[{"year":"2026","quality_controlled":"1","PlanS_conform":"1","issue":"2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"07","keyword":["Stellar physics","Stellar interiors","Asteroseismology","Stellar oscillations","Hydrodynamical simulations"],"department":[{"_id":"LiBu"}],"dataavailabilitystatement":"The kinetic energies and surface velocities shown in Figure 4, as well as the underlying spectral data of this work, can be found in a Zenodo repository at doi:10.5281/zenodo.18661976.","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_type":"original","article_number":"154","supplementarymaterial":"yes","publication_status":"published","file":[{"content_type":"application/pdf","date_updated":"2026-07-13T08:14:01Z","success":1,"relation":"main_file","file_size":14866194,"access_level":"open_access","file_id":"22275","creator":"dernst","checksum":"d32061d2341bac3adeb404975c6bd59e","file_name":"2026_AstrophysicalJour_deVries.pdf","date_created":"2026-07-13T08:14:01Z"}],"oa_version":"Published Version","external_id":{"arxiv":["2606.07125"]},"arxiv":1,"author":[{"last_name":"De Vries","full_name":"De Vries, Nils B.","first_name":"Nils B."},{"full_name":"Le Saux, Arthur","first_name":"Arthur","last_name":"Le Saux"},{"full_name":"Baraffe, Isabelle","first_name":"Isabelle","last_name":"Baraffe"},{"last_name":"Guillet","full_name":"Guillet, Thomas","first_name":"Thomas"},{"last_name":"Townsend","full_name":"Townsend, Richard H.D.","first_name":"Richard H.D."},{"last_name":"Leclerc","first_name":"Armand","id":"2a1fb1fc-f373-11ef-901a-87cee43a1217","full_name":"Leclerc, Armand"},{"last_name":"Morison","first_name":"Adrien","full_name":"Morison, Adrien"}],"intvolume":" 1005","project":[{"name":"Unveiling the mysteries of stellar dynamics: a pioneering journey in magnetoasteroseismology","_id":"914d8549-16d5-11f0-9cad-bbe6324c93a9","grant_number":"101165631"}],"DOAJ_listed":"1","has_accepted_license":"1","title":"Revealing mixed modes in compressible hydrodynamical simulations of red giant stars","OA_place":"publisher","ddc":["520"],"OA_type":"gold","type":"journal_article","researchdata_availability":"yes","scopus_import":"1","publication":"The Astrophysical Journal","das_tickbox":"1","date_published":"2026-07-10T00:00:00Z","date_created":"2026-07-12T22:02:17Z","oa":1,"_id":"22262","day":"10","publisher":"IOP Publishing","article_processing_charge":"Yes","status":"public","acknowledgement":"We would like to thank the referee for their careful reading of the manuscript and their constructive comments that helped improve the paper. N.B.V. would like to thank K. Belkacem and J. Philidet for helpful discussions. N.B.V. is supported by STFC grant ST/Y002164/1. A.L.S. acknowledges support from the European Research Council (ERC) under the Horizon Europe program (Synergy grant agreement 101071505: 4D-STAR) from the CNES SOHO-GOLF and PLATO grants at CEA-DAp, and from ATPS (CNRS/INSU). Part of this work was supported by the ERC grant No. 787361-COBOM. R.H.D.T. acknowledges support from NASA grants 80NSSC24K0895 and 80NSSC23K1517, and NSF grant 2407636. A.L. is supported by ERC Starting Grant 101165631 (“Calcifer”). The authors would like to acknowledge the use of the University of Exeter High-Performance Computing (HPC) facility, ISCA, in carrying out this work. This work used the DiRAC Memory Intensive service (Cosma8) at Durham University, managed by the Institute for Computational Cosmology, and the DiRAC Data Intensive service (DIaL3) at the University of Leicester, managed by the University of Leicester Research Computing Service. These facilities are managed on behalf of the STFC DiRAC HPC (www.dirac.ac.uk). The DiRAC services at Durham and Leicester were funded by BEIS, UKRI, and STFC capital funding, and STFC operations grants. The service at Durham received funding from Durham University. DiRAC is part of the UKRI Digital Research Infrastructure.","volume":1005,"language":[{"iso":"eng"}],"doi":"10.3847/1538-4357/ae7a3c","file_date_updated":"2026-07-13T08:14:01Z","citation":{"mla":"De Vries, Nils B., et al. “Revealing Mixed Modes in Compressible Hydrodynamical Simulations of Red Giant Stars.” The Astrophysical Journal, vol. 1005, no. 2, 154, IOP Publishing, 2026, doi:10.3847/1538-4357/ae7a3c.","short":"N.B. De Vries, A. Le Saux, I. Baraffe, T. Guillet, R.H.D. Townsend, A. Leclerc, A. Morison, The Astrophysical Journal 1005 (2026).","ama":"De Vries NB, Le Saux A, Baraffe I, et al. Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. The Astrophysical Journal. 2026;1005(2). doi:10.3847/1538-4357/ae7a3c","ista":"De Vries NB, Le Saux A, Baraffe I, Guillet T, Townsend RHD, Leclerc A, Morison A. 2026. Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. The Astrophysical Journal. 1005(2), 154.","chicago":"De Vries, Nils B., Arthur Le Saux, Isabelle Baraffe, Thomas Guillet, Richard H.D. Townsend, Armand Leclerc, and Adrien Morison. “Revealing Mixed Modes in Compressible Hydrodynamical Simulations of Red Giant Stars.” The Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae7a3c.","apa":"De Vries, N. B., Le Saux, A., Baraffe, I., Guillet, T., Townsend, R. H. D., Leclerc, A., & Morison, A. (2026). Revealing mixed modes in compressible hydrodynamical simulations of red giant stars. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae7a3c","ieee":"N. B. De Vries et al., “Revealing mixed modes in compressible hydrodynamical simulations of red giant stars,” The Astrophysical Journal, vol. 1005, no. 2. IOP Publishing, 2026."},"date_updated":"2026-07-13T08:16:25Z","abstract":[{"text":"Mixed modes are observed in many low-mass evolved stars. They provide information about core rotation rates of these stars, which are lower than predicted by stellar evolution models. The mixed modes themselves have been invoked as an angular momentum (AM) transport mechanism, but estimating their transport efficiency requires knowledge of their amplitudes. We constrain, for the first time, the mixed-mode amplitudes in 2D hydrodynamical simulations of a 1.3M⊙ red giant using the code MUSIC. We perform two simulations with outer radial truncations at fractional radii ro/r⋆ = 0.90 and 0.98. We compare the modes in the simulation with those found using both GYRE and a Dedalus eigenvalue solver. Excellent frequency agreement is found for all p-dominated modes, with minor discrepancies for g-dominated modes, especially in the frequency range [60, 240] μHz. We find excellent eigenfunction agreement for all modes except those in this frequency range. According to empirical predictions, the largest kinetic energies are located around Vmax= 312.μHz, but in both simulations, the modes with frequencies of ν < 50 μHz have the largest kinetic energies. In the simulation with r/r⋆ = 0.98, the simulated modes have extrapolated surface velocities comparable to the empirical predictions, with the highest surface velocities in a bell-shaped curve peaking around ν = 700 μHz. The extrapolated surface velocities of the low-frequency modes are small and thus hard to observe, but their large kinetic energies deeper in the interior could significantly impact AM transport, which has not yet been investigated.","lang":"eng"}],"publication_identifier":{"issn":["0004-637X"],"eissn":["1538-4357"]}},{"oa_version":"Published Version","file":[{"date_updated":"2026-07-13T07:12:35Z","content_type":"application/pdf","file_id":"22272","access_level":"open_access","creator":"dernst","success":1,"file_size":3870924,"relation":"main_file","file_name":"2026_CommEarthEnvironment_Andre.pdf","checksum":"fd8f57cbe180f7a4d49ab17b3571ad2b","date_created":"2026-07-13T07:12:35Z"}],"publication_status":"published","supplementarymaterial":"yes","project":[{"call_identifier":"H2020","grant_number":"805041","name":"Organization of CLoUdS, and implications of Tropical cyclones and for the Energetics of the tropics, in current and waRming climate","_id":"629205d8-2b32-11ec-9570-e1356ff73576"}],"intvolume":" 7","author":[{"last_name":"André","first_name":"Julie","full_name":"André, Julie"},{"full_name":"Chiabrando, Nicolas","first_name":"Nicolas","last_name":"Chiabrando"},{"id":"f978ccb0-3f7f-11eb-b193-b0e2bd13182b","first_name":"Caroline J","full_name":"Muller, Caroline J","orcid":"0000-0001-5836-5350","last_name":"Muller"},{"first_name":"Philippe","full_name":"Drobinski, Philippe","last_name":"Drobinski"},{"last_name":"D’Andrea","full_name":"D’Andrea, Fabio","first_name":"Fabio"}],"month":"07","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","year":"2026","article_number":"572","article_type":"original","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"dataavailabilitystatement":"ERA5 reanalysis and Euro-CORDEX simulations are publicly available from https://doi.org/10.24381/cds.143582cf and https://cordex.org/data-access/esgf/. The custom code developed and used for this paper can be accessed through Zenodo, https://doi.org/10.5281/zenodo.18995401.","department":[{"_id":"CaMu"}],"article_processing_charge":"Yes","acknowledgement":"J.A. gratefully acknowledges the JSPS postdoctoral fellowship (Japan Society for Promotion of Science, grant number P25709). C.J.M. gratefully acknowledges funding from the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation program (Project CLUSTER, Grant Agreement No. 805041). The authors also thank Samuel Somot (Centre National de Recherches Météorologiques, Toulouse) and Juliette Blanchet (Institut des Géosciences de l’Environnement, Grenoble) for their fruitful discussions on the project.","status":"public","_id":"22261","day":"06","publisher":"Springer Nature","date_created":"2026-07-12T22:02:16Z","oa":1,"publication_identifier":{"eissn":["2662-4435"]},"date_updated":"2026-07-13T07:13:21Z","abstract":[{"lang":"eng","text":"Climate change is significantly altering regional precipitation patterns across Europe and the Mediterranean. We analyze daily precipitation distribution changes in a 15-member Euro-CORDEX ensemble, through a diagnostic framework that separates occurrence changes, wet-days intensity shifts and distortions. At +4 ∘C global warming, Northern Europe shows a robust intensification of precipitation, driven by both higher occurrence and stronger events. Conversely, the Mediterranean exhibits a dominant drying signal, primarily due to fewer wet-days, which impacts daily precipitation distribution even for heavy rainfall. Transitional zones in the northern Mediterranean reveal “U-shape” regimes, with rising extremes but declining moderate rain. Comparing with ERA5 reanalysis over the past, low model agreement in the south highlights higher uncertainty in the Mediterranean region. The timing of robust signal emergence varies: Northern Europe shows robust patterns from +1 ∘C, while the Mediterranean exhibits delays until +3-4 ∘C. These findings are essential for informing risk-based adaptation strategies."}],"file_date_updated":"2026-07-13T07:12:35Z","citation":{"ista":"André J, Chiabrando N, Muller CJ, Drobinski P, D’Andrea F. 2026. Distinct regimes of precipitation changes across Europe and the Mediterranean under global warming. Communications Earth and Environment. 7, 572.","ama":"André J, Chiabrando N, Muller CJ, Drobinski P, D’Andrea F. Distinct regimes of precipitation changes across Europe and the Mediterranean under global warming. Communications Earth and Environment. 2026;7. doi:10.1038/s43247-026-03519-7","apa":"André, J., Chiabrando, N., Muller, C. J., Drobinski, P., & D’Andrea, F. (2026). Distinct regimes of precipitation changes across Europe and the Mediterranean under global warming. Communications Earth and Environment. Springer Nature. https://doi.org/10.1038/s43247-026-03519-7","chicago":"André, Julie, Nicolas Chiabrando, Caroline J Muller, Philippe Drobinski, and Fabio D’Andrea. “Distinct Regimes of Precipitation Changes across Europe and the Mediterranean under Global Warming.” Communications Earth and Environment. Springer Nature, 2026. https://doi.org/10.1038/s43247-026-03519-7.","ieee":"J. André, N. Chiabrando, C. J. Muller, P. Drobinski, and F. D’Andrea, “Distinct regimes of precipitation changes across Europe and the Mediterranean under global warming,” Communications Earth and Environment, vol. 7. Springer Nature, 2026.","mla":"André, Julie, et al. “Distinct Regimes of Precipitation Changes across Europe and the Mediterranean under Global Warming.” Communications Earth and Environment, vol. 7, 572, Springer Nature, 2026, doi:10.1038/s43247-026-03519-7.","short":"J. André, N. Chiabrando, C.J. Muller, P. Drobinski, F. D’Andrea, Communications Earth and Environment 7 (2026)."},"doi":"10.1038/s43247-026-03519-7","language":[{"iso":"eng"}],"volume":7,"OA_type":"gold","OA_place":"publisher","ddc":["550"],"has_accepted_license":"1","DOAJ_listed":"1","title":"Distinct regimes of precipitation changes across Europe and the Mediterranean under global warming","das_tickbox":"1","date_published":"2026-07-06T00:00:00Z","ec_funded":1,"publication":"Communications Earth and Environment","scopus_import":"1","researchdata_availability":"yes","type":"journal_article"},{"article_type":"original","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"dataavailabilitystatement":"We thank the staffs of the various observatories at\r\nwhich data were obtained. This work is partially based\r\non observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project\r\nof the Minist´erio da Ciˆencia, Tecnologia e Inova¸c˜oes\r\n(MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina\r\nat Chapel Hill (UNC), and Michigan State University\r\n(MSU). Some of the data presented herein were obtained\r\nat the W. M. Keck Observatory, which is operated as a\r\nscientific partnership among the California Institute of\r\nTechnology, the University of California, and NASA; the\r\nobservatory was made possible by the generous financial\r\nsupport of the W. M. Keck Foundation.\r\nThis research has made use of the Keck Observatory\r\nArchive (KOA), which is operated by the W. M. Keck\r\nObservatory and the NASA Exoplanet Science Institute\r\n(NExScI), under contract with the National Aeronautics\r\nand Space Administration.\r\nThis work has made use of data from the\r\nEuropean Space Agency (ESA) mission Gaia\r\n(https://www.cosmos.esa.int/gaia), processed\r\nby the Gaia Data Processing and Analysis Consortium\r\n(DPAC, https://www.cosmos.esa.int/web/gaia/\r\ndpac/consortium). Funding for the DPAC has been\r\nprovided by national institutions, in particular the\r\ninstitutions participating in the Gaia Multilateral\r\nAgreement.","department":[{"_id":"IlCa"}],"month":"06","keyword":["white dwarfs","binaries: close","stars: chemically peculiar"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","PlanS_conform":"1","quality_controlled":"1","year":"2026","intvolume":" 9","author":[{"first_name":"Kareem","full_name":"El-Badry, Kareem","last_name":"El-Badry"},{"last_name":"Werner","full_name":"Werner, Klaus","first_name":"Klaus"},{"last_name":"Shen","full_name":"Shen, Ken J.","first_name":"Ken J."},{"last_name":"Strader","first_name":"Jay","full_name":"Strader, Jay"},{"last_name":"Rodriguez","full_name":"Rodriguez, Antonio C.","first_name":"Antonio C."},{"full_name":"Han, Jiwon Jesse","first_name":"Jiwon Jesse","last_name":"Han"},{"last_name":"Chandra","full_name":"Chandra, Vedant","first_name":"Vedant"},{"last_name":"Chomiuk","first_name":"Laura","full_name":"Chomiuk, Laura"},{"last_name":"Vanderbosch","full_name":"Vanderbosch, Zachary P.","first_name":"Zachary P."},{"last_name":"Blomberg","first_name":"Lisa","full_name":"Blomberg, Lisa"},{"last_name":"Yamaguchi","first_name":"Natsuko","full_name":"Yamaguchi, Natsuko"},{"last_name":"Nagarajan","full_name":"Nagarajan, Pranav","first_name":"Pranav"},{"orcid":"0000-0002-4770-5388","last_name":"Caiazzo","full_name":"Caiazzo, Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","first_name":"Ilaria"},{"last_name":"van Roestel","id":"4d122fc8-6083-11f0-87a5-97d68b860333","first_name":"Joannes C","full_name":"van Roestel, Joannes C"},{"full_name":"Glanz, Hila","first_name":"Hila","last_name":"Glanz"},{"last_name":"Wong","full_name":"Wong, Tin Long Sunny","first_name":"Tin Long Sunny"},{"first_name":"Aakash","full_name":"Bhat, Aakash","last_name":"Bhat"},{"last_name":"Hollands","first_name":"Mark A.","full_name":"Hollands, Mark A."}],"arxiv":1,"external_id":{"arxiv":["2606.11293"]},"oa_version":"Published Version","file":[{"content_type":"application/pdf","date_updated":"2026-07-13T09:05:36Z","relation":"main_file","file_size":1994596,"success":1,"creator":"dernst","file_id":"22282","access_level":"open_access","date_created":"2026-07-13T09:05:36Z","checksum":"6320fd19e5ea3399f332be5aab022736","file_name":"2026_OpenJourAstrophysics_ElBadry.pdf"}],"publication_status":"published","supplementarymaterial":"no","date_published":"2026-06-30T00:00:00Z","das_tickbox":"1","publication":"The Open Journal of Astrophysics","researchdata_availability":"no","scopus_import":"1","type":"journal_article","OA_type":"gold","ddc":["520"],"OA_place":"publisher","title":"A systematic survey for hypervelocity runaways from thermonuclear supernovae","DOAJ_listed":"1","has_accepted_license":"1","publication_identifier":{"eissn":["2565-6120"]},"abstract":[{"text":"The explosion of a white dwarf (WD) in a close binary can launch a surviving runaway star at\r\nvelocities of ≳ 1000 km s−1\r\n. Such runaways provide a direct probe of thermonuclear supernovae (SNe)\r\nin double-degenerate binaries. Several candidate runaways are known, but their evolutionary states\r\nand the demographics of the broader population are uncertain. To enable robust population inference,\r\nwe carry out a systematic survey for hypervelocity runaways with a simple selection function, selecting\r\ncandidates based on large Gaia-inferred tangential velocities and blue colors. We classify 100% of the\r\nresulting 92 candidates using a combination of spectroscopic follow-up and archival data. The search\r\nyields ten suspected D6\r\nstars and three LP 40-365 stars. Three D6\r\nstars are new discoveries, including\r\ntwo hot (Teff ≳ 50,000 K) objects and one cool (Teff ≈ 7,000 K) object. We forward-model our survey\r\nunder several proposed D6\r\nstar evolutionary models, coupling each to a Galactic model and the survey\r\nselection function. No single model reproduces the observed diversity of D6\r\nstars, which likely reflects\r\na range of remnant masses, ages, and heating mechanisms. Models in which runaway companions\r\nare heated by SN shocks alone are too faint and short-lived to explain most of the observed sample,\r\nwhile fully reheated models are too luminous and long-lived. Models with intermediate heating,\r\nas occurs in some simulations of violent mergers and partially disrupted remnants, best match the\r\nobserved magnitude, distance, and kinematic-age distributions. The inferred D6\r\nstar birth rate is\r\nmodel dependent, but the models that best match the observed population require rates of only a\r\nfew percent of the Galactic SN Ia rate, perhaps implying that most SNe Ia result from WD binaries\r\nin which both components explode. If most SNe Ia do produce surviving runaways, these must be\r\nfainter or shorter-lived than the currently known runaways.","lang":"eng"}],"date_updated":"2026-07-13T09:09:34Z","file_date_updated":"2026-07-13T09:05:36Z","doi":"10.33232/001c.164326","citation":{"chicago":"El-Badry, Kareem, Klaus Werner, Ken J. Shen, Jay Strader, Antonio C. Rodriguez, Jiwon Jesse Han, Vedant Chandra, et al. “A Systematic Survey for Hypervelocity Runaways from Thermonuclear Supernovae.” The Open Journal of Astrophysics. Maynooth Academic Publishing, 2026. https://doi.org/10.33232/001c.164326.","apa":"El-Badry, K., Werner, K., Shen, K. J., Strader, J., Rodriguez, A. C., Han, J. J., … Hollands, M. A. (2026). A systematic survey for hypervelocity runaways from thermonuclear supernovae. The Open Journal of Astrophysics. Maynooth Academic Publishing. https://doi.org/10.33232/001c.164326","ama":"El-Badry K, Werner K, Shen KJ, et al. A systematic survey for hypervelocity runaways from thermonuclear supernovae. The Open Journal of Astrophysics. 2026;9. doi:10.33232/001c.164326","ista":"El-Badry K, Werner K, Shen KJ, Strader J, Rodriguez AC, Han JJ, Chandra V, Chomiuk L, Vanderbosch ZP, Blomberg L, Yamaguchi N, Nagarajan P, Caiazzo I, van Roestel JC, Glanz H, Wong TLS, Bhat A, Hollands MA. 2026. A systematic survey for hypervelocity runaways from thermonuclear supernovae. The Open Journal of Astrophysics. 9.","ieee":"K. El-Badry et al., “A systematic survey for hypervelocity runaways from thermonuclear supernovae,” The Open Journal of Astrophysics, vol. 9. Maynooth Academic Publishing, 2026.","mla":"El-Badry, Kareem, et al. “A Systematic Survey for Hypervelocity Runaways from Thermonuclear Supernovae.” The Open Journal of Astrophysics, vol. 9, Maynooth Academic Publishing, 2026, doi:10.33232/001c.164326.","short":"K. El-Badry, K. Werner, K.J. Shen, J. Strader, A.C. Rodriguez, J.J. Han, V. Chandra, L. Chomiuk, Z.P. Vanderbosch, L. Blomberg, N. Yamaguchi, P. Nagarajan, I. Caiazzo, J.C. van Roestel, H. Glanz, T.L.S. Wong, A. Bhat, M.A. Hollands, The Open Journal of Astrophysics 9 (2026)."},"language":[{"iso":"eng"}],"volume":9,"status":"public","acknowledgement":"We thank Lars Bildsten, Evan Bauer, Ruediger Pakmor, Jim Fuller, Logan Proust, Abinaya Rajamuthukumar, and Stephan Geier for useful discussion related to\r\nthis work.\r\nThis work was supported by NSF grants AST-2508988\r\nand AST-2205631, NASA/ESA Hubble Space Telescope\r\nprogram No. 17441, and Scialog grant #SA-LSST-2024-\r\n114c from the Research Corporation for Science Advancement. The Kavli Institute for Theoretical Physics\r\n(KITP) hosted the program, “White Dwarfs as Probes of\r\nthe Evolution of Planets, Stars, the Milky Way, and the\r\nExpanding Universe,” during which this project was initiated. This research was supported in part by the U.S.\r\nNational Science Foundation (NSF) under grants PHY1748958. This research benefited from discussions that\r\nwere funded by the Gordon and Betty Moore Foundation\r\nthrough Grant GBMF5076.\r\nWe thank the staffs of the various observatories at\r\nwhich data were obtained. This work is partially based\r\non observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project\r\nof the Minist´erio da Ciˆencia, Tecnologia e Inova¸c˜oes\r\n(MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina\r\nat Chapel Hill (UNC), and Michigan State University\r\n(MSU). Some of the data presented herein were obtained\r\nat the W. M. Keck Observatory, which is operated as a\r\nscientific partnership among the California Institute of\r\nTechnology, the University of California, and NASA; the observatory was made possible by the generous financial\r\nsupport of the W. M. Keck Foundation.\r\nThis research has made use of the Keck Observatory\r\nArchive (KOA), which is operated by the W. M. Keck\r\nObservatory and the NASA Exoplanet Science Institute\r\n(NExScI), under contract with the National Aeronautics\r\nand Space Administration.\r\nThis work has made use of data from the\r\nEuropean Space Agency (ESA) mission Gaia\r\n(https://www.cosmos.esa.int/gaia), processed\r\nby the Gaia Data Processing and Analysis Consortium\r\n(DPAC, https://www.cosmos.esa.int/web/gaia/\r\ndpac/consortium). Funding for the DPAC has been\r\nprovided by national institutions, in particular the\r\ninstitutions participating in the Gaia Multilateral\r\nAgreement.","article_processing_charge":"No","day":"30","publisher":"Maynooth Academic Publishing","_id":"22270","oa":1,"date_created":"2026-07-12T22:02:19Z"},{"department":[{"_id":"MaLo"},{"_id":"GradSch"}],"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.","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"pmid":1,"article_type":"original","year":"2026","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"07","main_file_link":[{"open_access":"1","url":"https://doi.org/10.1038/s41564-026-02403-6"}],"external_id":{"pmid":["42399561"]},"author":[{"last_name":"Navarro","first_name":"Paula P.","full_name":"Navarro, Paula P."},{"first_name":"Andrea","full_name":"Vettiger, Andrea","last_name":"Vettiger"},{"last_name":"Hajdu","full_name":"Hajdu, Roman","id":"ffab949d-133f-11ed-8f02-94de21ace503","first_name":"Roman"},{"first_name":"Virly Y.","full_name":"Ananda, Virly Y.","last_name":"Ananda"},{"full_name":"López-Tavares, Alejandro","first_name":"Alejandro","last_name":"López-Tavares"},{"last_name":"Schmid","first_name":"Ernst W.","full_name":"Schmid, Ernst W."},{"first_name":"Johannes C.","full_name":"Walter, Johannes C.","last_name":"Walter"},{"last_name":"Loose","orcid":"0000-0001-7309-9724","first_name":"Martin","id":"462D4284-F248-11E8-B48F-1D18A9856A87","full_name":"Loose, Martin"},{"full_name":"Chao, Luke H.","first_name":"Luke H.","last_name":"Chao"},{"full_name":"Bernhardt, Thomas G.","first_name":"Thomas G.","last_name":"Bernhardt"}],"supplementarymaterial":"yes","publication_status":"epub_ahead","oa_version":"Published Version","type":"journal_article","researchdata_availability":"yes","scopus_import":"1","publication":"Nature Microbiology","das_tickbox":"1","date_published":"2026-07-03T00:00:00Z","has_accepted_license":"1","title":"The penicillin-binding protein PBP1b fortifies the Escherichia coli division site against osmotic rupture","OA_place":"publisher","ddc":["570"],"OA_type":"hybrid","language":[{"iso":"eng"}],"citation":{"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).","mla":"Navarro, Paula P., et al. “The Penicillin-Binding Protein PBP1b Fortifies the Escherichia Coli Division Site against Osmotic Rupture.” Nature Microbiology, Springer Nature, 2026, doi:10.1038/s41564-026-02403-6.","ieee":"P. P. Navarro et al., “The penicillin-binding protein PBP1b fortifies the Escherichia coli division site against osmotic rupture,” Nature Microbiology. Springer Nature, 2026.","ama":"Navarro PP, Vettiger A, Hajdu R, et al. The penicillin-binding protein PBP1b fortifies the Escherichia coli division site against osmotic rupture. Nature Microbiology. 2026. doi:10.1038/s41564-026-02403-6","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.","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.” Nature Microbiology. Springer Nature, 2026. https://doi.org/10.1038/s41564-026-02403-6.","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. Nature Microbiology. Springer Nature. https://doi.org/10.1038/s41564-026-02403-6"},"doi":"10.1038/s41564-026-02403-6","date_updated":"2026-07-13T09:22:49Z","abstract":[{"lang":"eng","text":"The divisome apparatus synthesizes septal peptidoglycan (PG) during bacterial division. In Escherichia coli, the class A penicillin-binding protein (aPBP) called PBP1b has been implicated in division, but its role in the process has remained unclear. Here we show using in situ cryo-electron tomography, genetics and other imaging methods that PBP1b is required to produce a wedge-like density of PG at the division site and that loss of this structure weakens the division site, making it hypersusceptible to osmotic lysis. Surprisingly, the activator LpoB needed for general PBP1b function was not required for its role in division. Of the two PBP1b isoforms produced in cells, we show that the one with an extended cytoplasmic N terminus localizes to and functions at the division site, probably via recruitment by the FtsA component of the divisome. The conservation of aPBPs with extended cytoplasmic N termini suggests that other Gram-negative bacteria may use similar mechanisms for division site reinforcement."}],"publication_identifier":{"eissn":["2058-5276"]},"oa":1,"date_created":"2026-07-12T22:02:19Z","_id":"22269","day":"03","publisher":"Springer Nature","article_processing_charge":"Yes (in subscription journal)","status":"public","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.)."},{"intvolume":" 16","author":[{"full_name":"Bain, Nicolas","first_name":"Nicolas","last_name":"Bain"},{"full_name":"Wilen, Lawrence A.","first_name":"Lawrence A.","last_name":"Wilen"},{"first_name":"Dominic","full_name":"Gerber, Dominic","last_name":"Gerber"},{"last_name":"Zu","full_name":"Zu, Mengjie","first_name":"Mengjie","id":"26dd9e7c-e86a-11eb-a854-82ac731c9ae2"},{"first_name":"Carl Peter","id":"EB352CD2-F68A-11E9-89C5-A432E6697425","full_name":"Goodrich, Carl Peter","orcid":"0000-0002-1307-5074","last_name":"Goodrich"},{"full_name":"Duraivel, Senthilkumar","first_name":"Senthilkumar","last_name":"Duraivel"},{"last_name":"Varma","first_name":"Kaarthik","full_name":"Varma, Kaarthik"},{"last_name":"Koganti","full_name":"Koganti, Harsha","first_name":"Harsha"},{"first_name":"Robert W.","full_name":"Style, Robert W.","last_name":"Style"},{"full_name":"Dufresne, Eric R.","first_name":"Eric R.","last_name":"Dufresne"}],"arxiv":1,"external_id":{"arxiv":["2410.09158"]},"oa_version":"Published Version","file":[{"date_updated":"2026-07-13T11:16:47Z","content_type":"application/pdf","date_created":"2026-07-13T11:16:47Z","file_name":"2026_PhysicalReviewX_Bain.pdf","checksum":"47354f40981223fb0c9afe292f16ead1","creator":"dernst","file_id":"22309","access_level":"open_access","file_size":4367284,"relation":"main_file","success":1}],"publication_status":"published","supplementarymaterial":"yes","article_type":"original","article_number":"021063","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"dataavailabilitystatement":"The data that support the findings of this article are openly available https://github.com/nicobain/Multiscale_interfacial_mechanics_soft_solids_data","department":[{"_id":"CaGo"}],"month":"06","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"2","PlanS_conform":"1","quality_controlled":"1","year":"2026","publication_identifier":{"issn":["2160-3308"]},"abstract":[{"lang":"eng","text":"Soft solids and their surface deformations control the response of many natural and artificial systems. Yet, their underlying properties are vigorously debated, particularly for polymer networks. While molecular-scale theories predict no interfacial changes with macroscopic deformation, multiple experiments suggest otherwise. To settle this issue, we measure displacement fields near the interface of a silicone gel, in the limit of small deformations. We discover an unexpected multiscale response. The shear modulus decreases smoothly by half with 20  μ⁢m of the interface. At the same time we observe a surface excess elasticity, that depends on history and outer medium composition. These results reveal the fundamentally multiscale nature of polymeric surfaces, and call for further experimental and theoretical investigations into the basic understanding of soft solid interfaces."}],"date_updated":"2026-07-13T11:17:51Z","file_date_updated":"2026-07-13T11:16:47Z","doi":"10.1103/8msx-l8s7","citation":{"ama":"Bain N, Wilen LA, Gerber D, et al. Multiscale interfacial mechanics of soft solids. Physical Review X. 2026;16(2). doi:10.1103/8msx-l8s7","ista":"Bain N, Wilen LA, Gerber D, Zu M, Goodrich CP, Duraivel S, Varma K, Koganti H, Style RW, Dufresne ER. 2026. Multiscale interfacial mechanics of soft solids. Physical Review X. 16(2), 021063.","chicago":"Bain, Nicolas, Lawrence A. Wilen, Dominic Gerber, Mengjie Zu, Carl Peter Goodrich, Senthilkumar Duraivel, Kaarthik Varma, Harsha Koganti, Robert W. Style, and Eric R. Dufresne. “Multiscale Interfacial Mechanics of Soft Solids.” Physical Review X. American Physical Society, 2026. https://doi.org/10.1103/8msx-l8s7.","apa":"Bain, N., Wilen, L. A., Gerber, D., Zu, M., Goodrich, C. P., Duraivel, S., … Dufresne, E. R. (2026). Multiscale interfacial mechanics of soft solids. Physical Review X. American Physical Society. https://doi.org/10.1103/8msx-l8s7","ieee":"N. Bain et al., “Multiscale interfacial mechanics of soft solids,” Physical Review X, vol. 16, no. 2. American Physical Society, 2026.","mla":"Bain, Nicolas, et al. “Multiscale Interfacial Mechanics of Soft Solids.” Physical Review X, vol. 16, no. 2, 021063, American Physical Society, 2026, doi:10.1103/8msx-l8s7.","short":"N. Bain, L.A. Wilen, D. Gerber, M. Zu, C.P. Goodrich, S. Duraivel, K. Varma, H. Koganti, R.W. Style, E.R. Dufresne, Physical Review X 16 (2026)."},"volume":16,"language":[{"iso":"eng"}],"acknowledgement":"The authors thank Katharine Jensen, Stefanie Heyden, Thomas Salez, Francesco Stellacci, Denis Bartolo, Francesco Picella, Hélène Delanoë-Ayari, Mathieu Leocmach, Antoine Bérut, Cécile Cottin-Bizonne, Anne-Laure Biance, and Oriane Talabart for useful discussions. We also thank the reviewers for excellent suggestions that substantively improved the manuscript.","status":"public","article_processing_charge":"Yes","day":"30","publisher":"American Physical Society","_id":"22288","oa":1,"date_created":"2026-07-13T09:40:54Z","date_published":"2026-06-30T00:00:00Z","das_tickbox":"1","publication":"Physical Review X","scopus_import":"1","researchdata_availability":"yes","type":"journal_article","OA_type":"gold","ddc":["530"],"OA_place":"publisher","DOAJ_listed":"1","title":"Multiscale interfacial mechanics of soft solids","has_accepted_license":"1"},{"citation":{"short":"V. Leitner, E. Benková, Current Biology 36 (2026) R739–R744.","mla":"Leitner, Valentin, and Eva Benková. “Auxin and the Control of Plant Growth and Development.” Current Biology, vol. 36, no. 13, Elsevier, 2026, pp. R739–44, doi:10.1016/j.cub.2026.04.047.","ieee":"V. Leitner and E. Benková, “Auxin and the control of plant growth and development,” Current Biology, vol. 36, no. 13. Elsevier, pp. R739–R744, 2026.","ista":"Leitner V, Benková E. 2026. Auxin and the control of plant growth and development. Current Biology. 36(13), R739–R744.","ama":"Leitner V, Benková E. Auxin and the control of plant growth and development. Current Biology. 2026;36(13):R739-R744. doi:10.1016/j.cub.2026.04.047","chicago":"Leitner, Valentin, and Eva Benková. “Auxin and the Control of Plant Growth and Development.” Current Biology. Elsevier, 2026. https://doi.org/10.1016/j.cub.2026.04.047.","apa":"Leitner, V., & Benková, E. (2026). Auxin and the control of plant growth and development. Current Biology. Elsevier. https://doi.org/10.1016/j.cub.2026.04.047"},"doi":"10.1016/j.cub.2026.04.047","language":[{"iso":"eng"}],"volume":36,"publication_identifier":{"issn":["0960-9822"]},"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."}],"date_updated":"2026-07-13T11:11:56Z","day":"06","publisher":"Elsevier","_id":"22286","corr_author":"1","date_created":"2026-07-13T09:39:40Z","status":"public","article_processing_charge":"No","scopus_import":"1","researchdata_availability":"no","type":"journal_article","date_published":"2026-07-06T00:00:00Z","das_tickbox":"0","publication":"Current Biology","title":"Auxin and the control of plant growth and development","OA_type":"closed access","author":[{"last_name":"Leitner","full_name":"Leitner, Valentin","id":"4c665ce3-0016-11ec-bea0-e44de7a4fa3d","first_name":"Valentin"},{"full_name":"Benková, Eva","first_name":"Eva","id":"38F4F166-F248-11E8-B48F-1D18A9856A87","last_name":"Benková","orcid":"0000-0002-8510-9739"}],"external_id":{"pmid":["42407441"]},"intvolume":" 36","publication_status":"published","page":"R739-R744","supplementarymaterial":"no","oa_version":"None","department":[{"_id":"EvBe"},{"_id":"GradSch"}],"article_type":"original","pmid":1,"quality_controlled":"1","year":"2026","month":"07","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"13"},{"date_published":"2026-06-23T00:00:00Z","das_tickbox":"1","publication":"Journal of Symbolic Computation","scopus_import":"1","researchdata_availability":"yes","type":"journal_article","OA_type":"hybrid","ddc":["500"],"OA_place":"publisher","mathsc":["55N31","16G20"],"has_accepted_license":"1","title":"Additive partial matchings induced by persistence maps","publication_identifier":{"issn":["0747-7171"],"eissn":["1095-855X"]},"abstract":[{"text":"Persistent homology is a fundamental tool in Topological Data Analysis. The associated algebraic structure is the persistence module, a sequence of vector spaces connected by linear maps. Persistence modules admit a complete and fast-to-compute invariant known as the persistence diagram. However, this is no longer the case for maps between persistence modules (i.e. persistence maps). We propose a new invariant for persistence maps, consisting of a partial matching between the persistence diagrams of the domain and codomain modules. We show that this invariant is additive with respect to the direct sum decomposition of persistence maps, is more discriminative than the image module, and is computable in cubic time. Furthermore, we provide an implementation and demonstrate its efficiency by integrating it with edge collapse techniques for flag complexes (e.g., Vietoris–Rips complexes). As a key technical contribution, we describe how to induce a persistence map between two flag complexes that have been independently simplified via edge collapses, even when a direct simplicial map between them is no longer available.","lang":"eng"}],"date_updated":"2026-07-13T12:00:07Z","doi":"10.1016/j.jsc.2026.102598","citation":{"ieee":"R. Gonzalez-Diaz, M. Soriano Trigueros, and A. Torras-Casas, “Additive partial matchings induced by persistence maps,” Journal of Symbolic Computation, vol. 138. Elsevier, 2026.","ista":"Gonzalez-Diaz R, Soriano Trigueros M, Torras-Casas A. 2026. Additive partial matchings induced by persistence maps. Journal of Symbolic Computation. 138, 102598.","ama":"Gonzalez-Diaz R, Soriano Trigueros M, Torras-Casas A. Additive partial matchings induced by persistence maps. Journal of Symbolic Computation. 2026;138. doi:10.1016/j.jsc.2026.102598","apa":"Gonzalez-Diaz, R., Soriano Trigueros, M., & Torras-Casas, A. (2026). Additive partial matchings induced by persistence maps. Journal of Symbolic Computation. Elsevier. https://doi.org/10.1016/j.jsc.2026.102598","chicago":"Gonzalez-Diaz, Rocio, Manuel Soriano Trigueros, and Alvaro Torras-Casas. “Additive Partial Matchings Induced by Persistence Maps.” Journal of Symbolic Computation. Elsevier, 2026. https://doi.org/10.1016/j.jsc.2026.102598.","short":"R. Gonzalez-Diaz, M. Soriano Trigueros, A. Torras-Casas, Journal of Symbolic Computation 138 (2026).","mla":"Gonzalez-Diaz, Rocio, et al. “Additive Partial Matchings Induced by Persistence Maps.” Journal of Symbolic Computation, vol. 138, 102598, Elsevier, 2026, doi:10.1016/j.jsc.2026.102598."},"language":[{"iso":"eng"}],"volume":138,"status":"public","acknowledgement":"This project was partially funded by MCIN/AEI and the NextGenerationEU/PRTR, under project TED2021-129438B-I00. The authors thank IMUS-Maria de Maeztu grant CEX2024-001517-M - Apoyo a Unidades de Excelencia María de Maeztu for supporting this research, funded by MICIU/AEI/ 10.13039/501100011033. The authors would also like to thank Lars M Salbu for fruitful discussions regarding the operators from Definition 4.1 and their relation with the order relations introduced in Definition 3.2.","article_processing_charge":"No","publisher":"Elsevier","day":"23","_id":"22291","corr_author":"1","oa":1,"date_created":"2026-07-13T09:43:38Z","article_type":"original","article_number":"102598","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"dataavailabilitystatement":"The code used for the computational experiments is available in https://github.com/Cimagroup/IBloFunMatch","department":[{"_id":"HeEd"}],"month":"06","keyword":["Persistence module","Persistence map","Persistent homology"],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","PlanS_conform":"1","quality_controlled":"1","year":"2026","intvolume":" 138","author":[{"first_name":"Rocio","full_name":"Gonzalez-Diaz, Rocio","last_name":"Gonzalez-Diaz"},{"first_name":"Manuel","id":"15ebd7cf-15bf-11ee-aebd-bb4bb5121ea8","full_name":"Soriano Trigueros, Manuel","orcid":"0000-0003-2449-1433","last_name":"Soriano Trigueros"},{"last_name":"Torras-Casas","full_name":"Torras-Casas, Alvaro","first_name":"Alvaro"}],"arxiv":1,"external_id":{"arxiv":["2006.11100"]},"main_file_link":[{"url":"https://doi.org/10.1016/j.jsc.2026.102598","open_access":"1"}],"oa_version":"Published Version","publication_status":"epub_ahead","supplementarymaterial":"no"},{"das_tickbox":"1","date_published":"2026-06-09T00:00:00Z","publication":"Chemical Science","researchdata_availability":"yes","scopus_import":"1","type":"journal_article","OA_type":"gold","OA_place":"publisher","ddc":["540"],"DOAJ_listed":"1","has_accepted_license":"1","title":"Tailoring the major groove of DNA mimic foldamers","publication_identifier":{"issn":["2041-6520"],"eissn":["2041-6539"]},"date_updated":"2026-07-13T11:24:29Z","abstract":[{"text":"Single-stranded, helically folded aromatic oligoamides bearing anionic phosphonate side chains have been shown to bind to some DNA-binding proteins better than DNA itself. However, these DNA mimic foldamers have until now mainly consisted of a single repeat motif, like a poly(dA:dT) DNA duplex, and contained limited sequence information. Here, we introduce new monomers designed to display different chemical functionalities in the major groove of the DNA mimics. Four new Fmoc-protected amino acid monomers have been synthesized and incorporated into oligomers. Sixteen foldamer sequences were prepared on solid phase. Their conformations in solution and in the solid state and their conformational dynamics were investigated using nuclear magnetic resonance, circular dichroism, molecular modeling, and X-ray crystallography. The results show that three of the four new monomers behaved as designed and that their introduction enhances the conformational dynamics of the DNA mimic foldamers. In a fourth case, conformational behavior proved to be more complex than expected. The modified sequences retained the ability to bind to the bacterial histone-like protein HU. These results showcase design strategies to manipulate large molecular biomimetics in which not only side chains but also main chain components are varied. The new monomers pave the way to complex DNA mimic foldamer sequences targeting proteins that recognize sequence-selective DNA-binding proteins such as transcription factors or restriction enzymes.","lang":"eng"}],"doi":"10.1039/d6sc00798h","citation":{"ieee":"J. Wu, V. Corvaglia, T. Chakrabortty, P. K. Mandal, and I. Huc, “Tailoring the major groove of DNA mimic foldamers,” Chemical Science. Royal Society of Chemistry.","apa":"Wu, J., Corvaglia, V., Chakrabortty, T., Mandal, P. K., & Huc, I. (n.d.). Tailoring the major groove of DNA mimic foldamers. Chemical Science. Royal Society of Chemistry. https://doi.org/10.1039/d6sc00798h","chicago":"Wu, Jiaojiao, Valentina Corvaglia, Tulika Chakrabortty, Pradeep K Mandal, and Ivan Huc. “Tailoring the Major Groove of DNA Mimic Foldamers.” Chemical Science. Royal Society of Chemistry, n.d. https://doi.org/10.1039/d6sc00798h.","ista":"Wu J, Corvaglia V, Chakrabortty T, Mandal PK, Huc I. Tailoring the major groove of DNA mimic foldamers. Chemical Science.","ama":"Wu J, Corvaglia V, Chakrabortty T, Mandal PK, Huc I. Tailoring the major groove of DNA mimic foldamers. Chemical Science. doi:10.1039/d6sc00798h","short":"J. Wu, V. Corvaglia, T. Chakrabortty, P.K. Mandal, I. Huc, Chemical Science (n.d.).","mla":"Wu, Jiaojiao, et al. “Tailoring the Major Groove of DNA Mimic Foldamers.” Chemical Science, Royal Society of Chemistry, doi:10.1039/d6sc00798h."},"language":[{"iso":"eng"}],"article_processing_charge":"Yes","acknowledgement":"We acknowledge financial support from the European Research Council (ERC) under the European Union's Horizon Europe Framework Programme (grant agreement no. ERC-2021-ADG-320892) and from the China Scholarship Council (CSC, predoctoral fellowship to J. W.). We thank L. Allmendinger for assistance with NMR measurements, P. Mayer for his assistance in solving the crystal structures of 1 and 1d, L. Bodero for assistance with automated solid-phase synthesis, M. Rogovoi for providing monomer precursors, and M. Loos for the purification and analysis of compounds 15a–19a. We thank M. Soler-Lopez (ID23-1, ESRF, Grenoble) and I. Bento (EMBL P13, Petra III, DESY, Hamburg) for assistance during data collection at the synchrotron beamlines.","status":"public","_id":"22289","publisher":"Royal Society of Chemistry","day":"09","date_created":"2026-07-13T09:41:36Z","article_type":"original","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"dataavailabilitystatement":"CCDC 2514117, 2514118, 2286782 and 2478322 (compound 1, compound 1d, oligomer 5, and oligomer 6, respectively) contain the supplementary crystallographic data for this paper.54a–d \r\n\r\nThe supporting data have been provided as part of the supplementary information (SI). Supplementary information: SI figures, detailed experimental protocols, crystallographic studies, and characterisation of new compounds. See DOI: https://doi.org/10.1039/d6sc00798h.","department":[{"_id":"LifeSc"}],"month":"06","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","year":"2026","author":[{"last_name":"Wu","first_name":"Jiaojiao","full_name":"Wu, Jiaojiao"},{"first_name":"Valentina","full_name":"Corvaglia, Valentina","last_name":"Corvaglia"},{"last_name":"Chakrabortty","first_name":"Tulika","full_name":"Chakrabortty, Tulika"},{"first_name":"Pradeep K","id":"6a3def15-d4b4-11ef-9fa9-a24c1f545ec3","full_name":"Mandal, Pradeep K","orcid":"0000-0001-5996-956X","last_name":"Mandal"},{"first_name":"Ivan","full_name":"Huc, Ivan","last_name":"Huc"}],"oa_version":"Published Version","publication_status":"inpress","supplementarymaterial":"yes"},{"project":[{"name":"Random matrices beyond Wigner-Dyson-Mehta","_id":"62796744-2b32-11ec-9570-940b20777f1d","grant_number":"101020331","call_identifier":"H2020"},{"_id":"bda63fe5-d553-11ed-ba76-a16e3d2f256b","name":"Mathematical Challenges in BCS Theory of Superconductivity","grant_number":"I06427"}],"author":[{"orcid":"0000-0003-1106-327X","last_name":"Henheik","first_name":"Sven Joscha","id":"31d731d7-d235-11ea-ad11-b50331c8d7fb","full_name":"Henheik, Sven Joscha"},{"first_name":"Edwin","full_name":"Langmann, Edwin","last_name":"Langmann"},{"last_name":"Lauritsen","orcid":"0000-0003-4476-2288","first_name":"Asbjørn Bækgaard","id":"e1a2682f-dc8d-11ea-abe3-81da9ac728f1","full_name":"Lauritsen, Asbjørn Bækgaard"}],"arxiv":1,"external_id":{"arxiv":["2409.17297"]},"main_file_link":[{"open_access":"1","url":"https://doi.org/10.1007/s00023-026-01706-y"}],"oa_version":"Published Version","publication_status":"epub_ahead","supplementarymaterial":"not applicable","article_type":"original","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"dataavailabilitystatement":"Data sharing is not applicable to this article as no new data were created or analyzed in this study.","department":[{"_id":"LaEr"},{"_id":"RoSe"}],"month":"06","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","PlanS_conform":"1","quality_controlled":"1","year":"2026","publication_identifier":{"eissn":["1424-0661"],"issn":["1424-0637"]},"abstract":[{"text":"We introduce a multi-band BCS free energy functional and prove that for a multi-band superconductor the effect of inter-band coupling can only increase the critical temperature, irrespective of its attractive or repulsive nature and its strength. Further, for weak coupling and weaker inter-band coupling, we prove that the dependence of the increase in critical temperature on the inter-band coupling is (1) linear, if there are two or more equally strongly superconducting bands, or (2) quadratic, if there is only one dominating band.","lang":"eng"}],"date_updated":"2026-07-13T11:34:08Z","doi":"10.1007/s00023-026-01706-y","citation":{"mla":"Henheik, Sven Joscha, et al. “Multi-Band Superconductors Have Enhanced Critical Temperatures.” Annales Henri Poincaré, Springer Nature, 2026, doi:10.1007/s00023-026-01706-y.","short":"S.J. Henheik, E. Langmann, A.B. Lauritsen, Annales Henri Poincaré (2026).","ama":"Henheik SJ, Langmann E, Lauritsen AB. Multi-band superconductors have enhanced critical temperatures. Annales Henri Poincaré. 2026. doi:10.1007/s00023-026-01706-y","ista":"Henheik SJ, Langmann E, Lauritsen AB. 2026. Multi-band superconductors have enhanced critical temperatures. Annales Henri Poincaré.","chicago":"Henheik, Sven Joscha, Edwin Langmann, and Asbjørn Bækgaard Lauritsen. “Multi-Band Superconductors Have Enhanced Critical Temperatures.” Annales Henri Poincaré. Springer Nature, 2026. https://doi.org/10.1007/s00023-026-01706-y.","apa":"Henheik, S. J., Langmann, E., & Lauritsen, A. B. (2026). Multi-band superconductors have enhanced critical temperatures. Annales Henri Poincaré. Springer Nature. https://doi.org/10.1007/s00023-026-01706-y","ieee":"S. J. Henheik, E. Langmann, and A. B. Lauritsen, “Multi-band superconductors have enhanced critical temperatures,” Annales Henri Poincaré. Springer Nature, 2026."},"language":[{"iso":"eng"}],"status":"public","acknowledgement":"We would like to thank J. Lenells and R. Seiringer for their interest and helpful discussions, E. Babaev and Y. Yerin for useful comments about the literature, and the anonymous referee for their comments. J.H. gratefully acknowledges partial financial support by the ERC Advanced Grant “RMTBeyond” No. 101020331 and the ERC Consollidator Grant “ProbQuant” (jointly with the Swiss State Secretariat for Education, Research and Innovation). E.L. gratefully acknowledges support from the Swedish Research Council, Grant No. 2023-04726. A.B.L. gratefully acknowledges partial financial support by the Austrian Science Fund (FWF) through grant DOI: 10.55776/I6427 (as part of the SFB/TRR 352) and by the French State support managed by ANR under the France 2030 program through the MaQuI CNRS Risky and High-Impact Research programme (RI)^2 (grant agreement ANR-24-RRII-0001). Open access funding provided by Royal Institute of Technology.","article_processing_charge":"Yes (via OA deal)","day":"29","publisher":"Springer Nature","_id":"22290","date_created":"2026-07-13T09:42:22Z","oa":1,"date_published":"2026-06-29T00:00:00Z","das_tickbox":"1","publication":"Annales Henri Poincaré","ec_funded":1,"researchdata_availability":"not applicable","scopus_import":"1","related_material":{"record":[{"status":"public","id":"19550","relation":"earlier_version"}]},"type":"journal_article","OA_type":"hybrid","ddc":["500"],"OA_place":"publisher","has_accepted_license":"1","title":"Multi-band superconductors have enhanced critical temperatures"},{"publication":"Journal of Mathematical Physics","das_tickbox":"1","date_published":"2026-06-01T00:00:00Z","type":"journal_article","scopus_import":"1","researchdata_availability":"not applicable","OA_type":"green","title":"Arbitrary harmonic functions as Bose–Einstein condensates","OA_place":"repository","date_updated":"2026-07-13T12:20:59Z","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"}],"publication_identifier":{"issn":["0022-2488"],"eissn":["1089-7658"]},"volume":67,"language":[{"iso":"eng"}],"citation":{"mla":"De Wilde, Michiel, and Robert Seiringer. “Arbitrary Harmonic Functions as Bose–Einstein Condensates.” Journal of Mathematical Physics, vol. 67, no. 6, 061901, AIP Publishing, 2026, doi:10.1063/5.0325354.","short":"M. De Wilde, R. Seiringer, Journal of Mathematical Physics 67 (2026).","ista":"De Wilde M, Seiringer R. 2026. Arbitrary harmonic functions as Bose–Einstein condensates. Journal of Mathematical Physics. 67(6), 061901.","ama":"De Wilde M, Seiringer R. Arbitrary harmonic functions as Bose–Einstein condensates. Journal of Mathematical Physics. 2026;67(6). doi:10.1063/5.0325354","apa":"De Wilde, M., & Seiringer, R. (2026). Arbitrary harmonic functions as Bose–Einstein condensates. Journal of Mathematical Physics. AIP Publishing. https://doi.org/10.1063/5.0325354","chicago":"De Wilde, Michiel, and Robert Seiringer. “Arbitrary Harmonic Functions as Bose–Einstein Condensates.” Journal of Mathematical Physics. AIP Publishing, 2026. https://doi.org/10.1063/5.0325354.","ieee":"M. De Wilde and R. Seiringer, “Arbitrary harmonic functions as Bose–Einstein condensates,” Journal of Mathematical Physics, vol. 67, no. 6. AIP Publishing, 2026."},"doi":"10.1063/5.0325354","article_processing_charge":"No","status":"public","acknowledgement":"We are grateful to Rupert Frank and Jakob Yngvason for helpful discussions and suggestions.","oa":1,"date_created":"2026-07-13T09:45:09Z","corr_author":"1","_id":"22292","publisher":"AIP Publishing","day":"01","article_number":"061901","article_type":"original","department":[{"_id":"RoSe"},{"_id":"GradSch"}],"dataavailabilitystatement":"Data sharing is not applicable to this article as no new data were created or analyzed in this study.","issue":"6","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"06","year":"2026","quality_controlled":"1","intvolume":" 67","main_file_link":[{"url":"https://doi.org/10.48550/arXiv.2601.22883","open_access":"1"}],"external_id":{"arxiv":["2601.22883"]},"arxiv":1,"author":[{"full_name":"De Wilde, Michiel","id":"bebf1407-6635-11f0-9fef-9b7e2dd151d0","first_name":"Michiel","last_name":"De Wilde"},{"last_name":"Seiringer","orcid":"0000-0002-6781-0521","full_name":"Seiringer, Robert","id":"4AFD0470-F248-11E8-B48F-1D18A9856A87","first_name":"Robert"}],"oa_version":"Preprint","supplementarymaterial":"not applicable","publication_status":"published"},{"das_tickbox":"1","date_published":"2026-04-24T00:00:00Z","publication":"Regulation of Plant Development","place":"Singapore","scopus_import":"1","department":[{"_id":"JiFr"}],"type":"book_chapter","month":"04","OA_type":"closed access","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","year":"2026","title":"Pollination and Fertilization","publication_identifier":{"eisbn":["9789819570331"],"isbn":["9789819570324"]},"date_updated":"2026-07-13T12:25:19Z","abstract":[{"text":"In order to cope with arid terrestrial environments, angiosperms have evolved a unique fertilization way—siphonogamy. The success of siphonogamy requires several prerequisites, including the normal development of the female gametophyte and male gametophyte (pollen). Appropriate pollination methods ensure the successful encounter between pollen and the stigma. After pollen lands on the stigma, pollen/pollen tube interacts with different tissues and cells of the pistil, completing a series of male-female communications. The smooth progress of these interactions ensures that the pollen tube can enter the female gametophyte, burst, and release sperm cells to complete the double fertilization. In this chapter, we provide an overview of pollination and the interactions between male and female, comprehensively summarizing the factors involved in these processes.","lang":"eng"}],"citation":{"ieee":"S. Zhong, Z. Lan, Z. Ge, and L.-J. Qu, “Pollination and Fertilization,” in Regulation of Plant Development, F. Chang, Y. Wang, and H. Ma, Eds. Singapore: Springer Nature, 2026, pp. 537–615.","apa":"Zhong, S., Lan, Z., Ge, Z., & Qu, L.-J. (2026). Pollination and Fertilization. In F. Chang, Y. Wang, & H. Ma (Eds.), Regulation of Plant Development (pp. 537–615). Singapore: Springer Nature. https://doi.org/10.1007/978-981-95-7033-1_14","chicago":"Zhong, Sheng, Zijun Lan, Zengxiang Ge, and Li-Jia Qu. “Pollination and Fertilization.” In Regulation of Plant Development, edited by Fang Chang, Yingxiang Wang, and Hong Ma, 537–615. Singapore: Springer Nature, 2026. https://doi.org/10.1007/978-981-95-7033-1_14.","ista":"Zhong S, Lan Z, Ge Z, Qu L-J. 2026.Pollination and Fertilization. In: Regulation of Plant Development. , 537–615.","ama":"Zhong S, Lan Z, Ge Z, Qu L-J. Pollination and Fertilization. In: Chang F, Wang Y, Ma H, eds. Regulation of Plant Development. Singapore: Springer Nature; 2026:537-615. doi:10.1007/978-981-95-7033-1_14","short":"S. Zhong, Z. Lan, Z. Ge, L.-J. Qu, in:, F. Chang, Y. Wang, H. Ma (Eds.), Regulation of Plant Development, Springer Nature, Singapore, 2026, pp. 537–615.","mla":"Zhong, Sheng, et al. “Pollination and Fertilization.” Regulation of Plant Development, edited by Fang Chang et al., Springer Nature, 2026, pp. 537–615, doi:10.1007/978-981-95-7033-1_14."},"doi":"10.1007/978-981-95-7033-1_14","author":[{"first_name":"Sheng","full_name":"Zhong, Sheng","last_name":"Zhong"},{"first_name":"Zijun","full_name":"Lan, Zijun","last_name":"Lan"},{"first_name":"Zengxiang","id":"f43371a3-09ff-11eb-8013-bd0c6a2f6de8","full_name":"Ge, Zengxiang","last_name":"Ge","orcid":"0000-0001-9381-3577"},{"first_name":"Li-Jia","full_name":"Qu, Li-Jia","last_name":"Qu"}],"language":[{"iso":"eng"}],"oa_version":"None","editor":[{"last_name":"Chang","full_name":"Chang, Fang ","first_name":"Fang "},{"last_name":"Wang","first_name":"Yingxiang","full_name":"Wang, Yingxiang"},{"last_name":"Ma","first_name":"Hong","full_name":"Ma, Hong"}],"article_processing_charge":"No","status":"public","_id":"22293","publication_status":"published","publisher":"Springer Nature","day":"24","date_created":"2026-07-13T09:46:18Z","page":"537-615"},{"article_processing_charge":"Yes (in subscription journal)","acknowledgement":"We thank all members of the laboratory of J.d.J.-S. for insightful discussions and comments. We thank S. Perez for technical assistance. This work was made possible by the Paris Brain Institute Diane Barriere Chair in Synaptic Bioenergetics awarded to J.d.J.-S., who is also supported by an ERC Starting Grant (SynaptoEnergy, European Research Council; ERC-StG-852873), 2019 ATIP-Avenir Grant (CNRS, Inserm), a Big Brain Theory Grant (ICM Foundation) and a Kavli Exploratory Award (Kavli Foundation). This work was also supported by an ERC Advanced Grant (EnergyMeMo; ERC-AdG-741550) to T.P. and grants from the Agence Nationale de la Recherche to P.Y.P. (ANR-20-CE92-0047-01), T.P. (ANR-23-CE16-0029-01), A.P. and J.d.J.-S. (ANR-22-CE16-0020) and J.d.J.-S. (ANR-24-CE16-0221). T.P., P.Y.P. and J.d.J.-S. are permanent CNRS researchers. A.P. is a permanent ESPCI associate professor. T.C. was funded by the French Ministry of Research and the Fondation pour la Recherche Médicale. V.R. was funded by the Max Planck Society, the Chan Zuckerberg Initiative DAF, an advised fund of the Silicon Valley Community Foundation grant number 2024-349543 and the NIH Director’s New Innovator Award (DP2 MH140148). A.B.-G. and C.R.-D. received funding from an ERC Starting Grant (HighMemory; ERC-StG-948217), the Ministry of Economy and Competitiveness (PID2021-122795OB-I00) and the Departament d’Economia i Coneixement de la Generalitat de Catalunya (SGR 00022). T.P.V. was funded by the Wellcome Trust and a Royal Society Sir Henry Dale Research Fellowship (WT100000) and a Wellcome Trust Senior Research Fellowship (214316/Z/18/Z). K.G. was supported by the DIM C-BRAINS, funded by the Conseil Régional d’Ile-de-France. The contributions of H.F. and E.R.S. were supported by the Howard Hughes Medical Institute. The PHENO-ICMice animal Core at ICM is supported by two ‘Investissements d’avenir’ (ANR-10- IAIHU-06 and ANR-11-INBS-0011-NeurATRIS) and the Fondation pour la Recherche Médicale.","status":"public","oa":1,"date_created":"2026-03-02T10:04:49Z","_id":"21378","day":"11","publisher":"Springer Nature","date_updated":"2026-07-13T12:30:14Z","abstract":[{"text":"From insects to mammals, essential brain functions, such as forming long-term memories (LTMs), increase metabolic activity in stimulated neurons to meet the energetic demand associated with brain activation. However, while impairing neuronal metabolism limits brain performance, whether expanding the metabolic capacity of neurons boosts brain function remains poorly understood. Here, we show that LTM formation of flies and mice can be enhanced by increasing mitochondrial metabolism in central memory circuits. By knocking down the mitochondrial Ca2+ exporter Letm1, we favour Ca2+ retention in the mitochondrial matrix of neurons due to reduction of mitochondrial H+/Ca2+ exchange. The resulting increase in mitochondrial Ca2+ over-activates mitochondrial metabolism in neurons of central memory circuits, leading to improved LTM storage in training paradigms in which wild-type counterparts of both species fail to remember. Our findings unveil an evolutionarily conserved mechanism that controls mitochondrial metabolism in neurons and indicate its involvement in shaping higher brain functions, such as LTM.","lang":"eng"}],"publication_identifier":{"eissn":["2522-5812"]},"volume":8,"language":[{"iso":"eng"}],"doi":"10.1038/s42255-026-01451-w","citation":{"short":"A. Amrapali Vishwanath, T. Comyn, R.G. Mira, C. Brossier, C. Pascual-Caro, M. Faour, K. Boumendil, C. Chintaluri, C. Ramon-Duaso, R. Fan, K. Ghosh, H. Farrants, J.-P. Berwick, R. Sivakumar, M. Lopez-Manzaneda, E.R. Schreiter, T. Preat, T.P. Vogels, V. Rangaraju, A. Busquets-Garcia, P.-Y. Plaçais, A. Pavlowsky, J. de Juan-Sanz, Nature Metabolism 8 (2026) 467–488.","mla":"Amrapali Vishwanath, Anjali, et al. “Mitochondrial Ca2+ Efflux Controls Neuronal Metabolism and Long-Term Memory across Species.” Nature Metabolism, vol. 8, no. 2, Springer Nature, 2026, pp. 467–88, doi:10.1038/s42255-026-01451-w.","ieee":"A. Amrapali Vishwanath et al., “Mitochondrial Ca2+ efflux controls neuronal metabolism and long-term memory across species,” Nature Metabolism, vol. 8, no. 2. Springer Nature, pp. 467–488, 2026.","ista":"Amrapali Vishwanath A, Comyn T, Mira RG, Brossier C, Pascual-Caro C, Faour M, Boumendil K, Chintaluri C, Ramon-Duaso C, Fan R, Ghosh K, Farrants H, Berwick J-P, Sivakumar R, Lopez-Manzaneda M, Schreiter ER, Preat T, Vogels TP, Rangaraju V, Busquets-Garcia A, Plaçais P-Y, Pavlowsky A, de Juan-Sanz J. 2026. Mitochondrial Ca2+ efflux controls neuronal metabolism and long-term memory across species. Nature Metabolism. 8(2), 467–488.","ama":"Amrapali Vishwanath A, Comyn T, Mira RG, et al. Mitochondrial Ca2+ efflux controls neuronal metabolism and long-term memory across species. Nature Metabolism. 2026;8(2):467-488. doi:10.1038/s42255-026-01451-w","chicago":"Amrapali Vishwanath, Anjali, Typhaine Comyn, Rodrigo G. Mira, Claire Brossier, Carlos Pascual-Caro, Maya Faour, Kahina Boumendil, et al. “Mitochondrial Ca2+ Efflux Controls Neuronal Metabolism and Long-Term Memory across Species.” Nature Metabolism. Springer Nature, 2026. https://doi.org/10.1038/s42255-026-01451-w.","apa":"Amrapali Vishwanath, A., Comyn, T., Mira, R. G., Brossier, C., Pascual-Caro, C., Faour, M., … de Juan-Sanz, J. (2026). Mitochondrial Ca2+ efflux controls neuronal metabolism and long-term memory across species. Nature Metabolism. Springer Nature. https://doi.org/10.1038/s42255-026-01451-w"},"file_date_updated":"2026-03-02T15:21:27Z","OA_type":"hybrid","has_accepted_license":"1","title":"Mitochondrial Ca2+ efflux controls neuronal metabolism and long-term memory across species","OA_place":"publisher","ddc":["570"],"publication":"Nature Metabolism","das_tickbox":"1","date_published":"2026-02-11T00:00:00Z","type":"journal_article","scopus_import":"1","file":[{"checksum":"365932a599d05bc9ce8a57204e7a1465","file_name":"2026_NatureMetab_AmrapaliVishwanath.pdf","date_created":"2026-03-02T15:21:27Z","access_level":"open_access","file_id":"21392","creator":"dernst","success":1,"file_size":5326608,"relation":"main_file","date_updated":"2026-03-02T15:21:27Z","content_type":"application/pdf"}],"oa_version":"Published Version","page":"467-488","publication_status":"published","intvolume":" 8","project":[{"grant_number":"214316/Z/18/Z","_id":"c084a126-5a5b-11eb-8a69-d75314a70a87","name":"What’s in a memory? Spatiotemporal dynamics in strongly coupled recurrent neuronal networks."}],"external_id":{"pmid":["41673453"]},"author":[{"last_name":"Amrapali Vishwanath","first_name":"Anjali","full_name":"Amrapali Vishwanath, Anjali"},{"full_name":"Comyn, Typhaine","first_name":"Typhaine","last_name":"Comyn"},{"full_name":"Mira, Rodrigo G.","first_name":"Rodrigo G.","last_name":"Mira"},{"last_name":"Brossier","first_name":"Claire","full_name":"Brossier, Claire"},{"last_name":"Pascual-Caro","full_name":"Pascual-Caro, Carlos","first_name":"Carlos"},{"first_name":"Maya","full_name":"Faour, Maya","last_name":"Faour"},{"last_name":"Boumendil","full_name":"Boumendil, Kahina","first_name":"Kahina"},{"full_name":"Chintaluri, Chaitanya","first_name":"Chaitanya","id":"BA06AFEE-A4BA-11EA-AE5C-14673DDC885E","last_name":"Chintaluri","orcid":"0000-0003-4252-1608"},{"last_name":"Ramon-Duaso","first_name":"Carla","full_name":"Ramon-Duaso, Carla"},{"last_name":"Fan","full_name":"Fan, Ruolin","first_name":"Ruolin"},{"last_name":"Ghosh","first_name":"Kishalay","full_name":"Ghosh, Kishalay"},{"last_name":"Farrants","first_name":"Helen","full_name":"Farrants, Helen"},{"last_name":"Berwick","first_name":"Jean-Paul","full_name":"Berwick, Jean-Paul"},{"full_name":"Sivakumar, Riya","first_name":"Riya","last_name":"Sivakumar"},{"last_name":"Lopez-Manzaneda","full_name":"Lopez-Manzaneda, Mario","first_name":"Mario"},{"last_name":"Schreiter","full_name":"Schreiter, Eric R.","first_name":"Eric R."},{"first_name":"Thomas","full_name":"Preat, Thomas","last_name":"Preat"},{"full_name":"Vogels, Tim P","id":"CB6FF8D2-008F-11EA-8E08-2637E6697425","first_name":"Tim P","last_name":"Vogels","orcid":"0000-0003-3295-6181"},{"last_name":"Rangaraju","full_name":"Rangaraju, Vidhya","first_name":"Vidhya"},{"full_name":"Busquets-Garcia, Arnau","first_name":"Arnau","last_name":"Busquets-Garcia"},{"full_name":"Plaçais, Pierre-Yves","first_name":"Pierre-Yves","last_name":"Plaçais"},{"last_name":"Pavlowsky","full_name":"Pavlowsky, Alice","first_name":"Alice"},{"full_name":"de Juan-Sanz, Jaime","first_name":"Jaime","last_name":"de Juan-Sanz"}],"PlanS_conform":"1","issue":"2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"02","year":"2026","quality_controlled":"1","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"pmid":1,"article_type":"original","department":[{"_id":"TiVo"}]},{"external_id":{"arxiv":["2511.07515"]},"arxiv":1,"author":[{"full_name":"Kokorev, Vasily","first_name":"Vasily","last_name":"Kokorev"},{"full_name":"Chisholm, John","first_name":"John","last_name":"Chisholm"},{"last_name":"Naidu","first_name":"Rohan P.","full_name":"Naidu, Rohan P."},{"last_name":"Fujimoto","first_name":"Seiji","full_name":"Fujimoto, Seiji"},{"first_name":"Hakim","full_name":"Atek, Hakim","last_name":"Atek"},{"first_name":"Gabriel","full_name":"Brammer, Gabriel","last_name":"Brammer"},{"first_name":"Steven L.","full_name":"Finkelstein, Steven L.","last_name":"Finkelstein"},{"full_name":"Akins, Hollis B.","first_name":"Hollis B.","last_name":"Akins"},{"last_name":"Berg","full_name":"Berg, Danielle A.","first_name":"Danielle A."},{"full_name":"Furtak, Lukas J.","first_name":"Lukas J.","last_name":"Furtak"},{"last_name":"Fei","first_name":"Qinyue","full_name":"Fei, Qinyue"},{"last_name":"Hsiao","full_name":"Hsiao, Tiger Yu-Yang","first_name":"Tiger Yu-Yang"},{"full_name":"Labbé, Ivo","first_name":"Ivo","last_name":"Labbé"},{"full_name":"Matthee, Jorryt J","first_name":"Jorryt J","id":"7439a258-f3c0-11ec-9501-9df22fe06720","last_name":"Matthee","orcid":"0000-0003-2871-127X"},{"full_name":"Muñoz, Julian B.","first_name":"Julian B.","last_name":"Muñoz"},{"last_name":"Oesch","first_name":"Pascal A.","full_name":"Oesch, Pascal A."},{"last_name":"Pan","full_name":"Pan, Richard","first_name":"Richard"},{"first_name":"Pierluigi","full_name":"Rinaldi, Pierluigi","last_name":"Rinaldi"},{"full_name":"Saldana-Lopez, Alberto","first_name":"Alberto","last_name":"Saldana-Lopez"},{"first_name":"Daniel","full_name":"Schaerer, Daniel","last_name":"Schaerer"},{"last_name":"Volonteri","first_name":"Marta","full_name":"Volonteri, Marta"},{"last_name":"Zitrin","first_name":"Adi","full_name":"Zitrin, Adi"}],"intvolume":" 1004","supplementarymaterial":"no","publication_status":"published","file":[{"content_type":"application/pdf","date_updated":"2026-07-13T13:23:11Z","date_created":"2026-07-13T13:23:11Z","checksum":"464e60013bf14d087eb0968e9c81a269","file_name":"2026_AstrophysicalJour_Kokorev.pdf","file_size":2435643,"relation":"main_file","success":1,"creator":"dernst","access_level":"open_access","file_id":"22313"}],"oa_version":"Published Version","department":[{"_id":"JoMa"}],"dataavailabilitystatement":"The specific observations analyzed can be accessed via doi:10.17909/4byn-fe55 and doi:10.17909/zq0c-8t87. These observations are associated with programs GO #3293 and DDT #9223.\r\n\r\nFacilities: JWST - James Webb Space Telescope, HST - Hubble Space Telescope satellite.\r\n\r\nSoftware: EAZY (G. B. Brammer et al. 2008), grizli (G. Brammer 2023), msaexp (G. Brammer 2022), photutils (L. Bradley et al. 2020), pysersic (I. Pasha & T. B. Miller 2023), sep (K. Barbary 2016), SExtractor (E. Bertin & S. Arnouts1996).","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_type":"original","article_number":"153","year":"2026","quality_controlled":"1","issue":"2","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"06","language":[{"iso":"eng"}],"volume":1004,"file_date_updated":"2026-07-13T13:23:11Z","doi":"10.3847/1538-4357/ae4ed7","citation":{"ista":"Kokorev V, Chisholm J, Naidu RP, Fujimoto S, Atek H, Brammer G, Finkelstein SL, Akins HB, Berg DA, Furtak LJ, Fei Q, Hsiao TY-Y, Labbé I, Matthee JJ, Muñoz JB, Oesch PA, Pan R, Rinaldi P, Saldana-Lopez A, Schaerer D, Volonteri M, Zitrin A. 2026. The Deepest GLIMPSE of a dense gas cocoon enshrouding a Little Red Dot. The Astrophysical Journal. 1004(2), 153.","ama":"Kokorev V, Chisholm J, Naidu RP, et al. The Deepest GLIMPSE of a dense gas cocoon enshrouding a Little Red Dot. The Astrophysical Journal. 2026;1004(2). doi:10.3847/1538-4357/ae4ed7","apa":"Kokorev, V., Chisholm, J., Naidu, R. P., Fujimoto, S., Atek, H., Brammer, G., … Zitrin, A. (2026). The Deepest GLIMPSE of a dense gas cocoon enshrouding a Little Red Dot. The Astrophysical Journal. IOP Publishing. https://doi.org/10.3847/1538-4357/ae4ed7","chicago":"Kokorev, Vasily, John Chisholm, Rohan P. Naidu, Seiji Fujimoto, Hakim Atek, Gabriel Brammer, Steven L. Finkelstein, et al. “The Deepest GLIMPSE of a Dense Gas Cocoon Enshrouding a Little Red Dot.” The Astrophysical Journal. IOP Publishing, 2026. https://doi.org/10.3847/1538-4357/ae4ed7.","ieee":"V. Kokorev et al., “The Deepest GLIMPSE of a dense gas cocoon enshrouding a Little Red Dot,” The Astrophysical Journal, vol. 1004, no. 2. IOP Publishing, 2026.","mla":"Kokorev, Vasily, et al. “The Deepest GLIMPSE of a Dense Gas Cocoon Enshrouding a Little Red Dot.” The Astrophysical Journal, vol. 1004, no. 2, 153, IOP Publishing, 2026, doi:10.3847/1538-4357/ae4ed7.","short":"V. Kokorev, J. Chisholm, R.P. Naidu, S. Fujimoto, H. Atek, G. Brammer, S.L. Finkelstein, H.B. Akins, D.A. Berg, L.J. Furtak, Q. Fei, T.Y.-Y. Hsiao, I. Labbé, J.J. Matthee, J.B. Muñoz, P.A. Oesch, R. Pan, P. Rinaldi, A. Saldana-Lopez, D. Schaerer, M. Volonteri, A. Zitrin, The Astrophysical Journal 1004 (2026)."},"date_updated":"2026-07-13T13:25:09Z","abstract":[{"text":"The detection of strong Balmer breaks and absorption features in Little Red Dots (LRDs) suggests they host active galactic nuclei embedded within dense gas envelopes, potentially powered by super-Eddington accretion. We present GLIMPSE-17775, a luminous (Lbol ∼ 1045 erg s−1) LRD at z = 3.501 behind Abell S1063 (μ ∼ 2), observed with deep JWST/NIRCam and a ∼20 hr (80 hr delensed) NIRSpec G395M spectrum. The data reveal over 40 emission and absorption features, including a rich forest of low-ionization Fe ii lines and numerous broad hydrogen recombination transitions. We use this depth to test the dense-gas interpretation through five independent diagnostics. Nearly all permitted lines show exponential wings with consistent FWHM, a signature of Thomson scattering requiring ne ≳ 108 cm−3. Adopting this width yields MBH ∼ 106.7M⊙, a factor of 10 lower than Gaussian fits, and λEdd ∼ 1.8. Additional diagnostics support the same picture: a pronounced Balmer break (fν,4050/fν,3670 = 2.0 ± 0.1), enhanced He i λ7065 and λ10830 with P-Cygni absorption, Bowen-fluorescent O i λ8446–λ11290 emission requiring Lyβ pumping, and 16 Fe ii lines matching fluorescence models. These features indicate a dense (n ∼ 108 cm−3), partially ionized cocoon where scattering and fluorescence dominate line formation, providing strong evidence that at least some LRDs are powered by super-Eddington black hole growth in the early Universe.","lang":"eng"}],"publication_identifier":{"eissn":["1538-4357"],"issn":["0004-637X"]},"date_created":"2026-07-13T09:48:38Z","oa":1,"_id":"22296","day":"10","publisher":"IOP Publishing","article_processing_charge":"Yes","acknowledgement":"IOP Science home\r\nThe Astrophysical Journal\r\nThe American Astronomical Society, find out more.\r\n\r\nThe following article isOpen access\r\nThe Deepest GLIMPSE of a Dense Gas Cocoon Enshrouding a Little Red Dot\r\nVasily Kokorev, John Chisholm, Rohan P. Naidu, Seiji Fujimoto, Hakim Atek, Gabriel Brammer, Steven L. Finkelstein, Hollis B. Akins, Danielle A. Berg, Lukas J. FurtakShow full author list\r\n\r\nPublished 2026 June 10 • © 2026. The Author(s). Published by the American Astronomical Society.\r\nThe Astrophysical Journal, Volume 1004, Number 2\r\nCitation Vasily Kokorev et al 2026 ApJ 1004 153\r\nDOI 10.3847/1538-4357/ae4ed7\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\n5138 Total downloads\r\n\r\n22 total citations on Dimensions.\r\nShare this article\r\nArticle information\r\nAbstract\r\nThe detection of strong Balmer breaks and absorption features in Little Red Dots (LRDs) suggests they host active galactic nuclei embedded within dense gas envelopes, potentially powered by super-Eddington accretion. We present GLIMPSE-17775, a luminous (Lbol ∼ 1045 erg s−1) LRD at z = 3.501 behind Abell S1063 (μ ∼ 2), observed with deep JWST/NIRCam and a ∼20 hr (80 hr delensed) NIRSpec G395M spectrum. The data reveal over 40 emission and absorption features, including a rich forest of low-ionization Fe ii lines and numerous broad hydrogen recombination transitions. We use this depth to test the dense-gas interpretation through five independent diagnostics. Nearly all permitted lines show exponential wings with consistent FWHM, a signature of Thomson scattering requiring ne ≳ 108 cm−3. Adopting this width yields MBH ∼ 106.7M⊙, a factor of 10 lower than Gaussian fits, and λEdd ∼ 1.8. Additional diagnostics support the same picture: a pronounced Balmer break (fν,4050/fν,3670 = 2.0 ± 0.1), enhanced He i λ7065 and λ10830 with P-Cygni absorption, Bowen-fluorescent O i λ8446–λ11290 emission requiring Lyβ pumping, and 16 Fe ii lines matching fluorescence models. These features indicate a dense (n ∼ 108 cm−3), partially ionized cocoon where scattering and fluorescence dominate line formation, providing strong evidence that at least some LRDs are powered by super-Eddington black hole growth in the early Universe.\r\n\r\nExport citation and abstract\r\nBibTeXRIS\r\n\r\nPrevious article in issue\r\nNext article in issue\r\nRelated links\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\nOne of the most enticing puzzles brought about by the launch of the James Webb Space Telescope (JWST) has been the discovery of red, compact objects called “Little Red Dots” (LRDs; J. Matthee et al. 2024). Previously invisible to the Hubble Space Telescope (HST) due to their extreme faintness in the optical and lack of near-infrared (NIR) coverage, LRDs have emerged in abundance (V. Kokorev et al. 2024a; H. B. Akins et al. 2025a; D. D. Kocevski et al. 2025; G. Barro et al. 2026) thanks to the unprecedented NIR sensitivity of JWST.\r\n\r\nTheir unusual properties—such as compact morphologies in rest-optical and distinctive “V-shaped” spectral energy distributions (SEDs)—make LRDs easy to identify in JWST fields; however, this is where the simplicity ends. Explaining LRDs as either evolved or dusty compact galaxies proves difficult: The former scenario requires massive stellar populations that strain Lambda cold dark matter (ΛCDM) predictions (M. Boylan-Kolchin 2023; I. Labbé et al. 2023), while the latter implies significant dust emission, yet none is observed (C. M. Casey et al. 2024; G. C. K. Leung et al. 2025; H. B. Akins et al. 2025a; I. Labbé et al. 2025).\r\n\r\nOver time, the accumulating detections of broad Balmer-series emission lines (D. D. Kocevski et al. 2023, 2025; J. Matthee et al. 2024, just to name a few), often accompanied by signatures of extreme ionization (e.g., V. Kokorev et al. 2023), have begun to clarify the physical origin of LRDs, pointing increasingly toward active galactic nuclei (AGN) as the underlying power source. In parallel, the much needed advent of NIRSpec Micro Shutter Assembly (MSA) programs based on red targets selected from JWST imaging (e.g., A. de Graaff et al. 2025b) has provided critical confirmation: Nearly all point sources exhibiting “V-shaped” SEDs reveal broad emission lines upon spectroscopic follow-up (R. E. Hviding et al. 2025), solidifying their AGN interpretation.\r\n\r\nThe nature of the spectral inflection point in LRDs, typically located near ∼3600 Å, has also undergone significant revision. Initially interpreted as a stellar Balmer break (I. Labbé et al. 2023), this feature implied implausibly high stellar masses (M*) far too early in cosmic history (M. Boylan-Kolchin 2023; N. Sabti et al. 2024). A second hypothesis invoked differential dust attenuation and host-galaxy contamination in the rest-UV to explain the sharp discontinuity (M. Volonteri et al. 2025). However, this explanation was soon ruled out by D. J. Setton et al. (2025) and Y. Ma et al. (2025), who demonstrated that the break generally lies around the Balmer limit, albeit with a fundamentally different origin than initially proposed.\r\n\r\nMore recently, a series of theoretical and observational works have converged on a new picture in which LRDs may host accreting black holes enshrouded in exceptionally dense, partially ionized gas cocoons, often referred to as “black hole stars” (hereafter BH*; A. de Graaff et al. 2025b; K. Inayoshi & R. Maiolino 2025; R. P. Naidu et al. 2025; A. J. Taylor et al. 2025). Here, BH* is used in an empirical sense to denote cocooned black holes whose emergent spectra exhibit a combination of black-hole-like and star-like features, such as broad permitted lines, steep Balmer-limit breaks, and Balmer absorption, as observed in the archetypal BH* sources (A. de Graaff et al. 2025b; R. P. Naidu et al. 2025). This usage does not assume a specific geometry or formation channel: The underlying physical picture involves an AGN power-law ionizing spectrum processed through very dense gas, and similar phenomenology can arise in a range of dense-gas configurations (e.g., K. Inayoshi & R. Maiolino 2025; D. Kido et al. 2025; H. Liu et al. 2025; A. Sneppen et al. 2026). In such environments, suppressed X-ray and radio emission (e.g., K. Inayoshi & R. Maiolino 2025; R. P. Naidu et al. 2025) arise naturally from the high optical depth, while the UV emission and forbidden optical lines (e.g., [O iii] λλ4959, 5007) may originate in the more extended host (e.g., A. de Graaff et al. 2025d).\r\n\r\nThe dense-gas interpretation also offers a natural explanation for the P-Cygni-like Balmer and helium profiles frequently seen in high-signal-to-noise-ratio (S/N) spectra (J. Matthee et al. 2024), the non-Gaussian, exponentially winged line shapes predicted by radiative-transfer models of scattering in ionized gas (S.-J. Chang et al. 2026; V. Rusakov et al. 2026), and Lyα-like resonantly scattered shapes (R. P. Naidu et al. 2025; S.-J. Chang et al. 2026). Intriguingly, if electron and resonant scattering indeed dominate the broad-line widths, then the true virial velocities (traced by intrinsically narrower Gaussian cores)—and hence black hole masses—could be lower by an order of magnitude, alleviating the apparent tension between LRD black hole masses and their compact host galaxies (V. Rusakov et al. 2026).\r\n\r\nSo far, however, the BH*/dense-gas interpretation of LRDs has relied largely on the Balmer break, occasional absorption features (X. Lin et al. 2026), and, to a limited extent, the shapes of broad emission lines (V. Rusakov et al. 2026). While these features are consistent with the presence of dense, partially ionized gas, they stop short of providing direct spectroscopic confirmation of the physical conditions expected by the BH* scenario. What has been missing is an unambiguous demonstration—through emission-line physics—that LRDs indeed host dense, optically thick cocoons surrounding rapidly accreting black holes. Such evidence would directly tie the observed line formation, excitation, and radiative transfer to dense, stratified envelopes of gas surrounding the central engine.\r\n\r\nIn this work, we present precisely such a case: an exceptionally deep, ∼20 hr (equivalent to 80 hr without lensing magnification) JWST/NIRSpec G395M spectrum of a luminous LRD at z = 3.50102. The target, GLIMPSE-17775, lies in a highly magnified region of the massive galaxy cluster Abell S1063 (hereafter AS1063) and benefits from the combined power of JWST/NIRCam imaging from the GLIMPSE GO program (PID 3293; PIs: H. Atek & J. Chisholm) and recent NIRSpec spectroscopy from the GLIMPSEDirector's Discretionary Time (DDT) (hereafter GLIMPSE-D) program (PID 9223; PIs: S. Fujimoto & R. Naidu). This synergy of ultradeep spectroscopy and strong gravitational lensing enables an unprecedented view of GLIMPSE-17775, revealing rest-frame optical and NIR features at a level unseen before in any LRD. We detect over 40 emission and absorption features, including 16 Fe ii transitions that form a dense “iron forest.” The remarkable richness of this spectrum makes GLIMPSE-17775 a uniquely powerful laboratory for dissecting the dense, radiation-dominated environments that accompany early black hole growth.\r\n\r\nThis paper is organized as follows. In Section 2, we present the GLIMPSE-D NIRSpec dataset alongside the photometric datasets used in this study. In Section 3, we calculate the spectroscopic redshift, describe the identification of prominent emission/absorption features, and describe bespoke fitting of various line complexes. Section 4 describes the measurement of the source morphology, dust attenuation, and black hole masses. In Section 5, we comment on the various properties of the emission features in the our target. Finally, we discuss our findings in Section 6.\r\n\r\nThroughout this work, we assume a flat ΛCDM cosmology with Ωm,0 = 0.3, ΩΛ,0 = 0.7, and H0 = 70 km s−1 Mpc−1, and a G. Chabrier (2003) initial mass function between 0.1 and 100M⊙. All magnitudes are expressed in the AB system (J. B. Oke 1974).\r\n\r\n2. Observations and Data\r\nThe target, GLIMPSE-17775, was originally identified as a bright LRD candidate in JWST/NIRCam imaging captured by the GLIMPSE (PID: 3293; PIs: H. Atek & J. Chisholm) survey (H. Atek et al. 2025) of the lensed AS1063 Hubble Frontier Field (HFF; J. M. Lotz et al. 2017). The highly magnified area of AS1063 has already successfully yielded z > 16 galaxy candidates (V. Kokorev et al. 2025), potential Population III (Pop III) hosts (S. Fujimoto et al. 2025a), numerous faint and high-redshift galaxies (I. Chemerynska et al. 2026), new constraints on reionization (D. Korber et al. 2025), identification of intermediate-mass black holes (Q. Fei et al. 2025), and a wide variety of enigmatic LRDs, some moderately lensed. The LRD selection was based on the standard compactness plus “V-shape” criteria already laid out in J. E. Greene et al. (2024), V. Kokorev et al. (2024a), H. B. Akins et al. (2025a), and I. Labbé et al. (2025) using photometric redshifts derived with eazy (G. B. Brammer et al. 2008), a technique that has proven successful at consistently identifying many exciting sources (see, e.g., H. B. Akins et al. 2025b; A. de Graaff et al. 2025b; V. Kokorev et al. 2023; R. P. Naidu et al. 2025; A. J. Taylor et al. 2025). Located at zphot = 4.2 ± 0.1, GLIMPSE-17775 stood out in particular due to its extreme rest-optical brightness with mf444w ∼ 23.6 mag and a modest lensing magnification μ ∼ 2. While very little could be done with photometry alone, this marked GLIMPSE-17775 as a promising target for any future spectroscopic follow-up.\r\n\r\n2.1. Photometry\r\nWe use photometry both to select targets for the GLIMPSE-D NIRSpec observations and, during spectroscopic modeling, to constrain the overall shape of the SED and correct for NIRSpec slit losses. In addition to JWST/NIRCam data, we incorporate deep HST Advanced Camera for Surveys and Wide Field Camera 3 imaging from the HFF (J. M. Lotz et al. 2017) and BUFFALO (C. L. Steinhardt et al. 2020) programs. Our reprocessed HST mosaics are based on Gaia-aligned images from the CHArGE archive (V. Kokorev et al. 2022), hosted on the Dawn JWST Archive (F. Valentino et al. 2023). More descriptions of the image reduction and source extraction procedure can be found in R. Endsley et al. (2025), as well as in the GLIMPSE overview paper (H. Atek et al. 2025); we briefly summarize the latter procedure below.\r\n\r\nPhotometry is performed on point-spread function (PSF)-homogenized HST and JWST images, convolved to the resolution of the F480M filter. Source detection is carried out using SExtractor (E. Bertin & S. Arnouts 1996) through two parallel steps. We construct two inverse-variance-weighted detection images: one from the short-wavelength (SW; F090W, F115W, F150W, F200W) bands to preserve spatial resolution, and one from the long-wavelength (LW; F277W, F356W, F444W) bands to ensure sensitivity to red or dusty sources (e.g., LRDs). Unlike the science images, these have not been PSF-matched. These SW and LW detection catalogs are subsequently merged into a single, combined catalog. Photometry is then measured using photutils (L. Bradley et al. 2020) in a range of circular apertures (–). Photometric uncertainties are estimated by placing random apertures in empty regions around each source. Unless stated otherwise, we adopt total fluxes measured within a aperture throughout this work.\r\n\r\n2.2. NIRSpec Observations\r\nGLIMPSE-D NIRSpec data were obtained during a campaign (DDT #9223; PIs: S. Fujimoto & R. Naidu) to study a promising Pop III galaxy candidate (S. Fujimoto et al. 2025a). GLIMPSE-D obtained a total of three G395M/F295LP MSA pointings, totaling 29.78 hr of total exposure time. The pointing center differed for each of the three configurations to maximize the total object yield. In total, the GLIMPSE-D sample contains 384 spectra, with depths varying from 9.2 hr to ∼30 hr. All of the planned observations were successfully executed between 2025 June 30 and July 2. For each MSA configuration, GLIMPSE-D employed a standard three-point nod pattern at an aperture position angle PA_V3 = 2705, using 494 groups per integration with the NRSIRS2 readout mode. The full details of the target selection, prioritization, and MSA planning will be presented in a forthcoming survey paper (S. Fujimoto et al. 2025b).\r\n\r\n2.3. G395M Data Reduction and Calibration\r\nThe GLIMPSE-D MSA spectra were uniformly reduced using msaexp (v0.9.8; G. Brammer 2022). This procedure starts with the level-2 calibrated products obtained from MAST and applies a number of corrections that include 1/f noise, artifact detection and removal, and a bias correction in individual exposures (see J. Rigby et al. 2023 for more details). Together with the JWST pipeline, msaexp sets the slit World Coordinate System, performs flat-fielding, and computes an initial pass-loss correction. Each one of the two-dimensional shutters is then drizzled onto a common pixel grid. Using the standard approach, the background subtraction is performed locally using stacked, source-free shutters. The one-dimensional spectra are then obtained via the optimal extraction method (e.g., P. Arrabal Haro et al. 2023; A. de Graaff et al. 2024), in which the center and width of the extraction “aperture” vary depending on the best-fit Gaussian model (K. Horne 1986), similar to the methodology widely adopted by a variety of other works (e.g., B. Wang et al. 2023; J. E. Greene et al. 2024; V. Kokorev et al. 2024b).\r\n\r\nThe absolute flux calibration of MSA spectra can be influenced by several factors, including the position of the source within the shutter, calibration and astrometric uncertainties, and the intrinsic morphology of the source. To correct for these effects and derive an overall slit-loss correction, we rescale the extracted one-dimensional spectra by convolving them with all available NIRCam filters and comparing the resulting flux densities to the total photometry from the GLIMPSE catalog. A wavelength-dependent correction is then obtained by fitting a second-order polynomial to these differences.\r\n\r\nThe target in this paper was observed in all three configurations; however, one was severely contaminated by sources in the same row, making the data recovery for that configuration unfeasible. Despite this, GLIMPSE-17775 is securely detected in two configurations (33,262 s and 40,703 s), yielding a total integration time of 20.55 hr. We combine the extracted and separately calibrated one-dimensional spectra using inverse-variance weighting. The stacked spectrum is shown in Figure 1. We also make the spectrum publicly available.17\r\n\r\nZoom InZoom OutReset image size\r\nFigure 1. Top: JWST/NIRCam and HST 20 stamps and red, green, blue short-wavelength (SW) and long-wavelength (LW) color images, comprising the F115W, F150W, and F200W and F277W, F356W, and F444W bands, respectively. MSA shutters for both configurations covering GLIMPSE-17775 are shown in blue and red, respectively. The source morphology is resolved and extended up to ∼2 μm, and then appears to transition to a more PSF-dominated and compact shape, echoing a growing sample of LRDs with extended rest-UV morphology (I. Juodžbalis et al. 2024; I. Labbe et al. 2024; J. Matthee et al. 2024; P. Rinaldi et al. 2025a). This likely hints at the presence of the host galaxy in the filters covering the rest-UV. In each panel, we show the total AB magnitude as presented in the GLIMPSE catalog (H. Atek et al. 2025; V. Kokorev et al. 2025). The source is exceptionally bright (M444 ∼ 23.6) and is detected in most JWST bands at >100σ. Middle: two-dimensional MSA G395M spectra covering GLIMPSE-17775. Bottom: combined one-dimensional spectrum (see, e.g., V. Kokorev et al. 2023; A. de Graaff et al. 2025a for the extraction method) of the LRD in the observed frame. We show the data in black, and the uncertainty as a black shaded region. Fixing the systemic redshift to the [S iii] λ9071 line (zspec = 3.50102 ± 0.00019), we show the positions and label the prominent emission with significant (≥3σ) detections as solid vertical lines. Iron lines are shown separately in green. Due to the sheer number of features, not all could be labeled; we therefore display all features in Figure 2. Emission lines for which only upper limits are obtained are shown with dashed lines.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\n3. Emission-line Analysis\r\n3.1. Spectroscopic Redshift\r\nThe spectrum of GLIMPSE-17775 reveals a remarkably wide variety of significantly detected emission and absorption lines. Before focusing on individual features and their complex components, we perform an initial tally of all detectable lines using a heavily modified version of msaexp (G. Brammer 2022; V. Kokorev et al. 2024b). The key modifications allow varying the line widths and fitting multiple components, albeit tied to the same redshift.\r\n\r\nWe fit the full spectrum using msaexp, adopting Gaussian profiles for emission lines and a three-segment cubic spline to model the continuum. This minimal spline structure, appropriate given the high average S/N of GLIMPSE-17775 (≳30), helps prevent overfitting, particularly of features that may be slightly offset in wavelength or velocity space from the average redshift. Emission-line positions are fixed; narrow components are allowed a FWHM between 150 and 800 km s−1, and permitted transitions may include a broad component (800–5000 km s−1).\r\n\r\nThis yields a redshift of zspec = 3.5010 ± 0.0001 (see Table 1). However, several strong lines exhibit significant pixel-level offsets of 100–200 km s−1 relative to this value. These discrepancies are statistically robust and appear in both stacked and individual spectra, suggesting that the derived redshift reflects a weighted average dominated by high-S/N lines. To properly assess velocity structure, a consistent systemic redshift is required. In the following sections describing the detailed line analysis, we adopt the centroid of a narrow forbidden line as the systemic reference frame (specifically [S iii] λ9071; see Section 3.3).\r\n\r\nUsing the updated redshift alongside the strong-lensing model of AS1063 (A. Zitrin et al. 2015; L. Furtak et al. 2026, in preparation), we recalculate the lensing magnification to be μ = 2.04 ± 0.21, consistent with previous estimates based on zphot. With redshift and magnification now fixed, we turn to a deeper analysis of the emission-line properties.\r\n\r\n3.2. Line Identification\r\nBeyond velocity offsets, the initial msaexp fit highlights several notable features. Broad hydrogen lines, ubiquitous in LRDs (e.g., D. D. Kocevski et al. 2023; V. Kokorev et al. 2023; L. J. Furtak et al. 2024; J. Matthee et al. 2024; A. de Graaff et al. 2025b; R. E. Hviding et al. 2025; R. P. Naidu et al. 2025; A. J. Taylor et al. 2025), are strongly favored across the Balmer and Paschen series, with Δχ2 > 10. These include Hα and Pa10 through Paγ. Although Paβ falls near the edge of the detector, we nonetheless observe a prominent broad wing at its expected location (see Figure 1).\r\n\r\nBroad components are also detected in several helium and oxygen lines: He i λ6680, He i λ7065, O i λ8448, He i λ10830, and O i λ11290. Notably, the He i λ10830 line shows a classic P-Cygni profile with a clear blueshifted absorption trough. While Balmer absorption is becoming a familiar sight in LRDs (R. Maiolino et al. 2024; J. Matthee et al. 2024; A. de Graaff et al. 2025b; D. D. Kocevski et al. 2025; R. P. Naidu et al. 2025), helium absorption remains rare, with only a few published cases at high z (e.g., I. Juodžbalis et al. 2024; R. P. Naidu et al. 2024; B. Wang et al. 2025). Curiously, this was also recently reported in local analogs of LRDs (X. Lin et al. 2026).\r\n\r\nThe most striking feature is the detection of an extensive Fe ii emission forest in the rest-NIR—at least 16 distinct features are identified by msaexp and highlighted in green in Figure 1. Previous detections of permitted Fe ii in LRDs have been mostly limited to rest-UV/optical wavelengths using low-resolution PRISM spectra (R. Tripodi et al. 2025), with only few examples in the NIR (e.g., see broad Fe iiλ9200 I. Labbe et al. 2024). Iron has also been identified in local LRD analogs (X. Lin et al. 2026; X. Ji et al. 2026). Only recently have a few Fe ii emitters been reported in medium-resolution (F. D’Eugenio et al. 2025) and high-resolution spectra (A. Torralba et al. 2026). The richness of these lines in GLIMPSE-17775 hints at a dense, partially shielded gas phase, where processes such as Lyβ fluorescence and continuum pumping may be enhancing Fe ii emission (T. A. A. Sigut & A. K. Pradhan 1998, 2003; T. A. A. Sigut et al. 2004), offering a new diagnostic window into early AGN environments.\r\n\r\nIn summary, GLIMPSE-17775 exhibits an exceptionally rich and kinematically complex array of emission and absorption features. While the initial msaexp modeling provides a solid foundation for redshift estimation and line identification, it lacks the flexibility to capture the full diversity of line profiles in this high-S/N dataset. In the following sections, we peel back the spectral layers with increasing precision.\r\n\r\n3.3. Line Fitting\r\nThe exceptional depth of the G395M spectrum for GLIMPSE-17775 enables detailed modeling of both multiple kinematic components and potential velocity offsets between line species. Unless noted otherwise, each line is fit with a single Gaussian narrow component (FWHM = 100−800 km s−1). For permitted lines flagged by msaexp as potentially broad, we follow the approach of V. Rusakov et al. (2026) and model the profile as an intrinsic Gaussian core broadened by electron scattering, implemented via convolution with an exponential-wing component. The intrinsic Gaussian FWHM is allowed to vary between 500 and 5000 km s−1. The characteristic scattering width (i.e., the strength of the exponential wings, W) is treated as a free parameter and is allowed to vary independently between different transitions. For each broad line, we also perform an alternative fit with the W parameter fixed to zero (pure Gaussian) and compare the resulting goodness of fit to assess whether the exponential wings are statistically required. Line centers are allowed to vary independently unless otherwise specified.\r\n\r\nAbsorption lines are modeled using a Gaussian optical-depth profile, where the observed flux is Fobs = Fem e−τ(λ), where . The free parameters are then the central optical depth τ0, velocity width Δvabs, and redshift zabs (see I. Juodžbalis et al. 2024). Widths and redshifts (for both narrow and broad components) are typically free, with redshift limited to ± 0.1 from the msaexp value. Local continua are fit using first-order polynomials.\r\n\r\nAll individual model components are first initialized and coadded on an oversampled wavelength grid. To take into account the wavelength-dependent resolution of the grating, we interpolate our model onto a variable step grid while making sure that the total integrated flux is preserved. Further, we increase the nominal spectral resolution by a factor of 1.7, as it has been shown that the spectral resolution for a pointlike source falling within a shutter is higher than that of a uniformly illuminated slitlet (A. de Graaff et al. 2024). Fitting uses nonlinear χ2 minimization, with uncertainties derived from multivariate resampling of the covariance matrix.\r\n\r\nTable 1. Source Properties\r\n\r\nParametera\tGLIMPSE-17775\r\nID\t17775\r\nR.A. [deg]\t342.20080\r\nDecl. [deg]\t–44.54366\r\nzphot (eazy)\t4.2 ± 0.1\r\nzspec ([S iii] λ9071)\t3.50102 ± 0.00019\r\nμ\t2.04 ± 0.21\r\nMUV [AB mag]\t−17.27 ± 0.05\r\nreff,UV [pc]\t1000 ± 200\r\nreff,opt [pc]\t<300\r\nβ\t–0.69 ± 0.12\r\nlog10(MBH/M⊙)\t6.65 ± 0.15\r\nLbol [erg s−1]\t(1.06 ± 0.14)×1045\r\nλedd\t1.86 ± 0.25\r\nlog10(M*/M⊙)\t<7.5\r\nAV\t0.1 ± 0.3\r\nfν,4050Å/fν,3670Å\t2.02 ± 0.10\r\nNote. aPhysical parameters are corrected for the lensing magnification.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nGiven the complexity, the spectrum is divided into six windows grouped by line species or proximity (see Figure 2). Below, we describe the assumptions adopted for each window. Final fluxes and equivalent widths of the narrow and broad lines are listed in Tables 2 and 3, respectively, while kinematics are reported in Tables 4 and 5. We show detailed line fits in Figure 2.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 2. A staggering abundance of spectral lines in GLIMPSE-17775 at z = 3.501. For each spectral window defined in Section 3.3, we show the data (black), the best-fit narrow and broad components (dark purple and blue), and the total best-fit model including the continuum (red). All broad components were fit with models allowing exponential wings. The ΔBIC between exponential and Gaussian fits is reported in the top right of each panel; negative values indicate a preference for an exponential profile. The lower panels display the uncertainty-weighted residuals for each fit.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nTable 2. Fluxes of Narrow Emission Lines and Their Rest-frame Equivalent Widthsa\r\n\r\nLine\tλrest\tFlux\tEW0\r\n \t(Å)\t(10−20 erg s−1 cm−2)\t(Å)\r\nNarrow Emission Lines\r\nO i\t6302.0\t54.0 ± 21.2\t3.3 ± 1.2\r\n[N ii]\t6549.0\t25.6 ± 10.3\t1.6 ± 0.7\r\nHα\t6562.8\t2622.9 ± 200.7\t167.7 ± 12.8\r\n[N ii]\t6584.0\t77.1 ± 37.1\t4.9 ± 1.6\r\nHe i\t6680.0\t14.7 ± 11.1\t0.8 ± 0.7\r\n[S ii]\t6717.0\t22.2 ± 0.1\t1.5 ± 0.7\r\n[S ii]\t6731.0\t21.4 ± 0.1\t1.4 ± 0.5\r\nHe i\t7065.0\t461.7 ± 210.2\t31.0 ± 12.2\r\n[Ar iii]\t7138.0\t12.6 ± 3.4\t1.0 ± 0.3\r\nFe ii\t7156.0\t26.2 ± 7.2\t1.8 ± 0.2\r\n[O ii]\t7323.0\t26.0 ± 23.0\t1.7 ± 1.5\r\n[O ii]\t7325.0\t16.9 ± 1.8\t1.2 ± 0.1\r\n[O ii]\t7332.0\t26.2 ± 9.1\t1.8 ± 0.6\r\nFe ii\t8228.0\t23.7 ± 4.2\t2.0 ± 0.3\r\nFe ii\t8239.0\t7.2 ± 4.0\t0.6 ± 0.3\r\nFe ii\t8289.0\t6.3 ± 3.7\t0.5 ± 0.3\r\nFe iii\t8306.0\t5.7 ± 3.6\t0.5 ± 0.3\r\nO i\t8448.0\t67.6 ± 2.4\t6.1 ± 1.3\r\nFe ii\t8470.0\t16.2 ± 5.0\t1.4 ± 0.4\r\nFe ii\t8490.0\t26.7 ± 4.3\t2.4 ± 0.4\r\nPa10\t9015.0\t16.5 ± 5.0\t1.8 ± 0.5\r\n[S iii]\t9071.0\t27.2 ± 2.3\t3.5 ± 0.3\r\nFe ii\t9075.0\t30.0 ± 4.7\t3.4 ± 0.5\r\nFe ii\t9125.0\t16.8 ± 5.2\t1.9 ± 0.6\r\nFe ii\t9134.0\t36.9 ± 5.0\t4.1 ± 0.6\r\nFe ii\t9179.0\t95.0 ± 5.5\t10.6 ± 0.6\r\nFe ii\t9204.0\t50.1 ± 6.1\t5.6 ± 0.7\r\nPa9\t9229.0\t19.4 ± 7.0\t2.2 ± 0.8\r\nFe ii\t9394.0\t17.3 ± 3.9\t2.0 ± 0.5\r\n[S iii]\t9533.0\t84.7 ± 5.9\t10.2 ± 0.7\r\nPa8\t9545.0\t44.8 ± 11.3\t5.4 ± 1.4\r\nFe ii\t9997.0\t29.5 ± 4.5\t3.8 ± 0.6\r\nPaδ\t10049.0\t104.2 ± 12.2\t13.7 ± 1.7\r\nFe ii\t10490.0\t8.0 ± 2.7\t1.1 ± 0.4\r\nFe ii\t10501.0\t24.4 ± 5.9\t3.1 ± 0.8\r\nHe i\t10830.0\t163.0 ± 96.0\t22.6 ± 13.3\r\nPaγ\t10938.0\t146.3 ± 25.5\t20.9 ± 3.8\r\nFe ii\t11128.0\t12.3 ± 3.7\t1.8 ± 0.6\r\nO i\t11290.0\t49.2 ± 4.1\t7.7 ± 2.3\r\nNote. aNot corrected for lensing magnification.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nTable 3. Fluxes of Broad Emission Lines and Their Rest-frame Equivalent Widthsa\r\n\r\nLine\tλrest\tFlux\tEW0\r\n \t(Å)\t(10−20 erg s−1 cm−2)\t(Å)\r\nBroad Emission Lines\r\nHα\t6562.8\t14803.5 ± 198.6\t946.3 ± 15.6\r\nHe i\t6680.0\t144.6 ± 44.7\t9.4 ± 2.9\r\nHe i\t7065.0\t824.2 ± 210.0\t55.4 ± 15.1\r\nPa10\t9015.0\t53.7 ± 11.1\t5.8 ± 1.3\r\nPa9\t9229.0\t119.0 ± 13.5\t13.6 ± 1.5\r\nPa8\t9545.0\t191.2 ± 17.0\t23.1 ± 2.1\r\nPaδ\t10049.0\t370.6 ± 15.0\t48.8 ± 2.3\r\nHe i\t10830.0\t2294.9 ± 212.6\t318.8 ± 30.3\r\nPaγ\t10938.0\t652.3 ± 14.0\t92.9 ± 2.4\r\nO i\t8448.0\t93.7 ± 7.9\t8.4 ± 0.7\r\nO i\t11290.0\t106.2 ± 63.9\t16.6 ± 10.4\r\nNote. aNot corrected for lensing magnification.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nTable 4. Kinematic Properties of Narrow Lines\r\n\r\nLine\tλrest\tFWHM\tΔv\r\n \t(Å)\t(km s−1)\t(km s−1)\r\nNarrow Emission Lines\r\n[O i]\t6300.3\t455 ± 175\t−101 ± 81\r\nHα\t6562.8\t304 ± 8\t+145 ± 13\r\n[N ii]\t6583.4\t347 ± 117\t+84 ± 47\r\n[S ii]\t6716.4\t232 ± 62\t+82 ± 33\r\n[S ii]\t6731\t232 ± 62\t+82 ± 33\r\nHe i\t6678.2\t87 ± 14\t+40 ± 14\r\nHe i\t7065.2\t408 ± 644\t+112 ± 396\r\n[Ar iii]\t7135.8\t89 ± 50\t−26 ± 20\r\nFe ii\t7155.2\t96 ± 50\t+15 ± 15\r\n[O ii]\t7320.0\t400 ± 120\t−37 ± 72\r\nFe ii\t8228.0\t290 ± 48\t+21 ± 5\r\nFe ii\t8239.0\t290 ± 48\t+21 ± 5\r\nFe ii\t8289.0\t290 ± 48\t+21 ± 5\r\nFe iii\t8306.0\t290 ± 48\t+21 ± 5\r\nO i\t8446.4\t235 ± 30\t−43 ± 19\r\nFe ii\t8470.0\t290 ± 48\t+21 ± 5\r\nFe ii\t8490.0\t290 ± 48\t+21 ± 5\r\nPa10\t9014.9\t259 ± 36\t−46 ± 19\r\n[S iii]\t9071.0\t230 ± 13\t⋯\r\nFe ii\t9075.0\t486 ± 24\t−21 ± 17\r\nFe ii\t9125.0\t486 ± 24\t−21 ± 17\r\nFe ii\t9134.0\t486 ± 24\t−21 ± 17\r\nFe ii\t9179.0\t486 ± 24\t−21 ± 17\r\nFe ii\t9204.0\t486 ± 24\t−21 ± 17\r\nPa9\t9229.0\t259 ± 35\t−46 ± 19\r\nFe ii\t9394.0\t486 ± 24\t−21 ± 17\r\nPa8\t9545.6\t259 ± 36\t−46 ± 19\r\n[S iii]\t9533\t230 ± 13\t+23 ± 13\r\nFe ii\t9997.0\t331 ± 55\t+90 ± 25\r\nPaδ\t10049.4\t332 ± 22\t+21 ± 15\r\nHe i\t10830.3\t287 ± 46\t+112 ± 26\r\nPaγ\t10938.1\t267 ± 25\t+26 ± 17\r\nFe ii\t10490.0\t332 ± 96\t+44 ± 43\r\nFe ii\t10501.0\t332 ± 96\t+44 ± 43\r\nFe ii\t11128.0\t153 ± 116\t+37 ± 30\r\nO i\t11290.0\t260 ± 58\t−33 ± 24\r\nNote. Velocity offsets (Δv) calculated relative to [S iii] λ9071 at z = 3.50102.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\nTable 5. Kinematic Properties of Broad and Absorption Lines\r\n\r\nLine\tλrest\tFWHM\tW\tΔv\r\n \t(Å)\t(km s−1)\t(km s−1)\t(km s−1)\r\nBroad Emission Lines\r\nHα\t6562.8\t1024 ± 21\t3010 ± 450\t−7 ± 16\r\nHe i\t6678.2\t1041 ± 792\t3890 ± 2083\t−137 ± 151\r\nHe i\t7065.2\t473 ± 116\t1000 ± 600\t−136 ± 82\r\nO i\t8446.4\t562 ± 331\t1120 ± 590\t+39 ± 80\r\nPa10\t9014.9\t766 ± 202\t2100 ± 600\t−155 ± 39\r\nPa9\t9229.0\t766 ± 202\t2100 ± 600\t−155 ± 39\r\nPa8\t9545.6\t766 ± 202\t2100 ± 600\t−155 ± 39\r\nPaδ\t10049.4\t1672 ± 458\t3500 ± 400\t+23 ± 44\r\nHe i\t10830.3\t536 ± 45\t2760 ± 220\t+154 ± 22\r\nPaγ\t10938.1\t1035 ± 322\t2400 ± 260\t−75 ± 31\r\nO i\t11287.0\t1188 ± 1099\t4300 ± 2000\t+245 ± 214\r\nAbsorption Lines\r\nHα\t6562.8\t1000 ± 123\t⋯\t−200 ± 32\r\nHe i\t7065.2\t587 ± 1024\t⋯\t−52 ± 83\r\nHe i\t10830.3\t794 ± 21\t⋯\t+45 ± 22\r\nNote. Velocity offsets (Δv) calculated relative to [S iii] λ9071 at z = 3.50102.\r\n\r\nDownload table as: \r\nASCIITypeset image\r\n\r\n3.3.1. Hα Complex\r\nHα is modeled with independent narrow, broad, and absorption components. [O i] λ6302 and He i λ6680 are modeled with narrow and broad profiles. [N ii] lines are fixed at a 1:3 ratio and share kinematics; [S ii] lines have independent amplitudes but tied velocities and widths.\r\n\r\nWe find that broad Hα and He i λ6680 are strongly favored to have exponential wings (ΔBIC ∼ −500), yielding a FWHM (of the intrinsic Gaussian core) of ∼1000 km s−1—significantly narrower than the ∼3000 km s−1 derived from pure Gaussians. Although no distinct Hα absorption component is explicitly detected, likely due to insufficient resolution, the overall asymmetry of the line is best reproduced when a weak, blueshifted absorber is included in the fit. This may indicate subtle self-absorption or partial obscuration within the dense cocoon. We return to the implications of this profile shape later.\r\n\r\n3.3.2. He i λ7065\r\nThe He i λ7065 line shows a prominent blueshifted absorption component. We fit it with narrow, broad, and absorption profiles. The rest of the lines, including [Ar iii] λ7138, Fe ii λ7156, and the [O ii] triplet (λλ7323, 7325, 7332), are modeled as independent narrow lines.\r\n\r\nHe i λ7065 shows a strong preference for an exponential profile (ΔBIC ∼ − 16) with a FWHM = 473 ± 116 km s−1. A residual bump spanning from ∼λ7290 to λ7320 is likely a combination of multiple Fe ii, such as λ7290, λ7308, and potentially Fe iii λ7319.65 lines. Curiously, the latter line is often labeled as “hazy” in various emission-line libraries (e.g., A. Kramida et al. 2024), reflecting its undefined shape as a result of pressure broadening or scattering in very dense gas.\r\n\r\n3.3.3. O i λ8448 and Iron Lines\r\nIn this part of the spectrum the O i λ8448 is fit with narrow and broad components. All of the iron lines, including Fe ii λλ8228, 8239, 8289, 8470, 8490 as well as a potential Fe iii λ8306, are fit as narrow lines with shared kinematics. O i components are fit independently.\r\n\r\nWe find that the broad O i component is best described by a standard Gaussian profile, with a stronger statistical preference over exponential wings (ΔBIC ∼ 4). However, we caution that a trough at ∼3.77 μm, likely an artifact, may affect the reliability of the fit in this region.\r\n\r\n3.3.4. Iron Forest and Paschen Lines\r\nThis spectral region is among the most complex, due to the dense clustering of emission features. The Paschen lines Pa10–Pa8 are modeled with narrow and broad components. To reduce the number of free parameters, we tie all narrow Paschen components together kinematically, and do the same for the broad components. Fe ii λλ9075, 9125, 9134,9179, 9204, 9394 are fit with a shared centroid and width. [S iii] lines are fit independently.\r\n\r\nThe [S iii] λ9071 line is used to define the systemic redshift: z = 3.50102 ± 0.00019. This is done because forbidden lines, such as [S iii] or [O iii], have lower critical densities that are incompatible with the dense-gas envelopes giving rise to the other lines we observe. These lines may instead come from the host galaxy itself (e.g., R. Maiolino et al. 2024), and we therefore choose this line to define the overall redshift of the system and to measure all the offsets relative to it. All velocity offsets discussed in the subsequent sections are computed relative to this reference frame. The Paschen lines show strong preference for exponential wings (ΔBIC ∼ −38), with a FWHM = 766 ± 202 km s−1—narrower than Hα, but consistent within 2σ.\r\n\r\n3.3.5. Paδ\r\nThe Fe ii λ9997 and Paδ complex is modeled with an independent narrow component for Fe ii and both narrow and broad components for Paδ. There is no evidence for absorption. Exponential wings are again preferred (ΔBIC ∼ −26). The resulting FWHM of 1672 ± 458 km s−1 is notably larger than those of both higher-order Paschen lines and Hα, though still consistent with the latter within 2σ. It is also possible that the line shape is impacted by Fe ii λ9997 and the undetected (but likely present) Fe ii λλ10131, 10173 lines.\r\n\r\n3.3.6. He i λ10830 and Paγ\r\nThe final window contains a complicated blend of broad He i λ10830 and Paγ lines, with a clear blueshifted absorption in the former. We fit three components (narrow, broad, and absorption) to He iλ10830 and narrow plus broad components to Paγ, keeping everything kinematically independent. We fit narrow Fe ii lines at 10490, 10501, and 11128 Å with fixed redshift and line width. Finally, O i λ11290 is fit with independent narrow and broad components. Exponential wings are again preferred over a pure Gaussian profile.\r\n\r\n4. Data Analysis\r\n4.1. Morphology\r\nLRDs are unresolved in the rest-optical by definition, with measured sizes consistent with the PSF HWHM ( in F444W), and in some cases even smaller when dithers align favorably (e.g., I. Labbé et al. 2025). Gravitational lensing can further push constraints on their intrinsic sizes to ≲100 pc (L. J. Furtak et al. 2024).\r\n\r\nIn the rest-UV, however, a more complex picture is emerging. Several studies have now reported faint, extended, asymmetric components adjacent to the compact core (V. Kokorev et al. 2024b; I. Labbe et al. 2024; J. Matthee et al. 2024; P. Rinaldi et al. 2025a, 2025b), often suppressed by surface-brightness dimming. As shown in Figure 1, GLIMPSE-17775 likewise consists of two components out to F200W (rest ∼ 4000 Å), coincident with the Balmer break. However, we note that the break itself is much weaker than found in objects with very similar spectra (e.g., B. Wang et al. 2024; see Figure 3). At longer wavelengths, a point-source (PS) morphology dominates, consistent with a black-hole-dominated core. To quantify this transition, we model the NIRCam imaging using PYSERSIC (I. Pasha & T. B. Miller2023) with a minimal configuration: a fixed-center PS plus a freely offset Sérsic profile. Normalizations, n, and reff are all allowed to vary, and uncertainties are drawn from the Markov Chain Monte Carlo posteriors (e.g., V. Kokorev et al. 2024a).\r\n\r\nZoom InZoom OutReset image size\r\nFigure 3. The diversity of Balmer breaks in LRDs. The black points show the HST and JWST GLIMPSE photometry of GLIMPSE-17775. The blue line shows best-fit EAZY SED fit to the photometry only, fixing the redshift to the zspec. The maroon line show the combined and photometry-corrected G395M spectrum. While the red color in F200W–F277W is partially influenced by a bright Hα line, the Balmer break between F150W and F200W is still prominent. We further show spectra of various other LRDs (I. Labbe et al. 2024; B. Wang et al. 2024; A. de Graaff et al. 2025b; R. P. Naidu et al. 2025; A. J. Taylor et al. 2025), all shifted to z = 3.501 and normalized at 5100 Å. Finally, we show HST (blue) and JWST (orange) filter transmission curves below.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nOur fits show that the host galaxy dominates up to λrest ∼ 4000 Å, where the host and nucleus contribute roughly equally, beyond which the PS prevails to λrest ∼ 1 μm. Because the NIRCam LW detector has ≳2× poorer resolution than the SW, a clean separation of host and nucleus in the rest-optical is impractical (see, e.g., K. E. Whalen et al. 2026). Fortunately, F200W lies at the transition where both the resolution and flux ratio are favorable, so we use that band to illustrate our galaxy/LRD decomposition. We illustrate this in Figure 4, which also shows the increasing PS fraction with wavelength, while acknowledging the uncertainties at longer wavelengths.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 4. Top: two-component Sérsic+point-source (PS) fit to the F200W morphology of GLIMPSE-17775. Panels show, from left to right, the data, best-fit model, model with the extended component removed, and residuals. Bottom: fractional PS contribution vs. rest-frame wavelength. Shaded regions mark SW (blue) and LW (red) detectors, where the lower resolution of LW filters hinders reliable two-component decomposition.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nAfter applying the lensing correction, we find that the extended component dominating the UV light has a radius of reff ∼ 1000 pc, whereas the actual compact LRD, dominant in the rest-optical, is fully consistent with the PSF and reff < 300 pc.\r\n\r\n4.2. Dust Attenuation\r\nThe ratio between observed emission-line fluxes is commonly used to estimate dust extinction. For LRDs, this has typically been achieved through the Balmer decrement, provided that multiple Balmer lines are available. In our case, only Hα is detected. While the Paschen series, of which five lines are observed, could, in principle, be used to estimate extinction, the likely presence of stratified dense gas in LRDs (A. de Graaff et al. 2025b; R. P. Naidu et al. 2025) implies that the intrinsic line ratios may deviate significantly from standard Case B recombination expectations (S.-J. Chang et al. 2026). Further, at the wavelengths of the Paschen series, the attenuation curves are practically flat (e.g., D. Calzetti et al. 2000). Small offsets of the Case B ratios would have a significant effect on the derived dust attenuation, but in return require extreme precision on measured line fluxes to be meaningful. Our uncertainties on, e.g., Paγ/Paδ are small, roughly 10%–15%, yet this still leads to an impractically high uncertainty on AV. To circumvent this limitation, we instead employ the ratio between the permitted O i λ8448 and O i λ11290 lines.\r\n\r\nThese transitions share a common energy level, and under the assumption of Bowen (Lyβ) fluorescence, all transitions through the λ11290 transition also cascade through the λ8448. This makes their intrinsic intensity set solely by the ratio of the inverse of their wavelengths.\r\n\r\nTo ensure we are comparing the same physical gas component, we isolate the narrow emission peaks in both transitions, which show consistent widths of FWHM ∼ 250 km s−1. This similarity supports the use of their flux ratio as a dust probe. We adopt the Small Magellanic Cloud (SMC) attenuation curve (K. D. Gordon et al. 2003), widely used for high-redshift galaxies and reddened AGN (P. F. Hopkins et al. 2004; P. L. Capak et al. 2015; N. A. Reddy et al. 2015, 2018; V. Kokorev et al. 2023; A. J. Taylor et al. 2025). Assuming an intrinsic ratio of (8448/11290)int = 1.336 (D. E. Osterbrock1989), we infer AV = 0.1 ± 0.3 mag, consistent with negligible extinction.\r\n\r\nWe caution, however, that this ratio probes only the narrow-line-emitting gas, which could originate either in the host galaxy or within a narrow-line region associated with the AGN. If the latter is the case, then the red optical continuum slope (βopt ∼ 0.35) would suggest that the observed SED is intrinsically red rather than reddened by dust. If instead the narrow lines arise predominantly in the host galaxy, this constraint does not directly inform the origin of the continuum emission. Similar Case B–consistent narrow-line ratios have been reported in other LRDs (e.g., M. Brooks et al. 2025; G. P. Nikopoulos et al. 2025), where the broad lines were found to show significant departures from Case B.\r\n\r\nAlthough the wavelength coverage of the red grating does not allow a Balmer decrement test for the broad-line emission (only Hα is detected), we can perform a consistency check using the brightest broad Paschen lines (Paγ, Paδ, and Pa8). Adopting intrinsic Case B ratios from P. J. Storey & D. G. Hummer (1995; Paγ/Paδ ≃ 1.5 and Paδ/Pa8 ≃ 1.8), and comparing these to our measured values of Paγ/Paδ = 1.77 ± 0.15 and Paδ/Pa8 = 1.94 ± 0.20, we find the broad Paschen lines to be consistent with Case B within ≃2σ, particularly when systematic uncertainties from blending and profile decomposition are taken into account. If Case B is applicable in the dense environments surrounding the central AGN, this would be consistent with a low-dust or dust-free origin for the broad-line-emitting gas.\r\n\r\n5. Line Properties\r\nOur fitting procedure yields over 40 emission and absorption features, most of which are detected at a high (S/N> 3) significance. With all the pieces in place, we now comment on the line profiles, kinematics, and the specific line species that we identify.\r\n\r\n5.1. Exponential Wings\r\nAs already noted throughout Section 4, and further highlighted in Figure 2, all permitted lines in the spectrum, with the exception of O iλ8448, which is likely impacted by data-quality issues, are better fit when the broad component is convolved with an exponential profile. The statistical preference for this model (as measured by ΔBIC) is especially strong for our brightest line, Hα. To further demonstrate this, and to compare this fit with a more standard, Gaussian-only approach, we show both models in Figure 5. When the broad line is fit using only a Gaussian profile, large portions of the line are underfit at a ≳3σ significance level, whereas a model that includes exponential wings shows a much smoother, albeit not perfect, residual plot.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 5. Exponential wings are required. Comparison of a Gaussian×exponential model (red) and a single Gaussian profile (blue) for Hα. Uncertainties are shown as vertical lines in each spectral bin, although they are too small to be visible. The exponential model provides a far superior fit, with smoother residuals and a strongly preferred ΔBIC, highlighting the necessity of exponential wings to capture the broad-line shape.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nThis strong preference for exponential wings is consistent with expectations from electron scattering in dense, ionized gas. Unlike Gaussian profiles, which arise from Doppler broadening due to thermal and bulk motions around the supermassive black hole, exponential profiles arise in environments dominated by electron scattering (e.g., S.-J. Chang et al. 2026; V. Rusakov et al. 2026). The absence of strong broadening in the forbidden lines (e.g., [S ii], [S iii], and [N ii]) already suggests that the densities where these electron-scattered profiles originate must already exceed multiple times the critical densities of these transitions (ne > 106). Combined with the fact that these broad profiles are non-Gaussian in shape, both the likely volume and column densities are likely even higher, at ne = 108 cm−3 and Ne ∼ 1024 cm−2, respectively, as suggested by both K. Inayoshi & R. Maiolino (2025) and V. Rusakov et al. (2026).\r\n\r\nRecent work (e.g., M. Brazzini et al. 2025) argues that, in classical broad-line region (BLR) environments, an electron-scattering origin for broad wings requires similar intrinsic and scattering widths across recombination lines. We therefore examine these criteria for the hydrogen transitions and find that, within the uncertainties of our fits, both the intrinsic and exponential widths are broadly comparable among the recombination lines. However, unlike classical BLRs, LRDs are expected to be strongly stratified, with different recombination transitions forming at different depths and probing different effective electron columns (e.g., A. de Graaff et al. 2025d; A. Sneppen et al. 2026). In such a structure, strict equality of widths is not expected even if a common scattering kernel shapes the wings. The modest variations observed here are therefore consistent with electron scattering in a dense, stratified cocoon.\r\n\r\nIt is important to note that such detailed profile decomposition is only possible due to the exceptionally high S/N per pixel achieved in the line wings of our NIRSpec G395M spectrum. As emphasized in V. Rusakov et al. (2026), these features would be impossible to distinguish with shallower data or lower-resolution modes such as NIRSpec/PRISM, or even G395M exposures lacking comparable depth.\r\n\r\n5.2. Line Profiles\r\nFurther, in Figure 6, we compare the best-fit models for all broad lines. As noted previously, with the exception of O i λ8448, every broad line is better described by exponential wings, resulting in very similar overall line shapes. The main differences arise in their widths.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 6. Best-fit profiles of all broad lines, oversampled and shifted to a common center. The top panel shows hydrogen recombination (Hα, black, and Paschen series), the middle panel shows O i, and the bottom panel shows He i. Shaded regions indicate 1σ uncertainties for the least-constrained lines (Paδ, O i λ11290, and He i λ6680); uncertainties for the remaining lines are omitted for clarity. We note that hydrogen and O i lines show largely similar widths, consistent with their coupling through charge exchange. By contrast, He i lines are systematically narrower, likely reflecting their distinct metastable triplet physics and formation in a less dense outer region.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nDespite some fits having sizable uncertainties, a trend emerges across line species. Hydrogen recombination lines (with the exception of Paδ) and O i transitions consistently show comparable intrinsic FWHM values of ∼800 km s−1. This agreement is not coincidental. Neutral oxygen and ionized hydrogen have nearly identical ionization potentials, enabling rapid charge-exchange coupling between O+ + H0⇌ O0 + H+ (D. E. Osterbrock & G. J. Ferland 2006). This continual electron exchange tightly locks the spatial distribution, ionization state, and kinematics of neutral oxygen to ionized hydrogen (and vice versa), so their broad-line profiles are naturally expected to track one another. The observed similarity therefore provides an important consistency check, reinforcing that the O i emission originates in the same dense, ionized gas as the hydrogen recombination lines. In contrast, the Fe ii lines exhibit significantly narrower widths, matching the narrow cores of the permitted transitions rather than their exponential wings. This implies that the Fe ii emission arises in a cooler, less turbulent zone exterior to the scattering-dominated region, but still closely coupled to the AGN continuum source.\r\n\r\nBy contrast, He i emission is systematically narrower. He i lines such as λ7065 and λ10830 do not couple to hydrogen via charge exchange, and their lower metastable level (23S) has distinct population physics, being fed by both collisional and recombination pathways. Further, one has to take into account the radiative-transfer effects, which make it possible to radiatively excite metastable ground-state electrons. As a result, He i emission may arise from a somewhat different spatial or kinematic region than H and O. We return to this point in more detail below.\r\n\r\nTaken together, the similar FWHM of hydrogen and oxygen broad-line profiles, combined with the near-universal exponential wings seen across all permitted transitions, strongly suggests that the line shapes are set by a common, line-independent scattering kernel rather than by transition-specific processes. Electron (Thomson) scattering in a dense, ionized cocoon provides a natural explanation: It produces exponential wings of nearly identical form across species, with widths set primarily by the electron temperature and column density (typically ∼1024 cm−2), and leaves only secondary variations from species-specific excitation or optical-depth effects (e.g., S.-J. Chang et al. 2026; V. Rusakov et al. 2026). In this framework, the narrower He i lines reflect stratification within the cocoon, where He i emission arises from an outer region that has a lower density, temperature, or column density, while the bulk hydrogen and oxygen emission share a common kinematic imprint within an inner, denser region.\r\n\r\n5.3. Line Kinematics\r\nBefore we proceed to discussing the individual features in more detail, we would like to comment on the systematic velocity offsets between various line species in the spectrum of GLIMPSE-17775. As mentioned previously, we choose the redshift of the narrow forbidden [S iii] λ9701 as the systemic reference, due to it being relatively bright and isolated. We place all velocity offsets in context by plotting all values from Tables 4 and 5 in Figure 7.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 7. Velocity offsets (relative to [S iii]λ9071) and FWHM for all detected lines. Narrow permitted lines are shown as maroon circles (open for forbidden), broad lines as blue, absorption as gold, and Fe ii lines as green diamonds. The shaded band marks the velocity uncertainty set by the median spectral resolution. Narrow lines align closely with the systemic redshift, while absorption features show moderate blueshifts of ∼150 km s−1.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nWhile every fit formally yields a centroid, the significance of any offset is constrained by the spectral resolution and S/N of the data. To gauge which velocity shifts are meaningful, we adopt a conservative uncertainty of ΔV ∼ med(R)/5, with R = λ/Δλ. This corresponds to ∼60 km s−1, below which offsets are unlikely to be statistically significant.\r\n\r\nQualitatively, we do not find systematic shifts of either permitted or forbidden narrow lines relative to the systemic redshift. Iron lines also appear consistent with the systemic velocity. In contrast, the permitted broad lines, together with their associated absorption components, show a consistent blueshift of order ∼100 km s−1.\r\n\r\nSuch blueshifts are commonly interpreted as signatures of outflowing gas in the BLR, where scattering and absorption occur preferentially along outflowing sight lines. In the context of GLIMPSE-17775, this modest but systematic offset strengthens the case for a stratified cocoon, while the narrow lines trace gas in the outer regions at systemic velocity, the BLR and absorbing layers appear to be participating in bulk outflows. Confirming the detailed velocity structure, however, will require higher-resolution follow-up with the NIRSpec H-gratings (e.g., A. Saldana-Lopez et al. 2025; A. Torralba et al. 2026).\r\n\r\n5.4. Hydrogen Absorption Lines\r\nAlthough no strong hydrogen absorption lines are explicitly detected, the Hα profile (Figure 2) shows a noticeable asymmetry, with suppressed flux on the blue side of the line. This feature is best modeled by a blueshifted (∼−200 km s−1) absorption component, as already noted in Section 4. Similar nonresonant absorption signatures (e.g., Balmer lines) are now routinely observed in LRDs across a wide range of redshifts (e.g., J. E. Greene et al. 2024; V. Kokorev et al. 2024b; I. Labbe et al. 2024; X. Lin et al. 2024; A. J. Taylor et al. 2025). The presence of such absorption implies high gas densities of order n ∼ 109 cm−3 (P. B. Hall 2007; K. Inayoshi & R. Maiolino 2025). Interestingly, only atoms in the n = 2 state appear significantly populated, as we detect no evidence for Paschen absorption in any of the five lines present in our spectrum. This is not an instrumental effect of the M-grating, as we clearly detect an absorption feature in He i λ10830 but not in the immediately adjacent Paγ. This indicates that the n = 3 state is comparatively underpopulated.\r\n\r\nAnother key manifestation of the same physical mechanism is the Balmer break, corresponding to the n = ∞ → n = 2 transition limit. A prominent break is common in many LRD spectra (D. J. Setton et al. 2025), though not ubiquitous (e.g., V. Kokorev et al. 2023; R. Tripodi et al. 2025). While our spectral coverage does not extend to the Balmer limit itself, we observe a discontinuity of ∼1 mag between the F200W and F150W filters. Due to the F200W coverage of the SED, this flux jump cannot be attributed to line boosting from Hβ and the [O iii] doublet. Adopting the break parameterization of R. P. Naidu et al. (2025), we use our best-fit SED and measure fν,4050Å/fν,3670Å = 2.02 ± 0.10. Although weaker than the extreme values (∼4–7) reported for LRDz9 (A. J. Taylor et al. 2025), MoM BH*-1 (R. P. Naidu et al. 2025), or “the Cliff” (A. de Graaff et al. 2025b), this value lies close to the maximum achievable by evolved stellar populations (I. Labbe et al. 2024; B. Wang et al. 2024). However, this measurement is based on the total (PS+host) photometry. Given that the UV continuum is spatially resolved, as we have shown in Section 4.1, host-galaxy contamination may dilute the intrinsic break strength of the central component. While uncertainties on the PS/host decomposition increase significantly toward the rest-optical, we find that using the PS-only photometry produces a noticeably sharper break, increasing the inferred strength by ∼30%–50% to fν,4050Å/fν,3670Å ≈ 2.6–3.0. Although this does not allow us to robustly conclude whether the intrinsic PS break reaches the most extreme BH*-type objects (A. de Graaff et al. 2025b; R. P. Naidu et al. 2025; A. J. Taylor et al. 2025), it suggests that the Balmer discontinuity becomes stronger once the host contribution is removed, consistent with recent findings that host light can suppress the apparent break amplitude (e.g., A. de Graaff et al. 2025d; W. Q. Sun et al. 2026).\r\n\r\nTaken together, the presence of asymmetry in the Hα profile, likely caused by blueshifted Balmer absorption, and a Balmer break adds to the evidence, complementing the exponential line wings, that the emission in GLIMPSE-17775 arises from a dense, ionized cocoon of gas. The lack of a detectable Paschen break is consistent with this picture, as high densities and optical depths result in Thomson scattering while also naturally washing out higher-order continuum edges (e.g., B. Wang et al. 2025). Assuming LTE, an extremely low ratio n3/n2 ≲ 0.01 corresponds to an electron temperature of Te ∼ 5000 K or below, consistent with the warm, partially ionized gas expected in dense LRD cocoons.\r\n\r\nWe also observe moderately prominent and extremely prominent blueshifted absorption, respectively, in He i λ7065 and He i λ10830. The mechanism for this is similar, but not identical to, the hydrogen lines. We also note the prominent blueshifted absorption seen in both He i λ7065 and He i λ10830. However, the physical mechanism driving these helium features differs fundamentally from that of the hydrogen lines; we return to this in the following section.\r\n\r\n5.5. Helium Lines\r\nBoth He i λ7065 and He i λ10830 show blueshifted (∼70−80 km s−1 from the narrow-line center) absorption components with widths of ∼600−700 km s−1. Unlike the Balmer series, helium transitions are resonantly scattered, so the arguments regarding n = 2 state abundances do not apply. Before addressing the absorption itself, it is useful to consider what the observed line strengths already tell us.\r\n\r\nIn the spectrum of GLIMPSE-17775, we detect three He i lines: λ6680, λ7065, and λ10830. These originate from different physical mechanisms. The λ6680 singlet line is produced via recombination or radiative pumping, and is only weakly dependent on density. By contrast, λ7065 and λ10830 belong to the triplet system (along with λ3889, not covered by G395M), where the lower level is populated due to its very long lifetime. Electrons in this “ground state” can be collisionally or radiatively excited into higher energies, and therefore the triplet-line strengths depend strongly on density and, to a lesser extent, temperature. As emphasized by D. A. Berg et al. (2026), He i λ10830 is the most sensitive density diagnostic among these transitions, followed by λ7065. The fact that both are much stronger than λ6680 indicates that the region where they form is very dense. The prominence of λ10830 in particular already points to a high-density environment with a temperature T ≳ 104 K. Further, the broad λ6680 line has a noticeably larger FWHM than the triplet lines but is consistent with hydrogen recombination lines, which again makes sense since both originate from the same mechanism.\r\n\r\nWhat about absorption? Its presence further reinforces this picture. The lower level (23S) of the triplet system is a metastable, long-lived state that effectively acts as a ground state in dense or partially ionized gas. As a result, photons from the 23P → 23S transition can be resonantly absorbed and reemitted many times, analogous to Lyα or Mg ii. This mechanism naturally produces strong absorption features when the He i column density is high. The fact that He i λ10830 not only dominates the helium spectrum in emission but also shows the deepest absorption in the entire spectrum provides compelling evidence for a dense, ionized cocoon of gas enshrouding GLIMPSE-17775.\r\n\r\n5.6. Oxygen Lines\r\nAbove, we noted that O i λ8446 and λ11290 share very similar profiles with the hydrogen recombination lines. This is naturally expected because neutral oxygen is tightly coupled to hydrogen via charge exchange, which rapidly equilibrates the O/H ionization states in dense gas. When charge exchange is fast (high nH), the O i/O ii ratio tracks the H i/H ii ratio, so the O i-emitting gas shares the same kinematics as the hydrogen recombination region (B. T. Draine 2011). The observed agreement in FWHM between H and O i lines is therefore an important consistency check that both species originate in the same dense, partially ionized phase.\r\n\r\nA second, independent clue of high gas density and radiation field intensity comes from the excitation mechanism. The O iλ8446–λ11287 pair is the classic signature of Lyβ (Bowen) fluorescence: Lyβ pumps O i from the ground state and the ensuing cascade preferentially populates the levels that emit at 1.129 μm, which then cascade down through the 8446 Å line. In this channel, the line emissivity scales with both the neutral oxygen (or equivalently neutral hydrogen, via charge exchange) column and the local Lyβ radiation field. Therefore, producing strong O i fluorescence requires both a very bright Lyβ source and a dense neutral (or partially ionized) cocoon.\r\n\r\nFurther, we do not detect (5σ upper limit <12/[10−20 erg s−1 cm−2]) any of the other permitted O iλ7774, λ7254, and λ7790 lines, and the [O i] λ6302/O i λ8446 ratio is weak. If collisional excitation or pure recombination dominated, these lines would be comparatively strong; their absence strongly favors Bowen fluorescence as the primary driver of the observed O i emission.\r\n\r\nFinally, the velocity structure adds a natural stratification: hydrogen recombination and O i (fluorescent, charge-exchange coupled) share similar widths and profiles, while He i lines are systematically narrower. Since He i triplet transitions emerge from a metastable 23S level (with distinct, density-sensitive population pathways and resonant transfer), they likely trace a kinematically distinct layer within the same cocoon.\r\n\r\n5.7. Lyα Fluorescence in Iron Lines\r\nPermitted iron emission, primarily Fe ii and Fe iii (e.g., I. Labbe et al. 2024; R. Tripodi et al. 2025; A. Torralba et al. 2026), but in some cases extending to highly ionized species such as Fe vii (E. Lambrides et al. 2025; M. Tang et al. 2025) and Fe x (L. J. Furtak et al. 2024), has become a recurring feature in LRD spectra. In GLIMPSE-17775, the spectrum is exceptionally rich in NIR iron lines; we identify 16 Fe ii and one Fe iii transition. Understanding the origin of this emission is key to interpreting the dense-gas environment in LRDs.\r\n\r\nThe physics of Fe ii emission has long been a challenge for BLR photoionization models (M. Joly 1993). Thick, high-column-density (∼1025 cm−2) gas at the edges of the accretion disk has been invoked as a potential source (M. Joly 1987; S. Collin-Souffrin et al. 1988), where the scattering and absorption of the hard X-ray photons ionize the gas. Similarly, this would also enhance the Balmer and Paschen line luminosities. Further, extensive theoretical work has shown that Lyα fluorescence is fundamental in reproducing the observed Fe ii strengths (T. A. A. Sigut & A. K. Pradhan 1998, 2003). Lyα pumping not only boosts the UV and optical Fe ii emission, but also predicts strong lines in the NIR.\r\n\r\nThis expectation aligns closely with our observations. In Figure 8, we compare our measured Fe ii flux ratios (normalized to Fe ii λ9075) against the Lyα-pumped model predictions of T. A. A. Sigut & A. K. Pradhan (2003). With the exception of Fe ii λ9179, affected by blending with Fe ii λ9204 and Pa9, we find remarkably good agreement across the suite of detected features. In particular, the dense forest of Fe ii transitions spanning λλ9000–9200 (center-right panel in Figure 2) is reproduced almost exactly by the theoretical spectrum (see Figure 11 in T. A. A. Sigut & A. K. Pradhan 2003). We overlay the T. A. A. Sigut & A. K. Pradhan (2003) model directly on our continuum-subtracted fit in Figure 8, demonstrating that the observed Fe ii emission is fully consistent with fluorescence in dense gas near the BLR. The implication is that the majority of the Fe ii emission in GLIMPSE-17775 arises through Lyα pumping, directly tracing an extremely dense medium, ionized by an extremely luminous source, likely an accreting black hole. Given that the Fe ii lines are somewhat narrower than other permitted features, it is likely that the emitting region is located farther from the BLR—something that has already been shown in a classic example of a narrow Fe ii emitter, I Zw 1 (R. J. Rudy et al. 2000; A. O. M. Marinello et al. 2016).\r\n\r\nZoom InZoom OutReset image size\r\nFigure 8. Lyα-pumped iron emission in GLIMPSE-17775. Left: observed Fe ii flux ratios (black points), normalized to Fe iiλ9075, compared with predictions from Lyα fluorescence models of T. A. A. Sigut & A. K. Pradhan (2003, blue). The close correspondence across ∼14 lines indicates a common excitation mechanism driven by Lyα pumping in dense, partially shielded gas. Right: zoom in on the λλ9000–9400 complex, showing the remarkable agreement between the modeled continuum-subtracted Fe ii spectrum (black) and the T. A. A. Sigut & A. K. Pradhan (2003) model (blue). We show air wavelengths of each Fe ii line directly from T. A. A. Sigut & A. K. Pradhan (2003), including the blended features. Together, these comparisons support an origin in the dense inner regions of the cocoon surrounding the accreting black hole.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nTogether with the Balmer absorption, helium triplet features, and Bowen fluorescence in O i, the iron forest adds another piece of evidence that points to a dense cocoon enshrouding the black hole.\r\n\r\n5.8. Source Properties\r\nBased on the previous discussion, we now present the likely physical properties of the black hole and its host. The coexistence of broad permitted and narrow forbidden lines indicates, as in most LRDs (R. E. Hviding et al. 2025), that the broad components originate in an AGN BLR. Following J. E. Greene & L. C. Ho (2005), we derive MBH from the luminosity and width of the broad Hα line, assuming the exponential-wing profile demonstrated in Figures 2 and 5. With a FWHMHα = 1024 ± 21 km s−1, negligible dust, and μ = 2.04, we obtain , where the dominant uncertainty arises from the J. E. Greene & L. C. Ho (2005) calibration. A purely Gaussian fit, though statistically disfavored, would yield a FWHM 3 times larger and a black hole mass nearly a dex higher. Throughout this work, we adopt the MBH from the exponential model.\r\n\r\nFurther, by assuming that the bolometric luminosity (Lbol) scales as Lbol = 130 × LHα (G. T. Richards et al. 2006), we find Lbol = (1.06 ± 0.14) × 1045 erg s–1. Using our MBH derived by assuming exponential wings, we find that this object is accreting at a super-Eddington rate, Lbol/Ledd = 1.86 ± 0.25. This is higher than the vast majority of LRDs at all redshifts (e.g., V. Kokorev et al. 2023; L. J. Furtak et al. 2024; I. Juodžbalis et al. 2024; R. Maiolino et al. 2024; H. B. Akins et al. 2025b; D. D. Kocevski et al. 2025; A. J. Taylor et al. 2025), found to accrete at sub-Eddington rates. However, recent works examining LRDs with extreme Balmer breaks derive accretion rates that exceed the Eddington limit (E. Lambrides et al. 2024; A. de Graaff et al. 2025b; R. P. Naidu et al. 2025).\r\n\r\nA recent work examining multiwavelength LRD data suggests that the bolometric luminosity emerges predominantly from the rest-frame optical, with X-ray and radio contributions being largely subdominant (J. E. Greene et al. 2026). Given the suggested dominance of optical light in LRDs, the much lower bolometric corrections (×7–10 lower) would imply lower black hole masses and total bolometric luminosities (e.g., those derived from Hα) than standard AGN prescriptions (e.g., J. E. Greene & L. C. Ho 2005) might suggest. This adjustment would lower both the inferred black hole masses and bolometric luminosities. Because these two quantities scale together, the implied super-Eddington nature of GLIMPSE-17775 would remain unchanged, although the black hole mass could decrease to ∼105.5–105.8M⊙. This interpretation is consistent with dense-gas (BH*) models, which generically predict Eddington or super-Eddington accretion in heavily obscured environments (e.g., D. Kido et al. 2025; H. Liu et al. 2025; A. Sneppen et al. 2026). A more detailed reassessment of bolometric corrections for LRDs is clearly warranted, but such an analysis lies beyond the scope of this work. For consistency with previous studies, we adopt standard AGN bolometric corrections throughout, with all derived parameters listed in Table 1.\r\n\r\nFinally, we estimate an upper limit on the stellar mass in GLIMPSE-17775. Previous studies have modeled LRDs using joint galaxy+AGN SED decomposition (e.g., V. Kokorev et al. 2023; L. J. Furtak et al. 2024), and more recently, within the BH* framework, have assumed that most of the rest-UV flux arises from the host galaxy (R. P. Naidu et al. 2025; A. J. Taylor et al. 2025). Our spatial decomposition (Figure 4) supports this assumption: The extended component contributes >80% of the rest-UV light, implying that the bulk of the stellar mass resides in this resolved structure. Given this, we adopt a simple empirical approach using the MUV–M* relation (e.g., D. P. Stark et al. 2009; I. Labbé et al. 2013) and obtain a conservative upper limit on the stellar mass of M* ≲ 107.5M⊙. This in turn gives us a black hole-to-host mass ratio of ≲0.14, which is significantly elevated from local expectations (J. E. Greene & L. C. Ho 2005), but is not as extreme as some other LRDs reported in the literature (V. Kokorev et al. 2023; L. J. Furtak et al. 2024; R. Maiolino et al. 2024).\r\n\r\n6. Discussion and Summary\r\n6.1. Dense and Ionized Gas Surrounding the AGN\r\nOur NIRSpec G395M observations of GLIMPSE-17775 reveal a remarkably consistent picture: Across independent tracers, the line emission requires an environment of extremely high density and partial ionization.\r\n\r\nFirst, the broad permitted lines are universally better fit by exponential wings, a hallmark of electron scattering in gas with ne ≳ 108 cm−3 and column densities approaching Ne ∼ 1024 cm−2. Such profiles are not reproduced by Doppler broadening alone and point to an ionized scattering medium enveloping the source. The fact that hydrogen and O i lines share consistent FWHM values further anchors this interpretation, as charge exchange tightly couples neutral oxygen to the ionization and kinematics of hydrogen.\r\n\r\nSecond, the detection of blueshifted Balmer absorption and a significant Balmer break both require high n = 2 populations and densities n ∼ 109 cm−3. Helium transitions provide a complementary view: The triplet lines λ7065 and λ10830 are both strongly enhanced relative to the singlet states and show deep blueshifted absorption, consistent with resonant scattering from the metastable 23S level. Their systematically narrower widths compared to hydrogen and oxygen suggest stratification, with helium arising from denser, more compact layers of the cocoon.\r\n\r\nThird, the O i λ8446–λ11290 pair confirms Lyβ fluorescence, requiring both a bright Lyβ radiation field and a dense reservoir of neutral gas. The absence of other permitted O i lines not fed by Lyβ strengthens this conclusion. Finally, the detection of 16 Fe ii lines, forming an incredibly rich iron forest in this LRD, matches predictions from Lyα fluorescence models, again demanding an intense radiation field and very high densities.\r\n\r\nBecause the BLR is unresolved in essentially all AGN, broad-line widths are traditionally interpreted as virial tracers of the black hole potential. In GLIMPSE-17775, the virial story alone is insufficient: The issue is not how broad the lines are, but how they broaden. The profiles exhibit extended, nearly linear wings in velocity space that are incompatible with a Gaussian. Instead, the lines are systematically and significantly better described by a model consisting of a narrow Gaussian core (virial motion) plus exponential wings, the hallmark of Thomson scattering in a dense ionized medium. Thus, the line shape encodes both gravitational kinematics and radiative-transfer physics in the surrounding cocoon. Our schematic (Figure 9) summarizes this revised view: In LRDs, broad-line profiles are not set by dynamics alone, but by the scattering environment through which the photons escape.\r\n\r\nZoom InZoom OutReset image size\r\nFigure 9. Physical picture of the dense cocoon around GLIMPSE-17775. The inner region (1) corresponds to the dense, highly ionized broad-line region (BLR) where electron scattering (orange lines) produces exponential wings, H and O I share coupled kinematics (via charge exchange and Bowen fluorescence), and strong Balmer absorption/break signatures arise. The outer layer (2) represents an intermediate-density ionized medium, where He I triplet lines show resonant absorption from the metastable 23S level and Fe II emission is driven by Lyα fluorescence. Together, these zones form a stratified cocoon enshrouding the accreting black hole. The bottom-right panel shows stacked line profiles of H, O i, He i, and Fe ii.\r\n\r\nDownload figure:\r\n\r\nStandard imageHigh-resolution image\r\nSuch conditions—high optical depths, large column densities, and evidence for radiation-dominated gas—are precisely those expected in super-Eddington accretion flows. In this regime, radiation pressure inflates the inner accretion structure, driving powerful winds and forming the very dense, partially ionized envelope we infer here. The low X-ray luminosities and weak radio emission commonly observed in LRDs (e.g., T. T. Ananna et al. 2024; M. Yue et al. 2024; H. B. Akins et al. 2025a; M. Kokubo & Y. Harikane 2025) are consistent with this picture: The X-rays are likely absorbed or thermalized within the optically thick cocoon, while dust cannot survive in such an intense radiation field (e.g., E. Lambrides et al. 2024; A. de Graaff et al. 2025b; K. Inayoshi & R. Maiolino 2025; R. P. Naidu et al. 2025; A. J. Taylor et al. 2025). Thus, the spectroscopic signatures observed in GLIMPSE-17775—exponential wings, absorption features, and fluorescence-driven metal lines—fit naturally into a scenario where super-Eddington accretion onto a low-mass black hole powers the luminous yet heavily reprocessed emission.\r\n\r\nTaken together, the exponential wings, Balmer and helium absorption, Bowen oxygen lines, and Lyα-pumped iron forest all converge on the same physical picture: GLIMPSE-17775 is enshrouded in a dense, partially ionized cocoon of gas.\r\n\r\n6.2. Final Remarks\r\nUsing a combination of the intrinsically deepest NIRCam photometry and NIRSpec G395M observations of the lensed AS1063 field, we present a detailed investigation of a LRD at z = 3.501. The spectrum of GLIMPSE-17775 is exceptionally rich, with more than 40 detected features, allowing us to probe the physical conditions of the gas with unprecedented detail. Multiple independent diagnostics converge on the presence of a dense, partially ionized cocoon heated by a powerful ionizing source.\r\n\r\nTypical of other LRDs, GLIMPSE-17775 is extremely compact in the rest-optical (reff < 300 pc) but exhibits more extended structure in the rest-UV (reff ∼ 1000 pc; Figure 1). It shows unmistakable AGN signatures through broad permitted lines (e.g., D. D. Kocevski et al. 2023; V. Kokorev et al. 2023; J. E. Greene et al. 2024; L. J. Furtak et al. 2024). The uniquely deep G395M spectrum further reveals clues to the physical origin of both its continuum and line-emission properties: We detect exponential broad-line wings, Balmer and helium absorption, Bowen-pumped O i, Fe ii emission produced by Lyα fluorescence, and evidence for rapid, potentially super-Eddington growth.\r\n\r\nTogether, these diagnostics provide one of the clearest cases yet for the BH* “dense cocoon” scenario (A. de Graaff et al. 2025b; K. Inayoshi & R. Maiolino 2025; R. P. Naidu et al. 2025; A. J. Taylor et al. 2025). The same ingredients we observe—exponential broad wings, Balmer-break absorption, He i absorption, and rich Fe ii and O i fluorescence—have been detected individually in several other bright LRDs with medium- and high-resolution spectroscopy (e.g., L. J. Furtak et al. 2024; I. Juodžbalis et al. 2024; I. Labbe et al. 2024; F. D’Eugenio et al. 2025; E. Lambrides et al. 2025; B. Wang et al. 2025; A. Torralba et al. 2026), suggesting that dense, optically thick gas may be a common feature of the population rather than an anomaly. What distinguishes GLIMPSE-17775 is that all signatures are captured simultaneously and at high S/N, allowing a self-consistent physical interpretation. If such cocoons are widespread, then super-Eddington accretion may be a typical pathway for black hole growth in LRDs, especially among the most luminous systems. Establishing how these signatures vary with luminosity and redshift will be essential for determining whether dense cocoons represent a dominant mode of early black hole assembly.\r\n\r\nThe convergence of five independent diagnostics—exponential scattering wings, Balmer-limit absorption, helium triplet physics, and two distinct fluorescence channels—leaves little doubt: GLIMPSE-17775 hosts a dense (n ∼ 108−9 cm−3), optically thick (Ne ∼ 1024 cm−2) cocoon of partially ionized gas surrounding a super-Eddington accreting black hole. This represents some of the most direct and comprehensive spectroscopic evidence to date for the dense cocoon scenario in LRDs.\r\n\r\nAcknowledgments\r\nThe authors would like to thank Aaron Sigut and Anil Pradhan for their help with understanding iron emission in active galactic nuclei. The authors would like to acknowledge the National Institute of Standards and Technology (NIST) database of spectral lines (A. Kramida et al. 2024), which made identification of less-known emission features possible. V.K., J.C., S.F., D.B., L.F., T.H., and J.M. acknowledge support from the University of Texas at Austin Cosmic Frontier Center. A.Z. acknowledges support by the Israel Science Foundation grant No. 864/23. This work is based on observations made with the NASA/ESA/CSA James Webb Space Telescope, obtained at the Space Telescope Science Institute, which is operated by the Association of Universities for Research in Astronomy, Incorporated, under NASA contract NAS5-03127. The JWST 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:10.17909/4byn-fe55 and doi:10.17909/zq0c-8t87. These observations are associated with programs GO #3293 and DDT #9223.\r\n\r\nFacilities: JWST - James Webb Space Telescope, HST - Hubble Space Telescope satellite.\r\n\r\nSoftware: EAZY (G. B. Brammer et al. 2008), grizli (G. Brammer 2023), msaexp (G. Brammer 2022), photutils (L. Bradley et al. 2020), pysersic (I. Pasha & T. B. Miller 2023), sep (K. Barbary 2016), SExtractor (E. Bertin & S. Arnouts1996).","status":"public","type":"journal_article","scopus_import":"1","researchdata_availability":"no","publication":"The Astrophysical Journal","das_tickbox":"1","date_published":"2026-06-10T00:00:00Z","has_accepted_license":"1","DOAJ_listed":"1","title":"The Deepest GLIMPSE of a dense gas cocoon enshrouding a Little Red Dot","OA_place":"publisher","ddc":["520"],"OA_type":"gold"},{"OA_type":"gold","DOAJ_listed":"1","has_accepted_license":"1","title":"Active and probe-free intracellular rheology via phase-sensitive thermoviscous flows","ddc":["570"],"OA_place":"publisher","publication":"PNAS Nexus","date_published":"2026-06-01T00:00:00Z","das_tickbox":"1","type":"journal_article","researchdata_availability":"yes","scopus_import":"1","acknowledgement":"The authors gratefully acknowledge help from Dr. Benjamin Seelbinder, Mr. Claudius George, and Mr. Falk Elsner in designing and constructing the magnetic needle for force-driven rheology experiments. We thank Dr. Iain Patten for valuable discussions on the structure of the manuscript and Mr. Ivan Saraev for graphics support. I.D.S. and M.K. kindly acknowledge funding from the Life grant by Volkswagen Foundation (Life! grant no. 92772), Deutsche Forschungsgemeinschaft (DFG, German Research Foundation, Germany's Excellence Strategy, 2082/1 and grant no. 515462906), and the Hector Foundation. I.D.S. was additionally funded by the Karlsruhe Institute of Technology (Excellence Strategy via the Young Investigator Group Preparation Program). V.R.K., S.W., and M.K. thank the ERC Starting Grant GHOSTs (grant no. 853619).","status":"public","article_processing_charge":"Yes","date_created":"2026-07-13T09:50:12Z","oa":1,"day":"01","publisher":"Oxford University Press","_id":"22297","abstract":[{"lang":"eng","text":"Determination of the rheological properties of cells is known to require active measurements, which largely depend on the internalization of mechanical probes. Here, we circumvent this problem via the introduction of Rheological focused light-induced cytoplasmic streaming (Rheo-FLUCS): an active, yet probe-free approach that leverages light-induced flows to access mechanical changes in complex systems. While Rheo-FLUCS is facilitated by thermoviscous expansion phenomena rather than external forces, here we show equivalence in its ability to measure relative viscoelastic properties. Specifically, we demonstrate a phase-lag equivalence with probe-dependent active microrheology in a wide range of physically different, yet chemically identical materials. We exemplify the utility of Rheo-FLUCS in three distinctly different biological systems: compound-treated mouse fibroblasts (NIH-3T3), genetically modified human osteoblasts (U2OS) to elucidate the role of myosins in cytoplasmic mechanics, and early ascidian oocytes of Phallusia mammillata at fertilization stage. Our biological use-cases exemplify the application versatility of Rheo-FLUCS, which in the future may use phase information as a marker for developmental success."}],"date_updated":"2026-07-13T13:14:43Z","publication_identifier":{"eissn":["2752-6542"]},"language":[{"iso":"eng"}],"volume":5,"doi":"10.1093/pnasnexus/pgag190","citation":{"mla":"Stoev, Iliya D., et al. “Active and Probe-Free Intracellular Rheology via Phase-Sensitive Thermoviscous Flows.” PNAS Nexus, vol. 5, no. 6, pgag190, Oxford University Press, 2026, doi:10.1093/pnasnexus/pgag190.","short":"I.D. Stoev, M. Bolger-Munro, A. Minopoli, S. Wagner, V.R. Krishnaswamy, E. Erben, K. Weißenbruch, N. Maghelli, M. Bastmeyer, C.-P.J. Heisenberg, M. Kreysing, PNAS Nexus 5 (2026).","ista":"Stoev ID, Bolger-Munro M, Minopoli A, Wagner S, Krishnaswamy VR, Erben E, Weißenbruch K, Maghelli N, Bastmeyer M, Heisenberg C-PJ, Kreysing M. 2026. Active and probe-free intracellular rheology via phase-sensitive thermoviscous flows. PNAS Nexus. 5(6), pgag190.","ama":"Stoev ID, Bolger-Munro M, Minopoli A, et al. Active and probe-free intracellular rheology via phase-sensitive thermoviscous flows. PNAS Nexus. 2026;5(6). doi:10.1093/pnasnexus/pgag190","apa":"Stoev, I. D., Bolger-Munro, M., Minopoli, A., Wagner, S., Krishnaswamy, V. R., Erben, E., … Kreysing, M. (2026). Active and probe-free intracellular rheology via phase-sensitive thermoviscous flows. PNAS Nexus. Oxford University Press. https://doi.org/10.1093/pnasnexus/pgag190","chicago":"Stoev, Iliya D, Madison Bolger-Munro, Antonio Minopoli, Susan Wagner, Venkat Raghavan Krishnaswamy, Elena Erben, Kai Weißenbruch, et al. “Active and Probe-Free Intracellular Rheology via Phase-Sensitive Thermoviscous Flows.” PNAS Nexus. Oxford University Press, 2026. https://doi.org/10.1093/pnasnexus/pgag190.","ieee":"I. D. Stoev et al., “Active and probe-free intracellular rheology via phase-sensitive thermoviscous flows,” PNAS Nexus, vol. 5, no. 6. Oxford University Press, 2026."},"file_date_updated":"2026-07-13T13:13:56Z","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","PlanS_conform":"1","issue":"6","month":"06","keyword":["cell mechanics","active microrheology","noninvasiveness","thermoviscous flows","FLUCS"],"year":"2026","biorxivid":1,"quality_controlled":"1","tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_type":"original","article_number":"pgag190","department":[{"_id":"CaHe"}],"dataavailabilitystatement":"All data and materials are made available on Zenodo public repository under Creative Commons Attribution 4.0 International License: https://doi.org/10.5281/zenodo.20322020.","file":[{"file_size":3073062,"relation":"main_file","success":1,"creator":"dernst","file_id":"22312","access_level":"open_access","date_created":"2026-07-13T13:13:56Z","file_name":"2026_PNASNexus_Stoev.pdf","checksum":"bb2c89ea73da762ad6423ac299ac3533","content_type":"application/pdf","date_updated":"2026-07-13T13:13:56Z"}],"oa_version":"Published Version","supplementarymaterial":"yes","publication_status":"published","intvolume":" 5","external_id":{"biorxivid":["10.1101/2025.04.07.647540"]},"author":[{"last_name":"Stoev","first_name":"Iliya D","full_name":"Stoev, Iliya D"},{"orcid":"0000-0002-8176-4824","last_name":"Bolger-Munro","full_name":"Bolger-Munro, Madison","first_name":"Madison","id":"516F03FA-93A3-11EA-A7C5-D6BE3DDC885E"},{"first_name":"Antonio","full_name":"Minopoli, Antonio","last_name":"Minopoli"},{"full_name":"Wagner, Susan","first_name":"Susan","last_name":"Wagner"},{"last_name":"Krishnaswamy","first_name":"Venkat Raghavan","full_name":"Krishnaswamy, Venkat Raghavan"},{"first_name":"Elena","full_name":"Erben, Elena","last_name":"Erben"},{"full_name":"Weißenbruch, Kai","first_name":"Kai","last_name":"Weißenbruch"},{"full_name":"Maghelli, Nicola","first_name":"Nicola","last_name":"Maghelli"},{"last_name":"Bastmeyer","full_name":"Bastmeyer, Martin","first_name":"Martin"},{"full_name":"Heisenberg, Carl-Philipp J","id":"39427864-F248-11E8-B48F-1D18A9856A87","first_name":"Carl-Philipp J","orcid":"0000-0002-0912-4566","last_name":"Heisenberg"},{"last_name":"Kreysing","first_name":"Moritz","full_name":"Kreysing, Moritz"}]},{"language":[{"iso":"eng"}],"doi":"10.1017/9781009500678.022","citation":{"short":"G. Avni, T.A. Henzinger, in:, ‪Nathanaël Fijalkow (Ed.), Games on Graphs. From Logic and Automata to Algorithms, Cambridge University Press, 2026, pp. 529–569.","mla":"Avni, Guy, and Thomas A. Henzinger. “Bidding Games.” Games on Graphs. From Logic and Automata to Algorithms, edited by ‪Nathanaël Fijalkow, Cambridge University Press, 2026, pp. 529–69, doi:10.1017/9781009500678.022.","ieee":"G. Avni and T. A. Henzinger, “Bidding Games,” in Games on Graphs. From Logic and Automata to Algorithms, ‪Nathanaël Fijalkow, Ed. Cambridge University Press, 2026, pp. 529–569.","ama":"Avni G, Henzinger TA. Bidding Games. In: Fijalkow ‪Nathanaël, ed. Games on Graphs. From Logic and Automata to Algorithms. Cambridge University Press; 2026:529-569. doi:10.1017/9781009500678.022","ista":"Avni G, Henzinger TA. 2026.Bidding Games. In: Games on Graphs. From Logic and Automata to Algorithms. , 529–569.","chicago":"Avni, Guy, and Thomas A Henzinger. “Bidding Games.” In Games on Graphs. From Logic and Automata to Algorithms, edited by ‪Nathanaël Fijalkow, 529–69. Cambridge University Press, 2026. https://doi.org/10.1017/9781009500678.022.","apa":"Avni, G., & Henzinger, T. A. (2026). Bidding Games. In ‪Nathanaël Fijalkow (Ed.), Games on Graphs. From Logic and Automata to Algorithms (pp. 529–569). Cambridge University Press. https://doi.org/10.1017/9781009500678.022"},"author":[{"orcid":"0000-0001-5588-8287","last_name":"Avni","first_name":"Guy","id":"463C8BC2-F248-11E8-B48F-1D18A9856A87","full_name":"Avni, Guy"},{"last_name":"Henzinger","orcid":"0000-0002-2985-7724","full_name":"Henzinger, Thomas A","first_name":"Thomas A","id":"40876CD8-F248-11E8-B48F-1D18A9856A87"}],"date_updated":"2026-07-13T13:32:47Z","abstract":[{"lang":"eng","text":"As seen in previous chapters, a graph game proceeds by placing a token on one of the vertices and allowing the players to move it throughout the graph to produce an infinite trace, which determines the winner or payoff of the game."}],"publication_identifier":{"isbn":["9781009500685"],"eisbn":["9781009500678"]},"date_created":"2026-07-13T10:44:22Z","page":"529-569","corr_author":"1","_id":"22300","publication_status":"published","day":"26","publisher":"Cambridge University Press","article_processing_charge":"No","editor":[{"first_name":" ‪Nathanaël","full_name":"Fijalkow, ‪Nathanaël","last_name":"Fijalkow"}],"status":"public","oa_version":"None","department":[{"_id":"ToHe"}],"type":"book_chapter","scopus_import":"1","publication":"Games on Graphs. From Logic and Automata to Algorithms","das_tickbox":"1","date_published":"2026-04-26T00:00:00Z","year":"2026","title":"Bidding Games","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","OA_type":"closed access","month":"04"},{"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"article_type":"original","article_number":"stag678","department":[{"_id":"IlCa"}],"dataavailabilitystatement":"All photometry is provided in the supplementary data files. Spectroscopy will be made available on WISEREP, and is available on request to the lead author.","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"1","PlanS_conform":"1","month":"06","keyword":["stars: black holes","supernovae: individual: AT2024wpp","radio continuum: transients"],"year":"2026","quality_controlled":"1","intvolume":" 549","external_id":{"arxiv":["2601.03337"]},"author":[{"last_name":"Perley","first_name":"Daniel A","full_name":"Perley, Daniel A"},{"first_name":"Anna Y Q","full_name":"Ho, Anna Y Q","last_name":"Ho"},{"last_name":"McGrath","first_name":"Zoë","full_name":"McGrath, Zoë"},{"first_name":"Michael","full_name":"Camilo, Michael","last_name":"Camilo"},{"full_name":"Sevilla, Cassie","first_name":"Cassie","last_name":"Sevilla"},{"full_name":"Chen, Ping","first_name":"Ping","last_name":"Chen"},{"first_name":"Genevieve","full_name":"Schroeder, Genevieve","last_name":"Schroeder"},{"first_name":"Taya","full_name":"Govreen-Segal, Taya","last_name":"Govreen-Segal"},{"first_name":"Aleksandra","full_name":"Bochenek, Aleksandra","last_name":"Bochenek"},{"first_name":"Yu-Jing","full_name":"Qin, Yu-Jing","last_name":"Qin"},{"last_name":"Gillanders","first_name":"James H","full_name":"Gillanders, James H"},{"last_name":"Amend","full_name":"Amend, Benjamin","first_name":"Benjamin"},{"last_name":"Anderson","full_name":"Anderson, Joseph P","first_name":"Joseph P"},{"last_name":"Andreoni","first_name":"Igor","full_name":"Andreoni, Igor"},{"first_name":"Amar","full_name":"Aryan, Amar","last_name":"Aryan"},{"last_name":"Bellm","first_name":"Eric C","full_name":"Bellm, Eric C"},{"first_name":"Joshua S","full_name":"Bloom, Joshua S","last_name":"Bloom"},{"first_name":"Thomas","full_name":"de Boer, Thomas","last_name":"de Boer"},{"first_name":"Jonathan","full_name":"Carney, Jonathan","last_name":"Carney"},{"last_name":"Caiazzo","orcid":"0000-0002-4770-5388","first_name":"Ilaria","id":"8ae5b6e7-2a03-11ee-914d-b58ed7a3b47d","full_name":"Caiazzo, Ilaria"},{"first_name":"Ken C","full_name":"Chambers, Ken C","last_name":"Chambers"},{"last_name":"Charalampopoulos","first_name":"Panos","full_name":"Charalampopoulos, Panos"},{"first_name":"Ting-Wan","full_name":"Chen, Ting-Wan","last_name":"Chen"},{"first_name":"Tracy X","full_name":"Chen, Tracy X","last_name":"Chen"},{"first_name":"Eric R","full_name":"Coughlin, Eric R","last_name":"Coughlin"},{"full_name":"Coughlin, Michael","first_name":"Michael","last_name":"Coughlin"},{"full_name":"Dennefeld, Michel","first_name":"Michel","last_name":"Dennefeld"},{"first_name":"Georgios","full_name":"Dimitriadis, Georgios","last_name":"Dimitriadis"},{"first_name":"Christoffer","full_name":"Fremling, Christoffer","last_name":"Fremling"},{"first_name":"Danielle","full_name":"Frostig, Danielle","last_name":"Frostig"},{"full_name":"Gal-Yam, Avishay","first_name":"Avishay","last_name":"Gal-Yam"},{"last_name":"Galbany","first_name":"Lluís","full_name":"Galbany, Lluís"},{"last_name":"Gangopadhyay","full_name":"Gangopadhyay, Anjashay","first_name":"Anjashay"},{"first_name":"Melzie","full_name":"Ghendrih, Melzie","last_name":"Ghendrih"},{"last_name":"Graham","first_name":"Matthew J","full_name":"Graham, Matthew J"},{"last_name":"Gromadzki","full_name":"Gromadzki, Mariusz","first_name":"Mariusz"},{"last_name":"Groom","full_name":"Groom, Steven L","first_name":"Steven L"},{"last_name":"Gutiérrez","full_name":"Gutiérrez, Claudia P","first_name":"Claudia P"},{"full_name":"Hinds, K -Ryan","first_name":"K -Ryan","last_name":"Hinds"},{"first_name":"Mark E","full_name":"Huber, Mark E","last_name":"Huber"},{"last_name":"Inserra","full_name":"Inserra, Cosimo","first_name":"Cosimo"},{"full_name":"Kaiser, Benjamin C","first_name":"Benjamin C","last_name":"Kaiser"},{"last_name":"Kasliwal","full_name":"Kasliwal, Mansi M","first_name":"Mansi M"},{"last_name":"Koivisto","full_name":"Koivisto, Niilo E","first_name":"Niilo E"},{"first_name":"Chien-Cheng","full_name":"Lin, Chien-Cheng","last_name":"Lin"},{"last_name":"Liu","full_name":"Liu, Chang","first_name":"Chang"},{"full_name":"Lowe, Thomas B","first_name":"Thomas B","last_name":"Lowe"},{"last_name":"Magnier","first_name":"Eugene","full_name":"Magnier, Eugene"},{"full_name":"Mahabal, Ashish A","first_name":"Ashish A","last_name":"Mahabal"},{"first_name":"Andrew","full_name":"Milligan, Andrew","last_name":"Milligan"},{"first_name":"Paloma","full_name":"Minguez, Paloma","last_name":"Minguez"},{"last_name":"Mo","first_name":"Geoffrey","full_name":"Mo, Geoffrey"},{"last_name":"Müller-Bravo","first_name":"Tomás E","full_name":"Müller-Bravo, Tomás E"},{"last_name":"Nicholl","full_name":"Nicholl, Matt","first_name":"Matt"},{"full_name":"Pessi, Priscila J","first_name":"Priscila J","last_name":"Pessi"},{"full_name":"Pignata, Giuliano","first_name":"Giuliano","last_name":"Pignata"},{"last_name":"Purdum","full_name":"Purdum, Josiah","first_name":"Josiah"},{"first_name":"Nabeel","full_name":"Rehemtulla, Nabeel","last_name":"Rehemtulla"},{"first_name":"R Michael","full_name":"Rich, R Michael","last_name":"Rich"},{"full_name":"Sahu, Anwesha","first_name":"Anwesha","last_name":"Sahu"},{"last_name":"Singh","first_name":"Avinash","full_name":"Singh, Avinash"},{"first_name":"Stephen J","full_name":"Smartt, Stephen J","last_name":"Smartt"},{"full_name":"Smith, Ian A","first_name":"Ian A","last_name":"Smith"},{"first_name":"Jesper","full_name":"Sollerman, Jesper","last_name":"Sollerman"},{"last_name":"Srinivasaragavan","first_name":"Gokul","full_name":"Srinivasaragavan, Gokul"},{"last_name":"Srivastav","full_name":"Srivastav, Shubham","first_name":"Shubham"},{"full_name":"Stein, Robert D","first_name":"Robert D","last_name":"Stein"},{"full_name":"Schulze, Steve","first_name":"Steve","last_name":"Schulze"},{"full_name":"Tweddle, Jack W","first_name":"Jack W","last_name":"Tweddle"},{"first_name":"Richard","full_name":"Wainscoat, Richard","last_name":"Wainscoat"},{"full_name":"Wise, Jacob L","first_name":"Jacob L","last_name":"Wise"},{"last_name":"Yan","first_name":"Lin","full_name":"Yan, Lin"},{"first_name":"David R","full_name":"Young, David R","last_name":"Young"}],"arxiv":1,"file":[{"file_name":"2026_MNRAS_Perley.pdf","checksum":"a5827b9f68f1731b8c8df18142c0ef38","date_created":"2026-07-13T14:35:34Z","access_level":"open_access","file_id":"22314","creator":"dernst","success":1,"relation":"main_file","file_size":6208809,"date_updated":"2026-07-13T14:35:34Z","content_type":"application/pdf"}],"oa_version":"Published Version","supplementarymaterial":"yes","publication_status":"published","publication":"Monthly Notices of the Royal Astronomical Society","date_published":"2026-06-01T00:00:00Z","das_tickbox":"1","type":"journal_article","researchdata_availability":"upon request","scopus_import":"1","OA_type":"gold","title":"AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole","DOAJ_listed":"1","has_accepted_license":"1","ddc":["520"],"OA_place":"publisher","abstract":[{"text":"We present the discovery of AT 2024wpp (‘Whippet’), a fast and luminous 18cow-like transient. At a redshift of z = 0 . 0868 , revealed by Keck Cosmic Web Imager spectroscopy of its faint star-forming host, it is the fourth-nearest example of its class to date. Rapid identification of the source in the Zwicky Transient Facility data stream permitted ultraviolet-through- optical observations to be obtained prior to peak, allowing the first determination of the peak bolometric luminosity ( 2 ×1045 erg s−1 ), maximum photospheric radius ( 1015 cm), and total radiated energy ( 1051 erg) of an 18cow-like object. We present results from a comprehensive multiwavelength observing campaign, including a far-ultraviolet spectrum from the Cosmic Origins Spectrograph on the Hubble Space Telescope and deep imaging extending > 100 d post-explosion from the Very Large Telescope, Hubble Space Telescope , Very Large Array, and Atacama Large Millimetre Array. We interpret the observations under a model in which a rapidly accreting central engine blows a fast ( ∼0.2 c ) wind into the surrounding medium and irradiates it with X-rays. The high Doppler velocities and intense ionization within this wind prevent identifiable spectroscopic features from appearing in the ejecta or in the surrounding circumstellar material. Weak H and He signatures do emerge in the spectra after 35 d in the form of double-peaked narrow lines. Each peak is individually narrow (full width δv ∼3000 km s−1 ) but the two components are separated by \u0003v ∼6600 km s−1 , indicating stable structures of denser material, possibly representing streams of tidal ejecta or an ablated companion star.","lang":"eng"}],"date_updated":"2026-07-13T14:36:24Z","publication_identifier":{"eissn":["1365-2966"],"issn":["0035-8711"]},"volume":549,"language":[{"iso":"eng"}],"citation":{"mla":"Perley, Daniel A., et al. “AT 2024wpp: An Extremely Luminous Fast Ultraviolet Transient Powered by Accretion onto a Black Hole.” Monthly Notices of the Royal Astronomical Society, vol. 549, no. 1, stag678, Oxford University Press, 2026, doi:10.1093/mnras/stag678.","short":"D.A. Perley, A.Y.Q. Ho, Z. McGrath, M. Camilo, C. Sevilla, P. Chen, G. Schroeder, T. Govreen-Segal, A. Bochenek, Y.-J. Qin, J.H. Gillanders, B. Amend, J.P. Anderson, I. Andreoni, A. Aryan, E.C. Bellm, J.S. Bloom, T. de Boer, J. Carney, I. Caiazzo, K.C. Chambers, P. Charalampopoulos, T.-W. Chen, T.X. Chen, E.R. Coughlin, M. Coughlin, M. Dennefeld, G. Dimitriadis, C. Fremling, D. Frostig, A. Gal-Yam, L. Galbany, A. Gangopadhyay, M. Ghendrih, M.J. Graham, M. Gromadzki, S.L. Groom, C.P. Gutiérrez, K.-R. Hinds, M.E. Huber, C. Inserra, B.C. Kaiser, M.M. Kasliwal, N.E. Koivisto, C.-C. Lin, C. Liu, T.B. Lowe, E. Magnier, A.A. Mahabal, A. Milligan, P. Minguez, G. Mo, T.E. Müller-Bravo, M. Nicholl, P.J. Pessi, G. Pignata, J. Purdum, N. Rehemtulla, R.M. Rich, A. Sahu, A. Singh, S.J. Smartt, I.A. Smith, J. Sollerman, G. Srinivasaragavan, S. Srivastav, R.D. Stein, S. Schulze, J.W. Tweddle, R. Wainscoat, J.L. Wise, L. Yan, D.R. Young, Monthly Notices of the Royal Astronomical Society 549 (2026).","apa":"Perley, D. A., Ho, A. Y. Q., McGrath, Z., Camilo, M., Sevilla, C., Chen, P., … Young, D. R. (2026). AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole. Monthly Notices of the Royal Astronomical Society. Oxford University Press. https://doi.org/10.1093/mnras/stag678","chicago":"Perley, Daniel A, Anna Y Q Ho, Zoë McGrath, Michael Camilo, Cassie Sevilla, Ping Chen, Genevieve Schroeder, et al. “AT 2024wpp: An Extremely Luminous Fast Ultraviolet Transient Powered by Accretion onto a Black Hole.” Monthly Notices of the Royal Astronomical Society. Oxford University Press, 2026. https://doi.org/10.1093/mnras/stag678.","ista":"Perley DA, Ho AYQ, McGrath Z, Camilo M, Sevilla C, Chen P, Schroeder G, Govreen-Segal T, Bochenek A, Qin Y-J, Gillanders JH, Amend B, Anderson JP, Andreoni I, Aryan A, Bellm EC, Bloom JS, de Boer T, Carney J, Caiazzo I, Chambers KC, Charalampopoulos P, Chen T-W, Chen TX, Coughlin ER, Coughlin M, Dennefeld M, Dimitriadis G, Fremling C, Frostig D, Gal-Yam A, Galbany L, Gangopadhyay A, Ghendrih M, Graham MJ, Gromadzki M, Groom SL, Gutiérrez CP, Hinds K-R, Huber ME, Inserra C, Kaiser BC, Kasliwal MM, Koivisto NE, Lin C-C, Liu C, Lowe TB, Magnier E, Mahabal AA, Milligan A, Minguez P, Mo G, Müller-Bravo TE, Nicholl M, Pessi PJ, Pignata G, Purdum J, Rehemtulla N, Rich RM, Sahu A, Singh A, Smartt SJ, Smith IA, Sollerman J, Srinivasaragavan G, Srivastav S, Stein RD, Schulze S, Tweddle JW, Wainscoat R, Wise JL, Yan L, Young DR. 2026. AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole. Monthly Notices of the Royal Astronomical Society. 549(1), stag678.","ama":"Perley DA, Ho AYQ, McGrath Z, et al. AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole. Monthly Notices of the Royal Astronomical Society. 2026;549(1). doi:10.1093/mnras/stag678","ieee":"D. A. Perley et al., “AT 2024wpp: An extremely luminous fast ultraviolet transient powered by accretion onto a black hole,” Monthly Notices of the Royal Astronomical Society, vol. 549, no. 1. Oxford University Press, 2026."},"doi":"10.1093/mnras/stag678","file_date_updated":"2026-07-13T14:35:34Z","status":"public","acknowledgement":"We thank Eliot Quataert, Luc Dessart, Ben Margalit, Ross Ferguson, Aaron Tohuvavohu, Brad Cenko, and Jamie Kennea for useful discussions. We thank the referee for helpful suggestions that improved the manuscript.\r\n\r\nBased on observations obtained with the Samuel Oschin Telescope 48-in. and the 60-in. Telescope at the Palomar Observatory as part of the Zwicky Transient Facility project. ZTF is supported by the National Science Foundation under grant no. AST-2034437 and a collaboration including Caltech, IPAC, the Oskar Klein Center at Stockholm University, the University of Maryland, University of California, Berkeley, the University of Wisconsin at Milwaukee, University of Warwick, Ruhr University Bochum, Cornell University, Northwestern University and Drexel University. Operations are conducted by COO, IPAC, and UW.\r\n\r\nThe Liverpool Telescope is operated on the island of La Palma by Liverpool John Moores University in the Spanish Observatorio del Roque de los Muchachos of the Instituto de Astrofisica de Canarias with financial support from the UK Science and Technology Facilities Council.\r\n\r\nBased on observations made with the Nordic Optical Telescope, owned in collaboration by the University of Turku and Aarhus University, and operated jointly by Aarhus University, the University of Turku and the University of Oslo, representing Denmark, Finland and Norway, the University of Iceland and Stockholm University at the Observatorio del Roque de los Muchachos, La Palma, Spain, of the Instituto de Astrofisica de Canarias. The NOT data were obtained under program ID 68–501.\r\n\r\nThis work made use of data supplied by the UK Swift Science Data Centre at the University of Leicester. We are grateful to Phil Evans, Aaron Tohuvavohu, and Jamie Kennea for advice on the Swift/XRT data reduction.\r\n\r\nSome of the data presented herein were obtained at the W. M. Keck Observatory, which is operated as a scientific partnership among the California Institute of Technology, the University of California, and NASA. The Observatory was made possible by the generous financial support of the W. M. Keck Foundation. The authors wish to recognize and acknowledge the very significant cultural role and reverence that the summit of Maunakea has always had within the indigenous Hawaiian community. We are most fortunate to have the opportunity to conduct observations from this mountain.\r\n\r\nSome observations reported here were obtained at the MMT Observatory, a joint facility of the University of Arizona and the Smithsonian Institution.\r\n\r\nThe National Radio Astronomy Observatory and Green Bank Observatory are facilities of the U.S. National Science Foundation operated under cooperative agreement by Associated Universities, Inc. This paper makes use of the following ALMA data: ADS/JAO.ALMA no. 2023.1.01730.T ALMA is a partnership of ESO (representing its member states), NSF (USA) and NINS (Japan), together with NRC (Canada), NSTC and ASIAA (Taiwan), and KASI (Republic of Korea), in cooperation with the Republic of Chile. The Joint ALMA Observatory is operated by ESO, AUI/NRAO, and NAOJ.\r\n\r\nBased on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere under ESO programme 2114.D-5014(E). We thank John Pritchard and Paula Sanchez Saez, and the entire observatory staff, for their excellent support.\r\n\r\nBased on observations collected at the European Organisation for Astronomical Research in the Southern Hemisphere, Chile, as part of ePESSTO+ (the advanced Public ESO Spectroscopic Survey for Transient Objects Survey – PI: Inserra). ePESSTO+ observations were obtained under ESO program ID 112.25JQ.\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 programs 16714, 17477, and 17889.\r\n\r\nBased on observations obtained at the Southern Astrophysical Research (SOAR) telescope, which is a joint project of the Ministério da Ciência, Tecnologia e Inovações (MCTI/LNA) do Brasil, the US National Science Foundation’s NOIRLab, the University of North Carolina at Chapel Hill (UNC), and Michigan State University (MSU).\r\n\r\nThe Pan-STARRS1 Surveys (PS1) and the PS1 public science archive have been made possible through contributions by the Institute for Astronomy, the University of Hawaii, the Pan-STARRS Project Office, the Max-Planck Society and its participating institutes, the Max Planck Institute for Astronomy, Heidelberg and the Max Planck Institute for Extraterrestrial Physics, Garching, The Johns Hopkins University, Durham University, the University of Edinburgh, the Queen’s University Belfast, the Harvard-Smithsonian Center for Astrophysics, the Las Cumbres Observatory Global Telescope Network Incorporated, the National Central University of Taiwan, the Space Telescope Science Institute, the National Aeronautics and Space Administration under grant no. NNX08AR22G issued through the Planetary Science Division of the NASA Science Mission Directorate, the National Science Foundation grant no. AST–1238877, the University of Maryland, Eotvos Lorand University (ELTE), the Los Alamos National Laboratory, and the Gordon and Betty Moore Foundation.\r\n\r\nThis research made use of ccdproc, an astropy package for image reduction (M. Craig et al. 2025).\r\n\r\nGS and AYQH acknowledge support in part from a Sloan Research Fellowship (award no. FG-2024-21320) from the Alfred P. Sloan Foundation. CS and AYQH acknowledge support in part from National Aeronautics and Space Administration (NASA) grant 80NSSC24K0377, from HST grant HST-GO-17477.006-A, and from a Scialog award from the Research Corporation for Science Advancement (‘Early Science with the LSST’).\r\n\r\nPC acknowledges support from the Zhejiang Provincial Top-Level Research Support Program.\r\n\r\nIA and JC are supported by the National Science Foundation award AST 2505775, NASA grant 24-ADAP24-0159, Scialog award SA-LSST-2024-102a, and the Discovery Alliance Catalyst Fellowship Mentors award 2025-62192-CM-19\r\n\r\nAA acknowledges support from the Ministry of Education Yushan Fellow Program (MOE-111-YSFMS-0008-001-P1) and from the National Science and Technology Council, Taiwan (NSTC 114-2112-M-008-021-MY3).\r\n\r\nT-WC acknowledges support from the Ministry of Education Yushan Fellow Program (MOE-111-YSFMS-0008-001-P1) and from the National Science and Technology Council, Taiwan (NSTC 114-2112-M-008-021-MY3).\r\n\r\nERC acknowledges support from the National Aeronautics and Space Administration through the Astrophysics Theory Program, grant 80NSSC24K0897.\r\n\r\nGD acknowledges support from the European Union’s Horizon Europe research and innovation programme under the Marie Skłodowska-Curie grant agreement no. 101199369.\r\n\r\nDF’s contribution to this material is based upon work supported by the National Science Foundation under award no. AST-2401779.\r\n\r\nAGY’s research is supported by ISF, IMOS, and BSF grants, as well as the André Deloro Institute for Space and Optics Research, the Center for Experimental Physics, a WIS-MIT Sagol grant, the Norman E Alexander Family M Foundation ULTRASAT Data Center Fund, and Yeda-Sela; AGY is the incumbent of the The Arlyn Imberman Professorial Chair.\r\n\r\nLG acknowledges financial support from AGAUR, CSIC, MCIN, and AEI 10.13039/501100011033 under projects PID2023-151307NB-I00, PIE 20215AT016, and CEX2020-001058-M.\r\n\r\nMG acknowledges support from an STFC PhD studentship and from the Faculty of Science and Technology at Lancaster University.\r\n\r\nCPG acknowledges financial support from the Secretary of Universities and Research (Government of Catalonia) and by the Horizon 2020 Research and Innovation Programme of the European Union under the Marie Skłodowska-Curie and the Beatriu de Pinós 2021 BP 00168 programme, from the Spanish Ministerio de Ciencia e Innovación (MCIN) and the Agencia Estatal de Investigación (AEI) 10.13039/501100011033 under the PID2023-151307NB-I00 SNNEXT project, from Centro Superior de Investigaciones Científicas (CSIC) under the PIE project 20215AT016 and the program Unidad de Excelencia María de Maeztu CEX2020-001058-M, and from the Departament de Recerca i Universitats de la Generalitat de Catalunya through the 2021-SGR-01270 grant.\r\n\r\nCL is supported by DoE award no.  DE-SC0025599.\r\n\r\nZwicky Transient Facility, W. M. Keck Observatory, and MMT Observatory access was supported by Northwestern University and the Center for Interdisciplinary Exploration and Research in Astrophysics (CIERA).\r\n\r\nAM gratefully acknowledges support from an STFC PhD studentship and the Faculty of Science and Technology at Lancaster University.\r\n\r\nTEMB is funded by Horizon Europe ERC grant no. 101125877.\r\n\r\nMN is supported by the European Research Council (ERC) under the European Union’s Horizon 2020 research and innovation programme (grant agreement no. 948381).\r\n\r\nNR is supported by a Northwestern University Presidential Fellowship Award. We gratefully acknowledge the support of the NSF-Simons AI-Institute for the Sky (SkAI) via grants NSF AST-2421845 and Simons Foundation MPS-AI-00010513.\r\n\r\nAS acknowledges the Warwick Astrophysics PhD prize scholarship made possible thanks to a generous philanthropic donation.\r\n\r\nSJS acknowledges funding from STFC grant ST/Y001605/1, a Royal Society Research Professorship and the Hintze Family Charitable Foundation.","article_processing_charge":"Yes","date_created":"2026-07-13T10:50:10Z","oa":1,"day":"01","publisher":"Oxford University Press","_id":"22303"},{"month":"06","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","PlanS_conform":"1","quality_controlled":"1","year":"2026","article_type":"original","article_number":"jipb.70309","acknowledged_ssus":[{"_id":"Bio"},{"_id":"NanoFab"}],"pmid":1,"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"department":[{"_id":"JiFr"},{"_id":"GradSch"},{"_id":"NanoFab"},{"_id":"Bio"}],"oa_version":"Published Version","publication_status":"epub_ahead","supplementarymaterial":"yes","project":[{"grant_number":"101142681","_id":"8f347782-16d5-11f0-9cad-8c19706ee739","name":"Cyclic nucleotides as second messengers in plants"},{"_id":"bd76d395-d553-11ed-ba76-f678c14f9033","name":"Peptide receptors for auxin canalization in Arabidopsis","grant_number":"I06123"},{"grant_number":"P37051","name":"Guanylate cyclase activity of TIR1/AFBs auxin receptors","_id":"7bcece63-9f16-11ee-852c-ae94e099eeb6"}],"author":[{"first_name":"Adrijana","id":"cced8a85-223e-11ed-af04-b0596c55053b","full_name":"Smoljan, Adrijana","last_name":"Smoljan"},{"last_name":"Koutnik‐Abele","first_name":"Sarah","full_name":"Koutnik‐Abele, Sarah"},{"full_name":"Vladimirtsev, Dmitrii","first_name":"Dmitrii","id":"60466724-5355-11ee-ae5a-fa55e8f99c3d","last_name":"Vladimirtsev"},{"first_name":"Petr","full_name":"Klíma, Petr","last_name":"Klíma"},{"last_name":"Bírošíková","full_name":"Bírošíková, Anita","first_name":"Anita"},{"last_name":"Zhang","orcid":"0000-0003-2627-6956","full_name":"Zhang, Yuzhou","id":"3B6137F2-F248-11E8-B48F-1D18A9856A87","first_name":"Yuzhou"},{"id":"4515C308-F248-11E8-B48F-1D18A9856A87","first_name":"Jack","full_name":"Merrin, Jack","last_name":"Merrin","orcid":"0000-0001-5145-4609"},{"last_name":"Schuster","full_name":"Schuster, Maximilian","id":"37e65def-d415-11eb-ae59-a7b67be103db","first_name":"Maximilian"},{"last_name":"Kurtović","full_name":"Kurtović, Katarina","first_name":"Katarina"},{"last_name":"Hammes","full_name":"Hammes, Ulrich Z.","first_name":"Ulrich Z."},{"last_name":"Petrášek","full_name":"Petrášek, Jan","first_name":"Jan"},{"orcid":"0000-0002-8302-7596","last_name":"Friml","full_name":"Friml, Jiří","id":"4159519E-F248-11E8-B48F-1D18A9856A87","first_name":"Jiří"}],"external_id":{"pmid":["42271607"]},"main_file_link":[{"url":"https://doi.org/10.1111/jipb.70309","open_access":"1"}],"OA_type":"hybrid","ddc":["580"],"OA_place":"publisher","title":"Auxin response and PIN‐mediated transport in chlorophyte algae","has_accepted_license":"1","date_published":"2026-06-10T00:00:00Z","das_tickbox":"0","publication":"Journal of Integrative Plant Biology","scopus_import":"1","researchdata_availability":"no","type":"journal_article","status":"public","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.","article_processing_charge":"Yes (via OA deal)","publisher":"Wiley","day":"10","_id":"22301","corr_author":"1","oa":1,"date_created":"2026-07-13T10:44:55Z","publication_identifier":{"eissn":["1744-7909"],"issn":["1672-9072"]},"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."}],"date_updated":"2026-07-13T14:26:31Z","citation":{"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).","mla":"Smoljan, Adrijana, et al. “Auxin Response and PIN‐mediated Transport in Chlorophyte Algae.” Journal of Integrative Plant Biology, jipb. 70309, Wiley, 2026, doi:10.1111/jipb.70309.","ieee":"A. Smoljan et al., “Auxin response and PIN‐mediated transport in chlorophyte algae,” Journal of Integrative Plant Biology. 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.” Journal of Integrative Plant Biology. Wiley, 2026. https://doi.org/10.1111/jipb.70309.","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. Journal of Integrative Plant Biology. Wiley. https://doi.org/10.1111/jipb.70309","ama":"Smoljan A, Koutnik‐Abele S, Vladimirtsev D, et al. Auxin response and PIN‐mediated transport in chlorophyte algae. Journal of Integrative Plant Biology. 2026. doi:10.1111/jipb.70309","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."},"doi":"10.1111/jipb.70309","language":[{"iso":"eng"}]},{"das_tickbox":"1","date_published":"2026-06-24T00:00:00Z","publication":"Computer Graphics Forum","type":"conference","OA_type":"hybrid","OA_place":"publisher","ddc":["005"],"title":"Circles of confidence for multi-label geometry completion","has_accepted_license":"1","date_updated":"2026-07-13T14:58:48Z","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"}],"doi":"10.1111/cgf.70516","file_date_updated":"2026-06-23T09:07:22Z","citation":{"mla":"Wei, Ziyu, et al. “Circles of Confidence for Multi-Label Geometry Completion.” Computer Graphics Forum, vol. 45, no. 5, Wiley, doi:10.1111/cgf.70516.","short":"Z. Wei, C. Hafner, A. Kalinov, P. Synak, C. Wojtan, in:, Computer Graphics Forum, Wiley, n.d.","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.","ama":"Wei Z, Hafner C, Kalinov A, Synak P, Wojtan C. Circles of confidence for multi-label geometry completion. In: Computer Graphics Forum. Vol 45. Wiley. doi:10.1111/cgf.70516","chicago":"Wei, Ziyu , Christian Hafner, Aleksei Kalinov, Peter Synak, and Chris Wojtan. “Circles of Confidence for Multi-Label Geometry Completion.” In Computer Graphics Forum, Vol. 45. Wiley, n.d. https://doi.org/10.1111/cgf.70516.","apa":"Wei, Z., Hafner, C., Kalinov, A., Synak, P., & Wojtan, C. (n.d.). Circles of confidence for multi-label geometry completion. In Computer Graphics Forum (Vol. 45). Bern, Switzerland: Wiley. https://doi.org/10.1111/cgf.70516","ieee":"Z. Wei, C. Hafner, A. Kalinov, P. Synak, and C. Wojtan, “Circles of confidence for multi-label geometry completion,” in Computer Graphics Forum, Bern, Switzerland, vol. 45, no. 5."},"language":[{"iso":"eng"}],"volume":45,"article_processing_charge":"Yes (via OA deal)","status":"public","_id":"22129","publisher":"Wiley","day":"24","oa":1,"date_created":"2026-06-23T09:08:41Z","corr_author":"1","conference":{"end_date":"2026-07-03","location":"Bern, Switzerland","start_date":"2026-07-01","name":"Eurographics: Symposium on Geometry Processing"},"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"department":[{"_id":"ChWo"},{"_id":"GradSch"}],"month":"06","issue":"5","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","quality_controlled":"1","year":"2026","project":[{"grant_number":"101045083","name":"Computational Discovery of Numerical Algorithms for Animation and Simulation of Natural Phenomena","_id":"34bc2376-11ca-11ed-8bc3-9a3b3961a088"}],"intvolume":" 45","author":[{"last_name":"Wei","first_name":"Ziyu ","full_name":"Wei, Ziyu "},{"id":"400429CC-F248-11E8-B48F-1D18A9856A87","first_name":"Christian","full_name":"Hafner, Christian","last_name":"Hafner"},{"orcid":"0000-0003-2189-3904","last_name":"Kalinov","id":"44b7120e-eb97-11eb-a6c2-e1557aa81d02","first_name":"Aleksei","full_name":"Kalinov, Aleksei"},{"id":"331776E2-F248-11E8-B48F-1D18A9856A87","first_name":"Peter","full_name":"Synak, Peter","last_name":"Synak"},{"first_name":"Christopher J","id":"3C61F1D2-F248-11E8-B48F-1D18A9856A87","full_name":"Wojtan, Christopher J","last_name":"Wojtan","orcid":"0000-0001-6646-5546"}],"oa_version":"Published Version","file":[{"success":1,"file_size":14536575,"relation":"main_file","access_level":"open_access","file_id":"22132","creator":"mly","checksum":"365f986db34e3fbce74089207599253b","file_name":"document(3).pdf","date_created":"2026-06-23T09:07:22Z","content_type":"application/pdf","date_updated":"2026-06-23T09:07:22Z"}],"publication_status":"accepted"},{"year":"2026","quality_controlled":"1","user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","month":"05","keyword":["Algebraic topology","Lefschetz complexes","persistent homology","vines and vineyards","birth-death pairs","shallow pairs","relations","partial orders","transpositions","Theory of computation → Computational geometry"],"department":[{"_id":"HeEd"},{"_id":"GradSch"}],"alternative_title":["LIPIcs"],"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"conference":{"end_date":"2026-06-05","name":"SoCG: Symposium on Computational Geometry","location":"New Brunswick, NJ, United States","start_date":"2026-06-02"},"article_number":"41:1-41:18","supplementarymaterial":"no","publication_status":"published","file":[{"date_updated":"2026-07-14T06:08:05Z","content_type":"application/pdf","checksum":"9dfb96ee66985c724b499b0e5888dc8e","file_name":"2026_LIPIcSSoCG_Edelsbrunner.pdf","date_created":"2026-07-14T06:08:05Z","access_level":"open_access","file_id":"22329","creator":"dernst","success":1,"relation":"main_file","file_size":2902144}],"oa_version":"Published Version","external_id":{"arxiv":["2511.21961"]},"arxiv":1,"author":[{"full_name":"Edelsbrunner, Herbert","first_name":"Herbert","id":"3FB178DA-F248-11E8-B48F-1D18A9856A87","orcid":"0000-0002-9823-6833","last_name":"Edelsbrunner"},{"full_name":"Lipiński, Michał","id":"dfffb474-4317-11ee-8f5c-fe3fc95a425e","first_name":"Michał","orcid":"0000-0001-9789-9750","last_name":"Lipiński"},{"first_name":"Marian","full_name":"Mrozek, Marian","last_name":"Mrozek","orcid":"0000-0002-0619-6417"},{"full_name":"Soriano Trigueros, Manuel","id":"15ebd7cf-15bf-11ee-aebd-bb4bb5121ea8","first_name":"Manuel","orcid":"0000-0003-2449-1433","last_name":"Soriano Trigueros"},{"last_name":"Zimin","full_name":"Zimin, Fedor","id":"afd27eda-91c1-11f0-aad8-c6edbec24c04","first_name":"Fedor"}],"intvolume":" 367","project":[{"grant_number":"I02979-N35","call_identifier":"FWF","_id":"2561EBF4-B435-11E9-9278-68D0E5697425","name":"Persistence and stability of geometric complexes"},{"call_identifier":"H2020","grant_number":"101034413","name":"IST-BRIDGE: International postdoctoral program","_id":"fc2ed2f7-9c52-11eb-aca3-c01059dda49c"}],"title":"The depth poset under transpositions in the filter","has_accepted_license":"1","OA_place":"publisher","ddc":["500"],"OA_type":"gold","type":"conference","researchdata_availability":"no","scopus_import":"1","ec_funded":1,"publication":"42nd International Symposium on Computational Geometry","das_tickbox":"0","date_published":"2026-05-27T00:00:00Z","date_created":"2026-07-13T09:56:38Z","oa":1,"corr_author":"1","_id":"22299","publisher":"Schloss Dagstuhl – Leibniz-Zentrum für Informatik","day":"27","article_processing_charge":"Yes","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","status":"public","volume":367,"language":[{"iso":"eng"}],"file_date_updated":"2026-07-14T06:08:05Z","doi":"10.4230/LIPICS.SOCG.2026.41","citation":{"ieee":"H. Edelsbrunner, M. Lipiński, M. Mrozek, M. Soriano Trigueros, and F. Zimin, “The depth poset under transpositions in the filter,” in 42nd International Symposium on Computational Geometry, New Brunswick, NJ, United States, 2026, vol. 367.","apa":"Edelsbrunner, H., Lipiński, M., Mrozek, M., Soriano Trigueros, M., & Zimin, F. (2026). The depth poset under transpositions in the filter. In 42nd International Symposium on Computational Geometry (Vol. 367). New Brunswick, NJ, United States: Schloss Dagstuhl – Leibniz-Zentrum für Informatik. https://doi.org/10.4230/LIPICS.SOCG.2026.41","chicago":"Edelsbrunner, Herbert, Michał Lipiński, Marian Mrozek, Manuel Soriano Trigueros, and Fedor Zimin. “The Depth Poset under Transpositions in the Filter.” In 42nd International Symposium on Computational Geometry, Vol. 367. Schloss Dagstuhl – Leibniz-Zentrum für Informatik, 2026. https://doi.org/10.4230/LIPICS.SOCG.2026.41.","ama":"Edelsbrunner H, Lipiński M, Mrozek M, Soriano Trigueros M, Zimin F. The depth poset under transpositions in the filter. In: 42nd International Symposium on Computational Geometry. Vol 367. Schloss Dagstuhl – Leibniz-Zentrum für Informatik; 2026. doi:10.4230/LIPICS.SOCG.2026.41","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.","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.","mla":"Edelsbrunner, Herbert, et al. “The Depth Poset under Transpositions in the Filter.” 42nd International Symposium on Computational Geometry, vol. 367, 41:1-41:18, Schloss Dagstuhl – Leibniz-Zentrum für Informatik, 2026, doi:10.4230/LIPICS.SOCG.2026.41."},"date_updated":"2026-07-14T06:09:32Z","abstract":[{"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.","lang":"eng"}],"publication_identifier":{"eissn":["1868-8969"],"isbn":["9783959774185"]}},{"conference":{"end_date":"2025-12-17","start_date":"2025-12-15","location":"Tehran, Iran","name":"ISPRS: Conference on Photogrammetry, Remote Sensing and Spatial Information Sciences,"},"tmp":{"image":"/images/cc_by.png","legal_code_url":"https://creativecommons.org/licenses/by/4.0/legalcode","short":"CC BY (4.0)","name":"Creative Commons Attribution 4.0 International Public License (CC-BY 4.0)"},"department":[{"_id":"HeEd"}],"user_id":"2DF688A6-F248-11E8-B48F-1D18A9856A87","issue":"-4/W8-2025","keyword":["Air Traffic simulation","Dynamic Air Traffic Corridors","Origin Destination matrix","Interactive Web GIS","Iran Aviation Network","Spatiotemporal Modelling"],"month":"05","year":"2026","quality_controlled":"1","author":[{"full_name":"Eghbali Mardekheh, Masoumeh","first_name":"Masoumeh","last_name":"Eghbali Mardekheh"},{"full_name":"Argany, Meysam","first_name":"Meysam","last_name":"Argany"},{"id":"2A2BCDC4-CF62-11E9-BE5E-3B1EE6697425","first_name":"Farid","full_name":"Karimipour, Farid","last_name":"Karimipour","orcid":"0000-0001-6746-4174"},{"last_name":"Sedghitabar","first_name":"Seyed Mohammad","full_name":"Sedghitabar, Seyed Mohammad"}],"file":[{"file_size":2697680,"relation":"main_file","success":1,"creator":"dernst","file_id":"22328","access_level":"open_access","date_created":"2026-07-14T05:55:34Z","checksum":"7c088dd179cfee6074a350c95671dbe3","file_name":"2026_ISPRS_EghbaliMardekheh.pdf","content_type":"application/pdf","date_updated":"2026-07-14T05:55:34Z"}],"oa_version":"Published Version","page":"493-500","supplementarymaterial":"no","publication_status":"published","publication":"8th ISPRS Geospatial Conference","date_published":"2026-05-29T00:00:00Z","das_tickbox":"0","type":"conference","scopus_import":"1","researchdata_availability":"no","OA_type":"gold","has_accepted_license":"1","title":"Real time interactive web GIS based modelling of high traffic air corridors in Iran using origin destination matrix analysis","ddc":["500"],"OA_place":"publisher","abstract":[{"text":"Air traffic management is a critical component of aviation, aiming to balance safety, capacity and demand within controlled airspace. This research analyses Iran's domestic air transport network (2018-2021) by developing annual Origin-Destination (OD) impedance matrices based on flight frequency. The methodology quantifies network connectivity, revealing a highly centralized structure dominated by core corridors like Tehran-Mashhad, which carried over 10,500 flights in 2019. The COVID-19 pandemic caused a severe disruption in 2020, with traffic on major routes falling by nearly half, followed by a partial recovery in 2021. Analysis shows core hubs rebounded faster than peripheral airports, widening accessibility gaps. Through origin-destination matrix processing, the system identifies high density air routes and analyses historical trends in airspace utilization. The impedance matrix, validated against data (R²=0.87), successfully maps the intense service on hub links and the high impedance of sparse peripheral routes. Then an interactive Web GIS platform was implemented for spatiotemporal analysis of air traffic density.","lang":"eng"}],"date_updated":"2026-07-14T05:56:30Z","publication_identifier":{"issn":["2194-9050"]},"language":[{"iso":"eng"}],"volume":"X","doi":"10.5194/isprs-annals-x-4-w8-2025-493-2026","citation":{"ieee":"M. Eghbali Mardekheh, M. Argany, F. Karimipour, and S. M. Sedghitabar, “Real time interactive web GIS based modelling of high traffic air corridors in Iran using origin destination matrix analysis,” in 8th ISPRS Geospatial Conference, Tehran, Iran, 2026, vol. X, no. 4/W8-2025, pp. 493–500.","chicago":"Eghbali Mardekheh, Masoumeh, Meysam Argany, Farid Karimipour, and Seyed Mohammad Sedghitabar. “Real Time Interactive Web GIS Based Modelling of High Traffic Air Corridors in Iran Using Origin Destination Matrix Analysis.” In 8th ISPRS Geospatial Conference, X:493–500. Copernicus Publications, 2026. https://doi.org/10.5194/isprs-annals-x-4-w8-2025-493-2026.","apa":"Eghbali Mardekheh, M., Argany, M., Karimipour, F., & Sedghitabar, S. M. (2026). Real time interactive web GIS based modelling of high traffic air corridors in Iran using origin destination matrix analysis. In 8th ISPRS Geospatial Conference (Vol. X, pp. 493–500). Tehran, Iran: Copernicus Publications. https://doi.org/10.5194/isprs-annals-x-4-w8-2025-493-2026","ista":"Eghbali Mardekheh M, Argany M, Karimipour F, Sedghitabar SM. 2026. Real time interactive web GIS based modelling of high traffic air corridors in Iran using origin destination matrix analysis. 8th ISPRS Geospatial Conference. ISPRS: Conference on Photogrammetry, Remote Sensing and Spatial Information Sciences, vol. X, 493–500.","ama":"Eghbali Mardekheh M, Argany M, Karimipour F, Sedghitabar SM. Real time interactive web GIS based modelling of high traffic air corridors in Iran using origin destination matrix analysis. In: 8th ISPRS Geospatial Conference. Vol X. Copernicus Publications; 2026:493-500. doi:10.5194/isprs-annals-x-4-w8-2025-493-2026","short":"M. Eghbali Mardekheh, M. Argany, F. Karimipour, S.M. Sedghitabar, in:, 8th ISPRS Geospatial Conference, Copernicus Publications, 2026, pp. 493–500.","mla":"Eghbali Mardekheh, Masoumeh, et al. “Real Time Interactive Web GIS Based Modelling of High Traffic Air Corridors in Iran Using Origin Destination Matrix Analysis.” 8th ISPRS Geospatial Conference, vol. X, no. 4/W8-2025, Copernicus Publications, 2026, pp. 493–500, doi:10.5194/isprs-annals-x-4-w8-2025-493-2026."},"file_date_updated":"2026-07-14T05:55:34Z","status":"public","acknowledgement":"We sincerely thank the Iranian Airports and Air Navigation\r\nCompany for sharing statistical data on flights from Iranian\r\nairports, separated by origin and destination, for this research.","article_processing_charge":"No","date_created":"2026-07-13T09:51:29Z","oa":1,"publisher":"Copernicus Publications","day":"29","_id":"22298"}]