@article{21710, abstract = {Early results from JWST suggest that Epoch of Reionization (EoR) galaxies produce copious ionizing photons, which, if they escape efficiently, could cause reionization to occur too early. We study this problem using JWST imaging and prism spectroscopy for 412 galaxies at 4.5 < z < 9.0. We fit these data simultaneously with stellar population and nebular emission models that include a parameter for the fraction of ionizing photons that escape the galaxy, fesc. We find that the ionization production efficiency, ξion = Q(H0)/LUV, increases with redshift and decreasing UV luminosity, but shows significant scatter, (log ion z, MUV) 0.3 dex. The inferred escape fractions averaged over the population are low, ranging from〈fesc〉 ≃ 2.6% ± 1.4% at 6 < z < 9 to 6.5% ± 2.2% at 4.5 < z < 6, with weak or no indication of evolution with redshift. This implies that in our models most of the ionizing photons need to be absorbed to account for the nebular emission. We compute the impact of our results on reionization, including the distributions for ξion and fesc, and the evolution and uncertainty of the UV luminosity function. Considering galaxies brighter than MUV < −16 mag would produce an intergalactic medium hydrogen-ionized fraction of xe = 0.5 at 5.3 < z < 5.8, possibly too late compared to constraints from from quasistellar object (QSO) sight lines. Including fainter galaxies, MUV < −14 mag, we obtain xe = 0.5 at 6.0 < z < 8.1, fully consistent with QSO and cosmic microwave background data. This implies that EoR galaxies produce plenty of ionizing photons, but that these do not efficiently escape. This may be a result of high gas column densities combined with burstier star formation histories, which limit the time massive stars are able to clear channels through the gas for ionizing photons to escape.}, author = {Papovich, Casey and Cole, Justin W. and Hu, Weida and Finkelstein, Steven L. and Shen, Lu and Arrabal Haro, Pablo and Amorín, Ricardo O. and Backhaus, Bren E. and Bagley, Micaela B. and Bhatawdekar, Rachana and Calabrò, Antonello and Carnall, Adam C. and Cleri, Nikko J. and Daddi, Emanuele and Dickinson, Mark and Grogin, Norman A. and Holwerda, Benne W. and Jaskot, Anne E. and Koekemoer, Anton M. and Llerena, Mario and Lucas, Ray A. and Mascia, Sara and Pacucci, Fabio and Pentericci, Laura and Pérez-González, Pablo G. and Pirzkal, Nor and Raghunathan, Srinivasan and Seillé, Lise Marie and Somerville, Rachel S. and Yung, L. Y.Aaron}, issn = {1538-4357}, journal = {The Astrophysical Journal}, number = {1}, publisher = {IOP Publishing}, title = {{Galaxies in the epoch of reionization are all bark and no bite-plenty of ionizing photons, low escape fractions}}, doi = {10.3847/1538-4357/ae3b25}, volume = {1000}, year = {2026}, } @article{21726, abstract = {Quantum control of the many-body wavefunction is a central challenge in quantum materials research, as it could yield a precise control knob to manipulate emergent phenomena. Floquet engineering, the coherent dressing of quantum states with periodic non-resonant optical fields, has become an important strategy for quantum control. Most applications to solid-state systems have targeted weakly interacting or single-ion states, leaving the manipulation of many-body wavefunctions largely unexplored. Here we use Floquet engineering to achieve quantum control of a strongly correlated Hubbard exciton in the one-dimensional Mott insulator Sr2CuO3. A non-resonant mid-infrared optical field coherently dresses the exciton wavefunction, driving its rotation between bright and dark states. We use resonant third-harmonic generation to quantify ultrafast π/2 rotations on the Bloch sphere spanned by these exciton states. Our work advances the quest towards programmable control of correlated states and exciton-based quantum sensing.}, author = {Baykusheva, Denitsa Rangelova and Carmichael, Deven and Weber, Clara S. and Lu, I. Te and Glerean, Filippo and Meng, Tepie and De Oliveira, Pedro B.M. and Homes, Christopher C. and Zaliznyak, Igor A. and Gu, G. D. and Dean, Mark P.M. and Rubio, Angel and Kennes, Dante M. and Claassen, Martin and Mitrano, Matteo}, issn = {1476-4660}, journal = {Nature Materials}, publisher = {Springer Nature}, title = {{Quantum control of Hubbard excitons}}, doi = {10.1038/s41563-026-02517-6}, year = {2026}, } @article{21844, abstract = {Little red dots (LRDs) are a newly identified class of broad-line active galactic nuclei (AGNs) with a distinctive V-shaped spectrum characterized by red optical and blue UV continuum emission. Their high abundance at redshifts of z ∼ 6–8 and decline at lower redshifts suggest a transient origin. We propose that the spectral shape of LRDs originates from compact binary black hole systems, in which each black hole is surrounded by a mini-disk and embedded within a larger circumbinary disk. With a binary separation of ≲103 Schwarzschild radii, the Wien tail of a T ≃ 5000 K blackbody spectrum at the inner edge of the circumbinary disk produces the red optical emission, while the mini-disks power the UV continuum. Binary torques carve out a gap between the circumbinary disk and the mini-disks, setting the turnover wavelength of the V-shaped spectrum around the Balmer limit. This scenario naturally reproduces LRD spectra requiring only modest dust attenuation (AV ≲ 1 mag), resolving overestimated luminosities for LRDs in previous studies and alleviating a tension with the so-called Sołtan argument. This model predicts distinct spectral evolution as the binary orbit decays through binary disk interactions and gravitational-wave (GW) emission, linking early-stage “proto-LRD” binaries to the broader AGN population and late-stage “LRD descendants” to coalescing binaries detectable in GW experiments.}, author = {Inayoshi, Kohei and Shangguan, Jinyi and Chen, Xian and Ho, Luis C. and Haiman, Zoltán}, issn = {1538-4357}, journal = {The Astrophysical Journal}, number = {1}, publisher = {IOP Publishing}, title = {{The emergence of Little Red Dots from binary massive black holes}}, doi = {10.3847/1538-4357/ae548d}, volume = {1002}, year = {2026}, } @article{21896, abstract = {Redox-mediated flow batteries boost energy density by utilizing dissolved redox species as charge carriers for solid charge-storage materials. This strategy strongly depends on the thermodynamics and kinetics between the solid booster and dissolved redox species. Conventional electrochemical methods often convolute intrinsic reactivity with mass transport effects, introducing complexity in determining limiting steps. We propose a strategy that confines solid boosters within recessed microelectrodes and employs scanning electrochemical microscopy (SECM) to estimate reaction kinetics between booster and dissolved active redox species. Confining the solid booster in the recessed microelectrode overcomes mass transport limitations of dissolved redox species and enables controlled polarization of the booster material, allowing deconvolution of key rate-determining factors. As an initial model system, Prussian blue-ferricyanide/ferrocyanide [Fe(CN)6]3−/4− was used as solid booster and dissolved redox active species, respectively. The methodology was further explored for copper hexacyanoferrate with N,N,N-2,2,6,6-heptamethylpiperidinyl oxy-4-ammonium chloride and nickel hydroxide with [Fe(CN)6]3−/4− and extended to Mn-based Prussian blue analogues in combination with organic redox species. Our results demonstrate that SECM coupled with the proposed recessed microelectrode strategy provides a powerful platform to disentangle interfacial kinetics and guide the rational design of solid booster-dissolved redox species and electrolytes for high-performance redox-mediated flow batteries.}, author = {Santana Santos, Carla and Jiyane, Nomnotho and Quast, Thomas and Ibáñez, Maria and Rubio‐Presa, Rubén and Peljo, Pekka and Schuhmann, Wolfgang}, issn = {2566-6223}, journal = {Batteries & Supercaps}, number = {5}, publisher = {Wiley}, title = {{Evaluating reaction kinetics between solid booster and dissolved active species in redox‐mediated flow batteries using scanning electrochemical microscopy}}, doi = {10.1002/batt.70303}, volume = {9}, year = {2026}, } @article{21930, abstract = {We present the discovery of extreme nitrogen enrichment by Wolf Rayet nitrogen (WN) stars in the metal-poor (∼10%Z⊙), lensed, compact (Reff ∼ 20 pc) galaxy RXCJ2248 at z = 6.1, revealed by unprecedentedly deep JWST/NIRSpec medium-resolution spectroscopy from the GLIMPSE-D Survey. The exquisite signal-to-noise ratio reveals multiple high-ionization nebular lines and broad Balmer and [O III] components (FWHM ∼700–3000 km s −1 ). We detect broadened He II λ1640 and λ4687 (FWHM ∼ 530 km s −1 ) and strong N III λ4642 emission consistent with a population of WN stars, making RXCJ2248 the most distant galaxy with confirmed Wolf Rayet (WR) features to date. We measure the multiphase nebular density across five ions, the direct-method metallicity ( 12 + log(O/H) = 7.753 ± 0.025 ), and a nonuniform elemental enrichment pattern of extreme N/O enhancement ( log(N/O) = 0.391 ± 0.037 from N+, N+2 , and N+3 ) but suppressed C/O relative to empirical C/N trends. We show that this abundance pattern can be explained by enrichment from a dual-burst with a low WR carbon/WN ratio, as expected at low metallicities. Crucially, these signatures can only arise during a brief, rare evolutionary window shortly after a burst (∼3–6 Myr), when WN stars dominate chemical feedback but before dilution by later yields (e.g., supernovae). The observed frequency of strong N emitters at high−z implies a ∼50 Myr burst duty cycle, suggesting that N/O outliers may represent a brief but ubiquitous phase in the evolution of highly star-forming early galaxies. The WN detection in RXCJ2248, therefore, provides the first direct evidence of WR-driven nitrogen enrichment in the first billion years of the Universe and a novel timing argument for the bursty star formation cycles that shaped galaxies at cosmic dawn.}, author = {Berg, Danielle A. and Naidu, Rohan P. and Chisholm, John and Atek, Hakim and Fujimoto, Seiji and Kokorev, Vasily and Furtak, Lukas J. and Kobayashi, Chiaki and Schaerer, Daniel and Adamo, Angela and Fei, Qinyue and Korber, Damien and Matthee, Jorryt J and Marques-Chaves, Rui and Martinez, Zorayda and Mcquinn, Kristen B.W. and Muñoz, Julian B. and Oesch, Pascal A. and Saldana-Lopez, Alberto and Stark, Daniel P. and Stephenson, Mabel G. and Hsiao, Tiger Yu Yang}, issn = {1538-4357}, journal = {The Astrophysical Journal}, number = {2}, publisher = {IOP Publishing}, title = {{A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy}}, doi = {10.3847/1538-4357/ae5e4c}, volume = {1003}, year = {2026}, } @article{21341, abstract = {We aim to characterise the mass-metallicity relation (MZR) and the 3D correlation between the stellar mass, metallicity, and star formation rate (SFR) known as the fundamental metallicity relation (FMR) for galaxies at 5 < z < 7. Using ∼800 [O III] selected galaxies from deep NIRCam grism surveys, we present our stacked measurements of direct-Te metallicities, which we used to test recent strong-line metallicity calibrations. Our measured direct-Te metallicities (0.1–0.2 Z⊙ for M★ ≈ 5 × 107 − 9 M⊙, respectively) match recent JWST/NIRSpec-based results. However, there are significant inconsistencies between observations and hydrodynamical simulations. We observe a flatter MZR slope than the SPHINX20 and FLARES simulations, which cannot be attributed to selection effects. With simple models, we show that the effect of an [O III] flux-limited sample on the observed shape of the MZR is strongly dependent on the FMR. If the FMR is similar to the one in the local Universe, the intrinsic high-redshift MZR should be even flatter than is observed. In turn, a 3D relation where SFR correlates positively with metallicity at fixed mass would imply an intrinsically steeper MZR. Our measurements indicate that metallicity variations at fixed mass show little dependence on the SFR, suggesting a flat intrinsic MZR. This could indicate that the low-mass galaxies at these redshifts are out of equilibrium and that metal enrichment occurs rapidly in low-mass galaxies. However, being limited by our stacking analysis, we are yet to probe the scatter in the MZR and its dependence on SFR. Large carefully selected samples of galaxies with robust metallicity measurements can put tight constraints on the high-redshift FMR and help us to understand the interplay between gas flows, star formation, and feedback in early galaxies.}, author = {Kotiwale, Gauri and Matthee, Jorryt J and Kashino, Daichi and Vijayan, Aswin P. and Torralba Torregrosa, Alberto and Di Cesare, Claudia and Iani, Edoardo and Bordoloi, Rongmon and Leja, Joel and Maseda, Michael V. and Tacchella, Sandro and Shivaei, Irene and Heintz, Kasper E. and Danhaive, A. Lola and Mascia, Sara and Kramarenko, Ivan and Navarrete, Benjamín and Mackenzie, Ruari and Naidu, Rohan P. and Sobral, David}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{Rapid, out-of-equilibrium metal enrichment indicated by a flat mass-metallicity relation at z ∼ 6 from NIRCam grism spectroscopy}}, doi = {10.1051/0004-6361/202556597}, volume = {706}, year = {2026}, } @article{21385, abstract = {We prove that the average size of a mixed character sum (math. formular) (for a suitable smooth function w) is on the order of √x for all irrational real θ satisfying a weak Diophantine condition, where χ is drawn from the family of Dirichlet characters modulo a large prime r and where x 6 r. In contrast, it was proved by Harper that the average size is o(√x) for rational θ. Certain quadratic Diophantine equations play a key role in the present paper. }, author = {Wang, Victor and Xu, Max}, issn = {1473-7124}, journal = {Proceedings of the Royal Society of Edinburgh: Section A Mathematics}, pages = {1--15}, publisher = {Cambridge University Press}, title = {{Average sizes of mixed character sums}}, doi = {10.1017/prm.2026.10123}, year = {2026}, } @article{21453, abstract = {1. Collective behaviours are a fascinating study area due to the emergent properties that can only arise in groups of interacting individuals. However, their quantitative study is often impaired by technical difficulties, creating either low-quality and sparse data or impractical data amounts, particularly when capturing large groups over long periods of time. Common challenges arise from recording group members with as little obscuring of each other as possible, as well as in generating manageable data amounts with as high as possible information content. 2. We here provide a multicomponent system that allows to record, analyse and simulate the long-term spatiotemporal activity patterns of insect collectives, especially ant colonies. Our Ant Observing System, ALTAA, comprises a flat-nest design to prevent occlusion of individuals, a recording system running on a low-power single-board-computer, and a set of computer programmes performing quantitative analyses to guide the formation and validation of rules underlying the observed collective patterns. Our system is scalable in that it allows parallel, continuous observation of a high number of colonies using low memory space, with colony maintenance requirements (e.g. feeding, nest humidity) being achieved at lowest possible disturbance by the experimenter. 3. We showcase the potential of the system in a study using the black garden ant, Lasius niger, where we analyse the spatiotemporal effects of different group sizes (1, 6, 10 ants), brood (larvae) presence or absence, as well as of different nest geometries, over a period of 1 week. We show that the ants' motion activity has a weak periodicity in the range of 20 to 120 min promoted by larval presence, and that ants are spatially attracted to their larvae, the water source and the walls. We also find that the presence of nestmates lowers an individual ant's motion activity. Observed data are compared to simulations of the temporal activity of the ants. 4. ALTAA provides a powerful toolkit to quantify and interpret spatial and temporal collective activity patterns in (social) insects over extended periods.}, author = {Oh, Jinook and Cremer, Sylvia}, issn = {2041-210X}, journal = {Methods in Ecology and Evolution}, publisher = {Wiley}, title = {{ALTAA: Analysis of long-term activity patterns in ant colonies}}, doi = {10.1111/2041-210x.70277}, year = {2026}, } @article{21481, abstract = {The Hα emission line in galaxies is a powerful tracer of their recent star formation activity. With the advent of JWST, we are now able to routinely observe Hα in galaxies at high redshift (z ≳ 3) and thus measure their star formation rates (SFRs). However, using classical SFR(Hα) calibrations to derive the SFRs leads to biased results because high-redshift galaxies are commonly characterized by low metallicities and bursty star formation histories, affecting the conversion factor between the Hα luminosity (LHα) and the SFR. We developed a set of new SFR(Hα) calibrations that allowed us to predict the SFRs of Hα-emitters at z ≳ 3 with very little error. We used the SPHINX cosmological simulations to select a sample of star-forming galaxies representative of the Hα-emitter population observed with JWST. We then derived linear corrections to the classical SFR(Hα) calibrations that took variations in the physical properties (e.g., stellar metallicities) among individual galaxies into account. We obtained two new SFR(Hα) calibrations that compared to the classical calibrations reduce the root mean squared error (RMSE) in the predicted SFRs by ΔRMSE ≈ 0.04 dex and ΔRMSE ≈ 0.06 dex, respectively. Using the recent JWST NIRCam/grism observations of Hα-emitters at z ∼ 6, we show that the new calibrations affect the high-redshift galaxy population statistics: (i) the estimated cosmic SFR density decreases by ΔρSFR ≈ 12%, and (ii) the observed slope of the star formation main sequence increases by Δ∂logSFR/∂logM★ = 0.08 ± 0.02.}, author = {Kramarenko, Ivan and Rosdahl, J. and Blaizot, J. and Matthee, Jorryt J and Katz, H. and Di Cesare, Claudia}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{H α as a tracer of star formation in the SPHINX cosmological simulations}}, doi = {10.1051/0004-6361/202557114}, volume = {707}, year = {2026}, } @inproceedings{22003, abstract = {Let G be a finite, connected metric graph and let X be a subset of G. If X is sufficiently dense in G, we show that the Gromov-Hausdorff distance matches the Hausdorff distance, namely d_GH(G,X) = d_H(G,X). When the metric graph is the circle G = S¹ with circumference 2π, a recent study established the equality d_GH(S¹,X) = d_H(S¹,X) whenever d_GH(S¹,X) < π/6. Our results relax this hypothesis to d_GH(S¹,X) < π/3, and furthermore, we show that the constant π/3 is the best possible. We lower bound the Gromov-Hausdorff distance d_GH(G,X) by the Hausdorff distance d_H(G,X) via a simple topological obstruction: the existence of a possibly discontinuous function f: G → X with too small distortion contradicts the connectedness of G.}, author = {Adams, Henry and Majhi, Sushovan and Manin, Fedor and Virk, Ziga and Zava, Nicolò}, booktitle = {42nd International Symposium on Computational Geometry}, isbn = {9783959774185}, issn = {1868-8969}, keywords = {Gromov–Hausdorff distance, distortion, connectedness, Borsuk–Ulam theorem}, location = {New Brunswick, NJ, United States}, publisher = {Schloss Dagstuhl - Leibniz-Zentrum für Informatik}, title = {{Lower bounding the Gromov–Hausdorff distance in metric graphs}}, doi = {10.4230/LIPIcs.SoCG.2026.3}, volume = {367}, year = {2026}, } @article{21727, abstract = {We present a comprehensive analysis of the MIRI Extremely Red Object Virgil, a Lyα emitter at zspec = 6.6379 ± 0.0035 with the photometric properties of a Little Red Dot. Leveraging new JWST/MIRI imaging from the MIDIS and PAHSPECS programs, we confirm Virgil’s extraordinary nature among galaxies in JADES/GOODS-South, exhibiting a strikingly red NIRCam-to-MIRI color (F444W–F1500W = 2.84 ± 0.04 mag). Deep NIRSpec/PRISM spectroscopy from the OASIS program offers key insights into the host galaxy, revealing properties of an average star-forming galaxy during Cosmic Reionization, such as a subsolar metallicity, low-to-moderate dust content, and a relatively high ionization parameter and electron temperature. By estimating the star formation rate of Virgil from UV and Hα, we find evidence that the galaxy is either entering or fading out of a bursty episode. Although line-ratio diagnostics employed at high z would classify Virgil as an active galactic nucleus (AGN), this classification becomes ambiguous once redshift evolution is considered. Nonetheless, Virgil occupies the same parameter space as recently confirmed AGNs at similar redshifts. The new deep MIRI data at 15 μm reinforce the AGN nature of Virgil, as inferred from multiple spectral energy distribution (SED) fitting codes. Virgil’s rising infrared SED and UV excess resemble those of Dust-Obscured Galaxies (DOGs) studied with Spitzer at Cosmic Noon, particularly blue-excess HotDOGs. Our results highlight the need for a multiwavelength approach incorporating MIRI to uncover such extreme sources at z ≳ 6 and to shed light on the interplay between galaxy evolution and early black hole growth during Cosmic Reionization.}, author = {Rinaldi, Pierluigi and Pérez-González, Pablo G. and Rieke, George H. and Lyu, Jianwei and D’Eugenio, Francesco and Wu, Zihao and Carniani, Stefano and Looser, Tobias J. and Shivaei, Irene and Boogaard, Leindert A. and Diaz-Santos, Tanio and Colina, Luis and Östlin, Göran and Alberts, Stacey and Álvarez-Márquez, Javier and Annuziatella, Marianna and Aravena, Manuel and Bhatawdekar, Rachana and Bunker, Andrew J. and Caputi, Karina I. and Charlot, Stéphane and Crespo Gómez, Alejandro and Curti, Mirko and Eckart, Andreas and Gillman, Steven and Hainline, Kevin and Kumari, Nimisha and Hjorth, Jens and Iani, Edoardo and Inami, Hanae and Ji, Zhiyuan and Johnson, Benjamin D. and Jones, Gareth C. and Labiano, Álvaro and Maiolino, Roberto and Melinder, Jens and Moutard, Thibaud and Peissker, Florian and Rieke, Marcia and Robertson, Brant and Scholtz, Jan and Tacchella, Sandro and Van Der Werf, Paul P. and Walter, Fabian and Williams, Christina C. and Willott, Chris and Witstok, Joris and Übler, Hannah and Zhu, Yongda}, issn = {1538-4357}, journal = {The Astrophysical Journal}, number = {1}, publisher = {IOP Publishing}, title = {{Deciphering the nature of Virgil: An obscured active galactic nucleus lurking within an apparently normal Lyα emitter during cosmic reionization}}, doi = {10.3847/1538-4357/ae089c}, volume = {994}, year = {2025}, } @article{19278, abstract = {When two insulating, neutral materials are contacted and separated, they exchange electrical charge1. Experiments have long suggested that this ‘contact electrification’ is transitive, with different materials ordering into ‘triboelectric series’ based on the sign of charge acquired2. At the same time, the effect is plagued by unpredictability, preventing consensus on the mechanism and casting doubt on the rhyme and reason that series imply3. Here we expose an unanticipated connection between the unpredictability and order in contact electrification: nominally identical materials initially exchange charge randomly and intransitively, but—over repeated experiments—order into triboelectric series. We find that this evolution is driven by the act of contact itself—samples with more contacts in their history charge negatively to ones with fewer contacts. Capturing this ‘contact bias’ in a minimal model, we recreate both the initial randomness and ultimate order in numerical simulations and use it experimentally to force the appearance of a triboelectric series of our choosing. With a set of surface-sensitive techniques to search for the underlying alterations contact creates, we only find evidence of nanoscale morphological changes, pointing to a mechanism strongly coupled with mechanics. Our results highlight the centrality of contact history in contact electrification and suggest that focusing on the unpredictability that has long plagued the effect may hold the key to understanding it.}, author = {Sobarzo Ponce, Juan Carlos A and Pertl, Felix and Balazs, Daniel and Costanzo, Tommaso and Sauer, Markus and Foelske, Annette and Ostermann, Markus and Pichler, Christian M. and Wang, Yongkang and Nagata, Yuki and Bonn, Mischa and Waitukaitis, Scott R}, issn = {1476-4687}, journal = {Nature}, number = {8051}, publisher = {Springer Nature}, title = {{Spontaneous ordering of identical materials into a triboelectric series}}, doi = {10.1038/s41586-024-08530-6}, volume = {638}, year = {2025}, } @article{19284, abstract = {The Hα nebular emission line is an optimal tracer for recent star formation in galaxies. With the advent of JWST, this line has recently become observable at z > 3 for the first time. We present a catalog of 1050 Hα emitters at 3.7 < z < 6.7 in the GOODS fields obtained from a blind search in JWST NIRCam/grism data. We made use of the FRESCO survey’s 124 arcmin2 of observations in GOODS-North and GOODS-South with the F444W filter, probing Hα at 4.9 < z < 6.7, and the CONGRESS survey’s 62 arcmin2 of observations in GOODS-North with F356W, probing Hα at 3.8 < z < 5.1. We found an overdensity with 98 sources at z ∼ 4.4 in GOODS-N, and confirmed previously reported overdensities at z ∼ 5.2 in GOODS-N and at z ∼ 5.4 and z ∼ 5.9 in GOODS-S. We computed the observed Hα luminosity functions (LFs) in three bins centered at z ∼ 4.45, 5.30, and 6.15, which are the first such measurements at z > 3 obtained based purely on spectroscopic data, robustly tracing galaxy star formation rates (SFRs) beyond the peak of the cosmic star formation history. We compared our results with theoretical predictions from three different simulations and found good agreement at z ∼ 4 − 6. The UV LFs of this spectroscopically confirmed sample are in good agreement with pre-JWST measurements obtained with photometrically selected objects. Finally, we derived SFR functions and integrated them to compute the evolution of the cosmic SFR densities across z ∼ 4 − 6, finding values in good agreement with recent UV estimates from Lyman-break galaxies, which imply a continuous decrease in SFR density by a factor of three over z ∼ 4 to z ∼ 6. Our work shows the power of NIRCam grism observations to efficiently provide new tests for early galaxy formation models based on emission line statistics.}, author = {Covelo-Paz, Alba and Giovinazzo, Emma and Oesch, Pascal A. and Meyer, Romain A. and Weibel, Andrea and Brammer, Gabriel and Fudamoto, Yoshinobu and Kerutt, Josephine and Lin, Jamie and Matharu, Jasleen and Naidu, Rohan P. and Velichko, Anna and Bollo, Victoria and Bouwens, Rychard and Chisholm, John and Illingworth, Garth D. and Kramarenko, Ivan and Magee, Daniel and Maseda, Michael and Matthee, Jorryt J and Nelson, Erica and Reddy, Naveen and Schaerer, Daniel and Stefanon, Mauro and Xiao, Mengyuan}, issn = {1432-0746}, journal = {Astronomy & Astrophysics}, publisher = {EDP Sciences}, title = {{An Hα view of galaxy buildup in the first 2 Gyr: Luminosity functions at z ∼ 4−6.5 from NIRCam/grism spectroscopy}}, doi = {10.1051/0004-6361/202452363}, volume = {694}, year = {2025}, } @article{19366, abstract = {Staphylococcus aureus (S. aureus) is one of the most common causative agents of mammary gland infection and mastitis, but the specific role of S. aureus-derived extracellular vesicles (SaEVs) in mastitis has been poorly studied to date. Here, we aimed to investigate the response of bovine monocyte-derived macrophages (boMdM) to SaEVs of the genotype B (GTB) mastitis-related strain M5512B. Specifically, we evaluated the effects on the actin cytoskeleton, gene expression, and the SaEV proteomic cargo. Furthermore, we assessed to what extent the cellular and molecular response of boMdM to SaEVs differed from peripheral mononuclear blood cells (PBMCs) used for in vitro derivation of the former. We observed that SaEVs induced morphological changes in boMdM, leading to a pro-inflammatory and pyroptosis-related increased gene expression. Additionally, our study revealed that boMdM and PBMCs exhibited stimulus-specific differing responses. The proteomic analysis of SaEVs identified clusters of proteins related to virulence and antibiotic resistance, supporting the theory that S. aureus might use EVs to evade host defences and colonize the mammary gland. Our results bring new insights into how SaEVs might impact the host during an S. aureus infection, which can be useful for future S. aureus vaccine development.}, author = {Saenz-De-Juano, Mara D. and Silvestrelli, Giulia and Buri, Samuel and Zinsli, Léa V. and Schmelcher, Mathias and Ulbrich, Susanne E.}, issn = {2045-2322}, journal = {Scientific Reports}, pages = {6059}, publisher = {Springer Nature}, title = {{Mastitis-related Staphylococcus aureus-derived extracellular vesicles induce a pro-inflammatory response in bovine monocyte-derived macrophages}}, doi = {10.1038/s41598-025-90466-6}, volume = {15}, year = {2025}, } @article{19374, abstract = {In the present study, the new ternary rare earth intermetallic compound PrNi6Si6 has been investigated. This work completes the study of the RNi6Si6 series (R = rare earth). While the RNi6Si6 compounds for R = La and Ce adopt the CeNi6Si6-type (tP52, P4/nbm, No. 125), surprisingly PrNi6Si6 crystallizes in the YNi6Si6 prototype (tP52, P − 4b2, No. 117) as do all the heavier lanthanides (but Lu). The YNi6Si6-type and its homolog CeNi6Si6 are two tetragonal ordered derivative of the cubic NaZn13-type structure. Lattice parameters for PrNi6Si6 are a = 7.7846(1) Å, c = 11.2144(1) Å, with a unit cell volume, Vobs = 679.585(5) Å3. The temperature dependence of the inverse magnetic susceptibility χ−1(T) follows the Curie–Weiss law, with calculated values of the effective magnetic moment (µeff) and Weiss temperature (Θpm) of 3.55 μB and − 4.5 K, respectively. While the observed µeff is very close to the theoretical value of 3.58 µB for the free Pr3+ ions, a negative value of the Weiss temperature suggests antiferromagnetic interactions in PrNi6Si6. Magnetization measurements confirm that PrNi₆Si₆ orders antiferromagnetically (AFM) below a Néel temperature (TN) of 9 K. The Ni atoms contribute negligibly to the magnetic properties of this phase. The specific heat of PrNi₆Si₆ is approximately 0.42 J K  − 1  g − 1. Measurements of electric and thermal transport reveal that PrNi₆Si₆ exhibits metallic behavior across a wide temperature range of 2–900 K, accompanied by a relatively low thermal conductivity of around 6 W K − 1 m − 1 at room temperature. Such properties, together with its high-temperature refractory behavior, make PrNi₆Si₆ worthy of consideration in technological applications where fairly good electrical conductivity should be accompanied by a limited thermal conductivity.}, author = {Singh, Saurabh and Provino, A. and Pallecchi, I. and Caglieris, F. and Mödlinger, M. and Mele, P. and Latronico, G. and Takeuchi, T. and Manfrinetti, P.}, issn = {1573-4803}, journal = {Journal of Materials Science}, publisher = {Springer Nature}, title = {{The new PrNi6Si6 intermetallic: From crystal structure to thermal and electrical transport properties across a wide temperature range (2–900 K)}}, doi = {10.1007/s10853-024-10582-y}, volume = {60}, year = {2025}, } @article{19444, abstract = {As the field of neural organoids and assembloids expands, there is an emergent need for guidance and advice on designing, conducting and reporting experiments to increase the reproducibility and utility of these models. In this Perspective, we present a framework for the experimental process that encompasses ensuring the quality and integrity of human pluripotent stem cells, characterizing and manipulating neural cells in vitro, transplantation techniques and considerations for modelling human development, evolution and disease. As with all scientific endeavours, we advocate for rigorous experimental designs tailored to explicit scientific questions as well as transparent methodologies and data sharing to provide useful knowledge for current research practices and for developing regulatory standards.}, author = {Pașca, Sergiu P. and Arlotta, Paola and Bateup, Helen S. and Camp, J. Gray and Cappello, Silvia and Gage, Fred H. and Knoblich, Jürgen A. and Kriegstein, Arnold R. and Lancaster, Madeline A. and Ming, Guo Li and Novarino, Gaia and Okano, Hideyuki and Parmar, Malin and Park, In Hyun and Reiner, Orly and Song, Hongjun and Studer, Lorenz and Takahashi, Jun and Temple, Sally and Testa, Giuseppe and Treutlein, Barbara and Vaccarino, Flora M. and Vanderhaeghen, Pierre and Young-Pearse, Tracy}, issn = {1476-4687}, journal = {Nature}, number = {8054}, pages = {315--320}, publisher = {Springer Nature}, title = {{A framework for neural organoids, assembloids and transplantation studies}}, doi = {10.1038/s41586-024-08487-6}, volume = {639}, year = {2025}, } @article{19483, abstract = {We prove matching upper and lower bounds for the average of the6-torsionof class groups of quadratic fields. Furthermore, we count the number of integer solutions on an affine quartic threefold.}, author = {Chan, Yik Tung and Koymans, Peter and Pagano, Carlo and Sofos, Efthymios}, issn = {2036-2145}, journal = {Annali della Scuola Normale Superiore di Pisa, Classe di Scienze}, publisher = {Scuola Normale Superiore - Edizioni della Normale}, title = {{6-torision and integral points on quartic threefolds}}, doi = {10.2422/2036-2145.202412_006}, year = {2025}, } @article{19596, abstract = {We report the spectroscopic discovery of a massive quiescent galaxy at zspec = 7.29 ± 0.01, just ∼700 Myr after the big bang. RUBIES-UDS-QG-z7 was selected from public JWST/NIRCam and MIRI imaging from the PRIMER survey and observed with JWST/NIRSpec as part of RUBIES. The NIRSpec/PRISM spectrum reveals one of the strongest Balmer breaks observed thus far at z > 6, with no emission lines but tentative Balmer and Ca absorption features, as well as a Lyman break. Simultaneous modeling of the NIRSpec/PRISM spectrum and NIRCam and MIRI photometry (spanning 0.9–18 μm) shows that the galaxy formed a stellar mass of (math. formular) before z ∼ 8 and ceased forming stars 50–100 Myr prior to the time of observation, resulting in log (sSFR/Gyr- 1) < -1 . We measure a small physical size of (math formular) , which implies a high stellarmass surface density within the effective radius of (math formular) comparable to the highest densities measured in quiescent galaxies at z ∼ 2–5. The 3D stellar-mass density profile of RUBIES-UDS-QG-z7 is remarkably similar to the central densities of local massive ellipticals, suggesting that at least some of their cores may have already been in place at z > 7. The discovery of RUBIES-UDS-QG-z7 has strong implications for galaxy formation models: the estimated number density of quiescent galaxies at z ∼ 7 is >100 × larger than predicted from any model to date, indicating that quiescent galaxies have formed earlier than previously expected. }, author = {Weibel, Andrea and De Graaff, Anna and Setton, David J. and Miller, Tim B. and Oesch, Pascal A. and Brammer, Gabriel and Lagos, Claudia D.P. and Whitaker, Katherine E. and Williams, Christina C. and Baggen, Josephine F.W. and Bezanson, Rachel and Boogaard, Leindert A. and Cleri, Nikko J. and Greene, Jenny E. and Hirschmann, Michaela and Hviding, Raphael E. and Kuruvanthodi, Adarsh and Labbé, Ivo and Leja, Joel and Maseda, Michael V. and Matthee, Jorryt J and Mcconachie, Ian and Naidu, Rohan P. and Roberts-Borsani, Guido and Schaerer, Daniel and Suess, Katherine A. and Valentino, Francesco and Van Dokkum, Pieter and Wang, Bingjie}, issn = {1538-4357}, journal = {The Astrophysical Journal}, number = {1}, publisher = {IOP Publishing}, title = {{RUBIES reveals a massive quiescent galaxy at z = 7.3}}, doi = {10.3847/1538-4357/adab7a}, volume = {983}, year = {2025}, } @article{19636, abstract = {This summary of the second Terrestrial Very-Long-Baseline Atom Interferometry (TVLBAI) Workshop provides a comprehensive overview of our meeting held in London in April 2024 (Second Terrestrial Very-Long-Baseline Atom Interferometry Workshop, Imperial College, April 2024), building on the initial discussions during the inaugural workshop held at CERN in March 2023 (First Terrestrial Very-Long-Baseline Atom Interferometry Workshop, CERN, March 2023). Like the summary of the first workshop (Abend et al. in AVS Quantum Sci. 6:024701, 2024), this document records a critical milestone for the international atom interferometry community. It documents our concerted efforts to evaluate progress, address emerging challenges, and refine strategic directions for future large-scale atom interferometry projects. Our commitment to collaboration is manifested by the integration of diverse expertise and the coordination of international resources, all aimed at advancing the frontiers of atom interferometry physics and technology, as set out in a Memorandum of Understanding signed by over 50 institutions (Memorandum of Understanding for the Terrestrial Very Long Baseline Atom Interferometer Study).}, author = {Abdalla, Adam and Abe, Mahiro and Abend, Sven and Abidi, Mouine and Aidelsburger, Monika and Alibabaei, Ashkan and Allard, Baptiste and Antoniadis, John and Arduini, Gianluigi and Augst, Nadja and Balamatsias, Philippos and Balaž, Antun and Banks, Hannah and Barcklay, Rachel L. and Barone, Michele and Barsanti, Michele and Bason, Mark G. and Bassi, Angelo and Bayle, Jean Baptiste and Baynham, Charles F.A. and Beaufils, Quentin and Beldjoudi, Sélyan and Belić, Aleksandar and Bennetts, Shayne and Bernabeu, Jose and Bertoldi, Andrea and Bigard, Clara and Bigelow, N. P. and Bingham, Robert and Blas, Diego and Bobrick, Alexey and Boehringer, Samuel and Bogojević, Aleksandar and Bongs, Kai and Bortoletto, Daniela and Bouyer, Philippe and Brand, Christian and Buchmueller, Oliver and Buica, Gabriela and Calatroni, Sergio and Calmels, Léo and Canizares, Priscilla and Canuel, Benjamin and Caramete, Ana and Caramete, Laurentiu Ioan and Carlesso, Matteo and Carlton, John and Carman, Samuel P. and Carroll, Andrew and Casariego, Mateo and Chairetis, Minoas and Charmandaris, Vassilis and Chauhan, Upasna and Chen, Jiajun and Chiofalo, Maria Luisa Maria Luisa Marilù and Ciampini, Donatella and Cimbri, Alessia and Cladé, Pierre and Coleman, Jonathon and Constantin, Florin Lucian and Contaldi, Carlo R. and Corgier, Robin and Dash, Bineet and Davies, G. J. and De Rham, Claudia and De Roeck, Albert and Derr, Daniel and Dey, Soumyodeep and Di Pumpo, Fabio and Djordjevic, Goran S. and Döbrich, Babette and Dornan, Peter and Doser, Michael and Drougakis, Giannis and Dunningham, Jacob and Duspayev, Alisher and Easo, Sajan and Eby, Joshua and Efremov, Maxim and Elertas, Gedminas and Ellis, John and Entin, Nicholas and Fairhurst, Stephen and Fanì, Mattia and Fassi, Farida and Fayet, Pierre and Felea, Daniel and Feng, Jie and Flack, Robert and Foot, Chris and Freegarde, Tim and Fuchs, Elina and Gaaloul, Naceur and Gao, Dongfeng and Gardner, Susan and Garraway, Barry M. and Garrido Alzar, Carlos L. and Gauguet, Alexandre and Giese, Enno and Gill, Patrick and Giudice, Gian F. and Glasbrenner, Eric P. and Glick, Jonah and Graham, Peter W. and Granados, Eduardo and Griffin, Paul F. and Gué, Jordan and Guellati-Khelifa, Saïda and Gupta, Subhadeep and Gupta, Vishu and Hackermueller, Lucia and Haehnelt, Martin and Hakulinen, Timo and Hammerer, Klemens and Hanımeli, Ekim T. and Harte, Tiffany and Hartmann, Sabrina and Hawkins, Leonie and Hees, Aurelien and Herbst, Alexander and Hird, Thomas M. and Hobson, Richard and Hogan, Jason and Holst, Bodil and Holynski, Michael and Hosten, Onur and Hsu, Chung Chuan and Huang, Wayne Cheng Wei and Hughes, Kenneth M. and Hussain, Kamran and Hütsi, Gert and Iovino, Antonio and Isfan, Maria Catalina and Janson, Gregor and Jeglič, Peter and Jetzer, Philippe and Jiang, Yijun and Juzeliūnas, Gediminas and Kaenders, Wilhelm and Kalliokoski, Matti and Kehagias, Alex and Kilian, Eva and Klempt, Carsten and Knight, Peter and Koley, Soumen and Konrad, Bernd and Kovachy, Tim and Krutzik, Markus and Kumar, Mukesh and Kumar, Pradeep and Labiad, Hamza and Lan, Shau Yu and Landragin, Arnaud and Landsberg, Greg and Langlois, Mehdi and Lanigan, Bryony and Leone, Bruno and Le Poncin-Lafitte, Christophe and Lellouch, Samuel and Lewicki, Marek and Lien, Yu Hung and Lombriser, Lucas and Asamar, Elias Lopez and Lopez-Gonzalez, J. Luis and Lu, Chen and Luciano, Giuseppe Gaetano and Lundblad, Nathan and De J. López Monjaraz, Cristian and Lowe, Adam and Mackoit-Sinkevičienė, Mažena and Maggiore, Michele and Majumdar, Anirban and Makris, Konstantinos and Maleknejad, Azadeh and Marchant, Anna L. and Mariotti, Agnese and Markou, Christos and Matthews, Barnaby and Mazumdar, Anupam and Mccabe, Christopher and Meister, Matthias and Mentasti, Giorgio and Menu, Jonathan and Messineo, Giuseppe and Meyer-Hoppe, Bernd and Micalizio, Salvatore and Migliaccio, Federica and Millington, Peter and Milosevic, Milan and Mishra, Abhay and Mitchell, Jeremiah and Morley, Gavin W. and Mouelle, Noam and Müller, Jürgen and Newbold, David and Ni, Wei Tou and Niehof, Christian and Noller, Johannes and Odžak, Senad and Oi, Daniel K.L. and Oikonomou, Andreas and Omar, Yasser and Overstreet, Chris and Puthiya Veettil, Vishnupriya and Pahl, Julia and Paling, Sean and Pan, Zhongyin and Pappas, George and Pareek, Vinay and Pasatembou, Elizabeth and Paternostro, Mauro and Pathak, Vishal K. and Pelucchi, Emanuele and Pereira Dos Santos, Franck and Peters, Achim and Pichery, Annie and Pikovski, Igor and Pilaftsis, Apostolos and Pislan, Florentina Crenguta and Plunkett, Robert and Poggiani, Rosa and Prevedelli, Marco and Rafelski, Johann and Raidal, Juhan and Raidal, Martti and Rasel, Ernst Maria and Renaux-Petel, Sébastien and Richaud, Andrea and Rivero-Antunez, Pedro and Rodzinka, Tangui and Roura, Albert and Rudolph, Jan and Sabulsky, Dylan and Safronova, Marianna S. and Sakellariadou, Mairi and Salvi, Leonardo and Sameed, Muhammed and Sarkar, Sumit and Schach, Patrik and Schäffer, Stefan Alaric and Schelfhout, Jesse and Schilling, Manuel and Schkolnik, Vladimir and Schleich, Wolfgang P. and Schlippert, Dennis and Schneider, Ulrich and Schreck, Florian and Schwartzman, Ariel and Schwersenz, Nico and Sergijenko, Olga and Sfar, Haifa Rejeb and Shao, Lijing and Shipsey, Ian and Shu, Jing and Singh, Yeshpal and Sopuerta, Carlos F. and Sorba, Marianna and Sorrentino, Fiodor and Spallicci, Alessandro D.A.M. and Stefanescu, Petruta and Stergioulas, Nikolaos and Stoerk, Daniel and Thaivalappil Sunilkumar, Hrudya and Ströhle, Jannik and Tam, Zoie and Tandon, Dhruv and Tang, Yijun and Tell, Dorothee and Tempere, Jacques and Temples, Dylan J. and Thampy, Rohit P. and Tietje, Ingmari C. and Tino, Guglielmo M. and Tinsley, Jonathan N. and Tintareanu Mircea, Ovidiu and Tkalčec, Kimberly and Tolley, Andrew J. and Tornatore, Vincenza and Torres-Orjuela, Alejandro and Treutlein, Philipp and Trombettoni, Andrea and Ufrecht, Christian and Urrutia, Juan and Valenzuela, Tristan and Valerio, Linda R. and Van Der Grinten, Maurits and Vaskonen, Ville and Vázquez-Aceves, Verónica and Veermäe, Hardi and Vetrano, Flavio and Vitanov, Nikolay V. and Von Klitzing, Wolf and Wald, Sebastian and Walker, Thomas and Walser, Reinhold and Wang, Jin and Wang, Yan and Weidner, C. A. and Wenzlawski, André and Werner, Michael and Wörner, Lisa and Yahia, Mohamed E. and Yazgan, Efe and Zambrini Cruzeiro, Emmanuel and Zarei, M. and Zhan, Mingsheng and Zhang, Shengnan and Zhou, Lin and Zupanič, Erik}, issn = {2196-0763}, journal = {EPJ Quantum Technology}, publisher = {Springer Nature}, title = {{Terrestrial Very-Long-Baseline Atom Interferometry: Summary of the second workshop}}, doi = {10.1140/epjqt/s40507-025-00344-3}, volume = {12}, year = {2025}, } @article{19638, abstract = {The James Webb Space Telescope has revealed low-luminosity active galactic nuclei at redshifts of z ≳ 4–7, many of which host accreting massive black holes (BHs) with BH-to-galaxy mass (MBH/M⋆) ratios exceeding the local values by more than an order of magnitude. The origin of these overmassive BHs remains unclear but requires potential contributions from heavy seeds and/or episodes of super-Eddington accretion. We present a growth model coupled with dark matter halo assembly to explore the evolution of the MBH/M⋆ ratio under different seeding and feedback scenarios. Given the gas inflow rates in protogalaxies, BHs grow episodically at moderate super-Eddington rates, and the mass ratio increases early on, despite significant mass loss through feedback. Regardless of seeding mechanisms, the mass ratio converges to a universal value ∼0.1–0.3, set by the balance between gas feeding and star formation efficiency in the nucleus. This behavior defines an attractor in the MBH–M⋆ diagram, where overmassive BHs grow more slowly than their hosts, while undermassive seeds experience rapid growth before aligning with the attractor. We derive an analytical expression for the universal mass ratio, linking it to feedback strength and halo growth. The convergence of evolutionary tracks erases seeding information from the mass ratio by z ∼ 4–6. Detecting BHs with ∼105−6 M⊙ at higher redshifts that deviate from the convergence trend would provide key diagnostics of their birth conditions.}, author = {Hu, Haojie and Inayoshi, Kohei and Haiman, Zoltán and Ho, Luis C. and Ohsuga, Ken}, issn = {2041-8213}, journal = {The Astrophysical Journal Letters}, number = {2}, publisher = {IOP Publishing}, title = {{The convergence of heavy and light seeds to overmassive black holes at cosmic dawn}}, doi = {10.3847/2041-8213/adc680}, volume = {983}, year = {2025}, }