@article{19796, abstract = {Motivation: Boolean networks are popular dynamical models of cellular processes in systems biology. Their attractors model phenotypes that arise from the interplay of key regulatory subcircuits. A succession diagram (SD) describes this interplay in a discrete analog of Waddington’s epigenetic attractor landscape that allows for fast identification of attractors and attractor control strategies. Efficient computational tools for studying SDs are essential for the understanding of Boolean attractor landscapes and connecting them to their biological functions. Results: We present a new approach to SD construction for asynchronously updated Boolean networks, implemented in the biologist’s Boolean attractor landscape mapper, biobalm. We compare biobalm to similar tools and find a substantial performance increase in SD construction, attractor identification, and attractor control. We perform the most comprehensive comparative analysis to date of the SD structure in experimentally-validated Boolean models of cell processes and random ensembles. We find that random models (including critical Kauffman networks) have relatively small SDs, indicating simple decision structures. In contrast, nonrandom models from the literature are enriched in extremely large SDs, indicating an abundance of decision points and suggesting the presence of complex Waddington landscapes in nature. Availability and implementation: The tool biobalm is available online at https://github.com/jcrozum/biobalm. Further data, scripts for testing, analysis, and figure generation are available online at https://github.com/jcrozum/biobalm-analysis and in the reproducibility artefact at https://doi.org/10.5281/zenodo.13854760.}, author = {Trinh, Van Giang and Park, Kyu Hyong and Pastva, Samuel and Rozum, Jordan C.}, issn = {1367-4811}, journal = {Bioinformatics}, number = {5}, publisher = {Oxford University Press}, title = {{Mapping the attractor landscape of Boolean networks with biobalm}}, doi = {10.1093/bioinformatics/btaf280}, volume = {41}, year = {2025}, } @article{19797, abstract = {Stars stripped of their hydrogen-rich envelopes through binary interaction are thought to be responsible for both hydrogen-poor supernovae and the hard ionizing radiation observed in low-Z galaxies. A population of these stars was recently observed for the first time, but their prevalence remains unknown. In preparation for such measurements, we estimate the mass distribution of hot, stripped stars using a population synthesis code that interpolates over detailed single and binary stellar evolution tracks. We predict that for a constant star formation rate of 1 M⊙/yr and regardless of metallicity, a scalable model population contains ∼30 000 stripped stars with mass Mstrip > 1 M⊙ and ∼4000 stripped stars that are sufficiently massive to explode (Mstrip > 2.6 M⊙). Below Mstrip = 5 M⊙, the distribution is metallicity-independent and can be described by a power law with the exponent α ∼ −2. At higher masses and lower metallicity (Z ≲ 0.002), the mass distribution exhibits a drop. This originates from the prediction, frequently seen in evolutionary models, that massive low-metallicity stars do not expand substantially until central helium burning or later and therefore cannot form long-lived stripped stars. With weaker line-driven winds at low metallicity, this suggests that neither binary interaction nor wind mass loss can efficiently strip massive stars at low metallicity. As a result, a “helium-star desert” emerges around Mstrip = 15 M⊙ at Z = 0.002, covering an increasingly large mass range with decreasing metallicity. We note that these high-mass stars are those that potentially boost a galaxy’s He+-ionizing radiation and that participate in the formation of merging black holes. This “helium-star desert” therefore merits further study.}, author = {Hovis-Afflerbach, B. and Götberg, Ylva Louise Linsdotter and Schootemeijer, A. and Klencki, J. and Strom, A. L. and Ludwig, B. A. and Drout, M. R.}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{The mass distribution of stars stripped in binaries: The effect of metallicity}}, doi = {10.1051/0004-6361/202453185}, volume = {697}, year = {2025}, } @article{19798, abstract = {In an n×n array filled with symbols, a transversal is a collection of entries with distinct rows, columns and symbols. In this note we show that if no symbol appears more than βn times, the array contains a transversal of size (1−β/4−o(1))n . In particular, if the array is filled with n symbols, each appearing n times (an equi- n square), we get transversals of size (3/4−o(1))n. Moreover, our proof gives a deterministic algorithm with polynomial running time, that finds these transversals.}, author = {Anastos, Michael and Morris, Patrick}, issn = {1520-6610}, journal = {Journal of Combinatorial Designs}, number = {9}, pages = {338--342}, publisher = {Wiley}, title = {{A note on finding large transversals efficiently}}, doi = {10.1002/jcd.21990}, volume = {33}, year = {2025}, } @article{19833, abstract = {Eigenstates of quantum many-body systems are often used to define phases of matter in and out of equilibrium; however, experimentally accessing highly excited eigenstates is a challenging task, calling for alternative strategies to dynamically probe nonequilibrium phases. In this work, we characterize the dynamical properties of a disordered spin chain, focusing on the spin-glass regime. Using tensor-network simulations, we observe oscillatory behavior of local expectation values and bipartite entanglement entropy. We explain these oscillations deep in the many-body localized spin-glass regime via a simple theoretical model. From perturbation theory, we predict the timescales up to which our analytical description is valid and confirm it with numerical simulations. Finally, we study the correlation length dynamics, which, after a long-time plateau, resume growing in line with renormalization group (RG) expectations. Our work suggests that RG predictions can be quantitatively tested against numerical simulations and experiments, potentially enabling microscopic descriptions of dynamical phases in large systems.}, author = {Brighi, Pietro and Ljubotina, Marko and Serbyn, Maksym}, issn = {2469-9969}, journal = {Physical Review B}, number = {22}, publisher = {American Physical Society}, title = {{Probing the many-body localized spin-glass phase through quench dynamics}}, doi = {10.1103/9fms-ygfz}, volume = {111}, year = {2025}, } @article{19839, abstract = {The snow and glaciers of the Peruvian Andes provide vital water supplies in a region facing water scarcity and substantial glacier change. However, there remains a lack of understanding of snow processes and quantification of the contribution of melt to runoff. Here we apply a distributed glacio-hydrological model over the Rio Santa basin to disentangle the role of the cryosphere in the Andean water cycle. Only at the highest elevations (>5000 m a.s.l.) is the snow cover continuous; at lower elevations, the snowpack is thin and ephemeral, with rapid cycles of snowfall and melt. Due to the large catchment area affected by ephemeral snow, its contribution to catchment inputs is substantial (23% and 38% in the wet and dry season, respectively). Ice melt is crucial in the mid-dry season (up to 44% of inputs). Our results improve estimates of water fluxes and call for further process-based modelling across the Andes.}, author = {Fyffe, Catriona Louise and Potter, Emily and Miles, Evan and Shaw, Thomas and Mccarthy, Michael and Orr, Andrew and Loarte, Edwin and Medina, Katy and Fatichi, Simone and Hellström, Rob and Baraer, Michel and Mateo, Emilio and Cochachin, Alejo and Westoby, Matthew and Pellicciotti, Francesca}, issn = {2662-4435}, journal = {Communications Earth and Environment}, publisher = {Springer Nature}, title = {{Thin and ephemeral snow shapes melt and runoff dynamics in the Peruvian Andes}}, doi = {10.1038/s43247-025-02379-x}, volume = {6}, year = {2025}, } @article{19840, abstract = {We report the discovery of two new magnetic cataclysmic variables with brown dwarf companions and long orbital periods (P_{\rm orb}=95\pm1 and 104\pm2 min). This discovery increases the sample of candidate magnetic period bouncers with confirmed sub-stellar donors from four to six. We also find their X-ray luminosity from archival XMM–Newton observations to be in the range L_{\rm X}\approx10^{28}-10^{29} \mathrm{erg\,s^{-1}} in the 0.25–10 keV band. This low luminosity is comparable with the other candidates, and at least an order of magnitude lower than the X-ray luminosities typically measured in cataclysmic variables. The X-ray fluxes imply mass transfer rates that are much lower than predicted by evolutionary models, even if some of the discrepancy is due to the accretion energy being emitted in other bands, such as via cyclotron emission at infrared wavelengths. Although it is possible that some or all of these systems formed directly as binaries containing a brown dwarf, it is likely that the donor used to be a low-mass star and that the systems followed the evolutionary track for cataclysmic variables, evolving past the period bounce. The donor in long period systems is expected to be a low-mass, cold brown dwarf. This hypothesis is supported by near-infrared photometric observations that constrain the donors in the two systems to be brown dwarfs cooler than 1100 K (spectral types T5 or later), most likely losing mass via Roche Lobe overflow or winds. The serendipitous discovery of two magnetic period bouncers in the small footprint of the XMM–Newton catalogue implies a large space density of these type of systems, possibly compatible with the prediction of 40–70 per cent of magnetic cataclysmic variables to be period bouncers.}, author = {Cunningham, Tim and Caiazzo, Ilaria and Sienkiewicz, Gracjan and Wheatley, Peter J. and Gänsicke, Boris T. and El-Badry, Kareem and Arcodia, Riccardo and Charbonneau, David and Connor, Liam and De, Kishalay and Hakala, Pasi and Kenyon, Scott J. and Maheshwari, Sumit Kumar and Rodriguez, Antonio C. and Van Roestel, Jan and Tremblay, Pier Emmanuel}, issn = {1365-2966}, journal = {Monthly Notices of the Royal Astronomical Society}, number = {1}, pages = {633--649}, publisher = {Oxford University Press}, title = {{Discovery of two new polars evolved past the period bounce}}, doi = {10.1093/mnras/staf561}, volume = {540}, year = {2025}, } @article{19841, abstract = {Context. The blue supergiant (BSG) domain contains a large variety of stars whose past and future evolutionary paths are still highly uncertain. Since binary interaction plays a crucial role in the fate of massive stars, investigating the multiplicity among BSGs helps shed light on the fate of such objects. Aims. We aim to estimate the binary fraction of a large sample of BSGs in the Small Magellanic Cloud (SMC) within the Binarity at LOw Metallicity (BLOeM) survey. In total, we selected 262 targets with spectral types B0-B3 and luminosity classes I-II. Methods. This work is based on spectroscopic data collected by the FLAMES instrument, mounted on the Very Large Telescope, which gathered nine epochs over three months. Our spectroscopic analysis for each target includes the individual and peak-to-peak radial velocity measurements, an investigation of the line profile variability, and a periodogram analysis to search for possible short- and long-period binaries. Results. By applying a 20 km s−1 threshold on the peak-to-peak radial velocities above which we would consider the star to be binary, the resulting observed spectroscopic binary fraction for our BSG sample is 23 ± 3%. An independent analysis of line profile variability reveals 11 (plus 5 candidates) double-lined spectroscopic binaries and 32 (plus 41 candidates) single-lined spectroscopic binaries. Based on these results, we estimated the overall observed binary fraction in this sample to be 34 ± 3%, which is close to the computed intrinsic binary fraction of 40 ± 4%. In addition, we derived reliable orbital periods for 41 spectroscopic binaries and potential binary candidates, among which there are 17 eclipsing binaries, including 20 SB1 and SB2 systems with periods of less than 10 days. We reported a significant drop in the binary fraction of BSGs with spectral types later than B2 and effective temperatures less than 18 kK, which could indicate the end of the main sequence phase in this temperature regime. We found no metallicity dependence in the binary fraction of BSGs, compared to existing spectroscopic surveys of the Galaxy and Large Magellanic Cloud.}, author = {Britavskiy, N. and Mahy, L. and Lennon, D. J. and Patrick, L. R. and Sana, H. and Villaseñor, J. I. and Shenar, T. and Bodensteiner, J. and Bernini-Peron, M. and Berlanas, S. R. and Bowman, D. M. and Crowther, P. A. and De Mink, S. E. and Evans, C. J. and Götberg, Ylva Louise Linsdotter and Holgado, G. and Johnston, C. and Keszthelyi, Z. and Klencki, J. and Langer, N. and Mandel, I. and Menon, A. and Moe, M. and Oskinova, L. M. and Pauli, D. and Pawlak, M. and Ramachandran, V. and Renzo, M. and Sander, A. A.C. and Schneider, F. R.N. and Schootemeijer, A. and Sen, K. and Simón-Díaz, S. and Van Loon, J. T. and Vink, J. S.}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{Binarity at LOw Metallicity (BLOeM): Multiplicity of early B-type supergiants in the Small Magellanic Cloud}}, doi = {10.1051/0004-6361/202452963}, volume = {698}, year = {2025}, } @article{19842, abstract = {Given the uncertain evolutionary status of blue supergiant stars, their multiplicity properties hold vital clues to better understand their origin and evolution. As part of The Binarity at LOw Metallicity (BLOeM) campaign in the Small Magellanic Cloud, we present a multi-epoch spectroscopic survey of 128 supergiant stars of spectral type B5–F5, which roughly correspond to initial masses in the 6–30 M⊙ range. The observed binary fraction for the B5–9 supergiants is 25 ± 6% (10 ± 4%) and 5 ± 2% (0%) for the A–F stars, which were found using a radial-velocity (RV) variability threshold of 5 km s−1 (10 km s−1) as a criterion for binarity. Accounting for observational biases, we find an intrinsic multiplicity fraction of less than 18% for the B5–9 stars and 8−7+9% for the AF stars, for the orbital periods up to 103.5 days and mass ratios (q) in the 0.1 < q < 1 range. The large stellar radii of these supergiant stars prevent short orbital periods, but we demonstrate that this effect alone cannot explain our results. We assessed the spectra and RV time series of the detected binary systems and find that only a small fraction display convincing solutions. We conclude that the multiplicity fractions are compromised by intrinsic stellar variability, such that the true multiplicity fraction may be significantly smaller. Our main conclusions from comparing the multiplicity properties of the B5–9- and AF-type supergiants to that of their less evolved counterparts is that such stars cannot be explained by a direct evolution from the main sequence. Furthermore, by comparing their multiplicity properties to red supergiant stars, we conclude that the AF supergiant stars are neither progenitors nor descendants of red supergiants.}, author = {Patrick, L. R. and Lennon, D. J. and Najarro, F. and Shenar, T. and Bodensteiner, J. and Sana, H. and Crowther, P. A. and Britavskiy, N. and Langer, N. and Schootemeijer, A. and Evans, C. J. and Mahy, L. and Götberg, Ylva Louise Linsdotter and De Mink, S. E. and Schneider, F. R.N. and O’Grady, A. J.G. and Villaseñor, J. I. and Bernini-Peron, M. and Bowman, D. M. and De Koter, A. and Deshmukh, K. and Gilkis, A. and González-Torà, G. and Kalari, V. M. and K̃Eszthelyi, Z. and Mandel, I. and Menon, A. and Moe, M. and Oskinova, L. M. and Pauli, D. and Renzo, M. and Sander, A. A.C. and Sen, K. and Stoop, M. and Van Loon, J. T. and Toonen, S. and Tramper, F. and Vink, J. S. and Wang, C.}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{Binarity at LOw Metallicity (BLOeM): The multiplicity properties and evolution of BAF-type supergiants}}, doi = {10.1051/0004-6361/202452949}, volume = {698}, year = {2025}, } @article{19843, abstract = {Social dilemmas are collective-action problems where individual interests are at odds with group interests. Such dilemmas occur frequently at all scales of human interactions. When dealing with collective-action problems, people often act reciprocally. They adjust their behavior to match the previous behavior of the recipient. The literature distinguishes two kinds of reciprocity. According to direct reciprocity, individuals react to their immediate experiences with the recipient. They are more likely to cooperate if the recipient previously cooperated with them. According to indirect reciprocity, individuals react to the recipient’s general behavior, irrespectively of whether or not they benefited directly. In practice, the two kinds of reciprocity are often intertwined; people typically base their decisions on both direct experiences and indirect observations. Yet only recently have researchers begun to explore how the two kinds of reciprocity interact. So far, this research only addresses a single type of social dilemma, the donation game, where the effects of individual behaviors are independent. Instead, here we allow for all pairwise social dilemmas. By applying novel techniques to generalize the theory of zero-determinant strategies, we establish an important proof of principle: In all social dilemmas, socially optimal outcomes can be sustained as an equilibrium, using either direct or indirect reciprocity, or arbitrary mixtures thereof. These results neither require games to be repeated infinitely often, nor that individual opinions are synchronized. In this way, we considerably generalize the scope of models of reciprocity, and we build further bridges between the literatures on direct and indirect reciprocity.}, author = {Hübner, Valentin and Schmid, Laura and Hilbe, Christian and Chatterjee, Krishnendu}, issn = {2752-6542}, journal = {PNAS Nexus}, number = {5}, publisher = {Oxford University Press}, title = {{Stable strategies of direct and indirect reciprocity across all social dilemmas}}, doi = {10.1093/pnasnexus/pgaf154}, volume = {4}, year = {2025}, } @article{19844, abstract = {Context. Rapidly rotating classical OBe stars have been proposed as the products of binary interactions, and the fraction of Be stars with compact companions implies that at least some are. However, to constrain the interaction physics spinning up the OBe stars, a large sample of homogeneously analyzed OBe stars with well-determined binary characteristics and orbital parameters are required. Aims. We investigated the multiplicity properties of a sample of 18 Oe, 62 Be, and two Of?p stars observed within the BLOeM survey in the Small Magellanic Cloud. We analyzed the first nine epochs of spectroscopic observations obtained over approximately three months in 2023. Methods. Radial velocities (RVs) of all stars were measured using cross-correlation based on different sets of absorption and emission lines. Applying commonly used binarity criteria, we classified objects as binaries, binary candidates, and apparently single (RV stable) objects. We further inspected the spectra for double-lined spectroscopic binaries and cross-matched with catalogs of X-ray sources and photometric binaries. Results. We classify 14 OBe stars as binaries, and an additional 11 as binary candidates. The two Of?p stars are apparently single. We find two more objects that are most likely currently interacting binaries. Without those, the observed binary fraction for the remaining OBe sample of 78 stars is fobs+candOBe = 0.18 ± 0.04 (fobs+candOBe = 0.32±0.05 including candidates). This binary fraction is less than half of that measured for OB stars in BLOeM. Combined with the lower fraction of SB2s, this suggests that OBe stars do indeed have fundamentally different present-day binary properties than OB stars. We find no evidence for OBe binaries with massive compact companions, in contrast to expectations from binary population synthesis. Conclusions. Our results support the binary scenario as an important formation channel for OBe stars, as post-interaction binaries may have been disrupted or the stripped companions of OBe stars are harder to detect. Further observations are required to characterize the detected binaries, their orbital parameters, and the nature of their companions.}, author = {Bodensteiner, J. and Shenar, T. and Sana, H. and Britavskiy, N. and Crowther, P. A. and Langer, N. and Lennon, D. J. and Mahy, L. and Patrick, L. R. and Villaseñor, J. I. and Abdul-Masih, M. and Bowman, D. M. and De Koter, A. and De Mink, S. E. and Deshmukh, K. and Fabry, M. and Gilkis, A. and Götberg, Ylva Louise Linsdotter and Holgado, G. and Izzard, R. G. and Janssens, S. and Kalari, V. M. and Keszthelyi, Z. and Kubát, J. and Mandel, I. and Maravelias, G. and Oskinova, L. M. and Pauli, D. and Ramachandran, V. and Rocha, D. F. and Renzo, M. and Sander, A. A.C. and Schneider, F. R.N. and Schootemeijer, A. and Sen, K. and Stoop, M. and Toonen, S. and Van Loon, J. T. and Valli, R. and Vigna-Gómez, A. and Vink, J. S. and Wang, C. and Xu, X. T.}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{Binarity at LOw Metallicity (BLOeM): Multiplicity properties of Oe and Be stars}}, doi = {10.1051/0004-6361/202452623}, volume = {698}, year = {2025}, } @article{19845, abstract = {Context. The recently launched James Webb Space Telescope (JWST) is opening new observing windows on the distant Universe. Among JWST’s instruments, the Mid Infrared Instrument (MIRI) offers the unique capability of imaging observations at wavelengths of λ > 5 μm. This enables unique access to the rest frame near-infrared (NIR, λ ≥ 1 μm) emission from galaxies at redshifts of z > 4 and the visual (λ ≳ 5000 Å) rest frame for z > 9. We report here on the guaranteed time observations (GTO), from the MIRI European Consortium, of the Hubble Ultra Deep Field (HUDF), forming the MIRI Deep Imaging Survey (MIDIS), consisting of an on source integration time of ∼41 hours in the MIRI/F560W (5.6 μm) filter. The F560W filter was selected since it would produce the deepest data in terms of AB magnitudes in a given time. To our knowledge, this constitutes the longest single filter exposure obtained with JWST of an extragalactic field as of yet. Aims. The HUDF is one of the most observed extragalactic fields, with extensive multi-wavelength coverage, where (before JWST) galaxies up to z ∼ 7 have been confirmed, and at z > 10 suggested, from HST photometry. We aim to characterise the galaxy population in HUDF at 5.6 μm, enabling studies such as: the rest frame NIR morphologies for galaxies at z ≲ 4.6, probing mature stellar populations and emission lines in z > 6 sources, intrinsically red and dusty galaxies, and active galactic nuclei (AGNs) and their host galaxies at intermediate redshifts. Methods. We reduced the MIRI data using the official JWST pipeline, augmented by in-house custom scripts. We measured the noise characteristics of the resulting image. Galaxy photometry was obtained, and photometric redshifts were estimated for sources with available multi-wavelength photometry (and compared to spectroscopic redshifts when available). Results. Over the deepest part of our image, the 5σ point source limit is 28.65 mag AB (12.6 nJy), ∼0.35 mag better than predicted by the JWST exposure time calculator. We find ∼2500 sources, the overwhelming majority of which are distant galaxies, but we note that spurious sources likely remain at faint magnitudes due to imperfect cosmic ray rejection in the JWST pipeline. More than 500 galaxies with available spectroscopic redshifts, up to z ≈ 11, have been identified, the majority of which are at z < 6. More than 1000 galaxies have reliable photometric redshift estimates, of which ∼25 are at 6 < z < 12. The point spread function in the F560W filter has a full width at half maximum (FWHM) of ≈0.2″ (corresponding to 1.4 kpc at z = 4), allowing the NIR rest frame morphologies and stellar mass distributions to be resolved for z < 4.5. Moreover, > 100 objects with very red NIRCam vs MIRI (3.6–5.6 μm > 1 mag) colours have been found, suggestive of dusty or old stellar populations at high redshifts. Conclusions. We conclude that MIDIS surpasses preflight expectations and that deep MIRI imaging has great potential to characterise the galaxy population from cosmic noon to dawn.}, author = {Östlin, Göran and Pérez-González, Pablo G. and Melinder, Jens and Gillman, Steven and Iani, Edoardo and Costantin, Luca and Boogaard, Leindert A. and Rinaldi, Pierluigi and Colina, Luis and Nørgaard-Nielsen, Hans Ulrik and Dicken, Daniel and Greve, Thomas R. and Wright, Gillian and Alonso-Herrero, Almudena and Álvarez-Márquez, Javier and Annunziatella, Marianna and Bik, Arjan and Bosman, Sarah E.I. and Caputi, Karina I. and Gomez, Alejandro Crespo and Eckart, Andreas and Garcia-Marin, Macarena and Hjorth, Jens and Ilbert, Olivier and Jermann, Iris and Kendrew, Sarah and Labiano, Alvaro and Langeroodi, Danial and Le Fevre, Olivier and Libralato, Mattia and Meyer, Romain A. and Moutard, Thibaud and Peissker, Florian and Pye, John P. and Tikkanen, Tuomo V. and Topinka, Martin and Walter, Fabian and Ward, Martin and Van Der Werf, Paul and Van Dishoeck, Ewine F. and Güdel, Manuel and Henning, Thomas and Lagage, Pierre Olivier and Ray, Tom P. and Vandenbussche, Bart}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{MIRI Deep Imaging Survey (MIDIS) of the Hubble Ultra Deep Field: Survey description and early results for the galaxy population detected at 5.6 µm}}, doi = {10.1051/0004-6361/202451723}, volume = {696}, year = {2025}, } @article{19846, abstract = {The Ca2+-release-activated Ca2+ (CRAC) channel Orai1 is activated by interaction with the Ca2+ sensor Stromal Interaction Molecule 1 (STIM1). Owing to the lack of structurally resolved Orai1/STIM1 complexes, the impact of their coupling on individual Orai1 transmembrane domain (TM) movements is unclear. This study investigates STIM1-independent and STIM1-dependent Orai1-TM dynamics using photocrosslinking unnatural amino acids (UAAs) at each individual TM position. We primarily identify CRAC-channel-like currents directly after UAA incorporation or additional UV-light irradiation at TM3 sites that interface with non-pore-lining TMs. Using UAAs combined with conventional site-directed mutagenesis and molecular dynamics simulations, we discover that pore opening involves a widening of interfaces formed by TM3 with non-pore-lining TMs. Orai1 mutants with a UAA in TM3 exhibit weaker STIM1-induced activation after UV exposure, possibly caused by a restricted widening of non-pore-lining TM interfaces. We demonstrate that photocrosslinking UAAs are excellent tools for improving our understanding of key determinants and ion channel dynamics modulating pore opening.}, author = {Najjar, Hadil and Weiß, Sarah and Horvath, Ferdinand and Hopl, Valentina and Tiffner, Adéla and Höbarth, Lorenz and Söllner, Julia and Fröhlich, Maximilian and Prantl, Magdalena and Müller, Nora and Nazarenko, Yuliia and Harant, Selina and Weissenböck, Lukas and Grabmayr, Herwig and Sallinger, Matthias and Maltan, Lena and Echefu, Linda V. and Radiskovic, Tamara and Leopold, Melanie and Lindinger, Sonja and Humer, Christina and Höglinger, Carmen and Krobath, Heinrich and Renger, Thomas and Derler, Isabella}, issn = {2666-3864}, journal = {Cell Reports Physical Science}, number = {6}, publisher = {Elsevier}, title = {{STIM1-induced widening of non-pore-lining TM interfaces is crucial for Orai1 pore opening}}, doi = {10.1016/j.xcrp.2025.102623}, volume = {6}, year = {2025}, } @article{19847, abstract = {Prussian blue (PB) and Prussian blue analogues (PBAs) are a class of porous materials composed of transition metal cations, cyanide ligands, and alkali metal cations. Their ability to intercalate and deintercalate ions within their framework pores, coupled with the adaptability of their crystal structure to electrochemical changes, underpins their success in battery applications. PBAs with Fe or Co as the active site exhibit high redox potentials (vs SHE) and have been extensively explored as cathode materials, with well-documented chemistry, crystal structures, and electrochemical properties. In contrast, PBAs with Cr or Mn as the active site display lower redox potentials and remain significantly underexplored as anode materials. This gap has led to fewer reported compounds and a less comprehensive understanding of their structural and electrochemical behavior, leaving the field relatively opaque. In this perspective, we comprehensively analyze the challenges involved in producing and employing PBAs with low redox potentials as active battery materials. Conversely, we propose numerous horizons and ask fundamental questions that should pave the way for future research to advance the field.}, author = {Palacios Corella, Mario and Echevarría, Igor and Santana Santos, Carla and Schuhmann, Wolfgang and Ventosa, Edgar and Ibáñez, Maria}, issn = {1520-5002}, journal = {Chemistry of Materials}, number = {12}, pages = {4203--4226}, publisher = {American Chemical Society}, title = {{Prussian blue analogues as anode materials for battery applications: Complexities and horizons}}, doi = {10.1021/acs.chemmater.5c00213}, volume = {37}, year = {2025}, } @article{19848, abstract = {Binding precedents (súmulas vinculantes) constitute a juridical instrument unique to the Brazilian legal system and whose objectives include the protection of the Federal Supreme Court against repetitive demands. Studies of the effectiveness of these instruments in decreasing the Court’s exposure to similar cases, however, indicate that they tend to fail in such a direction, with some of the binding precedents seemingly creating new demands. We empirically assess the legal impact of five binding precedents, 11, 14, 17, 26, and 37, at the highest Court level through their effects on the legal subjects they address. This analysis is only possible through the comparison of the Court’s ruling about the precedents’ themes before they are created, which means that these decisions should be detected through techniques of Similar Case Retrieval, which we tackle from the angle of Case Classification. The contributions of this article are therefore twofold: on the mathematical side, we compare the use of different methods of Natural Language Processing — TF-IDF, LSTM, Longformer, and regex — for Case Classification, whereas on the legal side, we contrast the inefficiency of these binding precedents with a set of hypotheses that may justify their repeated usage. We observe that the TF-IDF models performed slightly better than LSTM and Longformer when compared through common metrics; however, the deep learning models were able to detect certain important legal events that TF-IDF missed. On the legal side, we argue that the reasons for binding precedents to fail in responding to repetitive demand are heterogeneous and case-dependent, making it impossible to single out a specific cause. We identify five main hypotheses, which are found in different combinations in each of the precedents studied.}, author = {Tinarrage, Raphaël and Ennes, Henrique and Resck, Lucas and Gomes, Lucas T. and Ponciano, Jean R. and Poco, Jorge}, issn = {1572-8382}, journal = {Artificial Intelligence and Law}, publisher = {Springer Nature}, title = {{Empirical analysis of binding precedent efficiency in Brazilian Supreme Court via case classification}}, doi = {10.1007/s10506-025-09458-6}, year = {2025}, } @article{19852, abstract = {Technology involving hybrid superconductor–semiconductor materials is a promising avenue for engineering quantum devices for information storage, manipulation, and transmission. Proximity-induced superconducting correlations are an essential part of such devices. While the proximity effect in the conduction band of common semiconductors is well understood, its manifestation in confined hole gases, realized for instance in germanium, is an active area of research. Lower-dimensional hole-based systems, particularly in germanium, are emerging as an attractive platform for a variety of solid-state quantum devices, due to their combination of efficient spin and charge control and long coherence times. The recent experimental realization of the proximity effect in germanium thus calls for a theoretical description that is tailored to hole gases. In this work, we propose a simple model to describe proximity-induced superconductivity in two-dimensional hole gases, incorporating both the heavy-hole (HH) and light-hole (LH) bands. We start from the Luttinger–Kohn model, introduce three parameters that characterize hopping across the superconductor–semiconductor interface, and derive explicit intraband and interband effective pairing terms for the HH and LH bands. Unlike previous approaches, our theory provides a quantitative relationship between induced pairings and interface properties. Restricting our general model to an experimentally relevant case where only the HH band crosses the chemical potential, we predict the coexistence of 𝑠-wave and 𝑑-wave singlet pairings, along with triplet-type pairings, and modified Zeeman and Rashba spin–orbit couplings. Our results thus present a starting point for theoretical modeling of quantum devices based on proximitized hole gases, fueling further progress in quantum technology.}, author = {Babkin, Serafim and Joecker, Benjamin and Flensberg, Karsten and Serbyn, Maksym and Danon, Jeroen}, issn = {2469-9969}, journal = {Physical Review B}, number = {21}, publisher = {American Physical Society}, title = {{Superconducting proximity effect in two-dimensional hole gases}}, doi = {10.1103/k4jh-pnxy}, volume = {111}, year = {2025}, } @phdthesis{19853, abstract = {The internal dynamical properties of red giant stars have been explored extensively in recent years as a result of the increase in high precision data availability from the space missions Kepler and TESS (Transiting Exoplanet Survey Satellite), and in this exploration, it has been discovered that some of these stars are not behaving as expected. Red giants are stars that have evolved off of the main sequence after having completed fusing hydrogen into helium in their core. Observational data shows that the cores are rotating significantly slower than models can recreate consistently across evolutionary stages. This discrepancy has prompted investigation into the efficiency of angular momentum transport mechanisms and mixing processes including meridional circulation, shear instability, internal gravity waves, Tayler-Spruit dynamo, fossil magnetic fields etc., to explain this behavior. Analyzing seismic oscillations in stars, via asteroseismology, is a powerful tool as it is the only way in which the deep stellar interior can be probed and subsequently characterized; this is possible as global oscillations modulating the stellar surface are effected by internal processes. For red giants, p-modes (pressure modes; resonating through the entire star) and g-modes (gravity-modes; resonating in the radiative interior) couple to create mixed modes. These mixed modes give access to the otherwise hidden stellar interior as g-modes couple to p-modes, delivering information from the interior to the surface. Internal magnetic signatures have been observationally confirmed in red giant stars via asteroseismology and characterized in two ways. One being that dipole mixed modes with ℓ = 1 will display a global asymmetric frequency shift of its azimuthal components; where the m = 0 and m = ±1 components of the ℓ = 1 dipole mode will be shifted by two different power laws, respectively. And the other being a reduced visibility of dipole mixed mode amplitudes in the power spectra, where stars presenting with this feature are denoted as suppressed. Several studies of the suppressed dipole mixed mode amplitudes have been carried out, but thus far, no dedicated studies of the asymmetric frequency shifts of suppressed red giants have been conducted; one reason being that the asymmetric frequency shifts cannot be characterized when the dipole mixed mode amplitudes are severely reduced in many of the suppressed stars. Sincefullysuppressedstarsdonothavedetectablemixed-modestoevaluate, partiallysuppressed stars, that is, red giant stars presenting with suppressed dipole mixed modes in select parts of their power spectra rather than across the entire spectra, will be the subject of this study as the respective mode amplitudes are still visible at high frequencies. As such, this study will search for asymmetric frequency shifts on the dipole mixed modes of partially suppressed red giant stars; the aim here is to investigate if both mode suppression and magnetic shifting of dipole mixed modes occur simultaneously. Thisstudywillbeconductedbycreatingapipelinetoestimatepriorsofasteroseismicparameters, use the priors to model the power spectra with the stellar modeling code sloscillations_ISTA, and perform a Bayesian fit of the parameters with the simulated data on the star KIC 6975038, a target with partially suppressed dipolar mode amplitudes identified in the literature, to fit its magnetic parameters. I present a novel method to model the stellar power spectra of partially suppressed red giants by application of a sigmoid profile to the ℓ= 1 dipolar mode component of the spectra. With the results of this study I aim at constraining the cause of this partial dipole mode amplitude suppression, allowing for more detailed studies regarding their astrophysical nature. Furthermore, the long term hope for the method used in this study will be to expand the sample of partially suppressed red giants and fit their asteroseismic parameters accordingly.}, author = {Smith, Kanah}, issn = {2791-4585}, keywords = {asteroseismology, stellar physics, red giant, magnetism, suppressed}, pages = {38}, publisher = {Institute of Science and Technology Austria}, title = {{Exploring internal magnetism in partially suppressed red giant stars}}, doi = {10.15479/AT-ISTA-19853}, year = {2025}, } @article{19854, abstract = {Asynchronous Boolean networks are a type of discrete dynamical system in which each variable can take one of two states, and a single variable state is updated in each time step according to pre-selected rules. Boolean networks are popular in systems biology due to their ability to model long-term biological phenotypes within a qualitative, predictive framework. Boolean networks model phenotypes as attractors, which are closely linked to minimal trap spaces (inescapable hypercubes in the system’s state space). In biological applications, attractors and minimal trap spaces are typically in one-to-one correspondence. However, this correspondence is not guaranteed: motif-avoidant attractors (MAAs) that lie outside minimal trap spaces are possible. MAAs are rare and poorly understood, despite recent efforts. In this contribution to the BMB & JMB Special Collection “Problems, Progress and Perspectives in Mathematical and Computational Biology”, we summarize the current state of knowledge regarding MAAs and present several novel observations regarding their response to node deletion reductions and linear extensions of edges. We conduct large-scale computational studies on an ensemble of 14 000 models derived from published Boolean models of biological systems, and more than 100 million Random Boolean Networks. Our findings quantify the rarity of MAAs; in particular, we only observed MAAs in biological models after applying standard simplification methods, highlighting the role of network reduction in introducing MAAs into the dynamics. We also show that MAAs are fragile to linear extensions: in sparse networks, even a single linear node can disrupt virtually all MAAs. Motivated by this observation, we improve the upper bound on the number of delays needed to disrupt a motif-avoidant attractor.}, author = {Pastva, Samuel and Park, Kyu Hyong and Huvar, Ondřej and Rozum, Jordan C. and Albert, Réka}, issn = {1432-1416}, journal = {Journal of Mathematical Biology}, publisher = {Springer Nature}, title = {{An open problem: Why are motif-avoidant attractors so rare in asynchronous Boolean networks?}}, doi = {10.1007/s00285-025-02235-8}, volume = {91}, year = {2025}, } @article{19855, abstract = {We present indirect constraints on the absolute escape fraction of ionizing photons (f_{\rm esc}^{\rm LyC}) of the system GN 42912 which comprises two luminous galaxies (M_{\rm UV} magnitudes of -20.89 and -20.37) at z\sim7.5, GN 42912-NE and GN 42912-SW, to determine their contribution to the ionizing photon budget of the Epoch of Reionization (EoR). The high-resolution James Webb Space Telescope NIRSpec and NIRCam observations reveal the two galaxies are separated by only ~0.1" (0.5 kpc) on the sky and have a 358 km s^{-1} velocity separation. GN 42912-NE and GN 42912-SW are relatively massive for this redshift (log(M_\ast/M_\odot) \sim 8.4 and 8.9, respectively), with gas-phase metallicities of 18 per cent and 23 per cent solar, O_{32} ratios of 5.3 and >5.8, and \beta slopes of -1.92 and -1.51, respectively. We use the Mg II\lambda\lambda2796,2803 doublet to constrain f_{\rm esc}^{\rm LyC}. Mg II has an ionization potential close to that of neutral hydrogen and, in the optically thin regime, can be used as an indirect tracer of the LyC leakage. We establish realistic conservative upper limits on f_{\rm esc}^{\rm LyC} of 8.5 per cent for GN 42912-NE and 14 per cent for GN 42912-SW. These estimates align with f_{\rm esc}^{\rm LyC} trends observed with \beta, O_{32}, and the H\beta equivalent width at z<4. The small inferred ionized region sizes (<0.3 pMpc) around both galaxies indicate they have not ionized a significant fraction of the surrounding neutral gas. While these z>7 f_{\rm esc}^{\rm LyC} constraints do not decisively determine a specific reionization model, they support a minor contribution from these two relatively luminous galaxies to the EoR.}, author = {Gazagnes, S. and Chisholm, J. and Endsley, R. and Berg, D. A. and Leclercq, F. and Jurlin, N. and Saldana-Lopez, A. and Finkelstein, S. L. and Flury, S. R. and Guseva, N. G. and Henry, A. and Izotov, Y. I. and Jung, I. and Matthee, Jorryt J and Schaerer, D.}, issn = {1365-2966}, journal = {Monthly Notices of the Royal Astronomical Society}, number = {3}, pages = {2331--2348}, publisher = {Oxford University Press}, title = {{A negligible contribution of two luminous z ∼7.5 galaxies to the ionizing photon budget of reionization}}, doi = {10.1093/mnras/staf768}, volume = {540}, year = {2025}, } @article{19856, abstract = {Unlike in crystals, it is difficult to trace emergent material properties of amorphous solids to their underlying structure. Nevertheless, one can tune features of a disordered spring network, ranging from bulk elastic constants to specific allosteric responses, through highly precise alterations of the structure. This has been understood through the notion of independent bond-level response—the observation that, in many cases, different springs have different effects on different properties. While this idea has motivated inverse design in numerous contexts, it has not been formalized and quantified in a general context that not just informs but enables and predicts inverse design. Here, we show how to quantify independent response by linearizing the simultaneous change in multiple emergent features, and introduce the much stronger notion of fully independent response. Remarkably, we find that the mechanical properties of disordered solids are always fully independent across a wide array of scenarios, regardless of the target features, tunable parameters, system size, dimensionality, and class of interactions. Furthermore, our formulation quantifies the susceptibility of features to parameter changes, which is correlated with the maximum linear tunability. We also demonstrate the implications for multifeature inverse design beyond the linear regime. These results formalize our understanding of a key fundamental difference between ordered and disordered solids while also creating a practical tool to both understand and perform inverse design.}, author = {Zu, Mengjie and Desai, Aayush A and Goodrich, Carl Peter}, issn = {1079-7114}, journal = {Physical Review Letters}, number = {23}, publisher = {American Physical Society}, title = {{Fully independent response in disordered solids}}, doi = {10.1103/PhysRevLett.134.238201}, volume = {134}, year = {2025}, } @article{19857, abstract = {Bacteria have evolved a wide range of defence strategies to protect themselves against bacterial viruses (phages). Most known bacterial antiphage defence systems target phages with DNA genomes, which raises the question of how bacteria defend against phages with RNA genomes. Bacterial toxin–antitoxin systems that cleave intracellular RNA could potentially protect bacteria against RNA phages, but this has not been explored experimentally. In this study, we investigated the role of a model toxin–antitoxin system, MazEF, in protecting Escherichia coli against two RNA phage species. When challenged with these phages, the native presence of mazEF moderately reduced population susceptibility and increased the survival of individual E. coli cells. Genomic analysis further revealed an underrepresentation of the MazF cleavage site in genomes of RNA phages infecting E. coli, indicating selection against cleavage. These results show that, in addition to other physiological roles, RNA-degrading toxin–antitoxin systems may also help defend against RNA phages.}, author = {Nikolic, Nela and Pleska, Maros and Bergmiller, Tobias and Guet, Calin C}, issn = {1744-957X}, journal = {Biology Letters}, number = {6}, publisher = {The Royal Society}, title = {{A bacterial toxin-antitoxin system as a native defence element against RNA phages}}, doi = {10.1098/rsbl.2025.0080}, volume = {21}, year = {2025}, }