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Dunajova, “Geometry-driven self-organization of migrating cells and chiral filaments,” Institute of Science and Technology Austria, 2026.","mla":"Dunajova, Zuzana. <i>Geometry-Driven Self-Organization of Migrating Cells and Chiral Filaments</i>. Institute of Science and Technology Austria, 2026, doi:<a href=\"https://doi.org/10.15479/AT-ISTA-21423\">10.15479/AT-ISTA-21423</a>.","ama":"Dunajova Z. Geometry-driven self-organization of migrating cells and chiral filaments. 2026. doi:<a href=\"https://doi.org/10.15479/AT-ISTA-21423\">10.15479/AT-ISTA-21423</a>","ista":"Dunajova Z. 2026. Geometry-driven self-organization of migrating cells and chiral filaments. Institute of Science and Technology Austria.","short":"Z. Dunajova, Geometry-Driven Self-Organization of Migrating Cells and Chiral Filaments, Institute of Science and Technology Austria, 2026.","apa":"Dunajova, Z. (2026). <i>Geometry-driven self-organization of migrating cells and chiral filaments</i>. 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Dunajova, “Supplementary movies to PhD thesis ‘Geometry-driven self-organization of migrating cells and chiral filaments.’” Institute of Science and Technology Austria, 2026.","ama":"Dunajova Z. Supplementary movies to PhD thesis “Geometry-driven self-organization of migrating cells and chiral filaments.” 2026. doi:<a href=\"https://doi.org/10.15479/AT-ISTA-21439\">10.15479/AT-ISTA-21439</a>","apa":"Dunajova, Z. (2026). Supplementary movies to PhD thesis “Geometry-driven self-organization of migrating cells and chiral filaments.” Institute of Science and Technology Austria. <a href=\"https://doi.org/10.15479/AT-ISTA-21439\">https://doi.org/10.15479/AT-ISTA-21439</a>","short":"Z. Dunajova, (2026).","ista":"Dunajova Z. 2026. Supplementary movies to PhD thesis “Geometry-driven self-organization of migrating cells and chiral filaments”, Institute of Science and Technology Austria, <a href=\"https://doi.org/10.15479/AT-ISTA-21439\">10.15479/AT-ISTA-21439</a>.","mla":"Dunajova, Zuzana. <i>Supplementary Movies to PhD Thesis “Geometry-Driven Self-Organization of Migrating Cells and Chiral Filaments.”</i> Institute of Science and Technology Austria, 2026, doi:<a href=\"https://doi.org/10.15479/AT-ISTA-21439\">10.15479/AT-ISTA-21439</a>."},"doi":"10.15479/AT-ISTA-21439","contributor":[{"contributor_type":"researcher","id":"4323B49C-F248-11E8-B48F-1D18A9856A87","first_name":"Saren","orcid":"0000-0003-1671-393X","last_name":"Tasciyan"},{"last_name":"Radler","orcid":"0000-0001-9198-2182 ","first_name":"Philipp","id":"40136C2A-F248-11E8-B48F-1D18A9856A87","contributor_type":"researcher"}],"date_updated":"2026-07-06T12:38:16Z","title":"Supplementary movies to PhD thesis “Geometry-driven self-organization of migrating cells and chiral filaments”","author":[{"id":"4B39F286-F248-11E8-B48F-1D18A9856A87","first_name":"Zuzana","last_name":"Dunajova","full_name":"Dunajova, Zuzana"}],"date_published":"2026-03-12T00:00:00Z","department":[{"_id":"GradSch"},{"_id":"EdHa"}],"article_processing_charge":"No","tmp":{"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)","image":"/images/cc_by_nc_sa.png","short":"CC BY-NC-SA (4.0)"},"oa":1,"month":"03","year":"2026","abstract":[{"lang":"eng","text":"These files contain supplementary movies accompanying the PhD thesis “Geometry-driven self-organization of migrating cells and chiral filaments” by Zuzana Dunajova (2026). The videos provide additional visual material supporting the experiments and results described in the thesis."}],"publisher":"Institute of Science and Technology Austria","project":[{"_id":"34d75525-11ca-11ed-8bc3-89b6307fee9d","name":"Motile active matter models of migrating cells and chiral filaments","grant_number":"26360"}]},{"article_number":"A147","article_type":"original","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>","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.","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>","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>.","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.","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>."},"volume":705,"doi":"10.1051/0004-6361/202555596","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"file_id":"21224","content_type":"application/pdf","relation":"main_file","checksum":"3782e03bc0843438aae8487f6af779c5","file_size":2259914,"date_updated":"2026-02-16T07:35:03Z","creator":"dernst","file_name":"2026_AstronomyAstrophysics_Torralba.pdf","success":1,"date_created":"2026-02-16T07:35:03Z","access_level":"open_access"}],"quality_controlled":"1","file_date_updated":"2026-02-16T07:35:03Z","type":"journal_article","oa_version":"Published Version","status":"public","publication":"Astronomy & Astrophysics","corr_author":"1","arxiv":1,"date_created":"2026-01-25T23:01:41Z","ddc":["520"],"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.","OA_type":"diamond","has_accepted_license":"1","scopus_import":"1","publication_identifier":{"issn":["0004-6361"],"eissn":["1432-0746"]},"_id":"21045","intvolume":"       705","OA_place":"publisher","day":"14","publication_status":"published","publisher":"EDP Sciences","abstract":[{"lang":"eng","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."}],"PlanS_conform":"1","project":[{"name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224","_id":"bd9b2118-d553-11ed-ba76-db24564edfea"}],"oa":1,"language":[{"iso":"eng"}],"year":"2026","month":"01","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"das_tickbox":"1","author":[{"last_name":"Torralba Torregrosa","orcid":"0000-0001-5586-6950","first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto"},{"full_name":"Matthee, Jorryt J","orcid":"0000-0003-2871-127X","last_name":"Matthee","id":"7439a258-f3c0-11ec-9501-9df22fe06720","first_name":"Jorryt J"},{"full_name":"Pezzulli, Gabriele","first_name":"Gabriele","last_name":"Pezzulli"},{"full_name":"Urrutia, Tanya","last_name":"Urrutia","first_name":"Tanya"},{"full_name":"Gronke, Max","last_name":"Gronke","first_name":"Max"},{"full_name":"Mascia, Sara","last_name":"Mascia","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","first_name":"Sara"},{"first_name":"Francesco","last_name":"D’Eugenio","full_name":"D’Eugenio, Francesco"},{"full_name":"Di Cesare, Claudia","last_name":"Di Cesare","id":"2d002343-372f-11ef-98ec-a164d20427cb","first_name":"Claudia"},{"full_name":"Eilers, Anna Christina","last_name":"Eilers","first_name":"Anna Christina"},{"full_name":"Greene, Jenny E.","first_name":"Jenny E.","last_name":"Greene"},{"first_name":"Edoardo","id":"4053390a-6b68-11ef-9828-a3b8adef8d0a","last_name":"Iani","orcid":"0000-0001-8386-3546","full_name":"Iani, Edoardo"},{"full_name":"Ishikawa, Yuzo","last_name":"Ishikawa","first_name":"Yuzo"},{"full_name":"Mackenzie, Ruari","last_name":"Mackenzie","first_name":"Ruari"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"last_name":"Navarrete","first_name":"Benjamín","id":"aa14a535-50c9-11ef-b52e-e0c373d10148","full_name":"Navarrete, Benjamín"},{"full_name":"Kotiwale, Gauri","first_name":"Gauri","id":"1438afc8-1ff6-11ee-9fa6-cd4a75d66875","last_name":"Kotiwale"}],"date_published":"2026-01-14T00:00:00Z","date_updated":"2026-07-08T06:38:23Z","title":"A weak Ly α halo for an extremely bright little red dot. Indications of enshrouded supermassive black hole growth","external_id":{"arxiv":["2505.09542"]},"article_processing_charge":"No","department":[{"_id":"JoMa"},{"_id":"GradSch"}]},{"publisher":"EDP Sciences","abstract":[{"text":"Dipolar (ℓ = 1) mixed modes have revealed a surprisingly weak differential rotation between the core and the envelope of evolved solar-like stars. Quadrupolar (ℓ = 2) mixed modes also contain information regarding internal dynamics but are very rarely characterised due to their low amplitude and the challenging identification of adjacent or overlapping rotationally split multiplets affected by near-degeneracy effects. We aim to extend the broadly used asymptotic seismic diagnostics beyond ℓ = 1 mixed modes by developing an analogue asymptotic description of ℓ = 2 mixed modes while explicitly accounting for near-degeneracy effects that distort their rotational multiplets. We have derived a new asymptotic formulation of near-degenerate mixed ℓ = 2 modes that describes off-diagonal terms representing the interaction between modes of adjacent radial orders. This formalism, expressed directly in the mixed-mode basis, provides analytical expressions for the near-degeneracy effects. We implemented the formalism within a global Bayesian mode-fitting framework for a direct fit of all ℓ = 0, 1, 2 modes in the power spectrum density. We were able to asymptotically model the asymmetric rotational splitting present in various radial orders of ℓ = 2 modes observed in young red giant stars without the need for any numerical stellar modelling. We applied our formalism to the Kepler target KIC 7341231, and it yielded core and envelope rotation rates consistent with previous numerical modelling while providing improved constraints from the global and model-independent approach. We also characterised the new target, KIC 8179973, measuring its rotation rate and mixed-mode parameters for the first time. As our framework relies on a direct global fit, it allows for much better precision on the asteroseismic parameters and rotation rate estimates than standard methods, yielding better constraints for rotation inversions. We have placed the first observational constraints on the asymptotic ℓ = 2 mixed-mode parameters (ΔΠ2, q2, and εg, 2), thus paving the way towards the use of asymptotic seismology beyond ℓ = 1 mixed modes.","lang":"eng"}],"PlanS_conform":"1","oa":1,"language":[{"iso":"eng"}],"year":"2026","month":"03","DOAJ_listed":"1","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"das_tickbox":"1","author":[{"full_name":"Liagre, Bastien Raymond Bernard","first_name":"Bastien Raymond Bernard","id":"662f1873-cab4-11f0-a719-8087d302868d","last_name":"Liagre"},{"full_name":"Desai, Aayush A","last_name":"Desai","id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","first_name":"Aayush A"},{"first_name":"Lukas","id":"f1497a1a-72ef-11ef-b75a-fd877bbf6e8c","last_name":"Einramhof","full_name":"Einramhof, Lukas"},{"full_name":"Bugnet, Lisa Annabelle","id":"d9edb345-f866-11ec-9b37-d119b5234501","first_name":"Lisa Annabelle","last_name":"Bugnet","orcid":"0000-0003-0142-4000"}],"date_published":"2026-03-01T00:00:00Z","date_updated":"2026-07-08T06:39:05Z","title":"Near-degeneracy effects in quadrupolar mixed modes: From an asymptotic description to data fitting","external_id":{"arxiv":["2511.05314 "]},"article_processing_charge":"No","department":[{"_id":"LiBu"},{"_id":"IlCa"},{"_id":"GradSch"}],"article_number":"A321","article_type":"original","volume":707,"citation":{"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>.","short":"B.R.B. Liagre, A.A. Desai, L. Einramhof, L.A. Bugnet, Astronomy &#38; Astrophysics 707 (2026).","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>","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.","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>","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.","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>."},"doi":"10.1051/0004-6361/202558023","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"file_size":12287607,"date_updated":"2026-04-07T09:00:50Z","checksum":"560cac19dc70184626b85e71a26ee22e","content_type":"application/pdf","relation":"main_file","file_id":"21664","access_level":"open_access","success":1,"date_created":"2026-04-07T09:00:50Z","creator":"dernst","file_name":"2026_AstronomyAstrophysics_Liagre.pdf"}],"quality_controlled":"1","file_date_updated":"2026-04-07T09:00:50Z","type":"journal_article","status":"public","publication":"Astronomy & Astrophysics","oa_version":"Published Version","corr_author":"1","date_created":"2026-04-05T22:01:32Z","arxiv":1,"ddc":["520"],"has_accepted_license":"1","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).","OA_type":"diamond","scopus_import":"1","publication_identifier":{"eissn":["1432-0746"],"issn":["0004-6361"]},"_id":"21658","intvolume":"       707","day":"01","OA_place":"publisher","publication_status":"published"},{"project":[{"_id":"bd9b2118-d553-11ed-ba76-db24564edfea","name":"Young galaxies as tracers and agents of cosmic reionization","grant_number":"101076224"}],"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"}],"publisher":"IOP Publishing","year":"2026","month":"07","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).","language":[{"iso":"eng"}],"oa":1,"das_tickbox":"1","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"DOAJ_listed":"1","department":[{"_id":"JoMa"},{"_id":"IlCa"},{"_id":"GradSch"}],"article_processing_charge":"Yes","researchdata_availability":"yes","external_id":{"arxiv":["2603.28335"]},"issue":"2","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","date_updated":"2026-07-13T08:08:41Z","date_published":"2026-07-10T00:00:00Z","supplementarymaterial":"yes","author":[{"last_name":"Torralba Torregrosa","orcid":"0000-0001-5586-6950","first_name":"Alberto","id":"018f0249-0e87-11f0-b167-cbce08fbd541","full_name":"Torralba Torregrosa, Alberto"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"first_name":"Andrea","last_name":"Weibel","full_name":"Weibel, Andrea"},{"full_name":"Naidu, Rohan P.","first_name":"Rohan P.","last_name":"Naidu"},{"last_name":"Ma","first_name":"Yilun","full_name":"Ma, Yilun"},{"full_name":"Cloonan, Aidan P.","last_name":"Cloonan","first_name":"Aidan P."},{"last_name":"Desai","first_name":"Aayush A","id":"502cfd30-32c1-11ee-a9a4-d8dad5c6739e","full_name":"Desai, Aayush A"},{"last_name":"De Graaff","first_name":"Anna","full_name":"De Graaff, Anna"},{"full_name":"Greene, Jenny E.","last_name":"Greene","first_name":"Jenny E."},{"first_name":"Christian Kragh","last_name":"Jespersen","full_name":"Jespersen, Christian Kragh"},{"last_name":"Kramarenko","orcid":"0000-0001-5346-6048","id":"9a9394cb-3200-11ee-973b-f5ba2a8b16e4","first_name":"Ivan","full_name":"Kramarenko, Ivan"},{"first_name":"Sara","id":"edaf889c-c7cd-11ef-ab1b-bb28c431bd29","last_name":"Mascia","full_name":"Mascia, Sara"},{"full_name":"Oesch, Pascal A.","last_name":"Oesch","first_name":"Pascal A."},{"full_name":"Sun, Wendy Q.","last_name":"Sun","first_name":"Wendy Q."},{"full_name":"Williams, Christina C.","last_name":"Williams","first_name":"Christina C."}],"doi":"10.3847/2041-8213/ae7bfd","citation":{"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.","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>.","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>","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).","ista":"Torralba Torregrosa A, Matthee JJ, Weibel A, Naidu RP, Ma Y, Cloonan AP, Desai AA, De Graaff A, Greene JE, Jespersen CK, Kramarenko I, Mascia S, Oesch PA, Sun WQ, Williams CC. 2026. A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7. The Astrophysical Journal Letters. 1005(2), L37.","ama":"Torralba Torregrosa A, Matthee JJ, Weibel A, et al. A black hole star at cosmic noon: Extreme Balmer break, photospheric continuum, and broad absorption by thick winds in a Little Red Dot at z = 1.7. <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>"},"volume":1005,"article_type":"original","article_number":"L37","file_date_updated":"2026-07-13T07:46:22Z","quality_controlled":"1","file":[{"file_size":5419071,"date_updated":"2026-07-13T07:46:22Z","checksum":"7600db260d799ddea45cf3bd01effe41","content_type":"application/pdf","relation":"main_file","file_id":"22274","access_level":"open_access","date_created":"2026-07-13T07:46:22Z","success":1,"creator":"dernst","file_name":"2026_AstrophysicalJourLetters_Torralba.pdf"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-07-12T22:02:17Z","arxiv":1,"corr_author":"1","publication":"The Astrophysical Journal Letters","oa_version":"Published Version","status":"public","type":"journal_article","publication_status":"published","day":"10","intvolume":"      1005","OA_place":"publisher","_id":"22263","publication_identifier":{"eissn":["2041-8213"],"issn":["2041-8205"]},"scopus_import":"1","has_accepted_license":"1","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).","OA_type":"gold","ddc":["520"]},{"oa":1,"month":"06","year":"2026","language":[{"iso":"eng"}],"dataavailabilitystatement":"All structures and metrics reported in this paper are openly available on Harvard Dataverse - https://doi.org/10.7910/DVN/PLYUHN. All code is openly available on GitHub (https://github.com/sai-advaith/guided_alphafold); the version used for this paper (version 0.9.1) is permanently archived on Zenodo https://doi.org/10.5281/zenodo.17307005","abstract":[{"text":"AlphaFold3 predicts highly accurate protein structures from sequence but tends to collapse to a single dominant conformation, even when the underlying structure is inherently heterogeneous. Moreover, its predictions are oblivious to experimental conditions that can alter local sequence conformation. In this work, we show that AlphaFold3 can be guided to match data obtained by nuclear magnetic resonance (NMR) spectroscopy, X-ray crystallography and cryogenic electron microscopy (cryo-EM) experiments and combinations thereof. Our approach can also incorporate data that explicitly report on dynamics, such as site-resolved order parameters. We demonstrate that this methodology generates compact structural ensembles whose ensemble-averaged observables agree with experiment, with fewer distance restraint violations than traditionally resolved NMR structures and with unmodeled alternate conformations uncovered in electron density. This methodology paves the way for experimentally aware predictive models that generate structural ensembles consistent with the measurements, potentially over multiple modalities, and that can be further refined toward thermodynamically grounded ensembles by incorporating energetics.","lang":"eng"}],"publisher":"Springer Nature","PlanS_conform":"1","title":"Experiment-guided AlphaFold3 resolves measurement-consistent protein ensembles","date_updated":"2026-07-13T09:34:36Z","author":[{"full_name":"Maddipatla, Sai A","first_name":"Sai A","id":"e957f5e5-91c9-11f0-a95f-e090f66ecb4d","last_name":"Maddipatla"},{"id":"ef280fe0-91c9-11f0-a95f-8dea3f5bc513","first_name":"Nadav E","last_name":"Sellam","full_name":"Sellam, Nadav E"},{"full_name":"Bojan, Meital I","id":"11d88cf5-91ca-11f0-a95f-edf9f08f47b7","first_name":"Meital I","last_name":"Bojan"},{"id":"ff7958eb-91c9-11f0-a95f-f3bf65828cf6","first_name":"Vova","last_name":"Masalitin","full_name":"Masalitin, Vova"},{"full_name":"Vedula, Sanketh","last_name":"Vedula","first_name":"Sanketh"},{"full_name":"Schanda, Paul","id":"7B541462-FAF6-11E9-A490-E8DFE5697425","first_name":"Paul","orcid":"0000-0002-9350-7606","last_name":"Schanda"},{"last_name":"Marx","first_name":"Ailie","full_name":"Marx, Ailie"},{"orcid":"0000-0001-9699-8730","last_name":"Bronstein","first_name":"Alexander","id":"58f3726e-7cba-11ef-ad8b-e6e8cb3904e6","full_name":"Bronstein, Alexander"}],"main_file_link":[{"url":"https://doi.org/10.1038/s41587-026-03166-5","open_access":"1"}],"supplementarymaterial":"yes","date_published":"2026-06-29T00:00:00Z","department":[{"_id":"PaSc"},{"_id":"AlBr"},{"_id":"GradSch"}],"external_id":{"pmid":["42374114"]},"researchdata_availability":"yes","article_processing_charge":"Yes (via OA deal)","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"das_tickbox":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","citation":{"short":"S.A. Maddipatla, N.E. Sellam, M.I. Bojan, V. Masalitin, S. Vedula, P. Schanda, A. Marx, A.M. Bronstein, Nature Biotechnology (2026).","apa":"Maddipatla, S. A., Sellam, N. E., Bojan, M. I., Masalitin, V., Vedula, S., Schanda, P., … Bronstein, A. M. (2026). Experiment-guided AlphaFold3 resolves measurement-consistent protein ensembles. <i>Nature Biotechnology</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41587-026-03166-5\">https://doi.org/10.1038/s41587-026-03166-5</a>","ista":"Maddipatla SA, Sellam NE, Bojan MI, Masalitin V, Vedula S, Schanda P, Marx A, Bronstein AM. 2026. Experiment-guided AlphaFold3 resolves measurement-consistent protein ensembles. Nature Biotechnology.","ama":"Maddipatla SA, Sellam NE, Bojan MI, et al. Experiment-guided AlphaFold3 resolves measurement-consistent protein ensembles. <i>Nature Biotechnology</i>. 2026. doi:<a href=\"https://doi.org/10.1038/s41587-026-03166-5\">10.1038/s41587-026-03166-5</a>","mla":"Maddipatla, Sai A., et al. “Experiment-Guided AlphaFold3 Resolves Measurement-Consistent Protein Ensembles.” <i>Nature Biotechnology</i>, Springer Nature, 2026, doi:<a href=\"https://doi.org/10.1038/s41587-026-03166-5\">10.1038/s41587-026-03166-5</a>.","ieee":"S. A. Maddipatla <i>et al.</i>, “Experiment-guided AlphaFold3 resolves measurement-consistent protein ensembles,” <i>Nature Biotechnology</i>. Springer Nature, 2026.","chicago":"Maddipatla, Sai A, Nadav E Sellam, Meital I Bojan, Vova Masalitin, Sanketh Vedula, Paul Schanda, Ailie Marx, and Alex M. Bronstein. “Experiment-Guided AlphaFold3 Resolves Measurement-Consistent Protein Ensembles.” <i>Nature Biotechnology</i>. Springer Nature, 2026. <a href=\"https://doi.org/10.1038/s41587-026-03166-5\">https://doi.org/10.1038/s41587-026-03166-5</a>."},"article_type":"original","doi":"10.1038/s41587-026-03166-5","scopus_import":"1","ddc":["570"],"acknowledgement":"A. Marx acknowledges the financial support of the Helmsley Fellowships Program for Sustainability and Health. A.M.B. and P.S. are supported by the Institute of Science and Technology Austria Internal Project Call grant Generative Protein NMR. S.V. was supported in part by funding from the Eric and Wendy Schmidt Center at the Broad Institute of MIT and Harvard. Open access funding provided by Institute of Science and Technology (IST Austria).","has_accepted_license":"1","OA_type":"hybrid","day":"29","OA_place":"publisher","publication_status":"epub_ahead","publication_identifier":{"issn":["1087-0156"],"eissn":["1546-1696"]},"_id":"22268","publication":"Nature Biotechnology","status":"public","oa_version":"Published Version","type":"journal_article","date_created":"2026-07-12T22:02:19Z","corr_author":"1","pmid":1},{"oa":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.","language":[{"iso":"eng"}],"year":"2026","month":"07","publisher":"Springer Nature","abstract":[{"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.","lang":"eng"}],"date_published":"2026-07-03T00:00:00Z","author":[{"first_name":"Paula P.","last_name":"Navarro","full_name":"Navarro, Paula P."},{"first_name":"Andrea","last_name":"Vettiger","full_name":"Vettiger, Andrea"},{"full_name":"Hajdu, Roman","last_name":"Hajdu","id":"ffab949d-133f-11ed-8f02-94de21ace503","first_name":"Roman"},{"full_name":"Ananda, Virly Y.","first_name":"Virly Y.","last_name":"Ananda"},{"last_name":"López-Tavares","first_name":"Alejandro","full_name":"López-Tavares, Alejandro"},{"first_name":"Ernst W.","last_name":"Schmid","full_name":"Schmid, Ernst W."},{"full_name":"Walter, Johannes C.","first_name":"Johannes C.","last_name":"Walter"},{"orcid":"0000-0001-7309-9724","last_name":"Loose","first_name":"Martin","id":"462D4284-F248-11E8-B48F-1D18A9856A87","full_name":"Loose, Martin"},{"first_name":"Luke H.","last_name":"Chao","full_name":"Chao, Luke H."},{"last_name":"Bernhardt","first_name":"Thomas G.","full_name":"Bernhardt, Thomas G."}],"supplementarymaterial":"yes","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1038/s41564-026-02403-6"}],"date_updated":"2026-07-13T09:22:49Z","title":"The penicillin-binding protein PBP1b fortifies the Escherichia coli division site against osmotic rupture","researchdata_availability":"yes","article_processing_charge":"Yes (in subscription journal)","external_id":{"pmid":["42399561"]},"department":[{"_id":"MaLo"},{"_id":"GradSch"}],"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"das_tickbox":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","article_type":"original","citation":{"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).","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>","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.","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>.","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>.","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","has_accepted_license":"1","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.).","OA_type":"hybrid","ddc":["570"],"scopus_import":"1","_id":"22269","publication_identifier":{"eissn":["2058-5276"]},"publication_status":"epub_ahead","OA_place":"publisher","day":"03","type":"journal_article","publication":"Nature Microbiology","status":"public","oa_version":"Published Version","pmid":1,"date_created":"2026-07-12T22:02:19Z"},{"publication":"Current Biology","status":"public","oa_version":"None","type":"journal_article","date_created":"2026-07-13T09:39:40Z","pmid":1,"corr_author":"1","scopus_import":"1","OA_type":"closed access","publication_status":"published","day":"06","intvolume":"        36","_id":"22286","publication_identifier":{"issn":["0960-9822"]},"citation":{"chicago":"Leitner, Valentin, and Eva Benková. “Auxin and the Control of Plant Growth and Development.” <i>Current Biology</i>. Elsevier, 2026. <a href=\"https://doi.org/10.1016/j.cub.2026.04.047\">https://doi.org/10.1016/j.cub.2026.04.047</a>.","ieee":"V. Leitner and E. Benková, “Auxin and the control of plant growth and development,” <i>Current Biology</i>, vol. 36, no. 13. Elsevier, pp. R739–R744, 2026.","mla":"Leitner, Valentin, and Eva Benková. “Auxin and the Control of Plant Growth and Development.” <i>Current Biology</i>, vol. 36, no. 13, Elsevier, 2026, pp. R739–44, doi:<a href=\"https://doi.org/10.1016/j.cub.2026.04.047\">10.1016/j.cub.2026.04.047</a>.","ama":"Leitner V, Benková E. Auxin and the control of plant growth and development. <i>Current Biology</i>. 2026;36(13):R739-R744. doi:<a href=\"https://doi.org/10.1016/j.cub.2026.04.047\">10.1016/j.cub.2026.04.047</a>","apa":"Leitner, V., &#38; Benková, E. (2026). Auxin and the control of plant growth and development. <i>Current Biology</i>. Elsevier. <a href=\"https://doi.org/10.1016/j.cub.2026.04.047\">https://doi.org/10.1016/j.cub.2026.04.047</a>","ista":"Leitner V, Benková E. 2026. Auxin and the control of plant growth and development. Current Biology. 36(13), R739–R744.","short":"V. Leitner, E. Benková, Current Biology 36 (2026) R739–R744."},"volume":36,"article_type":"original","doi":"10.1016/j.cub.2026.04.047","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","das_tickbox":"0","issue":"13","date_updated":"2026-07-13T11:11:56Z","title":"Auxin and the control of plant growth and development","date_published":"2026-07-06T00:00:00Z","author":[{"last_name":"Leitner","first_name":"Valentin","id":"4c665ce3-0016-11ec-bea0-e44de7a4fa3d","full_name":"Leitner, Valentin"},{"orcid":"0000-0002-8510-9739","last_name":"Benková","id":"38F4F166-F248-11E8-B48F-1D18A9856A87","first_name":"Eva","full_name":"Benková, Eva"}],"supplementarymaterial":"no","department":[{"_id":"EvBe"},{"_id":"GradSch"}],"article_processing_charge":"No","researchdata_availability":"no","external_id":{"pmid":["42407441"]},"abstract":[{"lang":"eng","text":"Plants are remarkable organisms. Unlike animals, they cannot flee and, rooted in one place, they must cope with whatever challenges arise — nutrient scarcity, drought, shade, wind or obstacles in the soil. Their extraordinary ability to survive in such unstable environmental conditions lies in their capacity to adapt. In response to environmental signals, plants can rapidly adjust the rate of organ growth, change the direction of growth, bend toward resources, or remodel their body architecture by promoting or suppressing the formation of new organs such as lateral roots, branches, leaves, or flowers. This unique developmental plasticity depends on chemical signals, plant hormones that serve as regulators and coordinators of endogenous molecular and cellular processes. Chief among these signals is auxin, a plant hormone central to nearly every aspect of plant life."}],"publisher":"Elsevier","page":"R739-R744","month":"07","year":"2026","language":[{"iso":"eng"}]},{"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","citation":{"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>","ista":"De Wilde M, Seiringer R. 2026. Arbitrary harmonic functions as Bose–Einstein condensates. Journal of Mathematical Physics. 67(6), 061901.","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>","short":"M. De Wilde, R. Seiringer, Journal of Mathematical Physics 67 (2026).","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>.","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>.","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."},"volume":67,"article_type":"original","article_number":"061901","doi":"10.1063/5.0325354","scopus_import":"1","acknowledgement":"We are grateful to Rupert Frank and Jakob Yngvason for helpful discussions and suggestions.","OA_type":"green","publication_status":"published","day":"01","OA_place":"repository","intvolume":"        67","_id":"22292","publication_identifier":{"issn":["0022-2488"],"eissn":["1089-7658"]},"status":"public","oa_version":"Preprint","publication":"Journal of Mathematical Physics","type":"journal_article","date_created":"2026-07-13T09:45:09Z","arxiv":1,"corr_author":"1","oa":1,"year":"2026","month":"06","dataavailabilitystatement":"Data sharing is not applicable to this article as no new data were created or analyzed in this study.","language":[{"iso":"eng"}],"abstract":[{"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.","lang":"eng"}],"publisher":"AIP Publishing","date_updated":"2026-07-13T12:20:59Z","issue":"6","title":"Arbitrary harmonic functions as Bose–Einstein condensates","date_published":"2026-06-01T00:00:00Z","author":[{"full_name":"De Wilde, Michiel","first_name":"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"}],"main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2601.22883","open_access":"1"}],"supplementarymaterial":"not applicable","department":[{"_id":"RoSe"},{"_id":"GradSch"}],"article_processing_charge":"No","researchdata_availability":"not applicable","external_id":{"arxiv":["2601.22883"]},"das_tickbox":"1"},{"doi":"10.1038/s41586-026-10679-1","citation":{"ieee":"L. A. Schwarz <i>et al.</i>, “Cortical development dynamics across autism spectrum disorder mouse models,” <i>Nature</i>. Springer Nature, 2026.","chicago":"Schwarz, Lena A, Christoph Dotter, Sergey Isaev, Michela Lisi, Daniel Malzl, Christoph Büschl, Sabrina Ladstätter, et al. “Cortical Development Dynamics across Autism Spectrum Disorder Mouse Models.” <i>Nature</i>. Springer Nature, 2026. <a href=\"https://doi.org/10.1038/s41586-026-10679-1\">https://doi.org/10.1038/s41586-026-10679-1</a>.","mla":"Schwarz, Lena A., et al. “Cortical Development Dynamics across Autism Spectrum Disorder Mouse Models.” <i>Nature</i>, Springer Nature, 2026, doi:<a href=\"https://doi.org/10.1038/s41586-026-10679-1\">10.1038/s41586-026-10679-1</a>.","ista":"Schwarz LA, Dotter C, Isaev S, Lisi M, Malzl D, Büschl C, Ladstätter S, Oliveira B, Barel M, Basilico B, Chintaluri C, Gorkiewicz S, Goudarzi M, Belinova T, Reichl S, Sendžikaitė G, Arcot Jayaram S, Koppensteiner P, Sommer CM, Vogels TP, Menche J, Adameyko I, Kharchenko PV, Bock C, Novarino G. 2026. Cortical development dynamics across autism spectrum disorder mouse models. Nature.","short":"L.A. Schwarz, C. Dotter, S. Isaev, M. Lisi, D. Malzl, C. Büschl, S. Ladstätter, B. Oliveira, M. Barel, B. Basilico, C. Chintaluri, S. Gorkiewicz, M. Goudarzi, T. Belinova, S. Reichl, G. Sendžikaitė, S. Arcot Jayaram, P. Koppensteiner, C.M. Sommer, T.P. Vogels, J. Menche, I. Adameyko, P.V. Kharchenko, C. Bock, G. Novarino, Nature (2026).","apa":"Schwarz, L. A., Dotter, C., Isaev, S., Lisi, M., Malzl, D., Büschl, C., … Novarino, G. (2026). Cortical development dynamics across autism spectrum disorder mouse models. <i>Nature</i>. Springer Nature. <a href=\"https://doi.org/10.1038/s41586-026-10679-1\">https://doi.org/10.1038/s41586-026-10679-1</a>","ama":"Schwarz LA, Dotter C, Isaev S, et al. Cortical development dynamics across autism spectrum disorder mouse models. <i>Nature</i>. 2026. doi:<a href=\"https://doi.org/10.1038/s41586-026-10679-1\">10.1038/s41586-026-10679-1</a>"},"article_type":"original","acknowledged_ssus":[{"_id":"Bio"},{"_id":"LifeSc"}],"quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","date_created":"2026-07-13T09:47:21Z","corr_author":"1","pmid":1,"oa_version":"Published Version","status":"public","publication":"Nature","type":"journal_article","day":"17","OA_place":"publisher","publication_status":"epub_ahead","publication_identifier":{"eissn":["1476-4687"],"issn":["0028-0836"]},"_id":"22295","scopus_import":"1","ddc":["570"],"OA_type":"hybrid","has_accepted_license":"1","acknowledgement":"We thank F. Freeman, V. Voronin and M. Ladron de Guevara for technical assistance; A. Stichelberger and S. Liegenfeld for the management of our animal colony; M. Schunn, C. Gold and the Preclinical Facility team for technical assistance; C. Jansen and the Scientific Computing Facility for bioinformatics support and technical assistance; the Biomedical Sequencing Facility at CeMM for assistance with next-generation sequencing; and J. Lin and T. Krausgruber in the laboratory of C. Bock for support with flow cytometry; J. Kirchner for illustrating the multi-omics approach depicted in Fig. 1; and all members of the laboratory of G.N. for their support and discussions. This study was supported by the Scientific Service Units of ISTA through resources provided by the Imaging & Optics Facility and the Laboratory Support Facility. Bulk RNA-seq was performed by the Next Generation Sequencing Facility at Vienna BioCenter Core Facilities, member of the Vienna BioCenter. This work was supported by a European Research Council Consolidator Grant (PR1028ERC02), by SFARI (PR1028SIM02) and by the Austrian Science Fund (PE1028W1232 and PR1028FG1803) to G.N. Open access funding provided by Institute of Science and Technology (IST Austria).","PlanS_conform":"1","project":[{"grant_number":"101044865","name":"Toward an understanding of the brain interstitial system and the extracellular proteome in health and autism spectrum disorders","_id":"34ba8964-11ca-11ed-8bc3-e15864e7e9a6"},{"grant_number":"707964","name":"Critical windows and reversibility of ASD associated with mutations in chromatin remodelers","_id":"9B91375C-BA93-11EA-9121-9846C619BF3A"},{"_id":"2548AE96-B435-11E9-9278-68D0E5697425","call_identifier":"FWF","name":"Molecular Drug Targets","grant_number":"W1232"},{"grant_number":"FG1803 49015","name":"Neurobiology of anxiety in autism spectrum disorders","_id":"ebb38b5d-77a9-11ec-83b8-a42e08120a88"}],"abstract":[{"lang":"eng","text":"Despite the functional diversity of over 100 causal genes1,2,3, phenotypic convergence across models may reveal common neurobiological processes in autism spectrum disorder (ASD). Here we profiled 251 samples from 11 monogenic mouse models of ASD using single-nucleus multi-omic sequencing across three developmental stages, both sexes and two brain regions. Despite genetic heterogeneity, ASD-linked mutations converged on perturbations of the radial glial cell lineage. These alterations reflect a transient developmental delay rather than lasting lineage misspecification and resolve by postnatal stages. Molecularly, the largest transcriptional differences emerged in neurons at early postnatal stages. These changes included downregulation of synaptic and ion channel-related genes, consistent with homeostatic adaptation or delayed maturation. Network analysis showed molecular convergence across models within each developmental stage, suggesting that diverse mutations linked to ASD impinge on common, stage-specific processes. Convergence becomes less pronounced by postnatal day 14, highlighting the dynamic nature of ASD-associated changes. Cross-genotype heterogeneity is superimposed on stage-specific effects. Electrophysiology corroborated this pattern: mutants generally showed altered neuronal excitability and synaptic properties with model-specific nuances. Our study also highlighted sex-specific gene expression alterations, with female mice often displaying larger effect sizes than male mice. Together, our findings provide a comprehensive view of developmental cellular and molecular dynamics across models of ASD."}],"publisher":"Springer Nature","month":"06","year":"2026","language":[{"iso":"eng"}],"dataavailabilitystatement":"Single-nucleus multiomics data are available from the Gene Expression Omnibus (GSE328363). The mm10 reference genome was used for the alignment (refdata-cellranger-arc-mm10-2020-A-2.0.0, obtained from https://cf.10xgenomics.com/supp/cell-arc/refdata-cellranger-arc-mm10-2020-A-2.0.0.tar.gz). Single-cell data can be accessed and visualized through a CELLxGENE database (https://adameykolab.hifo.meduniwien.ac.at/cellxgene_public/filecrawl/.2026_Nature_Schwarz). Source data are provided with this paper. Scripts and analyses that support the main findings of this study are accessible in a GitHub repository (https://git.ista.ac.at/research-sofware/mouseome).","oa":1,"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"department":[{"_id":"AnKi"},{"_id":"GaNo"},{"_id":"TiVo"},{"_id":"ScienComp"},{"_id":"GradSch"},{"_id":"Bio"},{"_id":"PreCl"}],"external_id":{"pmid":["42310454"]},"article_processing_charge":"Yes (via OA deal)","researchdata_availability":"yes","title":"Cortical development dynamics across autism spectrum disorder mouse models","date_updated":"2026-07-13T12:58:19Z","author":[{"full_name":"Schwarz, Lena A","last_name":"Schwarz","id":"29A8453C-F248-11E8-B48F-1D18A9856A87","first_name":"Lena A"},{"full_name":"Dotter, Christoph","id":"4C66542E-F248-11E8-B48F-1D18A9856A87","first_name":"Christoph","last_name":"Dotter","orcid":"0000-0002-9033-9096"},{"full_name":"Isaev, Sergey","last_name":"Isaev","first_name":"Sergey"},{"last_name":"Lisi","first_name":"Michela","id":"39383c1b-d3eb-11ef-8d6c-c8cdf4e10c8c","full_name":"Lisi, Michela"},{"full_name":"Malzl, Daniel","last_name":"Malzl","first_name":"Daniel"},{"id":"2a8c054c-0913-11ee-9159-f8ef515809ed","first_name":"Christoph","last_name":"Büschl","full_name":"Büschl, Christoph"},{"last_name":"Ladstätter","first_name":"Sabrina","full_name":"Ladstätter, Sabrina"},{"id":"3B03AA1A-F248-11E8-B48F-1D18A9856A87","first_name":"Bárbara","last_name":"Oliveira","full_name":"Oliveira, Bárbara"},{"full_name":"Barel, Matteo","last_name":"Barel","id":"8959927b-2236-11ed-bd6e-ea83d94ade0e","first_name":"Matteo"},{"orcid":"0000-0003-1843-3173","last_name":"Basilico","first_name":"Bernadette","id":"36035796-5ACA-11E9-A75E-7AF2E5697425","full_name":"Basilico, Bernadette"},{"last_name":"Chintaluri","orcid":"0000-0003-4252-1608","id":"BA06AFEE-A4BA-11EA-AE5C-14673DDC885E","first_name":"Chaitanya","full_name":"Chintaluri, Chaitanya"},{"last_name":"Gorkiewicz","id":"f141a35d-15a9-11ec-9fb2-fef6becc7b6f","first_name":"Sarah","full_name":"Gorkiewicz, Sarah"},{"full_name":"Goudarzi, Mohammad","first_name":"Mohammad","id":"3384113A-F248-11E8-B48F-1D18A9856A87","last_name":"Goudarzi"},{"full_name":"Belinova, Tereza","last_name":"Belinova","first_name":"Tereza","id":"0bf89b6a-d28b-11eb-8bd6-f43768e4d368"},{"full_name":"Reichl, Stephan","first_name":"Stephan","last_name":"Reichl"},{"first_name":"Gintarė","id":"dd6d52f2-c50d-11eb-9548-bcf0ff82b344","last_name":"Sendžikaitė","full_name":"Sendžikaitė, Gintarė"},{"full_name":"Arcot Jayaram, Satish","orcid":"0000-0002-2479-2669","last_name":"Arcot Jayaram","id":"b0bbee33-09f7-11eb-909c-8b358058d28a","first_name":"Satish"},{"id":"3B8B25A8-F248-11E8-B48F-1D18A9856A87","first_name":"Peter","orcid":"0000-0002-3509-1948","last_name":"Koppensteiner","full_name":"Koppensteiner, Peter"},{"full_name":"Sommer, Christoph M","id":"4DF26D8C-F248-11E8-B48F-1D18A9856A87","first_name":"Christoph M","last_name":"Sommer","orcid":"0000-0003-1216-9105"},{"full_name":"Vogels, Tim P","last_name":"Vogels","orcid":"0000-0003-3295-6181","id":"CB6FF8D2-008F-11EA-8E08-2637E6697425","first_name":"Tim P"},{"last_name":"Menche","first_name":"Jörg","full_name":"Menche, Jörg"},{"last_name":"Adameyko","first_name":"Igor","full_name":"Adameyko, Igor"},{"last_name":"Kharchenko","id":"0095641e-7eb7-11f1-8665-aec51a2ab5e0","first_name":"Peter Vasili","full_name":"Kharchenko, Peter Vasili"},{"last_name":"Bock","first_name":"Christoph","full_name":"Bock, Christoph"},{"id":"3E57A680-F248-11E8-B48F-1D18A9856A87","first_name":"Gaia","orcid":"0000-0002-7673-7178","last_name":"Novarino","full_name":"Novarino, Gaia"}],"supplementarymaterial":"yes","main_file_link":[{"url":"https://doi.org/10.1038/s41586-026-10679-1","open_access":"1"}],"date_published":"2026-06-17T00:00:00Z"},{"citation":{"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.","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).","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>","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>","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>.","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.","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>."},"article_type":"original","article_number":"jipb.70309","doi":"10.1111/jipb.70309","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","acknowledged_ssus":[{"_id":"Bio"},{"_id":"NanoFab"}],"oa_version":"Published Version","status":"public","publication":"Journal of Integrative Plant Biology","type":"journal_article","date_created":"2026-07-13T10:44:55Z","pmid":1,"corr_author":"1","scopus_import":"1","has_accepted_license":"1","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.","OA_type":"hybrid","ddc":["580"],"publication_status":"epub_ahead","day":"10","OA_place":"publisher","_id":"22301","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."}],"publisher":"Wiley","project":[{"grant_number":"101142681","name":"Cyclic nucleotides as second messengers in plants","_id":"8f347782-16d5-11f0-9cad-8c19706ee739"},{"grant_number":"I06123","name":"Peptide receptors for auxin canalization in Arabidopsis","_id":"bd76d395-d553-11ed-ba76-f678c14f9033"},{"name":"Guanylate cyclase activity of TIR1/AFBs auxin receptors","grant_number":"P37051","_id":"7bcece63-9f16-11ee-852c-ae94e099eeb6"}],"PlanS_conform":"1","oa":1,"year":"2026","month":"06","language":[{"iso":"eng"}],"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"das_tickbox":"0","date_updated":"2026-07-13T14:26:31Z","title":"Auxin response and PIN‐mediated transport in chlorophyte algae","date_published":"2026-06-10T00:00:00Z","author":[{"full_name":"Smoljan, Adrijana","last_name":"Smoljan","id":"cced8a85-223e-11ed-af04-b0596c55053b","first_name":"Adrijana"},{"last_name":"Koutnik‐Abele","first_name":"Sarah","full_name":"Koutnik‐Abele, Sarah"},{"full_name":"Vladimirtsev, Dmitrii","last_name":"Vladimirtsev","id":"60466724-5355-11ee-ae5a-fa55e8f99c3d","first_name":"Dmitrii"},{"full_name":"Klíma, Petr","first_name":"Petr","last_name":"Klíma"},{"first_name":"Anita","last_name":"Bírošíková","full_name":"Bírošíková, Anita"},{"full_name":"Zhang, Yuzhou","orcid":"0000-0003-2627-6956","last_name":"Zhang","id":"3B6137F2-F248-11E8-B48F-1D18A9856A87","first_name":"Yuzhou"},{"orcid":"0000-0001-5145-4609","last_name":"Merrin","id":"4515C308-F248-11E8-B48F-1D18A9856A87","first_name":"Jack","full_name":"Merrin, Jack"},{"first_name":"Maximilian","id":"37e65def-d415-11eb-ae59-a7b67be103db","last_name":"Schuster","full_name":"Schuster, Maximilian"},{"full_name":"Kurtović, Katarina","first_name":"Katarina","last_name":"Kurtović"},{"full_name":"Hammes, Ulrich Z.","last_name":"Hammes","first_name":"Ulrich Z."},{"full_name":"Petrášek, Jan","last_name":"Petrášek","first_name":"Jan"},{"full_name":"Friml, Jiří","orcid":"0000-0002-8302-7596","last_name":"Friml","first_name":"Jiří","id":"4159519E-F248-11E8-B48F-1D18A9856A87"}],"main_file_link":[{"url":"https://doi.org/10.1111/jipb.70309","open_access":"1"}],"supplementarymaterial":"yes","department":[{"_id":"JiFr"},{"_id":"GradSch"},{"_id":"NanoFab"},{"_id":"Bio"}],"researchdata_availability":"no","article_processing_charge":"Yes (via OA deal)","external_id":{"pmid":["42271607"]}},{"corr_author":"1","date_created":"2026-06-23T09:08:41Z","type":"conference","conference":{"name":"Eurographics: Symposium on Geometry Processing","start_date":"2026-07-01","location":"Bern, Switzerland","end_date":"2026-07-03"},"status":"public","publication":"Computer Graphics Forum","oa_version":"Published Version","_id":"22129","publication_status":"accepted","OA_place":"publisher","day":"24","intvolume":"        45","OA_type":"hybrid","has_accepted_license":"1","ddc":["005"],"doi":"10.1111/cgf.70516","volume":45,"citation":{"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.","short":"Z. Wei, C. Hafner, A. Kalinov, P. Synak, C. Wojtan, in:, Computer Graphics Forum, Wiley, n.d.","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>","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>","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>.","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.","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>."},"quality_controlled":"1","file_date_updated":"2026-06-23T09:07:22Z","file":[{"checksum":"365f986db34e3fbce74089207599253b","file_size":14536575,"date_updated":"2026-06-23T09:07:22Z","file_id":"22132","content_type":"application/pdf","relation":"main_file","access_level":"open_access","creator":"mly","file_name":"document(3).pdf","success":1,"date_created":"2026-06-23T09:07:22Z"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","das_tickbox":"1","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_processing_charge":"Yes (via OA deal)","department":[{"_id":"ChWo"},{"_id":"GradSch"}],"date_published":"2026-06-24T00:00:00Z","author":[{"full_name":"Wei, Ziyu ","last_name":"Wei","first_name":"Ziyu "},{"full_name":"Hafner, Christian","last_name":"Hafner","first_name":"Christian","id":"400429CC-F248-11E8-B48F-1D18A9856A87"},{"last_name":"Kalinov","orcid":"0000-0003-2189-3904","first_name":"Aleksei","id":"44b7120e-eb97-11eb-a6c2-e1557aa81d02","full_name":"Kalinov, Aleksei"},{"first_name":"Peter","id":"331776E2-F248-11E8-B48F-1D18A9856A87","last_name":"Synak","full_name":"Synak, Peter"},{"full_name":"Wojtan, Christopher J","orcid":"0000-0001-6646-5546","last_name":"Wojtan","id":"3C61F1D2-F248-11E8-B48F-1D18A9856A87","first_name":"Christopher J"}],"issue":"5","title":"Circles of confidence for multi-label geometry completion","date_updated":"2026-07-13T14:58:48Z","project":[{"name":"Computational Discovery of Numerical Algorithms for Animation and Simulation of Natural Phenomena","grant_number":"101045083","_id":"34bc2376-11ca-11ed-8bc3-9a3b3961a088"}],"publisher":"Wiley","abstract":[{"lang":"eng","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"}],"language":[{"iso":"eng"}],"year":"2026","month":"06","oa":1},{"type":"conference","alternative_title":["LIPIcs"],"conference":{"end_date":"2026-06-05","location":"New Brunswick, NJ, United States","start_date":"2026-06-02","name":"SoCG: Symposium on Computational Geometry"},"oa_version":"Published Version","status":"public","publication":"42nd International Symposium on Computational Geometry","corr_author":"1","date_created":"2026-07-13T09:56:38Z","arxiv":1,"acknowledgement":"The authors thank Jakub Leśkiewicz and Bartosz Furmanek for discussions\r\nthat helped improve the paper. Herbert Edelsbrunner: DFG Collaborative Research Center TRR 109, Austrian Science\r\nFund (FWF), grant no. I 02979-N35\r\nMichał Lipiński: European Union’s Horizon 2020 research and innovation programme under the\r\nMarie Skłodowska-Curie Grant Agreement No. 101034413\r\nMarian Mrozek: Polish National Science Center under Opus Grant 2019/35/B/ST1/00874 and Opus\r\nGrant 2025/57/B/ST1/00550","has_accepted_license":"1","OA_type":"gold","ddc":["500"],"scopus_import":"1","_id":"22299","publication_identifier":{"isbn":["9783959774185"],"eissn":["1868-8969"]},"publication_status":"published","intvolume":"       367","OA_place":"publisher","day":"27","article_number":"41:1-41:18","citation":{"chicago":"Edelsbrunner, Herbert, Michał Lipiński, Marian Mrozek, Manuel Soriano Trigueros, and Fedor Zimin. “The Depth Poset under Transpositions in the Filter.” In <i>42nd International Symposium on Computational Geometry</i>, Vol. 367. Schloss Dagstuhl – Leibniz-Zentrum für Informatik, 2026. <a href=\"https://doi.org/10.4230/LIPICS.SOCG.2026.41\">https://doi.org/10.4230/LIPICS.SOCG.2026.41</a>.","ieee":"H. Edelsbrunner, M. Lipiński, M. Mrozek, M. Soriano Trigueros, and F. Zimin, “The depth poset under transpositions in the filter,” in <i>42nd International Symposium on Computational Geometry</i>, New Brunswick, NJ, United States, 2026, vol. 367.","mla":"Edelsbrunner, Herbert, et al. “The Depth Poset under Transpositions in the Filter.” <i>42nd International Symposium on Computational Geometry</i>, vol. 367, 41:1-41:18, Schloss Dagstuhl – Leibniz-Zentrum für Informatik, 2026, doi:<a href=\"https://doi.org/10.4230/LIPICS.SOCG.2026.41\">10.4230/LIPICS.SOCG.2026.41</a>.","ama":"Edelsbrunner H, Lipiński M, Mrozek M, Soriano Trigueros M, Zimin F. The depth poset under transpositions in the filter. In: <i>42nd International Symposium on Computational Geometry</i>. Vol 367. Schloss Dagstuhl – Leibniz-Zentrum für Informatik; 2026. doi:<a href=\"https://doi.org/10.4230/LIPICS.SOCG.2026.41\">10.4230/LIPICS.SOCG.2026.41</a>","ista":"Edelsbrunner H, Lipiński M, Mrozek M, Soriano Trigueros M, Zimin F. 2026. The depth poset under transpositions in the filter. 42nd International Symposium on Computational Geometry. SoCG: Symposium on Computational Geometry, LIPIcs, vol. 367, 41:1-41:18.","apa":"Edelsbrunner, H., Lipiński, M., Mrozek, M., Soriano Trigueros, M., &#38; Zimin, F. (2026). The depth poset under transpositions in the filter. In <i>42nd International Symposium on Computational Geometry</i> (Vol. 367). New Brunswick, NJ, United States: Schloss Dagstuhl – Leibniz-Zentrum für Informatik. <a href=\"https://doi.org/10.4230/LIPICS.SOCG.2026.41\">https://doi.org/10.4230/LIPICS.SOCG.2026.41</a>","short":"H. Edelsbrunner, M. Lipiński, M. Mrozek, M. Soriano Trigueros, F. Zimin, in:, 42nd International Symposium on Computational Geometry, Schloss Dagstuhl – Leibniz-Zentrum für Informatik, 2026."},"volume":367,"doi":"10.4230/LIPICS.SOCG.2026.41","file":[{"access_level":"open_access","file_name":"2026_LIPIcSSoCG_Edelsbrunner.pdf","creator":"dernst","success":1,"date_created":"2026-07-14T06:08:05Z","checksum":"9dfb96ee66985c724b499b0e5888dc8e","date_updated":"2026-07-14T06:08:05Z","file_size":2902144,"file_id":"22329","relation":"main_file","content_type":"application/pdf"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","file_date_updated":"2026-07-14T06:08:05Z","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"ec_funded":1,"das_tickbox":"0","date_published":"2026-05-27T00:00:00Z","author":[{"last_name":"Edelsbrunner","orcid":"0000-0002-9823-6833","first_name":"Herbert","id":"3FB178DA-F248-11E8-B48F-1D18A9856A87","full_name":"Edelsbrunner, Herbert"},{"orcid":"0000-0001-9789-9750","last_name":"Lipiński","first_name":"Michał","id":"dfffb474-4317-11ee-8f5c-fe3fc95a425e","full_name":"Lipiński, Michał"},{"orcid":"0000-0002-0619-6417","last_name":"Mrozek","first_name":"Marian","full_name":"Mrozek, Marian"},{"orcid":"0000-0003-2449-1433","last_name":"Soriano Trigueros","id":"15ebd7cf-15bf-11ee-aebd-bb4bb5121ea8","first_name":"Manuel","full_name":"Soriano Trigueros, Manuel"},{"full_name":"Zimin, Fedor","first_name":"Fedor","id":"afd27eda-91c1-11f0-aad8-c6edbec24c04","last_name":"Zimin"}],"supplementarymaterial":"no","title":"The depth poset under transpositions in the filter","date_updated":"2026-07-14T06:09:32Z","keyword":["Algebraic topology","Lefschetz complexes","persistent homology","vines and vineyards","birth-death pairs","shallow pairs","relations","partial orders","transpositions","Theory of computation → Computational geometry"],"article_processing_charge":"Yes","researchdata_availability":"no","external_id":{"arxiv":["2511.21961"]},"department":[{"_id":"HeEd"},{"_id":"GradSch"}],"publisher":"Schloss Dagstuhl – Leibniz-Zentrum für Informatik","abstract":[{"lang":"eng","text":"The depth poset of a filtered Lefschetz complex reflects the dependencies between the cancellations of different shallow birth-death pairs. Using the fast algorithms for computing the depth poset in [Edelsbrunner et al., 2026] and for updating the persistence diagram under transpositions in [Cohen-Steiner et al., 2006], we give a complete case analysis of how transpositions of cells in the filter affect the depth poset. In addition, we present statistics on the depth poset for random point data and its sensitivity to the transpositions that occur in random straight-line homotopies."}],"project":[{"grant_number":"I02979-N35","name":"Persistence and stability of geometric complexes","call_identifier":"FWF","_id":"2561EBF4-B435-11E9-9278-68D0E5697425"},{"name":"IST-BRIDGE: International postdoctoral program","grant_number":"101034413","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c","call_identifier":"H2020"}],"oa":1,"language":[{"iso":"eng"}],"year":"2026","month":"05"},{"scopus_import":"1","ddc":["530"],"OA_type":"hybrid","has_accepted_license":"1","acknowledgement":"The authors acknowledge discussions with Lorenzo\r\nCaprini. A.G., M.P., and A.P. acknowledge funding from the\r\nItalianMinistero dell’Università e della Ricerca under the program\r\nPRIN 2022 (“Re-ranking of the final lists”), Grants No.\r\n2022KWTEB7 with CUP No. B53C24006470006. L.A. acknowledges\r\nfunding from the ItalianMinistero dell’Università\r\ne della Ricerca under the program PRIN 2020, Grant No.\r\n2020PFCXPE.","intvolume":"       113","day":"18","OA_place":"publisher","publication_status":"published","publication_identifier":{"issn":["2470-0045"],"eissn":["2470-0053"]},"_id":"22307","status":"public","publication":"Physical Review E","oa_version":"Published Version","type":"journal_article","date_created":"2026-07-13T10:53:06Z","arxiv":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"date_created":"2026-07-14T06:58:35Z","success":1,"file_name":"2026_PhysicalReviewE_Musacchio.pdf","creator":"dernst","access_level":"open_access","relation":"main_file","content_type":"application/pdf","file_id":"22332","date_updated":"2026-07-14T06:58:35Z","file_size":1836050,"checksum":"f029efcf6dd51e10e3bc7623b5365da6"}],"file_date_updated":"2026-07-14T06:58:35Z","quality_controlled":"1","volume":113,"citation":{"ieee":"M. Musacchio, M. Felber, M. Paoluzzi, A. Gnoli, A. Puglisi, and L. Angelani, “Fluidization induced by magnetic interactions in confined active matter,” <i>Physical Review E</i>, vol. 113, no. 5. American Physical Society, 2026.","chicago":"Musacchio, Marco, Markus Felber, Matteo Paoluzzi, Andrea Gnoli, Andrea Puglisi, and Luca Angelani. “Fluidization Induced by Magnetic Interactions in Confined Active Matter.” <i>Physical Review E</i>. American Physical Society, 2026. <a href=\"https://doi.org/10.1103/hylm-ljlf\">https://doi.org/10.1103/hylm-ljlf</a>.","ista":"Musacchio M, Felber M, Paoluzzi M, Gnoli A, Puglisi A, Angelani L. 2026. Fluidization induced by magnetic interactions in confined active matter. Physical Review E. 113(5), 055413.","short":"M. Musacchio, M. Felber, M. Paoluzzi, A. Gnoli, A. Puglisi, L. Angelani, Physical Review E 113 (2026).","apa":"Musacchio, M., Felber, M., Paoluzzi, M., Gnoli, A., Puglisi, A., &#38; Angelani, L. (2026). Fluidization induced by magnetic interactions in confined active matter. <i>Physical Review E</i>. American Physical Society. <a href=\"https://doi.org/10.1103/hylm-ljlf\">https://doi.org/10.1103/hylm-ljlf</a>","ama":"Musacchio M, Felber M, Paoluzzi M, Gnoli A, Puglisi A, Angelani L. Fluidization induced by magnetic interactions in confined active matter. <i>Physical Review E</i>. 2026;113(5). doi:<a href=\"https://doi.org/10.1103/hylm-ljlf\">10.1103/hylm-ljlf</a>","mla":"Musacchio, Marco, et al. “Fluidization Induced by Magnetic Interactions in Confined Active Matter.” <i>Physical Review E</i>, vol. 113, no. 5, 055413, American Physical Society, 2026, doi:<a href=\"https://doi.org/10.1103/hylm-ljlf\">10.1103/hylm-ljlf</a>."},"article_number":"055413","article_type":"original","doi":"10.1103/hylm-ljlf","date_updated":"2026-07-14T07:00:17Z","title":"Fluidization induced by magnetic interactions in confined active matter","issue":"5","supplementarymaterial":"no","author":[{"last_name":"Musacchio","first_name":"Marco","full_name":"Musacchio, Marco"},{"full_name":"Felber, Markus","last_name":"Felber","first_name":"Markus","id":"c12d7e3a-4e8f-11ef-ad48-ffba54b8aa10"},{"full_name":"Paoluzzi, Matteo","last_name":"Paoluzzi","first_name":"Matteo"},{"last_name":"Gnoli","first_name":"Andrea","full_name":"Gnoli, Andrea"},{"full_name":"Puglisi, Andrea","last_name":"Puglisi","first_name":"Andrea"},{"last_name":"Angelani","first_name":"Luca","full_name":"Angelani, Luca"}],"date_published":"2026-05-18T00:00:00Z","department":[{"_id":"ScWa"},{"_id":"GradSch"}],"external_id":{"arxiv":["2511.21472"]},"researchdata_availability":"no","article_processing_charge":"Yes (in subscription journal)","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"oa":1,"year":"2026","month":"05","language":[{"iso":"eng"}],"dataavailabilitystatement":"The data that support the findings of this article are not\r\npublicly available upon publication because it is not technically\r\nfeasible and/or the cost of preparing, depositing, and\r\nhosting the data would be prohibitive within the terms of this\r\nresearch project. The data are available from the authors upon\r\nreasonable request.","abstract":[{"lang":"eng","text":"We investigate magnetic active matter in confined geometries using both experiments with magnetic toy robots, Hexbugs, and simulations of elongated magnetic active Brownian particles in circular domains. Standard active particles tend to accumulate at boundaries, forming clusters even at relatively low densities. In the presence of magnetic interactions, we provide evidence for a  effect that inhibits clustering and shifts its onset to higher packing fractions. Moreover, magnetic dipolar interactions give rise to collective behaviors such as train-like formations, rotating pairs, and rotating clusters."}],"publisher":"American Physical Society","PlanS_conform":"1"},{"OA_place":"repository","day":"01","publication_status":"published","_id":"22302","scopus_import":"1","OA_type":"green","date_created":"2026-07-13T10:48:03Z","arxiv":1,"corr_author":"1","publication":"Proceedings of the 19th Conference of the European Chapter of the Association for Computational Linguistics","oa_version":"Preprint","status":"public","conference":{"name":"EACL:  Conference of the European Chapter of the Association for Computational Linguistics","start_date":"2026-03-24","location":"Rabat, Morocco","end_date":"2026-03-29"},"type":"conference","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","doi":"10.18653/v1/2026.eacl-long.301","citation":{"chicago":"Pankratov, Sergei, and Dan-Adrian Alistarh. “Speculative Decoding Speed-of-Light: Optimal Lower Bounds via Branching Random Walks.” In <i>Proceedings of the 19th Conference of the European Chapter of the Association for Computational Linguistics</i>, 6404–6418. Association for Computational Linguistics, 2026. <a href=\"https://doi.org/10.18653/v1/2026.eacl-long.301\">https://doi.org/10.18653/v1/2026.eacl-long.301</a>.","ieee":"S. Pankratov and D.-A. Alistarh, “Speculative decoding speed-of-light: Optimal lower bounds via branching random walks,” in <i>Proceedings of the 19th Conference of the European Chapter of the Association for Computational Linguistics</i>, Rabat, Morocco, 2026, pp. 6404–6418.","ama":"Pankratov S, Alistarh D-A. Speculative decoding speed-of-light: Optimal lower bounds via branching random walks. In: <i>Proceedings of the 19th Conference of the European Chapter of the Association for Computational Linguistics</i>. Association for Computational Linguistics; 2026:6404–6418. doi:<a href=\"https://doi.org/10.18653/v1/2026.eacl-long.301\">10.18653/v1/2026.eacl-long.301</a>","short":"S. Pankratov, D.-A. Alistarh, in:, Proceedings of the 19th Conference of the European Chapter of the Association for Computational Linguistics, Association for Computational Linguistics, 2026, pp. 6404–6418.","apa":"Pankratov, S., &#38; Alistarh, D.-A. (2026). Speculative decoding speed-of-light: Optimal lower bounds via branching random walks. In <i>Proceedings of the 19th Conference of the European Chapter of the Association for Computational Linguistics</i> (pp. 6404–6418). Rabat, Morocco: Association for Computational Linguistics. <a href=\"https://doi.org/10.18653/v1/2026.eacl-long.301\">https://doi.org/10.18653/v1/2026.eacl-long.301</a>","ista":"Pankratov S, Alistarh D-A. 2026. Speculative decoding speed-of-light: Optimal lower bounds via branching random walks. Proceedings of the 19th Conference of the European Chapter of the Association for Computational Linguistics. EACL:  Conference of the European Chapter of the Association for Computational Linguistics, 6404–6418.","mla":"Pankratov, Sergei, and Dan-Adrian Alistarh. “Speculative Decoding Speed-of-Light: Optimal Lower Bounds via Branching Random Walks.” <i>Proceedings of the 19th Conference of the European Chapter of the Association for Computational Linguistics</i>, Association for Computational Linguistics, 2026, pp. 6404–6418, doi:<a href=\"https://doi.org/10.18653/v1/2026.eacl-long.301\">10.18653/v1/2026.eacl-long.301</a>."},"department":[{"_id":"DaAl"},{"_id":"GradSch"}],"external_id":{"arxiv":["2512.11718"]},"researchdata_availability":"no","article_processing_charge":"No","title":"Speculative decoding speed-of-light: Optimal lower bounds via branching random walks","date_updated":"2026-07-14T06:18:11Z","author":[{"first_name":"Sergei","id":"f773bf05-72ef-11ef-b75a-a383d22f454b","last_name":"Pankratov","full_name":"Pankratov, Sergei"},{"first_name":"Dan-Adrian","id":"4A899BFC-F248-11E8-B48F-1D18A9856A87","last_name":"Alistarh","orcid":"0000-0003-3650-940X","full_name":"Alistarh, Dan-Adrian"}],"supplementarymaterial":"no","date_published":"2026-04-01T00:00:00Z","das_tickbox":"0","page":"6404–6418","month":"04","year":"2026","language":[{"iso":"eng"}],"abstract":[{"lang":"eng","text":"Speculative generation has emerged as a promising technique to accelerate inference in large language models (LLMs) by leveraging parallelism to verify multiple draft tokens simultaneously. However, the fundamental limits on the achievable speedup remain poorly understood. In this work, we establish the first “tight” lower bounds on the runtime of any deterministic speculative generation algorithm. This is achieved by drawing a parallel between the token generation process and branching random walks, which allows us to analyze the optimal draft tree selection problem. We prove, under basic assumptions, that the expected number of tokens successfully predicted per speculative iteration is bounded as \\mathbb{E}[X] ≤ (𝜇 + 𝜇(2))log(B )/𝜇2 + O(1), where B is the verifier’s batch size, 𝜇 is the expected entropy of the verifier’s output distribution, and 𝜇(2) is this entropy’s second moment. This result provides new insights into the limits of parallel token generation, and could guide the design of future speculative decoding systems. Empirical evaluations on Llama models validate our theoretical predictions, confirming the tightness of our bounds in practical settings."}],"publisher":"Association for Computational Linguistics"},{"oa":1,"language":[{"iso":"eng"}],"dataavailabilitystatement":"The MATLAB code for image analysis, and the full model code, including all parameter values\r\nand condition-specific settings, are available on GitHub at https://github.com/uday2607/EVL-tension-homeostasis.git.","year":"2026","month":"07","publisher":"Institute of Science and Technology Austria","abstract":[{"lang":"eng","text":"Tissue tension is a key determinant of tissue shape, and its regulation is essential for both morphogenesis and the maintenance of tissue integrity. During zebrafish embryogenesis, the enveloping layer (EVL) – an epithelial monolayer covering the blastoderm – undergoes extensive spreading that is driven by pulling forces exerted at its margin and more than doubles its surface area. Yet whether and how the EVL actively regulates its tissue tension during this process remains unclear. Here, we show that the EVL maintains constant tissue tension while spreading, and that it achieves this by reducing apical cell contractility in response to the same pulling forces that drive its spreading. We identify a mechanosensitive pathway underlying this response, mediated by the scaffold/adaptor protein Kibra regulating the activity of atypical protein kinase C (aPKC) at the apical domain of EVL cells. Under low mechanical stretch, Kibra forms condensates at the base of actin-based apical projections, where it activates Myosin II to increase apical contractility through aPKC downregulation. As mechanical stretch increases, apical projections disassemble, Kibra condensates dissolve, and aPKC activity rises. Elevated aPKC activity in turn reduces apical contractility by reducing Myosin II activity, thereby maintaining constant tissue tension despite increased mechanical stretch. Together, these findings reveal a mechanosensitive mechanism that enables robust adaptation of tissue tension to changing mechanical stretch, ensuring efficient tissue spreading and morphogenesis."}],"project":[{"grant_number":"PAT 5044023","name":"Keratins in epithelial tissue spreading","_id":"8f060199-16d5-11f0-9cad-f3253b266c46"},{"name":"Mechanosensitive signaling activation in the crosstalk between mechanical force and tissuefluidity","grant_number":"LTF 16-2022","_id":"34dd7f3b-11ca-11ed-8bc3-856f2c87f5da"}],"author":[{"first_name":"Naoya","id":"5299a9ce-7679-11eb-a7bc-d1e62b936307","last_name":"Hino","full_name":"Hino, Naoya"},{"id":"e3b3eda7-fd4d-11eb-8fd8-c40af7a478b1","first_name":"Tushna","last_name":"Kapoor","full_name":"Kapoor, Tushna"},{"first_name":"Uday R","id":"bb4a0dc4-32c9-11ee-b5ce-a97ceedd5924","last_name":"Gubbala","full_name":"Gubbala, Uday R"},{"full_name":"Hannezo, Edouard B","first_name":"Edouard B","id":"3A9DB764-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0001-6005-1561","last_name":"Hannezo"},{"full_name":"Heisenberg, Carl-Philipp J","last_name":"Heisenberg","orcid":"0000-0002-0912-4566","id":"39427864-F248-11E8-B48F-1D18A9856A87","first_name":"Carl-Philipp J"}],"supplementarymaterial":"yes","date_published":"2026-07-14T00:00:00Z","date_updated":"2026-07-14T07:07:41Z","title":"Apical domain mechanosensation regulates tissue tension homeostasis","keyword":["Epithelial spreading","tissue tension","mechanosensation","aPKC","Kibra","zebrafish"],"researchdata_availability":"yes","article_processing_charge":"No","department":[{"_id":"CaHe"},{"_id":"EdHa"},{"_id":"GradSch"}],"tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"das_tickbox":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"access_level":"open_access","date_created":"2026-07-13T09:16:20Z","success":1,"file_name":"Main_text_and_figures.pdf","creator":"nhino","date_updated":"2026-07-13T09:16:20Z","file_size":12477675,"checksum":"66444afd243dce7d383d52d44e8d34a4","relation":"main_file","content_type":"application/pdf","file_id":"22283"},{"file_id":"22284","content_type":"application/pdf","relation":"main_file","checksum":"90bceb34de64ec792c5de117f0890d05","file_size":4545901,"date_updated":"2026-07-13T09:16:25Z","creator":"nhino","file_name":"Supplementary_figures.pdf","success":1,"date_created":"2026-07-13T09:16:25Z","access_level":"open_access"},{"success":1,"date_created":"2026-07-13T09:16:28Z","creator":"nhino","file_name":"Supplementary_Video1.mp4","access_level":"open_access","content_type":"video/mp4","relation":"main_file","file_id":"22285","file_size":10349451,"date_updated":"2026-07-13T09:16:28Z","checksum":"9d9ab89c372142f2ffb6c8c625334d7f"}],"acknowledged_ssus":[{"_id":"Bio"},{"_id":"LifeSc"},{"_id":"EM-Fac"}],"file_date_updated":"2026-07-13T09:16:28Z","citation":{"chicago":"Hino, Naoya, Tushna Kapoor, Uday R Gubbala, Edouard B Hannezo, and Carl-Philipp J Heisenberg. “Apical Domain Mechanosensation Regulates Tissue Tension Homeostasis.” Institute of Science and Technology Austria, n.d.","ieee":"N. Hino, T. Kapoor, U. R. Gubbala, E. B. Hannezo, and C.-P. J. Heisenberg, “Apical domain mechanosensation regulates tissue tension homeostasis.” Institute of Science and Technology Austria.","ama":"Hino N, Kapoor T, Gubbala UR, Hannezo EB, Heisenberg C-PJ. Apical domain mechanosensation regulates tissue tension homeostasis.","apa":"Hino, N., Kapoor, T., Gubbala, U. R., Hannezo, E. B., &#38; Heisenberg, C.-P. J. (n.d.). Apical domain mechanosensation regulates tissue tension homeostasis. Institute of Science and Technology Austria.","ista":"Hino N, Kapoor T, Gubbala UR, Hannezo EB, Heisenberg C-PJ. Apical domain mechanosensation regulates tissue tension homeostasis.","short":"N. Hino, T. Kapoor, U.R. Gubbala, E.B. Hannezo, C.-P.J. Heisenberg, (n.d.).","mla":"Hino, Naoya, et al. <i>Apical Domain Mechanosensation Regulates Tissue Tension Homeostasis</i>. Institute of Science and Technology Austria."},"ddc":["570"],"OA_type":"green","has_accepted_license":"1","acknowledgement":"We thank all members of the Heisenberg group for discussion and feedback on the manuscript, and the Imaging and Optics Facility, the Life Science Support Facility and the Electron Microscopy Facility of the Institute of Science and Technology Austria (ISTA) for their continued support. We are grateful to M. Sonawane (Tata Institute of Fundamental Research, India) for providing the pCS2-HA-aPKC (PKCι)-V260F (DN) and pCS2-HA-aPKC (PKCι)-A122E (CA) plasmids, and to I. Mayer for the discussion. Molecular graphics and analyses were performed with UCSF ChimeraX, developed by the Resource for Biocomputing, Visualization, and Informatics at the University of California, San Francisco, with support from National Institutes of Health R01-GM129325 and the Office of Cyber Infrastructure and Computational Biology, National Institute of Allergy and Infectious Diseases. This research was funded in whole or in part by the Austrian Science Fund (FWF; grant no. PAT5044023) to C.-P.H., and by a JSPS Overseas Research Fellowship and an EMBO Postdoctoral Fellowship (ALTF 16-2022) to N.H.","_id":"22276","day":"14","OA_place":"publisher","publication_status":"draft","type":"preprint","status":"public","oa_version":"Preprint","corr_author":"1","related_material":{"record":[{"relation":"earlier_version","status":"public","id":"21864"}]},"date_created":"2026-07-13T09:03:26Z"},{"oa":1,"month":"06","year":"2026","page":"1-27","language":[{"iso":"eng"}],"abstract":[{"text":"We study the problem of continually releasing statistics of an evolving dataset under differential privacy. In the event-level setting, we show the first polynomial lower bounds on the additive error for insertions-only graph problems such as maximum matching, degree histogram and k-core number computation. These results represent an exponential improvement on the polylogarithmic lower bounds of Fichtenberger, Henzinger and Ost [ESA 2021] for the former two problems, and are the first lower bounds in the continual release setting for the latter problem. Our results run counter to the intuition that the difference between insertions-only vs fully dynamic updates causes the gap between polylogarithmic and polynomial additive error. Indeed, we show that for estimating the size of the maximum matching or k-core number of a vertex, allowing small multiplicative approximations is what brings the additive error down to polylogarithmic. We complement these results with improved upper bounds on the additive error when no multiplicative approximation is allowed.\r\nBeyond graphs, our techniques also show that polynomial additive error is unavoidable for the Simultaneous Norm Estimation problem in the insertions-only setting. When multiplicative approximations are allowed, we circumvent this lower bound by giving the first continual mechanism with polylogarithmic additive error under (1 + ζ) multiplicative approximations, for any ζ > 0, for estimating all monotone symmetric norms simultaneously.\r\nIn the item-level setting, we show polynomial lower bounds on the product of the multiplicative and the additive error of continual mechanisms for a large range of graph problems. To the best of our knowledge, these are the first lower bounds shown for any differentially private mechanism under continual release with multiplicative error. To obtain these results, we prove a new lower bound on the product of multiplicative and additive error for the 1-Way-Marginals problem, and give reductions from 1-Way-Marginals to our desired graph problems. This generalizes the prior results of Hardt and Talwar [STOC 2010] and Bun, Ullman and Vadhan [STOC 2014, SIAM J. Comput. 2018], who gave lower bounds on the additive error for the special case of mechanisms with no multiplicative error.","lang":"eng"}],"publisher":"Association for Computing Machinery","PlanS_conform":"1","project":[{"grant_number":"101019564","name":"The design and evaluation of modern fully dynamic data structures","_id":"bd9ca328-d553-11ed-ba76-dc4f890cfe62","call_identifier":"H2020"}],"date_updated":"2026-07-16T09:30:31Z","title":"Improved lower bounds for privacy under continual release","issue":"2","author":[{"full_name":"Aryanfard, Bardiya","id":"1e8f4084-31df-11ee-b195-f706b4b77091","first_name":"Bardiya","last_name":"Aryanfard"},{"full_name":"Henzinger, Monika H","id":"540c9bbd-f2de-11ec-812d-d04a5be85630","first_name":"Monika H","orcid":"0000-0002-5008-6530","last_name":"Henzinger"},{"id":"f8e48cf0-b0ff-11ed-b0e9-b4c35598f964","first_name":"David","last_name":"Saulpic","full_name":"Saulpic, David"},{"last_name":"Sricharan","first_name":"A. R.","full_name":"Sricharan, A. R."}],"supplementarymaterial":"no","date_published":"2026-06-01T00:00:00Z","department":[{"_id":"MoHe"},{"_id":"GradSch"}],"external_id":{"arxiv":["2512.15981"]},"researchdata_availability":"no","article_processing_charge":"Yes","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"das_tickbox":"0","ec_funded":1,"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"relation":"main_file","content_type":"application/pdf","file_id":"22349","date_updated":"2026-07-16T09:29:08Z","file_size":934963,"checksum":"21a48a620e415a31a3874077c55bc6c3","date_created":"2026-07-16T09:29:08Z","success":1,"file_name":"2026_ACMMgmtData_Aryanfard.pdf","creator":"dernst","access_level":"open_access"}],"file_date_updated":"2026-07-16T09:29:08Z","quality_controlled":"1","citation":{"ieee":"B. Aryanfard, M. Henzinger, D. Saulpic, and A. R. Sricharan, “Improved lower bounds for privacy under continual release,” <i>Proceedings of the ACM on Management of Data</i>, vol. 4, no. 2. Association for Computing Machinery, pp. 1–27, 2026.","chicago":"Aryanfard, Bardiya, Monika Henzinger, David Saulpic, and A. R. Sricharan. “Improved Lower Bounds for Privacy under Continual Release.” <i>Proceedings of the ACM on Management of Data</i>. Association for Computing Machinery, 2026. <a href=\"https://doi.org/10.1145/3801903\">https://doi.org/10.1145/3801903</a>.","apa":"Aryanfard, B., Henzinger, M., Saulpic, D., &#38; Sricharan, A. R. (2026). Improved lower bounds for privacy under continual release. <i>Proceedings of the ACM on Management of Data</i>. Association for Computing Machinery. <a href=\"https://doi.org/10.1145/3801903\">https://doi.org/10.1145/3801903</a>","short":"B. Aryanfard, M. Henzinger, D. Saulpic, A.R. Sricharan, Proceedings of the ACM on Management of Data 4 (2026) 1–27.","ista":"Aryanfard B, Henzinger M, Saulpic D, Sricharan AR. 2026. Improved lower bounds for privacy under continual release. Proceedings of the ACM on Management of Data. 4(2), 1–27.","ama":"Aryanfard B, Henzinger M, Saulpic D, Sricharan AR. Improved lower bounds for privacy under continual release. <i>Proceedings of the ACM on Management of Data</i>. 2026;4(2):1-27. doi:<a href=\"https://doi.org/10.1145/3801903\">10.1145/3801903</a>","mla":"Aryanfard, Bardiya, et al. “Improved Lower Bounds for Privacy under Continual Release.” <i>Proceedings of the ACM on Management of Data</i>, vol. 4, no. 2, Association for Computing Machinery, 2026, pp. 1–27, doi:<a href=\"https://doi.org/10.1145/3801903\">10.1145/3801903</a>."},"volume":4,"article_type":"original","doi":"10.1145/3801903","scopus_import":"1","ddc":["000"],"acknowledgement":"Bardiya Aryanfard and Monika Henzinger were supported by the European Research Council (ERC)\r\nunder the European Union’s Horizon 2020 research and innovation programme (Grant agreement\r\nNo. 101019564). For open access purposes, the author has applied a CC BY public copyright\r\nlicense to any author-accepted manuscript version arising from this submission. Funded by the\r\nEuropean union. Views and opinions expressed are however those of the author(s) only and do\r\nnot necessarily reflect those of the European Union or the European Research Council Executive\r\nAgency. Neither the European Union nor the granting authority can be held responsible for them","OA_type":"gold","has_accepted_license":"1","OA_place":"publisher","day":"01","intvolume":"         4","publication_status":"published","publication_identifier":{"issn":["2836-6573"]},"_id":"22322","oa_version":"Published Version","publication":"Proceedings of the ACM on Management of Data","status":"public","type":"journal_article","arxiv":1,"date_created":"2026-07-14T05:33:58Z","corr_author":"1"},{"scopus_import":"1","ddc":["530"],"acknowledgement":"This work was supported in part\r\nby European Research Council No. ERC-2023-SyG\r\n“DynaTrans” Grant No. 101118866 (G. T.). We thank\r\nPieter Rein ten Wolde and Vahe Galstyan for stimulating\r\ndiscussions.","OA_type":"hybrid","has_accepted_license":"1","intvolume":"       137","OA_place":"publisher","day":"15","publication_status":"published","publication_identifier":{"issn":["0031-9007"],"eissn":[" 1079-7114"]},"_id":"22326","publication":"Physical Review Letters","oa_version":"Published Version","status":"public","type":"journal_article","date_created":"2026-07-14T05:38:28Z","corr_author":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","file":[{"file_id":"22352","content_type":"application/pdf","relation":"main_file","checksum":"28861d31d0f6cf541aaca04faaed1767","file_size":2550345,"date_updated":"2026-07-16T09:54:55Z","creator":"dernst","file_name":"2026_PhysicalReviewLetters_Zhang.pdf","date_created":"2026-07-16T09:54:55Z","success":1,"access_level":"open_access"}],"file_date_updated":"2026-07-16T09:54:55Z","quality_controlled":"1","citation":{"mla":"Zhang, Chen Y., et al. “Nonlocal Decoding of Positional and Correlational Information during Development.” <i>Physical Review Letters</i>, vol. 137, 038401, American Physical Society, 2026, doi:<a href=\"https://doi.org/10.1103/mbjk-v4ym\">10.1103/mbjk-v4ym</a>.","short":"C.Y. Zhang, P. Mateu Hoyos, D. Brückner, G. Tkačik, Physical Review Letters 137 (2026).","ista":"Zhang CY, Mateu Hoyos P, Brückner D, Tkačik G. 2026. Nonlocal decoding of positional and correlational information during development. Physical Review Letters. 137, 038401.","apa":"Zhang, C. Y., Mateu Hoyos, P., Brückner, D., &#38; Tkačik, G. (2026). Nonlocal decoding of positional and correlational information during development. <i>Physical Review Letters</i>. American Physical Society. <a href=\"https://doi.org/10.1103/mbjk-v4ym\">https://doi.org/10.1103/mbjk-v4ym</a>","ama":"Zhang CY, Mateu Hoyos P, Brückner D, Tkačik G. Nonlocal decoding of positional and correlational information during development. <i>Physical Review Letters</i>. 2026;137. doi:<a href=\"https://doi.org/10.1103/mbjk-v4ym\">10.1103/mbjk-v4ym</a>","ieee":"C. Y. Zhang, P. Mateu Hoyos, D. Brückner, and G. Tkačik, “Nonlocal decoding of positional and correlational information during development,” <i>Physical Review Letters</i>, vol. 137. American Physical Society, 2026.","chicago":"Zhang, Chen Y, Pablo Mateu Hoyos, David Brückner, and Gašper Tkačik. “Nonlocal Decoding of Positional and Correlational Information during Development.” <i>Physical Review Letters</i>. American Physical Society, 2026. <a href=\"https://doi.org/10.1103/mbjk-v4ym\">https://doi.org/10.1103/mbjk-v4ym</a>."},"volume":137,"article_number":"038401","article_type":"original","doi":"10.1103/mbjk-v4ym","date_updated":"2026-07-16T09:58:04Z","title":"Nonlocal decoding of positional and correlational information during development","supplementarymaterial":"no","author":[{"id":"81b43fb8-c9d5-11ef-bf68-ade532a1f204","first_name":"Chen Y","last_name":"Zhang","full_name":"Zhang, Chen Y"},{"full_name":"Mateu Hoyos, Pablo","id":"50b236c7-50c1-11ef-bb9a-a2375694f8b5","first_name":"Pablo","last_name":"Mateu Hoyos"},{"last_name":"Brückner","orcid":"0000-0001-7205-2975","first_name":"David","id":"e1e86031-6537-11eb-953a-f7ab92be508d","full_name":"Brückner, David"},{"full_name":"Tkačik, Gašper","id":"3D494DCA-F248-11E8-B48F-1D18A9856A87","first_name":"Gašper","orcid":"0000-0002-6699-1455","last_name":"Tkačik"}],"date_published":"2026-07-15T00:00:00Z","department":[{"_id":"GaTk"},{"_id":"EdHa"},{"_id":"GradSch"}],"article_processing_charge":"Yes (via OA deal)","researchdata_availability":"no","tmp":{"image":"/images/cc_by.png","short":"CC BY (4.0)","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"das_tickbox":"1","oa":1,"year":"2026","month":"07","language":[{"iso":"eng"}],"dataavailabilitystatement":"Code to evaluate PI, to run algorithmic implementations of ALP and RLP decoding, and to\r\nperform simulations is publicly available at https://github.com/alex-chenyi-zhang/nonlocdec_pici.","abstract":[{"text":"In many developmental systems, cells differentiate into a tissue by reading out morphogen concentration fields, a process fundamentally limited by noise. How much can the precision of this process be improved by nonlocal information, e.g., via cell-cell communication? Using a Bayes-optimal framework, we show that positional inference depends crucially on morphogen spatial correlations and on the \"structural prior\" that encodes the geometry of the cellular lattice performing the readout, thereby determining what a cell can reliably assume about the position of its neighbors when interpreting nonlocal morphogen signals. We derive upper bounds on positional information gain due to nonlocal readout and identify signal processing algorithms that approximate optimal positional inference, as well as simple chemical reaction schemes which implement such algorithms. Our theory suggests that correlational information can be exploited to significantly enhance developmental precision.","lang":"eng"}],"publisher":"American Physical Society","PlanS_conform":"1","project":[{"_id":"7bfe6a29-9f16-11ee-852c-c0da5e2045d9","grant_number":"101118866","name":"Transcription in 4D: the dynamic interplay between chromatin architecture and gene expression in developing pseudo-embryos"}]},{"page":"59","year":"2026","month":"06","language":[{"iso":"eng"}],"publisher":"Institute of Science and Technology Austria","degree_awarded":"PhD","project":[{"_id":"9B8F7476-BA93-11EA-9121-9846C619BF3A","name":"HighTE: The Werner Siemens Laboratory for the High Throughput Discovery of Semiconductors for Waste Heat Recovery"}],"title":"Unraveling the origin and evolution of defects to enable advanced thermoelectric performance","date_updated":"2026-07-17T07:09:42Z","author":[{"full_name":"Kleinhanns, Tobias","last_name":"Kleinhanns","orcid":"0000-0003-1537-7436","first_name":"Tobias","id":"8BD9DE16-AB3C-11E9-9C8C-2A03E6697425"}],"date_published":"2026-06-18T00:00:00Z","department":[{"_id":"GradSch"},{"_id":"MaIb"}],"article_processing_charge":"No","das_tickbox":"1","user_id":"8b945eb4-e2f2-11eb-945a-df72226e66a9","file":[{"relation":"source_file","content_type":"application/vnd.openxmlformats-officedocument.wordprocessingml.document","file_id":"22226","date_updated":"2026-06-30T09:17:15Z","file_size":15658266,"checksum":"3df7e865a7d1da8972ccd8acb8b4c16c","date_created":"2026-06-30T09:17:15Z","file_name":"2026_Kleinhanns_Tobias_Thesis_Source_File.docx","creator":"tkleinha","access_level":"closed"},{"file_size":9909375,"embargo_to":"open_access","date_updated":"2026-07-01T07:35:17Z","checksum":"40ec279272a963636ff29c964032dcba","content_type":"application/pdf","relation":"main_file","file_id":"22232","access_level":"closed","date_created":"2026-07-01T07:35:17Z","creator":"tkleinha","embargo":"2026-12-18","file_name":"2026_Kleinhanns_Tobias_Thesis_Main_File_A4.pdf"}],"file_date_updated":"2026-07-01T07:35:17Z","citation":{"chicago":"Kleinhanns, Tobias. “Unraveling the Origin and Evolution of Defects to Enable Advanced Thermoelectric Performance.” Institute of Science and Technology Austria, 2026. <a href=\"https://doi.org/10.15479/AT-ISTA-22017\">https://doi.org/10.15479/AT-ISTA-22017</a>.","ieee":"T. Kleinhanns, “Unraveling the origin and evolution of defects to enable advanced thermoelectric performance,” Institute of Science and Technology Austria, 2026.","ama":"Kleinhanns T. Unraveling the origin and evolution of defects to enable advanced thermoelectric performance. 2026. doi:<a href=\"https://doi.org/10.15479/AT-ISTA-22017\">10.15479/AT-ISTA-22017</a>","ista":"Kleinhanns T. 2026. Unraveling the origin and evolution of defects to enable advanced thermoelectric performance. Institute of Science and Technology Austria.","short":"T. Kleinhanns, Unraveling the Origin and Evolution of Defects to Enable Advanced Thermoelectric Performance, Institute of Science and Technology Austria, 2026.","apa":"Kleinhanns, T. (2026). <i>Unraveling the origin and evolution of defects to enable advanced thermoelectric performance</i>. Institute of Science and Technology Austria. <a href=\"https://doi.org/10.15479/AT-ISTA-22017\">https://doi.org/10.15479/AT-ISTA-22017</a>","mla":"Kleinhanns, Tobias. <i>Unraveling the Origin and Evolution of Defects to Enable Advanced Thermoelectric Performance</i>. Institute of Science and Technology Austria, 2026, doi:<a href=\"https://doi.org/10.15479/AT-ISTA-22017\">10.15479/AT-ISTA-22017</a>."},"doi":"10.15479/AT-ISTA-22017","ddc":["546","530"],"has_accepted_license":"1","day":"18","OA_place":"publisher","publication_status":"published","doi_confirm":"1","supervisor":[{"full_name":"Ibáñez, Maria","last_name":"Ibáñez","orcid":"0000-0001-5013-2843","id":"43C61214-F248-11E8-B48F-1D18A9856A87","first_name":"Maria"}],"publication_identifier":{"issn":["2663-337X"],"isbn":["978-3-99078-081-7"]},"_id":"22017","status":"public","oa_version":"Published Version","type":"dissertation","alternative_title":["ISTA Thesis"],"date_created":"2026-06-18T08:00:03Z","related_material":{"record":[{"id":"15182","status":"public","relation":"part_of_dissertation"},{"id":"20326","status":"public","relation":"part_of_dissertation"},{"relation":"part_of_dissertation","status":"public","id":"12237"}]},"corr_author":"1"},{"type":"dissertation","alternative_title":["ISTA Thesis"],"status":"public","oa_version":"Published Version","related_material":{"record":[{"status":"public","id":"22105","relation":"part_of_dissertation"},{"relation":"part_of_dissertation","id":"12675","status":"public"},{"status":"public","id":"21777","relation":"part_of_dissertation"},{"id":"12114","status":"public","relation":"part_of_dissertation"}]},"corr_author":"1","date_created":"2026-07-14T08:08:51Z","ddc":["572"],"has_accepted_license":"1","acknowledgement":"During the work on this thesis, I was the recipient of a DOC Fellowship of the Austrian\r\nAcademy of Sciences at the Institute of Science and Technology Austria (grant no. PR10660EAW01).","publication_identifier":{"isbn":["978-3-99078-084-8"],"issn":["2663-337X"]},"_id":"22334","day":"13","OA_place":"publisher","doi_confirm":"1","publication_status":"published","supervisor":[{"full_name":"Schanda, Paul","last_name":"Schanda","orcid":"0000-0002-9350-7606","first_name":"Paul","id":"7B541462-FAF6-11E9-A490-E8DFE5697425"}],"citation":{"chicago":"Becker, Lea Marie. “Exploring Protein Dynamics Using Specific Labeling Approaches for Solid-State MAS NMR.” Institute of Science and Technology Austria, 2026. <a href=\"https://doi.org/10.15479/AT-ISTA-22334\">https://doi.org/10.15479/AT-ISTA-22334</a>.","ieee":"L. M. Becker, “Exploring protein dynamics using specific labeling approaches for solid-state MAS NMR,” Institute of Science and Technology Austria, 2026.","mla":"Becker, Lea Marie. <i>Exploring Protein Dynamics Using Specific Labeling Approaches for Solid-State MAS NMR</i>. Institute of Science and Technology Austria, 2026, doi:<a href=\"https://doi.org/10.15479/AT-ISTA-22334\">10.15479/AT-ISTA-22334</a>.","ama":"Becker LM. Exploring protein dynamics using specific labeling approaches for solid-state MAS NMR. 2026. doi:<a href=\"https://doi.org/10.15479/AT-ISTA-22334\">10.15479/AT-ISTA-22334</a>","ista":"Becker LM. 2026. Exploring protein dynamics using specific labeling approaches for solid-state MAS NMR. Institute of Science and Technology Austria.","apa":"Becker, L. M. (2026). <i>Exploring protein dynamics using specific labeling approaches for solid-state MAS NMR</i>. Institute of Science and Technology Austria. <a href=\"https://doi.org/10.15479/AT-ISTA-22334\">https://doi.org/10.15479/AT-ISTA-22334</a>","short":"L.M. Becker, Exploring Protein Dynamics Using Specific Labeling Approaches for Solid-State MAS NMR, Institute of Science and Technology Austria, 2026."},"doi":"10.15479/AT-ISTA-22334","user_id":"8b945eb4-e2f2-11eb-945a-df72226e66a9","file":[{"access_level":"closed","creator":"lbecker","file_name":"2026_Becker_Lea_source_files.zip","date_created":"2026-07-16T09:17:08Z","checksum":"8b85114eff543916c0e1445cd2189555","file_size":99472908,"date_updated":"2026-07-16T09:17:08Z","file_id":"22346","content_type":"application/zip","relation":"source_file"},{"checksum":"6c526862bc6dbd1e4c80ecb34580bc58","file_size":74647289,"date_updated":"2026-07-16T09:17:05Z","file_id":"22347","content_type":"application/pdf","relation":"main_file","access_level":"open_access","creator":"lbecker","file_name":"2026_Becker_Lea_Thesis.pdf","success":1,"date_created":"2026-07-16T09:17:05Z"}],"acknowledged_ssus":[{"_id":"LifeSc"},{"_id":"NMR"}],"file_date_updated":"2026-07-16T09:17:08Z","tmp":{"short":"CC BY-NC-ND (4.0)","image":"/images/cc_by_nc_nd.png","name":"Creative Commons Attribution-NonCommercial-NoDerivatives 4.0 International (CC BY-NC-ND 4.0)","legal_code_url":"https://creativecommons.org/licenses/by-nc-nd/4.0/legalcode"},"das_tickbox":"1","author":[{"last_name":"Becker","orcid":"0000-0002-6401-5151","id":"36336939-eb97-11eb-a6c2-c83f1214ca79","first_name":"Lea Marie","full_name":"Becker, Lea Marie"}],"date_published":"2026-07-13T00:00:00Z","title":"Exploring protein dynamics using specific labeling approaches for solid-state MAS NMR","date_updated":"2026-07-20T09:49:13Z","article_processing_charge":"No","department":[{"_id":"GradSch"},{"_id":"PaSc"}],"degree_awarded":"PhD","publisher":"Institute of Science and Technology Austria","abstract":[{"text":"Characterizing protein dynamics at the atomic level is essential for our understanding of biological mechanisms. Whether it is to facilitate metabolite transport, catalyze reactions, transmit signals, or regulate metabolism – proteins are constantly in motion and sample multiple conformational states to fulfill their function. Nuclear magnetic resonance (NMR) spectroscopy is particularly well suited to elucidate the dynamics of biomolecules on their complex free-energy landscape. In particular, solid-state magic-angle spinning (MAS) NMR enables the study of large molecular assemblies, protein crystals, or insoluble proteins at atomic resolution without an inherent molecular size limitation. MAS NMR experiments to probe protein dynamics are extremely versatile and sensitive to motional timescales from picoseconds to seconds. Over the past decades, technological advances, developments in experimental design, and new isotope-labeling approaches have further expanded the possibilities of this technique and significantly improved the accuracy of the determined motional parameters.\r\nFunctionally important sites of proteins often contain aromatic residues. Their side-chain motions have therefore long served as valuable indicators of mechanistically relevant dynamics in NMR studies. In this thesis, site-specifically labeled aromatic residues act as sensitive reporters for MAS NMR studies of protein dynamics. The first part addresses how different environments impact side-chain motion by probing ring flips of phenylalanines and tyrosines in crystalline proteins and amyloid fibrils. It provides important insights for the analysis of dynamics obtained in non-native protein environments and emphasizes the complex factors that determine the timescale of internal dynamics. In the second part, the focus shifts towards methodological questions regarding the investigation of protein dynamics by 19F MAS NMR. The fluorine nucleus exhibits promising characteristics for NMR studies but also presents significant challenges, which is why the full methodological potential of 19F MAS NMR has not been fully realized yet. This work demonstrates that paramagnetic doping can considerably reduce the measurement time and improve the sensitivity of fluorinated samples. Finally, 19F MAS NMR is evaluated as a tool for studying protein side-chain dynamics on the example of tryptophans. The results illustrate the challenges in analyzing such experiments and lay the foundation for further development of 19F MAS NMR relaxation studies.\r\nTaken together, this thesis highlights the potential of combining specific isotope labeling, MAS NMR, and complementary methods such as crystallography and computational simulations to elucidate internal protein dynamics. The further development of such integrative approaches will be crucial to improving our understanding of complex mechanisms and protein function.\r\n","lang":"eng"}],"project":[{"name":"Exploring protein dynamics by solid-state MAS NMR through specific labeling approaches","grant_number":"26777","_id":"7be609c4-9f16-11ee-852c-85015ce2b9b0"}],"oa":1,"language":[{"iso":"eng"}],"year":"2026","month":"07","page":"205"}]