti

Abstract: Observations of transiting gas giant exoplanets have revealed a pervasive depletion of methane, which has only recently been identified atmospherically. The depletion is thought to be maintained by disequilibrium processes such as photochemistry or mixing from a hotter interior. However, the interiors are largely unconstrained along with the vertical mixing strength and only upper limits on the CH… ▽ More Observations of transiting gas giant exoplanets have revealed a pervasive depletion of methane, which has only recently been identified atmospherically. The depletion is thought to be maintained by disequilibrium processes such as photochemistry or mixing from a hotter interior. However, the interiors are largely unconstrained along with the vertical mixing strength and only upper limits on the CH$_4$ depletion have been available. The warm Neptune WASP-107 b stands out among exoplanets with an unusually low density, reported low core mass, and temperatures amenable to CH$_4$ though previous observations have yet to find the molecule. Here we present a JWST NIRSpec transmission spectrum of WASP-107 b which shows features from both SO$_2$ and CH$_4$ along with H$_2$O, CO$_2$, and CO. We detect methane with 4.2$σ$ significance at an abundance of 1.0$\pm$0.5 ppm, which is depleted by 3 orders of magnitude relative to equilibrium expectations. Our results are highly constraining for the atmosphere and interior, which indicate the envelope has a super-solar metallicity of 43$\pm$8$\times$ solar, a hot interior with an intrinsic temperature of T$_{\rm int}$=460$\pm$40 K, and vigorous vertical mixing which depletes CH4 with a diffusion coefficient of Kzz = 10$^{11.6\pm0.1}$ cm$^2$/s. Photochemistry has a negligible effect on the CH$_4$ abundance, but is needed to account for the SO$_2$. We infer a core mass of 11.5$_{-3.6}^{+3.0}$ M$_{\odot}$, which is much higher than previous upper limits, releasing a tension with core-accretion models. △ Less

Submitted 17 May, 2024; originally announced May 2024.

Comments: Published in Nature at this URL, https://www.nature.com/articles/s41586-024-07395-z . This is the authors version of the manuscript, 20 pages including Methods. Data from Figs. 1, 2, and 3 are available at this URL, https://doi.org/10.5281/zenodo.10891400

Characterisation of the TOI-421 planetary system using CHEOPS, TESS, and archival radial velocity data

Authors: A. F. Krenn, D. Kubyshkina, L. Fossati, J. A. Egger, A. Bonfanti, A. Deline, D. Ehrenreich, M. Beck, W. Benz, J. Cabrera, T. G. Wilson, A. Leleu, S. G. Sousa, V. Adibekyan, A. C. M. Correira, Y. Alibert, L. Delrez, M. Lendl, J. A. Patel, J. Venturini, R. Alonso, G. Anglada, J. Asquier, T. Bárczy, D. Barrado Navascues , et al. (66 additional authors not shown)

Abstract: The TOI-421 planetary system contains two sub-Neptune-type planets and is a prime target to study the formation and evolution of planets and their atmospheres. The inner planet is especially interesting as the existence of a hydrogen-dominated atmosphere at its orbital separation cannot be explained by current formation models without previous orbital migration. We jointly analysed photometric dat… ▽ More The TOI-421 planetary system contains two sub-Neptune-type planets and is a prime target to study the formation and evolution of planets and their atmospheres. The inner planet is especially interesting as the existence of a hydrogen-dominated atmosphere at its orbital separation cannot be explained by current formation models without previous orbital migration. We jointly analysed photometric data of three TESS sectors and six CHEOPS visits as well as 156 radial velocity data points to retrieve improved planetary parameters. We also searched for TTVs and modelled the interior structure of the planets. Finally, we simulated the evolution of the primordial H-He atmospheres of the planets using two different modelling frameworks. We determine the planetary radii and masses of TOI-421 b and c to be $R_{\rm b} = 2.64 \pm 0.08 \, R_{\oplus}$, $M_{\rm b} = 6.7 \pm 0.6 \, M_{\oplus}$, $R_{\rm c} = 5.09 \pm 0.07 \, R_{\oplus}$, and $M_{\rm c} = 14.1 \pm 1.4 \, M_{\oplus}$. We do not detect any statistically significant TTV signals. Assuming the presence of a hydrogen-dominated atmosphere, the interior structure modelling results in both planets having extensive envelopes. While the modelling of the atmospheric evolution predicts for TOI-421 b to have lost any primordial atmosphere that it could have accreted at its current orbital position, TOI-421 c could have started out with an initial atmospheric mass fraction somewhere between 10 and 35%. We conclude that the low observed mean density of TOI-421 b can only be explained by either a bias in the measured planetary parameters (e.g. driven by high-altitude clouds) and/or in the context of orbital migration. We also find that the results of atmospheric evolution models are strongly dependent on the employed planetary structure model. △ Less

Submitted 17 April, 2024; originally announced April 2024.

Comments: 21 pages, 12 figures, accepted for publication in A&A

Growing a nuclear star cluster from star formation and cluster mergers: The JWST NIRSpec view of NGC 4654

Authors: Katja Fahrion, Torsten Böker, Michele Perna, Tracy L. Beck, Roberto Maiolino, Santiago Arribas, Andrew J. Bunker, Stephane Charlot, Matteo Ceci, Giovanni Cresci, Guido De Marchi, Nora Lützgendorf, Lorenzo Ulivi

Abstract: We present a detailed study of the centre of NGC4654, a Milky Way-like spiral galaxy in the Virgo cluster that has been reported to host a double stellar nucleus, thus promising a rare view of ongoing star cluster infall into a galaxy nucleus. Analysing JWST NIRSpec integral-field spectroscopic data and Hubble Space Telescope imaging of the inner 330 $\times$ 330 pc, we find that the nucleus harbo… ▽ More We present a detailed study of the centre of NGC4654, a Milky Way-like spiral galaxy in the Virgo cluster that has been reported to host a double stellar nucleus, thus promising a rare view of ongoing star cluster infall into a galaxy nucleus. Analysing JWST NIRSpec integral-field spectroscopic data and Hubble Space Telescope imaging of the inner 330 $\times$ 330 pc, we find that the nucleus harbours in fact three massive star clusters. Maps of infrared emission lines from NIRSpec show different morphologies for the ionised and molecular gas components. The emission from molecular hydrogen gas is concentrated at the NSC location, while emission from hydrogen recombination lines is more extended beyond the central cluster. The velocity fields of both gas and stars indicate that the three clusters are part of a complicated dynamical system, with the NSC having an elevated velocity dispersion in line with its high stellar mass. To investigate the stellar populations of the three clusters in more detail, we use surface brightness modelling to measure their fluxes from ultraviolet to mid-infrared wavelengths and fit their spectral energy distributions (SEDs). Two of the clusters are UV-bright and well described by single stellar populations with young ages ($\sim$ 3 and 5 Myr) and low masses ($M_\ast \sim 4 \times 10^{4} - 10^{5} M_\odot$), whereas the central cluster is much more massive ($3 \times 10^7 M_\odot$), and cannot be fitted by a single stellar population. Instead, we find that a minor young population ($\sim$ 1 Myr) embedded in a dominant old population ($\sim$ 8 Gyr) is needed to explain its SED. Given its complex composition and the close proximity of two young star clusters that are likely to merge with it within a few hundred million years, we consider NGC4654 a unique laboratory to study NSC growth from both in-situ star formation and the infall of star clusters. △ Less

Submitted 13 April, 2024; originally announced April 2024.

Comments: Main text: 13 pages, 8 figures, accepted for publication in A&A

Journal ref: A&A 687, A83 (2024)

Optical tools for laser machining along six orders of magnitude

Authors: Julian Hellstern, Christoph Tillkorn, Tim Hieronymus, Myriam Kaiser, Torsten Beck, Daniel Flamm

Abstract: We present an overview on the development and characterization of multiscale laser processing optics for versatile material modifications across more than six orders of magnitude. Starting with solutions for micromachining we present high-NA microscope objectives creating sub-wavelength material modifications on macroscopic scales with highest peak intensities. Moving on to the millimeter range, t… ▽ More We present an overview on the development and characterization of multiscale laser processing optics for versatile material modifications across more than six orders of magnitude. Starting with solutions for micromachining we present high-NA microscope objectives creating sub-wavelength material modifications on macroscopic scales with highest peak intensities. Moving on to the millimeter range, the adaptability and scalability of scanning optics is examined for large-area machining. Finally, we explore line beam optics in the meter range, evaluating their use in uniform material processing using average powers above 100kW. This study provides an insight into the design and performance characteristics of such optics and demonstrates their potential in advanced laser processing. △ Less

Submitted 28 March, 2024; originally announced March 2024.

Comments: Review article with 12 pages, 15 figures and 74 references

Journal ref: Proc. SPIE 12878, High-Power Laser Materials Processing: Applications, Diagnostics, and Systems XIII, 1287802 (12 March 2024)

Detailed cool star flare morphology with CHEOPS and TESS

Authors: G. Bruno, I. Pagano, G. Scandariato, H. -G. Florén, A. Brandeker, G. Olofsson, P. F. L. Maxted, A. Fortier, S. G. Sousa, S. Sulis, V. Van Grootel, Z. Garai, A. Boldog, L. Kriskovics, M. Gy. Szabó, D. Gandolfi, Y. Alibert, R. Alonso, T. Bárczy, D. Barrado Navascues, S. C. C. Barros, W. Baumjohann, M. Beck, T. Beck, W. Benz , et al. (57 additional authors not shown)

Abstract: Context. White-light stellar flares are proxies for some of the most energetic types of flares, but their triggering mechanism is still poorly understood. As they are associated with strong X and UV emission, their study is particularly relevant to estimate the amount of high-energy irradiation onto the atmospheres of exoplanets, especially those in their stars' habitable zone. Aims. We used the h… ▽ More Context. White-light stellar flares are proxies for some of the most energetic types of flares, but their triggering mechanism is still poorly understood. As they are associated with strong X and UV emission, their study is particularly relevant to estimate the amount of high-energy irradiation onto the atmospheres of exoplanets, especially those in their stars' habitable zone. Aims. We used the high-cadence, high-photometric capabilities of the CHEOPS and TESS space telescopes to study the detailed morphology of white-light flares occurring in a sample of 130 late-K and M stars, and compared our findings with results obtained at a lower cadence. We developed dedicated software for this purpose. Results. Multi-peak flares represent a significant percentage ($\gtrsim 30$\%) of the detected outburst events. Our findings suggest that high-impulse flares are more frequent than suspected from lower-cadence data, so that the most impactful flux levels that hit close-in exoplanets might be more time-limited than expected. We found significant differences in the duration distributions of single-peak and complex flare components, but not in their peak luminosity. A statistical analysis of the flare parameter distributions provides marginal support for their description with a log-normal instead of a power-law function, leaving the door open to several flare formation scenarios. We tentatively confirmed previous results about quasi-periodic pulsations in high-cadence photometry, report the possible detection of a pre-flare dip, and did not find hints of photometric variability due to an undetected flare background. Conclusions. The high-cadence study of stellar hosts might be crucial to evaluate the impact of their flares on close-in exoplanets, as their impulsive phase emission might otherwise be incorrectly estimated. Future telescopes such as PLATO and Ariel will help in this respect. △ Less

Submitted 25 March, 2024; originally announced March 2024.

Comments: 28 pages, 25 figures, 4 tables, to be published in Astronomy & Astrophysics

Precise characterisation of HD 15337 with CHEOPS: a laboratory for planet formation and evolution

Authors: N. M. Rosário, O. D. S. Demangeon, S. C. C. Barros, D. Gandolfi, J. A. Egger, L. M. Serrano, H. P. Osborn, M. Beck, W. Benz, H. -G. Florén, P. Guterman, T. G. Wilson, Y. Alibert, L. Fossati, M. J. Hooton, L. Delrez, N. C. Santos, S. G. Sousa, A. Bonfanti, S. Salmon, V. Adibekyan, A. Nigioni, J. Venturini, R. Alonso, G. Anglada , et al. (68 additional authors not shown)

Abstract: We aim to constrain the internal structure and composition of HD 15337 b and c, two short-period planets situated on opposite sides of the radius valley, using new transit photometry and radial velocity data. We acquire 6 new transit visits with the CHaracterising ExOPlanet Satellite (CHEOPS) and 32 new radial velocity measurements from the High Accuracy Radial Velocity Planet Searcher (HARPS) to… ▽ More We aim to constrain the internal structure and composition of HD 15337 b and c, two short-period planets situated on opposite sides of the radius valley, using new transit photometry and radial velocity data. We acquire 6 new transit visits with the CHaracterising ExOPlanet Satellite (CHEOPS) and 32 new radial velocity measurements from the High Accuracy Radial Velocity Planet Searcher (HARPS) to improve the accuracy of the mass and radius estimates for both planets. We reanalyse light curves from TESS sectors 3 and 4 and analyse new data from sector 30, correcting for long-term stellar activity. Subsequently, we perform a joint fit of the TESS and CHEOPS light curves, and all available RV data from HARPS and the Planet Finder Spectrograph (PFS). Our model fits the planetary signals, the stellar activity signal and the instrumental decorrelation model for the CHEOPS data simultaneously. The stellar activity was modelled using a Gaussian-process regression on both the RV and activity indicators. We finally employ a Bayesian retrieval code to determine the internal composition and structure of the planets. We derive updated and highly precise parameters for the HD 15337 system. Our improved precision on the planetary parameters makes HD 15337 b one of the most precisely characterised rocky exoplanets, with radius and mass measurements achieving a precision better than 2\% and 7\%, respectively. We are able to improve the precision of the radius measurement of HD 15337 c to 3\%. Our results imply that the composition of HD 15337 b is predominantly rocky, while HD 15337 c exhibits a gas envelope with a mass of at least $0.01\ M_\oplus$.Our results lay the groundwork for future studies, which can further unravel the atmospheric evolution of these exoplanets and give new insights into their composition and formation history and the causes behind the radius gap. △ Less

Submitted 25 March, 2024; originally announced March 2024.

Comments: 17 pages, including appendix

Journal ref: A&A 686, A282 (2024)