[{"volume":651,"OA_type":"hybrid","article_type":"original","pmid":1,"quality_controlled":"1","file":[{"file_name":"2026_Nature_Grosjean.pdf","access_level":"open_access","date_created":"2026-03-24T06:57:08Z","checksum":"dafef9ed575b44be4263e948a47ae056","relation":"main_file","date_updated":"2026-03-24T06:57:08Z","success":1,"file_id":"21494","content_type":"application/pdf","creator":"dernst","file_size":12245694}],"author":[{"full_name":"Grosjean, Galien M","first_name":"Galien M","id":"0C5FDA4A-9CF6-11E9-8939-FF05E6697425","last_name":"Grosjean","orcid":"0000-0001-5154-417X"},{"first_name":"Markus","full_name":"Ostermann, Markus","last_name":"Ostermann"},{"last_name":"Sauer","full_name":"Sauer, Markus","first_name":"Markus"},{"last_name":"Hahn","first_name":"Michael","full_name":"Hahn, Michael"},{"last_name":"Pichler","full_name":"Pichler, Christian M.","first_name":"Christian M."},{"full_name":"Fahrnberger, Florian","first_name":"Florian","last_name":"Fahrnberger"},{"last_name":"Pertl","orcid":"0000-0003-0463-5794","id":"6313aec0-15b2-11ec-abd3-ed67d16139af","first_name":"Felix","full_name":"Pertl, Felix"},{"full_name":"Balazs, Daniel","first_name":"Daniel","orcid":"0000-0001-7597-043X","last_name":"Balazs","id":"302BADF6-85FC-11EA-9E3B-B9493DDC885E"},{"last_name":"Link","first_name":"Mason M.","full_name":"Link, Mason M."},{"last_name":"Kim","first_name":"Seong H.","full_name":"Kim, Seong H."},{"first_name":"Devin L.","full_name":"Schrader, Devin L.","last_name":"Schrader"},{"first_name":"Adriana","full_name":"Blanco, Adriana","last_name":"Blanco"},{"first_name":"Francisco","full_name":"Gracia, Francisco","last_name":"Gracia"},{"last_name":"Mujica","first_name":"Nicolás","full_name":"Mujica, Nicolás"},{"first_name":"Scott R","full_name":"Waitukaitis, Scott R","last_name":"Waitukaitis","id":"3A1FFC16-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-2299-3176"}],"acknowledged_ssus":[{"_id":"M-Shop"},{"_id":"NanoFab"},{"_id":"ScienComp"},{"_id":"LifeSc"}],"day":"18","ec_funded":1,"OA_place":"publisher","page":"626-631","date_created":"2026-03-23T15:04:00Z","oa":1,"date_published":"2026-03-18T00:00:00Z","related_material":{"link":[{"url":"https://ista.ac.at/en/news/colliding-dust-and-the-sparks-of-creation/","relation":"press_release","description":"News on ISTA website"}]},"intvolume":"       651","year":"2026","status":"public","PlanS_conform":"1","issue":"8106","type":"journal_article","publication_status":"published","fulldoi":"https://doi.org/10.1038/s41586-025-10088-w","publication":"Nature","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"project":[{"grant_number":"949120","call_identifier":"H2020","_id":"0aa60e99-070f-11eb-9043-a6de6bdc3afa","name":"Tribocharge: a multi-scale approach to an enduring problem in physics"},{"_id":"260C2330-B435-11E9-9278-68D0E5697425","name":"ISTplus - Postdoctoral Fellowships","call_identifier":"H2020","grant_number":"754411"}],"language":[{"iso":"eng"}],"user_id":"ba8df636-2132-11f1-aed0-ed93e2281fdd","month":"03","oa_version":"Published Version","title":"Adventitious carbon breaks symmetry in oxide contact electrification","publisher":"Springer Nature","_id":"21485","date_updated":"2026-04-28T12:06:01Z","ddc":["540"],"acknowledgement":"This project has received support from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 949120) and from the Marie Skłodowska-Curie programme (grant agreement no. 754411). We acknowledge the state of Lower Austria and the European Regional Development Fund under grant no. WST3-F-542638/004-2021. N.M. acknowledges support from grant Fondecyt 1221597. G.G. is a Serra Húnter fellow. This research was supported by the Scientific Service Units of the Institute of Science and Technology Austria through resources provided by the Miba Machine Shop, Nanofabrication Facility, Scientific Computing facility and Lab Support Facility. We thank the Modic group for the use of the Laue camera, T. Zauner for the photography of the experimental set-up and R. Möller for insightful discussions. Open access funding provided by Institute of Science and Technology (IST Austria).","external_id":{"pmid":["41851325"]},"corr_author":"1","has_accepted_license":"1","department":[{"_id":"ScWa"},{"_id":"GradSch"},{"_id":"LifeSc"}],"article_processing_charge":"Yes (via OA deal)","citation":{"ieee":"G. M. Grosjean <i>et al.</i>, “Adventitious carbon breaks symmetry in oxide contact electrification,” <i>Nature</i>, vol. 651, no. 8106. Springer Nature, pp. 626–631, 2026.","ista":"Grosjean GM, Ostermann M, Sauer M, Hahn M, Pichler CM, Fahrnberger F, Pertl F, Balazs D, Link MM, Kim SH, Schrader DL, Blanco A, Gracia F, Mujica N, Waitukaitis SR. 2026. Adventitious carbon breaks symmetry in oxide contact electrification. Nature. 651(8106), 626–631.","short":"G.M. Grosjean, M. Ostermann, M. Sauer, M. Hahn, C.M. Pichler, F. Fahrnberger, F. Pertl, D. Balazs, M.M. Link, S.H. Kim, D.L. Schrader, A. Blanco, F. Gracia, N. Mujica, S.R. Waitukaitis, Nature 651 (2026) 626–631.","chicago":"Grosjean, Galien M, Markus Ostermann, Markus Sauer, Michael Hahn, Christian M. Pichler, Florian Fahrnberger, Felix Pertl, et al. “Adventitious Carbon Breaks Symmetry in Oxide Contact Electrification.” <i>Nature</i>. Springer Nature, 2026. <a href=\"https://doi.org/10.1038/s41586-025-10088-w\">https://doi.org/10.1038/s41586-025-10088-w</a>.","ama":"Grosjean GM, Ostermann M, Sauer M, et al. Adventitious carbon breaks symmetry in oxide contact electrification. <i>Nature</i>. 2026;651(8106):626-631. doi:<a href=\"https://doi.org/10.1038/s41586-025-10088-w\">10.1038/s41586-025-10088-w</a>","mla":"Grosjean, Galien M., et al. “Adventitious Carbon Breaks Symmetry in Oxide Contact Electrification.” <i>Nature</i>, vol. 651, no. 8106, Springer Nature, 2026, pp. 626–31, doi:<a href=\"https://doi.org/10.1038/s41586-025-10088-w\">10.1038/s41586-025-10088-w</a>.","apa":"Grosjean, G. M., Ostermann, M., Sauer, M., Hahn, M., Pichler, C. M., Fahrnberger, F., … Waitukaitis, S. R. (2026). Adventitious carbon breaks symmetry in oxide contact electrification. <i>Nature</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41586-025-10088-w\">https://doi.org/10.1038/s41586-025-10088-w</a>"},"doi":"10.1038/s41586-025-10088-w","file_date_updated":"2026-03-24T06:57:08Z","abstract":[{"lang":"eng","text":"Insulating oxides are among the most abundant solid materials in the universe1,2,3. Of the many ways in which they influence natural phenomena, perhaps the most consequential is their capacity to transfer electrical charge during contact4,5,6,7,8,9,10—which occurs even between samples of the same oxide—yet the symmetry-breaking parameter that causes this remains unidentified11,12. Here we show that adventitious carbonaceous molecules adsorbed from the environment are the symmetry-breaking factor in same-material oxide contact electrification (CE). We use acoustic levitation to measure charge exchange between a sphere and a plate composed of identical amorphous silicon dioxide (SiO2). Although charging polarity is random for co-prepared samples, we control it with baking or plasma treatment. Observing the charge-exchange relaxation afterwards, we see dynamics over a timescale of hours and connect this directly to the presence of adventitious carbon with time-of-flight mass spectrometry, low-energy ion scattering and infrared spectroscopy. Going further, we confirm that adventitious carbon can even determine charge exchange among different oxides. Our results identify the symmetry-breaking parameter that causes insulating oxides to exchange charge in settings ranging from desert sands4 to volcanic plumes5,6, while simultaneously highlighting an overlooked factor in CE more broadly."}],"publication_identifier":{"issn":["0028-0836"],"eissn":["1476-4687"]}},{"oa_version":"Published Version","month":"03","user_id":"8b945eb4-e2f2-11eb-945a-df72226e66a9","language":[{"iso":"eng"}],"article_processing_charge":"No","doi":"10.15479/AT-ISTA-21651","file_date_updated":"2026-04-15T07:37:25Z","citation":{"chicago":"Baig, Mirza Ahad. “On Secure Chain Selection Rules from Physical Resources in a Permissionless Setting.” Institute of Science and Technology Austria, 2026. <a href=\"https://doi.org/10.15479/AT-ISTA-21651\">https://doi.org/10.15479/AT-ISTA-21651</a>.","short":"M.A. Baig, On Secure Chain Selection Rules from Physical Resources in a Permissionless Setting, Institute of Science and Technology Austria, 2026.","ama":"Baig MA. On secure chain selection rules from physical resources in a permissionless setting. 2026. doi:<a href=\"https://doi.org/10.15479/AT-ISTA-21651\">10.15479/AT-ISTA-21651</a>","ieee":"M. A. Baig, “On secure chain selection rules from physical resources in a permissionless setting,” Institute of Science and Technology Austria, 2026.","ista":"Baig MA. 2026. On secure chain selection rules from physical resources in a permissionless setting. Institute of Science and Technology Austria.","mla":"Baig, Mirza Ahad. <i>On Secure Chain Selection Rules from Physical Resources in a Permissionless Setting</i>. Institute of Science and Technology Austria, 2026, doi:<a href=\"https://doi.org/10.15479/AT-ISTA-21651\">10.15479/AT-ISTA-21651</a>.","apa":"Baig, M. A. (2026). <i>On secure chain selection rules from physical resources in a permissionless setting</i>. Institute of Science and Technology Austria. <a href=\"https://doi.org/10.15479/AT-ISTA-21651\">https://doi.org/10.15479/AT-ISTA-21651</a>"},"abstract":[{"lang":"eng","text":"Blockchains enable distributed consensus in permissionless settings, where participants\r\nare unknown, dynamically changing, and do not trust each other. While Bitcoin,\r\nbased on Proof-of-Work (PoW), was the first protocol in this model, significant\r\nresearch has focused on permissionless protocols using alternative physical resources,\r\nspecifically Proof-of-Space (PoSpace) and Verifiable Delay Functions (VDFs). This\r\nthesis investigates the theoretical limits and design space of longest-chain protocols in\r\nthe fully permissionless and dynamically available settings using these three resources.\r\nFirst, we address the feasibility of blockchains relying solely on storage as a resource.\r\nWe prove a fundamental impossibility result: there exists no secure longest-chain\r\nprotocol based exclusively on Proof-of-Space in the fully permissionless or dynamically\r\navailable settings. Further, we quantify the adversarial capabilities required to execute\r\na double-spend attack. Our result formally justifies the necessity of coupling PoSpace\r\nwith time-dependent primitives (such as VDFs) or to move to less permissive settings\r\n(quasi-permissionless or permissioned) to ensure security.\r\nSecond, we generalize Nakamoto-like heaviest chain consensus to protocols utilizing\r\ncombinations of multiple physical resources. We analyze chain selection rules governed\r\nby a weight function Γ(S, V,W), which assigns weight to blocks based on recorded\r\nSpace (S), VDF speed (V ), and Work (W). We provide a complete classification\r\nof secure weight functions, proving that a weight function is secure against private\r\ndouble-spend attacks if and only if it is homogeneous in the timed resources (V,W)\r\nand sub-homogeneous in S. This framework unifies existing protocols like Bitcoin and\r\nChia under a single theoretical model and provides a powerful tool for designing new\r\nlongest-chain blockchains from a mix of physical resources."}],"publication_identifier":{"isbn":["978-3-99078-078-7"],"issn":["2663-337X"]},"alternative_title":["ISTA Thesis"],"corr_author":"1","has_accepted_license":"1","department":[{"_id":"GradSch"},{"_id":"KrPi"}],"_id":"21651","publisher":"Institute of Science and Technology Austria","date_updated":"2026-04-15T08:45:19Z","ddc":["000"],"degree_awarded":"PhD","title":"On secure chain selection rules from physical resources in a permissionless setting","OA_place":"publisher","license":"https://creativecommons.org/licenses/by-nc-sa/4.0/","author":[{"id":"3EDE6DE4-AA5A-11E9-986D-341CE6697425","last_name":"Baig","first_name":"Mirza Ahad","full_name":"Baig, Mirza Ahad"}],"day":"04","file":[{"relation":"source_file","date_updated":"2026-04-13T08:24:13Z","checksum":"c3986dba90653dac97adba662ebff238","date_created":"2026-04-03T17:28:48Z","access_level":"closed","file_name":"PhD-Thesis-Mirza-Ahad-Baig - Library Submission.zip","file_size":139353434,"creator":"mbaig","file_id":"21655","content_type":"application/x-zip-compressed"},{"file_id":"21656","content_type":"application/pdf","creator":"mbaig","file_size":1942037,"file_name":"2026_Baig_Mirza_Ahad_Thesis.pdf","date_created":"2026-04-03T17:29:30Z","access_level":"open_access","relation":"main_file","date_updated":"2026-04-15T07:37:25Z","checksum":"292a5989262521f7c145a109d1f348cb"}],"supervisor":[{"id":"3E04A7AA-F248-11E8-B48F-1D18A9856A87","last_name":"Pietrzak","orcid":"0000-0002-9139-1654","first_name":"Krzysztof Z","full_name":"Pietrzak, Krzysztof Z"}],"publication_status":"published","fulldoi":"https://doi.org/10.15479/AT-ISTA-21651","tmp":{"short":"CC BY-NC-SA (4.0)","image":"/images/cc_by_nc_sa.png","legal_code_url":"https://creativecommons.org/licenses/by-nc-sa/4.0/legalcode","name":"Creative Commons Attribution-NonCommercial-ShareAlike 4.0 International (CC BY-NC-SA 4.0)"},"related_material":{"record":[{"relation":"part_of_dissertation","status":"public","id":"21134"},{"status":"public","id":"20587","relation":"part_of_dissertation"}]},"year":"2026","status":"public","type":"dissertation","date_created":"2026-04-02T09:31:34Z","oa":1,"date_published":"2026-03-04T00:00:00Z"},{"citation":{"ista":"Chern A, Ishida S. L’Hopital rules for complex-valued functions in higher dimensions. arXiv, 2602.09958.","ieee":"A. Chern and S. Ishida, “L’Hopital rules for complex-valued functions in higher dimensions,” <i>arXiv</i>. .","ama":"Chern A, Ishida S. L’Hopital rules for complex-valued functions in higher dimensions. <i>arXiv</i>. doi:<a href=\"https://doi.org/10.48550/ARXIV.2602.09958\">10.48550/ARXIV.2602.09958</a>","short":"A. Chern, S. Ishida, ArXiv (n.d.).","chicago":"Chern, Albert, and Sadashige Ishida. “L’Hopital Rules for Complex-Valued Functions in Higher Dimensions.” <i>ArXiv</i>, n.d. <a href=\"https://doi.org/10.48550/ARXIV.2602.09958\">https://doi.org/10.48550/ARXIV.2602.09958</a>.","apa":"Chern, A., &#38; Ishida, S. (n.d.). L’Hopital rules for complex-valued functions in higher dimensions. <i>arXiv</i>. <a href=\"https://doi.org/10.48550/ARXIV.2602.09958\">https://doi.org/10.48550/ARXIV.2602.09958</a>","mla":"Chern, Albert, and Sadashige Ishida. “L’Hopital Rules for Complex-Valued Functions in Higher Dimensions.” <i>ArXiv</i>, 2602.09958, doi:<a href=\"https://doi.org/10.48550/ARXIV.2602.09958\">10.48550/ARXIV.2602.09958</a>."},"doi":"10.48550/ARXIV.2602.09958","file_date_updated":"2026-04-28T10:53:27Z","abstract":[{"text":"In calculus, l'Hopital's rule provides a simple way to evaluate the limits of quotient functions when both the numerator and denominator vanish. But what happens when we move beyond real functions on a real interval? In this article, we study when the quotient of two complex-valued functions in higher dimension can be defined continuously at the points where both functions vanish. Surprisingly, the answer is far subtler than in the real-valued setting. We provide a complete characterization for the continuity of the quotient function. We also point out why extending this result to smoother quotients remains an intriguing challenge.","lang":"eng"}],"article_processing_charge":"No","has_accepted_license":"1","department":[{"_id":"GradSch"},{"_id":"ChWo"}],"corr_author":"1","keyword":["l’Hopital theorem","complex functions"],"acknowledgement":"This project was funded in part by the European Research Council (ERC Consolidator Grant 101045083 CoDiNA) and the National Science Foundation CAREER Award 2239062.\r\n","external_id":{"arxiv":["2602.09958"]},"_id":"21737","date_updated":"2026-04-28T10:56:30Z","ddc":["510"],"title":"L'Hopital rules for complex-valued functions in higher dimensions","oa_version":"Preprint","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"month":"02","project":[{"name":"Computational Discovery of Numerical Algorithms for Animation and Simulation of Natural Phenomena","_id":"34bc2376-11ca-11ed-8bc3-9a3b3961a088","grant_number":"101045083"}],"article_number":"2602.09958","publication":"arXiv","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"arxiv":1,"publication_status":"submitted","fulldoi":"https://doi.org/10.48550/ARXIV.2602.09958","type":"preprint","year":"2026","status":"public","oa":1,"date_published":"2026-02-10T00:00:00Z","date_created":"2026-04-15T16:28:24Z","OA_place":"repository","day":"10","author":[{"last_name":"Chern","full_name":"Chern, Albert","first_name":"Albert"},{"full_name":"Ishida, Sadashige","first_name":"Sadashige","last_name":"Ishida","id":"6F7C4B96-A8E9-11E9-A7CA-09ECE5697425","orcid":"0000-0002-3121-3100"}],"file":[{"access_level":"open_access","date_created":"2026-04-28T10:53:27Z","file_name":"2026_arXiv_2602.09958.pdf","checksum":"6a76591c723d3e949ad5afa9f7dbb2ee","date_updated":"2026-04-28T10:53:27Z","relation":"main_file","file_id":"21771","content_type":"application/pdf","success":1,"file_size":867109,"creator":"dernst"}],"OA_type":"green"},{"title":"Navigating complex phase diagrams in soft matter systems","_id":"21764","publisher":"American Physical Society","ddc":["530"],"date_updated":"2026-04-28T07:03:48Z","acknowledgement":"The authors thank Ms. Katrin Muck for her guidance related to the use of HPC. The MC\r\ncomputer simulation results presented here were enabled via a generous share of CPU time, offered by the Vienna Scientific Cluster (VSC) under Project No. 71263. A. J. A. gratefully acknowledges support from the EPSRC under Grant No. EP/P015689/1. This research was funded in part by the Austrian Science Fund (FWF) [Grant DOI: 10.55776/PIN8759524], gratefully acknowledged by G. K .","external_id":{"arxiv":["2603.18918"]},"has_accepted_license":"1","department":[{"_id":"AnSa"},{"_id":"GradSch"}],"article_processing_charge":"Yes (in subscription journal)","file_date_updated":"2026-04-28T06:58:40Z","doi":"10.1103/nbvt-fgjy","citation":{"mla":"Wassermair, Michael, et al. “Navigating Complex Phase Diagrams in Soft Matter Systems.” <i>Physical Review Letters</i>, vol. 136, no. 14, 148203, American Physical Society, 2026, doi:<a href=\"https://doi.org/10.1103/nbvt-fgjy\">10.1103/nbvt-fgjy</a>.","apa":"Wassermair, M., Kahl, G., Roth, R., &#38; Archer, A. J. (2026). Navigating complex phase diagrams in soft matter systems. <i>Physical Review Letters</i>. American Physical Society. <a href=\"https://doi.org/10.1103/nbvt-fgjy\">https://doi.org/10.1103/nbvt-fgjy</a>","ieee":"M. Wassermair, G. Kahl, R. Roth, and A. J. Archer, “Navigating complex phase diagrams in soft matter systems,” <i>Physical Review Letters</i>, vol. 136, no. 14. American Physical Society, 2026.","ista":"Wassermair M, Kahl G, Roth R, Archer AJ. 2026. Navigating complex phase diagrams in soft matter systems. Physical Review Letters. 136(14), 148203.","chicago":"Wassermair, Michael, Gerhard Kahl, Roland Roth, and Andrew J. Archer. “Navigating Complex Phase Diagrams in Soft Matter Systems.” <i>Physical Review Letters</i>. American Physical Society, 2026. <a href=\"https://doi.org/10.1103/nbvt-fgjy\">https://doi.org/10.1103/nbvt-fgjy</a>.","short":"M. Wassermair, G. Kahl, R. Roth, A.J. Archer, Physical Review Letters 136 (2026).","ama":"Wassermair M, Kahl G, Roth R, Archer AJ. Navigating complex phase diagrams in soft matter systems. <i>Physical Review Letters</i>. 2026;136(14). doi:<a href=\"https://doi.org/10.1103/nbvt-fgjy\">10.1103/nbvt-fgjy</a>"},"abstract":[{"text":"Colloidal fluids can exhibit complex phase behavior and determining phase diagrams via experiments or computer simulations can be laborious. We demonstrate that the dispersion relation ω(k), obtained from dynamical density functional theory for the uniform density system, is a highly versatile tool for predicting where in the phase diagram complex crystals form. The sign of ω(k) determines whether density modes with wave number k grow or decay over time. We demonstrate the predictive power by investigating the complex phase behavior of particles interacting via core-shoulder pair potentials. With complementary Monte Carlo simulations, we show that regions of the phase diagram where ωðkÞ has one or several unstable (growing) wave numbers are also where crystalline phases occur. Going further, by tuning these\r\nunstable wave numbers via the interaction-potential and state-point parameters, we design systems with quasicrystals in the phase diagram. We identify a system with a certain shoulder range exhibiting at least ten different phases. Our general approach accelerates considerably the mapping of complex phase diagrams, crucial for the design of new materials.","lang":"eng"}],"publication_identifier":{"issn":["0031-9007"],"eissn":["1079-7114"]},"article_number":"148203","language":[{"iso":"eng"}],"month":"04","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","oa_version":"Published Version","date_created":"2026-04-26T22:01:47Z","oa":1,"date_published":"2026-04-10T00:00:00Z","intvolume":"       136","PlanS_conform":"1","year":"2026","status":"public","issue":"14","type":"journal_article","publication_status":"published","arxiv":1,"fulldoi":"https://doi.org/10.1103/nbvt-fgjy","publication":"Physical Review Letters","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"volume":136,"article_type":"original","OA_type":"hybrid","quality_controlled":"1","file":[{"date_updated":"2026-04-28T06:58:40Z","relation":"main_file","checksum":"8ffb139122a185fcddbe6a9c901a287c","date_created":"2026-04-28T06:58:40Z","access_level":"open_access","file_name":"2026_PhysicalReviewLetters_Wassermair.pdf","file_size":4336488,"creator":"dernst","file_id":"21769","content_type":"application/pdf","success":1}],"author":[{"id":"23d132c4-4e98-11ef-b275-9e8d4cd8c917","last_name":"Wassermair","orcid":"0009-0003-6339-4051","first_name":"Michael","full_name":"Wassermair, Michael"},{"full_name":"Kahl, Gerhard","first_name":"Gerhard","last_name":"Kahl"},{"last_name":"Roth","full_name":"Roth, Roland","first_name":"Roland"},{"last_name":"Archer","full_name":"Archer, Andrew J.","first_name":"Andrew J."}],"day":"10","OA_place":"publisher"},{"OA_place":"publisher","author":[{"full_name":"Petrik, Adam","first_name":"Adam","id":"e273d403-329f-11ee-a353-8c34c056f8ed","last_name":"Petrik"},{"last_name":"Bena","id":"4197c39e-e8ec-11ed-86cb-afed934cd664","full_name":"Bena, Aleksander","first_name":"Aleksander"},{"full_name":"Baunis, Haralds","first_name":"Haralds","id":"2eea55ec-e8ec-11ed-86cb-d9c76787acfe","last_name":"Baunis"},{"last_name":"Kelch","full_name":"Kelch, Riley M.","first_name":"Riley M."},{"full_name":"Yoon, Tehshik P.","first_name":"Tehshik P.","last_name":"Yoon"},{"last_name":"Pieber","orcid":"0000-0001-8689-388X","id":"93e5e5b2-0da6-11ed-8a41-af589a024726","first_name":"Bartholomäus","full_name":"Pieber, Bartholomäus"}],"day":"05","acknowledged_ssus":[{"_id":"LifeSc"},{"_id":"MassSpec"},{"_id":"NMR"},{"_id":"M-Shop"}],"article_type":"original","OA_type":"hybrid","file":[{"file_size":437184,"creator":"dernst","content_type":"application/pdf","file_id":"21833","success":1,"date_updated":"2026-05-07T07:29:24Z","relation":"main_file","checksum":"afe9752977898642c903abdc70b4a283","date_created":"2026-05-07T07:29:24Z","access_level":"open_access","file_name":"2026_AdvSynthCatal_Petrik.pdf"}],"quality_controlled":"1","volume":368,"fulldoi":"https://doi.org/10.1002/adsc.70417","publication_status":"published","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"publication":"Advanced Synthesis & Catalysis","status":"public","PlanS_conform":"1","year":"2026","intvolume":"       368","type":"journal_article","issue":"9","date_created":"2026-05-03T22:01:36Z","date_published":"2026-05-05T00:00:00Z","oa":1,"oa_version":"Published Version","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"month":"05","scopus_import":"1","project":[{"grant_number":"PAT 1250924","_id":"8f1d607d-16d5-11f0-9cad-ab453295ba5e","name":"Photoactive ligands for transformative nickel catalysis"}],"article_number":"e70417","article_processing_charge":"Yes (via OA deal)","publication_identifier":{"eissn":["1615-4169"],"issn":["1615-4150"]},"abstract":[{"lang":"eng","text":"Pyridyl motifs equipped with N-substituents can be powerful ligands for catalysis, yet their broader adoption is limited by the lack of a practical method to prepare these scaffolds. We report a modular, robust, and versatile Buchwald–Hartwig amination protocol that enables the rapid synthesis of bipyridine, phenanthroline, terpyridine, and pybox ligands bearing dialkylamine, diarylamine, and heteroaromatic N-substituents. These conditions streamline ligand library synthesis and will facilitate systematic studies in catalysis and related applications."}],"file_date_updated":"2026-05-07T07:29:24Z","doi":"10.1002/adsc.70417","citation":{"apa":"Petrik, A., Bena, A., Baunis, H., Kelch, R. M., Yoon, T. P., &#38; Pieber, B. (2026). Facile access to N-substituted pyridyl ligands. <i>Advanced Synthesis &#38; Catalysis</i>. Wiley. <a href=\"https://doi.org/10.1002/adsc.70417\">https://doi.org/10.1002/adsc.70417</a>","mla":"Petrik, Adam, et al. “Facile Access to N-Substituted Pyridyl Ligands.” <i>Advanced Synthesis &#38; Catalysis</i>, vol. 368, no. 9, e70417, Wiley, 2026, doi:<a href=\"https://doi.org/10.1002/adsc.70417\">10.1002/adsc.70417</a>.","ista":"Petrik A, Bena A, Baunis H, Kelch RM, Yoon TP, Pieber B. 2026. Facile access to N-substituted pyridyl ligands. Advanced Synthesis &#38; Catalysis. 368(9), e70417.","ieee":"A. Petrik, A. Bena, H. Baunis, R. M. Kelch, T. P. Yoon, and B. Pieber, “Facile access to N-substituted pyridyl ligands,” <i>Advanced Synthesis &#38; Catalysis</i>, vol. 368, no. 9. Wiley, 2026.","ama":"Petrik A, Bena A, Baunis H, Kelch RM, Yoon TP, Pieber B. Facile access to N-substituted pyridyl ligands. <i>Advanced Synthesis &#38; Catalysis</i>. 2026;368(9). doi:<a href=\"https://doi.org/10.1002/adsc.70417\">10.1002/adsc.70417</a>","chicago":"Petrik, Adam, Aleksander Bena, Haralds Baunis, Riley M. Kelch, Tehshik P. Yoon, and Bartholomäus Pieber. “Facile Access to N-Substituted Pyridyl Ligands.” <i>Advanced Synthesis &#38; Catalysis</i>. Wiley, 2026. <a href=\"https://doi.org/10.1002/adsc.70417\">https://doi.org/10.1002/adsc.70417</a>.","short":"A. Petrik, A. Bena, H. Baunis, R.M. Kelch, T.P. Yoon, B. Pieber, Advanced Synthesis &#38; Catalysis 368 (2026)."},"corr_author":"1","department":[{"_id":"BaPi"},{"_id":"GradSch"}],"has_accepted_license":"1","date_updated":"2026-05-07T07:33:33Z","ddc":["540"],"_id":"21776","publisher":"Wiley","acknowledgement":"We gratefully acknowledge ISTA for generous financial support. B.P. acknowledges the Austrian Science Fund (PAT 1250924) and the ACS GCI Pharmaceutical Roundtable for funding; T.P.Y acknowledges the NSF(CHE-2349003) for financial support. This research was supported by the Scientific Service Units (SSU) of ISTA through resources provided by the Lab Support Facility, Mass Spec Facility, NMR facility, and the Miba Machine Shop. We specifically thank Aikaterina Paraskevopoulou for HRMS measurements and Jan Pecak for support with ICP-OES experi-ments. NMR facilities at UW−Madison were supported by the NSF(CHE-1048642) and a generous gift from Paul J. and Margaret M. Bender. Open Access funding provided by Institute of Science and Technology Austria/KEMÖ. This study was supported by Austrian Science Fund (PAT 1250924), ACSGCI Pharmaceutical Roundtable, and National Science Foundation(CHE-2349003) and (CHE-1048642).","title":"Facile access to N-substituted pyridyl ligands"},{"quality_controlled":"1","file":[{"checksum":"8cb95b033ad2a1a7a8181f6f078c05b5","relation":"main_file","date_updated":"2026-05-11T06:32:12Z","access_level":"open_access","date_created":"2026-05-11T06:32:12Z","file_name":"2026_NatureComm_Zambra.pdf","file_size":1784917,"creator":"dernst","content_type":"application/pdf","file_id":"21850","success":1}],"article_type":"original","OA_type":"gold","volume":17,"OA_place":"publisher","acknowledged_ssus":[{"_id":"NanoFab"}],"day":"29","author":[{"last_name":"Zambra","id":"467ed36b-dc96-11ea-b7c8-b043a380b282","orcid":"0000-0002-8806-5719","first_name":"Valeska","full_name":"Zambra, Valeska"},{"id":"1a362536-4d02-11f1-8543-8351136efc50","last_name":"Nathwani","full_name":"Nathwani, Amit","first_name":"Amit"},{"first_name":"Muhammad","full_name":"Nauman, Muhammad","last_name":"Nauman","id":"32c21954-2022-11eb-9d5f-af9f93c24e71","orcid":"0000-0002-2111-4846"},{"full_name":"Lewin, Sylvia K.","first_name":"Sylvia K.","last_name":"Lewin"},{"last_name":"Frank","first_name":"Corey E.","full_name":"Frank, Corey E."},{"last_name":"Butch","full_name":"Butch, Nicholas P.","first_name":"Nicholas P."},{"first_name":"Arkady","full_name":"Shekhter, Arkady","last_name":"Shekhter"},{"first_name":"B. J.","full_name":"Ramshaw, B. J.","last_name":"Ramshaw"},{"first_name":"Kimberly A","full_name":"Modic, Kimberly A","last_name":"Modic","id":"13C26AC0-EB69-11E9-87C6-5F3BE6697425","orcid":"0000-0001-9760-3147"}],"type":"journal_article","related_material":{"record":[{"id":"21174","relation":"research_data","status":"public"}]},"intvolume":"        17","PlanS_conform":"1","year":"2026","status":"public","oa":1,"date_published":"2026-04-29T00:00:00Z","date_created":"2026-05-10T22:02:15Z","publication":"Nature Communications","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"arxiv":1,"publication_status":"published","fulldoi":"https://doi.org/10.1038/s41467-026-71899-7","project":[{"grant_number":"101078696","_id":"bd968c70-d553-11ed-ba76-cde40b0aba64","name":"Gaining leverage with spin liquids and superconductors"}],"article_number":"3742","oa_version":"Published Version","scopus_import":"1","month":"04","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"acknowledgement":"We appreciate technical support from Salvatore Bagiante, Evgeniia Volobueva, Lubuna Shafeek, Ali Bangura, and Zoltán Köllö, and scientific discussions with Daniel Agterberg, Johnpierre Paglione, Qimiao Si, Josephine Yu and Yue Yu. V.Z., A.N., M.N., and K.A.M. acknowledge funding received from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (TROPIC-101078696). V.Z., A.N., M.N., and K.A.M. thank the ISTA Nanofabrication Facility for technical support. B.J.R. acknowledges funding from the Office of Basic Energy Sciences of the United States Department of Energy under award number DE-SC0020143 for data analysis and writing. The National High Magnetic Field Laboratory is supported by the National Science Foundation through NSF/DMR-2128556*, the State of Florida, and the U.S. Department of Energy. A.S. acknowledges support from the DOE/BES “Science of 100 T” grant. A.S. thanks Downtown Subscription in Santa Fe, NM, for their patience in hosting him. Sample preparation and characterization were supported by the NSF through DMR-2105191.","external_id":{"arxiv":["2506.08984"]},"_id":"21845","publisher":"Springer Nature","ddc":["530"],"date_updated":"2026-05-11T06:36:00Z","title":"Giant transverse magnetic fluctuations at the edge of re-entrant superconductivity in UTe2","file_date_updated":"2026-05-11T06:32:12Z","citation":{"mla":"Zambra, Valeska, et al. “Giant Transverse Magnetic Fluctuations at the Edge of Re-Entrant Superconductivity in UTe2.” <i>Nature Communications</i>, vol. 17, 3742, Springer Nature, 2026, doi:<a href=\"https://doi.org/10.1038/s41467-026-71899-7\">10.1038/s41467-026-71899-7</a>.","apa":"Zambra, V., Nathwani, A., Nauman, M., Lewin, S. K., Frank, C. E., Butch, N. P., … Modic, K. A. (2026). Giant transverse magnetic fluctuations at the edge of re-entrant superconductivity in UTe2. <i>Nature Communications</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41467-026-71899-7\">https://doi.org/10.1038/s41467-026-71899-7</a>","ieee":"V. Zambra <i>et al.</i>, “Giant transverse magnetic fluctuations at the edge of re-entrant superconductivity in UTe2,” <i>Nature Communications</i>, vol. 17. Springer Nature, 2026.","ista":"Zambra V, Nathwani A, Nauman M, Lewin SK, Frank CE, Butch NP, Shekhter A, Ramshaw BJ, Modic KA. 2026. Giant transverse magnetic fluctuations at the edge of re-entrant superconductivity in UTe2. Nature Communications. 17, 3742.","chicago":"Zambra, Valeska, Amit Nathwani, Muhammad Nauman, Sylvia K. Lewin, Corey E. Frank, Nicholas P. Butch, Arkady Shekhter, B. J. Ramshaw, and Kimberly A Modic. “Giant Transverse Magnetic Fluctuations at the Edge of Re-Entrant Superconductivity in UTe2.” <i>Nature Communications</i>. Springer Nature, 2026. <a href=\"https://doi.org/10.1038/s41467-026-71899-7\">https://doi.org/10.1038/s41467-026-71899-7</a>.","short":"V. Zambra, A. Nathwani, M. Nauman, S.K. Lewin, C.E. Frank, N.P. Butch, A. Shekhter, B.J. Ramshaw, K.A. Modic, Nature Communications 17 (2026).","ama":"Zambra V, Nathwani A, Nauman M, et al. Giant transverse magnetic fluctuations at the edge of re-entrant superconductivity in UTe2. <i>Nature Communications</i>. 2026;17. doi:<a href=\"https://doi.org/10.1038/s41467-026-71899-7\">10.1038/s41467-026-71899-7</a>"},"doi":"10.1038/s41467-026-71899-7","publication_identifier":{"eissn":["2041-1723"]},"abstract":[{"lang":"eng","text":"UTe2 exhibits the remarkable phenomenon of re-entrant superconductivity, whereby the zero-resistance state reappears above 40 tesla after being suppressed with a field of around 10 tesla. One potential pairing mechanism, invoked in the related re-entrant superconductors UCoGe and URhGe, involves transverse fluctuations of a ferromagnetic order parameter. However, the requisite ferromagnetic order—present in both UCoGe and URhGe—is absent in UTe2, and neutron scattering shows instead that the magnetic susceptibility is peaked at an antiferromagnetic wavevector. Here, we measure the magnetotropic susceptibility of UTe2 across two field-angle planes. This quantity is sensitive to the magnetic susceptibility in a direction transverse to the applied magnetic field—a quantity that is not accessed in conventional magnetization measurements. We observe a very large decrease in the magnetotropic susceptibility over a broad range of field orientations, indicating a large increase in the transverse magnetic susceptibility. Because our technique probes the magnetic susceptibility in the long wavelength (q = 0) limit, this suggests that the strong transverse susceptibility arises from ferromagnetic spin fluctuations. These ferromagnetic fluctuations are likely important for understanding the pairing mechanism in UTe2, as all three superconducting phases of UTe2 surround this region of enhanced susceptibility in the field-angle phase diagram."}],"article_processing_charge":"Yes","DOAJ_listed":"1","has_accepted_license":"1","department":[{"_id":"KiMo"},{"_id":"GradSch"}],"corr_author":"1"},{"article_number":"2114","project":[{"_id":"23841C26-32DE-11EA-91FC-C7463DDC885E","name":"Non-Ergodic Quantum Matter: Universality, Dynamics and Control","call_identifier":"H2020","grant_number":"850899"}],"language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"05","oa_version":"Published Version","title":"Tensor cross interpolation of purities in quantum many-body systems","external_id":{"arxiv":["2503.17230"]},"acknowledgement":"We acknowledge useful discussions with Richard Küng\r\non the interpolation methods and error spreading, Ilia\r\nA. Luchnikov, Margarita Davydova, and, in particular, Hiroshi Shinaoka, Marc Ritter, Yuriel Nuñez\r\nfor useful discussions about TCI and the various\r\nworkarounds within the TensorCrossInterpolation.jl\r\nlibrary. We also acknowledge the comments of anonymous Referee B, that encouraged us to expand the\r\nmanuscript with discussion of additional applications\r\nof entanglement feature in Section 4.3. M.S. acknowledges discussions with D. V. Savostyanov at the 2nd\r\nInternational Quantum Tensor Networks (IQTN) plenary meeting at Flatiron Institute’s Center for Computational Quantum Physics (CCQ) for introduction\r\nto the TCI approach. D.K and M.S. acknowledge support by the European Research Council (ERC) under We acknowledge useful discussions with Richard Küng\r\non the interpolation methods and error spreading, Ilia\r\nA. Luchnikov, Margarita Davydova, and, in particular, Hiroshi Shinaoka, Marc Ritter, Yuriel Nuñez\r\nfor useful discussions about TCI and the various\r\nworkarounds within the TensorCrossInterpolation.jl\r\nlibrary. We also acknowledge the comments of anonymous Referee B, that encouraged us to expand the\r\nmanuscript with discussion of additional applications\r\nof entanglement feature in Section 4.3. M.S. acknowledges discussions with D. V. Savostyanov at the 2nd\r\nInternational Quantum Tensor Networks (IQTN) plenary meeting at Flatiron Institute’s Center for Computational Quantum Physics (CCQ) for introduction\r\nto the TCI approach. D.K and M.S. acknowledge support by the European Research Council (ERC) under We acknowledge useful discussions with Richard Küng\r\non the interpolation methods and error spreading, Ilia\r\nA. Luchnikov, Margarita Davydova, and, in particular, Hiroshi Shinaoka, Marc Ritter, Yuriel Nuñez\r\nfor useful discussions about TCI and the various\r\nworkarounds within the TensorCrossInterpolation.jl\r\nlibrary. We also acknowledge the comments of anonymous Referee B, that encouraged us to expand the\r\nmanuscript with discussion of additional applications\r\nof entanglement feature in Section 4.3. M.S. acknowledges discussions with D. V. Savostyanov at the 2nd\r\nInternational Quantum Tensor Networks (IQTN) plenary meeting at Flatiron Institute’s Center for Computational Quantum Physics (CCQ) for introduction\r\nto the TCI approach. D.K and M.S. acknowledge support by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (Grant Agreement No. 850899).\r\nR.V. acknowledges partial support from the US Department of Energy, Office of Science, Basic Energy\r\nSciences, under award No. DE-SC0023999, and the\r\nSwiss National Science Foundation (grant 10008234).\r\nThis research was supported in part by grant NSF\r\nPHY-2309135 to the Kavli Institute for Theoretical\r\nPhysics (KITP)","date_updated":"2026-06-02T09:15:13Z","ddc":["530"],"publisher":"Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften","_id":"21917","department":[{"_id":"MaSe"},{"_id":"GradSch"}],"has_accepted_license":"1","corr_author":"1","abstract":[{"lang":"eng","text":"A defining feature of quantum many-body systems is the exponential scaling of the Hilbert space with the number of degrees of freedom. This exponential complexity naïvely renders a complete state characterization, for instance via the complete set of bipartite Renyi entropies for all disjoint regions, a challenging task. Recently, a compact way of storing subregions' purities by encoding them as amplitudes of a fictitious quantum wave function, known as entanglement feature, was proposed. Notably, the entanglement feature can be a simple object even for highly entangled quantum states. However the complexity and practical usage of the entanglement feature for general quantum states has not been explored. In this work, we demonstrate that the entanglement feature can be efficiently learned using only a polynomial amount of samples in the number of degrees of freedom through the so-called tensor cross interpolation (TCI) algorithm, assuming it is expressible as a finite bond dimension MPS. We benchmark this learning process on Haar and random MPS states, confirming analytic expectations. Applying the TCI algorithm to quantum eigenstates of various one dimensional quantum systems, we identify cases where eigenstates have entanglement feature learnable with TCI. We conclude with possible applications of the learned entanglement feature, such as quantifying the distance between different entanglement patterns and finding the optimal one-dimensional ordering of physical indices in a given state, highlighting the potential utility of the proposed purity interpolation method."}],"publication_identifier":{"eissn":["2521-327X"]},"file_date_updated":"2026-06-02T09:12:11Z","citation":{"ista":"Kolisnyk D, Medina Ramos RA, Vasseur R, Serbyn M. 2026. Tensor cross interpolation of purities in quantum many-body systems. Quantum. 10, 2114.","ieee":"D. Kolisnyk, R. A. Medina Ramos, R. Vasseur, and M. Serbyn, “Tensor cross interpolation of purities in quantum many-body systems,” <i>Quantum</i>, vol. 10. Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften, 2026.","ama":"Kolisnyk D, Medina Ramos RA, Vasseur R, Serbyn M. Tensor cross interpolation of purities in quantum many-body systems. <i>Quantum</i>. 2026;10. doi:<a href=\"https://doi.org/10.22331/q-2026-05-22-2114\">10.22331/q-2026-05-22-2114</a>","short":"D. Kolisnyk, R.A. Medina Ramos, R. Vasseur, M. Serbyn, Quantum 10 (2026).","chicago":"Kolisnyk, Dmytro, Raimel A Medina Ramos, Romain Vasseur, and Maksym Serbyn. “Tensor Cross Interpolation of Purities in Quantum Many-Body Systems.” <i>Quantum</i>. Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften, 2026. <a href=\"https://doi.org/10.22331/q-2026-05-22-2114\">https://doi.org/10.22331/q-2026-05-22-2114</a>.","apa":"Kolisnyk, D., Medina Ramos, R. A., Vasseur, R., &#38; Serbyn, M. (2026). Tensor cross interpolation of purities in quantum many-body systems. <i>Quantum</i>. Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften. <a href=\"https://doi.org/10.22331/q-2026-05-22-2114\">https://doi.org/10.22331/q-2026-05-22-2114</a>","mla":"Kolisnyk, Dmytro, et al. “Tensor Cross Interpolation of Purities in Quantum Many-Body Systems.” <i>Quantum</i>, vol. 10, 2114, Verein zur Förderung des Open Access Publizierens in den Quantenwissenschaften, 2026, doi:<a href=\"https://doi.org/10.22331/q-2026-05-22-2114\">10.22331/q-2026-05-22-2114</a>."},"doi":"10.22331/q-2026-05-22-2114","DOAJ_listed":"1","article_processing_charge":"Yes","volume":10,"file":[{"checksum":"f8ce78607ad06120cdf894dc8cef55da","relation":"main_file","date_updated":"2026-06-02T09:12:11Z","file_name":"2026_Quantum_Kolisnyk.pdf","access_level":"open_access","date_created":"2026-06-02T09:12:11Z","creator":"dernst","file_size":3284798,"success":1,"file_id":"21939","content_type":"application/pdf"}],"quality_controlled":"1","article_type":"original","OA_type":"gold","day":"22","author":[{"first_name":"Dmytro","full_name":"Kolisnyk, Dmytro","id":"530a7320-5355-11ee-ae5a-82a46997aaa7","last_name":"Kolisnyk","orcid":"0000-0002-8612-8202"},{"last_name":"Medina Ramos","id":"CE680B90-D85A-11E9-B684-C920E6697425","orcid":"0000-0002-5383-2869","full_name":"Medina Ramos, Raimel A","first_name":"Raimel A"},{"last_name":"Vasseur","full_name":"Vasseur, Romain","first_name":"Romain"},{"id":"47809E7E-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-2399-5827","last_name":"Serbyn","full_name":"Serbyn, Maksym","first_name":"Maksym"}],"OA_place":"publisher","ec_funded":1,"date_published":"2026-05-22T00:00:00Z","oa":1,"date_created":"2026-05-26T19:39:12Z","type":"journal_article","PlanS_conform":"1","year":"2026","status":"public","intvolume":"        10","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"publication":"Quantum","fulldoi":"https://doi.org/10.22331/q-2026-05-22-2114","arxiv":1,"publication_status":"published"},{"corr_author":"1","alternative_title":["ISTA Thesis"],"department":[{"_id":"GradSch"},{"_id":"NiBa"},{"_id":"JaMa"}],"has_accepted_license":"1","article_processing_charge":"No","publication_identifier":{"issn":["2663-337X"]},"doi":"10.15479/AT-ISTA-21918","citation":{"ieee":"K. Khudiakova, “How epistasis and purifying selection shape genetic diversity,” Institute of Science and Technology Austria, 2026.","ista":"Khudiakova K. 2026. How epistasis and purifying selection shape genetic diversity. Institute of Science and Technology Austria.","chicago":"Khudiakova, Kseniia. “How Epistasis and Purifying Selection Shape Genetic Diversity.” Institute of Science and Technology Austria, 2026. <a href=\"https://doi.org/10.15479/AT-ISTA-21918\">https://doi.org/10.15479/AT-ISTA-21918</a>.","short":"K. Khudiakova, How Epistasis and Purifying Selection Shape Genetic Diversity, Institute of Science and Technology Austria, 2026.","ama":"Khudiakova K. How epistasis and purifying selection shape genetic diversity. 2026. doi:<a href=\"https://doi.org/10.15479/AT-ISTA-21918\">10.15479/AT-ISTA-21918</a>","mla":"Khudiakova, Kseniia. <i>How Epistasis and Purifying Selection Shape Genetic Diversity</i>. Institute of Science and Technology Austria, 2026, doi:<a href=\"https://doi.org/10.15479/AT-ISTA-21918\">10.15479/AT-ISTA-21918</a>.","apa":"Khudiakova, K. (2026). <i>How epistasis and purifying selection shape genetic diversity</i>. Institute of Science and Technology Austria. <a href=\"https://doi.org/10.15479/AT-ISTA-21918\">https://doi.org/10.15479/AT-ISTA-21918</a>"},"file_date_updated":"2026-06-11T12:14:53Z","title":"How epistasis and purifying selection shape genetic diversity","date_updated":"2026-06-12T12:43:35Z","ddc":["576"],"publisher":"Institute of Science and Technology Austria","_id":"21918","degree_awarded":"PhD","acknowledgement":"At different stages of my PhD, my work was supported by several grants: the\r\nDOC fellowship of the Austrian Academy of Sciences (26293, awarded to me),\r\nthe FWF-SFB grant (PT1032F06504 n. F65, awarded to Jan Maas), and the ERC\r\ngrant (PR1032ERC01 n. 716117, awarded to Jan Maas). I also appreciate the help\r\nfrom the Scientific Computing unit for their advice on the cluster usage.","user_id":"8b945eb4-e2f2-11eb-945a-df72226e66a9","month":"06","language":[{"iso":"eng"}],"oa_version":"Published Version","project":[{"_id":"256E75B8-B435-11E9-9278-68D0E5697425","name":"Optimal Transport and Stochastic Dynamics","call_identifier":"H2020","grant_number":"716117"},{"_id":"34d33d68-11ca-11ed-8bc3-ec13763c0ca8","name":"The impact of deleterious mutations on small populations","grant_number":"26293"},{"grant_number":"F6504","_id":"fc31cba2-9c52-11eb-aca3-ff467d239cd2","name":"Taming Complexity in Partial Differential Systems"}],"fulldoi":"https://doi.org/10.15479/AT-ISTA-21918","publication_status":"published","tmp":{"image":"/images/cc_by_nc_nd.png","short":"CC BY-NC-ND (4.0)","legal_code_url":"https://creativecommons.org/licenses/by-nc-nd/4.0/legalcode","name":"Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)"},"date_created":"2026-05-27T06:26:08Z","date_published":"2026-06-07T00:00:00Z","status":"public","year":"2026","related_material":{"record":[{"relation":"part_of_dissertation","id":"11447","status":"public"},{"relation":"part_of_dissertation","id":"12513","status":"deleted"},{"id":"21967","relation":"part_of_dissertation","status":"public"},{"relation":"part_of_dissertation","id":"21968","status":"public"}]},"type":"dissertation","author":[{"orcid":"0000-0002-6246-1465","id":"4E6DC800-AE37-11E9-AC72-31CAE5697425","last_name":"Khudiakova","first_name":"Kseniia","full_name":"Khudiakova, Kseniia"}],"day":"07","acknowledged_ssus":[{"_id":"ScienComp"}],"OA_place":"publisher","ec_funded":1,"page":"89","license":"https://creativecommons.org/licenses/by-nc-nd/4.0/","supervisor":[{"first_name":"Nicholas H","full_name":"Barton, Nicholas H","orcid":"0000-0002-8548-5240","last_name":"Barton","id":"4880FE40-F248-11E8-B48F-1D18A9856A87"},{"full_name":"Maas, Jan","first_name":"Jan","orcid":"0000-0002-0845-1338","id":"4C5696CE-F248-11E8-B48F-1D18A9856A87","last_name":"Maas"}],"file":[{"access_level":"closed","date_created":"2026-06-09T08:34:38Z","file_name":"thesis.zip","checksum":"0cff64ae74f0f9f2d7011700c82f700a","relation":"source_file","date_updated":"2026-06-09T08:40:48Z","file_id":"21965","content_type":"application/x-zip-compressed","file_size":20549813,"creator":"kkhudiak"},{"file_id":"21969","content_type":"application/pdf","creator":"kkhudiak","file_size":9387029,"embargo_to":"open_access","file_name":"2026_Khudiakova_Ksenia_Thesis.pdf","date_created":"2026-06-09T12:28:51Z","access_level":"closed","embargo":"2027-06-10","relation":"main_file","date_updated":"2026-06-11T12:14:53Z","checksum":"547ae42de37cc86894af283f1664dbc8"}]},{"department":[{"_id":"GradSch"},{"_id":"PaSc"}],"has_accepted_license":"1","corr_author":"1","publication_identifier":{"issn":["0961-8368"],"eissn":["1469-896X"]},"abstract":[{"lang":"eng","text":"The import of proteins into mitochondria poses fundamental mechanistic challenges: aggregation-prone precursor proteins must be maintained in aqueous compartments and threaded through narrow pores without becoming stuck or mislocalized. Recent evidence from mitochondrial protein import studies and other chaperone systems underscores the critical role of dynamics in balancing sufficiently tight binding, promiscuity, specificity, and release. Dynamic binding of client precursor proteins to import machinery components arises naturally from the avidity of their interactions. Conformational entropy enhances their stability, while the multivalent nature of these interactions ensures that client transfer to downstream insertases occurs without a substantial energy barrier. Here, we discuss this emerging paradigm of dynamic protein handling, using examples where dynamic structures have been resolved and highlight outstanding questions."}],"file_date_updated":"2026-06-02T07:23:12Z","citation":{"mla":"Schneider, Jakob, et al. “Dynamic Disorder Is Crucial for Mitochondrial Protein Import.” <i>Protein Science</i>, vol. 35, no. 6, e70630, Wiley, 2026, doi:<a href=\"https://doi.org/10.1002/pro.70630\">10.1002/pro.70630</a>.","apa":"Schneider, J., Guillerm, U., Simoes Pereira, C., &#38; Schanda, P. (2026). Dynamic disorder is crucial for mitochondrial protein import. <i>Protein Science</i>. Wiley. <a href=\"https://doi.org/10.1002/pro.70630\">https://doi.org/10.1002/pro.70630</a>","ieee":"J. Schneider, U. Guillerm, C. Simoes Pereira, and P. Schanda, “Dynamic disorder is crucial for mitochondrial protein import,” <i>Protein Science</i>, vol. 35, no. 6. Wiley, 2026.","ista":"Schneider J, Guillerm U, Simoes Pereira C, Schanda P. 2026. Dynamic disorder is crucial for mitochondrial protein import. Protein Science. 35(6), e70630.","chicago":"Schneider, Jakob, Undina Guillerm, Caroline Simoes Pereira, and Paul Schanda. “Dynamic Disorder Is Crucial for Mitochondrial Protein Import.” <i>Protein Science</i>. Wiley, 2026. <a href=\"https://doi.org/10.1002/pro.70630\">https://doi.org/10.1002/pro.70630</a>.","short":"J. Schneider, U. Guillerm, C. Simoes Pereira, P. Schanda, Protein Science 35 (2026).","ama":"Schneider J, Guillerm U, Simoes Pereira C, Schanda P. Dynamic disorder is crucial for mitochondrial protein import. <i>Protein Science</i>. 2026;35(6). doi:<a href=\"https://doi.org/10.1002/pro.70630\">10.1002/pro.70630</a>"},"doi":"10.1002/pro.70630","article_processing_charge":"Yes (via OA deal)","title":"Dynamic disorder is crucial for mitochondrial protein import","external_id":{"pmid":["42159315"]},"acknowledgement":"We gratefully acknowledge research funding by the Austrian Science Fund (FWF), projects 10.55776/PAT1647625 and 10.55776/I6223. We thank Prof. Long Li (Peking University) for providing structural models and EM density for the TOM and TIM23 complexes, used to generate part of Figure 3. Open Access funding provided by Institute of Science and Technology Austria.","ddc":["572"],"date_updated":"2026-06-02T07:26:34Z","publisher":"Wiley","_id":"21929","scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"06","language":[{"iso":"eng"}],"oa_version":"Published Version","article_number":"e70630","project":[{"grant_number":"I06223","_id":"bdb9578d-d553-11ed-ba76-ed5d39fce6f0","name":"Structure and mechanism of the mitochondrial MIM insertase"}],"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"publication":"Protein Science","fulldoi":"https://doi.org/10.1002/pro.70630","publication_status":"published","date_published":"2026-06-01T00:00:00Z","oa":1,"date_created":"2026-05-31T22:02:12Z","type":"journal_article","issue":"6","status":"public","year":"2026","PlanS_conform":"1","intvolume":"        35","day":"01","author":[{"id":"64368429-eb97-11eb-a6c2-c980b1f44415","last_name":"Schneider","full_name":"Schneider, Jakob","first_name":"Jakob"},{"full_name":"Guillerm, Undina","first_name":"Undina","last_name":"Guillerm","id":"bb74f472-ae54-11eb-9835-bc9c22fb1183"},{"full_name":"Simoes Pereira, Caroline","first_name":"Caroline","id":"87266c4a-96d2-11ef-be2c-fe5633233ec3","last_name":"Simoes Pereira"},{"first_name":"Paul","full_name":"Schanda, Paul","orcid":"0000-0002-9350-7606","id":"7B541462-FAF6-11E9-A490-E8DFE5697425","last_name":"Schanda"}],"OA_place":"publisher","volume":35,"file":[{"checksum":"e0163459a7238fdcc3fc5e17bedcce9a","date_updated":"2026-06-02T07:23:12Z","relation":"main_file","file_name":"2026_ProteinScience_Schneider.pdf","access_level":"open_access","date_created":"2026-06-02T07:23:12Z","creator":"dernst","file_size":3897305,"success":1,"content_type":"application/pdf","file_id":"21937"}],"quality_controlled":"1","pmid":1,"OA_type":"hybrid","article_type":"original"},{"date_published":"2026-05-05T00:00:00Z","oa":1,"date_created":"2026-06-09T08:08:53Z","type":"preprint","year":"2026","status":"public","tmp":{"image":"/images/cc_by_nc.png","short":"CC BY-NC (4.0)","name":"Creative Commons Attribution-NonCommercial 4.0 International (CC BY-NC 4.0)","legal_code_url":"https://creativecommons.org/licenses/by-nc/4.0/legalcode"},"publication":"bioRxiv","fulldoi":"https://doi.org/10.64898/2026.05.01.722191","publication_status":"submitted","OA_type":"green","day":"05","acknowledged_ssus":[{"_id":"Bio"},{"_id":"LifeSc"},{"_id":"PreCl"}],"author":[{"last_name":"Miranda","id":"862A3C56-A8BF-11E9-B4FA-D9E3E5697425","orcid":"0000-0001-6618-6889","first_name":"Osvaldo","full_name":"Miranda, Osvaldo"},{"full_name":"Contreras, Ximena","first_name":"Ximena","id":"475990FE-F248-11E8-B48F-1D18A9856A87","last_name":"Contreras"},{"last_name":"Pauler","orcid":"0000-0002-7462-0048","id":"48EA0138-F248-11E8-B48F-1D18A9856A87","first_name":"Florian","full_name":"Pauler, Florian"},{"full_name":"Davaatseren, Amarbayasgalan","first_name":"Amarbayasgalan","id":"70ADC922-B424-11E9-99E3-BA18E6697425","last_name":"Davaatseren"},{"id":"4CD6AAC6-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-3183-8207","last_name":"Amberg","full_name":"Amberg, Nicole","first_name":"Nicole"},{"first_name":"Carmen","full_name":"Streicher, Carmen","last_name":"Streicher","id":"36BCB99C-F248-11E8-B48F-1D18A9856A87"},{"full_name":"Villalba Requena, Ana","first_name":"Ana","last_name":"Villalba Requena","id":"68cb85a0-39f7-11eb-9559-9aaab4f6a247","orcid":"0000-0002-5615-5277"},{"last_name":"Heger","id":"4B76FFD2-F248-11E8-B48F-1D18A9856A87","first_name":"Anna-Magdalena","full_name":"Heger, Anna-Magdalena"},{"last_name":"Marie","first_name":"Corentine","full_name":"Marie, Corentine"},{"last_name":"Hassan","first_name":"Bassem A.","full_name":"Hassan, Bassem A."},{"full_name":"Rülicke, Thomas","first_name":"Thomas","last_name":"Rülicke"},{"first_name":"Simon","full_name":"Hippenmeyer, Simon","id":"37B36620-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0003-2279-1061","last_name":"Hippenmeyer"}],"license":"https://creativecommons.org/licenses/by-nc/4.0/","OA_place":"repository","ec_funded":1,"title":"Pten orchestrates neurogenic radial glia lineage progression and tunes neocortical astrocyte production","acknowledgement":"We thank Kay-Uwe Wagner (Wayne State University) for generously sharing Jak1/2–flox mouse lines; A.\r\nSommer (VBCF GmbH, NGS Unit) for technical support; N. Kim, V. Mick, S. Schnabl, S. Gobeil, and L.\r\nAndersen for technical assistance; all members of the Hippenmeyer lab for discussion and B. Novitch for\r\ncomments on earlier versions of the manuscript. This research was supported by the Scientific Service Units\r\n(SSU) of IST Austria through resources provided by the Imaging and Optics Facility (IOF), Lab Support-\r\n(LSF) and Preclinical Facilities (PCF). O.A.M received support from the Austrian Academy of Sciences\r\nÖAW (DOC 186584), and N.A. from FWF Elise Richter Program (Grant V1041T). This work was also\r\nsupported by IST Austria institutional funds; FWF SFB F78 (Neuro Stem Modulation) to S.H., and the\r\nEuropean Research Council (ERC) under the European Union’s Horizon 2020 research and innovation\r\nprogramme (grant agreement No 725780 LinPro) to S.H.","ddc":["570"],"date_updated":"2026-06-16T08:57:20Z","_id":"21963","department":[{"_id":"SiHi"},{"_id":"PreCl"},{"_id":"GradSch"}],"has_accepted_license":"1","corr_author":"1","abstract":[{"text":"The cerebral cortex consists of immense numbers of neuronal and glial cell-types derived from radial glial progenitor (RGP) cells. How RGPs generate appropriate quantities of distinct cortical cell-types to safeguard a brain of correct size, is not well understood. However, genetic aberration in human, including mutations in PTEN, lead to cortical malformation such as macrocephaly, albeit with unknown etiology. Here we utilized Mosaic Analysis with Double Markers (MADM)-based clonal analysis and single cell phenotyping to decipher the role of Pten in neurogenic and gliogenic RGP lineage progression during cortical ontogeny. While neurogenic RGP lineage progression and projection neuron production was moderately altered in the absence of Pten, cortical astrocyte production was drastically increased. Through genetic epistasis experiments we show that the loss of Pten uncouples astrocyte generation from essential growth factor signaling hubs, funneling into MAPK. Collectively, our results suggest that Pten regulates RGP lineage progression with distinct sequential functions in cortical projection neurogenesis and astrocyte production to ensure the emergence of a correctly-sized cerebral cortex.","lang":"eng"}],"doi":"10.64898/2026.05.01.722191","citation":{"ama":"Miranda O, Contreras X, Pauler F, et al. Pten orchestrates neurogenic radial glia lineage progression and tunes neocortical astrocyte production. <i>bioRxiv</i>. doi:<a href=\"https://doi.org/10.64898/2026.05.01.722191\">10.64898/2026.05.01.722191</a>","short":"O. Miranda, X. Contreras, F. Pauler, A. Davaatseren, N. Amberg, C. Streicher, A. Villalba Requena, A.-M. Heger, C. Marie, B.A. Hassan, T. Rülicke, S. Hippenmeyer, BioRxiv (n.d.).","chicago":"Miranda, Osvaldo, Ximena Contreras, Florian Pauler, Amarbayasgalan Davaatseren, Nicole Amberg, Carmen Streicher, Ana Villalba Requena, et al. “Pten Orchestrates Neurogenic Radial Glia Lineage Progression and Tunes Neocortical Astrocyte Production.” <i>BioRxiv</i>, n.d. <a href=\"https://doi.org/10.64898/2026.05.01.722191\">https://doi.org/10.64898/2026.05.01.722191</a>.","ista":"Miranda O, Contreras X, Pauler F, Davaatseren A, Amberg N, Streicher C, Villalba Requena A, Heger A-M, Marie C, Hassan BA, Rülicke T, Hippenmeyer S. Pten orchestrates neurogenic radial glia lineage progression and tunes neocortical astrocyte production. bioRxiv, <a href=\"https://doi.org/10.64898/2026.05.01.722191\">10.64898/2026.05.01.722191</a>.","ieee":"O. Miranda <i>et al.</i>, “Pten orchestrates neurogenic radial glia lineage progression and tunes neocortical astrocyte production,” <i>bioRxiv</i>. .","apa":"Miranda, O., Contreras, X., Pauler, F., Davaatseren, A., Amberg, N., Streicher, C., … Hippenmeyer, S. (n.d.). Pten orchestrates neurogenic radial glia lineage progression and tunes neocortical astrocyte production. <i>bioRxiv</i>. <a href=\"https://doi.org/10.64898/2026.05.01.722191\">https://doi.org/10.64898/2026.05.01.722191</a>","mla":"Miranda, Osvaldo, et al. “Pten Orchestrates Neurogenic Radial Glia Lineage Progression and Tunes Neocortical Astrocyte Production.” <i>BioRxiv</i>, doi:<a href=\"https://doi.org/10.64898/2026.05.01.722191\">10.64898/2026.05.01.722191</a>."},"article_processing_charge":"No","project":[{"_id":"059F6AB4-7A3F-11EA-A408-12923DDC885E","name":"Stem Cell Modulation in Neural Development and Regeneration/ P05-Molecular Mechanisms of Neural Stem Cell Lineage Progression","grant_number":"F7805"},{"grant_number":"725780","call_identifier":"H2020","name":"Principles of Neural Stem Cell Lineage Progression in Cerebral Cortex Development","_id":"260018B0-B435-11E9-9278-68D0E5697425"}],"language":[{"iso":"eng"}],"month":"05","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","oa_version":"Preprint","main_file_link":[{"open_access":"1","url":"https://doi.org/10.64898/2026.05.01.722191"}]},{"article_number":"105878","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"05","language":[{"iso":"eng"}],"scopus_import":"1","main_file_link":[{"url":"https://doi.org/10.1016/j.geomphys.2026.105878","open_access":"1"}],"oa_version":"Published Version","title":"An easier way to compute 2-cocycles coming from a reduction for semidirect products","ddc":["000"],"date_updated":"2026-06-16T09:23:39Z","_id":"21981","publisher":"Elsevier","external_id":{"arxiv":["2509.16169"]},"corr_author":"1","department":[{"_id":"GradSch"}],"has_accepted_license":"1","article_processing_charge":"Yes (via OA deal)","publication_identifier":{"eissn":["1879-1662"],"issn":["0393-0440"]},"abstract":[{"lang":"eng","text":"For Hamiltonian actions of semidirect products G = FxH, we study 2-cocycles arising from residual Hamiltonian actions of F on Hamiltonian reductions for H. The motivation comes from the study of Teichmüller spaces for surfaces with boundary, which carry Hamiltonian actions of the Virasoro algebra. In this paper, we give a general setup for the problem, and we suggest an easier way to obtain the Gelfand-Fuchs 2-cocycles for Hamiltonian actions on Teichmüller spaces."}],"citation":{"apa":"Goncharov, V. (2026). An easier way to compute 2-cocycles coming from a reduction for semidirect products. <i>Journal of Geometry and Physics</i>. Elsevier. <a href=\"https://doi.org/10.1016/j.geomphys.2026.105878\">https://doi.org/10.1016/j.geomphys.2026.105878</a>","mla":"Goncharov, Viacheslav. “An Easier Way to Compute 2-Cocycles Coming from a Reduction for Semidirect Products.” <i>Journal of Geometry and Physics</i>, vol. 227, 105878, Elsevier, 2026, doi:<a href=\"https://doi.org/10.1016/j.geomphys.2026.105878\">10.1016/j.geomphys.2026.105878</a>.","ista":"Goncharov V. 2026. An easier way to compute 2-cocycles coming from a reduction for semidirect products. Journal of Geometry and Physics. 227, 105878.","ieee":"V. Goncharov, “An easier way to compute 2-cocycles coming from a reduction for semidirect products,” <i>Journal of Geometry and Physics</i>, vol. 227. Elsevier, 2026.","ama":"Goncharov V. An easier way to compute 2-cocycles coming from a reduction for semidirect products. <i>Journal of Geometry and Physics</i>. 2026;227. doi:<a href=\"https://doi.org/10.1016/j.geomphys.2026.105878\">10.1016/j.geomphys.2026.105878</a>","chicago":"Goncharov, Viacheslav. “An Easier Way to Compute 2-Cocycles Coming from a Reduction for Semidirect Products.” <i>Journal of Geometry and Physics</i>. Elsevier, 2026. <a href=\"https://doi.org/10.1016/j.geomphys.2026.105878\">https://doi.org/10.1016/j.geomphys.2026.105878</a>.","short":"V. Goncharov, Journal of Geometry and Physics 227 (2026)."},"doi":"10.1016/j.geomphys.2026.105878","volume":227,"article_type":"original","OA_type":"hybrid","quality_controlled":"1","author":[{"full_name":"Goncharov, Viacheslav","first_name":"Viacheslav","id":"8a0e2993-7114-11f0-b60e-f50e633649d8","last_name":"Goncharov"}],"day":"21","OA_place":"publisher","date_created":"2026-06-10T07:29:13Z","date_published":"2026-05-21T00:00:00Z","oa":1,"PlanS_conform":"1","year":"2026","status":"public","intvolume":"       227","type":"journal_article","fulldoi":"https://doi.org/10.1016/j.geomphys.2026.105878","arxiv":1,"publication_status":"epub_ahead","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"publication":"Journal of Geometry and Physics"},{"title":"Constraining debris input to Oberaletsch Glacier using ensemble-based Lagrangian modelling","_id":"22119","publisher":"European Geosciences Union","ddc":["550"],"date_updated":"2026-07-02T06:42:37Z","has_accepted_license":"1","department":[{"_id":"FrPe"},{"_id":"GradSch"}],"corr_author":"1","file_date_updated":"2026-07-02T06:22:50Z","doi":"10.5194/egusphere-egu26-19367","citation":{"mla":"Muñoz Hermosilla, José M., et al. “Constraining Debris Input to Oberaletsch Glacier Using Ensemble-Based Lagrangian Modelling.” <i>EGU General Assembly 2026</i>, EGU26-19367, European Geosciences Union, 2026, doi:<a href=\"https://doi.org/10.5194/egusphere-egu26-19367\">10.5194/egusphere-egu26-19367</a>.","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 <i>EGU General Assembly 2026</i>. Vienna, Austria &#38; Virtual: European Geosciences Union. <a href=\"https://doi.org/10.5194/egusphere-egu26-19367\">https://doi.org/10.5194/egusphere-egu26-19367</a>","ieee":"J. M. Muñoz Hermosilla <i>et al.</i>, “Constraining debris input to Oberaletsch Glacier using ensemble-based Lagrangian modelling,” in <i>EGU General Assembly 2026</i>, Vienna, Austria &#38; Virtual, 2026.","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.","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 <i>EGU General Assembly 2026</i>. European Geosciences Union, 2026. <a href=\"https://doi.org/10.5194/egusphere-egu26-19367\">https://doi.org/10.5194/egusphere-egu26-19367</a>.","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.","ama":"Muñoz Hermosilla JM, Miles E, McCarthy M, et al. Constraining debris input to Oberaletsch Glacier using ensemble-based Lagrangian modelling. In: <i>EGU General Assembly 2026</i>. European Geosciences Union; 2026. doi:<a href=\"https://doi.org/10.5194/egusphere-egu26-19367\">10.5194/egusphere-egu26-19367</a>"},"article_processing_charge":"No","article_number":"EGU26-19367","month":"07","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"oa_version":"Published Version","oa":1,"date_published":"2026-07-02T00:00:00Z","date_created":"2026-06-22T12:16:50Z","type":"conference_abstract","year":"2026","status":"public","conference":{"location":"Vienna, Austria & Virtual","end_date":"2026-05-08","name":"EGU General Assembly","start_date":"2026-05-03"},"publication":"EGU General Assembly 2026","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"publication_status":"published","fulldoi":"https://doi.org/10.5194/egusphere-egu26-19367","file":[{"creator":"dernst","file_size":284023,"success":1,"content_type":"application/pdf","file_id":"22233","checksum":"2ea3e691cfa53176d0e801b9172842d6","date_updated":"2026-07-02T06:22:50Z","relation":"main_file","file_name":"2026_EGU26_MunozHermosilla.pdf","access_level":"open_access","date_created":"2026-07-02T06:22:50Z"}],"OA_type":"gold","day":"02","author":[{"full_name":"Muñoz Hermosilla, José M","first_name":"José M","id":"e1037a6d-646e-11ef-b402-e0ed9ab0901e","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","full_name":"McCarthy, Michael","first_name":"Michael"},{"last_name":"Melo Velasco","id":"2611dec0-b9c6-11ed-9bea-a81c2b17a549","full_name":"Melo Velasco, Juan Vicente","first_name":"Juan Vicente"},{"first_name":"Florian","full_name":"Hardmeier, Florian","last_name":"Hardmeier"},{"id":"02734268-3e8d-11ef-80a1-cec4a088d004","last_name":"GANTAYAT","first_name":"PRATEEK","full_name":"GANTAYAT, PRATEEK"},{"last_name":"Fontrodona-Bach","id":"f06891fd-9f42-11ee-8632-a20971c43046","first_name":"Adrià","full_name":"Fontrodona-Bach, Adrià"},{"last_name":"Jouvet","full_name":"Jouvet, Guillaume","first_name":"Guillaume"},{"last_name":"Pellicciotti","id":"b28f055a-81ea-11ed-b70c-a9fe7f7b0e70","orcid":"0000-0002-5554-8087","full_name":"Pellicciotti, Francesca","first_name":"Francesca"}],"OA_place":"publisher"},{"OA_place":"publisher","das_tickbox":"0","author":[{"last_name":"Xie","id":"488e236c-6bad-11f0-9831-859175c78e8a","first_name":"Peiyuan","full_name":"Xie, Peiyuan"},{"first_name":"Christian","full_name":"Hafner, Christian","id":"400429CC-F248-11E8-B48F-1D18A9856A87","last_name":"Hafner"},{"last_name":"Wojtan","orcid":"0000-0001-6646-5546","id":"3C61F1D2-F248-11E8-B48F-1D18A9856A87","full_name":"Wojtan, Christopher J","first_name":"Christopher J"}],"day":"03","OA_type":"hybrid","article_type":"original","file":[{"file_name":"2026_TransactionsGraphics_Xie.pdf","date_created":"2026-07-06T06:13:12Z","access_level":"open_access","date_updated":"2026-07-06T06:13:12Z","relation":"main_file","checksum":"7e36e69f377b680a893e65b620b43813","success":1,"content_type":"application/pdf","file_id":"22249","creator":"dernst","file_size":5212838}],"quality_controlled":"1","supplementarymaterial":"no","volume":45,"fulldoi":"https://doi.org/10.1145/3811339","publication_status":"published","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"publication":"ACM Transactions on Graphics","status":"public","year":"2026","PlanS_conform":"1","researchdata_availability":"no","intvolume":"        45","type":"journal_article","issue":"4","date_created":"2026-07-03T21:03:48Z","date_published":"2026-07-03T00:00:00Z","oa":1,"oa_version":"Published Version","month":"07","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"scopus_import":"1","project":[{"grant_number":"101045083","_id":"34bc2376-11ca-11ed-8bc3-9a3b3961a088","name":"Computational Discovery of Numerical Algorithms for Animation and Simulation of Natural Phenomena"}],"article_number":"41","article_processing_charge":"Yes (via OA deal)","publication_identifier":{"issn":["0730-0301"],"eissn":["1557-7368"]},"abstract":[{"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.","lang":"eng"}],"citation":{"chicago":"Xie, Peiyuan, Christian Hafner, and Chris Wojtan. “Fast and Exact Winding Numbers for Triangle Meshes.” <i>ACM Transactions on Graphics</i>. Association for Computing Machinery, 2026. <a href=\"https://doi.org/10.1145/3811339\">https://doi.org/10.1145/3811339</a>.","short":"P. Xie, C. Hafner, C. Wojtan, ACM Transactions on Graphics 45 (2026).","ama":"Xie P, Hafner C, Wojtan C. Fast and exact winding numbers for triangle meshes. <i>ACM Transactions on Graphics</i>. 2026;45(4). doi:<a href=\"https://doi.org/10.1145/3811339\">10.1145/3811339</a>","ieee":"P. Xie, C. Hafner, and C. Wojtan, “Fast and exact winding numbers for triangle meshes,” <i>ACM Transactions on Graphics</i>, 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.","mla":"Xie, Peiyuan, et al. “Fast and Exact Winding Numbers for Triangle Meshes.” <i>ACM Transactions on Graphics</i>, vol. 45, no. 4, 41, Association for Computing Machinery, 2026, doi:<a href=\"https://doi.org/10.1145/3811339\">10.1145/3811339</a>.","apa":"Xie, P., Hafner, C., &#38; Wojtan, C. (2026). Fast and exact winding numbers for triangle meshes. <i>ACM Transactions on Graphics</i>. Association for Computing Machinery. <a href=\"https://doi.org/10.1145/3811339\">https://doi.org/10.1145/3811339</a>"},"file_date_updated":"2026-07-06T06:13:12Z","doi":"10.1145/3811339","corr_author":"1","department":[{"_id":"GradSch"},{"_id":"ChWo"}],"has_accepted_license":"1","ddc":["000"],"date_updated":"2026-07-06T06:14:18Z","_id":"22241","publisher":"Association for Computing Machinery","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).","title":"Fast and exact winding numbers for triangle meshes"},{"project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","grant_number":"101076224"}],"article_number":"A147","oa_version":"Published Version","language":[{"iso":"eng"}],"month":"01","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","scopus_import":"1","publisher":"EDP Sciences","_id":"21045","ddc":["520"],"date_updated":"2026-07-08T06:38:23Z","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.","external_id":{"arxiv":["2505.09542"]},"title":"A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth","article_processing_charge":"No","citation":{"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. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202555596\">https://doi.org/10.1051/0004-6361/202555596</a>","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.” <i>Astronomy &#38; Astrophysics</i>, vol. 705, A147, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202555596\">10.1051/0004-6361/202555596</a>.","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. <i>Astronomy &#38; Astrophysics</i>. 2026;705. doi:<a href=\"https://doi.org/10.1051/0004-6361/202555596\">10.1051/0004-6361/202555596</a>","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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202555596\">https://doi.org/10.1051/0004-6361/202555596</a>.","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 &#38; Astrophysics 705 (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 &#38; Astrophysics. 705, A147.","ieee":"A. Torralba Torregrosa <i>et al.</i>, “A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth,” <i>Astronomy &#38; Astrophysics</i>, vol. 705. EDP Sciences, 2026."},"doi":"10.1051/0004-6361/202555596","file_date_updated":"2026-02-16T07:35:03Z","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"}],"corr_author":"1","has_accepted_license":"1","department":[{"_id":"JoMa"},{"_id":"GradSch"}],"article_type":"original","OA_type":"diamond","quality_controlled":"1","file":[{"success":1,"file_id":"21224","content_type":"application/pdf","creator":"dernst","file_size":2259914,"file_name":"2026_AstronomyAstrophysics_Torralba.pdf","date_created":"2026-02-16T07:35:03Z","access_level":"open_access","relation":"main_file","date_updated":"2026-02-16T07:35:03Z","checksum":"3782e03bc0843438aae8487f6af779c5"}],"volume":705,"OA_place":"publisher","das_tickbox":"1","author":[{"orcid":"0000-0001-5586-6950","last_name":"Torralba Torregrosa","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto","first_name":"Alberto"},{"first_name":"Jorryt J","full_name":"Matthee, Jorryt J","last_name":"Matthee","orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720"},{"last_name":"Pezzulli","first_name":"Gabriele","full_name":"Pezzulli, Gabriele"},{"last_name":"Urrutia","full_name":"Urrutia, Tanya","first_name":"Tanya"},{"last_name":"Gronke","full_name":"Gronke, Max","first_name":"Max"},{"first_name":"Sara","full_name":"Mascia, Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","last_name":"Mascia"},{"first_name":"Francesco","full_name":"D’Eugenio, Francesco","last_name":"D’Eugenio"},{"last_name":"Di Cesare","id":"2d002343-372f-11ef-98ec-a164d20427cb","full_name":"Di Cesare, Claudia","first_name":"Claudia"},{"last_name":"Eilers","full_name":"Eilers, Anna Christina","first_name":"Anna Christina"},{"last_name":"Greene","first_name":"Jenny E.","full_name":"Greene, Jenny E."},{"full_name":"Iani, Edoardo","first_name":"Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","last_name":"Iani","orcid":"0000-0001-8386-3546"},{"first_name":"Yuzo","full_name":"Ishikawa, Yuzo","last_name":"Ishikawa"},{"first_name":"Ruari","full_name":"Mackenzie, Ruari","last_name":"Mackenzie"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"id":"aa14a535-50c9-11ef-b52e-e0c373d10148","last_name":"Navarrete","first_name":"Benjamín","full_name":"Navarrete, Benjamín"},{"full_name":"Kotiwale, Gauri","first_name":"Gauri","last_name":"Kotiwale","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875"}],"day":"14","intvolume":"       705","PlanS_conform":"1","status":"public","year":"2026","type":"journal_article","date_created":"2026-01-25T23:01:41Z","oa":1,"date_published":"2026-01-14T00:00:00Z","publication_status":"published","arxiv":1,"fulldoi":"https://doi.org/10.1051/0004-6361/202555596","publication":"Astronomy & Astrophysics","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"}},{"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"publication":"Astronomy & Astrophysics","fulldoi":"https://doi.org/10.1051/0004-6361/202558023","arxiv":1,"publication_status":"published","type":"journal_article","year":"2026","PlanS_conform":"1","status":"public","intvolume":"       707","date_published":"2026-03-01T00:00:00Z","oa":1,"date_created":"2026-04-05T22:01:32Z","das_tickbox":"1","OA_place":"publisher","day":"01","author":[{"id":"662f1873-cab4-11f0-a719-8087d302868d","last_name":"Liagre","full_name":"Liagre, Bastien Raymond Bernard","first_name":"Bastien Raymond Bernard"},{"id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","last_name":"Desai","first_name":"Aayush A","full_name":"Desai, Aayush A"},{"id":"f1497a1a-72ef-11ef-b75a-fd877bbf6e8c","last_name":"Einramhof","first_name":"Lukas","full_name":"Einramhof, Lukas"},{"orcid":"0000-0003-0142-4000","id":"d9edb345-f866-11ec-9b37-d119b5234501","last_name":"Bugnet","first_name":"Lisa Annabelle","full_name":"Bugnet, Lisa Annabelle"}],"file":[{"file_size":12287607,"creator":"dernst","file_id":"21664","content_type":"application/pdf","success":1,"checksum":"560cac19dc70184626b85e71a26ee22e","date_updated":"2026-04-07T09:00:50Z","relation":"main_file","access_level":"open_access","date_created":"2026-04-07T09:00:50Z","file_name":"2026_AstronomyAstrophysics_Liagre.pdf"}],"quality_controlled":"1","article_type":"original","OA_type":"diamond","volume":707,"publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"abstract":[{"lang":"eng","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."}],"doi":"10.1051/0004-6361/202558023","citation":{"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,” <i>Astronomy &#38; Astrophysics</i>, vol. 707. EDP Sciences, 2026.","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 &#38; Astrophysics. 707, A321.","short":"B.R.B. Liagre, A.A. Desai, L. Einramhof, L.A. Bugnet, Astronomy &#38; 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.” <i>Astronomy &#38; Astrophysics</i>. EDP Sciences, 2026. <a href=\"https://doi.org/10.1051/0004-6361/202558023\">https://doi.org/10.1051/0004-6361/202558023</a>.","ama":"Liagre BRB, Desai AA, Einramhof L, Bugnet LA. Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. <i>Astronomy &#38; Astrophysics</i>. 2026;707. doi:<a href=\"https://doi.org/10.1051/0004-6361/202558023\">10.1051/0004-6361/202558023</a>","mla":"Liagre, Bastien Raymond Bernard, et al. “Near-Degeneracy Effects in Quadrupolar Mixed Modes: From an Asymptotic Description to Data Fitting.” <i>Astronomy &#38; Astrophysics</i>, vol. 707, A321, EDP Sciences, 2026, doi:<a href=\"https://doi.org/10.1051/0004-6361/202558023\">10.1051/0004-6361/202558023</a>.","apa":"Liagre, B. R. B., Desai, A. A., Einramhof, L., &#38; Bugnet, L. A. (2026). Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting. <i>Astronomy &#38; Astrophysics</i>. EDP Sciences. <a href=\"https://doi.org/10.1051/0004-6361/202558023\">https://doi.org/10.1051/0004-6361/202558023</a>"},"file_date_updated":"2026-04-07T09:00:50Z","article_processing_charge":"No","DOAJ_listed":"1","department":[{"_id":"LiBu"},{"_id":"IlCa"},{"_id":"GradSch"}],"has_accepted_license":"1","corr_author":"1","external_id":{"arxiv":["2511.05314 "]},"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).","ddc":["520"],"date_updated":"2026-07-08T06:39:05Z","_id":"21658","publisher":"EDP Sciences","title":"Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting","oa_version":"Published Version","scopus_import":"1","language":[{"iso":"eng"}],"month":"03","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","article_number":"A321"},{"has_accepted_license":"1","department":[{"_id":"JoMa"},{"_id":"IlCa"},{"_id":"GradSch"}],"corr_author":"1","citation":{"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.” <i>The Astrophysical Journal Letters</i>, vol. 1005, no. 2, L37, IOP Publishing, 2026, doi:<a href=\"https://doi.org/10.3847/2041-8213/ae7bfd\">10.3847/2041-8213/ae7bfd</a>.","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. <i>The Astrophysical Journal Letters</i>. IOP Publishing. <a href=\"https://doi.org/10.3847/2041-8213/ae7bfd\">https://doi.org/10.3847/2041-8213/ae7bfd</a>","ieee":"A. Torralba Torregrosa <i>et al.</i>, “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,” <i>The Astrophysical Journal Letters</i>, vol. 1005, no. 2. IOP Publishing, 2026.","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.","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).","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.” <i>The Astrophysical Journal Letters</i>. IOP Publishing, 2026. <a href=\"https://doi.org/10.3847/2041-8213/ae7bfd\">https://doi.org/10.3847/2041-8213/ae7bfd</a>.","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. <i>The Astrophysical Journal Letters</i>. 2026;1005(2). doi:<a href=\"https://doi.org/10.3847/2041-8213/ae7bfd\">10.3847/2041-8213/ae7bfd</a>"},"doi":"10.3847/2041-8213/ae7bfd","file_date_updated":"2026-07-13T07:46:22Z","publication_identifier":{"issn":["2041-8205"],"eissn":["2041-8213"]},"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"}],"article_processing_charge":"Yes","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","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).","external_id":{"arxiv":["2603.28335"]},"_id":"22263","publisher":"IOP Publishing","date_updated":"2026-07-13T08:08:41Z","ddc":["520"],"scopus_import":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"month":"07","oa_version":"Published Version","article_number":"L37","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).","project":[{"grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization"}],"publication":"The Astrophysical Journal Letters","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"arxiv":1,"publication_status":"published","fulldoi":"https://doi.org/10.3847/2041-8213/ae7bfd","oa":1,"date_published":"2026-07-10T00:00:00Z","date_created":"2026-07-12T22:02:17Z","issue":"2","type":"journal_article","intvolume":"      1005","year":"2026","researchdata_availability":"yes","status":"public","day":"10","author":[{"full_name":"Torralba Torregrosa, Alberto","first_name":"Alberto","orcid":"0000-0001-5586-6950","id":"018f0249-0e87-11f0-b167-cbce08fbd541","last_name":"Torralba Torregrosa"},{"orcid":"0000-0003-2871-127X","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","full_name":"Matthee, Jorryt J","first_name":"Jorryt J"},{"last_name":"Weibel","full_name":"Weibel, Andrea","first_name":"Andrea"},{"first_name":"Rohan P.","full_name":"Naidu, Rohan P.","last_name":"Naidu"},{"full_name":"Ma, Yilun","first_name":"Yilun","last_name":"Ma"},{"full_name":"Cloonan, Aidan P.","first_name":"Aidan P.","last_name":"Cloonan"},{"last_name":"Desai","id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","full_name":"Desai, Aayush A","first_name":"Aayush A"},{"last_name":"De Graaff","first_name":"Anna","full_name":"De Graaff, Anna"},{"full_name":"Greene, Jenny E.","first_name":"Jenny E.","last_name":"Greene"},{"last_name":"Jespersen","full_name":"Jespersen, Christian Kragh","first_name":"Christian Kragh"},{"last_name":"Kramarenko","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","orcid":"0000-0001-5346-6048","full_name":"Kramarenko, Ivan","first_name":"Ivan"},{"id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","last_name":"Mascia","first_name":"Sara","full_name":"Mascia, Sara"},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"last_name":"Sun","full_name":"Sun, Wendy Q.","first_name":"Wendy Q."},{"first_name":"Christina C.","full_name":"Williams, Christina C.","last_name":"Williams"}],"das_tickbox":"1","OA_place":"publisher","volume":1005,"supplementarymaterial":"yes","quality_controlled":"1","file":[{"date_updated":"2026-07-13T07:46:22Z","relation":"main_file","checksum":"7600db260d799ddea45cf3bd01effe41","file_name":"2026_AstrophysicalJourLetters_Torralba.pdf","date_created":"2026-07-13T07:46:22Z","access_level":"open_access","creator":"dernst","file_size":5419071,"success":1,"content_type":"application/pdf","file_id":"22274"}],"article_type":"original","OA_type":"gold"},{"main_file_link":[{"url":"https://doi.org/10.1038/s41564-026-02403-6","open_access":"1"}],"oa_version":"Published Version","month":"07","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"scopus_import":"1","dataavailabilitystatement":"The data, plasmids and strains that support the findings of this study are available from the corresponding authors by request. Representative tomograms are deposited in EMDB: EMD-27479 (wild-type), EMD-53351 (∆ponB), EMD-53357(∆lpoB) and EMD-53363 (∆ponA). Corresponding raw movie frames and stacks of tilt series are deposited as EMPIAR-11090 (wild type), EMPIAR-13502 (∆ponB), EMPIAR-13513 (∆lpoB) and EMPIAR-13512 (∆ponA), and will be released upon publication. Other data related to this manuscript (for example, AFM, light microscopy, growth curves and so on) can be found on Zenodo at https://doi.org/10.5281/zenodo.20841819 (ref. 101). Source data are provided with this paper. Scripts used in this study were deposited on GitHub at https://github.com/NavarroVettiger/Navarro-et-al_2022 and https://github.com/virlyananda/EM-ImageProcessing.","article_processing_charge":"Yes (in subscription journal)","abstract":[{"lang":"eng","text":"The divisome apparatus synthesizes septal peptidoglycan (PG) during bacterial division. In Escherichia coli, the class A penicillin-binding protein (aPBP) called PBP1b has been implicated in division, but its role in the process has remained unclear. Here we show using in situ cryo-electron tomography, genetics and other imaging methods that PBP1b is required to produce a wedge-like density of PG at the division site and that loss of this structure weakens the division site, making it hypersusceptible to osmotic lysis. Surprisingly, the activator LpoB needed for general PBP1b function was not required for its role in division. Of the two PBP1b isoforms produced in cells, we show that the one with an extended cytoplasmic N terminus localizes to and functions at the division site, probably via recruitment by the FtsA component of the divisome. The conservation of aPBPs with extended cytoplasmic N termini suggests that other Gram-negative bacteria may use similar mechanisms for division site reinforcement."}],"publication_identifier":{"eissn":["2058-5276"]},"citation":{"apa":"Navarro, P. P., Vettiger, A., Hajdu, R., Ananda, V. Y., López-Tavares, A., Schmid, E. W., … Bernhardt, T. G. (2026). The penicillin-binding protein PBP1b fortifies the Escherichia coli division site against osmotic rupture. <i>Nature Microbiology</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41564-026-02403-6\">https://doi.org/10.1038/s41564-026-02403-6</a>","mla":"Navarro, Paula P., et al. “The Penicillin-Binding Protein PBP1b Fortifies the Escherichia Coli Division Site against Osmotic Rupture.” <i>Nature Microbiology</i>, Springer Nature, 2026, doi:<a href=\"https://doi.org/10.1038/s41564-026-02403-6\">10.1038/s41564-026-02403-6</a>.","ama":"Navarro PP, Vettiger A, Hajdu R, et al. The penicillin-binding protein PBP1b fortifies the Escherichia coli division site against osmotic rupture. <i>Nature Microbiology</i>. 2026. doi:<a href=\"https://doi.org/10.1038/s41564-026-02403-6\">10.1038/s41564-026-02403-6</a>","short":"P.P. Navarro, A. Vettiger, R. Hajdu, V.Y. Ananda, A. López-Tavares, E.W. Schmid, J.C. Walter, M. Loose, L.H. Chao, T.G. Bernhardt, Nature Microbiology (2026).","chicago":"Navarro, Paula P., Andrea Vettiger, Roman Hajdu, Virly Y. Ananda, Alejandro López-Tavares, Ernst W. Schmid, Johannes C. Walter, Martin Loose, Luke H. Chao, and Thomas G. Bernhardt. “The Penicillin-Binding Protein PBP1b Fortifies the Escherichia Coli Division Site against Osmotic Rupture.” <i>Nature Microbiology</i>. Springer Nature, 2026. <a href=\"https://doi.org/10.1038/s41564-026-02403-6\">https://doi.org/10.1038/s41564-026-02403-6</a>.","ista":"Navarro PP, Vettiger A, Hajdu R, Ananda VY, López-Tavares A, Schmid EW, Walter JC, Loose M, Chao LH, Bernhardt TG. 2026. The penicillin-binding protein PBP1b fortifies the Escherichia coli division site against osmotic rupture. Nature Microbiology.","ieee":"P. P. Navarro <i>et al.</i>, “The penicillin-binding protein PBP1b fortifies the Escherichia coli division site against osmotic rupture,” <i>Nature Microbiology</i>. Springer Nature, 2026."},"doi":"10.1038/s41564-026-02403-6","department":[{"_id":"MaLo"},{"_id":"GradSch"}],"has_accepted_license":"1","date_updated":"2026-07-13T09:22:49Z","ddc":["570"],"_id":"22269","publisher":"Springer Nature","external_id":{"pmid":["42399561"]},"acknowledgement":"We thank all members of the Bernhardt, Rudner, Navarro and Vettiger Laboratories for support and helpful conversations. We thank C. Genoud, J. Daraspe, A. Mucciolo and D. de Bellis at the Electron Microscopy Facility of the University of Lausanne and E. Jeanvoine for providing access to workstations for cryo-ET image processing; S. Sterling, C. Borsa, J. Podgorski, P. Vinh Dip, E. Brignole and A. Osherov at the MIT.nano cryo-EM facility, K. Song and C. Xu at the University of Massachusetts cryo-EM facility, and R. Walsh and Z. Li at the cryo-EM at Harvard Medical School facility for providing access to the cryo-EM microscopes and for all their help, advice and maintenance of cryo-EM equipment. AFM was performed at the Harvard University Center for Nanoscale Systems (CNS), a member of the National Nanotechnology Coordinated Infrastructure Network (NNCI), which is supported by the National Science Foundation under NSF award no. ECCS-2025158. We thank N. S. Colella for excellent advice on AFM data acquisition and analysis; the MicRoN imaging core at Harvard Medical School for excellent advice on live cell imaging and maintenance of fluorescence microscopes; B. Krautz for creating the cartoon illustrations (www.sciencecommunicated.com); and L. Miles and R. Aeschimann for assistance with strain construction. A.V. was supported by an EMBO long-term postdoctoral fellowship ALTF_89-2019, the Swiss National Science Foundation (SNSF) Postdoc.Mobility fellowship P500PB_203143. P.P.N. was a recipient of early postdoc.mobility and postdoc.mobility fellowships (P2BSP3_188112 and P400PB_199252). This work was also supported by funding from the National Institutes of Health (R35GM142553 to L.H.C. and R01AI083365 to T.G.B.), investigator funds from the Howard Hughes Medical Institute (T.G.B.), an SNSF project grant (320030-236243 to A.V.), an SNSF Starting Grant (TMSGI3_218251 to P.P.N.), an SNSF Project grant (320030-236069 to P.P.N), an SNSF SPARK grant (CRSK-3_237167 to P.P.N.), cryo-EM funds from the Faculty of Biology and Medicine at University of Lausanne to P.P.N. and the Foundation Pierre Mercier pour la Science (to P.P.N.).","title":"The penicillin-binding protein PBP1b fortifies the Escherichia coli division site against osmotic rupture","OA_place":"publisher","das_tickbox":"1","author":[{"last_name":"Navarro","first_name":"Paula P.","full_name":"Navarro, Paula P."},{"last_name":"Vettiger","first_name":"Andrea","full_name":"Vettiger, Andrea"},{"full_name":"Hajdu, Roman","first_name":"Roman","id":"ffab949d-133f-11ed-8f02-94de21ace503","last_name":"Hajdu"},{"last_name":"Ananda","full_name":"Ananda, Virly Y.","first_name":"Virly Y."},{"first_name":"Alejandro","full_name":"López-Tavares, Alejandro","last_name":"López-Tavares"},{"first_name":"Ernst W.","full_name":"Schmid, Ernst W.","last_name":"Schmid"},{"last_name":"Walter","full_name":"Walter, Johannes C.","first_name":"Johannes C."},{"last_name":"Loose","id":"462D4284-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0001-7309-9724","full_name":"Loose, Martin","first_name":"Martin"},{"last_name":"Chao","first_name":"Luke H.","full_name":"Chao, Luke H."},{"last_name":"Bernhardt","full_name":"Bernhardt, Thomas G.","first_name":"Thomas G."}],"day":"03","pmid":1,"article_type":"original","OA_type":"hybrid","quality_controlled":"1","supplementarymaterial":"yes","fulldoi":"https://doi.org/10.1038/s41564-026-02403-6","publication_status":"epub_ahead","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"publication":"Nature Microbiology","researchdata_availability":"yes","year":"2026","status":"public","type":"journal_article","date_created":"2026-07-12T22:02:19Z","date_published":"2026-07-03T00:00:00Z","oa":1},{"issue":"6","type":"journal_article","intvolume":"        67","researchdata_availability":"not applicable","year":"2026","status":"public","oa":1,"date_published":"2026-06-01T00:00:00Z","date_created":"2026-07-13T09:45:09Z","publication":"Journal of Mathematical Physics","arxiv":1,"publication_status":"published","fulldoi":"https://doi.org/10.1063/5.0325354","quality_controlled":"1","article_type":"original","OA_type":"green","volume":67,"supplementarymaterial":"not applicable","das_tickbox":"1","OA_place":"repository","day":"01","author":[{"first_name":"Michiel","full_name":"De Wilde, Michiel","id":"bebf1407-6635-11f0-9fef-9b7e2dd151d0","last_name":"De Wilde"},{"full_name":"Seiringer, Robert","first_name":"Robert","id":"4AFD0470-F248-11E8-B48F-1D18A9856A87","last_name":"Seiringer","orcid":"0000-0002-6781-0521"}],"acknowledgement":"We are grateful to Rupert Frank and Jakob Yngvason for helpful discussions and suggestions.","external_id":{"arxiv":["2601.22883"]},"_id":"22292","publisher":"AIP Publishing","date_updated":"2026-07-13T12:20:59Z","title":"Arbitrary harmonic functions as Bose–Einstein condensates","doi":"10.1063/5.0325354","citation":{"ista":"De Wilde M, Seiringer R. 2026. Arbitrary harmonic functions as Bose–Einstein condensates. Journal of Mathematical Physics. 67(6), 061901.","ieee":"M. De Wilde and R. Seiringer, “Arbitrary harmonic functions as Bose–Einstein condensates,” <i>Journal of Mathematical Physics</i>, vol. 67, no. 6. AIP Publishing, 2026.","ama":"De Wilde M, Seiringer R. Arbitrary harmonic functions as Bose–Einstein condensates. <i>Journal of Mathematical Physics</i>. 2026;67(6). doi:<a href=\"https://doi.org/10.1063/5.0325354\">10.1063/5.0325354</a>","short":"M. De Wilde, R. Seiringer, Journal of Mathematical Physics 67 (2026).","chicago":"De Wilde, Michiel, and Robert Seiringer. “Arbitrary Harmonic Functions as Bose–Einstein Condensates.” <i>Journal of Mathematical Physics</i>. AIP Publishing, 2026. <a href=\"https://doi.org/10.1063/5.0325354\">https://doi.org/10.1063/5.0325354</a>.","apa":"De Wilde, M., &#38; Seiringer, R. (2026). Arbitrary harmonic functions as Bose–Einstein condensates. <i>Journal of Mathematical Physics</i>. AIP Publishing. <a href=\"https://doi.org/10.1063/5.0325354\">https://doi.org/10.1063/5.0325354</a>","mla":"De Wilde, Michiel, and Robert Seiringer. “Arbitrary Harmonic Functions as Bose–Einstein Condensates.” <i>Journal of Mathematical Physics</i>, vol. 67, no. 6, 061901, AIP Publishing, 2026, doi:<a href=\"https://doi.org/10.1063/5.0325354\">10.1063/5.0325354</a>."},"publication_identifier":{"issn":["0022-2488"],"eissn":["1089-7658"]},"abstract":[{"lang":"eng","text":"We show that a suitable choice of boundary conditions for the Laplacian allows for the appearance of an arbitrary number of condensates, described by arbitrary harmonic functions, in the thermodynamic limit of an ideal Bose gas."}],"article_processing_charge":"No","department":[{"_id":"RoSe"},{"_id":"GradSch"}],"corr_author":"1","article_number":"061901","dataavailabilitystatement":"Data sharing is not applicable to this article as no new data were created or analyzed in this study.","oa_version":"Preprint","main_file_link":[{"open_access":"1","url":"https://doi.org/10.48550/arXiv.2601.22883"}],"scopus_import":"1","month":"06","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}]},{"supplementarymaterial":"yes","OA_type":"hybrid","article_type":"original","pmid":1,"quality_controlled":"1","author":[{"last_name":"Smoljan","id":"cced8a85-223e-11ed-af04-b0596c55053b","first_name":"Adrijana","full_name":"Smoljan, Adrijana"},{"first_name":"Sarah","full_name":"Koutnik‐Abele, Sarah","last_name":"Koutnik‐Abele"},{"full_name":"Vladimirtsev, Dmitrii","first_name":"Dmitrii","last_name":"Vladimirtsev","id":"60466724-5355-11ee-ae5a-fa55e8f99c3d"},{"last_name":"Klíma","first_name":"Petr","full_name":"Klíma, Petr"},{"last_name":"Bírošíková","first_name":"Anita","full_name":"Bírošíková, Anita"},{"full_name":"Zhang, Yuzhou","first_name":"Yuzhou","last_name":"Zhang","id":"3B6137F2-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0003-2627-6956"},{"first_name":"Jack","full_name":"Merrin, Jack","id":"4515C308-F248-11E8-B48F-1D18A9856A87","last_name":"Merrin","orcid":"0000-0001-5145-4609"},{"id":"37e65def-d415-11eb-ae59-a7b67be103db","last_name":"Schuster","full_name":"Schuster, Maximilian","first_name":"Maximilian"},{"full_name":"Kurtović, Katarina","first_name":"Katarina","last_name":"Kurtović"},{"first_name":"Ulrich Z.","full_name":"Hammes, Ulrich Z.","last_name":"Hammes"},{"full_name":"Petrášek, Jan","first_name":"Jan","last_name":"Petrášek"},{"first_name":"Jiří","full_name":"Friml, Jiří","last_name":"Friml","id":"4159519E-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-8302-7596"}],"acknowledged_ssus":[{"_id":"Bio"},{"_id":"NanoFab"}],"day":"10","OA_place":"publisher","das_tickbox":"0","date_created":"2026-07-13T10:44:55Z","oa":1,"date_published":"2026-06-10T00:00:00Z","researchdata_availability":"no","PlanS_conform":"1","year":"2026","status":"public","type":"journal_article","publication_status":"epub_ahead","fulldoi":"https://doi.org/10.1111/jipb.70309","publication":"Journal of Integrative Plant Biology","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"article_number":"jipb.70309","project":[{"name":"Cyclic nucleotides as second messengers in plants","_id":"8f347782-16d5-11f0-9cad-8c19706ee739","grant_number":"101142681"},{"grant_number":"I06123","name":"Peptide receptors for auxin canalization in Arabidopsis","_id":"bd76d395-d553-11ed-ba76-f678c14f9033"},{"grant_number":"P37051","name":"Guanylate cyclase activity of TIR1/AFBs auxin receptors","_id":"7bcece63-9f16-11ee-852c-ae94e099eeb6"}],"language":[{"iso":"eng"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"06","scopus_import":"1","main_file_link":[{"url":"https://doi.org/10.1111/jipb.70309","open_access":"1"}],"oa_version":"Published Version","title":"Auxin response and PIN‐mediated transport in chlorophyte algae","_id":"22301","publisher":"Wiley","date_updated":"2026-07-13T14:26:31Z","ddc":["580"],"acknowledgement":"Research in the Friml group was supported by the European Research Council (ERC) under grant agreement No. 101142681 (CYNIPS), and by the Austrian Science Fund (FWF) through projects I 6123-B and P 37051-B. A DOC Fellowship from the Austrian Academy of Sciences (ÖAW; PR.C0102.1.F.1023.A.2) provided additional support. Work was partly supported by the Deutsche Forschungsgemeinschaft (DFG, German Research Foundation) under grant HA 3468/8-1. We thank the Imaging and Optics Facility (IOF) at the Institute of Science and Technology Austria (ISTA) for support with confocal imaging, and the Nanofabrication Facility at ISTA for assistance with microfluidic device fabrication. We also acknowledge the microscopy service of IFIEB CAS, supported by MEYS CR (LM2023050 Czech-BioImaging). Open Access funding provided by Institute of Science and Technology Austria.","external_id":{"pmid":["42271607"]},"corr_author":"1","has_accepted_license":"1","department":[{"_id":"JiFr"},{"_id":"GradSch"},{"_id":"NanoFab"},{"_id":"Bio"}],"article_processing_charge":"Yes (via OA deal)","doi":"10.1111/jipb.70309","citation":{"mla":"Smoljan, Adrijana, et al. “Auxin Response and PIN‐mediated Transport in Chlorophyte Algae.” <i>Journal of Integrative Plant Biology</i>, jipb. 70309, Wiley, 2026, doi:<a href=\"https://doi.org/10.1111/jipb.70309\">10.1111/jipb.70309</a>.","apa":"Smoljan, A., Koutnik‐Abele, S., Vladimirtsev, D., Klíma, P., Bírošíková, A., Zhang, Y., … Friml, J. (2026). Auxin response and PIN‐mediated transport in chlorophyte algae. <i>Journal of Integrative Plant Biology</i>. Wiley. <a href=\"https://doi.org/10.1111/jipb.70309\">https://doi.org/10.1111/jipb.70309</a>","ieee":"A. Smoljan <i>et al.</i>, “Auxin response and PIN‐mediated transport in chlorophyte algae,” <i>Journal of Integrative Plant Biology</i>. Wiley, 2026.","ista":"Smoljan A, Koutnik‐Abele S, Vladimirtsev D, Klíma P, Bírošíková A, Zhang Y, Merrin J, Schuster M, Kurtović K, Hammes UZ, Petrášek J, Friml J. 2026. Auxin response and PIN‐mediated transport in chlorophyte algae. Journal of Integrative Plant Biology., jipb. 70309.","chicago":"Smoljan, Adrijana, Sarah Koutnik‐Abele, Dmitrii Vladimirtsev, Petr Klíma, Anita Bírošíková, Yuzhou Zhang, Jack Merrin, et al. “Auxin Response and PIN‐mediated Transport in Chlorophyte Algae.” <i>Journal of Integrative Plant Biology</i>. Wiley, 2026. <a href=\"https://doi.org/10.1111/jipb.70309\">https://doi.org/10.1111/jipb.70309</a>.","short":"A. Smoljan, S. Koutnik‐Abele, D. Vladimirtsev, P. Klíma, A. Bírošíková, Y. Zhang, J. Merrin, M. Schuster, K. Kurtović, U.Z. Hammes, J. Petrášek, J. Friml, Journal of Integrative Plant Biology (2026).","ama":"Smoljan A, Koutnik‐Abele S, Vladimirtsev D, et al. Auxin response and PIN‐mediated transport in chlorophyte algae. <i>Journal of Integrative Plant Biology</i>. 2026. doi:<a href=\"https://doi.org/10.1111/jipb.70309\">10.1111/jipb.70309</a>"},"publication_identifier":{"issn":["1672-9072"],"eissn":["1744-7909"]},"abstract":[{"lang":"eng","text":"Auxin, primarily indole-3-acetic acid (IAA), is a central regulator of growth and development in land plants, but its physiological role in chlorophyte algae remains unclear. Here, we show that exogenous IAA modulates growth in Chlorella sorokiniana, Chlorella variabilis, and Chlamydomonas reinhardtii in a concentration-dependent manner. Low IAA concentrations promoted growth by accelerating the onset of cell division without affecting cell size, whereas higher concentrations inhibited proliferation. Radiotracer assays showed that all three species take up and release IAA across the plasma membrane through a combination of passive diffusion and energy-dependent, saturable processes. Competition by excess unlabeled natural and synthetic auxins further supported the presence of carrier-mediated transport with broad substrate recognition. Phylogenetic analyses identified potential PIN-like auxin exporters in chlorophytes and other non-plant eukaryotes, and structural modeling supported conservation of the overall PIN fold and predicted auxin-binding residues. However, functional assays in Xenopus laevis oocytes, tobacco BY-2 cultured cells, and Arabidopsis thaliana did not support a role for these proteins in directional auxin export. Instead, non-plant PIN homologs localized predominantly to the endoplasmic reticulum and showed limited or no transport activity in heterologous systems. Together, these findings indicate that auxin responsiveness and basic cellular auxin transport predate canonical PIN-mediated directional auxin export, which appears to be a later innovation of the streptophyte lineage."}]},{"month":"06","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","language":[{"iso":"eng"}],"oa_version":"Published Version","project":[{"_id":"34bc2376-11ca-11ed-8bc3-9a3b3961a088","name":"Computational Discovery of Numerical Algorithms for Animation and Simulation of Natural Phenomena","grant_number":"101045083"}],"corr_author":"1","has_accepted_license":"1","department":[{"_id":"ChWo"},{"_id":"GradSch"}],"article_processing_charge":"Yes (via OA deal)","file_date_updated":"2026-06-23T09:07:22Z","citation":{"ama":"Wei Z, Hafner C, Kalinov A, Synak P, Wojtan C. Circles of confidence for multi-label geometry completion. In: <i>Computer Graphics Forum</i>. Vol 45. Wiley. doi:<a href=\"https://doi.org/10.1111/cgf.70516\">10.1111/cgf.70516</a>","short":"Z. Wei, C. Hafner, A. Kalinov, P. Synak, C. Wojtan, in:, Computer Graphics Forum, Wiley, n.d.","chicago":"Wei, Ziyu , Christian Hafner, Aleksei Kalinov, Peter Synak, and Chris Wojtan. “Circles of Confidence for Multi-Label Geometry Completion.” In <i>Computer Graphics Forum</i>, Vol. 45. Wiley, n.d. <a href=\"https://doi.org/10.1111/cgf.70516\">https://doi.org/10.1111/cgf.70516</a>.","ista":"Wei Z, Hafner C, Kalinov A, Synak P, Wojtan C. Circles of confidence for multi-label geometry completion. Computer Graphics Forum. Eurographics: Symposium on Geometry Processing vol. 45.","ieee":"Z. Wei, C. Hafner, A. Kalinov, P. Synak, and C. Wojtan, “Circles of confidence for multi-label geometry completion,” in <i>Computer Graphics Forum</i>, Bern, Switzerland, vol. 45, no. 5.","apa":"Wei, Z., Hafner, C., Kalinov, A., Synak, P., &#38; Wojtan, C. (n.d.). Circles of confidence for multi-label geometry completion. In <i>Computer Graphics Forum</i> (Vol. 45). Bern, Switzerland: Wiley. <a href=\"https://doi.org/10.1111/cgf.70516\">https://doi.org/10.1111/cgf.70516</a>","mla":"Wei, Ziyu, et al. “Circles of Confidence for Multi-Label Geometry Completion.” <i>Computer Graphics Forum</i>, vol. 45, no. 5, Wiley, doi:<a href=\"https://doi.org/10.1111/cgf.70516\">10.1111/cgf.70516</a>."},"doi":"10.1111/cgf.70516","abstract":[{"text":"Inside–outside classification is widely used for geometry processing tasks such as surface reconstruction, geometry completion,\r\nand calculating signed distance fields. We introduce a new integral formulation of this problem, which assigns confidence\r\nscores that points are inside or outside, given incomplete boundary geometry. Even though our geometric construction does\r\nnot appear in previous work, we show that it is unexpectedly linked to both the well-established generalized winding number\r\n(GWN) and pseudonormal methods for geometry completion, and it provably reduces to either one of them for specific values\r\nof a control parameter. The results obtained with our method frequently outperform screened Poisson surface reconstruction\r\n(PSR), GWN, and the pseudonormal method in terms of quality, and are at least on par with them on all of our examples. Unlike\r\nthese methods, our algorithm naturally extends to the multi-label setting, in which regions with an arbitrary number of colors\r\nor physical materials can be reconstructed, and non-manifold features such as T-junctions may appear in the interface and\r\nboundary geometry","lang":"eng"}],"title":"Circles of confidence for multi-label geometry completion","_id":"22129","publisher":"Wiley","ddc":["005"],"date_updated":"2026-07-13T14:58:48Z","author":[{"first_name":"Ziyu ","full_name":"Wei, Ziyu ","last_name":"Wei"},{"full_name":"Hafner, Christian","first_name":"Christian","id":"400429CC-F248-11E8-B48F-1D18A9856A87","last_name":"Hafner"},{"first_name":"Aleksei","full_name":"Kalinov, Aleksei","id":"44b7120e-eb97-11eb-a6c2-e1557aa81d02","last_name":"Kalinov","orcid":"0000-0003-2189-3904"},{"first_name":"Peter","full_name":"Synak, Peter","last_name":"Synak","id":"331776E2-F248-11E8-B48F-1D18A9856A87"},{"orcid":"0000-0001-6646-5546","id":"3C61F1D2-F248-11E8-B48F-1D18A9856A87","last_name":"Wojtan","full_name":"Wojtan, Christopher J","first_name":"Christopher J"}],"day":"24","OA_place":"publisher","das_tickbox":"1","volume":45,"OA_type":"hybrid","quality_controlled":"1","file":[{"creator":"mly","file_size":14536575,"success":1,"content_type":"application/pdf","file_id":"22132","checksum":"365f986db34e3fbce74089207599253b","relation":"main_file","date_updated":"2026-06-23T09:07:22Z","file_name":"document(3).pdf","access_level":"open_access","date_created":"2026-06-23T09:07:22Z"}],"conference":{"start_date":"2026-07-01","end_date":"2026-07-03","name":"Eurographics: Symposium on Geometry Processing","location":"Bern, Switzerland"},"publication_status":"accepted","fulldoi":"https://doi.org/10.1111/cgf.70516","publication":"Computer Graphics Forum","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode"},"date_created":"2026-06-23T09:08:41Z","oa":1,"date_published":"2026-06-24T00:00:00Z","intvolume":"        45","status":"public","year":"2026","issue":"5","type":"conference"}]