--- OA_place: repository OA_type: green _id: '21870' abstract: - lang: eng text: Superconducting qubits are a leading candidate for utility-scale quantum computing due to their fast gate speeds and steadily decreasing error rates. The requirement for millikelvin operating temperatures, however, creates a significant scaling bottleneck. Modular architectures using optical fiber links could bridge separate cryogenic nodes, but superconducting circuits do not have coherent optical transitions and microwave-to-optical conversion has not been shown for any non-classical photon state. In this work, we demonstrate the on-demand generation and tomographic reconstruction of itinerant single microwave photons at 8.9 GHz from a superconducting qubit. We upconvert this non-Gaussian state with a transducer added noise below 0.012 quanta and count the converted telecom photons at 193.4 THz with a signal-to-noise ratio of up to 5.1$\pm$1.1. We characterize the trade-offs between throughput and noise, and establish a viable path toward heralded entanglement distribution and gate teleportation. Looking ahead, these results empower existing superconducting devices to take a key role in distributed quantum technologies and heterogeneous quantum systems. acknowledgement: "We thank Fritz Diorico and Onur Hosten who suggested the filter cavity design, and gave important insights about the assembly and the testing of the FabryPerot filter cavities. Ekatrina Fedotova and Diego A.\r\nLancheros Naranjo worked on the filter cavity setup in\r\nthe early stages of this work. Gustavo Wiederhecker and\r\nYiewen Chu provided insights as to the origins of the\r\nobserved optical noise and Nicola Carlon Zambon suggested using telecom filters to mitigate it further. This\r\nwork was supported by the European Research Council under grant agreement no. 101089099 (ERC CoG\r\ncQEO), and 101248662 (ERC POC CoupledEOT), the\r\nEuropean Unions Horizon 2020 research and innovation\r\nprogram under grant agreement no. 899354 (FETopen\r\nSuperQuLAN), the European Innovation Council no.\r\n101187231 (PathfinderOpen CIELO), and the Austrian\r\nScience Fund (FWF) no. F7105 (SFB BeyondC). J.F.\r\nand L.K. acknowledge support from the Horizon Europe\r\nProgram HORIZON-CL4-2022-QUANTUM-01-SGA via\r\nProject No. 101113946 OpenSuperQPlus100. A.M. acknowledges support from the NOMIS-ISTA fellowship." article_processing_charge: No arxiv: 1 author: - first_name: Thomas full_name: Werner, Thomas id: 1fcd8497-dba3-11ea-a45e-c6fbd715f7c7 last_name: Werner orcid: 0009-0001-2346-5236 - first_name: Erfan full_name: Riyazi, Erfan id: 53322f94-5355-11ee-ae5a-ff6f81c87d51 last_name: Riyazi - first_name: Samarth full_name: Hawaldar, Samarth id: 221708e1-1ff6-11ee-9fa6-85146607433e last_name: Hawaldar orcid: 0000-0002-1965-4309 - first_name: Rishabh full_name: Sahu, Rishabh id: 47D26E34-F248-11E8-B48F-1D18A9856A87 last_name: Sahu orcid: 0000-0001-6264-2162 - first_name: Georg M full_name: Arnold, Georg M id: 3770C838-F248-11E8-B48F-1D18A9856A87 last_name: Arnold orcid: 0000-0003-1397-7876 - first_name: Paul Falthansl-Scheinecker full_name: Paul Falthansl-Scheinecker, Paul Falthansl-Scheinecker last_name: Paul Falthansl-Scheinecker - first_name: Jennifer A. Sánchez full_name: Naranjo, Jennifer A. Sánchez last_name: Naranjo - first_name: Dante full_name: Loi, Dante last_name: Loi - first_name: Lucky N. full_name: Kapoor, Lucky N. last_name: Kapoor - first_name: Martin full_name: Zemlicka, Martin id: 2DCF8DE6-F248-11E8-B48F-1D18A9856A87 last_name: Zemlicka orcid: 0009-0005-0878-3032 - first_name: Liu full_name: Qiu, Liu id: 45e99c0d-1eb1-11eb-9b96-ed8ab2983cac last_name: Qiu orcid: 0000-0003-4345-4267 - first_name: Andrei full_name: Militaru, Andrei id: d67706f8-8eb1-11ee-ad1b-9c30dfa19e0b last_name: Militaru - first_name: Johannes M full_name: Fink, Johannes M id: 4B591CBA-F248-11E8-B48F-1D18A9856A87 last_name: Fink orcid: 0000-0001-8112-028X citation: ama: Werner T, Riyazi E, Hawaldar S, et al. Electro-optic conversion of itinerant Fock states. arXiv. doi:10.48550/arXiv.2602.00928 apa: Werner, T., Riyazi, E., Hawaldar, S., Sahu, R., Arnold, G. M., Paul Falthansl-Scheinecker, P. F.-S., … Fink, J. M. (n.d.). Electro-optic conversion of itinerant Fock states. arXiv. https://doi.org/10.48550/arXiv.2602.00928 chicago: Werner, Thomas, Erfan Riyazi, Samarth Hawaldar, Rishabh Sahu, Georg M Arnold, Paul Falthansl-Scheinecker Paul Falthansl-Scheinecker, Jennifer A. Sánchez Naranjo, et al. “Electro-Optic Conversion of Itinerant Fock States.” ArXiv, n.d. https://doi.org/10.48550/arXiv.2602.00928. ieee: T. Werner et al., “Electro-optic conversion of itinerant Fock states,” arXiv. . ista: Werner T, Riyazi E, Hawaldar S, Sahu R, Arnold GM, Paul Falthansl-Scheinecker PF-S, Naranjo JAS, Loi D, Kapoor LN, Zemlicka M, Qiu L, Militaru A, Fink JM. Electro-optic conversion of itinerant Fock states. arXiv, 10.48550/arXiv.2602.00928. mla: Werner, Thomas, et al. “Electro-Optic Conversion of Itinerant Fock States.” ArXiv, doi:10.48550/arXiv.2602.00928. short: T. Werner, E. Riyazi, S. Hawaldar, R. Sahu, G.M. Arnold, P.F.-S. Paul Falthansl-Scheinecker, J.A.S. Naranjo, D. Loi, L.N. Kapoor, M. Zemlicka, L. Qiu, A. Militaru, J.M. Fink, ArXiv (n.d.). corr_author: '1' date_created: 2026-05-12T13:58:18Z date_published: 2026-01-31T00:00:00Z date_updated: 2026-05-20T13:35:42Z day: '31' department: - _id: JoFi - _id: GradSch doi: 10.48550/arXiv.2602.00928 ec_funded: 1 external_id: arxiv: - '2602.00928' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.48550/arXiv.2602.00928 month: '01' oa: 1 oa_version: Preprint project: - _id: bdadfa0d-d553-11ed-ba76-fb85edbd456a grant_number: '101089099' name: 'Cavity Quantum Electro Optics: Microwave photonics with nonclassical states' - _id: 5b807754-ab3d-11f0-914f-ff8c34502cc9 grant_number: '101248662' name: Integrated optical coupling for low loss electro-optic interconnects - _id: 9B868D20-BA93-11EA-9121-9846C619BF3A call_identifier: H2020 grant_number: '899354' name: Quantum Local Area Networks with Superconducting Qubits - _id: 91aaf765-16d5-11f0-9cad-a8e7e44cccb7 grant_number: '101187231' name: 'Cavity-Integrated Electro-Optics: Measuring, Converting and Manipulating Microwaves with Light' - _id: 26927A52-B435-11E9-9278-68D0E5697425 call_identifier: FWF grant_number: F07105 name: Integrating superconducting quantum circuits - _id: 9B861AAC-BA93-11EA-9121-9846C619BF3A name: NOMIS Fellowship Program publication: arXiv publication_status: draft related_material: record: - id: '21863' relation: dissertation_contains status: public scopus_import: '1' status: public title: Electro-optic conversion of itinerant Fock states tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: preprint user_id: 8b945eb4-e2f2-11eb-945a-df72226e66a9 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21898' abstract: - lang: eng text: We investigate the nature and spectroscopic diversity of early galaxies from a sample of 41 sources at $z\geqslant 10$ with James Webb Space Telescope (JWST)/NIRSpec prism observations. We compare the properties of strong ultraviolet (UV) line emitters, traced by intense C iv emission, with those of more ‘typical’ sources with weak or undetected C iv. The more typical (or ‘C iv-weak’) sources reveal significant scatter in their C iii] line strengths, UV continuum slopes, and physical sizes, spanning C iii] equivalent widths (EWs) of $\sim$1–51 Å, UV slopes of $\beta \sim -1.6$ to $-2.6$, and half-light radii of $\sim$50–1000 pc. In contrast, C iv-strong sources occupy the tail of these distributions, with C iii] EWs of 16–51 Å, UV slopes $\beta \lesssim -2.5$, compact morphologies ($r_{\rm 50} \lesssim 100$ pc), and elevated star formation surface densities ($\Sigma _{\rm SFR} \gtrsim 100\, M_\odot \, \mathrm{yr}^{-1}\, \mathrm{kpc}^{-2}$). These properties suggest concentrated starbursts that temporarily outshine the host galaxy. Comparing average properties from composite spectra, we find the diversity of the sample is primarily driven by bursty star formation on very short time-scales ($\le$3 Myr), with strong C iv emitters observed at the apex of the bursts and sources devoid of emission lines during relative inactivity. An apparent association between strong C iv and enhanced nitrogen abundance suggests both may be modulated by the same duty cycle, reflecting a generic mode of star formation. We show that active galactic nuclei are unlikely to contribute significantly to this duty cycle based on UV line diagnostics and photoionization models. Our results support a picture whereby brief bursts and lulls can explain the spectral diversity and early growth of bright galaxies in the first 500 Myr. acknowledgement: "We thank the anonymous referee for useful and constructive\r\nfeedback that improved the manuscript. GRB is grateful to Vasily\r\nBelokurov and Sarah Kane for providing the relevant abundances\r\nforthe Aurora data in Fig. 11, as well asto Tiger Yu-Yang Hsiao for\r\nhelpful discussions regarding the MACS 0647-JD source. We are\r\nalso grateful to Gabe Brammerfor useful discussions and his continuous efforts in maintaining and improving the msaexp code,\r\nfrom which the high-z community continues to benefit greatly.\r\nLastly, we also thank the numerous teams of the observational\r\nprograms used in this study, for developing these valuable data\r\nsets. The data used in this study are derived from the following\r\nprograms: 1181 (PI Eisenstein; D. J. Eisenstein et al. 2023a), 1210\r\n(PI Luetzgendorf; D. J. Eisenstein et al. 2023a), 1211 (PI Isaak;\r\nM. V. Maseda et al. 2024), 1286 (PI Luetzgendorf; D. J. Eisenstein\r\net al. 2023a), 1287 (PI Isaak; D. J. Eisenstein et al. 2023a), 1345\r\n(PI Finkelstein; S. L. Finkelstein et al. 2025), 1433 (PI Coe; T. Y.-\r\nY. Hsiao et al. 2024a), 2561 (PI Labbé; R. Bezanson et al. 2022),\r\n2750 (PI Arrabal Haro; P. Arrabal Haro et al. 2023b), 3073 (PI\r\nCastellano; M. Castellano et al. 2024), 3215 (PIs Eisenstein &\r\nMaiolino; D. J. Eisenstein et al. 2023b), 5224 (PIs Oesch & Naidu;\r\nOesch et al. in preparation), 6368 (PI Dickinson; V. Kokorev et al.\r\n2025). The authors acknowledge the aforementioned teams and\r\nPIs where development of their observing program(s) was done\r\nwith a zero-exclusive-access period.\r\nThis work is based on observations made with the\r\nNASA/ESA/CSA JWST. The data were obtained from the\r\nMikulski Archive for Space Telescopes at the Space Telescope\r\nScience Institute, which is operated by the Association of\r\nUniversities for Research in Astronomy, Inc., under NASA\r\ncontract NAS 5-03127 for JWST. The specific observations\r\nanalysed can be accessed via DOI 10.17909/jqj3-ws37. Some\r\nof the data products presented herein were retrieved from the\r\nDawn JWST Archive (DJA). DJA is an initiative of the Cosmic\r\nDawn Center (DAWN), which is funded by the Danish National\r\nResearch Foundation under grant DNRF140.\r\nRSE acknowledges generous financial support from the Peter\r\nand Patricia Gruber Foundation. YF acknowledgessupportsfrom\r\nJSPS KAKENHI Grant Numbers JP22K21349 and JP23K13149.\r\nThis work has received funding from the Swiss State Secretariat\r\nfor Education, Research and Innovation (SERI) under contract\r\nnumber MB22.00072, as well as from the Swiss National Science\r\nFoundation (SNSF) through project grant 200020_207349." article_number: stag701 article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Guido full_name: Roberts-Borsani, Guido last_name: Roberts-Borsani - first_name: Pascal A full_name: Oesch, Pascal A last_name: Oesch - first_name: Richard full_name: Ellis, Richard last_name: Ellis - first_name: Andrea full_name: Weibel, Andrea last_name: Weibel - first_name: Emma full_name: Giovinazzo, Emma last_name: Giovinazzo - first_name: Rychard full_name: Bouwens, Rychard last_name: Bouwens - first_name: Pratika full_name: Dayal, Pratika last_name: Dayal - first_name: Adriano full_name: Fontana, Adriano last_name: Fontana - first_name: Kasper E full_name: Heintz, Kasper E last_name: Heintz - first_name: Jorryt J full_name: Matthee, Jorryt J id: 7439a258-f3c0-11ec-9501-9df22fe06720 last_name: Matthee orcid: 0000-0003-2871-127X - first_name: Romain A full_name: Meyer, Romain A last_name: Meyer - first_name: Laura full_name: Pentericci, Laura last_name: Pentericci - first_name: Alice full_name: Shapley, Alice last_name: Shapley - first_name: Sandro full_name: Tacchella, Sandro last_name: Tacchella - first_name: Tommaso full_name: Treu, Tommaso last_name: Treu - first_name: Fabian full_name: Walter, Fabian last_name: Walter - first_name: Hakim full_name: Atek, Hakim last_name: Atek - first_name: Sownak full_name: Bose, Sownak last_name: Bose - first_name: Marco full_name: Castellano, Marco last_name: Castellano - first_name: Yoshinobu full_name: Fudamoto, Yoshinobu last_name: Fudamoto - first_name: Takahiro full_name: Morishita, Takahiro last_name: Morishita - first_name: Rohan P full_name: Naidu, Rohan P last_name: Naidu - first_name: Ryan L full_name: Sanders, Ryan L last_name: Sanders - first_name: Arjen full_name: van der Wel, Arjen last_name: van der Wel citation: ama: 'Roberts-Borsani G, Oesch PA, Ellis R, et al. JWST spectroscopic insights into the diversity of galaxies in the first 500 Myr: Short-lived snapshots along a common evolutionary pathway. Monthly Notices of the Royal Astronomical Society. 2026;548(3). doi:10.1093/mnras/stag701' apa: 'Roberts-Borsani, G., Oesch, P. A., Ellis, R., Weibel, A., Giovinazzo, E., Bouwens, R., … van der Wel, A. (2026). JWST spectroscopic insights into the diversity of galaxies in the first 500 Myr: Short-lived snapshots along a common evolutionary pathway. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stag701' chicago: 'Roberts-Borsani, Guido, Pascal A Oesch, Richard Ellis, Andrea Weibel, Emma Giovinazzo, Rychard Bouwens, Pratika Dayal, et al. “JWST Spectroscopic Insights into the Diversity of Galaxies in the First 500 Myr: Short-Lived Snapshots along a Common Evolutionary Pathway.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/stag701.' ieee: 'G. Roberts-Borsani et al., “JWST spectroscopic insights into the diversity of galaxies in the first 500 Myr: Short-lived snapshots along a common evolutionary pathway,” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 3. Oxford University Press, 2026.' ista: 'Roberts-Borsani G, Oesch PA, Ellis R, Weibel A, Giovinazzo E, Bouwens R, Dayal P, Fontana A, Heintz KE, Matthee JJ, Meyer RA, Pentericci L, Shapley A, Tacchella S, Treu T, Walter F, Atek H, Bose S, Castellano M, Fudamoto Y, Morishita T, Naidu RP, Sanders RL, van der Wel A. 2026. JWST spectroscopic insights into the diversity of galaxies in the first 500 Myr: Short-lived snapshots along a common evolutionary pathway. Monthly Notices of the Royal Astronomical Society. 548(3), stag701.' mla: 'Roberts-Borsani, Guido, et al. “JWST Spectroscopic Insights into the Diversity of Galaxies in the First 500 Myr: Short-Lived Snapshots along a Common Evolutionary Pathway.” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 3, stag701, Oxford University Press, 2026, doi:10.1093/mnras/stag701.' short: G. Roberts-Borsani, P.A. Oesch, R. Ellis, A. Weibel, E. Giovinazzo, R. Bouwens, P. Dayal, A. Fontana, K.E. Heintz, J.J. Matthee, R.A. Meyer, L. Pentericci, A. Shapley, S. Tacchella, T. Treu, F. Walter, H. Atek, S. Bose, M. Castellano, Y. Fudamoto, T. Morishita, R.P. Naidu, R.L. Sanders, A. van der Wel, Monthly Notices of the Royal Astronomical Society 548 (2026). date_created: 2026-05-20T14:34:29Z date_published: 2026-05-01T00:00:00Z date_updated: 2026-05-21T06:16:04Z day: '01' ddc: - '520' department: - _id: JoMa doi: 10.1093/mnras/stag701 external_id: arxiv: - '2508.21708' file: - access_level: open_access checksum: b8f52c6fc5e06b3a505310e7d5898ecf content_type: application/pdf creator: dernst date_created: 2026-05-21T06:14:23Z date_updated: 2026-05-21T06:14:23Z file_id: '21902' file_name: 2026_MNRAS_RobertsBorsani.pdf file_size: 3539140 relation: main_file success: 1 file_date_updated: 2026-05-21T06:14:23Z has_accepted_license: '1' intvolume: ' 548' issue: '3' language: - iso: eng month: '05' oa: 1 oa_version: Published Version publication: Monthly Notices of the Royal Astronomical Society publication_identifier: eissn: - 1365-2966 issn: - 0035-8711 publication_status: published publisher: Oxford University Press quality_controlled: '1' scopus_import: '1' status: public title: 'JWST spectroscopic insights into the diversity of galaxies in the first 500 Myr: Short-lived snapshots along a common evolutionary pathway' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 548 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21897' abstract: - lang: eng text: Ultracompact binary systems, consisting of two compact objects in an orbit $\lesssim 0.5 {\rm R}_\odot$, should exhibit measurable rates of orbital period change ($\dot{P} \ne 0$) due to the emission of gravitational waves (GWs). Measurements of $\dot{P}$ have so far been limited to the shortest-period ultracompact binaries ($\lesssim 20$  min). Among the AM CVn-type subclass, several works have proposed the presence of extra angular momentum loss beyond GW emission, with magnetic braking being a widely discussed mechanism. If present, this magnetic braking would dominate the angular momentum loss of AM CVn-type binaries with orbital periods $\gtrsim 30$ min. In this work, we present a long-term eclipse timing study of two AM CVn-type binaries, YZ LMi and Gaia14aae, with respective orbital periods of 28.3 min and 49.7 min and continuous observations since 2006 and 2015. Both systems show $\dot{P}$ consistent with zero within $2\sigma$. Their $3\sigma$ upper limits are $1.1 \times 10^{-13}\, {\rm s \, s}^{-1}$ and $9.7 \times 10^{-14}\, {\rm s \, s}^{-1}$, respectively. These non-detections are most simply explained by a scenario in which secular angular momentum loss is not substantially stronger than GW emission at all orbital periods, but is combined with deviations from the secular $\dot{P}$ whose time-scales span decades but whose amplitude is $\lesssim 10^{-13}\, {\rm s \, s}^{-1}$. Our non-detections of $\dot{P}$ represent a limit on the strength of any enhanced angular momentum loss beyond pure GW emission. acknowledgement: "We are grateful to the anonymousreferee fortheirinsightful comments. MJG thanks Mitch Begelman and the JILA department at the University of Colorado, Boulder, for providing office space at which much of this paper was written. This work is supported in part by the United States National Aeronautics and Space Administration (NASA) under grants\r\n80NSSC24K0436, 80NSSC22K0479, and 80NSSC24K0380, and the United States National Science Foundation (NSF) under grant AST-2508429. VSD and HiPERCAM are funded by the Science and Technology Facilities Council (grant ST/Z000033/1). IP acknowledges support from the Royal Society through a University Research Fellowship (URF\\R1\\231496). This project has received funding from the European Research Council under the European Union’s Horizon 2020 research and innovation programme (grant agreement numbers 101002408 – MOS100PC). CMC receives funding from United Kingdom Research and Innovation grant numbers ST/X005933/1 and ST/W001934/1. This article is based in part on observations made in the Observatorios de Canarias del Instituto de Astrofísica de Canarias (IAC) with the the William Herschel Telescope (WHT) operated on the island of La Palma by the Isaac Newton Group (ING) in the Observatorio del Roque de los Muchachos. It is also based in part on observations made with the Gran Telescopio Canarias (GTC) under proposal ID GTC18-24A, installed at the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofísica de Canarias, in the island of La Palma. Further data were obtained using the 2.4 m Thai National Telescope (TNT) operated by the National Astronomy Research Institute of Thailand\r\n(NARIT), and the 200-inch Hale Telescope at Palomar Observatory operated by the California Institute of Technology. Software packages used in this work include the ultracam and hipercam reduction pipelines, lcurve (C. M. Copperwheat et al. 2010), numpy, astropy, matplotlib, and emcee (D. Foreman-Mackey et al. 2013)." article_number: stag673 article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Matthew J full_name: Green, Matthew J last_name: Green - first_name: Thomas R full_name: Marsh, Thomas R last_name: Marsh - first_name: Joannes C full_name: van Roestel, Joannes C id: 4d122fc8-6083-11f0-87a5-97d68b860333 last_name: van Roestel - first_name: Tin Long Sunny full_name: Wong, Tin Long Sunny last_name: Wong - first_name: Diogo full_name: Belloni, Diogo last_name: Belloni - first_name: Mukremin full_name: Kilic, Mukremin last_name: Kilic - first_name: Elmé full_name: Breedt, Elmé last_name: Breedt - first_name: Alex full_name: Brown, Alex last_name: Brown - first_name: Chris M full_name: Copperwheat, Chris M last_name: Copperwheat - first_name: Anurak full_name: Chakpor, Anurak last_name: Chakpor - first_name: V S full_name: Dhillon, V S last_name: Dhillon - first_name: Noel Castro full_name: Segura, Noel Castro last_name: Segura - first_name: Martin J full_name: Dyer, Martin J last_name: Dyer - first_name: James full_name: Garbutt, James last_name: Garbutt - first_name: Dan full_name: Jarvis, Dan last_name: Jarvis - first_name: Vasu full_name: Kengkriangkrai, Vasu last_name: Kengkriangkrai - first_name: Mark R full_name: Kennedy, Mark R last_name: Kennedy - first_name: Paul full_name: Kerry, Paul last_name: Kerry - first_name: Thomas full_name: Kupfer, Thomas last_name: Kupfer - first_name: S P full_name: Littlefair, S P last_name: Littlefair - first_name: James full_name: McCormac, James last_name: McCormac - first_name: James full_name: Munday, James last_name: Munday - first_name: Steven G full_name: Parsons, Steven G last_name: Parsons - first_name: Eleanor full_name: Pike, Eleanor last_name: Pike - first_name: Ingrid full_name: Pelisoli, Ingrid last_name: Pelisoli - first_name: Pablo full_name: Rodríguez-Gil, Pablo last_name: Rodríguez-Gil - first_name: David I full_name: Sahman, David I last_name: Sahman - first_name: Amalie full_name: Yates, Amalie last_name: Yates citation: ama: Green MJ, Marsh TR, van Roestel JC, et al. No period change in two long-period AM CVn binaries. Monthly Notices of the Royal Astronomical Society. 2026;548(3). doi:10.1093/mnras/stag673 apa: Green, M. J., Marsh, T. R., van Roestel, J. C., Wong, T. L. S., Belloni, D., Kilic, M., … Yates, A. (2026). No period change in two long-period AM CVn binaries. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stag673 chicago: Green, Matthew J, Thomas R Marsh, Joannes C van Roestel, Tin Long Sunny Wong, Diogo Belloni, Mukremin Kilic, Elmé Breedt, et al. “No Period Change in Two Long-Period AM CVn Binaries.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/stag673. ieee: M. J. Green et al., “No period change in two long-period AM CVn binaries,” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 3. Oxford University Press, 2026. ista: Green MJ, Marsh TR, van Roestel JC, Wong TLS, Belloni D, Kilic M, Breedt E, Brown A, Copperwheat CM, Chakpor A, Dhillon VS, Segura NC, Dyer MJ, Garbutt J, Jarvis D, Kengkriangkrai V, Kennedy MR, Kerry P, Kupfer T, Littlefair SP, McCormac J, Munday J, Parsons SG, Pike E, Pelisoli I, Rodríguez-Gil P, Sahman DI, Yates A. 2026. No period change in two long-period AM CVn binaries. Monthly Notices of the Royal Astronomical Society. 548(3), stag673. mla: Green, Matthew J., et al. “No Period Change in Two Long-Period AM CVn Binaries.” Monthly Notices of the Royal Astronomical Society, vol. 548, no. 3, stag673, Oxford University Press, 2026, doi:10.1093/mnras/stag673. short: M.J. Green, T.R. Marsh, J.C. van Roestel, T.L.S. Wong, D. Belloni, M. Kilic, E. Breedt, A. Brown, C.M. Copperwheat, A. Chakpor, V.S. Dhillon, N.C. Segura, M.J. Dyer, J. Garbutt, D. Jarvis, V. Kengkriangkrai, M.R. Kennedy, P. Kerry, T. Kupfer, S.P. Littlefair, J. McCormac, J. Munday, S.G. Parsons, E. Pike, I. Pelisoli, P. Rodríguez-Gil, D.I. Sahman, A. Yates, Monthly Notices of the Royal Astronomical Society 548 (2026). date_created: 2026-05-20T14:34:03Z date_published: 2026-04-09T00:00:00Z date_updated: 2026-05-21T06:41:41Z day: '09' ddc: - '520' department: - _id: IlCa doi: 10.1093/mnras/stag673 external_id: arxiv: - '2604.06460' file: - access_level: open_access checksum: 2c4463926c5cb84ce555ef2005b52ddd content_type: application/pdf creator: dernst date_created: 2026-05-21T06:37:42Z date_updated: 2026-05-21T06:37:42Z file_id: '21903' file_name: 2026_MNRAS_Green.pdf file_size: 3960296 relation: main_file success: 1 file_date_updated: 2026-05-21T06:37:42Z has_accepted_license: '1' intvolume: ' 548' issue: '3' keyword: - 'binaries: close – stars' - dwarf novae – novae - cataclysmic variables – white dwarfs language: - iso: eng month: '04' oa: 1 oa_version: Published Version publication: Monthly Notices of the Royal Astronomical Society publication_identifier: eissn: - 1365-2966 issn: - 0035-8711 publication_status: published publisher: Oxford University Press quality_controlled: '1' scopus_import: '1' status: public title: No period change in two long-period AM CVn binaries tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 548 year: '2026' ... --- OA_place: publisher OA_type: hybrid PlanS_conform: '1' _id: '21896' abstract: - lang: eng text: 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. acknowledgement: "The authors acknowledge funding from the European Union's Horizon Europe research and innovation programme— European Innovation Council (EIC) under the grant agreement No 101046742 (MeBattery). P.P. acknowledges the funding from the European Research Council through a Starting Grant (agreement no. 950038). Dr. Mahdi Moghaddam, University of Turku, is acknowledged for providing the CuHCF, and Prof. Hubert Girault, EPFL, is acknowledged for providing the TEMPTMA.\r\nOpen Access funding enabled and organized by Projekt DEAL." article_number: e70303 article_processing_charge: Yes (via OA deal) article_type: original author: - first_name: Carla full_name: Santana Santos, Carla last_name: Santana Santos - first_name: Nomnotho full_name: Jiyane, Nomnotho last_name: Jiyane - first_name: Thomas full_name: Quast, Thomas last_name: Quast - first_name: Maria full_name: Ibáñez, Maria id: 43C61214-F248-11E8-B48F-1D18A9856A87 last_name: Ibáñez orcid: 0000-0001-5013-2843 - first_name: Rubén full_name: Rubio‐Presa, Rubén last_name: Rubio‐Presa - first_name: Pekka full_name: Peljo, Pekka last_name: Peljo - first_name: Wolfgang full_name: Schuhmann, Wolfgang last_name: Schuhmann citation: ama: Santana Santos C, Jiyane N, Quast T, et al. Evaluating reaction kinetics between solid booster and dissolved active species in redox‐mediated flow batteries using scanning electrochemical microscopy. Batteries &amp; Supercaps. 2026;9(5). doi:10.1002/batt.70303 apa: Santana Santos, C., Jiyane, N., Quast, T., Ibáñez, M., Rubio‐Presa, R., Peljo, P., & Schuhmann, W. (2026). Evaluating reaction kinetics between solid booster and dissolved active species in redox‐mediated flow batteries using scanning electrochemical microscopy. Batteries &amp; Supercaps. Wiley. https://doi.org/10.1002/batt.70303 chicago: Santana Santos, Carla, Nomnotho Jiyane, Thomas Quast, Maria Ibáñez, Rubén Rubio‐Presa, Pekka Peljo, and Wolfgang Schuhmann. “Evaluating Reaction Kinetics between Solid Booster and Dissolved Active Species in Redox‐mediated Flow Batteries Using Scanning Electrochemical Microscopy.” Batteries &amp; Supercaps. Wiley, 2026. https://doi.org/10.1002/batt.70303. ieee: C. Santana Santos et al., “Evaluating reaction kinetics between solid booster and dissolved active species in redox‐mediated flow batteries using scanning electrochemical microscopy,” Batteries &amp; Supercaps, vol. 9, no. 5. Wiley, 2026. ista: Santana Santos C, Jiyane N, Quast T, Ibáñez M, Rubio‐Presa R, Peljo P, Schuhmann W. 2026. Evaluating reaction kinetics between solid booster and dissolved active species in redox‐mediated flow batteries using scanning electrochemical microscopy. Batteries &amp; Supercaps. 9(5), e70303. mla: Santana Santos, Carla, et al. “Evaluating Reaction Kinetics between Solid Booster and Dissolved Active Species in Redox‐mediated Flow Batteries Using Scanning Electrochemical Microscopy.” Batteries &amp; Supercaps, vol. 9, no. 5, e70303, Wiley, 2026, doi:10.1002/batt.70303. short: C. Santana Santos, N. Jiyane, T. Quast, M. Ibáñez, R. Rubio‐Presa, P. Peljo, W. Schuhmann, Batteries &amp; Supercaps 9 (2026). date_created: 2026-05-20T14:32:37Z date_published: 2026-05-01T00:00:00Z date_updated: 2026-05-21T06:57:25Z day: '01' ddc: - '530' department: - _id: MaIb doi: 10.1002/batt.70303 file: - access_level: open_access checksum: 292d65503a63cc7df92b960627634dad content_type: application/pdf creator: dernst date_created: 2026-05-21T06:54:57Z date_updated: 2026-05-21T06:54:57Z file_id: '21904' file_name: 2026_BatteriesSupercaps_SantanaSantos.pdf file_size: 756344 relation: main_file success: 1 file_date_updated: 2026-05-21T06:54:57Z has_accepted_license: '1' intvolume: ' 9' issue: '5' language: - iso: eng month: '05' oa: 1 oa_version: Published Version publication: Batteries & Supercaps publication_identifier: eissn: - 2566-6223 publication_status: published publisher: Wiley quality_controlled: '1' scopus_import: '1' status: public title: Evaluating reaction kinetics between solid booster and dissolved active species in redox‐mediated flow batteries using scanning electrochemical microscopy tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 9 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21895' abstract: - lang: eng text: The mammalian brain organises knowledge about entities in the world and relationships between them using cognitive maps. When forming a cognitive map, there is a necessary trade-off between extending the map to make novel inferences, and storing a veridical copy of past experience. However, the neural mechanisms that control this trade-off remain unknown. Using a cross-scale approach that combines a pharmacological intervention in humans with neural network modelling, we show that the neuromodulator noradrenaline elicits a significant ‘spread of association’ across hippocampal cognitive maps. This neural spread of association can be explained by changes in synaptic plasticity that predict overgeneralisation in behaviour. Thus, elevated noradrenaline during learning increases the ‘smoothing kernel’ for plasticity across the cognitive map, allowing disparate memories to become linked and distorted. acknowledgement: 'We would like to thank Chamith Halahakoon, Phil Cowen, Angharad De Cates, Beata Godlewska, Riccardo De Giorgi, Katherine Smith and Edoardo Ostinelli for enabling this study by providing medical cover. We would like to thank Douglas F. Tomé and Everton J. Agnes for their guidance and advice with earlier versions of the neural network model. We would like to thank Rob Froemke for helpful discussion when preparing the experiments. We thank Leonie Glitz and Valentina Mancini for comments on an earlier version of the manuscript. R.S.K. was supported by an EPSRC/MRC-funded studentship (EP/L016052/1). P.P. was supported by the Cambridge Trust, Trinity Henry Barlow Scholarship and Trinity Hall Brockhouse Scholarship. L.C. is supported by the Foundation for Science and Technology (FCT) (Portuguese State Budget: UID/PSI/01662/2020; Research fellowship: 2021.00415.CEECIND). W.T.C. is funded by the Wellcome Trust [225924/Z/22/Z]. H.C.B. is supported by a UKRI Future Leaders Fellowship (MR/W008939/1) and the Wellcome Institutional Strategic Support Fund. H.C.B. and J.X.O. are supported by the Medical Research Council (MR/W01971X/1). The study was supported by the NIHR Oxford Health Biomedical Research Centre (NIHR203316). The views expressed are those of the author(s) and not necessarily those of the NIHR or the Department of Health and Social Care. The Wellcome Centre for Integrative Neuroimaging is supported by core funding from the Wellcome Trust (203139/Z/16/Z and 203139/A/16/Z). This research was funded in part by the Wellcome Trust. For the purpose of open access, the author(s) have applied a CC BY public copyright license to any Author Accepted Manuscript version arising from this submission.' article_number: '3961' article_processing_charge: Yes article_type: original author: - first_name: Renée S. full_name: Koolschijn, Renée S. last_name: Koolschijn - first_name: Prakriti full_name: Parthasarathy, Prakriti last_name: Parthasarathy - first_name: Michael full_name: Browning, Michael last_name: Browning - first_name: Xenia full_name: Przygodda, Xenia last_name: Przygodda - first_name: Liliana P. full_name: Capitão, Liliana P. last_name: Capitão - first_name: William T. full_name: Clarke, William T. last_name: Clarke - first_name: Tim P full_name: Vogels, Tim P id: CB6FF8D2-008F-11EA-8E08-2637E6697425 last_name: Vogels orcid: 0000-0003-3295-6181 - first_name: Jill X. full_name: O’Reilly, Jill X. last_name: O’Reilly - first_name: Helen C. full_name: Barron, Helen C. last_name: Barron citation: ama: Koolschijn RS, Parthasarathy P, Browning M, et al. Noradrenaline causes a spread of association in the hippocampal cognitive map. Nature Communications. 2026;17. doi:10.1038/s41467-026-70659-x apa: Koolschijn, R. S., Parthasarathy, P., Browning, M., Przygodda, X., Capitão, L. P., Clarke, W. T., … Barron, H. C. (2026). Noradrenaline causes a spread of association in the hippocampal cognitive map. Nature Communications. Springer Nature. https://doi.org/10.1038/s41467-026-70659-x chicago: Koolschijn, Renée S., Prakriti Parthasarathy, Michael Browning, Xenia Przygodda, Liliana P. Capitão, William T. Clarke, Tim P Vogels, Jill X. O’Reilly, and Helen C. Barron. “Noradrenaline Causes a Spread of Association in the Hippocampal Cognitive Map.” Nature Communications. Springer Nature, 2026. https://doi.org/10.1038/s41467-026-70659-x. ieee: R. S. Koolschijn et al., “Noradrenaline causes a spread of association in the hippocampal cognitive map,” Nature Communications, vol. 17. Springer Nature, 2026. ista: Koolschijn RS, Parthasarathy P, Browning M, Przygodda X, Capitão LP, Clarke WT, Vogels TP, O’Reilly JX, Barron HC. 2026. Noradrenaline causes a spread of association in the hippocampal cognitive map. Nature Communications. 17, 3961. mla: Koolschijn, Renée S., et al. “Noradrenaline Causes a Spread of Association in the Hippocampal Cognitive Map.” Nature Communications, vol. 17, 3961, Springer Nature, 2026, doi:10.1038/s41467-026-70659-x. short: R.S. Koolschijn, P. Parthasarathy, M. Browning, X. Przygodda, L.P. Capitão, W.T. Clarke, T.P. Vogels, J.X. O’Reilly, H.C. Barron, Nature Communications 17 (2026). date_created: 2026-05-20T14:30:37Z date_published: 2026-05-01T00:00:00Z date_updated: 2026-05-21T07:05:01Z day: '01' ddc: - '570' department: - _id: TiVo doi: 10.1038/s41467-026-70659-x external_id: pmid: - '41832186' file: - access_level: open_access checksum: 1b529e06b1c5d6e085d60743317fd4f9 content_type: application/pdf creator: dernst date_created: 2026-05-21T07:01:35Z date_updated: 2026-05-21T07:01:35Z file_id: '21905' file_name: 2026_NatureComm_Koolschijn.pdf file_size: 2059139 relation: main_file success: 1 file_date_updated: 2026-05-21T07:01:35Z has_accepted_license: '1' intvolume: ' 17' language: - iso: eng month: '05' oa: 1 oa_version: Published Version pmid: 1 publication: Nature Communications publication_identifier: eissn: - 2041-1723 publication_status: published publisher: Springer Nature quality_controlled: '1' scopus_import: '1' status: public title: Noradrenaline causes a spread of association in the hippocampal cognitive map tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 17 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold _id: '21899' abstract: - lang: eng text: Cell extrusion is an essential mechanism for controlling cell density in epithelial tissues. Another essential element of epithelia is curvature, which is required to achieve complex shapes, like in the lung or intestine. Here, we introduce a three-dimensional bubbly vertex model to study the interplay between extrusion and curvature. We find a generic cellular bulging instability at topological defects, which is much stronger than for standard vertex models. Analyzing cell shapes in three-dimensional imaging data of spherical mouse colon organoids, we infer that pentagonal cells have an increased basal interfacial tension, suggesting that cells at topological defects react to the different force conditions. Using the bubbly vertex model, we show that such basal tensions stabilize against the predicted instability and result in better cell shape control than tissue-scale mechanisms such as lumen pressure and spontaneous curvature. Our theory suggests that epithelial curvature naturally leads to bulged and extrusionlike cell shapes because the interfacial curvature of individual cells at the defects strongly amplifies buckling effected by tissue-scale topological defects in elastic sheets. Our results highlight the complex interplay of forces across scales in three-dimensional tissue organization. acknowledgement: O. M. D., M. B., and U.S. S. acknowledge support from the Max Planck School Matter to Life, with funding by the German Federal Ministry of Education and Research (BMBF), the Dieter Schwarz Foundation, and the Max Planck Society. M. B. and U.S. S. acknowledge support from the cluster of excellence 3DMM2O (EXC 2082/1-390761711 and EXC 2082/2-390761711) funded by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation). The authors acknowledge the data storage service SDS@hd supported by the Ministry of Science, Research and the Arts Baden-Württemberg (MWK) and the DFG through Grant No. INST 35/1503-1 FUGG. For the publication fee we acknowledge financial support by Heidelberg University. O. M. D. thanks Edouard Hannezo for valuable discussions. U.S. S. is a member of the Interdisciplinary Center for Scientific Computing (IWR) at Heidelberg. article_number: '021023' article_processing_charge: Yes article_type: original author: - first_name: Oliver M full_name: Drozdowski, Oliver M id: cd4ed792-b872-11ef-bb90-b7b3a3f62f75 last_name: Drozdowski - first_name: Büşra full_name: "Kocameşe-Tamgac\U0001D6A4, Büşra" last_name: "Kocameşe-Tamgac\U0001D6A4" - first_name: Kim E. full_name: Boonekamp, Kim E. last_name: Boonekamp - first_name: Michael full_name: Boutros, Michael last_name: Boutros - first_name: Ulrich S. full_name: Schwarz, Ulrich S. last_name: Schwarz citation: ama: "Drozdowski OM, Kocameşe-Tamgac\U0001D6A4 B, Boonekamp KE, Boutros M, Schwarz US. Cell bulging and extrusion in a three-dimensional bubbly vertex model for curved epithelial sheets. Physical Review X. 2026;16(2). doi:10.1103/x82g-cq7n" apa: "Drozdowski, O. M., Kocameşe-Tamgac\U0001D6A4, B., Boonekamp, K. E., Boutros, M., & Schwarz, U. S. (2026). Cell bulging and extrusion in a three-dimensional bubbly vertex model for curved epithelial sheets. Physical Review X. American Physical Society. https://doi.org/10.1103/x82g-cq7n" chicago: "Drozdowski, Oliver M, Büşra Kocameşe-Tamgac\U0001D6A4, Kim E. Boonekamp, Michael Boutros, and Ulrich S. Schwarz. “Cell Bulging and Extrusion in a Three-Dimensional Bubbly Vertex Model for Curved Epithelial Sheets.” Physical Review X. American Physical Society, 2026. https://doi.org/10.1103/x82g-cq7n." ieee: "O. M. Drozdowski, B. Kocameşe-Tamgac\U0001D6A4, K. E. Boonekamp, M. Boutros, and U. S. Schwarz, “Cell bulging and extrusion in a three-dimensional bubbly vertex model for curved epithelial sheets,” Physical Review X, vol. 16, no. 2. American Physical Society, 2026." ista: "Drozdowski OM, Kocameşe-Tamgac\U0001D6A4 B, Boonekamp KE, Boutros M, Schwarz US. 2026. Cell bulging and extrusion in a three-dimensional bubbly vertex model for curved epithelial sheets. Physical Review X. 16(2), 021023." mla: Drozdowski, Oliver M., et al. “Cell Bulging and Extrusion in a Three-Dimensional Bubbly Vertex Model for Curved Epithelial Sheets.” Physical Review X, vol. 16, no. 2, 021023, American Physical Society, 2026, doi:10.1103/x82g-cq7n. short: "O.M. Drozdowski, B. Kocameşe-Tamgac\U0001D6A4, K.E. Boonekamp, M. Boutros, U.S. Schwarz, Physical Review X 16 (2026)." date_created: 2026-05-20T14:35:57Z date_published: 2026-04-30T00:00:00Z date_updated: 2026-05-21T06:08:11Z day: '30' ddc: - '530' department: - _id: EdHa doi: 10.1103/x82g-cq7n file: - access_level: open_access checksum: a90e905968648ac4425c256de901e9c3 content_type: application/pdf creator: dernst date_created: 2026-05-21T06:05:49Z date_updated: 2026-05-21T06:05:49Z file_id: '21901' file_name: 2026_PhysicalReviewX_Drozdowski.pdf file_size: 5603164 relation: main_file success: 1 file_date_updated: 2026-05-21T06:05:49Z has_accepted_license: '1' intvolume: ' 16' issue: '2' language: - iso: eng month: '04' oa: 1 oa_version: Published Version publication: Physical Review X publication_identifier: issn: - 2160-3308 publication_status: published publisher: American Physical Society quality_controlled: '1' scopus_import: '1' status: public title: Cell bulging and extrusion in a three-dimensional bubbly vertex model for curved epithelial sheets tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 16 year: '2026' ... --- OA_type: closed access _id: '21900' abstract: - lang: eng text: Individually silencing 125 fruit fly genes reveals opposing fitness effects of mutations between females and males, as well as between germline and somatic tissues. article_processing_charge: No article_type: comment author: - first_name: Filip full_name: Ruzicka, Filip id: 347955dd-57b0-11ee-9095-c28bdd368f4b last_name: Ruzicka citation: ama: Ruzicka F. Reverse genetics of sexual antagonism. Nature Ecology & Evolution. 2026. doi:10.1038/s41559-026-03036-y apa: Ruzicka, F. (2026). Reverse genetics of sexual antagonism. Nature Ecology & Evolution. Springer Nature. https://doi.org/10.1038/s41559-026-03036-y chicago: Ruzicka, Filip. “Reverse Genetics of Sexual Antagonism.” Nature Ecology & Evolution. Springer Nature, 2026. https://doi.org/10.1038/s41559-026-03036-y. ieee: F. Ruzicka, “Reverse genetics of sexual antagonism,” Nature Ecology & Evolution. Springer Nature, 2026. ista: Ruzicka F. 2026. Reverse genetics of sexual antagonism. Nature Ecology & Evolution. mla: Ruzicka, Filip. “Reverse Genetics of Sexual Antagonism.” Nature Ecology & Evolution, Springer Nature, 2026, doi:10.1038/s41559-026-03036-y. short: F. Ruzicka, Nature Ecology & Evolution (2026). corr_author: '1' date_created: 2026-05-20T14:36:45Z date_published: 2026-05-01T00:00:00Z date_updated: 2026-05-21T05:49:25Z day: '01' department: - _id: BeVi doi: 10.1038/s41559-026-03036-y language: - iso: eng month: '05' oa_version: None publication: Nature Ecology & Evolution publication_identifier: eissn: - 2397-334X publication_status: epub_ahead publisher: Springer Nature quality_controlled: '1' scopus_import: '1' status: public title: Reverse genetics of sexual antagonism type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 year: '2026' ... --- APC_amount: 1352,08 EUR OA_place: publisher OA_type: hybrid PlanS_conform: '1' _id: '21894' abstract: - lang: eng text: "The Dean–Kawasaki equation—one of the most fundamental SPDEs of\r\nfluctuating hydrodynamics—has been proposed as a model for density fluctuations in weakly interacting particle systems. In its original form, it is highly\r\nsingular and fails to be renormalizable, even by approaches such as regularity structures and paracontrolled distributions, hindering mathematical approaches to its rigorous justification. It has been understood recently that it is\r\nnatural to introduce a suitable regularization, for example, by applying a formal spatial discretization or by truncating high-frequency noise: This yields\r\nwell-posed equations that should still precisely approximate the law of the\r\nparticle density fluctuations.\r\nIn the present work, we prove that a regularization in the form of a formal\r\ndiscretization of the Dean–Kawasaki equation indeed accurately describes\r\ndensity fluctuations in systems of weakly interacting diffusing particles: We\r\nshow that, in suitable weak metrics, the law of fluctuations as predicted by\r\nthe discretized Dean–Kawasaki SPDE approximates the law of fluctuations\r\nof the original particle system, up to an error that is of arbitrarily high order in\r\nthe inverse particle number and a discretization error. In particular, the Dean–\r\nKawasaki equation provides a means for efficient and accurate simulations of\r\ndensity fluctuations in weakly interacting particle systems." acknowledgement: All authors gratefully acknowledge funding from the Austrian Science Fund (FWF) through the project F65. CR gratefully acknowledges support from the Austrian Science Fund (FWF), grants P30000, P33010, W1245. FC gratefully acknowledges funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 754411. article_processing_charge: Yes (in subscription journal) article_type: original arxiv: 1 author: - first_name: Federico full_name: Cornalba, Federico last_name: Cornalba - first_name: Julian L full_name: Fischer, Julian L id: 2C12A0B0-F248-11E8-B48F-1D18A9856A87 last_name: Fischer orcid: 0000-0002-0479-558X - first_name: Jonas full_name: Ingmanns, Jonas id: 71523d30-15b2-11ec-abd3-f80aa909d6b0 last_name: Ingmanns orcid: 0009-0008-1310-7946 - first_name: Claudia full_name: Raithel, Claudia last_name: Raithel citation: ama: Cornalba F, Fischer JL, Ingmanns J, Raithel C. Density fluctuations in weakly interacting particle systems via the Dean–Kawasaki equation. The Annals of Probability. 2026;54(1):155-215. doi:10.1214/25-aop1763 apa: Cornalba, F., Fischer, J. L., Ingmanns, J., & Raithel, C. (2026). Density fluctuations in weakly interacting particle systems via the Dean–Kawasaki equation. The Annals of Probability. Institute of Mathematical Statistics. https://doi.org/10.1214/25-aop1763 chicago: Cornalba, Federico, Julian L Fischer, Jonas Ingmanns, and Claudia Raithel. “Density Fluctuations in Weakly Interacting Particle Systems via the Dean–Kawasaki Equation.” The Annals of Probability. Institute of Mathematical Statistics, 2026. https://doi.org/10.1214/25-aop1763. ieee: F. Cornalba, J. L. Fischer, J. Ingmanns, and C. Raithel, “Density fluctuations in weakly interacting particle systems via the Dean–Kawasaki equation,” The Annals of Probability, vol. 54, no. 1. Institute of Mathematical Statistics, pp. 155–215, 2026. ista: Cornalba F, Fischer JL, Ingmanns J, Raithel C. 2026. Density fluctuations in weakly interacting particle systems via the Dean–Kawasaki equation. The Annals of Probability. 54(1), 155–215. mla: Cornalba, Federico, et al. “Density Fluctuations in Weakly Interacting Particle Systems via the Dean–Kawasaki Equation.” The Annals of Probability, vol. 54, no. 1, Institute of Mathematical Statistics, 2026, pp. 155–215, doi:10.1214/25-aop1763. short: F. Cornalba, J.L. Fischer, J. Ingmanns, C. Raithel, The Annals of Probability 54 (2026) 155–215. corr_author: '1' date_created: 2026-05-20T08:25:25Z date_published: 2026-01-01T00:00:00Z date_updated: 2026-05-21T07:21:25Z day: '01' ddc: - '510' department: - _id: JuFi doi: 10.1214/25-aop1763 ec_funded: 1 external_id: arxiv: - '2303.00429' file: - access_level: open_access checksum: 3e60c0e25a1c96342029a7d2b031505f content_type: application/pdf creator: dernst date_created: 2026-05-21T07:11:27Z date_updated: 2026-05-21T07:11:27Z file_id: '21906' file_name: 2026_AnnalsProbability_Cornalba.pdf file_size: 865745 relation: main_file success: 1 file_date_updated: 2026-05-21T07:11:27Z has_accepted_license: '1' intvolume: ' 54' issue: '1' keyword: - Weakly interacting particle systems - fluctuating hydrodynamics - Dean-Kawasaki equation - stochastic PDEs - numerical approximation language: - iso: eng month: '01' oa: 1 oa_version: Published Version page: 155-215 project: - _id: 260C2330-B435-11E9-9278-68D0E5697425 call_identifier: H2020 grant_number: '754411' name: ISTplus - Postdoctoral Fellowships - _id: fc31cba2-9c52-11eb-aca3-ff467d239cd2 grant_number: F6504 name: Taming Complexity in Partial Differential Systems publication: The Annals of Probability publication_identifier: eissn: - 2168-894X issn: - 0091-1798 publication_status: published publisher: Institute of Mathematical Statistics quality_controlled: '1' scopus_import: '1' status: public title: Density fluctuations in weakly interacting particle systems via the Dean–Kawasaki equation tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 54 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: diamond PlanS_conform: '1' _id: '21934' abstract: - lang: eng text: "An accurate characterisation of the physical properties of galaxies at cosmic dawn is key to understanding\r\nthe origin of the high abundance of UV-bright galaxies at z≳10. We exploit deep (9.1-hour exposure time)\r\nNIRSpec PRISM observations of GHZ2 to constrain the sources of ionising radiation and the properties of the\r\ninterstellar medium (ISM) in this bright, compact, and highly ionising galaxy at z=12.3. We measure with\r\nhigh significance the prominent N IV, C IV, He II, O III, C III, O II, and Ne III emission features previously\r\ndetected in shallower observations, and confirm the detection of the N III] λ1750 multiplet, yielding tight\r\nconstraints on the N/O ratio, which is found to be ≃2 times the solar value. We also detect the Mg II λ2800,\r\n[Fe IV] λ2833 and Si II λ1812 doublets, the H8+HeI λλ3889 blend, and the Si IV+O IV] λλ1400 absorption\r\ncomplex. The O III λ3133 fluorescence line is only detected in the first observing epoch, implying variability\r\non a rest-frame time span of 19 days, strongly suggesting the presence of an active nucleus. Combining the\r\nNIRSpec dataset with available optical and far-infrared constraints from MIRI and ALMA, we show that the\r\nemission spectrum of GHZ2 cannot be reproduced by single-density spectro-photometric models, even under\r\nextreme assumptions on the ionisation parameter and electron density. Multi-zone photoionisation modelling\r\nperformed with the HOMERUN code demonstrates that star formation must be occurring in a strongly stratified\r\nISM, where both low-/intermediate-density gas and high-density regions (log(ne/cm−3\r\n) ≳ 4) coexist. The\r\nGHZ2 emission landscape is consistent with either a composite star-formation plus AGN scenario, or with\r\nstar formation occurring in a combination of radiation- and matter-bounded regions. Purely radiation-bounded\r\nstellar models fail to reproduce the observed He II emission, making an additional hard ionising component\r\nunavoidable." acknowledgement: "We thank the referee for the constructive comments that\r\nhelped us improve the manuscript. We thank S. Finkelstein,\r\nY. Harikane, C. Mason, and D. Stark for the useful comments.\r\nWe thank Tony Roman (Program Coordinator) and Glenn\r\nWahlgren (NIRSpec reviewer) for the assistance in the\r\npreparation of GO-3073 observations. This work is based\r\non observations made with the NASA/ESA/CSA James\r\nWebb Space Telescope (JWST). The JWST data presented in this article were obtained from the Mikulski Archive for\r\nSpace Telescopes (MAST) at the Space Telescope Science\r\nInstitute. The specific observations analysed are associated with program JWST-GO-3073 and can be accessed\r\nvia https://doi.org/10.17909/4r6b-bx96 (first pointing) and\r\nhttps://doi:10.17909/zq4g-r525 (second pointing). We\r\nacknowledge financial support from NASA through grant\r\nJWST-ERS-1324 and JWST-GO-3073. Support was also\r\nprovided by the PRIN 2022 MUR project 2022CB3PJ3 –\r\nFirst Light And Galaxy aSsembly (FLAGS) funded by the\r\nEuropean Union – Next Generation EU, by INAF GO Grant\r\n2024 ”Revealing the nature of bright galaxies at cosmic\r\ndawn with deep JWST spectroscopy”, by INAF Mini-grant\r\n2022 “Reionization and Fundamental Cosmology with\r\nHigh-Redshift Galaxies”, and by INAF Large Grant 2022\r\n“Extragalactic Surveys with JWST”. L.N. acknowledges\r\nsupport from grant “Progetti per Avvio alla Ricerca - Tipo\r\n1, Unveiling Cosmic Dawn: Galaxy Evolution with CAPERS” (AR1241906F947685). EV acknowledges financial\r\nsupport through grants INAF GO Grant 2024 “Mapping Star\r\nCluster Feedback in a Galaxy 450 Myr after the Big Bang”\r\nand by the European Union – NextGenerationEU within\r\nPRIN 2022 project n.20229YBSAN - Globular clusters\r\nin cosmological simulations and lensed fields: from their\r\nbirth to the present epoch. AM acknowledges support\r\nfrom project PRIN-MUR project “PROMETEUS” financed\r\nby the European Union - Next Generation EU, Mission 4\r\nComponent 1 CUP B53D2300475000. AM acknowledges\r\nsupport from Ricerca Fondamentale INAF under Mini Grant\r\n2023 ”Quantitative Spectroscopy of Ionized Nebulae and\r\nGalaxies (QSING)” and under Data Analysis Grant 2024\r\n“Accurate measurements of metallicity in galaxies with a new\r\napproach to photoionization modelling”." article_processing_charge: No article_type: original arxiv: 1 author: - first_name: M. full_name: Castellano, M. last_name: Castellano - first_name: L. full_name: Napolitano, L. last_name: Napolitano - first_name: B. full_name: Moreschini, B. last_name: Moreschini - first_name: A. full_name: Calabrò, A. last_name: Calabrò - first_name: L. full_name: Christensen, L. last_name: Christensen - first_name: M. full_name: Llerena, M. last_name: Llerena - first_name: T. J.L.C. full_name: Bakx, T. J.L.C. last_name: Bakx - first_name: F. full_name: Belfiore, F. last_name: Belfiore - first_name: D. full_name: Bevacqua, D. last_name: Bevacqua - first_name: M. full_name: Dickinson, M. last_name: Dickinson - first_name: A. full_name: Fontana, A. last_name: Fontana - first_name: G. full_name: Gandolfi, G. last_name: Gandolfi - first_name: T. full_name: Gasparetto, T. last_name: Gasparetto - first_name: A. full_name: Marconi, A. last_name: Marconi - first_name: Sara full_name: Mascia, Sara id: edaf889c-c7cd-11ef-ab1b-bb28c431bd29 last_name: Mascia - first_name: E. full_name: Merlin, E. last_name: Merlin - first_name: T. full_name: Morishita, T. last_name: Morishita - first_name: T. full_name: Nanayakkara, T. last_name: Nanayakkara - first_name: D. full_name: Paris, D. last_name: Paris - first_name: L. full_name: Pentericci, L. last_name: Pentericci - first_name: B. full_name: Pérez-Díaz, B. last_name: Pérez-Díaz - first_name: G. full_name: Roberts-Borsani, G. last_name: Roberts-Borsani - first_name: S. full_name: Rojas-Ruiz, S. last_name: Rojas-Ruiz - first_name: P. full_name: Santini, P. last_name: Santini - first_name: T. full_name: Treu, T. last_name: Treu - first_name: E. full_name: Vanzella, E. last_name: Vanzella - first_name: B. full_name: Vulcani, B. last_name: Vulcani - first_name: X. full_name: Wang, X. last_name: Wang - first_name: I. full_name: Yoon, I. last_name: Yoon - first_name: J. full_name: Zavala, J. last_name: Zavala citation: ama: Castellano M, Napolitano L, Moreschini B, et al. Investigating ionising sources and the complex interstellar medium of GHZ2 at z=12.3. The Open Journal of Astrophysics. 2026;9. doi:10.33232/001c.160281 apa: Castellano, M., Napolitano, L., Moreschini, B., Calabrò, A., Christensen, L., Llerena, M., … Zavala, J. (2026). Investigating ionising sources and the complex interstellar medium of GHZ2 at z=12.3. The Open Journal of Astrophysics. Maynooth Academic Publishing. https://doi.org/10.33232/001c.160281 chicago: Castellano, M., L. Napolitano, B. Moreschini, A. Calabrò, L. Christensen, M. Llerena, T. J.L.C. Bakx, et al. “Investigating Ionising Sources and the Complex Interstellar Medium of GHZ2 at Z=12.3.” The Open Journal of Astrophysics. Maynooth Academic Publishing, 2026. https://doi.org/10.33232/001c.160281. ieee: M. Castellano et al., “Investigating ionising sources and the complex interstellar medium of GHZ2 at z=12.3,” The Open Journal of Astrophysics, vol. 9. Maynooth Academic Publishing, 2026. ista: Castellano M, Napolitano L, Moreschini B, Calabrò A, Christensen L, Llerena M, Bakx TJLC, Belfiore F, Bevacqua D, Dickinson M, Fontana A, Gandolfi G, Gasparetto T, Marconi A, Mascia S, Merlin E, Morishita T, Nanayakkara T, Paris D, Pentericci L, Pérez-Díaz B, Roberts-Borsani G, Rojas-Ruiz S, Santini P, Treu T, Vanzella E, Vulcani B, Wang X, Yoon I, Zavala J. 2026. Investigating ionising sources and the complex interstellar medium of GHZ2 at z=12.3. The Open Journal of Astrophysics. 9. mla: Castellano, M., et al. “Investigating Ionising Sources and the Complex Interstellar Medium of GHZ2 at Z=12.3.” The Open Journal of Astrophysics, vol. 9, Maynooth Academic Publishing, 2026, doi:10.33232/001c.160281. short: M. Castellano, L. Napolitano, B. Moreschini, A. Calabrò, L. Christensen, M. Llerena, T.J.L.C. Bakx, F. Belfiore, D. Bevacqua, M. Dickinson, A. Fontana, G. Gandolfi, T. Gasparetto, A. Marconi, S. Mascia, E. Merlin, T. Morishita, T. Nanayakkara, D. Paris, L. Pentericci, B. Pérez-Díaz, G. Roberts-Borsani, S. Rojas-Ruiz, P. Santini, T. Treu, E. Vanzella, B. Vulcani, X. Wang, I. Yoon, J. Zavala, The Open Journal of Astrophysics 9 (2026). date_created: 2026-05-31T22:02:14Z date_published: 2026-04-09T00:00:00Z date_updated: 2026-06-02T06:39:53Z day: '09' ddc: - '520' department: - _id: JoMa doi: 10.33232/001c.160281 external_id: arxiv: - '2512.08490' file: - access_level: open_access checksum: ec33ca56b8836c61cb01e26893d43cbf content_type: application/pdf creator: dernst date_created: 2026-06-02T06:38:59Z date_updated: 2026-06-02T06:38:59Z file_id: '21935' file_name: 2026_OpenJourAstrophysics_Castellano.pdf file_size: 4855934 relation: main_file success: 1 file_date_updated: 2026-06-02T06:38:59Z has_accepted_license: '1' intvolume: ' 9' language: - iso: eng month: '04' oa: 1 oa_version: Published Version publication: The Open Journal of Astrophysics publication_identifier: eissn: - 2565-6120 publication_status: published publisher: Maynooth Academic Publishing quality_controlled: '1' scopus_import: '1' status: public title: Investigating ionising sources and the complex interstellar medium of GHZ2 at z=12.3 tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 9 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21928' abstract: - lang: eng text: Antibiotic combination in time and space is a key strategy to combat antimicrobial resistance. The success of such treatment designs requires their robust efficacy across treatment conditions and a pathogen’s genomic diversity. This study found that an initial treatment with a β-lactam antibiotic causes robust cellular sensitization towards an aminoglycoside antibiotic across the high-risk human pathogen Pseudomonas aeruginosa, including resistant strains. This phenomenon of cellular sensitization, termed negative hysteresis, is modulated by the Cpx envelope stress response system and linked to membrane stress during growth. The increase in efficacy is achieved through a β-lactam induced elevated cellular uptake of the subsequently administered aminoglycoside. Negative hysteresis and the Cpx system are linked in several cases to the expression of synergistic drug interactions, thus enhancing efficacy of antibiotic combinations. Overall, our study identifies the phenomenon of negative hysteresis as a robustly inducible phenotype and thus a unique focus for optimizing antimicrobial therapy. acknowledgement: "We are very grateful to S. Hernando-Amado (Madrid, Spain), C. Pál (Szeged, Hungary), and T. Bollenbach (Cologne, Germany) for critical comments and advice on the manuscript. We further thank D. Rogers, J. Summers (Ploen, Germany) for guidance in allelic exchange, P. Rainey (Ploen, Germany) for providing the plasmids and strains, then J. Lorenzen, K. Flinder, N. Steinbach, S. Butze (all Schulenburg lab), and L. Kirchhoff (Rupp lab) for supporting the experimental work, and also the Rupp and Schulenburg groups for general feedback. We are grateful for financial support from the German Research Foundation within the Research and Training Group 2501 (RTG 2501) on Translational Evolutionary Research (project 4.2 to H.S.), within the Excellence cluster Precision Medicine in chronic Inflammation (PMI; funding under Germany’s Excellence Strategy EXC 2167-390884018, to B.K., K.R., J.R., H.S.), within the Clinician Scientist Program in Evolutionary Medicine (CSEM) – project number 413490537 (to EEG), and as part of the individual grants SCHU 1415/12-2 (to H.S.) and BR-2915/7-1 (to M.B.). We are grateful for financial support from the Swedish Research Council, project number 2021-02091 (to D.I.A.). We are also grateful for financial support from the Max-Planck Society (Fellowship to H.S.), the Leibniz Association within the Leibniz Science-Campus Evolutionary Medicine of the Lung (EvoLUNG, to H.S.), and the project SKILLED funded by the DAMP foundation (to J.R., H.S.). This work was also supported by the ZMB Young Scientist award and the FWF grant 10.55776/ESP219 (to R.R.) and the TransEvo Innovation prize (to F.B.). The funders had no role in study design, data collection and interpretation, or the decision to submit the work for publication. Open Access funding enabled and organized by Projekt DEAL.\r\n" article_number: '4487' article_processing_charge: Yes (via OA deal) article_type: original author: - first_name: Florian full_name: Buchholz, Florian last_name: Buchholz - first_name: Lina M. full_name: Upterworth, Lina M. last_name: Upterworth - first_name: Leif full_name: Tueffers, Leif last_name: Tueffers - first_name: Espen E. full_name: Groth, Espen E. last_name: Groth - first_name: Kira full_name: Haas, Kira last_name: Haas - first_name: Daniel full_name: Schütz, Daniel last_name: Schütz - first_name: Abigail full_name: Savietto Scholz, Abigail last_name: Savietto Scholz - first_name: Aditi full_name: Batra, Aditi last_name: Batra - first_name: Surajit full_name: Pal, Surajit last_name: Pal - first_name: Samarpita full_name: Banerjee, Samarpita last_name: Banerjee - first_name: Badri N. full_name: Dubey, Badri N. last_name: Dubey - first_name: Sören full_name: Franzenburg, Sören last_name: Franzenburg - first_name: Barbara full_name: Kalsdorf, Barbara last_name: Kalsdorf - first_name: Klaus F. full_name: Rabe, Klaus F. last_name: Rabe - first_name: Dennis full_name: Nurjadi, Dennis last_name: Nurjadi - first_name: Jan full_name: Rupp, Jan last_name: Rupp - first_name: Dan I. full_name: Andersson, Dan I. last_name: Andersson - first_name: Holger full_name: Sondermann, Holger last_name: Sondermann - first_name: Marc full_name: Bramkamp, Marc last_name: Bramkamp - first_name: Roderich full_name: Römhild, Roderich id: 68E56E44-62B0-11EA-B963-444F3DDC885E last_name: Römhild orcid: 0000-0001-9480-5261 - first_name: Hinrich full_name: Schulenburg, Hinrich last_name: Schulenburg citation: ama: Buchholz F, Upterworth LM, Tueffers L, et al. Robust antibiotic sensitization of pathogenic Pseudomonas aeruginosa via negative hysteresis in the cell envelope. Nature Communications. 2026;17. doi:10.1038/s41467-026-71178-5 apa: Buchholz, F., Upterworth, L. M., Tueffers, L., Groth, E. E., Haas, K., Schütz, D., … Schulenburg, H. (2026). Robust antibiotic sensitization of pathogenic Pseudomonas aeruginosa via negative hysteresis in the cell envelope. Nature Communications. Springer Nature. https://doi.org/10.1038/s41467-026-71178-5 chicago: Buchholz, Florian, Lina M. Upterworth, Leif Tueffers, Espen E. Groth, Kira Haas, Daniel Schütz, Abigail Savietto Scholz, et al. “Robust Antibiotic Sensitization of Pathogenic Pseudomonas Aeruginosa via Negative Hysteresis in the Cell Envelope.” Nature Communications. Springer Nature, 2026. https://doi.org/10.1038/s41467-026-71178-5. ieee: F. Buchholz et al., “Robust antibiotic sensitization of pathogenic Pseudomonas aeruginosa via negative hysteresis in the cell envelope,” Nature Communications, vol. 17. Springer Nature, 2026. ista: Buchholz F, Upterworth LM, Tueffers L, Groth EE, Haas K, Schütz D, Savietto Scholz A, Batra A, Pal S, Banerjee S, Dubey BN, Franzenburg S, Kalsdorf B, Rabe KF, Nurjadi D, Rupp J, Andersson DI, Sondermann H, Bramkamp M, Römhild R, Schulenburg H. 2026. Robust antibiotic sensitization of pathogenic Pseudomonas aeruginosa via negative hysteresis in the cell envelope. Nature Communications. 17, 4487. mla: Buchholz, Florian, et al. “Robust Antibiotic Sensitization of Pathogenic Pseudomonas Aeruginosa via Negative Hysteresis in the Cell Envelope.” Nature Communications, vol. 17, 4487, Springer Nature, 2026, doi:10.1038/s41467-026-71178-5. short: F. Buchholz, L.M. Upterworth, L. Tueffers, E.E. Groth, K. Haas, D. Schütz, A. Savietto Scholz, A. Batra, S. Pal, S. Banerjee, B.N. Dubey, S. Franzenburg, B. Kalsdorf, K.F. Rabe, D. Nurjadi, J. Rupp, D.I. Andersson, H. Sondermann, M. Bramkamp, R. Römhild, H. Schulenburg, Nature Communications 17 (2026). corr_author: '1' date_created: 2026-05-31T22:02:12Z date_published: 2026-05-20T00:00:00Z date_updated: 2026-06-02T07:14:35Z day: '20' ddc: - '570' department: - _id: CaGu doi: 10.1038/s41467-026-71178-5 file: - access_level: open_access checksum: aa29f8806908dc0469dff21e2d5ad01f content_type: application/pdf creator: dernst date_created: 2026-06-02T07:11:12Z date_updated: 2026-06-02T07:11:12Z file_id: '21936' file_name: 2026_NatureComm_Buchholz.pdf file_size: 1276166 relation: main_file success: 1 file_date_updated: 2026-06-02T07:11:12Z has_accepted_license: '1' intvolume: ' 17' language: - iso: eng month: '05' oa: 1 oa_version: Published Version project: - _id: bd6f94d1-d553-11ed-ba76-ae9f07250f74 grant_number: E219 name: Non-canonical antibiotic interactions publication: Nature Communications publication_identifier: eissn: - 2041-1723 publication_status: published publisher: Springer Nature quality_controlled: '1' scopus_import: '1' status: public title: Robust antibiotic sensitization of pathogenic Pseudomonas aeruginosa via negative hysteresis in the cell envelope tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 17 year: '2026' ... --- OA_place: repository OA_type: green _id: '21921' abstract: - lang: eng text: "A variety of problems in geometry processing boil down to finding the most\r\nparallel field relative to a connection. Instances of this prototypical problem\r\nshow up in computing direction fields and stripe patterns, quadrilateral\r\nmeshing, and visualization of fluid flows. When the class of allowed fields\r\nincludes those with topological defects, a relaxation is required to make\r\nthe problem well-posed. We observe that these problems can be viewed\r\nas synchronization problems, which admit a natural semidefinite relaxation.\r\nWe propose a unified method of solving all these problems via the efficient\r\nBurer-Monteiro factorization method. Geometrically, this amounts to lifting the field values to a higher-dimensional manifold, naturally resolving\r\nthe singular nature of defects. Practically, we show that our convex relaxation method achieves better and more reliable optima than previous work\r\nemploying alternative relaxations" acknowledgement: "The authors thank Steven J. Gortler and Nicolas Boumal for interesting discussions.\r\nDavid Palmer acknowledges the generous support of the NSF\r\nMSPRF under award #2303403 during his time at Harvard University.\r\nNatalia Pacheco-Tallaj was supported by the NSF DGE-2141064.\r\nMattéo Couplet was supported by Wallonie-Bruxelles International" article_processing_charge: No author: - first_name: Natalia full_name: Pacheco-Tallaj, Natalia last_name: Pacheco-Tallaj - first_name: Matteo full_name: Couplet, Matteo last_name: Couplet - first_name: Edward full_name: Chien, Edward last_name: Chien - first_name: David full_name: Palmer, David id: 6574708f-2fd3-11f0-89e2-ae42ebc712a4 last_name: Palmer orcid: 0000-0002-1931-5673 citation: ama: 'Pacheco-Tallaj N, Couplet M, Chien E, Palmer D. Synchronizing fields with singularities. In: SIGGRAPH Conference Papers. ACM. doi:10.1145/3799902.3811225' apa: 'Pacheco-Tallaj, N., Couplet, M., Chien, E., & Palmer, D. (n.d.). Synchronizing fields with singularities. In SIGGRAPH Conference Papers. Los Angeles, CA, United States: ACM. https://doi.org/10.1145/3799902.3811225' chicago: Pacheco-Tallaj, Natalia, Matteo Couplet, Edward Chien, and David Palmer. “Synchronizing Fields with Singularities.” In SIGGRAPH Conference Papers. ACM, n.d. https://doi.org/10.1145/3799902.3811225. ieee: N. Pacheco-Tallaj, M. Couplet, E. Chien, and D. Palmer, “Synchronizing fields with singularities,” in SIGGRAPH Conference Papers, Los Angeles, CA, United States. ista: 'Pacheco-Tallaj N, Couplet M, Chien E, Palmer D. Synchronizing fields with singularities. SIGGRAPH Conference Papers. SIGGRAPH: International Conference and Exhibition on Computer Graphics and Interactive Techniques.' mla: Pacheco-Tallaj, Natalia, et al. “Synchronizing Fields with Singularities.” SIGGRAPH Conference Papers, ACM, doi:10.1145/3799902.3811225. short: N. Pacheco-Tallaj, M. Couplet, E. Chien, D. Palmer, in:, SIGGRAPH Conference Papers, ACM, n.d. conference: end_date: 2026-07-23 location: Los Angeles, CA, United States name: 'SIGGRAPH: International Conference and Exhibition on Computer Graphics and Interactive Techniques' start_date: 2026-07-19 corr_author: '1' date_created: 2026-05-29T12:53:59Z date_published: 2026-06-01T00:00:00Z date_updated: 2026-06-02T06:26:52Z day: '01' ddc: - '000' department: - _id: ChWo doi: 10.1145/3799902.3811225 file: - access_level: open_access checksum: 384524659fbaf3b9da80c3852ba835af content_type: application/pdf creator: dpalmer date_created: 2026-05-29T12:53:25Z date_updated: 2026-05-29T12:53:25Z file_id: '21922' file_name: main.pdf file_size: 39491071 relation: main_file file_date_updated: 2026-05-29T12:53:25Z has_accepted_license: '1' language: - iso: eng month: '06' oa: 1 oa_version: Accepted Version publication: SIGGRAPH Conference Papers publication_identifier: eisbn: - '9798400725548' publication_status: accepted publisher: ACM quality_controlled: '1' status: public title: Synchronizing fields with singularities type: conference user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 year: '2026' ... --- OA_place: repository OA_type: green _id: '21933' abstract: - lang: eng text: We consider the liquid drop model with a positive background density in the thermodynamic limit. We prove a two-term asymptotics for the ground state energy per unit volume in the dilute limit. Our proof justifies the expectation that optimal configurations consist of droplets of unit size that arrange themselves according to minimizers for the Jellium problem for point particles. In particular, we provide the first rigorous derivation of what is known as the gnocchi phase in astrophysics. article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Rupert L. full_name: Frank, Rupert L. last_name: Frank - first_name: Mathieu full_name: Lewin, Mathieu last_name: Lewin - first_name: Robert full_name: Seiringer, Robert id: 4AFD0470-F248-11E8-B48F-1D18A9856A87 last_name: Seiringer orcid: 0000-0002-6781-0521 citation: ama: Frank RL, Lewin M, Seiringer R. Liquid drop model for nuclear matter in the low density limit. Communications on Pure and Applied Mathematics. 2026. doi:10.1002/cpa.70039 apa: Frank, R. L., Lewin, M., & Seiringer, R. (2026). Liquid drop model for nuclear matter in the low density limit. Communications on Pure and Applied Mathematics. Wiley. https://doi.org/10.1002/cpa.70039 chicago: Frank, Rupert L., Mathieu Lewin, and Robert Seiringer. “Liquid Drop Model for Nuclear Matter in the Low Density Limit.” Communications on Pure and Applied Mathematics. Wiley, 2026. https://doi.org/10.1002/cpa.70039. ieee: R. L. Frank, M. Lewin, and R. Seiringer, “Liquid drop model for nuclear matter in the low density limit,” Communications on Pure and Applied Mathematics. Wiley, 2026. ista: Frank RL, Lewin M, Seiringer R. 2026. Liquid drop model for nuclear matter in the low density limit. Communications on Pure and Applied Mathematics. mla: Frank, Rupert L., et al. “Liquid Drop Model for Nuclear Matter in the Low Density Limit.” Communications on Pure and Applied Mathematics, Wiley, 2026, doi:10.1002/cpa.70039. short: R.L. Frank, M. Lewin, R. Seiringer, Communications on Pure and Applied Mathematics (2026). date_created: 2026-05-31T22:02:13Z date_published: 2026-01-01T00:00:00Z date_updated: 2026-06-02T06:58:54Z day: '01' department: - _id: RoSe doi: 10.1002/cpa.70039 external_id: arxiv: - '2507.14012' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.48550/arXiv.2507.14012 month: '01' oa: 1 oa_version: Preprint publication: Communications on Pure and Applied Mathematics publication_identifier: eissn: - 1097-0312 issn: - 0010-3640 publication_status: epub_ahead publisher: Wiley scopus_import: '1' status: public title: Liquid drop model for nuclear matter in the low density limit type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21930' abstract: - lang: eng text: "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\r\nJWST/NIRSpec medium-resolution spectroscopy from the GLIMPSE-D Survey. The exquisite signal-to-noise\r\nratio reveals multiple high-ionization nebular lines and broad Balmer and [O III] components (FWHM\r\n∼700–3000 km s\r\n−1\r\n). We detect broadened He II λ1640 and λ4687 (FWHM ∼ 530 km s\r\n−1\r\n) and strong N III λ4642\r\nemission consistent with a population of WN stars, making RXCJ2248 the most distant galaxy with confirmed\r\nWolf Rayet (WR) features to date. We measure the multiphase nebular density across five ions, the direct-method\r\nmetallicity (\r\n12 + log(O/H) = 7.753 ± 0.025\r\n), and a nonuniform elemental enrichment pattern of extreme N/O\r\nenhancement (\r\nlog(N/O) = 0.391 ± 0.037\r\nfrom N+, N+2\r\n, and N+3\r\n) but suppressed C/O relative to empirical\r\nC/N trends. We show that this abundance pattern can be explained by enrichment from a dual-burst with a low\r\nWR carbon/WN ratio, as expected at low metallicities. Crucially, these signatures can only arise during a brief,\r\nrare evolutionary window shortly after a burst (∼3–6 Myr), when WN stars dominate chemical feedback but\r\nbefore dilution by later yields (e.g., supernovae). The observed frequency of strong N emitters at high−z implies a\r\n∼50 Myr burst duty cycle, suggesting that N/O outliers may represent a brief but ubiquitous phase in the\r\nevolution of highly star-forming early galaxies. The WN detection in RXCJ2248, therefore, provides the first\r\ndirect evidence of WR-driven nitrogen enrichment in the first billion years of the Universe and a novel timing\r\nargument for the bursty star formation cycles that shaped galaxies at cosmic dawn." acknowledgement: "\r\nThe American Astronomical Society, find out more.\r\n\r\nThe following article isOpen access\r\nA Fleeting GLIMPSE of N/O Enrichment at Cosmic Dawn: Evidence for Wolf Rayet N Stars in a z = 6.1 Galaxy\r\nDanielle A. Berg, Rohan P. Naidu, John Chisholm, Hakim Atek, Seiji Fujimoto, Vasily Kokorev, Lukas J. Furtak, Chiaki Kobayashi, Daniel Schaerer, Angela Adamo, Qinyue Fei, Damien Korber, Jorryt Matthee, Rui Marques-Chaves, Zorayda Martinez, Kristen. B. W. McQuinn, Julian B. Muñoz, Pascal A. Oesch, Alberto Saldana-Lopez, Daniel P. Stark, Mabel G. Stephenson, and Tiger Yu-Yang HsiaoHide full author list\r\n\r\nPublished 2026 May 20 • © 2026. The Author(s). Published by the American Astronomical Society.\r\nThe Astrophysical Journal, Volume 1003, Number 2\r\nCitation Danielle A. Berg et al 2026 ApJ 1003 112\r\nDOI 10.3847/1538-4357/ae5e4c\r\n\r\nDownloadArticle PDFDownloadArticle ePub\r\nAuthors\r\nFigures\r\nTables\r\nReferences\r\nArticle data\r\nDownload PDFDownload ePub\r\nArticle metrics\r\n173 Total downloads\r\n\r\nShare this article\r\nArticle information\r\nAbstract\r\nWe 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 (\r\n), and a nonuniform elemental enrichment pattern of extreme N/O enhancement (\r\n 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.\r\n\r\nExport citation and abstract\r\nBibTeXRIS\r\n\r\nPrevious article in issue\r\nNext article in issue\r\n\r\nOriginal content from this work may be used under the terms of the Creative Commons Attribution 4.0 licence. Any further distribution of this work must maintain attribution to the author(s) and the title of the work, journal citation and DOI.\r\n\r\n1. Introduction\r\nA key tracer of galaxy evolution is the change in their chemical composition over time. The metallicity of a galaxy is a sensitive observational diagnostic of its past star formation history and present-day evolutionary state given that metallicity increases with each successive generation of massive star yields (e.g., M. Tosi 1988; J.-R. Roy & D. Kunth 1995; D. A. Berg et al. 2019; R. Maiolino & F. Mannucci 2019). Oxygen is an important tracer of metallicity because it is the most abundant element in the Universe after H and He and is convenient to observe, with ubiquitous emission lines from H ii regions in the rest-frame optical regime. While O emission in dwarf and spiral galaxies has been widely observed in the rest-frame optical and UV (e.g., R. C. Kennicutt 1992; Y. I. Izotov & T. X. Thuan 1999; L. van Zee & M. Haynes2006; D. A. Berg et al. 2012, 2016, 2019; P. Senchyna et al. 2017; N. S. J. Rogers et al. 2022), the N emission in these same galaxies has been predominantly traced only in the optical through the low-ionization [N ii] λλ6550,6585 emission lines. In general, there is a surprising dearth of detections of the high-ionization N emission counterparts in local galaxies, totaling less than 10 galaxies with significant detections of either N iv] λλ1483,1486 or N iii] λ1750 (e.g., M. Mingozzi et al. 2022; Z. Martinez et al. 2025). However, with the advent of JWST, there is a growing prevalence of z ≳ 5 galaxies with extreme properties, including intense UV N emission (e.g., A. J. Bunker et al. 2023; Y. Isobe et al. 2023; M. Castellano et al. 2024; T. Y.-Y. Hsiao et al. 2024; X. Ji et al. 2024; R. Marques-Chaves et al. 2024; D. Schaerer et al. 2024; M. Curti et al. 2025a; Y. Harikane et al. 2025a; R. P. Naidu et al. 2026; M. W. Topping et al. 2025b).\r\n\r\nThe first noted, and one of the most distant, examples of extreme rest-frame UV N emission comes from the spectroscopically confirmed z = 10.6 galaxy, GN-z11. JWST spectra of GN-z11 revealed surprisingly strong N iv] λλ1483,1486 and N iii] λ1750 emission (e.g., A. J. Bunker et al. 2023) that corresponds to supersolar nitrogen-to-oxygen (N/O) enrichment (\r\n; e.g., A. J. Cameron et al. 2023). Subsequently, enhanced N/O has been reported in a number of high−z galaxies, including GDS 3073 (z = 5.55; X. Ji et al. 2024), RXCJ2248-ID (z = 6.10; M. W. Topping et al. 2024), A1703-zd6 (z = 7.04; M. W. Topping et al. 2025b), CEERS-1019 (z = 8.68; R. Marques-Chaves et al. 2024), GNz9p4 (z = 9.38; D. Schaerer et al. 2024), GHZ9 (z = 10.15; L. Napolitano et al. 2025), GHZ2 (z = 12.34; M. Castellano et al. 2024), and MoM-z14 (z = 14.44; R. P. Naidu et al. 2026). For a review of nitrogen line detections, see D. P. Stark et al. (2025). Such strong nebular N+3 emission requires a relatively hard ionizing radiation field (≳47.4 eV), where models of massive stars predict few photons. On the other hand, N+2 has a lower ionization potential (∼29.6 eV), but statistically significant detections are strikingly rare in integrated galaxy spectra (e.g., D. A. Berg et al. 2018; M. Mingozzi et al. 2022; A. J. Bunker et al. 2023; P. Senchyna et al. 2024) and are only expected to be strong at the highest possible nebular temperatures (∼2.5 × 104 K). Furthermore, the timing of the incredibly high N/O abundances reported for the high-redshift UV N emitters just a few 100 Myr after the Big Bang is unexpected.\r\n\r\nThe discovery of significant, rapid nitrogen enhancement so early in the Universe was surprising because it contradicts our longstanding understanding of N production. In typical chemical evolution modeling, some nitrogen enrichment can occur early on via core collapse supernova (CCSN), but substantial nitrogen enrichment only occurs 100 s of megayears after the onset of star formation via asymptotic giant branch (AGB) stars (e.g., F. Vincenzo et al. 2019; C. Kobayashi et al. 2020). Thus, alternative, faster enrichment methods are needed to explain substantial nitrogen enrichment in early galaxies. As a result, the necessary ionizing flux and conditions to produce the unexpectedly strong N+3 and N+2 emission observed in galaxies beyond z ∼ 5 have been attributed to more extreme sources, such as active galactic nuclei (AGN; R. Maiolino et al. 2024), Wolf Rayet (WR) stars (e.g., P. Senchyna et al. 2024; K. Watanabe et al. 2024; M. L. P. Gunawardhana et al. 2025), globular cluster precursors (e.g., C. Charbonnel et al. 2023; X. Ji et al. 2026), super star clusters (e.g., M. Pascale et al. 2023), very massive stars (VMSs: M⋆ > 102 M⊙; e.g., J. S. Vink 2023; Y. Shi et al. 2026), or supermassive stars (M⋆ > 103 M⊙; e.g., C. Charbonnel et al. 2023; C. Nagele & H. Umeda 2023), tidal disruption events (e.g., A. J. Cameron et al. 2023; K. Watanabe et al. 2024), and more.\r\n\r\nMost of our understanding of WR stars has been built from observations of individual resolved stars in a handful of galaxies in the Local Group, with almost no direct spectroscopic evidence for the prevalence of WR stars in more distant galaxies. To date, only two systems at Cosmic Noon (z ≈ 2–3) have confirmed signatures of WR stars: MARTA-4327 at z = 2.224 (hereafter, M4327; M. Curti et al. 2025b) and the Sunburst Arc at z = 2.37 (T. E. Rivera-Thorsen et al. 2024). Extending such detections to earlier cosmic epochs is crucial for understanding the role of massive stars in shaping the chemical evolution of galaxies in the first Gyr.\r\n\r\nHere, we investigate the z = 6.1 lensed galaxy RXCJ2248-ID3. RXCJ2248-ID was first identified by F. Boone et al. (2013), I. Balestra et al. (2013), and A. Monna et al. (2014) and discovered to be a high-ionization, compact, metal-poor, N-enhanced galaxy by R. Mainali et al. (2017), K. B. Schmidt et al. (2017), and M. W. Topping et al. (2024). We present extremely deep JWST/NIRSpec observations of RXCJ2248-ID3 that provide the highest-redshift spectroscopic evidence of WR nitrogen (WN) stars to date, which provide a physically consistent mechanism driving its extreme nitrogen enrichment (M. W. Topping et al. 2024). The remainder of this paper is organized as follows. The observations and data reduction are briefly described in Section 2.1, followed by a description of the emission-line fits, including the broad lines related to the WR feedback, in Section 2.2. We present the discovery of WN stars at z ∼ 6 via their spectral signatures in Section 3. We determine new nebular properties and O, C, N, and Si abundances in Section 4.3 and compare them to populations of both low- and high-redshift galaxies. We discuss the source of N enrichment in the early Universe and subsequently estimate mass production and timing arguments in Section 5. Finally, we present our conclusions in Section 6. Throughout this work, we adopt cosmological parameters of H0 = 70 km s−1 Mpc−1, Ωm = 0.30, and ΩΛ = 0.7 and the solar abundance pattern from M. Asplund et al. (2021).\r\n\r\n2. JWST/NIRSpec Spectra\r\nRXCJ2248 is a galaxy at z ∼ 6.1 that is lensed into multiple images by the Abell S1063 cluster (α = 22:48:44.13, δ =−44:31:57.50) at a redshift of z = 0.348. We present an analysis of the brightest image, RXCJ2248-ID3 (J = 25.0), which has a magnification of μ ∼ 7 (L. Furtak et al. 2025). RXCJ2248-ID was discovered as a z ∼ 6 candidate (F. Boone et al. 2013; A. Monna et al. 2014) using the 16-band HST photometry of the CLASH Survey and spectroscopically confirmed via VIsible Multi-Object Spectrograph (VIMOS)/VLT observations by I. Balestra et al. (2013). RXCJ2248-ID3 was soon found to be an exciting extreme emission-line galaxy via ground-based spectroscopy (R. Mainali et al. 2017), with strong detections of high-ionization emission such as O iii] λλ1661,1666 and C ivλλ1548,1550 but no He ii, suggesting star formation as the ionizing source rather than an AGN.\r\n\r\nThe early spectra of RXCJ2248-ID3 motivated further rest-UV+optical study with JWST/NIRSpec by M. W. Topping et al. (2024). This work performed direct metallicity calculations to show that RXCJ2248-ID3 is one of the most extreme N/O-enhanced (), metal-poor () galaxies, with high-ionization ([O iii] λ5008/[O ii] λ3728 = 184) and high nebular density (6.4 × 104 ≤ ne(cm−3) ≤3.1 × 105). They also used spectral energy distribution (SED) fitting with a constant star formation history to characterize its low stellar mass (M⋆ ∼ 108 M⊙) and the young-massive star population (∼2 Myr) of RXCJ2248. M. W. Topping et al. (2024), therefore, suggest that the N/O enrichment may be due to a short-lived phase that many z > 6 bursty galaxies experience. In this paper, we build on the work of M. W. Topping et al. (2024) with new, extraordinarily deep rest-optical JWST/NIRSpec observations of RXCJ2248-ID3 from the GLIMPSE-D Survey, a Director’s Discretionary Time (DDT) follow-up program described below.\r\n\r\n2.1. Observations and Reduction\r\nThe work presented here uses both the rest-UV JWST/NIRSpec archival spectra from JWST PID 2478 (PI Stark) and new rest-optical JWST/NIRSpec spectra from the GLIMPSE-D Survey, which is an extension of the GLIMPSE Survey. Properties of RXCJ2248-ID and observation details are presented in Table 1.\r\n\r\nTable 1. Properties of RXCJ2248-ID3\r\n\r\nJWST/NIRSpec Observations\r\nGrating/Filter\t(s)\tPI/PID\r\nG140M/F100LP\t6215\tStark/2478\r\nG235M/F170LP\t1576\tStark/2478\r\nG395M/F290LP\t107,228\tFujimoto & Naidu/9223\r\nMeasured Properties\r\nProperty\tValue\tReferences\r\nR.A.\t+22:48:45.81\tThis work\r\nDecl.\t−44:32:14.95\tThis work\r\nz\t6.1025 ± 0.0013\tThis work\r\nμ\t6.8877\tL. Furtak et al. (2025)\r\nReff (pc)\t\tA. Claeyssens (2025)\r\nM⋆ (M⊙)\t\tA. Claeyssens (2025)\r\nΣ⋆ (M⊙ pc−2)\t\tA. Claeyssens (2025)\r\nSFRHα (M⊙ yr−1)\t3.2\tThis work, Section 5.3\r\nSFRSED,1Myr\t4.7\tA. Claeyssens (2025)\r\nSFRSED,10Myr\t4.1\tA. Claeyssens (2025)\r\nΣSFR (M⊙ yr−1 kpc−2)\t1.34 × 103\tThis work\r\ntage (Myr)\t\tA. Claeyssens (2025)\r\n12+log(O/H)\t7.753 ± 0.025\tThis work, Section 4.3.1\r\nlog(N/O)\t−0.391 ± 0.037\tThis work, Section 4.3.2\r\nNote. Top: JWST/NIRSpec observations of RXCJ2248-ID3, including archival observations from PID 2478 (PI: Stark) and very deep GLIMPSE-D observations from PID 9223 (PI: Fujimoto & Naidu). Columns (1)–(3) list the grating/filter, exposure time, and principle investigator/PID. Bottom: Measured global properties of RXCJ2248-ID3. The R.A. and decl. are the extraction coordinates for RXCJ2248-ID3. The redshift was determined from the GLIMPSE-D spectrum emission lines. GLIMPSE imaging was used to determine the lensing model magnification, μ. Effective radius of the RXCJ2248-ID3 clump, stellar mass, and current massive star population age are from the SED modeling of A. Claeyssens (2025), while the SFR was determined from both the SED fitting and the narrow-component, collisions-corrected Hα flux (see Section 5.3), all corrected for the lensing factor. The star formation rate surface density was determined using the SFRHα. The metallicity and relative N/O abundance were determined using the direct method.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nThe GLIMPSE Survey is a large Cycle 2 JWST program (PID 3293; PIs Atek & Chisholm) that performed ultradeep NIRCam imaging (∼30.8 mag at 5σ over 0.8–5 μm) in seven broadband and two medium-band filters of the lensing cluster Abell S1063 (H. Atek et al. 2025). A. Claeyssens (2025) performed size and photometric measurements of RXCJ2248-ID in the different multiple images. The SED fitting was performed with the Bayesian Analysis of Galaxies for Physical Inference and Parameter Estimation (BAGPIPES; A. C. Carnall et al. 2018) code with Binary Population and Spectral Synthesis (BPASS v2.14, J. J. Eldridge et al. 2017) stellar population synthesis burst models and cloudy v23.01 photoionization models (M. Chatzikos et al. 2023; C. M. Gunasekera et al. 2023). Priors were used to be physically consistent with the source, i.e., high-ionization parameter (), low extinction (Av < 0.5 mag), low metallicity (Z < 0.4 Z⊙), and bursty star formation (τ = 1 Myr, i.e., close to a single burst, or τ = 10 Myr). The resulting best fit has a young age ( Myr) and low stellar mass of but within a compact size of pc such that the stellar mass surface density is . This value is akin to the highest densities found in globular clusters, similar to the ones reported for young star clusters and clumps at high redshift (A. Claeyssens et al. 2025; M. Messa et al. 2026), and broadly consistent with the conclusions presented in M. W. Topping et al. (2024).\r\n\r\nSubsequent medium-resolution (R ∼ 1000) spectra of RXCJ2248-ID3 were obtained as part of the follow-up GLIMPSE-D Survey: JWST DDT Program 9223 (PIs Fujimoto & Naidu) targeting a Pop III candidate in S. Fujimoto et al. (2025) using NIRSpec Multi-Object Spectroscopy (MOS) with the G395M grating and F290LP filter. As part of this program, RXCJ2248-ID3 was observed for a total of 13 exposures using a 3-point nod pattern and NRSIRS2 readout, totaling ∼30 hr of integration. The MSA slit positions covering RXCJ2248-ID3 of the three pointings are shown in Figure 1.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 1. JWST/NIRSpec MSA slits targeting RXCJ2248-ID3 for each of the three exposures in the GLIMPSE-D program. The two pointings that are closely aligned (solid purple regions) have the same wavelength coverage, while the pointing offset to the lower left (dashed region) has somewhat reduced blue coverage. All three pointings were used in the spectrum coaddition.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nWe augment the rest-optical GLIMPSE-D data with archival rest-far-UV G140M/F100LP and rest-near-UV G235M/F170LP observations from PID 2478 (PI Stark), covering the rest-frame ∼1400–4000 Å range. This program also observed the G395M/F290LP setting, but we only use the significantly deeper GLIMPSE-D G395M observations here. Multiple images of RXCJ2248 were identified and observed in program #2478. M. W. Topping et al. (2024) utilized these data by coadding the spectra of the individual images. In contrast, only the brightest image (ID3) was observed in the GLIMPSE-D Survey. To ensure consistency, we therefore restricted our analysis to the G140M and G235M spectra of ID3 obtained in program #2478. As a result, our G140M and G235M measurements are not directly comparable to those presented by M. W. Topping et al. (2024).\r\n\r\nThe data were reduced using v0.9.8 of the msaexp pipeline (G. Brammer 2022), following the standard routines described in A. de Graaff et al. (2025), K. E. Heintz et al. (2025), and F. Valentino et al. (2025). Briefly, level-2 calibrated products from MAST are subject to a series of custom corrections that account for, e.g., 1/f noise, bar vignetting, and detector bias. We used the “local” nodded background subtraction. The 2D spectra were drizzled onto a common wavelength grid and 1D spectra were optimally extracted using a profile model that accounts for, e.g., the wavelength-dependent PSF and offsets from the nominal position expected from the catalog. Line centers were measured for the strongest emission lines in the G395M spectrum (i.e., Hδ, Hγ, [O iii] λ4364, Hβ, [O iii] λλ4960,5008, He iλ5877, Hα, He iλ7067) and used to determine a redshift of z = 6.1025 ± 0.0013. Note that the bluest portion of the G395M tends to favor a slightly lower redshift (i.e., z ∼ 6.1000), while the reddest portion favors a slightly higher redshift (i.e., z ∼ 6.1034). The three individual 1D extracted spectra were then normalized to the common continuum flux scale of the first spectrum at rest-wavelengths of ∼6000–62000 Å prior to coadding. Spectral coaddition was performed as a weighted average using the inverse variance as the weight.\r\n\r\nThe resulting spectrum, shown in Figure 2, covers an observed wavelength range ∼2.8–5.5 μm, which corresponds to a rest-optical range of ∼3900–7740 Å. Note that the third pointing (dashed slits in Figure 1) has reduced wavelength coverage such that the blue end begins at ∼4265. The deep GLIMPSE-D spectra provide unparalleled signal-to-noise ratio (S/N; >5 at 5100 Å continuum) that enable rest-optical diagnostics typically reserved for nearby galaxies.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 2. JWST/NIRSpec rest-frame UV and optical spectra of RXCJ2248-ID3 highlighting the first object known with simultaneously detected emission from N+, N+2, and N+3 (see, also, M. W. Topping et al. 2024) and WR features. The second row shows the main emission UV emission-line detections from the archival G140M/F100LP spectrum, with significant detections of several high-ionization emission lines, including N iv] λλ1483,1486, C iv λλ1548,1550, He ii λ1640, O iii] λλ1661,1666, N iii] λ1750, and C iii] λλ1907,1909. The third row shows the blue end of the optical spectrum, where the left-hand panel shows the archival G235M/F170LP spectrum, which includes the low-ionization [O ii] λλ3727,3730 doublet. The right-hand panel of the third row and the fourth row shows the extremely high S/N GLIMPSE-D optical spectrum, enabling detections of several weak features. Note that some of the important features to this work are highlighted in the zoom in panels in the top row. In particular, the last panel reveals the most distant WR detection to date, with the λ4650 WR bump showing emission from N iii λ4642, indicative of nitrogen enrichment from WN stars. Note that not all of the labeled lines correspond to line detections.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n2.2. Emission-line Measurements\r\nIn order to perform a consistent analysis of our data, we measure emission-line fluxes for both the archival spectra and the new GLIMPSE-D spectra presented here. We fit neighboring emission lines simultaneously using Gaussian profiles with the lmfit package (M. Newville et al. 2015) in Python. Purely nebular lines (i.e., lines without possible stellar contributions or resonant effects) close in wavelengths were constrained to have the same full width at half-maximum (FWHM) velocity widths. Additionally, the relative wavelength spacing between lines was constrained to laboratory values and doublets with constant flux ratios set by atomic physics were constrained to their theoretical values, with small uncertainty allowances. The uncertainties on the line fluxes were estimated as the standard error derived from the least-squares minimization in lmfit, which considers the uncertainty on the Gaussian profile and linear continuum.\r\n\r\nBroad emission components are clearly visible at the base of some of the emission lines in the GLIMPSE-D spectrum of RXCJ2248-ID3. Such broad emission features can be produced by stellar winds, shocks, or turbulence. Since He iiλ1640 and λ4687 emission lines can be affected by stellar winds, we fit these features with an unconstrained Gaussian width. Using the jwst-msa package (A. de Graaff et al. 2024), we deconvolved all measured FWHMs with the modeled wavelength-dependent line spread function (LSF). We found the He ii lines to be broadened compared to purely nebular lines. For the He iiλ 4687 line, the velocity width is 528 ± 100 km s−1, which is more than two times broader than the narrow nebular Hβ component with vFWHM = 243 ± 25 km s−1.\r\n\r\nThe strongest rest-optical H (Hγ, Hβ, and Hα) and [O iii] (λ4364, λλ4960,5008) emission lines have complex profiles with both narrow and broad emission components. Such broad components may also be present in the rest-UV and fainter rest-optical emission lines, but none are obvious given the lower S/N of these emission features and/or underlying continuum. To fit these profiles, we tested three different multicomponent profile combination fits for the Hα + [N ii] complex. For all three fits, the narrow Hα and [N ii] λλ6550,6585 lines were fit by Gaussians with a single velocity width, but the broad component was fit with either: (1) a single Gaussian profile, (2) two Gaussian profiles, or (3) a single exponential profile. The single broad Gaussian profile fit had strong residuals near the center of the broad component, so did not provide a good fit to the observed emission profile. Both the double Gaussian profile and the exponential profile provided relatively good visual fits, but the double Gaussian fit had a lower reduced chi-squared ( vs ) and Bayesian inference criteria (BIC2Gauss = 36 versus (BICexp. = 87), and so was adopted as the better statistical fit.\r\n\r\nThe right panel of Figure 3 shows the best multicomponent fit to the Hα + [N ii] complex. Since all kinematically similar lines in the Balmer emission series arise from the same gas, we expect the Hβ and Hγ profiles to be well fit by scaling the Hα best fit. Therefore, we constrained the velocity widths of the Hβ and Hγ emission components to match the narrow + double broad Gaussian Hα fit, accounting for the wavelength-dependent LSF. We found excellent fit results, with similarly small reduced-χ2 and BIC values. This means that the H i lines are well fit by a profile with (1) a strong, narrow (∼250 km s−1) nebular component, (2) a moderate (∼20% of total flux), broad component (∼670 km s−1), and (3) a weak (∼10% of total flux), very broad (∼2530 km s−1) component.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 3. Multicomponent emission-line fits to the GLIMPSE spectrum of RXCJ2248-ID for Hα λ6565 + [N II] λλ6549,6585 (left panels), Hβ λ4863 + [O III] λλ4960,5008 (middle panels), and Hγ λ4342 + [O III] λ4364 (right panels). When fit with single, narrow Gaussian components (e.g., purple and yellow filled Gaussians), all three line complexes show strong, broad component residual flux. The resulting best fit to each line is comprised of a single narrow Gaussian plus two broad Gaussians, where the relevant component velocity widths are tied together: The Hα λ6565 + [N ii] λλ6549,6585 complex fit provided the velocity width constraints for the H Balmer line narrow (purple Gaussians) and broad components (blue and green Gaussians) and, subsequently, the Hβ λ4863 + [O iii] λλ4960,5008 fit constrained the [O iii] narrow (yellow Gaussian) and broad (orange and red Gaussians) velocity widths that were then used in the Hγ λ4342 + [O iii] λ4364 fit. Note that additional faint lines (e.g., He i λ5017) were included in the fit in the middle panel. Careful accounting for the residual broad flux has a significant impact on the derived nebular reddening, temperature, metallicity, and N/O abundance.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nThe [O iii] λλ4960,5008 doublet lines are also well fit by a narrow Gaussian plus double Gaussian broad component profile, with the relative fluxes of each component constrained to the theoretical ratio. While the narrow-component FWHM was set to the velocity width of the narrow Balmer lines, convolved with the LSF, we allowed the FWHM of the two broad [O iii] components to vary freely and found widths of ∼890 km s−1 and ∼2980 km s−1, respectively. The similarity between the [O iii] and H i velocity widths of the broad components argues against emission from an AGN directly (where high densities cause collisional de-excitation of [O iii]) and is more consistent with stellar or AGN driven winds (e.g., Y. I. Izotov & T. X. Thuan 2008; G. Gräfener & J. S. Vink2015; G. Gräfener et al. 2017; C. J. Burke et al. 2021). Interestingly, the broad components of the H i lines compose a larger fraction of their total flux (∼20% and 10%, respectively) than [O iii] (∼10% and 5%, respectively).\r\n\r\nThe resulting fit to the Hβ + [O iii] λλ4960,5008 complex is shown in the middle panel of Figure 3 to be an excellent fit, with minimal residuals. The exquisite S/N of the GLIMPSE spectrum also reveals broad wings on the [O iii] λ4364 profile, as seen in the left panel of Figure 3. Therefore, we also applied the narrow Gaussian plus double Gaussian broad component profile to [O iii] λ4364, constraining the velocity widths to the values measured for [O iii] λλ4960,5008.\r\n\r\nDouble broad components with similar velocity widths (750 and 2500 km s−1, respectively) are seen in the z ∼ 0 extreme emission-line galaxies, J1044+0353 and J1418+2102, reported in D. A. Berg et al. (2021). However, each broad component observed in these nearby analogs only accounts for 1%–3% of the total H i flux. This sort of broad component emission from the Balmer H and [O iii] lines with widths (1000–2000 km s−1) and fractional fluxes of 1%–2% is commonly found in spectra of blue compact dwarf galaxies (BCDs; e.g., Y. I. Izotov et al. 2006, 2007). This suggests that bulk motion of the gas is typical in these metal-poor, bursty environments, but for a larger mass of gas in RXCJ2248-ID3.\r\n\r\nThe sensitive accounting of broad component emission afforded by the deep GLIMPSE-D spectra is important because even a small fraction of broad emission around H emission line can significantly affect the fit to weak lines such as [N ii] λλ6550,6585 (e.g., D. A. Berg et al. 2021). In RXCJ2248-ID, the broad components compose a significant fraction of the total H and [O iii] fluxes, and so are critical to properly measure not only the [N ii] λ6585 emission but also the [O iii] λ4364, Hβ, [O iii] λλ4960,5008, and Hα narrow-line fluxes. For this reason, we adopt the narrow-line fluxes from our best multicomponent fits for the remaining analysis; we reserve further investigation of the the broad emission for a forthcoming paper.\r\n\r\nAs noted above, the UV spectra do not have sufficient S/N to decompose narrow and possible broad components. As a result, density diagnostics and relative abundance ratios determined from UV line ratios may include contributions from multiple kinematic components. If the broad components arise from gas with distinct physical conditions, this could introduce systematic offsets. We test the level of bias possible due to broad component contamination of narrow-line fluxes by adopting the relative narrow and broad component profiles of [O iii] λ5008 as a template for collisionally excited lines. The broad component areas overlap with the narrow profile such that the broad components are responsible for 8.6% and 2.2% of the narrow-component flux, or 10.8% in total. We use this fraction to set the upper contamination limit of potential broad components to the UV emission lines and determine the impact on nebular density, temperature, and abundance calculations in Section 4.4.\r\n\r\n2.3. Reddening Correction\r\nThe observed Balmer decrement of the narrow Hα/Hβ lines is FHα/FHβ = 3.48, implying either a moderate amount of dust is present or collisional enhancement of Hα. This value disagrees with the results of M. W. Topping et al. (2024), who measured an observed decrement of 2.55 ± 0.05 that they found to be consistent with no dust attenuation. Similarly, A. Crespo Gómez et al. (2025) used high-resolution NIRSpec/G395H data to fit multiple component Balmer decrements for RXCJ2248-ID3, finding a narrow-component FHα/FHβ = 2.7 that is consistent with no attenuation, but broad- and very broad-component decrements of 4.3 and 6.6, respectively, that imply differential extinction. We too find higher FHα/FHβ ratios for the broad components, but the source of this increase is not clear; it could indicate higher dust in the broad component gas, as suggested by A. Crespo Gómez et al. (2025), or result from significant collisional enhancement of Hα.\r\n\r\nFortunately, the GLIMPSE-D spectrum provides a significant increase in S/N in the continuum, allowing for more robust fitting of broad components, including in the Hγ and [O iii] λ4364 and λ5008 lines. Fitting the broad components directly in the [O iii] lines offers the advantage over previous works that we do not need to correct for broad component contamination with differential extinction in our Te calculation. Furthermore, by fitting the broad components in Hγ we were able to examine the narrow-component Hβ/Hγ ratio, finding a decrement of FHβ/FHγ = 2.16 that is consistent with very little dust (see Table 2). Note that we do not consider the Hβ/Hδ ratio here because the Hδ line is not strong enough to robustly fit the broad components in a consistent manner with the profile fitting of the Hγ, Hβ, and Hα lines.\r\n\r\nTable 2. Rest UV+Optical Emission-Line Fluxes\r\n\r\nIon+Wavelength\tI(λ)/I(C iii])\tEW\r\n(Å)\t \t(Å)\r\nN iv] λ1483.33\t42.78 ± 1.61\t6.67\r\nN iv] λ1486.50\t102.0 ± 0.82\t15.9\r\nHe iiλ1640.42\t22.46 ± 197\t4.88\r\nO iii] λ1666.15\t85.84 ± 0.59\t18.9\r\nN iii] λ1750a\t38.59 ± 0.64\t9.18\r\nSi iii] λ1883.00\t5.01 ± 3.25\t1.32\r\nSi iii] λ1892.03\t8.25 ± 1.98\t2.21\r\nC iii] λ1906.68\t35.11 ± 0.31\t9.65\r\n[C iii] λ1908.73\t64.89 ± 0.25\t17.9\r\nIon+Wavelength\tI(λ)/I(Hβ)\tEW\r\n(Å)\t \t(Å)\r\n[O ii] λ3728a\t4.09 ± 2.05\t6.22\r\nHγ λ4341.66b\t47.41 ± 3.07\t73.8\r\n[O iii] λ4364.44b\t42.45 ± 1.92\t66.5\r\nHe i λ4472.73\t8.90 ± 0.39\t27.8\r\nN iii λ4641.94\t1.40 ± 0.20\t4.4\r\nHe ii λ4687.01\t1.33 ± 0.29\t4.2\r\n[Ar iv] λ4712.69c\t2.30 ± 0.27\t10.3\r\nHe i λ4714.46c\t1.91 ± 0.19\t3.0\r\n[Ar iv] λ4741.49\t4.10 ± 0.26\t13.0\r\nHβ λ4862.71b\t100.0 ± 4.4\t356\r\n[O iii] λ4960.29b\t230.5 ± 9.0\t877\r\n[O iii] λ5008.24b\t708.9 ± 27.5\t2791\r\nHα λ6564.60b,d\t331.8 ± 14.4\t1755\r\nHα λ6564.60b,e\t274.1 ± 11.9\t1457\r\n[N ii] λ6585.27\t7.08 ± 0.91\t12.8\r\n[S ii] λ6718.29\t0.68 ± 0.29\t4.78\r\n[S ii] λ6732.67\t0.81 ± 0.30\t4.74\r\nE(B − V)\t\t⋯\r\nFC III]\t11.58 ± 0.49\t⋯\r\nb\t6.94 ± 0.15\t⋯\r\nNotes. Reddening-corrected emission-line intensities of lines used in this analysis from the archival rest-UV and GLIMPSE rest-optical JWST/NIRSpec spectra for RXCJ2248-ID3. Note that no scaling was performed between the archival UV and GLIMPSE-D optical pointings (not needed for this work). Thus, UV fluxes are given relative to the FC III]λλ1907,09 × 100 and optical fluxes are given relative to FHβ × 100. The last three rows list the dust attenuation derived using the J. A. Cardelli et al. (1989) reddening law and the rest-frame C iii] λλ1907,09 and Hβ flux in units of 10−18 erg s−1 cm−2. Additionally, the fluxes reported here are for a single image of RXCJ2248 (ID3), whereas M. W. Topping et al. (2024) report fluxes for coadded spectra of multiple images. aNote that N iii] λ1750 and [O ii] λ3728 fluxes are the integrated values for the N iii] λλ1746,1748,1749,1752,1754 quintuplet and [O ii] λλ3727,3730 doublet, respectively. bEmission-line profile was best fitted with a narrow Gaussian and two broad Gaussian components; only the corrected narrow-line flux is listed here (see Section 2.2 and Figure 3). c[Ar iv] λ4713+He iλ4714 is a blended line profile at the observed resolution. Thus, the [Ar iv] λ4713 is determined by subtracting the He iλ4714 flux, which is predicted from the He i λ4473 flux. dUncorrected for collisional excitation. eCorrected for collisional excitation.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nThe reddening due to dust, characterized by E(B − V), was determined by comparing the observed Balmer decrements with the theoretical Balmer ratios assuming case B and an extinction law, for which we tested the parameterization from both J. A. Cardelli et al. (1989) and D. Calzetti et al. (2000). The E(B − V) value for a given Balmer ratio was determined iteratively until convergence, recomputing the H i theoretical ratio using the updated electron temperature from the reddening-corrected [O iii] λ4364/λ5008 flux ratio and density from the reddening-corrected N iv] λ1483/λ1487 flux ratio in each iteration. In this way, the reddening, electron temperature, and electron density were solved for simultaneously and consistently.\r\n\r\nA greater enhancement of the observed FHα/FHβ decrement than of the FHβ/FHγ decrement can arise under high-density conditions, where collisional excitation selectively enhances the lowest excited level (n = 2; requires lowest energy to excite), leading to higher Hα flux relative to Hβ and Hγ. To assess whether such an enhancement is physically plausible, we examined the Cloudy photoionization models (M. Chatzikos et al. 2023; C. M. Gunasekera et al. 2023) presented in Z. Martinez et al. (2025), which span a wide range of nebular densities (up to ne = 109 cm−3). For the nebular conditions determined in this work (i.e., Te, , Z, N/O; see Section 4), densities of ne ∼ 106 cm−3 are needed to produce the observed Hα enhancement while minimally affecting Hβ and Hγ. Although this density is roughly an order of magnitude higher than the values measured in M. W. Topping et al. (2024) and in this study (see Section 4.1 and Table 3), it could indicate that the interstellar medium (ISM) contains unresolved clumps of even higher density than the volume-weighted values probed by the density diagnostics used in this work. We, therefore, attribute the observed Hα excess to collisional enhancement.\r\n\r\nTable 3. Nebular Conditions and Abundances for RXCJ2248-ID3\r\n\r\nProperty\tIon. E\tUsed\tValue\r\n \t(eV)\t \t \r\nTemperatures:\t \t \r\nTe,high meas. (K)\t35.11–54.93\tne(N+3)\t1.97 ± 0.03 × 104\r\nTe,int. used (K)\t23.33–34.83\tD. R. Garnett (1992)\t1.81 ± 0.02 × 104\r\nTe,low used (K)\t13.62–35.11\tD. R. Garnett (1992)\t1.68 ± 0.02 × 104\r\nDensities:\t \t \t \r\nne(N+3) (cm−3)\t47.45–77.47\tTe,high\t\r\nne(Ar+3) (cm−3)\t40.74–59.81\tTe,high\t\r\nne(C+2) (cm−3)\t24.38–47.89\tTe,int.\t\r\nne(Si+2) (cm−3)\t16.35–33.49\tTe,int.\t\r\nne(S+) (cm−3)\t10.36–23.33\tTe,low\t\r\nO Abundances:\r\nO+/H+ (×10−5)\t13.62–35.11\tTe,low; ne(Si+2)\t0.186 ± 0.148\r\nO+2/H+ (×10−5)\t35.11–54.93\tTe,high; ne(Ar+2)\t5.473 ± 0.261\r\n \t \t7.753 ± 0.023\r\nIonization Parameters:\r\nlogUint.(O32)\t13.62–54.93\tne = 104 cm−3\t−1.24 ± 0.23\r\nlogUhigh(N43)\t29.60–77.47\tne = 105 cm−3\t−0.69 ± 0.10\r\nN Abundances:\r\nN+3/O+2\t47.45–77.47\tTe,high; ne(N+3)\t0.277 ± 0.043\r\nN+2/O+2\t29.60–47.45\tTe,high; ne(C+2)\t0.145 ± 0.070\r\nN+/O+\t14.53–29.60\tTe,low; ne(Si+2)\t0.367 ± 0.259\r\nICF(N+3/O+2)\t47.45–77.47\tTe,high; ne(N+3)\t1.542\r\nICF(N+2/O+2)\t29.60–47.45\tTe,high; ne(C+2)\t2.547\r\nICF(N+/O+)\t14.53–29.60\tTe,low; ne(Si+2)\t0.814\r\nlog(N/O)\t⋯\t⋯\t−0.368 ± 0.062\r\nlog(N/O)\t⋯\t⋯\t−0.434 ± 0.071\r\nlog(N/O)\t⋯\t⋯\t−0.525 ± 0.257\r\nlog(N/O)all\t⋯\t⋯\t−0.375 ± 0.056\r\n⋯\t⋯\t−0.390 ± 0.035\r\nC Abundance:\r\nC+2/O+2\t24.38–47.89\tTe,int; ne(C+2)\t0.107 ± 0.014\r\nICF(C+2/O+2)\t24.38–47.89\tTe,int; ne(C+2)\t1.498\r\nlog(C/O)\t \t \t−0.795 ± 0.052\r\nSi Abundance:\r\nSi+2/O+2\t16.35–33.49\tTe,low; ne(Si+2)\t0.005 ± 0.001\r\nICF(Si+2/O+2)\t16.35–33.49\tTe,low; ne(Si+2)\t3.507\r\nlog(Si/O)\t⋯\t⋯\t−1.781 ± 0.157\r\nNote. Ionic and total abundances for RXCJ2248-ID3. Column (1) lists the property, while Column (2) lists the associated ionization potential energy range (eV), Column (3) lists the temperature and/or density used in the calculation, and Column (4) provides the final values. All calculations reported here only used the narrow components when multicomponent fits were performed. Note that the temperatures for the intermediate- and low-ionization zones were inferred from Te,high using the Te–Te relationships of D. R. Garnett (1992). Two ionization parameters are reported for the O32 and N43 indicators from Z. Martinez et al. (2025). The oxygen abundance was determined using the archival [O ii] λ3728 detection and the new [O iii] λ5008 fit. N/O was determined using four different ion+ICF (from Z. Martinez et al. 2025) combinations: (1) optical N+/O+; (2) UV N+2/O+2; (3) UV N+3/O+2; and (4) combination (N++N+2+N+3)/(O++O+2). C/O and Si/O were determined from the archival UV emission lines only.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nAccordingly, we adopted the reddening derived from Hγ/Hβ, mag using J. A. Cardelli et al. (1989) (the D. Calzetti et al. (2000) value is similar at E(B − V) = 0.050 ± 0.1215 mag), and corrected all emission lines for the resulting (minimal) dust attenuation. We used the D. Calzetti et al. (2000) reddening law for the rest-UV emission lines (λ < 3200 Å) and the J. A. Cardelli et al. (1989) reddening law for the rest-optical emission lines (λ > 3200 Å). After applying the reddening correction, the Hα/Hβ ratio still shows a collisional excess of 0.204 above the theoretical value; we correct for this excess and report a final FHα = 1.985 × 10−17 erg s−1 cm−2.\r\n\r\nThe adopted reddening and dereddened line intensities are listed in Table 2 for all line fluxes used in this work. Note that rest-UV and rest-optical lines should not be compared or combined in line ratios. Since the rest-UV and rest-optical spectra were obtained during different observing runs with distinct pointings and strategies, we report the UV lines relative to FCIII]λλ1907,1909 × 100 and the optical lines relative to FHβ × 100, without applying any relative scalings between the two datasets.\r\n\r\n3. Wolf Rayet Stars at z = 6.1\r\nThe WR stage of massive star evolution is an important, short-lived phase that can have significant effects on the chemical composition of the local ISM. We provide a brief overview here (see, e.g., P. A. Crowther 2007, for a more thorough review). WR stars are massive stars that have entered the core He-burning phase and have lost their outer envelope either via strong stellar winds or due to binarity effects (i.e., stripping via Roche Lobe overflow or mergers). The first phase of WR stars occurs when the outer H layer has been ejected, revealing the H core-burning products such that their spectra are characteristically He and N rich but are H-poor. Such stars are known as nitrogen-type WR, or WN, stars, and are often identified by strong N iii, N iv, and N v emission lines, especially the broad optical “blue bump” near λ4650. The blue bump is a complex of features, including N iii λλ4634,4642, C iii λ4649,4667, Fe iii λ4660, and He ii λ4687. Subsequently, stars that are massive enough for core He-burning and for their winds to remove their outer He envelope and expose the produced C enter the WR carbon (WC) phase. WC stars also have strong, broad He ii emission and strong C and O emission, such that they are identified by the optical WR C iv λλ5803,5814 doublet (the “red bump”). As a result, the typically very strong winds of the WR phase can produce significant N enrichment during the WN phase and drive strong C ejection during the WC phase. After the WC phase, a WR-oxygen phase may ensue, but we forgo discussion of this phase here.\r\n\r\nThe rest-frame UV and optical spectra shown in Figure 2 can be used to characterize the WR nature of the stellar population in RXCJ2248-ID3. Both the UV and optical He ii emission features are kinematically broadened compared to the narrow nebular emission features in RXCJ2248-ID3, indicative of WR or VMS winds. F. Martins et al. (2023, 2025) have shown that young star-forming regions dominated by VMSs can be distinguished from WR stars using the morphology of the blue and red bumps. In particular, VMSs produce blue bumps with He ii λ4687 emission but little to no N iii emission and red bumps with narrow C iv λλ5803,5814 emission. Thus, strong detections of N iii in the blue bump favor a WN interpretation (e.g., F. Martins et al. 2023; D. A. Berg et al. 2024; T. E. Rivera-Thorsen et al. 2024).\r\n\r\nThe upper right-hand panel of Figure 2 highlights the blue bump spectral regime, showing weak, broad He ii and N iii λ4642 in RXCJ2248-ID3, both of which are characteristic of metal-poor WN stars. Just redward of the N iii λ4642 line in the blue bump (but blueward of [Fe iii]), a second less prominent emission feature is seen, but it is difficult to determine whether this is due to C iii or O ii emission, or both. Furthermore, the red C iv bump is not detected, suggesting little to no contributions from WC stars or VMSs in the spectrum. Thus, we only significantly detect the blue WR bump, suggesting that WN stars are likely present.\r\n\r\n4. Nebular Properties\r\nUsing the updated narrow-component emission-line fits presented in Section 2.2, we determined the nebular properties of RXCJ2248-ID3. Following D. A. Berg et al. (2021), we adopt the four-zone ionization model to account for the high-ionization emission observed. In this model, the ionization potential energy ranges of N+, S+2, O+2, and He+2 define the low-, intermediate-, high-, and very high-ionization zones, respectively. For all calculations, we use the PyNeb package in Python with the atomic data adopted in D. A. Berg et al. (2019), which includes a six-level atom model for oxygen in order to utilize the UV O iii] λ1666 line. Below, we determine temperatures and densities, although Te(O+2) and ne(N+3) were codetermined during the iterative reddening calculation (see Section 2.3) in Section 4.1, ionization parameters in Section 4.2, and abundances in Section 4.3.\r\n\r\nWe note that the UV spectra do not have sufficient S/N to decompose narrow and broad components following the same method as the optical lines. As a result, density diagnostics and abundances determined from UV lines may include contributions from multiple kinematic components, while optical temperatures, densities, and abundances are derived from narrow components alone. If the broad component arises from gas with distinct physical conditions, this could introduce systematic offsets. For this reason, we examine the potential impact of UV broad components in Section 4.4.\r\n\r\n4.1. Temperature and Density\r\nOne of the unique characteristics of RXCJ2248-ID3 is its large number of density-sensitive emission-line ratios. M. W. Topping et al. (2024) previously reported densities from the three UV line ratios of Si iii] λ1883/λ1892, characterizing the intermediate-ionization zone, C iii] λ1907/λ1909, characterizing the intermediate- to high-ionization zone, and N iv] λ1483/λ1486, characterizing the high- to very high-ionization zone. The new high-S/N optical spectra enables us to measure, for the first time, densities from the low-ionization [S ii] λ6717/6731 ratio and the high- to very high-ionization [Ar iv] λ4713/λ4741 ratio.\r\n\r\nWe use our narrow-component dereddened flux measurements to compute densities for all five line ratios and the high-ionization zone temperature from the [O iii] λ4364/λ5008 ratio. The high-ionization zones Te(O+2) and ne(N+3) were simultaneously determined during the iterative reddening calculation in Section 2.3 to account for the sensitivities of both diagnostics. If the low density limit was assumed instead (ne ≲ 102 cm−3), as is common practice at low-redshift, the observed [O iii] λ4364/λ5008 flux ratio would lead to unphysical temperatures (i.e., above the limit set by H cooling of ∼2.5 × 104 K). Thus, a physical and robust solution requires high densities to properly account for the reduced λ5008 flux due to collisional de-excitation. Furthermore, Z. Martinez et al. (2025) recently showed that densities derived from both optical and UV diagnostics underpredict the true volume-averaged density in multiphase, high-density systems, with more severe underprediction from the optical diagnostics. Therefore, it is necessary to use UV density diagnostics in high-density environments, though the true density will still be underestimated in multiphase gas (see, e.g., Figure 11 of Z. Martinez et al. 2025).\r\n\r\nFor the high-ionization zone, we found a Te(O+2) = 1.97 ±0.03 × 104 K and ne(N+3) cm−3, which is consistent with the density of ne(N+3) cm−3 reported by M. W. Topping et al. (2024), but lower than their temperature of 2.46 ± 0.26 × 104 K due to our broad component fits of both [O iii] λ4364 and λ5008. Adopting our Te(O+2) as the high-ionization temperature (Te,high), we then applied the Te–Te relations of D. R. Garnett (1992) to estimate the intermediate-ionization temperature (Te,int.) and low-ionization temperature (Te,low).\r\n\r\nThe determined temperatures were used for the subsequent density calculations in their respective ionization zones. Note that the [Ar iv] λ4713 and He i λ4714 lines are blended in the G395M grating. Therefore, we corrected the [Ar iv] λ4713 flux for the He i λ4714 contribution, predicting the He i λ4714 flux from the measured He i λ4473 flux and the theoretical He i λ4714/λ4473 ratio (∼0.21 for the conditions in RXCJ2248-ID). The resulting densities, all of which fall within their respective diagnostic ranges, and temperatures are reported in Table 2.\r\n\r\nRemarkably, RXCJ2248-ID3 is one of few galaxies, and the only galaxy yet at high redshifts, to have significant (>3σ) electron density measurements from five different ions that span a large ionization range (∼10–77 eV). Furthermore, the densities in RXCJ2248-ID3 appear to be organized into an interesting nebular stratification. The UV emission lines trace the densest gas, with ne(N+3) = 2.65 × 105 cm−3 in the highest-ionization gas, followed by ne(C+2) = 7.94 × 104 cm−3 and ne(Si+2) = 4.77 × 104 cm−3. In contrast, the optical high-ionization lines are emitted from regions of lower densities: the optical [Ar iv] diagnostic has an overlapping ionization energy range with the UV N iv] diagnostic but a density that is an order of magnitude lower.\r\n\r\nThere are two possible interpretations of the measured array of densities. First, since the UV lines also have higher excitation energies, they could originate preferentially from hotter, denser clumps. This would imply a strongly inhomogeneous ISM, in which compact, high-pressure structures dominate the UV line emission while somewhat more diffuse gas produces much of the optical emission. Alternatively, the multiphase ISM may span a smaller dynamic range of densities than we measure due to the suppression of the optical diagnostics. Z. Martinez et al. (2025) showed that for an ISM with a mix of low- (e.g., 103 cm−3) and high-density gas (e.g., 105 cm−3) that has a true volumetric density that is somewhere in between, the low-ionization optical diagnostics will always be significantly biased low, close to the low-density gas value, until the fraction of high-density gas is very high (e.g., >95%). This effect occurs when ne-diagnostic line ratios have low critical densities (e.g., ne,crit([S ii])≈2 × 103–5 × 103 cm−3), such that emission from the high-density gas is collisionally suppressed beyond detection. The magnitude of this effect decreases with increasing critical density such that [S ii] is significantly affected, [Ar iv] is moderately affected (ne,crit ≈ 2 × 104–2 × 105 cm−3), and the UV Si iii], C iii], and N iv] (ne,crit ≈ 5 × 104–5 × 1010 cm−3) are minimally affected, albeit still biased low. In this scenario, there would still be density stratification, but with smaller differences.\r\n\r\nAll together, the nebular diagnostics in RXCJ2248-ID3 support a picture of a multiphase nebula with density and temperature stratification, likely reflecting a clumpy ISM shaped by the feedback and local radiation field variations of bursty star formation (see, also, N. Choustikov et al. 2025; Y. Harikane et al. 2025b; M. Usui et al. 2025). This picture is also consistent with the density stratification that has been reported for dwarf galaxies both near and far (e.g., B. L. James et al. 2016; D. A. Berg et al. 2021; M. Mingozzi et al. 2022; X. Ji et al. 2024; M. W. Topping et al. 2024), but with typical densities increasing with redshift (e.g., Y. Isobe et al. 2023; Abdurro’uf et al. 2024; Z. Martinez et al. 2025; M. W. Topping et al. 2025a).\r\n\r\n4.2. Ionization Parameter\r\nThe ionization parameter of RXCJ2248-ID3, , determined using the typical O32 = Iλ5008/Iλ3728 diagnostic is reported in M. W. Topping et al. (2024) to be in the high range of to −1. We recompute the ionization parameter for RXCJ2248-ID3 using the O32 and N43 = Iλλ1483,1486/Iλ1750 diagnostics from Z. Martinez et al. (2025) that are calibrated for densities in the 102 ≤ ne(cm−3) ≤ 106 range. We estimate a using O32, which is consistent with the value reported by M. W. Topping et al. (2024), and using N43. Note, however, that the O32 diagnostic is very sensitive to the assumed density (Z. Martinez et al. 2025), making this value highly uncertain in dense gas. For example, densities of ne = 103–105 cm−3 would lead to a range of to −2.04, respectively.\r\n\r\n4.3. Abundances\r\nHere, we present direct-method abundances of oxygen-to-hydrogen (O/H) (Section 4.3.1), N/O (Section 4.3.2), carbon-to-oxygen (C/O) (Section 4.3.3), and silicon-to-oxygen (Si/O) (Section 4.3.4) for RXCJ2248-ID3 using narrow-line flux ratios and the measured temperatures and densities presented in Section 4.1. Nearly all of the optical lines used in this work have sufficient S/N to simultaneously constrain broad and narrow emission components, but there are a few exceptions, all of which are low-ionization lines. The [O ii] λ3728 line was not covered by the GLIMPSE-D spectrum and so lacks the S/N to fit broad components. Both [N ii] λ6585 and [S ii] λλ6718,6733 are covered in the high-S/N GLIMPSE-D spectrum but are either blended with stronger features or too weak to fit broad components. On the other hand, the [O ii] and [S ii] lines have low critical densities around ne,crit ∼ 103 cm−3 such that any moderate to high-density broad components are likely collisionally de-excited away. Their narrow-component fluxes could also be significantly reduced by collisional de-excitation; however, the missing [O ii] emission is likely small in the absolute sense for such a high-ionization object. Emission from [N ii] is less likely to be collisionally de-excited (ne,crit ∼ 105 cm−3), so a hidden broad component could lead to an overestimate of the N/O abundance, but this effect would be somewhat countered by the underestimated [O ii] flux. In the end, the consistency of N/O derived independently from UV and optical tracers in Section 4.3.2 below suggests that these effects do not significantly impact our results.\r\n\r\nTo calculate the total or relative abundance of an element, we determine and sum the individual observed ions and then apply an ionization correction factor to account for unseen prominent ionization states. The abundance of an individual ionic species, Xi, relative to hydrogen is determined as\r\n\r\nwhere jλ(i) is the emissivity determined for the appropriate ionization zone temperature and density. Given the tendency of the optical density diagnostics to severely underestimate the density in high-density environments, we instead adopt the UV-derived densities. Note that the abundances presented below have not been corrected for the fraction of atoms embedded in dust. However, the level of depletion onto dust grains is expected to be small for the low metallicity of RXCJ2248-ID3 (e.g., A. Rémy-Ruyer et al. 2014; F. Galliano et al. 2018; J. Roman-Duval et al. 2022). Y. Isobe et al. (2026) also infer negligible dust depletion for RXCJ2248-ID3 based on the high value of Si/O that that they determine, but this is inconsistent with the value we determine below. Details of elemental abundance determinations are given below.\r\n\r\n4.3.1. Oxygen Abundance\r\nWe determine the total O/H abundance as the sum of the O+/H+ and O+2/H+ ionic abundances, determined from the [O ii] λ3728 and [O iii] λλ4960,5008 optical emission lines. We observe no strong O0 or O+3 emission, indicating that contributions from other ions are negligible. The resulting ionic and total oxygen abundances are presented in Table 2. Similar to M. J. Hayes et al. (2025) and Z. Martinez et al. (2025), we find that one of the most significant effects of accounting for high densities is the resulting decrease in electron temperature and subsequent increase in oxygen abundance (see, also, H. Katz et al. 2023). In our work, this results both from accounting for the missing [O iii] λ5008 flux due to collisional de-excitation and from correcting the narrow emission for broad emission components at their base. M. W. Topping et al. (2024) also incorporated the high densities seen in RXCJ2248-ID3 but did not have the S/N to fit the broad emission components in both [O iii] λ5008 and λ4364. As a result, we measure an oxygen abundance of . Note that if unresolved high-density clumps (ne ≳ 105 cm−3) are present (as suggested in, e.g., Section 2.3), it could introduce additional uncertainty by biasing the luminosity-weighted [O iii] λ4364/λ5008 ratio to higher densities, which would drive the derived Te higher and O/H abundance lower. However, Z. Martinez et al. (2025, see Figure 11), showed that the use of high-critical density UV density diagnostics largely mitigate this effect in a density stratified medium.\r\n\r\n4.3.2. Relative N/O Abundance\r\nThe extraordinary simultaneous detections of [N ii] λ6585, N iii] λ1750, and N iv] λλ1483,1487 enable multiple determinations of the N/O abundance. Therefore, we calculate N/O abundances using four different ionic methods\r\n\r\n\r\n\r\n\r\nwhere [O ii] λ3728 is used for the N+/O+ determination, O iii] λ1666 is used for the N+2/O+2 and N+3/O+2 calculations, and X(N+i) and X(O+i) are the N and O ionization fractions, respectively. We use the density-dependent ICFs from Z. Martinez et al. (2025), who provide prescriptions for densities of ne = 102, 103, 104, 105, and 106 cm−3. We, therefore, round our density measurements to the nearest order of magnitude and use the intermediate-ionization for the N+/O+ ICF and the high-ionization for the N+2/O+2 and N+3/O+2 ICFs. The resulting N ICFs and N/O abundances are reported in Table 3.\r\n\r\nThe four N/O determinations of RXCJ2248-ID3 are in close agreement, far above the expected value for its metallicity. Visually, this is shown in the upper left-hand panel of Figure 4, which plots the relative N/O versus O/H abundance with RXCJ2248-ID3 marked by purple diamonds. The traditional N/O–O/H trend has been established by many z ∼ 0 studies of H ii regions and galaxies (gray points: C. Esteban et al. 2002, 2009, 2014; L. S. Pilyugin & T. X. Thuan 2005; L. van Zee & M. Haynes 2006; J. García-Rojas & C. Esteban 2007; Á. R. López-Sánchez et al. 2007; D. A. Berg et al. 2012, 2016,2019, 2020). The empirical trend is a bimodal relationship, with a flat trend due to primary (or metallicity-independent) N production at low metallicities () and an increasing N/O trend with O/H as secondary (or metallicity-dependent) N production becomes increasingly important at higher metallicities (). As a visual guide, the primary N/O plateau from D. A. Berg et al. (2019, dashed purple line) is shown and the empirical stellar curve from D. C. Nicholls et al. (2017, solid green line) is shown as an example of the full primary and secondary curve.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 4. Relative C and N abundance trends versus metallicity. Nitrogen to oxygen ratio versus oxygen abundance for star-forming galaxies is plotted in the left panels, while C/O ratio versus oxygen abundance is plotted in the middle panels, and carbon to nitrogen abundance versus oxygen abundance is plotted in the right panels. Top row: RXCJ2248-ID3 is shown relative to the observed z ∼ 0 trend and other high-z galaxies. The abundances for RXCJ2248-ID3 are shown as purple diamonds, where multiple N/O points show the measurements for each ionic N/O calculation method. For comparison, we also plot the abundances derived for RXCJ2248-ID3 by M. W. Topping et al. (2024) as turquoise squares. The typical bimodal N/O trend is characterized by local dwarf (gray diamonds; L. van Zee & M. Haynes 2006; D. A. Berg et al. 2012, 2016, 2019) and spiral galaxy (gray circles; C. Esteban et al. 2002, 2009, 2014; L. S. Pilyugin & T. X. Thuan 2005; J. García-Rojas & C. Esteban 2007; Á. R. López-Sánchez et al. 2007; D. A. Berg et al. 2020) H ii region measurements. The primary N/O plateau from D. A. Berg et al. (2019) is shown as a dashed purple line, while the solid green line is the empirical stellar curve from D. C. Nicholls et al. (2017). Additional C/O literature measurements for dwarf galaxies are from M. A. Peña-Guerrero et al. (2017) and P. Senchyna et al. (2017). Abundances for z > 2 galaxies from Z. Martinez et al. (2025) are plotted as blue plus signs for galaxies with UV N+2/O+2 derived abundances and pentagons for optical N+/O+ derived abundances. Bottom row: The same observed samples are shown as the top row, but with the z ∼ 0 sample represented by the shaded gray regions. The observed abundances of RXCJ2248-ID3 are compared to updated dual-burst chemical evolution models of C. Kobayashi & A. Ferrara (2024, string of circles), color coded by age since onset of the second burst. The models have been modified to reproduce both the enhanced N/O and relatively deficient C/O observed for RXCJ2248-ID3, which requires enrichment from WN but very little WC enrichment, as expected at low metallicities.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nFor comparison, we plot the high-quality high-redshift N/O measurements that were calculated in a consistent manner as the present work (with direct-method Te and ne determinations and ne-dependent ICFs) by Z. Martinez et al. (2025). N/O abundances determined using N+2/O+2 are plotted as blue + symbols, while N+/O+ determinations are plotted as blue pentagons. Of these galaxies, the closest comparison to RXCJ2248-ID3 is CEERS-1019 (see, also, R. Marques-Chaves et al. 2024), while only GDS 3073 and GN-z11 have higher relative N/O abundances and only GDS 3073 is more enhanced in N/O for its O/H abundance.\r\n\r\nWe find that all four ionic methods produce consistently high N/O values within their uncertainties, with a weighted mean of . This is an important result because RXCJ2248-ID3 is the first galaxy to have consistently enhanced N/O abundances measured from both the rest-frame UV high-ionization and the optical low-ionization emission lines. Furthermore, measuring consistent N/O values from three different ionic methods strengthens our confidence in the robustness of the N/O measurement, although uniform N/O across the ionization structure of the nebula is not a given in a stratified medium. While there is strong evidence for a stratified, or perhaps very clumpy, density structure in RXCJ2248-ID, the N/O abundance appears to be well mixed.\r\n\r\n4.3.3. Relative C/O Abundance\r\nMeasuring the C/O abundance provides a crucial comparative baseline for interpreting the origin of elevated N/O in RXCJ2248-ID3. Similar to N, C has a pseudosecondary17 production pathway, but the dominant nucleosynthetic sources and timescales differ for C and N. Briefly, both C and O are primarily produced in massive stars (>8 M⊙) on relatively short timescales such that the C/O ratio is a relatively stable tracer of massive star yields, although some C is produced via low- to intermediate-mass AGB stars (∼1.5–3 M⊙). In contrast, some N is produced by massive stars (e.g., through rotational mixing and WR winds) but most N comes from intermediate-mass AGB stars (∼4–8 M⊙), which release N on longer timescales (∼200 Myr). Therefore, N/O and C/O together serve as diagnostics of the recent star formation history, constraining the recent enrichment mechanisms of galaxies (e.g., D. R. Garnett 1990; R. B. C. Henry et al. 2000; C. Chiappini et al. 2003; E. Pérez-Montero & T. Contini 2009; D. A. Berg et al. 2019; E. Pérez-Montero et al. 2021).\r\n\r\nRelative C/O abundances are typically determined using the C iii] λλ1907,1909/O iii] λ1666 ratio to calculate C+2/O+2 and assuming that C/O ≈ C+2/O+2. This method is sometimes used alone owing to the fact that (1) C+2 and O+2 have somewhat similar ionization potentials (24.38 and 35.12 eV, respectively), (2) the upper levels of the λ1666 and λλ1907,1909 transitions have similar excitation potentials (∼6.5 and ∼7.5 eV, respectively), and (3) the integrated fluxes of λ1666 and λλ1907,1909 are not sensitive to collisional de-excitation for the densities measured here. However, for the high-ionization nebulae in RXCJ2248-ID3, it is important to account for contributions from the C+3 species and any unseen species. We note that the C iv λλ1548,1550 doublet is clearly observed in the rest-UV spectrum of RXCJ2248-ID3, but these lines are resonant and can be affected by the C iv stellar wind feature and ISM absorption, and so determining the intrinsic flux and subsequent C+3 abundance is challenging. Instead, we use an ICF determined from the photoionization models presented in Z. Martinez et al. (2025) such that\r\n\r\nWe used the and a density of ne(C+2) ∼ 105 cm−3 to determine the C ICF. The resulting C ICF and C/O abundance are reported in Table 3.\r\n\r\nThe C/O and C/N abundances for RXCJ2248-ID3 are plotted in the upper middle and right-hand panels of Figure 4. Empirical trends of C/N at z ∼ 0 are found to be flat, albeit with significant scatter (see shading in Figure 4), suggesting that the dominant nucleosynthetic mechanisms of C are similar to those of N (e.g., D. R. Garnett et al. 1999; C. Esteban et al. 2014; D. A. Berg et al. 2016, 2019). However, while the production of both C and N appear to be metallicity-dependent, the scatter in their trend is consistent with differing production timescales due to stars of different masses. Thus, the variations observed in CNO abundance patterns of high-redshift galaxies may be the result of taking a snapshot of many galaxies at different times since their most recent onset of star formation.\r\n\r\nRXCJ2248-ID3 appears to have a similar CNO abundance pattern to other high-redshift N emitters, characterized by enhanced N/O but relatively deficient C/O such that their C/N is very deficient compared to the expectations from low-redshift trends. This suggests that these high-redshift N-emitting galaxies are enhanced in N relative to both O and C. If massive stars in the WN phase are present, they will have recently produced 14N at the expense of 12C through the CNO cycle, meaning C used as a catalyst in the cycle initiation will have been consumed as N is removed during the bottleneck step via dredged up, preventing the return of C at cycle completion. Thus, C/N-deficiency is consistent with a recent, intense episode of N enrichment and C consumption from WN stars. Conversely, if both N/O and C/O were elevated in tandem, it could point to broader enrichment by massive stars, such as enrichment from both WN and WC stars, whose contributions increase at higher metallicities.\r\n\r\n4.3.4. Relative Si/O Abundance\r\nDetecting Si iii] λλ1883,1892 in RXCJ2248-ID3 enables the rare opportunity to measure the silicon-to-oxygen (Si/O) abundance in a z > 5 galaxy (see, also, Y. Isobe et al. 2026, for Si/O in GN-z11). Silicon abundances are important for multiple reasons. Silicon is highly refractory, making the Si/O ratio a sensitive probe of dust depletion. Additionally, Si probes different channels of chemical enrichment than CNO elements, as it is primarily an α-element produced by CCSNe, but Type Ia SNe, AGB stars, and even pair-instability SNe are all expected to contribute to the total Si abundance. For RXCJ2248-ID3 we determine the Si/O abundance using the observed Si iii] λλ1883,1892/O iii] λ1666 ratio to calculate Si+2/O+2. Because Si+2 and O+2 have rather different ionization potentials (16.3 eV versus 35.1 eV, respectively), a Si ICF is required to convert Si+2/O+2 to total Si/O via\r\n\r\nSi ICFs have been reported previously (e.g., D. R. Garnett et al. 1995), but none account for the high-density conditions observed in RXCJ2248-ID3. Therefore, we determined a Si ICF = 3.507 using the photoionization models presented in Z. Martinez et al. (2025) using the and a density of ne(Si+2) ∼ 104 cm−3. Reported in Table 3, the resulting (Si/O) = −1.781 ± 0.157 abundance is typical of metal-poor dwarf galaxies (e.g., D. R. Garnett et al. 1995; Y. I. Izotov & T. X. Thuan 1999), consistent with normal massive star production and low dust depletion.\r\n\r\n4.4. Potential Impact of UV Broad Components\r\nThe exceptionally high S/N of the rest-optical GLIMPSE-D spectrum allows for broad emission component fits that the rest-UV spectrum does not. In Section 2.2, we found the broad emission component contribution to the narrow [O iii] λ5008 flux to be 10.8%. To examine the possible effects such contamination has on calculations of nebular conditions and abundances, we adopt 10.8% as the contamination upper limit to the UV emission lines. We first consider the impact on the UV density determinations, where we allow the broad components of the UV density-sensitive emission-line ratios to have densities ranging from 102–106 cm−3. After subtracting the potential broad component contribution, the revised densities change up to Δne(Si+2), Δne(C+2), and Δne(N+3) over the range of broad component densities considered. These values are within the reported uncertainties in Table 3, with the exception of the ∼1.2σ deviation for Δne of C+2.\r\n\r\nNext, we tested the subsequent impact of UV densities that have been revised for possible broad components on the properties determined from rest-optical emission lines: Te(O+2), O/H, and N/O. For the range of Δne(N+3) above, the resulting K, which is within 1σ–2σ of the reported value in Table 3. Similarly, the impact of the revised densities and temperatures on the oxygen abundance, dex, is also within 1σ–2σ. The impact is even smaller for the nitrogen abundance, with dex being much smaller than the N/O uncertainty.\r\n\r\nRelative UV abundances are impacted by changes in both the nebular conditions and the relevant abundance emission-line ratio. However, the resulting abundance deviations are small and within the original uncertainties: dex, dex, and dex. Thus, we conclude that while considering the impacts of hidden broad component contributions to the measured UV fluxes is important, the potential biases do not affect the main results or conclusions of this work.\r\n\r\n5. A Short Window of Intense WR Nitrogen Enrichment\r\nWe have presented evidence for WN stars in RXCJ2248-ID3 in two forms: first, the rest-frame optical WR blue bump discussed in Section 3 and shown in Figure 2; and second, a qualitative comparison of the CNO abundances to patterns expected for WR stars in Section 4.3 and Figure 4. Below, we examine the plausibility and impact of these WN stars by comparing RXCJ2248-ID3 to expected trends for WR stars with metallicity (Section 5.1), testing whether stellar yields can reproduce the observed CNO abundance pattern (Section 5.2) and assessing whether RXCJ2248-ID3’s stellar population can produce its inferred mass of ionized N (Section 5.3). Together, these lines of investigation suggest that the enhanced N/O and suppressed C/O in RXCJ2248-ID3 represent a short-lived enrichment phase, unique to metal-poor, highly star-forming galaxies in the early Universe (Section 5.4).\r\n\r\n5.1. WN Stars: The Dominant WR Phase at Low Metallicity\r\nTo date, no individual resolved WR stars have been directly observed at metallicities as low as RXCJ2248-ID3 (Z ∼ 0.1Z⊙). This is due, in part, to the lack of sufficiently close (D ≲ 1 Mpc for the young, crowded clusters hosting WR stars), metal-poor, star-forming galaxies (see C. Kehrig et al. 2013 for the closest metal-poor WR galaxy), but a scarcity of WR stars in metal-poor environments is also expected because mass loss through stellar winds scales with metallicity. We show the trend of the number of WC/WN stars as a function of metallicity in Figure 5. The observed number of WC/WN stars in M31 (∼175% Z⊙), the Milky Way (MW; Z⊙), M33 (∼40%–110% Z⊙), the Large Magellanic Cloud (LMC; ∼40% Z⊙), and the Small Magellanic Cloud (SMC; ∼20% Z⊙) suggest that the number of the WN/WC number ratio increases with decreasing metallicity (e.g., G. Meynet & A. Maeder 2005; P. A. Crowther 2007; P. Massey et al. 2015; K. Neugent & P. Massey 2019). This is because weaker metal line-driven winds, rotation, or binary effects in metal-poor stars may be able to expose their nitrogen-rich layers and initiate the WN phase but be insufficient to strip the stellar He atmosphere and reveal the carbon-rich core to initiate the WC phase. Thus, if WR stars form at Z ∼ 10% Z⊙, they are expected to be overwhelmingly WN-type. Additionally, A. A. C. Sander et al. (2026) recently discovered a new class of WN–WO stars that point to a low-metallicity WR evolutionary channel in which stars pass directly from the WN to WO phase, potentially explaining spectra that show evidence for WN-like enrichment and hard ionizing radiation without clear WC signatures.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 5. Observed and theoretical ratios of WC/WN star numbers as a function of metallicity. Observed values for the SMC, LMC, MW, and M31 were compiled by K. Neugent & P. Massey (2019), while newer values for M33 come from K. F. Neugent & P. Massey (2023). For comparison, we also plot the trend presented in P. Massey et al. (2017) for BPASS v2.0 binary stellar population synthesis burst models for 12+log(O/H) > 8 (solid line green line), which we extrapolate to lower metallicities (dashed line). Enrichment from WR stars was used to explain the CNO abundances in GN-z11 by C. Kobayashi & A. Ferrara (2024). We note the metallicity for GN-z11 determined by Z. Martinez et al. (2025) is consistent with a WC/WN ratio of ∼0.1–0.2 and the metallicity for RXCJ2248-ID3 from the current work, which predicts a much lower WC/WN ratio of ∼0.03–0.10. Therefore, very little carbon enrichment from WC stars is expected for RXCJ2248-ID3.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nThe spectral features of RXCJ2248-ID3 support the picture of WN star feedback at low metallicity. As shown in Figure 2, the He ii emission is moderately broadened, the N iii λ4642 line in the blue bump is prominent, and there is no evidence for the red bump C iv feature, all consistent with the presence of WN stars at low metallicity. The weakness of the He ii emission in terms of both flux and velocity width is expected for the low-metallicity environment of RXCJ2248-ID3 (∼10% Z⊙) due to reduced wind velocities and mass-loss rates (e.g., A. A. C. Sander et al. 2020). Similarly weak WN features have also been reported in the nearby metal-poor galaxy SBS 0335-052 (Y. I. Izotov et al. 2006) and, at cosmic noon, the z ∼ 2.37 lensed galaxy the Sunburst Arc (T. E. Rivera-Thorsen et al. 2024) and the z ∼ 2.22 M4327 galaxy (M. Curti et al. 2025b).\r\n\r\nWe plot the WR blue bump profile of RXCJ2248-ID3 relative to the Sunburst Arc and M4327 in Figure 6. For ease of comparison, we convolve the Sunburst Arc R ∼ 2700 JWST/NIRSpec G140H spectrum to the R ∼ 1000 resolution of the RXCJ2248-ID3 spectrum. For M4327, we retrieved the G140M spectrum obtained as part of the Measuring Abundance at High Redshift with the Te Approach Survey (MARTA; E. Cataldi et al. 2025) from the Dawn JWST Archive (DJA; K. E. Heintz et al. 2024; A. de Graaff et al. 2025). Both the Sunburst Arc and M4327 spectra were scaled to similar He ii strengths as RXCJ2248-ID3. These spectra immediately reveal similar profiles, but with three distinct differences: (1) RXCJ2248-ID3 exhibits higher gas ionization, as evidenced by the strong [Ar iv] λλ4713,4741 emission; (2) the He ii stellar wind feature is significantly broader in both the Sunburst Arc (FWHM = 1370 km s−1) and M4327 (FWHM = 1460 km s−1) than RXCJ2248-ID3 (FWHM = 530 km s−1), consistent with stronger stellar winds at the higher metallicities of the Sunburst Arc: (or Z ∼ 0.7 Z⊙; Z. Martinez et al. 2025) and M4327: (or Z ∼ 0.3 Z⊙; M. Curti et al. 2025b); and (3) the WR N iii λ4642 line is much stronger in RXCJ2248-ID3, which lacks WR C iv λλ5803,5814 emission, while the Sunburst Arc and M4327 exhibit both N iii and C iv emission. These differences support a scenario in which the z ∼ 2 WR galaxies hosts both WC and WN stars, but the more metal-poor RXCJ2248-ID3 hosts a young population of WN stars with no or very little WC contribution.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 6. The blue WR region of the optical spectrum of RXCJ2248-ID3 (purple) is shown in comparison to the z ∼ 2.37 Sunburst Arc spectrum from T. E. Rivera-Thorsen et al. (2024, blue), which has been convolved to R ∼ 1000 to match RXCJ2248-ID3, and the z = 2.22 M4327 spectrum obtained from the DJA, but originally presented in M. Curti et al. (2025b, turquoise). All three galaxies show characteristic signs of hosting WN stars but RXCJ2248-ID3 shows striking N iii λ4642 emission that is much stronger than both the Sunburst Arc and M4327. On the other hand, the Sunburst Arc and M4327 show broader He ii emission, which is expected for more metal-rich galaxies as stellar winds scale with metallicity.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n5.2. Relative Chemical Enrichment from WN Stars\r\nWith the highest redshift detection of WN stars to date, we now explore their chemical yields as a source of the abundance pattern in RXCJ2248-ID3. C. Charbonnel et al. (2023) performed a comparable analysis for the extreme N/O ratio observed in GN-z11 and found that such rapid nitrogen enrichment could arise from normal massive stars with M⋆ ∼ 20–120 M⊙ or from supermassive stars (M⋆ ≳ 1000 M⊙) in protoglobular cluster environments. Their results and those of R. Marques-Chaves et al. (2024) further demonstrated that the short-lived WN-like phase can produce large N/O ratios within a few megayears of the burst, consistent with the timescales inferred here, but that the observed C/O ratios are only compatible over a very short time interval. Building on this theoretical groundwork, C. Kobayashi & A. Ferrara (2024) showed that a dual-burst chemical evolution model with a short WR-dominated enrichment phase could also match GN-z11’s enrichment pattern. Similarly, R. Marques-Chaves et al. (2024) used N yields from rotating massive stars to demonstrate that a young, WR-dominated stellar population could reproduce the observed CNO enrichment pattern in CEERS-1019.\r\n\r\nThe models above provide a valuable physical framework for linking stellar yields to galaxy-scale abundance evolution at early times. To extend the methodologies outlined by these works to RXCJ2248-ID3, we first examine the dual-burst chemical evolution model of C. Kobayashi & A. Ferrara (2024), which was fine-tuned to reproduce the enhanced N/O in GN-z11 (reported by R. Maiolino et al. 2024). This model invokes two bursts of star formation, where the second triggers a narrow (≲1 Myr) phase of WR-dominated enrichment. While the model can easily reach the N/O enrichment level of RXCJ2248-ID3, it was also designed to yield the higher O/H and C/O abundances observed in GN-z11 than in RXCJ2248-ID3, which was achieved, in part, by enrichment from WC stars. The updated O/H abundance for GN-z11 determined by Z. Martinez et al. (2025) makes it consistent with some carbon enrichment from WC stars, as shown in Figure 5. However, with a metallicity of only Z ∼ 0.10 Z⊙, the WR population in RXCJ2248-ID3 is expected to consist of few WC stars, and so an updated chemical evolution model is needed to match its unique CNO abundance pattern.\r\n\r\nWe modify the C. Kobayashi & A. Ferrara (2024) dual-burst model to be more appropriate for the metal-poor conditions in RXCJ2248-ID3. In particular, the galactic chemical evolution (GCE) model uses the same star formation history and the standard IMF (for 0.01–120 M⊙) as in the fiducial model in C. Kobayashi & A. Ferrara (2024) but reduces the contribution from WC stars. C/O ratios of the nucleosynthesis yields vary depending on the uncertain nuclear reaction rates (e.g., 12C(α, γ)16O) and the treatment of convection and mass loss (C. Kobayashi et al. 2006). In the updated model, 12C and 16O yields are taken from C. Kobayashi et al. (2020) for all mass ranges of stars but the contributions from the WC wind phase is scaled to ∼15% in order to match the empirical trends and theoretical expectations that most massive stars will have insufficient winds to remove their He envelopes at such low metallicities.\r\n\r\nWe plot the updated metal-poor dual-burst model in the bottom row of Figure 4 as a time-series of points that are color coded by the age since the onset of the second burst. In this model, the observed N/O, O/H, and C/O abundances of RXCJ2248-ID3 are reached simultaneously ∼4.2 Myr after the onset of the second burst. This young age is consistent with enrichment from WN stars and with the derived clump age of Myr (A. Claeyssens 2025). Thus, the N/O-enhanced and relatively C/O-deficient conditions in RXCJ2248-ID3 are produced by a short-lived evolutionary phase following intense, bursty star formation.\r\n\r\nWe note that the duration and impact of the WN phase may be significantly extended if the stars evolve in binary systems. In the M. Limongi & A. Chieffi (2018) single-star models, the WN phase typically lasts ∼0.03–0.3 Myr and, due to the metallicity-dependent winds, require high initial masses (∼40 M⊙) to expose the He- and N-rich layers. However, in close binaries, envelope stripping via mass transfer or common-envelope evolution can induce WR phases in lower-mass stars (20–30 M⊙), largely independent of the stellar metallicity. This channel can significantly prolong the WN lifetime (up to ∼1 Myr) depending on the binary mass ratio and separation (e.g., J. J. Eldridge et al. 2017; Y. Götberg et al. 2019; D. R. Aguilera-Dena et al. 2022). As a result, binary evolution may enhance both the frequency and duration of the chemically selective N/O enrichment phase, such as that observed in RXCJ2248-ID. On the other hand, L. Boco et al. (2025) successfully modeled observations of single WR stars in the SMC, suggesting that binary stripping may not be required to produce WR stars at low metallicity. Clearly, the frequency, lifetimes, and formation channels of WR stars in low-metallicity environments are not yet well understood. Future work incorporating current binary and single star WR pathways into chemical evolution models may, therefore, be essential for capturing the full range of nitrogen feedback in low-metallicity starbursts at high redshift.\r\n\r\nTaken together, the massive star enrichment scenario presented here, and explored in C. Charbonnel et al. (2023), R. Marques-Chaves et al. (2024), and C. Kobayashi & A. Ferrara (2024), demonstrates that selective enrichment of nitrogen by WN-dominated feedback can naturally reproduce the observed CNO abundance pattern in compact, low-metallicity starbursts such as RXCJ2248-ID3. We can now paint a full picture of the ISM in RXCJ2248-ID3. The consistency of N/O across ions spanning a wide range of ionization potentials suggests that the WN-enriched material has been efficiently mixed throughout the ionized gas. This apparent chemical homogeneity does not contradict the strong density and temperature stratification inferred from our diagnostics: a clumpy or multiphase ISM can remain compositionally uniform if the enriched ejecta are well dispersed. Given the extreme compactness of RXCJ2248-ID3 (Re ≈ 20 pc), the characteristic dynamical and sound-crossing times are only a few ×105 yr, comparable to or shorter than the duration of the WN phase itself. Under such conditions, turbulent and radiative mixing can rapidly homogenize the heavy-element yields, producing a chemically uniform yet physically structured nebula.\r\n\r\n5.3. The N Mass Budget\r\nA crucial point of validation is whether an intense burst of star formation so early in the Universe could have produced the amount of N present in RXCJ2248-ID3. Similar to the analysis in R. Marques-Chaves et al. (2024), we test this by first estimating the ionized nitrogen mass using\r\n\r\nwhere the atomic mass ratio is mN/mH = 14 and N/H is the nitrogen abundance of the ionized gas. The hydrogen gas mass MH is derived from the Hα luminosity as\r\n\r\nwhere mH = 1.67 × 10−27 kg, h = 6.626 × 10−27 erg s−1, νHα is the frequency of the Hα emission line, and cm3 s−1 is the Case B effective recombination coefficient for Hα assuming a Te = 1.97 × 104 K. We estimate the Hα luminosity using a luminosity distance of dL(z = 6.1025) =1.817 × 1029 cm, the collision-corrected narrow-component Hα flux, and a magnification of μ = 6.8877 (L. Furtak et al. 2025) to be LHα = 1.20 × 1042 erg s−1. Combining this LHα with the equivalent width (EW)(Hα) = 1457 Å, we derive the star formation rate (SFR) using the simulation-based SFR(Hα) calibration from I. G. Kramarenko et al. (2026). This method was developed to be more appropriate for the bursty conditions at high redshift than traditional calibrations and gives SFR = 3.2 M⊙ yr−1, similar to the SED-derived SFRs assuming a constant SFH for 1 Myr () and 10 Myr (; see Table 1). Adopting a filling factor of ε = 0.01-0.10, assuming a compact starburst (e.g., R. C. Kennicutt 1984; G. Stasińska & D. Schaerer 1997), a density of 104 cm−3, and the measured N/H value, we calculate the ionized nitrogen mass to be .\r\n\r\nWe then compute the total nitrogen mass that can be produced by the recent burst of star formation using the integrated nitrogen yield produced by the modified C. Kobayashi & A. Ferrara (2024) model for the SED-derived stellar mass of assuming a continuous SFH over the duration of the second burst (∼4.2 Myr). This results in a total N mass of 435 M⊙, implying that ∼% of the gas is retained from the WN winds and ionized when matched to the expected ionized N mass (∼) from the crudely calculated observed value. Thus, WN stars formed in a recent burst within a compact, high-density, and very clumpy/inhomogeneous (low-filling-factor) environment can plausibly explain the N mass in RXCJ2248-ID3, even at low metallicity (∼10% Z⊙), without invoking a top-heavy IMF or exotic enrichment channels.\r\n\r\n5.4. The Ephemeral Imprint of WN Star on High−z Galaxies\r\nThe prominence of N/O enhancement at z ≳ 5 but relative rarity in local star-forming galaxies likely reflects a combination of environmental conditions and evolutionary factors that are unique to the early Universe. To examine the likely environments, we plot the SFR surface density (ΣSFR) versus EW of Hβ in Figure 7 for both z ≳ 6 N emitters (RXCJ2248-ID3: M. W. Topping et al. 2024, this work; GNz9p4: D. Schaerer et al. 2024; GN-z11, EW(Hβ) inferred from Hγ: A. J. Bunker et al. 2023; S. Tacchella et al. 2023; GDS 3073: E. Vanzella et al. 2010; H. Übler et al. 2023; X. Ji et al. 2024; CEERS-1019: R. L. Larson et al. 2023; R. Marques-Chaves et al. 2024; A1703-zd6: M. W. Topping et al. 2025b) and local star-forming galaxies with enhanced SFRs from the COS Legacy Archive Spectroscopic SurveY (CLASSY; B. L. James et al. 2021; D. A. Berg et al. 2022; N/O from K. Z. Arellano-Córdova et al. 2025). The high-redshift galaxies, such as RXCJ2248-ID3, exhibit compact morphologies (Re ≲ 102 pc) that lead to much higher SFR surface densities than seen at z ∼ 0, as well as bursty star formation histories that favor the rapid buildup of massive stars capable of entering the short-lived WN phases (M⋆ > 20 M⊙). The high-redshift N emitters also have high Hβ EWs (>200 Å) that are indicative of young current bursts of star formation (<5 Myr). This suggests that compactness alone is not enough to observe enhanced N/O; we must also observe these galaxies at the fleeting moments of very young bursts when WR stars are most active.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 7. SFR surface density versus Hβ EW for high-redshift (z > 5) N emitters versus z ∼ 0 galaxies from the CLASSY survey (SFR: D. A. Berg et al. 2022; N/O: K. Z. Arellano-Córdova et al. 2025), which have enhanced SFRs similar to z ∼ 2–3 galaxies. High-redshift N emitters are only observed at young ages (≲5 Myr), as indicated by the high Hβ EWs (EW> 200 Å), and in compact, dense environments (ΣSFR > 10 M⊙ yr−1 kpc−1). Note that RXCJ2248-ID3 is plotted here using the properties derived from M. W. Topping et al. (2024) for continuous star formation to be consistent with the other N-emitter measurements.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nFigure 7 suggests a scenario of elevated N/O at low metallicity being preferentially seen in galaxies with high SFR surface densities and young stellar ages (e.g., D. Schaerer et al. 2024; M. W. Topping et al. 2024; Z. Martinez et al. 2025). R. Marques-Chaves et al. (2024) also suggest that the elevated N/O and high-ionization spectrum of CEERS-1019 trace a short evolutionary window of a ≲5 Myr burst dominated by WN-like feedback. Furthermore, the theoretical models of C. Charbonnel et al. (2023) predict that such phases are characteristic of young, dense stellar systems, potentially analogous to protoglobular clusters, reinforcing that our observed WN-driven enrichment is a natural outcome of clustered, bursty star formation at early times.\r\n\r\nAt low metallicity, weaker stellar winds require higher initial masses for stars to reach the WR phase, so a larger total stellar mass must form in a burst to produce a detectable population of WN stars. In compact galaxies beyond cosmic noon, this condition is naturally met in systems with high SFR surface densities, which statistically sample the upper IMF more fully and produce a detectable population of WN stars (e.g., J. Brinchmann et al. 2008; M. Shirazi & J. Brinchmann 2012). Furthermore, the WR enrichment signature is short-lived: it must be captured during the brief WN-dominated phase (tburst ≲ 5 Myr and ΔtWN ≲ 0.3 Myr), before dilution from WC stars, CCSNe, or delayed AGB enrichment. These timing constraints imply that only a small fraction of the star-forming galaxies in the distant Universe will be caught in this phase. The detection of WR-driven N/O enhancement at high redshift thus reflects a brief evolutionary stage where intense, rapid feedback from a large number of WN stars briefly imprints nonuniform elemental enrichment patterns (i.e., elevated N/O), which are expected to be quickly washed away. As soon as the system evolves beyond the WN phase, subsequent WC or CCSN yields will rapidly dilute the N excess and alter the overall abundance patter (e.g., increasing C/O, lowering N/C).\r\n\r\nRecently, M. W. Topping et al. (2025b) showed that galaxies with significant N iv] emission (corresponding to extreme N/O enhancement), are found exclusively among galaxies with extreme [O iii]+Hβ EWs of 2600–4200 Å. Galaxies with such high [O iii]+Hβ EWs are in the upper 2% tail of the EW distribution at z ≳ 4 and are outliers at z ∼ 0. This strongly suggests that high N/O outliers are confined to the youngest stellar populations undergoing their most intense bursts of star formation in the early Universe (e.g., R. Endsley et al. 2023, 2025; J. Matthee et al. 2023; M. W. Topping et al. 2025b).\r\n\r\nIn this context, M. W. Topping et al. (2025b) found that 30% of galaxies with EW[O III] + Hβ > 2000 Å show strong nitrogen emission, corresponding to ∼0.6% of their UV-selected parent population. If this 0.6% population corresponds to enhanced N/O during the ΔtWN ∼ 0.3 Myr WN phase, it would imply a characteristic burst timescale of ∼50 Myr. A practical consequence is that young bursts substantially increase the light-to-mass ratios and, thus, the likelihood of detection in flux-limited samples (e.g., C. A. Mason et al. 2023; J. B. Muñoz et al. 2023; G. Sun et al. 2023). Therefore, the observed frequency of strong nitrogen emitters at fixed MUV is likely biased high relative to their intrinsic abundance (e.g., at fixed stellar mass). Given the detectability bias toward burst phases, this tburst may represent a lower limit, with the true interval plausibly longer. This timescale is supported by recent analyses of the scatter in the star-forming main sequence and time-resolved SFR indicators at z ∼ 3–9 that suggest burst cycles of tens-of-megayear timescales (albeit with broad distributions, e.g., C. Simmonds et al. 2025). Thus, the combination of extreme-EW selection and N iv] frequency provides a novel timing argument that WN-driven enrichment is tightly coupled to very young, transient starburst phases beyond cosmic noon.\r\n\r\nTaken together, the arguments presented in this work suggest that nitrogen outliers are not exotic exceptions, but rather a brief, WN-enriched phase that any high-redshift galaxy with sufficiently high SFR surface density can pass through. In contrast, numerous low-redshift WR galaxies exhibit young populations that include WN and WC stars but show little or no N/O enhancement (e.g., Y. I. Izotov et al. 2006; C. Kehrig et al. 2013). This difference underscores that similar stellar populations do not guarantee the same chemical signatures; instead, the extreme densities, compactness, and rapid mixing timescales of high-redshift starbursts likely make WN-driven enrichment both more pronounced and more transient. In this view, N/O outliers in the early Universe are not anomalies, but rather are the chemical fingerprints of galaxies caught midburst, showing fleeting yet inevitable markers of early galaxy evolution.\r\n\r\n6. Conclusions\r\nWe have presented a detailed enrichment scenario by WN stars that explains the extreme nitrogen enrichment in the metal-poor (∼10% Z⊙), high surface-density (1.34 × 103 M⊙ pc−2), high-redshift (z = 6.1025), lensed galaxy RXCJ2248-ID3. These measurements were made possible by exceptionally deep JWST/NIRSpec medium-resolution spectroscopy of RXCJ2248-ID3, obtained as part of the GLIMPSE-D survey. The unprecedented depth and S/N of the GLIMPSE-D spectrum allow spectral measurements typically limited to the nearby Universe, including consistent broad components in the Balmer series and [O iii] λ4364 and λλ4960,5008 lines, faint [Ar iv] λλ4713,4741 emission, and signatures of WR stars. Specifically, we detected the emission characteristic of WN-type stars, including strong N iii λ4642 and broadened He ii λ1640 and λ4687 emission, marking RXCJ2248-ID3 as the most distant galaxy to date with spectroscopic detections of WR stars.\r\n\r\nWe performed a detailed nebular analysis, self-consistently measuring the reddening, high-ionization temperature (Te(O+2)), and densities from five different diagnostics across a wide ionization range. We measure a low reddening value of from the Hγ/Hβ ratio but find an excess in the Hα/Hβ ratio of 0.204 due to collisional excitation of Hα. The measured densities span the range of 1.15 × 103 cm−3 ≤ ne ≤ 2.65 × 105 cm−3 and show strong evidence for nebular density stratification, with systematically higher densities in the highest-ionization gas and UV emission tracing gas at higher densities than those traced by optical diagnostics. This structure implies a highly clumpy, multiphase ISM. We note that such high-density, multiphase gas leads to densities from optical diagnostics that are biased to the low end of the density range due to their low critical densities. Therefore, we recommend using UV density diagnostics because they are more robust in high-density environments: ne(Si+2), ne(C+2), and ne(N+3) trace the densities in the low-, intermediate-, and high-ionization gas, respectively. As a result, we measure a direct-method metallicity of .\r\n\r\nUsing the full rest-UV+optical spectra, we present the first robust, consistent measurements of N/O abundance in any galaxy using three ionization stages of nitrogen (N+/O+, N+2/O+2, N+3/O+2). The uniformity of our N/O measurements suggests that the N/O enrichment is spatially extended and well mixed throughout the ionized ISM. Empirical trends suggest C/O should follow a similar trend as N/O, and thus also be enhanced. In contrast, we find C/O to be significantly depleted relative to N/O, suggesting nonuniform elemental enrichment likely driven by WN stars with little to no contribution from WC stars.\r\n\r\nThe CNO abundance pattern is best reproduced by a modified version of the dual-burst chemical evolution model from C. Kobayashi & A. Ferrara (2024) that reduces the contribution from WC stars relative to WN stars, as expected in metal-poor environments. The resulting short-lived WN phase ejects N-rich, C-poor material. We use this chemical evolution model to assess whether the observed N mass can plausibly arise from the recent star formation in RXCJ2248-ID3 and estimate an ionized N mass of 435 M⊙. This value is consistent with the N mass estimated from the observed emission lines of M⊙ if % of the N gas is ionized.\r\n\r\nThese results demonstrate that standard stellar evolution models can reproduce both the CNO pattern and the total nitrogen mass observed without invoking an exotic IMF or enrichment channel. The uniform N/O ratios across multiple ionization zones further suggest that the WN yields were rapidly mixed into a relatively pristine ambient ISM, preserving the global enhancement observed in RXCJ2248-ID3. Although RXCJ2248-ID3 exhibits strong density and temperature stratification, this structural complexity does not necessarily imply chemical inhomogeneity. The consistent N/O ratios across ions tracing vastly different physical conditions indicate that the enriched material was efficiently dispersed throughout the multiphase ISM. In such a compact (Re ≈ 20 pc), high-pressure environment, turbulent and radiative mixing can homogenize the chemical composition on timescales comparable to, or shorter than, the brief WN phase itself, yielding a chemically uniform yet physically clumpy nebula.\r\n\r\nImportantly, the abundance pattern and physical conditions observed in RXCJ2248-ID3 can only be explained if the galaxy is caught during a narrow evolutionary window within a few megayears of a massive, compact starburst when WN stars dominate chemical feedback. At low metallicity, stars require higher initial masses to reach the WR phase, making such enrichment episodes rare and dependent on sufficiently high SFRs to fully populate the upper IMF. Furthermore, the WN phase itself is extremely short-lived (∼0.03–0.3 Myr) and easily masked by subsequent WC winds, CCSNe, or AGB stars contributions. These timing and SFR constraints make WR-driven N/O enhancement a rare phenomenon associated with extreme starburst conditions that are more common in the early Universe, and which are scarce in the local Universe.\r\n\r\nOur results suggest that the WN-driven N/O enrichment we observe is not a peculiar property of a single system, but rather a brief phase that essentially all high-redshift galaxies (z > 5) with sufficiently high SFR surface densities to produce significant numbers of WN stars likely undergo. In particular, the work of M. W. Topping et al. (2025b) can be used to link N/O outliers to the most extreme [O iii]+Hβ EWs. The observed frequency of such EWs combined with the short lifetime of the WN phase implies a burst cycle of order ∼50 Myr, consistent with galaxies repeatedly cycling through short, bursty episodes of enrichment. Thus, the GLIMPSE-D spectrum of RXCJ2248-ID3 provides not only the first direct evidence of WN stars shaping the chemical evolution of z > 5 galaxies but also a timing argument that situates N/O outliers as a natural, fleeting, phase of high-redshift star formation.\r\n\r\nTaken together, our findings are a glimpse into a short-lived phase of chemically selective enrichment from WN stars at cosmic dawn, providing a physically self-consistent solution to the extreme N/O enhancement and relative C/O depletion observed in RXCJ2248-ID3 and galaxies like it. Thus, RXCJ2248-ID3 serves as a benchmark case for interpreting chemically enriched, stratified, multiphase starbursts in the early Universe.\r\n\r\nAcknowledgments\r\nWe thank the referee for their thorough review of our calculations and analysis and for their helpful suggestions, which greatly improved the robustness of our results and the clarity of the text. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope. The data were obtained from the Mikulski Archive for Space Telescopes at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127 for JWST. These observations are associated with program #9223. This work has received funding from the Swiss State Secretariat for Education, Research and Innovation (SERI) under contract No. MB22.00072, as well as from the Swiss National Science Foundation (SNSF) through project grant 200020_207349. The Cosmic Dawn Center (DAWN) is funded by the Danish National Research Foundation under grant DNRF140. The Dunlap Institute is funded through an endowment established by the David Dunlap family and the University of Toronto. We acknowledge the support of the Canadian Space Agency (CSA) [25JWGO4A06]. HA acknowledges support from CNES, focused on the JWST mission, and the Programme National Cosmology and Galaxies (PNCG) of CNRS/INSU with INP and IN2P3, co-funded by CEA and CNES and support by the French National Research Agency (ANR) under grant ANR-21-CE31-0838. The JWST data presented in this article from program #9223 were obtained from the Mikulski Archive for Space Telescopes (MAST) at the Space Telescope Science Institute. The specific observations analyzed can be accessed via DOI: 10.17909/8642-1k68." article_number: '112' article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Danielle A. full_name: Berg, Danielle A. last_name: Berg - first_name: Rohan P. full_name: Naidu, Rohan P. last_name: Naidu - first_name: John full_name: Chisholm, John last_name: Chisholm - first_name: Hakim full_name: Atek, Hakim last_name: Atek - first_name: Seiji full_name: Fujimoto, Seiji last_name: Fujimoto - first_name: Vasily full_name: Kokorev, Vasily last_name: Kokorev - first_name: Lukas J. full_name: Furtak, Lukas J. last_name: Furtak - first_name: Chiaki full_name: Kobayashi, Chiaki last_name: Kobayashi - first_name: Daniel full_name: Schaerer, Daniel last_name: Schaerer - first_name: Angela full_name: Adamo, Angela last_name: Adamo - first_name: Qinyue full_name: Fei, Qinyue last_name: Fei - first_name: Damien full_name: Korber, Damien last_name: Korber - first_name: Jorryt J full_name: Matthee, Jorryt J id: 7439a258-f3c0-11ec-9501-9df22fe06720 last_name: Matthee orcid: 0000-0003-2871-127X - first_name: Rui full_name: Marques-Chaves, Rui last_name: Marques-Chaves - first_name: Zorayda full_name: Martinez, Zorayda last_name: Martinez - first_name: Kristen B.W. full_name: Mcquinn, Kristen B.W. last_name: Mcquinn - first_name: Julian B. full_name: Muñoz, Julian B. last_name: Muñoz - first_name: Pascal A. full_name: Oesch, Pascal A. last_name: Oesch - first_name: Alberto full_name: Saldana-Lopez, Alberto last_name: Saldana-Lopez - first_name: Daniel P. full_name: Stark, Daniel P. last_name: Stark - first_name: Mabel G. full_name: Stephenson, Mabel G. last_name: Stephenson - first_name: Tiger Yu Yang full_name: Hsiao, Tiger Yu Yang last_name: Hsiao citation: ama: 'Berg DA, Naidu RP, Chisholm J, et al. A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy. The Astrophysical Journal. 2026;1003(2). doi:10.3847/1538-4357/ae5e4c' apa: 'Berg, D. A., Naidu, R. P., Chisholm, J., Atek, H., Fujimoto, S., Kokorev, V., … Hsiao, T. Y. Y. (2026). A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae5e4c' chicago: 'Berg, Danielle A., Rohan P. Naidu, John Chisholm, Hakim Atek, Seiji Fujimoto, Vasily Kokorev, Lukas J. Furtak, et al. “A Fleeting GLIMPSE of N/O Enrichment at Cosmic Dawn: Evidence for Wolf Rayet N Stars in a z = 6.1 Galaxy.” The Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae5e4c.' ieee: 'D. A. Berg et al., “A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy,” The Astrophysical Journal, vol. 1003, no. 2. IOP Publishing, 2026.' ista: 'Berg DA, Naidu RP, Chisholm J, Atek H, Fujimoto S, Kokorev V, Furtak LJ, Kobayashi C, Schaerer D, Adamo A, Fei Q, Korber D, Matthee JJ, Marques-Chaves R, Martinez Z, Mcquinn KBW, Muñoz JB, Oesch PA, Saldana-Lopez A, Stark DP, Stephenson MG, Hsiao TYY. 2026. A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy. The Astrophysical Journal. 1003(2), 112.' mla: 'Berg, Danielle A., et al. “A Fleeting GLIMPSE of N/O Enrichment at Cosmic Dawn: Evidence for Wolf Rayet N Stars in a z = 6.1 Galaxy.” The Astrophysical Journal, vol. 1003, no. 2, 112, IOP Publishing, 2026, doi:10.3847/1538-4357/ae5e4c.' short: D.A. Berg, R.P. Naidu, J. Chisholm, H. Atek, S. Fujimoto, V. Kokorev, L.J. Furtak, C. Kobayashi, D. Schaerer, A. Adamo, Q. Fei, D. Korber, J.J. Matthee, R. Marques-Chaves, Z. Martinez, K.B.W. Mcquinn, J.B. Muñoz, P.A. Oesch, A. Saldana-Lopez, D.P. Stark, M.G. Stephenson, T.Y.Y. Hsiao, The Astrophysical Journal 1003 (2026). date_created: 2026-05-31T22:02:12Z date_published: 2026-05-20T00:00:00Z date_updated: 2026-06-02T08:46:20Z day: '20' ddc: - '520' department: - _id: JoMa doi: 10.3847/1538-4357/ae5e4c external_id: arxiv: - '2511.13591' file: - access_level: open_access checksum: 1058555fdede45e10fca25d74e7977bc content_type: application/pdf creator: dernst date_created: 2026-06-02T08:46:08Z date_updated: 2026-06-02T08:46:08Z file_id: '21938' file_name: 2026_AstrophysicalJour_Berg.pdf file_size: 21249354 relation: main_file success: 1 file_date_updated: 2026-06-02T08:46:08Z has_accepted_license: '1' intvolume: ' 1003' issue: '2' language: - iso: eng month: '05' oa: 1 oa_version: Published Version publication: The Astrophysical Journal publication_identifier: eissn: - 1538-4357 issn: - 0004-637X publication_status: published publisher: IOP Publishing quality_controlled: '1' scopus_import: '1' status: public title: 'A fleeting GLIMPSE of N/O enrichment at cosmic dawn: Evidence for Wolf Rayet N stars in a z = 6.1 galaxy' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 1003 year: '2026' ... --- OA_place: publisher OA_type: hybrid _id: '21923' abstract: - lang: eng text: "The appearance of simulated natural phenomena heavily depends on the way surfaces are textured. However, applying texture maps to dynamic deformable surfaces presents a significant challenge, due to ever-shifting differences in length scales involved. When these surfaces move and advect the texture along with them, their final appearance degrades as deformed regions dramatically distort their texture map. Modifications to the texture directly at the pixel level in response to the deformation may introduce ghosting artifacts and look unnatural. In the real world, the appearance of surface details on a deforming material changes through the interplay of physical processes such as rupturing, exposure of internal structure, or wrinkling. Motivated by these behaviors, in this work we explore how physical principles can guide the texturing methods based on the measure of surface deformation.\r\nWe present two novel wave-based procedural texturing algorithms which reproduce common physical properties like advection and self-similarity, enabling the plausible animation of deforming objects with extreme texture map distortions. Our algorithms are fully procedural, require no actual physics simulation, and store no state or history of deformation besides the input UV map, making them highly parallelizable on the GPU and efficient enough for real-time applications. We show the versatility of the method by animating physical phenomena with extreme deformations such as flowing lava, stretching putty and outpouring sludge." acknowledged_ssus: - _id: ScienComp acknowledgement: "We thank the anonymous reviewers for their helpful comments, the members of the Visual Computing Group at ISTA for their feedback. We also thank Jonathan Gagnon for their help with running the Lapped Textures codes and SideFX for the Houdini Education software licenses.\r\nImages in Fig. 2 by Kisoulou and Vultured on Unsplash, Michal Jarmoluk and Public Domain Pictures from Pixabay and Hawai‘i Volcanoes NPS on flickr. This research was supported by the Scientific Service Units (SSU) of ISTA through resources provided by Scientific Computing and was funded in part by the European Union (ERC-2021-COG 101045083 CoDiNA)." article_number: '154' article_processing_charge: Yes article_type: original author: - first_name: Aleksei full_name: Kalinov, Aleksei id: 44b7120e-eb97-11eb-a6c2-e1557aa81d02 last_name: Kalinov orcid: 0000-0003-2189-3904 - first_name: Mickaël full_name: Ly, Mickaël id: 6340d7f0-b48d-11eb-b10d-b7487e71d9f1 last_name: Ly - first_name: Christian full_name: Hafner, Christian id: 400429CC-F248-11E8-B48F-1D18A9856A87 last_name: Hafner - first_name: Christopher J full_name: Wojtan, Christopher J id: 3C61F1D2-F248-11E8-B48F-1D18A9856A87 last_name: Wojtan orcid: 0000-0001-6646-5546 citation: ama: Kalinov A, Ly M, Hafner C, Wojtan C. Physics-inspired procedural texturing of extremely deformable surfaces. ACM Transactions on Graphics. 45(4). doi:10.1145/3811353 apa: 'Kalinov, A., Ly, M., Hafner, C., & Wojtan, C. (n.d.). Physics-inspired procedural texturing of extremely deformable surfaces. ACM Transactions on Graphics. Los Angeles, CA, United States: ACM. https://doi.org/10.1145/3811353' chicago: Kalinov, Aleksei, Mickaël Ly, Christian Hafner, and Chris Wojtan. “Physics-Inspired Procedural Texturing of Extremely Deformable Surfaces.” ACM Transactions on Graphics. ACM, n.d. https://doi.org/10.1145/3811353. ieee: A. Kalinov, M. Ly, C. Hafner, and C. Wojtan, “Physics-inspired procedural texturing of extremely deformable surfaces,” ACM Transactions on Graphics, vol. 45, no. 4. ACM. ista: Kalinov A, Ly M, Hafner C, Wojtan C. Physics-inspired procedural texturing of extremely deformable surfaces. ACM Transactions on Graphics. 45(4), 154. mla: Kalinov, Aleksei, et al. “Physics-Inspired Procedural Texturing of Extremely Deformable Surfaces.” ACM Transactions on Graphics, vol. 45, no. 4, 154, ACM, doi:10.1145/3811353. short: A. Kalinov, M. Ly, C. Hafner, C. Wojtan, ACM Transactions on Graphics 45 (n.d.). conference: end_date: 2026-07-23 location: Los Angeles, CA, United States name: 'SIGGRAPH: International Conference and Exhibition on Computer Graphics and Interactive Techniques' start_date: 2026-07-19 corr_author: '1' date_created: 2026-05-29T13:25:16Z date_published: 2026-07-01T00:00:00Z date_updated: 2026-06-02T08:56:50Z day: '01' ddc: - '006' department: - _id: GradSch - _id: ChWo doi: 10.1145/3811353 file: - access_level: open_access checksum: ea165bf731ddd3045f83878dcb833672 content_type: video/mp4 creator: akalinov date_created: 2026-05-29T13:19:33Z date_updated: 2026-05-29T13:19:33Z file_id: '21924' file_name: tog454-article154-supplemental.mp4 file_size: 77337231 relation: main_file success: 1 - access_level: open_access checksum: 6274cfb15ea5ba7324b74afc7b0d9629 content_type: video/mp4 creator: akalinov date_created: 2026-05-29T13:19:37Z date_updated: 2026-05-29T13:19:37Z file_id: '21925' file_name: tog454-article154-video.mp4 file_size: 226633977 relation: main_file success: 1 - access_level: open_access checksum: 9d41b322a7876be9a3311017b9973183 content_type: application/pdf creator: akalinov date_created: 2026-05-29T13:19:33Z date_updated: 2026-05-29T13:19:33Z file_id: '21926' file_name: tog454-article154-supplemental.pdf file_size: 6793867 relation: main_file success: 1 - access_level: open_access checksum: 51bc60d2de867fbfa570652dec7993b4 content_type: application/pdf creator: akalinov date_created: 2026-05-29T13:19:36Z date_updated: 2026-05-29T13:19:36Z file_id: '21927' file_name: tog454-article154-main-1.pdf file_size: 84173392 relation: main_file success: 1 file_date_updated: 2026-05-29T13:19:37Z has_accepted_license: '1' intvolume: ' 45' issue: '4' keyword: - Procedural animation language: - iso: eng month: '07' oa: 1 oa_version: Accepted Version project: - _id: 34bc2376-11ca-11ed-8bc3-9a3b3961a088 grant_number: '101045083' name: Computational Discovery of Numerical Algorithms for Animation and Simulation of Natural Phenomena publication: ACM Transactions on Graphics publication_identifier: issn: - 0730-0301 publication_status: inpress publisher: ACM quality_controlled: '1' status: public title: Physics-inspired procedural texturing of extremely deformable surfaces tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 45 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21915' abstract: - lang: eng text: Hydrological models commonly use very simple snow accumulation and melt models based on air temperature information, namely, a temperature threshold for snow accumulation as well as for snowmelt, and a melt factor. This utility emerges due to the simplicity, efficiency, and generally good performance of such models if sufficient calibration information is available. At scales beyond single gauged catchments, the estimation and evaluation of the temperature thresholds and the melt factor has been difficult due to a lack of observations on snow accumulation and melt. Using a recently published Northern Hemisphere snow water equivalent dataset (NH-SWE) and co-located climate station observations of temperature and precipitation (4736 stations across the Northern Hemisphere), this work estimates melt factors and temperature thresholds for snow modelling based on station observations and provides the first large-scale and long-term (1950–2023) evaluation of a simple temperature-index snow model and its parameters across a diverse range of snow climates. Our study reveals that the 0 °C as precipitation-phase threshold captures most snowfall days (89 %) and the 0 °C as snowmelt initiation threshold captures most snowmelt days (76 %). Adjusting large-scale uniform threshold values does not consistently improve performance across all snow accumulation and melt metrics. Estimated melt factors based on observations converge towards 3–5 mm (°C d)−1 for deeper snowpack climates (peak snow water equivalent >300 mm), but their estimation may be more challenging for colder climates with shallower snowpacks (<300 mm), conditions where the derived melt factors cover a wider range (1 to 12 mm (°C d)−1) and a much higher interannual and spatial variability. The temperature-index snow model performs consistently well, on average, across the available Northern Hemisphere data set for estimating long-term mean values of seasonal snow cover onset, snowmelt season onset, mean snow accumulation and snowmelt rates, but challenges may arise due to biases in temperature records or solid precipitation undercatch. Peak snow water equivalent is likely underestimated for deep or alpine snowpacks, while it is likely overestimated for shallow snowpacks in the coldest and continental climates. The best median performance of the temperature-index approach lies on relatively shallow snowpacks in temperate climates. This study provides valuable insights into temperature-threshold snowfall modelling and temperature-index melt modelling for applications across diverse climates and environments, and the results should help refine regional modelling approaches to enhance our understanding of snowpack responses to global warming. acknowledgement: 'AFB acknowledges funding from the UK''s Natural Environment Research Council (NERC) CENTA2 doctoral training program, grant number NE/S007350/1. AFB acknowledges support from the School of Geography, Earth and Environmental Science research fund. The computations described in this paper were performed using the University of Birmingham''s BlueBEAR HPC service, which provides a High Performance Computing service to the University''s research community. See http://www.birmingham.ac.uk/bear (last access: 15 December 2025) for more details. This research has been supported by the Natural Environment Research Council (grant no. CENTA2 NE/S007350/1).' article_processing_charge: Yes article_type: original author: - first_name: Adrià full_name: Fontrodona-Bach, Adrià id: f06891fd-9f42-11ee-8632-a20971c43046 last_name: Fontrodona-Bach - first_name: Bettina full_name: Schaefli, Bettina last_name: Schaefli - first_name: Ross full_name: Woods, Ross last_name: Woods - first_name: Joshua R. full_name: Larsen, Joshua R. last_name: Larsen citation: ama: Fontrodona-Bach A, Schaefli B, Woods R, Larsen JR. Estimating robust melt factors and temperature thresholds for snow modelling across the Northern Hemisphere. Hydrology and Earth System Sciences. 2026;30(9):2613-2636. doi:10.5194/hess-30-2613-2026 apa: Fontrodona-Bach, A., Schaefli, B., Woods, R., & Larsen, J. R. (2026). Estimating robust melt factors and temperature thresholds for snow modelling across the Northern Hemisphere. Hydrology and Earth System Sciences. Copernicus Publications. https://doi.org/10.5194/hess-30-2613-2026 chicago: Fontrodona-Bach, Adrià, Bettina Schaefli, Ross Woods, and Joshua R. Larsen. “Estimating Robust Melt Factors and Temperature Thresholds for Snow Modelling across the Northern Hemisphere.” Hydrology and Earth System Sciences. Copernicus Publications, 2026. https://doi.org/10.5194/hess-30-2613-2026. ieee: A. Fontrodona-Bach, B. Schaefli, R. Woods, and J. R. Larsen, “Estimating robust melt factors and temperature thresholds for snow modelling across the Northern Hemisphere,” Hydrology and Earth System Sciences, vol. 30, no. 9. Copernicus Publications, pp. 2613–2636, 2026. ista: Fontrodona-Bach A, Schaefli B, Woods R, Larsen JR. 2026. Estimating robust melt factors and temperature thresholds for snow modelling across the Northern Hemisphere. Hydrology and Earth System Sciences. 30(9), 2613–2636. mla: Fontrodona-Bach, Adrià, et al. “Estimating Robust Melt Factors and Temperature Thresholds for Snow Modelling across the Northern Hemisphere.” Hydrology and Earth System Sciences, vol. 30, no. 9, Copernicus Publications, 2026, pp. 2613–36, doi:10.5194/hess-30-2613-2026. short: A. Fontrodona-Bach, B. Schaefli, R. Woods, J.R. Larsen, Hydrology and Earth System Sciences 30 (2026) 2613–2636. corr_author: '1' date_created: 2026-05-24T22:01:32Z date_published: 2026-05-04T00:00:00Z date_updated: 2026-06-02T09:24:00Z day: '04' ddc: - '550' department: - _id: FrPe doi: 10.5194/hess-30-2613-2026 file: - access_level: open_access checksum: 8bde4775545f9e049ea3806144b0d5f1 content_type: application/pdf creator: dernst date_created: 2026-06-02T09:22:26Z date_updated: 2026-06-02T09:22:26Z file_id: '21940' file_name: 2026_HydrologyEarthSystemSciences_FontrodonaBach.pdf file_size: 11250378 relation: main_file success: 1 file_date_updated: 2026-06-02T09:22:26Z has_accepted_license: '1' intvolume: ' 30' issue: '9' language: - iso: eng month: '05' oa: 1 oa_version: Published Version page: 2613-2636 publication: Hydrology and Earth System Sciences publication_identifier: eissn: - 1607-7938 issn: - 1027-5606 publication_status: published publisher: Copernicus Publications quality_controlled: '1' scopus_import: '1' status: public title: Estimating robust melt factors and temperature thresholds for snow modelling across the Northern Hemisphere tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 30 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21917' abstract: - lang: eng text: A defining feature of quantum many-body systems is the exponential scaling of the Hilbert space with the number of degrees of freedom. This exponential complexity naïvely renders a complete state characterization, for instance via the complete set of bipartite Renyi entropies for all disjoint regions, a challenging task. Recently, a compact way of storing subregions' purities by encoding them as amplitudes of a fictitious quantum wave function, known as entanglement feature, was proposed. Notably, the entanglement feature can be a simple object even for highly entangled quantum states. However the complexity and practical usage of the entanglement feature for general quantum states has not been explored. In this work, we demonstrate that the entanglement feature can be efficiently learned using only a polynomial amount of samples in the number of degrees of freedom through the so-called tensor cross interpolation (TCI) algorithm, assuming it is expressible as a finite bond dimension MPS. We benchmark this learning process on Haar and random MPS states, confirming analytic expectations. Applying the TCI algorithm to quantum eigenstates of various one dimensional quantum systems, we identify cases where eigenstates have entanglement feature learnable with TCI. We conclude with possible applications of the learned entanglement feature, such as quantifying the distance between different entanglement patterns and finding the optimal one-dimensional ordering of physical indices in a given state, highlighting the potential utility of the proposed purity interpolation method. acknowledgement: "We acknowledge useful discussions with Richard Küng\r\non the interpolation methods and error spreading, Ilia\r\nA. Luchnikov, Margarita Davydova, and, in particular, Hiroshi Shinaoka, Marc Ritter, Yuriel Nuñez\r\nfor useful discussions about TCI and the various\r\nworkarounds within the TensorCrossInterpolation.jl\r\nlibrary. We also acknowledge the comments of anonymous Referee B, that encouraged us to expand the\r\nmanuscript with discussion of additional applications\r\nof entanglement feature in Section 4.3. M.S. acknowledges discussions with D. V. Savostyanov at the 2nd\r\nInternational Quantum Tensor Networks (IQTN) plenary meeting at Flatiron Institute’s Center for Computational Quantum Physics (CCQ) for introduction\r\nto the TCI approach. D.K and M.S. acknowledge support by the European Research Council (ERC) under We acknowledge useful discussions with Richard Küng\r\non the interpolation methods and error spreading, Ilia\r\nA. Luchnikov, Margarita Davydova, and, in particular, Hiroshi Shinaoka, Marc Ritter, Yuriel Nuñez\r\nfor useful discussions about TCI and the various\r\nworkarounds within the TensorCrossInterpolation.jl\r\nlibrary. We also acknowledge the comments of anonymous Referee B, that encouraged us to expand the\r\nmanuscript with discussion of additional applications\r\nof entanglement feature in Section 4.3. M.S. acknowledges discussions with D. V. Savostyanov at the 2nd\r\nInternational Quantum Tensor Networks (IQTN) plenary meeting at Flatiron Institute’s Center for Computational Quantum Physics (CCQ) for introduction\r\nto the TCI approach. D.K and M.S. acknowledge support by the European Research Council (ERC) under We acknowledge useful discussions with Richard Küng\r\non the interpolation methods and error spreading, Ilia\r\nA. Luchnikov, Margarita Davydova, and, in particular, Hiroshi Shinaoka, Marc Ritter, Yuriel Nuñez\r\nfor useful discussions about TCI and the various\r\nworkarounds within the TensorCrossInterpolation.jl\r\nlibrary. We also acknowledge the comments of anonymous Referee B, that encouraged us to expand the\r\nmanuscript with discussion of additional applications\r\nof entanglement feature in Section 4.3. M.S. acknowledges discussions with D. V. Savostyanov at the 2nd\r\nInternational Quantum Tensor Networks (IQTN) plenary meeting at Flatiron Institute’s Center for Computational Quantum Physics (CCQ) for introduction\r\nto the TCI approach. D.K and M.S. acknowledge support by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (Grant Agreement No. 850899).\r\nR.V. acknowledges partial support from the US Department of Energy, Office of Science, Basic Energy\r\nSciences, under award No. DE-SC0023999, and the\r\nSwiss National Science Foundation (grant 10008234).\r\nThis research was supported in part by grant NSF\r\nPHY-2309135 to the Kavli Institute for Theoretical\r\nPhysics (KITP)" article_number: '2114' article_processing_charge: Yes article_type: original arxiv: 1 author: - first_name: Dmytro full_name: Kolisnyk, Dmytro id: 530a7320-5355-11ee-ae5a-82a46997aaa7 last_name: Kolisnyk orcid: 0000-0002-8612-8202 - first_name: Raimel A full_name: Medina Ramos, Raimel A id: CE680B90-D85A-11E9-B684-C920E6697425 last_name: Medina Ramos orcid: 0000-0002-5383-2869 - first_name: Romain full_name: Vasseur, Romain last_name: Vasseur - first_name: Maksym full_name: Serbyn, Maksym id: 47809E7E-F248-11E8-B48F-1D18A9856A87 last_name: Serbyn orcid: 0000-0002-2399-5827 citation: ama: Kolisnyk D, Medina Ramos RA, Vasseur R, Serbyn M. Tensor cross interpolation of purities in quantum many-body systems. Quantum. 2026;10. doi:10.22331/q-2026-05-22-2114 apa: Kolisnyk, D., Medina Ramos, R. A., Vasseur, R., & Serbyn, M. (2026). Tensor cross interpolation of purities in quantum many-body systems. Quantum. Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften. https://doi.org/10.22331/q-2026-05-22-2114 chicago: Kolisnyk, Dmytro, Raimel A Medina Ramos, Romain Vasseur, and Maksym Serbyn. “Tensor Cross Interpolation of Purities in Quantum Many-Body Systems.” Quantum. Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften, 2026. https://doi.org/10.22331/q-2026-05-22-2114. ieee: D. Kolisnyk, R. A. Medina Ramos, R. Vasseur, and M. Serbyn, “Tensor cross interpolation of purities in quantum many-body systems,” Quantum, vol. 10. Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften, 2026. ista: Kolisnyk D, Medina Ramos RA, Vasseur R, Serbyn M. 2026. Tensor cross interpolation of purities in quantum many-body systems. Quantum. 10, 2114. mla: Kolisnyk, Dmytro, et al. “Tensor Cross Interpolation of Purities in Quantum Many-Body Systems.” Quantum, vol. 10, 2114, Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften, 2026, doi:10.22331/q-2026-05-22-2114. short: D. Kolisnyk, R.A. Medina Ramos, R. Vasseur, M. Serbyn, Quantum 10 (2026). corr_author: '1' date_created: 2026-05-26T19:39:12Z date_published: 2026-05-22T00:00:00Z date_updated: 2026-06-02T09:15:13Z day: '22' ddc: - '530' department: - _id: MaSe - _id: GradSch doi: 10.22331/q-2026-05-22-2114 ec_funded: 1 external_id: arxiv: - '2503.17230' file: - access_level: open_access checksum: f8ce78607ad06120cdf894dc8cef55da content_type: application/pdf creator: dernst date_created: 2026-06-02T09:12:11Z date_updated: 2026-06-02T09:12:11Z file_id: '21939' file_name: 2026_Quantum_Kolisnyk.pdf file_size: 3284798 relation: main_file success: 1 file_date_updated: 2026-06-02T09:12:11Z has_accepted_license: '1' intvolume: ' 10' language: - iso: eng month: '05' oa: 1 oa_version: Published Version project: - _id: 23841C26-32DE-11EA-91FC-C7463DDC885E call_identifier: H2020 grant_number: '850899' name: 'Non-Ergodic Quantum Matter: Universality, Dynamics and Control' publication: Quantum publication_identifier: eissn: - 2521-327X publication_status: published publisher: Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften quality_controlled: '1' status: public title: Tensor cross interpolation of purities in quantum many-body systems tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 10 year: '2026' ... --- OA_place: publisher OA_type: hybrid PlanS_conform: '1' _id: '21929' abstract: - lang: eng text: 'The import of proteins into mitochondria poses fundamental mechanistic challenges: aggregation-prone precursor proteins must be maintained in aqueous compartments and threaded through narrow pores without becoming stuck or mislocalized. Recent evidence from mitochondrial protein import studies and other chaperone systems underscores the critical role of dynamics in balancing sufficiently tight binding, promiscuity, specificity, and release. Dynamic binding of client precursor proteins to import machinery components arises naturally from the avidity of their interactions. Conformational entropy enhances their stability, while the multivalent nature of these interactions ensures that client transfer to downstream insertases occurs without a substantial energy barrier. Here, we discuss this emerging paradigm of dynamic protein handling, using examples where dynamic structures have been resolved and highlight outstanding questions.' acknowledgement: We gratefully acknowledge research funding by the Austrian Science Fund (FWF), projects 10.55776/PAT1647625 and 10.55776/I6223. We thank Prof. Long Li (Peking University) for providing structural models and EM density for the TOM and TIM23 complexes, used to generate part of Figure 3. Open Access funding provided by Institute of Science and Technology Austria. article_number: e70630 article_processing_charge: Yes (via OA deal) article_type: original author: - first_name: Jakob full_name: Schneider, Jakob id: 64368429-eb97-11eb-a6c2-c980b1f44415 last_name: Schneider - first_name: Undina full_name: Guillerm, Undina id: bb74f472-ae54-11eb-9835-bc9c22fb1183 last_name: Guillerm - first_name: Caroline full_name: Simoes Pereira, Caroline id: 87266c4a-96d2-11ef-be2c-fe5633233ec3 last_name: Simoes Pereira - first_name: Paul full_name: Schanda, Paul id: 7B541462-FAF6-11E9-A490-E8DFE5697425 last_name: Schanda orcid: 0000-0002-9350-7606 citation: ama: Schneider J, Guillerm U, Simoes Pereira C, Schanda P. Dynamic disorder is crucial for mitochondrial protein import. Protein Science. 2026;35(6). doi:10.1002/pro.70630 apa: Schneider, J., Guillerm, U., Simoes Pereira, C., & Schanda, P. (2026). Dynamic disorder is crucial for mitochondrial protein import. Protein Science. Wiley. https://doi.org/10.1002/pro.70630 chicago: Schneider, Jakob, Undina Guillerm, Caroline Simoes Pereira, and Paul Schanda. “Dynamic Disorder Is Crucial for Mitochondrial Protein Import.” Protein Science. Wiley, 2026. https://doi.org/10.1002/pro.70630. ieee: J. Schneider, U. Guillerm, C. Simoes Pereira, and P. Schanda, “Dynamic disorder is crucial for mitochondrial protein import,” Protein Science, vol. 35, no. 6. Wiley, 2026. ista: Schneider J, Guillerm U, Simoes Pereira C, Schanda P. 2026. Dynamic disorder is crucial for mitochondrial protein import. Protein Science. 35(6), e70630. mla: Schneider, Jakob, et al. “Dynamic Disorder Is Crucial for Mitochondrial Protein Import.” Protein Science, vol. 35, no. 6, e70630, Wiley, 2026, doi:10.1002/pro.70630. short: J. Schneider, U. Guillerm, C. Simoes Pereira, P. Schanda, Protein Science 35 (2026). corr_author: '1' date_created: 2026-05-31T22:02:12Z date_published: 2026-06-01T00:00:00Z date_updated: 2026-06-02T07:26:34Z day: '01' ddc: - '572' department: - _id: GradSch - _id: PaSc doi: 10.1002/pro.70630 external_id: pmid: - '42159315' file: - access_level: open_access checksum: e0163459a7238fdcc3fc5e17bedcce9a content_type: application/pdf creator: dernst date_created: 2026-06-02T07:23:12Z date_updated: 2026-06-02T07:23:12Z file_id: '21937' file_name: 2026_ProteinScience_Schneider.pdf file_size: 3897305 relation: main_file success: 1 file_date_updated: 2026-06-02T07:23:12Z has_accepted_license: '1' intvolume: ' 35' issue: '6' language: - iso: eng month: '06' oa: 1 oa_version: Published Version pmid: 1 project: - _id: bdb9578d-d553-11ed-ba76-ed5d39fce6f0 grant_number: I06223 name: Structure and mechanism of the mitochondrial MIM insertase publication: Protein Science publication_identifier: eissn: - 1469-896X issn: - 0961-8368 publication_status: published publisher: Wiley quality_controlled: '1' scopus_import: '1' status: public title: Dynamic disorder is crucial for mitochondrial protein import tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 35 year: '2026' ... --- DOAJ_listed: '1' OA_place: publisher OA_type: gold PlanS_conform: '1' _id: '21914' abstract: - lang: eng text: 'Cyclic adenosine monophosphate (cAMP) is a fundamental second messenger involved in diverse signaling pathways across both animals and plants. While the role of 3′,5′-cAMP has been extensively characterized, the biological significance of its structural isomer, 2′,3′-cAMP, remains largely unexplored, particularly in plants. Here, we show that 2′,3′-cAMP and 3′,5′-cAMP represent parallel signaling systems in Arabidopsis thaliana, with different enzymatic origins and largely distinct downstream effects. In vitro enzymatic assays show that plant adenylate cyclases (ACs), including AFB5 and HpAC1, produce specifically 3′,5′-cAMP from ATP, whereas the TIR domain of protein L7 also catalyzes the formation of 2′,3′-cAMP from RNA. Comprehensive multiomics analyses reveal that two isomers elicit distinct yet partially overlapping metabolic, proteomic, and transcriptional response: 2′,3′-cAMP activates broad, stress-adaptive gene expression reprogramming, while 3′,5′-cAMP fine-tunes responses related to nutrient status and cellular homeostasis. Our findings establish the existence of dual cAMP signaling systems in plants, each with specialized functions and provide insights into the complex regulatory networks governing plant physiology.' acknowledged_ssus: - _id: MassSpec - _id: LifeSc acknowledgement: " We thank J. Chai and D. Yu for providing the MBP-fused L7TIR plasmid and K. Jaworski (Nicolaus Copernicus University) for the GST-­HpAC1 plasmid. We also thank M. Randuch and L. Fiedler for providing vectors for recombinant AFB5 and ADCY. We are also grateful to E. Dutkiewicz, L. Trübestein, N. Krasnici and A. Michaelis for excellent technical\r\nassistance. We acknowledge the support of the LSF Mass Spectrometry Service and the Lab\r\nSupport Facility at the Institute of Science and Technology Austria for their contributions,\r\nincluding consultation on size exclusion chromatography, LC/MS experimental design,\r\nmetabolomics sample preparation, LC/MS method optimization, data acquisition, raw data\r\nanalysis, and absolute quantification. This project is supported by the European\r\nResearch Council (ERC) under the European Union’s Horizon 2020 research and innovation\r\nprogram (101142681 CYNIPS) and Austrian Science Fund (FWF; P 37051-B), both to J.Friml.\r\nWe acknowledge the generous support of the Taif University Researchers Supporting\r\nProject: TURSP-­HC2022/02 and Max-Planck-Society to A.S. " article_number: aea7828 article_processing_charge: Yes article_type: original author: - first_name: Mingyue full_name: Li, Mingyue id: 01f96916-0235-11eb-9379-a323192643b7 last_name: Li - first_name: Monika full_name: Chodasiewicz, Monika last_name: Chodasiewicz - first_name: Malavika full_name: Muraleedharan, Malavika last_name: Muraleedharan - first_name: Israel M. full_name: Lopez, Israel M. last_name: Lopez - first_name: Michal full_name: Gorka, Michal last_name: Gorka - first_name: Olga full_name: Kerber, Olga last_name: Kerber - first_name: Saqer S. full_name: Alotaibi, Saqer S. last_name: Alotaibi - first_name: Andrew D.L. full_name: Nelson, Andrew D.L. last_name: Nelson - first_name: Rene full_name: Lenobel, Rene last_name: Lenobel - first_name: Jaroslava full_name: Friedecká, Jaroslava last_name: Friedecká - first_name: Aleksandra full_name: Skirycz, Aleksandra last_name: Skirycz - first_name: Jiří full_name: Friml, Jiří id: 4159519E-F248-11E8-B48F-1D18A9856A87 last_name: Friml orcid: 0000-0002-8302-7596 citation: ama: Li M, Chodasiewicz M, Muraleedharan M, et al. Biogenesis and downstream effects of 3’,5’ and 2’,3’ cAMP isomers in plants. Science Advances. 2026;12(19). doi:10.1126/sciadv.aea7828 apa: Li, M., Chodasiewicz, M., Muraleedharan, M., Lopez, I. M., Gorka, M., Kerber, O., … Friml, J. (2026). Biogenesis and downstream effects of 3’,5’ and 2’,3’ cAMP isomers in plants. Science Advances. AAAS. https://doi.org/10.1126/sciadv.aea7828 chicago: Li, Mingyue, Monika Chodasiewicz, Malavika Muraleedharan, Israel M. Lopez, Michal Gorka, Olga Kerber, Saqer S. Alotaibi, et al. “Biogenesis and Downstream Effects of 3’,5’ and 2’,3’ CAMP Isomers in Plants.” Science Advances. AAAS, 2026. https://doi.org/10.1126/sciadv.aea7828. ieee: M. Li et al., “Biogenesis and downstream effects of 3’,5’ and 2’,3’ cAMP isomers in plants,” Science Advances, vol. 12, no. 19. AAAS, 2026. ista: Li M, Chodasiewicz M, Muraleedharan M, Lopez IM, Gorka M, Kerber O, Alotaibi SS, Nelson ADL, Lenobel R, Friedecká J, Skirycz A, Friml J. 2026. Biogenesis and downstream effects of 3’,5’ and 2’,3’ cAMP isomers in plants. Science Advances. 12(19), aea7828. mla: Li, Mingyue, et al. “Biogenesis and Downstream Effects of 3’,5’ and 2’,3’ CAMP Isomers in Plants.” Science Advances, vol. 12, no. 19, aea7828, AAAS, 2026, doi:10.1126/sciadv.aea7828. short: M. Li, M. Chodasiewicz, M. Muraleedharan, I.M. Lopez, M. Gorka, O. Kerber, S.S. Alotaibi, A.D.L. Nelson, R. Lenobel, J. Friedecká, A. Skirycz, J. Friml, Science Advances 12 (2026). corr_author: '1' date_created: 2026-05-24T22:01:31Z date_published: 2026-05-08T00:00:00Z date_updated: 2026-06-02T14:36:41Z day: '08' ddc: - '580' department: - _id: JiFr doi: 10.1126/sciadv.aea7828 external_id: pmid: - '42102187' file: - access_level: open_access checksum: 75b8ef2db078652c750e34e9cd98a808 content_type: application/pdf creator: dernst date_created: 2026-06-02T14:33:55Z date_updated: 2026-06-02T14:33:55Z file_id: '21941' file_name: 2026_ScienceAdv_Li2.pdf file_size: 2014452 relation: main_file success: 1 file_date_updated: 2026-06-02T14:33:55Z has_accepted_license: '1' intvolume: ' 12' issue: '19' language: - iso: eng month: '05' oa: 1 oa_version: Published Version pmid: 1 project: - _id: 8f347782-16d5-11f0-9cad-8c19706ee739 grant_number: '101142681' name: Cyclic nucleotides as second messengers in plants - _id: 7bcece63-9f16-11ee-852c-ae94e099eeb6 grant_number: P37051 name: Guanylate cyclase activity of TIR1/AFBs auxin receptors publication: Science Advances publication_identifier: eissn: - 2375-2548 publication_status: published publisher: AAAS quality_controlled: '1' scopus_import: '1' status: public title: Biogenesis and downstream effects of 3',5' and 2',3' cAMP isomers in plants tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 12 year: '2026' ... --- OA_place: repository OA_type: green _id: '21931' abstract: - lang: eng text: In 1873, James C. Maxwell conjectured that the electric field generated by n point charges in generic position has at most (n-1)^2 isolated zeroes. The first (nonoptimal) upper bound was only obtained in 2007 by Gabrielov, Novikov, and Shapiro, who also posed two additional interesting conjectures. In this article, we give the best upper bound known to date on the number of zeroes of the electric field, and construct a counterexample to Conjecture 1.8 by Gabrielov, Novikov, and Shapiro that the number of equilibria cannot exceed those of the distance function defined by the unit point charges. Finally, we note that it is quite possible that Maxwell's quadratic upper bound is not tight, so it is prudent to find lower bounds. Hence, we also explore examples and construct configurations of charges achieving the highest ratios of the number of electric field zeroes by point charges found to this day. article_number: e70163 article_processing_charge: No article_type: original arxiv: 1 author: - first_name: Herbert full_name: Edelsbrunner, Herbert id: 3FB178DA-F248-11E8-B48F-1D18A9856A87 last_name: Edelsbrunner orcid: 0000-0002-9823-6833 - first_name: Christopher D full_name: Fillmore, Christopher D id: 35638A5C-AAC7-11E9-B0BF-5503E6697425 last_name: Fillmore - first_name: Goncalo full_name: Oliveira, Goncalo id: 58abbde8-f455-11eb-a497-98c8fd71b905 last_name: Oliveira citation: ama: Edelsbrunner H, Fillmore CD, Oliveira G. Counting equilibria of the electrostatic potential. Proceedings of the London Mathematical Society. 2026;132(5). doi:10.1112/plms.70163 apa: Edelsbrunner, H., Fillmore, C. D., & Oliveira, G. (2026). Counting equilibria of the electrostatic potential. Proceedings of the London Mathematical Society. Wiley. https://doi.org/10.1112/plms.70163 chicago: Edelsbrunner, Herbert, Christopher D Fillmore, and Goncalo Oliveira. “Counting Equilibria of the Electrostatic Potential.” Proceedings of the London Mathematical Society. Wiley, 2026. https://doi.org/10.1112/plms.70163. ieee: H. Edelsbrunner, C. D. Fillmore, and G. Oliveira, “Counting equilibria of the electrostatic potential,” Proceedings of the London Mathematical Society, vol. 132, no. 5. Wiley, 2026. ista: Edelsbrunner H, Fillmore CD, Oliveira G. 2026. Counting equilibria of the electrostatic potential. Proceedings of the London Mathematical Society. 132(5), e70163. mla: Edelsbrunner, Herbert, et al. “Counting Equilibria of the Electrostatic Potential.” Proceedings of the London Mathematical Society, vol. 132, no. 5, e70163, Wiley, 2026, doi:10.1112/plms.70163. short: H. Edelsbrunner, C.D. Fillmore, G. Oliveira, Proceedings of the London Mathematical Society 132 (2026). corr_author: '1' date_created: 2026-05-31T22:02:13Z date_published: 2026-05-01T00:00:00Z date_updated: 2026-06-02T09:24:18Z day: '01' department: - _id: HeEd - _id: TaHa doi: 10.1112/plms.70163 external_id: arxiv: - '2501.05315' intvolume: ' 132' issue: '5' language: - iso: eng main_file_link: - open_access: '1' url: https://doi.org/10.48550/arXiv.2501.05315 month: '05' oa: 1 oa_version: Preprint publication: Proceedings of the London Mathematical Society publication_identifier: eissn: - 1460-244X issn: - 0024-6115 publication_status: published publisher: Wiley quality_controlled: '1' related_material: record: - id: '21050' relation: earlier_version status: public scopus_import: '1' status: public title: Counting equilibria of the electrostatic potential type: journal_article user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 132 year: '2026' ... --- OA_place: publisher OA_type: diamond _id: '21932' abstract: - lang: eng text: We present LLMQ, an end-to-end CUDA/C++ implementation for medium-sized language-model training, e.g. 3B to 32B parameters, on affordable, commodity GPUs. These devices are characterized by low memory availability and slow communication compared to datacentre-grade GPUs. Consequently, we showcase a range of optimizations that target these bottlenecks, including activation checkpointing, offloading, and copy-engine based collectives. LLMQ is able to train or fine-tune a 7B model on a single 16GB mid-range gaming card, or a 32B model on a workstation equipped with 4 RTX 4090s. This is achieved while executing a standard 8-bit training pipeline, without additional algorithmic approximations, and maintaining FLOP utilization of around 50%. The efficiency of LLMQ rivals that of production-scale systems on much more expensive cloud-grade GPUs. acknowledgement: "We would like to thank contacts at NVIDIA (Vartika Singh, Nina Carrejo, Kyla Wilkes, and Tijmen\r\nBlankevoort), HP (Curtis Burkhalter), and Datacrunch/Verda (Paul Chang and Antonio\r\nDominguez) for hardware support that was essential to this project. ES was supported in part\r\nby ERC Proof-of-Concept grant FastML." alternative_title: - PMLR article_processing_charge: No author: - first_name: Erik full_name: Schultheis, Erik id: 2786b299-e6b0-11f0-91da-9243fe3ef96b last_name: Schultheis - first_name: Dan-Adrian full_name: Alistarh, Dan-Adrian id: 4A899BFC-F248-11E8-B48F-1D18A9856A87 last_name: Alistarh orcid: 0000-0003-3650-940X citation: ama: 'Schultheis E, Alistarh D-A. LLMQ: Efficient lower-precision LLM training for consumer GPUs. In: 2nd Conference on Parsimony and Learning. Vol 328. ML Research Press; 2026:265-284.' apa: 'Schultheis, E., & Alistarh, D.-A. (2026). LLMQ: Efficient lower-precision LLM training for consumer GPUs. In 2nd Conference on Parsimony and Learning (Vol. 328, pp. 265–284). Stanford, CA, United States: ML Research Press.' chicago: 'Schultheis, Erik, and Dan-Adrian Alistarh. “LLMQ: Efficient Lower-Precision LLM Training for Consumer GPUs.” In 2nd Conference on Parsimony and Learning, 328:265–84. ML Research Press, 2026.' ieee: 'E. Schultheis and D.-A. Alistarh, “LLMQ: Efficient lower-precision LLM training for consumer GPUs,” in 2nd Conference on Parsimony and Learning, Stanford, CA, United States, 2026, vol. 328, pp. 265–284.' ista: 'Schultheis E, Alistarh D-A. 2026. LLMQ: Efficient lower-precision LLM training for consumer GPUs. 2nd Conference on Parsimony and Learning. CPAL: Conference on Parsimony and Learning, PMLR, vol. 328, 265–284.' mla: 'Schultheis, Erik, and Dan-Adrian Alistarh. “LLMQ: Efficient Lower-Precision LLM Training for Consumer GPUs.” 2nd Conference on Parsimony and Learning, vol. 328, ML Research Press, 2026, pp. 265–84.' short: E. Schultheis, D.-A. Alistarh, in:, 2nd Conference on Parsimony and Learning, ML Research Press, 2026, pp. 265–284. conference: end_date: 2025-03-27 location: Stanford, CA, United States name: 'CPAL: Conference on Parsimony and Learning' start_date: 2025-03-24 corr_author: '1' date_created: 2026-05-31T22:02:13Z date_published: 2026-04-06T00:00:00Z date_updated: 2026-06-03T05:53:30Z day: '06' ddc: - '000' department: - _id: DaAl file: - access_level: open_access checksum: 72f9a87c70f1e2105ef64050ee5017e5 content_type: application/pdf creator: dernst date_created: 2026-06-03T05:51:19Z date_updated: 2026-06-03T05:51:19Z file_id: '21942' file_name: 2026_CPAL_Schultheis.pdf file_size: 2099944 relation: main_file success: 1 file_date_updated: 2026-06-03T05:51:19Z has_accepted_license: '1' intvolume: ' 328' language: - iso: eng month: '04' oa: 1 oa_version: Published Version page: 265-284 publication: 2nd Conference on Parsimony and Learning publication_identifier: eissn: - 2640-3498 publication_status: published publisher: ML Research Press quality_controlled: '1' related_material: link: - relation: software url: https://github.com/IST-DASLab/llmq scopus_import: '1' status: public title: 'LLMQ: Efficient lower-precision LLM training for consumer GPUs' tmp: image: /images/cc_by.png legal_code_url: https://creativecommons.org/licenses/by/4.0/legalcode name: Creative Commons Attribution 4.0 International Public License (CC-BY 4.0) short: CC BY (4.0) type: conference user_id: 2DF688A6-F248-11E8-B48F-1D18A9856A87 volume: 328 year: '2026' ...