[{"author":[{"first_name":"José M","id":"e1037a6d-646e-11ef-b402-e0ed9ab0901e","full_name":"Muñoz Hermosilla, José M","orcid":"0000-0002-1990-8508","last_name":"Muñoz Hermosilla"},{"last_name":"Miles","first_name":"Evan","full_name":"Miles, Evan"},{"last_name":"McCarthy","id":"22a2674a-61ce-11ee-94b5-d18813baf16f","first_name":"Michael","full_name":"McCarthy, Michael"},{"full_name":"Melo Velasco, Juan Vicente","id":"2611dec0-b9c6-11ed-9bea-a81c2b17a549","first_name":"Juan Vicente","last_name":"Melo Velasco"},{"last_name":"Hardmeier","first_name":"Florian","full_name":"Hardmeier, Florian"},{"first_name":"PRATEEK","id":"02734268-3e8d-11ef-80a1-cec4a088d004","full_name":"GANTAYAT, PRATEEK","last_name":"GANTAYAT"},{"last_name":"Fontrodona-Bach","first_name":"Adrià","id":"f06891fd-9f42-11ee-8632-a20971c43046","full_name":"Fontrodona-Bach, Adrià"},{"last_name":"Jouvet","full_name":"Jouvet, Guillaume","first_name":"Guillaume"},{"orcid":"0000-0002-5554-8087","last_name":"Pellicciotti","id":"b28f055a-81ea-11ed-b70c-a9fe7f7b0e70","first_name":"Francesca","full_name":"Pellicciotti, Francesca"}],"file":[{"date_updated":"2026-07-02T06:22:50Z","content_type":"application/pdf","access_level":"open_access","file_id":"22233","creator":"dernst","success":1,"file_size":284023,"relation":"main_file","checksum":"2ea3e691cfa53176d0e801b9172842d6","file_name":"2026_EGU26_MunozHermosilla.pdf","date_created":"2026-07-02T06:22:50Z"}],"oa_version":"Published Version","publication_status":"published","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"conference":{"end_date":"2026-05-08","name":"EGU General Assembly","location":"Vienna, Austria & Virtual","start_date":"2026-05-03"},"article_number":"EGU26-19367","department":[{"_id":"FrPe"},{"_id":"GradSch"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"07","year":"2026","date_updated":"2026-07-02T06:42:37Z","language":[{"iso":"eng"}],"file_date_updated":"2026-07-02T06:22:50Z","doi":"10.5194/egusphere-egu26-19367","citation":{"ieee":"J. M. Muñoz Hermosilla et al., “Constraining debris input to Oberaletsch Glacier using ensemble-based Lagrangian modelling,” in EGU General Assembly 2026, Vienna, Austria & Virtual, 2026.","apa":"Muñoz Hermosilla, J. M., Miles, E., McCarthy, M., Melo Velasco, J. V., Hardmeier, F., GANTAYAT, P., … Pellicciotti, F. (2026). Constraining debris input to Oberaletsch Glacier using ensemble-based Lagrangian modelling. In EGU General Assembly 2026. Vienna, Austria & Virtual: European Geosciences Union. https://doi.org/10.5194/egusphere-egu26-19367","chicago":"Muñoz Hermosilla, José M, Evan Miles, Michael McCarthy, Juan Vicente Melo Velasco, Florian Hardmeier, PRATEEK GANTAYAT, Adrià Fontrodona-Bach, Guillaume Jouvet, and Francesca Pellicciotti. “Constraining Debris Input to Oberaletsch Glacier Using Ensemble-Based Lagrangian Modelling.” In EGU General Assembly 2026. European Geosciences Union, 2026. https://doi.org/10.5194/egusphere-egu26-19367.","ista":"Muñoz Hermosilla JM, Miles E, McCarthy M, Melo Velasco JV, Hardmeier F, GANTAYAT P, Fontrodona-Bach A, Jouvet G, Pellicciotti F. 2026. Constraining debris input to Oberaletsch Glacier using ensemble-based Lagrangian modelling. EGU General Assembly 2026. EGU General Assembly, EGU26-19367.","ama":"Muñoz Hermosilla JM, Miles E, McCarthy M, et al. Constraining debris input to Oberaletsch Glacier using ensemble-based Lagrangian modelling. In: EGU General Assembly 2026. European Geosciences Union; 2026. doi:10.5194/egusphere-egu26-19367","short":"J.M. Muñoz Hermosilla, E. Miles, M. McCarthy, J.V. Melo Velasco, F. Hardmeier, P. GANTAYAT, A. Fontrodona-Bach, G. Jouvet, F. Pellicciotti, in:, EGU General Assembly 2026, European Geosciences Union, 2026.","mla":"Muñoz Hermosilla, José M., et al. “Constraining Debris Input to Oberaletsch Glacier Using Ensemble-Based Lagrangian Modelling.” EGU General Assembly 2026, EGU26-19367, European Geosciences Union, 2026, doi:10.5194/egusphere-egu26-19367."},"article_processing_charge":"No","status":"public","date_created":"2026-06-22T12:16:50Z","oa":1,"corr_author":"1","_id":"22119","publisher":"European Geosciences Union","day":"02","publication":"EGU General Assembly 2026","date_published":"2026-07-02T00:00:00Z","type":"conference_abstract","OA_type":"gold","has_accepted_license":"1","title":"Constraining debris input to Oberaletsch Glacier using ensemble-based Lagrangian modelling","OA_place":"publisher","ddc":["550"]},{"OA_type":"gold","ddc":["000"],"OA_place":"publisher","title":"An improved quality hierarchical congestion approximator in near-linear time","has_accepted_license":"1","date_published":"2026-06-09T00:00:00Z","das_tickbox":"0","publication":"58th Annual ACM Symposium on Theory of Computing","ec_funded":1,"scopus_import":"1","researchdata_availability":"no","type":"conference","acknowledgement":"We thank Evangelos Kosinas for helpful discussions on this topic.\r\nFunded by the European Union. Views and opinions expressed\r\nare however those of the author(s) only and do not necessarily\r\nreflect those of the European Union or the European Research\r\nCouncil Executive Agency. Neither the European Union nor the\r\ngranting authority can be held responsible for them.\r\nThis project has received funding from the European Research\r\nCouncil (ERC) under the European Union’s Horizon 2020 research\r\nand innovation programme (MoDynStruct, No. 101019564)\r\nand the Austrian Science Fund (FWF) grant DOI 10.55776/I5982. For\r\nopen access purposes, the author has applied a CC BY public copyright license to any author-accepted manuscript version arising\r\nfrom this submission.\r\nThis project has received funding from the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) – 498605858.","status":"public","article_processing_charge":"No","publisher":"Association for Computing Machinery","day":"09","_id":"22245","corr_author":"1","oa":1,"date_created":"2026-07-05T22:01:36Z","publication_identifier":{"isbn":["9798400725364"],"issn":["0737-8017"]},"abstract":[{"text":"A single-commodity congestion approximator for a graph is a compact data structure that approximately predicts the edge congestion required to route any set of single-commodity flow demands in a network. A hierarchical congestion approximator (HCA) consists of a laminar family of cuts in the graph and has numerous applications in approximating cut and flow problems in graphs, designing efficient routing schemes, and managing distributed networks.\r\nThere is a tradeoff between the running time for computing an HCA and its approximation quality. The best polynomial-time construction in an n-node graph gives an HCA with approximation quality O(log1.5n loglogn). Among near-linear time algorithms, the best previous result achieves approximation quality O(log4 n). We improve upon the latter result by giving the first near-linear time algorithm for computing an HCA with approximation quality O(log2 n loglogn). Additionally, our algorithm can be implemented in the parallel setting with polylogarithmic span and near-linear work, achieving the same approximation quality. This improves upon the best previous such algorithm, which has an O(log9n) approximation quality. We also present a lower bound of Ω(logn) for the approximation guarantee of hierarchical congestion approximators.\r\nCrucial for achieving a near-linear running time is a new partitioning routine that, unlike previous such routines, manages to avoid recursing on large subgraphs. To achieve the improved approximation quality, we introduce the new concept of border routability of a cut and provide an improved sparsest cut oracle for general vertex weights.","lang":"eng"}],"date_updated":"2026-07-06T06:59:52Z","file_date_updated":"2026-07-06T06:57:16Z","doi":"10.1145/3798129.3800851","citation":{"ieee":"M. Henzinger, R. Münk, and H. Räcke, “An improved quality hierarchical congestion approximator in near-linear time,” in 58th Annual ACM Symposium on Theory of Computing, Salt Lake City, UT, United States, 2026, pp. 1417–1428.","ista":"Henzinger M, Münk R, Räcke H. 2026. An improved quality hierarchical congestion approximator in near-linear time. 58th Annual ACM Symposium on Theory of Computing. STOC: Symposium on the Theory of Computing, 1417–1428.","ama":"Henzinger M, Münk R, Räcke H. An improved quality hierarchical congestion approximator in near-linear time. In: 58th Annual ACM Symposium on Theory of Computing. Association for Computing Machinery; 2026:1417-1428. doi:10.1145/3798129.3800851","apa":"Henzinger, M., Münk, R., & Räcke, H. (2026). An improved quality hierarchical congestion approximator in near-linear time. In 58th Annual ACM Symposium on Theory of Computing (pp. 1417–1428). Salt Lake City, UT, United States: Association for Computing Machinery. https://doi.org/10.1145/3798129.3800851","chicago":"Henzinger, Monika, Robin Münk, and Harald Räcke. “An Improved Quality Hierarchical Congestion Approximator in Near-Linear Time.” In 58th Annual ACM Symposium on Theory of Computing, 1417–28. Association for Computing Machinery, 2026. https://doi.org/10.1145/3798129.3800851.","short":"M. Henzinger, R. Münk, H. Räcke, in:, 58th Annual ACM Symposium on Theory of Computing, Association for Computing Machinery, 2026, pp. 1417–1428.","mla":"Henzinger, Monika, et al. “An Improved Quality Hierarchical Congestion Approximator in Near-Linear Time.” 58th Annual ACM Symposium on Theory of Computing, Association for Computing Machinery, 2026, pp. 1417–28, doi:10.1145/3798129.3800851."},"language":[{"iso":"eng"}],"month":"06","keyword":["Congestion Approximators","Hierarchical Graph Decompositions"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","year":"2026","conference":{"end_date":"2026-06-26","start_date":"2026-06-22","location":"Salt Lake City, UT, United States","name":"STOC: Symposium on the Theory of Computing"},"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"department":[{"_id":"MoHe"}],"oa_version":"Published Version","file":[{"date_created":"2026-07-06T06:57:16Z","checksum":"2bef46be8da6d19a641697bb0d8ade65","file_name":"2026_STOC_HenzingerMo.pdf","creator":"dernst","access_level":"open_access","file_id":"22250","relation":"main_file","file_size":919005,"success":1,"date_updated":"2026-07-06T06:57:16Z","content_type":"application/pdf"}],"publication_status":"published","page":"1417-1428","supplementarymaterial":"no","project":[{"call_identifier":"H2020","grant_number":"101019564","_id":"bd9ca328-d553-11ed-ba76-dc4f890cfe62","name":"The design and evaluation of modern fully dynamic data structures"},{"grant_number":"I05982","_id":"bda196b2-d553-11ed-ba76-8e8ee6c21103","name":"Static and Dynamic Hierarchical Graph Decompositions"}],"author":[{"last_name":"Henzinger","orcid":"0000-0002-5008-6530","id":"540c9bbd-f2de-11ec-812d-d04a5be85630","first_name":"Monika H","full_name":"Henzinger, Monika H"},{"last_name":"Münk","first_name":"Robin","full_name":"Münk, Robin"},{"full_name":"Räcke, Harald","first_name":"Harald","last_name":"Räcke"}],"arxiv":1,"external_id":{"arxiv":["2511.03716"]}},{"author":[{"last_name":"Xie","full_name":"Xie, Peiyuan","first_name":"Peiyuan","id":"488e236c-6bad-11f0-9831-859175c78e8a"},{"last_name":"Hafner","first_name":"Christian","id":"400429CC-F248-11E8-B48F-1D18A9856A87","full_name":"Hafner, Christian"},{"orcid":"0000-0001-6646-5546","last_name":"Wojtan","first_name":"Christopher J","id":"3C61F1D2-F248-11E8-B48F-1D18A9856A87","full_name":"Wojtan, Christopher J"}],"project":[{"name":"Computational Discovery of Numerical Algorithms for Animation and Simulation of Natural Phenomena","_id":"34bc2376-11ca-11ed-8bc3-9a3b3961a088","grant_number":"101045083"}],"intvolume":" 45","publication_status":"published","supplementarymaterial":"no","oa_version":"Published Version","file":[{"content_type":"application/pdf","date_updated":"2026-07-06T06:13:12Z","success":1,"file_size":5212838,"relation":"main_file","file_id":"22249","access_level":"open_access","creator":"dernst","checksum":"7e36e69f377b680a893e65b620b43813","file_name":"2026_TransactionsGraphics_Xie.pdf","date_created":"2026-07-06T06:13:12Z"}],"department":[{"_id":"GradSch"},{"_id":"ChWo"}],"article_number":"41","article_type":"original","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"quality_controlled":"1","year":"2026","month":"07","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","PlanS_conform":"1","issue":"4","citation":{"ieee":"P. Xie, C. Hafner, and C. Wojtan, “Fast and exact winding numbers for triangle meshes,” ACM Transactions on Graphics, vol. 45, no. 4. Association for Computing Machinery, 2026.","ista":"Xie P, Hafner C, Wojtan C. 2026. Fast and exact winding numbers for triangle meshes. ACM Transactions on Graphics. 45(4), 41.","ama":"Xie P, Hafner C, Wojtan C. Fast and exact winding numbers for triangle meshes. ACM Transactions on Graphics. 2026;45(4). doi:10.1145/3811339","apa":"Xie, P., Hafner, C., & Wojtan, C. (2026). Fast and exact winding numbers for triangle meshes. ACM Transactions on Graphics. Association for Computing Machinery. https://doi.org/10.1145/3811339","chicago":"Xie, Peiyuan, Christian Hafner, and Chris Wojtan. “Fast and Exact Winding Numbers for Triangle Meshes.” ACM Transactions on Graphics. Association for Computing Machinery, 2026. https://doi.org/10.1145/3811339.","short":"P. Xie, C. Hafner, C. Wojtan, ACM Transactions on Graphics 45 (2026).","mla":"Xie, Peiyuan, et al. “Fast and Exact Winding Numbers for Triangle Meshes.” ACM Transactions on Graphics, vol. 45, no. 4, 41, Association for Computing Machinery, 2026, doi:10.1145/3811339."},"doi":"10.1145/3811339","file_date_updated":"2026-07-06T06:13:12Z","volume":45,"language":[{"iso":"eng"}],"publication_identifier":{"eissn":["1557-7368"],"issn":["0730-0301"]},"abstract":[{"lang":"eng","text":"We revisit the computation of 3D generalized winding numbers, a useful measure for inside-outside classification on triangle meshes with gaps, self-intersections, and open boundaries. At the core of our new method is an analytical reduction of the surface integral that defines the winding number, resulting in a single ray-mesh intersection test and an elementary sum over boundary edges per evaluation. This construction is orders of magnitude more efficient than the state of the art in practice, which we show in an extensive performance benchmark. Conveniently, the method also reduces to the best-available asymptotic complexity in the worst case, and it introduces no approximations apart from floating-point errors. Our algorithm is conceptually simple to understand, straightforward to implement and debug, and it works reliably even on extremely noisy and corrupt input geometry."}],"date_updated":"2026-07-06T06:14:18Z","publisher":"Association for Computing Machinery","day":"03","_id":"22241","corr_author":"1","date_created":"2026-07-03T21:03:48Z","oa":1,"status":"public","acknowledgement":"We thank Sadashige Ishida and Ryusuke Sugimoto for their insightful discussions and proofreading and other members of the ISTA\r\nVisual Computing Group for their general feedback. This project was\r\nfunded in part by the European Research Council (ERC Consolidator\r\nGrant 101045083 CoDiNA).","article_processing_charge":"Yes (via OA deal)","researchdata_availability":"no","scopus_import":"1","type":"journal_article","date_published":"2026-07-03T00:00:00Z","das_tickbox":"0","publication":"ACM Transactions on Graphics","ddc":["000"],"OA_place":"publisher","title":"Fast and exact winding numbers for triangle meshes","has_accepted_license":"1","OA_type":"hybrid"},{"author":[{"last_name":"Zu","full_name":"Zu, Mengjie","id":"26dd9e7c-e86a-11eb-a854-82ac731c9ae2","first_name":"Mengjie"},{"last_name":"Goodrich","orcid":"0000-0002-1307-5074","full_name":"Goodrich, Carl Peter","id":"EB352CD2-F68A-11E9-89C5-A432E6697425","first_name":"Carl Peter"}],"intvolume":" 4","supplementarymaterial":"no","publication_status":"published","file":[{"checksum":"e2d13c30bf9c036951fd2ba3455cf72a","file_name":"2026_PRXLife_Zu.pdf","date_created":"2026-07-06T07:24:43Z","success":1,"file_size":2758728,"relation":"main_file","access_level":"open_access","file_id":"22251","creator":"dernst","content_type":"application/pdf","date_updated":"2026-07-06T07:24:43Z"}],"oa_version":"Published Version","department":[{"_id":"CaGo"}],"dataavailabilitystatement":"The data that support the findings of this article are not\r\npublicly available. The data are available from the authors\r\nupon reasonable request.","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_number":"023029","article_type":"original","year":"2026","quality_controlled":"1","issue":"2","PlanS_conform":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"06","volume":4,"language":[{"iso":"eng"}],"file_date_updated":"2026-07-06T07:24:43Z","citation":{"ieee":"M. Zu and C. P. Goodrich, “Learning by Training: Emergent physical memory from cyclically tuning disordered sphere packings,” PRX Life, vol. 4, no. 2. American Physical Society, 2026.","ista":"Zu M, Goodrich CP. 2026. Learning by Training: Emergent physical memory from cyclically tuning disordered sphere packings. PRX Life. 4(2), 023029.","ama":"Zu M, Goodrich CP. Learning by Training: Emergent physical memory from cyclically tuning disordered sphere packings. PRX Life. 2026;4(2). doi:10.1103/48k2-cw3b","apa":"Zu, M., & Goodrich, C. P. (2026). Learning by Training: Emergent physical memory from cyclically tuning disordered sphere packings. PRX Life. American Physical Society. https://doi.org/10.1103/48k2-cw3b","chicago":"Zu, Mengjie, and Carl Peter Goodrich. “Learning by Training: Emergent Physical Memory from Cyclically Tuning Disordered Sphere Packings.” PRX Life. American Physical Society, 2026. https://doi.org/10.1103/48k2-cw3b.","short":"M. Zu, C.P. Goodrich, PRX Life 4 (2026).","mla":"Zu, Mengjie, and Carl Peter Goodrich. “Learning by Training: Emergent Physical Memory from Cyclically Tuning Disordered Sphere Packings.” PRX Life, vol. 4, no. 2, 023029, American Physical Society, 2026, doi:10.1103/48k2-cw3b."},"doi":"10.1103/48k2-cw3b","date_updated":"2026-07-06T07:28:45Z","abstract":[{"text":"Many living and artificial systems improve their fitness or performance by adapting to changing environments or diverse training data. However, it remains unclear how environmental variation shapes adaptation, what is learned, and when memory of past conditions is retained. Here we show how cyclic environmental change can produce robust memory. Using a model athermal disordered solid trained by inverse design to attain target elastic properties over a prescribed range, we find that the system evolves toward a marginally absorbing manifold (MAM), meaning that training is reversible within the training range but not beyond it, which encodes a memory of that range. We further propose a general mechanism for MAM formation and memory encoding based on discontinuities in the gradient of the trained quantity. These results provide a simple, broadly applicable physical framework for how adaptive systems learn under changing environments and retain memory of past conditions.","lang":"eng"}],"publication_identifier":{"eissn":["2835-8279"]},"date_created":"2026-07-05T22:01:37Z","oa":1,"corr_author":"1","_id":"22248","day":"18","publisher":"American Physical Society","article_processing_charge":"Yes","acknowledgement":"We thank Nathan Keim, Aayush Desai, Nicholas Barton,\r\nand Gašper Tkacik for important and stimulating discussions. ˇ\r\nThe work was funded by the Institute of Science and Technology Austria.","status":"public","type":"journal_article","scopus_import":"1","researchdata_availability":"upon request","publication":"PRX Life","das_tickbox":"1","date_published":"2026-06-18T00:00:00Z","DOAJ_listed":"1","has_accepted_license":"1","title":"Learning by Training: Emergent physical memory from cyclically tuning disordered sphere packings","OA_place":"publisher","ddc":["570"],"OA_type":"gold"},{"title":"Nanomechanical sensor resolving impulsive forces below its zero-point fluctuations","OA_place":"repository","OA_type":"green","type":"journal_article","scopus_import":"1","researchdata_availability":"yes","publication":"Physical Review Letters","date_published":"2026-06-12T00:00:00Z","das_tickbox":"1","oa":1,"date_created":"2026-07-05T22:01:36Z","publisher":"American Physical Society","day":"12","_id":"22244","acknowledgement":"We thank Oscar Schmitt Kremer for his help with the Kalman filter and the rest of our colleagues at the ETH Photonics Laboratory for fruitful discussions. This research has been supported by the Swiss SERI Quantum Initiative (Grants No. UeM019-2 and No. UeM029-3), the Swiss National Science Foundation (Grant No. 51NF40-160591), and the European Research Council (ERC) under the Grant Agreement No. [951234] (Q-Xtreme ERC-2020-SyG). M. C. S. acknowledges support through an SNSF Fellowship (Grant No. 224465).","status":"public","article_processing_charge":"No","volume":136,"language":[{"iso":"eng"}],"citation":{"ieee":"M. Skrabulis et al., “Nanomechanical sensor resolving impulsive forces below its zero-point fluctuations,” Physical Review Letters, vol. 136, no. 23. American Physical Society, 2026.","apa":"Skrabulis, M., Sosa, M. C., Zambon, N. C., Militaru, A., Rossi, M., Frimmer, M., & Novotny, L. (2026). Nanomechanical sensor resolving impulsive forces below its zero-point fluctuations. Physical Review Letters. American Physical Society. https://doi.org/10.1103/9wzm-3qyb","chicago":"Skrabulis, Martynas, Martin Colombano Sosa, Nicola Carlon Zambon, Andrei Militaru, Massimiliano Rossi, Martin Frimmer, and Lukas Novotny. “Nanomechanical Sensor Resolving Impulsive Forces below Its Zero-Point Fluctuations.” Physical Review Letters. American Physical Society, 2026. https://doi.org/10.1103/9wzm-3qyb.","ama":"Skrabulis M, Sosa MC, Zambon NC, et al. Nanomechanical sensor resolving impulsive forces below its zero-point fluctuations. Physical Review Letters. 2026;136(23). doi:10.1103/9wzm-3qyb","ista":"Skrabulis M, Sosa MC, Zambon NC, Militaru A, Rossi M, Frimmer M, Novotny L. 2026. Nanomechanical sensor resolving impulsive forces below its zero-point fluctuations. Physical Review Letters. 136(23), 233604.","short":"M. Skrabulis, M.C. Sosa, N.C. Zambon, A. Militaru, M. Rossi, M. Frimmer, L. Novotny, Physical Review Letters 136 (2026).","mla":"Skrabulis, Martynas, et al. “Nanomechanical Sensor Resolving Impulsive Forces below Its Zero-Point Fluctuations.” Physical Review Letters, vol. 136, no. 23, 233604, American Physical Society, 2026, doi:10.1103/9wzm-3qyb."},"doi":"10.1103/9wzm-3qyb","abstract":[{"lang":"eng","text":"The sensitivity of a mechanical transducer is ultimately limited by its inherent quantum fluctuations. Here, we use an optically levitated nanoparticle to measure impulsive forces smaller than the particle’s zero-point momentum uncertainty. Our approach relies on reversibly squeezing the levitated particle’s center-of-mass motion to coherently amplify the perturbation. We demonstrate an impulsive-force resolution as small as 6.9 keV/c, a value 0.6 dB below the sensor’s zero-point value."}],"date_updated":"2026-07-06T07:07:24Z","publication_identifier":{"eissn":["1079-7114"],"issn":["0031-9007"]},"year":"2026","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"23","month":"06","department":[{"_id":"JoFi"}],"dataavailabilitystatement":"The data that support the findings of this article are openly available DOI 10.3929/ethz-c-000798807","article_type":"original","article_number":"233604","supplementarymaterial":"yes","publication_status":"published","oa_version":"Preprint","external_id":{"arxiv":["2601.19392"]},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.2601.19392"}],"author":[{"last_name":"Skrabulis","first_name":"Martynas","full_name":"Skrabulis, Martynas"},{"first_name":"Martin Colombano","full_name":"Sosa, Martin Colombano","last_name":"Sosa"},{"last_name":"Zambon","first_name":"Nicola Carlon","full_name":"Zambon, Nicola Carlon"},{"last_name":"Militaru","id":"d67706f8-8eb1-11ee-ad1b-9c30dfa19e0b","first_name":"Andrei","full_name":"Militaru, Andrei"},{"full_name":"Rossi, Massimiliano","first_name":"Massimiliano","last_name":"Rossi"},{"full_name":"Frimmer, Martin","first_name":"Martin","last_name":"Frimmer"},{"last_name":"Novotny","full_name":"Novotny, Lukas","first_name":"Lukas"}],"arxiv":1,"intvolume":" 136"},{"das_tickbox":"0","date_published":"2026-05-04T00:00:00Z","ec_funded":1,"publication":"ACM Transactions on Computation Theory","scopus_import":"1","researchdata_availability":"no","related_material":{"record":[{"id":"15168","relation":"earlier_version","status":"public"}]},"type":"journal_article","OA_type":"gold","OA_place":"publisher","ddc":["500"],"title":"Hardness of linearly ordered 4-colouring of 3-colourable 3-uniform hypergraphs","has_accepted_license":"1","publication_identifier":{"eissn":["1942-3462"],"issn":["1942-3454"]},"date_updated":"2026-07-06T09:06:29Z","abstract":[{"text":"A linearly ordered (LO) k-colouring of a hypergraph is a colouring of its vertices with colours 1, …, k such that each edge contains a unique maximal colour. Deciding whether an input hypergraph admits LO k-colouring with a fixed number of colours is NP-complete (and in the special case of graphs, LO colouring coincides with the usual graph colouring).\r\nHere, we investigate the complexity of approximating the “linearly ordered chromatic number” of a hypergraph. We prove that the following promise problem is NP-complete: Given a 3-uniform hypergraph, distinguish between the case that it is LO 3-colourable, and the case that it is not even LO 4-colourable. We prove this result by a combination of algebraic, topological, and combinatorial methods, building on and extending a topological approach for studying approximate graph colouring introduced by Krokhin, Opršal, Wrochna, and Živný (2023).","lang":"eng"}],"file_date_updated":"2026-07-06T09:03:02Z","citation":{"ieee":"M. Filakovský, T. V. Nakajima, J. Opršal, G. Tasinato, and U. Wagner, “Hardness of linearly ordered 4-colouring of 3-colourable 3-uniform hypergraphs,” ACM Transactions on Computation Theory, vol. 18, no. 2. Association for Computing Machinery, 2026.","apa":"Filakovský, M., Nakajima, T. V., Opršal, J., Tasinato, G., & Wagner, U. (2026). Hardness of linearly ordered 4-colouring of 3-colourable 3-uniform hypergraphs. ACM Transactions on Computation Theory. Association for Computing Machinery. https://doi.org/10.1145/3779121","chicago":"Filakovský, Marek, Tamio Vesa Nakajima, Jakub Opršal, Gianluca Tasinato, and Uli Wagner. “Hardness of Linearly Ordered 4-Colouring of 3-Colourable 3-Uniform Hypergraphs.” ACM Transactions on Computation Theory. Association for Computing Machinery, 2026. https://doi.org/10.1145/3779121.","ama":"Filakovský M, Nakajima TV, Opršal J, Tasinato G, Wagner U. Hardness of linearly ordered 4-colouring of 3-colourable 3-uniform hypergraphs. ACM Transactions on Computation Theory. 2026;18(2). doi:10.1145/3779121","ista":"Filakovský M, Nakajima TV, Opršal J, Tasinato G, Wagner U. 2026. Hardness of linearly ordered 4-colouring of 3-colourable 3-uniform hypergraphs. ACM Transactions on Computation Theory. 18(2), 10.","short":"M. Filakovský, T.V. Nakajima, J. Opršal, G. Tasinato, U. Wagner, ACM Transactions on Computation Theory 18 (2026).","mla":"Filakovský, Marek, et al. “Hardness of Linearly Ordered 4-Colouring of 3-Colourable 3-Uniform Hypergraphs.” ACM Transactions on Computation Theory, vol. 18, no. 2, 10, Association for Computing Machinery, 2026, doi:10.1145/3779121."},"doi":"10.1145/3779121","volume":18,"language":[{"iso":"eng"}],"article_processing_charge":"Yes","acknowledgement":"This research was supported by the Charles University project PRIMUS/21/SCI/014, by the Ministry of Education, Youth\r\nand Sports of the Czech Republic under the project MSCAfellow5_MUNI (CZ.02.01.01/00/22_010/0003229), and by the\r\nAustrian Science Fund (FWF project P31312-N35). This research was funded by UKRI EP/X024431/1 and by a Clarendon\r\nFund Scholarship. This project has received funding from the European Union’s Horizon 2020 research and innovation\r\nprogramme under the Marie Skłodowska-Curie Grant Agreement No 101034413.\r\n","status":"public","_id":"22247","day":"04","publisher":"Association for Computing Machinery","oa":1,"date_created":"2026-07-05T22:01:37Z","corr_author":"1","article_number":"10","article_type":"original","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"department":[{"_id":"UlWa"}],"keyword":["Constraint satisfaction problem","hypergraph colouring","promise problem","topological methods"],"month":"05","PlanS_conform":"1","issue":"2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","year":"2026","project":[{"_id":"26611F5C-B435-11E9-9278-68D0E5697425","name":"Algorithms for Embeddings and Homotopy Theory","call_identifier":"FWF","grant_number":"P31312"},{"grant_number":"101034413","call_identifier":"H2020","name":"IST-BRIDGE: International postdoctoral program","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c"}],"intvolume":" 18","arxiv":1,"author":[{"first_name":"Marek","id":"3E8AF77E-F248-11E8-B48F-1D18A9856A87","full_name":"Filakovský, Marek","last_name":"Filakovský"},{"first_name":"Tamio Vesa","full_name":"Nakajima, Tamio Vesa","last_name":"Nakajima"},{"orcid":"0000-0003-1245-3456","last_name":"Opršal","full_name":"Opršal, Jakub","first_name":"Jakub","id":"ec596741-c539-11ec-b829-c79322a91242"},{"full_name":"Tasinato, Gianluca","id":"0433290C-AF8F-11E9-A4C7-F729E6697425","first_name":"Gianluca","last_name":"Tasinato"},{"last_name":"Wagner","orcid":"0000-0002-1494-0568","full_name":"Wagner, Uli","first_name":"Uli","id":"36690CA2-F248-11E8-B48F-1D18A9856A87"}],"external_id":{"arxiv":["2312.12981"]},"oa_version":"Published Version","file":[{"content_type":"application/pdf","date_updated":"2026-07-06T09:03:02Z","success":1,"relation":"main_file","file_size":941518,"file_id":"22252","access_level":"open_access","creator":"dernst","checksum":"0399ab94085878fc810084845eabd627","file_name":"2026_TransactionsGraphics_Filakovsky.pdf","date_created":"2026-07-06T09:03:02Z"}],"publication_status":"published","supplementarymaterial":"no"},{"citation":{"apa":"Chang, H. C., Conroy, J., Tan, Z., & Zheng, D. W. (2026). Cutting planarians: Planar emulators for string graphs. In 58th Annual ACM Symposium on Theory of Computing (pp. 2140–2151). Salt Lake City, UT, United States: Association for Computing Machinery. https://doi.org/10.1145/3798129.3800917","chicago":"Chang, Hsien Chih, Jonathan Conroy, Zihan Tan, and Da Wei Zheng. “Cutting Planarians: Planar Emulators for String Graphs.” In 58th Annual ACM Symposium on Theory of Computing, 2140–51. Association for Computing Machinery, 2026. https://doi.org/10.1145/3798129.3800917.","ista":"Chang HC, Conroy J, Tan Z, Zheng DW. 2026. Cutting planarians: Planar emulators for string graphs. 58th Annual ACM Symposium on Theory of Computing. STOC: Symposium on the Theory of Computing, 2140–2151.","ama":"Chang HC, Conroy J, Tan Z, Zheng DW. Cutting planarians: Planar emulators for string graphs. In: 58th Annual ACM Symposium on Theory of Computing. Association for Computing Machinery; 2026:2140-2151. doi:10.1145/3798129.3800917","ieee":"H. C. Chang, J. Conroy, Z. Tan, and D. W. Zheng, “Cutting planarians: Planar emulators for string graphs,” in 58th Annual ACM Symposium on Theory of Computing, Salt Lake City, UT, United States, 2026, pp. 2140–2151.","mla":"Chang, Hsien Chih, et al. “Cutting Planarians: Planar Emulators for String Graphs.” 58th Annual ACM Symposium on Theory of Computing, Association for Computing Machinery, 2026, pp. 2140–51, doi:10.1145/3798129.3800917.","short":"H.C. Chang, J. Conroy, Z. Tan, D.W. Zheng, in:, 58th Annual ACM Symposium on Theory of Computing, Association for Computing Machinery, 2026, pp. 2140–2151."},"file_date_updated":"2026-07-06T10:23:09Z","doi":"10.1145/3798129.3800917","language":[{"iso":"eng"}],"publication_identifier":{"issn":["0737-8017"],"isbn":["9798400725364"]},"abstract":[{"lang":"eng","text":"In this paper we construct distance sketches for intersection graphs of arbitrary path-connected regions in the plane (known as the string graphs) in the constant and 1+ε distortion regimes. Furthermore, the distance sketches themselves are planar graphs. First, we show that every unweighted string graph G has an O(1)-distortion planar emulator: that is, there exists an edge-weighted planar graph H containing every vertex in G, such that every pair of vertices (u,v) satisfies δG(u,v) ≤ δH(u,v) ≤ O(1) · δG(u,v). Furthermore, we show that for any constant ε > 0, there is an edge-weighted planar graph H′ such that every pair of vertices (u,v) satisfies δG(u,v) ≤ δH′(u,v) ≤ (1+ε) · δG(u,v) + O(ε−4polylogn). No previous constructions of sparse distance sketches were known even for intersection graphs of simple shapes like axis-parallel rectangles or fat convex polygons.\r\nAs applications, we construct the first (1+ε, +O(1)) mixed-distortion tree cover and distance oracle for arbitrary string graphs, as well as the first additive +(εΔ+O(1))-distortion embedding of string graphs G with diameter Δ into graphs of constant treewidth O(ε−4)."}],"date_updated":"2026-07-06T10:25:23Z","publisher":"Association for Computing Machinery","day":"09","_id":"22246","corr_author":"1","date_created":"2026-07-05T22:01:37Z","oa":1,"status":"public","acknowledgement":"Hsien-Chih Chang and Jonathan Conroy are supported by the U.S.\r\nNational Science Foundation CAREER Award under the Grant No.\r\nCCF-2443017.","article_processing_charge":"No","researchdata_availability":"no","scopus_import":"1","type":"conference","date_published":"2026-06-09T00:00:00Z","das_tickbox":"0","publication":"58th Annual ACM Symposium on Theory of Computing","ddc":["500","000"],"OA_place":"publisher","title":"Cutting planarians: Planar emulators for string graphs","has_accepted_license":"1","OA_type":"gold","author":[{"last_name":"Chang","first_name":"Hsien Chih","full_name":"Chang, Hsien Chih"},{"full_name":"Conroy, Jonathan","first_name":"Jonathan","last_name":"Conroy"},{"last_name":"Tan","first_name":"Zihan","full_name":"Tan, Zihan"},{"last_name":"Zheng","first_name":"Da Wei","id":"af77956b-e859-11ef-8dc9-d301b898e32f","full_name":"Zheng, Da Wei"}],"arxiv":1,"external_id":{"arxiv":["2510.21700"]},"publication_status":"published","page":"2140-2151","supplementarymaterial":"no","oa_version":"Published Version","file":[{"date_updated":"2026-07-06T10:23:09Z","content_type":"application/pdf","creator":"dernst","file_id":"22253","access_level":"open_access","file_size":2015699,"relation":"main_file","success":1,"date_created":"2026-07-06T10:23:09Z","checksum":"c184596a3e18fee912caef4c7751a96d","file_name":"2026_STOC_Chang.pdf"}],"department":[{"_id":"MoHe"}],"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"conference":{"start_date":"2026-06-22","location":"Salt Lake City, UT, United States","name":"STOC: Symposium on the Theory of Computing","end_date":"2026-06-26"},"quality_controlled":"1","year":"2026","month":"06","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"},{"language":[{"iso":"eng"}],"file_date_updated":"2026-03-13T11:19:21Z","citation":{"ieee":"Z. Dunajova, “Geometry-driven self-organization of migrating cells and chiral filaments,” Institute of Science and Technology Austria, 2026.","chicago":"Dunajova, Zuzana. “Geometry-Driven Self-Organization of Migrating Cells and Chiral Filaments.” Institute of Science and Technology Austria, 2026. https://doi.org/10.15479/AT-ISTA-21423.","apa":"Dunajova, Z. (2026). Geometry-driven self-organization of migrating cells and chiral filaments. Institute of Science and Technology Austria. https://doi.org/10.15479/AT-ISTA-21423","ista":"Dunajova Z. 2026. Geometry-driven self-organization of migrating cells and chiral filaments. Institute of Science and Technology Austria.","ama":"Dunajova Z. Geometry-driven self-organization of migrating cells and chiral filaments. 2026. doi:10.15479/AT-ISTA-21423","short":"Z. Dunajova, Geometry-Driven Self-Organization of Migrating Cells and Chiral Filaments, Institute of Science and Technology Austria, 2026.","mla":"Dunajova, Zuzana. Geometry-Driven Self-Organization of Migrating Cells and Chiral Filaments. Institute of Science and Technology Austria, 2026, doi:10.15479/AT-ISTA-21423."},"doi":"10.15479/AT-ISTA-21423","date_updated":"2026-07-06T12:38:16Z","publication_identifier":{"isbn":["978-3-99078-076-3"],"issn":["2663-337X"]},"corr_author":"1","date_created":"2026-03-11T08:30:49Z","license":"https://creativecommons.org/licenses/by-nc-sa/4.0/","day":"11","publisher":"Institute of Science and Technology Austria","_id":"21423","status":"public","acknowledgement":"Finally, I gratefully acknowledge funding from the DOC Fellowship of the Austrian Academy\r\nof Sciences (OeAW): grant agreement 26360.","article_processing_charge":"No","type":"dissertation","related_material":{"record":[{"status":"public","relation":"part_of_dissertation","id":"13314"},{"status":"public","relation":"research_data","id":"13116"},{"relation":"research_data","id":"21439","status":"public"},{"status":"public","id":"21427","relation":"part_of_dissertation"}]},"date_published":"2026-03-11T00:00:00Z","has_accepted_license":"1","title":"Geometry-driven self-organization of migrating cells and chiral filaments","ddc":["539","570"],"OA_place":"repository","author":[{"last_name":"Dunajova","id":"4B39F286-F248-11E8-B48F-1D18A9856A87","first_name":"Zuzana","full_name":"Dunajova, Zuzana"}],"project":[{"grant_number":"26360","_id":"34d75525-11ca-11ed-8bc3-89b6307fee9d","name":"Motile active matter models of migrating cells and chiral filaments"}],"page":"110","degree_awarded":"PhD","publication_status":"published","file":[{"date_updated":"2026-03-12T20:38:52Z","embargo_to":"open_access","content_type":"application/pdf","access_level":"closed","file_id":"21446","creator":"zdunajov","file_size":14662770,"relation":"main_file","checksum":"47ce6a48a0c63f28eca6e64c9ffd2c84","embargo":"2026-09-11","file_name":"2026_Dunajova_Zuzana_Thesis_pdfA.pdf","date_created":"2026-03-12T20:38:52Z"},{"date_updated":"2026-03-13T11:19:21Z","content_type":"application/vnd.openxmlformats-officedocument.wordprocessingml.document","date_created":"2026-03-12T20:40:18Z","checksum":"5dec5afdffd47c2b0b162d0fe1bed925","file_name":"Thesis-Dunajova_source_file.docx","creator":"zdunajov","access_level":"closed","file_id":"21447","file_size":32961408,"relation":"source_file"}],"oa_version":"Published Version","department":[{"_id":"GradSch"},{"_id":"EdHa"}],"alternative_title":["ISTA Thesis"],"tmp":{"image":"/images/cc_by_nc_sa.png","legal_code_url":"https://creativecommons.org/licenses/by-nc-sa/4.0/legalcode","short":"CC BY-NC-SA (4.0)","name":"Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)"},"supervisor":[{"id":"3A9DB764-F248-11E8-B48F-1D18A9856A87","first_name":"Edouard B","full_name":"Hannezo, Edouard B","last_name":"Hannezo","orcid":"0000-0001-6005-1561"}],"acknowledged_ssus":[{"_id":"ScienComp"}],"year":"2026","user_id":"8b945eb4-e2f2-11eb-945a-df72226e66a9","month":"03"},{"OA_type":"free access","ddc":["570"],"OA_place":"repository","contributor":[{"orcid":"0000-0003-1671-393X","last_name":"Tasciyan","contributor_type":"researcher","id":"4323B49C-F248-11E8-B48F-1D18A9856A87","first_name":"Saren"},{"contributor_type":"researcher","id":"40136C2A-F248-11E8-B48F-1D18A9856A87","first_name":"Philipp","last_name":"Radler","orcid":"0000-0001-9198-2182 "}],"title":"Supplementary movies to PhD thesis “Geometry-driven self-organization of migrating cells and chiral filaments”","has_accepted_license":"1","date_published":"2026-03-12T00:00:00Z","related_material":{"record":[{"status":"public","id":"13314","relation":"used_in_publication"},{"id":"21423","relation":"used_in_publication","status":"public"},{"status":"public","id":"21427","relation":"used_in_publication"}]},"type":"research_data","status":"public","article_processing_charge":"No","publisher":"Institute of Science and Technology Austria","day":"12","_id":"21439","corr_author":"1","oa":1,"date_created":"2026-03-11T21:05:20Z","abstract":[{"text":"These files contain supplementary movies accompanying the PhD thesis “Geometry-driven self-organization of migrating cells and chiral filaments” by Zuzana Dunajova (2026). The videos provide additional visual material supporting the experiments and results described in the thesis.","lang":"eng"}],"date_updated":"2026-07-06T12:38:16Z","citation":{"ieee":"Z. Dunajova, “Supplementary movies to PhD thesis ‘Geometry-driven self-organization of migrating cells and chiral filaments.’” Institute of Science and Technology Austria, 2026.","ista":"Dunajova Z. 2026. Supplementary movies to PhD thesis “Geometry-driven self-organization of migrating cells and chiral filaments”, Institute of Science and Technology Austria, 10.15479/AT-ISTA-21439.","ama":"Dunajova Z. Supplementary movies to PhD thesis “Geometry-driven self-organization of migrating cells and chiral filaments.” 2026. doi:10.15479/AT-ISTA-21439","chicago":"Dunajova, Zuzana. “Supplementary Movies to PhD Thesis ‘Geometry-Driven Self-Organization of Migrating Cells and Chiral Filaments.’” Institute of Science and Technology Austria, 2026. https://doi.org/10.15479/AT-ISTA-21439.","apa":"Dunajova, Z. (2026). Supplementary movies to PhD thesis “Geometry-driven self-organization of migrating cells and chiral filaments.” Institute of Science and Technology Austria. https://doi.org/10.15479/AT-ISTA-21439","short":"Z. Dunajova, (2026).","mla":"Dunajova, Zuzana. 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We thank the German Climate Computing Center DKRZ for providing computing resources and the Integrated Climate Data Center (ICDC), the Center for Earth System Research and Sustainability (CEN), University of Hamburg, for supporting the IMERG data. In addition, we would like to thank Jana Sillmann for suggesting the analysis of heat stress indices and Keno Riechers for providing a thorough internal review of the initial manuscript at the Max Planck Institute for Meteorology. Open Access funding is enabled and organized by Projekt DEAL. This research has been supported by the Deutsche Forschungsgemeinschaft (grant no. CLICCS 390683824 (A3)). The article processing charges for this open-access publication were covered by the Max Planck Society.","status":"public","article_processing_charge":"Yes (via OA deal)","volume":17,"language":[{"iso":"eng"}],"file_date_updated":"2026-02-23T10:26:29Z","citation":{"short":"A. Yoon, C. Hohenegger, J. Bao, L. Brunner, Earth System Dynamics 17 (2026) 167–179.","mla":"Yoon, Arim, et al. “Extreme Events in the Amazon after Deforestation.” Earth System Dynamics, vol. 17, no. 1, Copernicus Publications, 2026, pp. 167–79, doi:10.5194/esd-17-167-2026.","ieee":"A. Yoon, C. Hohenegger, J. Bao, and L. Brunner, “Extreme events in the Amazon after deforestation,” Earth System Dynamics, vol. 17, no. 1. Copernicus Publications, pp. 167–179, 2026.","apa":"Yoon, A., Hohenegger, C., Bao, J., & Brunner, L. (2026). Extreme events in the Amazon after deforestation. Earth System Dynamics. Copernicus Publications. https://doi.org/10.5194/esd-17-167-2026","chicago":"Yoon, Arim, Cathy Hohenegger, Jiawei Bao, and Lukas Brunner. “Extreme Events in the Amazon after Deforestation.” Earth System Dynamics. Copernicus Publications, 2026. https://doi.org/10.5194/esd-17-167-2026.","ista":"Yoon A, Hohenegger C, Bao J, Brunner L. 2026. Extreme events in the Amazon after deforestation. Earth System Dynamics. 17(1), 167–179.","ama":"Yoon A, Hohenegger C, Bao J, Brunner L. Extreme events in the Amazon after deforestation. Earth System Dynamics. 2026;17(1):167-179. doi:10.5194/esd-17-167-2026"},"doi":"10.5194/esd-17-167-2026","abstract":[{"lang":"eng","text":"Potential self-perpetuating dieback of the Amazon rain forest has been a topic of concern. The concern is that initial deforestation could critically impair the forest’s water recycling capacities, further harming the remaining forest through reduced annual precipitation. Many studies have focused on annual mean precipitation changes, due to its widespread perception as a central control on the Amazon rain forest’s stability. However, the impact of deforestation goes beyond changes in the annual mean precipitation. Yet, global coarse-resolution climate models are not well suited to investigate changes in short-duration and localized events due to their coarse resolution. Here, we circumvent these issues by analyzing a full-deforestation scenario simulated by a global storm-resolving model. We focus on changes in the tail of the hourly distribution of precipitation, temperature, and wind. Hourly precipitation becomes more extreme in the absence of the forest than in an intact forest, with an increased occurrence of both no rain and intense rainfall. These changes are driven by enhanced moisture convergence that strengthens vertical velocity. On average, the near-surface temperature rises significantly by about 3.84 °C, and the daily minimum temperature after deforestation becomes similar to the daily maximum temperature before deforestation. Except for wet-bulb temperature, human heat stress indicators shift to more severe levels, with implications for health and a significant reduction in work productivity. Finally, the mean 10 m wind speed intensifies by a factor of four, with the 99th percentile wind speed doubling. To summarize, our findings, while based on an idealized case, provide a stark warning of the effects of continuing deforestation of the Amazon."}],"date_updated":"2026-07-06T12:55:02Z","publication_identifier":{"eissn":["2190-4987"]},"DOAJ_listed":"1","has_accepted_license":"1","title":"Extreme events in the Amazon after deforestation","ddc":["550"],"OA_place":"publisher","OA_type":"gold","type":"journal_article","scopus_import":"1","publication":"Earth System Dynamics","date_published":"2026-02-04T00:00:00Z","das_tickbox":"1"},{"volume":706,"language":[{"iso":"eng"}],"citation":{"short":"W. Yu, A.F. Pala, T. Kupfer, B.T. Gänsicke, D. Koester, D. Belloni, T.L.S. Wong, M.R. Schreiber, J.C. van Roestel, A.J. Brown, E.O. Waagen, J.L. González-Carballo, S. Bednarz, K. Bernacki, D. De Martino, E. Fernández Mañanes, R. González Farfán, M.J. Green, P.J. Groot, F.J. Hambsch, C. Knigge, J.L. Martin-Velasco, M. Morales-Aimar, G. Myers, R. Naves Nogues, R. Poggiani, A. Popowicz, G. Ramsay, E. Reina-Lorenz, P. Rodríguez-Gil, J.L. Salto-González, E.M. Sion, D. Steeghs, P. Szkody, O. Toloza, G. Tovmassian, Astronomy & Astrophysics 706 (2026).","mla":"Yu, W., et al. “The Evolutionary History of Ultra-Compact Accreting Binaries: I. Chemical Abundances and the Formation Channel of the Eclipsing AM CVn System ZTF J225237.05-051917.4 from HST Spectroscopy.” Astronomy & Astrophysics, vol. 706, A14, EDP Sciences, 2026, doi:10.1051/0004-6361/202557568.","ieee":"W. Yu et al., “The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy,” Astronomy & Astrophysics, vol. 706. EDP Sciences, 2026.","chicago":"Yu, W., A. F. Pala, T. Kupfer, B. T. Gänsicke, D. Koester, D. Belloni, T. L.S. Wong, et al. “The Evolutionary History of Ultra-Compact Accreting Binaries: I. Chemical Abundances and the Formation Channel of the Eclipsing AM CVn System ZTF J225237.05-051917.4 from HST Spectroscopy.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557568.","apa":"Yu, W., Pala, A. F., Kupfer, T., Gänsicke, B. T., Koester, D., Belloni, D., … Tovmassian, G. (2026). The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557568","ista":"Yu W, Pala AF, Kupfer T, Gänsicke BT, Koester D, Belloni D, Wong TLS, Schreiber MR, van Roestel JC, Brown AJ, Waagen EO, González-Carballo JL, Bednarz S, Bernacki K, De Martino D, Fernández Mañanes E, González Farfán R, Green MJ, Groot PJ, Hambsch FJ, Knigge C, Martin-Velasco JL, Morales-Aimar M, Myers G, Naves Nogues R, Poggiani R, Popowicz A, Ramsay G, Reina-Lorenz E, Rodríguez-Gil P, Salto-González JL, Sion EM, Steeghs D, Szkody P, Toloza O, Tovmassian G. 2026. The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy. Astronomy & Astrophysics. 706, A14.","ama":"Yu W, Pala AF, Kupfer T, et al. The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy. Astronomy & Astrophysics. 2026;706. doi:10.1051/0004-6361/202557568"},"file_date_updated":"2026-02-16T09:33:56Z","doi":"10.1051/0004-6361/202557568","abstract":[{"lang":"eng","text":"Context. AM Canum Venaticorum (AM CVn) stars are ultra-compact binary systems composed of a white dwarf primary accreting from a hydrogen-deficient donor. They play a crucial role in astrophysics as potential progenitors of Type Ia supernovae and as laboratories for gravitational wave studies. However, their formation and evolutionary history remain incomplete. Three formation channels have been discussed in the literature: the white dwarf, He-star, and cataclysmic variable channels.\r\n\r\nAims. The chemical composition of the accretor atmosphere reflects the material transferred from the donor. In this work we took the first accurate measurements of the fundamental parameters of the accreting white dwarf in ZTF J225237.05−051917.4, including the abundances of key elements such as carbon, nitrogen, and silicon, by analysing ultraviolet spectra obtained with the Hubble Space Telescope (HST). These measurements provide new insight into the evolutionary history of the system and, together with existing optical observations, establish it as a benchmark to develop our pipeline, paving the way for its application to a larger sample of AM CVn systems.\r\n\r\nMethods. We determined the binary parameters through photometric analysis and constrained the atmospheric parameters of the white dwarf accretor, including its effective temperature, surface gravity, and chemical abundances, by fitting the HST ultraviolet spectrum with synthetic spectral models. We then inferred the system’s formation channel by comparing the results with theoretical evolutionary models.\r\n\r\nResults. According to our measurements, the accretor’s effective temperature (Teff) is 23 300 ± 600 K and the surface gravity (log g) is 8.4 ± 0.3, which imply an accretor mass (MWD) of 0.86 ± 0.16 M⊙. We find a high nitrogen-to-carbon abundance ratio by mass of > 153.\r\n\r\nConclusions. The accretor is significantly hotter than previous estimates based on simplified blackbody fits to the spectral energy distribution, underscoring the importance of detailed spectral modelling for accurately determining system parameters. Our results show that ultraviolet spectroscopy is well suited to constraining the formation channels of AM CVn systems. Of the three proposed formation channels, the He-star channel can be excluded given the high nitrogen-to-carbon ratio. Our results are consistent with both the white dwarf and cataclysmic variable channels."}],"date_updated":"2026-07-08T06:38:46Z","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"oa":1,"date_created":"2026-02-08T23:02:49Z","day":"01","publisher":"EDP Sciences","_id":"21160","status":"public","acknowledgement":"We thank Lars Bildsten for valuable insights and discussions. We acknowledge with thanks the variable star observations from the\r\nAAVSO International Database contributed by observers worldwide and used in this research. We thank the members of the Spanish Observers of Supernovae\r\n(ObSN) group for their valuable photometric contributions. This research was\r\nsupported by Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under Germany’s Excellence Strategy – EXC 2121 “Quantum Universe”\r\n– 390833306. Co-funded by the European Union (ERC, CompactBINARIES,\r\n101078773). Views and opinions expressed are however those of the author(s)\r\nonly and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority\r\ncan be held responsible for them. DB acknowledges support from the São Paulo\r\nResearch Foundation (FAPESP), Brazil, Process Numbers #2024/03736-2 and\r\n#2025/00817-4. MRS is supported by Fondecyt (grant 1221059). MJG acknowledges support from the European Research Council through ERC Advanced\r\nGrant No. 101054731, from the National Aeronautics and Space Administration under grants 80NSSC24K0436, 80NSSC22K0479, and 80NSSC24K0380,\r\nand from the National Science Foundation under grant AST-2205736. PJG\r\nis supported by NRF SARChI grant 111692. PR-G acknowledges support by\r\nthe Agencia Estatal de Investigación del Ministerio de Ciencia e Innovación\r\n(MCIN/AEI) and the European Regional Development Fund (ERDF) under grant\r\nPID2021–124879NB–I00. DS is supported by the UK Science and Technology Facilities Council (STFC, grant numbers ST/T007184/1, ST/T003103/1,\r\nand ST/T000406/1). OT acknowledges Proyectos Internos USM 2025, PI-LII2025-03. GT was supported by grants IN109723 from the Programa de Apoyo a\r\nProyectos de Investigación e Innovación Tecnológica (PAPIIT). This project has\r\nreceived funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (Grant agreement No. 101020057).","article_processing_charge":"No","type":"journal_article","scopus_import":"1","publication":"Astronomy & Astrophysics","date_published":"2026-02-01T00:00:00Z","das_tickbox":"1","title":"The evolutionary history of ultra-compact accreting binaries: I. Chemical abundances and the formation channel of the eclipsing AM CVn system ZTF J225237.05-051917.4 from HST spectroscopy","has_accepted_license":"1","ddc":["520"],"OA_place":"publisher","OA_type":"diamond","external_id":{"arxiv":["2512.04147"]},"author":[{"last_name":"Yu","full_name":"Yu, W.","first_name":"W."},{"full_name":"Pala, A. F.","first_name":"A. F.","last_name":"Pala"},{"full_name":"Kupfer, T.","first_name":"T.","last_name":"Kupfer"},{"last_name":"Gänsicke","first_name":"B. T.","full_name":"Gänsicke, B. T."},{"first_name":"D.","full_name":"Koester, D.","last_name":"Koester"},{"last_name":"Belloni","full_name":"Belloni, D.","first_name":"D."},{"last_name":"Wong","first_name":"T. L.S.","full_name":"Wong, T. L.S."},{"last_name":"Schreiber","first_name":"M. R.","full_name":"Schreiber, M. R."},{"full_name":"van Roestel, Joannes C","first_name":"Joannes C","id":"4d122fc8-6083-11f0-87a5-97d68b860333","last_name":"van Roestel"},{"full_name":"Brown, A. J.","first_name":"A. J.","last_name":"Brown"},{"last_name":"Waagen","first_name":"E. O.","full_name":"Waagen, E. O."},{"first_name":"J. L.","full_name":"González-Carballo, J. L.","last_name":"González-Carballo"},{"first_name":"S.","full_name":"Bednarz, S.","last_name":"Bednarz"},{"last_name":"Bernacki","first_name":"K.","full_name":"Bernacki, K."},{"last_name":"De Martino","full_name":"De Martino, D.","first_name":"D."},{"last_name":"Fernández Mañanes","full_name":"Fernández Mañanes, E.","first_name":"E."},{"first_name":"R.","full_name":"González Farfán, R.","last_name":"González Farfán"},{"last_name":"Green","full_name":"Green, M. J.","first_name":"M. J."},{"last_name":"Groot","first_name":"P. J.","full_name":"Groot, P. J."},{"last_name":"Hambsch","first_name":"F. J.","full_name":"Hambsch, F. J."},{"full_name":"Knigge, C.","first_name":"C.","last_name":"Knigge"},{"last_name":"Martin-Velasco","full_name":"Martin-Velasco, J. L.","first_name":"J. L."},{"last_name":"Morales-Aimar","first_name":"M.","full_name":"Morales-Aimar, M."},{"first_name":"G.","full_name":"Myers, G.","last_name":"Myers"},{"last_name":"Naves Nogues","first_name":"R.","full_name":"Naves Nogues, R."},{"full_name":"Poggiani, R.","first_name":"R.","last_name":"Poggiani"},{"first_name":"A.","full_name":"Popowicz, A.","last_name":"Popowicz"},{"last_name":"Ramsay","first_name":"G.","full_name":"Ramsay, G."},{"last_name":"Reina-Lorenz","first_name":"E.","full_name":"Reina-Lorenz, E."},{"last_name":"Rodríguez-Gil","first_name":"P.","full_name":"Rodríguez-Gil, P."},{"last_name":"Salto-González","full_name":"Salto-González, J. L.","first_name":"J. L."},{"last_name":"Sion","full_name":"Sion, E. M.","first_name":"E. M."},{"last_name":"Steeghs","full_name":"Steeghs, D.","first_name":"D."},{"full_name":"Szkody, P.","first_name":"P.","last_name":"Szkody"},{"last_name":"Toloza","full_name":"Toloza, O.","first_name":"O."},{"first_name":"G.","full_name":"Tovmassian, G.","last_name":"Tovmassian"}],"arxiv":1,"intvolume":" 706","publication_status":"published","file":[{"content_type":"application/pdf","date_updated":"2026-02-16T09:33:56Z","success":1,"relation":"main_file","file_size":4020466,"access_level":"open_access","file_id":"21227","creator":"dernst","checksum":"2faec710fd04f927aa43deb57e35c9b2","file_name":"2026_AstronomyAstrophysics_Yu.pdf","date_created":"2026-02-16T09:33:56Z"}],"oa_version":"Published Version","department":[{"_id":"IlCa"}],"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_number":"A14","article_type":"original","year":"2026","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","PlanS_conform":"1","month":"02"},{"project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"intvolume":" 705","author":[{"orcid":"0000-0001-5586-6950","last_name":"Torralba Torregrosa","full_name":"Torralba Torregrosa, Alberto","first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541"},{"first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"last_name":"Urrutia","full_name":"Urrutia, Tanya","first_name":"Tanya"},{"first_name":"Max","full_name":"Gronke, Max","last_name":"Gronke"},{"last_name":"Mascia","first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","full_name":"Mascia, Sara"},{"last_name":"D’Eugenio","full_name":"D’Eugenio, Francesco","first_name":"Francesco"},{"last_name":"Di Cesare","first_name":"Claudia","id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia"},{"full_name":"Eilers, Anna Christina","first_name":"Anna Christina","last_name":"Eilers"},{"last_name":"Greene","full_name":"Greene, Jenny E.","first_name":"Jenny E."},{"orcid":"0000-0001-8386-3546","last_name":"Iani","full_name":"Iani, Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","first_name":"Edoardo"},{"full_name":"Ishikawa, Yuzo","first_name":"Yuzo","last_name":"Ishikawa"},{"last_name":"Mackenzie","full_name":"Mackenzie, Ruari","first_name":"Ruari"},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"last_name":"Navarrete","full_name":"Navarrete, Benjamín","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148"},{"last_name":"Kotiwale","first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","full_name":"Kotiwale, Gauri"}],"arxiv":1,"external_id":{"arxiv":["2505.09542"]},"oa_version":"Published Version","file":[{"date_created":"2026-02-16T07:35:03Z","checksum":"3782e03bc0843438aae8487f6af779c5","file_name":"2026_AstronomyAstrophysics_Torralba.pdf","relation":"main_file","file_size":2259914,"success":1,"creator":"dernst","file_id":"21224","access_level":"open_access","content_type":"application/pdf","date_updated":"2026-02-16T07:35:03Z"}],"publication_status":"published","article_number":"A147","article_type":"original","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"department":[{"_id":"JoMa"},{"_id":"GradSch"}],"month":"01","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","PlanS_conform":"1","quality_controlled":"1","year":"2026","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"abstract":[{"text":"The abundant population of little red dots (LRDs), compact objects with red UV to optical colors and broad Balmer lines at high redshift, is revealing new insights into the properties of early active galactic nuclei (AGN). Perhaps the most surprising features of this population are the presence of Balmer absorption and ubiquitous strong Balmer breaks. Recent models link these features to an active supermassive black hole (SMBH) cocooned in very dense gas (NH ∼ 1024 cm−2). We present a stringent test of such models using VLT/MUSE observations of A2744-45924, the most luminous LRD known to date (LHα ≈ 1044 erg s−1), located behind the Abell-2744 lensing cluster at z = 4.464 (μ = 1.8). We detect a moderately extended Lyα nebula (h ≈ 5.7 pkpc), spatially offset from the point-like Hα seen by JWST by ≈1.6 pkpc. The Lyα emission is narrow (FWHM = 270 ± 15 km s−1), and faint (Lyα = 0.07Hα) compared to Lyα nebulae typically observed around quasars of similar luminosity. We detect compact N IV]λ1486 emission, spatially aligned with Hα, and a spatial shift in the far-UV continuum matching the Lyα offset. We discuss that Hα and Lyα have distinct physical origins: Hα originates from the AGN, while Lyα is powered by star formation. In the environment of A2744-45924, we identified four extended Lyα halos (Δz < 0.02, Δr < 100 pkpc). Their Lyα luminosities match the expectations based on Hα emission, and show no evidence for radiation from A2744-45924 affecting its surroundings. The lack of strong, compact, and broad Lyα and the absence of a luminous extended halo, suggest that the UV AGN light is obscured by dense gas cloaking the SMBH with a covering factor close to unity.","lang":"eng"}],"date_updated":"2026-07-08T06:38:23Z","doi":"10.1051/0004-6361/202555596","citation":{"short":"A. Torralba Torregrosa, J.J. Matthee, G. Pezzulli, T. Urrutia, M. Gronke, S. Mascia, F. D’Eugenio, C. Di Cesare, A.C. Eilers, J.E. Greene, E. Iani, Y. Ishikawa, R. Mackenzie, R.P. Naidu, B. Navarrete, G. Kotiwale, Astronomy & Astrophysics 705 (2026).","mla":"Torralba Torregrosa, Alberto, et al. “A Weak Ly α Halo for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” Astronomy & Astrophysics, vol. 705, A147, EDP Sciences, 2026, doi:10.1051/0004-6361/202555596.","ieee":"A. Torralba Torregrosa et al., “A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth,” Astronomy & Astrophysics, vol. 705. EDP Sciences, 2026.","ista":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, Urrutia T, Gronke M, Mascia S, D’Eugenio F, Di Cesare C, Eilers AC, Greene JE, Iani E, Ishikawa Y, Mackenzie R, Naidu RP, Navarrete B, Kotiwale G. 2026. A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. Astronomy & Astrophysics. 705, A147.","ama":"Torralba Torregrosa A, Matthee JJ, Pezzulli G, et al. A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. Astronomy & Astrophysics. 2026;705. doi:10.1051/0004-6361/202555596","apa":"Torralba Torregrosa, A., Matthee, J. J., Pezzulli, G., Urrutia, T., Gronke, M., Mascia, S., … Kotiwale, G. (2026). A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202555596","chicago":"Torralba Torregrosa, Alberto, Jorryt J Matthee, Gabriele Pezzulli, Tanya Urrutia, Max Gronke, Sara Mascia, Francesco D’Eugenio, et al. “A Weak Ly α Halo for an Extremely Bright Little Red Dot. Indications of Enshrouded Supermassive Black Hole Growth.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202555596."},"file_date_updated":"2026-02-16T07:35:03Z","volume":705,"language":[{"iso":"eng"}],"acknowledgement":"We thank the anonymous referee for constructive and useful comments. We thank Sebastiano Cantalupo for comments on the draft. Based on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 114.27M6.001. Funded by the European Union (ERC, AGENTS, 101076224). Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. We acknowledge funding from JWST program GO-3516. This work is based in part 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 #3516. MG thanks the Max Planck Society for support through the MPRG. FDE acknowledges support by the Science and Technology Facilities Council (STFC), by the ERC through Advanced Grant 695671 “QUENCH”, and by the UKRI Frontier Research grant RISEandFALL. TU acknowledges funding from the ERC-AdG grant SPECMAP-CGM, GA 101020943. GK acknowledges support from the MERAC foundation.","status":"public","article_processing_charge":"No","day":"14","publisher":"EDP Sciences","_id":"21045","corr_author":"1","date_created":"2026-01-25T23:01:41Z","oa":1,"date_published":"2026-01-14T00:00:00Z","das_tickbox":"1","publication":"Astronomy & Astrophysics","scopus_import":"1","type":"journal_article","OA_type":"diamond","ddc":["520"],"OA_place":"publisher","title":"A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth","has_accepted_license":"1"},{"department":[{"_id":"LiBu"},{"_id":"IlCa"},{"_id":"GradSch"}],"article_number":"A321","article_type":"original","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"quality_controlled":"1","year":"2026","month":"03","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","PlanS_conform":"1","author":[{"full_name":"Liagre, Bastien Raymond Bernard","first_name":"Bastien Raymond Bernard","id":"662f1873-cab4-11f0-a719-8087d302868d","last_name":"Liagre"},{"last_name":"Desai","first_name":"Aayush A","id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","full_name":"Desai, Aayush A"},{"last_name":"Einramhof","first_name":"Lukas","id":"f1497a1a-72ef-11ef-b75a-fd877bbf6e8c","full_name":"Einramhof, Lukas"},{"id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle","orcid":"0000-0003-0142-4000","last_name":"Bugnet"}],"arxiv":1,"external_id":{"arxiv":["2511.05314 "]},"intvolume":" 707","publication_status":"published","oa_version":"Published Version","file":[{"date_updated":"2026-04-07T09:00:50Z","content_type":"application/pdf","date_created":"2026-04-07T09:00:50Z","checksum":"560cac19dc70184626b85e71a26ee22e","file_name":"2026_AstronomyAstrophysics_Liagre.pdf","creator":"dernst","file_id":"21664","access_level":"open_access","relation":"main_file","file_size":12287607,"success":1}],"scopus_import":"1","type":"journal_article","date_published":"2026-03-01T00:00:00Z","das_tickbox":"1","publication":"Astronomy & Astrophysics","ddc":["520"],"OA_place":"publisher","DOAJ_listed":"1","has_accepted_license":"1","title":"Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting","OA_type":"diamond","doi":"10.1051/0004-6361/202558023","file_date_updated":"2026-04-07T09:00:50Z","citation":{"mla":"Liagre, Bastien Raymond Bernard, et al. “Near-Degeneracy Effects in Quadrupolar Mixed Modes: From an Asymptotic Description to Data Fitting.” Astronomy & Astrophysics, vol. 707, A321, EDP Sciences, 2026, doi:10.1051/0004-6361/202558023.","short":"B.R.B. Liagre, A.A. Desai, L. Einramhof, L.A. Bugnet, Astronomy & Astrophysics 707 (2026).","chicago":"Liagre, Bastien Raymond Bernard, Aayush A Desai, Lukas Einramhof, and Lisa Annabelle Bugnet. “Near-Degeneracy Effects in Quadrupolar Mixed Modes: From an Asymptotic Description to Data Fitting.” Astronomy & Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202558023.","apa":"Liagre, B. R. B., Desai, A. A., Einramhof, L., & Bugnet, L. A. (2026). Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. Astronomy & Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202558023","ama":"Liagre BRB, Desai AA, Einramhof L, Bugnet LA. Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. Astronomy & Astrophysics. 2026;707. doi:10.1051/0004-6361/202558023","ista":"Liagre BRB, Desai AA, Einramhof L, Bugnet LA. 2026. Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. Astronomy & Astrophysics. 707, A321.","ieee":"B. R. B. Liagre, A. A. Desai, L. Einramhof, and L. A. Bugnet, “Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting,” Astronomy & Astrophysics, vol. 707. EDP Sciences, 2026."},"language":[{"iso":"eng"}],"volume":707,"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"abstract":[{"text":"Dipolar (ℓ = 1) mixed modes have revealed a surprisingly weak differential rotation between the core and the envelope of evolved solar-like stars. Quadrupolar (ℓ = 2) mixed modes also contain information regarding internal dynamics but are very rarely characterised due to their low amplitude and the challenging identification of adjacent or overlapping rotationally split multiplets affected by near-degeneracy effects. We aim to extend the broadly used asymptotic seismic diagnostics beyond ℓ = 1 mixed modes by developing an analogue asymptotic description of ℓ = 2 mixed modes while explicitly accounting for near-degeneracy effects that distort their rotational multiplets. We have derived a new asymptotic formulation of near-degenerate mixed ℓ = 2 modes that describes off-diagonal terms representing the interaction between modes of adjacent radial orders. This formalism, expressed directly in the mixed-mode basis, provides analytical expressions for the near-degeneracy effects. We implemented the formalism within a global Bayesian mode-fitting framework for a direct fit of all ℓ = 0, 1, 2 modes in the power spectrum density. We were able to asymptotically model the asymmetric rotational splitting present in various radial orders of ℓ = 2 modes observed in young red giant stars without the need for any numerical stellar modelling. We applied our formalism to the Kepler target KIC 7341231, and it yielded core and envelope rotation rates consistent with previous numerical modelling while providing improved constraints from the global and model-independent approach. We also characterised the new target, KIC 8179973, measuring its rotation rate and mixed-mode parameters for the first time. As our framework relies on a direct global fit, it allows for much better precision on the asteroseismic parameters and rotation rate estimates than standard methods, yielding better constraints for rotation inversions. We have placed the first observational constraints on the asymptotic ℓ = 2 mixed-mode parameters (ΔΠ2, q2, and εg, 2), thus paving the way towards the use of asymptotic seismology beyond ℓ = 1 mixed modes.","lang":"eng"}],"date_updated":"2026-07-08T06:39:05Z","day":"01","publisher":"EDP Sciences","_id":"21658","corr_author":"1","date_created":"2026-04-05T22:01:32Z","oa":1,"status":"public","acknowledgement":"We thank the referee for their careful and constructive report, which has substantially enhanced both the quality and clarity of the manuscript. L. Bugnet and L. Einramhof gratefully acknowledge support from the European Research Council (ERC) under the Horizon Europe programme (Calcifer; Starting Grant agreement N°101165631). While partially funded by the European Union, views and opinions expressed are, however, those of the authors only and do not necessarily reflect those of the European Union or the European Research Council. Neither the European Union nor the granting authority can be held responsible for them. The authors acknowledge the great support and feedback provided during the redaction of this article by Pr. Rafael García and Pr. Savita Mathur. We would also like to thank Dr. Emily Hatt for her insights on uncertainty estimates. The authors also thank the members of the Asteroseismology and Stellar Dynamics group of the Institute of Science and Technology Austria (ISTA) for very useful discussions: L. Barrault, S.B. Das, K. Smith. This paper includes data collected by the Kepler mission and obtained from the MAST data archive at the Space Telescope Science Institute (STScI). Funding for the Kepler mission is provided by the NASA Science Mission Directorate. STScI is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. Software: AstroPy (Astropy Collaboration 2013, 2018), Matplotlib (Hunter 2007), NumPy (Harris et al. 2020), SciPy (Virtanen et al. 2020), emcee (Foreman-Mackey et al. 2013), celerite (Foreman-Mackey et al. 2017), slepc4py (Dalcin et al. 2011; Hernandez et al. 2005), KADACS (García et al. 2011), sloscillations (Kuszlewicz et al. 2019, 2023).","article_processing_charge":"No"},{"title":"Evaluating reaction kinetics between solid booster and dissolved active species in redox‐mediated flow batteries using scanning electrochemical microscopy","has_accepted_license":"1","OA_place":"publisher","ddc":["530"],"OA_type":"hybrid","type":"journal_article","scopus_import":"1","publication":"Batteries & Supercaps","das_tickbox":"1","date_published":"2026-05-01T00:00:00Z","date_created":"2026-05-20T14:32:37Z","oa":1,"_id":"21896","day":"01","publisher":"Wiley","article_processing_charge":"Yes (via OA deal)","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.","status":"public","language":[{"iso":"eng"}],"volume":9,"doi":"10.1002/batt.70303","citation":{"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 & 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 & Supercaps 9 (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 & Supercaps. 9(5), e70303.","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 & Supercaps. 2026;9(5). doi: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 & Supercaps. Wiley, 2026. https://doi.org/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 & Supercaps. Wiley. 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 & Supercaps, vol. 9, no. 5. Wiley, 2026."},"file_date_updated":"2026-05-21T06:54:57Z","date_updated":"2026-07-08T06:48:01Z","abstract":[{"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.","lang":"eng"}],"publication_identifier":{"eissn":["2566-6223"]},"year":"2026","quality_controlled":"1","issue":"5","PlanS_conform":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"05","department":[{"_id":"MaIb"}],"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_type":"original","article_number":"e70303","publication_status":"published","file":[{"checksum":"292d65503a63cc7df92b960627634dad","file_name":"2026_BatteriesSupercaps_SantanaSantos.pdf","date_created":"2026-05-21T06:54:57Z","success":1,"file_size":756344,"relation":"main_file","access_level":"open_access","file_id":"21904","creator":"dernst","content_type":"application/pdf","date_updated":"2026-05-21T06:54:57Z"}],"oa_version":"Published Version","author":[{"full_name":"Santana Santos, Carla","first_name":"Carla","last_name":"Santana Santos"},{"full_name":"Jiyane, Nomnotho","first_name":"Nomnotho","last_name":"Jiyane"},{"last_name":"Quast","first_name":"Thomas","full_name":"Quast, Thomas"},{"orcid":"0000-0001-5013-2843","last_name":"Ibáñez","full_name":"Ibáñez, Maria","first_name":"Maria","id":"43C61214-F248-11E8-B48F-1D18A9856A87"},{"full_name":"Rubio‐Presa, Rubén","first_name":"Rubén","last_name":"Rubio‐Presa"},{"last_name":"Peljo","first_name":"Pekka","full_name":"Peljo, Pekka"},{"full_name":"Schuhmann, Wolfgang","first_name":"Wolfgang","last_name":"Schuhmann"}],"intvolume":" 9"},{"title":"Off-diagonal Ramsey numbers for linear hypergraphs","mathsc":["05D10","05D40","05C65"],"OA_place":"publisher","ddc":["500"],"OA_type":"hybrid","type":"journal_article","scopus_import":"1","publication":"Combinatorics, Probability and Computing","date_published":"2026-04-14T00:00:00Z","oa":1,"date_created":"2026-06-29T10:47:02Z","_id":"22152","day":"14","publisher":"Cambridge University Press","article_processing_charge":"No","status":"public","language":[{"iso":"eng"}],"doi":"10.1017/s0963548326100443","citation":{"ieee":"X. He, J. Nie, Y. Wigderson, and H.-H. Yu, “Off-diagonal Ramsey numbers for linear hypergraphs,” Combinatorics, Probability and Computing. Cambridge University Press, pp. 1–14, 2026.","ama":"He X, Nie J, Wigderson Y, Yu H-H. Off-diagonal Ramsey numbers for linear hypergraphs. Combinatorics, Probability and Computing. 2026:1-14. doi:10.1017/s0963548326100443","ista":"He X, Nie J, Wigderson Y, Yu H-H. 2026. Off-diagonal Ramsey numbers for linear hypergraphs. Combinatorics, Probability and Computing., 1–14.","chicago":"He, Xiaoyu, Jiaxi Nie, Yuval Wigderson, and Hung-Hsun Yu. “Off-Diagonal Ramsey Numbers for Linear Hypergraphs.” Combinatorics, Probability and Computing. Cambridge University Press, 2026. https://doi.org/10.1017/s0963548326100443.","apa":"He, X., Nie, J., Wigderson, Y., & Yu, H.-H. (2026). Off-diagonal Ramsey numbers for linear hypergraphs. Combinatorics, Probability and Computing. Cambridge University Press. https://doi.org/10.1017/s0963548326100443","short":"X. He, J. Nie, Y. Wigderson, H.-H. Yu, Combinatorics, Probability and Computing (2026) 1–14.","mla":"He, Xiaoyu, et al. “Off-Diagonal Ramsey Numbers for Linear Hypergraphs.” Combinatorics, Probability and Computing, Cambridge University Press, 2026, pp. 1–14, doi:10.1017/s0963548326100443."},"date_updated":"2026-07-08T07:24:54Z","abstract":[{"lang":"eng","text":"We study off-diagonal Ramsey numbers 𝑟(𝐻,𝐾(𝑘)\r\n𝑛) of 𝑘-uniform hypergraphs, where 𝐻 is a fixed linear 𝑘-uniform hypergraph and 𝐾(𝑘)\r\n𝑛 is complete on 𝑛 vertices. Recently, Conlon, Fox, Gunby, He, Mubayi, Suk, and Verstraëte disproved the folklore conjecture that 𝑟(𝐻,𝐾(3)\r\n𝑛) always grows polynomially in 𝑛. In this paper, we show that much larger growth rates are possible in higher uniformity. In uniformity 𝑘 ≥4, we prove that for any constant 𝐶 >0, there exists a linear 𝑘-uniform hypergraph 𝐻 for which\r\n\r\n𝑟(𝐻,𝐾(𝑘)\r\n𝑛)≥twr𝑘−2(2(log𝑛)𝐶)."}],"publication_identifier":{"issn":["0963-5483"],"eissn":["1469-2163"]},"year":"2026","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","extern":"1","month":"04","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_type":"original","page":"1-14","publication_status":"epub_ahead","oa_version":"Published Version","main_file_link":[{"url":"https://doi.org/10.1017/S0963548326100443","open_access":"1"}],"external_id":{"arxiv":["2507.05641"]},"arxiv":1,"author":[{"first_name":"Xiaoyu","full_name":"He, Xiaoyu","last_name":"He"},{"first_name":"Jiaxi","full_name":"Nie, Jiaxi","last_name":"Nie"},{"full_name":"Wigderson, Yuval","first_name":"Yuval","id":"2d0023a0-1567-11f0-833d-d5c1e476d4b5","last_name":"Wigderson"},{"full_name":"Yu, Hung-Hsun","first_name":"Hung-Hsun","last_name":"Yu"}]},{"author":[{"first_name":"Carolina","id":"20565186-803f-11ed-ab7e-96a4ff7694ef","full_name":"De Castro Barbosa Rodrigues Barata, Carolina","orcid":"0000-0003-1945-2245","last_name":"De Castro Barbosa Rodrigues Barata"},{"orcid":"0000-0002-4579-8306","last_name":"Vicoso","full_name":"Vicoso, Beatriz","id":"49E1C5C6-F248-11E8-B48F-1D18A9856A87","first_name":"Beatriz"}],"external_id":{"pmid":["41592777"]},"project":[{"name":"Does genetic drift set a limit on the adaptive evolution of sex-biased expression?","_id":"90ef7108-16d5-11f0-9cad-e6e116913473","grant_number":"ESP 6331524"}],"intvolume":" 293","publication_status":"published","oa_version":"Published Version","file":[{"content_type":"application/pdf","date_updated":"2026-02-16T09:26:02Z","date_created":"2026-02-16T09:26:02Z","file_name":"2026_RoyalSocPubProceedingsB_Barata.pdf","checksum":"d76afebca0a6f112df0146ae2d929f36","file_size":2230841,"relation":"main_file","success":1,"creator":"dernst","file_id":"21226","access_level":"open_access"}],"department":[{"_id":"BeVi"}],"article_number":"20252471","article_type":"original","pmid":1,"acknowledged_ssus":[{"_id":"ScienComp"},{"_id":"Bio"}],"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"quality_controlled":"1","year":"2026","month":"01","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","PlanS_conform":"1","issue":"2063","citation":{"ieee":"C. de Castro Barbosa Rodrigues Barata and B. Vicoso, “Single-nucleus resolution of sex-biased expression and dosage compensation in Drosophila melanogaster,” Proceedings of the Royal Society B Biological Sciences, vol. 293, no. 2063. Royal Society of London, 2026.","apa":"de Castro Barbosa Rodrigues Barata, C., & Vicoso, B. (2026). Single-nucleus resolution of sex-biased expression and dosage compensation in Drosophila melanogaster. Proceedings of the Royal Society B Biological Sciences. Royal Society of London. https://doi.org/10.1098/rspb.2025.2471","chicago":"Castro Barbosa Rodrigues Barata, Carolina de, and Beatriz Vicoso. “Single-Nucleus Resolution of Sex-Biased Expression and Dosage Compensation in Drosophila Melanogaster.” Proceedings of the Royal Society B Biological Sciences. Royal Society of London, 2026. https://doi.org/10.1098/rspb.2025.2471.","ama":"de Castro Barbosa Rodrigues Barata C, Vicoso B. Single-nucleus resolution of sex-biased expression and dosage compensation in Drosophila melanogaster. Proceedings of the Royal Society B Biological Sciences. 2026;293(2063). doi:10.1098/rspb.2025.2471","ista":"de Castro Barbosa Rodrigues Barata C, Vicoso B. 2026. Single-nucleus resolution of sex-biased expression and dosage compensation in Drosophila melanogaster. Proceedings of the Royal Society B Biological Sciences. 293(2063), 20252471.","short":"C. de Castro Barbosa Rodrigues Barata, B. Vicoso, Proceedings of the Royal Society B Biological Sciences 293 (2026).","mla":"de Castro Barbosa Rodrigues Barata, Carolina, and Beatriz Vicoso. “Single-Nucleus Resolution of Sex-Biased Expression and Dosage Compensation in Drosophila Melanogaster.” Proceedings of the Royal Society B Biological Sciences, vol. 293, no. 2063, 20252471, Royal Society of London, 2026, doi:10.1098/rspb.2025.2471."},"doi":"10.1098/rspb.2025.2471","file_date_updated":"2026-02-16T09:26:02Z","volume":293,"language":[{"iso":"eng"}],"publication_identifier":{"eissn":["1471-2954"]},"abstract":[{"text":"In many species, sex-biased expression is widespread and thought to contribute to sexual dimorphism. While bulk RNA-sequencing has been instrumental in identifying strongly sex-biased genes, it lacks resolution to assess variation across cell-types and tissue compartments. Using single-nucleus expression data from the Fly Cell Atlas, we investigate sex differences in adult Drosophila melanogaster. We find that differences in cell-type composition between the sexes are not a major source of sex-bias, as for the vast majority of genes, the degree of sex-bias is similar regardless of whether sex differences in cell-type composition are controlled for or not. Our analysis confirms a deficit of X-linked male-biased genes in the body’s somatic tissues that is widespread across cell-types. We also find the excess of X-linked female-biased genes to be associated with nervous system cells in the head but with epithelial cells in the body’s somatic tissues, showing that single-nucleus data crucially resolves sex-bias at the cell-type level. We investigate dosage compensation (DC) across 15 tissues and 17 cell-types. We observe that it varies throughout the body. Surprisingly, we observe a lack of DC in a cluster of main cells within the male accessory glands. This result highlights the importance of understanding context-dependent DC.","lang":"eng"}],"date_updated":"2026-07-08T09:17:41Z","day":"28","publisher":"Royal Society of London","_id":"21161","corr_author":"1","oa":1,"date_created":"2026-02-08T23:02:49Z","acknowledgement":"This work was partly funded by an Austrian Science Foundation FWF ESPRIT fellowship (10.55776/ESP6331524) to C.B. We would like to thank the Vicoso group for their invaluable input and discussions throughout this work. We thank Filip Ruzicka for his insightful comments on the manuscript. All computational resources were provided by the Scientific Computing Unit at ISTA. This research was also supported through resources provided by the Imaging & Optics Facility (IOF) at ISTA.","status":"public","article_processing_charge":"Yes (via OA deal)","scopus_import":"1","type":"journal_article","date_published":"2026-01-28T00:00:00Z","das_tickbox":"1","publication":"Proceedings of the Royal Society B Biological Sciences","ddc":["570"],"OA_place":"publisher","has_accepted_license":"1","title":"Single-nucleus resolution of sex-biased expression and dosage compensation in Drosophila melanogaster","OA_type":"hybrid"},{"OA_type":"gold","title":"Kineochelins - A new group of siderophores from an antarctic bacterium","has_accepted_license":"1","DOAJ_listed":"1","OA_place":"publisher","ddc":["570"],"publication":"Microbial Biotechnology","das_tickbox":"1","date_published":"2026-06-01T00:00:00Z","type":"journal_article","scopus_import":"1","article_processing_charge":"Yes","status":"public","acknowledgement":"This work was supported by the Czech Antarctic Research Programme 2025–2027 (VAN 2025) and the University of Vienna via the Research Platform Secondary Metabolomes of Bacterial Communities (MetaBac). S.K. has received funding from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie grant agreement No. 101020356 (DEFCOMANT, https://doi.org/10.3030/101020356) and MASH StG/CoG (MUNI/SC/1946/2024) by Masaryk University. T.R. and A.L. were funded in part by the Austrian Science Fund FWF [grant DOI https://doi.org/10.55776/COE7]. M.B. was funded by the Ministry of Health, Czech Republic—conceptual development of research organization (FNBr, 65269705). The Life Science Compute Cluster LiSC at the University of Vienna provided the high-performance computing infrastructure for this study. We thank Julia Ramesmayer and Sara Malinowski (Joint Microbiome Facility of the Medical University of Vienna and the University of Vienna) for assistance during high molecular weight extraction and RNA extraction. The authors thank Anna Fabisikova and Michael Klemm-Abraham from the Mass Spectrometry Centre and the team of the NMR Centre (both core facilities of the Faculty of Chemistry, University of Vienna, and members of the Vienna Life Science Instruments) for assistance with data acquisition. We are thankful to Dr. Jaime Felipe Guerrero Garzón for helpful discussions on the use of a rrn operon promoter strategy. For open access purposes, the authors have applied for a CC BY public copyright licence to any author-accepted manuscript version arising from this submission. Dr. Martin Kello (Department of Pharmacology, Faculty of Medicine, Pavol Jozef Šafárik University, Košice, Slovakia) and Dr. Michal Goga (Department of Plant Biology, Faculty of Science and Center for Interdisciplinary Biosciences, Technology and Innovation Park, Pavol Jozef Šafárik University in Košice, Košice, Slovakia), funded by VEGA 1/0498/23, are acknowledged for their assistance with the antiproliferative assays. This work was supported by Horizon 2020 Framework Programme, 101020356; Universität Wien, MetaBac; Ministry of Education, Youth and Sports, VAN 2025; Masarykova Univerzita, MUNI/SC/1946/2024; Austrian Science Fund, 10.55776/COE7; Ministerstvo Zdravotnictví České Republiky, FNBr, 65269705; Vedecká grantová agentúra Ministerstva školstva, výskumu, vývoja a mládeže Slovenskej republiky a Slovenskej akadémie vied, VEGA 1/0498/23.","oa":1,"date_created":"2026-07-08T09:19:43Z","corr_author":"1","_id":"22254","day":"01","publisher":"Wiley","date_updated":"2026-07-13T06:59:08Z","abstract":[{"text":"The global rise of antimicrobial resistance has intensified the search for new microbial metabolites from underexplored environments and taxonomic groups. Extreme and geographically isolated habitats such as Antarctic terrestrial ecosystems represent promising reservoirs of biosynthetic diversity, particularly among rare and difficult-to-cultivate actinomycetes that may produce chemically diverse metabolites with potential biotechnological applications. Here, we report the characterization of kineochelins, a previously undescribed group of siderophores produced by the Antarctic isolate Actinokineospora sp. UV203, representing a difficult-to-cultivate actinomycete lineage. Structural elucidation revealed a set of closely related congeners with a mixed-ligand architecture consistent with metal-chelating activity. Genome mining combined with transcriptomic analysis identified a dedicated nonribosomal peptide synthetase-encoding biosynthetic gene cluster responsible for kineochelin production. Comparative genomic analyses indicated that, although kineochelin biosynthetic genes share limited similarity with known mixed-ligand siderophores, their gene content and organization differ substantially, suggesting a distinct biosynthetic lineage. Functional characterization of the culture supernatant and an enriched pre-purified kineochelin fraction demonstrated strong and selective iron chelation, with high affinity for ferric and ferrous iron. Crude culture extracts inhibited the growth of bacterial strains isolated from the same Antarctic environment, indicating that kineochelins may contribute to iron-mediated microbial competition. In addition, kineochelin-enriched pre-purified fractions showed moderate selective inhibitory activity against the opportunistic yeast pathogen Nakaseomyces glabratus and a clinical isolate of Saccharomyces cerevisiae associated with invasive infection. These findings expand the chemical and biosynthetic diversity known within the genus Actinokineospora and demonstrate that Antarctic rare actinomycetes represent valuable sources of previously unexplored natural products. The discovery of kineochelins highlights the potential of genome-guided exploration of polar microorganisms for identifying bioactive metabolites with relevance for antimicrobial discovery and biotechnology.","lang":"eng"}],"publication_identifier":{"eissn":["1751-7915"]},"language":[{"iso":"eng"}],"volume":19,"doi":"10.1111/1751-7915.70386","citation":{"mla":"Kralova, Stanislava, et al. “Kineochelins - A New Group of Siderophores from an Antarctic Bacterium.” Microbial Biotechnology, vol. 19, no. 6, e70386, Wiley, 2026, doi:10.1111/1751-7915.70386.","short":"S. Kralova, P. Spacek, J. Gafriller, M. Bezdicek, V. Medvedcova, J. Séneca, J. Osvatic, U. Grienke, T. Rattei, O.N. Sekurova, S.B. Zotchev, M. Zehl, A. Loy, Microbial Biotechnology 19 (2026).","chicago":"Kralova, Stanislava, Peter Spacek, Johannes Gafriller, Matej Bezdicek, Viktoria Medvedcova, Joana Séneca, Jay Osvatic, et al. “Kineochelins - A New Group of Siderophores from an Antarctic Bacterium.” Microbial Biotechnology. Wiley, 2026. https://doi.org/10.1111/1751-7915.70386.","apa":"Kralova, S., Spacek, P., Gafriller, J., Bezdicek, M., Medvedcova, V., Séneca, J., … Loy, A. (2026). Kineochelins - A new group of siderophores from an antarctic bacterium. Microbial Biotechnology. Wiley. https://doi.org/10.1111/1751-7915.70386","ista":"Kralova S, Spacek P, Gafriller J, Bezdicek M, Medvedcova V, Séneca J, Osvatic J, Grienke U, Rattei T, Sekurova ON, Zotchev SB, Zehl M, Loy A. 2026. Kineochelins - A new group of siderophores from an antarctic bacterium. Microbial Biotechnology. 19(6), e70386.","ama":"Kralova S, Spacek P, Gafriller J, et al. Kineochelins - A new group of siderophores from an antarctic bacterium. Microbial Biotechnology. 2026;19(6). doi:10.1111/1751-7915.70386","ieee":"S. Kralova et al., “Kineochelins - A new group of siderophores from an antarctic bacterium,” Microbial Biotechnology, vol. 19, no. 6. Wiley, 2026."},"file_date_updated":"2026-07-13T06:57:19Z","issue":"6","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"06","keyword":["Actinokineospora","Antarctica","antimicrobial discovery","biosynthetic gene cluster","genome mining","microbial competition","nonribosomalpeptide synthetase","siderophores"],"year":"2026","quality_controlled":"1","biorxivid":1,"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"pmid":1,"article_type":"original","article_number":"e70386","department":[{"_id":"MassSpec"}],"dataavailabilitystatement":"The genome sequence and transcriptomic data of strain Actinokineospora sp. UV203 are available on NCBI (BioProject accession number PRJNA1331526). The nearly full-length 16S rRNA gene (1395 bp) of strain Actinokineospora sp. UV203 is available on NCBI (accession number PX090945). The NMR data of kineochelin E1 and A1 are deposited in the Natural Products Magnetic Resonance Database (NP-MRD) under accession numbers NP0352113 and NP0352114, respectively.","file":[{"date_updated":"2026-07-13T06:57:19Z","content_type":"application/pdf","creator":"dernst","file_id":"22271","access_level":"open_access","relation":"main_file","file_size":2497486,"success":1,"date_created":"2026-07-13T06:57:19Z","checksum":"4f735714644f1049b22b014225843d8d","file_name":"2026_MicrobialBiotechnology_Kralova.pdf"}],"oa_version":"Published Version","supplementarymaterial":"yes","publication_status":"published","intvolume":" 19","external_id":{"biorxivid":["10.64898/2026.02.23.707395"],"pmid":["42210522"]},"author":[{"last_name":"Kralova","first_name":"Stanislava","full_name":"Kralova, Stanislava"},{"last_name":"Spacek","full_name":"Spacek, Peter","first_name":"Peter"},{"first_name":"Johannes","full_name":"Gafriller, Johannes","last_name":"Gafriller"},{"first_name":"Matej","full_name":"Bezdicek, Matej","last_name":"Bezdicek"},{"full_name":"Medvedcova, Viktoria","first_name":"Viktoria","last_name":"Medvedcova"},{"last_name":"Séneca","full_name":"Séneca, Joana","first_name":"Joana"},{"first_name":"Jay","full_name":"Osvatic, Jay","last_name":"Osvatic"},{"last_name":"Grienke","full_name":"Grienke, Ulrike","first_name":"Ulrike"},{"last_name":"Rattei","first_name":"Thomas","full_name":"Rattei, Thomas"},{"last_name":"Sekurova","full_name":"Sekurova, Olga N.","first_name":"Olga N."},{"first_name":"Sergey B.","full_name":"Zotchev, Sergey B.","last_name":"Zotchev"},{"orcid":"0000-0001-9685-0373","last_name":"Zehl","first_name":"Martin","id":"8e016d5b-5d77-11f0-86d2-96cdb3922a55","full_name":"Zehl, Martin"},{"full_name":"Loy, Alexander","first_name":"Alexander","last_name":"Loy"}]},{"PlanS_conform":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","keyword":["galaxies: evolution","galaxies: interactions","galaxies: statistics"],"month":"07","year":"2026","quality_controlled":"1","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_type":"original","article_number":"A12","department":[{"_id":"JoMa"}],"dataavailabilitystatement":"This work has made use of the Euclid Quick Release Q1 data from the Euclid mission of the European Space Agency (ESA), 2025, https://doi.org/10.57780/esa-2853f3b. This work has made use of CosmoHub, developed by PIC (maintained by IFAE and CIEMAT) in collaboration with ICE-CSIC. CosmoHub received funding from the Spanish government (MCIN/AEI/10.13039/501100011033), the EU NextGeneration/PRTR (PRTR-C17.I1), and the Generalitat de Catalunya. Based on data from UNIONS, a scientific collaboration using three Hawaii-based telescopes: CFHT, Pan-STARRS, and Subaru www.skysurvey.cc. Based on data from the Dark Energy Camera (DECam) on the Blanco 4-m Telescope at CTIO in Chile https://www.darkenergysurvey.org","file":[{"creator":"dernst","access_level":"open_access","file_id":"22277","file_size":3482066,"relation":"main_file","success":1,"date_created":"2026-07-13T08:42:10Z","file_name":"2026_AstronomyAstrophysics_Euclid.pdf","checksum":"29c087abb97eed26d4aa2a19bbb46666","date_updated":"2026-07-13T08:42:10Z","content_type":"application/pdf"}],"oa_version":"Published Version","supplementarymaterial":"no","publication_status":"published","intvolume":" 711","external_id":{"arxiv":["2511.02964"]},"arxiv":1,"author":[{"full_name":"Gentile, F.","first_name":"F.","last_name":"Gentile"},{"full_name":"Daddi, E.","first_name":"E.","last_name":"Daddi"},{"last_name":"Elbaz","first_name":"D.","full_name":"Elbaz, D."},{"full_name":"Enia, A.","first_name":"A.","last_name":"Enia"},{"last_name":"Magnelli","full_name":"Magnelli, B.","first_name":"B."},{"first_name":"J. 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B.","full_name":"Sanders, D. B.","last_name":"Sanders"},{"last_name":"Sarpa","first_name":"E.","full_name":"Sarpa, E."},{"full_name":"Scarlata, C.","first_name":"C.","last_name":"Scarlata"},{"last_name":"Schneider","full_name":"Schneider, A.","first_name":"A."},{"last_name":"Schultheis","full_name":"Schultheis, M.","first_name":"M."},{"last_name":"Sciotti","full_name":"Sciotti, D.","first_name":"D."},{"last_name":"Sellentin","full_name":"Sellentin, E.","first_name":"E."},{"full_name":"Smith, L. C.","first_name":"L. C.","last_name":"Smith"},{"last_name":"Stanford","full_name":"Stanford, S. A.","first_name":"S. A."},{"last_name":"Tanidis","full_name":"Tanidis, K.","first_name":"K."},{"last_name":"Testera","full_name":"Testera, G.","first_name":"G."},{"first_name":"R.","full_name":"Teyssier, R.","last_name":"Teyssier"},{"first_name":"S.","full_name":"Tosi, S.","last_name":"Tosi"},{"last_name":"Troja","first_name":"A.","full_name":"Troja, A."},{"first_name":"M.","full_name":"Tucci, M.","last_name":"Tucci"},{"first_name":"C.","full_name":"Valieri, C.","last_name":"Valieri"},{"full_name":"Venhola, A.","first_name":"A.","last_name":"Venhola"},{"full_name":"Vergani, D.","first_name":"D.","last_name":"Vergani"},{"first_name":"G.","full_name":"Verza, G.","last_name":"Verza"},{"last_name":"Vielzeuf","full_name":"Vielzeuf, P.","first_name":"P."},{"last_name":"Walton","full_name":"Walton, N. A.","first_name":"N. A."}],"OA_type":"gold","has_accepted_license":"1","title":"Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field","DOAJ_listed":"1","OA_place":"publisher","ddc":["520"],"publication":"Astronomy and Astrophysics","das_tickbox":"1","date_published":"2026-07-01T00:00:00Z","type":"journal_article","researchdata_availability":"no","scopus_import":"1","article_processing_charge":"Yes","acknowledgement":"FaGe, AnEn, EmDa, LoGa, SaQu, GaDe, MaTa, ChDe, LuPo acknowledge support from the ELSA project. “ELSA: Euclid Legacy Science Advanced analysis tools” (Grant Agreement no. 101135203) is funded by the European Union. Views and opinions expressed are however those of the author(s) only and do not necessarily reflect those of the European Union or Innovate UK. Neither the European Union nor the granting authority can be held responsible for them. UK participation is funded through the UK HORIZON guarantee scheme under Innovate UK grant 10093177. AnEn acknowledge support from the INAF MiniGrant 2023 “ADIEU: Anomaly Detections In EUclid”. CaLo acknowledges support by FCT-Fundação para a Ciência e a Tecnologia through grants UIDB/04434/2020 DOI: 10.54499/UIDB/04434/2020, UIDP/04434/2020 DOI: 10.54499/UIDP/04434/2020. The Euclid Consortium acknowledges the European Space Agency and a number of agencies and institutes that have supported the development of Euclid, in particular the Agenzia Spaziale Italiana, the Austrian Forschungsförderungsgesellschaft funded through BMK, the Belgian Science Policy, the Canadian Euclid Consortium, the Deutsches Zentrum für Luft-und Raumfahrt, the DTU Space and the Niels Bohr Institute in Denmark, the French Centre National d’Etudes Spatiales, the Fundação para a Ciência e a Tecnologia, the Hungarian Academy of Sciences, the Ministerio de Ciencia, Innovación y Universidades, the National Aeronautics and Space Administration, the National Astronomical Observatory of Japan, the Netherlandse Onderzoekschool Voor Astronomie, the Norwegian Space Agency, the Research Council of Finland, the Romanian Space Agency, the State Secretariat for Education, Research, and Innovation (SERI) at the Swiss Space Office (SSO), and the United Kingdom Space Agency. A complete and detailed list is available on the Euclid website (www.euclid-ec.org). This work has made use of the Euclid Quick Release Q1 data from the Euclid mission of the European Space Agency (ESA), 2025, https://doi.org/10.57780/esa-2853f3b. This work has made use of CosmoHub, developed by PIC (maintained by IFAE and CIEMAT) in collaboration with ICE-CSIC. CosmoHub received funding from the Spanish government (MCIN/AEI/10.13039/501100011033), the EU NextGeneration/PRTR (PRTR-C17.I1), and the Generalitat de Catalunya. Based on data from UNIONS, a scientific collaboration using three Hawaii-based telescopes: CFHT, Pan-STARRS, and Subaru www.skysurvey.cc. Based on data from the Dark Energy Camera (DECam) on the Blanco 4-m Telescope at CTIO in Chile https://www.darkenergysurvey.org","status":"public","date_created":"2026-07-12T22:02:18Z","oa":1,"_id":"22265","publisher":"EDP Sciences","day":"01","date_updated":"2026-07-13T08:43:41Z","abstract":[{"lang":"eng","text":"The well-known bimodality between star-forming discs and quiescent spheroids requires the existence of two main processes: galaxy quenching, causing the strong reduction of star formation, and morphological transformation, causing the transition from disc-dominated structures to bulge-dominated ones. In this paper, we aim to understand the link between these two processes and their relation with the stellar mass of galaxies and their local environment. Taking advantage of the first data released by the Euclid Collaboration, covering more than 60 deg2 with space-based imaging and photometry, we analyse a mass-complete sample of nearly one million galaxies in the range 0.25 < z < 1 with M* > 109.5 M⊙, using a combination of photometric and spectroscopic redshifts. We divide the sample into four sub-populations of galaxies, based on their star-formation activity (star-forming and quiescent) and morphology (disc-dominated and bulge-dominated). We then analyse the physical properties of these populations and their relative abundances in the stellar mass versus local density plane. Together with confirming the passivity-density relation and the morphology-density relation, we find that quiescent discy galaxies are more abundant in the low-mass regime of high-density environment where log10(1 + δ) > 1.3. At the same time, star-forming bulge-dominated galaxies are more common in field regions with log10(1 + δ) < 0.8, preferentially at high masses. Building on these results and interpreting them through comparison with simulations, we propose a scenario where the evolution of galaxies in the field significantly differs from that in higher-density environments. The morphological transformation in the majority of field galaxies takes place before the onset of quenching and is mainly driven by secular processes taking place within the main sequence, leading to the formation of star-forming bulge-dominated galaxies as intermediate-stage galaxies. Conversely, quenching of star formation precedes morphological transformation for most galaxies in higher-density environments. This causes the formation of quiescent disc-dominated galaxies before their transition into bulge-dominated ones."}],"publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"language":[{"iso":"eng"}],"volume":711,"citation":{"chicago":"Gentile, F., E. Daddi, D. Elbaz, A. Enia, B. Magnelli, J. B. Billand, P. Corcho-Caballero, et al. “Euclid Quick Data Release (Q1): XII. Quenching Precedes Bulge Formation in Dense Environments but Follows It in the Field.” Astronomy and Astrophysics. EDP Sciences, 2026. https://doi.org/10.1051/0004-6361/202557633.","apa":"Gentile, F., Daddi, E., Elbaz, D., Enia, A., Magnelli, B., Billand, J. B., … Walton, N. A. (2026). Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field. Astronomy and Astrophysics. EDP Sciences. https://doi.org/10.1051/0004-6361/202557633","ama":"Gentile F, Daddi E, Elbaz D, et al. Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field. Astronomy and Astrophysics. 2026;711. doi:10.1051/0004-6361/202557633","ista":"Gentile F et al. 2026. Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field. Astronomy and Astrophysics. 711, A12.","ieee":"F. Gentile et al., “Euclid Quick Data Release (Q1): XII. Quenching precedes bulge formation in dense environments but follows it in the field,” Astronomy and Astrophysics, vol. 711. EDP Sciences, 2026.","mla":"Gentile, F., et al. “Euclid Quick Data Release (Q1): XII. Quenching Precedes Bulge Formation in Dense Environments but Follows It in the Field.” Astronomy and Astrophysics, vol. 711, A12, EDP Sciences, 2026, doi:10.1051/0004-6361/202557633.","short":"F. Gentile, E. Daddi, D. Elbaz, A. Enia, B. Magnelli, J.B. Billand, P. Corcho-Caballero, C. Cleland, G. De Lucia, C. D’Eugenio, M. Fossati, M. Franco, C. Lobo, Y. Lyu, M. Magliocchetti, G.A. Mamon, L. Quilley, J.G. Sorce, M. Tarrasse, M. Bolzonella, F. Durret, L. Gabarra, S. Guo, L. Pozzetti, S. Quai, F. Shankar, V. Sangalli, M. Talia, M. Baes, H. Fu, M. Girardi, J.J. Matthee, P.A. Oesch, D. Roberts, J. Schaye, D. Scott, L. Spinoglio, B. Altieri, A. Amara, S. Andreon, N. Auricchio, C. Baccigalupi, M. Baldi, A. Balestra, S. Bardelli, R. Bender, A. Biviano, E. Branchini, M. Brescia, J. Brinchmann, S. Camera, G. Cañas-Herrera, V. Capobianco, C. Carbone, J. Carretero, S. Casas, M. Castellano, G. Castignani, S. Cavuoti, K.C. Chambers, A. Cimatti, C. Colodro-Conde, G. Congedo, L. Conversi, Y. Copin, F. Courbin, H.M. Courtois, M. Cropper, A. Da Silva, H. Degaudenzi, C. Dolding, H. Dole, F. Dubath, C.A.J. Duncan, X. Dupac, S. Dusini, S. Escoffier, M. Fabricius, M. Farina, R. Farinelli, S. Ferriol, F. Finelli, N. Fourmanoit, M. Frailis, E. Franceschi, M. Fumana, S. Galeotta, K. George, B. Gillis, C. Giocoli, J. Gracia-Carpio, A. Grazian, F. Grupp, S. Gwyn, S.V.H. Haugan, J. Hoar, W. Holmes, I.M. Hook, F. Hormuth, A. Hornstrup, K. Jahnke, M. Jhabvala, B. Joachimi, E. Keihänen, S. Kermiche, A. Kiessling, B. Kubik, M. Kümmel, M. Kunz, H. Kurki-Suonio, A.M.C. Le Brun, S. Ligori, P.B. Lilje, V. Lindholm, I. Lloro, G. Mainetti, D. Maino, E. Maiorano, O. Mansutti, O. Marggraf, M. Martinelli, N. Martinet, F. Marulli, R.J. Massey, E. Medinaceli, S. Mei, M. Melchior, Y. Mellier, M. Meneghetti, E. Merlin, G. Meylan, A. Mora, M. Moresco, L. Moscardini, R. Nakajima, S.M. Niemi, C. Padilla, S. Paltani, F. Pasian, K. Pedersen, W.J. Percival, V. Pettorino, S. Pires, G. Polenta, M. Poncet, L.A. Popa, F. Raison, A. Renzi, J. Rhodes, G. Riccio, E. Romelli, M. Roncarelli, R. Saglia, Z. Sakr, D. Sapone, B. Sartoris, P. Schneider, T. Schrabback, A. Secroun, G. Seidel, S. Serrano, P. Simon, C. Sirignano, G. Sirri, J. Skottfelt, L. Stanco, J. Steinwagner, P. Tallada-Crespí, A.N. Taylor, H.I. Teplitz, I. Tereno, N. Tessore, S. Toft, R. Toledo-Moreo, F. Torradeflot, I. Tutusaus, L. Valenziano, J. Valiviita, T. Vassallo, G. Verdoes Kleijn, A. Veropalumbo, Y. Wang, J. Weller, A. Zacchei, G. Zamorani, I.A. Zinchenko, E. Zucca, V. Allevato, M. Ballardini, E. Bozzo, C. Burigana, R. Cabanac, M. Calabrese, A. Cappi, D. Di Ferdinando, J.A. Escartin Vigo, W.G. Hartley, M. Huertas-Company, J. Martín-Fleitas, S. Matthew, N. Mauri, R.B. Metcalf, A. Pezzotta, M. Pöntinen, I. Risso, V. Scottez, M. Sereno, M. Tenti, M. Viel, M. Wiesmann, Y. Akrami, I.T. Andika, S. Anselmi, M. Archidiacono, F. Atrio-Barandela, D. Bertacca, M. Bethermin, L. Bisigello, A. Blanchard, L. Blot, H. Böhringer, M. Bonici, S. Borgani, M.L. Brown, S. Bruton, A. Calabro, B. Camacho Quevedo, F. Caro, C.S. Carvalho, T. Castro, F. Cogato, S. Conseil, T. Contini, A.R. Cooray, O. Cucciati, G. Desprez, A. Díaz-Sánchez, S. Di Domizio, J.M. Diego, P. Dimauro, P.A. Duc, M.Y. Elkhashab, Y. Fang, A. Finoguenov, A. Fontana, F. Fontanot, A. Franco, K. Ganga, J. García-Bellido, T. Gasparetto, V. Gautard, R. Gavazzi, E. Gaztanaga, F. Giacomini, F. Gianotti, A.H. Gonzalez, G. Gozaliasl, M. Guidi, C.M. Gutierrez, A. Hall, S. Hemmati, H. Hildebrandt, J. Hjorth, J.J.E. Kajava, Y. Kang, V. Kansal, D. Karagiannis, K. Kiiveri, J. Kim, C.C. Kirkpatrick, S. Kruk, L. Legrand, M. Lembo, F. Lepori, G. Leroy, G.F. Lesci, J. Lesgourgues, L. Leuzzi, T.I. Liaudat, A. Loureiro, J. Macias-Perez, E.A. Magnier, F. Mannucci, R. Maoli, C.J.A.P. Martins, L. Maurin, M. Miluzio, P. Monaco, C. Moretti, G. Morgante, K. Naidoo, A. Navarro-Alsina, S. Nesseris, D. Paoletti, F. Passalacqua, K. Paterson, L. Patrizii, A. Pisani, D. Potter, M. Radovich, G. Rodighiero, S. Sacquegna, M. Sahlén, D.B. Sanders, E. Sarpa, C. Scarlata, A. Schneider, M. Schultheis, D. Sciotti, E. Sellentin, L.C. Smith, S.A. Stanford, K. Tanidis, G. Testera, R. Teyssier, S. Tosi, A. Troja, M. Tucci, C. Valieri, A. Venhola, D. Vergani, G. Verza, P. Vielzeuf, N.A. Walton, Astronomy and Astrophysics 711 (2026)."},"file_date_updated":"2026-07-13T08:42:10Z","doi":"10.1051/0004-6361/202557633"},{"article_number":"L37","article_type":"original","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"dataavailabilitystatement":"Based on observations made with ESO Telescopes at the Paranal Observatory under program IDs 116.294D and 116.2AQ0.\r\n\r\nThis work is based in part 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 programs #2514 and #9433. C.C.W. gratefully acknowledges support for program JWST-GO-2514 provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. The authors acknowledge the team led by co-PIs R. Maiolino and F. D’Eugenio for developing their observing program with a zero-exclusive-access period.\r\n\r\nThis research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated with program #15117.\r\n\r\nThe JWST and HST data presented in this article 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/ydwx-st06.\r\n\r\nThis work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The Spitzer data used in this work can be found in doi:10.26131/IRSA3.\r\n\r\nThis work was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project #25-659 “Little Red Dots, Big Open Questions.”\r\n\r\nJWST cartoon in Figure 6, credit: NASA.\r\n\r\nFacilities: VLT:Kueyen - Very Large Telescope (Kueyen) (X-Shooter), VLT:Yepun (HAWK-I), JWST - James Webb Space Telescope (NIRCam, NIRspec), HST - Hubble Space Telescope satellite (ACS), Spitzer - Spitzer Space Telescope satellite (IRAC, MIPS) - .\r\n\r\nSoftware: astropy (Astropy Collaboration et al. 2013, 2018; Astropy Collaboration et al. 2022), NumPy (C. R. Harris et al. 2020), SciPy (P. Virtanen et al. 2020), pysersic (I. Pasha & T. B. Miller 2023), stpsf (M. D. Perrin et al. 2014), lmfit (M. Newville et al. 2014), EsoRex (ESO CPL Development Team 2015), Claude (used for Python coding; https://claude.ai/), SEP (K. Barbary 2016).","department":[{"_id":"JoMa"},{"_id":"IlCa"},{"_id":"GradSch"}],"month":"07","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"2","quality_controlled":"1","year":"2026","project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"intvolume":" 1005","author":[{"orcid":"0000-0001-5586-6950","last_name":"Torralba Torregrosa","full_name":"Torralba Torregrosa, Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","first_name":"Alberto"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","orcid":"0000-0003-2871-127X","last_name":"Matthee"},{"full_name":"Weibel, Andrea","first_name":"Andrea","last_name":"Weibel"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"last_name":"Ma","first_name":"Yilun","full_name":"Ma, Yilun"},{"full_name":"Cloonan, Aidan P.","first_name":"Aidan P.","last_name":"Cloonan"},{"last_name":"Desai","full_name":"Desai, Aayush A","first_name":"Aayush A","id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e"},{"full_name":"De Graaff, Anna","first_name":"Anna","last_name":"De Graaff"},{"full_name":"Greene, Jenny E.","first_name":"Jenny E.","last_name":"Greene"},{"last_name":"Jespersen","first_name":"Christian Kragh","full_name":"Jespersen, Christian Kragh"},{"last_name":"Kramarenko","orcid":"0000-0001-5346-6048","first_name":"Ivan","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","full_name":"Kramarenko, Ivan"},{"full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara","last_name":"Mascia"},{"last_name":"Oesch","full_name":"Oesch, Pascal A.","first_name":"Pascal A."},{"last_name":"Sun","first_name":"Wendy Q.","full_name":"Sun, Wendy Q."},{"first_name":"Christina C.","full_name":"Williams, Christina C.","last_name":"Williams"}],"arxiv":1,"external_id":{"arxiv":["2603.28335"]},"oa_version":"Published Version","file":[{"date_created":"2026-07-13T07:46:22Z","file_name":"2026_AstrophysicalJourLetters_Torralba.pdf","checksum":"7600db260d799ddea45cf3bd01effe41","relation":"main_file","file_size":5419071,"success":1,"creator":"dernst","access_level":"open_access","file_id":"22274","content_type":"application/pdf","date_updated":"2026-07-13T07:46:22Z"}],"publication_status":"published","supplementarymaterial":"yes","date_published":"2026-07-10T00:00:00Z","das_tickbox":"1","publication":"The Astrophysical Journal Letters","scopus_import":"1","researchdata_availability":"yes","type":"journal_article","OA_type":"gold","ddc":["520"],"OA_place":"publisher","DOAJ_listed":"1","title":"A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7","has_accepted_license":"1","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"abstract":[{"text":"Recent studies at high redshift have revealed an enigmatic class of little red dots (LRDs) with extreme Balmer breaks, stronger than in any stellar atmosphere. However, it is unclear whether such objects exist at lower redshift, especially given the low number of LRDs reported at z ≲ 2. Here, we report the discovery of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.73, identified from JWST/NIRCam pure-parallel imaging taken by the PANORAMIC survey, and confirmed by deep VLT/X-Shooter spectroscopy. The rest-optical to near-infrared spectral energy distribution of PAN-BH*-1 is consistent with a photospheric continuum with effective temperature Teff ≈ 4800 K. The broad Hα emission line shows remarkably deep absorption, stronger than previously measured in any LRD. The absorption trough spans from −520 to +267 km s−1 with respect to the systemic redshift. The presence of blue- and red-shifted absorption suggests complex dynamics of the obscuring gas along the line of sight. We speculate that the absorption trough can be produced by a thick wind launched from a thick, rotating photospheric disk, the latter being the source of the red optical continuum. While the source is unresolved in the rest-optical JWST data (reff < 47 pc), the rest-near-UV Hubble Space Telescope imaging shows an extended morphology with (formular displayed) kpc, which we interpret as a host galaxy with a stellar mass of ∼10^8 M⊙, in line with the narrow Hα emission. The discovery of this object at cosmic noon highlights the feasibility of systematic searches for extreme LRDs with wide-area facilities such as Euclid and Roman.","lang":"eng"}],"date_updated":"2026-07-13T08:08:41Z","citation":{"ieee":"A. Torralba Torregrosa et al., “A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7,” The Astrophysical Journal Letters, vol. 1005, no. 2. IOP Publishing, 2026.","chicago":"Torralba Torregrosa, Alberto, Jorryt J Matthee, Andrea Weibel, Rohan P. Naidu, Yilun Ma, Aidan P. Cloonan, Aayush A Desai, et al. “A Black Hole Star at Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and Broad Absorption by Thick Winds in a Little Red Dot at z = 1.7.” The Astrophysical Journal Letters. IOP Publishing, 2026. https://doi.org/10.3847/2041-8213/ae7bfd.","apa":"Torralba Torregrosa, A., Matthee, J. J., Weibel, A., Naidu, R. P., Ma, Y., Cloonan, A. P., … Williams, C. C. (2026). A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7. The Astrophysical Journal Letters. IOP Publishing. https://doi.org/10.3847/2041-8213/ae7bfd","ista":"Torralba Torregrosa A, Matthee JJ, Weibel A, Naidu RP, Ma Y, Cloonan AP, Desai AA, De Graaff A, Greene JE, Jespersen CK, Kramarenko I, Mascia S, Oesch PA, Sun WQ, Williams CC. 2026. A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7. The Astrophysical Journal Letters. 1005(2), L37.","ama":"Torralba Torregrosa A, Matthee JJ, Weibel A, et al. A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7. The Astrophysical Journal Letters. 2026;1005(2). doi:10.3847/2041-8213/ae7bfd","short":"A. Torralba Torregrosa, J.J. Matthee, A. Weibel, R.P. Naidu, Y. Ma, A.P. Cloonan, A.A. Desai, A. De Graaff, J.E. Greene, C.K. Jespersen, I. Kramarenko, S. Mascia, P.A. Oesch, W.Q. Sun, C.C. Williams, The Astrophysical Journal Letters 1005 (2026).","mla":"Torralba Torregrosa, Alberto, et al. “A Black Hole Star at Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and Broad Absorption by Thick Winds in a Little Red Dot at z = 1.7.” The Astrophysical Journal Letters, vol. 1005, no. 2, L37, IOP Publishing, 2026, doi:10.3847/2041-8213/ae7bfd."},"file_date_updated":"2026-07-13T07:46:22Z","doi":"10.3847/2041-8213/ae7bfd","language":[{"iso":"eng"}],"volume":1005,"acknowledgement":"IOP Science home\r\nThe Astrophysical Journal Letters\r\nThe American Astronomical Society, find out more.\r\n\r\nThe following article isOpen access\r\nA Black Hole Star at Cosmic Noon: Extreme Balmer Break, Photospheric Continuum, and Broad Absorption by Thick Winds in a Little Red Dot at z = 1.7\r\nAlberto Torralba, Jorryt Matthee, Andrea Weibel, Rohan P. Naidu, Yilun Ma, Aidan P. Cloonan, Aayush Desai, Anna de Graaff, Jenny E. Greene, Christian Kragh JespersenShow full author list\r\n\r\nPublished 2026 June 30 • © 2026. The Author(s). Published by the American Astronomical Society.\r\nThe Astrophysical Journal Letters, Volume 1005, Number 2\r\nCitation Alberto Torralba et al 2026 ApJL 1005 L37\r\nDOI 10.3847/2041-8213/ae7bfd\r\n\r\nPDFOpens in a new tab.ePub\r\nAuthors\r\nFigures\r\nTables\r\nReferences\r\nArticle data\r\nPDFOpens in a new tab.ePub\r\nArticle metrics\r\n122 Total downloads\r\n\r\nShare this article\r\nArticle information\r\nAbstract\r\nRecent studies at high redshift have revealed an enigmatic class of little red dots (LRDs) with extreme Balmer breaks, stronger than in any stellar atmosphere. However, it is unclear whether such objects exist at lower redshift, especially given the low number of LRDs reported at z ≲ 2. Here, we report the discovery of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.73, identified from JWST/NIRCam pure-parallel imaging taken by the PANORAMIC survey, and confirmed by deep VLT/X-Shooter spectroscopy. The rest-optical to near-infrared spectral energy distribution of PAN-BH*-1 is consistent with a photospheric continuum with effective temperature Teff ≈ 4800 K. The broad Hα emission line shows remarkably deep absorption, stronger than previously measured in any LRD. The absorption trough spans from −520 to +267 km s−1 with respect to the systemic redshift. The presence of blue- and red-shifted absorption suggests complex dynamics of the obscuring gas along the line of sight. We speculate that the absorption trough can be produced by a thick wind launched from a thick, rotating photospheric disk, the latter being the source of the red optical continuum. While the source is unresolved in the rest-optical JWST data (reff < 47 pc), the rest-near-UV Hubble Space Telescope imaging shows an extended morphology with \r\n kpc, which we interpret as a host galaxy with a stellar mass of ∼108 M⊙, in line with the narrow Hα emission. The discovery of this object at cosmic noon highlights the feasibility of systematic searches for extreme LRDs with wide-area facilities such as Euclid and Roman.\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\nThe unprecedented sensitivity of JWST has enabled the discovery of a new, abundant population of objects at redshifts z ≈ 3–9 nicknamed the “little red dots” (LRDs). These are characterized by their compact rest-frame optical morphology, broad emission lines, and a characteristic rest-UV to optical “V-shape” in their spectral energy distributions (SED; e.g., D. D. Kocevski et al. 2023; V. Kokorev et al. 2024; J. Matthee et al. 2024; I. Labbe et al. 2025).\r\n\r\nThe nature of LRDs is highly debated (see K. Inayoshi & L. C. Ho 2025, for a recent overview) as the LRDs show systematic differences with respect to other types of active galactic nuclei (AGN), such as faintness in X-rays (e.g., T. T. Ananna et al. 2024; M. Yue et al. 2024), mid-to-far-infrared dust emission (e.g., G. C. K. Leung et al. 2025; C. C. Williams et al. 2024; I. Delvecchio et al. 2025; D. J. Setton et al. 2025; M. Xiao et al. 2025), and radio (e.g., G. Mazzolari et al. 2026; M. A. Latif et al. 2025; K. Perger et al. 2025, see A. J. Gloudemans et al. 2025).\r\n\r\nA recurring spectral feature of LRDs is the presence of a strong Balmer break (e.g., D. J. Setton et al. 2025; B. Wang et al. 2024; R. E. Hviding et al. 2025; W. Q. Sun et al. 2026), in some cases stronger than any star or stellar population can produce. The two most prominent examples known to date are The Cliff at z ≈ 3.5 (A. de Graaff et al. 2025a) and MoM-BH* at z ≈ 7.8 (R. P. Naidu et al. 2025). The joint appearance of strong Balmer lines as well as strong Balmer breaks has been modeled as being due to absorption by a dense, neutral gas with a high column density in the line of sight to a highly ionizing source (K. Inayoshi & R. Maiolino 2025; X. Ji et al. 2025; A. Sneppen et al. 2026; A. Torralba et al. 2026). These observations have sparked the development of new theoretical models, ranging from a spherical envelope analogous to stellar atmospheres (e.g., M. C. Begelman & J. Dexter 2026; D. Kido et al. 2025; H. Liu et al. 2025; D. Nandal & A. Loeb 2026) or a thick accretion disk (e.g., H. Liu et al. 2025, 2026; K. Inayoshi et al. 2025; Y.-X. Chen et al. 2026).\r\n\r\nBesides their spectral features, the evolution of the LRD number densities is also in stark contrast to other types of AGNs (e.g., K. Inayoshi 2025). At 4 ≲ z ≲ 7, LRDs represent a few percent of the galaxy population (e.g., D. D. Kocevski et al. 2023, 2025; J. E. Greene et al. 2024; V. Kokorev et al. 2024; X. Lin et al. 2024; R. Maiolino et al. 2024; J. Matthee et al. 2024), with number densities of ≳10−5 Mpc−3. The number density does not appear to drop quickly beyond z > 5 (e.g., J. Zhang et al. 2026), with various LRDs having been confirmed at z > 8 (V. Kokorev et al. 2023; A. J. Taylor et al. 2025; R. Tripodi et al. 2025), well beyond the quasar redshift record (F. Wang et al. 2021). Photometric LRD candidates exist beyond z > 10 (T. S. Tanaka et al. 2025). In turn, the number density of LRDs seems to decline steeply at z < 4 (e.g., Y. Ma et al. 2026), with estimates of a number density of ∼10−6 cMpc−3 at z ∼ 2 and even ∼10−10 cMpc−3 at z ≈ 0.3 (X. Lin et al. 2026). While it is challenging to ensure a uniform selection function across such a large redshift baseline and dedicated spectroscopic follow-up of such lower redshift candidates has only just started, it is challenging to attribute five orders of magnitude to such effects.\r\n\r\nMotivated by the discovery of rare objects with extreme Balmer breaks at z > 3 and the very small number of known LRDs at lower redshift, we performed a dedicated search for extreme Balmer break objects using a template-match approach on a large compilation of JWST NIRCam data over ≈0.3 deg2 and z ≈ 1.5–7.0. This survey is presented in A. Weibel et al. (2026a). As part of an ongoing ground-based spectroscopic campaign of LRD candidates at z ∼ 2 (Y. Ma et al. 2026), we followed up the most luminous candidate with a photometric redshift of z ≈ 2 with the X-Shooter spectrograph on the Very Large Telescope (VLT). In this Letter, we present the discovery and spectroscopic confirmation of PAN-BH*-1, a luminous LRD at z = 1.73 with an extreme Balmer break comparable to the strongest observed in any LRD (and, in general, any astrophysical source). The low redshift of this source enables high-resolution spectroscopy from ground-based observatories that is otherwise impossible to obtain at high redshift.\r\n\r\nThroughout this Letter, we use a ΛCDM cosmology with Ωm = 0.31, ΩΛ = 0.69, and h = 0.677 as described by Planck Collaboration et al. (2020). All the magnitudes are given in the AB system (J. B. Oke & J. E. Gunn 1983).\r\n\r\n2. Observations\r\n2.1. Photometry and Source Selection\r\nWe identified PAN-BH*-1 (ID: PAN-1115, RA, DEC: 40.015835, −1.659363 J2000) as part of a systematic search across ≈0.3 deg2 of JWST NIRCam legacy imaging comprising at least six filters of coverage (A. Weibel et al. 2026b). Notably, this dataset includes the Cycle 1 pure parallel survey PANORAMIC (PID: 2514, PIs: Williams & Oesch; C. C. Williams et al. 2025) that contributes 28 of the 35 independent lines of sight, thereby enabling the discovery of rare objects such as PAN-BH*-1 across diverse large-scale structure environments. Specifically, this source was identified in the footprint j024000m0142 of the PANORAMIC DR1,15 which is adjacent to the A370 field (G. O. Abell et al. 1989), where archival images by the Hubble Space Telescope (HST) are available from the BUFFALO survey (C. L. Steinhardt et al. 2020). The HST/ACS images were processed with grizli and also released as part of the PANORAMIC dataset.\r\n\r\nPAN-BH*-1 is in the outskirts of the A370 lensing cluster, but the magnification is only μ ≈ 1.05 according to the models from A. Niemiec et al. (2023). Throughout the rest of the paper, we report the uncorrected flux measurements, since the effect of magnification (∼5%) is negligible given the uncertainties in the observations and the lensing model.\r\n\r\nThe search strategy and full photometric selection are described in a companion paper (A. Weibel et al. 2026a). Briefly, that work presents a new selection of LRDs as a combination of a “black hole star” template (BH*; R. P. Naidu et al. 2025) embedded in a host galaxy, instead of the typically used “V-shaped” selections (e.g., D. D. Kocevski et al. 2025; V. Kokorev et al. 2024). The host galaxies are modeled using eazy’s blue_sfhz templates. The BH*s are modeled using a novel template set comprising empirical luminosity-based stacks constructed in W. Q. Sun et al. (2026), the cloudy template from R. P. Naidu et al. (2025), and by using spectra of prominent LRDs spanning the observed effective temperature range (I. Labbe et al. 2024; A. de Graaff et al. 2025a; B. Wang et al. 2026).\r\n\r\nPAN-BH*-1 stood out as one of the few sources where the BH* template effectively dominated all the light over the full wavelength range covered by NIRCam (hence the name). The redshift of PAN-BH*-1 was estimated to be zphot = 1.85. Follow-up VLT/X-Shooter spectroscopy confirmed the redshift as zspec = 1.731 (see Section 3.2).\r\n\r\nPAN-BH*-1 is also covered by archival data from the VLT with the HAWK-I camera in the Ks band (G. B. Brammer et al. 2016) and in data from the Spitzer Space Telescope in IRAC bands 1 and 3 (3.6 and 5.7 μm), and MIPS 24 μm (P. Capak 2019). PAN-BH*-1 is detected in the Ks band and in the two IRAC filters. Performing Spitzer photometry of this source is challenging due to the large point spread function (PSF) and a neighboring source, especially in the MIPS band. However, the NIRCam photometry of the neighboring source suggests it has a limited contribution to the IRAC fluxes. The details of the photometry extraction are described in Appendix A, and the measured magnitudes in Table 2.\r\n\r\n2.2. VLT/X-Shooter Spectroscopy\r\nPAN-BH*-1 was observed for 5.8 ks with the X-Shooter spectrograph (J. Vernet et al. 2011) on the VLT as a bright backup target for program 116.294D (PI: Matthee) in visitor mode on 2025 December 17. The main aim of this program was to confirm candidate LRDs at cosmic noon (Y. Ma et al. 2026). These observations confirmed the redshift through the detection of Hα at z = 1.731. A DDT program (ID 116.2AQ0; PI: Matthee) obtained additional follow-up data of PAN-BH*-1 in service mode for 26.2 ks during 2026 January 10–26, yielding a total exposure time of 8.9 hr. X-Shooter observes with three arms simultaneously, UVB, VIS, and near-infrared (NIR), covering rest-frame wavelengths of ≈0.14–0.9 μm, albeit hampered by skyline emission and telluric absorption, primarily in the rest-frame optical.\r\n\r\nThe observing conditions were clear, with a seeing ranging from 05 to 07 (median 06). The service mode observations were primarily conducted during dark nights, with some gray (FLI = 0.03–0.6, median 0.1), and a typical airmass of 1.35. We used UVB, VIS, and NIR slits with widths 10, 09, and 09, yielding a nominal resolution of R = 5400, 8900, and 5600, respectively (FWHM ∼53 km s−1 for NIR). The target acquisition was done using blind offsets from a reference star, due to the target being too faint for direct acquisition. We used a standard nodding on the slit pattern, with 4″ nod throws in an ABBA pattern, and 1″ jitters in the NIR arm to improve the sky subtraction. In each observing block of ≈1 hr, the exposure times were 700, 655, and (2×)365 s for the three arms at each nod position.\r\n\r\nThe reduction of the X-Shooter data uses a combination of EsoRex libraries16 and Python code based on the reduction pipeline employed in J. Matthee et al. (2021). Each observing block was reduced separately. We used standard stars taken during the observing night for a first-pass flux calibration. Telluric corrections were applied using the molecfit tool (A. Smette et al. 2015) implemented in the X-Shooter EsoRex pipeline. Telluric stars were observed during the visitor nights, but they were not always observed during the service mode observations in January. For those observations, we took the telluric star that was observed at the closest observing date. Based on the variation in telluric absorption among the reference stars taken during this period, we estimate the variation in the transmission and propagate the uncertainty in the telluric correction. For each observing block, we then extracted an optimally extracted 1D spectrum using the spatial profile of the Hα line, thus accounting for seeing variations and (more importantly) minor errors in the accuracy of the slit pointing. Before median combining these spectra, we normalize them by the median Hα flux of all observations to account for variations in slit losses and flux calibrations.\r\n\r\nBesides Hα (integrated S/N = 75) and Hβ (integrated S/N = 6; Section 3.2), we also detect continuum emission in the best regions in the H and K bands at 1.6 μm and 2.1 μm, respectively, with a low signal-to-noise ratio (S/N) of ∼1 per resolution element. Unfortunately, the [O iii] λλ4960, 5008 doublet is undetectable because the observed wavelengths are impacted by very strong telluric absorption. No other lines or continuum are detected in the X-Shooter spectrum.\r\n\r\n3. Properties of PAN-BH*-1\r\n3.1. Spectral Shape: A Photospheric Continuum with Strong Hα Emission\r\nThe photometric SED of PAN-BH*-1 has remarkable similarities with The Cliff (Figure 1): luminous in the rest optical, with a sudden drop toward the rest-UV around the Balmer limit, and very weak near-to-mid infrared continuum emission. With a rough extrapolation of the two HST photometric points using a power-law fit (fλ ∝ λβ), we obtain a UV slope of β = −0.1 ± 1.2, and MUV = −16.7 ± 0.7. For the rest-frame optical to NIR data, we fit a Planck blackbody law to the JWST data points, after subtracting the measured Hα flux (see Section 3.2) from the F200W photometry. The rest-optical and NIR photometry of PAN-BH*-1 is remarkably well described by a single temperature blackbody with T = 4204 K (with a best-fit ). We measure the strength of the Balmer break from the fν ratio F115W/F814W = 7 ± 1, in line with the Balmer break strengths of The Cliff (; A. de Graaff et al. 2025a)17 and MoM-BH* (7.8 ± 1.8; R. P. Naidu et al. 2025), measured from JWST/NIRSpec PRISM spectra as fν,4000–4100/fν,3620−3720. In Figure 2, we compare the Balmer break strength with the spectroscopic sample of A. de Graaff et al. (2025b), showing that out of 134 sources, only two have breaks significantly above 5. This suggests that PAN-BH*-1 has among the most extreme Balmer breaks known, although we caution that our value is derived from wide-band photometry with pivot wavelengths corresponding to 4212 and 3042 Å, respectively, rather than from spectroscopy.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 1. SED of PAN-BH*-1 Top: cutouts from all the HST and JWST images in which PAN-BH*-1 is covered. It shows a remarkably compact morphology in all the wavelengths, resolved only in the HST F606W and F814W bands (Section 3.3). Bottom: photometry from JWST/NIRCam (blue squares), HST/ACS (purple pentagons), and Spitzer/IRAC+MIPS (red hexagons, and red triangle for the 5σ upper limit). The empty square is the F200W flux after subtracting the Hα flux measured from X-Shooter spectroscopy. We show the spectrum of The Cliff for comparison (gray line), shifted to z = 1.73 and normalized to the F150W flux of PAN-BH*-1. We also show the best-fitting blackbody spectrum (blue dashed line) and the best model from the synthetic LRD atmosphere models from H. Liu et al. (2026), shifted to z = 1.73 (green line), undersampled by a factor of 500 for clarity.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nZoom InZoom OutReset image size\r\nFigure 2. Spectroscopic sample of LRDs by redshift and Balmer break strength. We plot the redshift and Balmer break strength of PAN-BH*-1, and the JWST sample from A. de Graaff et al. (2025b) (purple diamonds), and three local LRDs in X. Lin et al. (2026), for comparison. We also highlight three sources with a particularly strong Balmer break: The Cliff (A. de Graaff et al. 2025a), MoM-BH* (R. P. Naidu et al. 2025), and CAPERS-LRDz9 (A. J. Taylor et al. 2025). The Balmer break strength of the JWST spectroscopic sample is computed as fν,4000–4100/fν,3620–3720, whereas the value for PAN-BH*-1 is directly obtained from the F115W/F814W photometry.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n3.2. Hα and Hβ Emission Lines\r\nThe Hα profile appears as a complex combination of a broad line with strong absorption close to the systemic redshift. We fit the Hα emission line with a similar model as the one used in A. Torralba et al. (2026) and J. Matthee et al. (2026). The Hα model consists of two Gaussian emission components (with narrow and intermediate line widths), and a broad symmetric exponential convolved with the intermediate profile and parameterized as in F. D’Eugenio et al. (2025a). The absorption is implemented as an opacity law defined as e−τ(λ), where τ(λ) also follows a single Gaussian velocity distribution (F. D’Eugenio et al. 2025a, 2025b; A. Torralba et al. 2026). For simplicity, we assume a covering factor of Cf = 1 for the absorbing gas. In previous works, the width of the narrow component is tied to that of [O iii], assuming both components come from the same region, often interpreted as the interstellar medium (ISM) of the host galaxy. In this case, we have no information about [O iii] due to this doublet falling in a wavelength range heavily affected by strong telluric absorption. We fit the Hα line after masking relevant skylines and strong telluric absorption bands. The fitted Hα parameters are listed in Table 1 and the best-fit model is shown in Figure 3. The absorption feature is notably strong, with an equivalent width of EWabs = −148 ± 12 Å with respect to the fitted continuum and 12.2 ± 0.2 Å if including the broad emission component. The absorption corresponds to a Balmer optical depth at the line center of , reaching roughly the continuum level. The FWHM of the single Gaussian fitted to the absorber is 283 ± 8 km s−1, and is offset from the systemic redshift by −94 ± 4 km s−1. We note that this parameterization is somewhat arbitrary, and we discuss in detail the absorber properties in Section 4.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 3. Hα spectrum, and the best fit to our fiducial model. We show the X-Shooter R ∼ 5600 spectrum of the Hα line of PAN-BH*-1, along with the best-fit to the model described in Section 3.2; total model (red solid line) and individual components (discontinuous color lines). The red wing of the line is severely affected by telluric absorption, thus the large uncertainties.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nTable 1. Properties of PAN-BH*-1\r\n\r\nParameter\tValue\tUnit\r\nWidth (FWHM; Hα)\r\nExponential\t1257 ± 27\tkm s−1\r\nIntermediate\t687 ± 43\tkm s−1\r\nNarrow\t184 ± 12\tkm s−1\r\nAbsorption\t283 ± 8\tkm s−1\r\nFlux (Hα)\r\nExponential\t643 ± 7\t10−18 erg s−1 cm−2\r\nIntermediate\t19 ± 5\t10−18 erg s−1 cm−2\r\nNarrow\t38 ± 3\t10−18 erg s−1 cm−2\r\nTotal\t522 ± 7\t10−18 erg s−1 cm−2\r\nGeneral properties\r\n(LHα/erg s−1)\t43.046 ± 0.006\t⋯\r\nEW0(Hα)\t520 ± 20\tÅ\r\nSFR(Hα, narrow)a\t2.1 ± 0.2\tM⊙ yr−1\r\nSFR(Hα, narrow)b\t3.3 ± 0.3\tM⊙ yr−1\r\nreff,UV (F606W+F814W)\t\tkpc\r\nreff,opt (F200W)\t<0.047\tkpc\r\nHα/Hβ (total)\t>9.4\t⋯\r\nHα/Hβ (narrow)\t5 ± 1\t⋯\r\nNotes. aCalibration from I. G. Kramarenko et al. (2026). bCalibration from R. C. Kennicutt & N. J. Evans (2012). SFR values calculated assuming no dust attenuation.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nThe Hβ line is marginally detected. After undersampling the spectrum by a factor 5, a hint of a weak narrow component can be identified (Figure 4), along with a tentative absorption at the same mean velocity as in Hα. We fit the best Hα model to the Hβ spectrum, only rescaling it by a multiplicative factor, and adding a flat continuum component. By doing this, we find an Hβ flux of (47 ± 8) × 10−18 erg s−1 cm−2 (S/N ≈ 6). Conservatively, we obtain a Balmer decrement of Hα/Hβ > 9.4 (at a 3σ confidence level), in line with the high decrements found for the LRD population (e.g., G. P. Nikopoulos et al. 2026; A. de Graaff et al. 2025b; J. Matthee et al. 2026). In Figure 5, we show the Hβ spectrum compared to the rescaled Hα model. By matching the best-fit Hα profile with the data at the expected observed wavelength for Hβ (±5000 km s−1), we obtain a better agreement (, BIC = 1537) than fitting a flat continuum only (, BIC = 1658) with ΔBIC = 121 ≫ 10, strongly favoring a detection of a broad Hβ emission line, and securing the spectroscopic redshift. Similarly, we fit a narrow Gaussian to Hβ with the same width and velocity as the Hα best-fit model, assuming a completely saturated absorption. We obtain a Balmer decrement for the narrow component of Hα/Hβ = 5 ± 1, which would imply a dust extinction of using a J. A. Cardelli et al. (1989) attenuation law, under the assumption of case B recombination. However, due to the low S/N of Hβ this result is only tentative, and compatible with a standard Case B value within ∼2σ.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 4. X-Shooter spectrum of Hα and Hβ of PAN-BH*-1 (blue). We compare to the spectrum of The Cliff (gray; data from JWST DDT #9433), normalized in each panel to the flux of PAN-BH*-1 in the range v ∈ (−3000, −2000) km s−1. Due to the low S/N, the Hβ spectrum of PAN-BH*-1 is rebinned to a coarser grid by a factor 5, after masking the most relevant skylines.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nZoom InZoom OutReset image size\r\nFigure 5. Hβ spectrum. The spectrum is rebinned by a factor of 10 with inverse variance flux weighting for visual clarity, due to the low S/N. We compare to the best-fit Hα model, scaled by a factor of 0.112. In the bottom panel, we show the χ residuals between the spectrum and the rescaled Hα model in black, and for only the continuum in pink (ΔBIC = 121 strongly favoring the presence of a broad Hβ line).\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n3.3. Spatial Morphology\r\nIn order to assess whether PAN-BH*-1 is spatially resolved, we use the Bayesian profile fitting software pysersic (I. Pasha & T. B. Miller 2023)18 to fit a single Sérsic profile to the JWST and HST imaging data of PAN-BH*-1. For JWST/NIRCam, we choose F200W as the filter with the highest S/N in the short wavelength channel, benefiting from a high spatial resolution and probing rest-frame optical wavelengths. To model its PSF, we use version 2.2.0 of the stpsf software (formerly webbpsf, M. D. Perrin et al. 2014). For the two HST bands F606W and F814W, we instead construct empirical PSFs from public imaging data in the GOODS-S field following A. Weibel et al. (2024). In all three bands, we sample the posterior with the No U-turn sampler in two chains with 1000 warm-up and 2000 sampling steps each. We find that PAN-BH*-1 is unresolved with NIRCam in F200W where the effective radius converges toward the edge of the prior at 0.25 pixels. Using the 95th percentile of the posterior chains as an upper limit on the effective radius, we find a rest-optical size of reff < 47 pc.\r\n\r\nPAN-BH*-1 appears to be resolved in the HST images corresponding to rest-frame pivot 0.2 and 0.3 μm, respectively. Due to the low signal-to-noise of the F606W and F814W photometry, we fit both bands simultaneously fixing all the morphological parameters in both images. We measure physical effective radii of kpc (see Appendix B). The modest stretching by the foreground A370 lensing cluster could imply a correction of ∼10% to the measured radius (A. Niemiec et al. 2023), which we disregard given the uncertainties. These measured sizes are consistent with the typical sizes for galaxies with a stellar mass ≲ 109 M⊙ at z = 1.75 (A. van der Wel et al. 2014). These findings are consistent with the scenario of a compact LRD “engine” dominating the rest-optical light embedded in a host galaxy, whose contribution becomes significant blueward of the Balmer break (see A. P. Cloonan et al. 2026, for a relevant discussion).\r\n\r\n4. Absorber Kinematics\r\nAs described in Section 3.2, the velocity distribution of the absorber is empirically modeled with a Gaussian, which we find has a central velocity of −94 ± 4 km s−1 relative to the redshift of the narrow emission component (adopted as systemic). The absorption trough extends from negative to positive velocities with respect to the redshift of the narrow component, but also with respect to the center of the symmetric exponential wings. However, there are several degeneracies between the shape of the absorber and other components of the emission line, such as the narrow central emission (see Section 3.2). Furthermore, direct interpretation of the absorber center velocity shift is challenging in an optically thick gas with presumably complex dynamics, and it does not necessarily trace bulk motion. A more robust, physically motivated pair of quantities is the minimum and maximum absorber velocities. We define them as the values where the transmission of the Balmer absorber increases to 99%, km s−1 and km s−1. These values trace the largest velocities in the line of sight of gas with significant Balmer absorption. The absorbing trough extends over 787 ± 17 km s−1 under this definition. The values of and are relatively agnostic to the choice of the shape of the absorber, since they are determined by the wavelength where the line profile deviates from a broad, symmetric exponential profile. In Figure 6, we illustrate three proposed configurations of the velocity distribution of the absorbing gas that could explain the shape of the observed Balmer absorption, and we discuss these scenarios below.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 6. Geometric configurations for the absorber. We illustrate three scenarios that could give rise to the observed Balmer absorption in PAN-BH*-1. In scenario (a), the obscuring agent is a thick screen of gas with a certain bulk velocity, and turbulent motions produce the broadening of the absorption trough. In (b), there are two (or more) absorbers with opposite velocities in the line of sight. These first two scenarios are dynamically unstable; therefore, variability is expected in the absorption. Lastly, in (c), we observed an extended source through a disk wind with a rotational component (vϕ) in addition to the poloidal (nonazimuthal) velocity (vp). In the last scenario, the redshifted absorption is produced by streamlines that oppose the observer when projected along the line of sight, despite the fact that the gas is outflowing from the central source.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n4.1. Unstable Gas Flows?\r\nThe fact that there is significant absorption at both negative and positive velocities with respect to the systemic redshift cannot be simply explained by an axisymmetric outflowing or inflowing wind. In the case of observing a compact object through a spherically symmetric, nonturbulent bulk flow, a classical P Cygni profile is expected, with a purely blueshifted absorption (or redshifted if the wind is infalling). The fact that we also see redshifted absorption rules out this simple scenario. In principle, turbulent motions could also produce broadening of the absorbing medium (scenario a in Figure 6). However, the required turbulent velocity dispersion σturb ≈ 120 km s−1 (from the Gaussian fit in Section 3.2) is comparable to the mean velocity of the absorption trough, meaning that turbulence dominates the gas flow. In such a case, strong variability of the absorption profile would be expected, given the typical dynamical crossing times (see Sect. 4.1 in F. D’Eugenio et al. 2025b). For example, for a radius of 1016 cm (e.g., A. Torralba et al. 2026) and a mass of 106 M⊙, the dynamical freefall time is yr. Moreover, the turbulent velocity would be highly supersonic, and the dissipation timescale would be comparable to the dynamical time (e.g., M.-M. Mac Low 1999). Alternatively, in the context of a strong Balmer absorber at z ∼ 7, F. D’Eugenio et al. (2026) recently discussed a “breathing mode” scenario with cyclic inflows and outflows along the same line of sight, with the gas being in different phases at different depths (scenario b in Figure 6; see also K. Park et al. 2017). In this case, the same arguments regarding the stability of the absorber would apply, and absorber variability is expected on observed timescales of ∼5 yr (for a source at z = 1.7), which is testable with future observations.\r\n\r\n4.2. The Case for the Disk Wind Hypothesis\r\nAn alternative, dynamically stable scenario is a disk wind configuration (scenario c in Figure 6). Here, the wind would be launched from a thick disk near the central engine, which we speculate could be the source of the optical continuum emission (e.g., H. Liu et al. 2025, 2026; L. Zwick et al. 2025; Y.-X. Chen et al. 2026). A rotating disk would imprint to the wind an azimuthal velocity component (vϕ). Observations at specific lines of sight, particularly for high inclination angles (close to edge-on) where the rotational component dominates the poloidal velocity, can give rise to both blueshifted and redshifted absorption features (D. Proga et al. 2000; P. B. Hall et al. 2002, 2013; D. Proga & T. R. Kallman 2004; M. Giustini & D. Proga 2012). Most observed LRDs have blueshifted P Cygni–like absorbers (J. Matthee et al. 2026), which can be naively interpreted as a uniformly expanding shell. The low incidence of redshifted Balmer absorbers in LRD spectra (e.g., I. Labbe et al. 2024; A. de Graaff et al. 2025a; F. D’Eugenio et al. 2025b, 2026; Y. Ma et al. 2026) can therefore be explained by the requirement of high inclination angles to observe such features (see also A. Sneppen et al. 2026). Such a picture is broadly in line with disk wind models for AGN with broad absorption lines (e.g., P. B. Hall et al. 2002; H. Zhou et al. 2019) and around stars with circumstellar disks (e.g., J. Erkal et al. 2022), such as accreting T Tauri stars (S. Edwards et al. 2006) or cataclysmic variables (D. Proga 2003).\r\n\r\n4.3. Implications of Rotating Winds for the Emission Lines of LRDs\r\nThe disk wind hypothesis would imply that a photosphere in the shape of a rotating disk is the source of the optical continuum emission, and drives winds that can explain the observed absorption trough. Emission lines originating in a thin rotating disk would have a double-peaked profile in the idealized case (for most inclination angles), but this is not necessarily true if the disk is not sufficiently thin (e.g., N. Murray & J. Chiang 1997), for instance, in the case of a puffed-up disk associated with super-Eddington accretion (e.g., H. Liu et al. 2026). In addition, most line emission would not be produced directly at the base of the disk, but slightly outside (e.g., via collisional cooling or residual recombination; A. Torralba et al. 2026), where the rotational velocity is lower, and the dynamics are complex (e.g., G. A. Shields 1977).\r\n\r\nThe Balmer lines of most LRDs are dominated by broad, symmetric exponential components that are associated with broadening by electron scattering (e.g., V. Rusakov et al. 2026; J. Matthee et al. 2026). For PAN-BH*-1, the Hα line profile of PAN-BH*-1 is compatible with a broad exponential profile emerging through a dense wind where the absorption trough is produced. In dense gas with a large column density of neutral hydrogen, and optically thick to Balmer transitions (NHI,2s ≳ 1014 cm−2), resonant scattering effects become important. Crucially, resonant scattering impacts Hα and Hβ differently (e.g., S.-J. Chang et al. 2026), hence the 3D radiative transfer and photon redistribution of both lines may produce different profiles (see, e.g., Figure 2 in D. Proga 2003). Therefore, the empirical fitting and interpretation of the absorption profiles becomes nontrivial. Dedicated radiative transfer modeling is necessary to study such effects, and they can be tested in other emission lines with high optical depth, such as He i λ10830 Å, or resonant lines like C iv λ1550.\r\n\r\n5. Implications for the Galaxy and Black Hole Masses\r\n5.1. Properties of the Host Galaxy\r\nAssuming that the narrow component of Hα corresponds to ISM emission in the host galaxy, we compute the associated star formation rate using the local calibration from R. C. Kennicutt & N. J. Evans (2012) and assuming no dust attenuation. We obtain SFR(Hα) = 3.3 ± 0.3 M⊙ yr−1. A somewhat lower value of SFR(Hα) = 2.1 ± 0.2 M⊙ yr−1 is obtained using the high-redshift (z ≳ 4) calibrations in I. G. Kramarenko et al. (2026), which might be more appropriate for a young dwarf galaxy with a bursty star formation history. The star formation rates are low, but in line with a main-sequence galaxy with (extrapolating the relation from J. S. Speagle et al. 2014). Assuming zero dust attenuation, the UV absolute magnitude (MUV = −16.7 ± 0.7; Section 3.1) would imply SFR(UV) = 0.18 ± 0.12 M⊙ yr−1 (R. C. Kennicutt & N. J. Evans 2012). The discrepancy between the UV and Hα inferred star formation rate suggests there is some amount of dust attenuation in the host galaxy.\r\n\r\nWe derive a dynamical mass from the width of the narrow component Hα line and the estimated UV size as , adopting the empirical virial correction K(n)K(q) from A. van der Wel et al. (2022), where K(n) and K(q) are functions of the best-fit ellipticity and Sérsic index (see Appendix B). Adopting a Mdyn/M* factor of 40 as found by A. de Graaff et al. (2024) for dwarf galaxies at high redshift, we infer a stellar mass of . However, the Mdyn/M* is very uncertain in this regime, and the uncertainty can span over 1 dex (A. Saldana-Lopez et al. 2025). We advise caution in interpreting this result, as there are large uncertainties in the measurements of the narrow Hα component, the HST morphology, and the empirical relations used.\r\n\r\nAs discussed in Section 4, the absorption profile is compatible with broadening by a rotating disk wind, and numerical modeling of such configurations often predicts a narrow component arising from increased transmission due to purely kinematic effects in the wind geometry (D. Proga et al. 2000; D. Proga 2003; D. Proga & T. R. Kallman 2004). This would be an alternative explanation for at least part of the narrow component flux. On the other hand, most LRDs present narrow [O iii] emission that is often associated with the host galaxy. Indeed, the ionized gas producing [O iii] emission should have associated emission in the Hα and higher-order Balmer lines. However, constraining this component largely depends on the assumptions on dust attenuation or ISM conditions, and requires very high S/N and resolution data. Deep, space-based follow-up observations of PAN-BH*-1 would be very constraining for the wind kinematics (e.g., by the joint analysis of Hβ) and to assess whether a narrow component comes from a host galaxy (e.g., by comparing to a narrow Hβ component or [O iii] λλ4960, 5008).\r\n\r\n5.2. Black Hole Mass From Photosphere Models\r\nThe general physical setup of LRDs is an open debate, and their masses are a major unknown. Due to the multiple differences with respect to the classical AGN population, the validity of standard virial calibrations has been questioned (e.g., V. Rusakov et al. 2026; J. E. Greene et al. 2026; A. Sneppen et al. 2026; A. Torralba et al. 2026, although see, e.g., M. Brazzini et al. 2025, 2026; J. Scholtz et al. 2026 for an alternative interpretation).\r\n\r\nOne can obtain a mass estimate assuming a system in radiative equilibrium with Lbol/LEdd = 1 (e.g., H. Umeda et al. 2026); this yields a total mass of ≈106 M⊙, using the bolometric luminosity from integrating the best-fit blackbody in Section 3.1. Recently, H. Liu et al. (2026) developed a synthetic spectral library of LRD atmosphere models. In these models, the density of the photosphere is regulated by the net surface gravity of an optically thick atmosphere, enabling constraints on the mass of the system. We fit the JWST photometry of PAN-BH*-1 using the models from H. Liu et al. (2026), assuming a negligible contribution from a host galaxy to the optical continuum. The best-fit model has effective temperature Teff = 4800 K, surface gravity , and metallicity (; see Figure 1). The best-fit implies a total mass of the system (BH plus gas) of (Equation (6) in H. Liu et al. 2026, assuming hydrostatic equilibrium). For the second and third best fits, we obtain and −2, respectively (, respectively; with the same metallicity and effective temperature), which would imply lower limits to the system mass between and 4. The bolometric luminosity of PAN-BH*-1 (from the integral of the best-fit green curve in Figure 1) implies an Eddington luminosity ratio of L/LEdd ≲ 13, assuming the best-fit mass from the H. Liu et al. (2026) models. The elevated Eddington ratio is in line with the hypothesis of a radiation-driven wind discussed in Section 4, and allows for somewhat larger system masses. The low masses obtained with this model, combined with the stellar mass inferred from dynamical arguments for the host galaxy (Section 3.3) set lower limits to the BH-to-stellar mass ratio of MBH/M* ≳ 10−4–10−2, which are compatible with the relations observed in the Local Universe, within the large uncertainties (A. E. Reines & M. Volonteri 2015).\r\n\r\n6. Conclusions\r\nIn this Letter, we presented the discovery and spectroscopic confirmation of PAN-BH*-1, an LRD with an extreme Balmer break at z = 1.731. The strength of the Balmer break (F115W/F814W = 7 ± 1) is comparable to the most extreme LRDs known, The Cliff (A. de Graaff et al. 2025a) and MoM-BH* (R. P. Naidu et al. 2025). We summarize the observations and our main conclusions as follows.\r\n\r\n\r\n1. \r\nWe obtained deep VLT/X-Shooter spectroscopy of PAN-BH*-1. The Hα emission line is luminous and broad (LHα = 1043 erg s−1), and has an unusually strong absorption. Hβ is detected with an S/N ≈ 6, and we conservatively estimate a lower limit for the Balmer decrement of Hα/Hβ > 9.4 (at a 3σ confidence level), in line with other LRDs in the literature (e.g., A. de Graaff et al. 2025b; G. P. Nikopoulos et al. 2026).\r\n2. \r\nThe absorption trough spans from −520 to 267 km s−1 (at a transmission level of 99%). We interpret the presence of blue- and redshifted absorption as produced by a disk wind, analogous to those analyzed in the context of broad absorption line quasars or accreting stars. This hypothesis would imply that the source of the optical continuum is likely a thick photospheric disk.\r\n3. \r\nWe detect a narrow Hα component (FWHM = 184 ± 12 km s−1), which we interpret as probing a host galaxy with M* ≈ 108 M⊙ and SFR = 2–3 M⊙. This interpretation is in line with the extended rest-NUV morphology measured in the HST bands (\r\n kpc).\r\n4. \r\nBy fitting the synthetic atmosphere models of H. Liu et al. (2026), we estimate a system mass (BH+envelope) of 104–106 M⊙. The inferred masses, together with the stellar mass inferred from morphology and narrow emission line dynamics, imply BH-to-stellar mass ratios of 10−2–10−4, close to the extrapolated trend in the local Universe (A. E. Reines & M. Volonteri 2015).\r\n5. \r\nThe confirmation of this source at cosmic noon (magnitude of ≈22 in the K band, Hα flux ≈5 × 10−16 erg s−1 cm−2) proves the feasibility of detecting extreme LRDs at such epochs with wide-area spectroscopic surveys like Euclid or the forthcoming Nancy Grace Roman Space Telescope.\r\n\r\nAcknowledgments\r\nA.T. thanks Debasish Dutta and Tamara Bogdanović for useful conversations about stellar and AGN winds.\r\n\r\nWe thank the scientific referee for the useful and constructive feedback, which helped improve the quality of this paper.\r\n\r\nJ.M. and A.T. acknowledge funding by the European Union (ERC, AGENTS, 101076224). The work of CCW is supported by NOIRLab, which is managed by the Association of Universities for Research in Astronomy (AURA) under a cooperative agreement with the National Science Foundation. A.P.C. warmly acknowledges the support of the National Science Foundation through the NSF Graduate Research Fellowship Program. A.d.G. acknowledges support from a Clay Fellowship awarded by the Smithsonian Astrophysical Observatory.\r\n\r\nBased on observations made with ESO Telescopes at the Paranal Observatory under program IDs 116.294D and 116.2AQ0.\r\n\r\nThis work is based in part 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 programs #2514 and #9433. C.C.W. gratefully acknowledges support for program JWST-GO-2514 provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. The authors acknowledge the team led by co-PIs R. Maiolino and F. D’Eugenio for developing their observing program with a zero-exclusive-access period.\r\n\r\nThis research is based on observations made with the NASA/ESA Hubble Space Telescope obtained from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5–26555. These observations are associated with program #15117.\r\n\r\nThe JWST and HST data presented in this article 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/ydwx-st06.\r\n\r\nThis work is based in part on observations made with the Spitzer Space Telescope, which was operated by the Jet Propulsion Laboratory, California Institute of Technology under a contract with NASA. The Spitzer data used in this work can be found in doi:10.26131/IRSA3.\r\n\r\nThis work was supported by the International Space Science Institute (ISSI) in Bern, through ISSI International Team project #25-659 “Little Red Dots, Big Open Questions.”\r\n\r\nJWST cartoon in Figure 6, credit: NASA.\r\n\r\nFacilities: VLT:Kueyen - Very Large Telescope (Kueyen) (X-Shooter), VLT:Yepun (HAWK-I), JWST - James Webb Space Telescope (NIRCam, NIRspec), HST - Hubble Space Telescope satellite (ACS), Spitzer - Spitzer Space Telescope satellite (IRAC, MIPS) - .\r\n\r\nSoftware: astropy (Astropy Collaboration et al. 2013, 2018; Astropy Collaboration et al. 2022), NumPy (C. R. Harris et al. 2020), SciPy (P. Virtanen et al. 2020), pysersic (I. Pasha & T. B. Miller 2023), stpsf (M. D. Perrin et al. 2014), lmfit (M. Newville et al. 2014), EsoRex (ESO CPL Development Team 2015), Claude (used for Python coding; https://claude.ai/), SEP (K. Barbary 2016).","status":"public","article_processing_charge":"Yes","day":"10","publisher":"IOP Publishing","_id":"22263","corr_author":"1","oa":1,"date_created":"2026-07-12T22:02:17Z"},{"citation":{"short":"Z. Lewis, M.V. Maseda, A. De Graaff, J. Leja, B. Wang, H.W. Rix, I. Mcconachie, N.J. Cleri, R. Bezanson, L.A. Boogaard, G. Brammer, J.E. Greene, M. Hirschmann, H. Katz, I. Labbé, J.J. Matthee, T.B. Miller, R.P. Naidu, P.A. Oesch, D.J. Setton, K.A. Suess, A. Weibel, K.E. Whitaker, C.C. Williams, The Astrophysical Journal 1005 (2026).","mla":"Lewis, Zach, et al. “The Mass–Metallicity Relation and Its Observational Effects at z ∼ 3–6.” The Astrophysical Journal, vol. 1005, no. 2, 159, IOP Publishing, 2026, doi:10.3847/1538-4357/ae7bfc.","ieee":"Z. Lewis et al., “The mass–metallicity relation and its observational effects at z ∼ 3–6,” The Astrophysical Journal, vol. 1005, no. 2. IOP Publishing, 2026.","chicago":"Lewis, Zach, Michael V. Maseda, Anna De Graaff, Joel Leja, Bingjie Wang, Hans Walter Rix, Ian Mcconachie, et al. “The Mass–Metallicity Relation and Its Observational Effects at z ∼ 3–6.” The Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae7bfc.","apa":"Lewis, Z., Maseda, M. V., De Graaff, A., Leja, J., Wang, B., Rix, H. W., … Williams, C. C. (2026). The mass–metallicity relation and its observational effects at z ∼ 3–6. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae7bfc","ama":"Lewis Z, Maseda MV, De Graaff A, et al. The mass–metallicity relation and its observational effects at z ∼ 3–6. The Astrophysical Journal. 2026;1005(2). doi:10.3847/1538-4357/ae7bfc","ista":"Lewis Z, Maseda MV, De Graaff A, Leja J, Wang B, Rix HW, Mcconachie I, Cleri NJ, Bezanson R, Boogaard LA, Brammer G, Greene JE, Hirschmann M, Katz H, Labbé I, Matthee JJ, Miller TB, Naidu RP, Oesch PA, Setton DJ, Suess KA, Weibel A, Whitaker KE, Williams CC. 2026. The mass–metallicity relation and its observational effects at z ∼ 3–6. The Astrophysical Journal. 1005(2), 159."},"file_date_updated":"2026-07-13T07:35:16Z","doi":"10.3847/1538-4357/ae7bfc","language":[{"iso":"eng"}],"volume":1005,"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]},"date_updated":"2026-07-13T07:40:41Z","abstract":[{"text":"The correlation between galaxy stellar mass and gas-phase metallicity, known as the mass–metallicity relation (MZR), gives key insights into the processes that govern galaxy evolution. However, unquantified observational and selection biases can result in systematic errors in attempts to recover the intrinsic MZR, particularly at higher redshifts. We characterize the MZR at z ∼ 3–6 within a fully Bayesian framework using JWST/NIRSpec spectra of 191 galaxies from the RUBIES survey. We forward model the observed mass–metallicity surface using prospector-generated spectra to account for two selection biases: the survey selection function and the success in observing high signal-to-noise ratio emission lines. We demonstrate that the RUBIES selection function, based on F444W magnitude and F150W – F444W color, has a negligible effect on our measured MZR. A correct treatment of the non-Gaussian metallicity uncertainties from strong-line calibrations lowers the derived MZR normalization by 0.2 dex and flattens the slope by ∼20%; forward modeling the effect of emission line observability steepens the slope by ∼15%. Both of these biases must be taken into account in order to properly measure the intrinsic MZR. This novel forward-modeling process motivates careful consideration of selection functions in future surveys, and paves the way for robust, high-redshift chemical enrichment studies that trace the evolution of the MZR across cosmic time.","lang":"eng"}],"_id":"22264","publisher":"IOP Publishing","day":"10","date_created":"2026-07-12T22:02:17Z","oa":1,"article_processing_charge":"Yes","acknowledgement":"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 ID 4233. This material is based upon work supported by the National Science Foundation Graduate Research Fellowship under grant No. 2137424 as well as work supported by NASA under Award No. 2025_3-0, issued through the Wisconsin Space Grant Consortium, and JWST-GO-4233. Any opinions, findings, and conclusions or recommendations expressed in this material are those of the author(s) and do not necessarily reflect the views of the National Aeronautics and Space Administration. Support for program ID 4233 was provided by NASA through a grant from the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Inc., under NASA contract NAS 5-03127. M.V.M. is supported by the National Science Foundation via grant AAG 2205519. A.d.G. acknowledges support from a Clay Fellowship awarded by the Smithsonian Astrophysical Observatory. T.B.M. was supported by a CIERA Fellowship. Part of the computations for this research were performed on the Pennsylvania State University’s Institute for Computational and Data Sciences’ Roar supercomputer. Some/all of the data presented in this article 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/qk5z-7p30. The scripts used to generate the data and results in this work can be found in Zenodo at doi:10.5281/zenodo.20513668 and GitHub \r\nhttps://github.com/zachlewis99/rubies_mzr ","status":"public","researchdata_availability":"yes","scopus_import":"1","type":"journal_article","das_tickbox":"1","date_published":"2026-07-10T00:00:00Z","publication":"The Astrophysical Journal","OA_place":"publisher","ddc":["520"],"has_accepted_license":"1","DOAJ_listed":"1","title":"The mass–metallicity relation and its observational effects at z ∼ 3–6","OA_type":"gold","arxiv":1,"author":[{"last_name":"Lewis","first_name":"Zach","full_name":"Lewis, Zach"},{"full_name":"Maseda, Michael V.","first_name":"Michael V.","last_name":"Maseda"},{"last_name":"De Graaff","full_name":"De Graaff, Anna","first_name":"Anna"},{"last_name":"Leja","first_name":"Joel","full_name":"Leja, Joel"},{"last_name":"Wang","full_name":"Wang, Bingjie","first_name":"Bingjie"},{"last_name":"Rix","first_name":"Hans Walter","full_name":"Rix, Hans Walter"},{"last_name":"Mcconachie","full_name":"Mcconachie, Ian","first_name":"Ian"},{"full_name":"Cleri, Nikko J.","first_name":"Nikko J.","last_name":"Cleri"},{"last_name":"Bezanson","full_name":"Bezanson, Rachel","first_name":"Rachel"},{"last_name":"Boogaard","full_name":"Boogaard, Leindert A.","first_name":"Leindert A."},{"full_name":"Brammer, Gabriel","first_name":"Gabriel","last_name":"Brammer"},{"full_name":"Greene, Jenny E.","first_name":"Jenny E.","last_name":"Greene"},{"last_name":"Hirschmann","first_name":"Michaela","full_name":"Hirschmann, Michaela"},{"first_name":"Harley","full_name":"Katz, Harley","last_name":"Katz"},{"last_name":"Labbé","first_name":"Ivo","full_name":"Labbé, Ivo"},{"last_name":"Matthee","orcid":"0000-0003-2871-127X","full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Miller","first_name":"Tim B.","full_name":"Miller, Tim B."},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"first_name":"Pascal A.","full_name":"Oesch, Pascal A.","last_name":"Oesch"},{"last_name":"Setton","first_name":"David J.","full_name":"Setton, David J."},{"last_name":"Suess","first_name":"Katherine A.","full_name":"Suess, Katherine A."},{"full_name":"Weibel, Andrea","first_name":"Andrea","last_name":"Weibel"},{"last_name":"Whitaker","full_name":"Whitaker, Katherine E.","first_name":"Katherine E."},{"full_name":"Williams, Christina C.","first_name":"Christina C.","last_name":"Williams"}],"external_id":{"arxiv":["2512.03134"]},"intvolume":" 1005","publication_status":"published","supplementarymaterial":"no","oa_version":"Published Version","file":[{"success":1,"file_size":1854628,"relation":"main_file","file_id":"22273","access_level":"open_access","creator":"dernst","file_name":"2026_AstrophysicalJour_Lewis.pdf","checksum":"9b13fbbc5e5e921c04676ebc532d9c42","date_created":"2026-07-13T07:35:16Z","content_type":"application/pdf","date_updated":"2026-07-13T07:35:16Z"}],"dataavailabilitystatement":"The specific observations analyzed can be accessed via doi:10.17909/qk5z-7p30. The scripts used to generate the data and results in this work can be found in Zenodo at doi:10.5281/zenodo.20513668 and GitHub https://github.com/zachlewis99/rubies_mzr","department":[{"_id":"JoMa"}],"article_type":"original","article_number":"159","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"quality_controlled":"1","year":"2026","keyword":["Galaxy evolution","Chemical enrichment","Metallicity","Galaxy abundances","Scaling relations"],"month":"07","PlanS_conform":"1","issue":"2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87"}]